National Optical Astronomy - noao.edu Q3... · Cepheids in M101, agalaxy of fundamental importance to the extragalactic distance scale. M101 contains a number of red supergiants,

NationalOpticalAstronomyObservatories

National Optical Astronomy Observatories

Quarterly Report

April - June 1986

I. INTRODUCTION

NOAO management's efforts during the third quarter were focussed on completingthe FY 1987 Preliminary Program Plan for review by AURA and submission to theNSF by 30 June 1986. The FY 1987 Preliminary Program Plan espouses adifferent approach to operating NOAO, one to which we have been led through asuccession of substantial program reductions made necessary by fundingconstraints. Specifically we have attempted to provide for new starts in NOAOwhile retaining our essential base elements—telescope operations,instrumentation, and in-house science—all intact and vital. An additionalstep in this process was that of further defining what NOAO's options will beshould there be further budget reductions in FY 1987 in response to Gramm-Rudman-Hollings (GRH) legislation to reduce the national deficit.

During this quarter the method of handling instrumentation and projects inTucson was restructured. There were three components to the change: (1)ETS/Tucson was restructured, (2) a steering committee was identified for eachof several areas of instrumentation, and (3) a committee was formed to adviseNOAO management on overall priorities. The Project Management Office (PMO)continues, in coordination with ETS, to furnish cost and manpower estimatesfor the development of project proposals. PMO also provides project planning,reporting and management functions to assist in monitoring the implementationof established priorities.

II. SCIENTIFIC HIGHLIGHTS

A. Cepheids in M101.

K. Cook and M. Aaronson (U. Arizona), and G. Illingworth (ST Scl) havereported (Ap. J. Letters, 301, L45, 1986) the first definite detection ofCepheids in M101, a galaxy of fundamental importance to the extragalacticdistance scale. M101 contains a number of red supergiants, which have beenproposed as standard candles on the assumption that they have a maximumluminosity of My 8 independent of the luminosity of the parent galaxy.

The Cepheid observations were carried out with an 800 x 800 TI CCD at theprime focus of the KPN0 4-m telescope. To date, this observing team has atleast six epochs of observations in the R filter for four regions in M101.Preliminary analysis indicates that the distance modulus for M101 is in therange 29.0 - 29.5. If further observations substantiate this result, then italso follows that the luminosity of the brightest M supergiants depends on theabsolute magnitude of the parent galaxy, thus limiting the usefulness of thesestars as distance indicators.

B. Globular Clusters in NGC 5128.

J. Hesser (DAO), G. Harris (Waterloo), and H. Harris (USNO) have studied theglobular clusters associated with the peculiar radio galaxy Cen A (NGC 5128),and have obtained the first information regarding its old stellar halocomponent. Their results, from direct CCD images and spectroscopy, are thefollowing:

a) A large cluster system, numbering more than 1500, has beendiscovered, supplanting long-held beliefs that this large ellipticalwas devoid of globulars.

b) For radii greater than 4', a r1/4 surface brightness law holds.There is either a large deficiency of clusters for r <. 4', or ther ' law slope is lower for the globulars than the bulge light.

c) Over the 5 mag range observed, the dispersion in the luminosityfunction is o» 1.2 mag, which is roughly the same as that observedfor M31 and the Galaxy.

d) The distance to Cen A implied from the cluster luminosity function israther small, d » 3.3 Mpc.

One of the more interesting results concerns the radial velocities: while thegalactocentric velocities of the 10 outermost globulars are roughly the sameas the bulge light, the velocities of the 25 innermost clusters are 130 km/seclarger than the background halo light. That is, the innermost clusters of NGC5128 appear to be receding from it! These inner clusters are also redder,i.e., more metal rich, and it thus appears that they might be explained interms of a merger.

C. Probing the Homogeneity of the Interstellar Medium.

The brightness temperature of the microwave background at moderate redshifthas been studied by D. Meyer (U. Chicago) and I. Hawkins (UCLA) fromexcitation of the CN lines at A3824 A. High signal-to-noise spectra of the CNlines in the star HD154368 will, after an analysis, set limits on thetemperature of the background, and any departures from a Planckiandistribution. In addition, the precise C/ C isotope ratios derivable fromobservations of the CH+ and CH+ lines provide unique opportunity to probethe homogeneity of the interstellar medium (ISM) and the history ofnucleosynthesis in the Galaxy. The CH+ molecule does not suffer from chemicalfractionation and isotope photodissociation and excitation that make the

C/ C ratios derived from radio observations of CO and other species

difficult to interpret. By observing the strong CH+ lines towards distantstars, Meyer and Hawkins are comparing C/ C ratios at differentgalactocentric distances. In particular, their C/ C abundance gradientwill be compared with that obtained from radio observations. The resultinggradient will place stringent constraints on the homogeneity of the ISM, andon the models of galactic chemical evolution by determining the amount ofstellar processing that has occurred in the ISM since the formation of theSun.

D. Solar Rotation from Oscillation Data.

F. Hill (NOAO) has completed the analysis of two sets of full disk oscillationobservations, acquired by entirely different instruments, which proveconsistent with each other. A three day run with the Applied PhysicsLaboratory Fabry-Perot Filter gave a power spectrum where the splittingbetween prograde and retrograde modes leads to well-defined rotation rates. Adecrease in rate is inferred over depths of 15,000 to 50,000 km below thephotosphere. This is in agreement with the Duvall and Harvey results.

Hill also re-analyzed 1981 data taken with the Sacramento Peak echellespectrograph and old diode array. These data yield rotation rates over theouter 16,000 km and connect with the Fabry-Perot analysis. Previously thissame data set had suggested variable rates from day to day. But thisvariability is now ascribed to beating between unresolved modes. The inferredrate increase below the surface can be used to explain the higher rate thathas always been found for sunspots, assuming that these objects have theirroots in the hydrogen ionization zone.

All of this seems to hold together quite nicely in that two data sets arequite consistent with each other and with a third. The rise to a maximum canexplain the faster sunspot rotation rate but requires the pushing to occurquite close to the photosphere. The maximum occurs in the hydrogen ionizationzone, which is also presumed to be the region of driving for thegranulation. It may be that granulation is turbulence produced by shearinstabilities, or perhaps the maximum in the rotation rate is produced by thedriving of the granulation.

There are two major caveats to this pleasing scenario, however. The first isthe unexplained discrepancy in the surface rates. This discrepancy was notedin Hill's study of the surface rate inferred from the /-mode and cannot be

explained by a scale error in the spatial dimension. The second caveat is thefailure to obtain any sensible, let alone consistent results from a differentinversion technique (spectral expansion). The spectral expansion appears towork on artificial data, but does not work on this real data set. It iscurrently unknown whether there is a problem with the code, or whethersystematic errors exist in the data which dominate the results.

E. Solar Magnetic Flux Tubes.

In the solar photosphere, magnetic flux is concentrated into flux tubes whichhave field strengths of the order of a kilogauss and diameters well below anarcsecond. These flux tubes are the fundamental magnetic structures thatcombine to form pores, sunspots, the coarse network and active regions. Twobasic methods for investigating the properties of these flux tubes are beingpursued: direct imaging (with sub-arcsecond resolution) and precision Stokesspectroscopy (with coarser spatial resolution).

J. Stenflo and S. Solanki (Inst. f«r Astronomie, Zurich), and J. Harvey (NOAO)have a paper in press that reports on their analysis of Stokes spectra ofspatially-unresolved flux tubes. In May 1984 they observed ten solar regions,distributed across the solar disk, with the Fourier Transform Spectrometer onKitt Peak over the spectrum range X4880 - 6000 A. They analyzed a smallsubset of these data to explore their utility for studying magnetic fluxtubes.

The center-to-limb variations of different Stokes line-ratio parameters, andthe asymmetry between different components of a linearly-polarized spectrumline, suggest a decrease of flux tube field strength with height above thephotosphere. Moreover, the temperature difference between the interior andexterior of the flux tubes, at the same optical depth, decreases withheight. However, the correspondence between altitude and center-to-limbvariation of the line profiles must be derived from future radiative transfercalculations.

Mass motions within flux tubes affect the amplitude and area asymmetry, aswell as the Doppler shift of the Stokes "V" profile. The absence of a Dopplershift suggests that these mass motions are not stationary.

III. PERSONNEL

A. Visiting Scientists.

The following visitors arrived at NOAO facilities for periods of one month ormore during the April 1 - June 30, 1986 quarter.

date arrived

4/01/86

5/01/86

5/07/86

5/14/866/13/86

6/15/86

name

William Jeffrey

Paul Hintzen

Julie Lutz

Thomas Lutz

Michael Rich

Linda French

institution

NOAO facilityvisited

Harvard Smithsonian Ctr.

for Astrophys. NSONASA-Goddard Space Flight Ctr. KPNOWashington State Univ. CTIOWashington State Univ. CTIOUniv. of California, Santa Cruz CTIO

Massachusetts Inst, of Tech. CTIO

The following summer research assistants arrived at NOAO during this quarter.

date arrived

5/12/86

5/16/86

5/20/86

5/22/86

5/27/865/27/86

6/02/866/02/86

6/03/866/03/86

6/09/866/09/86

6/09/866/11/86

6/16/86

name

Andrea Dobson-Hockey

Kelley McDonaldKaren Scott

Hartmut Grosser

Mark Elowitz

Robert Parker

Issac Chen

Michelle Fitzurka

Sophie RemyRobert Ronan

John Booth

Amy Mossman

Robert Smith

Eberhard Pehlemann

Tzuu-Huey Guo

NOAO facilityinstitution visited

New Mexico State Univ. NSO

Univ. of Oklahoma NSO

Pomona College KPNO

Universitats-Sternwarte,West Germany NSO

Univ. of Arizona NSO

Grinnell College NSO

Beloit College NSO

Loyola College CCS

Univ. of Paris NSO

Harvard Univ. NSO

Wesleyan Univ. KPNO

Wellesley College NSO

Indiana Univ. KPNO

Universitats-Sternwarte,

West Germany NSO

Ohio State Univ. NSO

B. New Appointees.

The table below shows details of new appointments made to the NOAO during thequarter, April 1, 1986 - June 30, 1986.

date of appointment name position5/01/86 Claude Roddier Scientist ADP6/23/86 Kent Doggett Sr. Associate-In-Research NSO

NOAO division

C. Terminations.

date

4/11/865/30/86

6/13/866/13/86

name

Robert NagelDonald Hayes

Thomas McCurnin

Ker-li Shu

position NOAO division

Department Manager NOAO

Assistant Support Scientist KPNO

Project Manager NSO

Senior Engineer ADP

IV. INSTRUMENTATION AND NEW PROJECTS

A. Advanced Development Program.

In the past three months we have proceeded with our plan to control thesurface of a borosilicate honeycomb mirror by controlling, (a) the thermalgradients and, (b) the support forces. The 1.8-m prototype mirror wasmeasured in four separate ventilation tests, with airflow rates of 0, 1, 2,and 3 mirror masses/hour. While there is a systematic temperature differencebetween ventilated and unventilated cavities in the mirror, there is nosignificant improvement in the surface for flow rates above one mirror

mass/hour. After this test was done, we disassembled the mirror setup toinstall 240 thermistors (compared to the 54 we had been using) for morethorough monitoring of the glass surfaces. We are also installing forceactuator mechanisms at 16 locations, to compensate for distortions caused bythermal gradients and gravity. A computer model predicts what the mirror'sresponse should be. With funds from a contract with the Rome Air DevelopmentCenter, we are designing a new optical test that uses a CCD camera for realtime analysis of Hartmann exposures.

