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⃝charles j byrne] lunar orbiter photographic atla
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Lunar Orbiter Photographic Atlas of theNear Side of the Moon
Charles J. Byrne
Lunar OrbiterPhotographic Atlas ofthe Near Side of theMoon
With 619 Illustrations and a CD-ROM
Charles J. ByrneImage AgainMiddletown, NJUSA
Cover illustration: Earth-based photograph of the full Moon from the “Consolidated Lunar Atlas” onthe Website of the Lunar and Planetary Institute.
British Library Cataloging-in-Publication DataByrne, Charles J., 1935–
Lunar Orbiter photographic atlas of the near side of the Moon1. Lunar Orbiter (Artificial satellite) 2. Moon–Maps 3. Moon–Photographs from spaceI. Title523.3 0223
ISBN 1852338865
Library of Congress Cataloging-in-Publication DataByrne, Charles J., 1935–
Lunar Orbiter photographic atlas of the near side of the Moon : with 619 figures / Charles J. Byrne.
p. cm.Includes bibliographical references and index.ISBN 1-85233-886-5 (acid-free paper)1. Moon–Maps. 2. Moon–Photographs from space. 3. Moon–Remote-sensing images.
4. Lunar Orbiter (Artificial satellite) I. Title.G1000.3.B9 2005523.3 022 3–dc22 2004045006
ISBN 1-85233-886-5 Printed on acid-free paper.
© 2005 Springer-Verlag London LimitedApart from any fair dealing for the purposes of research or private study, or criticism, or review, aspermitted under the Copyright, Designs and Patents Act 1988, this publication may only be repro-duced, stored or transmitted, in any form or by any means, with the prior permission in writing of thepublishers, or in the case of reprographic reproduction in accordance with the terms of licenses issuedby the Copyright Licensing Agency. Enquiries concerning reproduction outside those terms should besent to the publishers.The use of registered names, trademarks, etc, in this publication does not imply, even in the absenceof a specific statement, that such names are exempt from the relevant laws and regulations and there-fore free for general use.
Printed in Singapore. (EXP/EVB)
9 8 7 6 5 4 3 2 1 SPIN 10978726
Springer Science+Business Mediaspringeronline.com
Additional material to this book can be downloaded from http://extras.springer.com.
Preface
The Moon is Earth’s nearest neighbor. Since the dawn of intelligence, our eyeshave seen the Moon, puzzling over its shady figures, its phases, its motions in thesky, and its relation to tides. Even the smallest telescopes resolve the shadowsinto a heavily cratered surface, stimulating the imagination. Each advance of theastronomer’s art has revealed new insights into the nature of the lunar surface,until curiosity and competition led the American and Russian space programs tosend orbital cameras, robotic landers and rovers, and the Apollo astronaut explo-ration teams to the Moon.
The Lunar Orbiter program, a series of five photographic spacecraft launchedin 1966 and 1967, was motivated by the need to find and certify safe and interest-ing landing sites for the Apollo spacecraft. When the Lunar Orbiter program wasstarted (1964), no spacecraft had landed on the Moon, but the Apollo programwas committed to safely land the Lunar Module, with two astronauts on board. Atthe time, I was working in the lunar environment group of Bellcomm, Inc. AT&Testablished Bellcomm at the request of the National Aeronautics and SpaceAdministration (NASA) to support the Apollo project headquarters group. Ourresponsibility included the challenging assignment of finding a safe landing sitefor a vehicle about the size of a helicopter, with a half-meter (0.5-m, 20-inch)ground clearance and limited ability to land on a slope. Of course, we had verylittle information about the lunar surface at such scales. There was some informa-tion from lunar photometry and radar scatter measurements, but there werestrong uncertainties about what aspects of the surface were being measured; inparticular, the soil strength was an unknown. Speculation raised possibilities ofdust floated by static electricity or fragile glasslike lava.
The requirements for Lunar Orbiter were established to achieve the best possi-ble resolution within the state of the art and to obtain imagery of that resolutionover a significant percentage of the area available for Apollo landings. TargetedApollo landing sites had to be as smooth as possible over a large enough area toaccommodate the down-range and cross-range navigation errors, determined bythe tracking, and control uncertainties associated with factors such as the largelyunknown gravity anomalies.
NASA’s Langley Research Center was chosen to manage the Lunar Orbiterprogram. I had the pleasure of drafting the specifications and participating in theselection of contractors. The resulting spacecraft and camera designs of BoeingAircraft and Eastman Kodak (respectively) were capable of enormous data collec-tion capacity, even in today’s terms. All together, about 1000 pairs of medium-and high-resolution exposures were made during the five missions. The negativeswere developed in orbit, scanned, and transmitted to photographic and magnetictape recorders in the three stations of the Deep Space Network operated by the JetPropulsion Laboratory (JPL) in California, Spain, and Australia. Each exposureresults in one medium-resolution frame and one long high-resolution frame,usually presented as three subframes.
Although five missions were planned to compensate for possible failures, eitherof spacecraft or rejection of initial target sites, the survey for early Apollo landingsites was completed in the first three missions. As a result, the fourth mission wasused for a comprehensive survey of the near side of the Moon; these are the pho-tographs that are the primary contents of this book. The fifth mission examinedmany scientific sites at very high resolution, surveyed a few additional landingsites for later Apollo missions, and improved coverage of the far side of theMoon. Since the Lunar Orbiter missions returned their extensive photographic
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coverage of Earth’s Moon, the pictures have been the basic reference for high-resolution topographic information. The most often referenced images are thecomprehensive set of about 600 images selected by Bowker (1971) and the nearside set of about 450 images selected by Whitaker (1970).
Following the thorough coverage of the Lunar Orbiter program, the ApolloCommand and Service Module, in orbit during landing missions, provided addi-tional coverage of the equatorial regions with its mapping and panoramiccameras. The Clementine mission provided a comprehensive survey of altitude,albedo (intrinsic brightness), and multispectral data in 1994. Lunar Prospectorprovided gamma ray spectroscopy in 1998. The data from these spacecraft hasadded insight into the mineral composition of nearly all the lunar surface,extending surveys of the equatorial region by Apollo. The interpretation of theremote sensing data has been supported by ground truth from analysis of lunarrocks and soil returned by Apollo and Luna missions. Despite the advances ofthese later missions, the Lunar Orbiter photographs, taken at a low sun angle,remain the primary source of topographic images and are used extensively incurrent scientific presentations, papers, and books.
At the time of Lunar Orbiter’s design, image scanning technology was muchless advanced than it is today. The methods used resulted in artifacts in theimages that distract a viewer. Scanning and transmission limitations required thesubframes to be reassembled from 20 to 30 framelets of 35-millimeter film. Thereare fine bright lines running across each subframe between the framelets, andthere are brightness variations from the spacecraft’s scanner that appear asstreaks within the framelets. The artifacts are particularly distracting when theimages are printed at high contrast to show subtle topographic features andbrightness variations. Lunar scientists have become used to these artifacts, butthey detract from their value to students and casual observers.
Since the first photos were received, I have wanted to clean up the scanningartifacts, but at the time it would have been very expensive. The priorities were toexamine the photos and start using them, rather than to improve their visualquality. Advances in the art of computation and the capacity of modern comput-ers have enabled processing of the photos to remove nearly all the scanning arti-facts, resulting in clear images that are much easier to view. Drawing on anunderstanding of the nature of the artifacts, I have written programs thatmeasure and compensate for the systematic artifacts and in addition applyfiltering techniques similar to those published by Lisa Gaddis of the United StatesGeological Survey (USGS) (Gaddis, 2001).
Lunar Orbiter photography has been archived as hard copy photographs, eachabout 60 centimeters (cm) (about 2 feet) wide, at each NASA Regional PlanetaryImage Facility, including one at the Lunar and Planetary Institute (LPI) inHouston, Texas. LPI has digitized this important archival source and publishedthe images in the Digital Lunar Orbiter Photographic Atlas of the Moon on theLPI web site (www.lpi.usra.edu/research/lunar_orbiter/). Further, the LPI staffhas added annotations to the photos, clearly outlining many of the features andlabeling them with their internationally recognized names.
A team led by Jeff Gillis carried out this important work; Jeff was supported byWashington University at St. Louis and LPI. He is currently with the University ofHawaii. LPI technical and administrative support was provided by Michael S.O’Dell, Debra Rueb, Mary Ann Hager, and James A. Cowan with assistance fromSandra Cherry, Mary Cloud, Renee Dotson, Kin Leung, Jackie Lyon, Mary Noel,Barbara Parnell, and Heather Scott. The selection of photos on the LPI DigitalArchive is that selected for Lunar Orbiter Photographic Atlas of the Moon byBowker and Hughes (see the reference section for details).
The annotated photos in this atlas provide full coverage of the near side,including nearly all the features whose names have been approved by theInternational Astronomical Union (IAU). All the high- and medium-resolutionphotos of Lunar Orbiter 4 (except for a few that were found unacceptable forBowker, 1971) have been cleaned and are in the enclosed compact disc. Most ofthese, selected for nonredundancy and interest of features, are printed along withthe annotated photos. All the photos (before processing by the author) are cour-tesy of NASA and LPI.
Photos with annotated overlays label the major features within each of thephotos, including the landing sites of manned and unmanned spacecraft. These
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overlays were extracted digitally from those published by LPI. I added additionalannotations to provide latitude, longitude, and scale information and also to bringthe set of features up to date with the Gazetteer of Planetary Nomenclature, the list maintained for the IAU by the United States Geological Survey (USGS)Astrogeology Program. Notes with each photo point out salient aspects of the fea-tures. The combination of cleaned photos, labeled features, and notes are intendedto serve as powerful aids to learning the geography and geology of the near side ofthe Moon as well as valuable reference material.
Throughout the project of cleaning the photos and writing this book, helpfulsuggestions and comments were made by Jeff Gillis, Mary Ann Hager, PaulSpudis, Lisa Gaddis, Debbie Martin, Michael Martin, Ewen Whitaker, and BradJolliff.
My dear wife Mary worked long and patiently as system administrator, pictureprocessor, and reviewer.
Special gratitude goes to Don Wilhelms, USGS Astrogeology (retired), whosebooks have been major sources and who was kind enough to review this bookand set me straight on lunar geology.
Charles J. Byrne
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Table of Contents
1. Overview of the Atlas ........................................................................................ 11.1. Content...................................................................................................... 11.2. How to Use This Atlas ............................................................................ 11.3. Large-Scale Maps .................................................................................... 2
2. Lunar Orbiter Mission 4.................................................................................... 52.1. The Mission .............................................................................................. 52.2. Mission Design ........................................................................................ 52.3. The Cameras ............................................................................................ 52.4. The Film .................................................................................................... 52.5. Scanning and Reconstruction ................................................................ 72.6. Scanning Artifacts.................................................................................... 72.7. Cleaning the Images ................................................................................ 7
3. Overview of the Near Side of the Moon .......................................................... 83.1. Origin of the Moon .................................................................................. 83.2. The Near Side Versus the Far Side ........................................................ 83.3. Mare and Highlands ................................................................................ 83.4. Basins ........................................................................................................ 93.5. Landmarks for Geography ...................................................................... 93.6. Descriptions of Landmark Regions ........................................................ 9
Orientale Basin Region .......................................................................... 10Humorum Basin Region........................................................................ 10Imbrium Basin Region .......................................................................... 10Nectaris Basin Region............................................................................ 10Serenitatis Basin Region........................................................................ 10Eastern Basins Region .......................................................................... 10North Polar Region ................................................................................ 10South Polar Region ................................................................................ 10
3.7. The Ages of the Lunar Features ............................................................ 10Estimating Ages...................................................................................... 10Named Age Ranges ................................................................................ 10
4. Organization of the Photos ............................................................................ 114.1. Grouping by Landmark Regions .......................................................... 114.2. Order: West to East and South to North .............................................. 114.3. Clean and Annotated Images ................................................................ 114.4. High-Resolution Frames and Subframes ............................................ 114.5. Discussion Notes.................................................................................... 114.6. Enclosed Compact Disc (CD)................................................................ 11
5. Orientale Basin Region .................................................................................. 135.1. Overview ................................................................................................ 13
Orientale, the Archetype Multi-Ringed Basin .................................... 13Crater Morphology as a Function of Size ............................................ 14Surroundings of the Orientale Basin.................................................... 14
5.2. High-Resolution Images........................................................................ 14
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6. Humorum Basin Region ................................................................................ 556.1. Overview ................................................................................................ 55
Basins, Maria, and Highlands .............................................................. 55Apollo Landings .................................................................................... 56
6.2. High-Resolution Images........................................................................ 56
7. Imbrium Basin Region.................................................................................. 1007.1. Overview .............................................................................................. 100
The Imbrium Basin.............................................................................. 100Oceanus Procellarum .......................................................................... 100Fra Mauro Formation .......................................................................... 101
7.2. High-Resolution Images...................................................................... 102
8. Nectaris Basin Region .................................................................................. 1558.1. Overview .............................................................................................. 155
Basins, Maria, and Highlands ............................................................ 155Apollo Landing .................................................................................... 156
8.2. High-Resolution Images...................................................................... 156
9. Serenitatis Basin Region .............................................................................. 2009.1. Overview .............................................................................................. 200
Serenitatis Basin .................................................................................. 201Apollo Landings .................................................................................. 201
9.2. High-Resolution Images...................................................................... 201
10. Eastern Basins Region .................................................................................. 24410.1. Overview .............................................................................................. 244
The Crisium Basin................................................................................ 244The Australe Basin .............................................................................. 244The Smythii Basin ................................................................................ 244
10.2. High-Resolution Images...................................................................... 244
11. North Polar Region ...................................................................................... 26311.1. Overview .............................................................................................. 263
Mare Frigoris ........................................................................................ 263The Humboldtianum Basin ................................................................ 264The North Polar Highlands ................................................................ 264The North Pole .................................................................................... 264
11.2. High-Resolution Images...................................................................... 264
12. South Polar Region........................................................................................ 29112.1. Overview .............................................................................................. 291
Western Sector of the South Polar Region ........................................ 291Central Sector of the South Polar Region .......................................... 291Eastern Sector of the South Polar Region .......................................... 291The South Pole .................................................................................... 291
12.2. High-Resolution Images...................................................................... 292
Glossary .................................................................................................................. 323
References .............................................................................................................. 324
General Index ........................................................................................................ 325
IAU Named Features .............................................................................................. 327
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1.1. ContentThe atlas presents full coverage of the nearside of the Moonwith a series of photos all taken from orbit by LunarOrbiter 4, with a nearly vertical viewpoint and sunlight at approximately 20 degrees (°) from the horizontal.Extensive computer processing has been used to improvethe quality of these photos. Features whose names havebeen recognized by the International Astronomical Union(IAU) have been identified on an overlay and listed in theindex of features. Notes on each page discuss the geologicprocesses that formed the features and controlled theirinteractions.
The high-resolution photos of this book typically coverabout 200 by 300 kilometers (km). Approximately 350 ofthese photos cover the nearside of the Moon (with someoverlap). The photos are grouped into chapters that eachpresent one of the regions of the Moon. Six of these regionshave been selected to focus on basins of the Moon, thelargest coherent lunar features. Chapters on the North andSouth Polar Regions complete the coverage of the nearside.Figure 1.1 identifies these regions against the background ofa photograph of the full Moon. Figure 1.2 identifies theregions of the central latitudes against a Mercator projectionmap, Figure 1.3 shows the North Polar Region, and Figure 1.4shows the South Polar Region.
An introduction to each chapter surveys the relevantregion, using wide coverage photos. An overview of thegeology of each region and its features introduces the spe-cialized vocabulary needed to describe lunar processes. Eachchapter provides a guide to the high-resolution photos as anaid to relating them to the wide-angle views and to the Moonas a whole. Each high-resolution photo is marked with thelatitude and longitude as a further guide to locating featureson the maps of Figures 1.2 to 1.4.
An enclosed compact disc (CD) contains all the cleaned-up photographs of Lunar Orbiter Mission 4, with an indexlisting all the officially named lunar features shown in thisbook. These photos, when viewed on a monitor with appro-priate magnification, show more detail than can be seen inthe printed pictures.
1.2. How to Use This AtlasA telescopic observer or photographer of the Moon, workingat high resolution, views a small area under lighting thatvaries both with time and with position. The angle of view isnearly vertical at the center of the Moon as we see it, but se-verely foreshortened near the limb (edge of the visibleMoon). One might ask: What features are in the area? Howdo they relate to the rest of the Moon? How would the featurelook relative to others if seen at similar lighting conditionsand viewing angles? What is the current understanding of theprocesses that formed these features?
The following is a summary of how an interested observermight answer these questions, with the aid of this atlas:
1. Relate a feature viewed in a telescope, photo, or electronicimage to its position on the full Moon photo of Figure 1.1.
2. Note the region in which it appears; consult the Table ofContents to find the appropriate chapter.
3. Determine the approximate latitude and longitude of thefeature from the maps in Figures 1.2 and 1.3. These coor-dinates can be used with the chart in the beginning of therelevant chapter to narrow the search for the correspond-ing photo.
4. Once the photo or photos that cover the area of interest arelocated, annotations will identify the name of the feature (ifit has a formal name) and the names of nearby features.
5. The notes on the page or pages describe something of theprocesses that took place to form the feature or itssurroundings.
6. The reference section refers to more detailed descriptionsin the literature for many of the photos.
The process described above can be followed in reverse. Ifan observer is interested in a feature found by browsing thebook, the latitude and longitude on the annotated photo canbe used to locate the feature relative to larger features on themaps of Figures 1.2 to 1.4. Then an observer can feature-walka telescopic field of view to the appropriate part of the Moon,just as one star-walks a field of view from one star group toanother to bring dim deep-sky objects into sight.
Chapter 1
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Of course, these are only examples of ways this atlas can beuseful. The overview chapters and the introductions to theregional chapters can be read as a book summarizing thelargest features on the Moon and their relationships. Anotherway to use the atlas is to browse it. The notes need not be readsequentially. The atlas can also be used as a reference book.The feature index in the CD lists near side features with IAUnames and directs the reader to a relevant page. The SourceNotes section of the enclosed CD often identifies discussion offeatures in books of comprehensive coverage of the Moon,which refer in turn to additional research publications.
1.3. Large-Scale MapsFigure 1.1 is the full Moon, photographed from Earth. A fewoutstanding features are identified as an aid to orientationwhen looking at the Moon. The dark maria (low-lying areasflooded by lava) form the patterns variously known as theman in the Moon, the rabbit, and so on.
The map in Figure 1.2 is based on data from theClementine spacecraft. Clementine scanned the Moon from apolar orbit whose plane was aligned with the sun, so that thelunar surface shows its inherent brightness (called albedo),
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Figure 1.1. These regions of the Moon establish the scope of the corresponding chapters of this atlas. The base photo is from the Consolidated Lunar Atlas(LPI Web site).
2
as it appears from Earth when the Moon is full. This mapshows features of the eastern and western limbs more clearlythan they can be seen from Earth.
Figures 1.3 and 1.4 are polar projections, mosaics ofClementine scans of the polar regions. Clementine’s bright-
ness sensor continued to look almost directly down at thesurface as the spacecraft passed nearly over the poles, butthese maps show the topography of the features rather thanthe albedo because the sun is always low near the poles.Under such low illumination, crater walls throw shadows.
90 W 60 W
60 S
30 S
0 N/S
30 N
60 N
Mare Humorum
Mare Imbrium
MareOrientale
MareSerenitatis Mare
Crisium MareMarginis
MareSmythii
MareFecunditatis
Mare Nectaris
MareAustrale
30 W 30 E 60 E 90 E0 E/W
Lunar Longitude
Luna
r Lat
itude
Figure 1.2. Map of the near side of the Moon, based on Clementine brightness data (NRL Web site). Region names are the same as in Figure 1.1; the north-south regional boundaries are curved to follow the Lunar Orbiter 4 photos, planned for uniformity of the sun angle. Mare Orientale and the features on theeastern limb are visible from Earth only at times of favorable libration and then are much foreshortened. Note that features in the polar regions are stretchedhorizontally in this Mercator projection.
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Figure 1.4. South Polar Region; near side is at top. This circumpolar projection is based on Clementine brightness data (USGS Web site). The boundary ofthe South Polar Region (not shown) is at 55° south latitude.
Figure 1.3. North Polar Region; near side is at bottom. This circumpolar projection is based on Clementine brightness data (USGS Web site). The boundaryof the North Polar Region (not shown) is at 55° north latitude.
2.1. The MissionLunar Orbiter Mission 4 produced most of the photos in thisbook. This scientific mission was planned to systematicallycover the nearside of the Moon. Extensive 1-meter (1-m)photography had been taken of the candidate Lunar Orbiterlanding sites by missions 1 through 3, and the geologistswanted moderate-resolution photography (about 50 m) of somany large features on the nearside that a systematic surveymission was appropriate.
2.2. Mission DesignThe layout of exposures from orbit depends on many aspectsof the mission design. The spacecraft was placed in a high-in-clination (nearly polar) orbit to provide full coverage of thenearside of the Moon. The orbit was such that the incidenceangle of sunlight was about 20° (east to west; morning sun)throughout the photographic mission. While the 2-weekphotographic mission continued, the Moon revolved underthe orbit with approximately uniform sun angle from theeast limb to the west limb, presenting a new surface underthe spacecraft at each orbital pass. The period of the orbit,the altitude of the spacecraft, and the width of the high-resolution image were coordinated so that high-resolutionimages taken on successive orbits overlapped by about 10%at the lunar equator, with more overlap at high latitudes.Successive high-resolution photographs taken on the sameorbit were timed to overlap between about 10% as well. Theoverlap of photos avoids gaps in coverage, assists the con-struction of mosaics, and provides partial stereo coverage.
Most of the photos were taken vertically, except for thosenear the poles, where this could not be done because of thenature of the chosen orbit. The vertical photography mini-mizes foreshortening of the features to aid interpretation ofthe images.
Although all five of the Lunar Orbiters successfully pro-vided extensive new photographic coverage, there were oftenproblems, and Mission 4 was no exception. In this case, theproblem involved erratic operation of the thermal door, alens cap intended to protect the cameras from the cold ofdeep space when they were not actually making an exposure.Early in the mission, the optics chilled to the dew point ofthe moisture within the cameras and became fogged. The
Boeing operations team and the science team designed awork-around. The thermal door was left open, but the space-craft was oriented toward the sunlit part of the Moon so thatthe optics would be kept warm as much as possible.
Many photos of the eastern nearside were lost while theproblem was analyzed and resolved, but additional expo-sures were made at the end of the mission to replace most ofthe missed coverage. These photos were taken on the “backside” of the orbit, with the spacecraft near apolune. As a con-sequence they are at lower resolution than the other photosand lighting is reversed, coming from west to east.
A schematic of the layout of the high-resolution imagesacross the nearside of the Moon is shown in Table 2.1.
2.3. The CamerasThe Lunar Orbiter photography system consisted of twocameras, one with a short focal length and wide field of view(called the “medium-resolution camera”) and one with along focal length and a narrower field of view (called the“high-resolution camera”). The high-resolution field ofview was centered within the field of view of the medium-resolution camera and was more than three times longerthan it was wide.
The image motion compensation was provided by a feed-back loop based on a circular scan of part of the high-resolu-tion image. This mechanism, which had failed on LunarOrbiter Mission 1 but worked flawlessly on all the later mis-sions, moved the film platen in two dimensions to track theimage.
Six fiducial marks (“sawteeth”) for mapping were pro-vided at the edge of the field of view. These marks have beentrimmed from the images in this book.
2.4. The FilmThe negative film was a fine-grained low-contrast 70-millimeter (70-mm) black-and-white standard Kodakproduct. The fine grain assured low graininess at high resolu-tion. The low contrast (about 1 to 1) was selected to tolerateunknown variations in the brightness of the lunar surface athigh resolution. A gray scale, resolution charts, and reticulemarks (small crosses, barely visible on the images in this
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Chapter 2
Lunar Orbiter Mission 4
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le 2
.1.L
ayou
t of
the
hig
h-re
solu
tion
pho
tos
from
Lun
ar O
rbit
er M
issi
on 4
. Num
bers
are
exp
osur
e nu
mbe
rs: t
he fu
ll ti
tle
of e
ach
high
-res
olut
ion
subf
ram
e is
LO
4-X
XX
H1,
-H
2, o
r -H
3, w
here
XX
X is
the
Pho
toN
umbe
r sh
own
abov
e. S
ee C
hapt
er 4
for
an e
xpla
nati
on o
f the
sub
fram
e su
ffixe
s H
1, H
2, a
nd H
3. P
hoto
s w
hose
num
bers
are
und
erlin
ed w
ere
take
n at
the
end
of th
e m
issi
on, a
t hig
her
alti
tude
, and
wit
h re
vers
ed s
unlig
ht(f
rom
the
wes
t). I
mag
es s
how
n ne
xt to
eac
h ot
her
in th
is ta
ble,
eit
her
vert
ical
ly o
r ho
rizo
ntal
ly, o
verl
ap. A
ll th
ese
phot
os a
re in
clud
ed in
the
encl
osed
CD
, but
som
e re
dund
ant p
hoto
s ha
ve n
ot b
een
prin
ted
in th
is b
ook.
Ata
ble
in e
ach
chap
ter
show
s th
e hi
gh-r
esol
utio
n ph
otos
for
that
reg
ion
and
indi
cate
s w
hich
one
s ar
e pr
inte
d.
Latit
ude
Phot
o N
umbe
rRa
nge
56 N
–90
N19
017
616
415
214
012
811
610
409
208
006
805
6
27 N
–56
N18
918
317
517
016
315
815
114
513
913
412
712
211
511
010
309
809
108
607
907
406
706
205
517
716
502
4
0–27
N19
616
818
217
416
916
215
715
014
413
813
312
612
111
410
910
209
709
008
507
807
306
606
105
418
101
8
0–27
S19
518
718
117
316
816
115
614
914
313
713
212
512
011
310
810
109
608
908
407
707
206
506
005
304
603
902
7
27 S
–56
S19
418
618
017
216
716
015
514
814
213
613
112
411
911
210
710
009
508
808
307
607
106
405
905
218
4 ,
038
178
009
045
56 S
–90
S19
317
916
615
413
011
810
609
408
207
005
804
400
5
Long
itude
95
W89
W82
W76
W68
W62
W56
W49
W41
W35
W30
W23
W16
W10
W3W
4E10
E16
E24
E30
E38
E43
E49
E57
E63
E70
E83
E90
Eat
Equ
ator
book) were exposed on the negative to assist in reconstruc-tion and calibration of the images after scanning.
The film was developed in the spacecraft by the KodakBimat process. A second 70-mm film, its thick emulsion satu-rated with developing fluid, was pressed against the exposednegative by rollers. The two-film sandwich was stored in abuffer of rollers until development was complete and thenthey were separated.
Unfortunately, the Bimat process was susceptible to cer-tain flaws. Small bubbles sometimes interposed between thenegative and developer film, leaving various patterns on thenegative. Also, rollers sometimes left bars across the filmwhere the film was paused. These defects are easily distin-guished from lunar features but unfortunately degrade aminority of the images.
2.5. Scanning andReconstructionThe developed film was scanned by the available technologyof the time; charge-controlled devices (CCDs) were still wellin the future. Instead, a cathode ray tube (CRT) was used toprovide a single scan line. Of course, this scan line couldprovide only the equivalent of about 800 pixels because oflimitations on the phosphor grain and focus of the electronbeam. This short (about 4 mm) scan line was aligned withthe long dimension of the film. A mirror directed it acrossthe 70-mm width of the film. A photocell detected variationsin brightness as a measure of the density of the developednegative. After the width of the film was scanned, the filmwas advanced by a little less than the width of the scan line,providing overlap between scans to avoid gaps.
On the ground, the recorded signal was received at a DeepSpace Network (DSN) site in California, Spain, or Australia,operated by the Jet Propulsion Laboratory (JPL). A CRT inthe Kodak Ground Recording Equipment (GRE) transformedthe signal into an image on 35-mm film. A segment of thisfilm (called a framelet) represented a scan of the mirroracross the 70-mm film in the spacecraft. There were twoGREs, backed up by two Ampex video tape recorders (theoriginal rotating head recorders) at each DSN site.
Once the 35-mm framelets were developed, they weretrimmed by automatic machines and assembled on a lighttable. This was done at JPL (during the mission), LangleyResearch Center, and the Army Mapping Service. The assem-
bled framelets were limited to about 60 centimeters (cm), 24 inches, in length; this was sufficient to fully reconstructthe medium-resolution frames, but the long high-resolutionframes were reconstructed as a set of three subframes.Contact prints were made from these reconstructed framesand subframes; these are the primary records of the photos.Second-generation images at the same scale are stored atNASA Regional Planetary Image Facilities around the world.
The Army Mapping Service often used the tape recordersto adjust the contrast and brightness of the surface. Typicalimages are at a contrast of about 3 to 1 relative to the bright-ness variations of the lunar surface. This contrast exagger-ates the brightness variation of topography, compressing thevariations in the brightest and darkest parts of an image, butalso amplifies the inherent brightness variation of rays andejecta blankets from craters.
2.6. Scanning ArtifactsThe complex deconstruction and reconstruction processes,involving multiple electrical, mechanical, optical, photo-graphic, and manual processes, introduced several types ofscanning artifacts. Thin bright lines, leaks from the lighttable between framelets, appear in most reconstructedframes and subframes. Sometimes negative framelets wereassembled on the light tables, so these lines are dark on thepositive prints. Variations in sensitivity of the phosphors onthe two CRTs used in the process (one in the spacecraft andone on the ground) and possibly variations in the sensitivityof the rotating heads of the tape recorder cause systematicbrightness variations in the series of framelets. This effect,which is quite distracting, is sometimes called the “venetianblind effect” because it appears as if the image has beenprojected on a set of venetian blinds.
2.7. Cleaning the ImagesA computer program written by the author specifically forthis purpose has cleaned the photographs in this book.Appendix A, in the enclosed CD, describes this process indetail. As a result, residual scanning artifacts are only occa-sionally visible in the printed photos. However, artifactsassociated with the development process in the spacecraftremain.
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3.1. Origin of the MoonTo understand these photos, one must understand the Moon,its geography, and the factors that have influenced its nearside surface. The origin of the Moon was a matter of vigorousdebate until about 12 years after the last Apollo mission. In1984, after many years of analysis of the 300 kilograms (kg),800 pounds, of rocks and soil returned by Apollo and Lunamissions, a consensus was struck that has lasted for the sub-sequent 20 years. The following narrative retells this consen-sus origin story, without attempting to review the debate ofalternative theories. The curious reader is encouraged toreview the references.
As unlikely as it seems, another planet perhaps about thesize of Mars and formed in the general orbital vicinity ofMars had its orbit perturbed by some unknown event andstruck the early Earth a glancing blow. Just as a small carabsorbs much of the energy of an impact with a large truck,the smaller planet, known as Theia, was partly vaporized,partly melted, and largely pulverized and thrown into space.Some of Theia escaped from Earth or fell to Earth, but mostof it ended up in an orbit near Earth. Modeling suggests thatmuch of the core of Theia, relatively dense, was pulled intoEarth and joined Earth’s core.
The pulverized and molten orbital components in near-Earth orbit (perhaps about four Earth radii according to thecomputer simulations) coalesced. As a result, the resultingbody was heated by gravitational energy, supplemented byradioactive energy, and largely melted into a deep magmaocean. Part of Theia had become the Moon.
The strong tidal forces generated by the orbital proximityof these two bodies caused a loss of energy in the total systemand a transfer of angular momentum between them. TheMoon’s rotation relative to its revolution about Earthstopped, so that the near side of the Moon always faces Earth(synchronism). The Moon’s orbital radius increased, absorb-ing some of the angular momentum of the early Earth; thatchange slowed Earth’s rotation to its current 24-hour period.
Most of these events occurred within the first 500 millionyears after the Earth had itself coalesced and took place in arelatively short interval, perhaps 100 million years (the coa-lescence of the Moon could have taken place within weeksafter the impact). Of course, the chaotic impact would havethrown material into many orbits, some of which may havetaken very much longer to impact the Moon. The heavilycratered surface reflects the arrival of many such delayed im-
pactors as well as new arrivals from the solar system after theouter surface had cooled and become solid. The rate ofarrival of these later impactors is a matter of intense interest.There is some evidence of a quiet period followed after atime by a brief period of a high rate of arrival, sometimescalled the cataclysm to suggest a major chaotic event in theSolar System.
As a result of this history, our Moon is somewhat unusualin the solar system. It contains much the same chemical ele-ments as the other rocky planets, but its crust contains a dis-tinctly different quantitative distribution of those elements.The mineralogy is often familiar to geologists from theirterrestrial experience, even to the point of the relevance ofan extensive descriptive vocabulary. But the Moon is (to ourcurrent knowledge) unique in having experienced two dis-tinct melting phases, one when Theia was formed as a planetand one when the Moon was formed from a part of Theia’sdebris. Each melting phase resulted in differentiation of theminerals, as heavy material sank and light material rose in two different gravity fields and two different thermaldomains. A set of elements called KREEP that is concen-trated when massive quantities of material are melted andsolidified are unusually abundant in some maria. Eruptingmagma carried the doubly concentrated material to thesurface.
3.2. The Near Side Versus theFar SideThe synchronization of the Moon’s rotation with its revolu-tion in the intense early tidal environment established that thenear side would always face Earth and be the visible side(visible to humanity before the mid-twentieth century, that is).
Measurements of the Moon’s gravitational field have es-tablished that the depth of the crust is less on the near sidethan on the far side. This implies that, for a given size of im-pactor or strength of internal processes, penetration of thecrust is more likely on the near side.
3.3. Mare and HighlandsThe Moon exhibits significant differences between the nearside and near side. In particular, much more mare material is
Chapter 3
Overview of the Near Side of the Moon
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found on the near side. Mare material is the relatively darkmaterial visible on the face of the Moon, contrasting with themore reflective highlands. It is made of relatively heavy min-erals that have risen from the mantle of the Moon, below thecrust. How can we explain this paradox of the rise of heavymaterials through light materials? The answer lies in the de-crease of density that accompanies heating. The materialbecomes lighter than crust because it is hotter. When itbecomes exposed, it quickly cools and is locked in place bythe rigidity of a surface exposed to the cold of deep spacehalf the time. The association of most mare material withpositive gravity anomalies called mascons (an abbreviationof “mass concentrations”) also reveals their high density.Both remote sensing and analysis of lunar rock and soilsamples returned to Earth have established that the materialsof the maria are heavier than highland materials because oftheir higher proportion of iron and magnesium.
Historically, the distinction between mare materials and themore pristine highland materials (so called because they are infact higher than mare, but also resemble terrestrial highlandsin their relatively rugged topography) has been very impor-tant, because elementary observation distinguishes the dark,flat mare from the relatively bright, rugged, highlands.
3.4. BasinsAs understanding grew, it no longer appeared that maria arefundamental to the structure of the lunar surface. Rather, itseems that mare regions are secondary to the formation oflarge basins by impactors that are large enough to compro-mise the integrity of the lunar crust. Such basins allow heavy,dark minerals to rise through the fractured crust from thehotter upper mantle below the crust. The basin associatedwith a mare region can be much larger and has a much moreextensive effect on lunar topography. Typically, only the inte-rior of the depression formed by the basin impactor floods(or partly floods) with mare material. However, depositsejected from the basin can extend for a distance that is a mul-tiple of the crater radius. Such basin ejecta blankets cover orpartially cover much more area than the central depression.
Basins that have been flooded with lava to form a mare arenamed for the mare they contain (the Orientale Basin isnamed for Mare Orientale). Basins that lack mare fill arenamed for two craters that happen to be superposed on thebasin (the Schiller-Zucchius Basin).
Because basins are more fundamental than their includedmaria, this introductory section emphasizes basins as land-marks for the geography of the Moon.
3.5. Landmarks forGeographyStrictly speaking, perhaps we should say selenography orlunography (writing about the Moon) instead of geography(writing about the Earth), but the term geography seems tobe more evocative of what we mean. Geography is notgeology: it refers to landforms and their relation, withoutemphasis on the mineralogy or the formation process of thelandforms. It is difficult to grasp a good mental image of the
major features of the Moon in terms of their global distribu-tion and relationships. There is no equivalent of the organi-zation of terrestrial geography in terms of continents andoceans that are so useful in establishing a mental and visualimage of Earth.
This section introduces a high-level list of eight regions,centered on interesting, memorable focal points. They arechosen for broad distribution, to ensure roughly uniformcoverage of the lunar near side. Each region is sufficientlysmall to support photographic and other images with rea-sonable distortion. The proposed regions, and the latitudeand longitude of their focal points, are shown in Table 3.1.
Basins were chosen as many of the focal points becausethey are major modifiers of the surface geology, not onlythrough their central rings and maria but also through theirejecta blankets. Specific basins were chosen as much for uni-formity of spacing around the lunar globe as for size or inter-est. In addition to basins, the North and South Polar Regionswere included because of the special significance of the shad-owed craters in those regions and also because the photo-graphic quality is quite different.
3.6. Descriptions of LandmarkRegionsThe following sections summarize the characteristics andprominent features of each region. Only enough descriptionis included to differentiate the regions from each other; thesedescriptions are not intended to be comprehensive or todiscuss the geology or stratigraphy of the regions in detail.No attempt is made to establish precise boundaries betweenthe regions: that would be like attempting a precise boundarybetween the Atlantic and Arctic Oceans. These regions are
Region Latitude Longitude
Orientale Basin Region (includes Grimaldi Basin) 19° S 95° W
Humorum Basin Region (includes Nubium Basin) 24° S 39.5° W
Imbrium Basin Region (includes Oceanus Procellarum) 35° N 17° W
Nectaris Basin Region (includes Tranquillitatis and Fecunditatis Basins and nearby highlands) 16° S 34° E
Serenitatis Basin Region (includes the Crisium Basin and nearby highlands) 17.5° N 58.5° E
Eastern Basins Region (the Smythii Basin, the Humboldtianum Basin, the Australe Basin, and intervening highlands) 2° S 87° E
North Polar Region (North Pole) 90° N NA
South Polar Region (South Pole) 90° S NA
Table 3.1. Landmarks for the regions of the Moon and their coordinates.Landmarks are in bold print. Note that the center of the Orientale Basin isactually around the western limb; it is included because much of the basinand its ejecta are on the near side.
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sproposed to serve as a method to organize imagery, an alter-native to latitude and longitude, and no representation ismade that they are of fundamental geologic or cartographicsignificance.
Orientale Basin RegionThe Orientale Basin, with its central mare and multiple rings,has been called the archetype of basins because it is bothlarge and relatively recent. Consequently, its structure is veryclear. The region includes the smaller Grimaldi Basin andcraters Schickard and Bailly.
Humorum Basin RegionThe Humorum Basin region includes the Nubium Basin andcraters Pitatus and Tycho. This region is particularly inter-esting for understanding the interactions of different typesof features such as the manner in which mare floors en-counter crater rims and highlands. The Fra Mauro Peninsulais an example of such a feature.
Imbrium Basin RegionThe Imbrium Basin and its ejecta blanket dominate much ofthe near side. The region includes Oceanus Procellarum, andother neighboring maria: Vaporum, Serenitatis, and Frigoris.Craters in this region include Kepler, Copernicus, Archimedes,and Aristoteles. This entire region is rich in maria, ejectablankets, and rays of craters. It also has a number of features(such as Vallis Schroteri) that are associated with the floodingof the mare floors.
Nectaris Basin RegionThe northeastern part of the Nectaris region is rich in maria,including Fecunditatis and Tranquillitatis as well as MareNectaris. To the west and south, the region includes exten-sive highlands. To the west, parts of these highlands arecovered with ejecta from the Imbrium Basin.
Serenitatis Basin RegionThis region includes the Serenitatis and TranquillitatisBasins, the northern part of the Fecunditatis Basin, and thewestern part of the Crisium Basin. The region shows theinterplay of overlapping basins.
Eastern Basins RegionFrom Earth, this region covers the eastern limb (edge, as wesee it) of the Moon. It includes the eastern part of theCrisium Basin, the Australe Basin, the Smythii Basin, andMare Marginis.
North Polar RegionThe heavy shadowing in both polar regions obscures bothphotography and passive spectral measurements, especiallyfor the floors of basins and craters. The near side part of theregion and the North Pole itself are largely covered withejecta from the Imbrium Basin. Craters in this region includeNansen, Shackleton, and Anaxagoras. The region includesthe Humboldtianum Basin.
South Polar RegionThe South Polar Region is dominated by the rim of the SouthPole–Aiken Basin and several smaller basins such as
Schrodinger, Planck, and Bailly. Permanently shadowedcrater floors in this region (as well as in the North PolarRegion) are believed to harbor deposits of hydrogen or waterice. Permanently sunlit crater rims nearby are proposed assites for solar power.
3.7. The Ages of the LunarFeaturesAn interesting attribute of a lunar feature is the time it wasformed. The ages of different features on the Moon are in-ferred from several sources.
Estimating AgesThe most precise ages are determined from measurement of isotope ratios in our precious rock samples; association ofthe samples with specific features establishes their time offormation.
When rock samples are unavailable, geologists resort toless precise measures. For example, sharply defined fea-tures are inferred to be recent because meteorite bombard-ment softens the edges of features by a process calledmass-wasting. Also, counts of crater densities can be used to estimate the time a surface has been exposed tobombardment.
Very often, even though absolute time cannot be deter-mined, the sequence of formation can be determined. Forexample, ejecta from a basin may overlay a crater or lavafrom a mare may flow into a crater. Such layering and thebranch of geology that studies it are called stratigraphy.
Named Age RangesSystematic study of stratigraphy, together with other clues,establishes a chain of evidence that leads to relative ages andestimated age ranges of most of the features of the Moon.These age ranges are named for associated archetypefeatures. In order from the oldest to the youngest, theranges are the Pre-Nectarian, Nectarian, Early Imbrian, LateImbrian, Eratosthenian, and Copernican Periods or Epochs.Geologists use the term “epoch” as a subdivision of a period.The Early Imbrian and the Late Imbrian Epochs are subdivi-sions of the Imbrian Period. The boundary between the Pre-Nectarian and Nectarian Periods is the time of the impactthat produced the Nectaris Basin. The Nectarian Period endswith the event that produced the Imbrium Basin. The EarlyImbrian Epoch spans the time between the Imbrium andOrientale events.
Large basin-forming events are used to divide these timeperiods because such events spread their deposits so very far,as much as halfway around the Moon. This method allows usto relate many other features to large basin events by analyz-ing interactions with the widespread deposits. BecauseOrientale is the last big basin, however, the younger ageranges are based on large craters. The Eratosthenian Periodis next, and then the Copernican Period (this interval is openended; we live in the Copernican Period). These last twoperiods are not distinguished by bounding events, but on thedegree of degradation of craters and their ejecta (especiallythe fading of rays) as they are exposed to further impacts andto the solar wind.
4.1. Grouping by LandmarkRegionsEach chapter that follows displays images of a particularlandmark region. A few medium-resolution frames areshown for each region to provide an overview. Only a few ofthe medium-resolution photos are presented because theyhave a high degree of overlap. The high-resolution photosare selected in rectangular blocks so that a reasonable degreeof organization is imposed. The relation of the photos andtheir assignment to regions is shown in a table in eachchapter.
4.2. Order: West to East andSouth to NorthThe regions are presented from the west limb around thenearside to the east limb; that is because Orientale, thenewest and clearest basin and Imbrium, the largest nearsidebasin, are both toward the west and are should be viewedbefore the other regions. Keep in mind, however, that themission and the rising sun move from east to west. To mini-mize confusion, the photos covering a particular longituderange are presented from south to north (in the order mostof the photos were taken, and in order of the numbering con-vention for those photos). A few of the photos in the EasternBasin Region were taken in reverse of the usual orbital direc-tion, to compensate at the end of the mission for photos lostat the beginning of the mission.
4.3. Clean and AnnotatedImagesOne page is provided for each high-resolution subframe orframe. The cleaned image is shown on the right side of eachpage and an overlay with the major features of the imagelabeled is on the left. A title line shows the photo number,lighting conditions, and spacecraft altitude at the time of theexposure. Latitude and longitude marks and a scale bar areshown in the annotated overlay. The scale bar is derivedfrom the size of prominent surface features, as listed on the
USGS Web site. Except for the apostrophe, diacritical marksin feature names have been omitted in both photos and textbecause they are not supported in the software used to anno-tate the photos. A list of names with diacritical marks asguides to pronunciation is in the enclosed CD.
4.4. High-Resolution Framesand SubframesIn most cases, subframes (designated H1, H2, and H3) aredisplayed. In some cases, the three subframes are reassem-bled as a full high-resolution frame (designated H). This isdone either to show the relationship of the features acrossthe full exposure or because the features displayed aredeemed to be of relatively little interest, usually because ofsimilarity to their surroundings. All subframes are presentedat full detail in the enclosed CDs.
4.5. Discussion NotesThe photo pages contain notes that point out and discuss rel-evant aspects of the features and their relationships. Thesenotes draw on an extensive lunar literature to include aspectsof the stratigraphy, geology, and possible formation andmodification processes of the features.
4.6. Enclosed Compact Disc(CD)The enclosed CD contains:
● All high-resolution subframes from Lunar OrbiterMission 4 (JPEG files)
● All medium-resolution frames from Lunar OrbiterMission 4 (JPEG files)
● An index of nearside features whose names are recognizedby the International Astronomical Union (IAU)
● A description of the process used to clean up scanningartifacts
● Source notes related to individual photos
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The feature index includes all the near side features in themaster IAU list maintained by the USGS that are larger than6 km. Several smaller features and some far side featuresnear the eastern limb, the western limb, the North Pole, or
the South Pole are also included. Each of the features listedin the index can be found in the annotated photo (and thephoto number) on the indicated page.
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5.1. OverviewOrientale, the Archetype Multi-RingedBasinFigure 5.1 shows the spectacular Orientale Basin, thenewest large basin on the Moon. It is often called the ar-chetype of basins because it reveals the structure of basinsso clearly. Like typical large basins, it is multi-ringed; thatis, there are a number of concentric rings both inside andoutside of its major raised rim. Mare surfaces have beenformed from lava seeping up from below its central floor.Additional lava has seeped up into the low troughs betweenthe external rings.
Although the Orientale Basin has many features incommon with all basins, it must be considered that there aresignificant differences between basins as well. The detailedstructure of a basin depends on the nature of the target mate-rial. Orientale has formed in an area of thick, somewhatuniform crust. Although there are no major basins in itsimmediate vicinity, large craters have been identified thatinfluenced its detailed structure.
Orientale Basin and its included Mare Orientale arelocated on the western edge of the Moon, the edge that risesand sets last. Terrestrial astronomers glimpse its easternrings as the libration of the Moon turns that edge a bittoward us. Spacecraft Zond 3 photographed it in 1965 at es-sentially Earth-based resolution. However, the Lunar Orbiter4 coverage showed the magnificence of its structure at amuch higher resolution.
These photos created a major paradigm shift in minds ofgeologists who had been debating whether volcanism orimpacts dominated the lunar surface. This newest basin hada fresh ejecta blanket, revealed in detail by the high-resolutionphotos. The unavoidable conclusion was that many geologicunits whose origins were debated were in fact formed byejecta, not only from Orientale but also from larger, olderbasins such as Imbrium. This insight was confirmed andstrengthened by the pervasive discovery of impact breccia inthe rocks returned by Apollo missions. Such rocks areformed by the hypervelocity shock of impacts welding preex-isting rock fragments from diverse sources into larger rocks.They show a diverse set of shock effects, from changes of crystalline structure to partial or complete melting(Wilhelms, 1987).
A remarkable property of multi-ringed basins is the regu-larity of the radii of the concentric rings. Such rings arefound not only on the Moon (where there is evidence ofabout 60 multi-ringed basins), but also on Earth, Mercury,Mars, the Jupiter moons Ganymede and Callisto, and the Saturn moons Tethys and Rhea (Spudis, 1993). Measure-ments of the rings of basins on all these bodies fit a specificrelationship; successive rings, both internal and external tothe topographic rim (the ring of highest elevation also calledthe main ring), have radii in the ratio of the square root of 2.
Chapter 5
Orientale Basin Region
Figure 5.1. LO4-187M. The Orientale Basin is the archetype of multi-ringed basins. The lava flow of Mare Orientale is in the dark center of theconcentric rings. The dark mare surface to the upper right is OceanusProcellarum, the largest deposit of mare on the Moon. The small dark circu-lar feature is a mare deposit on the floor of the 440-km Grimaldi Basin. Thebright rays in the upper right corner of the photo radiate from Glushko, asmall crater near Oceanus Procellarum, not from Orientale.
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This relationship, equivalent to the doubling of the area ofeach successive ring, is very regular, but has no consensustheoretical basis at this time.
Crater Morphology as a Function ofSizeSmall impact craters do not have such concentric rings. Thesmallest craters have a transient cavity that is nearly hemi-spherical. The transient cavity is the zone of target materialthat was melted and pulverized by the hypervelocity impact.Some of this material is ejected, with most of it landingwithin one radius of the transient cavity from the rim of the transient cavity. This rim is a single topographic ring.Medium-sized craters have a distinctive central peak; thefocused sound wave rebounding from the mass of pulverizedand compressed material has lifted material nearly vertically,and it forms a mountain in the center of the crater. As the di-ameters of lunar craters exceed about 300 km (200 miles), thecentral peak breaks up into one or more internal rings, andexternal rings form as well. It is these very large craters thatwe call multi-ringed basins, or basins for short. The bottomsof large craters may penetrate near or through the boundarybetween the crust and the mantle.
Surroundings of the Orientale BasinTo the north and west, the ejecta blanket from Orientale hasbeen deposited on highlands. To the northeast, the ejecta fellon the surface later covered by the mare material of OceanusProcellarum. To the east and south lie highlands interruptedby other, smaller basins: Grimaldi and Humorum. The flankof Grimaldi shows fine striations radial to Orientale, so itmust have formed earlier. Similarly, the Humorum Basinpredates Orientale.
Figure 5.2 shows a mosaic of the eastern sector of theOrientale Basin Region, illustrating the structure of its rings.
5.2. High-Resolution ImagesTable 5.1 shows the high-resolution images of the OrientaleBasin region in schematic form.
The following pages show the high-resolution subframesfrom south to north and west to east; that is, they are in theorder LO4-194H, LO4-195H1, LO4-195H2, LO4-195H3, LO4-186H1 . . . LO4-161H3. Note that the photos taken on a givenorbit are presented in order; both frame and subframenumbers increase in the same order as the pages of thisbook. However, in moving from west to east to a new orbitalsequence, the numbers decrease.
LO4-194H has been assembled as a complete frame. Itshows the range of Orientale ejecta from the topographic rimto one radius away from that rim. In addition, it illustrateshow subframes are contiguous parts of high-resolutionframes. Similarly, LO4-169H and LO4-161H are displayed asfull frames.
Subframes LO4-180H1 and LO4-167H1 are not printed inthis chapter because they are redundant with the subframesto their east and west and show no additional features. Thebase photos are included in the enclosed CD.
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s Figure 5.2. Mosaic of Lunar Orbiter 4 high-resolution photos of theOrientale Basin, from the central mare at the left out past the concentricrings to the right. Dark mare material is found not only in the central part ofthe basin, but also in the troughs between the rings. Note the striations inthe ejecta blanket radiating from the central portion of the basin. They havea stronger appearance to the northeast and southeast rather than directlytoward the east. Because of the direction of solar illumination, ridges ori-ented in the east-west direction do not cast shadows. The smaller GrimaldiBasin in the upper right of the mosaic shows both a topographic ring thathas contained most of the mare lava and a lower outer ring.
Latitude Range Photo Number
27 N–56 N 189 183 175 170 163 158
0–27 N 188 182 174 169 162 157
0–27 S 195 187 181 173 168 161 156
27 S–56 S 194 186 180 172 167 160 155
56 S–90 S 179 166 154
Longitude 95 W 89 W 82 W 76 W 68 W 62 W 56 Wat Equator
Table 5.1. The cells shown in white represent the high-resolution photosof the Orientale Basin Region (LO4-XXX H1, -H2, and -H3, where XXX is thePhoto Number; LO4 means Lunar Orbiter Mission 4). The Imbrium BasinRegion is to the northeast, the Humorum Basin Region is to the east, and theSouth Polar Region is to the south. The far side is to the west. The nextnumber after LO4 is the exposure number, which increased as the missionprogressed from east to west.
LO4-194HSun Elevation: 16.10°Altitude: 3002.79 km
This full high-resolution frame showsthe inner Orientale Basin at the top.Montes Cordillera is the topographicring. Its scarp bounds the floor of thebasin. The arc of Montes Rook shownhere is the first inner ring of theOrientale Basin.
Striations show a heavy deposit ofejecta (the Hevelius Formation) fromthe inner Orientale Basin to the south.The character of the ejecta changesfrom the heavy, striated inner HeveliusFormation to the lighter, more uniformouter Hevelius Formation about 440 kmaway from the rim of the MontesCordillera ring (930 km in diameter).Graff, Catalan, and Baade have beencovered with a heavy deposit whileYakovin has received a lighter deposit.Several other craters in the 10- to 30-kmrange (probably secondaries fromOrientale) left deposits of fine ejectaoutside their rims.
The crater Hausen (out of the pictureto the southwest) has more recentlydeposited chains of small secondarycraters that can be seen on the floor of crater Pingre and outside its rim.Pingre may lie on the floor of an olderbasin called the Pingre-Hausen Basin.The large semicircular ridge east andnorth of Pingre is the boundary of thatbasin.
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cally
unr
elat
ed M
aund
er c
rate
r no
rth
of M
are
Ori
enta
le (
see
LO4-
195H
2).
The
Mau
nder
For
mat
ion
has
been
inte
rpre
ted
as th
e m
elt s
heet
of t
he b
asin
. The
frac
ture
sre
lieve
str
esse
s th
at c
ould
hav
e be
en a
ssoc
iate
d w
ith
cool
ing
of t
he m
elt
shee
t, se
ttlin
g of
und
erly
ing
pulv
eriz
ed m
ater
ial,
or fl
oodi
ng o
f th
e m
are.
Oth
er b
asin
s m
ay h
ave
had
sim
ilar
mel
t sh
eets
tha
t w
ere
com
plet
ely
hidd
en b
y a
late
r co
veri
ngof
mar
e la
va.
16
Luna
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
195H
1Su
n El
evat
ion:
14.
50°
Alt
itud
e: 2
721.
44 k
m
Mau
nder
was
obv
ious
ly f
orm
ed a
fter
the
mar
e flo
or h
adso
lidifi
ed. I
t has
a ty
pica
l pro
file
for
a la
rge
(55-
km)
prim
ary
crat
er,
wit
h a
wel
l-fo
rmed
cen
tral
pea
k, t
erra
ced
wal
ls,
anej
ecta
bla
nket
wit
h ra
dial
fur
row
s, a
nd a
fiel
d of
sec
onda
rycr
ater
s. T
he m
elt
shee
t of
the
Mau
nder
For
mat
ion
(nam
edaf
ter
the
crat
er)
appe
ars
to h
ave
part
ially
col
laps
ed a
t ei
ther
side
of t
he M
aund
er c
rate
r, p
ossi
bly
due
to th
e im
pact
sho
ck.
The
eje
cta
of s
ome
post
-mar
e cr
ater
s su
ch a
s Il
’in a
ppea
r to
have
flow
cha
ract
eris
tics
, as
if t
hey
impa
cted
whi
le t
he m
are
was
sti
ll se
mim
olte
n or
sti
ll ho
t en
ough
to
be m
elte
d by
the
impa
cts.
See
the
note
for
Kop
ff w
ith
phot
o LO
4-18
7H2.
LO4-
195H
2Su
n El
evat
ion:
14.
50°
Alt
itud
e: 2
721.
44 k
m
17
Ori
enta
leBa
sin R
egio
n
The
are
a in
thi
s ph
oto
show
s m
any
diff
eren
ces
in s
truc
ture
and
text
ure.
Com
pare
the
sm
ooth
mar
e la
va o
f La
cus
Ver
isw
ith
the
rugg
ed c
liffs
of t
he in
ner
ridg
e of
Mon
tes
Roo
k an
dth
e kn
obby
, fla
t M
onte
s R
ook
Form
atio
n be
twee
n M
onte
sR
ook
and
Mon
tes
Cor
dille
ra. N
ote
the
stee
p sc
arp
of th
e ri
mof
Mon
tes
Cor
dille
ra a
nd t
he t
hick
, ro
py n
atur
e of
the
in
ner
Hev
eliu
s Fo
rmat
ion
of b
asin
eje
cta
beyo
nd M
onte
sC
ordi
llera
. C
rate
rs K
ram
arov
and
Cou
der,
abo
ut t
he s
ame
size
and
age
(ju
dgin
g by
rim
sha
rpne
ss),
sho
w a
n in
tere
stin
gco
ntra
st i
n st
ruct
ure.
Kra
mar
ov,
impa
ctin
g th
e H
evel
ius
Form
atio
n, h
as t
hrow
n m
ore
ejec
ta a
nd p
art
of i
ts w
all
has
colla
psed
. C
oude
r, i
mpa
ctin
g th
e R
ook
Form
atio
n, h
as a
smal
ler
ejec
ta b
lank
et a
nd s
moo
th w
all.
Its
oval
sha
pe i
ndi-
cate
s a
low
impa
ct a
ngle
.
LO4-
195H
3Su
n El
evat
ion:
14.
50°
Alt
itud
e: 2
721.
44 k
m
18
Luna
r O
rbiter
Photo
gra
phic
Atla
s
Thi
s ar
ea
has
been
co
vere
d w
ith
the
oute
r H
evel
ius
Form
atio
n, e
ject
a fr
om O
rien
tale
, as
can
be
seen
fro
m t
hech
ain
of O
rien
tale
sec
onda
ry c
rate
rs d
own
thro
ugh
the
cent
er o
f th
e ph
oto.
On
the
righ
t is
a s
erie
s of
con
cent
ric-
wal
led
crat
ers
that
may
hav
e fo
rmed
as
they
enc
ount
ered
afir
m la
yer
bene
ath
a so
fter
laye
r of
reg
olit
h, t
he e
ject
a fr
omO
rien
tale
and
oth
er b
asin
s. S
imul
atio
ns s
ugge
st t
hat
such
stru
ctur
es fo
rm w
hen
the
appa
rent
cra
ter
diam
eter
is 8
to 1
0ti
mes
the
dept
h of
the
rego
lith.
Yak
ovki
n ap
pear
s to
hav
e re
-ce
ived
a r
elat
ivel
y lig
ht c
oati
ng o
f ej
ecta
. It
als
o m
ay h
ave
been
floo
ded
wit
h la
va a
fter
the
eje
cta
had
been
dep
osit
ed;
its
surf
ace
seem
s ve
ry s
moo
th a
nd fr
ee o
f sm
all c
rate
rs.
LO4-
186H
1Su
n El
evat
ion:
15.
60°
Alt
itud
e: 3
005.
57 k
m
19
Ori
enta
leBa
sin R
egio
n
Thi
s ar
ea, l
ike
muc
h of
the
Moo
n, h
as b
een
repe
ated
ly o
ver-
laid
wit
h ba
sin
ejec
ta. T
he la
rges
t sca
le li
near
feat
ures
rad
iate
from
the
Ori
enta
le B
asin
, ju
st t
o th
e no
rthw
est.
