28
National Optical Astronomy Observatories National Optical Astronomy Observatories Quarterly Report October - December 1985
NationalOpticalAstronomyObservatories
National Optical Astronomy Observatories
Quarterly Report
October - December 1985
TABLE OF CONTENTS
I. Introduction \
II. Scientific Highlights 2A. The Kinematics of Radio Galaxies 2B. Chemical Abundances of Planetary Nebulae in M31...2C. Object Gomez 3D. Globular Clusters in External Galaxies 4E. Coordinated Space-Ground Observations of
Small-Scale Structure 4F. Solar Convection and the Activity Cycle 5
III. Personnel 5A. Visiting Scientists 6B. New Appointees 6C. Terminations 5D. Change in Status 6
Instrumentation and New Projects 7A. Advanced Development Program 7B. Instrumentation Projects ....8
Telescope Operations 11A. Kitt Peak National Observatory 11B. Cerro Tololo Inter-American Observatory 11C. National Solar Observatory 11
VI. Program Support 13A. Director's Office 13B. Public Information 13C. Office of Resource and Program Management 13D. Central Computer Services 14E. Engineering and Technical Services 15
IV
V.
Appendices
A. Observational Programs8. Telescope Usage Statistics
I. INTRODUCTION
This Quarterly Report, the first for FY 1986, is in a new format. The majorchanges are in sections IV. Instrumentation and New Projects, V. TelescopeOperations, and VI. Program Support. Previous reports combined all of thesecomponents of NOAO under a section titled Division Reports.
This quarter saw the NOAO management beginning a new fiscal year under acontinuing resolution—and resultant spending limitations—until a budgetfigure was assigned by the NSF. Late in the quarter unofficial notice wasgiven of a budget figure which was $750K below the figure in the FY 1986Program Plan. In addition we were asked to carry out a budgeting exercise atseveral different levels in response to the probable implementation of theGramm-Rudman-Hollings legislation to reduce the national deficit.
II. SCIENTIFIC HIGHLIGHTS
A. The Kinematics of Radio Galaxies.
The role of the host galaxy in generating an active nucleus has recently beenstudied by R. Davies (NOAO) and M. Birkinshaw (Harvard) and by T. Heckman(U. of Maryland), G. Illingworth (ST Scl), G. Miley (ST Scl) and W. vanBreugel (U.C. Berkeley) using the Cryogenic camera to measure the kinematicsof radio galaxies.
After the discovery that the elliptical galaxies that host radio sources couldbe triaxial, early work on the kinematics of a small number of radio galaxiesproduced some surprising results. It appeared that the radio galaxies rotatedfaster than quiescent elliptical galaxies and that their rotation and minoraxes were grossly misaligned, indicating that their figures were stronglytriaxial. These conclusions suggested that the intrinsic properties of agalaxy play a vital role in the generation of activity.
The kinematic surveys carried out at Kitt Peak were aimed at searching foralignments between radio structure and the rotation axes of the host galaxyand for other correlations between the optical and radio properties that wouldindicate the mechanism involved in the onset of activity. The two groupsstudied more than 30 galaxies and concluded that there are no_ differencesbetween kinematics of active and quiescent galaxies. In particular they foundno evidence that radio galaxies rotate faster and for only a small fraction oftheir sample do the rotation and minor axes significantly misalign. (Byrepeating the earlier observations they demonstrated them to be in error).Both groups showed that the stellar rotation axis does not align with theradio structure. Heckman et al. demonstrated that for those galaxies with anextended interstellar medium the ionized gas rotation axis is often notaligned with that of the stars but does tend to align with the radiostructure. Davies and Birkinshaw demonstrated that the host ellipticalgalaxies display the full range of figure types, most galaxies being close tooblate, but with a few cases of triaxial forms and one galaxy that is prolate.
These groups found no evidence to suggest that the galaxies hosting radioactivity are kinematically different from quiescent ellipticals. Theirresults support the hypothesis that activity is generated when gas is accretedfrom outside; this gas can remain on the stable orbits that rotate about the
long axis of a triaxial ellipsoid and thus are "misaligned" with respect tothe stars. The ionized gas is usually enriched in heavy elements so that itwas accreted from another galaxy; searches are now underway for directevidence of that accretion event.
3. Chemical Abundances of Planetary Nebulae in M31.
G. Jacoby (NOAO) and H. Ford (ST Scl) have measured the chemical compositionin three planetary nebulae and an H II region in the Andromeda galaxy. Nearly400 planetary nebulae were discovered using the Kitt Peak 0.9-m and 4-mtelescopes, and the Lick 3-m telescope. The three planetaries that werestudied in detail were chosen for their wide separation across the face of theAndromeda galaxy to sample the chemical composition at a variety of locationsin that galaxy. The planetaries have distances from the center of the galaxy
The evolutionary stage of the objects is uncertain, and has been muchdebated. Because of the configuration of the dust surrounding the hot stars,it is clear that these objects are in a relatively brief, short-lived phase intheir evolution. The dust could represent accreted material in a cloud out ofwhich the stars have just formed, or it could be material which has beenejected by the stars in a late stage of stellar evolution as the systemsbecome planetary nebulae. Further research will discriminate between thedifferent alternatives, however the fact that so few objects in our Galaxyhave these characteristics points out how rare it is that this particularevolutionary phase can be observed directly.
D. Globular Clusters in External Galaxies.
Globular clusters are excellent tools for investigating galaxy formation andthe structure of galactic halos. In addition, they are being used tocalibrate the extragalactic distance scale. The Cerro Tololo 4-m prime focusCCD is an ideal detector for doing photometry to establish the clusterluminosity function, and several groups have done this for relatively nearbyelliptical galaxies.
The globular clusters have been discovered to have a distribution that is lesscentrally condensed than the host galaxy's halo light. This is a generalfeature of large E galaxies, and taken with the lower cluster metallicitieswith respect to halo stars, suggests a galaxy formation picture in whichglobular clusters form first, before the halo material has finished its
collapse. If this is confirmed for many galaxies, it is strong evidence thatglobular clusters are probably the most direct link between the much suspected"dark matter" and the visible galactic halos.