At the University of Arizona mirror casting facility the large furnace isbeing built for the first spin-casting of a 3.5-m borosilicate blank. Thefurnace wall sections and lid have been welded and orders are being placed forparts and materials such as hearth plates, electrical power boxes, and heaterpanels. The first three batches of E6 glass have been received from Ohara(Japan). This blank is slated for use in the 3.5-m telescope planned by theAstrophysical Research Consortium.

The NOAO analysis of the structure of the NNTT has continued, with a firstiteration to optimize the design of the optical support structure. The goalsof this optimization are to reduce the moving weight, minimize the secondarymirror excursions under the influence of gravity, increase the overallstructural stiffness, and insure that no structural members areoverstressed. The secondary mirror excursions have so far been reduced by afactor of two, still not enough to do away with the need for activeadjustments.

The working groups for the first complement of NNTT instrumentation havefurther specified the designs of the infrared instruments. The IRImaging/Photometry camera report is nearly finished. The High-Resolution IRSpectrograph will be much more complex and has not yet been thoroughlydesigned, but a layout is now on paper. Both designs may be changed as IRarray detectors become better defined.

In the NNTT Site Evaluation Project, recent work has centered on the processof reducing and summarizing all of the site-testing data from Mauna Kea andMt. Graham. Much of the data-reduction had been done while testing was inprogress, but some work remains on the seeing data and the intercomparisonbetween Echosonde and mlcrothermal measurements. We set ourselves the goal ofcompleting our report by September 30. In this report, NOAO management willarrive at a recommendation concerning the NNTT site; we will then present itto an outside committee (to be chaired by Art Hoag) for a thorough review.The NNTT group and other members of the NOAO staff participated in an

international conference on "Identification, Optimization and Protection ofOptical Telescope Sites," in Flagstaff, May 22-23. This conference was heldin honor of Art Hoag, who retired as Director of Lowell Observatory on June30.

The new adaptive mirror kinematic mount was completed and tested during thisquarter. With this mount, the mirror exhibits a 145 Hz resonance when movedas a piston. This is not expected to affect the utility of the mirror for theadaptive optics project. The mirror was tested at temperatures down to ~15° Fto simulate mountain nighttime conditions. The best static mirror figure wasat ~65° F, where the figure was flat to better than V2 wave. At 40° F, thefigure was distorted globally about three waves, with individual distortionsabout each actuator of one wave. These distortions were roughly doubled at15° F. At 40° F, the manual control panel was used to adjust each actuator toflatten the mirror to better than V2 wave.

A preliminary design of the tip-tilt mirror for the system was begun and therequired actuators ordered.

Initial tests of the Varo image tube were completed. The tube showssatisfactory gain and uniformity. We were surprised by the longer-than-expected decay time of the P-37 phosphor (~10 microseconds). The Varo highvoltage power supply failed and was returned to Varo for replacement orrepair.

Work was begun on the development of a different type of adaptive mirrorutilizing a monolithic PZT layer to induce bending moments in the opticalsurface of the mirror.

For potential use in the NNTT Infrared Camera, we have examined the propertiesof grisms for infrared observations. For wavelengths up to 2.8ym,conventional grisms can be used, combining a CaF~ prism as a substrate with areplicated transmission grating. At longer wavelengths, the grating resinabsorbs the IR radiation and different techniques have to be used. We arebuilding a resin grism for the J, H, and K bands to be used for the SBRC IRimager, to give a spectral resolution R = 150. We will also experiment withdirect ruling of a grism in ZnSe material (See ADP R&D Note 86-2).

CaF2 optics have been designed and procured to be used in front of the SBRC IRarray to give the magnification needed to do speckle imaging in the 1.5 - 5vanwavelength region. These foreoptics will be included in a mechanical modulewhich will be inserted between the 4-m Cassegrain focus and the SBRC IRimager. The first observing run is scheduled for January 1987.

We have successfully reconstructed one-dimensional IR images from speckle datausing a new technique called triple correlation. We have shown that triplecorrelation is theoretically related to phase closure techniques and thereforeshould be insensitive to telescope aberrations.

On the basis of laboratory results obtained with a broad-band interferometerwhose two arms each have a single-mode fiber optic, we believe that longbaseline astronomical interferometry will be feasible using single-mode fibersas waveguides. Dispersion and temperature effects are easily corrected, andpolarization-preserving fibers solve the time and wavelength dependent

polarization problem. Theoretical calculations show that couplingefficiencies up to 74% are possible in perfect seeing, and that rapid imagestabilization can double throughput in moderate seeing.

B. Instrumentation Projects.

There were currently twenty-three instrumentation development and improvementprojects active in Tucson during this quarter. Four projects, the McMathWindscreen, Fourier Tachometer (FY 1986 segment), the Supercomputer Antennaand hardware link, and the McMath Stellar Improvements (FY 1986 segment) werecompleted during the third quarter of FY 1986.

Projects in various stages of completion include the NOAO InfraredInstrumentation Project being conducted jointly between the ETS group atTucson and CTIO. Work is progressing for each section as follows:

Imager: Construction of all mechanical parts are complete. The optics forthe CTIO imager were unacceptable as received from the vendor and werereturned. The vendor is re-working the optics to meet our specifications andwill ship in July 1986. The optics for the KPNO imager were also unacceptableas received from the vendor and were returned. Our optical shop is producingthis piece in-house. There is still no update from SBRC as to when anacceptable array will be available.

Electronics: Construction of all electronics is essentially complete exceptfor minor modifications implemented during test and check-out. Testing ofvarious electronic modules is continuing in a satisfactory manner. Notechnical problems are expected.

Spectrometer: Concept design is continuing with some detail designunderway. Construction is scheduled for FY 1987.

The Cryogenic Camera Project is complete as originally specified, however,improvements may be required in the future to improve grism transmission forhigh dispersion applications.

Removal of the Varian computer associated with the McMath Computer Projectwill not be completed until the necessary software has been converted to runon the DEC computers. The software conversion is scheduled for completionduring the next quarter. Changes in the telescope interface chassis andgrating motor drivers are planned for next year. Observing room modificationshave been delayed until FY 1987.

Investigation of environmental effects on ruling quality associated with theMcMath Grating Project continues. No serious rulings will be attempted untilafter the summer rainy season.

Work continues on the construction of the electronics and mechanical parts forthe McMath CCD system. The system is scheduled for installation in mid-FY1987.

The footings for the Vacuum Telescope Lightning Protection towers have beeninstalled. The towers are due to arrive by 1 August, with installationscheduled for August 1986.

Additional software development continues for the 512 Magnetograph SoftwareProject.

The Mountain Computers Project is continuing with the installation of the DECsystems and removal of the Varian computers. The Varians will not be removeduntil all software conversions are complete which, due to programmershortages, will continue for another six months. The DEC computer system forthe Coude" Feed is ready for installation in September 1986. The SBRC displaysystem was completed and implemented.

A major design change was started this quarter for the Kitt Peak PhotonCounting Array Project. A full frame sub-tract is being added to the inputdata chain before centroiding is accomplished. This hardware modification isscheduled to be completed in time for laboratory and telescope testing in Julyand August 1986. If successful, this should be the last major hardware changerequired for the instrument. The fiberoptic couplers for mating theintensifier with the CCD were received but not in accordance with

specifications. The couplers are being returned to the vendor.

The Tektronic CCD Evaluation is continuing with mechanical and electronicconstruction on dewars for both the 512 x 512 and 2048 x 2048 chips. Theimaging module for the laboratory test projector has been completed andimplemented.

The UV Fast Camera Project is basically complete. All optical and mechanicalparts for the main camera unit have been assembled and tested. Miscellaneousfield lenses and mounting brackets will be required for future applications.

A new rotary uninterruptable power supply (RUPS) was purchased for the 4-mtelescope computers and instrumentation as part of the Instrument and ComputerPower Project. The RUPS is due to be received by 1 August 1986, withinstallation and conversion scheduled for August and September 1986.

Two TI CCDs were received and are being tested as part of the TexasInstruments CCD Evaluation Project for various performance characteristics.

The NOAO Workstations Project remains behind schedule due to budgetaryuncertainties. The hardware procurement schedule will be modified whenfunding availability becomes more certain. The major efforts in this quarterinvolved solving problems associated with the Sun-3/LSI-II link, and softwaredevelopment for IRAF on the Sun-3.

Ruling Engine Improvements are continuing. The control laser was sent back tothe vendor for tube replacement. Temperature measurements of the engine androom uncovered an unexpected heat source from a pressure measuring sensorwhich has now been relocated. An independent monitor for pressure correctionhas been constructed. A three color laser has been ordered for efficiency

measurements.

The GONG Project is continuing on schedule. Work is progressing for eachsection as follows:

GONG Lab Systems: The design phase on this project is nearing completion withthe construction and installation scheduled for completion by 1 September1986. Construction of the support structure and welding is beingsubcontracted.

