National Optical Astronomy Observatories

National Optical Astronomy Observatories

Quarterly Report

October - December 1987

TABLE OF CONTENTS

I. INTRODUCTION 1

II. SCIENTIFIC HIGHLIGHTS 2

A. Observations at CTIO 2 B. M31: New Insight into the Nearest Spiral Galaxy 3 C. South Pole Observing Run 3 D. Magnetic Fields Near HH Objects: Clues to the Collimation of Outflows 4 E. IR Imaging of L1551-IRS5: Inside Collimated Outflows 4 F. Rings and Trumpets: Three Dimensional 1^ -k -co Diagrams 4 G. Light Pollution Report y 5

III. PERSONNEL 6

A. Visiting Scientists 6 B. New Appointees 6 C. Terminations 6 D. Change of Status 7

IV. INSTRUMENTATION AND NEW PROJECTS 8

A. Advanced Development Program 8 B. Instrumentation Projects 9

V. TELESCOPE OPERATIONS 14

A. Kitt Peak National Observatory . 14 B. Cerro Tololo Inter-American Observatory 14 C. National Solar Observatory 15

VI. PROGRAM SUPPORT 17

A. Director's Office 17 B. Publications and Information Resources 17 C. Central Computer Services 17 D. Central Administrative Services 18 E. Central Facilities Operations 18

Appendices

A. Telescope Usage Statistics B. Observational Programs C. NOAO Annual Safety Report

I. INTRODUCTION

In the first quarter of FY 1988, AURA and NOAO submitted a proposal for AURA management and operation of the National Optical Astronomy Observatories, to the National Science Foundation. The proposal was widely distributed. The Director of the National Solar Observatory/Associate Director, NOAO resigned and Dr. Sidney Wolff formed a search committee. The Manager of NOAO's Public Information Office also resigned during this quarter. The AURA Observatories Visiting Committee presented its final report to the Director, NOAO and to AURA from its September visit to Sacramento Peak.

H. SCIENTIFIC HIGHLIGHTS

A. Observations at CTIO.

The advent of the infrared imager at CTIO afforded a unique new opportunity to do high-resolution mapping in the infrared. The imager provides seeing-limited observations on the 4-m, with a resolution of better than 1 arcsec. J. Elias (CTIO) has observed a set of the more prominent Magellanic Cloud star formation regions with the Imager and the 4-m and 1.5-m telescopes in order to study their structure in the infrared. A sample of luminous, compact objects have been selected using a combination of available ground-based data (still relatively sparse) and the complete far-infrared data provided by IRAS. Individual regions of star formation have been observed at all wavelengths, including far-infrared observations by the Infrared Astronomical Satellite (IRAS). Most have visible counterparts or radio counterparts. To date, though, any attempt at studying the structure of these regions has been limited in the infrared by relatively low resolution of conventional photometric maps-typically no better than 5 arcsec. Resolutions of this order correspond to linear distances in the Clouds of over a parsec, yet most of the interesting structure in regions of active star formation is likely to be on scales a few times smaller, judging from observations of galactic sources.

The quasar IRAS 00275=2859, redshift 0.28, was discovered in October 1987 during a redshift survey with the CTIO l-m/2D-Frutti instrument by P. Vader (Yale). It is the second quasar discovered from the IRAS data base. Its far-infrared colors are typical of previously known active nuclei, with a luminosity at 60 microns of 10**12 solar luminosities. It belongs to the high energy tail of the most luminous quasars at 60 microns. It is radio-quiet and has an optical spectrum characterized by very strong Fe II emission. UBV imaging with the 0.9-m/CCD system resulted in the detection of a host galaxy system which consists of three distinct parts: the central QSO source, a second fainter point source, and an extended low surface brightness region.

Spectroscopy of the QSO has been obtained with the 4-m/Air Schmidt camera/CCD, and will be used to investigate the spectral type of the stellar population and estimate the strength of the burst of star formation. Deep 4-m PFCCD B and V images of the QSO system have been obtained in order to better study the morphology of the interaction as revealed by the low surface brightness features. This research will contribute to our understanding of the importance of galaxy interactions and merging for the quasar phenomenon and the fact that QSO host galaxies are significantly more luminous than the general population of galaxies.

December 1987 saw the first use of the new 1.5-m fiber fed echelle system, with the detector actually located in the 1.5-m coude room instead of the 4-m. The much shorter fiber run should improve throughput significantly. P. Gamavich (U. of Washington) began a program to measure radial velocities of wide binary candidates at the south galactic pole.

Because collisions of stars and clouds can be modelled, wide binaries are excellent tools for probing the characteristics of dark matter in the galaxy. For example, Bahcall (Princeton) et al. derived an upper limit of 2M© on the mass of objects that constitute the dark matter. This estimate was based on the largest separation seen in a sample of only eight wide binaries. The same sample was used by Hut and Tremaine to estimate the lifetime of the Oort cloud of comets, and to test the existence of the hypothetical Solar companion, Nemesis. Because of the large separation between components of a wide binary, it is difficult to distinguish them from chance alignments of unrelated stars; thus, there exists a bias against these objects in the binary star catalogs. Latham (CFA) et al. showed that the radial velocities of the candidate pairs can be used to differentiate between a chance alignment of two stars and a true binary. Latham found eight bound pairs and, at present, these constitute the only scientifically selected sample of wide binaries in existence. Using the fiber-fed echelle, T. Lutz (Washington State U.) and T. Ingerson (CTIO) achieved accuracy of the radial velocity measurements near one km/s.

B. M31: New Insight into the Nearest Spiral Galaxy.

The spiral galaxy M31 is the nearest large galaxy, and for some time it has been thought to be similar to our own and to be quiescent in nature. These ideas may have to be modified, for not only are differences in the stellar populations between the two galaxies becoming apparent, there is in addition growing evidence that the center of M31 may share some of the characteristics of active galactic nuclei. An important new contribution to this investigation is a recent study of deep images and spectroscopy of the ionized gas in the central region of M31. R. Ciardullo (KPNO), V. Rubin (Carnegie Inst.), G. Jacoby (KPNO), H. Ford (STScI), and W. Ford (Carnegie Inst.) have combined 334 CCD frames taken with the KPNO #1 0.9-m telescope to produce detailed images of the ionized gas in the central bulge of M31. These data are supplemented by spectroscopy of the region obtained with the KPNO 4-m and Palomar 5-m telescopes. The narrow band images reveal a spiral-like filamentary structure in the ionized gas which appears more face on than the large stellar disk of the galaxy. Filaments of emission lines extend to 500 pc from the center, and spectroscopy of the forbidden sulfur lines shows the gas density to decrease by a factor of 100 in the central arcmin of the galaxy. These data, together with the observed gas kinematics and the lack of a significant amount of interstellar gas in the bulge region, all argue for the presence of a galactic wind in M31. The presence of such a wind, similar to that found in more active galaxies, could indicate a different evolutionary history for the center of M31 than for the rest of the galaxy. Such a conclusion is also supported by the indication of a more face-on orientation for the ionized gas in the center of the galaxy. C. South Pole Observing Run.

In 1981, a joint project between NSO, Bartol Research Foundation and NASA led to an expedition to the South Pole to observe solar oscillations. The advantages of such an exotic observing site are no night time (during the summer), only a slowly changing solar elevation and excellent sky conditions. The disadvantages are great distance, high altitude and low temperatures. Our 1981 observations were successful and comparison of our measured frequencies of solar oscillations with similar, later measurements made elsewhere showed some small discrepancies that we were unable to assign to observational sources. Equipment was set up and data taking started on November 13. During the next two and one-half weeks about 290 hours of observations for an overall duty cycle of about 2/3 were recorded. The longest single run was more than 70 hours. Some instrumental problems were encountered, the main one being scattered light produced within the instrument but this should be adequately correctable during data reduction. Transcription of the data tapes has started and some results should be available next quarter. D. Magnetic Fields Near H H Objects: Clues to the Collimation of Outflows. Herbig Haro objects and their associated optical jets of shock excited gas are indicators of collimated, high speed outflow from young stellar objects. Recent studies of these objects show that the outflows tend to be aligned with neighboring flows nearby, and that they are often aligned with the large scale magnetic field in the surrounding interstellar medium. The nature of the collimation mechanism is not well understood, and a natural suggestion that arises from this observed alignment is that the large scale field geometry plays some role in the collimation mechanism. However, observations and theoretical models both suggest that collimation of the outflow occurs quite near to the star (within 1000 AU), yet previous studies provided magnetic field orientation only on scales larger than about one parsec. Until field geometry is determined on a finer scale, little can be said about the role of magnetic fields in the collimation process. An important step in this direction has been made by M. Heyer (Carnegie Inst.), S. Strom (U. Mass) and K. Strom (U. Mass). Using the KPNO #1 0.9-m telescope, they have obtained CCD imaging polarimetry of embedded or background stars to study the magnetic fields Herbig-Haro objects HH7-11, HH12, and HH33/40. These observations allow the determination of the magnetic field geometry on a smaller scale than before, and the results of this work show that the local magnetic field is indeed aligned with the outflow in some, but not all, cases. For HH7-11 and HH33/40 the field is parallel to the outflow, but in HH12 the two are misaligned by about 60 degrees. While this tantalizing result does not resolve the question of the field being responsible for the collimation, it shows that in some cases there is a correlation between the small scale field geometry and the local collimation processes. E. IR Imaging of L1551-IRS5: Inside Collimated Outflows. Collimated or bipolar outflows are a common phenomenon around young stellar objects, and in addition to the role of magnetic fields discussed above, there is a need to discover the gas dynamics in the immediate circumstellar envelope in order to understand the outflow process itself. Insight into the nature of this envelope has been provided by using the KPNO 1.3-m telescope to provide infrared images of the source IRS 5 in L1551. The observations were obtained by A. Moneti, W. Forrest, J. Pipher (all at U. of Rochester), and C. Woodward(U. of Wyoming). These investigators find the object elongated, with axes of 4.1 and 2.8 arcsec. The results are consistent with a flattened circumstellar envelope 1000 AU in diameter and viewed from about 20 degrees above its equatorial plane.