Throughout the report year G. Da Costa (Yale) and J. Mould (Caltech) havecontinued their studies of the intermediate age globular clusters in the Largeand Small Magellanic Clouds using data obtained with the 4-m prime focus CCDsystem. Color-magnitude diagrams have been completed for the SMC cluster NGC121 and for the LMC cluster NGC 2213. For NGC 121 the age was found from mainsequence isochrone fitting to be 12 ± 2 billion years if a distance modulusthat assumes Mv = +0.6 for the field RR Lyrae variables near the cluster isused. The cluster is known to contain both RR Lyrae variables and a marginalcarbon star. Using cluster ages derived in this study, a new look at thechemical evolution of the SMC suggests that, unlike our Galaxy where the rateof enrichment has been steady after the initial phase, the enrichment in theSMC remained small for a long interval before increasing rapidly sometime inthe last one or two billion years. This age estimate is considerably youngerthan the age obtained by M. Aaronson (U. of Arizona) and Mould from theluminosity of the brightest carbon stars in the cluster. Reduction andanalysis of observations of other Magellanic Cloud clusters is continuing.
E. Coordinated Space-Ground Observations of Small-Scale Structure.
Most Calcium II K-line emission and magnetic field on the quiet Sun isconcentrated on the supergranulation network. Inside a typical network cell,however, five to 10 small "bright points" are found. These points haveaverage lifetimes of 50 seconds. Similar small features are also found inultraviolet spectroheliograms (near X1600 A) and in high-qualitymagnetograms. M. Bruner (Lockheed Palo Alto Research Lab) and her co-workers
III. PERSONNEL
A. Visiting Scientists.
The following visitors arrived at NOAO facilities for periods of one month ormore, during the October 1 to December 31, 1985 quarter.
date arrived
10/01/8510/01/85
10/15/85
10/15/85
12/01/85
12/17/85
name
You-ran HuangZhenda Zhang
Ciro Marraolino
Edward FitzpatrickElizabeth Ribes
Neil Sheeley, Jr.
institution NOAO facility
visited
Nanjing University, China NSONanjing University, China NSO
Universita di Napoli, Italy NSOUniversity of Colorado CTIO
Observatoire de Meudon, France NSONaval Research Laboratory NSO
B. New Appointees.
The table below shows details of new appointments made to the NOAO during thequarter, October 1, 1985 - December 31, 1985.
namedate of appointment10/01/85
11/01/85
11/08/85
Khairy Abdel-GawadGlenn Spence
Elaine Sadler
position
Senior EngineerSenior Engineer
Research Associate
NOAO division
NOAO
NSO
KPNO
Terminations.
date
12/13/85
12/23/85
12/27/85
12/30/85
name
Nelson Caldwell
Brian Jarvis
Steve Howell
Henry Erikson
D. Change in Status.
date name
10/01/85 Jon Settlemyre
11/16/85 Anthony Abraham11/16/85 Robert Nagel11/16/85 Richard Reed
i1/16/85 William Robinson,11/16/85 Nigel Sharp
12/01/85 Frank Valdes
position
Assistant Astronomer
Research Associate
Scientific Programmer II
Senior Engineer
change in status(from/to)
NOAO division
CTIO
CTIO
NOAO
NOAO
NOAO division
Asst. Mgr. Mtn. Oper./Technician Assoc.-Gen. KPNO
Section Head/Department Manager NOAOEngineering Mgr./Department Manager NOAOSection Head/Senior Engineer NOAOEngineering Mgr./Senior Proj. Mgr. NOAOResearch Associate/
Asst. Support Scientist NOAO
Asst. Support Scientist/Assoc. Support Scientist NOAO
IV. INSTRUMENTATION AND NEW PROJECTS
A. Advanced Development Program.
A major part of the work in the NNTT Program this quarter was in thedevelopment of technology for the large primary mirrors. At NOAO, the opticaltesting of a prototype 1.8-m honeycomb mirror is demonstrating the ratherstringent thermal requirements for V4arcsecond imaging. Especially useful inthis evaluation is a new computer code developed at NOAO to model the opticaleffects of a given temperature distribution in the mirror. Along withimprovements in the optical testing, this computer modeling providesspecifications for the allowable temperature gradients and the glasshomogeneity of the mirrors.
At the Mirror Casting Facility at the University of Arizona, substantialprogress was made on the 25-ton steel turntable that will hold the furnace forthe 3.5-m spin casting and, ultimately, the furnace for 7.5-m mirrors. A 40-ton bridge crane was installed, welding proceeded apace, the furnace controlsystem was mapped out, and Ohara E6 glass was ordered for the first 3.5-mcasting.
The optical support structure for the NNTT continues to undergo a structuralanalysis. The computer model was fully developed this quarter, and the firstresults show the structural effects of temperature gradients along andperpendicular to the telescope's pointing direction^ Meanwhile, a 1/60 scalemodel of the NNTT was completed in December and was sent to Houston for an
unveiling at the January meeting of the American Astronomical Society.
Two of the Instrument Working Groups met in November and December to refinethe specifications for the NNTT's infrared instrumentation. In consultationwith these groups, the optical engineers at NOAO developed the penultimatelayouts for the IR imaging system (central combined Cassegrain focus) and thehigh-resolution IR spectrograph (Nasmyth focus).
2Tests continued with the coalignment/cophasing system (C S) mockup in thelaboratory. These included primarily tolerancing tests for tilt anddisplacements. Measurements are consistent with calculations.
NNTT site testing ended at Mauna Kea as planned, on December 31. Full-scaletesting will continue at Mt. Graham through March, to fill in the "winter gap"caused by the logistical impossibility of keeping the site open duringprevious winters. At both sites, automatic data loggers will continue tomonitor wind, temperature, and microthermals.
A dummy load was developed for the testing of the Itek electronics for theadaptive mirror for the adaptive optics project and the testing was begun.The major optical components for coupling the adaptive mirror to the telescopeand IR detectors were delivered and prepared for installation. The mount forthe adaptive mirror was designed and fabricated. The design of a high speedtip-tilt mirror (to remove mean wavefront tilts) was initiated. A pilotprogram was outlined for the investigation of techniques for the constructionof large adaptive mirrors. Adaptive Optics Associates completed constructionof the chassis and major processor boards for the wavefront tilt sensor andbegan testing of the Reticon detector.
camera body is mostly complete with final assembly expected during the thirdquarter.