How
ever
,th
ere
are
smal
ler-
scal
e lin
ear
feat
ures
run
ning
fro
m s
outh
-w
est
to n
orth
east
fro
m t
he o
lder
Men
del-
Ryd
berg
Bas
in t
oth
e so
uthw
est.
Baa
de, f
orm
ed in
a th
ick
ejec
ta b
lank
et, h
as a
wea
k ce
ntra
l pe
ak.
Val
lis
Bou
vard
and
Val
lis
Baa
de a
rech
ains
of
seco
ndar
y cr
ater
s an
d ot
her
ejec
ta f
rom
Ori
enta
leth
at p
low
ed t
hese
val
leys
in
low
-ang
le i
mpa
cts.
Sim
ilar
valle
ys a
ppea
r ar
ound
the
Imbr
ium
and
Nec
tari
s ba
sins
.
LO4-
186H
2Su
n El
evat
ion:
15.
60°
Alt
itud
e: 3
005.
57 k
m
20
Luna
r O
rbiter
Photo
gra
phic
Atla
s
Mon
tes
Cor
dille
ra i
s th
e to
pogr
aphi
c (h
ighe
st)
rim
of
the
Ori
enta
le B
asin
. The
out
er r
ange
of M
onte
s R
ook
is th
e ne
xtm
ount
aino
us a
rea
tow
ard
the
cent
er o
f th
is m
ulti
-rin
ged
basi
n. B
etw
een
Mon
tes
Cor
dille
ra a
nd M
onte
s R
ook
is
the
flat
knob
by p
lain
of
the
Mon
tes
Roo
k Fo
rmat
ion.
The
bott
om o
f the
trou
gh b
etw
een
the
two
ring
s of
Mon
tes
Roo
kis
eve
n lo
wer
tha
n th
e M
onte
s R
ook
Form
atio
n. C
rate
rsPe
ttit
, Nic
hols
on, W
righ
t, an
d Sh
aler
sho
w s
lum
ping
of t
heir
crat
er w
alls
, sug
gest
ing
that
the
y m
ay h
ave
impa
cted
a lo
w-
stre
ngth
mat
eria
l, a
cont
rast
to
crat
ers
impa
ctin
g th
e m
elt
shee
t of
the
Mau
nder
For
mat
ion
wit
hin
the
Mon
tes
Roo
kri
ngs.
LO4-
186H
3Su
n El
evat
ion:
15.
60°
Alt
itud
e: 3
005.
57 k
m
21
Ori
enta
leBa
sin R
egio
n
Bet
wee
n th
e ou
ter
and
inne
r ra
nges
of
Mon
tes
Roo
k is
ava
lley
of c
haot
ic m
ater
ial.
Thi
s hu
mm
ocky
zon
e co
uld
be a
mix
of r
ubbl
e an
d m
elte
d m
ater
ial f
rom
the
impa
ct, t
oget
her
wit
h ex
trus
ions
fro
m b
elow
. Ex
tens
ive
frac
turi
ng i
n th
iszo
ne, a
ppea
ring
at
the
surf
ace
as R
imae
Pet
tit
(LO
4-19
5H1)
,m
ay i
ndic
ate
cont
ract
ion
or s
ubsi
denc
e re
late
d to
coo
ling
and
othe
r ad
just
men
ts a
fter
the
impa
ct. P
etti
t and
Nic
hols
onap
pear
to
have
impa
cted
the
out
er M
onte
s R
ook
ridg
e w
hile
it w
as n
ewly
form
ed; t
heir
eje
cta
seem
s to
hav
e be
en m
olte
nan
d th
eir
wal
ls e
ithe
r sl
umpe
d to
the
ir fl
oors
or
addi
tion
alm
ater
ial l
ande
d in
them
. The
y m
ay b
e se
cond
arie
s ex
cava
ted
by e
ject
a th
row
n in
a h
igh
traj
ecto
ry fr
om th
e O
rien
tale
eve
ntit
self.
LO4-
187H
1Su
n El
evat
ion:
13.
90°
Alt
itud
e: 2
722.
79 k
m
22
Luna
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
187H
2Su
n El
evat
ion:
13.
90°
Alt
itud
e: 2
722.
79 k
m
23
Ori
enta
leBa
sin R
egio
n
Lacu
s V
eris
is
a sm
all
mar
e ar
ea f
orm
ed i
n th
e tr
ough
betw
een
the
two
ridg
es o
f Mon
tes
Roo
k. S
tres
s fr
actu
res
cir-
cum
fere
ntia
l to
the
basi
n ri
m a
long
the
edg
e of
Lac
us V
eris
.O
ther
fra
ctur
es r
un a
cros
s an
d ne
ar i
t. T
hese
fra
ctur
e lin
esdi
sapp
ear
as th
ey e
ncou
nter
mar
e m
ater
ial,
whi
ch m
ust h
ave
flood
ed a
fter
str
ess
was
rel
ease
d by
frac
turi
ng. T
his
frac
ture
dte
rrai
n, th
e M
aund
er F
orm
atio
n, is
thou
ght b
y m
ost a
naly
sts
to b
e im
pact
mel
t. C
rate
r K
opff
, un
like
Mau
nder
(se
e LO
-195
H2)
, has
a s
hallo
w, fl
at fl
oor,
a s
moo
th r
im w
itho
utte
rrac
es, a
nd n
o ce
ntra
l pe
ak. I
ts e
ject
a se
ems
mol
ten,
lik
eth
at o
f Pe
ttit
and
Nic
hols
on. K
opf
may
als
o be
a s
econ
dary
that
im
pact
ed a
sti
ll-m
olte
n m
elt
shee
t an
d w
as fl
oode
d by
mar
e m
uch
late
r.
LO4-
187H
3Su
n El
evat
ion:
13.
90°
Alt
itud
e: 2
722.
79 k
m
24
Luna
r O
rbiter
Photo
gra
phic
Atla
s
Thi
s ar
ea n
orth
of
the
inne
r ba
sin
show
s th
e kn
obby
ter
rain
betw
een
Mon
tes
Roo
k an
d M
onte
s C
ordi
llera
and
the
stri
ated
eje
cta
blan
ket
beyo
nd M
onte
s C
ordi
llera
. M
onte
sC
ordi
llera
typi
cally
sho
ws
a sc
arp
(clif
f) a
t its
inne
r ed
ge. T
hesu
btle
cir
cula
r fe
atur
e ju
st n
orth
of
the
crat
er C
oude
rap
pear
s to
be
a pr
eexi
stin
g cr
ater
tha
t w
as c
over
ed b
y th
eej
ecta
from
Ori
enta
le.
Thi
s ar
ea, c
over
ed b
y th
e st
riat
ed in
ner
Hev
eliu
s Fo
rmat
ion
of O
rien
tale
eje
cta,
has
no
feat
ure
wit
h an
IA
U n
ame.
The
radi
al s
tria
tion
s ar
e em
phas
ized
by
the
righ
t-to
-lef
t su
ndi
rect
ion.
An
80-k
m c
rate
r on
the
upp
er r
ight
sid
e of
the
phot
o ha
s be
en s
ubm
erge
d by
the
eje
cta,
but
see
ms
to h
ave
focu
sed
the
flow
line
s at
its
far
edge
.
LO4-
188H
1Su
n El
evat
ion:
14.
50°
Alt
itud
e: 2
675.
46 k
m
25
Ori
enta
leBa
sin R
egio
n
Eins
tein
, Sun
dman
, and
Boh
r ar
e pr
eexi
stin
g cr
ater
s co
vere
dby
Ori
enta
le d
epos
its,
inc
ludi
ng fi
elds
of
seco
ndar
ies.
The
seco
ndar
y ch
ain
of V
allis
Boh
r an
d se
cond
arie
s on
the
floo
rof
Ein
stei
n ar
e ty
pica
l of
the
oute
r H
evel
ius
Form
atio
n. T
hetr
ansi
tion
fro
m t
he i
nner
For
mat
ion
is n
ear
the
bott
om o
fth
is p
ictu
re, a
bout
one
rad
ius
away
from
Mon
tes
Cor
dille
ra.
The
80-
km c
rate
r in
the
low
er r
ight
cor
ner
is fi
ssur
ed, s
ug-
gest
ing
that
the
ejec
ta th
ere
may
hav
e be
en m
olte
n an
d th
encr
acke
d as
it c
oole
d. V
ario
us lo
bate
flow
pat
tern
s ca
n be
see
nhe
re. T
he 1
0-km
cra
ter
abou
t 70
km s
outh
east
of S
undm
an is
in a
ver
y da
rk, l
ow-l
ying
are
a, a
nd th
e cr
ater
has
a r
are
dark
ray
patt
ern
in C
lem
enti
ne a
lbed
o da
ta.
LO4-
188H
2Su
n El
evat
ion:
14.
50°
Alt
itud
e: 2
675.
46 k
m
26
Luna
r O
rbiter
Photo
gra
phic
Atla
s
The
Ori
enta
le e
ject
a is
bec
omin
g th
in h
ere,
in
an a
rea
wel
lno
rth
of th
e ba
sin
floor
. Mar
e su
rfac
es o
n th
e ri
ght a
re a
t the
edge
of
Oce
anus
Pro
cella
rum
. C
rate
rs V
oskr
esen
skiy
and
Bar
tels
app
ear
to h
ave
been
floo
ded,
as
is c
omm
on n
ear
the
edge
of
a la
rge
mar
e. A
pos
sibl
e se
cond
ary
from
Ori
enta
leha
s hi
t the
nor
thea
st c
rate
r w
all o
f Bar
tels
and
left
deb
ris
onit
s flo
or. T
he s
catt
erin
g of
cra
ters
abo
ut 1
0 km
in
diam
eter
,w
ith
sim
ilar
fre
sh a
ppea
ranc
es,
are
prob
ably
sec
onda
ries
from
Ori
enta
le. T
he fl
oor
of M
osel
ey h
as a
com
plex
app
ear-
ance
, as
if a
lava
flow
ent
ered
it fr
om th
e no
rth.
LO4-
188H
3Su
n El
evat
ion:
14.
50°
Alt
itud
e: 2
675.
46 k
m
27
Ori
enta
leBa
sin R
egio
n
LO4-
180H
2Su
n El
evat
ion:
16.
10°
Alt
itud
e: 3
008.
99 k
m
28
Luna
r O
rbiter
Photo
gra
phic
Atla
s
Like
Val
lis
Baa
de,
Val
lis
Ingh
iram
i an
d it
s bo
undi
ng
ridg
es h
ave
been
for
med
by
the
inne
r H
evel
ius
Form
atio
nej
ecte
d fr
om O
rien
tale
. Suc
h ej
ecta
als
o co
vere
d th
e cr
ater
Ingh
iram
i an
d a
sim
ilar
cra
ter
nort
hwes
t of
the
hea
d of
Val
lis
Ingh
iram
i. N
ote
the
21-k
m c
rate
r ne
ar t
hat
valle
yhe
ad.
Its
conc
entr
ic c
rate
r fo
rm (
a lit
tle
off
cent
er i
n th
isca
se)
sugg
ests
that
it h
as p
ulve
rize
d ab
out 2
km
of d
epos
ited
mat
eria
l fr
om t
he fl
oor
of t
he v
alle
y be
fore
enc
ount
erin
gm
ore
resi
stan
ce. S
hado
win
g on
the
val
ley
wal
l ind
icat
es t
hat
the
ridg
es r
ise
2 or
3 k
m a
bove
the
valle
y flo
or.
The
cra
ter
Kra
snov
and
the
unn
amed
45-
km c
rate
r ab
ove
itst
radd
le th
e ar
ea o
f the
sca
rp a
nd p
rovi
de c
lues
to it
s na
ture
.T
he u
nnam
ed c
rate
r is
kno
wn
to h
ave
form
ed b
efor
e or
in
an e
arly
pha
se o
f th
e O
rien
tale
seq
uenc
e of
eve
nts
beca
use
its
rim
has
bee
n ex
tens
ivel
y m
odifi
ed b
y ej
ecta
. Bec
ause
the
rim
of
Kra
snov
is
shar
p, i
t m
ust
have
for
med
aft
er t
heO
rien
tale
eve
nt o
r la
te i
n it
s se
quen
ce. T
he m
assi
ve d
epos
iton
the
floo
r of
the
unn
amed
cra
ter
sugg
ests
tha
t th
e ri
m o
fM
onte
s C
ordi
llera
, w
hose
sca
rp i
s of
sim
ilar
dep
th,
isco
vere
d w
ith
depo
site
d m
ater
ial.
A n
arro
w t
erra
ce o
n th
ein
ner
wal
l of K
rasn
ov m
ay in
dica
te e
ithe
r th
e le
vel o
f the
pre
-O
rien
tale
sur
face
or
an in
terf
ace
betw
een
succ
essi
ve la
yers
of
ejec
ta.
LO4-
180H
3Su
n El
evat
ion:
16.
10°
Alt
itud
e: 3
008.
99 k
m
29
Ori
enta
leBa
sin R
egio
n
The
inne
r ed
ge o
f Mon
tes
Cor
dille
ra h
as a
sha
rp s
carp
(st
eep
slop
e). S
uch
scar
ps m
ay b
e fo
rmed
by
exca
vati
on o
f th
e lo
wsi
de o
r by
lift
ing
of th
e hi
gh s
ide
(suc
h as
by
tilt
ing
a bl
ock)
.St
rong
str
iati
ons
appe
ar t
o cr
oss
the
valle
y be
twee
n M
onte
sR
ook,
red
uce
the
scar
p of
Mon
tes
Cor
dille
ra s
outh
of
Eich
stad
t, a
nd c
onti
nue
acro
ss M
onte
s C
ordi
llera
(se
e LO
4-17
2H1
for
the
cont
inua
tion
to th
e so
uthe
ast)
. The
se s
tri-
atio
ns a
re r
elat
ivel
y su
bdue
d in
the
val
ley
betw
een
the
two
mou
ntai
n ra
nges
. Thi
s su
gges
ts th
at th
e va
lley
floor
was
flui
d(e
ithe
r m
olte
n or
fine
ly p
ulve
rize
d) a
nd p
erha
ps s
tron
gly
shak
en b
y a
soni
c or
tec
toni
c w
ave
afte
r th
e ej
ecta
bla
nket
was
dep
osit
ed.
LO4-
181H
1Su
n El
evat
ion:
14.
80°
Alt
itud
e: 2
723.
98 k
m
30
Luna
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
181H
2Su
n El
evat
ion:
14.
80°
Alt
itud
e: 2
723.
98 k
m
31
Ori
enta
leBa
sin R
egio
n
Mar
e la
va fl
oode
d no
t on
ly M
are
Ori
enta
le i
n th
e ce
ntra
lin
ner
basi
n bu
t al
so L
acus
Ver
is i
n th
e tr
ough
bet
wee
n th
ein
ner
and
oute
r ri
dges
of
Mon
tes
Roo
k an
d La
cus
Aut
umni
in t
he v
alle
y flo
or b
etw
een
Mon
tes
Roo
k an
d M
onte
sC
ordi
llera
. Cra
ter
coun
ts in
dica
te t
hat
the
orde
r of
floo
ding
is f
rom
the
cen
ter
of t
he b
asin
(w
here
a m
asco
n in
dica
tes
apl
ume
of m
antle
mat
eria
l has
ris
en)
outw
ard.
Lac
us A
utum
niha
s be
en j
ust
part
ially
floo
ded.
Som
e st
riat
ions
and
sec
-on
dary
cra
ters
in L
acus
Aut
umni
may
be
ejec
ta f
rom
cra
ter
Schl
uter
, jus
t to
the
nort
h (s
ee L
O4-
181H
3).
Cra
ters
Sch
lute
r an
d H
artw
ig,
just
out
side
the
Mon
tes
Cor
dille
ra,
are
inte
rest
ing
exam
ples
of
the
effe
ct o
f ba
sin
ejec
ta (
Hev
eliu
s Fo
rmat
ion)
. Har
twig
was
bla
nket
ed b
y th
isej
ecta
, but
Sch
lute
r im
pact
ed a
fter
war
d. T
his
stra
tific
atio
n,pl
us t
he la
va fl
oodi
ng in
par
t of
the
floo
r of
Sch
lute
r, e
stab
-lis
hes
its
age
as L
ate
Imbr
ian.
LO4-
181H
3Su
n El
evat
ion:
14.
80°
Alt
itud
e: 2
723.
98 k
m
32
Luna
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
182H
1Su
n El
evat
ion:
16.
10°
Alt
itud
e: 2
674.
44 k
m
33
Ori
enta
leBa
sin R
egio
n
Thi
s ar
ea i
s do
min
ated
by
the
inne
r H
evel
ius
Form
atio
n of
Ori
enta
le e
ject
a. T
he t
wo
20-k
m c
rate
rs in
the
upp
er h
alf
ofth
e ph
oto
may
sho
w c
lues
abo
ut t
he c
onsi
sten
cy o
f th
isej
ecta
. T
he m
ater
ial
on t
heir
floo
rs s
eem
s to
hav
e be
enm
olte
n, b
ut w
ith
grea
ter
visc
osit
y th
an t
he m
are
lava
flow
s.T
he m
ater
ial
seem
s to
hav
e be
en f
ract
ured
, pe
rhap
s by
cool
ing
or b
y se
ttlin
g on
the
pre
exis
ting
top
ogra
phy
of t
hecr
ater
floo
rs. A
long
thin
str
ing
of s
econ
dary
cra
ters
run
ning
from
sou
th-s
outh
east
to
nort
h-no
rthw
est
acro
ss t
he l
ower
half
of t
he p
hoto
rad
iate
s fr
om c
rate
r Sc
hlut
er t
o th
e so
uth
(see
LO
4-18
1H3)
. LO
4-17
4H1
show
s m
uch
of th
e ar
ea o
n th
eri
ght
side
of t
his
phot
o w
itho
ut t
he d
evel
opm
ent
arti
fact
s in
this
exp
osur
e.
Thi
s re
gion
sho
ws
clus
ters
of
Ori
enta
le s
econ
dary
cra
ters
,so
me
stri
atio
n an
d se
cond
ary
chai
ns f
rom
the
cen
tral
Ori
enta
le B
asin
, and
som
e de
posi
ts th
at a
ppea
r to
hav
e be
enm
olte
n (w
ith
flow
edg
es).
The
se a
re t
ypic
al f
eatu
res
of t
heou
ter
Hev
eliu
s Fo
rmat
ion.
Cra
ters
Bal
boa,
Dal
ton,
Vas
co d
aG
ama,
and
the
unn
amed
50-
km c
rate
r so
uth
of V
asco
da
Gam
a al
l ha
ve f
ract
ures
in
floor
s. S
uch
shal
low
fra
ctur
edflo
ors
are
com
mon
(bu
t no
t un
iver
sal)
nea
r th
e bo
unda
ries
of O
cean
us P
roce
llaru
m, w
hich
can
be
seen
nea
r th
e up
per
righ
t cor
ner
of th
e ph
oto.
The
frac
turi
ng m
ay b
e du
e to
upl
ift
of th
e flo
ors.
LO4-
182H
2Su
n El
evat
ion:
16.
10°
Alt
itud
e: 2
674.
44 k
m
34
Luna
r O
rbiter
Photo
gra
phic
Atla
s
Seve
ral s
ubm
erge
d cr
ater
s su
ch a
s St
ruve
can
be
seen
in th
isar
ea o
f wes
tern
Oce
anus
Pro
cella
rum
. The
dep
th o
f the
mar
ela
va c
an b
e ju
dged
by
the
esti
mat
ed d
epth
of fl
oode
d cr
ater
s.T
he o
uter
Hev
eliu
s Fo
rmat
ion
of O
rien
tale
eje
cta
is th
inni
nghe
re, a
s in
dica
ted
by th
e de
crea
sing
rat
e of
sec
onda
ry c
rate
rsto
the
nort
heas
t.
LO4-
182H
3Su
n El
evat
ion:
16.
10°
Alt
itud
e: 2
674.
44 k
m
35
Ori
enta
leBa
sin R
egio
n
36
Luna
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
172H
1Su
n El
evat
ion:
16.
30°
Alt
itud
e: 3
010.
71 k
m
Mol
ten
mat
eria
l ha
s flo
oded
cra
ters
War
gent
in,
Nas
myt
h,an
d Ph
ocyl
ides
to
form
pla
ins,
but
it is
not
dar
k lik
e ty
pica
lm
are
lava
. The
mat
eria
l has
flow
ed o
ut o
f gap
s in
the
sou
th-
ern
edge
of
War
gent
in. T
he m
elt
may
hav
e be
en t
hrow
n ou
tfr
om t
he i
nner
Ori
enta
le B
asin
. It
appe
ars
to h
ave
cove
red
som
e of
the
str
iate
d ej
ecta
; if
it w
ere
thro
wn
out
at a
hig
her
angl
e an
d a
low
er v
eloc
ity,
it
wou
ld h
ave
arri
ved
late
r th
anth
e m
ater
ial
that
for
med
the
str
iati
ons.
The
clu
ster
s of
crat
ers
in t
he r
ight
sid
e of
thi
s ph
oto
are
seco
ndar
ies
from
Ori
enta
le,
whi
ch m
ay h
ave
been
thr
own
at a
n ev
en h
ighe
ran
gle
than
the
mel
t.
To
the
sout
heas
t, th
e ej
ecta
fro
m O
rien
tale
mee
ts a
nd o
ver-
lies
earl
ier
ejec
ta f
rom
the
160
-km
cra
ter
Schi
ckar
d (L
O4-
167H
2),
crea
ting
a c
ross
-hat
ched
ter
rain
. T
he fl
oor
ofIn
ghir
ami i
s co
vere
d w
ith
ejec
ted
mat
eria
l tha
t ha
s pi
led
upin
the
sout
heas
t qua
dran
t.
LO4-
172H
2Su
n El
evat
ion:
16.
30°
Alt
itud
e: 3
010.
71 k
m
37
Ori
enta
leBa
sin R
egio
n
The
inn
er H
evel
ius
Form
atio
n gr
ades
fro
m t
he v
ery
deep
mat
eria
l th
at c
ompo
ses
Mon
tes
Cor
dille
ra t
o th
e no
rthw
est
to th
inne
r m
ater
ial t
o th
e so
uthe
ast.
In th
e th
inne
r re
gion
s of
the
ejec
ta b
lank
et,
the
pree
xist
ing
topo
grap
hy c
an b
egl
imps
ed. T
he 2
25-k
m c
rate
r La
gran
ge h
as b
een
near
ly o
blit
-er
ated
. The
Ori
enta
le e
ject
a se
ems
to h
ave
push
ed m
ater
ial
from
the
nor
thw
est
rim
of
Lagr
ange
ont
o th
e cr
ater
’s fl
oor.
The
re is
a g
ap in
the
Ori
enta
le e
ject
a on
par
t of
the
floo
r of
the
old
80-k
m c
rate
r in
the
low
er r
ight
han
d co
rner
of
the
phot
o.
38
Luna
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
172H
3Su
n El
evat
ion:
16.
30°
Alt
itud
e: 3
010.
71 k
m
The
re i
s an
int
eres
ting
int
erac
tion
her
e be
twee
n th
e ol
d 12
0-km
cra
ter
betw
een
Eich
stad
t and
Lam
arck
and
the
heav
yflo
w o
f O
rien
tale
eje
cta
that
has
obl
iter
ated
its
wes
tern
rim
and
thro
wn
the
mat
eria
l ont
o th
e w
este
rn h
alf
of t
he c
rate
rflo
or. W
hen
ejec
ta h
it th
e sm
all c
rate
r in
the
low
er r
ight
han
dco
rner
of
the
pict
ure,
it
pile
d up
aga
inst
the
eas
tern
wal
l,ne
arly
up
to th
e to
p of
the
rim
.
LO4-
173H
1Su
n El
evat
ion:
15.
40°
Alt
itud
e: 2
724.
03 k
m
39
Ori
enta
leBa
sin R
egio
n
The
wes
tern
rim
s of
cra
ter
Roc
ca a
nd t
wo
smal
ler
crat
ers
toth
e so
uth
have
par
tly s
hiel
ded
the
wes
tern
floo
rs fr
om e
ject
a,bu
t it
has
acc
umul
ated
on
the
east
ern
floor
s an
d ag
ains
t th
efa
r w
alls
to th
e ea
st.
LO4-
173H
2Su
n El
evat
ion:
15.
40°
Alt
itud
e: 2
724.
03 k
m
40
Luna
r O
rbiter
Photo
gra
phic
Atla
s
Like
the
floor
of S
chlu
ter
to th
e w
est,
Ric
ciol
i’s fl
oor
is p
artl
yflo
oded
wit
h m
are
lava
. T
he p
erva
sive
ness
of
ejec
ta f
rom
Ori
enta
le i
n th
is r
egio
n es
tabl
ishe
s th
at t
he m
are
flood
ing
mus
t ha
ve f
ollo
wed
the
Ori
enta
le e
vent
. R
icci
oli
coul
d no
tha
ve s
urvi
ved
the
Gri
mal
di B
asin
eve
nt (
LO4-
168H
3),
soR
icci
oli
mus
t ha
ve f
ollo
wed
Gri
mal
di. T
he s
eque
nce
is t
hus
Gri
mal
di, R
icci
oli,
Ori
enta
le, a
nd m
are
flood
ing
of t
he fl
oor
of R
icci
oli.
Rim
ae R
icci
oli
are
part
of
a la
rger
pat
tern
of
linea
tion
s to
the
nor
th (
LO4-
174H
1) a
nd e
ast
(LO
4-16
8H3)
.Pl
ains
-for
min
g un
its
nort
h of
the
rim
of
Ric
ciol
i, th
e so
uth-
east
floo
r of
Ric
ciol
i, an
d ab
out 8
0 km
sou
th o
f the
sou
ther
nri
m o
f R
icci
oli
are
inte
rpre
ted
as m
olte
n or
sem
imol
ten
ejec
ta fr
om O
rien
tale
.
LO4-
173H
3Su
n El
evat
ion:
15.
40°
Alt
itud
e: 2
724.
03 k
m
41
Ori
enta
leBa
sin R
egio
n
Cra
ter
Hed
in a
ppea
rs t
o be
sim
ilar
in a
ge t
o R
icci
oli.
It h
asbe
en c
over
ed w
ith
Ori
enta
le e
ject
a. T
o th
e no
rthe
ast,
jus
tbe
yond
Hed
in, t
here
is a
dep
osit
wit
h a
scal
lope
d sc
arp
that
seem
s to
hav
e co
me
from
the
sou
thea
st,
prob
ably
fro
mG
rim
aldi
. The
se d
epos
its
exte
nd b
eyon
d H
edin
to
the
east
.In
the
low
er h
alf o
f thi
s ph
oto
is a
ref
eren
ce a
rea
for
illus
tra-
tion
of
the
inne
r H
evel
ius
Form
atio
n, w
ith
its
stro
nglin
eati
ons
and
thic
k de
posi
ts o
f O
rien
tale
eje
cta.
The
upp
erri
ght
part
of
the
phot
o sh
ows
the
seco
ndar
y cr
ater
s an
dth
inne
r de
posi
ts o
f the
out
er H
evel
ius
Form
atio
n.
LO4-
174H
1Su
n El
evat
ion:
15.
50°
Alt
itud
e: 2
673.
10 k
m
42
Luna
r O
rbiter
Photo
gra
phic
Atla
s
Cle
men
tine
dat
a sh
ow G
lush
ko t
o be
the
sou
rce
of a
str
ong
ray
patt
ern,
inc
ludi
ng t
he l
ight
str
eaks
tha
t ca
n be
see
n ex
-te
ndin
g to
Car
danu
s an
d K
raff
t. G
lush
ko h
as im
pact
ed a
uni
tof
pla
ins-
form
ing
mel
t fr
om O
rien
tale
. C
rate
rs K
raff
t an
dC
arda
nus,
whi
ch a
re s
o si
mila
r in
siz
e an
d ap
pare
nt a
ge th
atth
ey m
ay h
ave
orig
inat
ed i
n a
twin
im
pact
, hav
e de
posi
ted
thei
r ej
ecta
on
an
ol
der
mar
e un
it
wit
hin
Oce
anus
Proc
ella
rum
. N
ewer
mar
e un
its
have
floo
ded
out
part
s of
thei
r fie
lds
of s
econ
dary
cra
ters
. T
he c
rate
r ch
ain
Cat
ena
Kra
fft i
s co
mpo
sed
of s
econ
dari
es fr
om c
rate
r K
raff
t.
LO4-
174H
2Su
n El
evat
ion:
15.
50°
Alt
itud
e: 2
673.
10 k
m
43
Ori
enta
leBa
sin R
egio
n
LO4-
174H
3Su
n El
evat
ion:
15.
50°
Alt
itud
e: 2
673.
10 k
m
44
Luna
r O
rbiter
Photo
gra
phic
Atla
s
Cra
ters
Str
uve,
Edd
ingt
on, a
nd R
usse
ll ar
e ri
nged
pla
ins,
old
crat
ers
flood
ed b
y m
are
lava
wit
hin
Oce
anus
Pro
cella
rum
.T
he o
uter
Hev
eliu
s Fo
rmat
ion
from
Ori
enta
le h
as l
eft
de-
posi
ts o
n th
e cr
ater
rim
s. N
ote
the
furr
ow o
n th
e w
este
rn r
imof
Rus
sell
and
the
ridg
e on
the
rim
wal
l bet
wee
n St
ruve
and
Eddi
ngto
n. T
he li
ght
area
s m
ay h
ave
been
dep
osit
ed o
n th
eflo
or o
f St
ruve
by
Ori
enta
le a
nd n
ot fl
oode
d ov
er w
ith
mar
ela
va. O
r, t
he O
rien
tale
eje
cta
may
hav
e fa
llen
on p
rece
ding
lava
flow
s.
The
str
iate
d in
ner
Hev
eliu
s Fo
rmat
ion
grad
es i
nto
the
smoo
ther
out
er d
epos
its
in th
is p
hoto
. The
se d
epos
its
som
e-ti
mes
cre
ate
smoo
th p
lain
s in
are
as o
f m
ild
pree
xist
ing
topo
grap
hy, s
uch
as c
rate
r flo
ors.
The
eje
cta
from
the
earl
ier
(Pre
-Nec
tari
an)
crat
er S
chic
kard
is
so r
ugge
d th
at i
ts f
orm
can
be s
een
belo
w t
he n
ewer
eje
cta
blan
ket.
Floo
ding
of
the
floor
of
Schi
ckar
d w
ith
lava
see
ms
to h
ave
prec
eded
dep
osit
of O
rien
tale
eje
cta.
LO4-
167H
2Su
n El
evat
ion:
17.
40°
Alt
itud
e: 3
009.
04 k
m
45
Ori
enta
leBa
sin R
egio
n
The
dar
k, s
moo
th p
lain
s ar
eas
sout
h of
Byr
gius
see
m t
o be
isol
ated
lava
lake
s, a
ssoc
iate
d w
ith
no p
arti
cula
r to
pogr
aphi
cfe
atur
es.
The
se u
nits
esc
aped
hea
vy e
ject
a fr
om O
rien
tale
,bu
t nar
row
ly: n
ote
the
long
furr
ow fr
om O
rien
tale
just
to th
eso
uth
of t
he d
ark
plai
ns a
nd t
he h
eavi
ly s
tria
ted
terr
ain
furt
her
to t
he s
outh
as
wel
l. T
he fr
esh
crat
er o
n th
e ea
st r
imof
Byr
gius
is
very
you
ng;
Cle
men
tine
alb
edo
data
sho
w a
stro
ng r
ay p
atte
rn fr
om it
, whi
ch c
an b
e se
en o
n th
e flo
or o
fB
yrgi
us a
nd b
eyon
d. S
ome
of th
ese
rays
can
be
seen
cro
ssin
gth
e da
rk p
lain
s un
it n
ear
the
righ
t ed
ge o
f th
e ph
oto.
The
floor
of P
iazz
i als
o sh
ows
a sm
all a
rea
of s
moo
th d
ark
plai
ns.
The
rem
aind
er o
f tha
t floo
r is
mas
sive
ly fi
lled
wit
h O
rien
tale
Hev
eliu
s Fo
rmat
ion
mat
eria
l an
d m
ater
ial
from
the
nor
th-
wes
tern
rim
of P
iazz
i.
LO4-
167H
3Su
n El
evat
ion:
17.
40°
Alt
itud
e: 3
009.
04 k
m
46
Luna
r O
rbiter
Photo
gra
phic
Atla
s
The
floo
r of
Lam
arck
has
bee
n co
vere
d w
ith
stri
ated
mat
eria
lfr
om O
rien
tale
. Dar
win
is in
a la
rge
regi
on o
f fau
lts a
long
the
bord
er o
f Oce
anus
Pro
cella
rum
, pre
sum
ably
str
ess
frac
ture
sre
late
d to
the
for
mat
ion
of t
hat
giga
ntic
fea
ture
. The
str
ess
may
hav
e be
en in
duce
d by
an
impa
ct fo
rmin
g a
basi
n be
low
sout
hern
Oce
anus
Pro
cella
rum
(C
hapt
er I
mbr
ium
Bas
inR
egio
n) o
r m
ay h
ave
been
ind
uced
by
subs
eque
nt m
otio
nsof
the
cru
st a
nd m
antl
e ad
just
ing
to t
he r
edis
trib
utio
n of
mas
s of
Oce
anus
Pro
cella
rum
. The
faul
ts t
end
to b
e ci
rcum
-fe
rent
ial
and
radi
al t
o th
e bo
rder
of
Oce
anus
Pro
cella
rum
.R
imae
Dar
win
are
nea
rly
circ
umfe
rent
ial.
Rim
a Si
rsal
is,
ara
dial
faul
t mor
e th
an 3
00 k
m lo
ng, h
as it
s so
uthw
este
rn te
r-m
inus
in
a ne
twor
k of
fau
lts
(Rim
ae S
irsa
lis)
inte
rspe
rsed
wit
h R
imae
Dar
win
.
LO4-
168H
1Su
n El
evat
ion:
16.
50°
Alt
itud
e: 2
722.
18 k
m
47
Ori
enta
leBa
sin R
egio
n
Div
erse
sur
face
s of
the
out
er H
evel
ius
Form
atio
n ar
e sh
own
here
. U
nder
neat
h th
is e
ject
a bl
anke
t is
top
ogra
phy
from
olde
r im
pact
s su
ch a
s th
e tw
o cr
ater
s w
hose
floo
rs h
ave
been
flood
ed a
fter
the
Ori
enta
le e
vent
to fo
rm L
acus
Aes
tati
s. T
heR
imae
Dar
win
can
be
seen
to
mod
ify
the
stri
atio
ns f
rom
Ori
enta
le, s
o th
e ri
mae
mus
t hav
e be
en fo
rmed
late
r. A
cha
r-ac
teri
stic
tex
ture
of
the
oute
r H
evel
ius
Form
atio
n is
the
pitt
ed t
erra
in f
orm
ed b
y in
tens
e ar
rays
of
seco
ndar
y cr
ater
san
d se
cond
ary
crat
er c
hain
s in
the
are
a no
rth
of C
ruge
r.C
ruge
r’s
ejec
ta b
lank
et c
over
s an
d sm
ooth
s th
e sp
rink
ling
ofO
rien
tale
sec
onda
ries
. Cru
ger
is th
eref
ore
Late
Im
bria
n. T
heflo
or o
f Cru
ger
was
late
r re
surf
aced
by
mar
e la
va.
LO4-
168H
2Su
n El
evat
ion:
16.
50°
Alt
itud
e: 2
722.
18 k
m
48
Luna
r O
rbiter
Photo
gra
phic
Atla
s
The
Gri
mal
di B
asin
is o
lder
than
Ori
enta
le, a
s ca
n be
see
n by
the
Ori
enta
le s
tria
tion
s in
its
rin
gs. H
owev
er, i
ts m
are
floor
was
form
ed a
fter
Ori
enta
le. T
he s
moo
th a
rea
to t
he n
orth
of
Gri
mal
di a
t the
rad
ius
of L
ohrm
ann
lies
betw
een
two
ring
s of
the
Gri
mal
di B
asin
(se
e LO
4-16
8H2
for
the
sout
hern
par
t of
thes
e ri
ngs
and
a si
mila
r sm
ooth
are
a be
twee
n th
em).
Thi
sar
ea m
ay h
ave
had
a te
xtur
e si
mila
r to
the
plai
ns b
etw
een
the
Mon
tes
Roo
k an
d M
onte
s C
ordi
llera
bef
ore
bein
g co
vere
dw
ith
Ori
enta
le e
ject
a. A
hea
vy lo
be o
f pla
ins
depo
sits
(pr
oba-
bly
from
Ori
enta
le)
cove
rs t
he w
este
rn r
im o
f G
rim
aldi
,cr
osse
d by
the
sou
thea
st e
nds
of t
he R
imae
Ric
ciol
i. R
imae
Hev
eliu
s an
d R
imae
Ric
ciol
i are
par
t of
the
fra
ctur
e pa
tter
nar
ound
the
rim
of O
cean
us P
roce
llaru
m. T
he fl
ower
y pa
tter
nin
the
sou
thea
st q
uadr
ant
of G
rim
aldi
is
a de
velo
pmen
tar
tifa
ct.
LO4-
168H
3Su
n El
evat
ion:
16.
50°
Alt
itud
e: 2
722.
18 k
m
49
Ori
enta
leBa
sin R
egio
n
LO4-169HSun Elevation: 17.10°Altitude: 2672.11 km
Where Oceanus Procellarum meetshighlands, the younger mare invadeslow-lying parts of the older highlandsjust as water meets a shoreline on Earth.Ejecta and secondaries from Krafft andCardanus overlie the mare, so they areyounger yet.
The lava flooding Eddington is ofvery low viscosity; it finds its way intoevery crevice. The flow may be not onlyhorizontal but may also seep up frombelow, through the fractured rock of thecrater floor.
The bright rays come from Coper-nican crater Glushko (LO4-174H2).
The linear trough just east of Hedin(radial to Orientale) terminates in aplains deposit, as if the trough wereplowed by a body of material that was(or became) molten. The long fault that crosses the floor of Hevelius andextends nearly to the rim of Riccioli hasa graben form (flat floor) in the high-lands outside of Hevelius, but is nar-rower (a rille) as it crosses the craterfloor at a lower elevation; this is whatone would expect of a fracture zone thathas a V shape in the vertical plane.
50
Luna
r O
rbiter
Photo
gra
phic
Atla
s
Schi
ller
is a
rar
e el
onga
te c
rate
r. I
f it
was
form
ed b
y im
pact
,it
mus
t ha
ve b
een
by a
sm
all n
umbe
r of
pri
mar
y im
pact
ors
arri
ving
at
a sh
allo
w i
mpa
ct a
ngle
, pe
rhap
s as
low
as
3°.
Schi
ller
is m
ostl
y in
the
tro
ugh
betw
een
two
rais
ed r
ings
of
the
Pre-
Nec
tari
an S
chill
er-Z
ucch
ius
Bas
in.
Ori
enta
le e
ject
aha
s im
pact
ed m
are
that
has
floo
ded
this
bas
in b
efor
e th
eO
rien
tale
im
pact
. C
rate
rs W
eige
l, R
ost,
and
Nog
gera
th a
reex
ampl
es o
f ol
d cr
ater
s th
at h
ave
rece
ived
im
pact
s on
the
irri
ms.
Not
e th
e m
anne
r in
whi
ch th
e im
pact
s ca
use
the
crat
erw
alls
to c
olla
pse
onto
the
crat
er fl
oor.
LO4-
160H
1Su
n El
evat
ion:
17.
30°
Alt
itud
e: 3
012.
04 k
m
51
Ori
enta
leBa
sin R
egio
n
The
lig
hter
mat
eria
l in
the
int
erio
r of
cra
ter
Schi
ckar
d is
map
ped
as O
rien
tale
pla
ins-
form
ing
mat
eria
l lik
e th
at o
n th
eflo
or o
f War
gent
in a
nd P
hocy
lides
(LO
4-17
2H1)
. The
dar
ker
mat
eria
l in
side
Sch
icka
rd i
s m
appe
d as
mar
e ba
salt
, whi
chap
pear
s to
pre
date
the
pla
ins-
form
ing
mat
eria
l. Le
hman
nw
as fo
rmed
in th
e sa
me
peri
od a
s Sc
hick
ard
and
was
ove
rrun
by th
e pl
ains
-for
min
g m
ater
ial.
LO4-
160H
2Su
n El
evat
ion:
17.
30°
Alt
itud
e: 3
012.
04 k
m
52
Luna
r O
rbiter
Photo
gra
phic
Atla
s
Sout
hwes
t of
Vie
ta is
an
irre
gula
r la
ke o
f da
rk m
are
mat
er-
ial,
the
wes
tern
mos
t m
embe
r of
a c
ircu
lar
patt
ern
of s
uch
feat
ures
(se
e C
hapt
er 6
). T
hese
lake
s ar
e si
mila
r to
tho
se i
nth
e ri
ngs
of t
he O
rien
tale
Bas
in, s
uch
as L
acus
Ver
itas
and
Lacu
s A
utum
nis.
How
ever
, the
re is
no
cent
ral d
epre
ssio
n or
mar
e un
it w
ithi
n th
is m
yste
riou
s ri
ng o
f la
kes.
The
are
aar
ound
the
m a
ppea
rs t
o be
cov
ered
wit
h pl
ains
-for
min
gm
ater
ial o
f the
out
er H
evel
ius
Form
atio
n.
LO4-
160H
3Su
n El
evat
ion:
17.
30°
Alt
itud
e: 3
012.
04 k
m
53
Ori
enta
leBa
sin R
egio
n
LO4-161HSun Elevation: 16.50°Altitude: 2722.66 km
This chaotic region has been overlaid by ejecta from the Grimaldi Basin andthen by the Orientale Basin. Damoiseauappears to have been mostly floodedwith a heavy, viscous material, probablymolten or semimolten material fromOrientale. Some of this material hasbackflowed over and down the north-east crater wall. The lowest part of thefloor may have been flooded with marelike the flat-floored craters nearby. Thefloor material has fractured because ofthe cooling of the molten material.
Rimae Grimaldi and Rimae Sirsalisare part of the fracture pattern aroundthe border of Oceanus Procellarum.They can be seen to cross and modifythe secondary craters of Orientale, es-tablishing their younger age. The mainrima of the Sirsalis feature is the longestsuch feature on the Moon, leaving its mark on crater floors, rims, andejecta until it disappears into OceanusProcellarum (LO4-156H2). It is overlaidonly by the youngest crater in its path,the 13-km crater just to the south ofcrater Sirsalis.
The 22-km crater on the east rim ofByrgius is Copernican, with an exten-sive ray field. Some of these rays can beseen extending eastward. Henry Frereshas a slumped wall, possibly caused bythe impact that caused the 8-km youngcrater in its floor.
54
Luna
r O
rbiter
Photo
gra
phic
Atla
s
6.1. OverviewBasins, Maria, and HighlandsFigure 6.1 shows the Humorum Basin Region. The HumorumBasin is of the Nectarian Period, younger than the NubiumBasin and older than the Orientale Basin. It is sufficientlydistant from later basins that it has not been extensivelymodified, except by mare flooding of its floor and outer
trough. Its neighboring basins have been more modified,partly by Humorum itself. The highland regions to the south-east are relatively isolated from basins and preserve theheavily cratered surface of the crust. One would like to saythat they are “pristine” highlands, but in consideration of thefact that the highland surface is formed from intense crateringbombardment, that term is misleading. The point is that thishighland area has not been covered by such a heavy layer ofbasin ejecta that earlier cratering events have been obscured.
Chapter 6
Humorum Basin Region
Figure 6.1. LO4-137M. The Humorum Basin Region, the middle and lower area of this photo, includes the multi-ringed Humorum Basin itself, the NubiumBasin to the east, southern Oceanus Procellarum to the north, and the heavily cratered highland area to the south. The bright-rayed crater Tycho is also withinthis highland region. Northeast of the Humorum Basin Region is the Imbrium Basin and the bright craters (left to right) Aristarchus, Kepler, and Copernicus.
55
Hum
oru
mBa
sin R
egio
n
The juxtaposition of so many basins in the vicinity ofOceanus Procellarum has allowed rising mare lava to form anearly continuous sea, interrupted only by the rims of basinsand craters. The extent of this mare material is clear in theClementine albedo map of Figure 6.2.
The albedo map distinguishes between the bright crustmaterial, the dark mare material from the upper mantle, andthe rays, which are newly exposed crust material thrown outfrom young craters. The rays will darken with exposure tothe solar wind, which frees metallic iron from the surfacemineral grains in a process known as maturing. Rays fromimpacts into highlands that fall on mare are different in com-
position than mare, so the brightness contrast persists longafter maturing (Hawke, 2004). In additional time, gardeningby subsequent crater bombardment will cause the ray mater-ial to blend with the mare surface as well.
Apollo LandingsApollo 12, the second mission of humans on the Moon, ex-plored and returned samples from a shallow mare surface ofsoutheast Oceanus Procellarum (LO4-125H3). The missionconfirmed the character of maria established for MareTranquillitatis by Apollo 11. However, this mare proved tobe 500 million years younger and much richer in KREEP.Some samples appear to be from rays of Copernicus andestablish the time of that impact as 810 million years ago.
Apollo 12 landed within walking distance of Surveyor 3,establishing a new level of landing accuracy that permittedfuture missions to be targeted for even more interestinglanding sites. Parts of Surveyor 3 were returned to Earth andexamined for the character and rate of micrometeoroidimpacts.
Apollo 14 explored and sampled a geologic structurecalled the Fra Mauro Formation (LO4-120H3). The FraMauro Formation is material ejected from the ImbriumBasin. The samples, together with samples from Apollo 15,establish the time of the Imbrian impact as 3.85 billion yearsago. Other samples returned by Apollo 14 are older, in therange of 3.87 to 3.96 billion years, and may come fromimpacts in the subsurface below the Imbrian ejecta.
6.2. High-Resolution ImagesTable 6.1 shows the high-resolution images of the HumorumBasin Region in schematic form.
The following pages show the high-resolution subframesfrom south to north and west to east; that is, they are in theorder LO4-155H2, LO4-155H3, LO4-156H, LO4-148H1…LO4-108H3.
Subframes LO4-155H1, LO4-142H1, LO4-131H1, LO4-119H1, and LO4-107H1 are not included in print becausethey are redundant with adjacent exposures to the east andwest (they are included in the enclosed CD). The subframesof exposures 156H, 132H, and 113H have each been com-bined into full rectangular images.
56
Luna
r O
rbiter
Photo
gra
phic
Atla
s Figure 6.2. Clementine albedo display of the Humorum region. The floorsof the basins in this region are flooded with dark mare material. MareHumorum is left and above the center of the image and Mare Nubium is tothe upper right. Oceanus Procellarum is near the top of the image. Tycho’sbright ray pattern can be seen across both highland and mare surfaces. Thisis a section of the PIGWAD1 Mercator projection; the center of this figure isat 30° west longitude and 30° south latitude and the squares are 30° on aside. Sources: NRL and USGS, with permission.
Latitude Range Photo Number
0–27 N 162 157 150 144 138 133 126 121 114 109 102
0–27 S 161 156 149 143 137 132 125 120 113 108 101
27 S–56 S 160 155 148 142 136 131 124 119 112 107 100
56 S–90 S 154 130 118 106 094
Table 6.1. The cells shown in white represent the high-resolution photos of the Humorum Basin Region (LO4-XXX H1, -H2, and -H3, where XXX is thePhoto Number). The Orientale Basin Region is to the west, the Imbrium Basin Region is to the north, the Eastern Basins Region is to the northeast, theNectaris Basin Region is to the east, and the South Polar Region is to the south.
Longitude 62 W 58 W 49 W 41 W 35 W 30 W 23 W 16 W 10 W 3 W 4 Eat Equator
1 Planetary Interactive G.I.S.-on-the-Web Analyzable Database(USGS)
The
rid
ge i
n th
e lo
wer
rig
ht c
orne
r of
thi
s ph
oto
radi
ates
from
the
Sch
ille
r-Z
ucch
ius
Bas
in.
Subt
le s
tria
tion
s in
the
uppe
r le
ft r
adia
te fr
om O
rien
tale
.
LO4-
155H
2Su
n El
evat
ion:
17.
1°A
ltit
ude:
301
1.10
km
57
Hum
oru
mBa
sin R
egio
n
The
str
iati
ons
and
crat
er c
hain
s th
roug
h V
ieta
and
Fou
rier
are
radi
al t
o O
rien
tale
. T
he b
righ
tnes
s in
the
vic
init
y of
Four
ier
is d
ue t
o ra
ys f
rom
sm
all
prim
ary
crat
ers
of t
heC
oper
nica
n Pe
riod
. T
here
are
at
leas
t fo
ur;
one
is o
n th
eno
rthe
ast r
im o
f Vie
ta a
nd th
e ot
hers
are
abo
ut 5
0 km
nor
thof
Fou
rier
, ab
out
35 k
m n
orth
east
of
Four
ier,
and
abo
ut
35 k
m s
outh
east
of
Four
ier.
The
ir r
ay p
atte
rns
are
show
ncl
earl
y in
alb
edo
data
from
the
Cle
men
tine
mis
sion
.
LO4-
155H
3Su
n El
evat
ion:
17.
1°A
ltit
ude:
301
1.10
km
58
Luna
r O
rbiter
Photo
gra
phic
Atla
s
LO4-156HSun Elevation: 16.6°Altitude: 2721.57 km
This frame shows the transitionbetween the highlands and southernOceanus Procellarum. The linearfeature that runs southeast fromHermann is an example of a wrinkleridge, also known as a mare ridge; suchfeatures often appear in a large maresurface. Their origin is unclear, but it may be related to cooling andsolidification of the lava.
As is common along the “shore” ofOceanus Procellarum, radial fracturesare revealed by rimae (rilles) at thesurface. Flooding by lava, cooling, andpossible isostatic adjustment are likelysources of the fracturing.
Note the 80-km buried crater at the edge of Oceanus Procellarum nearRimae Sirsalis; only part of its rimremains visible, like the smile of the Cheshire Cat. Striations betweenFontana and the mare support thehypothetical basin under southernOceanus Procellarum, as discussed inthe introduction to the chapter on theImbrium Basin Region (Chapter 7).
59
Hum
oru
mBa
sin R
egio
n
The
furr
ow a
nd r
idge
run
ning
nor
thea
st o
f Sch
eine
r is
pro
b-ab
ly e
ject
a fr
om t
he S
chill
er-Z
ucch
ius
Bas
in.
Sim
ilar,
les
spr
onou
nced
line
ar f
eatu
res
run
para
llel t
o th
e fu
rrow
in t
hem
iddl
e pa
rt o
f the
pic
ture
. Eje
cta
from
Cla
vius
par
tly o
verl
ies
the
furr
ow. T
he fl
oor
of th
e fu
rrow
is v
ery
flat a
nd s
moo
th; i
tm
ay b
e th
e re
sult
of
mol
ten
mat
eria
l in
the
bas
in e
ject
a.B
ayer
is
a co
ncen
tric
rin
g cr
ater
tha
t m
ay h
ave
pene
trat
edth
roug
h th
e Sc
hille
r-Z
ucch
ius
ejec
ta l
ayer
int
o m
ore
prim
i-ti
ve te
rrai
n be
low
.
LO4-
148H
1Su
n El
evat
ion:
17.
9°A
ltit
ude:
300
9.38
km
60
Luna
r O
rbiter
Photo
gra
phic
Atla
s
The
deg
rade
d st
ate
of M
ee in
dica
tes
that
it is
a r
elat
ivel
y ol
d,Pr
e-N
ecta
rian
cra
ter.
The
eje
cta
blan
ket
in t
he l
ower
rig
htha
lf of
the
phot
o ha
s be
en d
epos
ited
by
the
Hum
orum
Bas
into
the
nor
th. C
hain
s of
sm
all s
econ
dary
cra
ters
rad
iate
from
the
Ori
enta
le B
asin
far
to th
e no
rthw
est.
LO4-
148H
2Su
n El
evat
ion:
17.
9°A
ltit
ude:
300
9.38
km
61
Hum
oru
mBa
sin R
egio
n
Thi
s pi
ctur
e fe
atur
es a
n un
usua
l ran
ge o
f fea
ture
type
s. L
acus
Exce
llent
iae
is p
art o
f a r
ing
of m
are
lake
s in
a tr
ough
of t
heH
umor
um B
asin
. A
n ou
ter
ring
of
Hum
orum
can
be
seen
pass
ing
betw
een
Four
ier
and
Cla
usiu
s, in
terr
upte
d by
val
leys
blas
ted
by H
umor
um e
ject
a. R
imae
Pal
mie
ri a
nd R
imae
Dop
pelm
ayer
are
exa
mpl
es o
f the
rad
ial a
nd c
ircu
mfe
rent
ial
stre
ss fr
actu
res
near
the
edge
of M
are
Hum
orum
, who
se e
dge
can
be s
een
in th
e up
per
righ
t.
LO4-
148H
3Su
n El
evat
ion:
17.
9°A
ltit
ude:
300
9.38
km
62
Luna
r O
rbiter
Photo
gra
phic
Atla
s
Thi
s pi
ctur
e ill
ustr
ates
the
str
uctu
re o
f th
e H
umor
um B
asin
. The
inne
r ba
sin
has
been
floo
ded
wit
h la
va. R
upes
Lie
big
(rup
es m
eans
a s
carp
, a c
liff)
may
have
bee
n fo
rmed
as
lava
ros
e pa
rtw
ay a
cros
s th
e sh
elf (
whi
ch m
ay h
ave
been
sim
ilar
to t
he M
aund
er F
orm
atio
n of
Ori
enta
le)
and
then
sub
side
d as
the
sour
ce p
lum
e re
laxe
d. A
s of
ten
is t
he c
ase
whe
re a
mar
e ha
s a
thin
edg
e, t
he
63
Hum
oru
mBa
sin R
egio
n
LO4-
149H
1Su
n El
evat
ion:
17.
5°A
ltit
ude:
272
0.28
km
shel
f is
cove
red
wit
h da
rk p
lain
s-fo
rmin
g m
ater
ial.
The
topo
grap
hic
ring
sur
-ro
unds
Mar
e H
umor
um w
est o
f thi
s fla
t pla
in. A
trou
gh o
utsi
de th
is fi
rst r
idge
has
been
par
tly
flood
ed w
ith
lava
. A s
econ
d ci
rcum
fere
ntia
l rid
ge, l
ower
and
less
con
tinu
ous
than
the
firs
t, lie
s ou
tsid
e th
e tr
ough
. Mos
t of
the
rim
a fe
a-tu
res
reve
al s
tres
s fa
ults
from
the
mar
e flo
odin
g an
d co
olin
g pr
oces
ses.
It h
as b
een
sugg
este
d th
at M
ons
Han
stee
n co
uld
be a
n Ea
rth-
styl
e vo
lcan
o (i
tlo
oks
muc
h lik
e M
t. Fu
ji, fo
r ex
ampl
e). H
owev
er, t
hat w
ould
req
uire
a s
ourc
eof
hig
h-vi
scos
ity
lava
onl
y a
few
kilo
met
ers
away
fro
m B
illy,
whi
ch h
as b
een
flood
ed w
ith
typi
cal l
ow-v
isco
sity
lava
. Ano
ther
exp
lana
tion
wou
ld b
e th
at it
isa
rem
nant
of
an in
teri
or b
asin
rin
g (l
ike
Mon
tes
Roo
k, w
hich
is r
ich
in s
uch
pyra
mid
al b
lock
s).
64
Luna
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
149H
2Su
n El
evat
ion:
17.
5°A
ltit
ude:
272
0.28
km
Thi
s is
the
sout
heas
t sec
tion
of O
cean
us P
roce
llaru
m. M
any
furt
her
pict
ures
of
this
gig
anti
c m
are
are
cove
red
in t
he c
hapt
er o
n th
e Im
briu
m B
asin
(C
hapt
er7)
. Int
eres
ting
feat
ures
of t
his
pict
ure
are
the
segm
ents
of c
rate
r w
alls
that
hav
esu
rviv
ed i
nund
atio
n by
the
mar
e la
va. S
ome
of t
he w
alls
are
so
high
tha
t it
seem
s th
at t
he m
issi
ng s
egm
ents
mus
t ha
ve m
elte
d in
to t
he m
are
floor
. The
righ
t sid
e of
this
pic
ture
con
tain
s la
rge
swir
ls o
f dev
elop
men
t bub
bles
.
65
Hum
oru
mBa
sin R
egio
n
LO4-
149H
3Su
n El
evat
ion:
17.
5°A
ltit
ude:
272
0.28
km
Thi
ck e
ject
a an
d se
cond
ary
crat
ers
of t
he H
umor
um B
asin
cove
r th
is a
rea.
Thi
s te
rrai
n is
cal
led
the
Vit
ello
For
mat
ion
(cra
ter
Vit
ello
is
in L
O4-
142H
3); i
t is
the
equ
ival
ent
of t
heH
evel
ius
Form
atio
n of
the
Ori
enta
le B
asin
or
the
Fra
Mau
roFo
rmat
ion
of t
he I
mbr
ium
Bas
in.
The
tw
o Er
atos
then
ian
crat
ers
that
obs
cure
Hai
nzel
may
hav
e la
nded
ess
enti
ally
sim
ulta
neou
sly,
as
indi
cate
d by
the
stra
ight
seg
men
t bet
wee
nth
em. H
ainz
el h
ad a
lrea
dy b
een
form
ed w
hen
they
lan
ded,
alth
ough
the
inte
rval
may
hav
e be
en s
hort
.
66
Luna
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
142H
2Su
n El
evat
ion:
19.
5°A
ltit
ude:
300
6.60
km
One
rin
g of
Hum
orum
pas
ses
thro
ugh
or n
ear
Vit
ello
.A
noth
er,
prob
ably
the
hig
hest
rin
g, p
asse
s ju
st n
orth
of
Lacu
s Ex
celle
ntia
e, w
hich
floo
ds a
tro
ugh
exte
rnal
to
that
ring
. T
he m
ater
ial
on t
he fl
oor
of V
itel
lo a
ppea
rs t
o ha
vebe
en m
olte
n be
fore
har
deni
ng a
nd t
hen
frac
turi
ng,
very
muc
h lik
e K
opff
in
Ori
enta
le (
LO4-
187H
2). D
oppe
lmay
er i
ssl
ante
d; i
t m
ay h
ave
form
ed p
artl
y on
the
bas
in fl
oor
and
part
ly o
n a
terr
ace
or s
callo
p of
the
rim
. As
a re
sult
, it i
s on
lypa
rtly
floo
ded.
If
Puis
eux
was
floo
ded
thro
ugh
a ve
ry s
mal
lbr
eak
in it
s no
rthe
rn r
im (
and
not f
rom
bel
ow),
the
visc
osit
yof
the
lava
mus
t hav
e be
en v
ery
low
to s
prea
d ev
enly
ove
r th
ecr
ater
floo
r.
LO4-
142H
3Su
n El
evat
ion:
19.