F. Ringsand Trumpets: Three-Dimensional kx -k -co Diagrams. F. Hill (NSO) has developed a new way to use the solar oscillations as probes of the solar convection zone. The method uses three-dimensional Fourier power spectra of solar Doppler data, rather than two-dimensional spectra. In the new analysis, the familiar ridges appears as tilted trumpets in the three-dimensional space of co, the temporal frequency, k and k and the x- and y- components of the horizontal wave number vector. When sliced at a constant co, the trumpets appear as rings that are offset and distorted in shape. The position and shape of each ring provides information on both components of the horizontal flow field over a specific range of depths in the convection zone. Hill has derived the relationship between the ring parameters and the flow field. The information from many rings obtained from different regions on the Sun can be combined using inverse techniques to obtain a map of the horizontal velocity as a function of depth and longitude in the convection zone. Error analysis suggests that the technique has an accuracy of 25 m/s for a single ring. A preliminary analysis of 189 rings obtained at a single longitude shows the presence of a meridional flow of some 100 m/s from the equator towards the South Pole. This is a rather high value, and there may be systematic errors in the data (such as a drift of the telescope) that can account for at least part of this effect. Future plans for this project are to measure the ring parameters for the remaining 5000 rings, and to derive the convection zone flow map, to derive great circle techniques to describe the oscillations, and to use the rings to provide information on the thermodynamics of the convection zone.

G. Light Pollution Report.

The International Dark-sky Association is now formed, incorporated as a non-profit corporation in Arizona. D. Crawford (KPNO) and planners of Star Valley Development are working together to set minimum standards for outdoor lighting. The City of Tucson/Pima County governments approved recommended changes to the outdoor lighting laws. A major change prohibits sale of any lighting fixture that does not meet the specifications of the lighting codes. Hughes Aircraft Company agreed to retrofit all outdoor lighting at their Tucson facility to LPS. The project is expected to be completed by the end of the first quarter of 1988. In the total project, about 1,200 fixtures will be replaced. The estimated total fixture cost is about $375,000. In order to maximize benefits from recent code changes, we organized a mailing to the following: lighting equipment manufacturers (nationally), Association of Architects in S. Arizona, Association of Consulting Engineers statewide, electrical contractors in S. Arizona, illuminating engineers in S. Arizona, dealers and distributors locally, amateur astronomers locally, S. Arizona homebuilders, billboard companies locally, and so forth. The mailing consisted of approximately 1,500 packets. Each contained among other things a copy of the current lighting code. We received $1,000 each from Steward and SAO to assist in this effort. At our urging and with our support, the U. of Arizona has organized an effort to increase awareness of the public to the problem of light pollution, code changes, etc. The effort will include TV and newspaper coverage. The first media release was done in late December, and resulted in good media coverage (press, radio, and TV). In connection with our educational effort, we have asked city/county officials, the Electric League, and Pima College to formulate coursework and seminars to train city/county staff and local industry people concerning code requirements and basic fixture and lighting design. D. Crawford's year as President of the local IES is over. The new president is very supportive to the cause. Crawford presented the case for dark skies and a clean space environment to the Dept. of Transportation in Washington, along with S. van den Bergh, on behalf of the AAS and the IAU. A great deal of time was spent organizing IAU Colloquium 112, of which Crawford is the Chairman. m. PERSONNEL

A. Visiting Scientists.

The following visitors arrived at NOAO facilities for periods of one month or more during the quarter October 1 - December 31, 1987.

date NOAO facilitv arrived name institution visited

10/01/87 Guiseppe Cutispoto Osservatorio Astrofisico NSO di Catania, Italy 10/01/87 Karel Schrijver JILA/U. of Colorado NSO 10/01/87 Serge Koutchmy Centre Nat. de la Recherche NSO Scientifique, France 10/11/87 Helen Dara Astronomical Institute NSO Nat. Observatory, Athens 10/26/87 Goetz Stellmacher Institut d'Astrophysique, NSO CNRS, France 11/03/87 Matthias Steffen Institut fur Theoretische NSO Physik un Sternwarte, FRG 11/16/87 Thomas Rimelle Kiepenheuer Institut fur NSO Sonnenphysik, FRG 12/01/87 Christopher Corbally Vatican Research Group NOAO Steward Observ., Tucson

B. New Appointees.

The table below shows details of new appointments made to NOAO during the quarter October 1 - December 31, 1987.

date of NOAO appointment name position division

10/01/87 Deborah Haber Research Associate NSO 11/01/87 Oskar von der Liihe Associate Scientist NSO 12/09/87 Andrew McWilliam Research Associate CTIO

C. Terminations. NOAO date name position division

11/17/87 Guiseppe Guarini Head Santiago Office, CTIO CTIO 12/04/87 Elaine Sadler Research Associate KPNO 12/28/87 Carl Posey Public Information Officer NOAO D. Change of Status. NOAO date name position division

10/01/87 Sidney Wolff Acting Dir. to Director, NOAO NOAO 11/01/87 George Jacoby Assist. Astron. to KPNO Associate Astronomer 11/01/87 Douglas Rabin Assist. Astron. to NSO Associate Astronomer 11/01/87 Alistair Walker Assist. Astron. to CTIO Associate Astronomer 12/01/87 William Weller Assist. Sup. Sci. to CTIO Associate Support Scientist 12/16/87 Scott Bulau Engineer to Senior Engineer KPNO IV. INSTRUMENTATION AND NEW PROJECTS

A. Advanced Development Program.

1. Planning for 8-m NOAO Telescopes.

Many members of the NOAO staff have contributed to a detailed draft of the research projects that could be done with 8-m telescopes in the Northern and Southern Hemispheres; ADP and engineering staff members have been working in collaboration with the Magellan Project staff to consider concepts for the optical support structure and the alt-az mount; and several small working groups (comprising experts both inside and outside NOAO) are discussing the plans for a first complement of instruments.

2. Modelling and Testing Mirrors at NOAO.

The New Telescope Technology program at NOAO is currently concentrating on ways to make large primary mirrors perform at their very best. A finite-element analysis technique being developed at NOAO is making it possible to model 8-m honeycomb mirrors on in-house computers, with very reasonable run times. Work continues on modifications to the 4-m polishing machine at NOAO, in preparation for testing driven-lap polishing. The new lap and control system are under construction. A thousand-sensor thermal monitoring system, which will make use of integrated-circuit sensors, will keep track of internal mirror temperatures during the polishing.

3. University of Arizona Mirror Lab.

The first test casting in the new large furnace was made on November 10. After three weeks of annealing and cooling, a 48-inch honeycomb blank was removed from the furnace on December 7. Both core geometry and bubble content are better than for any of the previous castings.

A new type of borosilicate glass, Coming's 7761, was tested for the first time. Surface roughness of the developmental glass production resulted in some thin veils (very fine bubbles) which allow the outlines of the initial glass blocks to be seen in the faceplate. Previous tests show that this has no effect on polishing. No evidence of phase separation or interaction with the mold material is seen. Inhomogeneities in the glass resulted in stress of up to 40 nm/cm through the casting. It is not expected that these local stress levels will affect mirror quality, but Corning plans to eliminate them in future production by improving the manufacturing process. The uniform stress from annealing is very low.

The casting provided a full checkout of the new hardware and software for temperature control. The control algorithms proved to be very accurate and robust against individual component failure. At the annealing temperature (500°C), temporal and spatial variations were within the range ±1°C. In all, the furnace operation and blank are considered very successful.

4. Adaptive Optics.

The adaptive optics system has been installed at the McMath telescope and is now being tested by L. Goad. Initial attempts to record and analyze real-time atmospheric wavefronts were hampered by excessive readout noise in the 100 X 100

8 Reticon array and the lack of control of the system cycle time (600 Hz). We have therefore reworked the system to incorporate an external trigger to control cycle (and Reticon integration) times. Now the system speed is continuously variable up to ~450 Hz, under external control. A modification of the clocking sequence for the Reticon has reduced system noise. The alignment of the system to the McMath Main telescope has been completed, and the alignment to the East Auxiliary telescope is in progress.

5. Two-Dimensional Infrared Speckle Interferometry.

J. Beckers and J. Christou (ADP), R. Probst and S. Ridgway (KPNO) had a highly successful Test and Evaluation run on the KPNO 4-m telescope in November, with the SBRC imaging array operating in a speckle mode. This run demonstrated the capability to record high-quality IR specklegrams routinely. The NOAO camera is apparently the only operational 2-D IR speckle camera anywhere. All the observations were made at 2.2 \xm, and approximately 10-20% of the observations were dominated by a single speckle. The seeing was estimated to be slightly poorer than 1 arcsec, and the field of view of the camera was ~3.3 arcsec. Preliminary results were presented at the Austin AAS meeting in January.

6. Seeing at Mauna Kea.

F. and C. Roddier (ADP) organized a two-week campaign of measurements in November at Mauna Kea, to better understand the seeing conditions and the origin of image degradation at the summit. This was done in cooperation with the University of Hawaii and the University of Nice (France). The techniques were similar to those used at La Silla during an analogous campaign organized by ESO in February 1986.

B. Instrumentation Projects.

The Global Oscillation Network Group (GONG), a community-based project to conduct a detailed study of solar internal structure and dynamics using helioseismology, is developing a six-station network of extremely sensitive, and stable solar velocity imagers located around the Earth to obtain nearly continuous observations of the Sun's "five-minute" oscillations, or pulsations. GONG is also establishing a major, distributed data reduction and analysis system to facilitate the coordinated scientific investigation of these measurements.

Substantial progress and several technical difficulties marked the last few months of work on the GONG breadboard and prototype projects. The breadboard system is intended to validate concepts while the prototype system is intended to demonstrate performance before making final hardware purchases. Both projects are proceeding in parallel with the emphasis in the breadboard project on the least certain instrumental aspects and in the prototype project on the most certain aspects. The heliostat for GONG on the roof of the Tucson laboratory started driving erratically in December. Examination of the instrument revealed that dirt from reroofing operations was the source of the trouble. This problem interrupted tests of the high-speed, tiltable, metal mirror that is intended to reduce noise caused by rapid image motion due to poor seeing. It also stopped other testing. The problem was fixed and full scale testing has again resumed. Additions to the foreoptics are underway. Two lenses have been fabricated to interchange pupil and solar images in the optical system after the first focus. Tests of this calibration system show that it works as planned. An entrance window/filter has been ordered but not yet delivered.

The image cache, designed by S. Colley (NOAO) and built by the GONG team at Sacramento Peak, has been integrated with the GONG lab workstation in Tucson and, after some debugging, has been serving its function of acquiring images for further analysis.

We are starting to evaluate potential vendors for construction of long lead time optical elements for the GONG prototype instrument. These include the calcite crystals for the birefringent filter, polarizing beamsplitter cubes and various half and quarter-wave plates.