All of the major design, fabrication, and integration required for theKPNO 4-m PF CCD Mounting project was completed this quarter with majoremphasis on final documentation, technical support of telescope engineeringruns, and software development.
All of the McMath Computer System hardware has been installed. Work on theproject during this quarter involved the conversion of software from theVarian computers to the new DEC machines. This conversion is expected tocontinue through FY 1986.
Design concepts were completed and structural analysis of the design wasstarted for the McMath Windscreen Project. Final design is expected to becompleted next quarter with installation planned for late May 1986.
After a delay of approximately three months caused by image tube problems, thesecond of the "2D-Frutti" two-dimensional photon counting detectors was putinto regular service on the Cassegrain spectrograph of the 1-m Yale telescope(CTIO). The 2D-Frutti offers more than a factor of two to increase in speedover the image tube plus photographic plates combination used for many yearson this spectrograph.
A new dectector array was installed in the Cerro Tololo Infrared Spectrometer(IRS) and this instrument was successfully tested at the telescope. The IRShardware is now nearly complete, although some software work is stillrequired.
The Cerro Tololo 4-m Telescope Prime Focus CCD (PFCCD) System data acquisitioncomputer was upgraded to include a faster, 22-bit LSI-11/73 CPU and a 160MByte disk. Until now, the PFCCD system, which was built in Tucson andinstalled on the CTIO 4-m in 1982, employed a dedicated 18-bit LSI-11/23 andan old version of the FORTH-11 software. With the upgrade, the same computersystem is now used to control both the PFCCD and the other CCD detectorsemployed on the 4-m telescope spectrographs.
The first of two computer-controlled shutter/filter wheel assemblies designedto accommodate large-format CCD chips for imaging at the Cassegrain foci ofthe CTIO 4-m, 1.5-m, and 0.9-m telescopes was put into regular service. Thisfirst assembly has one precision-controlled filter wheel which can hold up toeight 3-inch filters and a special "preflash" unit (used to improve chargetransfer efficiency with certain chips).
The second VAX-U/750 computer for CTIO was successfully installed in LaSerena in December. The two VAX computers will be used exclusively for datareduction and analysis, principally with IRAF software.
Two essential steps have been taken during this past quarter to convert theVacuum Tower Telescope at Sacramento Peak into a facility for studying vectormagnetic field measurements at sub-arcsecond resolution. A new entrancewindow has been tested and installed. The new window is only 4-cm thick (thepresent window is 10-cm thick). Tests under vacuum showed that radialinternal stresses are present to a much smaller extent than in the original
V. TELESCOPE OPERATIONS
A. Kitt Peak National Observatory.
Operations efforts at Kitt Peak for the period October - December 1985included: refurbishing the 4-m prime focus pedestal; cleaning and/oraluminizing optics on the Coude* feed, #1-0.9-m and Burrell-Schmidt; completionof the design to interface the 2.1-m drive encoders to the TCP computer; beganfabrication of new drive preload power supplies for the #2-0.9-m; andcompletion of the Emergency Center on Kitt Peak.
B. Cerro Tololo Inter-American Observatory.
The biannual collective bargaining sessions with the Observatory's unionizedChilean hires began on 21 November when they presented their requests in theform of a proposed contract. Various counter-proposals by NOAO and the Unionfollowed in negotiation sessions during December. A new, two-year contract(for calendar years 1986 - 1987) was signed on 31 December.
The GOC's original estimate for inflation in CY 1985 was 20%. When inflationreached 21% as of 30 September, this estimate was revised upward to 25-30%.The actual inflation turned out to be 26.4%. The GOC is presently predictingan inflation of 15 - 20% in CY 1986.
Statistics for the first three months of FY 1986 are:
AVG. MONTHLY
MONTH % CHANGE IN CPI CUM. CHANGE IN CPI PESOS/DOLLAROct. 1.5 1.5 179.24Nov. 1.6 3.1 180.57
Dec. 1.3 4.5 182.48
On the mountain, the effects of the new work schedule which began in Augustbegan to be felt. Although block scheduling of telescope time helped todecrease manpower requirements, the overall level of support offered tovisitors and staff astronomers, particularly on the smaller telescopes,definitely declined. The reduced personnel levels also had an adverse effecton routine maintenance of instrumentation and telescopes.
C. National Solar Observatory.
NSO operations efforts for this quarter were centered around two majorinstruments—the Fourier Tachometer and the McMath telescope.
The High Altitude Observatory Fourier Tachometer was moved from the Sac PeakBig Dome to a basement room of the Tucson offices in November. The objectiveof this move is increased synoptic observing time due to increased freedomfrom orographic clouds and the circumstance of being a dedicated (non-shared)facility. The existing roof-top 40-cm heliostat was refurbished, an opticaltable and LSI 11/23 computer provided, and ETS has designed a high speedguider with X-Y scan capability.
1 1
VI. PROGRAM SUPPORT
A. Director's Office.
With the beginning of a new fiscal year efforts in the Director's Office werefocused toward developing a long range plan for NOAO (FY 1987-91) andcompleting the Annual Report for submission to the NSF as well as to the AAS
for inclusion in the BAAS to be published in early 1986.
In December the Director was given (verbally) the FY 1986 budget figure andasked to prepare budget exercises at several levels in anticipation of furtherbudget reductions in response to Congressional action to reduce the nationaldeficit. It became apparent that efforts to define NOAO's program in relationto the funding situation are of utmost importance and must be continued untila solid program is defined.
B. Public Information.
Eight Halley images from Kitt Peak and Cerro Tololo were issued to the mediaduring this period. On November 18, a press workshop on Comet Halley was heldon Kitt Peak, where a four-astronomer team briefed journalists on the cometand their preceding four-day observing run on the Mayall 4-m. John Wilford ofthe NEW YORK TIMES, Robert Cowen of the CHRISTIAN SCIENCE MONITOR, Arlen Largeof THE WALL STREET JOURNAL, and Hill Williams of THE SEATTLE TIMES were amongthe 50-plus journalists attending. There was also strong internationalrepresentation, with reporters from Italian and German magazines, and, throughthe USIA's Foreign Press Centers, television crews from Japan, Korea, andSweden. Numerous regional and lccal stations also participated. Ten KittPeak public evenings were conducted during the period.
