OPTICAL ASTRONOMY OBSERVATORIES Q1...QUARTERLY REPORT OCTOBER -DECEMBER 1996 February 20,1997. I. INTRODUCTION II. SCIENTIFIC HIGHLIGHTS TABLE OF CONTENTS A. Cerro Tololo Inter-AmericanObservatory

NATIONAL

OPTICAL

ASTRONOMY

OBSERVATORIES

#1320

Sidney C WolffN0A0/DIR

NATIONAL OPTICAL ASTRONOMY OBSERVATORIES

QUARTERLY REPORT

OCTOBER - DECEMBER 1996

February 20,1997

I. INTRODUCTION

II. SCIENTIFIC HIGHLIGHTS

TABLE OF CONTENTS

A. Cerro Tololo Inter-American Observatory

1. Carbon Stars in the Large Magellanic Cloud.

2. The Interstellar Medium of NGC 55

3. Magnetic Activity and Dwarf M Stars

B. Kitt Peak National Observatory 2

1. Primordial Helium Revisited 2

2. Rotation, Activity, and Evolution of Hyades M Dwarfs 3

3. The Continuing Mystery of Warm Gas Layers 4

C. National Solar Observatory 6

1. SoHO and the Solar Oscillations Imager Experiment Measure Tiny Changesin the Shape of the Sun 6

2. NSO/SP Completes First Observations with Fast 2K x 2K CCD Camera 6

D. US Gemini Program 6

IE. PERSONNEL AND BUDGET STATISTICS, NOAO 7

A. Visiting Scientists 8

B. Hired 8

C. Completed Employment 8

D. Changed Status 8

E. Gemini 8-m Telescopes Project 8

F. Chilean Economic Statistics FY 1996 8

G. NSF Foreign Travel Fund 9

Appendices

Appendix A: Telescope Usage StatisticsAppendix B: Observational ProgramsAppendix C: US Sites Safety Report

I. INTRODUCTION

This document covers scientific highlights and personnel changes for the period 1 October through 31December 1996. Highlights emphasize concluded projects rather than work in progress. The March1997 NOAO Newsletter Number 49 contains information on major projects, new instrumentation, andoperations. The appendices to this report summarize telescope usage statistics, observational programs,and US sites safety reports.

II. SCIENTIFIC HIGHLIGHTS

A. Cerro Tololo Inter-American Observatory

1. Carbon Stars in the Large Magellanic Cloud

Carbon stars (C stars) are asymptotic-giant branch stars having masses perhaps a few timesgreater than the Sun which are seen in a relatively short-lived phase of their post-mainsequence evolution. One needs an extremely large parent population of stars e.g., thecontents of an entire galaxy, in order to find a large sample of C stars to study since anindividual star will only spend a brief fraction of its life as a C star. And fortunately, carbonstars are sufficiently luminous to be studied in nearby galaxies.

Edgardo Costa (U. de Chile) and Jay Frogel (Ohio State U.) have recently reported theirresults of an extensive study of the optical and infrared brightnesses and colors for a sampleof 895 carbon stars in the Large Magellanic Cloud from observations made at CTIO overseveral years. The absence of any very bright C stars in this large sample confirms andemphasizes the results from previous work which was based upon samples of smaller size.This deficiency in bright C stars in the LMC translates into an abrupt cutoff in the luminosityfunction at a bolometric absolute magnitude of Mbol = -6. Either a presently unknownphysical mechanism exists which acts to truncate the evolution of asymptotic giants as theyapproach this limiting luminosity or subtleties in their internal evolution prevent the mostmassive stars (which might be expected to become C stars) from actually following thatevolutionary path.

2. The Interstellar Medium of NGC 55

A detailed understanding of how interstellar gas may be cycled through the disk and betweenthe disk and halo of a spiral galaxy is an important factor in eventually understanding theprocesses of galaxy evolution. There is the potential for a complex interaction between starformation, the energy and momentum input from the winds of young stars and supernovae,the ejection of material from the disk into the halo and the return flow of halo gas back intothe disk.

The galaxy NGC 55, a highly inclined disk galaxy and a member of the nearby SculptorGroup of galaxies, is a unique system for studying the disk-halo interface in a late-typegalaxy at high spatial resolution. Using the CTIO 1.5-m telescope Annette Ferguson andRosemary Wyse (Johns Hopkins U.) and Jay Gallagher (U. of Wisconsin) imaged NGC 55 inlight from emission lines of hydrogen, nitrogen, sulfur and oxygen. Because of the proximityof this galaxy, the images have a spatial scale corresponding to 4 pc per pixel.

A great variety of morphologies are visible in Ferguson, et al.'s images of NGC 55 includingnormal H U regions, loops and plumes protruding typically 1-2 kpc out of the plane of thedisk and diffuse emission throughout the disk and extending out into the halo.

Combining images taken in different atomic transitions, Ferguson, et al. demonstrate thatthere is a continuous trend as one proceeds from regions of high surface brightness to low.The diffuse, low surface brightness gas has oxygen to hydrogen and sulfur to hydrogenemission line ratios that are enhanced by an average factor 2 compared to the bright H IIregions. Both of these results are consistent with the expectations for photoionization of thediffuse medium by a dilute radiation field.

3. Magnetic Activity and Dwarf M Stars

Main sequence stars with masses smaller than about 0.4 of a solar mass make up the class ofdwarf M (dM) stars. Although dM stars are by far the most common and closest stars in thesolar neighborhood, their intrinsic faintness has made dM stars difficult to study in anydetail.

To complete the first detailed spectroscopic survey of the nearby dM stars, Suzanne Hawley(Michigan State U.), John Gizis and Neill Reid (Caltech) used the CTIO 1.5-m to obtainspectra for 317 southern M dwarfs. Combining these observations with data from thenorthern hemisphere, Hawley, et al. use their total sample of 2063 stars to investigate theincidence of magnetic activity in dM stars. As an indicator of chromospheric activity andunderlying magnetic activity, Hawley, et al. choose to use the presence of emission in Ha,i.e., magnetically active stars are the stars that would be classified as dMe.

As had been previously noted by others, Hawley, et al. found the incidence of stellar activityincreased with decreasing temperature (color, spectral type) and mass. By comparing thedMe stars with the dM stars, Hawley, et al. found several empirical differences between thedM and dMe stars in their sample. At spectral type earlier than about M4, dMe stars appearto be 0.5 magnitude brighter and perhaps 0.1 magnitude redder than dM stars of the samespectral type. The dMe stars show variations in the strengths of their Balmer lines ofhydrogen and of the molecular bands of TiO that depend on the level of chromosphericactivity. A kinematic analysis shows that the dMe stars are, as a whole, kinematicallyyounger than the dM stars.

Their relative youth suggests that activity in dM stars, as in the more massive F,G and Kstars, is related to age, possibly via rotation. This is a somewhat surprising result since thesame dynamo mechanism that is presumed to be responsible for producing the activity inmore massive stars should not be operating in these fully convective late M dwarfs.

B. Kitt Peak National Observatory

1. Primordial Helium Revisited

The primordial abundance of helium is a key indicator of physical conditions in the hot BigBang. In the "standard" model of Big Bang nucleosynthesis, the abundances of the lightelements produced near the end of the first three minutes depend on only three physical

parameters: the number of neutrino species, the neutron lifetime, and the ratio of baryons tophotons. The neutron lifetime has been determined experimentally to be around 890 seconds,and further experiments suggest that there are three neutrino species. The recent diversity ofmeasurements of light element abundances, particularly for deuterium, and theirinconsistency with the simplest picture of Big Bang nucleosynthesis have suggested to somethat there is a crisis in the model. Alternatives have been proposed, based on two neutrinospecies or inhomogeneities in physical conditions. Another possibility, however, is that thederivation of abundances from the difficult spectroscopic measurement needs revision.

Y. Izotov (Ukraine), T.X. Thuan (U. of Viriginia), and the late V. Lipovetsky (Russian 6-mObservatory) report in the January 1997, Astrophysical Journal Supplement, on newobservations and interpretation of the primordial helium abundance. No system of purelyprimordial gas, untouched by stellar processing, has been unambiguously identified. Thetechnique is to measure the helium abundances in a variety of locations with differentabundances of stellar processed material, and extrapolate the observed relationship to thevalue for no stellar nucleosynthesis. The authors used a sample of emission-line galaxiesfrom the Second Byurakan Survey to derive abundances from emission lines arising in starforming regions. The galaxies of the sample typically have very low enrichment fromgenerations of star formation, and provide an excellent basis for extrapolating to primordialvalues.

Izotov and collaborators examined a number of systematic effects that would distort thederived helium abundances from their true values. They found that the strongest effect by farwas in the basic atomic physics, through the difference in the physical coefficients predictingthe relative strengths of helium emission lines and the enhancement of those lines throughelectron collisions. The result is a much weaker dependence of helium abundance on theabundances of stellar synthesized elements such as oxygen and nitrogen. The extrapolation tozero then leads to a higher value of the primordial helium fraction of 0.243 by mass, almost10% higher than some recent determinations. That value is essentially consistent with themeasured neutron lifetime and three neutrino species, and with the baryon to photon ratioderived from the current estimate for primordial lithium and the lower values quoted recentlyfor deuterium. This redetermination of the helium abundance weakens the claim of crisis in

the simple Big Bang model, and raises the interest in resolving the wide variance in thecurrent measurements of deuterium.

Izotov and Lipovetsky were scientific visitors at NOAO Tucson for the analysis that theyreported. The support of their projects has led to a series of significant results, that reinforcethe value of such international collaborations.