Considerable support was given last quarter for the KPCA with its visitor run on the KPNO 4-m. Performance was hampered by some component failures and an air conditioner break-down in the dome computer room. System stability and throughput were restored after the run. Routine dewar and controller repairs were also made. Progress has continued on the implementation of a CCD system at the Burrell Schmidt Telescope.

The successful implementation of TI-5 for telescope use at the KPNO 2.1-m required the use of the camera electronics box from the laboratory dewar. Two Texas Instruments CCDs were received from JPL in the NSF distribution. One was characterized as being cosmetically excellent with superior charge transfer efficiency. It was desperately needed by Cerro Tololo to relieve the pressure on the one other TI chip, so it was shipped to them, in accordance with the original proposal to NSF. The second chip is also very good according to the lab tests, but with a region of bad columns in the middle of the format. Its disposition will await decision on future instrumentation projects. A new chip mount was constructed for Tektronix 512 square CCDs; testing will begin on clock voltages and gate inversions to test for pixel to pixel variations and dark noise reduction.

The KPNO Infrared Imager, with addition of warm foreoptics and shutter provided by J. Beckers (ADP), was successfully used for two dimensional speckle imaging at the 4-m. To our knowledge this is the only working 2-D system in the world; it is fully competitive with instruments proposed or under construction elsewhere. Optics for use at f/8 were successfully tested at the 4-m and 2.1-m. The user software package has been extensively exercised and debugged. Our major filter procurement is nearing completion. Improved cryogen transfer tubes have been received and tested, allowing cryogen fills to be turned over to mountain technical staff as a standard operation. We have evaluated and rejected one further array offered by the vendor; two arrays remain outstanding for contract fulfillment.

The array spectrometer was assembled and the telescope tested in two separate telescope runs. These verified installation and operational procedures, optics performance, spectral resolution and sensitivity. Some filters and a refigured mirror have yet to be installed, and there are some problems with implementation of driver motors for grating tilt and filter selection. These are relatively minor, and we are in good shape for scheduled telescope runs in spring 1988.

CCD controllers is a new project spearheaded by CTIO. Conceptual design has begun for a new generation CCD controller. Current thinking is that it will

10 interface to a Sun workstation, serving as a memory buffer for data and instruction generator for read-out formats and clock-level functions. Collaboration with the IR instrumentation group is underway to investigate the feasibility of transputer architecture for both CCD and Infrared arrays, with the hope of establishing a standard interface for a majority of mountain instruments. Face to face meetings between CTIO and KPNO science and engineering staff members will be held in March.

Several attempts were made to get precise measurements of doppler shifts of the 530.3mm coronal line over enhanced regions of the inner corona in order to search for coronal waves. In collaboration with J. Zirker and R. Smartt (NSO), S. Koutchmy (NRC) tried the use of new CCD cameras. Tests showed the detector is not sensitive enough. They designed a new system which includes a low light level image tube (brought from Koutchmy's home institution in Paris) and a better adapted transfer optics. New tests performed in September-October during moments of good coronal sky have shown the system very promising but not yet operational.

S. Keil (AFGL) made a run using an agile mirror in front of the echelle spectrograph at the Sac Peak Vacuum Tower Telescope. During this run he measured the offset signals being sent to the active mirror in addition to recording the solar spectrum. The goal of the observation is to measure the solar acoustic flux at high frequencies that can propagate through the solar photosphere and perhaps serve as a source of energy for heating at higher layers. The previous run using an agile mirror indicated that this flux was about 2x108 ergs/cm /sec which is a factor of 100 times that needed to heat the chromosphere and about 10 higher than previously measured by other authors. It is extremely important to establish the validity of the measurement. One possible source of systematic error would be spurious oscillations of the mirror. Thus, the mirror was locked onto a sunspot and the mirror offset signals were monitored for a period of about 20 minutes at a .05 sec rate. The power spectra of the mirror driving signals agree very well with what one would expect for seeing in the Earth's atmosphere. The mirror did not appear to add any spurious power to the data. Keil and associates are now in the process of reducing the solar data. A fiber spectrograph and positioners are a new start on a multi-year project to replace the custom plug boards for multiple object spectroscopy at the KPNO 4-m with a mechanical actuator system. The decision was made to go to the R-C focus in order to use larger diameter optical fibers and for mechanical stability and access to the equipment. Since several other observatories are embarked on similar projects, this quarter involved a survey of their techniques and obtaining quotations from manufacturers for components.

The bench spectrograph project is also a new start on a multi-year venture. The goal is to have a stable, thermally controlled spectrograph that is easily reconfigured for different applications. It can be used in both high and low dispersion modes while having a longer slit than the current echelle spectrograph, and feeding a detector with larger resolution elements (approximately 50 \i). Performance specifications were defined this quarter, commercially available optical benches were identified, and the exact location in the KPNO 4-m dome is now under study, which will determine the shape and sizeof the bench and layout. TV Acquisition Cameras is a study program with the goal of replacing the existing and inadequate ISIT plus leaky memory acquisition cameras. Various combinations of commercial CCDs plus intensifiers will be tried on the KPNO 0.9-m for initial

11 characterization. One vendor will bring an intensified package in January to the telescope; uncooled devices without intensification were found to be inadequate. PC hardware with a frame grabber is being studied for improvement over the current undersampling with the leaky memory.

The Cryogenic Echelle project is still hindered by lack of a mechanical engineer, although recruitment efforts are continuing. The optical design has been checked in detail and no problems found. Extensive conversations with industry experts in diamond turning have been very helpful, and specifications have been sent to five potential vendors for bids. Grating blanks were ordered, and a closed cycle cooler received for testing. A concept design is underway for a second generation array imager, tentatively called the Cryogenic Optical Bench. This instrument will incorporate numerous spatial and spectral filters in a convenient, modular design. There are a number of possibilities for the detector. An array with significantly larger format than the current 58x62 is a reasonable probability. The optical design allows for a focal plane substantially larger than that of the present imager. Numerous projects are underway in the R&D laboratory. An extrinsic silicon array on loan from Hughes was successfully telescope tested. Senior engineer, A. Fowler (NOAO), travelled to Hughes and Rockwell to finalize contractual arrangements for loan and test of ten micron BIB arrays and to keep abreast of their internal array work. The laboratory test dewar is being reconfigured for vibrational tests using a closed cycle cooler in place of liquid cryogens. Engineer J. Little (NOAO) began definition of a high-speed fiber optics link from telescope mounted instruments to remote controllers and computers. The high-speed capability is essential for long-wavelength operation; the link would also allow removal of heat sources from the telescope environment. The first link is to be installed in the KPNO 2.1-m cable wrapup when it is rewired in summer 1988.

The GONG staff held its semi-annual technical meeting in Tucson on November 4 and 5. The systems document was discussed in great detail and responsibility for the continued development of the various systems was reviewed and assigned to specific working groups. The priority, scope, and extent of the development work for each of the systems during FY '88 was explored, with work schedules produced and coordinated. Teams involved in several of the major systems grouping held a number of topical meetings to discuss and resolve design and implementation issues.

Although GONG still has no budget figure some four months into the fiscal year, with the spector of Gramm-Rudman clouding the FY '88 budget prospects, considerable effort has been expended looking at alternative short- and long-range plans, based on different funding scenarios.

We now have a full year of six site network data, from November 10 1986, to November 12, 1987. A preliminary analysis of the canonical anonymous network shows that a duty cycle of about 90% was achieved over the full year. An instrument at Urumqi, Xinjiang in Western China, will provide alternative coverage during the Boreal summer months. This site should avoid the summer monsoons.

Progress has been made on the analysis of the site survey database. R. Kupke, a student from the University of Arizona, has been extremely helpful in developing programs and taking care of the regular chores in maintaining the data. She is about to run the entire database through an improved atmospheric correcting

12 program developed by H. Jones (NSO). J. Leibacher (NSO) is hard at work modifying the analysis program to separate the instrumental downtime from the weather, and thus provide the best possible measurement of the fraction of clear time at each site.

13 V. TELESCOPE OPERATIONS

A. Kitt Peak National Observatory.

A final design was agreed to for the NASA/MIT Explosive Transient Camera/Rapidly Moving Telescope (ETC/RMT) facility on Kitt Peak. This project is a scaled down effort, from the previous plan, and construction is expected to start this spring.

On November 30, a joint effort between the Kitt Peak Operations and Engineering groups culminated in the completion of the OSHA-required-and-approved modifications to the 4-m building and dome. The purpose of these changes was to enhance the level of safety for anyone having to access the catwalk.

Installation of the hardware for an Ethernet communications system between the 2.1-m, 4-m and 1.3-m was completed. A fiber optics cable, holding 12 fibers, was chosen for the connection between domes. Two of the fibers are now in use with an Ethernet link between the 2.1-m and 4-m Sun workstations, a PC in the programmer's office in the 2.1-m building, and a PC in the Administration Building.

The telescope control system (TCS) initiative work, a collaborative effort with CTIO, continues. The basic hardware and software for the downtown VME computer system are installed and working at a modest level. The software development system on the PC-AT is not satisfactory; we are looking for better software. Astrometry software written by P. Wallace (STARLINK, UK) was obtained for inclusion in the new TCS. This code does extremely precise coordinate conversions, precession, nutation, etc., and is in use at a number of other observatories. Using this code is yet another step toward a standard system.

Minor alterations to the Visitor Center were begun. The modifications are being made to provide a crowd-controlled access to the auditorium during periods when films are being shown. In the process of doing so, it will be possible to make improvements in the crowded sales area.

B. Cerro Tololo Inter-American Observatory.

The mechanical shop in La Serena was kept busy most of this quarter fabricating the first 12 fiber optic positioners of "Argus"—a fiber optic fed, multiple object spectrometer for the CTIO 4-m telescope. Argus will be the first multi-object fiber feed designed specifically for a bench-mounted (and, therefore, highly stable) spectrograph. This will be housed in the "small" coude room, which was renovated recently to provide a suitably stable environment. The spectrograph will initially be configured to offer dispersions similar to those currently available with the 4-m RC spectrograph, with a higher dispersion echelle mode soon to follow.

A high speed data link was installed between the CTIO 4-m telescope LSI-11/73 data acquisition computer and the Sun 3/180 workstation housed in the same dome. The purpose of the link is to allow the astronomer to examine and reduce his or her data in essentially real time with the IRAF (Image Reduction and Analysis Facility) system available on the Sun workstation. The Sun computers, which are currently installed in the 4-m and 1-m (and, very soon, 1.5-m) domes have been extremely popular with visitors and staff, allowing many to completely reduce and calibrate their data before leaving the mountain. In addition to facilitating such usage, the new link should allow astronomers to more rapidly assess the quality of

14 their data, helping them to make more efficient use of the telescope time granted to them. Plans call for a similar link to be installed on the CTIO 1-m telescope Sun workstation in late January.