A video news clip produced for the Halley workshop went out nationally andinternationally, and marked the beginning of a new series of information
products, which included a second clip on the discovery of oxygen-richfilaments in the Puppis A supernova remnant, the major science story issuedduring the period. A contract videographer was sent to Chile to tape materialfor a series of video features and newsclips on CTIO and its research program.
Confirmation was received that National Television of Chile will provide, atno cost to NOAO, satellite uplinking almost dailv for near-real-time video
feeds of the comet from Cerro Tololo to the Atlantic International Satellite,from which any user can bring it down.
A new computer print-out NOAO photo catalogue was received from the printer.
C. Office of Resource and Program Management.
During this quarter the Project Management system was applied to all NOAOFY 1986 projects. The system involving central ETS personnel is functioningquite well in its early stages of implementation. Scientists are becomingmuch more involved in their projects, and a realistic project priority andscheduling system, set and maintained by the NOAO Director and Associate
Directors, has been implemented NOAO-wide. The system has also identified andcorrected unapproved increases in the scope of certain projects.
13
Coudg, IRS, and IIDS. Numerous analysis tools were written. IRAF wasexported to Sunspot, CTIO and Johns Hopkins University.
E. Engineering and Technical Services.
An attempt was made to rule a 632 lines/mm, 57° blaze ruling for the McMathTelescope. This was done in collaboration with the Milton-Roy Company whichfurnished the master blank and coating under letter of agreement signed duringthe previous summer.
The Coatings Lab provided coatings on 66 surfaces during this quarter.
The Optical Shop completed polishing of 57 surfaces. The 90-inch grindingmachine was removed from the Main Optics Lab and a large vibration isolatedtest bench was installed in its place.
15
CERRO TOLOLO INTER-AMERICAN OBSERVATORY
APPENDIX A
OBSERVATIONAL PROGRAMS
October - November - December 1985
Individual telescope assignments are listed below. Graduatestudents are indicated by an asterisk after their name. Nightsassigned, (Hours worked), and telescope used are included.
C. Anguita and M.T. Ruiz, Universidad de Chile: "CCD Parallaxesfor Faint High Proper Motion Stars", 5(32.5)1.5m.
B.J. Anthony-Twarog, 3. Twarog, University of Kansas, and J. Laird,University of Michigan: "Extension of the uvby System to CoolDwarfs", 7(32)0.6.
V . M Blanco, NOAO, and M.F. McCarthy, Vatican Observatory ResearchGroup, Tucson: "Discrepant Mean Magnitudes of LMC CarbonStars", 4 ( 31* .7 )4m .
B.M. Blanco and V.M. Blanco, NOAO: "Calibration of a StellarSequence in the Large Magellanic Cloud", S.O. 1(8)4m.
B. Bohannan, University of Col or ado:'" Photometry of LMC Emission-Line Supergiants", 7(62. 5)1m, 3(26)1.5m.
N. Caldwell, NOAO: "Spectral Survey of Galaxies", 12(57 )1m , 1(8)0.9m.
G.A. Channan, D.J. Helfand and T.T. Hamilton*, Columbia University: "Search for Low Surface Brightness Optical Counterparts of Extended X-ray Sources in the LMC", 3(24.5)4m.
G.S. Da Costa, T. Armandroff* and R. Zinn, Yale University: "Velocity Dispersion and Metallicity Range in the Sculptor DwarfSpheroid", 4(32.2)4m.
J.T. Davidge* and C.J. Scarfe, University of Victoria, Canada:"UBV Photoelectric Photometry of LMC Eclipsing Binaries",10(63)1m.
K. De Gioia-Eastwood, University of Wisconsin, P. Massey, NOAO,E. Olszewski, University of Arizona, and G. Garmany, University of Colorado: "H-R Diagrams for Massive Stars in the OBAssociations of the Magellanic Clouds", 10(81 .5)0.9m.
S. Demers, F. Wessemaei, G. Fontaine, University of Montreal,E. Kibblewhite and M. Irwin, University of Cambridge: "MontrealCambridge Survey of Blue Subluminous Stars", 9(71.7)MS.
O.J. Eggen, NOAO: "Intermediate Band and RI Photometry of GalacticCepheids" , 5(39 .4 )1 .5m.
J. Elias, California Institute of Technology, and J.A. Frogel,NOAO: "CN Band Strengths in Magellanic Cloud M Supergiants",4(37.8)1.5m.
T. Heckman, Johns Hopkins University, G. Miley, STScI, and L. Armus,University of Maryland: "Super-Luminous Infrared StarburstNuclei", 3(19.25)4m, 3(19.5)1.5m.
G. Illingworth, and M. Franx*, STScI, and T. Heckman, Johns HopkinsUniversity: "The Shapes of Elliptical Galaxies; Prolate Triaxialor Merely Oblate?", 5(20. 5)4m, 6(28)0.9m.
K. Kawara, NOAO: "The Infrared Spectroscopy of Emission LineGalaxies", 4(39.8)4m.
C. King, and G. Da Costa, Yale University: "Stellar Populations inthe Bulges of Spiral Galaxies", 3(31.5)4m, 4(5)1.5m.
A.U. Landolt, and A. Uomoto, Louisiana State University: "UBVRIPhotometric Sequences I, II, III and IV", 8(49.6)4m,7(33-2)1.5m, 2(14)0.9m, 2(16)0.6m.
A.U. Landolt, Louisiana State University: "A Photometric Study ofthe Open Cluster NGC 2818" , S.O. 1(8.9)4m.
J. Maza, and M. Hamuy, Universidad de Chile: "Study of ActiveGalactic Nuclei", 9(22.5)0.6m.
J. Maza, and M. Hamuy, Universidad de Chile: "Photometric SequencesAround NGC 1313 and Fornax A". 2(12)0.9m.
D.J. MacConnell, Michigan State University, R. Wing, Ohio StateUniversity, and E. Costa, Universidad de Chile: "Follow-upPhotometry and Spectroscopy of Suspected M Supergiants",3(27)1.5m, 3(24.9)1m.