GONG Analyzer: The conceptual design for the analyzer has been completed andvarious project tasks have been allocated. Large, high quality, calcitecrystals were inspected and the best were selected for purchase and componentfabrication. A prototype temperature controller for the wide field Michelsonelement has been built. Tests are underway for constructing specialwaveplates.

Site Survey: Monitors at nine locations around the world produced reliabledata on site conditions during the quarter. A data base access system for thearchived records has been developed. Also, routines to analyze atmospherictrends in the data base have been developed. Initial survey results have beenreviewed and they confirm or exceed the network duty cycle predicted bymodels.

Design studies continue for the 512 Channel Magnetograph Replacement withvarious technical trade-offs being analyzed. A design that uses vendorhardware for the front-end data processing is being investigated. A CCDcamera has been found that appears to meet the imaging specificationsrequired; future tests will confirm this assumption. Integration of aprototype system will begin during the first quarter of FY 1987.

The Coude" Feed Improvements Project is processing in accordance with themanagement plan, but behind schedule. Electronic fabrication and software(VENIX) development are progressing, and every effort is being made tocomplete the project within the original schedule.

Secondary focus drive and readout, associated with the #1-0.9-m TelescopeImprovements Project are complete. The f13 secondary collimation improvementis also complete. Primary mirror supports will be changed back to the oldsystem in August. Torque motor preloads are in the shop; installation will beon a time available basis. Absolute encoders are in the design stage.

The Tektronics Direct Camera Interface Project has been temporarily suspendedpending delivery of a 2048 x 2048 CCD. The large filters have been specifiedand will be ordered at a time appropriate to the delivery of the CCD.

An order has been placed for Zerodur blanks to be fabricated into replicationand master blanks as a part of the RC Gratings Project. The RC "G" mastergrating was successfully replicated and efficiencies of the grating weremeasured to be good. A second replication has been ordered for CTIO.

A replica of the 226 i/mm cross disperser is being ordered for CTIO as a partof the Echelle Gratings Project.

Conversion of the applications software for the IRS at the #2-0.9-m TelescopeProject ls progressing. This project is on schedule, and completion isexpected during the next quarter.

10

During this quarter, the TI 800 x 800 CCD was finally put into routine serviceon Cerro Tololo. This detector is offered for direct imaging on the 1.5-m and0.9-m telescopes, and for echelle spectroscopy on the 4-m telescope. A UV-flooding technique has been successfully implemented for the TI chip allowingconsiderable enhancement of the UV and blue quantum efficiency.

A GEC epitaxial CCD with a special fluorescent coating designed to improve UVsensitivity was tested on the CTIO 0.9-m telescope in April. This coating wasdeveloped at the European Southern Observatory who kindly offered to coat oneof the CTIO's chips for testing. Initial results look very promising; furthertesting as a spectroscopic detector of the 1.5-m telescope is planned forAugust.

Good progress was made on completing the installation of UPS power to the CTIO1.5-m, 1-m, and 0.9-m telescope domes. This project should be completed bythe next quarter.

11

V. TELESCOPE OPERATIONS

A. Kitt Peak National Observatory.

The NOAO-designed and built UV fast camera has been completed. Performancetests were carried out in May on the KPNO 4-m echelle spectrograph. Thecamera performed very well and produced 25 - 35u images everywhere in thefield (3300 - 6800 A). The overall throughput is excellent. The telescope-spectrograph-camera efficiency is ~3.4%—good by echelle standards. Thecamera has been used for science by staff and visitors in both a direct CCDmode and an intensified CCD mode. Further applications with the KPCA and RCspectrograph are planned over the summer.

Site work on Kitt Peak for the VLBA was completed; construction is nowscheduled to begin in July. Lack of precipitation at Kitt Peak, 1.76 inchesApril-June, made it necessary to truck considerable amounts of water from ourlake—an expensive and time-consuming project.

The bids for asbestos abatement at the KPNO 4-m telescope building werereceived. The successful contractor was Southwest Hazard Control with asubcontract cost of approximately $70,000. Work will proceed shortly with acompletion time of 45 days.

The IRS software is essentially finished; it now incorporates the new guider,which uses the recently installed motor ramper. An IRS reference manual hasbeen written.

A new observing/reduction package for the MKIII photometer was written,4C0L0R+HB, which allows observing with H-Beta and Stromgren 4-color filters.A new UBV photometry package that assumes a blocked U filter and no red leakwas written.

A new version of Forth, v86.04, similar to last quarter's v86.02, was releasedfor general use. As with 86.02, the new system allows use of disk packs withbad blocks and permits full utilization of the 4 MB 11/73 address space.

B. Cerro Tololo Inter-American Observatory.

A new grating, "RC-F", ruled at the grating lab in Tucson is now available foruse at CTIO.

The pointing accuracy of the CTIO 4-m telescope control program has now beenimproved to 7" RMS in right ascension and 2" in declination.

There were no Chilean Economic Statistics available for this quarter.

C. National Solar Observatory.

The annual GONG workshop was held in Tucson on April 21-23. The 35participants were introduced to the instrument concept, data analysis plansand apprised of the general project status. The balance of the workshop wastaken up with discussions about the implementation of community participationin the project.

12

VI. PROGRAM SUPPORT

A. Director's Office.

Considerable attention was given to the continuing concern for NOAO's fiscalstate for FY 1987 and beyond. The NOAO Preliminary Program for FY 1987 wassubmitted to the NSF by AURA at the completion of this quarter. However,

planning and preparation efforts for the plan were carried out during theentire quarter. Included in the planning efforts were meetings with: theAURA Executive Committee and the AURA Board of Directors in Washington, D.C;

AURA's Observatories Advisory Committee in Washington, D.C. and in Tucson, andtwice by teleconference; an ad hoc Advisory Committee to the NOAO Director;and the NOAO Senior Staff. Also, the NOAO Director held a special session at

the June meeting of the AAS in Ames, Iowa.

The NOAO Director has elected to vacate the Warren Avenue building, which iscurrently leased from AURA, as a cost savings measure. Therefore, aconsiderable portion of this quarter's effort was put into rearranging spaceutilization within the Cherry Avenue building and planning for the usage ofthe West La Quintas.

B. Public Information.

Live images of Comet Halley continued to be transmitted from Cerro Tololo viaChilean Channel 13 and a satellite uplink to the rest of the world, moving toa near-daily schedule for the first half of April. While there is no detailedrecord available of where or when the Cerro Tololo images played, downlinkswere subscribed for most transmissions in the U.S., Europe, and other South

American countries, with Japan and Korea tapping an occasional transmission.

A Comet Halley media workshop was held at Cerro Tololo on April 11 withattendance by El Mercurio, Channel 13, and other Chilean media, the AssociatedPress, Los Angeles Times, CBS-News, the Arizona Republic, and others from the

U.S.

A full-color Spanish language Cerro Tololo pamphlet was received from theprinter in June. Major science stories released during the period included asupernova in Centaurus A and, at the AAS-Ames meeting, design of a deep-polarspectroscopic survey. Reprints were received in June of a 4,000 word article,"A Journey Just Begun: Optical Astronomy at the National Centers," fromBritannica's 1987 Yearbook of Science and the Future.

C. Office of Resource and Program Management.

During this quarter detailed planning and scheduling for the implementation ofthe Early Retirement Incentive Program was initiated. Planning was also

initiated for conversion of the NOAO grounds to a desert landscaping motif asa cost savings measure.

The main thrust of the Project Management Office was to assist in thetransition of project management coordination within the recently formedDirector's Advisory Committee for Instrumentation and Projects and sub-Committee structure.

13

Modifications and renovation of the three units on the west side of the LaQuinta complex were begun. The modifications include converting andinterconnecting the three units (two apartments and storage unit) andconstructing an addition connecting the east and west sides. Themodifications, scheduled to be completed by September 30, 1986, will provide3,600 square feet of office space for CAS personnel (except Personnel) who nowoccupy space in the NOAO Director's office building and the Cherry Avenuebuilding. At that time, all personnel occupying the NOAO Director's officebuilding will have been relocated. This is an additional cost savings measureto preclude annual payment of lease rent for the AURA building (WarrenAvenue).

Design and construction of the foundation system for the 2.4-m satellitesupercomputer antenna was completed in accordance with specificationsfurnished by the American Satellite Company, the project contractor. Theinstallation of power and interface equipment was also completed. The newSupercomputer Link is expected to be operational in early July.

D. Central Computer Services.

A great deal of work was spent this quarter on preparing and testing the IRAFV2.3, the primary purpose of which is to support the imminent first release ofthe ST Scl Science Data Analysis System (SDAS) which runs under IRAF andVAX/VMS. With completion of V2.3, essentially done by the end of the quarter,the first IRAF Newsletter was written and distributed widely throughout thecommunity, along with the IRAF overview paper written during the last quarter.

Hardware and software for a 56 Kbps satellite link to the San DiegoSupercomputer Center was installed. The hardware consists of a satellite diskon the roof feeding a rack of electronics which connects to a PDP-11/24 whichis linked to the VAX-cluster. VMS programs were installed on the VAX tosupport the satellite link and to facilitate use of the San Diego Cray.

14

April - June 1986 Quarterly Report

TELESCOPE USAGE

Appendix A

Astronomical Observations

Hours

Scheduled Hours Used Hours 1Lost

Scheduled

Maintenance,

Engineering,Instrument

Tests,

Telescope Visitors Staff Weather

Equipment

Failure

EquipmentChanges, etc.