2. Rotation, Activity, and Evolution of Hyades M Dwarfs

The distribution of rotational velocities in stars of a nearly coeval cluster is the result of theevolutionary processes at work since formation. There is probably a real spread in initialangular momentum for low-mass stars at birth. The presence of a pre-main sequence diskinhibits the spin-up of a star as it contracts. Those stars with short-lived disks may thereforespin up more and arrive on the main sequence as rapid rotators. Young clusters like thePleiades show a large range in rotational velocities for low-mass stars, consistent with thispicture. Stellar winds carry off angular momentum, with more rapidly rotating stars havinghigher loss rates. The range of rotational velocities therefore decreases with increasing age ofa cluster. The older Hyades cluster shows a limited spread of rotational velocities for solar-

type G and K stars. It is interesting to ask what happens to the less massive M stars, whichwould have slower angular momentum loss rates and longer times to contraction onto themain sequence.

J. Stauffer (Harvard-Smithsonian), S. Balachandran (U. of Maryland), A. Krishnamurthi,M. Pinsonneault, and D. Terndrup (Ohio State), and R. Stern (Lockheed-Martin) report in the1 February 1997 Astrophysical Journal on their observations of the rotational velocities ofM dwarfs in the Hyades cluster. They used the echelle spectrographs on the Kitt Peak andCTIO 4-m telescopes for 52 late K and M dwarfs. Their upper limit to detectable rotationalvelocity was 6 km/s. They found that lA of their sample had detectable rotational velocitiesabove that limit, with a maximum velocity of about 25 km/s. That maximum corresponds to amain sequence rotational period of only 18 hours, which is quite rapid. They compared thisresult to theoretical models of regulation of angular momentum by a pre-main sequence diskfollowed by spin-up after the disk dissipates. Disk lifetimes typical for the observed rotationlimits of higher mass stars (of about 1 million years) were consistent with the observedmaximum rotation rate for the M dwarfs, but there could be little angular momentum losscaused by stellar winds. Six of the 48 M dwarfs in the sample were double-linedspectroscopic binaries, which is a higher frequency than found in radial velocity surveys inthe field. The frequency of binaries among solar-type stars in the Hyades is also higher thanthat in the field. It is therefore possible that the frequency of such binaries increases with thedensity of the formation region. Curiously, all of the M dwarfs in binaries are slow rotators,which is not consistent with the early dissipation of the pre-main sequence disks anticipatedin close binary systems.

As seen in field stars, the level of activity of the M stars correlates with rotational velocity.That activity is measured in the chromosphere through the strength of hydrogen Balmeralpha emission and in the corona through the strength of X-ray flux. At high rotationalvelocities, the activity level saturates. The authors found some evidence that their randomlychosen sample of stars does not show a distribution of rotational velocities consistent with arandom draw of inclination angles, but may show a two-branch distribution of high and lowrotational velocities at maximum chromospheric and coronal activity. The authors speculateabout two paths to saturated stellar activity. The rapid rotators would originate as weakT-Tauri stars with disks that dissipated early, but the stars then lost some angular momentumfrom winds. The other path originates from classical T Tauri stars with longer-lived disks.These stars may have slower surface rotation from the disk braking, but stronger differentialrotation, leading to saturated activity levels at slower rotational velocities. The binaries withslow rotation are still curiosities in this context, because they uniformly show high levels ofactivity, but again are unlikely to have long-lived disks.

The drive for echelle spectroscopy on large-aperture telescopes becomes strong for thisproblem through the need to extend these faint star studies to yet later spectral types andmore distant clusters.

3. The Continuing Mystery of Warm Gas Layers

Over 90% of the free electrons in the Galaxy come from a warm ionized layer of gas with ascale height above the disk of some 900 parsecs. The existence of this diffuse material, calledthe Reynolds layer, is well established through measurements of hydrogen recombinationradiation and the dispersion of pulsar pulses that have traversed this medium. The mystery is

the source of ionization of this gas, since the energy requirements are comparable to theenergy released by all Galactic supernovae. A plausible source is the ionizing flux fromO and B stars leaking out of the neutral gas layer in the Galactic plane. Some 15% of thetotal output from the OB stars must escape to higher layers. Determining the physicalconditions in the gas provides diagnostics for the photoionization energy source. The studyof similar warm gas layers in other spiral galaxies should provide further clues to thismystery.

R. J. Rand (U. of New Mexico) reports in the 1 January 1997,Astrophysical Journal on hisobservation of the extended ionizedgas in the edge-onspiral galaxyNGC 891. That galaxy isknown to have a very high rate of star formation in its inner regions, with the X-ray signatureof hot gas ejectedby supernovae extending for kiloparsecs away from its plane. Rand reportson spectra with the Kitt Peak 4-m telescope and RC Spectrograph that were taken at amidplane distance of 5 kiloparsecs from the center of the galaxy, at which conditions aremore quiescent. The spectra recorded three spectral diagnostics to very faint intensities:Hydrogen Balmer alpha, an important helium recombination line (X5876), and the forbiddensingly-ionized nitrogen lines. The line ratios provide the diagnostic of the far and extremeultraviolet energy distribution of the ionizing field. The helium to hydrogen ratio wasmeasured to be 0.034. That value suggests that the gas layer is about 70% ionized and thatthe source of ionization has a significantly stronger extreme ultraviolet to far ultraviolet fluxratio than the source in the Milky Way. The nitrogen to hydrogen ratio peaks at 1.4, whichrequires yet stronger extreme ultraviolet than is permitted by the helium to hydrogen ratio inthe simple photoionization model. The line measurements allow an upper limit to be set onthe temperature of 10-13,000 K depending on location. That value is not yet a sensitiveenough upper limit to resolve the other contradictions, and is considerably above the range of6000-8000 K modeled for the Reynolds layer.

Both the nitrogen and hydrogen were detected to beyond 5 kiloparsecs above the plane. Thedistribution of ionized gas was best fitted by a two-component model, one with a scale heightof around 1 kiloparsec (comparable to that of the Reynolds layer) and the other more diffusecomponent with a scale height of 5-6 kiloparsecs. The gas follows the rotation of the galaxyat small distances above the plane, but shows a decreasing rotation farther from the plane.This effect is qualitatively consistent with models of hot gas being ejected from the plane bysupernova explosions, cooling, and falling back in a galactic fountain. Two physical effectswill force the gas to move radially outward as it is expelled upward: the conservation ofangular momentum as the pull of gravity is weakened by increasing distance, and a gradientin the pressure of gas above the plane. In both cases, the rotation of the gas will decreasewith height. The emission lines may be produced, however, by both warm gas rising and hotgas cooling and falling back, which complicates the picture.

The collection of further information and interpretation is still required, since the elusivesource of ionizing energy has not been unambiguously identified in NGC 891. There is oneimportant caution that we learn about our own Galaxy from studying this neighbor. We mustbe very careful in inferring the location of halo clouds of absorbing gas from their radialvelocities along the lines of sight to stellar and extragalactic probes. The warm gas may notbe rotating on cylinders, and the full complexity of an explosion-induced fountain needs tobe considered.

C. National Solar Observatory

1. SoHO and the Solar Oscillations Imager Experiment Measure Tiny Changes inthe Shape of the Sun

From the constant environment of space, the SoHO/MDI experiment provides researcherswith the longest series of finely detailed electronic images of the Sun that have ever beenobtained. Because the spacecraft is above the blurring effects of the atmosphere, and with thehelp of sophisticated computer analysis, it is possible to measure exceedingly small changesin the shape of the Sun. These changes are caused by "oscillations" analogous to terrestrialearthquakes. Other ground measurements have observed such oscillations before, but neverhave we been able to actually detect fluctuations in the shape of the Sun because of thesesound waves. The SoHO/MDI experiment is able to detect the edge of the Sun move byabout 10 feet. This sensitivity is equivalent to measuring the size of a quarter placed at theedge of the moon as seen from the surface of the earth.

By observing the Sun as it rotates, the MDI experiment has also revealed that the solarsurface is "corrugated." Its surface is covered with hills and valleys about 5 times thediameter of the earth in lateral size, but with a height of only about Vi kilometer. Althoughthe Sun is gaseous, and has no solid surface, these hills and valleys of hot gas rotate with theaverage 27-day solar surface rotation rate. They are probably caused by a complex magneticfield "network" that threads through the visible surface of the Sun.

2. NSO/SP Completes First Observations with Fast 2K x 2K CCD Camera

A new high-speed, high-dynamic-range CCD camera has been developed in collaboration withXedar Inc. (Boulder, Colorado). This instrument was developed for the RISE/PSPT project andused a new Thomson 2K x 2K CCD array. One 2K x 2K camera has been purchased forgeneral use at NSO/SP. We plan to purchase a second such general-use 2K x 2K camera unit asfunds become available.

The first two RISE/PSPT camera units have been received at NSO/SP and have passedpreliminary tests. A detailed performance characterization is currently being performed atNSO/SP. The 2K x 2K cameras have a linear well depth of about 200,000 electrons, with a readnoise of about 34 electrons, when operated at a read rate of 8 million pixels/sec. The cameraelectronics allow a second fiber optic connection to a Sun/SPARC controller that will allow atotal readout rate of 16 Mpix/s. The cameras can also be used in a IK x IK mode using on-chipbinning. The data can be stored to exabyte tape or hard disk. A fast, high-capacity DLT tapedrive will also be available for the 2K x 2K system. The first of these cameras is available on ashared risk basis for observations during the spring 1997 quarter at NSO/SP. The first observingrun, which used the NSO/SP 2K x 2K camera behind the UBF to study acoustic flux events inthe solar photosphere, was successfully completed in January 1997.

D. US Gemini Program

During this quarter, important milestones were passed for two of the first generation Geminiinstruments, the Near-IR spectrograph and the High-Resolution Optical Spectrograph. The Near-IR spectrograph is being designed and fabricated by the NOAO Instrument Project Group. Inmid-October, this instrument passed its preliminary design review. Detailed design work is

proceeding towards a critical design review to be held in October 1997. At a much morepreliminary stage, the High-Resolution Optical Spectrograph completed its conceptual designreview in London, England in November 1996. It is being designed by a group at UniversityCollege, London. The USGP was represented by Sam Barden, who also sat on the reviewcommittee.