V.S. Niemela, Instituto de Astronomia y Fisica del EspacioBinaries", 10(79)1m.
"OB
R 0'Connell, D.A. Crocker* and R.T. Rood, University of Virginia"Helium Abundances in Globular Cluster Horizontal Branches",5(50.5 )4m.
Olszewski, University of Arizona, R. Schommer, Rutgers University,and H. Harris, Lowell Observatory: "Outlying LMC Clusters",4(33)1-5m.
M. Pedreros, Universidad ae Chile: "CCD BVRI Photometry of Southern(23.4)0.9mOpen Clusters'
R.L. Pennington and R. Humphreys, University of Minnesota: "DigitalSurface Photometry of Dusty Ellipticals", 4(33)1.5m, 8(56.4)1m
M.M. Phillips and A.C. Phillips, NOAO: "A Search for Supernova inStarburst Nuclei", 6(30.5)0.9m.
H. Quintana, Universidad Catolica de Chile: "Multiple NucleiBrightest Galaxies in a Complete Cluster Sample", 4(29)0.9m.
Yale Programs:
J. A. Eder* and A. Oemler: "The correlation Between Neutral HydrogenContent and Optical Properties for Early-TyDe Disk Galaxies",7(33.5)0.9m.
G.S. Da Costa: "Surface Photometry of Magellanic Cloud Clusters",7(46.8)0.9m.
J.P. Vader: "Morphology and B-R colors of Dwarf Ellipticals inthe Fornax Cluster and of Optically Idetified, Infrared Luminous(IRAS), Galaxies", 5(40.3)0.9m.
KITT PEAK NATIONAL OBSERVATORY
APPENDIX A - OBSERVATIONAL PROGRAMS
EXECUTED PROPOSALS 10/1/85 - 12/31/85
Nights Hours Days Hours5678 f85
H Abt, Kitt Peak National ObservatoryA Search for Low-Mass Companions to High-VelocityStars 2.1m Coude Feed 10.00 69.50 0.00 0.00
5918 f85
H Abt, Kitt Peak National ObservatoryMK Classification of Visual Multiple Stars
Nr. 1 0.9 meter 6.00 22.50 0.00 0.00
5920 f85
B Balick, R Owen, University of WashingtonR Hjellming,National Radio Astronomy Observatory, VLAWind-Induced Structure & Motions of PlanetaryNebulae 4 meter 5.00 25.00 0.00 0.00
2.1 meter 5.00 49.50 0.00 0.00
5981 f85
S Barden, Kitt Peak National ObservatorySpectroscopic Investigations of Short PeriodLate-Type 2.1 meter 4.00 34.75 0.00 0.00
9011 f85
M Belton, Kitt Peak National ObservatoryObservations of P/Halley for AstrometricPurposes Nr. 1 0.9 meter 3.00 7.50 0.00 0.00
6033 f85
W Blair, Johns Hopkins UniversityR Fesen, University of Colorado, LASPSpectroscopy of Young Supernova Remnants
2.1 meter 4.00 5.00 0.00 0.00
6041 f85
B Bohannan, University of ColoradoJ Vreux, University of LiegeT Hua, Canada-France-Hawaii Telescope Corp.Coordinated Observations of Line-Profile
Variations 2.1 meter 4.50 39.50 0.00 0.00
Nights Hours Days Hours6040 f85
G Chincarini, R Henry, University of OklahomaInfrared Magnitudes of SuperclusterGalaxies-Perseus-Pisces 1.3 meter 7.00 44.00 0.00 0.00
6039 f85
J Cowan, R Henry, D Branch,University of OklahomaA Search for Optical Emission from RecentGalactic 2.1 meter 4.00 32.50 0.00 0.00
6115 f85
R Davies, Kitt Peak National ObservatoryM Birkinshaw, Harvard UniversityAn Imaging Survey of Galaxies Hosting RadioSources 4 meter 3.00 19.25 0.00 0.00
6009 f85
P Demarque, W van Altena, Yale UniversityP Lu, Western Connecticut State CollegeH McAlister, Georgia State UniversityBinary Search Among High Velocity Dwarf STars
4 meter 2.00 17.50 0.00 0.00
6058 f85
S Djorgovski, H Spinrad,University of California, BerkeleyEvolution of Galaxies at High Redshifts: Imaging& 4 meter 3.00 34.75 0.00 0.00
5965 f85
J Drilling, Louisiana State UniversityK Hunger, D Schonberner, Kiel UniversityA Spectroscopic Study of Blue Stragglers in NGC7789 4 meter
1.3 meter
6148 f85
P Eisenhardt, NOAO-ADP
R Davies, Kitt Peak National ObservatorySpectrophotometry of Galaxies at ModerateRedshifts 4 meter 2.00 16.50 0.00 0.00
4.00 19.00 0.00 0.00
4.00 5.00 0.00 0.00
Nights Hours Days Hours6155 f85
J Gallagher, R Joyce,Kitt Peak National ObservatoryD Hunter, Carnegie Institution of WashingtonImage Galaxies to Determine the Distributions ofCool Stars 2.1 meter 3.00 24.00 0.00 0.00
6025 f85
F Gillett, R Joyce,Kitt Peak National ObservatoryK Merrill, NOAO-ADP
Followup of IRAS Galactic Sources1.3 meter 8.00 27.00 0.00 0.00
5901 f85
R Green, Kitt Peak National ObservatoryJ Liebert, University of ArizonaA Deep Sky Near Infrared/Optical Survey
2.1 meter 5.00 7.00 0.00 0.00
6001 f85
J Grigsby, N Morrison, University of ToledoHigh Dispersion Spectroscopy of Early B-TypeStars in 2.1m Coude Feed 5.00 45.00 0.00 0.00
6046 f85
D Hall, University of HawaiiK Hinkle, Kitt Peak National ObservatoryA Search for Dark Companions of K and M Giants
4 meter 0.00 0.00 1.50 10.75
6037 f85
T Heckman, Johns Hopkins UniversityS Baum, A Bridle,