4m 1079.5 611.1 102.8 277.6 10.9 77.1

1.5m 1069.0 446.5 157.3 381.2 47.0 37.0

lm 1066.0 521.0 8.5 463.1 11.0 62.4

CTIO 0.9m 1018.7 299.9 175.3 347.0 11.5 185.0

* 0.6/0.9m 386.9 206.5 -0- 155.4 -0- 25.0

0.6m 817.9 491.8 -0- 311.3 7.8 7.0

0.4m

4m 1006.9 609.28 76.20 233.92 68.75 18.75

2.1m 765.15 472.16 83.24 180.75 20.50 8.50

CF 695.25 383.25 56.00 228.00 5.00 23.00

1.3m 753.20 328.25 62.00 315.95 10.00 37.00

KPNO #1-0.9m 698.00 302.77 97.23 253.50 17.50 27.00

#2-0.9m 683.49 298.55 30.94 275.00 37.00 42.00

#3-0.4m 83.00 8.04 3.96 28.00 2.00 41.00

Schmidt 270.00 220.00 -0- 50.00 -0- -0-

Hilltop 2222.0 2005.0 -0- 217.0 -0- -0-

Tower 1032.0 536.5 254.5 161.0 72.0 8.0

Big Dome 2062.0 789.0 215.0 1021.0 37.0 -0-

NSO **FTS Lab 149.0 130.0 -0- -0- 19.0 -0-

**McMath 1574.0 740.0 211.5 465.0 77.5 80.0

Vacuum811.0 559.0 -0- 225.0 27.0 -0-

* Use restricted to dark of the moon.** Totals include both day and night hours. (All others are day only),

Executed Proposals 04/01/86 - 06/30/86 Page 1 Mon Jul 14 20:47:36 1986

Nights Hours Days Hours5678 s86

H Abt, Kitt Peak National ObservatoryA Search for Low-Mass Companions to High-VelocityStars 2.1m Coude Feed 5.00 28.00 0.00 0.00

6206 s86

H Abt, Kitt Peak National ObservatoryMK Classification of A & F SpectroscopicBinaries Nr. 1 0.9 meter 5.00 34.00 0.00 0.00

6319 s86

S Anderson, University of ArizonaB Margon, University of WashingtonA Discovery Program for Very High Redshift QSOs x

4 meter 3.00 18.00 0.00 0.00 co

6280 s86 o

B Balick, R Owen, University of Washington ^G Jacoby, N0A0-CCS mWind-Induced Structure & Motions of Planetary ;2Nebulae 4 meter 4.00 24.00 0.00 0.00 3>

6202 s86

T Barker, Wheaton CollegeSpectrophotometry of Planetary Nebula OuterEnvelopes Nr. 2 0.9 meter 5.00 30.50 0.00 0.00 5

9023 s86

T Beers, California Institute of Technology ^ 3>Detecting Starts of Extremely Low MetalAbundance Burrell Schmidt 7.00 48.00 0.00 0.00 =?

6364 s86

3>

ZD

o

3=

oenTO3=

o

J Black, P Bernath, University of Arizona n>S Ridgvay, N0A0-CCS r_J Keady, Los Alamos National Laboratory oE van Dis hoeck. Center for Astrophysics ^

4 meter 2.00 3.50 2.00 2.50 ^3>—\OTO

Infrared Spectroscopy-of Comet Halley


6033 s86 Nights Hours Days HoursV Blair, K Long, Johns Hopkins UniversityR Fesen, University of ColoradoSpectroscopy of Young Supernova Remnants

2.1 meter 4.00 7.75 0.00 0.00

6272 s86

B Bohannan, University of ColoradoS Voels, D Abbott, D HummerUniversity of Colorado, JILAPrecision Spectroscopy of Early-Type Stars

2.1m Coude Feed 10.00 66.00 0.00 0.00

6335 s86

H Bond, Space Telescope Science InstituteA Grauer, University of ArkansasHigh Speed Photometry of Nuclei of PlanetaryNebulae 1.3 meter 12.00 82.50 0.00 0.00

6318 s86

J Cardelli, University of WashingtonSpectrophotometric Properties of Field ft GlobularCluster R Nr. 2 0.9 meter 13. 00 61.00 0.00 0.00

6268 s86

B Carney, University of North CarolinaPossible Background Objects of Dwarf SpheroidalGalaxies 2.1 meter 1.00 5.50 0 00 0.00

6252 s86

C Chapman, D Davis, S Weidenschilling,R Greenberg, D Levy, M Magee, S VailB Marcialis, T Lappin, P BrownPlanetary Science InstitutePhotometric Geodesy of Main-Belt Asteroids

Nr. 2 0.9 meter 8.00 37.50 0.00 0.00

6238 s86J Cowan, R Henry, D BranchUniversity of OklahomaA Search for Optical Emission from RecentSupernovae 2.1 meter 4.00 30.75 0.00 0 00



A Cowie, L Cowie,Space Telescope Science InstituteDistances to the High Velocity Neutral HydrogenClouds 4 meter 4.00 24.00 0.00 0.00

6207 s86G Da Costa, P Demarque, Yale UniversityPhotometric Monitoring of Blue Stragglers in M3Globular... Nr. 1 0.9 meter 4.00 21.50 0.00 0.00

6370 s86S Djorgovski, Center for AstrophysicsH Spinrad, University of California, BerkeleyGalaxy Evolution at High Redshifts: Photometry of3CR ..... 4 meter 3.00 18.08 0.00 0.00

6371 s86S Djorgovski, Center for AstrophysicsH Spinrad, University of California, BerkeleyA Search for Companion Galaxies near QSOs at Z >3 4 meter 3.00 24.00 0.00 0.00

6212 s86

J Eder, Yale University ObservatoryA Oemler, Jr., Yale UniversityCCD Surface Photometry: Early Disk Galaxies inTwo Density. Nr. 1 0.9 meter 6.00 43.50 0.00 0.00

6368 s86P Eisenhardt, N0A0-ADPJ Frogel, Kitt Peak National Observatory-Color Luminosity Relation in Isolated EllipticalGalaxies 1.3 meter 4.00 13.75 0.00 0.00

6181 s86F Fekel, Vanderbilt UniversitySpectroscopy of Binary ft Multiple Stars for theDetermina.. 2.1m Coude Feed 10.00 72.50 0.00 0.00


617g 8 Nights Hours Days HoursF Fekel, Vanderbilt UniversityDetermination of B and A Star Radial VelocityStandards 2.1m Coude Feed 4.00 26.50 0.00 0.00

6356 s86

T Fleming, J Liebert, University of ArizonaI Gioia, Center for AstrophysicsOptical Spectroscopy of an X-Ray Selected Sampleof Stars Nr. 2 0.9 meter 5.00 20.00 0.00 0.00

5456 s86

G Fontaine, F Wesemael, University of MontrealR Green, Kitt Peak National ObservatoryStromgren Photometry of Hot B Subdwarfs in thePalomar-Gree 1.3 meter 9.00 31.50 0.00 0.00

6331 s86

P Frlsch, D York, University of ChicagoRadial Velocities of ISM Target Stars

2.1m Coude Feed 5.00 19.75 0.00 0.00

6288 s86

J Gallagher, Kitt Peak National ObservatoryJ Goad, N0A0-ADP JEmission Line Strengths ft Kinematics in the OuterReaches.. 4 meter 2.00 1.00 0.00 0.00

6347 s86F Gillett, R Joyce, D Backman,Kitt Peak National ObservatoryFollovup of IRAS Galactic Sources: Classification* 1.3 meter 5.50 12.00 0.00 0.00

6263 s86

R Green, Kitt Peak National ObservatoryJ Bechtold,Mt. Wilson ft Las Campanas ObservatoriesD York, University of ChicagoPhysical Conditions in Distant Galaxy HaloRegions 4 meter 3.00 13.50 0.00 0.00



J Grigsby, N Morrison, University of ToledoHigh-Dispersion Spectroscopy of Early B-TypeStars in 2.1 meter 4.00 14.25 0.00 0.00

2.1m Coude Feed 4.00 13.50 0.00 0.00

6204 s86

J Hackwell, G Grasdalen, S Gillam,University of WyomingMass of Galactic Center from Stellar Radial

Velocities 4 meter 2.75 14.75 3.00 9.75

6330 s86

D Hall, University of HawaiiK Hinkle, Kitt Peak National ObservatoryA Search for Dark Companions of K and M Giants

4 meter 1.00 0.00 1.00 0.00

6373 s86

F Hamann, M Simon, SUNY at Stony Brook0.85-1.8 Mu High Resolution Spectroscopy ofLuminous 4 meter 2.00 6.50 0.00 0.00

6282 s86D Hamilton,National Optical Astronomy ObservatoriesCalibration of a Deep Photographic Survey

Nr. 1 0.9 meter 4.00 19.00 0.00 0.00

6193 s86T Heckman, University of MarylandS Baum, A Bridle,National Radio Astronomy ObservatoryG Miley, Space Telescope Science InstituteCCD Imaging of Gas Associated with the Lobes ofExtra 4 meter 3.00 21.50 0.00 0.00

6336 s86T Herter, M Haynes, Cornell UniversityJ Pipher, C Woodward, University of RochesterInfrared Imaging of Galaxies ft Galactic HIIRegions 1.3 meter 10.00 34.00 0.00 0.00


6328 S86 N1ShtS H°UrS DayS HoursK Hinkle, Kitt Peak National ObservatoryPaschen B Observations of Mira Variables

4 meter 0.00 0.00 2.00 6.25

6236 s86

P Hodge, M Mateo, University of WashingtonUBVR Photometry of Galactic Clusters ContainingCepheid.... Nr. 1 0.9 meter 7.00 40.00 0.00 0.00

6216 s86

P Hodge, University of WashingtonR Kennicutt, Jr., University of MinnesotaStructure of HII Regions in Local Group DwarfGalaxies 2.1 meter 4.00 28.00 0.00 0.00

6189 s86

P Hodge, M Mateo, University of WashingtonCalibration of a Photometric System to DetermineSurface Gr Nr. 1 0.9 meter 5.00 24.00 0.00 0.00

6322 s86

E Hu, L Cowie, Space Telescope Science InstituteEmission Line Kinematics of Gas in BrightestCluster 4 meter 3.00 22.50 0.00 0.00

6345 s86W Hubbard, University of Arizona4 May 1986 Neptune Occultation

1.3 meter 2.00 14.00 0.00 0.00

6344 s86

G Illingworth, Space Telescope Science InstituteM Aaronson, K Cook, University of ArizonaA Search for Cepheids ft the Distance to M101

4 meter 4.00 36.15 0.00 0.00

6363 s86D Jevitt, K Meech,Massachusetts Institute of TechnologyDoppler Observations of a Cometary Plasma Tail