Scientific discussions, both national and international, on the operations strategy for the Geminitelescopes took place during this quarter. A meeting of the Gemini Operations Science WorkingGroup refined the processes that are being defined for the data flow through the Geminifacilities, with emphasis on the implementation of queue scheduling and the proposal process. Ithas been decided that the national project offices will have much of the responsibility forcommunity interaction in the operations phase of Gemini. This will include such activities assupporting the preparation of observing proposals, soliciting and evaluating those proposals, andsupporting data reduction and archive access.

Operations were also a major focus of both the US Gemini Science Advisory CommitteeMeeting, and the Gemini Science Committee Meeting, both held in Tucson. In addition toreviewing strategies for operations, these groups developed the plan for the Gemini ongoinginstrumentation program. Preliminary discussions (starting with a US workshop that the USGPheld in August) had led to a "strawman" instrument complement including upgrades, newinstruments, and instruments to be shared with the national observatories of the partner countries.This US perspective was merged with similar plans from the other partners and discussed by boththe US Gemini SAC, and the GSC. The scientific basis for this plan was to be the subject of aninternational workshop in January 1997 with international participation.

The USGP also participated in the meeting of the KPNO/CTIO joint users' committee inDecember. It has been recognized that there must be increasing crosstalk between USGP and theother divisions in order to develop common solutions to common problems. This point was madeby the US Gemini SAC and the joint users' committee, both of which desire to merge parts oftheir activities and discussions.

IV. PERSONNEL AND BUDGET STATISTICS, NOAO

A. Visiting Scientists (visitors who arrived this quarter for a stay of one month or more).

Arrived Name

10/01/96 Sangeeta Malhortra10/13/96 Debi Prasad Choudhary10/30/96 Frank Winkler

11/01/96 Gerald Cecil

11/05/96 Matthias Roeser

11/18/96 Nadege Meunier12/29/96 David Fierry-Fraillon

NOAO Facilitv

Institution Visited

IPAC/Caltech KPNO

Udaipur Observatory NSOfl

Middlebury College CTIO

University of North Carolina NOAO

Kiepenheuer Institute NSO/SP

Observatoire de Paris NSO/T

Universite de Nice GONG

. Hired

Date Name Position NOAO Division10/01/96 C. Jason Pun Research Associate STIS

10/01/96 Ivan Hubeny Associate Scientist STIS

10/14/96 James Rhoads Research Associate KPNO

10/14/96 Mauricio Navarrete Obser. Supp. Spec. 2 CTIO

11/05/96 Ginny Beal Astro Project Coordinator NOAO

11/11/96 Frederic Baudin Research Associate NSO/T

12/02/96 Suzan Ecker Secretary 3 CTIO

C. Completed Employment

Date Name Position NOAO Division

10/18/96 Stephane Courteau Research Associate KPNO

10/25/96 Nancy Burns Technical Writer GONG

11/01/96 Robert Perry Data Reduction Specialist GONG

12/08/96 Jorge Bravo Instrument. Spec. 3 CTIO

12/31/96 Richard Elston Associate Astronomer CTIO

12/31/96 Thomas Kinman Astronomer/Tenure KPNO

D. Changed Status

Date Name

01/07/96 Jack Baldwin

10/01/96 OlinEggen

10/09/96 Suzanne Jacoby

Position

Astronomer, Tenure

On sabbatical until 12/15/96

Astronomer, Tenure

Change from full-time to part-timeEducation Officer

Change from part-time to full-time

NOAO Division

CTIO

E. Gemini 8-m Telescopes Project

Hired

Date

10/01/96

10/15/96

Name

Steven Smith

Mark Hunten

Position

Software EngineerSr. Engineer

F. Chilean Economic Statistics FY 1996

October November December

CPI Change 0.7% 0.4% 0.4%

Cum. Change on CPI FY 1997 0.7% 1.1% 1.5%

Avg. Monthly Peso/Dollar Rate 416.84 419.76 422.82

Monthly Dollars Changed $190,000 $590,000 $420,000

CTIO

NOAO

G. NSF Foreign Travel Fund

For the quarter 1 October through 31 December 1996, a total of $1,273.95 was paid out of the NSFForeign Travel account for visits to the following site and institutions:

OCIW/Las Campanas Observatory, Chile

APPENDIX A

Telescope Usage Statistics

October - December 1996

Astronomical Observations Scheduled maintenance,

instrument tests,

equipment changes,

engineering, etc.Telescope

Hours

Scheduled

Hours Used Hours Lost

Visitors Staff Weather Equipment

4-m 876.5 640.2 96.9 28.0 11.4 100.0

1.5-m 857.8 638.4 40.1 16.2 7.5 155.6

CTIO 1-m 662.1 560.8 -0- 90.1 2.0 9.2

0.9-m 834.4 639.3 51.5 19.0 7.6 117.0

*0.6/0.9-m 697.7 493.4 93.6 53.0 7.7 50.0

4-m 981.0 609.28 122.73 170.0 27.0 52.0

WIYN 3.5-m 441.5 234.44 8.06 110.2 22.8 66.0

2.1-m 1021.0 648.7 15.3 190.25 35.25 131.5

KPNO Coude Feed 624.5 406.03 36.47 139.0 14.0 29.0

0.9-m 973.7 408.3 202.7 267.2 39.5 56.0

Schmidt 365.0 220.5 31.5 111.0 -0- 2.0

Evans Facility 1158.0 111.0 663.0 278.0 19.0 87.0

**FTS Lab 475.0 463.0 -0- -0- 12.0 -0-

Hilltop Dome 1701.0 15.0 1107.0 506.0 73.0 -0-

NSO **McMath-Pierce 1326.5 891.5 178.0 178.5 78.5 -0-

Vac. Tower/SP 790.0 190.0 317.0 169.0 18.0 96.0

Vacuum/KP 466.5 13.0 294.5 152.0 7.0 -0-

Note: Scheduled hours are calculated according to the ephemerides for CTIO:

**

October

November

December

9.9 hours/night;8.9 hours/night;8.2 hours/night.

Use restricted to dark of the moon.

Totals include both day and night hours. All others are day only.

APPENDIX B

Cerro Tololo Inter-American Observatory

October - December 1996: Individual Telescope Assignments are listed below. Graduate students areindicated by an asterisk after their names. Nights assigned (hours worked), and telescope used areindicated. Service Observing programs are denoted by S.O. instead of nights assigned. A total of 66programs were carried out during this quarter.

C. Anguita, M. Ruiz, P. Loyola (U. de Chile): "CCD Parallaxes, Cool Degenerates." 3(27)1.5-m

F. Barrientos*, S. Lilly (U. of Toronto, Canada): "Precision Photometry of Early Type Galaxies in HighRedshift Clusters." 5(48)4-m

M. Belton, B. Mueller, N. Samarasinha (KPNO): "Determination of the Shape and Spin State of46P/Wirtanen." 2(19)1.5-m

L. Berdnikov (Sternberg Astronomical Inst., Russia), D. Turner (Saint Mary's U., Canada): "PhotometricMonitoring of Southern Cepheid Variables." 22(183)l-m

G. Bernstein, D. Smith* (U. of Michigan), A. Tyson, I. DeH'Antonio (AT&T Bell Labs): "The Nature ofthe Dark Matter: Slope of the Cosmic Power Spectrum at 25 Mpc from Weak Lensing." 4(31)4-m

M. Bolte (U. of California, Santa Cruz), C. Mendes de Oliveira (U. de Sao Paulo, Brazil): "TheFormation of the Galaxy and LMC." 4(44)1.5-m

D. Bomans, S. Points* (U. of Illinois): "Star Formation History (SFH) of the Magellanic Clouds."3(25)0.9-m

L. Campusano (U. de Chile), E. Hardy (Laval U., Canada), R. Giovanelli, M. Haynes, D. Dale*,M. Scodeggio (Cornell U.): "Towards a Local Kinematical Reference Frame in Cosmology." 3(23)4-m

B. Carney, M. Habgood* (U. of North Carolina), L. Fullton (STScI), J. Laird (Bowling Green State U.),S. Balachandran (National Air & Space Museum): "°=/Fe] Ratios in Clusters of Different Age and[Fe/H]."2(20)0.9-m

P. Cote, P. Stetson (Dominion Astrophys. Obs., Canada): "The Binary Ionization Rate and TidalDynamics of Globular Clusters." 3(31)4-m

A. Cowley, P. Schmidtke (Arizona State U.), D. Crampton, J. Hutchings (Dominion Astrophys. Obs.,Canada): "Understanding the 'Supersoft' X-Ray Sources." 5(50)4-m

A. Crotts (Columbia U.), S. Heathcote (CTIO): "The Dynamics and Morphology of the Emission-LineNebula Surrounding SN 1987A." 2(18)4-m

A. Crotts (Columbia U.), S. Heathcote (CTIO): "The Formation of Supernova Remnant 1987A: IRImaging." 2(5)4-m

S. Demers (U. de Montreal, Canada), P. Battinelli (Oss. Ast. di Roma, Italy): "3-D Mapping of the Inter-Cloud Region." 4(34)1.5-m

D. DePoy, A. Stephens* (Ohio State U.), J- Elias (KPNO), R. Probst (CTIO): "Infrared Spectroscopy ofProtostar Candidates in the LMC." 3(28)4-m

E. Deutsch*, B. Margon (U. of Washington): "A Systematic Discovery Program for Globular EclipsingBinaries." 13(118)0.9-m

H. Duerbeck (Muenster U., Germany), S. Rucinski (U. of Toronto, Canada), R. Covarrubias (CTIO):"Mini-Survey of Hipparcos Contact Binary Systems in U BV Ic" 2(12)l-m