National Radio Astronomy ObservatoryG Miley, Space Telescope Science InstituteCCD Imaging of Gas Associated with the Lobes ofExtragalact 4 meter 3.00 30.75 0.00 0.00
6055 f85
A Henden, NASA Goddard Space Flight CenterUBVRI Photometry of the Binary Cepheid CE Cas
Nr. 1 0.9 meter 5.00 26.00 0.00 0.00
Nights Hours Days Hours6035 f85
K Josafatsson, University of Colorado, APAST Snow, Jr., University of Colorado, LASPDiffuse Interstellar Bands & Micrograins
2.1 meter
2.lm Coude Feed
5938 f85
R Joyce, Kitt Peak National ObservatoryT Brooke, R Knacke, SUNY at Stony BrookInfrared Polarimetry & Spectrophotometry of CometHalleY 2.1 meter 3.00 7.50 0.00 0.00
6130 f85
V Junkkarinen, Kitt Peak National ObservatoryA Spectroscopic Study of Narrow & Broad QSOEmission Lines 2.1 meter 4.00 41.50 0.00 0.00
6017 f85
S Kenyon, Center for AstrophysicsE Seaquist, University of TorontoA Taylor, University of GroningenInfrared & Optical Observations of SymbioticStars 1.3 meter
Nr. 2 0.9 meter
5976 f85
K Kwitter, Williams CollegeG Jacoby, NOAO-CCS
A Deep Search for Faint Central Stars ofPlanetary Nebulae 2
Nr. 1 0
5975 f85
K Kwitter, Williams CollegeP Massey, Kitt Peak National ObservatoryA Deep Search for Faint Remnant Planetary NebulaeAround... Nr. 1 0.9 meter
Nr. 2 0.9 meter
4.00 8.75 0.00 0.00
4.00 43.50 0.00 0.00
4.00 6.50 0.00 0.00
7.00 40.00 0.00 0.00
1 meter 4.00 40.50 0.00 0.00
9 meter 5.00 42.00 0.00 0.00
5.00 0.00 0.00 0.00
5.00 11.00 0.00 0 .00
Nights Hours Days Hours6154 f85
P Massey, S Wolff,Kitt Peak National ObservatoryPhotometry of Clusters in the AnticenterDirection Nr. 1 0.9 meter 4.50 15.00 0.00 0.00
5932 f85
P Massey, Kitt Peak National ObservatoryP Conti, University of ColoradoT Armandroff, Yale UniversityWolf-Rayet Stars in M31's OB Associations
4 meter 3.00 9.00 0.00 0.00
5913 f85
R Mathieu, Smithsonian Astrophysical ObservatoryInternal Kinematics of OB Associations
2.1 meter 4.00 50.00 0.00 0.00
5654 f85
H McAlister, W Hartkopf, D Hutter, H Miller,Georgia State University0 Franz, Lowell ObservatoryP Schmidtke, Arizona State UniversityAstronomical Speckle Interferometry with the GSUSpeckle .. 4 meter 6.00 49.25 0.00 0.00
6150 f85
D McCarthy, University of ArizonaNear-Infrared Imaging of Low Mass Companions toNearby 4 meter 5.00 26.50 0.00 0.00
6027 f85
K Meech, D Jewitt,
Massachusetts Institute of TechnologyPlasma Tail Dynamics of Comet p/Halley
Burrell Schmidt 11.00 41.50 0.00 0.00
5905 f85
K Merrill, NOAO-ADP
R Joyce, F Gillett, K Gillies,Kitt Peak National ObservatoryInfrared Monitoring of Late-Type Stars &Protostellar Objec 1.3 meter 6.50 23.00 0.00 0.00
Nights Hours Days Hours
6117 f85
R Oliversen, T Gull,
NASA Goddard Space Flight CenterT Williams, Rutgers UniversityR Fesen, University of Colorado, LASPKinematics of the Crab Nebula
2.1 meter 6.00 45.50 0.00 0.00
6065 f85
J Patterson, Columbia UniversityRotational Period Changes in Accreting WhiteDwarfs Nr. 2 0.9 meter 8.50 58.00 0.00 0.00
5997 f85
C Pilachowski, A Saha,Kitt Peak National ObservatoryLithium in Old Galactic Clusters: Studies of New
Giants 2.1m Coude Feed 6.00 43.00 0.00 0.00
6067 f85
C Pilachowski, Kitt Peak National ObservatoryR Milkey, Space Telescope Science InstituteRotation in White Dwarfs
4 meter 3.00 26.00 0.00 0.00
6098 f85
R Probst, Kitt Peak National ObservatoryC Dahn, U.S. Naval ObservatoryJ Liebert, University of ArizonaP Boeshaar, Rider CollegeInfrared Photometry of Late Type Subdwarfs
2.1
1.3
6099 f85
R Probst, Kitt Peak National ObservatorySearch for Substellar Companions To Ursa MajorStream Stars 1.3 meter
Nr. 1 0.9 meter
9016 f85
S Ridgway, NOAO-CCSJ Mariotti, Observatoire de LyonDouble Fourier Spatio-Spectral Interferometer
4 meter 0.25 1.50 1.00 0.50
meter 4.00 16.25 0.00 0.00
meter 3.00 34.00 0.00 0.00
5.00 35.00 0.00 0.00
3.00 20.00 0.00 0.00
Fnnr> Nights Hours Days Hours5928 f85
M Shara, P Stockman,Space Telescope Science InstituteNarrowband Imagery of Dwarf & MagneticCataclysmic Variable Nr. 1 0.9 meter 7.00 15.50 0.00 0.00
6003 f85
M Simon, SUNY at Stony BrookJ Vader, Yale UniversityStar Formation in IR-luminous Galaxies
2.1 meter 4.00 33.75 0.00 0.00
6004 f85
M Simon, F Hamann, SUNY at Stony BrookR Joyce, Kitt Peak National ObservatoryLunar Occultation Observation of Young Stars inTaurus 4 meter 0.50 6.50 0.00
6151 f85
M Sitko, Kitt Peak National Observatory
0.00
Simultaneous UV, Optical and IR Observations ofthe Variabl 1-3 meter 5i00 44.00 0,00