5°A
ltit
ude:
300
6.60
km
67
Hum
oru
mBa
sin R
egio
n
Alt
houg
h th
e H
umor
um B
asin
doe
s no
t app
ear
to b
e as
larg
eas
the
Ori
enta
le B
asin
, th
e ce
ntra
l m
are
is a
bout
the
sam
esi
ze, p
roba
bly
beca
use
the
crus
t is
thi
nner
in t
he H
umor
umre
gion
. As
a re
sult
, the
inne
r de
tail
and
perh
aps
inne
r ri
ngs
are
lost
bec
ause
of t
he fl
oodi
ng o
f lav
a. In
stea
d th
ere
is a
ver
ysm
ooth
, but
not
feat
urel
ess,
sur
face
. The
sca
rp a
t the
wes
tern
edge
of
the
mar
e (R
upes
Lie
big)
sug
gest
s th
at t
he m
are
surf
ace
rose
to
a le
vel
high
er t
han
its
pres
ent
elev
atio
n an
d th
en s
ubsi
ded
a bi
t, pa
rtly
as
a re
sult
of
cont
ract
ion
onco
olin
g. S
tres
ses
indu
ced
by t
he s
ubsi
denc
e fin
d su
rfac
e ex
-pr
essi
on i
n R
imae
Dop
pelm
ayer
and
wri
nkle
rid
ges
such
as
the
one
near
the
left
edg
e of
the
pic
ture
. The
bri
ght
stre
aks
acro
ss th
e m
are
are
rays
from
Tyc
ho.
68
Luna
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
143H
1Su
n El
evat
ion:
18.
8°A
ltit
ude:
271
9.10
km
Gas
send
i w
as f
orm
ed b
y an
im
pact
pre
cise
ly o
n th
e sc
arp
boun
ding
Mar
e H
umor
um. I
ts fl
oor,
slig
htly
low
er t
han
the
near
by la
va s
urfa
ce, a
ppea
rs to
hav
e be
en a
mel
t she
et, h
eavi
lyfr
actu
red
upon
coo
ling
or is
osta
tic a
djus
tmen
t. A
nea
rly
con-
tinuo
us r
im h
as p
rote
cted
it fr
om fl
oodi
ng w
ith la
va e
xcep
t for
a sm
all b
reac
h in
the
sou
ther
n ri
m, w
hich
has
allo
wed
som
ela
va t
o en
ter
a se
ctor
of
the
floor
. The
floo
r of
Gas
send
i ha
sbe
en h
eavi
ly fr
actu
red,
pos
sibl
y by
upw
ard
pres
sure
of l
ava
ona
mel
t sh
eet.
Letr
onne
has
bee
n fu
lly b
reac
hed
and
flood
edfr
om th
e no
rth
by O
cean
us P
roce
llaru
m.
LO4-
143H
2Su
n El
evat
ion:
18.
8°A
ltit
ude:
271
9.10
km
69
Hum
oru
mBa
sin R
egio
n
The
cro
ss m
arks
the
June
196
6 la
ndin
g of
Sur
veyo
r 1,
who
seso
ft la
ndin
g co
nfirm
ed th
e sa
fe b
eari
ng s
tren
gth
of th
e lu
nar
soil,
pre
viou
sly
affir
med
by
Luna
9. T
he S
urve
yor
1 ca
mer
ash
owed
the
loc
al s
urfa
ce t
o be
flat
, w
ith
boul
ders
nea
r a
crat
er i
n th
e di
stan
ce. S
urve
yor
1 la
nded
in
a re
mna
nt o
f a
crat
er r
im le
ft b
ehin
d by
an
inun
date
d “g
host
cra
ter,
” in
for-
mal
ly c
alle
d th
e Fl
amst
eed
ring
. Dor
sa R
ubey
is a
n ex
ampl
eof
a w
rink
le r
idge
, a
com
mon
fea
ture
of
mar
e su
rfac
es.
Asm
alle
r ri
dge
form
s an
inte
rior
rin
g w
ithi
n th
e ve
stig
ial r
imof
the
Flam
stee
d ri
ng.
70
Luna
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
143H
3Su
n El
evat
ion:
18.
8°A
ltit
ude:
271
9.10
km
Cla
vius
, at
225
km i
n di
amet
er, i
s in
a t
rans
itio
n re
gion
bet
wee
n cr
ater
s an
dba
sins
. T
he r
im s
how
s m
ulti
ple
colla
pse
feat
ures
, pr
esen
ting
a s
callo
ped
appe
aran
ce. T
he p
eak
stru
ctur
e is
com
plex
, an
inte
rmed
iate
ste
p to
an
inne
rri
ng. T
he s
trea
ks o
n th
e flo
or o
f C
lavi
us a
nd L
ongo
mon
tanu
s ar
e ra
ys f
rom
Tyc
ho. P
orte
r ha
s hi
t the
nor
thea
ster
n co
rner
of C
lavi
us, p
iling
the
mat
eria
l of
the
rim
of C
lavi
us n
eatly
to th
at s
ide.
71
Hum
oru
mBa
sin R
egio
n
LO4-
136H
1Su
n El
evat
ion:
19.
2°A
ltit
ude:
300
2.96
km
The
gou
ges
in t
he n
orth
ern
rim
of
Long
omon
tanu
s ar
e fr
om t
he d
irec
tion
of
the
Nub
ium
and
Im
briu
m B
asin
s an
d ar
e lik
ely
to b
e se
cond
arie
s fr
om o
ne
of th
ose
basi
ns. T
he fo
rmat
ion
of th
e go
uges
sug
gest
s th
at th
e in
cide
nce
angl
eof
the
sec
onda
ry im
pact
ors
was
abo
ut t
he s
ame
as t
he a
ngle
of t
he r
im b
efor
eim
pact
. The
val
ley
of L
acus
Tim
oris
may
hav
e be
en g
ouge
d ou
t by
ejec
ta fr
omth
e H
umor
um B
asin
.
72
Luna
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
136H
2Su
n El
evat
ion:
19.
2°A
ltit
ude:
300
2.96
km
Palu
s Ep
idem
iaru
m m
ay b
e si
mila
r to
the
lak
es i
n th
e tr
ough
rin
g ar
ound
basi
ns, s
impl
y an
unu
sual
ly la
rge
area
of m
are
in th
e tr
ough
. Lav
a fr
om P
alus
Epid
emia
rum
see
ms
to h
ave
flow
ed i
nto
Mar
e H
umor
um t
hrou
gh a
sin
uous
chan
nel t
hat p
asse
s th
roug
h a
valle
y in
the
ring
that
bou
nds
Mar
e H
umor
um.
73
Hum
oru
mBa
sin R
egio
n
LO4-
136H
3Su
n El
evat
ion:
19.
2°A
ltit
ude:
300
2.96
km
The
rad
ial a
nd c
ircu
mfe
rent
ial R
imae
Ram
sden
are
typ
ical
of
the
surf
ace
fea-
ture
s ov
erly
ing
stre
ss f
ract
ures
nea
r th
e ed
ge o
f m
aria
. R
upes
Kel
vin
is t
hebo
unda
ry o
f th
e ri
ng t
hat
boun
ds M
are
Hum
orum
; thi
s ri
ng is
sim
ilar
to t
heou
ter
rang
e of
Mon
tes
Roo
k. A
noth
er h
ighe
r ri
ng p
asse
s th
roug
h C
apua
nus.
Wri
nkle
rid
ges
(dor
sa)
such
as
thos
e in
the
mid
dle
of t
his
pict
ure
ofte
n ap
pear
on
mar
e su
rfac
es.
Her
e th
ey f
orm
ase
ries
of
circ
umfe
rent
ial
ridg
es.
The
y co
uld
have
bee
nfo
rmed
by
extr
usio
n of
the
mar
e la
va a
long
cra
cks
in t
heco
oled
and
har
dene
d su
rfac
e. S
carp
s in
the
mar
e su
rfac
e(b
etw
een
the
ridg
es a
nd t
he r
im)
indi
cate
tha
t th
e di
rect
ion
of lo
w-v
isco
sity
lava
flow
ed fr
om th
e ce
nter
tow
ard
the
edge
of th
e m
are.
74
Luna
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
137H
1Su
n El
evat
ion:
18.
8°A
ltit
ude:
271
8.01
km
Thi
s ph
oto
show
s a
brea
ch in
the
rim
of M
are
Hum
orum
that
allo
wed
the
mar
e su
rfac
e to
con
nect
wit
h th
at o
f O
cean
usPr
ocel
laru
m i
n th
e no
rthe
ast
corn
er o
f th
is p
hoto
. Per
haps
the
lava
ros
e w
ithi
n M
are
Hum
orum
to
a po
int
whe
re i
tov
erflo
wed
the
wal
l an
d op
ened
the
bre
ach.
The
dar
ker
(you
nger
?) s
urfa
ce o
f M
are
Hum
orum
see
ms
to h
ave
ex-
tend
ed t
hrou
gh t
he b
reac
h to
war
d O
cean
us P
roce
llaru
m.
Scar
ps in
dica
ting
flow
bou
ndar
ies
and
the
sinu
ous
chan
nels
of R
imae
Her
igon
ius
may
be
rela
ted
to th
e m
ovem
ent o
f lav
afr
om M
are
Hum
orum
int
o (o
r on
to)
Oce
anus
Pro
cella
rum
.D
orsa
Ew
ing
and
othe
r ne
arby
wri
nkle
rid
ges
may
be
rela
ted
to u
nder
lyin
g to
pogr
aphy
; the
mar
e is
sha
llow
her
e (s
ee t
hegh
ost c
rate
rs in
LO
4-13
7H3)
.
75
Hum
oru
mBa
sin R
egio
n
LO4-
137H
2Su
n El
evat
ion:
18.
8°A
ltit
ude:
271
9.10
km
The
re w
as p
roba
bly
an e
ject
a bl
anke
t fr
om t
he H
umor
um B
asin
her
e, b
ut i
tw
as c
over
ed b
y th
e m
are
surf
ace
of O
cean
us P
roce
llaru
m,
just
as
it n
earl
yer
ased
the
larg
e “g
host
” cr
ater
s.
76
Luna
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
137H
3Su
n El
evat
ion:
18.
8°A
ltit
ude:
271
9.10
km
The
str
iati
ons
betw
een
Hai
ding
er a
nd H
eins
ius
are
ejec
ta fr
om th
e H
umor
umB
asin
, si
mil
ar i
n na
ture
to
the
inne
r H
evel
ius
Form
atio
n of
the
Ori
enta
leB
asin
. Cra
ter
chai
ns in
Wilh
elm
are
rad
ial t
o bo
th t
he N
ubiu
m B
asin
and
the
mor
e re
mot
e Im
briu
m B
asin
. Thi
s ar
ea is
als
o ov
erla
in w
ith
rays
from
Tyc
ho.
77
Hum
oru
mBa
sin R
egio
n
LO4-
131H
2Su
n El
evat
ion:
19.
5°A
ltit
ude:
299
9.00
km
The
dee
per
(sm
ooth
er, r
elat
ivel
y fe
atur
eles
s) p
art o
f Pal
us E
pide
mia
rum
is th
ela
rges
t of a
set
of s
mal
l tra
cts
of m
are
form
ed in
a tr
ough
rin
g of
the
Hum
orum
Bas
in. I
ts s
ize
may
be
influ
ence
d by
an
inte
rsec
tion
of
the
Hum
orum
tro
ugh
wit
h an
ear
lier
trou
gh o
f th
e N
ubiu
m B
asin
. Alt
houg
h th
ese
smal
l mar
e un
its
coul
d al
l be
term
ed “
lacu
s” (
lake
), th
e ex
tens
ion
of P
alus
Epi
dem
iaru
m to
the
78
Luna
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
131H
3Su
n El
evat
ion:
19.
5°A
ltit
ude:
299
9.00
km
sout
heas
t ap
pear
s to
be
rela
tive
ly s
hallo
w,
so t
his
feat
ure
has
been
nam
ed“p
alus
” (s
wam
p). R
upes
Mer
cato
r is
par
t of
the
deg
rade
d ri
m o
f th
e N
ubiu
mB
asin
. Mer
cato
r ha
s im
pact
ed th
is r
im, a
nd th
en s
omew
hat l
ater
Cam
panu
s as
wel
l. T
he r
elat
ive
ages
of C
ampa
nus
and
Mer
cato
r ar
e in
dica
ted
by th
e “w
orn-
away
” ap
pear
ance
of M
erca
tor
and
its
ejec
ta.
LO4-132HSun Elevation: 18.9°Altitude: 2717.39 km
Montes Riphaeus is a remnant of veryold crust. It may be an arc of the rim of a large crater containing MareCognitum. The intersecting ray patternscome from Copernicus to the northeastand Kepler to the northwest. The small,sharp, rayed craters such as Euclidescould be secondaries from Copernicus.
In the lower left of this picture, thedark mare is probably in a trough of theHumorum Basin. The remains of anouter ring appear as an island above it.
Rimae Hippalus are nearly concentricwith the Humorum Basin, but theytrend outward toward the north insteadof curving around to the northwest.Rima Agatharchides is part of the totalsystem of rimae, which is influenced byMare Humorum and Mare Nubium andthe underlying basin structures. Theserimae traverse older features like therim of Hippalus, but are interrupted by newer craters such as the one about30 km southeast of Hippalus. The ejectafrom the newer craters fills in the rimae.The bounding ring of the HumorumBasin has been suppressed here, pos-sibly because of interactions with thepreexisting ring and melt sheet of theNubium Basin.
79
Hum
oru
mBa
sin R
egio
n
Whi
ch c
ame
first
, Cla
vius
or
Mag
inus
? T
he r
elev
ant
brig
ht-
ness
of t
he fl
oor
of M
agin
us is
due
to it
s pr
oxim
ity
to T
ycho
,so
tha
t is
not
a c
lue.
It
is d
iffic
ult
to s
ee s
tron
g ev
iden
cew
heth
er t
he e
ject
a of
Cla
vius
ove
rlie
s th
at o
f Mag
inus
or
the
reve
rse,
pos
sibl
y be
caus
e of
the
ove
rbur
den
of e
ject
a fr
omnu
mer
ous
othe
r cr
ater
s an
d ba
sins
. M
agin
us s
how
s m
ore
crat
erin
g ar
ound
its
rim
tha
n C
lavi
us.
Thi
s es
tabl
ishe
s a
sign
ifica
ntly
old
er a
ge fo
r M
agin
us, w
hich
is m
appe
d as
Pre
-N
ecta
rian
whe
reas
Cla
vius
is m
appe
d as
Nec
tari
an. S
tria
tion
son
the
rim
of M
agin
us in
the
dire
ctio
n of
Cla
vius
are
map
ped
as e
ject
a fr
om C
lavi
us.
80
Luna
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
124H
1Su
n El
evat
ion:
19.
9°A
ltit
ude:
299
4.47
km
The
floo
r, r
im, a
nd r
ays
of T
ycho
are
ver
y br
ight
, ind
icat
ing
its
youn
g ag
e (C
oper
nica
n Pe
riod
). C
onse
quen
tly,
the
re h
asno
t be
en t
ime
for
sign
ifica
nt d
egra
dati
on o
f it
s to
pogr
aphy
.T
he c
entr
al p
eak
is t
ypic
al o
f cr
ater
s of
thi
s si
ze, f
orm
ed o
fm
ater
ial t
hrow
n di
rect
ly u
pwar
d by
the
com
pres
sion
al s
hock
wav
e re
boun
ding
from
ori
gina
l cru
st b
elow
the
bou
ndar
y of
frac
ture
d cr
ater
mat
eria
l. Su
rvey
or 7
was
bol
dly
targ
eted
for
the
fres
h ej
ecta
fro
m T
ycho
, la
ndin
g in
Jan
uary
196
8. T
heSu
rvey
or 7
cam
era
show
ed a
sur
face
of b
lock
s up
to
a m
eter
in s
ize.
The
sur
face
was
rou
ghly
tex
ture
d, b
ut w
ith
few
ercr
ater
s th
an w
ere
seen
in
the
mar
e la
ndin
g si
tes.
The
low
erra
te o
f cra
teri
ng r
esul
ts fr
om th
e yo
ung
age
of th
e te
rrai
n.
LO4-
124H
2Su
n El
evat
ion:
19.
9°A
ltit
ude:
299
4.47
km
81
Hum
oru
mBa
sin R
egio
n
The
Nub
ium
Bas
in is
muc
h ol
der
than
the
Hum
orum
Bas
in.
Exte
nsiv
e flo
odin
g, i
nflue
nced
by
its
prox
imit
y to
Oce
anus
Proc
ella
rum
, has
hid
den
muc
h of
its
rid
ge a
nd t
roug
h ri
ngst
ruct
ures
. Rup
es M
erca
tor
is a
par
t of
a r
idge
, pro
babl
y th
eto
pogr
aphi
c ri
ng, o
f the
Nub
ium
Bas
in. T
his
ring
is e
llipt
ical
in s
hape
, an
indi
cati
on o
f an
obliq
ue im
pact
.
82
Luna
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
124H
3Su
n El
evat
ion:
19.
9°A
ltit
ude:
299
4.47
km
The
con
cent
ric
stru
ctur
e of
Kon
ig a
nd t
he s
light
ly s
mal
ler
crat
er to
the
east
of i
t sug
gest
that
they
hav
e bo
ttom
ed o
ut in
a la
yer
belo
w t
he s
urfa
ce o
f M
are
Nub
ium
. The
sm
ooth
top
laye
r of
the
cra
ter
wal
l of
Bul
liald
us a
nd g
host
cra
ter
rim
ssu
ch a
s K
ies
sugg
est
a si
mila
r sh
allo
w d
epth
to
the
mar
e, in
the
rang
e of
1 t
o 2
km.
The
ray
fro
m T
ycho
tha
t ex
tend
sac
ross
the
mar
e al
so c
over
s th
e ej
ecta
of
Bul
lial
dus.
Thi
sej
ecta
is
thic
k fo
r ab
out
one
crat
er r
adiu
s ou
tsid
e of
Bul
liald
us a
nd th
en b
reak
s up
into
cha
ins
of s
mal
l sec
onda
rycr
ater
s. R
ima
Hes
iodu
s is
a t
ypic
al s
tres
s fr
actu
re n
ear
the
edge
of M
are
Nub
ium
.
LO4-
125H
1Su
n El
evat
ion:
18.
9°A
ltit
ude:
271
6.97
km
83
Hum
oru
mBa
sin R
egio
n
Mar
e C
ogni
tum
(kn
own
sea)
was
so
nam
ed b
ecau
se R
ange
r7,
the
first
fully
suc
cess
ful R
ange
r, tr
ansm
itte
d a
nest
ed s
et o
fpi
ctur
es. T
he r
esol
utio
n of
the
las
t pi
ctur
e w
as s
uffic
ient
to
show
cra
ters
as
smal
l as
1 m
in
diam
eter
, m
ore
than
tw
oor
ders
of
mag
nitu
de b
ette
r th
an t
he r
esol
utio
n of
Ear
th-
base
d ph
otog
raph
y. T
he p
ictu
res
esta
blis
hed
that
the
surf
ace
smoo
thne
ss o
f m
are
surf
aces
sim
ilar
to t
hat
phot
ogra
phed
wou
ld b
e su
itab
le fo
r an
Apo
llo la
ndin
g an
d as
tron
aut e
xcur
-si
ons.
The
pre
senc
e of
blo
cks
in s
ome
of t
he R
ange
r 7
pic-
ture
s in
dica
ted
sign
ifica
nt b
eari
ng s
tren
gth,
but
dou
bt s
till
rem
aine
d in
som
e m
inds
on
this
sub
ject
. D
arne
y is
on
the
rim
of a
240
-km
cra
ter
that
und
erlie
s M
are
Cog
nitu
m.
84
Luna
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
125H
2Su
n El
evat
ion:
18.
9°A
ltit
ude:
271
6.97
km
LO4-
125H
3Su
n El
evat
ion:
18.
9°A
ltit
ude:
271
6.97
km
85
Hum
oru
mBa
sin R
egio
n
The
sou
thea
st r
ange
of
Mon
tes
Rip
haeu
s is
a s
ecto
r of
the
rim
of
the
crat
er t
hat
unde
rlie
s M
are
Cog
nitu
m. T
he r
ays
inth
e up
per
righ
t cor
ner
of th
is p
ictu
re c
ome
from
Cop
erni
cus.
Mar
e In
sula
rum
(se
a of
isl
ands
, na
med
for
the
old
top
o-gr
aphy
tha
t pr
otru
des)
may
be
an e
xten
sion
of
Oce
anus
Proc
ella
rum
or
may
be
part
of
an o
uter
tro
ugh
of t
heIm
briu
m B
asin
. Lun
a 5
cras
hed
(May
196
5) b
ecau
se it
s re
tro-
rock
et fa
iled
to fi
re. S
urve
yor
3, t
he s
econ
d Su
rvey
or t
o su
c-ce
ssfu
lly l
and
(Apr
il 19
67),
con
firm
ed t
he s
uita
bilit
y of
thi
sar
ea f
or a
n A
pollo
lan
ding
, w
hich
was
acc
ompl
ishe
d by
Apo
llo 1
2 (N
ovem
ber
1969
). T
he t
ouch
dow
n of
Apo
llo 1
2,th
e se
cond
man
ned
land
ing,
was
abo
ut 1
60 m
from
Sur
veyo
r3;
the
astr
onau
ts v
isit
ed th
e Su
rvey
or a
nd r
emov
ed p
arts
for
exam
inat
ion
on e
arth
.
Alt
houg
h th
e flo
or, r
im, a
nd r
ays
of T
ycho
are
ver
y br
ight
,th
e in
ner
ejec
ta (
out
to a
bout
one
dia
met
er f
rom
the
rim
) is
only
as
brig
ht a
s th
e ty
pica
l hig
hlan
ds. T
his
dim
mer
eje
cta
ispr
obab
ly r
elat
ivel
y co
arse
and
fro
m a
dee
per
laye
r of
the
targ
et. F
urro
ws
in th
e ej
ecta
bla
nket
are
lim
ited
to th
e da
rker
area
, but
cha
ins
of s
mal
l se
cond
ary
crat
ers
exte
nd t
hrou
ghbo
th d
arke
r an
d lig
hter
are
as.
The
lig
ht e
ject
a m
ater
ial
ispr
obab
ly v
ery
fine
grai
ned.
Suc
h m
ater
ial
dark
ens
wit
h ex
-po
sure
to
the
sola
r w
ind
(whi
ch f
rees
iro
n pa
rtic
les
wit
hin
the
grai
ns)
and
from
met
eoro
id g
arde
ning
(w
hich
mix
es t
heun
derl
ying
soi
l wit
h th
e gr
ains
). T
he T
ycho
impa
ct o
ccur
red
too
rece
ntly
(on
ly a
bout
100
mill
ion
year
s ag
o) fo
r th
e ra
ys to
have
had
tim
e to
dar
ken.
86
Luna
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
119H
2Su
n El
evat
ion:
20.
3°A
ltit
ude:
299
0.55
km
Pita
tus
is a
bout
the
sam
e si
ze a
s T
ycho
and
sho
ws
a si
mila
rce
ntra
l pe
ak.
How
ever
, it
is
muc
h ol
der
(Nec
tari
an).
The
chai
n of
sec
onda
ries
fro
m t
he I
mbr
ium
Bas
in is
sup
erpo
sed
on t
he r
im o
f Pi
tatu
s, a
nd i
ts fl
oor
was
floo
ded
alon
g w
ith
that
of
the
Nub
ium
Bas
in. R
ays
from
Tyc
ho a
ppea
r on
bot
hth
e flo
or o
f Pit
atus
and
Mar
e N
ubiu
m. R
imae
Pit
atus
, aro
und
the
edge
of t
he fl
oor
of P
itat
us, h
ave
been
att
ribu
ted
to fr
ac-
ture
s ca
used
by
uplif
t of t
he fl
oor,
per
haps
in th
e co
urse
of i
tsflo
odin
g. I
t ap
pear
s th
at l
ava
has
flow
ed f
rom
the
floo
r of
Pita
tus
into
Hes
iodu
s th
roug
h th
e w
ide
chan
nel i
n th
e ri
ms.
LO4-
119H
3Su
n El
evat
ion:
20.
3°A
ltit
ude:
299
0.55
km
87
Hum
oru
mBa
sin R
egio
n
Wol
f, sh
aped
like
a V
alen
tine
hea
rt, w
ould
req
uire
a s
alvo
of f
our
crat
ers
if it
wer
e sh
aped
by
impa
ct. A
n al
tern
ate
expl
anat
ion
is th
at it
is a
cal
dera
form
edby
inte
rnal
pro
cess
es d
urin
g th
e fo
rmat
ion
of t
he m
are.
The
con
cent
ric
inne
rri
ng o
f th
e sm
all
crat
er t
o th
e so
uthw
est
of H
esio
dus
may
ind
icat
e th
at t
he
88
Luna
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
120H
1Su
n El
evat
ion:
20.
1°A
ltit
ude:
271
7.50
km
crat
er “
bott
omed
out
” in
the
rel
ativ
ely
shal
low
laye
r of
lava
nea
r th
e ed
ge o
fM
are
Nub
ium
. Not
e th
at s
imila
r-si
zed
and
larg
er c
rate
rs s
uch
as N
icol
let
dono
t sho
w s
imila
r m
orph
olog
y in
the
mor
e ce
ntra
l, pr
esum
ably
dee
per,
par
ts o
fth
e m
are.
The
nor
ther
n ri
m o
f th
e N
ubiu
m B
asin
, as
infe
rred
fro
m t
he n
earl
y ci
rcul
arsh
ape
of t
he r
ing
arou
nd M
are
Nub
ium
, run
s th
roug
h th
e ri
dges
nea
r R
imae
Ope
lt a
nd s
outh
of G
ueri
cke.
The
eje
cta
blan
ket f
rom
the
Nub
ium
Bas
in p
rob-
ably
sur
vive
s un
der
the
ridg
es a
nd tr
ough
s in
the
vici
nity
of G
ueri
cke,
but
the
89
Hum
oru
mBa
sin R
egio
n
LO4-
120H
2Su
n El
evat
ion:
20.
1°A
ltit
ude:
271
7.50
km
stri
atio
ns a
re f
rom
Im
briu
m.
Cop
erni
cus
is t
he s
ourc
e of
the
bri
ght
rays
runn
ing
nort
h to
sou
th th
roug
h th
is p
ictu
re. M
are
Nub
ium
app
ears
to b
e co
n-ne
cted
to
Mar
e C
ogni
tum
(th
e da
rk a
rea
nort
h of
Rim
ae O
pelt
) th
roug
h a
broa
d ch
anne
l eas
t of R
imae
Ope
lt.
The
hea
vily
furr
owed
lum
py d
epos
its
nort
h an
d so
uth
of F
ra M
auro
are
cal
led
the
Fra
Mau
ro F
orm
atio
n, n
ow k
now
n to
be
ejec
ta f
rom
the
Im
briu
m B
asin
,af
ter
anal
ysis
of
rock
s re
turn
ed f
rom
the
Apo
llo 1
4 m
issi
on. T
he F
ra M
auro
Form
atio
n co
rres
pond
s (a
s a
terr
ane
type
) to
the
inne
r H
evel
ius
Form
atio
n of
the
Ori
enta
le B
asin
. A
mon
g th
e 43
kg
of r
ock
retu
rned
by
Apo
llo 1
4 ar
e
90
Luna
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
120H
3Su
n El
evat
ion:
20.
1°A
ltit
ude:
271
7.50
km
sam
ples
fro
m n
ear
the
rim
of
the
370-
m C
one
crat
er. T
his
crat
er b
roug
ht u
pro
cks
from
the
Fra
Mau
ro F
orm
atio
n th
at h
ad n
ot b
een
grou
nd u
p in
the
“top
soil”
of
the
rego
lith.
Ana
lysi
s of
the
se r
ocks
has
est
ablis
hed
the
tim
e of
the
Imbr
ium
impa
ct a
s ab
out 3
.8 b
illio
n ye
ars
ago.
The
are
a ar
ound
Jac
obi,
beyo
nd th
e T
ycho
ray
s ne
ar th
e to
p,is
abo
ut a
s fa
r fr
om m
are,
bas
ins,
and
lar
ge c
rate
rs a
s on
eca
n ge
t on
the
near
sid
e of
the
Moo
n. I
t is
calle
d “i
nter
crat
erte
rran
e” (
a te
rran
e is
an
area
wit
h sp
ecifi
c fo
rmat
ion
cha-
ract
eris
tics
) an
d is
bel
ieve
d to
be
Pre-
Nec
tari
an i
n ag
e.C
lem
enti
ne a
ltit
ude
data
sho
w a
dep
ress
ion
equi
vale
nt t
o a
200-
km c
rate
r ce
nter
ed o
n th
e no
rthe
ast
rim
of
Jaco
bi(C
uvie
r w
ould
be
beyo
nd t
he r
im o
f su
ch a
cra
ter)
. Suc
h an
anci
ent,
degr
aded
cra
ter
may
exp
lain
the
rel
ativ
e fla
tnes
s of
this
are
a. L
ilius
is
larg
e en
ough
(61
km
) to
hav
e a
cent
ral
peak
like
tha
t of
Tyc
ho. C
entr
al p
eaks
occ
ur i
n cr
ater
s w
ith
diam
eter
s in
the
rang
e of
20
to 2
00 k
m.
LO4-
112H
1Su
n El
evat
ion:
20.
4°A
ltit
ude:
298
6.04
km
91
Hum
oru
mBa
sin R
egio
n
Soft
ray
pat
tern
s an
d ch
ains
of
very
sm
all s
econ
dary
cra
ters
radi
ate
from
Tyc
ho ju
st to
the
wes
t of t
his
pict
ure.
Cha
ins
ofel
onga
te lo
w-a
ngle
-of-
inci
denc
e cr
ater
s be
twee
n N
asir
eddi
nan
d Li
cetu
s co
uld
have
com
e ov
er t
he S
outh
Pol
e fr
om t
heSc
hrod
inge
r B
asin
. T
hey
coul
d al
so h
ave
com
e fr
om t
heso
uthw
este
rn s
ecto
r of
Im
briu
m.
It i
s in
tere
stin
g to
stu
dy
the
sequ
ence
of
the
clus
ter
of la
rge
crat
ers
in t
he u
pper
hal
fof
thi
s pi
ctur
e. N
asir
eddi
n ha
s cl
earl
y im
pact
ed a
nd c
ol-
laps
ed t
he w
alls
of
Hug
gins
and
Mil
ler;
Hug
gins
has
col
-la
psed
the
wal
l of
Oro
ntiu
s. S
auss
ure
seem
s yo
unge
r th
anO
ront
ius.
A c
rate
r ev
en o
lder
tha
n O
ront
ius
is r
epre
sent
edon
ly b
y pa
rt o
f its
rim
, jus
t to
the
east
of S
auss
ure.
92
Luna
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
112H
2Su
n El
evat
ion:
20.
4°A
ltit
ude:
298
6.04
km
The
lar
ge c
hain
of
seco
ndar
ies
from
the
Im
briu
m B
asin
betw
een
Pita
tus
and
Des
land
res
lies
on
the
inne
r ej
ecta
blan
ket o
f the
Nub
ium
Bas
in. E
ject
a fr
om th
e N
ubiu
m B
asin
appe
ars
to h
ave
erod
ed t
he w
alls
of
Des
land
res
and
de-
posi
ted
fluid
(m
olte
n or
frag
men
ted)
mat
eria
l on
the
floor
of
Hel
l an
d th
e sm
alle
r cr
ater
sou
th o
f H
ell.
How
ever
, th
epa
tter
n of
eje
cta
seem
s to
dis
appe
ar o
n th
e flo
or o
f Des
land
res.
The
cra
ter
abou
t 80
km
to
the
nort
heas
t of
Hel
l lo
oks
like
crat
ers
that
hav
e be
en fl
oode
d w
ith m
are
lava
, but
the
mat
eria
lis
muc
h lig
hter
tha
n m
are.
The
wal
ls o
f th
e D
esla
ndre
s de
-pr
essi
on c
an b
e se
en a
s sq
uare
, ra
ther
tha
n ro
und.
Is
the
Des
land
res
depr
essi
on a
n im
pact
cra
ter
or t
he r
esul
t of
tec
-to
nic
forc
es p
rodu
cing
upl
ift
and
sink
ing?
Cou
ld t
ecto
nic
shak
ing
have
res
urfa
ced
the
smoo
th p
art
of t
he fl
oor
ofD
esla
ndre
s?
LO4-
112H
3Su
n El
evat
ion:
20.
4°A
ltit
ude:
298
6.04
km
93
Hum
oru
mBa
sin R
egio
n
LO4-113HSun Elevation: 20.1°Altitude: 2718.02 km
Lalande has a spectacular ejecta patternbecause it impacted an area with in-herently light-colored material and de-posited it on the dark surface of MareInsularum. The deep troughs to thesoutheast of Lalande and radial to it aretoo large to be caused by Lalande andare from the Imbrium Basin.
An ancient 160-km flooded cratermay underlie the mare surface in thecenter of this picture. PromontoriumTaenarium could be a remainder of therim of this crater, associated with theintersection between that rim and a ringof the Nubium Basin. The mountainnorthwest of Lassell would be the top ofa complex central peak of the 160-kmflooded crater.
Rupes Recta (straight wall) is hard toexplain. It is not curved like the scarpson the inside of basin rings, and it doesnot appear to be directly related to theshore of Mare Nubium. It may be acontinuation of the degraded scarp nearDeslandres. Albedo patterns on theeastern border of Mare Nubium are alsounusual. Perhaps this is dark mantlingmaterial, pyroclastic fountain materialthat occurs near mare borders andspreads ballistically beyond the mare.
94
Luna
r O
rbiter
Photo
gra
phic
Atla
s
Stofl
er is
one
of m
any
larg
e cr
ater
s w
hose
floo
r is
rem
arka
bly
flat
and
smoo
th, a
ter
rain
typ
e th
at h
as b
een
calle
d “s
moo
thte
rra
plai
ns.”
The
floo
r ap
pear
s to
be
youn
ger
than
the
crat
erri
m, w
hich
sho
ws
degr
adat
ion.
One
exp
lana
tion
of
smoo
thte
rra
plai
ns i
s th
at t
hey
are
flat
surf
aces
tha
t ha
ve b
een
cove
red
by t
he o
uter
(sm
ooth
er)
type
of
basi
n ej
ecta
. T
his
type
of e
ject
a st
arts
at l
east
one
rad
ius
away
from
the
basi
n’s
topo
grap
hic
ring
and
usu
ally
end
s be
twee
n tw
o an
d th
ree
radi
i aw
ay. T
o ha
ve t
his
type
of
terr
ain,
a fl
at-fl
oore
d cr
ater
mus
t be
wit
hin
thre
e ra
dii
of s
ome
subs
eque
nt b
asin
and
mus
t no
t be
wit
hin
one
radi
us o
f an
y su
bseq
uent
bas
in.
Furt
her,
the
cra
ter
mus
t no
t ha
ve b
een
flood
ed w
ith
mar
ela
va o
r su
ffer
ed s
ome
othe
r ev
ent t
hat s
erio
usly
dis
rupt
ed it
sflo
or. T
ecto
nic
shak
ing
may
fur
ther
sm
ooth
and
flat
ten
sur-
face
s w
ith
such
dep
osit
s.
LO4-
107H
2Su
n El
evat
ion:
21.
6°A
ltit
ude:
298
1.85
km
95
Hum
oru
mBa
sin R
egio
n
Her
e is
a c
lust
er o
f cra
ters
, all
of s
imila
r si
ze (
70 to
140
km
),th
at a
re c
lust
ered
tog
ethe
r. T
heir
age
s va
ry, b
ut a
ll pr
obab
lyfo
llow
ed t
he N
ubiu
m B
asin
eve
nt. T
heir
cen
ters
are
wit
hin
120
km o
f a
cent
ral
poin
t, in
uni
form
tar
get
mat
eria
l. T
heov
erla
ppin
g ej
ecta
fro
m t
he t
hese
cra
ters
res
ulte
d in
the
chao
tic
inte
rcra
ter
area
s, w
ith
rim
s im
ping
ing
on e
ach
othe
ran
d m
ater
ial
pilin
g up
bet
wee
n an
d so
met
imes
wit
hin
the
crat
ers.
Sub
sequ
entl
y, t
he I
mbr
ium
Bas
in e
vent
has
de-
posi
ted
a un
ifor
m la
yer
of m
ater
ial t
hat h
as s
moo
thed
pre
vi-
ousl
y un
dist
urbe
d pa
rts
of t
he c
rate
r flo
ors.
Im
briu
m a
lso
drop
ped
a fe
w s
econ
dari
es h
ere.
Wer
ner
arri
ved
late
r; i
tsflo
or h
as n
ot b
een
smoo
thed
. Fin
ally
, Tyc
ho h
as d
ropp
ed it
sra
ys o
ver
the
clus
ter.
96
Luna
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
107H
3Su
n El
evat
ion:
21.
6°A
ltit
ude:
298
1.85
km
The
bit
(Lat
e Im
briu
m)
and
Wer
ner
(Era
tost
heni
an)
are
free
from
evi
denc
e of
sm
ooth
ter
ra p
lain
s an
d Im
briu
m s
econ
-da
ries
and
exh
ibit
lit
tle
rim
ero
sion
. O
n th
e ot
her
hand
,Pu
rbac
h, R
egio
mon
tanu
s, D
esla
ndre
s, a
nd L
a C
aille
(Pr
e-N
ecta
rian
) sh
ow s
moo
th t
erra
pla
ins
unit
s an
d so
me
seco
n-da
ries
, bot
h fr
om th
e Im
briu
m e
vent
.
LO4-
108H
1Su
n El
evat
ion:
21.
1°A
ltit
ude:
271
9.01
km
97
Hum
oru
mBa
sin R
egio
n
The
rim
s of
Pto
lem
aeus
and
Alp
hons
us s
how
str
iati
ons
from
the
Imbr
ium
Bas
in, b
ut t
he e
ffec
ts o
n th
eir
floor
s ha
ve b
een
all
or p
artl
y er
ased
by
lava
flow
s th
at h
ave
redu
ced
the
dept
hs o
f th
ese
crat
ers.
The
se c
rate
rs s
how
an
unus
ual h
igh
leve
l of
tho
rium
in
Luna
r Pr
ospe
ctor
dat
a. C
lem
enti
neal
bedo
dat
a sh
ow P
tole
mae
us t
o be
dar
k, b
ut n
ot a
s da
rk a
sne
arby
Oce
anus
Pro
cella
rum
and
Sin
us M
edii.
The
cra
ters
wit
h da
rk h
alos
in A
lpho
nsus
may
be
sour
ces
of fo
unta
ins
ofda
rk g
lass
bea
ds. R
ange
r 9
phot
os s
how
ed t
hat
part
s of
the
floor
of
Alp
hons
us w
ere
smoo
th li
ke m
are
surf
aces
at
scal
essi
gnifi
cant
for
land
ing
and
surf
ace
oper
atio
ns.
98
Luna
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
108H
2Su
n El
evat
ion:
21.
1°A
ltit
ude:
271
9.01
km
The
Apo
llo p
rogr
am w
as v
ery
inte
rest
ed i
n Si
nus
Med
ii(“
Cen
tral
Bay
”) a
s a
land
ing
site
bec
ause
its
cent
ral p
osit
ion,
rela
tive
to
mar
e si
tes
to t
he e
ast
and
wes
t, pr
ovid
ed a
ddi-
tion
al la
unch
win
dow
opp
ortu
niti
es. S
urve
yor
4 fa
iled
befo
reto
uchd
own,
but
Sur
veyo
r 6
land
ed s
ucce
ssfu
lly (
Nov
embe
r19
67).
Its
alp
ha-s
catt
erin
g in
stru
men
t co
nfirm
ed r
esul
tsfr
om t
hat
of S
urve
yor
5, s
how
ing
that
the
ele
men
t co
mpo
si-
tion
of
mar
e su
rfac
es c
orre
spon
ded
to t
he b
road
ran
ge o
fro
ck t
ypes
cal
led
basa
lt.
Thi
s im
plie
d th
at a
t le
ast
a m
ajor
port
ion
of t
he M
oon
had
unde
rgon
e a
mel
t ph
ase
that
sup
-po
rted
dif
fere
ntia
tion
of
min
eral
s. S
inus
Med
ii is
not
lar
geen
ough
to b
e a
basi
n; it
is a
cra
ter
that
has
bee
n flo
oded
wit
hla
va. I
t m
ay b
e in
fluen
ced
by t
he s
econ
d ex
tern
al t
roug
h of
the
Imbr
ium
Bas
in,
the
sam
e tr
ough
tha
t un
derl
ies
Mar
eFr
igor
is.
LO4-
108H
3Su
n El
evat
ion:
21.
1°A
ltit
ude:
271
9.01
km
99
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7.1. OverviewThe Imbrium Basin Region includes a number of interestingfeatures such as Oceanus Procellarum, Copernicus, Kepler,the Aristarchus plateau, and Vallis Schroteri (Schroter’sValley) as well as Mare Imbrium, the Fra Mauro Formationof Imbrium ejecta, and surrounding maria. Because thesefeatures are so large, yet closely related, the region stretchesfrom the western edge of the visible Moon to the centralmeridian and from the equator to 60° north.
The Imbrium BasinThe Imbrium Basin (Figure 7.1) has had a larger influence onthe current appearance of the near side surface of the Moonthan any other single feature. Although mare flooding hidesmuch of the structure of Imbrium, enough remains to associ-ate its major features with those of Orientale and otherbasins. Specifically, the basin has an inner circular depressedfloor, largely flooded with mare. A scarped rim bounds thisdepression, and beyond the rim is a trough and then addi-tional raised rings. Flooding by surrounding mare has ob-scured much of the ejecta blanket except for the southeastsector. Here the Fra Mauro Formation can be seen to besimilar to the Hevelius Formation of the Orientale Basin.Chains of secondary craters that radiate from the central partof the Imbrium Basin extend beyond this region nearly to theeastern limb.
When the mountain ranges that form the topographic ringof the Imbrium Basin were named, they were not perceivedto be parts of a continuous circle; the sectors of the ring were given the names of familiar mountain ranges on Earth.Clockwise from the north they are Montes Alpes (Alps,France, Switzerland, and Italy), Montes Caucasus (Caucasus,Georgia), Montes Apenninus (Apennines, Italy), MontesCarpatus (Carpathians, Romania), and Montes Jura (JuraMountains, Switzerland, France).
Oceanus ProcellarumOceanus Procellarum (Figure 7.2) contains the largest dis-tinctly named area of mare on the Moon. It has often beenconsidered as evidence of a possible enormous ancient basin,the Procellarum Basin, perhaps three times the size of theImbrium Basin and underlying that basin as well as OceanusProcellarum. This hypothesis is supported by the determina-tion that the crust under this area is thinner than in the rest
of the Moon, perhaps caused by the removal of the top layerof crust by the massive impact. Additional evidence of theuniqueness of this region is provided by remote sensing, andby sample collection, which shows the region to be rich inKREEP minerals and thorium.
However, there are problems with that hypothesis. In par-ticular, there is little sign of massive radial ridges and troughsof an ejecta blanket or external rings that would be expectedto accompany such a large basin. Also, there are positive fea-tures (mountains) that protrude from the mare that are hardto reconcile with a large, flat central floor, even allowing for
Chapter 7
Imbrium Basin Region
Figure 7.1. LO4-134M. The inner edge of the topographic ring of theImbrium Basin is shown as a dashed circle, actually an ellipse here becausethe center of the photo does not coincide with the center of the basin.Within this ring, most of the area is covered with mare material (MareImbrium). Beyond this ring is a trough partly filled with mare (Mare Frigoristo the north and Mare Insularum and Mare Vaporum to the south). Thediameter of the topographic rim is 1160 km.
internal rings. It has also been suggested that OceanusProcellarum is an outer trough of the Imbrium Basin. If so, it is an extraordinarily large area of mare to fill a trough.
Examination of elevation data from Clementine andearlier spacecraft missions suggests a third explanation ofOceanus Procellarum. Mare lava shrinks as it cools, leavingdepressions where it is deepest. Roughly circular depressionssuggest multiple basin-sized depressions beneath OceanusProcellarum (McEwen, 1994). Supporting evidence of thedepth of the flooded depressions has come from analysis ofpartially flooded crater rims (De Hon, 1979). Further, arcs oftwo circular rims can be seen in the northern part of thismare (Figure 7.3).
The proposed Lavoissier-Mairan and Cardanus-HerodotusBasins have influenced the formation of two plateaus, whichhelp in determining the basin sizes and locations. The plateauwest of the Montes Jura (Jura Mountains) was formed byejecta from the proposed Lavoissier-Mairan Basin, theImbrium Basin, and a large crater under Sinus Roris. TheAristarchus plateau may have been built up by the easternintersection of the main rings of these two proposed basins(Byrne, 2004). Analysis of data from Lunar Prospector hasrevealed patches of high-thorium material surrounding theseproposed basins, especially the northern one (Gasnault,2002).
A similar examination of the topography of the southernpart of Oceanus Procellarum (Figure 7.4) shows a depressionthat may reveal a basin. In this case, the lava has left exposedremnants of crater rims and perhaps part of a complexcentral peak or inner ring. There are indications that a basin
in this area could be south of the position shown in Figure7.4 (the possible Flamsteed-Billy Basin of Wilhelms, 1987),but striations beyond the mare to the southwest are a betterfit to the location shown. Clementine data show a distinctlyhigher elevation of the mare floor between the Cardanus-Herodotus Basin shown in Figure 7.3 and the Reiner-Letronne Basin in Figure 7.4.
The possible existence of these basins does not refute thecontribution of an outer trough of the Imbrium Basin to the depression beneath the northeastern part of OceanusProcellarum. Nor do these basins in themselves explain thethinness of the crust and the unusual distribution of ra-dioactive, rare earth, and related elements (KREEP) in thispart of the Moon. This leaves room for the ProcellarumBasin hypothesis, so long as the basin formed when thecrust and early mantle were still soft enough for isostaticadjustment.
Fra Mauro FormationAt one time the Fra Mauro Formation was thought to containnumerous volcanic features, but other geologists believed it to be ejecta from the Imbrium Basin. The formation is so widespread that dating the Imbrium impact helps estab-lish ages of many other features. Analysis of samples fromApollo 14 (Humorum Basin Region) and Apollo 16 (NectarisBasin Region) established that this formation was depositedfrom the Imbrium Basin impact. See the chapters for theseregions for further discussion of these Apollo landings and
Figure 7.2. LO4-162M. The large dark area in this picture is OceanusProcellarum. Mare Imbrium is in the upper right part of the picture. Thebright-rayed craters are Aristarchus and Kepler (below and to the right ofAristarchus). The Grimaldi Basin is to the lower left of Oceanus Procellarumand the Humorum Basin is to the lower right.
Figure 7.3. LO4-175M. These two possible basins, called here theLavoissier-Mairan Basin (to the north) and the Cardanus-Herodotus Basin(each named after craters near their proposed main rings) are inferred fromcircular depressions revealed in Clementine elevation data. These basinsmay have attracted the lava that flooded the northern part of OceanusProcellarum.
10
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their contributions to our understanding of the ImbriumBasin.
7.2. High-Resolution ImagesTable 7.1 shows the high-resolution images of the ImbriumBasin Region in schematic form.
The following pages show the high-resolution subframesfrom south to north and west to east. That is, they are in the
order LO4-189H1, LO4-189H2, LO4-189H3, LO4-183H1,LO4-183H2 … LO4-162H1, LO4-162H2… LO4-110H3.
High-resolution photos of Mission 4 did not cover theextreme northwestern part of this region. Therefore, the firstphoto in this chapter is LO4-189M, which completes the nearside coverage in this area.
Subframes LO4-183H3, LO4-170H3, LO4-158H3, LO4-145H3, LO4-134H3, LO4-122H3, and LO4-110H3 have notbeen printed because of redundancy but are in the enclosedCD. The subframes of LO4-152, LO4-144, LO4-138, LO4-121,and LO4-114 have been merged into full frames.
Figure 7.4. Part of LO4-162M. The dashed circle outlines a possible basin, the Reiner-Letronne Basin that is inferred from a depression in Clementineelevation data. This basin may have attracted the lava that flooded the southern part of Oceanus Procellarum. The Grimaldi Basin is to the west and theHumorum Basin is to the southeast. The southeastern part of this possible basin is in the Orientale Basin Region and the southeast part is in the HumorumBasin Region.
Lattitude Range Photo Number
56 N–90 N 190 176 164 152 140 128 116 104
27 N–56 N 189 183 175 170 163 158 151 145 139 134 127 122 115 110 103
0–27 N 188 182 174 169 162 157 150 144 138 133 126 121 114 109 102
0–27 S 195 187 181 173 168 161 156 149 143 137 132 125 120 113 108 101
Longitude 89 W 82 W 76 W 68 W 62 W 56 W 49 W 41 W 35 W 30 W 23 W 16 W 10 W 3 W 4 E at Equator
Table 7.1. The cells shown in white represent the high-resolution photos of the Imbrium Region (LO4-XXX H1, -H2, and -H3, where XXX is the PhotoNumber). The Orientale Basin Region is to the southwest, the Humorum Basin Region is to the south, the Eastern Basins Region is to the east, and the NorthPolar Region is to the north.
Thi
s m
ediu
m-r
esol
utio
n ph
oto
is p
rovi
ded
to fi
ll in
fea
ture
s in
the
wes
tern
limb
area
of
the
Imbr
ium
Bas
in R
egio
n (a
nd s
ome
of t
he a
djoi
ning
far
sid
e)th
at w
ere
not
phot
ogra
phed
in
high
res
olut
ion.
The
lim
b ar
ea f
rom
Vol
tano
rth
is b
ette
r se
en i
n LO
4-19
0M,
show
n in
the
Nor
th P
olar
Reg
ion.
The
Ori
enta
le B
asin
ext
ends
its
eje
cta
blan
ket
and
seco
ndar
ies
beyo
nd E
inst
ein.
The
ray
s in
nor
ther
n O
cean
us P
roce
llaru
m c
ome
from
Har
palu
s, s
outh
of
Pyth
agor
as in
the
Nor
th P
olar
Reg
ion.
LO4-
188M
Sun
Elev
atio
n: 1
4.5°
Alt
itud
e: 3
645.
75 k
m
10
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LO4-189HSun Elevation: 18.4°Altitude: 2877.84 km
Striations on and within the rims of Repsold, Gerard, von Braun, andLavoisier may have come from the pos-sible Lavoissier-Mairan Basin. The east-west ridges and valleys northeast ofRepsold may be ejecta from a craterunder the nearby bay of OceanusProcellarum. In the 50-km crater west ofvon Braun, there is a moat of lavaaround the inside of the rim.
The bulging floors of these craters areheavily fractured, probably caused bytensile failure of the floor material, amelt sheet, as it is forced to expand. Thefractures on the floor of Repsold crosscrater rims without deflection; they areresponses to deep stress.
The eastern edge of Oceanus Pro-cellarum shows a thinning layer ofmare, leaving many crater rims. Somecraters such as Aston and Voskesenkiyare internally flooded with mare, whichmust have come from below. Thedegraded 55-km crater southeast ofVoskesenkiy shows striations that mayhave come from the possible basin innorthern Oceanus Procellarum.
10
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Thi
s ph
oto
show
s th
e tr
ansi
tion
bet
wee
n th
e hi
ghla
nd r
egio
nto
the
wes
t, th
roug
h th
e sh
allo
w m
are
part
ly fl
oodi
ng c
rate
rs,
to v
ery
deep
mar
e. T
he d
eep
mar
e co
mpl
etel
y co
vers
lar
gecr
ater
s an
d pe
rhap
s ev
en a
n en
tire
bas
in.
LO4-
183H
1Su
n El
evat
ion:
19.
8°A
ltit
ude:
287
4.59
km
10
5Im
bri
um
Ba
sin R
egio
n
The
hig
hlan
d ar
ea e
ast o
f von
Bra
un il
lust
rate
s ho
w c
ompl
exto
pogr
aphy
can
be
scul
pted
by
a se
ries
of
circ
ular
cra
ters
,pa
rtly
floo
ded
wit
h m
are.
The
mat
eria
l in
the
wes
tern
hal
f of
the
floor
of
von
Bra
un c
ould
be
ejec
ta f
rom
the
pos
sibl
eba
sin
bene
ath
nort
hern
Oce
anus
Pro
cella
rum
. Str
iati
ons
inth
e ri
m o
f th
e 90
-km
floo
ded
crat
er n
orth
of
von
Bra
un a
ndin
the
resi
dual
hig
hlan
d m
ater
ial i
n th
e up
per
left
cor
ner
are
esse
ntia
lly r
adia
l to
that
pos
sibl
e ba
sin.
LO4-
183H
2Su
n El
evat
ion:
19.
8°A
ltit
ude:
287
4.59
km
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LO4-175HSun Elevation: 19.2°Altitude: 2871.76 km
The field of sharp secondaries south ofOenopides and Babbage was depositedfrom the Eratosthenian crater Pytha-goras. Later in the Eratosthenian Perioda fresh lava flow south and west ofMarkov submerged parts of the sec-ondary field. A deep trough and ridgepattern runs about 15 km south fromMarkov. It may be ejecta from thepossible basin under northern OceanusProcellarum.
Rays from a crater on the north rimof Oenopides intersect with rays fromLichtenberg; this cloudy appearancehelped give Oceanus Procellarum itsname (“Ocean of Storms”). The darkstreak running east to west, passing justsouth of Lichtenberg, is one of the latestflows of lava in the maria. It covers raysand ejecta of the bright-rayed craterLichtenberg. Although very few lavaflows have taken place after the Era-tosthenian Period, this particular flowhas taken place in the CopernicanPeriod, which began on the order of 1 billion years ago. Nearly all mare sur-faces formed during the earlier LateImbrian Epoch and the EratosthenianPeriod. 1
07
Imb
rium
Ba
sin R
egio
n
The
dar
k yo
ung
lava
flow
tha
t co
vers
the
ray
s an
d ej
ecta
from
the
Cop
erni
can
crat
er L
icht
enbe
rg (
see
note
for
LO
4-17
5H)
cont
inue
s to
the
eas
t, w
here
it
is i
n tu
rn c
over
ed b
yra
ys f
rom
the
sm
all
crat
er n
ear
Dor
sum
Sci
lla.
Nei
ther
Dor
sum
Sci
lla n
or t
he w
rink
le r
idge
nea
r Li
chte
nber
gim
pede
d th
e da
rk fl
ow, w
hich
sug
gest
s th
at t
hey
may
hav
efo
rmed
aft
er th
e flo
w, p
erha
ps a
s it
coo
led.
LO4-
170H
1Su
n El
evat
ion:
19.
8°A
ltit
ude:
287
0.64
km
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Seve
ral
wri
nkle
rid
ges
mee
t at
Mon
s R
umke
r, w
hich
is
form
ed o
f mul
tipl
e ro
und
dom
es. P
erha
ps c
ontr
acti
on o
f the
cool
ing,
sol
idif
ying
mar
e su
rfac
e ca
used
lava
to
be e
xtru
ded
in t
his
area
a m
ulti
ple
num
ber
of t
imes
, ult
imat
ely
form
ing
Mon
s R
umke
r. I
f th
e la
va h
ere
was
of
a di
ffer
ent
chem
ical
com
posi
tion
or
cool
er t
han
the
usua
l m
are
mat
eria
l, it
svi
scos
ity
may
hav
e be
en g
reat
er, a
llow
ing
the
prom
inen
ce to
build
up.
LO4-
170H
2Su
n El
evat
ion:
19.
8°A
ltit
ude:
287
0.64
km
10
9Im
bri
um
Ba
sin R
egio
n
LO4-162HSun Elevation: 17.1°Altitude: 2669.94 km
These spectacular bright rays radiatefrom the Copernican crater Glusko, farto the southwest (L04-174H1 and -H2,in the Orientale Basin Region). Wrinkleridges are major topographic features ofthis area of deep mare, probably formedto relieve compression stresses as lavasubsided under a hardening surface.
Luna 8 (1965) was nearly successfulbut fired its retro-rocket a bit late andwas destroyed by an excessively hardlanding.
Luna 9 was fully successful, the firstspacecraft to land beyond Earth. Itscamera viewed the surrounding area,named Planitia Descensus (Plain ofDescent).
Rimae Hevelius reveal fractures thatare radial and circumferential to therounded edge of the mare. The densemare material makes the surroundingareas bend inward toward the mare,inducing tensional forces that are re-lieved by V-shaped fractures (whosewidth is greatest where the surface ele-vation is highest). Striations in the rimof Hevelius and the area southeast ofLohrman are radial to the OrientaleBasin, about one radius away from therim of that basin. This is the “type area”of the Hevelius Formation (ejecta fromOrientale).
11
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The
mar
e ri
dges
sho
wn
here
giv
e th
e im
pres
sion
of b
reak
ing
wav
es i
n a
larg
e bo
dy o
f flu
id.
Thi
s m
ay b
e as
muc
h an
anal
ogy
as a
met
apho
r be
caus
e th
ey w
ere
poss
ibly
form
ed b
yco
mpr
essi
on f
ract
urin
g of
the
har
deni
ng s
urfa
ce o
f a
fluid
ocea
n of
lava
. Suc
h fr
actu
res
wou
ld n
ot h
ave
been
sim
ulta
ne-
ous:
eac
h fr
actu
re w
ould
rel
ieve
str
ess
for
a ti
me
unti
l it
agai
n bu
ilt u
p. A
n in
divi
dual
fra
ctur
e m
ight
be
unlik
ely
tobr
eak
a se
cond
tim
e be
caus
e it
wou
ld a
ctua
lly b
e a
thic
ker,
stro
nger
par
t of t
he s
urfa
ce a
fter
coo
ling,
esp
ecia
lly if
the
un-
derl
ying
lava
mel
t wel
ded
the
frac
ture
d m
ater
ial t
oget
her.
LO4-
163H
1Su
n El
evat
ion:
20.
1°A
ltit
ude:
286
6.72
km
11
1Im
bri
um
Ba
sin R
egio
n
Rim
a Sh
arp
is s
inuo
us,
unli
ke o
ther
rim
ae t
hat
are
mor
elin
ear.
Alth
ough
line
ar r
imae
are
inte
rpre
ted
as s
urfa
ce m
an-
ifes
tati
ons
of f
ract
ures
tha
t re
lieve
ten
sion
, si
nuou
s ri
mae
(rill
es)
are
inte
rpre
ted
as th
e re
sult
of fl
ows
of fl
uid
alon
g lo
wsl
opes
. On
Eart
h, t
he m
ost
fam
iliar
ana
logy
is t
hat
of m
ean-
deri
ng s
trea
ms
and
rive
rs fl
owin
g in
allu
vial
val
leys
. T
hecu
rvin
g an
d re
curv
ing
mea
nder
s ar
e dy
nam
ical
ly c
ause
d by
late
ral
osci
llati
ons
of t
he m
omen
tum
of
a m
ovin
g flu
id,
whi
ch i
s pr
obab
ly l
ow-v
isco
sity
lav
a on
the
Moo
n. S
uch
mea
nder
s m
ay h
ave
been
ver
y co
mm
on d
urin
g fil
ling
of t
hem
are,
but
per
haps
onl
y th
ose
asso
ciat
ed w
ith
the
last
flow
sha
ve s
urvi
ved
bein
g su
bmer
ged.
LO4-
163H
2Su
n El
evat
ion:
20.