2.1 meter 4.00 29.75 0.00 0.00



R Joyce, Kitt Peak National ObservatoryT Brooke, R Knacke, SUNY at Stony BrookInfrared Polarimetry ft Spectrophotometry of CometHalley 1.3 meter 6.00 36.50 0.00 0.00

6276 s86

V Junkkarinen, Kitt Peak National ObservatoryA Bright QS0 Mg II Absorption Survey

4 meter 3.00 26.50 0.00 0.00

6190 s86

R Kennicutt, Jr., University of MinnesotaY Chu, University of IllinoisThe Stellar IMF in Giant HII Regions ft a CriticalTest of 2.1 meter 7.00 28.00 0.00 0.00

6188 s86

R Kennicutt, Jr., University of MinnesotaIntegrated Spectrophotometry of Nearby Galaxies

Nr. 2 0.9 meter 8.00 49.00 0.00 0.00

6239 s86

S Kenyon, Center for AstrophysicsE Seaquist, University of TorontoA Taylor, University of GroningenInfrared and Optical Observations of SymbioticStars 1.3 meter 4.00 31.25 0.00 0.00

Nr. 2 0.9 meter 5.00 20.00 0.00 0.00

6184 s86T Kinman, Kitt Peak National ObservatoryR Kraft, University of California, Santa CruzN Suntzeff,Mt. Wilson ft Las Campanas ObservatoriesE Friel, Lick ObservatoryAbundance Determinations for RR Lyrae Stars inTwo Fields 2.1 meter

1.3 meter

Nr. 1 0.9 meter

6 00 33 00 0 00 0 00

5 00 30 25 0 00 0 00

2 00 14 00 0 00 0 00


6302 s86 N1ShtS HOUFS Da^S H°UrsD Koo, Space Telescope Science InstituteR Kron, University or Chicago, Yerkes Obs.A Szalay, Eotvos UniversityRedshifts to Study Evolution of Faint Quasars ftLarge-Scale 4 meter 4.00 33.75 0.00 0.00

6267 s86

D Koo, Space Telescope Science InstituteR Kron, S Majewski,University of Chicago, Yerkes Obs.Faint U-Band Imaging of Field Galaxies

4 meter 3.00 23.00 0.00 0.00

6248 s86

K Krishnasvamy, University of Texas, AustinCarbon Isotope Ratios in Open Cluster Giants

2.1m Coude Feed 4.00 21.00 0.00 0.00

6334 s86

R Kron, University of Chicago, Yerkes Obs.A Crotts, University of ChicagoThe Spatial Clustering of QS0 Absorbers

4 meter 3.00 28.50 0.00 0.00

6366 s86

K Kvitter, T Lydon, Williams CollegeG Jacoby, Kitt Peak National ObservatoryA Deep Search for Faint Central Stars ofPlanetary Nebulae 2.1 meter 4.00 23.25 0.00 0 00

Nr. 1 0.9 meter 4.00 18.00 0.00 0.00

6372 s86

K Kvitter, C Congdon, Williams CollegeP Massey, Kitt Peak National ObservatoryA Deep Search for Faint Remnant Planetary NebulaeAround... Nr. 2 0.9 meter 4.00 15.00 0.00 0 00

Nr. 1 0.9 meter 4.00 13.00 0.00 0.00

6160 s86

A Landolt, A Uomoto, Louisiana State UniversityUBVRI Photometry of Space TelescopeSpectrophotometry 1.3 meter 6.00 39.00 0 00 0 00


Nights Hours Days Hours•6166 s86

R Luck, Case Western Reserve UniversityCNO Abundances in Luminosity Class II and CN WeakStars 2.1m Coude Feed 9.00 73.00 0.00 0.00

6220 s86

E Malumuth, University of VirginiaG Kriss, Johns Hopkins UniversityThe Phase Space Distribution Function of cDClusters of.... 2.1 meter 5.00 24.50 0.00 0.00

6132 s86

P Massey, Kitt Peak National ObservatoryJ Barnes, E Anderson, N0A0-CCSSpectrophotometric Standards at the Faint End

2.1 meter 5.00 40.70 0.00 0.00

5654 s86

H McAlister, W Hartkopf, H Miller,Georgia State UniversityP Scnmidtke, Arizona State UniversityD Hutter, Applied Research Corporation0 Franz, Lowell ObservatoryAstronomical Speckle Interferometry with the GSUSpeckle... 4 meter 3.00 22.00 0.00 0.00

6343 s86

D McCarthy, M Cobb, University of ArizonaNear-Infrared Imaging of Low Mass Companions

4 meter 5.00 40.25 0.00 0.00

6167 s86

D McNamara, Brigham Young UniversityPhotometric Investigation of BL Herculis ft DwarfCepheid... 1.3 meter 6.00 45.25 0.00 0.00

6357 s86

U Mebold, University of BonnJ Black, University of ArizonaOptical Absorption Line Studies of High-LatitudeDust ft.... 2.1m Coude Feed 5.00 40.00 0.00 0.00


6298 S86 NlghtS H°UrS DayS H°UrSG Miley, Space Telescope Science InstituteT Heckman, University of MarylandImaging of High-Z Quasars with Bent RAdioStructures 4 meter 2.00 11.00 0.00 0.00

6165 s86

J Moody, University of MichiganThe Distribution of Emission-Line Galaxies inVoids * Burrell Schmidt 7.00 42.00 0.00 0.00

5110 s86

J Mould, California Institute of TechnologyT Kinman, Kitt Peak National ObservatoryD Ketelsen, University of ArizonaLPVs in Late-Type Galaxies and the ExtragalacticDistance.. 4 meter 1.00 8.00 0.00 0.00

6085 s86

R O'Connell, M Fanelli, University of VirginiaD Ketelsen, University of ArizonaM Roberts, National Radio Astronomy ObservatoryThe Ultraviolet Imaging Telescope UV/OpticalAtlas Nr. 3 0.4 meter 5.00 12.00 0.00 0.00

6229 s86R 0"Connell, D Crocker, R Rood,University of VirginiaHelium Abundances on Globular Cluster HorizontalBranches 2.1 meter 5.00 42.50 0.00 0.00

6209 s86

A Oemler, Jr., Yale UniversityH Butcher, Kapteyn SterrenvacntThe Role of Environment in the Evolution ofGalaxies in.... 4 meter 2.00 14.50 0.00 0.00

6208 s86A Oemler, Jr., Yale UniversityR Ellis, Durham UniversityThe Evolution of Galaxies in Radio-SelectedGrouPs 4 meter 2.00 5.25 0.00 0 00

Nr. 1 0.9 meter 4.00 26.00 0.00 0.00



J Peterson, Princeton UniversityGalaxy-Cluster Alignment

Nr. 1 0.9 meter 4.00 9.50 0.00 0.00

6198 s86

A Philip, Van Vleck ObservatoryD Hayes, Kitt Peak National ObservatoryCCD Observations of Blue Horizontal Branch Starsin Nr. 1 0.9 meter 4.00 29.00 0.00 0.00

6175 s86

C Pilachovski, Kitt Peak National ObservatoryC Sneden, University of Texas, AustinCarbon Isotopes in Subdvarfs - Another Constrainton Popula 2.1 meter 4.00 33.75 0.00 0.00

6174 s86C Pilachowski, Kitt Peak National ObservatoryC Sneden, University of Texas, AustinThe Composition of the Globular Cluster M71

4 meter 4.00 19.00 0.00 0.00

9026 s86

C Pilachowski, G Jacoby,Kitt Peak National ObservatorySearch Edge-on Dusty Spiral Galaxies for LithiumAbsorption Nr. 2 0.9 meter 3.00 25.50 0.00 0.00

6339 s86

J Pipher, C Woodward, M Shure, W Forrest,University of RochesterArc Second Spectroscopic Imaging of Galactic HIIRegions... 1.3 meter 2.00 3.50 0.00 0.00

9028 s86R Probst, Kitt Peak National ObservatoryOpen Time-Spectroscopy of dM and sdM Stars

2.1 meter 3.00 5.75 0.00 0.00


9033 s86 Nights Hours Days HoursR Probst, Kitt Peak National ObservatoryPhotometry of Faint Proper Motion Stars

Nr. 1 0.9 meter 1.75 5.00 0.00 0.00

6338 s86

R Probst, Kitt Peak National ObservatorySearch for Young Brown Dwarf Companions to UrsaMaJor Nr. 1 0.9 meter 3.00 9.00 0.00 0.00

6349 s86S Ridgway, N0A0-CCSG Jacoby, R Joyce,Kitt Peak National ObservatoryAngular Diameters of Late-Type Stars

4 meter 0.25 1.50 0.00 0.00

6320 s86

W Romanishin, Arizona State UniversityThe Stellar IMF in Grand Design ft FlocculentSpiral Galaxie Nr. 2 0.9 meter 6.80 22.00 0.00 0.00

6219 s86V Rubin, J Graham,Carnegie Institution of WashingtonVelocity Structure of Near-Nuclear Gas in DiskGalaxies 4 meter 3.00 28.25 0.00 0.00

6218 s86V Rubin, D Hunter,Carnegie Institution of WashingtonEnvironmental Influences on Spiral ft EllipticalGalaxies... Nr. 1 0.9 meter 4.00 22.00 0.00 0.00

6260 s86

S Saar, J Llnsky, University of Colorado, JILAM Giampapa, National Solar Observatory/TucsonDetecting Magnetic Fields on Active M Dwarf StarsUsing the 4 meter 3.00 32.00 3.00 13.25



E Sadler, Kitt Peak National ObservatoryObserve Triaxial Structure in the Bars of SeyfertGalaxies Nr. 1 0.9 meter 0.25 2.00 0.00 0.00

6341 s86

R Sahai, University of Texas, AustinP Wannier, Jet Propulsion LaboratoryJ Keady, Los Alamos National LaboratoryD Jennings, G Wiedemann,NASA Goddard Space Flight Center8 Mu Vibration-Rotation Lines of SiO fromMass-Losing 4 meter 0.00 0.00 9.00 58.50

6253 s86

J Salzer, T Boroson, G MacAlpine,University of MichiganSpectroscopy of Emission-Line Galaxies in theUniversity... 2.1 meter 4.00 19.00 0.00 0.00