0.00
6062 f85
V Smith, University of Texas, AustinK Gillies, Kitt Peak National ObservatoryInfrared Excesses in Barium Stars
1.3 meter 2.00 15.25 0.00 0.00
5971 f85
J Sowell, R Sears, University of MichiganDetailed Observations of Galactic SuperluminousGiants 2.1m Coude Feed
Nr. 2 0.9 meter
5934 f85
H Spinrad, S Djorgovski,University of California, BerkeleyLyAlpha & Ionized C Emission Lines - New RedshiftKeys for. 4 meter 3 00 14>50 0#00 0_00
5.00 18.50 0.00 0.004.50 25.00 0.00 0.00
Nights Hours Days Hours
5073 f85
P Wehinger, S Wyckoff, Arizona State UniversityH Spinrad, University of California, BerkeleyM Belton, Kitt Peak National ObservatoryD Yeomans, Jet Propulsion LaboratoryPhysical & Chemical Properties of the Atmosphere,Ionospher 4 meter 4.00 38.00 0.00 0.00
5321 f85
E Weis, Wesleyan UniversityA Photometric Search for Nearby Dwarf M Stars
Nr. 2 0.9 meter 5.50 42.50 0.00 0.00
5954 f85
F Winkler, Middlebury CollegeR Kirshner, University of MichiganChemistry & Kinematics of Cassiopeia A
4 meter 3.50 29.00 0.00 0.00
6153 f85
S Wolff, Kitt Peak National ObservatoryHelium Abundances in Orion
2.1m Coude Feed 4.00 29.00 0.00 0.00
6036 f85
D York, G Burks, University of ChicagoDistances to 21 cm High Velocity CloudsInteracting with... 2.1m Coude Feed 4.00 12.00 0.00 0.00
5998 f85
A Young, San Diego State UniversityA Skumanich, High Altitude ObservatoryRadiative Diagnostics of Stellar Activity Part I:The Low-M 2.1 meter 4.00 44.50 0.00 0.00
Executed Proposals 10/01/85 - 12/31/85 Page 1 Wed Jar. 29 15:02:54 1986
Nights Hours Days Hours1023 485
R Altrock, Sacramento Peak ObservatoryS/B003-Coronal Observations
Big Dome/SP 0.00 0.00 144.00 174.00
1152 485
R Altrock, Sacramento Peak ObservatoryD Sime, R Fisher, High Altitude ObservatoryS/B172-Vertical Structure of Coronal Features
Big Dome/SP 0.00 0.00 7.00 34.00
1029 485
R Altrock, Sacramento Peak ObservatoryS/B136-Coronal Transient Patrol
Big Dome/SP 0.00 0.00 15.00 60.00
5569 485
B Bopp, P Noah, University of ToledoJ Riggs.T/Synoptic Line Profile Variability in the ActiveChromo... McMath Main 8.00
1087 485
P Brandt, Klepenheuer Institut fur SonnenphysikR Smartt, National Solar Observatory/Sac PeakS/T223-Ro Measurements at Sac Peak VTT
Vacuum Tower/SP 0.00
43.00 0.00 0.00
0.00 £.00 25.00
1044 485
L Brown, R Toth, Jet Propulsion LaboratoryT/Laboratory Spectroscopy in Support ofAtmospheric Remote. McMath FTS Lab 3.00 28.00 3.00 33.00
1032 485
T Brown, High Altitude ObservatoryC Morrow, University of Colorado, APASS/B158-Global Solar P-mode Oscillations
Big Dome/SP 0.00
1153 485
M Bruner, W Brown,Lockheed Palo Alto Research Lab.L Dame", L.A.S.P.S/B178-Small Scale Structure/Weak MagneticFields, Call/UV Big Dome/SP 0.00
0.00 8.00 40.00
0.00 2.00 4.00
c
23>HM
D Oc a
1-1 1-1>r1
m o coDUOa. m r1n> ^ >
• • pa0>
i— "aho O CO
O
LO rr 3>HO
>-a
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Executed Proposals 10/01/85 - 12/31/85 Page 3 Wed Jan 29 15:02:54 1986
Ni8nts Hours Days HourslUoU too
T Fleming, J Liebert, University of ArizonaI Gioia, Center for AstrophysicsT/High Resolution Spectroscopy of Bright, X-rayActive Star McMath Main 3.00 3,00 0.00 0.00
1051 485
P Forsberg, S Johansson, University of LundT/The Spectrum of Ti I, the Spectrum of Cr II
McMath FTS Lab 2.00 11.00 2.00 19.00
5572 485P Foukal,Cambridge Research & Instrumentation, Inc.W Rosen, Naval Air Development CenterL Petro,Atmospheric A Environmental Research, Inc.A Pierce, National Solar Observatory/TucsonT/Variations in Solar Limb Darkening and TotalLuminosity McMath Main 0.00 0.00 5.00 18.00
1052 485
M Giampapa, National Solar Observatory/TucsonJ Riggs,T/Synoptic Rotational Modulation of the He I D3Line in.... McMath Main 6.00 24.50 0.00 0.00
5273 485
M Giampapa, National Solar Observatory/TucsonS Worden, 0SUDRE/ADEWL Golub, Center for AstrophysicsA Title, Lockheed Palo Alto Research Lab.T/Simultaneous Ca II Resonance Line & Infrared Hand K McMath Main 0.00 0.00 4.00 0.00
1039 485
L Gilliam, National Solar Observatory/Sac PeakS/H008-White Light Sunspot Drawing
Hilltop Dome/SP 0.00 0.00 92.00 86.00
Executed Proposals 10/01/85 - 12/31/85 Page 5 Wed Jan 29 15:02:54 1986
Nights Pours Days Hours1054 485 JJ Gurman, Applied Research CorporationJ Leibacher, National Solar Observatory/TucsonJ Riggs,T/A Search for Chromospheric p-Modes in G Giants
McMath Main 4.00 10.75 0.00 0.00
3790 485