R. Elston (CTIO): "Stellar Populations in the Most Distant Normal Galaxies." 4(40)4-m

J. Finley (Purdue U.), J. Cordes (Cornell U.), J. Middleditch (Los Alamos National Lab.), M. Ulmer(Northwestern U.): "A Multi-Wavelength Study of the LMC Pulsar PSR 0540-69: CTIO+XTECharacterization of the Crab's Twin." 3(27)1.5-m

J. Frogel, A. Quillen, R. Pogge, D. DePoy, D. Terndrup, K. Sellgren (Ohio State U.), R. Davies (U. ofDurham, UK): "IR and Optical Surface Photometry of Spiral Galaxies: "A Study of Structure and StellarContent." 2(22)1.5-m

D. Geisler (KPNO), J. Claria, A. Piatti (Obs. Astron. de Cordoba, Argentina), H. Dottori, E. Bica(UFRGS, Brazil): "A Search for the Oldest Star Clusters in the Large Magellanic Cloud." 5(45)0.9-m

M. Giavalisco (Carnegie Obs.), M. Dickinson (STScI), C. Steidel, K. Adelberger* (California Inst, ofTech.): "Searching for Galaxies and Clusters at Redshifts z > 3." 3(29)4-m

M. Gregg (Lawrence Livermore Nat. Lab.), M. Drinkwater (Anglo-Australian Obs., Australia):"Multicolor Imaging Survey of the Fornax Cluster of Galaxies." S.O.(20)CS

C. Griffith (Northern Arizona U.), B. Bezard (Obs. de Paris-Meudon, France), M. Marley (New MexicoState U.), J. Lunine (U. of Arizona): "High Spectral Resolution, Near-IR Studies of the Composition andThermal Structure of Brown Dwarf G1229B." 2(14)4-m

P. Guhathakurta, A. Szomoru (U. of California, Santa Cruz), R. Cutri (California Inst, of Tech.),F. Boulanger (Inst. d'Ap. Spat., France), J. Bernard (California Inst, of Tech.): "Wide Field OpticalImaging of the Infrared Cirrus: Probing the Properties of Interstellar Dust." 4(29)CS

D. Hamilton (Max-Planck Inst., Germany), V. Testa (U. of Bologna, Italy): "Stellar Proper MotionSurvey to G = 22." 6(41 )4-m

T. Huard*, D. Weintraub (Vanderbilt U.): "Are Isolated Protostars Born in Bok Globules: A Near-Infrared Survey." 4(37)1.5-m

P. Jablonka (Obs. de Paris-Meudon, France), P. Goudfrooij (ESO, Germany), N. Arimoto (U. of Tokyo,Japan): "The Metallicity of the Old Stellar Population in Spiral Galaxies." 2(17)4-m

M. Joner, B. Taylor (Brigham Young U.): "Consistency and Extension of Strbmgren-p-Ca PhotometricSystems." 6(50) 1-m

M. Keane (CTIO): "Bright Quasars Behind the Magellanic Clouds." 4(36)CS

D. Koo, J. Lowenthal, A. Phillips (U. of California, Santa Cruz): "Near-Infrared (Ks) Observations of anISO Deep Survey Field." 7(59)1.5-m

M. Krockenberger, D. Sasselov, R. Noyes (Center for Astrophys.): "Accurate Distance to the LMC."5(47)4-m, 7(66)1.5-m

A. Landolt (LouisianaState U.): "UBVRI Photoelectric Photometric Sequences."4(35)1.5-m

A. Landolt (Louisiana State U.): "UBVRI Photometry of Standard and Variable Stars." 7(15)l-m

O. Le Fevre, J. Deltorn* (Obs. de Paris-Meudon, France), D. Crampton (Dominion Astrophys. Obs.,Canada), M. Dickinson (STScI): "Clustering Around the Radio-Galaxy 0316-257, at z = 3.14."S.O.(ll)4-m

P. Lu (Case Western Reserve U.). A. Chen*, W. Tsay (National Central U., Taiwan): "Continuation of aSpectrophotometric Study of Faint Dwarf F-Stars at the SGP and Multicolor Photometry of SouthernGlobular Clusters Using BATC 15 Filters." 10(73) 1-m, 3(27)0.9-m

R. Marzke (Dominion Astrophys. Obs., Canada), L. da Costa, V. Alonso (Obs. Nacional, Brazil): "TheColor Dependence of the Local Galaxy Luminosity Function." 10(105)0.9-m

P. Massey (KPNO): "The Evolution of Massive Stars: "Closing the Loop" in the Magellanic Clouds."5(49)1.5-m, l(9)0.9-m

J. Maza, P. Ortiz, M. Wischnjewski (U. de Chile): "Spectroscopy of Calan-Tololo Survey QuasarCandidates." 3(30)4-m

J. Maza, P. Ortiz, M. Wischnjewsky, R. Antezana, G. Valladares, L. Campusano (U. de Chile),M. Phillips, N. Suntzeff, R. Schommer, A. Clocchiatti, R. Covarrubias (CTIO), R. Leiton (U. de LaSerena), B. Schmidt (MSSSO, Australia), B. Leibundgut, J. Spyromilio (ESO, Germany): "A Search forSupernovae in Galaxy Clusters." l(10)4-m, 2(16)1.5-m, 6(56)0.9-m, 11(100)CS

R. Mennickent, J. Arenas* (U. de Concepcion, Chile), M. Diaz (INPE, Brazil): "Testing Models ofDwarf Novae Outbursts by Means of H« Doppler Tomography in VI159 Ori." 4(40)1.5-m

A. Moffat, N. St-Louis, J. Bertrand* (U. de Montreal, Canada), N. Walborn (STScI): "Measuring theMasses of the Most Massive Stars." 5(52)4-m

M. McCall, H. Lee*, R. Ross* (York U., Canada), M. Richer (Obs. de Paris-Meudon, France): "TheEnvironmental Impact of the Cluster Environment on Dwarf Irregular Galaxies." 4(43) 1.5-m

D. O'Donoghue (U. of Cape Town, South Africa), C. Koen (SAAO, South Africa), M. Barstow (U. ofLeicester, UK), D. Sullivan (Victoria U., New Zealand): "Asteroseismology of the Rapidly OscillatingsdB StarPB 8783." 15(101)l-m

in

P. Ortiz, J. Maza, R. Antezana (U. de Chile): "Extensive Search for Quasars with Redshift up to z = 5.0."8(73)CS

J. Patterson, J. Kemp, J. Zimmerman, D. Sanders (Columbia U.), R. Hynes* (U. of Sussex, UK):"Superhumps in Cataclysmic Variables." 17(127)1-m

S. Perlmutter, A. Kim*, G. Goldhaber, I. Hook, M. Kim, R. Pain, D. Groom, R. Knop (U. of California,Berkeley), S. Duestua (Case Western Reserve U.), D. Branch (U. of Oklahoma): "Discovery and Multi-Band Photometry of -10 Type la Supernovae at z = 0.4-0.75: A Measurement of q0." 2(18)4-m

M. Phillips, N. Suntzeff (CTIO): "Observations of SN 1987A at Late Epochs." 2(5)4-m

M. Postman (STScI), M. Strauss (Princeton U.), T. Lauer (KPNO): "Velocity Dispersions of BrightestCluster Galaxies: Bulk Flows to 240 h"1 Mpc." 4(38)4-m

M. Postman, C. Sturch, J. Doggett (STScI), E. Costa (U. de Chile): "The Second Guide Star PhotometricCatalog." 7(62)0.9-m

M. Rubio, J. Garcia (U. de Chile), M. Roth (Las Campanas Obs.): "Near IR Observations of MolecularClouds in the SMC." 5(45)1.5-m

W. Saunders (Edinburgh U., UK), S. Maddox (Royal Greenwich Obs., UK), B. Mobasher (ImperialCollege, UK), B. Tully (U. of Hawaii): "An All-Sky K-Band Tully-Fisher Survey of IRAS Galaxies."3(24) 1.5-m, 2(18)0.9-m

P. Schmidtke, A. Cowley (Arizona State U.), D. Crampton, J. Hutchings (Dominion Astrophys. Obs.,Canada): "Photometry of the 'Supersoft' X-Ray Sources in the Magellanic Clouds." 7(60)0.9-m

C. Smith (U. of Michigan), F. Winkler (Middlebury College), Y. Chu (U. of niinois), R. Kennicutt (U. ofArizona): "The UM/CTIO Magellanic Cloud Emission-Line Survey." 2(19)1.5-m, 7(63)CS

M. Smith (CTIO), J. Kennefick, P. Osmer (Ohio State U.), R. de Carvalho (Observatorio Nacional,Brazil), A. Athey* (Pomona College), E. Friel (Maria Mitchell Obs.): "A Search for Quasars at Redshiftsz > 4.8 using DPOSS and z Band Imaging." 3(25)CS

M. Strauss (Princeton U.), S. Courteau (KPNO), J. Willick (Stanford U.), D. Schlegel (U. of Durham,UK), M. Postman (STScI): "The Bulk Flow in a Shell at 6000 km s"1 from a Fully-Sky Tully-FisherSample." 6(63)4-m, 7(66)0.9-m

C. Stubbs, M. Pratt* (U. of Washington), K. Cook, S. Marshall (Lawrence Livermore Nat. Lab.):"Characterization of Microlensed Stars." 2(16)1.5-m