1°A
ltit
ude:
286
6.72
km
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Thi
s is
the
wid
est
part
of
Rim
a Sh
arp,
and
is
prob
ably
the
sour
ce o
f it
s flo
w (
see
LO4-
163H
2). A
t it
s no
rthe
rn e
xtre
me,
it a
ctua
lly b
reak
s in
to r
elat
ivel
y sm
alle
r tr
ibut
arie
s, a
ppar
-en
tly
gath
erin
g la
va b
efor
e ca
rryi
ng i
t so
uthw
ard.
Per
haps
lava
upw
elli
ng i
nto
the
area
sou
thw
est
of H
arpa
lus
was
bloc
ked
by t
he h
ighl
and
prom
inen
ce i
n th
e lo
wer
rig
htco
rner
of
the
phot
o (p
art
of t
he r
im r
ing
of t
he I
mbr
ium
Bas
in)
and
form
ed R
ima
Shar
p as
it fo
und
a ro
ute
to a
low
erel
evat
ion.
The
hig
hly
erod
ed c
rate
r So
uth
is c
over
ed w
ith
Fra
Mau
ro F
orm
atio
n, e
ject
a fr
om th
e Im
briu
m B
asin
. Har
palu
sis
a C
oper
nica
n cr
ater
wit
h a
broa
d ra
y pa
tter
n.
LO4-
163H
3Su
n El
evat
ion:
20.
1°A
ltit
ude:
286
6.72
km
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bri
um
Ba
sin R
egio
n
Rei
ner
Gam
ma
is a
ver
y un
usua
l fe
atur
e. T
he I
AU
cla
ssifi
es i
t as
an
albe
dofe
atur
e, t
o fin
esse
the
que
stio
n of
its
orig
in a
s an
impa
ct o
r in
tern
al p
roce
ss.
Alt
houg
h ra
re, t
here
are
a f
ew o
ther
fea
ture
s w
ith
sim
ilar
brig
ht s
wir
ls. T
hey
occu
r in
are
as w
ith
mag
neti
c an
omal
ies.
It
has
been
sug
gest
ed t
hat
the
mag
-
neti
c fie
lds
defle
ct t
he i
oniz
ed s
olar
win
d. W
itho
ut s
uch
prot
ecti
on, i
oniz
edhy
drog
en (
prot
ons)
red
uces
oxi
des
in t
he s
urfa
ce g
rain
s, f
reei
ng e
lem
enta
lir
on. T
he ir
on a
bsor
bs li
ght,
dark
enin
g th
e su
rfac
e. W
hat c
ause
s th
e m
agne
tic
anom
alie
s is
unk
now
n.
LO4-
157H
1Su
n El
evat
ion:
16.
9°A
ltit
ude:
266
8.85
km
11
4Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
The
Mar
ius
Hill
s ha
ve b
een
inte
rpre
ted
as a
vol
cani
cally
act
ive
regi
on. R
ima
Gal
ilaei
see
ms
to h
ave
colle
cted
and
tran
spor
ted
lava
from
two
trib
utar
ies
near
its
sout
heas
t en
d. O
ther
rim
ae i
n th
e ar
ea s
eem
to
star
t at
cra
ters
tha
t m
ayha
ve f
orm
ed a
roun
d an
und
ergr
ound
sou
rce
of la
va. T
he n
orth
ern
boun
dary
of t
he e
leva
ted
hilly
ter
rain
occ
urs
alon
g th
e ri
ng o
f th
e pr
opos
ed L
avoi
ssie
r-
Mai
ran
Bas
in,
so i
t m
ay b
e an
eje
cta
blan
ket
of t
hat
basi
n. I
f so
, th
e ej
ecta
wou
ld h
ave
been
mod
ified
by
flood
ing
wit
h la
va fr
om b
elow
, filli
ng a
ny r
adia
ltr
ough
s. A
s in
man
y ca
ses
whe
re th
in la
va c
omes
in c
onta
ct w
ith
high
land
ma-
teri
al, t
he a
rea
may
hav
e be
en c
over
ed w
ith
dark
man
tlin
g m
ater
ial,
gene
rate
dby
foun
tain
s of
gla
ss b
eads
.
LO4-
157H
2Su
n El
evat
ion:
16.
9°A
ltit
ude:
266
8.85
km
11
5Im
bri
um
Ba
sin R
egio
n
The
hig
hlan
d ar
ea in
the
uppe
r ri
ght q
uadr
ant o
f thi
s ph
oto
is th
e ea
ster
n ha
lfof
a l
arge
isl
and
in O
cean
us P
roce
llaru
m k
now
n as
the
Ari
star
chus
Pla
teau
.T
he e
aste
rn h
alf
can
be s
een
in L
O4-
150H
3. T
his
plat
eau
may
hav
e be
enfo
rmed
by
a tr
iple
inte
rsec
tion
of
ring
s; t
he fi
rst
exte
rnal
ele
vate
d ri
ng o
f th
e
Imbr
ium
Bas
in, t
he s
outh
east
ern
rim
of
the
Lavo
issi
er-M
aira
n ba
sin,
and
the
nort
heas
tern
rim
of
the
poss
ible
Car
danu
s-H
erod
otus
Bas
in. V
allis
Sch
rote
rise
ems
to b
e ca
rryi
ng l
ava
dow
n to
the
mar
e su
rfac
e. S
ee L
O4-
158H
1 an
d it
sno
tes
for
mor
e on
this
feat
ure.
LO4-
157H
3Su
n El
evat
ion:
16.
9°A
ltit
ude:
266
8.85
km
11
6Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
The
nor
thea
ster
n se
ctor
of
the
Ari
star
chus
pla
teau
(lo
wer
righ
t in
this
pho
to)
is r
ich
in e
vide
nce
of s
ubsu
rfac
e th
erm
al(e
ndot
herm
ic)
acti
vity
. M
ulti
ple
sinu
ous
rille
s ca
rry
lava
dow
n to
the
mar
e su
rfac
e fr
om s
ourc
e cr
ater
s. V
alli
sSc
hrot
eri
show
s ev
iden
ce o
f a
mas
sive
out
pour
ing
of l
ava
that
exc
avat
ed t
he v
alle
y, f
allin
g ne
arly
4 k
m f
rom
Cob
raH
ead,
the
sou
rce
crat
er,
to t
he m
are
surf
ace
140
km a
way
(LO
157H
3).
Pres
umab
ly t
he m
assi
ve A
rist
arch
us P
late
aubl
ocke
d up
wel
ling
of
mag
ma,
whi
ch w
as fi
nally
flow
ing
thro
ugh
Val
lis
Schr
oter
i, R
ima
Agr
icol
a,
and
Rim
aeA
rist
arch
us.
LO4-
158H
1Su
n El
evat
ion:
19.
6°A
ltit
ude:
286
5.60
km
11
7Im
bri
um
Ba
sin R
egio
n
LO4-
158H
2Su
n El
evat
ion:
19.
6°A
ltit
ude:
286
5.60
km
11
8Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
Thi
s cu
rved
sho
relin
e of
Oce
anus
Pro
cella
rum
cou
ld b
e th
eri
m a
nd e
ject
a pa
tter
n of
the
pos
sibl
e La
vois
sier
-Mai
ran
Bas
in. S
ome
stri
atio
ns a
nd c
rate
r ch
ains
in
this
are
a ar
e in
the
appr
opri
ate
radi
al d
irec
tion
, no
rthw
est
to s
outh
east
,w
hile
oth
ers
radi
ate
from
the
Imbr
ium
Bas
in. T
his
area
may
be c
over
ed w
ith
two
laye
rs o
f ba
sin
ejec
ta b
lank
ets,
the
Fra
Mau
ro F
orm
atio
n be
ing
the
uppe
r la
yer.
The
ray
pas
sing
to
the
sout
h of
Sue
ss is
fro
m K
eple
r, t
o th
eea
st-n
orth
east
. Act
ually
, all
but t
he u
pper
and
low
er le
ft s
ides
of t
he a
rea
in t
his
imag
e ar
e lig
htly
cov
ered
wit
h K
eple
r ra
ym
ater
ial.
The
nea
rly
subm
erge
d cr
ater
s to
the
sout
h in
dica
teth
at th
e m
are
laye
r is
rel
ativ
ely
thin
ther
e, n
ear
the
sout
hern
edge
of O
cean
us P
roce
llaru
m.
LO4-
150H
1Su
n El
evat
ion:
17.
8°A
ltit
ude:
266
8.40
km
11
9Im
bri
um
Ba
sin R
egio
n
Thi
s is
the
eas
tern
edg
e of
the
Mar
ius
Hill
s (s
ee L
O4-
157H
2fo
r th
e w
este
rn e
dge)
. Lun
a 7
faile
d du
e to
pre
mat
ure
igni
-ti
on o
f its
ret
ro-r
ocke
t in
Oct
ober
196
5 an
d cr
ashe
d at
the
in-
dica
ted
site
. R
ima
Mar
ius
flow
s no
rth
into
the
mar
e flo
orfr
om th
e hi
lls w
hile
Rim
a Su
ess
flow
s do
wn
to th
e so
uth.
The
chai
ns o
f sm
all
crat
ers
to t
he e
ast
and
sout
heas
t of
Mar
ius
radi
ate
from
Kep
ler.
LO4-
150H
2Su
n El
evat
ion:
17.
8°A
ltit
ude:
266
8.40
km
12
0Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
Thi
s is
the
eas
tern
par
t of
the
Ari
star
chus
Pla
teau
: th
ew
este
rn p
art
can
be s
een
in L
O4-
157H
3. C
oper
nica
n cr
ater
Ari
star
chus
, it
s ej
ecta
, an
d it
s ra
y pa
tter
n do
min
ate
this
phot
o. C
ount
s of
cra
ters
on
its
floor
sho
w A
rist
arch
us t
o be
very
you
ng, n
earl
y as
you
ng a
s T
ycho
. Cle
arly
, the
re h
as b
een
a gr
eat
deal
of
upw
elli
ng o
f la
va h
ere,
to
gene
rate
all
the
ridg
es a
nd la
va s
trea
ms.
Rem
ote
sens
ing
of th
e su
rfac
e of
this
area
sho
ws
a hi
gh p
erce
ntag
e of
REE
(ra
re e
arth
ele
men
ts),
whi
ch i
ndic
ate
radi
oact
ivit
y, b
ecau
se o
f hi
gh c
hem
ical
affin
ity
to th
e ur
aniu
m-t
hori
um s
erie
s. T
he L
unar
Pro
spec
tor
spac
ecra
ft c
onfir
med
a h
igh
leve
l of
tho
rium
. Rad
ioac
tivi
tyge
nera
tes
heat
and
the
hea
t ca
uses
the
mel
ting
roc
k to
expa
nd a
nd r
ise.
LO4-
150H
3Su
n El
evat
ion:
17.
8°A
ltit
ude:
266
8.40
km
12
1Im
bri
um
Ba
sin R
egio
n
The
nor
ther
n pa
rt o
f the
Ari
star
chus
Pla
teau
is s
how
n in
the
low
er h
alf
of t
his
phot
o. O
cean
us P
roce
llaru
m s
eem
s th
inhe
re, l
eavi
ng r
emna
nts
of o
lder
fea
ture
s su
ch a
s Pr
inz
and
Mon
tes
Har
bing
er p
roje
ctin
g ab
ove
the
mar
e flo
or. H
owev
er,
ther
e ar
e ex
tens
ive
sign
s of
lav
a flo
win
g ou
t fr
om v
ario
usso
urce
s on
the
Ari
star
chus
Pla
teau
and
run
ning
thro
ugh
the
rim
ae d
own
to t
he m
are
surf
ace.
Not
e th
at e
ach
rim
a se
ems
to s
tart
fro
m a
cra
ter.
The
Ari
star
chus
im
pact
or p
roba
bly
arri
ved
long
aft
er th
e er
upti
ons
ende
d.
LO4-
151H
1Su
n El
evat
ion:
20.
9°A
ltit
ude:
286
5.91
km
12
2Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
Sinu
s Ir
idum
, a b
ay o
ff o
f Mar
e Im
briu
m, r
esul
ts fr
om a
cir
-cu
lar
impa
ct f
eatu
re w
hose
rim
dia
met
er o
f 26
0 km
res
ults
in i
t be
ing
char
acte
rize
d as
a c
rate
r ra
ther
tha
n as
a b
asin
.M
onte
s Ju
ra c
onst
itut
es t
he r
im o
f th
e Ir
idum
cra
ter.
The
chai
ns o
f se
cond
ary
crat
ers
and
othe
r li
neat
ions
in
this
pict
ure
tend
to
be r
adia
l to
Sin
us I
ridu
m,
rath
er t
han
toIm
briu
m,
indi
cati
ng t
hat
the
Irid
ium
cra
ter
occu
rred
lat
erth
an t
he I
mbr
ium
Bas
in.
Mon
s G
ruit
huis
en G
amm
a an
dD
elta
, wit
h a
crat
er o
n to
p of
eac
h of
them
, hav
e be
en c
onsi
d-er
ed t
o be
vol
cani
c, b
ut t
hey
may
sim
ply
be r
elic
s of
the
Imbr
ium
Bas
in,
mod
ified
by
the
Irid
um e
ject
a an
d co
inci
-de
ntal
pri
mar
y or
sec
onda
ry c
rate
rs a
t the
ir p
eaks
. The
re a
rese
vera
l suc
h fe
atur
es o
n th
e flo
or o
f Mai
ran.
LO4-
151H
2Su
n El
evat
ion:
20.
9°A
ltit
ude:
286
5.91
km
12
3Im
bri
um
Ba
sin R
egio
n
LO4-
151H
3Su
n El
evat
ion:
20.
9°A
ltit
ude:
286
5.91
km
12
4Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
The
nor
thw
este
rn r
im o
f th
e Im
briu
m B
asin
cro
sses
dia
-go
nally
acr
oss
this
pic
ture
. M
are
Frig
oris
has
floo
ded
the
oute
r tr
ough
of
the
Imbr
ium
Bas
in.T
he a
rea
betw
een
Sinu
sIr
idum
and
Mar
e Fr
igor
is h
as b
een
cris
scro
ssed
wit
h ej
ecta
from
dif
fere
nt d
irec
tion
s. S
tron
g so
uthe
ast
to n
orth
wes
tlin
eati
ons
from
the
dire
ctio
n of
the
Imbr
ium
Bas
in a
re c
lear
,as
are
line
atio
ns r
adia
l to
the
Irid
um c
rate
r.
LO4-144HSun Elevation: 19.1°Altitude: 2668.99 km
This area just east of the Aristarchusplateau has relatively thin mare cover-age; it is higher than the central maresurfaces of either Oceanus Procellarumor Mare Imbrium. Numerous rilles (andthe lakes that fed them) carried lavafrom the vicinity of Prinz to the north.Montes Harbinger is probably a rem-nant of the topographic ring of theImbrium Basin.
Some of the valleys of Rimae Prinzare quite wide. Like meanderingstreams on Earth, some sinuous rilles oflava on the Moon are dynamic. In time,their individual bends move in a down-stream direction and sweep out a widevalley.
The rays from Kepler, coming from the southeast, meet rays fromAristarchus, coming from the north-west. Kepler is larger than Aristarchusbut is further away from the center ofthe picture. Note the pair of overlappingcraters near 7° N, 43° W (the larger of the overlapping craters is calledBessarion B). The unusually sharpseptum between the two suggests a si-multaneous impact of the two craters;neither has pushed wall material intothe other.
The flooded crater rims belowMaestlin show striations from theImbrium Basin.
12
5Im
bri
um
Ba
sin R
egio
n
Mon
s D
elis
le a
nd t
he a
rchi
pela
go o
f “i
slan
ds”
in t
he m
are
that
le
ad
to
Mon
s G
ruit
huis
en
Gam
ma
and
Mon
sG
ruit
huis
en D
elta
are
rem
nant
s of
the
mos
tly
subm
erge
dto
pogr
aphi
c ri
ng o
f the
Imbr
ium
Bas
in.
LO4-
145H
1Su
n El
evat
ion:
20.
7°A
ltit
ude:
286
8.12
km
12
6Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
Prom
onto
rium
Her
aclid
es i
s a
resu
lt o
f th
e in
ters
ecti
on o
fth
e ri
m o
f the
cra
ter
unde
rlyi
ng S
inus
Irid
um (
Mon
tes
Jura
ispa
rt o
f tha
t ri
m)
and
the
high
est
ring
of t
he I
mbr
ium
Bas
in.
The
cur
ve a
t th
e so
uthe
rn b
orde
r of
the
pro
mon
tori
um(p
enin
sula
) is
not
the
cur
ve o
f th
e Im
briu
m r
im,
but
isfo
rmed
by
the
Irid
um c
rate
r pu
shin
g th
e Im
briu
m r
ing
and
floor
mat
eria
l out
war
d. T
he la
rge
vert
ical
rid
ge a
t the
bas
e of
the
peni
nsul
a is
mor
e re
pres
enta
tive
of
the
Imbr
ium
rin
g in
this
are
a. M
ost
of t
he h
eavy
eje
cta
terr
ain
on t
he l
eft
of t
hepi
ctur
e is
from
the
Irid
um e
vent
, but
trac
es o
f str
iati
ons
from
the
Imbr
ium
Fra
Mau
ro F
orm
atio
n (p
roba
bly
light
ly c
over
edby
Iri
dum
eje
cta
as w
ell)
can
be
seen
in th
e lo
wer
left
and
inth
e up
per
left
of t
he p
hoto
.
LO4-
145H
2Su
n El
evat
ion:
20.
7°A
ltit
ude:
286
8.12
km
12
7Im
bri
um
Ba
sin R
egio
n
LO4-138HSun Elevation: 18.3°Altitude: 2670.70 km
Oceanus Procellarum meets MareImbrium (upper right) near MonsVinogradov, which is part of the highestring of the Imbrium Basin. The dark-ness of the mare surface, plus the pat-terns of Dorsum Aduino and the long,narrow Rima Brayley suggest a younglava flow of low viscosity. Rima Brayleyappears to guide lava in each directionaway from a low rise near craterBrayley.
The knobby terrain curving along theright side of this picture is part of a circular feature that bounds MareInsularum. The shapes of the interior ofKepler and its wall have been disruptedby the crater near its northern rim. Thisimpact, being younger than Kepler,must have added its ray pattern on topof the one from Kepler itself. Southwestof Kepler, projecting from the maresurface of Oceanus Procellarum, areridges and valleys radial to the ImbriumBasin. They are probably exposed be-cause they top the first circumferentialring of the Imbrium Basin outside of itshighest ring, the ring that bounds thetrough occupied by Mare Frigoris.
12
8Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
It is
dif
ficul
t to
assi
gn th
e ag
e of
Dio
phan
tus.
Sha
rpne
ss a
ndcr
ater
cou
nts
are
sim
ilar
to
thos
e ch
arac
teri
stic
s of
old
erC
oper
nica
n Pe
riod
cra
ters
. How
ever
, the
lack
of a
ray
pat
tern
has
resu
lted
in
assi
gnm
ent
to t
he p
revi
ous
Erat
osth
enia
nPe
riod
. The
pro
lifer
atio
n of
dor
sa (
mar
e ri
dges
), m
ostl
y ci
r-cu
mfe
rent
ial
to t
he I
mbr
ium
Bas
in,
refle
ct t
he s
tres
ses
ofm
assi
ve fl
ow a
nd s
ubse
quen
t coo
ling.
LO4-
139H
1Su
n El
evat
ion:
20.
2°A
ltit
ude:
287
2.43
km
12
9Im
bri
um
Ba
sin R
egio
n
The
pr
esen
ce
of
Sinu
s Ir
idum
, m
ore
clea
rly
seen
in
LO
4-14
5H2,
app
ears
to
have
str
ongl
y af
fect
ed t
he p
atte
rn o
fm
are
ridg
es i
n th
is a
rea.
Pro
mon
tori
um H
erac
lide
s an
dPr
omon
tori
um L
apla
ce m
ark
the
inte
rsec
tion
of
the
rim
of
the
crat
er t
hat
unde
rlie
s Si
nus
Irid
um w
ith
the
high
est
ring
of t
he I
mbr
ium
Bas
in. A
lar
ge u
nnam
ed m
are
ridg
e cu
rves
betw
een
thes
e tw
o pr
omon
tori
es a
nd m
ay m
ark
the
east
ern
and
sout
hern
rim
s of
the
crat
er b
enea
th S
inus
Irid
um.
LO4-
139H
2Su
n El
evat
ion:
20.
2°A
ltit
ude:
287
2.43
km
13
0Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
Mon
tes
Rec
ti is
a p
art o
f the
mai
n ri
ng o
f the
Imbr
ium
Bas
in.
Mar
e la
va h
as p
enet
rate
d th
e ri
ng a
nd fl
oode
d pa
rt o
f th
eIm
briu
m e
ject
a bl
anke
t (F
ra M
auro
For
mat
ion,
cov
ered
by
ejec
ta fr
om th
e Ir
idum
cra
ter)
. Thi
s se
ctio
n of
Mar
e Fr
igor
isha
s flo
oded
the
tro
ugh
beyo
nd t
he m
ain
ring
. The
str
iati
ons
runn
ing
from
sou
thw
est
to n
orth
east
com
e fr
om t
he I
ridu
mcr
ater
and
hav
e ne
arly
(bu
t no
t en
tire
ly)
eras
ed t
he r
idge
san
d va
lleys
rad
iati
ng fr
om th
e in
teri
or o
f the
Imbr
ium
Bas
in.
The
re a
re s
tron
g ev
iden
ces
of fl
ow o
n th
e flo
or o
f Mau
pert
uis
and
Rim
ae M
aupe
rtui
s th
at m
ay h
ave
resu
lted
from
a d
epos
itof
mol
ten
ejec
ta fr
om th
e Si
nus
Irid
um c
rate
r.
LO4-
139H
3Su
n El
evat
ion:
20.
2°A
ltit
ude:
287
2.43
km
13
1Im
bri
um
Ba
sin R
egio
n
The
arc
of h
ills
larg
ely
subm
erge
d by
the
mar
e su
rfac
e, in
terp
rete
d as
isla
nds,
help
ed g
ive
Mar
e In
sula
rum
its
nam
e. T
his
curv
ed r
idge
of s
umm
its
may
rep
-re
sent
the
rim
of t
he p
ossi
ble
Insu
laru
m B
asin
und
erly
ing
Mar
e In
sula
rum
. A
clus
ter
of lo
w d
omes
, eac
h w
ith
a cr
ater
in it
s ce
nter
can
be
seen
nor
thea
st o
fH
orte
nsiu
s. T
hese
dom
es m
ay b
e th
e re
sult
of l
ava
extr
usio
ns. R
etre
atin
g la
vale
aves
a c
entr
al c
rate
r in
the
top
of th
e do
me,
a c
alde
ra.
LO4-
133H
1Su
n El
evat
ion:
18.
5°A
ltit
ude:
267
3.45
km
13
2Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
A l
ow 8
-km
dom
e w
ith
a ce
ntra
l cr
ater
or
cald
era
can
be s
een
abou
t 20
km
wes
t of
Mili
chiu
s. T
his
dom
e is
sur
roun
ded
by a
lava
flow
wit
h vi
sibl
e ed
ges
(sca
rps)
that
ext
end
to th
e ri
m o
f Mili
chiu
s. R
ima
T. M
ayer
has
bee
n de
flect
edar
ound
ano
ther
low
dom
e w
ith
a ce
ntra
l cra
ter.
Mon
tes
Car
patu
s is
par
t of t
heri
m o
f M
are
Imbr
ium
. T
he fl
oodi
ng o
f ev
ery
poss
ible
sm
all
inle
t al
ong
the
nort
hern
sho
re o
f th
e M
onte
s C
arpa
tus
illus
trat
es h
ow e
asily
the
lava
flow
ed.
The
vis
cosi
ty m
ust
have
bee
n m
uch
low
er t
han
typi
cal
terr
estr
ial
lava
, lo
wen
ough
to
over
com
e th
e ef
fect
of
low
er l
unar
gra
vity
(on
e-si
xth
of E
arth
’sgr
avit
y). T
he d
iffe
renc
e is
att
ribu
ted
to a
rel
ativ
e la
ck o
f vo
lati
le e
lem
ents
in
luna
r la
va.
LO4-
133H
2Su
n El
evat
ion:
18.
5°A
ltit
ude:
267
3.45
km
13
3Im
bri
um
Ba
sin R
egio
n
A v
ery
larg
e la
va fl
ow e
xten
ds f
rom
an
area
nor
th o
f Eu
ler
thro
ugh
the
gap
betw
een
Mon
s La
Hir
e an
d th
e hi
lls 3
0 km
to
the
nort
hwes
t, al
l th
e w
ay t
oD
orsu
m Z
irke
l. T
he e
dges
of t
his
flow
are
just
bar
ely
visi
ble
in th
is im
age
and
in L
O4-
126H
3, b
ut c
an b
e se
en m
ore
clea
rly
in A
pollo
15
fram
e M
-155
6, ta
ken
at a
low
er s
un a
ngle
.
LO4-
133H
3Su
n El
evat
ion:
18.
5°A
ltit
ude:
267
3.45
km
13
4Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
Cra
ters
Cha
rles
, Mav
is, A
nneg
rit,
Ver
ne, a
nd F
elix
are
sm
all
crat
ers
that
wer
e gi
ven
spec
ial
atte
ntio
n be
caus
e th
ey w
ere
phot
ogra
phed
at
high
res
olut
ion
by o
rbit
ing
Apo
llo s
pace
-cr
aft.
The
offi
cial
IAU
nam
es o
f suc
h la
ndm
ark
crat
ers
are
all
“firs
t na
mes
” (p
erso
nal n
ames
from
a v
arie
ty o
f cul
ture
s) o
rin
a fe
w c
ases
the
nam
es o
f god
s an
d go
ddes
ses.
Thi
s pa
rtic
u-la
r ar
ea,
if c
hose
n as
a l
andi
ng s
ite,
wou
ld h
ave
allo
wed
surf
ace
expl
orat
ion
of d
isti
nctl
y di
ffer
ent l
ava
flow
s.
LO4-
134H
1Su
n El
evat
ion:
21.
4°A
ltit
ude:
287
8.51
km
13
5Im
bri
um
Ba
sin R
egio
n
Pair
s of
im
pact
cra
ters
wit
h ve
ry s
imil
ar s
izes
, ag
es,
and
othe
r ch
arac
teri
stic
s ar
e fo
und
on t
he M
oon
and
also
on
Eart
h. H
elic
on a
nd L
e V
erri
er a
re a
n ex
ampl
e of
suc
h a
pair
on t
he M
oon.
Rec
ent
mod
elin
g of
col
lisio
ns o
f K
uipe
r be
ltob
ject
s in
dica
tes
that
the
re i
s a
sign
ifica
nt p
opul
atio
n of
pair
s of
obj
ects
of s
imila
r si
ze th
at m
utua
lly o
rbit
eac
h ot
her.
Plut
o an
d C
haro
n ar
e th
e la
rges
t ex
ampl
e of
suc
h a
pair
, if
inde
ed t
hey
cam
e fr
om t
he K
uipe
r re
gion
. C
omet
s co
me
from
the
Kui
per
regi
on a
nd a
re a
n im
port
ant
com
pone
nt o
fpr
imar
y im
pact
ors
on th
e M
oon,
so
it is
ver
y re
ason
able
that
thes
e pa
irs
of c
rate
rs c
ome
from
pai
red
com
ets.
See
the
note
sfo
r LO
4-12
7H1
for
furt
her
disc
ussi
on o
f H
elic
on a
nd L
eV
erri
er.
LO4-
134H
2Su
n El
evat
ion:
21.
4°A
ltit
ude:
287
8.51
km
13
6Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
Mas
sive
dep
osit
s fr
om C
oper
nicu
s co
ver
the
east
ern
rim
of
the
Insu
laru
m B
asin
, jus
t nor
thea
st o
f Rei
nhol
d. L
una
5 (M
ay19
65)
suff
ered
a b
ad m
idco
urse
cor
rect
ion
and
cras
hed
inM
ay 1
965.
Sur
veyo
r 3
(Apr
il 19
67),
see
king
a s
oft l
andi
ng o
na
wes
tern
mar
e, b
ounc
ed t
hree
tim
es b
efor
e fin
ally
tou
chin
gdo
wn
safe
ly. I
ts c
amer
as a
nd s
oil
scoo
p co
nfirm
ed s
uita
ble
terr
ain
and
flatn
ess
for
an A
pollo
land
ing
site
. Mat
chin
g fe
a-tu
res
in S
urve
yor’
s ph
otos
wit
h Ea
rth-
base
d m
aps
and
Luna
rO
rbit
er 3
pho
togr
aphy
ide
ntifi
ed t
he p
reci
se l
andi
ng l
oca-
tion
. Thi
s al
low
ed A
pollo
12
to la
nd (
Nov
embe
r 19
69)
wit
hin
200
m o
f the
Sur
veyo
r, a
sho
rt w
alk
away
(in
spa
cesu
its!
) fo
rA
lan
Bea
n an
d Pe
te C
onra
d. T
his
Apo
llo m
issi
on c
onfir
med
the
abili
ty to
land
at a
pre
cise
loca
tion
on
the
Moo
n, a
cap
a-bi
lity
that
was
cri
tica
l for
late
r A
pollo
pla
nnin
g.
LO4-
126H
1Su
n El
evat
ion:
19.
5°A
ltit
ude:
267
7.28
km
13
7Im
bri
um
Ba
sin R
egio
n
Cop
erni
cus
dom
inat
es
this
dr
amat
ic
scen
e of
M
onte
sC
arpa
tus,
the
sout
hern
rim
of t
he Im
briu
m B
asin
. Rim
a G
ay-
Luss
ac, l
ike
man
y ot
her
lava
rill
es, s
tart
s fr
om a
cra
ter
on th
eou
tsid
e of
the
rin
g bo
undi
ng a
mar
e; h
owev
er,
Rim
a G
ay-
Luss
ac fi
nds
a va
lley
lead
ing
acro
ss t
he r
ing
into
the
bas
inflo
or.
Rim
a G
ay-L
ussa
c ap
pear
s m
ore
like
a co
llaps
ed l
ava
tube
than
a s
urfa
ce c
hann
el. A
lava
tube
is fo
rmed
whe
n la
vaflo
ws
bene
ath
the
cool
ed s
urfa
ce a
nd is
kep
t ope
n by
the
con-
tinu
ous
flow
of h
ot la
va. T
he h
arde
ned
roof
of t
he tu
be in
su-
late
s th
e la
va fr
om c
oolin
g by
rad
iati
on in
to s
pace
. An
inta
ctla
va tu
be is
, of c
ours
e, n
ot v
isib
le fr
om th
e su
rfac
e bu
t if t
hero
of o
f th
e tu
be i
s le
ss t
han
a fe
w m
eter
s in
dep
th, p
rim
ary
and
seco
ndar
y im
pact
s ca
n co
llaps
e it
in ti
me.
LO4-
126H
2Su
n El
evat
ion:
19.
5°A
ltit
ude:
267
7.28
km
13
8Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
Ejec
ta f
rom
Cop
erni
cus,
land
ing
alon
g it
s ra
y ne
ar t
he r
ight
edge
of
this
im
age,
plo
wed
a n
umbe
r of
cra
ters
of
unus
ual
shap
es (
indi
cati
ng a
low
ang
le o
f ap
proa
ch t
o th
e su
rfac
e).
Sout
h of
Lam
bert
, a 6
0-km
bur
ied
crat
er (
Lam
bert
R)
has
left
a fa
int
imag
e of
its
rim
on
the
mar
e su
rfac
e, li
ke t
he f
adin
gsm
ile o
f th
e C
hesh
ire
Cat
of
“Alic
e in
Won
derl
and.
” Su
chpa
tter
ns a
re s
omet
imes
cal
led
ghos
t cr
ater
s. T
his
crat
er h
asar
rive
d af
ter
the
Imbr
ium
Bas
in e
vent
, bu
t be
fore
Mar
eIm
briu
m c
over
ed t
he b
asin
floo
r. T
he c
rate
r ri
m w
as p
roba
-bl
y co
mpl
etel
y co
vere
d w
ith
mar
e la
va,
but
afte
r th
e la
vaco
oled
and
con
trac
ted,
the
rim
rea
ppea
red
as a
mar
e ri
dge.
The
n La
mbe
rt a
rriv
ed, c
over
ing
the
ridg
e ov
er t
he n
orth
ern
rim
of
the
ghos
t cr
ater
wit
h ej
ecta
. Cop
erni
cus
then
dra
ped
rays
ove
r th
e co
mpo
siti
on fo
r fu
rthe
r in
tere
st.
LO4-
126H
3Su
n El
evat
ion:
19.
5°A
ltit
ude:
267
7.28
km
13
9Im
bri
um
Ba
sin R
egio
n
The
30-
km c
rate
r La
mbe
rt h
as m
ulti
ple
circ
umfe
rent
ial r
ings
in i
ts fl
oor,
sug
gest
ing
that
it
has
pene
trat
ed t
he s
olid
mar
esu
rfac
e an
d hi
t so
met
hing
dif
fere
nt b
elow
, sem
imol
ten
lava
or p
erha
ps t
he m
elt
shee
t of
the
bas
in fl
oor
bene
ath
the
mar
e. S
ince
Lam
bert
lef
t it
s ej
ecta
bla
nket
on
the
mar
esu
rfac
e, a
fre
sh fl
ow (
Apo
llo 1
5 fr
ame
M10
09)
has
cove
red
muc
h of
the
east
ern
sect
or o
f Lam
bert
’s s
econ
dary
fiel
d. T
heti
ny c
rate
r Sa
mps
on is
in th
e ce
nter
of a
sha
llow
30-
km d
ome
and
coul
d be
a s
ourc
e of
thi
s flo
w.
The
pyr
amid
al r
ocks
nort
heas
t of
Lam
bert
cou
ld b
e pe
aks
of a
n in
ner
ring
of
the
Imbr
ium
Bas
in. T
he c
ente
r of
the
basi
n (3
3°N
, 18°
W)
is n
ear
the
top
of th
is p
hoto
.
LO4-
127H
1Su
n El
evat
ion:
21.
8°A
ltit
ude:
288
6.35
km
14
0Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
The
cen
ter
of M
are
Imbr
ium
, nea
r th
e bo
ttom
of t
his
pict
ure
and
the
top
of L
O4-
127H
1, i
s ne
arly
dev
oid
of m
are
ridg
esan
d ri
lles.
Onl
y im
pact
cra
ters
and
ray
s re
lieve
the
uni
for-
mit
y of
sur
face
topo
grap
hy.
LO4-
127H
2Su
n El
evat
ion:
21.
8°A
ltit
ude:
288
6.35
km
14
1Im
bri
um
Ba
sin R
egio
n
The
Mon
tes
Alp
es c
onst
itut
e th
e no
rthe
rn r
im o
f th
eIm
briu
m B
asin
, whi
ch p
asse
s th
roug
h th
e no
rthe
rn p
art
ofth
e m
agni
ficen
t La
te I
mbr
ian
crat
er P
lato
. Pl
ato
falls
on
a“c
onti
nent
al d
ivid
e” i
n a
sens
e: r
ima
dire
ct fl
ows
from
its
oute
r ra
mpa
rts
sout
h to
war
d th
e ce
nter
of
the
Imbr
ium
Bas
in a
nd n
orth
tow
ard
the
basi
n’s
oute
r tr
ough
, w
hich
unde
rlie
s M
are
Frig
oris
. The
rill
e la
bele
d R
imae
Pla
to in
this
phot
o is
a
trib
utar
y of
a
larg
er
syst
em.
It
seem
s to
flo
w b
enea
th th
e su
rfac
e ne
ar th
e ed
ge o
f the
pho
to, p
ossi
bly
into
a l
ava
tube
tha
t su
rfac
es a
bout
15
km d
owns
lope
(L
O4-
115H
3). P
lato
and
Mar
e Fr
igor
is a
re b
elie
ved
to h
ave
been
floo
ded
in t
he E
rato
sthe
nian
age
, wel
l aft
er t
he p
art
ofM
are
Imbr
ium
see
n so
uth
of P
lato
in th
is p
ictu
re. T
he s
harp
crat
ers
in t
he 1
0-km
ran
ge a
re p
roba
bly
seco
ndar
ies
from
Plat
o.
LO4-
127H
3Su
n El
evat
ion:
21.
8°A
ltit
ude:
288
6.35
km
14
2Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
LO4-121HSun Elevation: 19.6°Altitude: 2681.82 km
Timocharis is a crater with moderatelysharp features but whose ray pattern hasblended with the surrounding terrain due to exposure to the solar wind andgardening by meteorite bombardment.These characteristics, plus measurementsof craters on its floor and ejecta, establishits age as Eratosthenian.
Copernicus is just south of MontesCarpatus, the local name of the highestring of the Imbrium Basin. The ejectapattern of this moderately young andspectacular crater is typical of both largecraters and basins. A rampart of materialis thrown outside of the rim. Further out,there is a heavy blanket of ejecta withradial striations. At about one radiusaway from the rim, the ejecta blanketthins, leaving uncovered areas, and thenbecomes a field of secondary craters for adistance of about one diameter awayfrom the rim. Rays of fine, bright mater-ial extend for many diameters.
Well south of Copernicus, there areridges and valleys from the NubiumBasin (overlain with Imbrium secon-daries). A pair of simultaneous im-pactors produced Fauth and its smallerunnamed companion. 1
43
Imb
rium
Ba
sin R
egio
n
The
sur
face
of
Mar
e Im
briu
m, l
ike
that
of
all l
arge
mar
e, i
str
aver
sed
by lo
w r
idge
s be
lieve
d to
res
ult
from
com
pres
sion
stre
sses
as
the
mar
e co
ols
and
cont
ract
s. L
ava
may
find
its
way
to
the
surf
ace
thro
ugh
faul
ts i
n th
ese
ridg
es. T
here
is
alo
w 3
0-km
dom
e to
pped
by
crat
er S
amps
on t
hat
may
be
aso
urce
for
such
a fl
ow.
LO4-
122H
1Su
n El
evat
ion:
20.
7°A
ltit
ude:
289
5.02
km
14
4Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
Bas
ins
ofte
n ha
ve r
ings
ins
ide
thei
r ri
m a
s w
ell
as o
utsi
de.
Mon
tes
Ten
erif
fe, M
ons
Pico
, and
the
pea
k to
the
sou
th o
fM
ons
Pico
may
be
sign
s of
suc
h a
ring
, m
ost
of w
hich
is
cove
red
by d
eep
lava
flow
s.
LO4-
122H
2Su
n El
evat
ion:
20.
7°A
ltit
ude:
289
5.02
km
14
5Im
bri
um
Ba
sin R
egio
n
LO4-114HSun Elevation: 19.3°Altitude: 2687.21 km
Montes Apenninus marks the rim of theImbrium Basin and the edge of MareImbrium. As in other maria and otherparts of Mare Imbrium, there are radialand circumferential ridges near thisedge of the mare. Pupin is interestingbecause it is a bright mound with acentral crater and no ray pattern, sug-gesting that it may be a volcanic feature.A pair of matched impactors may havecaused Feuillee and Beer. Wallace hasbeen nearly flooded, an indication ofthe depth of lava there.
Sinus Aestuum was formed by lavaflowing into the valley south of the rimof Imbrium, as Mare Frigoris covers the valley north of the Montes Alpes.Eratosthenes is the type crater of theEratosthenian Period; it formed afterSinus Aestuum was flooded. long afterthe Imbrium impact. However, rays havebeen nearly blended away and its rimstructure has been slightly degraded.
Stadius, flooded by lava that has beencovered by ejecta from Eratosthenes,must be from an earlier time. Darkmantling material surrounds Gambartand the nearby striations from Nubium.Surveyor 2 (September 1966) crashedafter an unsuccessful midcourse cor-rection.
14
6Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
Mon
tes
Spiz
berg
en a
nd th
e ne
arby
isla
nd a
rcs
mar
k an
inne
rri
ng o
f th
e Im
briu
m B
asin
, la
rgel
y su
bmer
ged
unde
r th
em
are
surf
ace;
cir
cum
fere
ntia
l mar
e ri
dges
mar
k it
s lo
cati
onin
oth
er s
ecto
rs. T
he M
onte
s A
rchi
med
es r
ange
s, a
ltho
ugh
over
lain
by
ejec
ta fr
om A
rchi
med
es, s
eem
too
mas
sive
to
beca
used
onl
y by
tha
t cr
ater
and
pro
babl
y w
ere
rais
ed b
y on
eor
mor
e ri
ngs
wit
hin
the
Imbr
ium
Bas
in. T
he t
wo
ring
s m
aybe
ana
logo
us to
the
two
rang
es o
f Mon
tes
Roo
k. T
he p
late
auth
ey r
est u
pon
is c
alle
d th
e A
penn
ine
benc
h. A
n ou
ter
ring
of
the
Insu
laru
m B
asin
to
the
sout
hwes
t m
ay a
lso
have
hel
ped
to r
aise
the
elev
atio
n of
the
Ape
nnin
e be
nch.
LO4-
115H
1Su
n El
evat
ion:
20.
9°A
ltit
ude:
290
5.14
km
14
7Im
bri
um
Ba
sin R
egio
n
Prom
onto
rium
Aga
ssiz
mar
ks t
he e
aste
rn e
nd o
f M
onte
sA
lpes
, at
the
nort
heas
tern
sec
tor
of t
he r
im o
f th
e Im
briu
mB
asin
. Mon
s Pi
ton
mar
ks a
rin
g w
ithi
n th
e ba
sin
(see
LO
4-12
2H2
for
mor
e pe
aks
mar
king
tha
t ri
ng).
The
lar
ge m
are
ridg
e th
at u
nder
lies
Piaz
zi S
myt
h m
ay a
lso
be r
elat
ed to
that
ring
. The
ray
s co
me
from
Ari
still
us to
the
sout
heas
t.
LO4-
115H
2Su
n El
evat
ion:
20.
9°A
ltit
ude:
290
5.14
km
14
8Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
Val
lis
Alp
es c
ould
be
a va
lley
form
ed i
n th
e ri
m o
f th
eIm
briu
m B
asin
dur
ing
impa
ct o
r co
uld
rela
te to
a d
eep
frac
-tu
re o
pene
d by
str
esse
s du
ring
or
shor
tly
afte
r th
e im
pact
. It
may
hav
e be
en fl
oode
d w
ith
lava
fro
m M
are
Imbr
ium
, but
the
lava
may
als
o ha
ve c
ome
from
bel
ow, a
s w
ith
rim
ae in
the
area
, flow
ing
in t
his
case
bot
h to
Mar
e Im
briu
m a
nd t
owar
dM
are
Frig
oris
.
LO4-
115H
3Su
n El
evat
ion:
20.
9°A
ltit
ude:
290
5.14
km
14
9Im
bri
um
Ba
sin R
egio
n
Sinu
s M
edii
and
the
unam
ed c
ircu
lar
area
of m
are
to th
e w
est
of it
may
hav
e be
en fo
rmed
in c
rate
rs. B
ode
has
impa
cted
the
first
out
er r
ing
of I
mbr
ium
; Pal
las
and
Mur
chis
on h
ave
been
degr
aded
by
the
form
atio
n of
tha
t ri
ng a
nd t
hen
part
lyco
vere
d by
Im
briu
m e
ject
a. T
he s
quar
e br
ight
are
a in
the
ridg
e be
twee
n Si
nus
Med
ii an
d it
s co
mpa
nion
to
the
wes
t is
an a
rtif
act
due
to a
tem
pora
ry l
oss
of c
omm
unic
atio
nbe
twee
n Lu
nar
Orb
iter
and
the
Dee
p Sp
ace
Net
wor
k.
LO4-
109H
1Su
n El
evat
ion:
20.
5°A
ltit
ude:
269
3.03
km
15
0Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
Sinu
s A
estu
um a
nd M
are
Vap
orum
hav
e flo
oded
the
val
ley
outs
ide
of t
he r
im o
f th
e Im
briu
m B
asin
, w
hich
is
rep-
rese
nted
her
e by
the
Mon
tes
Ape
nnin
us a
nd M
ons
Wol
ff.
Her
e, la
rge
radi
al v
alle
ys fo
rmed
by
the
Imbr
ium
impa
ct c
anbe
see
n. V
allis
Alp
es (
LO4-
115H
3) c
ould
be
a si
mila
r (b
utde
eper
) va
lley.
Mar
co P
olo
can
just
bar
ely
be p
erce
ived
unde
r it
s th
ick
cove
r of
Ape
nnin
us m
ater
ial,
the
inne
r Fr
aM
auro
For
mat
ion,
whi
ch is
equ
ival
ent
to t
he in
ner
Hev
eliu
sFo
rmat
ion
of O
rien
tale
. Thi
s m
ater
ial h
as b
een
esti
mat
ed t
obe
1 t
o 2
km t
hick
nea
r th
e cr
est
of t
he M
onte
s A
penn
inus
.D
ark
man
tlin
g m
ater
ial
cove
rs b
oth
mar
e an
d hi
ghla
ndsu
rfac
es in
the
vici
nity
of R
imae
Bod
e.
LO4-
109H
2Su
n El
evat
ion:
20.
5°A
ltit
ude:
269
3.03
km
15
1Im
bri
um
Ba
sin R
egio
n
The
Ape
nnin
e be
nch
stre
tche
s be
twee
n A
rchi
med
es a
ndM
onte
s A
penn
inus
(se
e th
e no
te f
or L
O4-
115H
1).
Rim
aB
radl
ey is
pre
sum
ably
a s
uper
ficia
l sig
n of
a c
ircu
mfe
rent
ial
faul
t cau
sed
by te
nsio
nal s
tres
s in
this
are
a. I
t cro
sses
mat
er-
ial s
lum
ped
from
the
rim
of
the
Imbr
ium
Bas
in (
here
cal
led
Mon
s B
radl
ey)
and
mar
e su
rfac
e w
ith
seem
ing
indi
ffer
ence
,an
ind
icat
ion
of a
dee
p fr
actu
re.
Not
e th
at t
he s
ize
of t
hesl
ump
bloc
ks s
eem
to
fit t
he c
orre
spon
ding
edg
es o
f M
ons
Bra
dley
. T
his
phot
o an
d LO
4-11
0H1
are
as c
lose
to
the
east
ern
edge
of
the
Imbr
ium
Bas
in a
s is
cov
ered
in
this
chap
ter
on th
e Im
briu
m B
asin
Reg
ion.
The
eas
tern
edg
e an
dej
ecta
to th
e ea
st a
re c
over
ed in
the
chap
ter
on th
e Se
reni
tati
sB
asin
Reg
ion.
LO4-
109H
3Su
n El
evat
ion:
20.
5°A
ltit
ude:
269
3.03
km
15
2Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
The
Apo
llo 1
5 la
ndin
g si
te w
as b
oldl
y ch
osen
to
be n
ear
Rim
a H
adle
y an
d M
ons
Had
ley
beyo
nd t
he e
aste
rn e
dge
ofth
is p
ictu
re.
Aut
olyc
us h
as i
mpa
cted
a p
lain
s un
it i
n th
eIm
briu
m B
asin
tha
t ap
pear
s to
be
rich
in
KR
EEP
min
eral
s(p
otas
sium
, rar
e ea
rth
elem
ents
, and
pho
spho
rus)
. It
is t
hepr
obab
le s
ourc
e of
a b
ould
er c
onta
inin
g K
REE
P th
at w
assa
mpl
ed (
1540
5) b
y th
e A
pollo
15
crew
. T
he a
ge o
f th
esa
mpl
e (a
s it
was
pre
sum
ably
res
truc
ture
d by
the
sho
ck o
fth
e A
utol
ycus
impa
ct)
was
foun
d to
be
1.29
bill
ion
year
s, th
eyo
unge
st a
ge o
f all
date
d lu
nar
rock
sam
ples
. If A
utol
ycus
isno
t th
e so
urce
of
this
sam
ple,
the
n it
may
hav
e co
me
from
Ari
still
us. F
or a
ddit
iona
l dis
cuss
ion
of th
e A
pollo
15
site
, see
the
note
for
LO
4-10
3H1
in t
he c
hapt
er o
n th
e Se
reni
tati
sB
asin
Reg
ion
(Cha
pter
9).
LO4-
110H
1Su
n El
evat
ion:
20.
8°A
ltit
ude:
291
5.82
km
15
3Im
bri
um
Ba
sin R
egio
n
LO4-
110H
2Su
n El
evat
ion:
20.
8°A
ltit
ude:
291
5.82
km
15
4Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
Bey
ond
Mon
tes
Alp
es l
ies
the
Alp
es F
orm
atio
n. A
ltho
ugh
sim
ilar
in
rela
tion
ship
to
the
Imbr
ium
Bas
in,
the
Alp
esFo
rmat
ion
has
a ve
ry d
iffe
rent
app
eara
nce
than
the
Fra
Mau
ro F
orm
atio
n (L
O4-
109H
2).
An
obli
que
impa
ct m
ayha
ve i
nduc
ed a
sym
met
ry o
f th
e ej
ecta
bla
nket
. T
he h
um-
moc
ky a
ppea
ranc
e of
the
Alp
es F
orm
atio
n, w
hich
ext
ends
far
beyo
nd M
are
Imbr
ium
, is
sim
ilar
to th
at o
f the
Mon
tes
Roo
kFo
rmat
ion
of t
he O
rien
tale
Bas
in. C
assi
ni a
nd o
ther
nea
rby
crat
ers
of s
imila
r si
ze s
eem
to h
ave
supp
ress
ed th
e ri
m o
f the
Imbr
ium
Bas
in. T
he e
ject
a bl
anke
t of
Cas
sini
has
a m
olte
nap
pear
ance
, as
if t
he im
pact
or la
nded
in m
are
mat
eria
l tha
tha
d no
t ful
ly s
olid
ified
or
that
was
suf
ficie
ntly
hot
that
it w
asliq
uefie
d by
the
ener
gy o
f im
pact
.
8.1. OverviewBasins, Maria, and HighlandsThe Nectaris region (Figure 8.1) has extensive highlands, in-tensively cratered terrain whose large-scale topography hasbeen established in very ancient times (in the Pre-NectarianPeriod).
From the time of the formation of the Nectaris Basin, thehighlands have been affected by ejecta (including secondaryimpactors) from basins such as Nectaris and Imbrium and alsofrom craters such as Tycho, whose rays can be seen streakingacross the southeast portion of the photo in Figure 8.1.
An especially interesting part of this region is the areawhere the Nectaris Basin intersects with the FecunditatisBasin to the west and the Tranquillitatis Basin to the north.
Figure 8.2 illustrates the size of the Nectaris Basin, muchlarger than Mare Nectaris.
Figure 8.3 shows three of the rings of the Nectaris Basin.These rings have been drawn so that the second ring fromthe center is the square root of 2 greater than the inner ringand the third ring from the center is the square root of 2greater than the second ring. With this constraint, the sizeand center of the set of rings have been adjusted to matchtopographic highs.
Like other major basins, Nectaris has thrown a heavyblanket of ejecta that forms radial ridges and troughs outsideof its major ring, the rim. In the case of Nectaris, this ejectablanket has been degraded by further basin impacts to itsnorth and east. However, the formation is clearly seen to thesouth (Figure 8.4).
Chapter 8
Nectaris Basin Region
Figure 8.1. LO4-096M. This picture is centered on the southeastern partof the central highlands of the near side. The small mare east of the centralhighlands is Mare Nectaris. It occupies the middle of the Nectaris Basin,which is much larger than the mare. East of Mare Nectaris, at the edge of thepicture, is the western portion of Mare Fecunditatis. North of Mare Nectarisand Mare Fecunditatis is Mare Tranquillitatis in the Crisium Basin Region.
15
5N
ecta
ris
Ba
sin R
egio
n
Figure 8.2. Part of LO4-083M. The arc of cliffs outlined by the morningsun is the Rupes Altai (the Altai scarp). It outlines the major ring of theNectaris Basin.
Apollo LandingApollo Mission 16 landed in the midst of the south-centralhighlands (LO4-089H3), near the boundary between theCayley and Descartes Formations. This was the first missionwith a Lunar Roving Vehicle, which permitted the astronautsto reach both formations. Before the mission, these terraintypes were thought to be volcanic. In the course of the mis-sion it became clear to both the astronauts, who were partic-ularly well trained in geology, and the support geologists atMission Control that ejecta from Imbrium had covered bothareas. The astronauts revised their sample collection strategyto improve characterization of the impact-dominatedterrain. Analysis of the samples helped establish the age ofthe Imbrium impact event (3.85 billion years). In addition,some samples from the Descartes Formation, probably exca-
vated from an underlying layer of ejecta from the NectarisBasin, were dated at 3.92 billion years.
8.2. High-Resolution ImagesTable 8.1 shows the high-resolution images of the NectarisBasin Region in schematic form.
The following pages show the high-resolution subframesfrom south to north and west to east. That is, they are in theorder LO4-100H1, LO4-100H2, LO4-100H3, LO4-101H1,LO4-101H2, LO4-101H3, LO4-095H1… LO4-053H3.
Photos LO-095H1, LO-083H1, and LO4-071H1 are redun-dant and have not been printed, although the cleaned imagesare in the enclosed CD.
LO096H and LO077H are printed as full frame.
15
6Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
Figure 8.3. LO4-084M. The ridge marked by the innermost ring, whoseeastern sector passes over the Montes Pyrenaeus (LO4-065H2), bounds thecentral area of mare flooding (partly blocked or covered by ejecta from latercraters). The outer ring is the main ring; aligned with Rupes Altai. Troughsbetween the rings are partly filled with mare.
Figure 8.4. LO4-052M. These deep troughs and ridges south of theNectaris Basin were produced by ejecta from that basin. The pattern issimilar to the Fra Mauro Formation of the Imbrium Basin, to the HeveliusFormation of the Orientale Basin, and to the secondary-impact crater fieldsof those basins.
Latitude Range Photo Number
0–27 N 109 102 097 090 085 078 073 66 061 054
0–27 S 108 101 096 089 084 077 072 65 060 053 046
27 S–56 S 107 100 095 088 083 076 071 64 059 052
56 S–90 S 094 082 070 058 044
Longitude 3 W 4 E 10 E 10 E 16 E 24 E 30 E 38 E 49 E 57 E 63 Eat Equator
Table 8.1. The cells shown in white represent the high-resolution photos of the Nectaris Basin Region (LO4-XXX H1, -H2, and -H3, where XXX is the PhotoNumber). The Humorum Basin Region is to the west, the Imbrium Basin Region is to the northwest, the Serenitatis Basin Region is to the north, the EasternBasins Region is to the east, and the South Polar Region is to the south.
In t
his
high
land
s re
gion
, th
e re
lati
ve a
ges
of c
rate
rs a
reju
dged
by
the
amou
nt o
f de
grad
atio
n of
the
ir r
ims
and
the
dens
ity
of s
mal
l cr
ater
s on
the
ir fl
oors
. A
ltho
ugh
the
larg
ecr
ater
s he
re a
re a
ssig
ned
to t
he P
re-N
ecta
rian
Per
iod,
Bac
ose
ems
muc
h fr
eshe
r th
an H
omm
el,
but
Tan
neru
s m
ay b
eyo
unge
r th
an B
aco.
Fre
sh-l
ooki
ng c
rate
rs in
the
5-k
m r
ange
in t
his
area
are
bel
ieve
d to
be
Ori
enta
le B
asin
sec
onda
ries
,ev
en t
houg
h th
e ce
nter
of
that
bas
in i
s fu
lly 9
0°ar
ound
the
Moo
n (a
bout
150
0 km
to
the
wes
t) a
way
. Lig
ht r
ays
in t
heea
st-w
est
dire
ctio
n an
d th
e st
ring
s of
cra
ters
sou
th o
fT
anne
rus
are
from
Tyc
ho.
LO4-
100H
1Su
n El
evat
ion:
21.
3°A
ltit
ude:
297
8.20
km
15
7N
ecta
ris
Ba
sin R
egio
n
The
clu
ster
of
crat
ers
near
the
int
erse
ctio
n of
Sto
fler
and
Fara
day
is a
ligne
d in
the
dir
ecti
on o
f th
e Im
briu
m B
asin
,w
hose
rim
is
abou
t 20
00 k
m a
way
. T
he c
lust
ers
alon
g th
e 10
°ea
st m
erid
ian
are
alig
ned
wit
h th
e di
rect
ion
of th
e So
uth
Pole
–Aik
en B
asin
, abo
ut 1
300
km a
way
, but
may
com
e fr
omth
e yo
unge
r Se
reni
tati
s B
asin
, abo
ut 1
800
km t
o th
e no
rth-
nort
heas
t.
LO4-
100H
2Su
n El
evat
ion:
21.
3°A
ltit
ude:
297
8.20
km
15
8Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
The
nei
ghbo
ring
cra
ters
Wer
ner
and
Alia
cens
is r
evea
l muc
hof
the
mec
hani
cs o
f cra
ter
form
atio
n an
d su
bseq
uent
ero
sion
in t
his
high
land
are
a. T
he e
ject
a fr
om W
erne
r ha
s be
en d
e-po
site
d on
the
rim
of A
liace
nsis
; the
forc
e of
the
dep
osit
ion,
perh
aps
aide
d by
the
sho
ck w
ave
of t
he im
pact
, has
pus
hed
abou
t 20
km
of
the
rim
of
Alia
cens
is o
nto
its
floor
. Bec
ause
thes
e tw
o cr
ater
s ar
e si
mila
r in
siz
e an
d ha
ve im
pact
ed s
im-
ilar
terr
ain,
they
pro
babl
y ha
d si
mila
r to
pogr
aphy
whe
n th
eyw
ere
form
ed. T
he o
lder
Alia
cens
is h
as h
ad t
he t
extu
re o
f it
sej
ecta
bla
nket
ero
ded
away
by
subs
eque
nt i
mpa
cts.
Man
ym
ore
smal
l cra
ters
(le
ss th
an 5
km
) ca
n be
see
n in
the
area
of
its
form
er e
ject
a bl
anke
t tha
n in
that
of W
erne
r.
LO4-
100H
3Su
n El
evat
ion:
21.
3°A
ltit
ude:
297
8.20
km
15
9N
ecta
ris
Ba
sin R
egio
n
Rad
ial e
ject
a fe
atur
es fr
om E
rato
sthe
nian
cra
ter
Wer
ner
can
be s
een
up t
o tw
o ra
dii
from
its
rim
. Thi
s ej
ecta
bla
nket
is
supe
rim
pose
d on
irr
egul
ar c
rate
rs,
ridg
es,
and
valle
ys t
hat
are
radi
al t
o th
e Im
briu
m B
asin
, pa
rt o
f th
e Fr
a M
auro
Form
atio
n. S
econ
dary
cra
ters
fro
m t
he I
mbr
ium
Bas
in a
lso
perv
ade
this
are
a, e
xcep
t w
here
the
y ar
e co
vere
d by
the
Wer
ner
ejec
ta b
lank
et.
Ben
eath
the
Fra
Mau
ro F
orm
atio
n,Pl
ayfa
ir,
Api
anus
, an
d K
ruse
nste
rn h
ave
redi
stri
bute
d th
eri
m m
ater
ial
from
an
olde
r un
nam
ed 1
15-k
m c
rate
r. T
hecr
ater
clu
ster
nea
r th
e ri
ght
edge
of
this
pho
to i
s fr
om t
heN
ecta
ris
Bas
in.