6249 s86

E Schlegel, R Honeycutt, Indiana UniversityTime-Resolved Spectroscopy of Accretion DiskStructure in.. 2.1 meter 7.00 44.50 0.00 0.00

9029 s86

P Schmidtke, A Cowley, Arizona State UniversityD Crampton, Dominion Astrophysical ObservatoryOpen Time-Luminosity Function and PossibleClustering of... Nr. 1 0.9 meter 2.00 14.00 0.00 0.00

6294 s86

P Schmidtke, Arizona State UniversityL Goad, J Africano, R Joyce,Kitt Peak National ObservatoryG Jacoby, S Ridgway, N0A0-CCSThe Variation of Stellar Angular Diameter withWavelength 2.1 meter 1.00 4.75 0.00 0.00


5628 s86 NlghtS H°UrS DayS H°UrSP Schmidtke, Arizona State UniversityJ Africano, Kitt Peak National ObservatoryR Quigley, University of ArizonaLunar Occultations of Double Stars

Nr. 2 0.9 meter 2.20 1.50 0.00 0.00

6177 s86M Shara, M Potter,Space Telescope Science InstituteA Moffat, University of MontrealSearch for Cataclysmic Binary Stars in GlobularClusters 2.1 meter 4.00 33.75 0.00 0.00

6151 s86

M Sitko, Kitt Peak National ObservatorySimultaneous UV, Optical and IR Observations oftne 1.3 meter 4.00 6.25 0.00 0.00

6214 s86

H Spinrad, University of California, BerkeleyS Djorgovski, Center for AstrophysicsSpectroscopy of Lya Companions to Quasars ft VeryFaint 4 meter 3.00 27.00 0.00 0.00

6359 s86S Tapla, J Liebert, University of ArizonaRelative Spectrophotometry of Calibration Targetsfor the.. Nr. 2 0.9 meter 3.00 22.50 0.00 0.00

6012 s86

E Tedesco, R Nelson, B Buratti,Jet Propulsion LaboratoryR Binzel, University of Texas, AustinD Tholen, Institute for AstronomyPhotometry of Pluto-Charon Mutual Eclipse Events

1.3 meter 2.00 10.50 0.00 0.00

6226 s86

T Thuan, E Malumuth, University of VirginiaT Williams, T Williams, Rutgers UniversityKinematics of the Ionized Gas in Blue CompactDwarf Galaxle 4 meter 4.00 31.75 0.00 0 00



T Thuan, University of VirginiaH Loose, University of GottingenCCD Photometry of Very-Large-Size, Low SurfaceBrightness.. Nr. 1 0.9 meter 4.00 11.00 0.00 0.00

9027 s86

T Thuan, University of VirginiaM Whittle, C Moss, Institute of AstronomyStar-Formation Rates in Virgo Blue Compact DwarfGalaxies Burrell Schmidt 9.00 81.00 0.00 0.00

9031 s86

D Turner, Saint Mary's UniversityD Forbes, Trent UniversityUBV Photometry of Open Clusters with AssociatedCepheid... Nr. 2 0.9 meter 2.00 1.50 0.00 0.00

6237 s86

J Vader, Yale UniversityM Simon, SUNY at Stony BrookSpectroscopy of IRAS Selected Seyfert GalaxyCandidates 2.1 meter

Nr. 1 0.9 meter

6279 s86

S VanDyk, University of WashingtonSupernovae and HII Regions in Spiral Galaxies

Nr. 1 0.9 meter 5.00 25.00 0.00 0.00

6170 s86

F Walter, University of Colorado, LASPP Myers, Center for AstrophysicsE Feigelson, Pennsylvania State UniversityA Brown, University of Colorado, JILAF Vrba, U.S. Naval Observatory, FlagstaffNaked T Tauri Stars in Oph, CrA, and Cyg

2.1 meter 7.00 47.75 0.00 0.00

5321 s86E Weis, Wesleyan UniversityA Photometric Search for Nearby Dwarf M Stars

Nr. 2 0.9 meter 8.00 23.50 0.00 0.00

7.00 58.20 0.00 0.001.00 9.00 0.00 0.00


6264 s86 Nights Hours Days HoursB Whitmore, D McElroy, M Bell,Space Telescope Science InstituteStructure ft Dynamics of Polar Ring Galaxies

4 meter 2.00 15.50 0.00 0.00

6377 s86

S Wolff, Kitt Peak National ObservatoryAbundances of Early Type Stars

2.1m Coude Feed 4.00 28.00 0.00 0.00

9030 s86

C Woodward, University of RochesterOpen Time-Obtain H alpha, V ft I Band Images ofNGC 7027 Nr. 1 0.9 meter 3.00 11.50 0.00 0.00

6337 s86

D York, G Burks, University of ChicagoThe Search for Distant Halo RRLyrae Stars in theDirection. Burrell Schmidt 7.00 49.00 0.00 0.00

6355 s86D York, G Burks, University of ChicagoU Mebold, University of BonnDistances to 21cm High Velocity CloudsInteracting vith 2.lm Coude Feed 4.00 11.00 0.00 0.00

6241 s86

A Young, San Diego State UniversityA Skumanich, R Gilliland,High Altitude ObservatoryChromospherlc Activity in Evolved Stars: TheBinary 2.1m Coude Feed 8.00 40.00 0.00 0.00

CERRO TOLOLO INTER-AMERICAN OBSERVATORY

APPENDIX "B"

OBSERVATIONAL PROGRAMS

April-May-June 1986: Individual telescope asignments arelisted below. Graduate students are indicated by an asteriskafter their name. Nights assigned, (hours worked), and telescopeused are indicated.

C. Anguita and M.T. Ruiz, Universidad de Chile: "CCD Parallaxesof Faint High Proper Motion Stars", 3(29)1.5m.

B.M. Blanco and V.M. Blanco, NOAO/CTIO: "RR Lyraes in theGalactic Bulge", 3(31)1.5m, 4(0)1m, 2(13)0.9m.

A.P. Cowley, Arizona State University; D. Crampton and J.B.Hutchings, Dominion Astrophysical Observatory: "Spectroscopyand Kinematics of Galactic Bulge X-ray Sources", 3(34)4m.

M. Davis and M. Strauss, University of California Berkeley; J.Tonry, Massachusetts Institute of Technology; and A. Yahil,SUNY Stonybrook: "A Redshift Survey of IRAS Galaxies",7(75)1.5m.

O.J. Eggen, NOAO/CTIO: "Intermediate Band and RI Photometry",6(34)1.5m.

G.G. Fahlman and H.B. Richer, University of British Columbia:"Search for Young Globular Clusters", 4(17)4m.

H. Ford and R. Ciardullo, Space Telescope Science Institute:"Halo Dynamics and the Mass Distribution in NGC 5128",5(55)4m.

L.M. French, Massachusetts Insitute of Technology: "Light CurveStudies of Trojan Asteroids", 9(94)0.9m.

J.A. Frogel, NOAO/KPNO; V.M. Blanco, NOAO/CTIO; and D. Terndrup,University of California Santa Cruz: "The Stellar Populationof the Nuclear Bulge", 6(11)4m, 1(12)1.5m.

J.E. Grindlay, Harvard Smithsonian Center for Astrophysics; P.Lugger abd H. Cohn, Indiana University; P. Hertz, NationalResearch Lab; and C. Bailyn, Harvard University: "Identification of X-ray Sources in Globular Clusters and theGalactic Bulge", 6(10)4m.

D. Hamilton and B.M. Blanco, NOAO/CTIO: "Kinematics of the OldBulge Population", 4(1 3 )it m .

M.L. Hazen, Harvard College Observatory: "Search for VariableStars in Globular Clusters", 8(56)1m.

S.R. Heathcote, NOAO/CTIO: "High Dispersion Spectroscopy of HHObjects Associated with Bipolar Flows", 2(24)4m, 4(37)0.9m.

W.D. Heintz, Swarthmore College: "Micrometer Observations ofSouthern Double Stars", 8(77)1.5m.

J.E. Hesser, Dominion Astrophysical Observatory; G.L.H. HarrisUniversity of Waterloo; and H.C. Harris, U.S. Naval Observatory: "Dynamics of the NGC 5128(Cen A) Globular ClusterSystem", 3(33)4m.

T. Ichikawa, and M. Nishida, University of Kyoto: "OpticalIdentification of IRAS Objects", 3(32)1m, 10(33)MS.

K. Kawara and B. Gregory, NOAO/CTIO: "IR Spectroscopy ofBrightest IRAS Galaxies", 3(34)1.5m.

W. Keel, Sterrewacht Leiden: "Imaging of Southern Galaxies withOptical Jets", 5(48)1.5m.

I.R. King, University of California Berkeley; and S. DjorgovskiCenter for Astrophysics: "Faint Stellar Photometry inGlobular Clusters", 4(30)4m.

D.L. Lambert and V.V. Smith, University of Texas: "HighResolution Spectroscopy and Abundances in to Centauri"4(39)4m.

A.U. Landolt and A.K. Uomoto, Louisiana State University: "UBVRIPhotometric Sequences", 19(58)1.5m.

H. Levato and S. Malaroda, Complejo Astronomico El Leoncito- NMorrell, B. Garcia, and M. Arnal, Universidad Nacional dePlata: "Spectroscopic Binary Frequency in Open ClustAssociations", 12(104)1m.

E.R. Luck, Case Western Reserve University: "CNO Abundances inYoung Open Clusters", 5(59)4m.

B.L. Lutz, R.L. Millis, D.J. Lein, and D.G. Schleicher, LowellObservatory: a) "High Resolution Observations of P/Halley

D?H R^^^2L5)n4em.0f ^ ' " "^ ^' "C Ratl°"' C) "ThiJ. Lutz and B. Balick, University of Washington: "Morphology and

Radii of Planetary Nebula Shells", 19(84)0.9m.

J. Maza and M.T. Ruiz, Universidad de Chile: a) "Study ofEmission Line Objects", b) Spectroscopy of Faint High-Proper Motion Stars 1(11)4m.

La

er

D.H. McNamara, Brigham Young UniversityHerculis Variables", 4(8)1.5m, 7(53)1m.