Design work began this quarter on two CCD-related projects. The first of these is a faint object CCD TV acquisition camera similar in concept to the highly successful Lick Observatory camera. CTTO's version will be based on either a GEC or Thomson CCD which should provide performance similar to that obtained at Lick (see Robinson and Osborne, Publications of the Astronomical Society of the Pacific, 99, 234, 1987). Testing of the prototype camera is tentatively scheduled to begin in mid-1988. The second CCD-related project consists of the design and fabrication of a "next generation" controller which should offer a number of significant improvements over the "VEB" controller currently in use on the 4-m, 1.5-m, and 0.9-m telescopes. CCDs, which have quickly become the "work horses" of optical astronomy, are in use every night of the year on Cerro Tololo. In addition to providing low noise and highly stable performance, the new generation controller will include important features such as the ability to handle multiple CCDs, sub-rasters of CCDs, and slow scanning.

Chilean economic statistics, FY 1988:

Month % Change Cum. Change Avg. Monthly

Oct 2.4 2.4 241.47 Nov 1.9 2.4 242.11 Dec 0.3 4.7 240.92

C. National Solar Observatory.

Along with J. Harvey (NSO), T. Duvall, and H. Jones (NASA), F. Hill (NSO) is proposing to develop a high-degree helioseismometer to be installed with the new spectromagnetograph at the Vacuum Tower/SP. This device would provide synoptic observations of the high-degree oscillations, allowing study of solar cycle changes in the frequencies of the modes. Coupled with the ring analysis, it would also allow studies of the convection zone flows during the cycle; an important piece of information for theories of the activity of the Sun. Steady progress was made in the effort to secure the use of array-based infrared imagers and spectrometers for NSO visiting observers and staff members: twelve days of engineering/observing time with the infrared imager at the McMath telescope have been granted for the February-July semester. The first user will be a visiting observer. As a contribution to the effort at CTIO to develop a high-speed data system for infrared imaging, D. Rabin (NSO) obtained relevant technical specifications of the NSO/NASA spectromagnetograph data system and forwarded them to CTIO. Rabin and J. Jefferies (NOAO) submitted a proposal for an FY 1989 instrumentation project that would partially fund the purchase of a new science-grade InSb 58x62 infrared array detector.

The bi-annual "Santa Fe Meeting", hosted this year by the National Solar Observatory, was held October 7-9, 1987, at the Santa Fe Hilton. M. Giampapa (NSO) was responsible for the scientific and local organization of the meeting. In contrast to the previous two Santa Fe meetings, it was decided to adopt an "AAS format" in which all participants had an opportunity to present a short oral

15 contribution on their recent work. Approximately 80 participants from the High Altitude Observatory and NSO attended.

16

VI. PROGRAM SUPPORT

A. Director's Office.

During this quarter, the Director's Office submitted its Annual Report, for the period July 1986 - June 1987, to the NSF. This information was also given to the Bulletin of the American Astronomical Society for publication. The Director, NOAO and the President, AURA provided the AURA Observatories Visiting Committee with their separate responses to its final report. Dr. Sidney Wolff formed the NSO Director Search Committee, chaired by Dr. Juri Toomre. The position has been widely advertised through an ad in the AAS Newsletter and through the Solar Physics Division of the AAS. The Committee is moving along at a rapid pace; the search should be completed next quarter. Upon resignation of the Manager of NOAO's Public Information Office, Sidney Wolff reconfigured the office to become the Publications and Information Resources Office. This office will continue to respond to requests from the media for support and information, and it will assist with the preparation of printed materials for the NSF. AURA has provided a management consultant, at no cost, to NOAO. This person will assist NOAO in looking for additional economies. The Director's Office submitted a proposal for supplemental funding to the NSF for the Research Experiences for Undergraduates Site Program. With NSF support, NOAO intends to continue to offer this valuable opportunity for students to work with projects ranging from solar convection studies to star formation studies in elliptical galaxies. The NSF-funded travel to foreign telescopes program is going well. This quarter has already provided six astronomers with support to the AAT, UKIRT, the Calar Alto Observatory in Spain, and the INT and Herschel telescopes in La Palma.

B. Publications and Information Resources. Major science stories released during the period included reports on the highest redshift quasars recently detected by NOAO and Cambridge scientists, luminous arcs as a gravitationally lensed mirage, further infrared evidence of planets around nearby stars, the 25th anniversary of the McMath solar telescope, and a story gathered from three separate papers describing what appears to be different steps in a quasar ignition sequence. Preparations were underway at the end of the period to provide informational support for a quasar workshop to be held the first week of January 1988, and for the January meeting of the American Astronomical Society, in Austin a week later.

A half-hour video feature, largely narrated by CTIO Director Robert Williams, was completed during the period, following extensive taping in Chile during early October. The office took delivery on an extensively revised Kitt Peak pamphlet during the period, as well as a large painting of the National New Technology Telescope concept, commissioned some time ago. The Public Information Officer resigned effective the end of December to accept an editorial position with Time-Life Books.

C. Central Computer Services. The image display software for the Sun went through some major upgrades during December. IRAF was ported to the Convex vector computer in late November in collaboration with the Convex office in Greenbelt, Maryland. Prototype software

17 was developed during the latter part of 1987 for generating image mosaics and installation of the hardware for a communications system between the 2.1-m, 4-m, and 1.3-m was completed. A fiber optics cable, holding 12 fibers, was chosen for the connection between domes. Two of the fibers are now in use with an Ethernet link between the 2.1-m and 4-m Sun workstations, a PC in the programmer's office in the 2.1-m building, and a PC in the administration building. Connecting other computers in these buildings is mostly a matter of installing a computer interface board.

A Sun-4/280 system and five Sun-3/60 color diskless workstations were installed in Tucson. The Sun-4 and three 3/60 systems form a powerful IRAF system for interactive reduction and analysis. The other two 3/60 systems will be used with the existing Tucson Sun-3/180 for IRAF development. A Sun-3/280 system, installed in Tucson for testing, was shipped to Kitt Peak and installed at the 2.1-m telescope. Two Sun-3/280 systems destined for CTIO were installed in Tucson for testing and burn-in. Two Sun-3/60 color workstations (with local disks) also destined for CTIO were similarly installed and tested. An NOAO-wide alias system was set up for electronic mail. This system serves both to connect La Serena and Sunspot to the world, using the network connection in Tucson, and to rationalize the mail name for all members of NOAO.

D. Central Administrative Services.

During the quarter ended December 31, 1987 the CAS Manager/Controller's Office completed tables for inclusion in the proposal to NSF for operation and management of NOAO; NOAO property administration was reviewed and a report was submitted to the AURA Administrative Steering Committee; and the FY 1987 audit was completed by Coopers & Lybrand.

The NOAO Personnel Office wrote an AURA Sexual Harassment policy, updated the AURA General Information booklet, and reissued the AURA policy regarding outside employment. A Rideshare Campaign was conducted, an Investment Committee formed, and an Affirmative Action questionnaire instituted. Personnel staff also attended a seminar on Affirmative Action. The annual performance review process was initiated and J. Ruffino, Personnel Manager, joined the Employers Advisory Board of the Tucson Urban League. NOAO exceeded its goal of $12,000 in the United Way campaign.

E. Central Facilities Operations.

Reroofing of the west wing and engineering wing of the downtown building was completed during the quarter with the exception of painting the roof, which is underway and will be completed early next quarter.

In conjunction with MCI, we upgraded our long distance telephone service to an MCI Prism Plus system at a savings of approximately 2.5 cents per minute of usage.

18 TELESCOPE USAGE STATISTICS Appendix A

Astronomica Observations Scheduled Maintenance, Engineering, Hours Instrument Tests, Scheduled Hours Used Hours Lost Equipment Changes, etc. Telescope Visitors Staff Weather Failure

4m 892.6 503.9 181.6 137.8 9.7 59.6

1.5m 840.7 478.0 94.1 151.6 23.4 93.6

lm 776.2 416.3 135.2 159.2 9.5 56.0

CTIO 0.9m 816.0 385.3 191.5 150.6 10.0 78.6

*0.6/0.9m 234.3 158.8 6.0 69.5 0 0

0.6m 114.9 20.0 42.2 52.7 0 0

**0.4m 32.0 0 32.0 0 0 0

4m 1153.25 535.17 129.58 372.75 57.75 58.0

2.1m 1072.34 593.55 125.54 316.25 26.5 10.5

CF 842.75 438.13 93.12 238.5 36.5 36.5

1.3m 996.0 376.69 134.81 310.5 122.0 52.0

KPNO #l-0.9m 981.5 448.81 122.94 322.0 15.75 72.0

#2-0.9m 908.85 402.75 79.75 347.6 26.75 52.0

#3-0.4m

Schmidt 271.5 138.5 12.0 98.0 17.0 6.0

Hilltop 1967.0 1477.0 55.0 403.0 32.0 0

Tower 727.0 373.5 104.5 107.0 60.0 82.0

Evans Fac 1596.1 605.8 263.3 677.0 49.0 1.0

NSO ***FTS Lab 551.5 374.5 4.5 52.0 8.0 112.5

***McMath 1444.5 384.9 444.1 469.0 18.5 128.0

Vacuum 738.0 401.0 0 305.0 0 32.0

Note: Scheduled hours are calculated according to the ephemendes for CTIO: October - 9.9 hours/night; November - 8.9 hours/night; December - 8.2 hours/night. * Use restricted to dark of the moon. ** Recommissioned on 24 February 1987 to observe LMC Supernova 1987a. *** Totals include both day and night hours. (All others are day only.)

CERRO TOLOLO INTER-AMERICAN OBSERVATORY

11

APPENDIX "B"

OBSERVATIONAL PROGRAMS

October-November-December: Individual telescope assignments are listed below. Graduate Students are indicated by an asterisk after their names. Nights assigned, (hours worked), and telescope used are included. Service Observing programs are denoted by S.O. instead of nights assigned.

M. Aaronson and E. Olszewski, U. of Arizona: "A Snapshot Abundance Survey of Magellanic Cloud Clusters", 4(33)4m. M. Aaronson, U. of Arizona, J. Mould, Caltech, and G. Bothun, U. of Michigan: "Motion of the Local Group", 4(35)1.5m.