N. Suntzeff, A. Clocchiatti, R. Schommer, M. Phillips (CTIO), B. Schmidt (MSSSO, Australia), C. Smith(U. of Michigan), M. Hamuy (U. of Arizona), J. Maza (U. de Chile), A. Riess, P. Garnavich, R. Kirshner(Harvard U.), J. Spyromilio, B. Leibundgut (ESO, Germany), C. Stubbs, C. Hogan, D. Reiss (U. ofWashington), A. Filippenko (U. of California, Berkeley): "A Search for Distant Type la Supernovae toMeasure q0." 4(43)4-m, 5(57)1.5-m

IV

N. Suntzeff (CTIO), B. Schmidt (MSSSO, Australia), K. Cook (Lawrence Livermore Nat. Lab.): "A PilotProject to Discover Distant RR Lyrae Variables." 6(52)0.9-m

A. Tyson, I. DeH'Antonio, P. Boeshaar (AT&T Bell Labs), G. Bernstein, P. Fischer (U. of Michigan),D. Smith* (U. of Michigan): "Dark Matter Distribution in Clusters of Galaxies: A Direct Observation."3(26)4-m

P. van der Werf, G. Miley (Leiden Obs., The Netherlands): Confirmation of H°c Emission from 6Galaxies at z = 2.2-2.4." l(7)4-m

A. Walker (CTIO), J. Nemec (Dominion Astrophys. Obs., Canada): "Period Changes for the RR Lyraesin the LMC Clusters NGC 2257 and NGC 2210." 2(14)0.9-m

M. Way* (U. of Missouri), H. Quintana, L. Infante (U. Catolica de Chile): "Core Radii and DynamicalCusps in 4 Abell Clusters of Galaxies." 3(25)CS

A. Zijlstra, J. van Loon* (ESO, Germany), M. Groenewegen (Max-Planck Inst., Germany): "ObscuredCarbon Stars in the Magellanic Clouds?." l(10)4-m

MICHIGAN PROGRAM

C. Smith, M. Tavarez* (U. of Michigan), E. Friel (Maria Mitchell Obs): "Michigan Program."27(216)CS

MACHO PROGRAM

"Macho Program." 2(14)0.9-m

Executed Proposals 10/01/96 - 12/31/96 Page 1 Wed Feb 19 14:44:48 1997

Nights Hours Days Hours2622 0 f96

B Andersson, P Wannier,Jet Propulsion LaboratoryS Federman, University of ToledoB Penprase, Pomona CollegeThe Envelope of the Molecular Cloud B5 III,Temperature ... Coude Feed 6.00 64.00 0.00 0.00

2510 0 f96S Balachandran, University of MarylandJ Carr, Naval Research LaboratoryThe Oxygen Abundance in the Trapezium Cluster

4 meter 3.00 26.00 0.00 0.00 ^

2511 0 f96S Balachandran, R Bell, University of Maryland ""dA Spectroscopic Investigation into the "MissingUV Opacity" Coude Feed 6.00 27.00 0.00 0.00 ^

> >1681 0 f96T Beers, S Hawley, J Tourtellot, H "0Michigan State UniversityA Sarajedini,National Optical Astronomy Observatories

T3O M

> OB Twarog, B Anthony-Twarog, University of Kansas f MDiscovery & Analysis of Extremely Metal-Poor XStars in the.. 2.1 meter 8.00 76.50 0.00 0.00 O

w wCO

w

<

>

O

2568 0 f96M Bershady, D Andersen,Pennsylvania State University

0.9 meter

00 76.50 0.00 0.00

00 6.00 0.00 0.00

M Subbarao, A Connolly, Johns Hopkins University ^Pinning Down the Faint End of the Galaxy _.Luminosity Functio WIYN 0.00 19.50 0.00 0.00

2621 0 f96

M Bershady, Pennsylvania State UniversityS Majewski, University of VirginiaConfirmation of High Redshift Galaxy Candidatesat Bright.. 4 meter 4.00 46.00 0.00 0.00

Executed Proposals 10/01/96 - 12/31/96 Page 2 Thu Feb 20 15:08:22 1997


E Blanton, D Helfand, Columbia UniversityBent Double Radio Galaxies & the Search for

Distant Cluster 2.1 meter 4.00 25.00 0.00 0.00

2449 0 f96

G Bothun, University of OregonT Heckman, Johns Hopkins UniversityR Schommer,National Optical Astronomy ObservatoriesWind Kinematics in Starburst Galaxies with

Extended X-Ray.. 4 meter 4.00 45.00 0.00 0.00

2486 0 f96

R Brunner, A Connolly, A Szalay,Johns Hopkins UniversityGalaxy Redshifts from Broadband Photometry

4 meter 3.00 24.50 0.00 0.00

2502 0 f96

J Chen, University of HawaiiSearching for the Trojan Asteroids BeyondJupiter Burrell Schmidt 3.80 26.00 0.00 0.00

2548 0 f96

R Ciardullo, J Feldmeier,Pennsylvania State UniversityG Jacoby,National Optical Astronomy ObservatoriesPlanetary Nebulae Measurements in NGC 891 and NGC925 4 meter 2.00 22.50 0.00 0.00

2643 0 f96

C Claver,National Optical Astronomy ObservatoriesD Winget, K Winget, University of Texas, AustinCalibrating Stellar Ages: Searching for WhiteDwarfs in... 4 meter 3.90 46.50 0.00 0.00



S Courteau,

National Optical Astronomy ObservatoriesM Strauss, Princeton UniversityJ Willick, D Kasen, Stanford UniversityD Schlegel, University of DurhamThe Bulk Flow in a Shell at 6000 kms-1 fromFull-Sky Tully 4 meter

0.9 meter

2499 0 f96R Cutri, California Institute of TechnologyP Guhathakurta,University of California, Santa CruzF Boulanger, Institut d'Astrophysique SpatialeJ Bernard, Institut d'Astrophysique de ParisWide Field Optical Imaging of the InfraredCirrus: Probing Burrell Schmidt

2482 0 f96

G Da Costa,

Mt. Stromlo & Siding Spring ObservatoryT Armandroff,National Optical Astronomy ObservatoriesC Caldwell, Whipple ObservatoryP Seitzer, University of MichiganCalibration of HST Photometry of the DwarfSpheroidal Galax WIYN 2-hour

4.00 37.00 0.00 0.00

5.00 49.00 0.00 0.00

4.00 21.50 0.00 0.00

0.00 4.40 0.00 0.00

2634 0 f96D Devine, J Bally, University of ColoradoB Reipurth, European Southern ObservatoryThe Interclump Medium & Outflow Shock Statisticsin... Burrell Schmidt 6.00 34.50 0.00 0.00

2544 0 f96A Dey, National Optical Astronomy ObservatoriesJ Graham, University of California, BerkeleyNear-IR Spectroscopy of Extremely Red Galaxies

4 meter 3.00 26.50 0.00 0.00



A Dey, National Optical Astronomy ObservatoriesH Spinrad, University of California, BerkeleyLy alpha Imaging of the Most Distant KnownGalaxy WIYN 2-hour 0.00 4.20 0.00 0.00

2536 0 f96

M Donahue, M Dickinson, M Postman,Space Telescope Science InstituteJ Stocke, University of ColoradoAn Imaging Survey for High Redshift X-RayClusters 4 meter 3.00 1.00 0.00 0.00

2640 0 f96

R Elston,National Optical Astronomy ObservatoriesJ Bechtold, University of ArizonaStar Formation in z=2.3 Damped Lyman-a Galaxies

4 meter 3.80 12.00 0.00 0.00

2450 0 f96

F Fekel, Tennessee State UniversitySpectroscopy of Close Multiple Stars & SpeckleBinaries Coude Feed 6.00 68.75 0.00 0.00

2452 0 f96

F Fekel, Tennessee State UniversityThe Properties of IR-Excess Giants

Coude Feed 6.00 39.75 0.00 0.00

2529 0 f96

L Fullton, E Barrett, D Kramer,Space Telescope Science InstituteE Friel, Maria Mitchell ObservatoryS Balachandran, University of MarylandAre the Old Open Clusters as Old as the YoungestGlobular.. 4 meter 5.00 55.50 0.00 0.00

2462 0 f96

D Geisler, A Sarajedini,National Optical Astronomy ObservatoriesM Lee, University of SeoulW Harris, McMaster UniversityA Modern Survey of the M31 Globular ClusterSystem 0.9 meter 10.50 61.50 0.00 0.00



M Giampapa,National Optical Astronomy ObservatoriesS Baliunas,Harvard-Smithsonian Center for AstrophysicsR Radick, Phillips LabThe Chromospheric Ages & Activity of Solar-TypeStars WIYN 0.00 7.00 0.00 0.00

1944 0 f96

R Giovanelli, M Haynes, D Kornreich,Cornell UniversityMeasurement of Peculiar Velocities of SpiralGalaxies 0.9 meter 12.50 107.50 0.00 0.00

2469 0 f96

P Green,Harvard-Smithsonian Center for AstrophysicsR Saffer, Space Telescope Science InstituteR Napiwotzki, Universitat Sternwarte, KielIR Photometry of Hot White Dwarfs Detected in EUVAll Sky.. 2.1 meter 4.00 35.50 0.00 0.00

2623 0 f96P Hartigan, Rice UniversityD Devine, J Bally, University of ColoradoJ Morse, Space Telescope Science InstituteSpatially Resolved Kinematics of L1551-IRS 5 HHFlow 4 meter 4.00 33.50 0.00 0.00

2475 0 f96T Heckman, J Wang, Johns Hopkins UniversityM Lehnert, Leiden ObservatoryDetermining the Nature of the DiffuseInterstellar Medium.. 4 meter 2.90 36.50 0.00 0.00

2476 0 f96

T Heckman, Johns Hopkins UniversityR Delgado, C Leitherer,Space Telescope Science InstituteStarbursts and the Seyfert Galaxy Phenomenon

4 meter 3.00 33.00 0.00 0.00



R Henry, University of OklahomaK Kwitter, Williams CollegeSulfur and Argon Abundances in Selected PlanetaryNebulae 2.1 meter 3.00 38.50 0.00 0.00