"Photometry of BL

K.J. Meech*, Massachusetts Institute of Technology: "Plasma TailDynamics of Comet P/Halley", 11(57)MS.

D.M. Meyer, University of Chicago, and I. Hawkins, University ofCalifornia Los Angeles: "The Application of Interstellar

Molecules to Problems in Cosmology and Galactic ChemicalEvolution", 5(55)4m,

H. Moreno, A. Gutierrez-Moreno, and E. Wenderoth, Universidad de

Chile: "Photometric Observations of Comet Halley", I4(77)1m.

J.R. Mould and J.K. McCarthy*, California Institute ofTechnology, and J. Graham, Carnegie Institution ofWashington: "Are the Carbon Mixed Stars in w Cen Binaries?",

6(64)4m.

M. Nishida, Kyoto University, and K. Kawara, NOAO/CTIO: "The

Near-InfraredPhotometry of Merging'Galaxies", 3(27)1.5m.

W. Osborn, Central Michigan University: "Radial Velocities andMetal Abundance Estimates of Halo Stars", 5(19)1m.

M. Pedreros, Universidad de Chile: "Photoelectric Study of OpenClusters with Cepheids", 4(0) 1m.

M.M. Phillips and A.C. Phillips, NOAO/CTIO: "A Search for

Supernovae in Starburst Nuclei", 6(57)0.9m.

H. Quintana, U. Catolica de Chile: "Multiple Nuclei BrightestGalaxies in a Complete Cluster Sample", 2(3)4m.

A. Raga and M. Mateo*, University of Washington: "CCD Imaging ofHerbig-Haro Objects in the Light of Forbidden' EmissionLines", 2(24)0.9m.

R. Remillard, H. Bradt, and A. Ghez, Massachusetts Institute of

Technology, and W. Roberts, Harvard-Smithsonian Center forAstrophysics: "Optical Identification of HEAO-1 X-ray

Sources", 9(7)MS.

M.T. Ruiz and J. Maza, Universidad de Chile: "Spectroscopy ofFaint High-Proper Motion Stars", 1(11)4m.

P.S. Schmidtke, Arizona State University: "Photometric Studies of

Galactic Low-Mass X-ray Sources", 5(18)1.5m.

P. Seitzer, NOAO/KPNO; H. Cohn and P. Lugger, Indiana University;and G. Da Costa, Yale University: "Kinematics of GlobularClusters", 4(37)4m, 2(20)0.9m.

Smith and B. Campbell, Dominion Astrophysical Observatory:"Search for KI Variations Within Globular Clusters",2(25 )4m.

H. Smith, Michigan State Univesity: "Metal Rich RR Lyraes Farfrom the Galactic Plane", 4(0)1.5m, 5(24)1m.

J.E. Steiner, D. Ceislinski, and F.J. Jablonski, Universidad doSao Paulo: "Spectroscopy of Color Selected IrregularVariables", 11(92)1m .

J. Thorstensen, Dartmouth College, and P.A. Charles and W. HoneyOxford University: "Physical Properties of Low-Mass X-rav

Binaries", 4(49)1.5m.

B. Twarog and B.J. Anthony-Twarog , University of Kansas:"Extension of the uvby System to G and K Stars", 10(81)0.6m.

F. Vrba, U.S. Naval Observatory; F. Walter, University ofColorado; and P. Myers, Harvard-Smithsonian Center forAstrophysics: "Optical and IR Photometry of Southern 'NakedT Tauri' Stars", 3(33)4m, 6(12)1m.

G. Wallerstein, University of Washington, and D. GeislerNOAO/CTIO: "Physical Properties of Short-Period Variables into Cen", 6(30)1.5m, 4(20)0.9m.

P.A. Wehinger and S. Wyckoff, Arizona State University: H.Spinrad, University of California Berkeley; M. BeltonNOAO/KPNO; and D.K. Yeomans, Jet Propulsion Lab: "CometHalley: Physical and Chemical Properties of Its AtmosphereIonosphere and Plasma Tail", 4(50)4.

W. Weller and S. Heathcote, NOAO/CTIO: "Formation, Dynamics andExcitation Of Planetary Nbulae", 2(23)4m, 4(9)1m, 5(37)0.9m.

A. E

R . E

Whitford, University of California Santa Cruz, and J AFrogel, NOAO/KPNO: "Spectra of Bulge M Giants, 1.0-2 4 urn"'4(37) 4m. M '

Williams, NOAO/CTIO, and W.A. Christiansen, University ofNorth Carolina: "Surface Photometry of Shell Galaxies"2(20)4m.

H.K.C. Yee, University of Montreal: "Quasar-Galaxy ClusterAssociation", 4(35)1.5m.

MICHIGAN PROGRAM

F. Miller, University of Michigan, and W. Liller, Vina del MarCurtis Schmidt Observations of Comet Halley", 19(110)MS.

10

LOWELL PROGRAMS

B.L. Lutz, R.L. Millis, D.J.James, and L. Martin, Lowell

Photometry of Halley's Comet",77 (150)0.6m.

Lein, D. Schleicher, C. Gully, P.Observatory: a) "Photoelectricb) "Patrol Photography of Mars",

YALE PROGRAMS

G. Da Costa, Yale University: "Photometry of Al-Vel Type VariableBlue Stragglers in to Centauri", 5(53)0.9m.

P. Vader, Yale University: "The Nature of Galaxies withSeyfert-like IRAS Colors", 4(4l)1m, 2(20)0.9m.

Y-W Lee* and R. Zinn, Yale University: "Photometry of GlobularClusters hear the Galactic Center", 6(14)0.9m.

11


Nights Hours Days Hours1023 286

R Altrock, Sacramento Peak ObservatoryS/B003-Coronal Observations

Big Dome/SP 0.00 0.00 80.00 89.00

1161 286

R Altrock, Sacramento Peak ObservatoryR Harrison, High Altitude ObservatoryS/B181-Coronal Transient Patrol

Big Dome/SP 0.00 0.00 10.00 38.00

1160 286

R Altrock,L Gilliam,S/B180-He

Sacramento Peak ObservatoryNational Solar Observatory/Sac Peak10830 Spectroheliograms

Big Dome/SP

1143 286

G Basri, University of California, BerkeleyC Plymate, National Solar Observatory/TucsonT/Concurrent Activity and Magnetic FieldObservations McMath Main

1043 286

B Bopp, University of ToledoC Plymate, National Solar Observatory/TucsonT/Synoptic H-alpha Variability ft Orbits of TwoNew Bright.. McMath Main

1087 286

P Brandt, Kiepenheuer Institut fur SonnenphysikR Smartt, National Solar Observatory/Sac PeakS/T223-RO Measurements at Sac Peak VTT

Vacuum Tower/SP

1092 286

R Dunn, National Solar Observatory/Sac PeakL November, Sacramento Peak ObservatoryS/T233-Focus/Seeing Studies

Vacuum Tower/SP

0.00 0.00 4.00 0.00

2.00 6.00 0.00 0.00

6.00 30.50 0.00 0.00

0.00 0.00 1.00 3.00

0.00 0.00 6.00 14.00

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1206 286 Nights Hours Days HoursG Elste, University of MichiganS/T257-Limb Darkening Freed from Scattered Lightin Telesco Vacuum Tower/SP 0.00 0.00 5.00 29.00

1180 286

G Elste, University of MichiganS/B183-Limb Darkening

Big Dome/SP 0.00 0.00 23.00 176.00

1140 286

R Engleman, Jr., R Hinsley,Los Alamos National LaboratoryR Bohlin, M Sirk,Space Telescope Science InstituteT/Wavelength Calibration Spectra for the HubbleSpace Teles McMath FTS Lab 2.00 6.00 2.00 7.00

1050 286

T Fleming, University of ArizonaC Plymate, National Solar Observatory/TucsonT/Synoptic High Resolution Spectroscopy ofBright, X-ray... McMath Main 4.00 14.50 0.00 0.00

5273 286

M Giampapa, National Solar Observatory/TucsonT/Simultaneous Call Resonance Line ft Infrared Hand K Band McMath Main 0.00 0.00 2.00 13.00

1052 286

M Giampapa, C Plymate,National Solar Observatory/TucsonT/Synoptic Rotational Modulation of the He I D3Lines In... McMath Main 6.00 34.00 0.00 0.00

1039 286

L Gilliam, National Solar Observatory/Sac PeakS/H008-Whilte Light Sunspot Drawing

Hilltop Dome/SP 0.00 0.00 91.00 95.00



L Gilliam, National Solar Observatory/Sac PeakS/HOOl-Flare Patrol (Monitor only)

Hilltop Dome/SP 0.00 0.00 91.00 926.00

1035 286

L Gilliam, National Solar Observatory/Sac PeakS/H002-White Light Patrol (Monitor only)

Hilltop Dome/SP 0.00 0.00 91.00 926.00

1026 286

L Gilliam, National Solar Observatory/Sac PeakS/B062-Coronograph Monitor

Big Dome/SP 0.00 0.00 29.00 54.00

1036 286

L Gilliam, National Solar Observatory/Sac PeakS/H003-Multiple Band Polarimeter (Monitor only)

Hilltop Dome/SP 0.00 0.00 13.00 58.00

1126 286

L Gilliam, National Solar Observatory/Sac PeakS/BOlO-H-Alpha Slitjaw Movie (Monitoring)

Big Dome/SP 0.00 0.00 1.00 5.00

1025 286

L Gilliam, National Solar Observatory/Sac PeakS/B057-Monitoring: Community

Big Dome/SP 0.00 0.00 81.00 177.00

1169 286

L Gilliam, National Solar Observatory/Sac PeakS/B007-USG-Disk Activity Program

Big Dome/SP 0.00 0.00 2.00 1.00

1053 286

L Goldberg, Kitt Peak National ObservatoryC Plymate, National Solar Observatory/TucsonT/Synoptic Radial Velocity Variations in alphaOri and ... McMath Main 5.50 13.50 0.00 0.00


Nights Hours Days Hours1139 286 JP Griffiths, L Gross,University of California, RiversideT/Temperature Broadening Coefficient of C02 LaserLines McMath FTS Lab 4.00 23.00 4.00 44.00