LO4-
101H
1Su
n El
evat
ion:
21.
1°A
ltit
ude:
272
0.44
km
16
0Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
Dee
p gr
oove
s fo
rmed
by
chai
ns o
f cra
ters
illu
stra
te th
is a
rea
of t
he F
ra M
auro
For
mat
ion.
Tra
ces
of s
uch
groo
ves
rem
ain
on t
he fl
oor
of A
lbat
egni
us, b
ut a
ppea
r to
hav
e be
en b
urie
dby
a r
elat
ivel
y sm
ooth
laye
r of
pla
ins
mat
eria
l. In
som
e ar
eas
such
mat
eria
l may
hav
e be
en d
epos
ited
by
basi
n ej
ecta
, but
the
abru
pt t
rans
itio
n he
re b
etw
een
groo
ves
and
plai
ns s
ug-
gest
s a
volc
anic
ori
gin
from
wit
hin
the
crat
er.
Vog
el a
nd
its
com
pani
on t
o th
e no
rth
seem
to
be s
econ
dari
es f
rom
Imbr
ium
ass
ocia
ted
wit
h a
larg
e gr
oove
. Air
y, o
n th
e ot
her
hand
, has
bee
n ne
arly
bur
ied
by Im
briu
m e
ject
a.
LO4-
101H
2Su
n El
evat
ion:
21.
1°A
ltit
ude:
272
0.44
km
16
1N
ecta
ris
Ba
sin R
egio
n
Thi
s ar
ea is
dom
inat
ed b
y th
e Fr
a M
auro
For
mat
ion,
em
erg-
ing
from
the
mar
e su
rfac
e of
Sin
us M
edii
and
the
floor
of
the
Hip
parc
hus
crat
er. T
he fl
oor
of P
tole
mae
us, l
ike
that
of
Alb
eteg
nius
(LO
4-10
1H2)
, is
cove
red
wit
h lig
ht p
lain
s m
ater
-ia
l tha
t has
obs
cure
d th
e Fr
a M
auro
For
mat
ion.
LO4-
101H
3Su
n El
evat
ion:
21.
1°A
ltit
ude:
272
0.44
km
16
2Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
095H
2Su
n El
evat
ion:
21.
6°A
ltit
ude:
297
5.51
km
16
3N
ecta
ris
Ba
sin R
egio
n
The
nor
thw
est
floor
s of
Mau
roly
cus
and
Bar
ociu
s ar
eco
vere
d w
ith
heav
y de
posi
ts o
f ej
ecta
tho
ught
to
be t
hem
argi
n of
the
oute
r de
posi
ts fr
om th
e Im
briu
m B
asin
. Som
ech
ains
of
smal
l se
cond
arie
s fr
om t
he n
orth
-nor
thea
st a
refr
om N
ecta
ris,
who
se r
im i
s ab
out
1.5
radi
i aw
ay.
Fres
her
clus
ters
of
crat
ers
are
prob
ably
fro
m t
he I
mbr
ium
Bas
in,
even
tho
ugh
this
are
a is
tw
o ba
sin
radi
i aw
ay f
rom
the
Imbr
ium
rim
.
Thi
s in
tere
stin
g pi
ctur
e sh
ows
cros
sing
pat
tern
s of
cra
ter
chai
ns a
nd s
tria
tion
s fr
om I
mbr
ium
to
the
nort
h-no
rthw
est
and
Nec
tari
s to
the
eas
t-no
rthe
ast.
The
floo
rs o
f G
emm
aFr
isiu
s, G
ooda
cre,
and
the
cra
ters
to
the
sout
heas
t sh
owre
surf
acin
g by
ligh
t pla
ins
mat
eria
ls.
LO4-
095H
3Su
n El
evat
ion:
21.
6°A
ltit
ude:
297
5.51
km
16
4Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
LO4-096H1Sun Elevation: 21.8°Altitude: 2722.26 km
The fresh, sharp craters in the clustersoutheast of Hipparchus are all bright inClementine albedo data. The rays andbright ejecta come mostly from thecrater to the northeast of Hind. Themottled dark areas are concentrated inlow-lying terrain, with the exception ofa dark plateau south of Lade with sharpedges that may be a flow. Clementinegravity data show a positive anomalyhere that is similar to those under mareareas, but weaker. Could there havebeen an early stage of mare formationhere that did not go to completion?
Burnham, in the midst of light plains,has a roughly circular raised rim, butthe floor is not depressed. Further, the rim is breached with grooves thatsuggest flow to the outside. BetweenBurnham and Abulfeda there is anotherirregular rim, surrounded by a flow witha lobate edge. These features may havebeen produced by molten ejecta fromthe Nectaris Basin.
The ridge and the crater chain nearPlayfair are from the direction of theNectaris Basin to the east-northeast, as are many other striations in thisarea. Many of the craters show signs ofbeing covered by Nectaris ejecta and soare considered Pre-Nectarian. However,Playfair is relatively unmarked, so it hasbeen classified as Nectarian.
16
5N
ecta
ris
Ba
sin R
egio
n
Not
e ho
w fl
at t
his
area
see
ms,
rel
ativ
e to
sur
roun
ding
are
as.
It w
ould
be
the
nort
heas
t qu
adra
nt o
f the
floo
r of
a p
ossi
ble
larg
e Pr
e-N
ecta
rian
bas
in n
amed
Mut
us-V
laq.
The
bas
inflo
or w
ould
hav
e ob
liter
ated
any
ear
lier
crat
erin
g an
d pr
o-vi
ded
the
basi
c fla
tnes
s. T
hen,
sec
onda
ries
and
oth
er e
ject
afr
om th
e N
ecta
ris
Bas
in w
ould
hav
e ar
rive
d, fo
llow
ed b
y se
c-on
dari
es fr
om Im
briu
m.
LO4-
088H
2Su
n El
evat
ion:
21.
7°A
ltit
ude:
297
3.74
km
16
6Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
Pons
, W
ilki
ns,
Zag
ut,
Lind
emau
, an
d R
abbi
Lev
i li
e on
am
assi
ve h
ighl
ands
rid
ge th
at h
as th
e hi
ghes
t ele
vati
on o
n th
een
tire
nea
r si
de, a
bout
400
0 m
abo
ve t
he fl
oor
of t
he n
earb
yN
ecta
ris
Bas
in. T
he h
ighl
y er
oded
cra
ters
Zag
ut a
nd R
abbi
Levi
are
Pre
-Nec
tari
an in
age
and
hav
e be
en c
over
ed in
eje
cta
from
the
Nec
tari
s B
asin
. Gro
oves
and
rid
ges
from
Nec
tari
sca
n be
see
n in
the
nort
heas
t rim
of Z
agut
and
on
the
floor
of
Rab
bi L
evi.
Cha
ins
of s
econ
dari
es fr
om Im
briu
m li
e be
twee
nPo
ntan
us a
nd W
ilkin
s.
LO4-
088H
3Su
n El
evat
ion:
21.
7°A
ltit
ude:
297
3.74
km
16
7N
ecta
ris
Ba
sin R
egio
n
Cle
men
tine
ele
vati
on d
ata
show
a d
epre
ssio
n th
at m
ay m
ark
a ve
ry o
ld c
rate
r ab
out
225
km i
n di
amet
er,
cent
ered
nea
r 17
°ea
st, 2
6°so
uth
(das
hed
circ
le).
The
floo
r of
thi
s po
ssib
lecr
ater
wou
ld b
e ab
out 1
500
m b
elow
the
rim
. The
are
a to
the
east
is h
eavi
ly c
over
ed w
ith
the
Nec
tari
s ej
ecta
bla
nket
.
LO4-
089H
1Su
n El
evat
ion:
21.
9°A
ltit
ude:
272
4.41
km
16
8Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
Thi
s un
usua
l te
rrai
n ha
s be
en c
alle
d th
e D
esca
rtes
For
-m
atio
n; t
he a
rea
is h
eavi
ly c
over
ed b
y ej
ecta
fro
m t
heN
ecta
ris
Bas
in, w
hose
mai
n ri
ng is
onl
y on
e ba
sin
radi
us t
oth
e ea
st. D
esca
rtes
its
elf
has
been
nea
rly
buri
ed b
y N
ecta
ris
ejec
ta. A
bulfe
da, h
owev
er, s
how
s no
sig
n of
eje
cta,
and
mus
tbe
of
the
Nec
tari
an P
erio
d or
you
nger
. C
aten
a A
bulf
eda
isno
t qui
te r
adia
l to
the
cent
er o
f the
Imbr
ium
Bas
in, a
ltho
ugh
it a
ligns
wit
h th
e so
uthw
este
rn r
im o
f tha
t bas
in. T
he c
aten
a’s
impa
ctor
s co
uld
be a
set
of p
rim
arie
s fr
om a
dis
rupt
ed c
omet
like
Shoe
mak
er-L
evy
9.
LO4-
089H
2Su
n El
evat
ion:
21.
9°A
ltit
ude:
272
4.41
km
16
9N
ecta
ris
Ba
sin R
egio
n
Apo
llo 1
6 la
nded
in t
his
site
to
expl
ore
both
the
ligh
t pl
ains
(Cay
ley
Form
atio
n) a
nd t
he n
earb
y hu
mm
ocky
Des
cart
esFo
rmat
ion.
A m
ajor
obj
ecti
ve w
as t
o co
nfirm
tha
t th
e tw
ofo
rmat
ions
wer
e vo
lcan
ic.
Inst
ead,
ana
lysi
s of
the
roc
ksa
mpl
es s
how
ed t
hat
the
form
atio
ns w
ere
ejec
ta d
epos
its.
Bot
h D
esca
rtes
and
Cay
ley
Form
atio
ns a
re p
roba
bly
loca
las
pect
s of
eje
cta
from
the
Im
briu
m B
asin
. M
ost
of t
hesa
mpl
es w
ere
of c
ours
e of
the
uppe
r la
yer,
from
the
youn
ger
Imbr
ium
Bas
in, b
ut s
ome
sam
ples
may
be
from
Nec
tari
s. I
fso
, the
age
s of
thes
e sa
mpl
es e
stab
lish
the
age
of th
e N
ecta
ris
Basi
n (a
nd th
us th
e bo
unda
ry b
etw
een
the
Pre-
Nec
tari
an a
ndN
ecta
rian
Per
iods
) as
3.9
2 ae
ons
(bill
ions
of y
ears
bef
ore
the
pres
ent)
.
LO4-
089H
3Su
n El
evat
ion:
21.
9°A
ltit
ude:
272
4.41
km
17
0Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
The
reg
ion
cove
red
by h
eavy
, hu
mm
ocky
dep
osit
s in
the
vici
nity
of J
anss
en is
the
type
are
a of
the
Jans
sen
Form
atio
n,an
eje
cta
blan
ket
from
the
Nec
tari
s B
asin
. It
is c
ompa
rabl
eto
the
Inn
er H
evel
ius
Form
atio
n of
the
Ori
enta
le B
asin
and
the
Fra
Mau
ro F
orm
atio
n of
the
Imbr
ium
Bas
in. T
his
form
a-ti
on h
as b
een
obsc
ured
by
Imbr
ium
eje
cta
to t
he w
est
of t
heba
sin
(not
e th
e ch
ain
of s
econ
dari
es in
the
uppe
r le
ft c
orne
r).
The
floo
r an
d ej
ecta
of
Jans
sen
(LO
4-07
6H2)
are
cov
ered
wit
h N
ecta
ris
ejec
ta.
LO4-
083H
2Su
n El
evat
ion:
22.
8°A
ltit
ude:
297
1.86
km
17
1N
ecta
ris
Ba
sin R
egio
n
Rup
es A
ltai
(LO
4-08
4H1)
mar
ks t
he m
ain
ring
of
the
Nec
tari
s B
asin
. Thi
s ar
ea il
lust
rate
s th
e m
etho
ds o
f ass
igni
ngag
es t
o la
rge
crat
ers.
Zag
ut,
Rab
bi L
evi,
and
Ric
cius
hav
ebe
en c
ompl
etel
y or
par
tly
cove
red
by e
ject
a fr
om N
ecta
ris
and
are
ther
efor
e as
sign
ed t
o th
e Pr
e-N
ecta
rian
Per
iod.
Lind
enau
and
Sti
bori
us a
re p
unch
ed i
nto
the
Nec
tari
anej
ecta
and
in
addi
tion
are
fre
e of
Im
briu
m s
econ
dari
es t
hat
are
com
mon
her
e. T
he s
harp
ness
of t
heir
rim
s, c
entr
al p
eaks
,an
d ej
ecta
are
sim
ilar
to t
hose
of
Schl
uter
, w
hich
ove
rlie
sO
rien
tale
(LO
4-18
1H3)
; the
refo
re, t
hey
have
bee
n as
sign
ed to
the
Late
Im
bria
n Ep
och.
Rot
hman
n, s
harp
er y
et a
nd r
ela-
tive
ly u
ncra
tere
d, is
con
side
red
Erat
osth
enia
n.
LO4-
083H
3Su
n El
evat
ion:
22.
8°A
ltit
ude:
297
1.86
km
17
2Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
Rup
es A
ltai
(A
ltai
Sca
rp)
cont
inue
s no
rth
of t
his
(LO
4-08
4H2)
. It
fol
low
s th
e m
ain
ring
of
the
Nec
tari
s B
asin
and
is
sim
ilar
in
natu
re t
o M
onte
s A
penn
ine
and
Mon
tes
Cor
dille
ra. B
ecau
se it
is s
o sh
arp,
it h
as b
een
sugg
este
d th
at it
was
for
med
or
fres
hene
d by
a l
ater
tec
toni
c fa
ult
that
fol
-lo
wed
the
ring
. On
the
othe
r ha
nd, t
he s
harp
ness
may
sim
ply
have
bee
n m
aint
aine
d by
slu
mpi
ng o
f the
wal
l.
LO4-
084H
1Su
n El
evat
ion:
23.
1°A
ltit
ude:
272
6.79
km
17
3N
ecta
ris
Ba
sin R
egio
n
The
nor
ther
n en
d of
Rup
es A
ltai
is
in t
he l
ower
lef
t-ha
ndco
rner
of t
his
phot
o. F
irst
Cyr
illus
and
then
The
ophi
lus
have
land
ed i
n th
e ar
ea b
etw
een
the
mai
n ri
ng a
nd o
ne o
f th
ein
ner
ring
s of
the
Nec
tari
s B
asin
. Cyr
illus
is c
onsi
dere
d to
be
of t
he N
ecta
rian
Per
iod
and
The
ophi
lus,
whi
ch a
ppea
rs t
oha
ve p
ushe
d ri
m m
ater
ial o
f Cyr
illus
ont
o it
s flo
or, i
s fr
ee o
fIm
briu
m s
tria
tion
s, a
nd h
as a
low
inc
iden
ce o
f cr
ater
s on
it
s flo
or,
has
been
ass
igne
d to
the
Era
tost
heni
an P
erio
d.T
heop
hilu
s is
bel
ieve
d to
hav
e th
row
n so
me
frag
men
ts o
fM
are
Nec
tari
s to
the
high
land
land
ing
site
of A
pollo
16
(LO
4-89
H3)
. Sa
mpl
es f
rom
suc
h ro
cks
wer
e ag
ed a
t 3.
74 a
eons
(bil
lion
s of
yea
rs a
go).
The
Nec
tari
an i
mpa
ct w
ould
be
earl
ier,
est
imat
ed a
t 3.9
2 ae
ons.
LO4-
084H
2Su
n El
evat
ion:
23.
1°A
ltit
ude:
272
6.79
km
17
4Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
Mar
e T
ranq
uilli
tati
s an
d th
e A
pollo
11
land
ing
site
are
dis
-cu
ssed
in
the
chap
ter
on t
he S
eren
itat
is B
asin
Reg
ion
(Cha
pter
9).
The
Kan
t Pl
atea
u, f
rom
Mon
s Pe
nck
to e
ast
ofZ
olne
r (L
O4-
089H
3),
rise
s 2
km a
bove
the
sur
roun
ding
plai
ns.
Upl
ift
from
a t
ripl
e in
ters
ecti
on o
f ri
ngs
from
the
Nec
tari
s, I
mbr
ium
, an
d T
ranq
uilli
tati
s ba
sins
may
hav
era
ised
it.
Sin
us A
sper
itat
is h
as a
sm
all
grav
ity
anom
aly
(mas
con)
tha
t in
dica
tes
that
thi
s ba
y ha
s it
s ow
n so
urce
of
lava
. M
uch
of S
inus
Asp
erit
atis
has
bee
n co
vere
d w
ith
The
ophi
lus
ejec
ta,
the
ligh
ter
mat
eria
l in
the
low
er r
ight
corn
er o
f the
pho
to. B
eyon
d th
e T
heop
hilu
s ej
ecta
is a
hea
vyej
ecta
bla
nket
fro
m t
he I
mbr
ium
Bas
in, w
hose
rim
is
abou
t1.
5 ba
sin
radi
i aw
ay.
LO4-
084H
3Su
n El
evat
ion:
23.
1°A
ltit
ude:
272
6.79
km
17
5N
ecta
ris
Ba
sin R
egio
n
Wat
t is
clea
rly
of th
e Pr
e-N
ecta
rian
Per
iod
beca
use
the
stri
a-ti
ons
of N
ecta
rian
eje
cta
trav
erse
its
wal
l and
floo
r. S
tein
heil
and
Bie
la h
ave
sim
ilar
leve
ls o
f de
grad
atio
n an
d ar
e th
ere-
fore
like
ly to
be
of th
e sa
me
peri
od. B
ecau
se S
tein
heil
is in
an
area
of h
eavy
Nec
tari
an e
ject
a bu
t is
free
of i
t, th
ey m
ust b
oth
be N
ecta
rian
or
youn
ger.
The
cra
ters
tha
t ha
ve i
mpa
cted
Bie
la a
re Im
briu
m s
econ
dari
es, s
o bo
th c
rate
rs m
ust b
e ol
der
than
the
Ear
ly I
mbr
ian
Epoc
h. T
here
fore
, bo
th B
iela
and
Stei
nhei
l ar
e cl
assi
fied
as o
f th
e N
ecta
rian
Per
iod.
Lig
htpl
ains
are
nor
th a
nd e
ast o
f Bie
la.
LO4-
076H
1Su
n El
evat
ion:
22.
1°A
ltit
ude:
297
1.56
km
17
6Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
Fabr
iciu
s an
d Ja
nsse
n ar
e a
stud
y in
con
tras
ting
age
. Jan
ssen
,of
the
Pre
-Nec
tari
an P
erio
d, h
as i
ts r
im o
bscu
red
by e
ject
afr
om th
e N
ecta
ris
Bas
in a
nd b
oth
rim
and
floo
r ar
e im
pact
edby
Imbr
ium
sec
onda
ries
. Fab
rici
us, o
n th
e ot
her
hand
, sho
ws
shar
p te
xtur
e in
its
eje
cta,
cen
tral
pea
k, a
nd t
erra
ced
wal
l.T
he F
abri
cius
im
pact
cou
ld b
e as
lat
e as
the
Era
tost
heni
anPe
riod
. Rim
ae J
anss
en c
ould
be
the
surf
ace
man
ifes
tati
on o
ffa
ults
cau
sed
by s
tres
s fr
om t
he h
eavy
Nec
tari
an e
ject
a or
coul
d be
fau
lts
indu
ced
by t
he im
pact
of
Fabr
iciu
s. A
n ev
enol
der,
mor
e de
grad
ed,
unna
med
cra
ter
unde
rlie
s Ja
nsse
n,w
ith
its
cent
er n
ear
the
nort
heas
tern
rim
of J
anss
en.
LO4-
076H
2Su
n El
evat
ion:
22.
1°A
ltit
ude:
297
1.56
km
17
7N
ecta
ris
Ba
sin R
egio
n
Picc
olom
ini
has
oblit
erat
ed t
he s
outh
east
ern
end
of R
upes
Alt
ai T
he P
icco
lom
ini e
ject
a bl
anke
t ha
s sp
read
into
cra
ters
thou
ght
to b
e se
cond
arie
s of
Im
briu
m (
to t
he n
orth
wes
t).
Picc
olom
ini
is d
ated
in
the
Late
Im
bria
n Ep
och,
as
isSt
ibor
ius.
Rot
hman
n, w
hich
has
sha
rper
det
ail,
is d
ated
in
the
Erat
osth
enia
n Pe
riod
.
LO4-
076H
3Su
n El
evat
ion:
22.
1°A
ltit
ude:
297
1.56
km
17
8Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
LO4-077HSun Elevation: 22.9°Altitude: 2729.55 km
Torricelli may have been formed by apair of impactors. The rim of a flooded88-km crater surrounding Torricelli canbe seen just above the mare surface.There is a positive gravity anomaly atSinus Asperitatis, suggesting that it hadits own source of lava. The last (surface)flow of southern Mare Tranquillitatisdid not enter the sinus; its edge can beseen at the northeast sector of SinusAsperitatis.
The northwestern part of MareNectaris has been covered with ejectafrom Theophilus, covered in turn withrays from Madler. A couple of small(about 2 km) craters have penetratedthe Theophilus ejecta to produce theirown dark halos of mare material. Itappears that a landslide from a hill tothe north has cascaded over the rim ofMadler onto its floor, as well as over theejecta blanket of Madler, exposing verylight material.
The next ring inside of Rupes Altaican be seen arcing across this image,passing halfway between Piccolominiand Fracastorius. The next inner ring is tangent to the southern rim of Fra-castorius. Imbrium secondaries, craterchains, and other ejecta cover this partof the floor of the Nectaris Basin.
17
9N
ecta
ris
Ba
sin R
egio
n
Val
lis R
heit
a an
d cr
ater
cha
ins
to it
s w
est a
re r
adia
ting
from
the
Nec
tari
s B
asin
. Thi
s ar
ea is
the
best
pre
serv
ed p
art o
f the
Jans
sen
Form
atio
n, t
he e
ject
a bl
anke
t fr
om t
he N
ecta
ris
Bas
in.
The
vis
ibil
ity
of J
anss
en i
tsel
f, a
ltho
ugh
clea
rly
cove
red
by t
he d
epos
it f
rom
Nec
tari
s, i
ndic
ates
tha
t th
ebl
anke
t is
less
than
1 k
m th
ick.
The
Ste
inhe
il im
pact
or
som
eot
her
acti
vity
see
ms
to h
ave
thro
wn
an u
nusu
al l
ayer
edej
ecta
ont
o th
e so
uthe
ast fl
oor
of Ja
nsse
n.
LO4-
071H
2Su
n El
evat
ion:
23.
5°A
ltit
ude:
29.
72.2
9 km
18
0Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
Nea
nder
has
im
pact
ed t
he s
outh
ern
sect
or o
f th
e m
ain
ring
of t
he N
ecta
ris
Bas
in. I
t ap
pear
s th
at l
ava
has
flow
ed f
rom
the
outs
ide
of th
e m
ain
ring
sou
th to
the
crat
er B
renn
er. T
hefla
t-flo
ored
val
ley
has
subs
eque
ntly
bee
n co
vere
d w
ith
ejec
ta,
prob
ably
from
Pic
colo
min
i or
Imbr
ium
. Sim
ilar
flow
s fr
om a
mai
n ri
ng o
utw
ard
(but
wit
h na
rrow
er v
alle
ys)
can
be s
een
atR
ima
Plat
o an
d R
ima
Arc
hyta
s in
the
Imbr
ium
Bas
in R
egio
n(L
O-1
22H
3).
LO4-
071H
3Su
n El
evat
ion:
23.
5°A
ltit
ude:
29.
72.2
9 km
18
1N
ecta
ris
Ba
sin R
egio
n
Thi
s so
uthe
rn s
ecto
r of
the
Nec
tari
s B
asin
cov
ers
thre
e ri
ngs.
The
inn
er r
ing
graz
es t
he s
outh
ern
rim
of
Frac
asto
rius
, the
next
rin
g (s
omew
hat
inte
rmit
tent
) pa
sses
to
the
nort
h of
Wei
nek,
and
the
mai
n ri
ng p
asse
s th
roug
h N
eand
er. E
ject
afr
om F
raca
stor
ius
and
Imbr
ium
obs
cure
whe
ther
the
floor
of
the
basi
n ha
s be
en fl
oode
d w
ith
mar
e an
d th
en c
over
ed, b
utth
e fla
tnes
s su
gges
ts t
hat
it h
as b
een
flood
ed. T
he s
moo
th-
ness
and
flat
ness
of
the
plai
ns a
rea
to t
he n
orth
east
sug
gest
that
unc
onso
lida
ted
mat
eria
l ha
s be
en s
tron
gly
shak
endo
wn.
Thi
s is
onl
y on
e si
gn t
hat
part
s of
the
floo
r of
the
Nec
tari
s B
asin
hav
e su
bsid
ed i
n on
e or
mor
e su
dden
epis
odes
.
LO4-
072H
1Su
n El
evat
ion:
24.
3°A
ltit
ude:
274
2.43
km
18
2Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
Thi
s ce
ntra
l par
t of t
he N
ecta
ris
Bas
in is
ver
y de
eply
cov
ered
wit
h m
are
lava
. Dag
uerr
e, B
ohne
nber
ger,
the
crat
er s
outh
of
Boh
nenb
erge
r, a
nd p
ossi
bly
a cr
ater
wes
t of
Boh
nenb
erge
r(a
ll ne
ar th
e m
argi
ns o
f the
bas
in a
nd a
ll in
the
35-
to 5
0-km
rang
e) h
ave
been
floo
ded.
Thi
s in
dica
tes
that
the
dept
h at
the
mar
gins
is o
f the
ord
er o
f 2 k
m; t
he d
epth
at t
he c
ente
r of
the
basi
n, w
here
the
re i
s no
sig
n of
cra
ters
, is
likel
y to
be
even
mor
e. M
onte
s Py
rena
eus
is t
he e
aste
rn s
ecto
r of
the
inn
er-
mos
t rin
g of
Fig
ure
8.3.
The
cur
ved
ridg
e ab
out 3
5 km
to th
ew
est
of M
onte
s Py
rena
eus
is l
ikel
y to
be
sim
ply
com
pose
d of
ves
tigi
al s
ecto
rs o
f su
bmer
ged
crat
er r
ims.
The
floo
r of
Gau
dibe
rt is
an
extr
eme
exam
ple
of u
plif
t in
crat
ers
near
the
mar
gins
of m
aria
.
LO4-
072H
2Su
n El
evat
ion:
24.
3°A
ltit
ude:
274
2.43
km
18
3N
ecta
ris
Ba
sin R
egio
n
Imbr
ium
eje
cta
has
cove
red
all b
ut t
he la
rger
feat
ures
of t
heN
ecta
ris
Bas
in, s
uch
as V
allis
Cap
ella
, Rim
ae G
uten
berg
, and
the
mai
n ri
ng. T
he p
late
au n
orth
of L
eake
y ha
s be
en r
aise
d at
the
inte
rsec
tion
of
ring
s of
thr
ee b
asin
s (L
O4-
065H
3). V
allis
Cap
ella
was
pro
babl
y fo
rmed
by
ejec
ta fr
om N
ecta
ris.
Rim
aeG
uten
berg
app
ear
to m
ark
radi
al fr
actu
res,
oft
en fo
und
near
mar
e ed
ges
(bot
h M
are
Nec
tari
s an
d M
are
Fecu
ndit
atis
are
near
by).
Cen
sori
nus
is a
sm
all
4.5-
km C
oper
nica
n cr
ater
who
se m
uch
larg
er r
ay s
yste
m i
s ab
out
30 k
m a
cros
s. T
his
crat
er a
nd i
ts r
ay p
atte
rn h
ave
been
pho
togr
aphe
d at
ver
yhi
gh r
esol
utio
n (L
O5-
063H
1, -
H2,
and
-H
3; 2
-m r
esol
utio
n)an
d di
spla
y de
taile
d m
echa
nism
s of
eje
cta
and
ray
form
a-ti
on.
Gut
enbe
rg h
as p
rodu
ced
a la
rge
ejec
ta b
lank
et a
ndpo
ssib
ly s
moo
thed
out
pre
exis
ting
Im
briu
m e
ject
a by
its
impa
ct.
LO4-
072H
3Su
n El
evat
ion:
24.
3°A
ltit
ude:
274
2.43
km
18
4Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
The
hea
vy N
ecta
ris
ejec
ta b
lank
et f
orm
ed V
allis
Rhe
ita
and
cove
rs R
eim
anus
tho
roug
hly.
The
eje
cta
thin
s ou
t to
the
sout
h an
d so
uthw
est,
beco
min
g pa
tchy
tow
ard
Pont
ecou
lant
and
Han
no. T
he fl
oode
d cr
ater
s be
twee
n V
allis
Rhe
ita
and
crat
er H
anno
are
par
t of t
he A
ustr
ale
Bas
in. E
ject
a fr
om th
atba
sin
prob
ably
und
erlie
s th
e re
gion
of
this
pho
to b
ut h
asbe
en o
verl
ain
wit
h N
ecta
ris
ejec
ta. T
he h
igh
brig
htne
ss in
the
uppe
r ri
ght c
orne
r of
this
imag
e is
an
arti
fact
.
LO4-
064H
1Su
n El
evat
ion:
22.
5°A
ltit
ude:
297
2.87
km
18
5N
ecta
ris
Ba
sin R
egio
n
18
6Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
Thi
s ar
ea is
cov
ered
wit
h th
e Ja
nsse
n Fo
rmat
ion,
eje
cta
from
Nec
tari
s. V
allis
Rhe
ita,
for
med
by
the
impa
ct o
f a
chai
n of
seco
ndar
y im
pact
ors
from
the
Nec
tari
s B
asin
, has
exc
avat
edtw
o se
ctor
s of
the
rim
and
the
floo
r of
Pre
-Nec
tari
an c
rate
rY
oung
, bu
t ha
s be
en i
nter
rupt
ed i
n tu
rn b
y th
e yo
unge
rcr
ater
(Y
oung
D).
You
ng D
has
plo
wed
mat
eria
l fr
om t
hew
all o
f Val
lis R
heit
a ac
ross
its
floor
and
ove
r th
e ot
her
side
of
the
valle
y. T
he h
igh
brig
htne
ss i
n th
e up
per
righ
t co
rner
of
this
imag
e is
an
arti
fact
.
LO4-
064H
2Su
n El
evat
ion:
22.
5°A
ltit
ude:
297
2.87
km
The
muc
h-cr
ater
ed m
ain
ring
of
the
Nec
tari
s B
asin
pas
ses
from
Nea
nder
to
the
uppe
r ri
ght
corn
er o
f th
is i
mag
e.Be
twee
n N
eand
er a
nd R
eich
enba
ch th
ere
is a
ligh
t pla
ins
unit
wit
h a
faul
t run
ning
thro
ugh
it in
a d
irec
tion
that
is r
adia
l to
the
near
by M
are
Nec
tari
s. R
eich
enba
ch i
tsel
f ha
s a
ligh
tpl
ains
uni
t on
its
floo
r. T
he g
reat
er b
righ
tnes
s on
the
rig
htsi
de o
f th
is i
mag
e, a
nd t
he fi
ne c
rate
r ch
ains
sou
thw
est
of R
eich
enba
ch,
com
e fr
om n
earb
y St
evin
ius
to t
he e
ast
(LO
4-05
9 in
the
Aus
tral
e B
asin
Reg
ion)
. The
ray
pat
tern
of
Stev
iniu
s m
ay b
e ac
com
pani
ed w
ith
a fin
e ej
ecta
dep
osit
that
form
s lig
ht p
lain
s un
its
in th
is a
rea.
LO4-
064H
3Su
n El
evat
ion:
22.
5°A
ltit
ude:
297
2.87
km
18
7N
ecta
ris
Ba
sin R
egio
n
The
Nec
tari
an c
rate
r B
orda
is
on t
he b
orde
r be
twee
n th
em
ain
ring
of
the
Nec
tari
s B
asin
and
the
tro
ugh
wit
hin
it.
Sant
bech
lies
on
the
mid
dle
ring
sho
wn
in F
igur
e 8.
4 (d
isco
n-ti
nuou
s he
re).
The
trou
gh m
ay h
ave
been
floo
ded
wit
h m
are
in t
his
sect
or (
the
surf
ace
has
been
lig
hten
ed b
y ra
ys f
rom
Stev
iniu
s). I
mbr
ium
dep
osit
s ha
ve la
nded
in t
he t
roug
h an
dpi
led
up a
gain
st t
he m
ain
ring
, blo
ckin
g su
rfac
e la
va fl
ow in
this
are
a.
LO4-
065H
1Su
n El
evat
ion:
23.
8°A
ltit
ude:
273
5.07
km
18
8Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
The
Mon
tes
Pyre
naeu
s ra
nge
form
s th
e ea
ster
n se
ctor
of t
hein
nerm
ost
ring
of
the
Nec
tari
s B
asin
and
the
hil
ls s
outh
of
Col
ombo
mar
k th
e m
iddl
e ri
ng o
f Fi
gure
8.3
. R
imae
Goc
leni
us m
ark
typi
cal
radi
al a
nd c
ircu
mfe
rent
ial
frac
ture
sne
ar t
he e
dge
of a
mar
e. I
n th
is c
ase,
the
fau
lts
may
rel
ieve
stre
sses
due
to
both
Mar
e N
ecta
ris
and
Mar
e Fe
cund
itat
is,
whi
ch m
eet
near
the
rig
ht e
dge
of t
his
pict
ure.
Mar
eFe
cund
itat
is is
cov
ered
in t
he c
hapt
er o
n th
e Ea
ster
n B
asin
sR
egio
n (C
hapt
er 1
0).
The
floo
rs o
f G
ocle
nius
and
Mag
el-
haen
s ar
e flo
oded
wit
h la
va, b
ut p
roba
bly
not
from
the
sur
-ro
undi
ng m
are,
bec
ause
the
se fl
oors
are
at
a m
uch
low
erle
vel t
han
the
surr
ound
ing
mar
e.
LO4-
065H
2Su
n El
evat
ion:
23.
8°A
ltit
ude:
273
5.07
km
18
9N
ecta
ris
Ba
sin R
egio
n
Thi
s im
age
is p
artl
y fo
gged
, ap
pare
ntly
by
grou
nd p
ro-
cess
ing,
as
LO4-
065H
2 w
as n
ot a
ffec
ted.
Mar
e Fe
cund
itat
isin
trud
es o
n th
e N
ecta
ris
Bas
in n
ear
Gut
enbe
rg, a
nd p
art
ofM
are
Tra
nqui
llita
tis
appe
ars
near
the
nort
hwes
tern
cor
ner
ofth
e ph
oto.
A t
ripl
e in
ters
ecti
on o
f th
e m
ain
ring
s of
the
Nec
tari
s, F
ecun
dita
tis,
and
Tra
nqui
llita
tis
Bas
ins
lifts
the
Cen
sori
nus
plat
eau,
who
se e
aste
rn e
dge
can
be s
een
abou
t10
0 km
dow
n fr
om th
e to
p of
this
pho
to, a
long
the
left
-han
ded
ge. S
ee L
O4-
072
H3
for
a fu
ll vi
ew o
f th
is i
nter
esti
ng p
la-
teau
. The
Tra
nqui
llita
tis
Bas
in i
s co
vere
d in
the
cha
pter
on
the
Sere
nita
tis
Bas
in R
egio
n (C
hapt
er 9
).
LO4-
065H
3Su
n El
evat
ion:
23.
8°A
ltit
ude:
273
5.07
km
19
0Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
The
mai
n ri
ng o
f the
anc
ient
, deg
rade
d A
ustr
ale
Bas
in p
asse
sth
roug
h H
anno
, bou
ndin
g th
e ea
ster
n pa
rt o
f Mar
e A
ustr
ale.
Sign
s of
eas
t-w
est
ridg
es a
nd v
alle
ys r
adia
l to
Aus
tral
e ha
vebe
en e
rase
d by
lat
er d
epos
its.
The
dep
ress
ion
sout
hwes
t of
Bri
sban
e an
d th
e N
ecta
rian
cra
ter
Pont
ecou
lant
lie
in
anou
ter
trou
gh o
f th
e A
ustr
ale
Bas
in.
Cra
ter
Bri
sban
e w
asna
med
for
ast
rono
mer
Sir
Tho
mas
Bri
sban
e, a
Sco
t w
hose
rved
as
gove
rnor
of
New
Sou
th W
ales
in
Aus
tral
ia b
efor
ees
tabl
ishi
ng o
bser
vato
ries
in A
ustr
alia
and
Sco
tlan
d.
LO4-
059H
1Su
n El
evat
ion:
21.
7°A
ltit
ude:
297
4.56
km
19
1N
ecta
ris
Ba
sin R
egio
n
Val
lis R
heit
a an
d th
e ot
her
chai
ns o
f lar
ge s
econ
dary
cra
ters
radi
ate
from
the
Nec
tari
s B
asin
. In
the
are
a ne
ar P
re-
Nec
tari
an V
ega,
abo
ut o
ne b
asin
rad
ius
from
the
mai
n ri
ngof
Nec
tari
s, t
he h
eavy
Jan
ssen
For
mat
ion
give
s w
ay t
o fie
lds
of s
econ
dary
cra
ters
.
LO4-
059H
2Su
n El
evat
ion:
21.
7°A
ltit
ude:
297
4.56
km
19
2Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
059H
3Su
n El
evat
ion:
21.
7°A
ltit
ude:
297
4.56
km
19
3N
ecta
ris
Ba
sin R
egio
n
The
bri
ghtn
ess
in th
is a
rea
com
es fr
om a
20-
km c
rate
r ab
out
70 k
m s
outh
east
of
the
rim
of
Stev
inus
and
a 5
-km
cra
ter
abou
t 35
km
nor
thea
st o
f th
e ri
m o
f St
evin
us,
as w
ell
asSt
evin
us it
self.
Ste
vinu
s ha
s be
en a
ssig
ned
to th
e C
oper
nica
nPe
riod
bec
ause
of
its
fres
h, s
harp
app
eara
nce.
Com
pare
its
shar
pnes
s w
ith
the
35-k
m E
rato
sthe
nian
cra
ter
nort
h of
Rei
chen
bach
(ca
lled
Rie
chen
bach
A).
The
eje
cta
blan
ket
from
the
sm
alle
r cr
ater
has
los
t it
s de
tail
. T
he v
ery
long
Val
lis S
nelli
us (
radi
al to
the
Nec
tari
s B
asin
) co
ntin
ues
to th
eso
uthe
ast
tow
ard
the
Aus
tral
e B
asin
, be
com
ing
muc
h le
ssdi
stin
ct. T
here
may
act
ually
be
two
valle
ys (
one
from
eac
hba
sin)
tha
t ap
prox
imat
ely
mee
t. T
he r
idge
and
val
ley
that
com
es
from
th
e no
rth-
nort
hwes
t,
cont
inui
ng
beyo
ndSt
evin
us, i
s ra
dial
to th
e Fe
cund
itat
is B
asin
.
LO4-060HSun Elevation: 23.3°Altitude: 2737.76 km
Messier and its companion to the west(called Messier A) are characteristic inshape to low-angle (about 5° from thehorizontal) impacts of a lower-densitymaterial into a higher-density material.Messier A may actually have been causedby a pair of impactors. The ray pattern ofthese Copernican craters takes threedirections: to the left and right of theimpact axis and downstream. Except forthe few surface features, this area showsa deep mare lava floor fed by a pluton ofrising lava from the mantle.
The southern part of Mare Fecun-ditatis (east of Monge and Cook) hasprobably flooded an intersection oftroughs (LO4-060H1). The main ring ofthe Fecunditatis Basin passes throughthe low ridge between Crozier andMcClure.
This area of Mare Fecunditatis mayhave flooded a depression formed bythe intersection of troughs from theFecunditatis, Nectaris, and Balmer-Kapteyn Basins. The main ring of theNectaris Basin passes through Bordaand runs west of Biot. Vallis Snellius isradial to the Nectaris Basin.
19
4Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
In t
he l
ower
rig
ht h
alf
of t
his
pict
ure
is a
sha
llow
are
a of
Mar
e A
ustr
ale,
the
nor
thw
est
sect
or o
f th
e pa
rtia
lly fl
oode
dba
sin.
Cra
ters
onl
y a
few
kilo
met
ers
acro
ss,
and
ther
efor
eon
ly h
undr
eds
of m
eter
s de
ep, a
re o
nly
part
ially
floo
ded
The
mai
n ri
ng o
f th
e an
cien
t, d
egra
ded
Aus
tral
e B
asin
pas
ses
thro
ugh
Han
no, b
ound
ing
the
east
ern
part
of M
are
Aus
tral
e.La
ter
depo
sits
hav
e er
ased
mos
t sig
ns o
f Aus
tral
e ej
ecta
. The
depr
essi
on s
outh
wes
t of
Bri
sban
e an
d th
e N
ecta
rian
cra
ter
Pont
ecou
lant
lies
in a
n ou
ter
trou
gh o
f the
Aus
tral
e B
asin
.
LO4-
052H
1Su
n El
evat
ion:
23.
1°A
ltit
ude:
297
6.44
km
19
5N
ecta
ris
Ba
sin R
egio
n
An
inte
rrup
tion
of
tran
smis
sion
bet
wee
n th
e sp
acec
raft
and
Eart
h re
sult
ed i
n th
e lo
ss o
f m
ost
of s
ubfr
ame
LO4-
052H
3.T
he s
ix fr
amel
ets
that
hav
e be
en r
ecei
ved
have
bee
n ad
ded
toth
e to
p of
LO
4-05
2H2
in t
his
mos
aic.
Cha
ins
of s
econ
dary
crat
ers
in th
is a
rea
radi
ate
from
the
Nec
tari
s B
asin
. Veg
a an
dth
e cr
ater
s w
ithi
n it
are
cle
arly
Pre
-Nec
tari
an b
ecau
se t
heva
lleys
alig
ned
wit
h th
e cr
ater
cha
ins
scar
them
all.
Fur
neri
usis
a P
re-N
ecta
rian
cra
ter;
bes
ides
bei
ng f
ract
ured
, it
is o
ver-
lain
wit
h ej
ecta
from
Nec
tari
s.
LO4-
052H
2 Su
n El
evat
ion:
23.
1°A
ltit
ude:
297
6.44
km
and
-H3
19
6Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
Peta
vius
is
a “p
oste
r ch
ild”
of f
ract
ured
-floo
r cr
ater
s. I
t is
larg
e en
ough
to h
ave
a pr
omin
ent c
entr
al p
eak
of s
ome
com
-pl
exit
y an
d a
heig
ht o
f 3.5
km
abo
ve th
e cr
ater
floo
r. In
add
i-ti
on, R
imae
Pet
aviu
s re
veal
fra
ctur
es t
hat
seem
lar
ger
than
can
be e
xpla
ined
by
cool
ing
and
mor
e lik
ely
to r
eflec
t str
ong
uplif
t fo
rces
act
ing
on a
mel
t sh
eet.
The
upw
ard
pres
sure
may
be
rela
ted
to th
e la
va fl
oodi
ng th
e ne
arby
sou
ther
n pa
rtof
Mar
e Fe
cund
itat
is, t
o th
e up
per
left
in th
e ph
oto.
The
dar
kar
eas
near
the
wal
ls o
f Pe
tavi
us s
ugge
st t
he r
elea
se o
f da
rkgl
ass
part
icle
s (d
ark
man
tlin
g m
ater
ials
) fr
om f
ount
ains
driv
en b
y th
e re
leas
e of
vol
atile
s. C
rate
r co
unts
hav
e re
sult
edin
Pet
aviu
s be
ing
assi
gned
to th
e Ea
rly
Imbr
ian
Epoc
h.
LO4-
053H
1Su
n El
evat
ion:
23.
3°A
ltit
ude:
273
7.76
km
19
7N
ecta
ris
Ba
sin R
egio
n
The
mai
n ri
ng o
f the
Fec
undi
tati
s B
asin
can
be
seen
ent
erin
gth
is i
mag
e ju
st n
orth
of
15°
sout
h la
titu
de a
nd c
urvi
ngto
war
d La
ngre
nus
in t
he u
pper
rig
ht c
orne
r. T
his
ring
may
have
bee
n su
bseq
uent
ly d
estr
oyed
by
the
impa
ct o
f on
e or
mor
e pr
imar
y ob
ject
s, a
llow
ing
join
t flo
odin
g by
mar
e la
va.
Lang
renu
s, v
ario
usly
ass
igne
d to
the
you
nger
Era
tost
heni
anPe
riod
or
the
olde
r pa
rt o
f th
e C
oper
nica
n Pe
riod
, ha
s a
mod
est
set
of r
ays
for
such
a la
rge
crat
er. T
he 3
5-km
cra
ter
near
the
bott
om o
f thi
s im
age
(and
the
top
of L
O4-
053H
1) is
mor
e cl
earl
y C
oper
nica
n, w
ith
a th
ree-
pron
ged
ray
syst
emty
pica
l of
a p
rim
ary
crat
er t
hat
has
appr
oach
ed f
rom
the
nort
h w
ith
a lo
w a
ngle
. Ven
delin
us a
nd L
ohse
may
be
in a
trou
gh o
f the
Bal
mer
-Kap
teyn
Bas
in (
see
Cha
pter
10)
, whi
chw
ould
influ
ence
thei
r be
ing
flood
ed w
ith
lava
.
LO4-
053H
2Su
n El
evat
ion:
23.
3°A
ltit
ude:
273
7.76
km
19
8Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
The
suc
cess
ful
land
ing
of L
una
16 i
s di
scus
sed
in t
hech
apte
r on
the
Ser
enit
atis
Bas
in R
egio
n (
LO4-
054H
1)(C
hapt
er 9
). T
his
phot
o co
vers
the
dee
pest
par
t of
Mar
eFe
cun
dita
tis
(the
cen
ter
of t
he F
ecun
dita
tis
Bas
in i
s at
4°
S an
d 52
°E
). A
ric
h fie
ld o
f ej
ecta
an
d se
con
dari
es
from
Lan
gren
us h
as c
over
ed t
he m
are
floor
, es
tabl
ishi
ngLa
ngre
nus
as e
ithe
r Er
atos
then
ian
or C
oper
nica
n. T
hem
odes
t ray
sys
tem
(fo
r su
ch a
larg
e cr
ater
) pl
aces
its
age
near
the
bord
er b
etw
een
thos
e tw
o pe
riod
s. B
ilhar
z, N
aono
bu, a
ndA
twoo
d, fo
rmed
by
thre
e im
pact
ors
that
may
hav
e la
nded
ina
salv
o, a
re o
lder
than
the
mar
e flo
or b
ut a
re c
lear
ly y
oung
erth
an L
angr
enus
. A
s in
oth
er m
aria
, a
few
wri
nkle
rid
ges
(dor
sa)
appe
ar o
n it
s su
rfac
e. N
orth
ern
Mar
e Fe
cund
itat
isco
ntin
ues
into
the
Ser
enit
atis
Bas
in R
egio
n. T
he e
aste
rnsh
ore
can
be fo
und
in th
e Ea
ster
n B
asin
s R
egio
n.
LO4-
053H
3Su
n El
evat
ion:
23.
3°A
ltit
ude:
273
7.76
km
19
9N
ecta
ris
Ba
sin R
egio
n
9.1. OverviewThe Serenitatis Basin Region stretches from Mare Imbrium,whose eastern edge is near the 0° meridian, across MareSerenitatis and Mare Tranquillitatis to the western edge ofMare Crisium.
A series of four basins, Imbrium, Serenitatis, Tranquillitatis,and Fecunditatis, cover an arc of 120°, one-third of the cir-cumference of the Moon. Each member of this chain of basins
has formed a circular depression that was subsequently (longafter the impact event) filled with lava erupted from below,forming a mare. The Fecunditatis Basin, whose edge is visiblein the lower right-hand corner of Figure 9.1, is covered in theNectaris Basin Region (see Chapter 8).
The diameters of the main rings of these four basins(Spudis, 1993) are as follows:
● Imbrium: 1160 km● Serenitatis: 920 km
Chapter 9
Serenitatis Basin Region
Figure 9.1. LO4-097M: Serenitatis Basin Region. The Imbrium, Serenitatis, and Tranquillitatis Basins underlie their respective maria. Sinus Aestuum lies inan outer trough of the Imbrium Basin, and Mare Vaporum lies in a depression formed by the intersection of outer troughs of the Imbrium and SerenitatisBasins. Mare Frigoris lies partly in the northern part of the same outer trough of the Imbrium Basin as Sinus Aestuum and Mare Vaporum.
20
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Photo
gra
phic
Atla
s
● Tranquillitatis: 700 km● Fecunditatis: 690 km
To provide a sense of scale, Spain and Portugal would be aclose fit in Mare Serenitatis. Massive mountain ranges werethrown up at arcs of the main ring of these basins, especiallywhere the main rings of two or more basins come together.For example, at the boundary between the Imbrium andSerenitatis Basins, Montes Apenninus (to the south) rise asmuch as 4,430 m (14,400 feet) above the nearby mare surface.Radial ridges formed by ejecta from the Imbrium event canbe seen south of Mare Serenitatis, running for 500 km. Suchranges and ridges are formed by impact in a matter ofminutes and hours.
Serenitatis BasinMare Serenitatis is unusual in that it has apparently coveredtwo basins: the Serenitatis Basin and an older, smaller basinnorth-northeast of the main Serenitatis Basin called theNorthern Serenitatis Basin. The main ring of the SerenitatisBasin is interrupted in the sector where it would havecrossed the floor of the older basin, perhaps suppressed by amelt sheet within the main ring of that basin. Similarly, themelt sheet of the Serenitatis Basin may have suppressed themain ring of the younger Imbrium Basin where it would havecrossed the floor of the Serenitatis Basin. In the same way,the melt sheet of the Tranquillitatis Basin may have sup-pressed the main ring of the Serenitatis Basin where theyintersect.
Apollo LandingsApollo 11 landed on Mare Tranquillitatis (LO4-085H1), thefirst landing of humans beyond Earth and the first mission toreturn rock samples from beyond Earth. The samples col-lected by Armstrong and Aldrin established many of thecharacteristics confirmed by subsequent missions. The rockswere composed of basalt, a complex material that hardensfrom lava flows when molten rock from the mantle (theregion of relatively dense rock below a crust) rises to thesurface. On Earth, basalt paves the floors of the oceans anderupts from volcanoes. The lunar soil and rocks are free oforganic compounds and of volatile elements and compounds(hydrogen, sulfur, sodium, and water). The age of the basaltat Tranquillitatis Base was found to be 3.65 aeons (billionyears).
A few rock samples were not basalt but had been thrownfrom highlands by impacts. These rocks contain plagioclase,a low-density mineral composed of calcium and aluminumsilicates. This is the material, along with other minerals thatcombine easily with it, that rises from a body of molten rock(the magma ocean of the primitive Moon) to form the crust.
Apollo 15 landed near the sinuous canyon of Rima Hadleyand Mons Hadley, a mountain in the Montes Apenninusrange, part of the main ring of the Imbrium Basin (LO4-102H3). Equipped with a Lunar Roving Vehicle, Scott andIrwin explored a wide variety of terrain types. The walls ofRima Hadley showed layers of mare material from a series offlows; the deepest flow was 60 m in depth. “Genesis Rock,” acrustal rock aged at 4.15 billion years, was collected from theslope below the mountain Hadley Delta. Some samples, richin highland plagioclase, were probably thrown to this areafrom the crater Autolycus from 150 km away; the impactevent was aged at 1.29 million years.
Apollo 17 landed in a valley (Taurus-Littrow Valley) ofMontes Taurus, part of the main ring of the SerenitatisBasin (LO4-078H3). Schmitt and Cernan, their travels aidedby a Lunar Roving Vehicle, sampled ejecta from theSerenitatis Basin. Radioactive aging of the samples estab-lished the age of the Serenitatis Basin to be 3.86 or 3.87 billion years. One-meter layers of orange and blackglass beads were discovered, establishing the character ofdark mantling material that is common near the edges ofmaria. Some samples of material from a ray of Tycho weredated at 109 million years.
9.2. High-Resolution ImagesTable 9.1 shows the high-resolution images of the SerenitatisBasin Region in schematic form.
The following pages show the high-resolution subframesfrom south to north and west to east. That is, they are in theorder LO4-102H1, LO4-102H2, LO4-102H3, LO4-103H1,LO4-103H2 … LO4-054H1, LO4-054H2… LO4-055H3.
Subframes LO4-098H3, LO4-086H3, LO4-074H3, and LO4-062H3 are redundant and are not printed, although they areincluded in the enclosed CD.
Photos LO4-078H, LO4-073H, LO4-066H, and LO4-054Hare printed as complete frames.
20
1Se
renita
tis
Ba
sin R
egio
n
Latitude Range Photo Number
56 N–90 N 104 092 080 068 191H1
27 N–56 N 110 103 098 091 086 079 074 067 062 055 191H2
0–27 N 109 102 097 090 085 078 073 066 061 054 191H3
0–27 S 108 101 096 089 084 077 072 065 060 053 046
Longitude 3 W 4 E 10 E 16 E 24 E 30 E 38 E 43 E 49 E 57 E 63 Eat Equator
Table 9.1. The cells shown in white represent the high-resolution photos of the Serenitatis Basin Region (LO4-XXX H1, -H2, and -H3, where XXX is thePhoto Number). The Imbrium Basin Region is to the west, the Nectaris Basin Region is to the south, the Eastern Basins Region is to the west, and the NorthPolar Region is to the north.
Surv
eyor
s 4
and
6 ar
e di
scus
sed
in t
he n
ote
for
LO4-
108H
3, in
the
Hum
orum
Bas
in R
egio
n. T
he c
ompl
ex p
atte
rn o
f Rim
ae T
ries
neck
er r
eflec
ts s
tret
chin
g of
the
surf
ace
of S
inus
Med
ii aw
ay fr
om it
s bo
rder
as
lava
coo
led.
The
last
maj
orflo
w o
f lav
a ca
me
from
the
east
, as
indi
cate
d by
the
scar
p th
at r
uns
nort
h fr
omR
eaum
ur a
nd c
onti
nues
pas
t B
lagg
. A l
arge
pos
itiv
e gr
avit
y an
omal
y in
the
Cle
men
tine
dat
a, c
ente
red
abou
t 50
km
nor
thea
st o
f th
e ea
rly
Cop
erni
can
crat
er T
ries
neck
er, m
ay m
ark
the
sour
ce o
f th
e flo
w. T
he r
idge
s an
d va
lleys
are
Fra
Mau
ro F
orm
atio
n, e
ject
a fr
om t
he I
mbr
ium
Bas
in w
hose
mai
n ri
ng is
abou
t a
radi
us a
way
. A d
etai
led
exam
inat
ion
of M
urch
ison
ind
icat
es t
hat
its
floor
has
bee
n flo
oded
from
nea
r it
s w
alls
.
20
2Lu
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Photo
gra
phic
Atla
s
LO4-
102H
1Su
n El
evat
ion:
21.
6°A
ltit
ude:
269
9.13
km
Mar
e V
apor
um, s
outh
of t
he fo
othi
lls o
f the
Mon
tes
Ape
nnin
us, h
as fi
lled
the
trou
gh o
utsi
de t
he m
ain
ring
of
the
Imbr
ium
Bas
in. I
ts s
outh
ern
boun
dary
isth
e lo
wer
hill
s of
the
nex
t ou
ter
ring
of
the
Imbr
ium
Bas
in, 1
700
km i
n di
a-m
eter
. The
nea
rest
gra
vity
ano
mal
y in
Cle
men
tine
dat
a th
at c
ould
mar
k th
eso
urce
of t
he la
va is
nea
r T
ries
neck
er (
LO4-
102H
1) to
the
sout
h. R
ima
Hyg
inus
may
be
a co
llaps
ed l
ava
tube
tha
t ra
n to
the
nor
thw
est
to h
elp
form
Mar
eV
apor
um. T
he c
rate
rs a
long
Rim
a H
ygin
us, n
otab
le fo
r th
eir
lack
of r
ims,
may
have
bee
n in
divi
dual
col
laps
e ev
ents
. Hyg
inus
its
elf,
a ri
mle
ss c
rate
r w
ith
ada
rk h
alo,
may
hav
e be
en a
n en
doge
nic
sour
ce fo
r so
me
of th
e la
va c
arri
ed b
yth
e tu
be.
20
3Se
renita
tis
Ba
sin R
egio
n
LO4-
102H
2Su
n El
evat
ion:
21.
6°A
ltit
ude:
269
9.13
km
The
land
ing
site
for
Apo
llo 1
5, P
alus
Put
redi
nis
(“Sw
amp
of D
ecay
”) n
ear
the
edge
of
Mar
e Im
briu
m, w
as c
hose
n fo
r th
e op
port
unit
y to
exp
lore
bot
h hi
gh-
land
s fo
rmed
by
the
mai
n ri
ng o
f the
Imbr
ium
Bas
in a
nd th
e de
ep c
ut th
roug
hm
are
mat
eria
l of R
ima
Had
ley.
As
in o
ther
bas
in r
ims,
ris
ing
lava
see
ms
to b
ebl
ocke
d by
a m
assi
ve r
im r
ange
, flow
ing
out t
hrou
gh a
ven
t and
dow
n th
e si
deof
the
ran
ge.
Onc
e it
rea
ches
the
flat
ter
terr
ain
of P
alus
Put
redi
nus,
Rim
aH
adle
y (l
ike
Val
lis S
chro
teri
) m
eand
ers
like
terr
estr
ial
rive
rs i
n ne
arly
flat
land
. The
ast
rona
uts
saw
laye
rs in
the
wal
ls o
f Rim
a H
adle
y, in
dica
ting
a s
erie
sof
lava
flow
s. O
ne o
f the
roc
ks s
ampl
ed fr
om th
e sl
ope
of M
ons
Had
ley
delta
isth
e “G
enes
is r
ock,
” co
ntai
ning
whi
te p
lagi
ocla
se. T
his
low
-den
sity
min
eral
isty
pica
l of t
he o
rigi
nal c
rust
form
ed 4
.5 b
illio
n ye
ars
ago.
How
ever
, it
appe
ars
to h
ave
been
sho
cked
and
rec
ryst
alliz
ed b
y an
im
pact
, res
etti
ng i
ts “
atom
iccl
ock”
so
that
its
mea
sure
d ag
e is
4.1
5 bi
llion
yea
rs.
20
4Lu
na
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Photo
gra
phic
Atla
s
LO4-
102H
3Su
n El
evat
ion:
21.
6°A
ltit
ude:
269
9.13
km
See
LO4-
102H
3 fo
r no
tes
on t
he A
pollo
15
land
ing
site
. The
bubb
ly d
evel
opm
ent
arti
fact
lie
s al
ong
a “s
trai
t” o
f m
are
mat
eria
l th
at c
onne
cts
Mar
e Im
briu
m (
left
) w
ith
Mar
eSe
reni
tati
s (r
ight
). I
n th
is a
rea,
the
Im
briu
m m
ain
ring
,m
arke
d by
Mon
tes
Ape
nnin
us a
nd M
onte
s C
auca
sus,
cro
sses
insi
de o
f th
e m
ain
ring
of
Sere
nita
tis.
A m
elt
shee
t th
ere
may
hav
e in
hibi
ted
form
atio
n of
mou
ntai
ns i
n th
e st
rait
.A
ltho
ugh
the
Sere
nita
tis
Bas
in w
as f
orm
ed b
efor
e th
eIm
briu
m B
asin
, the
last
maj
or m
are
flow
see
ms
to h
ave
been
from
Ser
enit
atis
, as
show
n by
the
scar
p th
at r
uns
nort
h fr
omPr
omon
tori
um F
resn
el.