C. Anguita and M.T. Ruiz, U. de Chile: "CCD Parallaxes for Faint High Proper Motion Stars", 3(18)1.5m. T. Armandroff and G. Da Costa: Yale U.: "A Search for Outlying Members of the Sculptor Dwarf Galaxy", 2(4)MS. B. Balik and G. Wallerstein, U. of Washington: "Structure of High Excitation Filaments Near Two Stars in the Vela Remnant" S.O. (10)1m.

T. Beers, Michigan State U., G. Preston and S. Shectman, Mt. Wilson and Las Campanas Observ.: "Search for Stars of Very Low Metal Abundance", 15 (48 )M S .

V. Blanco and A. Walker: CTIO: "Photometric Sequence Near the LMC Supernova", 6(42)0.9m

N. Caldwell, Whipple Observatory, and R.A. Schommer , Rutgers U.: "Cepheid Variables in Nearby Galaxies", S.0.(10)4m. W.A. Christiansen, U. of North Carolina, and R.E. Williams, CTIO: "Photometry and Polarimetry of Shell Galaxies", 2(6)4m.

Y.-H. Chu, U. of Illinois, R.C. Kennicutt, U. of Minnesota, and R.A. Schommer, Rutgers U.: "High Velocity Gas in HII Regions - SNRs of Wind-Blown Bubbles?", 2(19)1.5m G. Da Costa, T. Armandroff, and R. Light, Yale U.: "Velocity Dispersion and Matellicity Range of Sculptor and Carina", 4(34)4m, 5(20)0.9m.

L.N. da Costa and R.R. de Carvalho, Observatorio Nacional Brazil, and S.G. Djorgovski, Harvard Smithsonian: "Fundamental Properties of Elliptical Galaxies", 5(48)0.9m. 12

M. Davis and M. Strauss*, U. California Berkeley, J. Tonry, MIT, and A. Yahil, SUNY Stonybrook: "A Redshift Survey of IRAS Galaxies" , 5(40)1 .5m.

S.G. Djorgovski, Harvard Smithsonian, and G. Meylan, ESO: "Dynamical Structure and Evolution of Magellanic Clouds Globular Clusters: A Search for Post-Collapse Cores" 3(26)1.5m

O.J. Eggen, CTIO: "Photoelectric Photometry in the Visual and Near Infrared", 6(0)1.5m J. Elias, M. Phillips, D. Geisler, B. Gregory, M. Hamuy, S. Heathcote, N. Suntzeff, D. Terndrup, A. Walker, and R. Williams, CTIO, and S. Kirhakos, Sao Paulo, Brazil: "Optical and Infrared Observations of SN 1987a", 1(10)4m, 25(135)im 13(89)0.9m.

J. Elias, CTIO: "IR Imaging of Magellanic Cloud Star Formation" 2(20)4m, 2(22)1.5m, 2(20)0.9m.

J. Elias, CTIO, and J. Frogel, KPNO: "Evolved Stars in the Magellanic Clouds Detected by IRAS", 4(37)4m. E. Fitzpatrick, U. of Colorado: "Photometry and Spectroscopy of 0B Supergiants in the SMC", 17(106)1m. W.L. Freedman, Mt. Wilson & Las Campanas Observ., M. Aaronson U of Arizona, J. Mould and B. Madore, Caltech, and J. Graham,' Carnegie Institution of Washington: "Cepheid Distances to Sculptor Group Galaxies", 1(7)4m.

P.M. Gamavich*, U. of Washington: "Radial Velocities of Wide Binary Candidates at the South Galactic Pole", 6(55)1.5m. D. Geisler, CTIO, and M. Mateo, U. of Washington: "Abundances of LMC Clusters", 3(28)1.5m. D. Geisler, CTIO, and J.C. Forte, Inst. Astronomia y Fisica del Espacio, Argentina : "The NGC 1399 Globular Cluster System" 3(27)4m.

J. Graham, Carnegie Institution of Washington: "Infra-Red Photometry and Imagery of Young Stellar Objects", 4(38)4m. M. Gregg, Mt. Wilson & Las Campanas Observatories: "Red Spectra of Elliptical Galaxies", 8(53)1.5m. M. Gregg, Mt. Wilson & Las Campanas Observatories: "Integrated Light of Globular Clusters", 5(24)1m. E. Hardy Universite Laval, and N. Suntzeff, CTIO: "A Kinematical Study of the Magellanic Clouds using Carbon Stars", 5(22)4m. 13

G.L.H. Harris and M.P. FitzGerald, U. of Waterloo, and P. Stetson, Dominion Astrophysical Observatory: "The Lower Main Sequence of NGC 2287", 4(37)0.9m.

C. Hazard, U. of Pittsburgh, R.G. McMahon, IOA Cambridge, and D.G. Morton, National Research Council of Canada: "High Resolution Spectroscopy of the Remarkable BAL QSO 0105- 2735", 3(34)4m.

C. Hazard, U. of Pittsburgh, and R.G. McMahon, IOA Cambridge: "QSOs with 3.6 < z < 4.6", 3(34)4m.

E.K. Hege and J.C. Christou, U. of Arizona: "Speckle Imaging of SN1987A, R136a, VY CMa, and , Pic", 3(32)4m.

P. Hodge, M.G. Lee*, D. Boggs, and M. Mateo, U. of Washington: "Extinction in HII Regions of the LMC", 3(25)1m, 4(37)0.9m.

G. Illingworth, G. Miley, and C. Norman, STScI, and T. Heckman, U. of Maryland: "Are Nearby Radio-Loud Ellipticals Peculiar? -A Careful Comparative Study", 4(34)4m, 4(38)1.5m.

R.C. Kennicutt, U. of Minnesota: "Ionization Structure and Stellar Content of HII Regions", 2(18)1.5m, 4(31)1.0m.

S. Kent, Harvard Smithsonian: "Kinematics of Barred Galaxies", 5(37)1.5m

R. Lamontagne and S. Demers, F. Wesemael, and G. Fontaine, U. de Montreal: "Photometric Calibration of the Montreal-Cambridge Survey Fields", 5(32)0.9m, 7(56)MS.

B.M. Lasker, STScI, M. Azzopardi, N. Meyssonnier, and J. Lequeux, Observ. de Marseille, and M. Potter, STScI: "A Deep Survey for H0 Emission Objects in the LMC", 1(8)1.5m.

C. Leitherer, U. of Colorado: "Mass-Loss Rates for a Statistically Significant Sample of 0B Stars in the Magellanic Clouds", 10(90)1m.

E. Luck, Case Western Reserve U., and D.L. Lambert, U. of Texas "CN0 Abundances in Magellanic Cloud Cepheids", 4(37)4m.

P.K. Lu, Western Connecticut State U.: "0bjective-Prism Survey and Identification of Faint Main-Sequence F-Stars to Determine K(Z) Force", 8(51)MS.

M. Mateo and P. Hodge, U. of Washington: "Deep Luminosity Functions of Magellanic Cloud Star Clusters", 3(27)4m.

M. Mateo, U. of Washington, E. Olszewski, U. of Arizona, B. Madore, Caltech, and P. Hodge, U. of Washington: "Cepheids in Large Magellanic Cloud Clusters", 17(119)0.9m. 14

D.M. Meyer and D.G. York, U. of Chicago: "Observations of Fe, Ni, Cr, Zn, and Co at Large Redshifts", 4(36)4m.

P. Nisenson, M. Karovska, and C. Papaliolios, Harvard Smithsonian: "Speckle Imaging of SN1987A", 2(19)4m. E. Olszewski, U. of Arizona, H. Harris, U.S. Naval Observ., R. Schommer, Rutgers U., and N. Suntzeff, CTIO: 5(37)4m 2(12)0.6m.

C. Perry, Louisiana State U.: "Interstellar Reddening in the Solar Neighborhood. II. The Southern Hemisphere", 4(8)0.6m.

M.M. Phillips and N.B. Suntzeff, CTIO, A. Cowley, Arizona State U., and F.D.A. Hartwick, U. of Victoria: "IR Photometry of LMC CH Stars", 1(8)4m.

H. Quintana and M. Ramirez, U. Catolica de Chile: "Dynamics of Selected Dumb-Bell Galaxies", 3(13)0.9m

H. Quintana, X. Gomez, and L. Valladares, U. Catolica de Chile: "Dynamics of Galaxy Groups with a Dominant Member", 4(32)1m 5(34)0.9m.

J. Rose, U. of North Carolina, and G. Da Costa, Yale U.: "Integrated and Individual Star Spectroscopy in 47 Tuc" 4(1 9)1 .5m

M. Rubio, U. de Chile, and M. Roth, U. Nacional Autonoma de Mexico: "IR Observations of LMC Molecular Clouds" 4(36)1.5m. A. Saha, Mt. Wilson & Las Campanas Observatories, and P. Seitzer, KPNO: "RR Lyrae Variables in the Fornax Galaxy", 1(6)4m. P.C. Schmidtke, Arizona State U.: "Search for the Low-Mass X-ray Binaries in the Large Magellanic Cloud", 4(35)1.5m. P. Seitzer and J. Frogel, KPNO: "Kinematics of the Fornax Dwarf Galaxy", 4(37)4m.

H.A. Smith, Michigan State U., and D. Geisler, CTIO: "Abundances of SMC Giants", 4(27)1.5m. J. Steiner and S. Kirhakos, Sao Jose dos Campos, Brazil: "Spectroscopy of Edge-on AGN", 3(14)1m. N.B. Suntzeff, CTIO, and J.A. Graham, Carnegie Institution of Washington: "The Nature of the LMC Halo Population" 2(l8)4m, 4(27)1.5m. N.B. Suntzeff, CTIO: "CCD Photometric Sequence for Sculptor Dwarf Galaxy", 2(16 ) 1 .5m 15

D. Terndrup, CTIO: "New Photometric Standards for CCD Observations", 6(42)0.9m. J.A. Tyson, AT&T Bell Labs, and P. Boeshaar , Rider College: "Faint Object CCD Survey - Spectroscopy", 4(28)4m. P. Vader and G. Da Costa, Yale U.: "Morphology, Spectroscopy, and Environment of the QSO 00275-2859 Host Galaxy" S.O.(4)4m. S. van den Bergh and D. Welch, Dominion As trophy sical Observatory: "Ellipticals of Magellanic Cloud -Super-clusters" 4(37)0.9m.

A.R. Walker, CTIO, CD. Laney, South African Astronomical Observatory, and V. Castellani, Istituto Astronomico Univ. Degli Study-Roma 'La Sapienza': "CMD for NGC 1866", 2(l3)4m. D.L. Welch and P.B. Stetson, Dominion Astrophysical Observatory "The Rotation Curve of the Galaxy for R>R0", 8(68)1m. B. Zuckerman, U. California Los Angeles, D. Backman, R. Probst, and I. Gatley, NOAO: "Infrared Coronographic Observations! A Study of the Beta Pictoris Disk and a Search for Brown Dwarfs", 4(16)1.5m.