J Harvey, National Solar Observatory/TucsonT/Vacuum Telescope Synoptic Program DailyMagnetograms Solar Vacuum 0.00 0.00 88.00 337.00
1067 485
F Hill, National Solar Observatory/TucsonL November, Sacramento Peak ObservatoryD Haber, J Toomre, University of Colorado, JILAS/T209-Acoustic Waves/Global Oscillations
Vacuum Tower/SP 0.00 0.00 14.00 75.00
1158 485
F Hill, National Solar Observatory/TucsonL November, Sacramento Peak ObservatoryS/T247-Solar Oscillations Using 2 MDA Arrays
Vacuum Tower/SP 0.00 0.00 3.00 3.00
1171 ' 485S Keil, Sacramento Peak ObservatoryC Marmolino, Institute of Experimental PhysicsS/T195-Granular Profiles #1
Vacuum Tower/SP 0.00 0.00 1.00 4.00
1074 485
S Keil, Sacramento Peak ObservatoryS/T226-Solar Atmospheric Dynamics
Vacuum Tower/SP 0.00 0.00 11.00 62.00
1028 485
J Kuhn, Princeton UniversityL Gilliam, National Solar Observatory/Sac PeakS/B134-Five Minute OscillationAnisotropy/Aplitude Studies Big Dome/SP 0.00 0.00 10.00 34.00
Executed Proposals 10/01/85 - 12/31/85 Page 7 Wed Jan 29 15:02:54 1986
Nights Hours Days Hours5581 485 JM Mumma, D Deming, F Espenak, T Kostiuk,U Kauf1, J Goldstein,NASA Goddard Space Flight CenterJ Hillman,National Aeronautics ft Space AdministrationD Glenar, Colgate UniversityT/Astronomical ft Stratospheric InfraredHeterodyne Spectro. McMath Main 3.00 7,00 6.00 18.00
5879 485
A Pierce, National Solar Observatory/TucsonJ LoPresto, Edinboro State CollegeT/Solar Rotation from Several Fraunhofer Lines ftthe Einste McMath Main 0.00 0.00 17.00 57.00
1064 485
A Potter, NASA Johnson Space Flight CenterT Morgan, Southwestern UniversityT/Observation of Sodium Vapor excaping fromMercury McMath Main 0.00 0.00 4.00 21.00
1156 485
D Rabin, National Solar Observatory/TucsonL November, Sacramento Peak ObservatoryS/T244-Relationship/Small-Med Scale Magnetic FluxEvolution Vacuum Tower/SP 0.00 0.00 9.00 50.00
5582 485
L Ramsey, D Huenemoerder,Pennsylvania State University
T/Synoptic Observations of Long Period RS CVnSystems McMath Main 2.00 5.25 0.00 0.00
1006 485
F Roesler, F Scherb, J Harlender, K Magee,R Reynolds, University of WisconsinT/Observations of Comet Halley, CometGiacobini-Zinner McMath West 31.00 237.00 0.00 0 00
Executed Proposals 10/01/85 - 12/31/85 Page 9 Wed Jan 29 15:02:54 1986
Nights Hours Days Hours1037 485
R Smartt, National Solar Observatory/Sac PeakS/H004-Coronal One Shot (monitor only)
Hilltop Dome/SP 0.00 0.00 11.00 108.00
1008 485M Smith, M Giampapa,National Solar Observatory/TucsonJ Riggs,T/Synoptic Detection of the Coronal Green Line inLate... McMath Main 5.50 10.00 0.00 0.00
1058 485
M Smith, National Solar Observatory/TucsonG Penrod, Lick ObservatoryR Polidan, Center for Space SciencesT/Nonradial Oscillations and Be Activity inLambda Eridani McMath Main 9.00 30.00 0.00 0.00
1060 485
J Sowell, R Sears, University of MichiganJ Riggs,T/High-Resolution H-alpha Scans of PossiblePre-Planetary.. McMath Main 2.00 10.50 0,00 0.00
1021 485
G Spear, B Nottingham, Sonoma State UniversityJ Riggs,T/Correlation of the 01 Triplet (7774A) andH-alpha in Be.. McMath Main 7.00 45.50 0.00 0.00
4337 485
G Stokes, Battelle Northwest LaboratoriesJ Brault, B Graves,National Solar Observatory/TucsonT/Telluric Absorption Spectroscopy
McMath Main 0.00 0.00 5.00 20.00
5587 485S Vogt, G Penrod, Lick ObservatoryJ Riggs,T/Synoptic Doppler Imaging Spotted RS CVn Stars
McMath Main 8.00 37.00 0.00 0.00
TELESCOPE USAGE
Appendix B
Astronomical Observations
Scheduled
Maintenance,
Hours
Scheduled Hours Us ed Hours Lost
Engineering,
Instrument
Tests,
Telescope Visitors Staff Weather
Equipment
Failure
EquipmentChanges, etc.
4m 830.9 404.4 267.8 106.2 25.6 26.9
1.5m 823.3 414.2 104.2 178.5 22.0 104.4
lm 794.4 402.6 119.5 196.7 28.1 47.5
CTIO 0.9m 720.8 263.5 203.0 157.4 44.6 52.3
0.6/0.9m* 340.6 235.4 6.7 98.5 0.0 0.0
0.6m 318.2 92.0 33.0 193.2 0.0 0.0
0.4m
4m 1152.20 530.87 124.13 336.25 86.20 74.75
2.1m 1024.50 466.77 132.98 342.50 63.25 19.00
CF 708.60 249.00 141.50 232.70 48.90 36.50
1. 3m 946.25 235.26 196.99 451.00 34.00 29.00
KPNO //l-0.9m 942.50 349.17 149.08 383.00 35.50 25.75
//2-0.9m 999.50 424.36 7.64 479.00 32.00 56.50
//3-0.4m 101.50 47.50 — 41.50 6.00 6.50
Schmidt 183.50 58.25 — 109.25 12.50 3.50
Hilltop 1952.0 1776.0 0.0 176.0 0.0 0.0
Tower 798.0 299.5 346.5 120.0 24.0 8.0
Big Dome 1596.0 636.5 266.5 644.0 49.0 0.0
NSO **FTS Lab 276.0 257.0 0.0 0.0 19.0 0.0
**McMath 1831.5 753.4 152.6 703.5 140.0 82.0
Vacuum 734.0 337.0 0.0 352.0 22.0 23.0