LO4-
103H
1Su
n El
evat
ion:
22.
3°A
ltit
ude:
292
6.55
km
20
5Se
renita
tis
Ba
sin R
egio
n
The
hum
moc
ky (
bum
py)
area
in
the
uppe
r le
ft q
uadr
ant
ofth
is p
hoto
is
the
Alp
es F
orm
atio
n of
the
Im
briu
m B
asin
,si
mila
r to
the
Mon
tes
Roo
k Fo
rmat
ion
of th
e O
rien
tale
Bas
in.
Thi
s ar
ea i
s be
twee
n th
e m
ain
ring
of
the
Imbr
ium
Bas
in(M
onte
s C
auca
sus)
and
an
inne
r ri
ng.
Eudo
xus
is f
resh
look
ing
and
show
s no
sig
n of
bei
ng a
ffec
ted
by e
ject
a fr
omth
e la
rge
crat
er A
rist
otel
es ju
st to
the
nort
h (L
O4-
103H
3), s
oit
is
prob
ably
Cop
erni
can.
Ale
xand
er f
orm
ed b
efor
e th
eIm
briu
m B
asin
; it
is
over
lain
wit
h Im
briu
m s
tria
tion
s.C
assi
ni h
as o
ccur
red
afte
r th
e Im
briu
m B
asin
was
form
ed, o
rit
wou
ld h
ave
been
obl
iter
ated
. Sub
sequ
entl
y flo
oded
by
one
of t
he fi
rst
lava
flow
s in
Mar
e Im
briu
m, i
t is
ass
igne
d to
the
Earl
y Im
bria
n Pe
riod
.
LO4-
103H
2Su
n El
evat
ion:
22.
3°A
ltit
ude:
292
6.55
km
20
6Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
The
Era
tost
heni
an c
rate
r A
rist
otel
es (
87 k
m)
prov
ides
an
ex-
celle
nt e
xam
ple
of th
e ej
ecta
pat
tern
of a
cra
ter
of th
is s
ize.
Ahe
avy
ejec
ta b
lank
et w
ith
radi
al r
idge
s ex
tend
s be
yond
the
rim
to
a di
stan
ce o
f ab
out
one
rim
rad
ius.
Bey
ond
that
, the
thin
ning
eje
cta
beco
mes
an
arra
y of
sec
onda
ry i
mpa
ctor
s,w
hich
oft
en fo
rm c
hain
s of
cra
ters
. Gal
le h
as a
ppar
entl
y ha
da
gap
in i
ts n
orth
ern
rim
inv
aded
by
mar
e la
va, w
hich
cas
-ca
ded
to i
ts fl
oor
in o
ne o
r po
ssib
ly t
wo
epis
odes
. The
lav
aflo
w(s
) m
ust h
ave
been
the
last
flow
s in
the
area
, or
the
crat
erw
ould
hav
e be
en c
ompl
etel
y in
unda
ted.
The
mar
e ar
ea i
spa
rt o
f Mar
e Fr
igor
is. I
n th
is a
rea,
it h
as fo
rmed
in a
n in
ter-
sect
ion
of th
e fir
st o
uter
trou
gh o
f the
Imbr
ium
Bas
in a
nd th
efir
st o
uter
trou
gh o
f the
Nor
ther
n Se
reni
tati
s B
asin
.
LO4-
103H
3Su
n El
evat
ion:
22.
3°A
ltit
ude:
292
6.55
km
20
7Se
renita
tis
Ba
sin R
egio
n
The
str
iate
d ri
dges
of
the
Fra
Mau
ro F
orm
atio
n fr
omIm
briu
m h
ave
impa
cted
rug
ged
high
land
s ab
out
one
radi
usaw
ay fr
om th
e m
ain
ring
of I
mbr
ium
. Rim
ae T
ries
neck
er a
rein
terl
ocki
ng r
adia
l an
d ci
rcum
fere
ntia
l st
ress
fau
lts
at t
heed
ge o
f M
are
Vap
orum
. T
he C
oper
nica
n cr
ater
God
in h
asse
nt i
ts e
ject
a bl
anke
t ov
er t
hat
of t
he E
rato
sthe
nian
cra
ter
Agr
ippa
, whi
ch i
n tu
rn, a
long
wit
h Im
briu
m, i
mpa
cted
the
anci
ent
crat
er T
empe
l. T
he fl
oor
of L
ade
is c
over
ed w
ith
hum
moc
ky m
ater
ial
that
may
hav
e be
en e
ject
ed f
rom
Imbr
ium
and
bee
n de
cele
rate
d by
gla
ncin
g of
f th
e ri
m o
fLa
de.
Som
e of
thi
s m
ater
ial
may
be
from
the
rim
its
elf.
Nor
thea
st o
f R
haet
icus
, th
ere
is a
cha
in o
f fr
esh-
look
ing
seco
ndar
y cr
ater
s th
at is
rad
ial t
o O
rien
tale
.
20
8Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
097H
1Su
n El
evat
ion:
21.
6°A
ltit
ude:
270
5.28
km
Mon
tes
Hae
mus
mar
ks t
he m
ain
ring
of
the
Sere
nita
tis
Bas
in. T
his
area
of
Mar
e V
apor
um f
orm
ed in
the
firs
t ou
ter
trou
gh o
f the
Ser
enit
atis
Bas
in, a
long
wit
h La
cus
Gau
dii a
ndLa
cus
Leni
tati
s. O
nce
thou
ght
to b
e vo
lcan
ic, t
he e
long
ated
form
atio
n ne
ar B
osco
vich
is n
ow c
onsi
dere
d to
be
a ch
ain
ofse
cond
ary
crat
ers
from
an
earl
y st
age
of th
e Im
briu
m im
pact
,m
odifi
ed b
y an
eje
cta
flow
from
the
sam
e im
pact
. The
se t
wo
stag
es w
ould
hav
e be
en s
epar
ated
in
tim
e by
onl
y a
few
min
utes
. Fl
oodi
ng b
y m
are
wou
ld h
ave
been
mil
lion
s of
year
s la
ter.
Ope
ning
of
the
stre
ss c
rack
s un
der
Rim
aeB
osco
vich
wou
ld h
ave
been
sti
ll la
ter.
Man
ilius
is c
onsi
dere
dto
be
of t
he L
ate
Imbr
ian
Epoc
h be
caus
e it
s ej
ecta
ove
rlie
sth
e m
are.
LO4-
097H
2Su
n El
evat
ion:
21.
6°A
ltit
ude:
270
5.28
km
20
9Se
renita
tis
Ba
sin R
egio
n
At t
he b
orde
r of
Mar
e Se
reni
tati
s, b
etw
een
Joy
and
Sulp
iciu
sG
allu
s, is
a d
epos
it th
at d
arke
ns th
e m
are,
the
bum
py te
rrai
nbe
twee
n M
onte
s H
aem
us a
nd t
he m
are
(Alp
es F
orm
atio
n;se
e th
e no
te fo
r LO
4-10
3H2)
, and
Lac
us O
dii.
Thi
s de
posi
t is
char
acte
rize
d as
dar
k m
antl
ing
mat
eria
l, a
type
that
is fo
und
on t
he b
orde
r of
oth
er m
aria
. It
may
be
due
to “
fire-
foun
tain
” vo
lcan
ic e
rupt
ions
fro
m d
epth
or
poss
ibly
res
ult
from
vol
atile
s re
leas
ed w
here
a t
hin
laye
r of
lava
flow
s ov
ercr
usta
l m
ater
ial.
Cir
cum
fere
ntia
l ri
dges
suc
h as
Dor
sum
Buc
klan
d an
d D
orsu
m G
ast
and
frac
ture
s su
ch a
s R
imae
Sulp
iciu
s G
allu
s ar
e co
mm
on a
t th
e ed
ges
of m
aria
. Lin
ne is
a
Cop
erni
can
crat
er t
hat
has
impa
cted
Mar
e Se
reni
tati
s. A
chai
n of
suc
h cr
ater
s m
arch
es a
cros
s th
e ed
ge o
f M
are
Sere
nita
tis
into
Mon
tes
Hae
mus
.
21
0Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
097H
3Su
n El
evat
ion:
21.
6°A
ltit
ude:
270
5.28
km
The
pro
ject
ion
in th
e lo
wer
left
of t
he p
hoto
mar
ks th
e in
ters
ecti
on o
f the
mai
nri
ng o
f th
e Se
reni
tati
s B
asin
wit
h th
at o
f th
e N
orth
ern
Sere
nita
tis
Bas
in. T
hese
ctio
n of
the
Mon
tes
Cau
casu
s in
the
upp
er l
eft
corn
er o
f th
is p
hoto
is
the
mai
n ri
ng o
f the
Nor
ther
n Se
reni
tati
s B
asin
. Mar
e Se
reni
tati
s sh
ows
few
indi
-
cati
ons
of d
row
ned
crat
ers,
exc
ept
for
som
e fa
int
circ
ular
rid
ges,
ind
icat
ing
that
the
mar
e is
dee
p. T
here
is
a st
rong
mas
con
asso
ciat
ed w
ith
Mar
eSe
reni
tati
s, i
ndic
atin
g th
at a
lar
ge p
lum
e of
lav
a fr
om t
he m
antl
e fe
d th
eflo
odin
g of
the
over
lapp
ing
pair
of b
asin
s.
21
1Se
renita
tis
Ba
sin R
egio
n
LO4-
098H
1Su
n El
evat
ion:
22.
3°A
ltit
ude:
292
6.55
km
In t
his
area
nor
th o
f M
are
Sere
nita
tis
ther
e ar
e ov
erla
ppin
g de
posi
ts e
ject
edfr
om t
he S
eren
itat
is,
Nor
ther
n Se
reni
tati
s, a
nd I
mbr
ium
Bas
ins
(wit
h th
eIm
briu
m e
ject
a up
perm
ost)
. Bec
ause
of i
ts h
umm
ocky
cha
ract
er, i
t is
map
ped
as a
n ex
tens
ion
of th
e A
lpes
For
mat
ion
of th
e Im
briu
m B
asin
. How
ever
, it m
ayha
ve a
dif
fere
nt fo
rmin
g m
echa
nism
than
the
area
insi
de o
f the
Im
briu
m r
im.
The
por
tion
sou
th o
f 40°
nort
h la
titu
de m
ay b
e pr
imar
ily N
orth
ern
Sere
nita
tis
mat
eria
l w
ithi
n it
s ri
m,
and
the
nort
hern
por
tion
may
not
rea
lly b
e “h
um-
moc
ky”;
it
may
be
sim
ply
cros
shat
ched
wit
h st
riat
ions
fro
m I
mbr
ium
and
Sere
nita
tis.
21
2Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
098H
2Su
n El
evat
ion:
22.
3°A
ltit
ude:
292
6.55
km
In m
any
part
s of
the
Moo
n, th
ere
are
smal
l pat
ches
of s
moo
th p
lain
s in
oth
er-
wis
e ru
gged
hig
hlan
d re
gion
s si
mila
r to
thi
s ar
ea s
urro
undi
ng C
ayle
y, t
hear
chet
ype
of th
e C
ayle
y Fo
rmat
ion.
The
se r
egio
ns a
re a
ssoc
iate
d w
ith
the
oute
rej
ecta
bla
nket
fro
m m
ajor
bas
ins
such
as
Imbr
ium
, Ori
enta
le, a
nd N
ecta
ris.
The
se h
ighl
and
plai
ns m
ay r
esul
t fr
om r
elat
ivel
y un
ifor
m b
lank
ets
of fi
nely
pulv
eriz
ed e
ject
a th
at a
re s
hake
n do
wn
by lo
cal t
ecto
nic
forc
es. T
o qu
ote
Ken
Mat
ting
ly, t
he C
omm
and
Mod
ule
Pilo
t for
Apo
llo 1
6, “
The
Cay
ley
repr
esen
ts a
pool
of
unco
nsol
idat
ed m
ater
ial
whi
ch h
as b
een
‘sha
ken’
unt
il th
e su
rfac
e is
rela
tive
ly fl
at.”
Rim
a A
riad
aeus
, a
larg
e fa
ult
wit
h an
off
set,
may
ind
icat
est
rong
tect
onic
act
ion
in th
is a
rea
arou
nd C
ayle
y.
21
3Se
renita
tis
Ba
sin R
egio
n
LO4-
090H
1Su
n El
evat
ion:
21.
6°A
ltit
ude:
271
1.26
km
Thi
s in
tere
stin
g re
gion
sou
th o
f M
are
Sere
nita
tis
show
s M
onte
s H
aem
us, t
heso
uthe
rn m
ain
ring
of
the
Sere
nita
tis
Bas
in, i
mpa
cted
by
stri
atio
ns f
rom
the
Imbr
ium
Bas
in. T
he o
uter
trou
gh o
f the
Ser
enit
atis
Bas
in h
as b
een
flood
ed b
yLa
cus
Gau
dii,
Lacu
s H
iem
alis
, La
cus
Leni
tati
s, a
nd S
inus
Hon
oris
. M
are
Tra
nqui
llita
tis
is t
o th
e so
uthe
ast
of S
inus
Hon
oris
; the
muc
h-de
grad
ed m
ain
ring
of
the
Tra
nqui
llita
tis
Bas
in t
rave
rses
Jul
ius
Cae
sar.
Rim
ae M
acle
ar a
ndR
imae
Sos
igen
es a
re c
ircu
mfe
rent
ial f
ault
s at
the
edge
of M
are
Tra
nqui
llita
tis.
Men
elau
s ha
s im
pact
ed p
reci
sely
on
the
inne
r ri
m o
f th
e m
ain
ring
of
the
Sere
nita
tis
Bas
in, p
roje
ctin
g ra
ys in
all
dire
ctio
ns.
21
4Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
090H
2Su
n El
evat
ion:
21.
6°A
ltit
ude:
271
1.26
km
The
floo
ded
floor
of t
he S
eren
itat
is B
asin
sho
ws
only
sub
tle
vari
atio
n. D
orsu
mA
zara
may
rep
rese
nt a
flow
bou
ndar
y or
may
be
part
of
a pa
tter
n m
arki
ng a
subm
erge
d cr
ater
. T
he b
righ
t st
reak
s ra
diat
e no
t fr
om B
esse
l, bu
t fr
omM
enel
aus
to th
e so
uth
(LO
4-09
0H2)
.
21
5Se
renita
tis
Ba
sin R
egio
n
LO4-
090H
3Su
n El
evat
ion:
21.
6°A
ltit
ude:
271
1.26
km
In th
is n
orth
east
ern
part
of M
are
Sere
nita
tis,
an
incr
ease
d fr
eque
ncy
of r
idge
sin
dica
te a
tra
nsit
ion
from
the
dee
p la
va o
f M
are
Sere
nita
tis
to t
he s
hallo
wer
Lacu
s So
mni
orum
(LO
4-09
1H2)
, no
rthe
ast
of L
uthe
r. T
he b
righ
tnes
s of
the
mar
e su
rfac
e co
mes
fro
m r
ays
from
Cop
erni
can
crat
ers
Bur
g (t
o th
e no
rth)
and
Tha
les
(far
to th
e no
rthe
ast)
.
21
6Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
091H
1Su
n El
evat
ion:
23.
7°A
ltit
ude:
294
7.25
km
Lacu
s So
mni
orum
has
bee
n fo
rmed
by
the
flood
ing
of a
com
plex
dep
ress
ion
that
sho
ws
sign
s of
mul
tipl
e un
derl
ying
cra
ters
. A s
ingl
e la
rge
crat
er s
eem
s to
unde
rlie
Lac
us M
orti
s. B
urg
is a
Cop
erni
can
crat
er w
ith
a w
ell-
deve
lope
d ra
ypa
tter
n. T
he fl
oor
of L
acus
Mor
tis
show
s ex
tens
ive
frac
turi
ng,
incl
udin
g a
scar
p th
at is
abo
ut 8
00 m
in h
eigh
t, ju
dgin
g by
its
shad
ow a
t 23
.7°
sun
elev
a-ti
on. T
here
is s
ome
evid
ence
of
dark
dep
osit
s in
the
vic
init
y of
fau
lts
(rim
ae)
in L
acus
Mor
tis,
sug
gest
ing
the
rele
ase
of v
olat
iles
afte
r th
e de
posi
t of
ray
sfr
om th
e B
urg
impa
ct.
21
7Se
renita
tis
Ba
sin R
egio
n
LO4-
091H
2Su
n El
evat
ion:
23.
7°A
ltit
ude:
294
7.25
km
Thi
s ea
ster
n pa
rt o
f Mar
e Fr
igor
is is
old
er th
an th
e w
este
rn p
art,
acco
rdin
g to
crat
er c
ount
s. T
here
are
sig
ns o
f a p
ossi
ble
basi
n (3
60 k
m, 5
5°N
, 30°
E) u
nder
this
par
t of M
are
Frig
oris
. The
rid
ge r
unni
ng th
roug
h B
aily
and
aro
und
to ju
stso
uthe
ast
of G
artn
er,
coul
d be
the
rim
of
a ba
sin
unde
rlyi
ng w
este
rn M
are
Frig
oris
(LO
4-09
8H3)
. Thi
s ar
ea s
how
s a
num
ber
of m
are
ridg
es (
dors
a) t
hat
are
influ
ence
d by
the
unde
rlyi
ng to
pogr
aphy
. Bai
ly s
eem
s to
hav
e be
en fo
rmed
by a
pai
r of
impa
ctor
s ar
rivi
ng s
ide
by s
ide
into
a h
ighl
and
area
at a
low
ang
lefr
om t
he e
ast-
nort
heas
t. T
he c
ompo
und
crat
er w
as s
ubse
quen
tly
flood
ed b
yla
va a
nd th
en it
s flo
or w
as fr
actu
red,
form
ing
the
rim
ae in
the
crat
er fl
oor.
21
8Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
091H
3Su
n El
evat
ion:
23.
7°A
ltit
ude:
294
7.25
km
Mar
e T
ranq
uilli
tati
s w
as a
pri
me
choi
ce f
or t
he fi
rst
Apo
llo l
andi
ng s
ite
beca
use
of it
s la
rge
smoo
th a
rea
and
equa
tori
al p
osit
ion.
Fur
ther
, its
eas
tern
loca
tion
mad
e it
a fi
rst
choi
ce w
ithi
n a
laun
ch w
indo
w. R
ange
r 8
was
the
firs
tto
ret
urn
deta
iled
pict
ures
fro
m t
his
site
in
Febr
uary
196
5, c
onfir
min
g th
eto
pogr
aphi
c su
itab
ility
for
a m
anne
d la
ndin
g bu
t lea
ving
ope
n th
e qu
esti
on o
fso
il st
reng
th. S
urve
yor
5 (S
epte
mbe
r 19
67)
confi
rmed
the
firm
ness
of
luna
rso
il he
re. A
n al
pha-
scat
teri
ng e
xper
imen
t fo
und
that
the
che
mic
al c
ompo
si-
tion
of
the
mar
e so
il w
as c
hara
cter
isti
c of
bas
alt.
As
can
be s
een
from
thi
sLu
nar
Orb
iter
pho
to, t
he la
ndin
g si
te fo
r A
pollo
11
was
cho
sen
to b
e as
flat
and
feat
urel
ess
as p
ossi
ble,
nea
rly
free
of l
arge
cra
ters
and
rid
ges
that
cou
ld je
opar
-di
ze a
land
ing.
On
July
20,
196
9, E
agle
land
ed a
t Tra
nqui
lity
Bas
e. T
he m
issi
onre
turn
ed 2
2 kg
of s
ampl
es c
olle
cted
from
the
mar
e by
Arm
stro
ng a
nd A
ldri
n,in
clud
ing
rock
s 3.
6 bi
llion
yea
rs o
ld.
21
9Se
renita
tis
Ba
sin R
egio
n
LO4-
085H
1Su
n El
evat
ion:
22.
5°A
ltit
ude:
271
6.89
km
Nea
r Pl
iniu
s, t
he m
ain
ring
of
the
Sere
nita
tis
Bas
in i
nter
sect
s th
e m
ain
ring
of
the
pre
exis
ting
Tra
nqui
llita
tis
Bas
in. S
eren
itat
is d
oubt
less
dem
olis
hed
and
disp
erse
d th
e m
ain
ring
of
Tra
nqui
llita
tis.
The
mel
t sh
eet
of T
ranq
uilli
tati
sm
ay h
ave
supp
ress
ed t
he s
ecto
r of
the
mai
n ri
ng o
f Se
reni
tati
s be
yond
Prom
onto
rium
Arc
heru
sia.
An
exte
nsiv
e fr
actu
re z
one,
mar
ked
by R
imae
Plin
ius,
pas
ses
whe
re th
e m
ain
ring
of S
eren
itat
is w
ould
be
expe
cted
. The
last
laye
r of
lava
to fl
ow b
etw
een
the
two
basi
ns h
as c
ome
from
Tra
nqui
llita
tis;
its
boun
dary
can
be
seen
nor
thw
est o
f Pro
mon
tori
um A
rche
rusi
a. R
idge
s in
Mar
eT
ranq
uilli
tati
s sh
ow e
vide
nce
of t
he u
nder
lyin
g to
pogr
aphy
, ind
icat
ing
that
the
mar
e m
ay b
e sh
allo
w h
ere.
22
0Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
085H
2Su
n El
evat
ion:
22.
5°A
ltit
ude:
271
6.89
km
The
are
a to
the
righ
t of t
his
phot
o, to
war
d th
e ea
ster
n ed
ge o
f Mar
e Se
reni
tati
s,is
not
onl
y da
rker
but
of
a di
ffer
ent
spec
tral
cla
ss t
han
the
cent
ral
mar
esu
rfac
e. I
t m
ay b
e co
vere
d w
ith
dark
man
tlin
g m
ater
ial.
See
also
LO
4-07
8H3,
who
se v
iew
con
tinu
es to
the
east
.
22
1Se
renita
tis
Ba
sin R
egio
n
LO4-
085H
3Su
n El
evat
ion:
22.
5°A
ltit
ude:
271
6.89
km
The
cen
tral
and
sou
ther
n se
ctio
ns o
f D
orsa
Sm
irno
v m
aym
ark
an in
ner
ring
of t
he S
eren
itat
is B
asin
. The
ext
ensi
on o
fM
are
Sere
nita
tis
to t
he n
orth
may
rep
rese
nt a
flow
of
lava
nort
h fr
om M
are
Sere
nita
tis
thro
ugh
Lacu
s So
mni
orum
and
Lacu
s M
orti
s to
war
d M
are
Frig
oris
. Thi
s ph
oto
was
exp
osed
for
the
mar
e, n
ot f
or t
he b
righ
ter
high
land
s. T
here
is
bett
erco
vera
ge o
f Pos
idon
ius
in L
O4-
079H
1.
LO4-
086H
1Su
n El
evat
ion:
23.
7°A
ltit
ude:
295
6.08
km
22
2Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
22
3Se
renita
tis
Ba
sin R
egio
n
Cra
ters
Pla
na a
nd M
ason
hav
e im
pact
ed th
e m
ain
ring
of t
hela
rge
crat
er b
enea
th L
acus
Mor
tis
(see
LO
4-09
1H2)
, cau
sing
the
stra
nge
patt
ern
of r
edis
trib
uted
mat
eria
l su
rrou
ndin
gth
em. I
n pa
rtic
ular
, cra
ter
Mas
on h
as t
hrow
n he
avy
lobe
s of
debr
is t
o th
e so
uthe
ast,
mod
ifyi
ng e
ject
a fr
om t
he c
rate
rw
hose
rim
it h
as im
pact
ed.
LO4-
086H
2Su
n El
evat
ion:
23.
7°A
ltit
ude:
295
6.08
km
LO4-078HSun Elevation: 23.6°Altitude: 2722.07 km
One objective of the Apollo 17 Mission(December 1972) in the Taurus-Littrowvalley was to sample the dark mantlingmaterial in this area. Although the ma-terial was mostly covered, it was ex-cavated and exposed by the impact oflocal craters. Sampled by Schmitt andCernan, it is composed of beads of a ti-tanium-rich composition that is darkorange if a glass and black if crystal-lized. Aged at 3.4 billion years old, it isgenerated by volcanic fountains drivenby an unknown volatile material.
Lava may have risen through a hard-ening surface at Dorsa Barlow, runningthrough Rima Jansen to the northwestand filling a crater about 50 km north of Jansen. The main rings of Tranquil-litatis and Serenitatis each pass betweenDawes and Fabbroni, but there are nomountains there. Perhaps Serenitatis de-stroyed this sector of the Tranquillitatisring and the melt sheet of Tranquillitatissuppressed the Serenitatis ring.
The highlands near Copernican craterCensorinus in the bottom right cornerof this photo mark the remains of thesouthwest sector of the much-degradedmain ring of the Tranquillitatis Basin(see Photos LO4-077H3 and LO4-072H3in the Nectaris Basin Region).
22
4Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
Luna
21,
the
firs
t of
thr
ee p
ost-
Apo
llo u
nman
ned
succ
esse
sof
the
USS
R l
unar
pro
gram
, la
nded
in
Janu
ary
1973
. It
depl
oyed
the
sec
ond
Luno
khod
rov
er.
On
the
floor
of
LeM
onni
er, t
his
rove
r en
coun
tere
d sl
ippe
ry g
oing
(80
% w
heel
slip
) an
d sa
nk to
its
axle
s at
one
poi
nt in
side
a c
rate
r. T
his
isco
nsis
tent
wit
h Le
Mon
nier
bei
ng h
eavi
ly c
over
ed w
ith
un-
com
pact
ed d
ark
man
tlin
g m
ater
ial.
The
rov
er m
oved
fro
mth
e la
ndin
g si
te in
to th
e fo
othi
lls o
f Mon
tes
Tau
rus,
find
ing
ade
crea
se i
n ir
on c
onte
nt f
rom
9%
to
4%.
It a
lso
expl
ored
an
ope
n cr
ack
in t
he b
asal
t m
ore
than
300
m w
ide.
Upl
ift
from
ris
ing
lava
has
rai
sed
the
grea
ter
part
of
the
floor
of
Lat
e Im
bria
n Po
sido
nius
nea
rly
to t
he t
op o
f it
s ri
m
(LO
4-07
9H3)
.
LO4-
079H
1Su
n El
evat
ion:
24.
5°A
ltit
ude:
296
3.78
km
22
5Se
renita
tis
Ba
sin R
egio
n
Atl
as i
s be
lieve
d to
be
Late
Im
bria
n in
age
and
Her
cule
s to
be
Era
tost
heni
an (
the
next
you
nger
per
iod)
. It
is in
tere
stin
gto
com
pare
the
degr
ee o
f deg
rada
tion
and
inte
rpla
y of
eje
cta
betw
een
the
two
crat
ers
of c
ompa
rabl
e si
ze,
impa
ctin
gsi
mil
ar t
erra
in.
Mor
e of
the
se c
rate
rs c
an b
e se
en i
n LO
4-07
9H3.
Lac
us S
omni
orum
is q
uite
sha
llow
, as
indi
cate
dby
the
man
y pa
rtia
lly fl
oode
d cr
ater
s an
d is
land
s ab
ove
the
mar
e su
rfac
e.
LO4-
079H
2Su
n El
evat
ion:
24.
5°A
ltit
ude:
296
3.78
km
22
6Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
Atl
as h
as a
n up
lift
ed fl
oor,
lik
e th
e flo
ors
of P
osid
oniu
s(L
O4-
079H
1) a
nd H
umbo
ldt,
othe
r La
te I
mbr
ian
crat
ers
init
s si
ze r
ange
. Per
haps
thi
s is
cha
ract
eris
tic
of l
arge
cra
ters
that
impa
cted
in th
is p
erio
d bu
t wer
e no
t floo
ded
wit
h m
are.
Smal
l lak
es o
f mar
e m
ater
ial i
n th
e up
per
righ
t of t
his
phot
oal
so a
ppea
r ne
ar o
ther
mar
ia.
LO4-
079H
3Su
n El
evat
ion:
24.
5°A
ltit
ude:
296
3.78
km
22
7Se
renita
tis
Ba
sin R
egio
n
LO4-073HSun Elevation: 24.9°Altitude: 2756.52 km
Montes Taurus separates the Serenitatisand Crisium Basins; it is within a radiusfrom the rim of each, and no doubt re-ceived ejecta from both, overlaid withImbrium ejecta. An 85-km crater mayunderlie Sinus Amoris. Romer, Hill, and Carmichael are fresh Copernicancraters. Chains and clusters of Imbriumsecondary craters are east of Romer.
The IAU named Diana and Grace in1979. Were the IAU representativesthinking of two commoners who mar-ried royalty? Mons Esam is a moundsurmounted by a crater, in the middleof a mare. It looks like an ash cone orfumarole, a possible source of darkmantling material. Rima Cauchy (arille) and Rupes Cauchy (a scarp) prob-ably are both surface expressions offaults in the mare.
The Censorinus Highlands arelocated at a triple intersection of themain rings of the Tranquillitatis andFecunditatis Basins and the first outerring of the Nectaris Basin. Shaking may have leveled Imbrium ejecta in theterra plains unit between Censorinusand Leakey. There are deposits of darkmantling along the shoreline of MareTranquillitatis and on the Censorinushighlands.
22
8Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
Ejec
ta w
ith
stri
atio
ns r
adia
l to
the
Cri
sium
Bas
in c
an b
e se
en in
the
low
er r
ight
corn
er o
f th
is p
hoto
, sou
th o
f N
ewco
mb.
New
com
b an
d R
omer
see
m f
ree
ofsu
ch e
ject
a, b
ut K
irch
off s
how
s pr
obab
le s
econ
dari
es fr
om C
risi
um. N
ewco
mb
is a
ver
y co
mpl
ex c
rate
r. E
xten
sive
slu
mpi
ng h
as le
ft d
eep
scal
lops
on
its
rim
.T
he im
pact
of
the
20-k
m c
rate
r ju
st s
outh
wes
t of
New
com
b m
ay h
ave
caus
edth
e ex
tens
ive
colla
pse
of th
e ne
arby
wal
l.
22
9Se
renita
tis
Ba
sin R
egio
n
LO4-
074H
1Su
n El
evat
ion:
25.
2°A
ltit
ude:
296
9.81
km
The
str
uctu
re n
orth
of
Mau
ry i
s ve
ry u
nusu
al. I
t lo
oks
like
a sh
ield
vol
cano
that
has
eru
pted
in
abou
t fo
ur e
piso
des,
eac
h w
ith
lava
tha
t is
muc
h m
ore
visc
ous
than
oth
er fl
ows
on th
e M
oon.
Mor
e lik
ely,
how
ever
, it i
s m
olte
n ej
ecta
or a
sal
vo o
f la
va b
ombs
fro
m C
risi
um t
o th
e so
uth.
Pri
mar
y cr
ater
s in
thi
s
23
0Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
074H
2Su
n El
evat
ion:
25.
2°A
ltit
ude:
296
9.81
km
area
are
ass
igne
d to
div
erse
age
ran
ges.
Fra
nklin
is o
f the
Ear
ly Im
bria
n Ep
och,
Atl
as i
s of
the
Lat
e Im
bria
n Ep
och,
Her
cule
s is
of
the
Erat
osth
enia
n Pe
riod
,an
d C
ephe
us is
Cop
erni
can.
LO4-066HSun Elevation: 24.2°Altitude: 2730.73 km
This part of Montes Taurus is a high-lands area between the Serenitatis, Tran-quillitatis, and Crisium Basins. Theridges near Lacus Bonitatis are radial tothe Crisium Basin, whose main ring runs through Macrobius. Lacus Bonitatis,running at right angles to the ridges, is inan outer trough of Crisium.
The complex region east of MareTranquillitatis has been influenced bymany basins. Sinus Concordiae hasflooded part of an outer trough of theFecunditatis Basin, beyond the ring thatpasses north of da Vinci. Palus Somni hasreceived deposits from Tranquillitatis,Fecunditatis, Crisium, Serenitatis, andImbrium (in that order). These depositscover the eastern sector of the main ringof Tranquillitatis as it passes east of Lyell.The highland peaks between Cauchy andda Vinci are at an intersection of ringsfrom the Tranquillitatis and FecunditatisBasins.
An outer ring of the FecunditatisBasin passes near Zahringer, and themain ring of Tranquillitatis passes byMontes Secchi. The intersection ofthese two rings, just north of Lawrence,has raised a plateau (LO4-066H3). TheCensorinus highlands are in the bottomleft. Dark mantling material has slid offsteep slopes of these mountains, leavingbright areas.
23
1Se
renita
tis
Ba
sin R
egio
n
The
lar
ge t
roug
h be
twee
n N
ewco
mb
and
Deb
es m
ay h
ave
been
ini
tial
ly f
orm
ed b
y a
chai
n of
cra
ters
fro
m t
he T
ran-
quil
lita
tis
impa
ct a
nd t
hen
been
rei
nfor
ced
as a
n ou
ter
trou
gh o
f th
e C
risi
um B
asin
. Sh
akin
g fr
om t
he C
risi
umim
pact
may
hav
e se
rved
to le
vel d
epos
its
in th
e ar
ea fr
om th
eFe
cund
itat
is B
asin
as
wel
l.
LO4-
067H
1Su
n El
evat
ion:
24.
7°A
ltit
ude:
297
5.55
km
23
2Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
The
are
a be
twee
n Fr
ankl
in a
nd L
acus
Tem
pori
s is
too
flat
to
be
crat
er-s
atur
ated
hig
hlan
ds,
yet
it i
s no
t co
mpl
etel
yflo
oded
wit
h m
are
mat
eria
l ev
en t
houg
h cr
ater
s su
ch a
sC
heva
llier
, Shu
ckbu
rgh,
and
Oer
sted
hav
e be
en p
artl
y su
b-m
erge
d. C
lem
enti
ne e
leva
tion
dat
a sh
ows
a ro
ughl
y ci
r-cu
lar
depr
essi
on c
ente
red
at 5
3.5°
E an
d 42
.0°
N (
near
Shuc
kbur
gh),
abo
ut 4
00 k
m i
n di
amet
er (
incl
udin
g bo
thFr
ankl
in a
nd L
acus
Tem
pori
s). T
his
depr
essi
on m
ay m
ark
aba
sin
that
has
leve
led
this
reg
ion.
LO4-
067H
2Su
n El
evat
ion:
24.
7°A
ltit
ude:
297
5.55
km
23
3Se
renita
tis
Ba
sin R
egio
n
The
Nec
tari
an c
rate
r En
dym
ion
has
been
sca
rred
by
ejec
tafr
om t
he H
umbo
ldti
anum
Bas
in, o
f th
e sa
me
peri
od. E
ndy-
mio
n is
loc
ated
in
an o
uter
tro
ugh
of t
he H
umbo
ldti
anum
Basi
n; th
e m
ain
ring
of t
he H
umbo
ldtia
num
Bas
in c
an b
e se
encr
ossi
ng th
e up
per
righ
t cor
ner
of th
is p
hoto
. The
sho
ck o
f the
Hum
bold
tian
um i
mpa
ct m
ay h
ave
been
the
cau
se o
f th
eun
usua
lly s
tron
g sl
umpi
ng o
f the
wal
l of E
ndym
ion.
LO4-
067H
3Su
n El
evat
ion:
24.
7°A
ltit
ude:
297
5.55
km
23
4Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
Failu
re o
f Lu
nar
Orb
iter
’s t
herm
al d
oor
(len
s ca
p) c
ause
dgl
are
that
str
ongl
y af
fect
ed t
his
phot
o. T
his
area
inc
lude
s th
e no
rthw
este
rn p
orti
on o
f th
e flo
or o
f M
are
Fecu
ndit
atis
(the
sou
ther
n po
rtio
n is
in
the
Nec
tari
s B
asin
Reg
ion)
. The
brig
hter
are
a in
the
upp
er r
ight
-han
d co
rner
is
a hi
ghla
ndar
ea c
lose
to
Mar
e C
risi
um (
LO4-
061H
2).
The
Cop
erni
can
crat
er T
arun
tius
im
pact
ed a
fter
the
mar
e flo
odin
g. R
isin
gla
va h
as u
plif
ted
a m
elt
shee
t on
its
floor
; the
res
ulti
ng f
rac-
ture
s un
derl
ie R
imae
Tar
unti
us.
Cat
ena
Tar
unti
us l
ies
betw
een
Tar
unti
us a
nd A
nvill
e bu
t ca
nnot
be
seen
in
this
phot
o.
LO4-
061H
1Su
n El
evat
ion:
24.
6°A
ltit
ude:
273
4.00
km
23
5Se
renita
tis
Ba
sin R
egio
n
Thi
s vi
ew o
f th
e w
este
rn s
hore
of
Mar
e C
risi
um s
how
sst
riat
ions
of t
he li
mit
ed e
ject
a pa
tter
n in
this
dir
ecti
on. O
ther
coar
ser
stri
atio
ns
(and
re
mot
e se
nsin
g da
ta
from
Cle
men
tine
) in
dica
te th
at th
is C
risi
um e
ject
a ha
s be
en s
ubse
-qu
entl
y co
vere
d w
ith
ejec
ta f
rom
the
Im
briu
m a
nd/o
rSe
reni
tati
s B
asin
to
the
nort
hwes
t (b
oth
in t
he s
ame
dire
c-ti
on a
nd b
oth
rim
s be
ing
two
basi
n ra
dii a
way
). T
he s
moo
thsl
opin
g w
alls
of
Proc
lus
indi
cate
tha
t it
has
im
pact
ed r
ela-
tive
ly u
nlay
ered
, un
com
pact
ed m
ater
ial.
Such
is
typi
cal
ofth
e ej
ecta
bla
nket
jus
t ou
tsid
e a
basi
n ri
m, i
n th
is c
ase
the
Cri
sium
Bas
in. P
rocl
us i
s a
youn
g C
oper
nica
n cr
ater
wit
h a
spec
tacu
lar
ray
patt
ern.
Par
t of
the
pat
tern
can
be
seen
on
the
floor
of M
are
Cri
sium
.
LO4-
061H
2Su
n El
evat
ion:
24.
6°A
ltit
ude:
273
4.00
km
23
6Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
Thi
s ar
ea t
o th
e no
rthw
est
of M
are
Cri
sium
pro
babl
y sh
ows
ejec
ta f
rom
the
Tra
nqui
llita
tis
Bas
in t
o th
e so
uthw
est,
only
abou
t on
e ba
sin
radi
us fr
om t
he m
ain
ring
, as
wel
l as
ridg
esan
d va
lleys
fr
om
the
dire
ctio
n of
th
e Im
briu
m
and
Sere
nita
tis
Bas
ins.
The
out
er t
roug
h of
the
Cri
sium
Bas
in i
sflo
oded
wit
h m
are,
whi
ch c
onti
nues
int
o th
e flo
or o
fC
leom
edes
. The
bro
ad e
long
ated
dep
ress
ion
in th
e up
per
left
corn
er i
s ra
dial
to
Tra
nqui
llita
tis
(LO
4-06
7H1)
. A
val
ley
half
way
bet
wee
n T
isse
rand
and
Cle
omed
es i
s ra
dial
to
Cri
sium
.
LO4-
061H
3Su
n El
evat
ion:
24.
6°A
ltit
ude:
273
4.00
km
23
7Se
renita
tis
Ba
sin R
egio
n
Thi
s ar
ea i
s ab
out
two
basi
n ra
dii
away
fro
m t
he I
mbr
ium
,Se
reni
tati
s, T
ranq
uilli
tati
s, a
nd H
umbo
ldti
anum
Bas
ins
and
is a
bout
one
bas
in r
adiu
s aw
ay fr
om t
he C
risi
um B
asin
. It
islik
ely
that
rug
ged
high
land
s ar
e co
vere
d w
ith
a th
ick
blan
ket
of p
ulve
rize
d ej
ecta
that
has
som
ewha
t lev
eled
the
terr
ain.
Ave
ry s
moo
th a
rea
in a
dep
ress
ion
that
may
hav
e be
en fo
rmed
by a
cha
in o
f cr
ater
s fr
om t
he C
risi
um B
asin
lie
s be
twee
nG
emin
us a
nd B
erze
lius.
Per
haps
it
is e
ject
a th
at h
as b
een
furt
her
leve
led
by l
ocal
tec
toni
c fo
rces
. G
emin
us h
as a
com
plex
, ter
race
d w
all,
sugg
esti
ng t
hat
it i
mpa
cted
lay
ered
mat
eria
l. C
leom
edes
, som
ewha
t de
grad
ed, b
ut w
ith
its
own
ejec
ta p
atte
rn in
tact
, is
thou
ght t
o be
Nec
tari
an.
LO4-
062H
1Su
n El
evat
ion:
25.
4°A
ltit
ude:
297
9.32
km
23
8Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
The
wes
tern
par
ts o
f M
essa
la h
ave
rece
ived
hea
vy d
epos
its
from
Cri
sium
to
the
sout
h. A
ddit
iona
l bu
t fin
er d
epos
its
from
C
risi
um
can
be
seen
be
twee
n C
arri
ngto
n an
dSc
hum
ache
r. L
acus
Tem
port
is, S
huck
burg
h, a
nd H
ooke
may
be l
ocat
ed i
n th
e flo
or o
f an
anc
ient
cra
ter
or b
asin
(se
e LO
4-06
7H2)
. M
essa
la a
nd t
he 3
0-km
cra
ter
in i
ts w
este
rnflo
or a
re b
oth
iden
tifie
d as
of t
he P
re-N
ecta
rian
Per
iod.
LO4-
062H
2Su
n El
evat
ion:
25.
4°A
ltit
ude:
297
9.32
km
23
9Se
renita
tis
Ba
sin R
egio
n
LO4-054HSun Elevation: 25.5°Altitude: 2736.65 km
The ring that bounds Mare Crisium hasa flat-topped structure like a plateau. In comparison with Orientale rings, this ring is more like one of the MontesRook rings (inner rings) than likeMontes Cordillera (the main ring).There is sporadic lava flooding beyondthis inner ring, just as in the OrientaleBasin.
The Crisium Basin has its ownmascon, revealing an internal source of lava from beneath the crust. An“isthmus” of about 200 km separatesMare Crisium and Mare Fecunditatis.This narrow strip of highlands is deeplyscored by ejecta from the youngerCrisium.
Luna 16 (September 1970) landed onMare Fecunditatis, drilled a 35-cm core,and returned a 101-gram (101-g) sam-ple to earth. It showed a mineral com-position similar to that of other mariasamples, with some quantitative differ-ences. Luna 18 (September 1971) failedupon landing, possibly due to the rough-ness of its landing site. Luna 20 (February1972) returned 50 g of samples, probablyCrisium ejecta. The samples are distinctlydifferent from mare material; lighter incolor and higher in density, the samplesare similar to those gathered by Apollofrom other basin rims.
24
0Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
The
lar
ge fl
at a
rea
east
of
Bur
ckha
rdt
is i
n an
out
er t
roug
h of
the
Cri
sium
Bas
in. I
n C
lem
enti
ne a
lbed
o da
ta, i
t has
a d
ark,
mot
tled
look
as
if it
is in
com
-pl
etel
y flo
oded
wit
h m
are
mat
eria
l. T
he fl
atte
ning
may
hav
e be
en p
artly
cau
sed
by t
he f
orm
atio
n of
the
tro
ugh
of C
risi
um, p
artl
y by
tec
toni
c sh
akin
g of
un-
cons
olid
ated
hig
hlan
ds, a
nd p
artly
by
mar
e flo
odin
g.
24
1Se
renita
tis
Ba
sin R
egio
n
LO4-
055H
1Su
n El
evat
ion:
25.
8°A
ltit
ude:
298
2.10
km
LO4-
055H
2Su
n El
evat
ion:
25.
8°A
ltit
ude:
298
2.10
km
24
2Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
Cha
ins
of s
econ
dary
cra
ters
in
this
are
a ra
diat
e fr
om t
he H
umbo
ldti
anum
Bas
in t
o th
e no
rthe
ast.
In C
lem
enti
ne a
lbed
o da
ta, L
acus
Spe
i is
a d
ark
and
wel
l-de
fined
are
a of
mar
e flo
odin
g. S
chum
ache
r is
als
o flo
oded
wit
h m
are
mat
eria
l. Fo
r a
clea
rer
phot
ogra
ph o
f th
is a
rea
see
LO4-
165H
2 in
the
Eas
tern
Bas
ins
Reg
ion,
Cha
pter
10.
Ray
s fr
om H
ayn
to th
e no
rthe
ast a
ppea
r ve
rtic
al in
this
pic
ture
bec
ause
of i
tsor
ient
atio
n. T
he m
ain
ring
of
the
Hum
bold
tian
um B
asin
pas
ses
acro
ss t
helo
wer
left
cor
ner
of t
his
phot
o; a
n in
ner
ring
bou
nds
Mar
e H
umbo
ldti
anum
.B
etw
een
the
two
ring
s is
an
area
tha
t ha
s be
en fl
atte
ned
by t
he f
orce
s th
atcr
eate
d th
e tr
ough
.
24
3Se
renita
tis
Ba
sin R
egio
n
LO4-
055H
3Su
n El
evat
ion:
25.
8°A
ltit
ude:
298
2.10
km
10.1. OverviewThe Eastern Basins Region covers roughly the area between60° east longitude and the eastern limb (90° east longitude)and between 60° south latitude and 60° north latitude.
The region contains part of several definite ringed basins,Crisium, Australe, Smythii, and Humboldtianum (southernpart) in downward order of size, and the probable basin,Balmer-Kapteyn. Each of these basins has some mare mater-ial within it, but (with the exception of Mare Crisium) themare is irregular, probably because this region is midwaybetween the thin crust of the western and central near sideand the thick crust of the far side.
Although the basins in this region are older than Imbrium,they are relatively free of its influence becausee the region ismostly beyond a basin radius away from the main ring ofImbrium.
The Crisium BasinThe Crisium Basin has a topographic rim 740 km in diame-ter. It is one of the younger basins and is particularly inter-esting. It represents the transition between the older basinsto the west, strongly dominated by ejecta from the giant,relatively young Imbrium Basin, and basins near the easternlimb and on the far side that are relatively free of theinfluence of Imbrium.
In a first impression, the Crisium Basin appears to be elon-gated in form, which might be taken as evidence of a glanc-ing impact. On closer inspection, the shape resolves into twocircular basins, as shown in Figure 10.1.
The western, northern, and southern shores of the CrisiumBasin are nearly covered with ridges and valleys formed byejecta from the Imbrium Basin to the northwest. To the east,the topography is dominated by ejecta from Crisium itself.Clementine multispectral data show a strong differencebetween the mineral signatures to the west, which is uppercrust ejected from the Imbrium Basin, and the signatures tothe east, which are believed to contain portions of lowercrust below the Crisium Basin.
The Australe BasinThe Australe Basin is partly on the near side and partly onthe far side; its center is at 52° south latitude and 95° eastlongitude. Since it was formed in the Pre-Nectarian Period, ithas been severely degraded. No rings outside of the main
ring have been identified, but at least one inner ring has beentraced.
The central part of this basin has been only partiallyflooded with mare lava. As seen in Figure 10.2, lava haserupted only where impactors have formed large craters inthe basin floor. Perhaps the central Australe Basin had an ex-tensive melt sheet that inhibited the rise of lava except whereit has been penetrated.
The Smythii BasinThe Smythii Basin, as large as Crisium, is at 2° south latitudeand 87° east longitude and straddles the eastern limb. It isbest seen in Lunar Orbiter 2 photograph 196M, shown inFigure 10.3. There is a mascon associated with Mare Smythii.
10.2. High-Resolution ImagesLunar Orbiter 4 was planned to start its photographicmission at the eastern limb with a series of photos like the
Chapter 10
Eastern Basins Region
Figure 10.1. Crisium Basin (part of LO4-060M). Mare Crisium lookssomewhat like a flounder. Mare Fecunditatis and Mare Tranquillitatis are inthe lower left corner of the figure. Mare Marginis is far to the right. MareUndarum, the dark area southeast of Crisium, is in an intersection of outertroughs of the Crisium and Fecunditatis Basins. Mare Crisium has floodeddepressions from a complex series of impacts. The circular shape of thelargest depression has been modified by a large crater or basin to the west-northwest of the main impact and a smaller crater to the east (the “tail of thefish”).
24
4Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
rest of the mission, systematically taking four to six expo-sures on each orbit from near perilune, at an altitude ofabout 3000 km.
Unfortunately, the thermal door (a lens cap) locked open,leaving the optics open to the cold of space. As a resultmoisture condensed on the inside of the lenses (much as dewmight settle on the outside of a lens), fogging the pho-tographs. After analysis, the spacecraft was kept pointing atthe lunar surface (warmer than deep space) and the lenscleared. Meanwhile, many exposures were lost or badly de-graded. Of the planned high-resolution photos in this region,only LO4-009H and LO4-018H are printed in this chapter.
The mission operators compensated for the loss by schedul-ing a series of photos near the end of the mission, when theapolune (the other end of the orbit, at about 5500 km) cameover the eastern limb. These are the photos used to cover theEastern Basins Region. The resolution is of course lower andthe coverage larger. As a result, two subframes from each ofthese exposures cover parts of this region. The remaining sub-frames cover parts of the North and South Polar Regions. Table10.1 shows the high-resolution images of the Eastern BasinsRegion in schematic form.
The following pages show the high-resolution subframesfrom south to north and west to east. The apolune photos arein the order LO4-191H3, LO4-191H2, LO4-184H2, LO4-184H1, LO4-178H2, LO4-178H1, LO4-177H3, LO4-177H2,
LO4-165H3, and LO4-165H2. This seems like a confusing se-quence but it results from the spacecraft flying from north tosouth, in reverse of the usual direction. For consistency, wefollow the usual south to north convention, despite having topresent the pictures in the reverse order of their numbers.The perilune photos are presented in the order of LO4-018H1… LO4-018H3, LO4-009H1 … LO4-009H3 (the usual order).
Because of the loss of photography early in Lunar OrbiterMission 4, high-resolution exposures in the southern part ofthe Eastern Basins Region (with the exception of LO4-009)have been lost. To identify the features of this region, amedium-resolution photo from Mission 2 (LO2-196M) isprovided at the end of this chapter.
Figure 10.2. Australe Basin (LO4-009M). The center of the basin is slightlyleft and below the center of the photo. The main ring, most pronounced in theeastern sector, spans 30° of the lunar circumference. The dark circular featurenear the top is Mare Smythii, with radial ridges and valleys of the SmythiiBasin ejecta surrounding it. The Balmer-Kapteyn Basin straddles the termina-tor southwest of Mare Smythii. Near the bottom of the picture is Schrodinger,a small far side basin that nonetheless has strong radial valleys extending fromits main ring. The dark far side feature to the right is the flooded craterTsiolkovskiy. Half of the ancient South Pole–Aiken Basin of the far side is inthis picture. Its main ring intersects that of Australe. Schrodinger, but notTsiolkovskiy, is within the South Pole–Aiken Basin.
Figure 10.3. The Smythii Basin (LO2-196M). The dark compact mare tothe upper left is Mare Smythii, with Mare Marginis above it and a small areaof mare below it. The southeastern sector of the main topographic ring ofthe Smythii Basin can be seen curving from the top center and out the lowerleft side of this photo.
Lattitude Range Photo Number
56 N–90 N 191H1 177H1 165H1 191H1
27 N–56 N 062 191H2 177H2 165H2
0–27 N 061 191H3 177H3 165H3 018
0–27 S 060 184H1178H1
27 S–56 S 059 184H2178H2 009
56 S–90 S 184H3178H3
Longitude 57 E 54 E 70 E 75 E 81 E 90 E 96 Eat Equator
Table 10.1. The cells shown in white represent the high-resolutionphotos of the Eastern Basins Region (LO4-XXX H1, -H2, and -H3, whereXXX is the Photo Number). The North Polar Region is to the north, theSerenitatis Basin Region is to the northwest, the Nectaris Basin Region is tothe southwest, and the South Polar Region is to the south. The far side is tothe east. Exposures 165 to 191 were taken from apolune in afternoon sun,and exposures 009 and 018 were taken at perilune in morning sun. Apolunephotos were taken at about twice the altitude of perilune photos, so theyhave about half the resolution and four times the area of coverage.
24
5Ea
ster
nBa
sins
Reg
ion
Mar
e A
ngui
s ha
s flo
oded
an
oute
r tr
ough
of
the
Cri
sium
Basi
n. T
he e
dge
of M
are
Fecu
ndit
atis
can
be
seen
in th
e lo
wer
left
cor
ner
of th
is p
hoto
. Dor
sum
Opp
el, t
oget
her
wit
h D
orsa
Tet
yaev
(LO
4-17
7H3)
, may
out
line
an in
ner
ring
, alo
ng w
ith
Dor
sum
Ter
mie
r an
d D
orsa
Har
ker
(not
vis
ible
her
e). D
ays
befo
re A
pollo
11
land
ed (
July
196
9), t
he r
etro
-roc
ket o
f Lun
a15
faile
d an
d it
cra
shed
. Lun
a 24
suc
cess
fully
land
ed (
Aug
ust
1976
) an
d re
turn
ed a
cor
e sa
mpl
e fr
om a
mar
e un
visi
ted
byA
pollo
. T
his
was
the
las
t sa
mpl
e re
turn
ed t
o Ea
rth
to t
his
day.
LO4-
191H
3Su
n El
evat
ion:
16.
3°A
ltit
ude:
550
3.39
km
24
6Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
The
eas
tern
par
t of t
his
area
is in
the
East
ern
Bas
ins
Reg
ion,
but
the
wes
tern
par
t is
in
the
Sere
nita
tis
Bas
in R
egio
n.B
ecau
se o
f th
e ov
erla
p, t
here
is
an o
ppor
tuni
ty t
o co
mpa
reth
e af
tern
oon
sun
illum
inat
ion
of t
his
phot
o (c
omin
g fr
omth
e ea
st)
wit
h th
e m
orni
ng s
un o
f th
e ph
otos
in
the
Sere
nita
tis
chap
ter
(Cha
pter
9).
Str
iati
ons
from
the
sout
h ar
era
dial
to
Cri
sium
and
tho
se f
rom
the
nor
thea
st a
re f
rom
Hum
bold
tian
um.
LO4-
191H
2Su
n El
evat
ion:
16.
3°A
ltit
ude:
550
3.39
km
24
7Ea
ster
nBa
sins
Reg
ion
Thi
s hi
ghla
nd a
rea
sout
heas
t of t
he F
ecun
dita
tis
Bas
in h
as e
xten
sive
cha
ins
ofse
cond
ary
crat
ers,
som
e ra
dial
to P
etav
ius
and
som
e fr
om th
e N
ecta
ris
Bas
in.
Rim
ae H
ase
are
stre
ss fr
actu
res
radi
al to
the
Nec
tari
s B
asin
. The
mai
n ri
ng o
fth
e m
uch-
degr
aded
Aus
tral
e B
asin
pas
ses
thro
ugh
Mar
inus
. T
he fl
at a
rea
LO4-
184H
2Su
n El
evat
ion:
6.9
°A
ltit
ude:
579
0.16
km
betw
een
thes
e cr
ater
s an
d Fu
rner
ius
(Lat
e Im
bria
n) m
ay b
e in
an
oute
r tr
ough
of t
his
larg
e, d
egra
ded,
Pre
-Nec
tari
an B
asin
. See
LO
4-05
3H1
and
LO4-
052H
3in
the
Nec
tari
s ch
apte
r (C
hapt
er 8
)for
a d
iscu
ssio
n of
the
fra
ctur
ed-fl
oor
crat
ers
Peta
vius
and
Fur
neri
us.
24
8Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
Thi
s so
mew
hat
obliq
ue p
hoto
sho
ws
an o
verv
iew
of
the
equa
tori
al r
egio
n in
the
vici
nity
of
70°
east
lon
gitu
de.
The
Pre
-Nec
tari
an B
alm
er-K
apte
yn B
asin
can
clea
rly
be s
een.
Bal
mer
has
impa
cted
the
mai
n ri
ng o
f thi
s ba
sin.
Str
iati
ons
cros
sing
thi
s ba
sin
coul
d be
fro
m L
angr
enus
or
the
Fecu
ndit
atis
Bas
in. N
ote
the
larg
e di
ffer
ence
in
albe
do b
etw
een
Pre-
Nec
tari
an V
ende
linu
s an
d th
e
LO4-
184H
1Su
n El
evat
ion:
6.9
°A
ltit
ude:
579
0.16
km
Erat
osth
enia
n cr
ater
Lan
gren
us, w
hose
terr
aced
wal
l is
rela
tive
ly s
harp
. Lam
eha
s pu
shed
mat
eria
l fro
m t
he w
all o
f V
ende
linus
ont
o it
s flo
or. T
he c
hain
of
larg
e cr
ater
s be
twee
n K
apte
yn a
nd M
acLa
urin
and
the
sm
alle
r ch
ain
cros
sing
Lam
e ra
diat
e fr
om M
are
Cri
sium
. Se
e LO
4-05
4H1
(the
Ser
enit
atis
cha
pter
,C
hapt
er 9
) fo
r Lu
na 1
6, 1
8, a
nd 2
0.
24
9Ea
ster
nBa
sins
Reg
ion
Hum
bold
t is
a c
rate
r w
ith
an e
xten
sive
dep
osit
tha
t ex
tend
s in
to t
he A
ustr
ale
Bas
in,
who
se m
ain
ring
pas
ses
near
Oke
n an
d H
arla
n. H
umbo
ldt
has
a flo
or w
ith
a fr
actu
re p
atte
rn t
hat
reve
als
sign
s of
upl
ift
(see
the
ins
et f
rom
LO4-
027H
1, a
per
ilune
pho
to w
ith
mor
ning
ligh
t). D
ark
man
tling
mat
eria
l can
be s
een
on th
e flo
or o
f thi
s cr
ater
, nea
r th
e w
all.
Stri
atio
ns in
this
pho
to r
adia
tefr
om th
e N
ecta
ris
Bas
in.
LO4-
178H
2Su
n El
evat
ion:
1.5
°A
ltit
ude:
579
6.24
km
25
0Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
Thi
s sh
ows
the
wes
tern
sec
tor
of t
he m
ain
ring
of
the
Smyt
hii
Bas
in, a
long
wit
h an
out
er tr
ough
(un
derl
ying
Kas
tner
) an
d ou
ter
ring
. Mar
e U
ndar
um fi
llsan
out
er t
roug
h of
the
Cri
sium
Bas
in,
to t
he n
orth
wes
t of
thi
s ph
oto.
Hec
atae
us a
nd t
he s
mal
ler
crat
er t
o it
s no
rth
show
sig
ns o
f a
sim
ulta
neou
sim
pact
. Spe
cific
ally
, the
eas
tern
rim
s of
the
tw
o cr
ater
s in
terl
ock;
nei
ther
can
be s
aid
to b
e su
peri
mpo
sed
on th
e ot
her.
LO4-
178H
1Su
n El
evat
ion:
1.5
°A
ltit
ude:
579
6.24
km
25
1Ea
ster
nBa
sins
Reg
ion
LO4-
177H
3 w
as t
aken
nea
r th
e en
d of
the
mis
sion
(su
n fr
om t
he w
est)
to
repl
ace
cove
rage
los
t at
the
beg
inni
ng b
ut g
lare
has
des
troy
ed m
ost
of t
heph
oto.