YALE PROGRAMS

S. Kawaler, Yale U. and S.O. Kepler, Universidad Federal Rio Grande do Sul, Brazil: "Time Resolved Spectrophotometry of the Rapidly Oscillating Ap Star HD 24712" 6(38)1m.

Executed Proposals 10/01/87 - 12/31/87 Page 1 Mon Jan 18 13:49:08 1988

Nights Hours Days Hours 6708 f87 H Abt, Kitt Peak National Observatory Improved Study of Duplicity among F8-G1 Stars. Coude Feed 7.00 15.50 0.00 0.00

6836 f87 H Abt, Kitt Peak National Observatory C Corbally, S.J., Vatican Observatory UBV Photometry with a CCD of Trapezium Systems Nr. 1 0.9 meter 5.00 27.50 0.00 0.00

6835 f87 w H Abt, Kitt Peak National Observatory f_J Classification of Bright Star Catalogue (-3 Supplement Stars Nr. 1 0.9 meter 5.00 52.00 0.00 0.00 1-3 6867 f87 ^ C Ambruster, University of Colorado j^ A Hull, Perkin-Elmer Corportion M Lallo, Villanova University > Z The First Rotation Periods of Fully Convective M 2 ^ Dwarfs Nr. 2 0.9 meter 10.83 78.25 0.00 0.00 2 2 z o O 2 7051 f87 H > D Backman, Kitt Peak National Observatory X tr* I Gatley, NOAO-ADP w _ B Zuckerman, ^ University of California, Los Angeles (^ Coronographic Search for 3.3 urn PAH Emission from tq Grains... 1.3 meter 3.00 32.00 0.00 0.00 » < >

6949 f87 O_ M Balcells, J Hoessel, University of Wisconsin ;# Rotation Properties of Post-Merger Galaxies K Nr. 1 0.9 meter 4.00 10.00 0.00 0.00

6922 f87 S Barden, Kitt Peak National Observatory R Wade, University of Arizona Spectral Imaging of Nova Shells and Related Objects 4 meter 3.00 27.50 0.00 0.00 Executed Proposals 10/01/87 - 12/31/87 Page 2 Mon Jan 18 13:49:08 1988

Nights Hours Days Hours 6906 f87 R Binzel, C Chapman, D Davis, S Weidenschilling, D Levy, M Magee, A Ott, Planetary Science Institute Photometric Investigation of Asteroid Collissional Evolutio Nr. 2 0.9 meter 6.50 47.50 0.00 0.00

6936 f87 W Blair, Johns Hopkins University Y Chu, University of Illinois R Kennicutt, Jr., University of Minnesota Kinematic Study of and Search for M33 Supernova Remnants 4 meter 4.00 44.00 0.00 0.00

6866 f87 B Bohannan, S McCandlis, University of Colorado Spectral Time Series of Two Wolf-Rayet Stars Coude Feed 4.00 31.00 0.00 0.00

6918 f87 H Bond, Space Telescope Science Institute R Ciardullo, Carnegie Institution of Washington A Shafter, University of Texas CCD Photometry of the Nuclei of Bright Planetary Nebulae Nr. 1 0.9 meter 5.00 47.00 0.00 0.00

6952 f87 R Boyle, Dickinson College J Keady, Los Alamos National Laboratory D Jennings, NASA Goddard Space Flight Center Mass Loss from Heavily Obscured Carbon Stars 4 meter 0.00 0.00 6.00 17.00

7036 f87 A Brown, F Walter, J Neff, University of Colorado F Vrba, U.S. Naval Observatory, Flagstaff Naked T Tauri Stars: UBVRI Photometry - Survey and Variabi Nr. 2 0.9 meter 12.00 45.50 0.00 0.00 Executed Proposals 10/01/87 - 12/31/87 Page 3 Mon Jan 18 13:49:08 1988

Nights Hours Days Hours 6853 f87 J Brown, Indiana University R Levreault, Harvard-Smithsonian Center for Astrophysics Line Profiles in FU Orions Coude Feed 1.00 5.00 0.00 0.00

6911 f87 H Bushouse, M Werner, NASA Ames Research Center Near-Infrared Imaging of Interacting and Merging Galaxies 2.1 meter 4.00 48.00 0.00 0.00

6849 f87 B Carney, M Laycox, University of North Carolina UBV Photometry of High-Velocity Proper Motion Stars 1.3 meter 5.00 42.50 0.00 0.00

6919 f87 R Ciardullo, V Rubin, Carnegie Institution of Washington Velocity Structure in the Near-Nuclear Ionized Gas in M31 4 meter 4.00 26.00 0.00 0.00

6969 f87 A Crotts, University of Texas, Austin Large Scale Structure in the Lyman Alpha Forest 4 meter 3.50 16.00 0.00 0.00

6845 f87 G Da Costa, T Armandroff, Yale University The Mass-to-Light Ratio of the Dwarf Elliptical Galaxies... 4 meter 4.00 32.50 0.00 0.00 Nr. 1 0.9 meter 4.00 46.00 0.00 0.00

6993 f87 R Davies, Kitt Peak National Observatory D Burstein, Arizona State University G Wegner, Dartmouth College M Colless, Kitt Peak National Observatory, Visitor R McMahan, Harvard-Smithsonian Center for Astrophysics Elliptical Galaxies as Tracers of Non-Uniformities in the.. Nr. 1 0.9 meter 6.00 40.75 0.00 0.00 Executed Proposals 10/01/87 - 12/31/87 Page 4 Mon Jan 18 13:49:08 1988

Nights Hours Days Hours 6951 f87 R Davies, T Kinman, B Schoening, Kitt Peak National Observatory Test Photometric Observations for a Faint Galaxy Redshift.. 4 meter 1.00 0.00 0.00 0.00 Burrell Schmidt 4.00 12.00 0.00 0.00

6921 f87 R Davies, E Sadler, Kitt Peak National Observatory Line-Strength Gradients in Elliptical Galaxies 4 meter 3.00 29.50 0.00 0.00

7002 f87 J Dickel, Y Chu, University of Illinois Physical Condition in the Filaments of IC 443 2.1 meter 4.00 17.25 0.00 0.00

6954 f87 F Fekel, K Strassmeier, Vanderbilt University Spectroscopy of Binary and Multiple Stars Coude Feed 6.00 37.00 0.00 0.00

6953 f87 F Fekel, Vanderbilt University Determination of B and A Star Radial Velocity Standards Coude Feed 5.00 26.50 0.00 0.00

9058 f87 D Forbes, P Dawson, Trent University BVRI Photometry of Selected High Proper-Motion Stars 1.3 meter 4.00 11.50 0.00 0.00

7053 f87 J Frogel, R Davies, Kitt Peak National Observatory P Eisenhardt, I Gatley, NOAO-ADP IR Camera Evaluation on the 4-M: Cosmologically Interest.. 4 meter 6.00 15.50 0.00 0.00 Executed Proposals 10/01/87 - 12/31/87 Page 5 Mon Jan 18 13:49:08 1988

Nights Hours Days Hours 7050 f87 J Frogel, R Davies, Kitt Peak National Observatory I Gatley, NOAO-ADP IR Camera Evaluation: Infrared Surface Photometry of 2.1 meter 3.00 36.25 0.00 0.00

7010 f87 J Gallagher, D Hunter, Lowell Observatory I Gatley, NOAO-ADP R Joyce, Kitt Peak National Observatory IR Imaging of Luminous Blue Galaxies 2.1 meter 2.00 2.00 0.00 0.00

6852 f87 T Gehrels, University of Arizona J Anderson, Jet Propulsion Laboratory R Hill, Kitt Peak National Observatory\CWRU A Search for the Tenth Planet Burrell Schmidt 4.00 12.00 0.00 0.00

6959 f87 R Giovanelli, NAIC\Arecibo Observatory M Haynes, Cornell University Deviations from Hubble Flow around the Void in Pisces Nr. 1 0.9 meter 7.00 17.50 0.00 0.00

6831 f87 A Grauer, University of Arkansas Time-Series Photometry of Hot Evolved Stars 1.3 meter 10.00 66.50 0.00 0.00

7003 f87 J Grigsby, N Morrison, L Anderson, University of Toledo High-Dispersion Spectroscopy of Early B-type Stars in.... Coude Feed 5.00 29.25 0.00 0.00

6956 f87 E Halbedel, Corralitos Observatory A Study of Be Stars with Large Photometric Variations Coude Feed 4.00 46.50 0.00 0.00 Executed Proposals 10/01/87 - 12/31/87 Page 6 Mon Jan 18 13:49:08 1988

Niqhts Hours Days Hours 6957 f87 D Hall, University of Hawaii I Heyer, University of Massachusetts K Hinkle, Kitt Peak National Observatory A Search for Dark Companions of K and M Giants 4 meter 0.00 0.00 2.00 2.00

7032 f87 F Hamann, M Simon, SUNY at Stony Brook Near IR Spectroscopy of Luminous YSO's 4 meter 3.00 37.50 0.00 0.00

7033 f87 D Hamilton, National Optical Astronomy Observatories Multicolor CCD Photometryof Faint Red Galaxies 2.1 meter 4.00 33.50 0.00 0.00

6851 f87 D Hamilton, National Optical Astronomy Observatories Large Aperture Spectrophotometry of Nearby Galaxies Nr. 2 0.9 meter 8.00 28.00 0.00 0.00

7047 f87 S Heap, P Hintzen, NASA Goddard Space Flight Center The Hottest Central Stars of Planetary Nebulae 2.1 meter 4.00 46.50 0.00 0.00

7041 f87 T Heckman, E Smith, University of Maryland G Illingworth, Space Telescope Science Institute The Stellar Dynamics of Radio Galaxies with Strong, Seyfert 4 meter 4.00 47.25 0.00 0.00

6855 f87 R Henry, University of Oklahoma B Pagel, Royal Greenwich Observatory Abundance Gradients in Massive Spiral Galaxies 2.1 meter 4.00 7.00 0.00 0.00 Executed Proposals 10/01/87 - 12/31/87 Page 7 Mon Jan 18 13:49:08 1988

Nights Hours Days Hours 6999 f87 R Honeycutt, Indiana University E Schlegel, Harvard-Smithsonian Center for Astrophysics Time-resolved Spectrophotometry of Accretion Disks in.... 2.1 meter 6.00 64.25 0.00 0.00