3790 286

J Harvey, National Solar Observatory/TucsonT/Vacuum Telescope Synoptic Program DailyMagnetograms Solar Vacuum 0.00 0.00 71.00 384.00

1158 286

F Hill, National Solar Observatory/TucsonL November, Sacramento Peak ObservatoryS/T247-Solar Oscillations Using 2 MDS Arrays

Vacuum Tower/SP 0.00 0.00 8.00 52.00

1142 286Y Huang, University of NanjingS/B184-High Resolution Spectra-Prominences,Filaments, Suns Big Dome/SP 0.00 0.00 20.00 77.00

1137 286R Hubbard, J Harvey,National Solar Observatory/TucsonT/G0NG Candidate Absorption Line Studies

McMath Main 0.00 0.00 2.00 17.00

1055 286D Jennings, D Denting, G Wiedemann,NASA Goddard Space Flight CenterJ Keady, Los Alamos National LaboratoryR Boyle, Dickinson CollegeT/Infrared Spectroscopy of the Sun and Planetsusing a ... McMath Main 0.00 0.00 6.00 20.00

1207 286S Keil, Sacramento Peak ObservatoryS/T258-Tests of the Agile Mirror on the ESG

Vacuum Tower/SP 0.00 0.00 6.00 24.00



J Kuhn, Princeton UniversityL Gilliam, National Solar Observatory/Sac PeakS/B134-Five Minute OscillationsAnisotropy/Amplitude Studie Big Dome/SP 0.00 0.00 3.00 32.00

1005 286

B Lites, T Brown, High Altitude ObservatoryT/Line Asymmetries in Solar Features Near theLimb McMath Main 0.00 0.00 4.00 0.00

1199 286W Livingston, National Solar Observatory/TucsonS/B190-CaK Spectroheliograms, 0.0 ft 0.38Angstrom Big Dome/SP 0.00 0.00 1.00 1.00

1149 286W Livingston, National Solar Observatory/TucsonL Wallace, Kitt Peak National ObservatoryT/Solar Irradiance Line Bisectors

McMath Main 0.00 0.00 1.00 11.00

4936 286W Livingston, National Solar Observatory/Tucson0 White, High Altitude ObservatoryZ Liu, Yunnan ObservatoryY Huang, University of NanjingT/Solar Cycle Variation of Sun as a Star

McMath Main 0.00 0.00 7.00 63.00

1201 286J LoPresto, Edinboro University of PA.S/T252-Variations of Solar Photospherlc SpectralLines Vacuum Tower/SP 0.00 0.00 6.00 65.00

5877 286

J LoPresto, Edinboro University of PA.A Pierce, National Solar Observatory/TucsonT/Solar Gravitational Redshift

McMath Main 0.00 0.00 2.00 0.00


n81 28g Nights Hours Days HoursJ LoPresto, Edinboro University of PA.S/B185-Variations of Photospheric Spectral Lines

Big Dome/SP 0.00 0.00 8.00 0.00

1041 286

R Mann, National Solar Observatory/Sac PeakS/T038-Telescope/Computer Updating/Maintenance

Vacuum Tower/SP 0.00 0.00 6.00 16.00

1147 286S Martin, H Wang,California Institute of TechnologyC Zwaan, ObservatoryK Harvey, %KPN0T/An Evolutionary Study of Quiet Sun Features

Solar Vacuum 0.00 0.00 7.00 81.00

1197 286

S Martin, California Institute of TechnologyK Harvey, %KPN0 &JS/B188-H-alpha, CaK Spectroheliograms

Big Dome/SP 0.00 0.00 5.00 5.00

1200 286S Martin, H Wang,California Institute of TechnologyK Harvey, 5?KPN0C Zwaan, ObservatoryS/T251-An Evolutionary Study of Quiet SunFeatures Vacuum Tower/SP 0.00 0.00 18.00 196.00

1198 286P Mcintosh,National Oceanic ft Atmospheric Admin.,BoulderS/B189-Filament and Prominence Spectra

Big Dome/SP 0.00 0.00 5.00 2.00

1135 286P Mcintosh,National Oceanic ft Atmospheric Admin.,BoulderL Gilliam, National Solar Observatory/Sac PeakS/BOOl-NOAA-Monitoring Program

Big Dome/SP 0.00 0.00 90.00 153.00


Nights Hours Days Hours5581 286M Mumma, D Deming, J Goldstein,NASA Goddard Space Flight CenterD Zipoy, T Hewagama, University of MarylandT/Astronomical ft Stratospheric InfraredHeterodyne Spectros McMath Main 6.00 75.00 2.00 20.00

1136 286H Neckel, Hamburger SternwarteD Labs, Landessternwarte HeidelbergT/FTS Spectra

McMath Main 0.00 0.00 2.00 13.00

1150 286H Neckel, Hamburger SternwarteD Labs, Landessternwarte HeidelbergT/Limb Darkening

McMath Main 0.00 0.00 7.00 65.00

5879 286A Pierce, National Solar Observatory/TucsonJ LoPresto, Edinboro University of PA.T/Solar Rotation from Several Fraunhofer Linesand the Ein. McMath Main 0.00 0.00 11.00 46.00

1122 286A Potter, NASA Johnson Space Flight CenterT Morgan, Southwestern UniversityT/Observations of Sodium in the Atmosphere atCrucial... McMath Main 0.00 0.00 4.00 40.00

1151 286K Rao, Ohio State UniversityS Davis, M Abrams,University of California, BerkeleyT/Infrared Bands of Aluminum Oxide

McMath FTS Lab 3.00 22.00 3.00 28.00

1006 286F Roesler, F Scherb, K Magee, J Harlender,J Brinkmann, University of WisconsinR Oliversen, NASA Goddard Space Flight CenterT/Continued Observations of Comet Halley

McMath West 26.00 208.00 0.00 0.00


1204 286 Nights Hours Days HoursB Rompolt, High Altitude Observatory/NCARS/T255-Rotational Motions in Spicules ft FineProminence Fil Vacuum Tower/SP 0.00 0.00 15.00 75.00

1148 286

B Rompolt, High Altitude Observatory/NCART Duvall, Jr., NASA Goddard Space Flight CenterT/Rotation of Supergranular Cells

Solar Vacuum 0.00 0.00 5.00 37.00

1205 286

B Rompolt, High Altitude Observatory/NCARS/T256-Rotation of Supergranular Cells-II

Vacuum Tower/SP 0.00 0.00 5.00 20.00

1112 286

D Rust, Johns Hopkins UniversityF Hill, National Solar Observatory/TucsonS/T238-Fabry-Perot Filter for Solar OscillationObservation Vacuum Tower/SP 0.00 0.00 10.00 102.00

1123 286

S Saar, University of ColoradoC Plymate, National Solar Observatory/TucsonT/Synoptic Observations of Stellar MagneticFields McMath Main 12.00 62.00 0.00 0.00

1057 286

S Saar, J Linsky, University of ColoradoT/A Survey of Magnetic Fields on Late-type Stars

McMath Main 3.00 25.00 0.00 0.00

1203 286

G Severino, Osservatorio CapodimonteC Marmolino, Institute of Experimental PhysicsG Roberti, Experimental Physics InstituteS/T254-CaII Lines as Diagnostics of SolarAtmospheric Dynam Vacuum Tower/SP 0.00 0 00 11 00 83 00


Nights Hours Days Hours1159 286E Seykora, East Carolina UniversityS/B179-Very Low Contrast White Light SolarStructures Big Dome/SP 0.00 0.00 2.00 12.00

1131 286

E Seykora, East Carolina UniversityS/B174-CaK, H-alpha Spectroheliograms, Supt B168

Big Dome/SP 0.00 0.00 2.00 2.00

1027 286

E Seykora, East Carolina UniversityR Smartt, National Solar Observatory/Sac PeakS/B113-Differential Photometry-Limb Darkening

Big Dome/SP 0.00 0.00 5.00 26.00

1018 286J Singh, Indian Institute of AstrophysicsK Harvey, %KPN0S Martin, California Institute of TechnologyT/Time Sequence of 10830 Spectroheliograms ftMagnetograms Solar Vacuum 0.00 0.00 8.00 57.00

1145 286

M Smith, C Plymate,National Solar Observatory/TucsonD Baade, European Space AgencyT/Nonradial Mode and Emission Activity in mu Cen

McMath Main 12.00 76.00 0.00 0.00

1144 286M Smith, National Solar Observatory/TucsonT/Nonradial Oscillations in Arcturus (Phase II)

McMath Main 6.00 28.00 0.00 0.00

1059 286W Smith, H Rivercomb, E Howell, A Arriaga,University of WisconsinH Bull, California State University, Long BeachT/Atmospheric Transmission Support of the NASAU-2 High... McMath Main 0.00 0.00 3.00 22.00


1146 286 Nights Hours Days HoursG Spear, Sonoma State Universityc.plymate. National Solar Observatory/TucsonJ(A lUTVey of the ° 1 Triplet for Cool Stars nearthe Main. McMath Main 5.50 29.00 0.00 0.00

1202 286

G Toot, University of ColoradoS/T253-Quiescent Solar Prominences

Vacuum Tower/SP 0.00 0.00 1.00 2.00

4942 286

0 White, High Altitude ObservatoryW Livingston, National Solar Observatory/TucsonZ Hu, Yunnan ObservatoryY Huang, University of NanlingT/Ca IT Variability 5

McMath Main 0.00 0.00 3.00 20.00

1154 286P Wiborg, USAFGLE/™auf*er- National Solar Observatory/Sac PeakS/T242-Tower/Sigma Three Conversion

Vacuum Tower/SP 0.00 0.00 12.00 82.00

1085 286

P Wilson, University of SydneyG Simon, USAFGLS/T213-Small Scale Magnetic Fields

Vacuum Tower/SP 0.00 0.00 7.00 28.00

1024 286

S Worden, 0SUDRE/ADEWS Keil, Sacramento Peak ObservatoryS/B044-Solar Rotation

Big Dome/SP 0.00 0.00 56.00 154.00

Documents

National Optical Astronomy - noao.edu Q3... · Cepheids in M101, agalaxy of fundamental importance to the extragalactic distance scale. M101 contains a number of red supergiants,