The
los
t ar
ea h
as b
een
repl
aced
her
e w
ith
part
of
med
ium
-res
olut
ion
phot
o LO
4-06
0M (
sun
from
the
east
). D
orsa
Tet
yaev
is p
art o
f a c
ircl
e of
mar
eri
dges
tha
t m
ay o
verl
ie a
n in
tern
al r
ing
of t
he C
risi
um B
asin
. The
rid
ges
and
LO4-
177H
3 an
d LO
4-06
0MSu
n El
evat
ion:
14.
8°A
ltit
ude:
549
1.85
km
valle
ys n
ear
Wild
t ar
e C
risi
um e
ject
a, p
roba
bly
over
lyin
g de
posi
ts f
rom
the
Smyt
hii
Bas
in. T
his
is t
he o
nly
area
whe
re C
risi
um e
ject
a is
exp
osed
: eje
cta
from
Im
briu
m a
nd S
eren
itat
is o
verl
ies
Cri
sium
eje
cta
to t
he w
est.
Mar
eU
ndar
um li
es in
an
oute
r tr
ough
of t
he C
risi
um B
asin
.
25
2Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
Not
e th
e da
rk a
reas
thro
ugho
ut th
is r
egio
n, w
hich
may
indi
cate
dar
k m
antli
ngm
ater
ial.
The
str
ong
ridg
es a
nd v
alle
ys in
the
cen
ter
of t
his
phot
o ar
e pa
rt o
fth
e ej
ecta
bla
nket
from
the
Hum
bold
tian
um B
asin
dir
ectl
y to
the
nort
h, in
the
Nor
th P
olar
Reg
ion.
Hum
bold
tian
um is
cla
ssifi
ed a
s N
ecta
rian
, lik
e C
risi
um,
LO4-
177H
2Su
n El
evat
ion:
14.
8°A
ltit
ude:
549
1.85
km
but
is b
elie
ved
to b
e ol
der.
Zen
o, G
auss
, an
d ej
ecta
fro
m G
auss
are
sup
er-
impo
sed
on t
he H
umbo
ldti
anum
eje
cta
and
thus
mus
t be
you
nger
, but
the
yar
e st
ill c
lass
ified
as
Nec
tari
an fe
atur
es. N
ote
the
diff
eren
ce in
text
ure
sout
h of
Ber
osus
, as
Hum
bold
tian
um e
ject
a is
cov
ered
wit
h th
at o
f Cri
sium
.
25
3Ea
ster
nBa
sins
Reg
ion
(Jea
n-)
Fred
eric
Jol
iot
mar
ried
Ire
ne C
urie
, the
dau
ghte
r of
Pier
re a
nd M
arie
Cur
ie (
LO4-
165H
3).
Iren
e an
d Fr
eder
icJo
liot-
Cur
ie w
orke
d to
geth
er a
nd s
hare
d th
e N
obel
Pri
ze f
orsy
nthe
sizi
ng n
ew r
adio
acti
ve e
lem
ents
by
bom
bard
ing
targ
ets
wit
h al
pha
part
icle
s.
Mar
e M
argi
nis
is
not
deep
, an
dC
lem
enti
ne e
leva
tion
dat
a sh
ow a
pat
tern
tha
t is
mor
e lik
e a
colle
ctio
n of
cra
ters
suc
h as
Nep
er t
han
a ba
sin
floor
. The
pitt
ed a
rea
sout
h of
Can
non
and
Hub
ble
is a
t the
ant
ipod
es o
fth
e O
rien
tale
Bas
in (
see
also
LO
4-18
H2
and
-H3)
. As
in o
ther
such
cas
es, r
ocks
eje
cted
in a
ll di
rect
ions
from
Ori
enta
le h
ave
conv
erge
d he
re a
fter
tra
velin
g ha
lfw
ay a
roun
d th
e M
oon,
lead
ing
to a
loca
l hig
h de
nsit
y of
sm
all s
econ
dari
es.
LO4-
165H
3Su
n El
evat
ion:
13.
9°A
ltit
ude:
548
6.51
km
25
4Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
Thi
s re
gion
is
dom
inat
ed b
y ri
dges
, va
lleys
and
sec
onda
rycr
ater
s of
the
Hum
bold
tian
um B
asin
to
the
nort
h, i
n th
eN
orth
Pol
ar R
egio
n. Z
eno
and
Gau
ss h
ave
been
sup
er-
impo
sed
on t
he H
umbo
ldti
anum
eje
cta.
Sec
onda
ries
fro
mC
risi
um t
o th
e so
uth
have
lan
ded
near
Zen
o. G
auss
is
unus
ual,
for
its
size
, in
havi
ng a
min
imal
cen
tral
pea
k.
LO4-
165H
2Su
n El
evat
ion:
13.
9°A
ltit
ude:
548
6.51
km
25
5Ea
ster
nBa
sins
Reg
ion
Mar
e Sm
ythi
i is
in a
wel
l-fo
rmed
Pre
-Nec
tari
an b
asin
. Cle
men
tine
dat
a sh
ow a
circ
ular
dep
ress
ion
(cen
tere
d ne
ar th
e m
iddl
e bo
ttom
edg
e of
this
pho
to)
wit
hth
e flo
or fl
oode
d by
mar
e m
ater
ial.
A m
asco
n in
dica
tes
a pl
ume
of la
va r
ose
from
the
man
tle.
Nec
tari
an c
rate
r N
eper
, whi
ch im
pact
ed th
e m
ain
ring
of t
heSm
ythi
i Bas
in, m
ay h
ave
been
floo
ded
thro
ugh
subs
urfa
ce la
va fl
ows
unde
r th
e
LO4-
018H
1Su
n El
evat
ion:
28.
4°A
ltit
ude:
273
9.66
km
chan
nel w
est
of T
acch
ini.
Sim
ilar
stru
ctur
es t
o th
e pl
atea
us a
nd v
alle
ys s
outh
of J
ansk
y ar
e se
en i
n th
e no
rthe
rn p
art
of t
he r
im o
f th
e O
rien
tale
Bas
in(M
onte
s C
ordi
llera
). O
ther
sim
ilari
ties
to
Ori
enta
le m
ay r
eflec
t th
e de
eper
crus
t und
er th
ese
basi
ns. T
acch
ini a
nd Ja
nsky
hav
e ex
tens
ive
depo
sits
of e
ject
afr
om th
e Sm
ythi
i Bas
in.
25
6Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
018H
2Su
n El
evat
ion:
28.
4°A
ltit
ude:
273
9.66
km
crat
er w
alls
of
Al-
Bir
uni
have
bee
n ov
erla
id w
ith
thes
e st
riat
ions
and
wit
hth
ose
from
the
Sm
ythi
i Bas
in, s
o A
l-B
irun
i’s c
rate
r m
ust
have
for
med
bef
ore
thos
e ba
sins
. T
he m
are
surf
ace
in A
l-B
irun
i ha
s be
en a
ssig
ned
to t
he L
ate
Imbr
ian
Peri
od.
25
7Ea
ster
nBa
sins
Reg
ion
The
val
leys
and
rid
ges
cros
sing
Nep
er a
nd G
odda
rd r
adia
te f
rom
the
Sm
ythi
iB
asin
. C
oper
nica
n cr
ater
God
dard
A (
12 k
m,
just
nor
th o
f G
odda
rd)
has
spre
ad i
ts r
ay p
atte
rn a
s fa
r as
Mar
e M
argi
nis.
The
nor
thw
est
to s
outh
east
stri
atio
ns i
n th
e vi
cini
ty o
f G
odda
rd a
re r
adia
l to
the
Im
briu
m B
asin
. T
he
Jolio
t’s c
entr
al p
eaks
form
wha
t m
ay b
e th
e be
ginn
ing
of a
n in
ner
ring
. Jol
iot
and
Hub
ble
have
had
thei
r flo
ors
flood
ed w
ith
lava
, des
pite
bei
ng fa
r fr
om a
nym
asco
n th
at m
ay m
ark
a pl
ume
from
the
man
tle.
Str
iati
ons
on th
e no
rthe
ast-
ern
wal
l of
Jol
iot
are
from
the
far
sid
e cr
ater
Lya
puno
v (a
djac
ent
and
muc
h
LO4-
018H
3Su
n El
evat
ion:
28.
4°A
ltit
ude:
273
9.66
km
youn
ger)
, who
se fl
oor
is a
lso
flood
ed w
ith
lava
. Ver
y lit
tle
mar
e m
ater
ial
isin
volv
ed b
ecau
se t
he c
rate
rs a
re n
ot f
ully
floo
ded.
The
cru
st i
s th
icke
r he
re,
alon
g th
e ea
ster
n li
mb,
and
tha
t m
ay e
xpla
in w
hy r
elat
ivel
y li
ttle
lav
a is
avai
labl
e.
25
8Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
The
cen
ter
of t
he A
ustr
ale
Bas
in (
52°
S, 9
5°E)
is
near
the
uppe
r le
ft c
orne
r of
thi
s ph
oto.
The
cir
cula
r se
gmen
t of
ari
dge
pass
ing
thro
ugh
Prie
stly
and
Leb
edev
is
an i
nner
rin
gof
this
bas
in. T
he b
asin
is o
bvio
usly
ver
y ol
d (P
re-N
ecta
rian
);m
any
crat
ers
of v
ario
us le
vels
of d
egra
dati
on h
ave
impa
cted
its
floor
. Kug
ler
and
near
by c
rate
rs h
ave
been
floo
ded
wit
hla
va, r
esur
faci
ng t
hose
are
as m
uch
late
r (e
spec
ially
in t
erm
sof
cra
ter
coun
ts)
than
the
form
atio
n of
the
floor
of t
he b
asin
.C
lem
enti
ne e
leva
tion
dat
a sh
ow th
is s
outh
ern
port
ion
of th
eba
sin
floor
to b
e hi
gher
than
the
nort
hern
floo
r.
LO4-
009H
1Su
n El
evat
ion:
24.
8°A
ltit
ude:
298
9.14
km
25
9Ea
ster
nBa
sins
Reg
ion
Ejec
ta o
f Lat
e Im
bria
n cr
ater
Jenn
er o
verl
ies
the
mar
e m
ater
-ia
l her
e, b
ut la
va fl
oodi
ng t
he fl
oor
of G
um h
as i
nter
rupt
edth
e se
cond
ary
field
of
Jenn
er,
and
Jenn
er i
tsel
f is
floo
ded.
App
aren
tly
Jenn
er i
mpa
cted
Mar
e A
ustr
ale
betw
een
two
orm
ore
lava
floo
ding
eve
nts.
Ano
ther
exa
mpl
e of
two
Aus
tral
ela
va fl
ows
stra
ddlin
g a
crat
er e
vent
can
be
seen
in L
O4-
009H
3ne
ar H
umbo
ldt.
Like
the
Sou
th P
ole–
Aik
en B
asin
of
the
far
side
, the
Aus
tral
e B
asin
has
onl
y a
very
wea
k po
siti
ve g
ravi
tyan
omal
y, s
ugge
stin
g ei
ther
a w
eak,
dif
fuse
sou
rce
of la
va o
ris
osta
tic
adju
stm
ent
of t
he s
urfa
ce o
f th
ese
very
old
bas
ins:
perh
aps
the
crus
t was
sti
ll pl
asti
c w
hen
they
wer
e fo
rmed
.
LO4-
009H
2Su
n El
evat
ion:
24.
8°A
ltit
ude:
298
9.14
km
26
0Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
A s
ecto
r of
the
mai
n ri
ng o
f th
e A
ustr
ale
Bas
in p
asse
sbe
twee
n A
bel
and
Bar
nard
, fo
rmin
g th
e no
rthe
rn s
hore
of
Mar
e A
ustr
ale.
The
sec
onda
ry fi
eld
of L
ate
Imbr
ian
crat
erH
umbo
ldt h
as b
een
cove
red
by a
you
ng m
are
flow
. Com
pare
this
wit
h th
at o
f Je
nner
(LO
4-00
9H2)
. Nei
ther
Bar
nard
nor
its
smal
ler
com
pani
on to
the
sout
h do
min
ates
the
crat
er w
all
betw
een
them
, sug
gest
ing
a si
mul
tane
ous
impa
ct. A
bel
has
had
its
wal
l pu
shed
ont
o it
s flo
or b
y B
arna
rd’s
com
pani
on.
Mar
ie C
urie
(bo
rn S
klod
owsk
a) a
nd h
er h
usba
nd P
ierr
eC
urie
rec
eive
d a
Nob
el P
rize
for
stu
dies
of
radi
oact
ivit
y.A
fter
Pie
rre’
s de
ath,
Mar
ie w
on a
sec
ond
Nob
el P
rize
for
the
disc
over
y of
rad
ium
and
pol
oniu
m (
see
LO4-
165H
3 fo
r m
ore
Cur
ie fa
mily
his
tory
).
LO4-
009H
3Su
n El
evat
ion:
24.
8°A
ltit
ude:
298
9.14
km
26
1Ea
ster
nBa
sins
Reg
ion
The
pla
n fo
r Lu
nar
Orb
iter
Mis
sion
4 w
as t
o ta
ke e
xten
sive
hig
h-re
solu
tion
phot
os o
f th
e ea
ster
n lim
b. H
owev
er, m
any
of t
hese
pho
tos
wer
e lo
st, e
spe-
cial
ly in
the
sout
h, b
ecau
se o
f the
failu
re o
f the
lens
cap
. Thi
s m
ediu
m-r
esol
u-ti
on p
hoto
fro
m L
unar
Orb
iter
Mis
sion
2 (
also
sho
wn
in F
igur
e 10
.3)
ispr
ovid
ed t
o fil
l in
the
gap
and
loca
te t
he n
amed
fea
ture
s ne
ar t
his
part
of
the
limb.
The
sou
thea
st s
ecto
r of
the
mai
n ri
ng o
f th
e Sm
ythi
i Bas
in c
an b
e se
en
LO2-
196M
Sun
Elev
atio
n: 1
9.9°
Alt
itud
e: 1
519.
03 k
m
ente
ring
the
phot
o at
the
top
and
curv
ing
arou
nd to
war
d th
e le
ft e
dge.
The
re is
a m
asco
n be
low
Mar
e Sm
ythi
i (w
hich
nea
rly
fills
an
inne
r ri
ng o
f th
e ba
sin)
but
not
belo
w M
are
Mar
gini
s. B
eyon
d th
e m
ain
ring
lies
the
tra
nsit
ion
to t
hehi
ghla
nd r
egio
n of
the
far
side
, wit
h it
s th
icke
r cr
ust.
Lacu
s So
litud
inus
may
be
a pa
rt o
f th
e sp
otty
ext
rusi
ons
of m
are
mat
eria
l ass
ocia
ted
wit
h th
e A
ustr
ale
Bas
in to
the
sout
h.
26
2Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
11.1. OverviewThe North Polar Region covers the area between the NorthPole and about 55° south latitude and between the westernand eastern limbs.
Mare Frigoris extends along the southern boundary of theregion. The area near the pole is heavily cratered highlands.Mare Humboldtianum is near the eastern limb of this regionat the center of the Humboldtianum Basin.
Mare FrigorisMare Frigoris (Figure 11.1) extends about 1500 km in theeast-west direction but only about 300 km in the north-southdirection. Its western section is clearly circumferential to theImbrium Basin, filling the outer trough of that basin. It con-nects with Sinus Roris, a large bay at the northern extremityof Oceanus Procellarum. The eastern section of MareFrigoris is northeast of the Serenitatis Basin. The lava surfaceof Mare Frigoris connects to that of Mare Serenitatis throughLacus Somniorum.
Chapter 11
North Polar Region
Figure 11.1. Mare Frigoris (LO4-190M). The white dashed lines are the 90° W and 0° E/W meridians. Mare Frigoris is the dark area stretching around theNorth Pole, a little more than halfway to the edge of the Moon. Mare Imbrium is near the bottom of the photo and Mare Serenitatis is to its right.
26
3N
ort
h
Pola
r R
egio
n
The Humboldtianum BasinThe Humboldtianum Basin (Figure 11.2), near the northeast-ern limb of the Moon, is a ringed basin that, like theOrientale and Nectaris Basins, is sufficiently far fromyounger basins that its structure is well preserved. Theringed structure can be seen in LO4-065H1 in this chapter.
The North Polar HighlandsThe heavily cratered region at the polar cap (see Figures 11.1and 11.2) extends across the pole into the far side highlands.The crust is thicker here, relative to the mare-filled areas tothe south. Even though there are large craters (not quitebasin sized), there is no sign of lava flooding beyond 70°north latitude on either the near side or far side.
The North PoleThe best parts of the photos taken near the North Pole oneach of the orbits of Clementine have been carefully assem-bled and are shown in Figure 11.3.
The highest points in this area, such as on the rims of largecraters, are in sunlight all or nearly all the time because theaxis of the Moon is within 1.5° of a right angle to the plane of
its travel around the sun (the ecliptic plane). Such a site isespecially interesting for a long-term base on the Moonbecause continuous or nearly continuous solar cell powerwould be available. Conceivably, solar panel farms could beestablished there (or near the South Pole) and the powercould be beamed to Earth.
Nearby, on the floors of smaller, deeper craters withinRozhdesvenskiy and Peary, there are very cold areas thatnever receive light or heat from the sun (see Chapter 12).Analysis of data from the neutron spectrometer instru-ments on the Lunar Prospector spacecraft has detected de-posits of hydrogen in the vicinity of these cold traps nearboth poles. If the hydrogen is in water molecules, it is inthe form of crystals distributed in the lunar soil, not assolid ice. The neutron spectrometer detects the energy ofsolar wind neutrons that rebound from the nuclei of atomson the lunar surface. A neutron that rebounds from thesingle proton in the nucleus of a hydrogen atom loses muchmore energy than if it rebounds from a nucleus of a heavierelement.
See the overview in the chapter on the South Polar Region(Chapter 12) for a discussion of how these hydrogen concen-trations can be used.
11.2. High-Resolution ImagesThe Lunar Orbiter photos of the North Polar Region, likethose of the South Polar Region, have a high degree ofoverlap because they were taken from a near-polar orbit. Allthe rectangular sets of three subframes in a high-resolutionexposure have the pole in or near the top of the northernsubframe. The illumination angle in the middle subframes isabout 10° but the angle approaches zero toward the pole. Ofcourse, the pole is always within 1.5° of the terminator.
Although the polar photos were not taken on every orbitover the poles, there is still so much overlap in the middleand northern subframes that only every other photo isprinted here (all the photos are in the enclosed CD). Table11.1 shows the high-resolution images of the North PolarBasin Region in schematic form.
The following pages show the high-resolution subframesfrom south to north and west to east. The photos are in theorder LO4-190H1, LO4-190H2, LO4-190H3, LO4-178H1,LO4-164H1, LO4-164H2, …. The last photo is LO4-165H1, anapolune photo.
To fill in an area in the southwestern part of the NorthPolar region, which was not photographed in high resolu-tion, the first following page shows medium-resolutionphoto LO4-189M. The planned high-resolution LunarOrbiter photos of the far eastern part of the North PolarRegion were spoiled by the failure of the thermal door. Nearthe end of the mission, apolune photos were taken of thatarea. One of these (LO4-165H1) is presented at the end ofthis chapter to complete coverage of the near side NorthPolar Region.
Figure 11.2. Humboldtianum Basin (LO4-128M). The black dashed linesmark the 0° E/W and 90° E meridians. The small dark area in the upper rightof this picture (near the 90° E meridian) is Mare Humboldtianum in thefloor of the Humboldtianum Basin. The basin structure is obscured in thisphoto by the bright ejecta and rays of the nearby Copernican craterBelkovitch. The large dark area near the bottom left of the picture is MareImbrium; Mare Serenitatis is to the east. Mare Frigoris is north of the twomaria.
26
4Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
26
5N
ort
h
Pola
r R
egio
n
Lattitude Range Photo Number
75 N–90 N 190H3 176H3 164H3 152H1 140H3 128H1 116H3 104H1 092H3 080H1 068H3 165H1
60 N–75 N 190H2 176H2 164H2 152H1 140H2 128H1 116H2 104H1 092H2 080H1 068H2
50 N–60 N 190H1 176H1 164H1 152H1 140H1 128H1 116H1 104H1 092H1 080H1 068H1
27 N–56 N 189, 175, 163, 151, 175, 139, 127, 115, 103, 091, 079, 067, 055 165H2183 170 158 145 170 134 122 110 098 086 074 062
Longitude at 75 W 63 W 51 W 38 W 22 W 12 W 0 E/W 7 E 15 E 28 E 42 E 56 E 66 E 85 E50 N
Table 11.1. The cells shown in white represent the high-resolution Lunar Orbiter photos of the North Polar Region (LO4-XXX H1, -H2, and -H3, whereXXX is the Photo Number). The shaded cells within the North Polar Region represent photos that are not printed in this chapter because of redundancy; theyare included in the CD. South of this region are the Imbrium Basin Region, the Serenitatis Basin Region, and the Eastern Basins Region. Exposure 165H1 wastaken from apolune in afternoon sun. The apolune photo was taken at about twice the altitude of perilune photos, so it has about half the resolution and fourtimes the area of coverage.
Figure 11.3. North Pole (USGS Astrogeology, PIA00002, NASA). This mosaic covers the North Polar Region within 10° of the pole. The near side is in thelower half of the photo.
Bec
ause
of
the
desi
gn o
f Lu
nar
Orb
iter
Mis
sion
4,
the
spac
ecra
ft o
rbit
was
tilt
ed s
light
ly t
owar
d th
e ea
st o
f th
e N
orth
Pol
e. A
s a
resu
lt, h
igh-
reso
luti
onph
otos
of
the
wes
tern
par
t of
the
Nor
th P
olar
Reg
ion
are
not
avai
labl
e. T
hem
ediu
m-r
esol
utio
n ph
oto
abov
e is
pro
vide
d to
fill
in t
his
area
and
sho
w t
helo
cati
on o
f th
e na
med
fea
ture
s w
ithi
n it
. T
he m
are
surf
ace
of n
orth
ern
Oce
anus
Pro
cella
rum
is d
omin
ated
by
the
ray
patt
ern
of a
sm
all c
rate
r so
uth
ofPy
thag
oras
(LO
4-19
0H1)
. T
he s
ubdu
ed n
atur
e of
the
top
ogra
phy
near
the
wes
tern
sho
re o
f O
cean
us P
roce
llaru
m m
ay b
e du
e to
an
oute
r tr
ough
of
the
prop
osed
Lav
oisi
er-M
aira
n B
asin
.LO4-
189
MSu
n El
evat
ion:
18.
4°A
ltit
ude:
287
7.87
km
26
6Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
The
mar
e in
the
low
er p
art
of t
his
phot
o flo
ods
two
larg
ecr
ater
s, o
ne b
etw
een
Oen
opid
es a
nd R
epso
ld a
nd a
noth
er to
the
sout
heas
t of
Rep
sold
. Py
thag
oras
is
an e
xam
ple
of a
youn
g Er
atos
then
ian
crat
er; t
here
is d
etai
led,
sha
rply
del
in-
eate
d st
ruct
ure
in i
ts c
rate
r w
all a
nd e
ject
a bl
anke
t, bu
t th
era
y st
ruct
ure
has
been
sup
pres
sed
by a
com
bina
tion
of
gard
enin
g by
met
eor
impa
cts
and
dark
enin
g by
the
sol
arw
ind.
The
ray
s in
this
are
a, e
xten
ding
into
nor
ther
n O
cean
usPr
ocel
laru
m, a
re d
ue t
o a
smal
l cr
ater
on
the
nort
h ri
m o
fO
enip
edes
. N
ote
the
seco
ndar
y fie
ld o
f Py
thag
oras
in
the
vici
nity
of O
enop
ides
.
LO4-
190H
1Su
n El
evat
ion:
13.
5°A
ltit
ude:
337
8.38
km
26
7N
ort
h
Pola
r R
egio
n
Pyth
agor
as h
as s
prea
d it
s ej
ecta
bla
nket
to
the
wes
t an
dno
rth
as w
ell
as t
o th
e so
uth
(LO
4-19
0H1)
. In
the
nort
hern
lati
tude
s, a
bove
70°
from
the
equ
ator
, th
e te
rrai
n be
com
escl
earl
y hi
ghla
nd, w
ith
crat
ers
of e
very
siz
e ov
erla
ppin
g.
LO4-
190H
2Su
n El
evat
ion:
13.
5°A
ltit
ude:
337
8.38
km
26
8Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
Thi
s is
the
wes
tern
app
roac
h to
the
Nor
th P
ole.
Her
mit
e,de
eply
sha
dow
ed i
n th
is p
ictu
re,
is a
bout
to
have
its
floo
rill
umin
ated
wit
h su
nlig
ht. N
ear
the
Nor
th P
ole,
the
sun
does
not i
llum
inat
e pa
rts
of c
rate
r flo
ors
duri
ng e
ntir
e lu
nar
rota
-ti
ons
(mon
ths)
. H
owev
er,
the
sun
illum
inat
es m
ore
of t
heflo
ors
over
a y
ear’
s ti
me
beca
use
of t
he s
ligh
t ti
lt o
f th
eM
oon’
s ax
is r
elat
ive
to th
e ec
lipti
c pl
ane.
You
ng, s
harp
, sm
all
crat
ers
near
the
pol
e ha
ve m
ore
of t
heir
floo
rs p
erm
anen
tly
dark
bec
ause
the
y ar
e re
lati
vely
dee
p an
d th
eir
floor
s ar
em
ore
shad
ed b
y th
eir
rim
s th
an t
he fl
oors
of
old,
deg
rade
d,la
rge
crat
ers.
LO4-
190H
3Su
n El
evat
ion:
13.
5°A
ltit
ude:
337
8.38
km
26
9N
ort
h
Pola
r R
egio
n
The
anc
ient
cra
ter
Bab
bage
has
influ
ence
d th
e fo
rmat
ion
ofth
e Py
thag
oras
cra
ter
in th
is a
rea.
cra
ter
Sout
h, a
ltho
ugh
rel-
ativ
ely
degr
aded
in
com
pari
son
to B
abba
ge, i
s ne
vert
hele
ssyo
unge
r, b
ecau
se a
sec
tor
of it
s w
all t
rave
rses
Bab
bage
. Sin
usR
oris
has
thi
nly
flood
ed t
his
regi
on, l
eavi
ng t
race
s of
cra
ter
wal
ls s
uch
as t
hat
sout
heas
t of
Mar
kov.
Sec
onda
ry c
rate
rsfr
om P
ytha
gora
s ha
ve f
alle
n on
muc
h of
thi
s ar
ea.
A m
are
unit
(so
uth
of c
rate
r So
uth)
has
floo
ded
part
of t
he s
econ
dary
field
of P
ytha
gora
s, s
how
ing
that
that
mar
e un
it fo
rmed
late
r.B
oth
Pyth
agor
as a
nd t
he m
are
unit
are
ass
igne
d to
the
Erat
osth
enia
n Pe
riod
.
27
0Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
176H
1Su
n El
evat
ion:
12.
8°A
ltit
ude:
335
3.98
km
The
are
a no
rth
of M
are
Frig
oris
, suc
h as
the
floor
s of
cra
ters
Sout
h an
d J.
Her
sche
l, is
hea
vily
cov
ered
wit
h ej
ecta
from
the
Imbr
ium
Bas
in t
o th
e ea
st-s
outh
east
. In
par
ticu
lar,
rid
ges
and
valle
ys i
n th
e cr
ater
wal
l of
J.
Her
sche
l po
int
to t
hece
nter
of
the
Imbr
ium
Bas
in. T
he c
rate
r ch
ain
in t
he s
outh
-ea
ster
n flo
or o
f cr
ater
Sou
th i
s lik
ely
to b
e fo
rmed
by
sec-
onda
ry i
mpa
ctor
s fr
om a
cra
ter
that
has
bee
n flo
oded
by
Sinu
s Ir
idum
(to
the
sout
heas
t).
LO4-
164H
1Su
n El
evat
ion:
12.
9°A
ltit
ude:
334
5.81
km
27
1N
ort
h
Pola
r R
egio
n
The
int
eres
ting
hig
hlan
d pl
ains
bet
wee
n J.
Her
sche
l an
dA
naxi
men
es h
ave
a m
ottl
ed a
ppea
ranc
e be
caus
e th
ey h
ave
been
ove
rlai
n w
ith
rays
fro
m C
oper
nica
n cr
ater
s C
arpe
nter
and
Philo
laus
. The
sm
ooth
app
eara
nce
of t
his
area
cou
ld b
edu
e to
unc
onso
lida
ted
ejec
ta f
rom
the
Im
briu
m B
asin
,sh
aken
dow
n an
d co
nsol
idat
ed b
y th
e la
ter
impa
cts
ofC
arpe
nter
and
Phi
lola
us,
whi
ch c
ould
hav
e be
en v
irtu
ally
sim
ulta
neou
s. O
r, s
ome
maj
or t
ecto
nic
even
t co
uld
have
occu
rred
in th
is a
rea
to s
hake
dow
n th
e ej
ecta
bla
nket
.
LO4-
164H
2Su
n El
evat
ion:
12.
9°A
ltit
ude:
334
5.81
km
27
2Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
164H
3Su
n El
evat
ion:
12.
9°A
ltit
ude:
334
5.81
km
27
3N
ort
h
Pola
r R
egio
n
The
hea
vy r
idge
s an
d va
lleys
sou
th o
f B
yrd
and
Gio
ja a
rera
dial
to
the
Imbr
ium
Bas
in,
part
of
its
oute
r de
posi
t. T
hecl
uste
r of
sha
rp c
rate
rs in
the
10-
to
15-k
m r
ange
of
diam
e-te
rs in
the
sou
ther
n pa
rt o
f th
is a
rea
coul
d ha
ve c
ome
from
Imbr
ium
. A
lter
nati
vely
, th
ey c
ould
hav
e be
en c
ause
d by
asa
lvo
of s
econ
dari
es fr
om th
e fa
r si
de c
rate
r R
ozhd
estv
ensk
iyco
min
g ov
er th
e N
orth
Pol
e.
The
rin
g of
the
Im
briu
m B
asin
tha
t bo
unds
Mar
e Im
briu
m p
asse
s be
twee
nBo
ugue
r an
d Bi
anch
ini.
Its
cros
shat
ched
cha
ract
er m
ay b
e du
e to
fine
-tex
ture
dej
ecta
fro
m t
he c
rate
r be
neat
h Si
nus
Ror
is o
verl
ying
the
coa
rser
rid
ges
and
valle
ys c
ause
d by
the
Imbr
ium
eve
nt. T
he d
ark
area
in th
e ea
ster
n pa
rt o
f Mar
eFr
igor
is i
n th
is p
hoto
is
typi
cal
mar
e m
ater
ial,
whi
ch h
as fl
oode
d an
out
er
27
4Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
152H
1Su
n El
evat
ion:
13.
0°A
ltit
ude:
339
4.33
km
trou
gh o
f the
Im
briu
m B
asin
. In
the
east
, Mar
e Fr
igor
is a
ppea
rs t
o ha
ve b
een
cove
red
wit
h a
laye
r of
lig
hter
ray
ed m
ater
ial,
prob
ably
fro
m C
oper
nica
ncr
ater
Ana
xago
ras
(LO
4-14
0H2)
. U
nder
neat
h th
is c
ould
be
ejec
ta f
rom
Philo
laus
, als
o C
oper
nica
n.
The
rin
g of
the
Im
briu
m B
asin
tha
t bo
unds
its
mar
e pa
sses
betw
een
La C
onda
min
e an
d M
aupe
rtui
s. R
imae
Mau
pert
isar
e ou
tflow
cha
nnel
s or
col
laps
ed la
va t
ubes
whe
re la
va h
asco
me
up t
hrou
gh t
he r
ing
and
flow
ed n
orth
int
o M
are
Frig
oris
and
sou
th in
to M
are
Imbr
ium
. Thi
s ty
pe o
f flow
sug
-ge
sts
that
upw
ellin
g la
va,
part
ially
blo
cked
by
mel
t sh
eets
and
earl
ier
lava
flow
s (n
ow h
arde
ned)
, can
find
its
way
up
thro
ugh
the
frac
ture
d ri
ng m
ater
ial a
nd th
en d
ownh
ill.
LO4-
140H
1Su
n El
evat
ion:
12.
5°A
ltit
ude:
335
5.14
km
27
5N
ort
h
Pola
r R
egio
n
Philo
laus
and
Ana
xago
ras
are
Cop
erni
can
crat
ers.
Ana
xa-
gora
s, i
n pa
rtic
ular
, ha
s im
pact
ed u
ncon
solid
ated
mat
eria
lon
the
rim
of
Gol
dsch
mid
t an
d ej
ecte
d pa
rtic
ular
ly m
assi
veflo
ws
of fi
nely
bro
ken
mat
eria
l th
at s
moo
ths
the
floor
of
Gol
dsch
mid
t an
d th
e ar
ea s
outh
of G
olds
chm
idt.
The
se r
ays
exte
nd to
Mar
e Fr
igor
is (
LO-1
52H
1). T
ecto
nic
forc
es a
nd th
esh
ock
of th
e im
pact
of A
naxa
gora
s m
ay a
lso
have
had
a p
art
in th
e le
velin
g of
the
plai
ns s
outh
of G
olds
chm
idt.
LO4-
140H
2Su
n El
evat
ion:
12.
5°A
ltit
ude:
335
5.14
km
27
6Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
The
rid
ges
that
com
e fr
om t
he s
outh
are
rad
ial
to t
heIm
briu
m B
asin
. O
ther
str
iati
ons
from
the
sou
th-s
outh
east
,fin
er in
text
ure,
are
rad
ial t
o th
e Se
reni
tati
s B
asin
. Mai
n an
dC
halli
s, t
wo
crat
ers
of a
ppro
xim
atel
y th
e sa
me
size
and
age
,co
uld
have
bee
n ca
used
by
near
ly s
imul
tane
ous
impa
cts.
Alt
houg
h M
ain
has
impi
nged
on
the
Cha
llis
rim
, the
eje
cta
blan
ket o
f Cha
llis
appe
ars
to h
ave
been
bet
ter
pres
erve
d. T
hear
ea i
mm
edia
tely
to
the
wes
t of
Mai
n an
d C
halli
s ha
s be
ende
pres
sed
and
smoo
thed
, wit
h al
l sig
ns o
f ej
ecta
fro
m M
ain
and
Cha
llis
eras
ed. T
ecto
nic
acti
on b
enea
th a
thi
ck u
ncon
-so
lidat
ed s
urfa
ce la
yer
coul
d be
the
cau
se. R
ober
t Pe
ary
led
an e
xped
itio
n of
50
Eski
mos
and
rea
ched
the
Nor
th P
ole
bydo
gsle
d in
190
9. R
icha
rd E
. B
yrd
flew
ove
r th
e N
orth
Pol
ew
ith
Floy
d B
enne
tt in
192
6. H
e la
ter
flew
ove
r th
e So
uth
Pole
in 1
929.
He
was
an
acti
ve e
xplo
rer
of A
ntar
ctic
a by
air
plan
esan
d do
gsle
ds fr
om 1
928
to 1
956.
LO4-
140H
3Su
n El
evat
ion:
12.
5°A
ltit
ude:
335
5.14
km
27
7N
ort
h
Pola
r R
egio
n
Thi
s ar
ea o
f M
are
Frig
oris
is
rich
in
ridg
es a
nd s
carp
s(p
erha
ps t
he e
dges
of
flow
s).
Its
surf
ace
expr
essi
on i
spi
nche
d be
twee
n th
e ej
ecta
of P
lato
and
the
hig
hlan
d pe
nin-
sula
nor
th o
f it
. Bot
h Pl
ato
and
the
Irid
um c
rate
r ar
e da
ted
in t
he U
pper
Im
bria
n Ep
och.
The
sec
onda
ry fi
eld
of P
lato
seem
s to
ove
rlie
the
Iri
dum
eje
cta,
esp
ecia
lly t
o th
e no
rth-
east
, but
str
iati
ons
from
Iri
dum
see
m t
o ov
erlie
Pla
to e
ject
aju
st t
o th
e no
rth
and
sout
h of
its
rim
. Pla
to’s
floo
r ha
s be
enflo
oded
wit
h m
are
mat
eria
l, up
wel
ling
thro
ugh
the
brok
enm
ater
ial o
f the
mai
n ri
ng o
f the
Imbr
ium
Bas
in.
LO4-
128H
1Su
n El
evat
ion:
11.
7°A
ltit
ude:
336
9.17
km
27
8Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
Just
to
the
east
of
Plat
o th
ere
is m
ore
evid
ence
of
lava
up-
wel
ling
thro
ugh
the
brok
en m
ater
ial o
f th
e m
ain
ring
of
the
Imbr
ium
Bas
in.
Rim
ae P
lato
dra
in p
ools
of
dark
lav
a in
tola
rger
cha
nnel
s su
ch a
s V
allis
Alp
es. V
allis
Alp
es m
ay b
e a
stre
ss c
rack
rad
ial t
o th
e Im
briu
m B
asin
that
has
bee
n ne
arly
fille
d w
ith
lava
. A la
va c
hann
el r
uns
thro
ugh
its
cent
er. T
heno
rthe
rn p
art
of R
imae
Pla
to s
eem
s to
dis
appe
ar a
nd r
e-ap
pear
; it
is p
roba
bly
a ch
anne
l in
som
e se
ctor
s an
d an
un-
derg
roun
d tu
be in
oth
ers.
Gar
deni
ng b
y im
pact
ors
may
hav
ebr
oken
thro
ugh
the
roof
of t
he tu
bes
in s
ome
sect
ors,
leav
ing
chan
nels
.
LO4-
116H
1Su
n El
evat
ion:
11.
6°A
ltit
ude:
339
6.94
km
27
9N
ort
h
Pola
r R
egio
n
The
coa
rse
ridg
es i
n th
is p
hoto
are
rad
ial
to t
he I
mbr
ium
Basi
n. T
he e
ject
a bl
anke
t of t
he Im
briu
m B
asin
cha
nges
cha
r-ac
ter
betw
een
W. B
ond
and
Met
on, s
hift
ing
from
the
thi
ckFr
a M
auro
For
mat
ion
to t
hinn
er o
uter
dep
osit
s. C
oper
nica
ncr
ater
Ana
xago
ras
send
s it
s ra
ys a
cros
s Pr
e-N
ecta
rian
Gol
dsch
mid
t, W
. Bon
d, B
arro
w, a
nd M
eton
. The
cra
ter
wal
lof
Bar
row
is
mor
e po
lygo
nal
than
cir
cula
r. I
t ha
s be
enst
rong
ly i
nflue
nced
by
pree
xist
ing
stru
ctur
es i
n it
s ta
rget
area
. For
exa
mpl
e, t
he c
rate
r w
all
seem
s to
be
furt
her
from
the
cent
er w
here
it p
enet
rate
s th
e br
oken
mat
eria
l of t
he r
imof
Gol
dsch
mid
t. R
ima
W. B
ond
runs
nea
rly
acro
ss c
rate
r W
.B
ond,
sug
gest
ing
uplif
t pr
essu
re b
enea
th a
mel
t sh
eet
unde
rit
s flo
or.
LO4-
116H
2Su
n El
evat
ion:
11.
6°A
ltit
ude:
339
6.94
km
28
0Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
The
low
sun
ele
vati
on o
f th
is p
hoto
nea
r th
e te
rmin
ator
at
the
pole
sho
ws
that
the
floor
of B
yrd
is v
ery
flat.
LO4-
116H
3Su
n El
evat
ion:
11.
6°A
ltit
ude:
339
6.94
km
28
1N
ort
h
Pola
r R
egio
n
The
eje
cta
from
Era
tost
heni
an c
rate
r A
rist
otel
es h
ave
been
laid
dow
n in
two
phas
es, s
epar
ated
by
only
min
utes
. The
firs
tph
ase
cons
iste
d of
fine
ly d
ivid
ed m
ater
ial
ejec
ted
at a
ver
ylo
w a
ngle
. T
his
form
atio
n ha
s sm
ooth
rad
ial
ridg
es a
ndtr
ough
s. S
ubse
quen
tly,
cha
ins
and
loop
s of
sm
all s
harp
sec
-on
dary
cra
ters
for
m f
rom
im
pact
ors
that
hav
e be
en t
hrow
nhi
gh a
bove
the
sur
face
and
land
aft
er t
he in
itia
l bla
nket
has
sett
led.
The
mar
e to
the
nor
th, s
till
part
of
Mar
e Fr
igor
is, i
sno
long
er in
the
Imbr
ium
trou
gh th
at li
es o
utsi
de o
f its
mai
nri
ng.
The
dep
ress
ion
that
has
bee
n flo
oded
to
form
the
east
ern
part
of
Mar
e Fr
igor
is m
ay h
ave
been
for
med
by
the
inte
rsec
tion
of t
he s
econ
d ou
ter
trou
ghs
of th
e Im
briu
m a
ndSe
reni
tati
s B
asin
s. O
f co
urse
, th
ese
circ
les
inte
rsec
t at
tw
opo
ints
; th
e ot
her
inte
rsec
tion
is
at S
inus
Med
ii,
anot
her
flood
ed d
epre
ssio
n.
LO4-
104H
1Su
n El
evat
ion:
12.
2°A
ltit
ude:
342
7.64
28
2Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
Seve
ral c
lues
sug
gest
that
this
are
a of
Mar
e Fr
igor
is is
rel
ativ
ely
shal
low
. The
sein
dica
tion
s in
clud
e th
e pr
ojec
ting
rim
of
Gar
tner
and
its
fain
t co
mpa
nion
to
the
nort
hwes
t, th
e pr
esen
ce o
f so
man
y m
are
ridg
es, s
ome
wit
h ci
rcul
ar s
truc
-tu
re s
ugge
stin
g un
derl
ying
cra
ter
rim
s, a
nd t
he c
once
ntri
c pa
tter
n of
Gal
le,
28
3N
ort
h
Pola
r R
egio
n
LO4-
092H
1Su
n El
evat
ion:
12.
2°A
ltit
ude:
345
7.15
sugg
esti
ng t
hat
it h
as b
otto
med
out
int
o a
laye
r be
neat
h th
e m
are
mat
eria
l.T
he m
ajor
ity
of fl
ow s
carp
s dr
op t
owar
d th
e no
rthw
est,
sugg
esti
ng t
hat
this
area
was
floo
ded
from
the
sout
heas
t.
The
floo
rs o
f Met
on a
nd it
s si
mila
r co
mpa
nion
s ar
e no
t inh
eren
tly d
arke
r th
anth
e su
rrou
ndin
g m
ater
ial (
see
Figu
re 1
.3);
they
are
just
clo
ser
to th
e te
rmin
ator
.
28
4Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
092H
2Su
n El
evat
ion:
12.
2°A
ltit
ude:
345
7.15
28
5N
ort
h
Pola
r R
egio
n
LO4-
092H
3Su
n El
evat
ion:
12.
2°A
ltit
ude:
345
7.15
The
clu
ster
of s
econ
dary
cra
ters
eas
t of B
yrd
and
Pear
y m
ay in
clud
e im
pact
ors
from
eac
h of
the
Im
briu
m a
nd H
umbo
ldti
anum
Bas
ins;
the
pol
e is
abo
uteq
uidi
stan
t fro
m th
e ce
nter
of e
ach
basi
n, r
elat
ive
to th
eir
size
s. T
he la
rger
sec
-on
dari
es a
re li
kely
to b
e fr
om Im
briu
m a
nd th
e sm
alle
r fr
om H
umbo
ldti
anum
.C
ontr
ibut
ions
may
als
o ha
ve c
ome
over
the
pol
e fr
om f
ar s
ide
crat
erR
ozhd
estv
ensk
iy.
The
nor
thea
ster
n sh
ore
of M
are
Frig
oris
is
boun
ded
by a
high
land
pla
ins
unit
, fo
rmed
by
a du
sty
cove
ring
of
ejec
tafr
om t
he H
umbo
ldti
anum
Bas
in. D
e La
Rue
is ju
st o
utsi
de a
ring
of
Hum
bold
tian
um, p
roba
bly
the
mai
n ri
ng; t
hat
puts
this
are
a in
an
exte
rnal
trou
gh o
f the
bas
in. T
hat i
mpa
ct m
ayha
ve e
ssen
tial
ly l
evel
ed t
he h
ighl
and
mat
eria
l in
thi
s ar
eash
ortl
y be
fore
dep
osit
ion
of t
he p
ulve
rize
d ej
ecta
, w
hich
furt
her
smoo
thed
the
are
a. D
ark
man
tlin
g m
ater
ial,
ofte
nse
en n
ear
the
shal
low
edg
es o
f m
aria
, no
t on
ly c
over
s th
ispa
rt o
f Mar
e Fr
igor
is b
ut a
lso
dark
ens
the
near
by h
ighl
ands
.
28
6Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
080H
1Su
n El
evat
ion:
13.
0°A
ltit
ude:
347
9.03
Endy
mio
n an
d D
e La
Rue
are
just
out
side
the
650
km
mai
nri
ng o
f th
e H
umbo
ldti
anum
Bas
in,
in t
he fi
rst
exte
rnal
trou
gh (
see
LO4-
165H
1). B
oth
are
olde
r th
an t
hat
basi
n, b
utD
e La
Rue
mus
t be
old
er t
han
Endy
mio
n, j
udgi
ng b
y th
ere
lati
ve d
egre
e of
deg
rada
tion
. En
dym
ion
is c
lass
ified
as
Nec
tari
an. T
he b
righ
tnes
s co
veri
ng D
e La
Rue
, Str
abo,
and
the
surr
ound
ing
area
is
the
resu
lt o
f th
e fr
esh
ejec
ta f
rom
Cop
erni
can
crat
er T
hale
s (L
O4-
165H
1).
LO4-
068H
1Su
n El
evat
ion:
11.
5°A
ltit
ude:
348
7.74
28
7N
ort
h
Pola
r R
egio
n
The
mai
n ri
ng o
f th
e H
umbo
ldti
anum
Bas
in (
LO4-
165H
1)cr
osse
s di
agon
ally
acr
oss
the
low
er r
ight
cor
ner
of th
is p
hoto
,so
uth
of C
usan
us a
nd e
ast
of S
chw
abe.
Rad
ial
ridg
es a
ndva
lleys
of e
ject
a pa
ss b
etw
een
Baill
aud
and
Pete
rman
n. T
here
are
clus
ters
of
smal
l se
cond
arie
s on
the
floo
r of
Pet
erm
ann
and
the
very
deg
rade
d gr
oup
of t
hree
cra
ters
of
sim
ilar
size
to th
e w
est o
f Pet
erm
ann.
28
8Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
068H
2Su
n El
evat
ion:
11.
5°A
ltit
ude:
348
7.74
The
are
a of
the
righ
t sid
e of
this
pho
to is
dom
inat
ed b
y ej
ecta
from
the
Hum
bold
tian
um B
asin
. Som
e ri
dges
, at r
ight
ang
les
to t
hose
fro
m H
umbo
ldti
anum
, ar
e ra
dial
to
the
Imbr
ium
Bas
in. F
ridt
jof N
anse
n al
low
ed h
is s
peci
ally
con
stru
cted
shi
pFr
amto
be
froz
en in
to p
olar
ice
near
Sib
eria
in 1
993,
inte
nd-
ing
to d
rift
wit
h th
e ic
e to
war
d G
reen
land
. As
Fram
mad
e it
scl
oses
t ap
proa
ch t
o th
e po
le, N
anse
n an
d a
com
pani
on l
eft
the
ship
by
dogs
led
and
reac
hed
86°
13’
nort
h la
titu
de.
Nan
sen’
s le
ader
ship
in
prog
ram
s to
rep
atri
ate
pris
oner
s of
war
aft
er W
orld
War
I a
nd r
elie
f of
fam
ine
resu
lted
in
his
rece
ivin
g th
e N
obel
Pea
ce P
rize
in 1
922.
LO4-
068H
3Su
n El
evat
ion:
11.
5°A
ltit
ude:
348
7.74
28
9N
ort
h
Pola
r R
egio
n
The
rin
ged
stru
ctur
e of
the
Hum
bold
tian
um B
asin
can
cle
arly
be
seen
in t
his
apol
une
phot
o ta
ken
near
the
end
of
the
mis
sion
. M
are
Hum
bold
tian
umne
arly
fills
a r
ing
that
may
be
an in
ner
ring
. The
nex
t ri
ng is
sub
dued
in t
his
sect
or, b
ut t
he r
ing
afte
r th
at, r
unni
ng ju
st e
ast
of t
he r
ims
of D
e La
Rue
and
29
0Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
165H
1Su
n El
evat
ion:
13.
9°A
ltit
ude:
548
6.51
Stra
bo, m
ay b
e th
e m
ain
ring
. Mar
e pa
rtly
floo
ds t
he a
rea
betw
een
the
ring
boun
ding
the
mar
e an
d th
e m
ain
ring
. Rad
ial r
idge
s an
d va
lleys
, suc
h as
thos
ecr
ossi
ng th
e ri
m o
f Str
abo
and
both
nor
th a
nd s
outh
of M
are
Hum
bold
tian
um,
are
radi
al to
this
rin
ged
basi
n.
12.1. OverviewThe near side South Polar Region covers the area betweenabout 55° south latitude and the South Pole and between thewestern and eastern limbs.
The region is entirely highlands. On a large scale, itstopography records the early over-cratered bombardment ofthe Moon after the crust formed. The entire South PolarRegion is within one diameter of the main ring of the SouthPole–Aiken Basin on the far side, so it has been essentiallycovered with ejecta from that basin. However, that ejecta hasbeen so degraded by further bombardment that it is difficultto identify specific features such as ridges and secondarycraters that might have been due to the South Pole–Aikenimpact.
Western Sector of the South PolarRegionThe Bailly Basin, unflooded by mare, is within this sector,toward the western limb (Figure 12.1). The lack of mareflooding is an indicator of a relatively thick crust in this area.
Central Sector of the South PolarRegionFigure 12.2 shows the central part of the near side SouthPolar Region. The highlands here are a continuation of thenear side central highlands, a feature that reaches all the wayto the lunar equator.
Eastern Sector of the South PolarRegionFigure 12.3 shows the eastern limb of the Moon, includingthe eastern edge of the near side South Polar region. Thesouthern part of the Australe Basin is in this sector.
The South PoleThe best parts of the photos taken near the South Pole oneach of the orbits of Clementine have been carefully assem-bled and are shown in Figure 12.4.
As can be seen from Figure 12.4, the sun is rarely seen atthe floors of craters that are deep relative to their sizebecause the lunar axis is inclined by only 1.5° relative to theplane of its travel around the sun. More of this permanentlyshadowed area is near the South Pole than near the North
Pole. As the surface is radiating heat to deep space andbecause the dusty surface (gardened by small meteorites) is areasonably good insulator against thermal conductivity, thetemperature at the floors of these craters is near absolutezero, as low as 40 degrees Kelvin. The surface dust at suchcold ambient temperatures is a good trap for volatiles suchas hydrogen that arrive there by chance. Hydrogen is avail-able from the solar wind, in the form of ionized protons.Such protons that impact in sunlit areas on the Moon arelikely to be neutralized and thermally excited into the space
29
1So
uth
Pola
r R
egio
n
Chapter 12
South Polar Region
Figure 12.1. Western Sector of the South Polar Region (LO4-193M). Thewhite dashed line marks the western limb, the meridian at 90° degrees westlongitude. The Bailly ringed basin is in the center of this photo, in the north-ern part of the South Polar Region. The 90° meridian runs through the craterHausen, adjacent to Bailly. The Orientale Basin is to the north, near thevisible edge of the Moon in this photo. Ridges of Orientale ejecta can be seenreaching all the way to the edge of the South Polar Region.
around the Moon. If they do not escape, they “hop” fromplace to place (landing and being reemitted).
The Lunar Prospector Mission carried instruments todetect concentrations of hydrogen and found them near eachof the poles. The hydrogen, perhaps combined with oxygen(plentiful in the minerals of the lunar surface) in the form ofice, is likely to have been trapped at or near the surface ofthese permanently shadowed areas.
The nature of these concentrations of hydrogen andperhaps of ice is of great interest. If sufficiently rich concen-trations of suitable materials can be found in the low gravityof the Moon, they might provide a useful source of rocketfuel or propellant, rather than lifting supplies from Earth.
Another special characteristic of this region near the poleis its location near the South Pole–Aiken Basin. Rocks scat-tered here could be the deepest ever excavated from the crust(and possibly from the upper mantle of the Moon). An expe-dition to gather these rocks could also establish the age ofthe oldest lunar basin and help determine whether basinbombardment was continuous from the time of thesolidification of the crust or whether there was a separate,later event of basin bombardment.
12.2. High-Resolution ImagesThe Lunar Orbiter photos of the South Polar Region (Table12.1), like those of the North Polar Region, have a highdegree of overlap because they were taken from a near polarorbit. The rectangular sets of three subframes in a high-reso-lution exposure taken at perilune have the pole in or near thebottom of the southern subframe (designated H1). The illu-mination angle in the more northern subframes (H2 and H3)is about 10°, but the angle approaches 0 toward the pole. Ofcourse, the pole is always within 1.5° of the terminator. Theactual South Pole was in shadow during this mission.
Although the polar photos were not taken on every orbitover the poles, there is still so much overlap in the middleand southern subframes that only every other photo isshown here.
After an early success (LO4-005H1, -H2, and -H3). theplanned high-resolution photos of the eastern South PolarRegion were spoiled by the failure of the thermal door. Nearthe end of the mission, apolune photos were taken of thatarea. One subframe of these (LO4-184H3) is presented nearthe end of this chapter to provide complete coverage of thenear side South Polar Region. Table 12.1 shows the high-reso-lution images of the South Polar Region in schematic form.
The following pages show the high-resolution subframesfrom south to north and west to east. The photos are in theorder LO4-193H1, LO4-193H2, LO4-193H3, LO4-179H3,LO4-186H1, LO4-186H2, …. After LO4-184H3, an apolunephoto, are LO4-005H1, LO4-005H2, and LO4-005H3.
29
2Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
Figure 12.2. Central South Polar Region (LO4-106M). The dashed line isthe zero meridian. The small dark area in the upper left corner of thispicture is Mare Nubium, in the floor of the Nubium Basin. The very sharpcrater south of Mare Nubium is Tycho, which spreads its rays preferentiallyto the east, over the southern part of the near side central highlands. Thelarge crater Clavius is directly to the south of Tycho, just within the SouthPolar Region. The bright area southeast of the center of the photo is due tothe ejecta of Copernican crater Stevinus. The dark splotchy area in the lowerright is the western portion of Mare Australe. The shadowed floor of thesmall far side Schrodinger Basin is below and to the right of the South Pole.
Figure 12.3. Eastern South Polar Region (LO4-008M). The dashed line isthe eastern limb, the 90° east meridian. Mare Australe is in the upper left.The smaller Schrodinger Basin is below it, with deep valleys runningbetween it and the Australe Basin.
Lattitude Range Photo Number
27 S–56 S N 194, 180, 167, 155, 142, 124, 112, 100, 188, 076, 064, 076, 184H1, 178H1, 009186 172 160 148 136, 119 107 095 083 071 059 071 H2 H2
131
55S–65S 193H3 179H3 166H3 154H3 130H3 118H3 106H3 094H3 082H3 070H3 058H3 044H3 184H3 178H3 005H3
65 S–75 S 193H2 179H2 166H2 154H2 130H2 118H2 106H2 094H2 082H2 070H2 058H2 044H2 005H2
75 S–90 S 193H1 179H1 166H1 154H1 130H1 118H1 106H1 094H1 082H1 070H1 058H1 044H1 005H1
Longitude 90 W, 70 W 60 W, 50 W, 40 W, 10 W 0 E/W, 20 E 30 E 40 E 50 E 60 E 50 E, 60 E, 80 E, at 50 S 80 W 50 W 40 W 30 W, 10 E 70 E 90 E
20 W
Table 12.1. The cells shown in white represent the high-resolution photos of the South Polar Region that are printed in this chapter (LO4-XXX H1, -H2, and-H3, where XXX is the Photo Number). The shaded cells within the South Polar Region represent photos that are not shown in this chapter because of redun-dancy; however, they are in the included CD. North of this region are the Orientale Basin Region, the Humorum Basin Region, the Nectaris Basin Region, andthe Eastern Basin Region. Exposure 184H3 was taken from apolune in afternoon sun.
Figure 12.4. South Pole (USGS Astrogeology PIA00002, NASA). This mosaic covers the South Polar Region within 10° of the pole. The near side is in theupper half of the photo. Crater Shoemaker, near the pole, was in shadow throughout the Lunar Orbiter 4 and Clementine Missions.
29
3So
uth
Pola
r R
egio
n
Dry
gals
ki is
a P
re-N
ecta
rian
cra
ter
(149
km
dia
met
er).
It h
asa
stro
ng c
entr
al p
eak
and
a w
ell-
defin
ed r
im, a
ltho
ugh
it h
asbe
en d
egra
ded
by d
epos
its
from
sub
sequ
ent
impa
cts.
It
has
been
cov
ered
wit
h ej
ecta
fro
m t
he B
ailly
Bas
in (
LO4-
193H
2,LO
4-17
9H3)
, who
se m
ain
ring
pas
ses
just
to th
e no
rthe
ast o
fLe
Gen
til.
Stri
atio
ns n
ear
Dry
gals
ki t
hat
com
e fr
om t
heno
rthe
ast
are
radi
al t
o B
ailly
. D
ryga
lski
has
im
pact
edbr
oade
r ri
dges
and
val
leys
at
righ
t an
gles
to
thos
e fr
omB
ailly
; th
ey a
re r
adia
l to
the
Sou
th P
ole–
Aik
en B
asin
.D
ryga
lski
is o
n th
e to
pogr
aphi
c ri
ng o
f tha
t bas
in.
LO4-
193H
1Su
n El
evat
ion:
9.3
°A
ltit
ude:
351
9.21
km
29
4Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
Hau
sen
is a
wel
l-fo
rmed
cra
ter
wit
h a
rugg
ed c
entr
al p
eak,
asu
gges
tion
of
an i
nner
rin
g, a
nd a
wel
l-pr
eser
ved
ejec
tabl
anke
t. I
t is
the
lar
gest
cra
ter
(167
km
) of
eit
her
the
Erat
osth
enia
n Pe
riod
or
the
Cop
erni
can
Peri
od. O
nly
Hum
-bo
ldt
(207
km
, Lat
e Im
bria
n) is
larg
er a
mon
g im
pact
eve
nts
afte
r O
rien
tale
. T
he e
ject
a of
Hau
sen,
whi
ch o
verl
ies
the
mai
n ri
ng a
nd fl
oor
of th
e B
ailly
Bas
in, s
how
s a
herr
ingb
one
patt
ern,
esp
ecia
lly t
o th
e no
rth.
Thi
s pa
tter
n re
sult
s fr
omla
tera
l ve
loci
ty i
mpa
rted
to
the
edge
s of
a t
ongu
e of
eje
cta
duri
ng la
ndin
g. O
utsi
de o
f the
Hau
sen
ejec
ta, t
o th
e no
rth
ofB
ailly
, is
a he
avy
clus
ter
of O
rien
tale
sec
onda
ries
that
hel
p to
esta
blis
h th
e se
quen
ce a
s fir
st B
ailly
, th
en O
rien
tale
, th
enH
ause
n.