6924 f87 J Houck, M Dow, E Salpeter, N Lu, Cornell University Surveying Extremes in Extinction and Reddening Nr. 1 0.9 meter 3.00 17.00 0.00 0.00

7011 f87 D Hunter, J Gallagher, Lowell Observatory R Joyce, Kitt Peak National Observatory I Gatley, NOAO-ADP JHK Imaging of Young Stellar Complexes in the Local Group 2.1 meter 3.00 35.25 0.00 0.00 1.3 meter 1.00 3.00 0.00 0.00

6859 f87 D Jewitt, J Luu, Massachusetts Institute of Technology Bulk Study of Small Asteroids Burrell Schmidt 4.00 38.00 0.00 0.00

7042 f87 R Joyce, F Gillett, Kitt Peak National Observatory Followup of Galactic IRAS Sources: Classification and 1.3 meter 8.00 54.50 0.00 0.00

6939 f87 M Karovska, P Nisenson, R Noyes, B Sams, C Papaliolios, Harvard-Smithsonian Center for Astrophysics High Angular Observations of the Circumstellar Environment. 4 meter 1.00 2.50 0.00 0.00 Executed Proposals 10/01/87 - 12/31/87 Page 8 Mon Jan 18 13:49:08 1988

Nights Hours Days Hours 6933 f87 S Kenyon, L Hartmann, Harvard-Smithsonian Center for Astrophysics Continuum T Tauri Stars: Boundary Layer or Chromospheric.. Nr. 2 0.9 meter 6.50 33.75 0.00 0.00

6932 f87 S Kenyon, L Hartmann, Harvard-Smithsonian Center for Astrophysics FTS Observations of Young Stellar Objects 4 meter 5.00 29.50 4.50 7.75

6935 f87 T Kinman, Kitt Peak National Observatory M Rieke, G Rieke, University of Arizona Visual and I.R. Photometry of Nearby RR Lyrae Stars 1.3 meter 5.00 20.50 0.00 0.00

6996 f87 R Kirshner, Harvard-Smithsonian Center for Astrophysics K Long, W Blair, T Smecker, Johns Hopkins University P Winkler, Middlebury College Discovering Supernova Remnants in M33 4 meter 3.00 32.50 0.00 0.00

6899 f87 S Kleinmann, University of Massachusetts B Goodrich, J Africano, B Binkert, Kitt Peak National Observatory BV Photometry of a Flux-Limited IRAS Sample Nr. 2 0.9 meter 4.00 15.00 0.00 0.00

6878 f87 S Kleinmann, University of Massachusetts D Backman, Kitt Peak National Observatory Photometry/Spectrophotometry of Very Red Stars Found by IRA Nr. 2 0.9 meter 5.50 9.50 0.00 0.00

6980 f87 S Kleinmann, University of Massachusetts I Gatley, NOAO-ADP N Scoville, California Institute of Technology IR Spectroscopy of Nearby Bright Star-Forming Galaxies 1.3 meter 5.00 18.50 0.00 0.00 Executed Proposals 10/01/87 - 12/31/87 Page 10 Mon Jan 18 13:49:08 1988

Nights Hours Days Hours 6856 f87 R Luck, S Challener, Case Western Reserve University Chemical Abundances in SMR Stars Coude Feed 7.00 58.50 0.00 0.00

6934 f87 L Marschall, R Mathieu, Harvard-Smithsonian Center for Astrophysics N Comins, University of Maine Photometry of the lambda Orionis Association and Trumpler 3 1.3 meter 6.00 33.00 0.00 0.00

6858 f87 P Massey, C Pilachowski, Kitt Peak National Observatory The Spectrum of the Kitt Peak Night Sky Nr. 2 0.9 meter 1.00 0.00 0.00 0.00

6927 f87 M Mateo, M Lee, University of Washington CCD Washington Photometry of Globular Clusters in M31 Nr. 1 0.9 meter 4.00 42.00 0.00 0.00

7037 f87 M Mateo, University of Washington The Metallicities of Cepheids in Local Group Galaxies 2.1 meter 7.00 42.75 0.00 0.00

6824 f87 J Matthews, University of Western Ontario W Gieren, Observatorio Astronomico Nacional Spectroscopy and photometry of double mode Cepheids Coude Feed 9.00 60.00 0.00 0.00 Nr. 2 0.9 meter 10.00 86.50 0.00 0.00

6721 f87 H McAlister, W Hartkopf, J Sowell, E Dombrowski, Georgia State University 0 Franz, Lowell Observatory Binary Star Speckle Interferometry. 4 meter 5.00 54.25 0.00 0.00 Executed Proposals 10/01/87 - 12/31/87 Page 9 Mon Jan 18 13:49:08 1988

Nights Hours Days Hours / U14 f 8 7 D Koo, Space Telescope Science Institute CCD Imaging of a Luminous Arc in a Rich Cluster of Galaxies 4 meter 0.50 0.00 0.00 0.00

7016 f87 R Kron, J Munn, S Majewski, M Bershady, University of Chicago, Yerkes Obs. A Complete Spectroscopic Survey of Very Faint UV-Excess Obj 4 meter 4.00 7.00 0.00 0.00

7028 f87 E Lada, N Evans II, University of Texas, Austin I Gatley, NOAO-ADP D DePoy, National Optical Astronomy Observatories Near-IR Survey of Dense Molecular Cores in the Orion B... 1.3 meter 5.00 41.50 0.00 0.00

6973 f87 D Lambert, Y Sheffer, University of Texas, Austin K Hinkle, Kitt Peak National Observatory Circumstellar CO Around Two Luminous Yellow Supergiants 4 meter 0.50 5.50 3.00 8.75

6829 f87 A Landolt, Louisiana State University UBVRI Photometry of Space Telescope Spectrophotometric .... 1.3 meter 4.00 0.00 0.00 0.00

7026 f87 T Lauer, Princeton University Morphology of Multiple-Nucleus First-Ranked Galaxies 4 meter 1.50 10.50 0.00 0.00

6871 f87 T Liu, Boston University Radial Velocities and Photometry of Field RR Lyrae Stars 2.1 meter 4.00 40 75 0 00 0 00 Coude Feed 2.00 24 00 0 00 0 00 1.3 meter 4.00 30 50 0 00 0 00 Nr. 2 0.9 meter 4.00 29.50 0.00 0.00 Executed Proposals 10/01/87 - 12/31/87 Page 12 Mon Jan 18 13:49:08 1988

Nights Hours Days Hours 9054 f87 C Neese, Kitt Peak National Observatory BV Photometry of Stars in the Galactic Anticenter Nr. 2 0.9 meter 3.00 22.00 0.00 0.00

6967 f87 A Oemler, Jr., E Zirbel, Yale University J Allington-Smith, T Broadhurst, University of Durham R Ellis, Durham University The Evolution of Galaxies in Radio Selected Groups 2.1 meter 4.00 37.75 0.00 0.00

6958 f87 R Patterson, Southwest Missouri State University Spectrophotometery of F, G, and K Spectral Class, Nr. 2 0.9 meter 6.50 59.50 0.00 0.00

6854 f87 M Peimbert, S Torres-Peimbert, Instituto de Astronomia, UNAM Chemical Composition of Gaseous Nebulae and Chemical 2.1 meter 4.00 32.50 0.00 0.00

9052 f87 C Pilachowski, Kitt Peak National Observatory Exploration of the Universe 4 meter 2.00 7.25 0.00 0.00

6916 f87 C Pilachowski, Kitt Peak National Observatory T Duvall, Jr., NASA Goddard Space Flight Center Global Oscillations in Jupiter 2.1 meter 5.00 23.00 0.00 0.00

6915 f87 C Pilachowski, Kitt Peak National Observatory C Sneden, University of Texas, Austin Carbon Isotopes in Subdwarfs Coude Feed 3.00 31.50 0.00 0.00 Executed Proposals 10/01/87 - 12/31/87 Page 11 Mon Jan 18 13:49:08 1988

Nights Hours Days Hours 6880 f87 P McCarthy, H Spinrad, W van Breugel, University of California, Berkeley S Djorgovski, Harvard-Smithsonian Center for Astrophysics [Oil] Interference Filter Imaging of Distant Radio Galaxies 2.1 meter 4.00 35.50 0.00 0.00

7008 f87 G Miley, Space Telescope Science Institute K Chambers, Johns Hopkins University R Joyce, Kitt Peak National Observatory Infrared Imaging of Ultra-Steep Spectrum Radio Galaxies 2.1 meter 4.00 42.00 0.00 0.00

6990 f87 H Miller, J Wilson, Georgia State University M Carini, George State University An Investigation of Short-term Variability for Selected BL. Nr. 1 0.9 meter 5.00 51.00 0.00 0.00

6910 f87 J Moody, J Burns, University of New Mexico L Wells, National Optical Astronomy Observatories The Distribution of Emission-line Galaxies in Voids and Burrell Schmidt 7.00 45.00 0.00 0.00

9060 f87 M Mumma, A Storr, S Nadler, NASA Goddard Space Flight Center Observe Comet Bradfield 4 meter 1.50 16.50 1.50 0.00

6877 f87 C Neese, Kitt Peak National Observatory The Kinematic-Age Relationship in Distant Anticenter F Star Nr. 1 0.9 meter 8.00 14.50 0.00 0.00 Executed Proposals 10/01/87 - 12/31/87 Page 13 Mon Jan 18 13:49:08 1988

Nights Hours Days Hours 6817 f87 C Pilachowski, J Africano, B Goodrich, B Binkert, Kitt Peak National Observatory Sky Brightness on Kitt Peak. Nr. 2 0.9 meter 1.00 0.00 0.00 0.00

6637 f87 L Ramsey, D Huenemoerder, D Buzasi, Pennsylvania State University S Barden, Kitt Peak National Observatory Monitoring of RS CVn and Related Objects. 2.1 meter 5.00 33.50 0.00 0.00 Coude Feed 10.00 105.50 0.00 0.00

6940 f87 M Rao, A Landolt, Louisiana State University A Study of Selected Galactic Star Clusters Nr. 1 0.9 meter 5.00 45.50 0.00 0.00

6988 f87 R Remillard, Massachusetts Institute of Technology W Roberts, Harvard-Smithsonian Center for Astrophysics Optical Identification of HEAO-1 X-Ray Sources Burrell Schmidt 7.00 43.50 0.00 0.00