2489 0 f96

L Hillenbrand,University of California, BerkeleyThe Stellar Population of the Orion NebulaCluster: Still T 4 meter

WIYN

2212 0 f96

K Hinkle, R Joyce,National Optical Astronomy ObservatoriesF Fekel, Tennessee State UniversityInfrared Spectroscopy of Late-type Variables inBinary... Coude Feed 4.00 41.00 0.00 0.00

2547 0 f96

I Hook, G Squires,University of California, BerkeleyHigh Redshift Radio-Loud Quasars: Imaging of0.2Jy Radio... 2.1 meter 4.50 53.25 0.00 0.00

2602 0 f96

S Hunsberger, J Charlton, R Ciardullo, A Glenn,Pennsylvania State UniversityOxygen Abundances of Tidal Dwarf GalaxyCandidates in.... 2.1 meter 4.00 34.00 0.00 0.00

2490 0 f96

C Impey, D Norman, University of WashingtonStatistical Gravitational Lensing as aCosmological Tool Burrell Schmidt 6.00 46.00 0.00 0.00

2505 0 f96

R Jameson, S Hodgkin, University of LeicesterN Devereux, New Mexico State UniversityA Very Large Area Imaging Survey of the Pleiadesfor Brown Burrell Schmidt 5.00 61.00 0.00 0.00

2.00 24.50 0.00 0.00

0.00 20.00 0.00 0.00


Nights Hours Days Hours2540 0 f96L Jones, E Perlman, C Scharf,NASA Goddard Space Flight CenterH Ebeling, University of HawaiiG Wegner, Dartmouth CollegeImaging of Candidate Distant Clusters ofGalaxies WIYN 2-hour 0.00 0.30 0.00 0.00

2611 0 f96L Jones, University of North CarolinaB Hufnagel, Michigan State UniversityIntegrated Light of Old Open Clusters

WIYN 0.00 11.00 0.00 0.00

2633 0 f96L Jones, University of North CarolinaF Valdes,National Optical Astronomy ObservatoriesR Gulati,Inter-University Centre for Astronomy/PhysicsM Gregg, Lawrence Livermore LaboratoryA Coude Feed Stellar Spectral Library

Coude Feed 7.00 36.00 0.00 0.00

2637 0 f96

T Kinman,National Optical Astronomy ObservatoriesDoes the Flat Component of Stellar Field HaloExist? 0.9 meter 8.00 87.50 0.00 0.00

2517 0 f96

R Kirshner, P Garnavich,Harvard-Smithsonian Center for AstrophysicsL Wells, University of ArizonaSupernova Light Curves

2.1 meter 1.00 16.75 0.00 0.00

2522 0 f96

R Kirshner, P Garnavich,Harvard-Smithsonian Center for AstrophysicsLight Curves of High Redshift Supernovae

WIYN 0.00 6.80 0.00 0.00

Executed Proposals 10/01/96 - 12/31/96 Page 8

2638 0 f96

A Landolt, Louisiana State UniversityBroad-Band Standards at Declination +45 Degrees

0.9 meter

Thu Feb 20 15:08:22 1997

Nights Hours Days Hours

2590 0 f96

R Lavery, C Kim, Iowa State UniversityDeep Photometry of the Lensing Cluster GHO2154+0508 WIYN 2-hour

2521 0 f96

S Lemley, University of MichiganSpectroscopic Confirmation of Very High RedshiftQuasar.... WIYN

2551 0 f96

W Li, N Evans II, University of Texas, AustinE Lada, University of MarylandR Elston, University of FloridaTesting the Photoionization-regulated StarFormation Model 2.1 meter

2601 0 f96

S Majewski, J Ostheimer, University of VirginiaS Hawley, Michigan State UniversityJ Munn, U.S. Naval ObservatorySpectroscopy of Complete Proper Motion Survey:Phase Space WIYN

2436 0 f96

P Massey,National Optical Astronomy ObservatoriesM Hanson, University of ArizonaMassive Star Evolution as a Function of

Metallicity: What.. 4 meter

2541 0 f96

B McNamara,

Harvard-Smithsonian Center for AstrophysicsB Jannuzi, R Elston,National Optical Astronomy ObservatoriesM Wise, Massachusetts Institute of TechnologyU-Band Polarimetry of Active Central ClusterGalaxies 4 meter

8.00 41.00 0.00

0.00 2.20 0.00

0.00 20.70 0.00

3.80 8.00 0.00

2.00 20.00 0.00

2.80 31.00 0.00

3.00 34.50 0.00

0.00

0.00

0.00

0.00

0.00

0.00

0.00



D Meyer, Northwestern UniversityAn Interstellar Absorption-Line Survey of HeavilyReddened WIYN 2-hour 0.00 3.30 0.00 0.00

2433 0 f96

D Meyer, Northwestern UniversityJ Cardelli, Villanova UniversityProbing the Small-Scale Structure ofHigh-Velocity Gas.... WIYN 2-hour 0.00 3.00 0.00 0.00

2434 0 f96

D Meyer, Northwestern UniversityThe Interstellar Lithium Isotope Ratio Toward X2Ori Coude Feed 7.00 77.00 0.00 0.00

2569 0 f96J Mohr, D Richstone, University of MichiganG Wegner, Dartmouth CollegeAbell 576: 1) Field - Core Transition in GalaxyPopulation WIYN 0.00 12.30 0.00 0.00

2608 0 f96B Mueller, N Samarasinha, M Fishburn,National Optical Astronomy ObservatoriesPhotometric Observations of Comet Hale-Bopp

0.9 meter 1.00 11.00 0.00 0.00

2557 0 f96

F Owen, G Morrison,National Radio Astronomy ObservatoryW Keel, University of AlabamaRadio Sources and the Galaxy Population inCL0024+24 WIYN 0.00 7.00 0.00 0.00

2588 0 f96

S Pak, D Jaffe, L Keller,University of Texas, AustinUV Excited near-IR H2 Emission From NearbyGas-Rich Galax.. 2.1 meter 4.50 27.00 0.00 0.00



B Penprase, Pomona CollegeB Andersson, P Wannier,Jet Propulsion LaboratoryDigital Classification Spectroscopy of StarsToward the... WIYN 2-hour 0.00 1.30 0.00 0.00

2493 0 f96

E Perlman, R Sambruna, L Jones,NASA Goddard Space Flight CenterP Padovani, Universita di RomaP Giommi, ASI/SAXA Deep X-ray/Radio Survey for Blazars

2.1 meter 3.00 24.50 0.00 0.00

2620 0 f96

S Perlmutter, S Duestua, A Kim,University of California, BerkeleyD Branch, University of OklahomaMulti-Band Photometry of -10 Type la Supernovaeat z = 0.4... WIYN 0.00 30.70 0.00 0.00

2619 0 f96G Peters, University of Southern CaliforniaM Plavec, University of California, Los AngelesR Polidan, NASA Goddard Space Flight CenterAccretion and Mass Loss in Algol-Type BinarySystems Coude Feed 4.00 29.50 0.00 0.00

2506 0 f96

D Peterson, SUNY at Stony BrookA-F Supergiants in M31

WIYN 2-hour 0.00 7.50 0.00 0.00

2563 0 f96

R Peterson, University of California, Santa CruzE Green, J Liebert, University of ArizonaHot Stars in Old Open Clusters

4 meter 4.00 43.50 0.00 0.00

2537 0 f96

R Phelps, Carnegie Observatories, (OCIW)E Lada, University of MarylandEvolutionary Status of Embedded Clusters inRosette.... 4 meter 3.90 24.00 0.00 0.00



C Pilachowski, T Kinman, L Davis,National Optical Astronomy ObservatoriesKitt Peak Sky Brightness at Solar Minimum

0.9 meter 1.00 16.00 0.00 0.00

2468 0 f96M Postman, C Sturch, J Doggett, M Meakes,T Borgman, Space Telescope Science InstituteThe Second Guide Star Photometric Catalog

0.9 meter 4.50 46.00 0.00 0.00

2494 0 f96

F Primas, D Duncan, J Truran,University of ChicagoL Hobbs,University of Chicago, Yerkes ObservatoryOxygen, Beryllium and their role in spallativeprocesses Coude Feed 1.00 11.50 0.00 0.00

2498 0 f96

B Rachford, R Canterna, University of WyomingJ Rustman, Colorado CollegeThe Onset of Chromospheric Activity in OpenCluster Stars Coude Feed 6.00 48.00 0.00 0.00

2516 0 f96

R Rand, University of MarylandFurther Spectroscopy of Diffuse Ionized Gas inNGC 891 4 meter 2.00 26.00 0.00 0.00

2438 0 f96

G Rhee, University of Nevada, Las VegasJ Stocke, M Harvanek, E Ellingson,University of ColoradoA Study of 3C Radio Galaxy Environments atIntermediate z 0.9 meter 5.00 51.00 0.00 0.00

2571 0 f96J Rhoads, Princeton UniversityS Malhotra, California Institute of TechnologyDetermining the Nature of the Optical/IRCounterpart of... 4 meter

WIYN 2-hour

3.00 21.00 0.00 0.00

0.00 5.30 0.00 0.00



R Romani, Stanford UniversityTest Observations for A Spectroscopic Search forHigh Redsh WIYN 2-hour 0.00 3.00 0.00 0.00

2606 0 f96

A Sarajedini, D Geisler, R Schommer,National Optical Astronomy ObservatoriesP Harding, University of ArizonaFormation History of Globular Clusters in M33

WIYN 2-hour 0.00 3.30 0.00 0.00

9165 0 f96

A Sarajedini, T von Hippel,National Optical Astronomy ObservatoriesOpen Cluster Photometry