LO4-
193H
2Su
n El
evat
ion:
9.3
°A
ltit
ude:
351
9.21
km
29
5So
uth
Pola
r R
egio
n
Thi
s ar
ea i
s co
vere
d w
ith
the
scul
pted
rid
ges
and
valle
ys(s
uch
as V
allis
Baa
de)
of t
he I
nner
Hev
eliu
s Fo
rmat
ion,
the
heav
y ej
ecta
bla
nket
fro
m t
he O
rien
tale
Bas
in. M
any
of t
hecr
ater
s su
ch a
s C
atal
an a
re c
ause
d by
obj
ects
thr
own
high
from
Ori
enta
le t
hat
subs
eque
ntly
fel
l on
the
fre
sh e
ject
abl
anke
t of O
rien
tale
(th
e ej
ecta
bla
nket
follo
wed
a fa
ster
pat
hat
a lo
w in
clin
atio
n to
the
surf
ace)
. The
flat
ness
of t
he te
rrai
nin
the
low
er l
eft
of t
his
phot
o re
sult
s fr
om i
ts f
orm
atio
n as
the
floor
of
the
anci
ent
Men
del-
Ryd
berg
Bas
in, w
hich
con
-ti
nues
wes
t in
to t
he f
ar s
ide.
The
mai
n ri
ng o
f th
is b
asin
is
nort
h of
Gut
hnic
k an
d ea
st o
f Yak
ovki
n; th
e ea
ster
n se
ctor
of
this
rin
g ca
n be
see
n in
LO
4-17
9H3.
29
6Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
193H
3Su
n El
evat
ion:
9.3
Alt
itud
e: 3
519.
21 k
m
Hea
vy c
lust
ers
of O
rien
tale
sec
onda
ry c
rate
rs d
omin
ate
this
area
. The
mai
n ri
ng o
f the
Med
el-R
ydbe
rg B
asin
can
be
seen
ente
ring
thi
s ph
oto
from
the
upp
er l
eft
corn
er,
curl
ing
arou
nd P
ingr
e, a
nd i
nter
sect
ing
the
mai
n ri
ng o
f th
e B
ailly
Bas
in (
the
Bai
lly B
asin
has
obl
iter
ated
the
old
er r
ing)
.A
ltho
ugh
the
ring
s of
the
Men
del-
Ryd
berg
Bas
in a
re m
uch
degr
aded
, th
e de
pres
sion
of
its
floor
is
very
cle
ar i
n th
eC
lem
enti
ne e
leva
tion
dat
a.
LO4-
179H
3Su
n El
evat
ion:
7.1
°A
ltit
ude:
359
1.83
km
29
7So
uth
Pola
r R
egio
n
As
is t
ypic
al i
n th
e ph
otos
of
this
mis
sion
tha
t co
ver
the
Sout
h Po
le,
not
only
the
pol
e it
self
but
muc
h of
the
sur
-ro
undi
ng t
erri
tory
is
in s
hado
w,
som
e of
it
in p
erm
anen
tsh
adow
, exp
osed
to th
e co
ld o
f dee
p sp
ace
wit
hout
hea
t fro
mth
e su
n. T
his
is o
ne o
f the
bet
ter
view
s of
Mal
aper
t, sh
owin
git
to b
e of
a c
haot
ic fo
rm. I
t is
not c
lear
whe
ther
it is
a c
rate
rw
hose
wal
ls w
ere
push
ed a
side
by
othe
r im
pact
s or
sim
ply
ach
ance
arr
ange
men
t of d
ebri
s fr
om m
ulti
ple
impa
cts.
LO4-
166H
1Su
n El
evat
ion:
7.0
°A
ltit
ude:
359
2.60
km
29
8Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
Thi
s is
the
mos
t co
mpl
ete
view
of
Bai
lly, j
ust
big
enou
gh a
t30
0 km
to fo
rm a
mul
ti-r
inge
d ba
sin.
An
oute
r ri
ng r
uns
near
the
righ
t ed
ge o
f thi
s ph
oto
and
into
Le
Gen
til;
sect
ors
of a
nin
ner
ring
are
als
o vi
sibl
e. S
econ
dari
es fr
om O
rien
tale
dom
i-na
te t
he r
egio
n, b
ut e
arlie
r cr
ater
s ha
ve b
een
cove
red
wit
h a
mor
e un
ifor
m p
ulve
rize
d m
ater
ial,
prob
ably
als
o pa
rt o
fO
rien
tale
eje
cta.
LO4-
166H
2Su
n El
evat
ion:
7.0
°A
ltit
ude:
359
2.60
km
29
9So
uth
Pola
r R
egio
n
The
cha
ins
of s
econ
dari
es a
re r
adia
l to
Ori
enta
le. T
he h
eavy
ejec
ta b
lank
et s
eem
s to
end
at
a ri
dge
that
is
runn
ing
from
the
east
ern
edge
of P
hocy
lides
dow
n to
the
nort
hern
edg
e of
Zuc
chiu
s. T
his
is a
sec
tor
of t
he m
ain
ring
of
the
Schi
ller-
Zuc
chiu
s B
asin
. Pl
ains
uni
ts h
ave
been
for
med
by
the
pow
dery
out
er H
evel
ius
Form
atio
n of
Ori
enta
le c
over
ing
flat
crat
er fl
oors
suc
h as
tho
se o
f Ph
ocyl
ides
, W
arge
ntin
, an
dN
asm
yth
and
the
floor
of
the
Schi
ller-
Zuc
chiu
s B
asin
(L
O4-
154H
3).
LO4-
166H
3Su
n El
evat
ion:
7.0
°A
ltit
ude:
359
2.60
km
30
0Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
The
80t
h so
uthe
rn p
aral
lel
(the
80°
S li
ne o
f la
titu
de)
issh
own
here
as
a da
shed
arc
. In
thre
e-di
men
sion
al g
eom
etry
,a
para
llel i
s a
circ
le, b
ut in
thi
s ph
otog
raph
, tak
en w
hen
the
spac
ecra
ft w
as a
t 72.
07°S
, the
cir
cle
is fo
resh
orte
ned.
Cra
ters
near
the
Sou
th P
ole,
lik
e th
ose
at t
he N
orth
Pol
e, a
re o
ften
nam
ed a
fter
exp
lore
rs o
f th
e po
les
of E
arth
. Rob
ert
Falc
onSc
ott,
who
se c
rate
r is
sho
wn
part
icul
arly
wel
l in
this
pho
to,
led
the
seco
nd p
arty
to
reac
h th
e So
uth
Pole
of
Eart
h in
Janu
ary
1912
, 1 m
onth
aft
er A
mun
dsen
had
bee
n th
ere.
Sco
ttdi
ed a
long
wit
h tw
o of
his
men
on
the
retu
rn fr
om th
e Po
le.
LO4-
154H
1Su
n El
evat
ion:
10.
8°A
ltit
ude:
361
3.43
km
30
1So
uth
Pola
r R
egio
n
Thi
s ar
ea h
as n
ot o
nly
been
bom
bard
ed w
ith
prim
ary
im-
pact
ors
duri
ng th
e fo
rmat
ion
of th
e M
oon
and
afte
r, b
ut h
asbe
en
subj
ecte
d to
bu
rial
w
ith
ejec
ta
from
th
e So
uth
Pole
–Aik
en B
asin
, th
e B
ailly
Bas
in,
and
seco
ndar
y cr
ater
spr
obab
ly f
rom
the
Ori
enta
le B
asin
. Kla
prot
h, y
oung
eno
ugh
to h
ave
a re
ason
ably
inta
ct r
im in
its
nort
heas
tern
sec
tor,
has
had
othe
r se
ctor
s of
its
rim
impa
cted
in tu
rn b
y C
asat
us a
ndtw
o ot
her
crat
ers.
How
ever
, its
floo
r se
ems
youn
g, fl
at, a
ndre
lati
vely
sm
ooth
. Per
haps
tec
toni
c fo
rces
hav
e le
vele
d pu
l-ve
rize
d ej
ecta
in th
at a
rea.
Wha
teve
r ha
ppen
ed to
sm
ooth
the
floor
hap
pene
d lo
ng a
go. U
nder
hig
h m
agni
ficat
ion,
a h
eavy
pepp
erin
g of
sm
alle
r (2
km
and
less
) cr
ater
s ca
n be
see
n.
30
2Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
154H
2Su
n El
evat
ion:
10.
8°A
ltit
ude:
361
3.43
km
An
oute
r ri
ng o
f th
e Sc
hille
r-Z
ucch
ius
Bas
in c
an b
e se
enru
nnin
g ju
st e
ast
of S
chill
er, s
outh
to
the
edge
of
Ros
t, an
dar
ound
ben
eath
Zuc
chiu
s. W
ithi
n th
is o
uter
rin
g is
the
mai
nri
ng, i
ncom
plet
e in
its
nort
hern
sec
tor.
Sec
onda
ry c
hain
s on
the
floor
of
this
bas
in a
re f
rom
Ori
enta
le t
o th
e no
rthw
est.
Schi
ller
was
pro
babl
y fo
rmed
by
the
sim
ulta
neou
s ar
riva
l of
two
or m
ore
prim
ary
impa
ctor
s co
min
g in
at a
ver
y lo
w a
ngle
to th
e su
rfac
e.
LO4-
154H
3Su
n El
evat
ion:
10.
8°A
ltit
ude:
361
3.43
km
30
3So
uth
Pola
r R
egio
n
Smal
ler
crat
ers,
less
than
30
km in
siz
e, a
re r
elat
ivel
y de
ep. I
fth
ey a
re n
ear
a po
le th
eir
floor
s ar
e lik
ely
to b
e in
per
man
ent
shad
ow.
Thi
s is
esp
ecia
lly t
rue
if t
hey
are
on t
he n
orth
ern
part
of
the
floor
s of
lar
ger
crat
ers
who
se r
ims
then
hel
p to
shad
e th
em.
LO4-
130H
1Su
n El
evat
ion:
8.7
°A
ltit
ude:
357
4.83
km
30
4Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
The
anc
ient
, ove
r-cr
ater
ed t
erra
in o
f thi
s ar
ea is
inte
rrup
ted
by E
rato
sthe
nian
Cra
ter
Mor
etus
, wit
h a
wel
l-fo
rmed
cen
tral
peak
and
an
inta
ct e
ject
a pa
tter
n.
LO4-
130H
2Su
n El
evat
ion:
8.7
°A
ltit
ude:
357
4.83
km
30
5So
uth
Pola
r R
egio
n
The
sm
ooth
ing
of t
he t
erra
in n
orth
and
sou
th o
f C
lavi
us i
spr
obab
ly c
ause
d by
eit
her
its
ejec
ta b
lank
et o
r th
e sh
ock
ofit
s im
pact
on
a pr
eexi
stin
g ac
cum
ulat
ion
of e
ject
a fr
om o
ther
impa
cts.
At
225
km, i
t is
abo
ut a
s bi
g as
a c
rate
r ca
n be
; it
isin
the
tran
siti
on r
ange
bet
wee
n cr
ater
s an
d ba
sins
. The
ori
gi-
nal c
entr
al p
eak
may
hav
e be
en la
rger
tha
n it
is n
ow. I
t m
ayha
ve b
een
larg
ely
buri
ed b
y ej
ecta
. R
ays
from
Cop
erni
can
crat
er T
ycho
to
the
nort
h ha
ve a
lso
land
ed i
n th
is r
egio
n.T
his
area
may
con
tain
sec
onda
ries
fro
m b
oth
the
Ori
enta
lean
d Im
briu
m B
asin
s.
30
6Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
130H
3Su
n El
evat
ion:
8.7
°A
ltit
ude:
357
4.83
km
Slum
ps f
rom
the
rim
of
Cla
vius
to
its
floor
are
abo
ut 1
5 to
20
km
in
wid
th. T
his
size
is
typi
cal
of t
he s
lum
ps i
n cr
ater
wal
ls,
inde
pend
ent
of t
he d
iam
eter
of
the
crat
er.
Smal
ler
crat
ers
tend
to h
ave
slum
ps in
the
sam
e ab
solu
te s
ize
rang
e.
LO4-
118H
3Su
n El
evat
ion:
7.8
°A
ltit
ude:
355
4.96
km
30
7So
uth
Pola
r R
egio
n
Euge
ne M
. Sh
oem
aker
, th
e fo
unde
r of
the
USG
S A
stro
-ge
olog
y B
ranc
h, h
as b
een
a m
ajor
lead
er in
rev
ealin
g th
e im
-pa
ct o
rigi
n of
mos
t Moo
n cr
ater
s an
d so
me
on E
arth
. Gen
e’s
succ
essf
ul c
aree
r w
as e
nded
by
a fa
tal
auto
mob
ile a
ccid
ent
as h
e so
ught
to in
vest
igat
e ye
t ano
ther
cra
ter
in A
ustr
alia
. At
the
end
of i
ts s
ucce
ssfu
l m
issi
on,
the
spac
ecra
ft L
unar
Pros
pect
or w
as c
rash
ed i
nto
this
per
man
entl
y co
ld c
rate
rflo
or (
now
nam
ed a
fter
Gen
e) in
an
atte
mpt
to
dete
ct w
ater
in t
he c
rash
plu
me.
The
spa
cecr
aft
carr
ied
a vi
al c
onta
inin
ghi
s as
hes,
and
Gen
e be
cam
e th
e fir
st p
erso
n to
be
inte
rred
beyo
nd E
arth
.
LO4-
106H
1Su
n El
evat
ion:
9.1
°A
ltit
ude:
353
4.50
km
30
8Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
The
re i
s a
tran
siti
on i
n th
is a
rea,
esp
ecia
lly t
o th
e ea
st,
betw
een
heav
y cr
ater
ing
in c
haot
ic d
ebri
s an
d cr
ater
ing
in a
rela
tive
ly fl
at s
urfa
ce. T
his
coul
d m
ark
the
tran
siti
on b
etw
een
the
inne
r he
avy
ejec
ta fr
om th
e So
uth
Pole
–Aik
en B
asin
and
the
oute
r pl
ains
-for
min
g an
d se
cond
ary
field
of
that
bas
in.
To
the
wes
t, t
he e
quiv
alen
t ar
ea h
as b
een
tran
sfor
med
by
smal
ler
basi
ns f
rom
im
pact
s th
at a
rriv
ed lo
ng a
fter
the
for
-m
atio
n of
the
Sou
th P
ole–
Aik
en B
asin
, but
to
the
east
the
rear
e fe
wer
suc
h ba
sins
.
LO4-
106H
2Su
n El
evat
ion:
9.1
°A
ltit
ude:
353
4.50
km
30
9So
uth
Pola
r R
egio
n
Thi
s ar
ea i
s ab
out
one
basi
n di
amet
er f
rom
Nub
ium
and
Nec
tari
s, a
bout
1.5
dia
met
ers
from
Im
briu
m,
and
abou
t 0.
5 di
amet
er f
rom
the
Sou
th P
ole–
Aik
en B
asin
. Thi
s fie
ld o
ffr
esh
30-k
m s
econ
dary
cra
ters
is
radi
al t
o Im
briu
m.
Som
egr
oups
of
smal
l (2
-km
) se
cond
arie
s ar
e th
ough
t to
com
efr
om t
he N
ecta
ris
Bas
in f
ar t
o th
e no
rthe
ast.
Stri
atio
ns n
ear
the
left
edg
e of
this
pho
to a
re r
adia
l to
Cla
vius
.
31
0Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
106H
3Su
n El
evat
ion:
9.1
°A
ltit
ude:
353
4.50
km
Thi
s fla
t ar
ea is
abo
ut a
s fa
r as
one
can
get
fro
m b
asin
s an
dla
rge
crat
ers
on t
he n
ear
side
. St
ill,
ther
e ar
e m
any
crat
ercl
uste
rs o
f va
riou
s si
zes
and
degr
ees
of d
egra
dati
on t
hat
are
prob
ably
sec
onda
ries
fro
m r
emot
e ba
sins
. A b
asin
has
bee
npr
opos
ed t
o be
nor
th o
f M
utus
, bu
t C
lem
enti
ne e
leva
tion
data
sho
w t
hat
area
to
be r
elat
ivel
y hi
gh. T
he a
rea
may
be
crus
t tha
t has
esc
aped
maj
or im
pact
s by
cha
nce.
LO4-
094H
3Su
n El
evat
ion:
9.8
°A
ltit
ude:
351
6.92
km
31
1So
uth
Pola
r R
egio
n
Thi
s is
the
sun
nies
t vi
ew o
f cr
ater
Am
unds
en f
rom
Lun
arO
rbit
er M
issi
on 4
. Roa
ld A
mun
dsen
led
the
first
exp
edit
ion
to r
each
the
Sou
th P
ole
of E
arth
, su
ccee
ding
in
Dec
embe
r19
10. H
e re
turn
ed s
afel
y an
d co
ntin
ued
expl
orat
ions
of b
oth
pola
r re
gion
s. T
he c
lust
er o
f fr
esh-
look
ing
crat
ers
in t
he 1
0-to
30-
km s
ize
rang
e ar
e pr
obab
ly s
econ
dari
es fr
om Im
briu
m,
a fu
ll tw
o di
amet
ers
away
from
its
mai
n ri
ng. T
his
is fu
rthe
rth
an s
econ
dari
es a
re u
sual
ly t
hrow
n, b
ut b
ecau
se o
f the
siz
eof
Im
briu
m,
the
curv
atur
e of
the
Moo
n m
ay e
xten
d th
eir
trav
el. T
o pu
t it a
noth
er w
ay, t
he e
ject
ion
velo
city
was
pro
ba-
bly
clos
er to
esc
ape
velo
city
.
31
2Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
082H
1Su
n El
evat
ion:
8.7
°A
ltit
ude:
350
2.94
km
The
pro
min
ent c
hain
s of
cra
ters
her
e ar
e ra
dial
to I
mbr
ium
.Sc
hom
berg
er h
as e
scap
ed s
uch
impa
cts;
in fa
ct, i
ts e
ject
a ha
sfa
llen
on s
ome
seco
ndar
y cr
ater
s. I
t has
bee
n as
sign
ed to
the
Late
Imbr
ian
Epoc
h.
LO4-
082H
2Su
n El
evat
ion:
8.7
°A
ltit
ude:
350
2.94
km
31
3So
uth
Pola
r R
egio
n
Vla
cq, N
earc
h, a
nd M
utus
are
bel
ieve
d to
be
Pre-
Nec
tari
an.
A c
hain
of s
econ
dary
cra
ters
rad
ial t
o th
e N
ecta
ris
Bas
in c
anbe
see
n on
the
nor
thw
est
rim
of N
earc
h. O
ther
cra
ter
chai
nsbe
twee
n T
anne
rus
and
Nea
rch
are
radi
al to
Ori
enta
le.
LO4-
082H
3Su
n El
evat
ion:
8.7
°A
ltit
ude:
350
2.94
km
31
4Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
The
lon
g ch
ain
of s
mal
l cr
ater
s in
the
low
er r
ight
of
this
phot
o is
rad
ial
to t
he N
ecta
ris
Bas
in. S
imila
r ch
ains
can
be
seen
nor
th o
f Bie
la.
LO4-
070H
3Su
n El
evat
ion:
9.7
°A
ltit
ude:
349
6.53
km
31
5So
uth
Pola
r R
egio
n
Nob
ile is
wel
l illu
min
ated
in th
is p
hoto
, but
its
floor
rem
ains
in s
hado
w.
Um
bert
o N
obile
was
an
aero
naut
ical
eng
inee
ran
d an
exp
lore
r of
the
Art
ic. H
e an
d R
oald
Am
unds
en w
ere
the
first
to fl
y ov
er th
e N
orth
Pol
e of
Ear
th (
1926
); th
ey u
sed
a di
rigi
ble.
Tw
o ye
ars
late
r, o
n an
othe
r vo
yage
of
ex-
plor
atio
n, N
obil
e cr
ashe
d in
a d
irig
ible
on
the
ice
near
Spit
sber
gen.
Am
unds
en d
ied
in a
n at
tem
pt t
o fly
in
and
resc
ue N
obile
, who
sur
vive
d.
31
6Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
058H
1Su
n El
evat
ion:
8.5
°A
ltit
ude:
349
3.64
Bous
sing
ault
is n
ot a
nes
ted
crat
er p
rodu
ced
by im
pact
into
ala
yere
d ta
rget
: a s
ubse
quen
t im
pact
has
hit
its
floor
to c
reat
eth
is u
nusu
al t
opog
raph
y. T
he r
elat
ive
ages
of
crat
ers
in t
his
area
can
be
infe
rred
from
the
shar
pnes
s of
thei
r fe
atur
es a
ndde
gree
of s
ubse
quen
t cra
teri
ng. A
ll th
e na
med
cra
ters
in th
isph
oto
are
assi
gned
to th
e Pr
e-N
ecta
rian
Per
iod.
LO4-
058H
2Su
n El
evat
ion:
8.5
°A
ltit
ude:
349
3.64
km
31
7So
uth
Pola
r R
egio
n
Nea
r th
e to
p of
thi
s ph
oto
ther
e ar
e st
riat
ion
s ra
dial
to
Nec
tari
s, to
the
nort
hwes
t. C
rate
r ch
ains
on
the
righ
t sid
e of
the
phot
o ar
e ra
dial
to
the
Fecu
ndit
atis
Bas
in t
o th
e no
rth,
but
they
see
m t
oo f
resh
to
have
com
e fr
om a
bas
in t
hat
old.
Per
haps
the
y ca
me
from
the
Cri
sium
Bas
in,
beyo
ndFe
cund
itat
is.
31
8Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
058H
3Su
n El
evat
ion:
8.5
°A
ltit
ude:
349
3.64
km
Thi
s is
an
apol
une
phot
o, t
aken
at
the
end
of t
he m
issi
on t
o fil
l in
cov
erag
eth
at w
as m
isse
d at
the
beg
inni
ng o
f th
e m
issi
on d
ue t
o th
e th
erm
al d
oor
prob
lem
. Con
sequ
entl
y, t
he s
unlig
ht c
omes
fro
m t
he w
est.
Cra
ter
chai
ns t
hat
are
alig
ned
wit
h V
alli
s R
heit
a co
me
from
Nec
tari
s. T
hose
tha
t ar
e m
ore
31
9So
uth
Pola
r R
egio
n
LO4-
184H
3Su
n El
evat
ion:
6.9
°A
ltit
ude:
579
0.16
km
alig
ned
wit
h th
e no
rth-
sout
h di
rect
ion
are
radi
al t
o th
e Fe
cund
itat
is a
ndC
risi
um B
asin
s. T
he p
lain
s no
rth
of B
iela
are
cov
ered
wit
h N
ecta
ris
ejec
ta.
Pont
ecou
lant
is o
f the
Nec
tari
an P
erio
d.
Phot
o LO
4-00
5 w
as t
aken
ear
ly i
n th
e m
issi
on,
befo
re t
hepr
oble
m w
ith
the
ther
mal
doo
r oc
curr
ed. T
his
phot
o sp
ans
the
90°
east
mer
idia
n, t
he b
ound
ary
betw
een
the
near
sid
ean
d fa
r si
de. T
race
s of
a v
ery
old,
larg
e (2
00-k
m)
crat
er c
anbe
see
n in
the
upp
er r
ight
of
this
pho
to,
lyin
g be
neat
hG
answ
indt
and
Ide
l’son
. Its
deg
rade
d ri
m i
s ta
ngen
t to
the
nort
h ri
m o
f Gan
swin
dt a
nd r
uns
abov
e th
e ed
ge o
f the
pho
toar
ound
to H
eder
vari
.
32
0Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
005H
1Su
n El
evat
ion:
8.9
°A
ltit
ude:
349
7.58
km
LO4-
005H
2Su
n El
evat
ion:
8.9
°A
ltit
ude:
349
7.58
km
32
1So
uth
Pola
r R
egio
n
The
hea
vy r
idge
s an
d va
lleys
com
ing
from
the
nor
thea
st,
pass
ing
wes
t of
Wex
ler
and
east
of
Neu
may
er, a
re r
adia
l to
the
Aus
tral
e Ba
sin.
The
rid
ges
and
valle
ys th
at c
ross
them
are
radi
al t
o th
e Sc
hrod
inge
r B
asin
on
the
far
side
(se
e Fi
gure
12.3
). N
eum
ayer
is
Nec
tari
an.
Hal
e ap
pear
s to
be
muc
hyo
unge
r, p
roba
bly
Erat
osth
enia
n.
The
cen
ter
of t
he a
ncie
nt A
ustr
ale
Bas
in i
s ea
st o
f Ly
ot a
ndno
rth
of J
eans
. The
floo
r of
thi
s ba
sin
near
ly, b
ut n
ot q
uite
,flo
oded
wit
h m
are
lava
. Lar
ge c
rate
rs s
uch
as L
yot a
nd L
amb
(LO
4-00
9H2
in th
e Ea
ster
n B
asin
Reg
ion)
see
m to
hav
e st
im-
ulat
ed t
he fl
ow. T
he ja
gged
dag
ger
in t
he lo
wer
rig
ht c
orne
rof
the
pho
to i
s th
e ti
p of
Val
lis S
chro
ding
er, a
310
-km
-lon
gra
dial
fra
ctur
e fr
om t
he f
ar s
ide
Schr
odin
ger
Bas
in (
see
Figu
re 1
2.3)
.
32
2Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
LO4-
005H
3Su
n El
evat
ion:
8.9
°A
ltit
ude:
349
7.58
km
Latin Words in Names of Features
Catena: Bowl, a chain of craters.Dorsum: Backbone, a ridge, often wrinkled, in the surface of a mare.Lacus: Hollow, a small depression filled with lava flows.Mare: Sea, dark, smooth plains formed by lava flows in a large
depression.Mons, Montes: Mount, mountains, a peak or range of mountains.Palus: Swamp, a small area with shallow lava flows.Planitia: Plain, a low flat area.Promontorium: Promontory, a highland peninsula extending into a
mare.Rima: Crack, leak, a narrow, long channel that may be sinuous (a
sign of meandering lava flow), straight, or in an arc (signs of afault).
Rupes: Cliff, a long abrupt change in elevation; a cliff along a verti-cal fault or an edge of a lava flow.
Sinus: Bay, an extension of a mare.Vallis: Valley, a wide, long depression.
Age Ranges on the Moon (Oldest First)
Pre-Nectarian Period: The age range between the hardening of the crust and the impact event that formed the Nectaris Basin.
Nectarian Period: The age range between the formation of theNectaris Basin and the Imbrium Basin.
Early Imbrian Epoch: The age range from the formation of theImbrium Basin through that of the Orientale Basin.
Late Imbrian Epoch: The age range from the formation of theOrientale Basin through the most voluminous lava flows.
Eratosthenian Period: The age range of declining heavy lava flowand declining rate of impact. This period includes the formationof rayless post-mare craters like Eratosthenes.
Copernican Period: This age range extends from the time of forma-tion of the oldest bright-rayed craters to the present. Copernicus,with very bright rays, is the typical young crater of this period.Since the rays of craters fade with time, craters with dimmer raysare assigned older ages in this period.
General Terms
Albedo: The inherent brightness of a surface.
Apolune: The point on a lunar orbit farthest from the surface of theMoon.
Basin: A large crater-like depression containing one or more ringsin addition to a rim. Also “multi-ringed basin.”
Crater: A compact depression. Nearly all craters on the Moon arecaused by impact; when fresh, impact craters usually are nearlycircular and have raised rims.
Crust: The upper layer of rock, composed of minerals that have sep-arated from a melt and risen because of their low density.
Ejecta: Material thrown out from a transient crater as a result of theenergy released by an impact.
Limb: An edge of a celestial body like the Moon, as viewed. KREEP: An acronym representing potassium (chemical symbol K),
Rare Earth Elements, and Phosphor. These elements are late tocrystallize from a cooling melt.
Main ring: The highest ring of a basin. Also called the rim of thebasin or the topographic ring.
Mantle: The layer of rock below the crust, composed of mineralsthat have separated from a melt and fallen because of their highdensity.
Mascon: A concentrated mass that affects the gravity field of theMoon. Mascons are associated with pipes of high-density mantlematerial that flooded maria.
Perilune: The point on a lunar orbit closest to the surface of theMoon.
Ring: A circular ridge that is formed along with a basin. Internalrings are inside the main ring and external rings are outside themain ring.
Secondary crater: A crater formed by the impact of material ejectedfrom another (primary) crater or basin.
Theia: The small planet that impacted Earth to form the Moon,named for a Greek goddess whose daughter was said to be Selene,the goddess of the Moon.
Topographic rim: The highest ring around a crater. Also called themain ring if the crater exhibits multiple rings and troughs (amulti-ringed basin).
Topography: The shape of a surface.Transient crater: The material that is fractured, melted, and vapor-
ized by a hypervelocity impact before further dynamic processesredistribute the material as ejecta, secondary impactors, and soon.
Trough: A shallow linear or curved depression, especially a circularvalley between rings of a basin.
Glossary
32
3G
loss
ary
Bowker, 1971: D.E. Bowker and J.K. Hughes, Lunar OrbiterPhotographic Atlas of the Moon, NASA SP 206.
Bussey, 2004: Ben Bussey and Paul D. Spudis, The Clementine Atlasof the Moon, Cambridge University Press, Cambridge.
Byrne, 2002a: C.J. Byrne, Automated Cosmetic Improvements ofMosaics from the Lunar Orbiter, Lunar and Planetary ScienceConference (LPSC) 33, #1099.
Byrne, 2002b: C.J. Byrne, A New Moon: Improved Lunar OrbiterMosaics, The Moon Beyond 2002: Next Steps in Lunar Scienceand Exploration, p. 7, LPI Contribution No. 1128, Lunar andPlanetary Institute, Houston.
Byrne, 2003: C.J. Byrne, Proposed High-Level Regional Focal Pointsfor Lunar Geography, LPSC 34, #1517.
Byrne, 2004: C.J. Byrne, Evidence for Three Basins beneath OceanusProcellarum, Lunar and Planetary Science Conference (LPSC) 35,#1103.
De Hon, 1979: R.E. De Hon, Thickness of the Western MareBasalts, Lunar and Planetary Science Conference (LPSC) 10, pp. 2935–2955.
Gaddis, 1997: L. Gaddis, et al., An Overview of the IntegratedSoftware for Imaging Spectrometers (ISIS), Lunar and PlanetaryScience Conference (LPSC) 28, #387.
Gaddis, 2001: L. Gaddis, et al., Cartographic Processing of DigitalLunar Orbiter Data, LPS 32, Abstract #1892, Lunar and PlanetaryInstitute, Houston (CDROM).
Gasnault, 2002: O. Gasnault, W.C. Feldman, C. d’Uston, D.J.Lawrence, S. Maurice, S.D. Chevral, P.C. Pinet, R.C. Elphic, I.Genetay, and K.R. Moore, JGR 107 (E10).
Gault, 1978: D.E. Gault and J.A. Wedekind, Experimental Studies ofOblique Impact, Lunar and Planetary Science Conference (LPSC)9, v. 3, pp. 3843–3875.
Gillis, 2002: J. Gillis (ed.), Digital Lunar Orbiter Photographic Atlasof the Moon, www.lpi.usra.edu/research/lunarorbiter, Lunar andPlanetary Institute, Houston.
Gonzalez, 2002: Rafael C. Gonzalez and Richard E. Woods, DigitalImage Processing, Second Edition, Addison Wesley, Reading.
Greeley, 1976: R. Greeley and M.H. Carr, Editors, A Geological Basisfor the Exploration of the Planets, NASA Report SP-417.
Hawke, 2004: B.R. Hawke et al., The Origin of Lunar Crater Rays,LPSC 35, Abstract #1477, Lunar and Planetary Institiute(CDROM).
McEwen, 1994: A. McEwen, P. Davis, and A. Howington-Kraus,Evidence for a Pre-Nectarian Impact Basin in NorthwesternOceanus Procellarum, Lunar and Planetary Science Conference(LPSC) 25, Abstract # 869, Lunar and Planetary Institute,Houston.
Quaide, 1968: W.L. Quaide and V.R. Oberbeck, Thickness determi-nations of the lunar surface layer from lunar impact craters,Journal of Geophysics Research 73:5247–5270.
Schultz, 1972: P.H. Schultz, Moon Morphology, University of TexasPress.
Spudis, 1993: P.D. Spudis, The Geology of Multi-Ring Impact Basins:The Moon and Other Planets, Cambridge University Press,Cambridge.
Spudis, 1996: P.D. Spudis, The Once and Future Moon, SmithsonianInstitution Press, Washington, DC.
Stevens, 1999: R. Stevens, Visual Basic Graphics Programming,Second Edition, Wiley, New York.
Whitaker, 1999: E.A. Whitaker, Mapping and Naming the Moon,Cambridge University Press, Cambridge.
Whitaker, 1970; E.A. Whitaker et al., Atlas and Gazetteer of theNear Side of the Moon, NASA SP-241.
Wilhelms, 1987: D.E. Wilhelms et al., The Geologic History of theMoon, USGS Professional Paper 1348, US Government PrintingOffice, Washington, DC.
Wilhelms, 1993: D.E. Wilhelms, To a Rocky Moon, The University ofArizona Press.
References
32
4Lu
na
r O
rbiter
Photo
gra
phic
Atla
s
32
5G
ener
al
Ind
ex
Basins (continued)—Humorum, 55, 63, 68, 72, 76, 77,
79, 82 (see Vitello Formation) —Imbrium, 100–102, 125–158 (see
Fra Mauro and Alps Formations)—Lavoissier-Mairan, 101, 104, 118—Mendel-Rydberg, 296, 297—Nectaris, 155, 156, 164–194 (see
Janssen Formation)—Northern Serenitatis, 201, 207, 217—Nubium, 55, 77–79, 82, 87, 89, 93,
94—Orientale, 13–16, 20, 24, 34, 36,
53, 54 (see Hevelius Formation)—Reiner-Letronne, 102—Schiller-Zucchius, 57, 60, 300, 303—Schrodinger, 92, 292, 322—Serenitatis, 200, 201, 204–207,
209–211, 214–217, 220–225—Smythii, 244, 245, 251, 252, 256,
257, 262—South Pole-Aiken, 245, 260, 291,
292, 309—Tranquillitatis, 155, 190, 201,
219–220, 224, 231
Cataclysm, 8Censorinus Highlands, 228, 231Compact Disc, 11Crustal depth, 8
Deep Space Network, 7
Formations—Alpes, 154, 206, 210, 212—Cayley, 156, 169, 170, 213—Descartes, 156, 169, 170—Fra Mauro, 90, 100–102, 131, 151—Hevelius, 15, 42, 46, 49—Inner Hevelius, 15, 18, 25, 28, 32,
38, 42—Janssen, 171, 180, 186, 192—Maunder, 16, 17, 21, 23—Montes Rook, 18, 21—Outer Hevelius, 15, 19, 26, 34, 42,
48
Formations (continued)—Vitello, 66, 67
Gravity field, 9
Highlands, 8
Jet Propulsion Laboratory, 7
Kant Plateau, 175Kodak BimatTM process, 7Kuiper Belt, 136
Landmarks, 9—Humorum Basin, 9, 10—Imbrium Basin, 9, 10—Nectaris Basin, 9, 10—North Pole, 9, 10—Orientale Basin, 9, 10—Serenitiatis Basin, 9, 10—Smythii Basin, 9, 10—South Pole, 9, 10Langley Research Center, 7Luna missions—Luna 05, 85, 137—Luna 07, 120—Luna 15, 246, 249—Luna 16, 199, 240, 249—Luna 18, 240, 249—Luna 20, 240, 249—Luna 21, 224, 225—Luna 24, 246Lunar Orbiter—Cameras, 5—Famelet, 7 —Film, 5—Ground Recording Equipment, 7—High-resolution camera, 5—Image motion compensation, 5—Medium-resolution camera, 5—Mission 2—Mission 4, 5—Order of photos, 6, 11—Scanning artifacts, 7
Lunar Orbiter (continued)—Subframes, 7, 11—Venetian blind effect, 7
Magma ocean, 8Maps, large scale, 2–4Marius Hills, 115, 120 Mascons, 9
North Pole, 269, 273, 277, 281, 285,289
Origin of the Moon, 8
Ranger missions—Ranger 7, 84—Ranger 8, 219—Ranger 9, 98Regional Planetary Image Facilities, 7Regions, 2–4—Eastern Basins Region, 10, 244—Humorum Basin Region, 10, 55—Imbrium Basin Region, 10, 100—Nectaris Basin Region, 10, 155—North Polar Region, 10, 263—Orientale Basin Region, 10, 13—Serenitatis Basin Region, 10, 200—South Polar Region, 10, 291
Shoemaker-Levy 9, 169South Pole, 298, 301, 304, 308, 312,
316, 320Surveyor missions—Surveyor 1, 70—Surveyor 3, 85, 137—Surveyor 4, 99, 202—Surveyor 5, 219—Surveyor 6, 99, 202—Surveyor 7, 86Synchronization of the Moon’s
orbit, 8
Theia, 301
Age periods and epochs, 10—Copernican Period, 10, 323—Early Imbrian Epoch, 10, 323—Eratosthenian Period, 10, 323—Late Imbrian Epoch, 10, 323—Nectarian Period, 10, 323—Pre-Nectarian Period, 10, 323Apollo missions—Apollo 11, 175, 219—Apollo 12, 85, 137—Apollo 14, 90—Apollo 15, 153, 204, 205—Apollo 16, 170—Apollo 17, 224Apennine Bench, 152Apollo astronauts—Aldrin, Buzz, 175, 219—Armstrong, Neil, 175, 219—Bean, Alan, Apollo, 85, 137—Cernan, Eugene, Apollo, 224—Conrad, Charles (Pete), 85, 137—Duke, Charles, Apollo, 170 —Irwin, James, 153, 204, 205—Mattingly, T. Kenneth, 213—Mitchell, Edgar, 90—Schmitt, Harrison (Jack), 224—Scott, David R., 153, 204, 205—Shepard, Alan, 90—Young, John, 170Aristarchus Plateau 121, 122Army Mapping Service, 7
Basin ejecta blankets, 9Basins, 9—Australe, 244, 245, 248, 250,
259–261, 290, 322—Bailly, 290, 291, 294, 295, 297, 299,
302—Balmer-Kapteyn, 244, 245, 249—Cardanus-Herodotus, 101, 116—Crisium, 244, 245, 248, 250, 254,
260, 261—Fecunditatis, 155, 193, 194,
197–199, 228, 231, 232, 244—Flamsteed-Billy, 101—Grimaldi, 13, 14, 41, 49, 54—Humboldtianum, 234, 243, 253,
255, 263, 264, 285–290
General Index
Albedo feature—Reiner Gamma, 114
Catena (chain of craters)—Abulfeda, 169—Brigitte, 224—Davy, 94, 98—Deslandres, 94—Humboldt, 262—Krafft, 43—Littrow, 224—Sylvester, 269—Taruntius, 235—Timocharis, 144—Yuri, 1Craters —Abel, 261—Abulfeda, 165, 169—Agrippa, 208—Airy, 161—Alexander, 212—Aliacensis, 96, 159, 160—Alphonsus, 98—Amundsen, 301, 304, 308, 312,
316, 320—Anaxagoras, 276, 280—Anaximenes, 268, 272—Annegrit, 135—Anville, 194, 235—Apianus, 159, 160, 164, 165—Aristarchus, 121, 122—Aristillus, 153—Aristoteles, 282, 283—Aston, 103—Atlas, 226, 227, 230, 247—Atwood, 199, 249—Autolycus, 153, 205—Baade, 20, 296—Babbage, 267, 270, 271—Baco, 157, 311—Baillaud, 284, 288, 290—Bailly, 295, 297, 299, 300—Balmer, 249, 251—Barnard, 261, 262—Barocius, 158, 163—Barrow, 280—Bartels, 27, 103—Bayer, 60, 303—Beer, 144, 147—Berosus, 253, 255—Berzelius, 233, 238, 247—Bessarion, 128—Bessel, 215—Bianchini, 124, 274—Biela, 176, 185, 315, 318, 319—Bilharz, 199, 249
Craters (continued)—Billy, 64—Blagg, 202—Bode, 150—Bohnenberger, 183, 189—Bohr, 26, 34—Borda, 188, 194—Bouguer, 124, 274—Boussingault, 319—Brayley, 128—Brisbane, 191, 195, 319—Buisson, 262—Bullialdus, 83, 84—Burckhardt, 238, 240, 241, 247,
253—Burg, 217, 223—Burnham, 161, 165—Byrd, 269, 273, 277, 281, 285, 289,
317—Byrgius, 46, 47, 54—Campanus, 78, 79—Capuanus, 73, 78—Cardanus, 43—Carmichael, 228, 231—Carpenter, 272—Carrington, 239, 242, 247, 253—Casatus, 302, 305—Cassini, 154—Catalan, 296—Cauchy, 228, 231—Cayley, 213—Censorinus, 184, 224, 228—Cepheus, 230, 233, 247—Challis, 277, 281, 285—Charles, 135—Chevallier, 230, 233, 247, 253—Clausius, 62—Clavius, 60, 71, 80, 306, 307—Cleomedes, 237, 238, 240, 241,
246—Cook, 194—Copernicus, 138, 143—Couder, 18—Crozier, 194—Cruger, 48, 54—Curie, 261, 262—Cusanus, 288, 290, 320—Cuvier, 91, 157, 310, 311—Cyrillus, 174—da Vinci, 231—Daguerre, 183—Damoiseau, 54—Darney, 84—Darwin, 47, 48—De La Rue, 227, 230, 234, 286, 287,
290—Debes, 232, 237, 238
Craters (continued)—Descartes, 169—Deslandres, 87, 93, 96, 97—Diana, 228—Diophantus, 128, 129—Drygalski, 294, 298, 299—Eddington, 44—Eichstadt, 30, 39—Einstein, 26, 27, 103, 266—Endymion, 227, 230, 234, 247, 287,
290—Euclides, 79—Eudoxus, 212—Euler, 129, 134—Faraday, 95, 138, 158—Fauth, 137, 143—Felix, 135—Feuillee, 144, 147—Flamsteed, 70—Fontana, 59—Fourier, 58, 59, 62—Fra Mauro, 90—Fracastorius, 179, 182, 183—Franklin, 230, 233, 247—Furnerius, 192, 196, 248—Galle, 282, 283—Gambart, 90, 143—Gartner, 283, 286—Gassendi, 69, 75—Gaudibert, 183—Gauss, 253, 255—Geminus, 238, 241, 247, 253—Gemma Frisius, 164—Gerard, 104, 146—Gioja, 269, 273, 277, 281, 285—Glushko, 42, 43—Goclenius, 189, 194—Goddard, 254, 257—Goldschmidt, 276, 280—Goodacre, 164, 167—Grace, 228—Graff, 20, 296—Grimaldi, 49, 54, 103—Guericke, 89, 94—Gum, 260—Gutenberg, 184, 190—Guthnick, 296—Haidinger, 72, 77—Hainzel, 66, 72—Hale, 321—Hanno, 185, 191, 195, 319—Harlan, 250—Harpalus, 113, 218, 271, 274—Hartwig, 32, 41—Hausen, 295, 297—Hayn, 290—Hecataeus, 251
—Hedervari, 320—Hedin, 33, 42—Heinsius, 77—Helicon, 130, 136—Hell, 87, 93, 94—Henry, 54—Henry Freres, 54—Hercules, 226, 227, 230, 247—Hermite, 266, 269, 273, 277—Herodotus, 116, 121—Hesiodus, 82, 87, 88—Hevelius, 49—Hill, 228—Hind, 165—Hippalus, 74, 79—Hipparchus, 162, 165—Hommel, 157, 314—Hooke, 233, 239, 247, 253—Hortensius, 132, 137—Hubble, 254, 258—Huggins, 86, 92—Humboldt, 250, 261, 262—Hyginus, 203, 208—Idel’son, 308, 320—Inghirami, 28, 37—J. Herschel, 271, 272, 274—Jacobi, 91, 310, 311—Jansen, 224—Jansky, 254, 256, 257, 262—Janssen, 171, 177, 180—Jeans, 322—Jenner, 260—Joliot, 254, 258—Joy, 204, 210—Kapteyn, 249—Kepler, 128—Kies, 82—Kiess, 262—Kirchoff, 225, 229—Klaproth, 302, 305—Konig, 78, 79, 83—Kopff, 23—Krusenstern, 159, 160—Kugler, 259—La Caille, 97, 140, 160—La Condamine, 124, 131, 274, 275—Lade, 165, 208—Lagrange, 38, 46—Lalande, 94—Lamarck, 39, 47—Lamb, 260—Lambert, 139, 140—Lame, 249—Langrenus, 198, 199, 249—Lassell, 94—Lavoisier, 103, 105, 106, 206—Lawrence, 231
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All of the annotated features are listed here, with the exception of the craters. These craters are only those that are mentioned at least once in the notes. For afull list of annotated craters, see the CD.
Craters (continued)—Le Gentil, 294, 299—Le Monnier, 222, 224, 225—Le Verrier, 136—Leakey, 184, 228—Lebedev, 259—Letronne, 69, 70—Licetus, 91, 92, 95, 138, 158—Lichtenberg, 107, 108—Lilius, 80, 91, 310—Lindenau, 167, 172, 173—Linne, 210, 211—Lohrmann, 49, 54—Lohse, 198—Longomontanus, 71, 72, 77, 306—Luther, 216, 222—Lyapunov, 254, 258—Lyell, 228, 231—Lyot, 322—Madler, 179—Maestlin, 125, 128—Magelhaens, 189—Maginus, 80, 86, 92, 307, 310—Main, 277, 281, 285—Mairan, 118, 123—Malapert, 298, 301, 304, 308—Manilius, 209—Marco Polo, 151—Marinus, 248, 250—Markov, 267, 270—Mason, 217, 223—Maunder, 17, 23—Maupertuis, 131, 274, 275—Maurolycus, 95, 138, 158, 163—Maury, 226, 230—Mavis, 135—McClure, 194—Mee, 61, 66, 72—Menelaus, 214—Mercator, 78, 79, 82, 83—Mercurius, 239, 242, 253, 255—Messala, 239, 242, 247, 253—Messier, 194, 235—Meton, 280, 284, 290—Milichius, 133—Miller, 92, 95—Milne, 262—Monge, 189, 194—Moretus, 305, 309—Moseley, 27, 103—Murchison, 150, 202—Mutus, 311, 314—Nansen, 289, 317—Naonobu, 199, 249—Nasireddin, 92, 95—Nasmyth, 36, 51, 52, 300—Neander, 181, 182, 187—Nearch, 314, 315, 319—Neper, 254, 256, 257, 262—Neumayer, 321—Newcomb, 229, 231, 232, 247—Newton, 302, 305—Nicholson, 21, 22, 30—Nicollet, 88, 94—Nobile, 316—Noggerath, 51, 57—Oenopides, 267, 270—Oersted, 230, 233, 247—Oken, 248, 250—Orontius, 86, 92—Pallas, 150, 202—Peary, 269, 273, 277, 281, 285, 289,
317—Petavius, 197, 248—Petermann, 288, 290—Pettit, 21
Craters (continued)—Philolaus, 272, 276—Phocylides, 36, 51—Piazzi, 46—Piazzi Smyth, 145, 148—Piccolomini, 178, 179, 181—Pingre, 19, 295, 297—Pitatus, 87, 88, 93, 94—Plana, 217, 223—Plato, 142, 278, 279—Playfair, 160, 165—Plinius, 220—Plutarch, 252, 254—Pons, 167, 168, 173—Pontanus, 164, 165, 167, 168—Pontecoulant, 185, 191, 319—Posidonius, 222, 225—Priestly, 259—Prinz, 121, 122, 125—Ptolemaeus, 98, 99, 162—Puiseux, 67, 68, 73, 74—Pupin, 146—Purbach, 96, 97, 140—Pythagoras, 266, 267, 268, 270—Rabbi Levi, 167, 172—Reaumur, 99, 162, 202—Regiomontanus, 96, 97, 159—Reichenbach, 187, 188, 193, 194—Reimanus, 185, 191, 192, 319—Reinhold, 137—Repsold, 104, 146, 266, 267—Riccioli, 41, 42, 49—Riccius, 166, 172—Rocca, 48—Romer, 225, 228, 229—Rosse, 183—Rost, 51, 60, 303—Rothmann, 172, 173, 178, 179—Russell, 35, 44, 105, 107—Sampson, 140, 144—Santbech, 188, 189—Saussure, 86, 92—Scheiner, 60, 303, 306—Schickard, 45, 52, 57—Schiller, 51, 60, 61, 303—Schluter, 32—Schomberger, 309, 313—Scott, 301, 308, 312, 316—Shaler, 21, 29—Shoemaker, 308—Shuckburgh, 233, 239, 247, 253—Sirsalis, 54—South, 113, 218, 270, 271—Steinheil, 176, 180, 186, 319—Stevinus, 193—Stiborius, 172, 178—Stofler, 95, 158—Strabo, 287, 290—Struve, 35, 44, 105, 266—Suess, 119, 125—Sulpicius Gallus, 210—Sundman, 26—Tacchini, 256, 262—Tannerus, 157, 311, 314—Taruntius, 235, 246—Tempel, 208, 213—Thales, 286, 287, 290—Theaetetus, 154, 205—Thebit, 94, 97—Theophilus, 174, 179—Timocharis, 143, 144, 147—Tisserand, 231, 237, 246—Torricelli, 179—Triesnecker, 202—Tycho, 86—Vasco da Gama, 26, 34
Craters (continued)—Vega, 192, 196, 248, 319—Vendelinus, 198, 249—Verne, 135—Vieta, 53, 54, 58, 59—Vitello, 67, 68, 73, 74—Vlacq, 176, 314, 315—von Braun, 104, 106, 146, 206—Voskresenskiy, 27, 103, 104, 146—W. Bond, 280—Wallace, 146—Wallach, 224, 228—Wargentin, 36, 45, 300—Weigel, 51, 303—Weinek, 181, 182—Werner, 96, 97, 159, 160—Wexler, 321—Wildt, 252, 254—Wilhelm, 72, 77—Wilkins, 167, 168—Wolf, 88—Wright, 21, 22—Yakovkin, 19, 296—Young, 186, 192—Zagut, 167, 172, 173—Zahringer, 231—Zollner, 170, 175—Zucchius, 300, 303
Dorsum, Dorsa (mare ridge, ridges)—Dorsa Aldrovandi, 222—Dorsa Andrusov, 199—Dorsa Argand, 126—Dorsa Barlow, 224—Dorsa Burnet, 111, 116, 117—Dorsa Cato, 194—Dorsa Dana, 256—Dorsa Ewing, 69, 75, 76—Dorsa Geikie, 199—Dorsa Harker, 246—Dorsa Lister, 215, 221—Dorsa Mawson, 199—Dorsa Rubey, 70—Dorsa Smirnov, 216, 221, 222—Dorsa Stille, 139—Dorsa Tetyaev, 246, 252—Dorsa Whiston, 111, 116, 117,
222—Dorsum Arduino, 128—Dorsum Azara, 215, 216—Dorsum Bucher, 126—Dorsum Buckland, 210, 214, 215—Dorsum Cayeaux, 194—Dorsum Cushman, 194—Dorsum Gast, 210—Dorsum Grabau, 143, 144—Dorsum Guettard, 89, 90—Dorsum Heim, 129, 135—Dorsum Higazy, 143, 144—Dorsum Nichol, 220, 221—Dorsum Niggli, 116, 117—Dorsum Oppel, 246—Dorsum Owen, 210—Dorsum Scilla, 111—Dorsum Termier, 246—Dorsum Von Cotta, 210, 211—Dorsum Zirkel, 134, 135, 139,
140
Mare (sea), 8—Anguis, 240, 246, 252, 253—Australe, 191, 195, 259–261, 322—Cognitum, 84, 85—Crisium, 237, 240, 246, 249, 252
Mare (continued)—Fecunditatis, 190, 194, 198, 199,
231, 235, 240, 249—Frigoris, 124, 131, 227, 230, 271,
274, 275, 278, 286—Humboldtianum, 243, 290—Humorum, 62, 63, 73, 74—Imbrium, 130, 131, 133, 136, 139,
140, 143–145, 147, 148, 151, 266—Insularum, 85, 90, 132, 137—Marginis, 254, 257, 262—Nectaris, 179, 183—Nubium, 78, 79, 83, 87– 89, 93, 94—Orientale, 17, 23, 103—Serenitatis, 210, 211, 214–216,
222, 224—Smythii, 251, 256, 262—Spumans, 249—Tranquillitatis, 175, 179, 220, 224,
228, 231—Undarum, 249, 251—Vaporum, 151, 209Mons, Montes (mountain,
mountains)—Mons Ampere, 152—Mons Argaeus, 224—Mons Bradley, 152, 204—Mons Delisle, 128—Mons Esam, 228—Mons Gruithuisen Delta, 123, 126—Mons Gruithuisen Gamma, 123,
126—Mons Hadley, 204, 205—Mons Hadley Delta, 204—Mons Hansteen, 64—Mons Herodotus, 116, 117—Mons Huygens, 152—Mons La Hire, 134, 135, 139—Mons Maraldi, 228—Mons Moro, 84—Mons Penck, 175—Mons Pico, 145—Mons Piton, 148, 154—Mons Rumker, 109, 112—Mons Usov, 246—Mons Vinogradov, 128, 134—Mons Vitruvius, 224—Mons Wolff, 151—Mont Blanc, 148, 154—Montes Agricola, 111, 116, 117—Montes Alpes, 142, 148, 149, 154,
279—Montes Apenninus, 151, 152, 204,
205—Montes Archimedes, 152—Montes Carpatus, 133, 138, 143—Montes Caucasus, 154, 205—Montes Cordillera, 18, 21, 24, 29,
30, 31, 32—Montes Haemus, 209—Montes Harbinger, 122, 126—Montes Jura, 123, 124, 127—Montes Pyrenaeus, 183, 189—Montes Recti, 131, 142, 150—Montes Riphaeus, 79, 85—Montes Rook, 18, 21, 22, 23, 24,
30, 31—Montes Secchi, 231—Montes Spitzbergen, 147—Montes Taurus, 228, 229, 231—Montes Teneriffe, 142, 145, 150,
275, 278
Oceanus Procellarum, 59, 65, 70, 76,79, 100–122, 125, 128, 266, 267
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Palus (swamp)—Epidemiarum, 73, 74, 78, 79, 82—Putredinis, 152, 153, 204, 205Promontorium (promontory)—Agassiz, 148, 154—Archerusia, 220—Deville, 148, 154—Fresnel, 204, 205—Heraclides, 127, 130—Kelvin, 73, 74—Laplace, 130, 136—Taenarium, 94
Rima, Rimae (rille, rilles)—Rima Agatharchides, 79—Rima Agricola, 117—Rima Ariadaeus, 208, 213—Rima Billy, 64—Rima Birt, 94—Rima Bradley, 152, 153, 204—Rima Brayley, 125, 128—Rima Calippus, 212—Rima Cardanus, 43—Rima Carmen, 224—Rima Cauchy, 228—Rima Cleomedes, 240, 246—Rima Cleopatra, 117—Rima Conon, 204—Rima Dawes, 224—Rima Diophantus, 128, 129—Rima Draper, 133—Rima Euler, 134—Rima Flammarion, 99, 150—Rima Furnerius, 196, 248—Rima G. Bond, 225, 229—Rima Galilaei, 115—Rima Gartner, 286—Rima Gay-Lussac, 138
Rima, Rimae (continued)—Rima Hadley, 153, 204, 205—Rima Hansteen, 59, 64—Rima Hesiodus, 82, 83, 87—Rima Hyginus, 203, 208, 209—Rima Jansen, 224—Rima Krieger, 122—Rima Mairan, 118, 123—Rima Marius, 120—Rima Milichius, 128, 132—Rima Oppolzer, 162, 202—Rima Reaumur, 162, 202—Rima Rudolf, 224—Rima Schroter, 99, 150—Rima Sharp, 112, 113, 118, 218—Rima Suess, 120, 125—Rima T. Mayer, 133—Rima Vladimir, 152—Rima Yangel’, 203—Rimae Alphonsus, 98—Rimae Apollonius, 240—Rimae Archimedes, 152—Rimae Aristarchus, 116, 117, 121,
122—Rimae Arzachel, 98—Rimae Atlas, 227, 230—Rimae Bode, 150, 151—Rimae Boscovich, 209—Rimae Burg, 212, 217, 223—Rimae Chacornac, 225—Rimae Daniell, 217, 223—Rimae Darwin, 47, 48, 54—Rimae de Gasparis, 58, 59, 63—Rimae Doppelmayer, 62, 63, 67, 68—Rimae Fresnel, 153, 205—Rimae Gassendi, 69, 75—Rimae Gerard, 104, 146—Rimae Goclenius, 189, 190—Rimae Grimaldi, 54
Rima, Rimae (continued)—Rimae Gutenberg, 184, 190—Rimae Hase, 248—Rimae Herigonius, 75—Rimae Hevelius, 49—Rimae Hippalus, 73, 74, 78, 79—Rimae Hypatia, 175, 219—Rimae Janssen, 171, 177—Rimae Kopff, 23—Rimae Liebig, 63—Rimae Littrow, 224—Rimae Maclear, 214, 220—Rimae Maestlin, 128—Rimae Maupertuis, 131, 275—Rimae Menelaus, 214—Rimae Mersenius, 63, 64, 68, 69—Rimae Opelt, 89—Rimae Palmier, 62—Rimae Palmieri, 63—Rimae Parry, 90—Rimae Petavius, 197, 248—Rimae Pitatus, 87, 88, 93, 94—Rimae Plato, 142, 147, 149, 279—Rimae Plinius, 220—Rimae Posidonius, 222, 225—Rimae Prinz, 121, 122, 126—Rimae Ramsden, 73, 74, 78—Rimae Repsold, 104, 146—Rimae Riccioli, 41, 42, 49—Rimae Ritter, 213, 219—Rimae Romer, 224, 225, 228, 229—Rimae Secchi, 231—Rimae Sirsalis, 47, 54, 59—Rimae Sosigenes, 213, 214, 219, 220—Rimae Sulpicius Gallus, 210—Rimae Taruntius, 235—Rimae Theaetetus, 153, 205—Rimae Triesnecker, 202, 208—Rimae Vasco da Gama, 34
Rima, Rimae (continued)—Rimae Zupus, 59Rupes (scarp)—Altai, 172, 173, 178, 179—Boris, 129—Cauchy, 228—Kelvin, 73, 74—Liebig, 62, 63—Mercator, 78, 79, 82, 83—Recta, 94—Toscanelli, 121, 122
Sinus (bay)—Aestuum, 151—Amoris, 228, 231—Asperitatis, 175, 179, 219—Concordiae, 231—Fidei, 203—Honoris, 214—Iridum, 123, 124, 127, 130—Lunicus, 147—Medii, 99, 150, 162—Roris, 112, 113, 218, 270, 271—Successus, 240, 249
Vallis (valley)—Alpes, 149, 154, 279, 282—Baade, 20, 28, 296—Bohr, 26—Bouvard, 20, 21, 28, 29—Capella, 184—Inghirami, 28, 37—Palitzch, 248—Rheita, 180, 185, 186, 192, 319—Schrodinger, 322—Schroteri, 116, 117, 121, 122—Snellius, 188, 193, 194 3
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