0.9 meter 7.00 44.00 0.00 0.00

2514 0 f96

P Schechter,Massachusetts Institute of TechnologyTime Delay Measurement of Quadruply Lensed QuasarPG .... WIYN 0.00 5.10 0.00 0.00

2545 0 f96

E Smith, NASA Goddard Space Flight CenterC O'Dea, W de Vries,Space Telescope Science InstituteR Gelderman, University of Western KentuckyThe Hubble Diagram and Alignment Effect in YoungRadio.... 2.1 meter 3.90 41.00 0.00 0.00

2472 0 f96

A Stanford, IGPPM Dickinson, Space Telescope Science InstituteP Eisenhardt, Jet Propulsion LaboratoryPushing the Red Envelope: Galaxy Evolution inHigh-z .... 2.1 meter 4.50 49.50 0.00 0.00

2437 0 f96

J Stocke, M Harvanek, E Ellingson,University of ColoradoG Rhee, P Rogers,University of Nevada, Las VegasTesting Unification Scenarios for Radio-Loud AGN

2.1 meter 5.00 58.00 0.00 0.00



J Stocke, T Rector, University of ColoradoHost Galaxies of Radio-Selected BL Lacs

WIYN 0.00 11.30 0.00 0.00

2618 0 f96J Stocke, T Rector, University of ColoradoM Hanson, University of ArizonaIR Spectroscopy of "Featureless" Radio SelectedBL Lacs 2.1 meter 3.67 24.50 0.00 0.00

2626 0 f96

J Stocke, S Penton, J Shull,University of ColoradoThe Local Lya Forest: Determining theRelationship Between WIYN 0.00 11.80 0.00 0.00

9172 0 f96J Stocke, M Harvanek, E Ellingson,University of ColoradoG Rhee, University of Nevada, Las VegasTesting Unification Scenarios for Radio-loud AGN

WIYN 2-hour 0.00 10.60 0.00 0.00

2479 0 f96S Strom, R Makidon, University of MassachusettsL Hillenbrand,University of California, BerkeleyM Adams, McDonald ObservatoryAngular Momentum Evolution of Low Mass Stars

WIYN 0.00 8.40 0.00 0.00

2539 0 f96D Terndrup, A Krishnamurthi,Ohio State UniversityJ Stauffer,Harvard-Smithsonian Center for AstrophysicsS Balachandran, National Air & Space MuseumS Wolff,National Optical Astronomy ObservatoriesCompletion of Key Project to Constrain AngularMomentum... 4 meter 4.00 49.50 0.00 0.00



T Thuan, University of VirginiaY Izotov, N Guseva,

Academy of Sciences of UkraineV Lipovetsky, Special Astrophysical ObservatoryA Search for Low-Metallicity Blue CompactGalaxies in First 2.1 meter 6.00 75.00 0.00 0.00

2457 0 f96

P Winkler, K Ericksen, Middlebury CollegeB Williams,National Optical Astronomy ObservatoriesSpectra & High Resolution Imaging of NewCandidate Super 4 meter 3.00 32.50 0.00 0.00

2613 0 f96

P Winkler, K Ericksen, Middlebury CollegeB Williams,National Optical Astronomy ObservatoriesSpectra & High Resolution Imaging of NewCandidate Super... WIYN 2-hour 0.00 2.50 0.00 0.00

2497 0 f96

S Wolk, F Walter, SUNY at Stony BrookVery Low Mass Pre-Main Sequence Objects in theOrion OBlb A 0.9 meter 1.00 5.00 0.00 0.00

2585 0 f96

S Wyckoff, P Wehinger, A Kader, R Heyd,Arizona State UniversityA Ferro, University of ArizonaAmmonia Abundance & Temporal Variations in CometHale-Bopp 0.9 meter 2.00 22.00 0.00 0.00

2587 0 f96

S Wyckoff, P Wehinger, R Heyd,Arizona State UniversityA Ferro, University of ArizonaMolecular Abundances in Comet Hale-Bopp (C/199501) 2.1 meter 2.00 23.00 0.00 0.00



K Yu, J Bally, University of ColoradoS Stern, Southwest Research InstituteImaging Shock Excited H2 from Embedded JetsDriven by Young 2.1 meter 5.00 54.00 0.00 0.00

2533 0 f96L van Zee, Cornell UniversityUBV Colors & Star Formation Rates of IsolatedDwarf Galax.. 0.9 meter 7.90 63.50 0.00 0.00

2576 0 f96T von Hippel, A Sarajedini, C Mackey,National Optical Astronomy ObservatoriesJ Roche, University of Wisconsin, MadisonWide Field Photometry of Selected Open Clusters:Support of Burrell Schmidt 8.00 63.00 0.00 0.00

Total number of proposals: 93

Appendix BNational Solar ObservatoryOctober - December 1996

1661

Linda Brown Jet Propulsion Laboratory

Toth Jet Propulsion Laboratory

Laboratory Infrared Spectroscopy

FTSLab

1858

William Livingston National Optical Astronomy Observatories

Cycle Variability of the Solar Spectrum

Mc-P Main Main spectrograph

1860

James LoPresto

Pierce

Schrader

Solar Gravitational Redshift

McMP Main spectrograph

Edinboro University of Pennsylvania

National Optical Astronomy Observatories

Edinboro University of Pennsylvania

1862

Oran White High Altitude Observatory

Livingston National Optical Astronomy Observatories

The Sun as a Star: Ca II K Variability


1863

Keith Pierce National Optical Astronomy Observatories

LoPresto Edinboro University of Pennsylvania

The Absolute Value of the Solar Limb Effects for Different Fraunhofer Lines

Mc-P Main Main spectrograph

1928

Charles Chackerian

Giver

Brown

Goularte

NASA Ames Research Center


Jet Propulsion Laboratory


Nights

Temperature Dependence of Oxygen Braodening of Nitric Oxide HN03 Line Intensities

FTSLab

Days Hours

61

54

17

100

1948

Peter Bernath

Ram

Lamb

Huffman

Tinker

Laboratory Spectroscopy of Molecules Found in the Sun

Mc-P Main FTS Lab

University of Waterloo

1964

Rolf Engleman, Jr. University of New Mexico

Germanium Hollow Cathode and Other Emission Spectra

FTSLab

1983

Todd Brown

Daily White Light Patrol

Hilltop Dome Sac Peak

1984

Todd Brown

Daily Flare Patrol




1991

Ernest Hildner National Oceanic & Atmospheric Administration

November National Optical Astronomy Observatories

H-Alpha and Ca K Spectroheliograms

Evans Facility Sac Peak

1997

Frank Hill National Optical Astronomy Observatories

Harvey National Optical Astronomy Observatories

Bachmann Birmingham-Southern College

Niedbala Birmingham-Southern College

Measurement of High-Degree Solar Oscillations Frequencies

KPVT High-L

2016

Matt Penn

Guhathakurta

Fisher

One-shot CCD Camera Testing



NASA/Goddard Space Flight Center


Nights Days Hours

48

48

91 509

91 517

49

18 23

54

2018

Joe Elrod

Ceolostat Activity Monitor


2019

Todd Brown



Coronagraph Activity Monitor


2020

Joe Elrod

Brown

Maintenance - General


2025

Christoph Keller

Rabin

Jaksha

NIM-2 Engineering


2029

Roberto Falciani

Smaldone

Cauzzi

Balasubramaniam

Keil






University of Florence

University of Naples

Osservatorio Astronomico di Capodimonte


USAF/PL/GPSS

Dynamical Studies of Minor Solar Activity Phenomena

KPVT Spectromagnetograph

2032

Donald Jennings NASA/Goddard Space Flight CenterMcCabe NASA Goddard Space Flight Center

Reuter NASA/Goddard Space Flight Center

Sada NASA Goddard Space Flight Center

Observations of Comet Hale-Bopp in the near- and mid-Infrared


Nights Days Hours

62 224

42 80

16 80

21 86

13

22

2033

Donald Jennings

McCabe

Deming

Sada


NASA Goddard Space Flight Center

NASA/Goddard Space Right Center

NASA Goddard Space Right Center

Observations of Jupiter and Saturn in the near- and mid-Infrared


2034

Jack Margolis Jet Propulsion Laboratory

Foreign Gas Broadening of Methane Absorptions

FTSLab

2036

Richard Altrock USAF/PL/GPSS

Three Line Coronal Photometer


2037

Steven Keil

Worden

Ca K Solar Rotation


2041

Jeffrey Kuhn

Lin

Keil

Gullixson

IR Coronal Spectroscopy


2042

Steve Hegwer

Armstrong

Wilkins

Stauffer

Gilliam

V IT Maintenance

Vacuum Tower TelVSP Sac Peak

USAF/PL/GPSS

USAF



USAF/PL/GPSS







Nights Days Hours

20

86 125

59 182

10 40

90

2043

Steven Keil USAF/PL/GPSS

Balasubramaniam National Optical Astronomy Observatories

Gullixson National Optical Astronomy Observatories

USAF Infrared Vector Magnetograph Project Engineering

Vacuum Tower Tel./SP Sac Peak

2044

Thomas Rimmele

Radick

Dunn

Wavefront Sensor Tests



Phillips Lab/Solar Research Branch





2046

Haosheng Lin

Kuhn

Rimmele

IR Polarimetry


2047

Krishna Balasubramaniam

Cauzzi

Falciani

Keil

Smaldone


Osservatorio Astronomico di Capodimonte

University of Florence

USAF/PL/GPSS

University of Naples

Dynamical Studies of Minor Solar Activity Phenomena


2048

Gordon Love USAF Phillips Laboratory

Radick Phillips Lab/Solar Research Branch

Rimmele National Optical Astronomy Observatories

Active Image Correction of the Vacuum Tower Telescope


2049

Bruce Lites High Altitude Observatory

Skumanich High Altitude Observatory

Bommier Observatoire de Paris

Magnetic Fields of Solar Prominences


Nights Days Hours

8.75 50

13 90

12.25 74

15 15

55

33

Nights

2053

Robert Field Massachusetts Institute of Technology

Clevenger Massachusetts Institute of Technology

Coy Massachusetts Institute of Technology

Vibrational Dynamics of Ammonia: New Analysis Methods

FTSLab

2055

Dennis Reuter NASA/Goddard Space Flight Center

Sirota Univ. of Maryland Baltimore County

Hillman NASA/Goddard SpaceFlightCenter

Laboratory Spectra of Molecules of Planetary Interest

FTSLab

2056

Drake Deming NASA/Goddard Space Flight CenterMoran NASA/Goddard Space Flight Center

Jennings NASA/Goddard Space Flight Center

Solar Magnetic Studies Using Fabry-Perot Spectroscopy of the 12-Micron Mgl Line

FTSLab

2057



Bartol Research Institute

Solar-stellar Oscillation Studies

McMP Stellar spectrograph

Christoph Keller

Harvey

Jefferies

2059

Peter Bernath

Hinkle

Rabin

Phoenix Engineering


2060

Klaus Strassmeier

Weber

Washuettl

Kiirster

University of Waterloo



University of Vienna




Time-series Doppler Imaging of Stellar Surface Structure

McMP Stellar spectrograph

60

Days Hours

48

69

105

32

120

634.50

2063

Thomas Ayres

Rabin

Hill

University of Colorado, CASA



Coordinated SOHO/NSO Observations of Acoustic Waves and the COmosphere


2065

Jack Margolis Jet Propulsion Laboratory

Characterization of Correlation Spectroscopy Grating

McMP FTS/Mc-P

2068

Thomas Rimmele

Stauffer

Wilkins




Correlation Tracker Test


2070

John Varsik

Altrock

Stauffer

Smartt


USAF/PL/GPSS



Emission-Line Coronal-Loop Studies


2071

Steve Hegwer

Elrod

Brown

Armstrong

Gilliam

Daily Sunspot Drawing







Nights Days

1.2

14

66

0 02073

Don Neidig

Svestka

Cliver

USAF/PL/GPSS

Space Research Organization

PL/GPSG

McKenna-Lawlor St. Patrick's College

Investigation of the Flare Nimbus Phenomenon, I: Effect of Filter Transmission Profiles on the Appearance of the


Hours

30

33

2074

Krishna Balasubramaniam National Optical Astronomy Observatories

Keil USAF/PL/GPSS

Rimmele National Optical Astronomy Observatories

High Resolution Structure and Mass Rows in Filaments


2075

Serge Koutchmy Paris Institut d'AstrophysiqueGeorgakilas National Observatory of Athens

Delaboudiniere Institut d'Astropysique Spatiale CNRS,

Shibata NAOJ

Suematsu National Astronomical Observatory

Observation of Polar Chromospheric Activity and Spikes


2081

Roger Angel

Hege

U of A IR Observations

McPE Main spectrograph

Steward Observatory

University of Arizona

2087

Serge Koutchmy Paris Institut d'AstrophysiqueGeorgakilas National Observatory of Athens

Observation of Polar Chromospheric Activity and Spikes


3790

Vacuum Synoptic Program: Daily/Community

KPVT Spectromagnetograph

Nights Days Hours

35

8.5 49

64

90 271.50

APPENDIX C

US Sites Safety Report

Following is the summary of recordable occupational injuries and illnesses for the US sites as reportedon the respective CY 1996 OSHA 200 logs. As required, the respective data will be posted at each site nolater than 1 February.

Fatalities

Injuries involving days off or daysof restricted work activity or both

Injuries involving days off

Days off from work

Days of restricted work activity

Injuries without lost workdays

Illnesses

Illnesses without lost workdays

Total recordable injuries/illnesses:

KPNO NSO/SP Tucson Total

3 0 2 5

3 0 2 5

1 0 127 138

0 0 1 1

0 0 0 0

0 0 0 0

0 0 0 0

3 0 2 5

Compared to last year, NOAO experienced a decrease in the number of recordable injuries, from 8 to 5.However, there was an increase in the average lost workdays, from 6.9 to 27.6 per person. This increasewas mainly due to one back injury which resulted in 126 lost workdays. Illnesses decreased from 2 to 0.

The types of injuries broke down as follows:

Sprain/strains (back)Slips/falls

NOAO Accident/Illness Cases -1996

5 Total Recordable Cases

13 Total Non-Recordable Cases

1

4

5

Recordable Accidents/Illnesses

Note: Injuries are recordable when they are work related and when they involve one or more of thefollowing factors: medical treatment (other than first aid); loss of consciousness; restriction of work or

motion; transfer to another job. Illnesses are always recordable when they result from an exposure in thework environment.

S. Mendez-strained back in process of lifting a box onto scale. Existing back problems exacerbated bythis incident. He has retired on disability. 126 lost workdays.

R. Ramon-bruised/strained leg; in process of filling salad bar, she slipped and fell on wet floor. 4 lostworkdays.

V. Garcia-cut/infected finger; in process of dividing posters, she cut her finger on the edge of a poster. 1lost workday.

Z. Hudson - bruised hip and thigh resulting from a slip/fall due to oil on the floor in the automotivegarage. 6 lost workdays.

L. Sanou - sprained ankle as she slipped and fell while walking in hallway. 1 lost workday.

Non-Recordable Accident/Illnesses

B. Moore-contusion to left knee. She was going down stairs, tripped or missed the last step and fell landingon her left knee. No lost workdays.

J. Kennedy-back strain; in the process of deplaning with carry on luggage in hand, he felt pain in hisback. No lost workdays or medical attention.

C. Baker-low sugar attack (fainted); likely caused by under/over medication for her diabetes. No lostworkdays and not work related. TFD paramedic was called.

D. Rosin - punctured finger; while reaching for calendar to change month, hand brushed against woodshelf divider catching wood sliver in finger. No lost workdays.

A. Zaki - cut on arm; was exiting bus, lost balance and cut arm on divider/handrail. No lost workdays.

M. Rhoades - cut on head; in process of preparing wood chipping machine for return to rental agency,chute struck top of head. No lost workdays.

C. Baker - sprained back, bruised leg; tripped over curb on way to lunch. No lost workdays.

R. Good - bruised knee; slipped and fell on wet concrete porch slab. No lost workdays.

J. Stein - lacerated finger on a large aluminum chip he was removing with his hand while jig boring adeep hole in a piece of aluminum. No lost workdays.

J. Scott - punctured foot; stepped on a board with nail turned up. No lost workdays.

J. Stuart - sprained wrist; slipped on wet spot in hallway and fell. No lost workdays.

T. Tilleman - sprained ankle when she hopped down a 2-foot step in the McMath-Pierce telescope tunnel.

S. LaFayette - temporary weld flash in both eyes, caused by improper lense shade while heliarc weldingaluminum. No lost workdays.

Enviable Safety Record:

NSO/SP achieved an enviable and well deserved safety record: no reported accidents.

Fire Alarm System:

The antiquated fire alarm system in the Tucson facility main Computer Room was replaced with a state-of-the-art system.

Fire Prevention - Brush/Tree Removal:

An extensive brush-tree removal effort was carried out at KPNO. This was a much needed preventivemeasure to reduce the risk of a wildfire destroying major facilities. The majority of the work was done bythe fire crews from the BIA/Tohono O'Odham Wildfire Management at no cost to NOAO. KPNOassisted with loading and hauling off the cuttings.

In conjunction with this a document titled "Wildfire at Kitt Peak National Observatory" was producedfor information and training purposes. It describes in detail what KPNO's and the responding agencies'role would be in the event of a wildfire.

Department of Labor/BLS Statistics Survey:

A mandatory survey of the 1995 occupational injuries for the KPNO and Tucson Sites was prepared andsent to the Arizona Industrial Commission.

Loss Prevention Surveys/Reviews:

Various surveys/reviews were conducted and the resultant recommendations furnished in regards to thefollowing:

4-m shutter DC drive motor and controller.

Transporting and handling MOSAIC and Phoenix instruments.

8-m Safety Program Plan and Procedures for construction activities at the Mauna Kea andCerro Pachon Sites.

Procedures for removal of a 100 foot antenna tower (formerly used for communicationsbetween the Tucson and CTIO sites.

Personnel access to top of WIYN dome for snow and ice removal from shutter.

Safety Plan for 4-m Shutdown.

Plan for visitor access to the McMath-Pierce Telescope.Safety specifications for construction of the EOS Observatory at KPNO.

Gemini Safety Policy for Instruments.

General survey of NSO/SP facilities and safety program.

Fall protection procedures when installing/removing MOSAIC at 4-m.

Fire Prevention at the US Sites.

Training:

NSO/SP maintenance personnel received training and recertification in asbestos handling and abatement,including refresher training in the use of respirators.

Several KPNO and NSO/SP staff members received fire and emergency medical training.

iii

Approximately 75% of the NSO/SP staff members received training in Right-to-Know/chemical hazardcommunication.

The KPNO fire alarm maintenance person received training in the operations and maintenance of theirnew mountainwide fire alarm system.

CTIO Safety Report

CTIO Recordable Occupational Injuries: Calendar Year 1996

Fatalities: 0

Injuries involving days off or days of restricted work activities or both: 2Injuries involving days off: 2Days off from work: 0Days of restricted work activity: 15Injuries without lost workdays: 0Illnesses 0

IV

Documents

OPTICAL ASTRONOMY OBSERVATORIES Q1...QUARTERLY REPORT OCTOBER -DECEMBER 1996 February 20,1997. I. INTRODUCTION II. SCIENTIFIC HIGHLIGHTS TABLE OF CONTENTS A. Cerro Tololo Inter-AmericanObservatory