6994 f87 S Ridgway, NOAO-CCS J Beckers, F Roddier, J Christou, NOAO-ADP R Probst, Kitt Peak National Observatory Two-dimensional IR Imaging — Demonstration of the Techniqu 4 meter 3.00 28.50 2.00 0.00

6888 f87 P Schmidtke, Arizona State University J Africano, Kitt Peak National Observatory Lunar Occultations of Double Stars 1.3 meter 0.50 0.00 0.00 0.00 Nr. 2 0.9 meter 3.33 27.50 0.00 0.00

6830 f87 R Schwartz, D Jennings, University of Missouri, St. Louis The Ionization and Excitation Structure of Herbig-Haro Obje 2.1 meter 3.00 33.60 0.00 0.00 Executed Proposals 10/01/87 - 12/31/87 Page 14 Mon Jan 18 13:49:08 1988

Nights Hours Days Hours 6879 f87 * M Shara, B Lasker, M Potter, Space Telescope Science Institute A Search for Supernova Remnants in M33 2.1 meter 5.00 28.50 0.00 0.00

6930 f87 M Simon, SUNY at Stony Brook W Chen, State University of New York R Joyce, Kitt Peak National Observatory Lunar Occulation Observation of Young Stellar Objects in Ta 4 meter 0.50 4.00 0.00 0.00

6841 f87 M Sitko, University of Cincinnati Continuum Variability in GO COMAE 1.3 meter 4.00 31.50 0.00 0.00

6885 f87 H Smith, P Schwartz, D Mozurkewich, J Fischer, Naval Research Laboratory IR Imaging of Outflow Regions in Dark Clouds 1.3 meter 5.00 34.00 0.00 0.00

6914 f87 J Stauffer, NASA Ames Research Center R Probst, Kitt Peak National Observatory The Luminosity Function of the Pleiades to Mv = 14-5 Nr. 1 0.9 meter 7.00 65.00 0.00 0.00

6872 f87 K Strassmeier, F Fekel, D Hall, Vanderbilt University Doppler Imaging of HD 26337 Coude Feed 4.00 35.00 0.00 0.00

6882 f87 S Strom, K Strom, University of Massachusetts A Spectroscopic Study of Young Stellar Objects Associated.. 2.1 meter 4.00 30.00 0.00 0.00 Executed Proposals 10/01/87 - 12/31/87 Page 15 Mon Jan 18 13:49:08 1988

Nights Hours Days Hours 6904 f87 T Tsuji, Tokyo Astronomical Observatory S Ridgway, NOAO-CCS K Hinkle, Kitt Peak National Observatory Spectroscopy of Circumstellar Envelopes of Late-type Giants 4 meter 1.50 0.00 4.00 10.00

6991 f87 A Uomoto, Johns Hopkins University Spectrophotometry of Type II Supernovas 4 meter 3.00 22.50 0.00 0.00

6889 f87 F Vrba, U.S. Naval Observatory, Flagstaff F Walter, A Brown, University of Colorado P Myers, R Mathieu, Harvard-Smithsonian Center for Astrophysics Near Infrared Photometry of Taurua-Aurigae and Orion "Naked 1.3 meter 5.00 32.00 0.00 0.00

6886 f87 G Wallerstein, University of Washington J Dominy, Digital Systems Group, Inc. CNO Abundances and Isotopies in CH Stars 4 meter 1.00 14.50 1.50 1.50

6873 f87 F Walter, A Brown, University of Colorado F Vrba, U.S. Naval Observatory, Flagstaff R Mathieu, P Myers, Harvard-Smithsonian Center for Astrophysics Naked T Tauri Stars: Space Densities and IMFs 2.1 meter 5.00 44.50 0.00 0.00

7024 f87 R Walterbos, Institute for Advanced Study R Braun, National Radio Astronomy Observatory, VLA Narrow-band Imagery of HII Regions and Supernova Remnants i Nr. 1 0.9 meter 1.00 9.00 0.00 0.00 Executed Proposals .10/01/87 - 12/31/87 Page 16 Mon Jan 18 13:49:08 1988

,„__ Nights Hours Days Hours 6950 f87 J M Ward, L Bryant, University of Washington C Boisson, Observatoire de Meudon Infrared Array Imaging of Active Nuclei 2.1 meter 1.00 4.75 0.00 0.00

9057 f87 D Willmarth, National Optical Astronomy Observatories Feasibility Study of a Technique to Improve the Accuracy... Coude Feed 2.00 2.00 0.00 0.00

6864 f87 A Wolfe, K Lanzetta, University of Pittsburgh D Turnshek, Space Telescope Science Institute Lyman Alpha Emission from High Redshift Disk Galaxies 4 meter 4.00 44.50 0.00 0.00

9059 f87 S Wolff, Kitt Peak National Observatory Luminosities and Abundances of Orion B-Type stars Coude Feed 3.00 24.00 0.00 0.00

7004 f87 D York, University of Chicago R Green, Kitt Peak National Observatory QSC Absorption Lines at High Redshift 4 meter 4.00 43.00 0.00 0.00

6978 f87 D York, G Burks, University of Chicago The Search for Distant Halo RR Lyrae Stars in the Direction Nr. 1 0.9 meter 4.00 27.00 0.00 0.00

7005 f87 D York, B Yanny, University of Chicago J Gallagher, Lowell Observatory Forbidden Oil Emission from QSO Absorbing Systems 4 meter 4.00 19.50 0.00 0.00 Executed Proposals 10/01/87 - 12/31/87 Page 17 Mon Jan 18 13:49:08 1988

Nights Hours Days Hours 7023 f87 J Young, S Kleinmann, L Allen, University of Massachusetts Star Formation in Infrared Bright Galaxies Nr. 1 0.9 meter 6.00 60.00 0.00 0.00

6976 f87 B Zuckerman, H Epps, University of California, Los Angeles I Gatley, NOAO-ADP D Backman, R Probst, Kitt Peak National Observatory J Stauffer, NASA Ames Research Center A Search for Brown Dwarfs in the Pleiades and Hyades Cluste 1.3 meter 5.00 60.00 0.00 0.00

Executed Proposals 10/01/87 - 12/31/87 Page 1 Tue Jan 26 12:44:22 1988

,o 53 Nights Hours Days Hours c 3> 1161 487 pj H l-t M R Altrock, Sacramento Peak Observatory rt O S/B181-Coronal Transient patrol Supts SMM ft> 25 i-l > Evans Solar Facility/SP 0.00 0.00 9.00 47.00 r1 M 3 w a. o 1023 487 rt> R Altrock, Sacramento Peak Observatory a. £ S/B003-Coronal Observations •• 5*> Evans Solar Facility/SP 0.00 0.00 85.00 99.00 H O NJ w —^ VI u> w 1212 487 1—' & ^^ < P Bernath, University of Arizona CO > T/Spectroscopy of Molecules of Astrophysical -J H O Interest McMath FTS Lab 5.00 45.00 5.00 45.00 5*1 >-<

1348 487 s D Bonaccini, Instituto de Astronomia TJ O S/T299-Narrow Band Filtergrams 5*J VT 0.00 0.00 16.00 50.00 H

1346 487 D Bonaccini, Instituto de Astronomia S/T296-Calibration of Line Ratio Techniques VT 0.00 0.00 19.00 159.00

1237 487 L Brown, Jet Propulsion Laboratory T/High Resolution Lab Spectroscopy to Support Atmospheric. McMath FTS Lab 6.00 55.00 6.00 54.00

> 1101 487 R Canfield, University of Hawaii (D S/T205-Flare, H-alpha Extreme Wing Observations 5 VT 0.00 0.00 7.00 24.00 H

1315 487

H Dara, o_ Research Center for AstronomyNAcad. of Athens o" S/B206-Measurements of Small Scale Magnetic § Fields and .... Evans Solar Facility/SP 0.00 0.00 11.00 30.00 H

TJ i-l O X) o CO Executed Proposals 10/01/87 - 12/31/87 Page 2 Tue Jan 26 12:44:22 1988

Nights Hours Days Hours 1299 487 S Davis, University of California, Berkeley T/Observation of the Emission Spectrum of FeD McMath FTS Lab 5.00 36.00 5.00 36.00

1138 487 D Deming, NASA Goddard Space Flight Center T/Monitoring Apparent Velocity of Integrated Sunlight McMath FTS Lab 2.00 4.50 2.00 4.50

1291 487 J Doyle, Armagh Observatory T/High Signal to Noise Line Profiles on II Peg McMath Main 6.00 17.50 0.00 0.00

1338 487 G Elste, University of Michigan S/B215-Spectroheliograms at 4019.7A Evans Solar Facility/SP 0.00 0.00 2.00 3.00

1303 487 P Foukal, Cambridge Research & Instrumentation, Inc. S/B209-Electric Field Measurements in Chromospherical Cor.. Evans Solar Facility/SP 0.00 0.00 26.00 48.00

5273 487 M Giampapa, National Optical Astronomy Observatories T/simultaneous Call Resonance Line & Infrared H& K McMath Main 0.00 0.00 2.00 16.00

1219 487 M Giampapa, National Optical Astronomy Observatories T/H\(*a Emission & Rotation in Selected dMe Stars McMath Main 19.00 43.00 0.00 0.00

10 5.? 4 87 M Giampapa, National Optical Astronomy Observatories T/Rotational Modulation of the He I De Line in Active .... McMath Main 11.00 48.50 0.00 0.00 Executed Proposals 10/01/87 - 12/31/87 Page 3 Tue Jan 26 12:44:22 1988

Nights Hours Days Hours 1294 487 M Giampapa, National Optical Astronomy Observatories T/Simultaneous IUE & McMath Observations of T Tauri Stars.. McMath Main 27.00 94.50 0.00 0.00

1026 487 L Gilliam, National Solar Observatory/Sac Peak S/B062 - Coronagraph Monitor Evans Solar Facility/SP 0.00 0.00 33.00 35.00

1025 487 L Gilliam, National Solar Observatory/Sac Peak S/B057-Monitoring Community Evans Solar Facility/SP 0.00 0.00 61.00 79.00

1034 487 L Gilliam, National Solar Observatory/Sac Peak S/HOOl-Flare Patrol (monitoring) Hilltop Dome/SP 0.00 0.00 91.00 614.00

1035 487 L Gilliam, National Solar Observatory/Sac Peak S/H002-White Light Patrol (Monitoring) Hilltop Dome/SP 0.00 0.00 87.00 543.00

1036 487 L Gilliam, National Solar Observatory/Sac Peak S/H003 - Multiple Bank Polimeter (Monitoring) Hilltop Dome/SP 0.00 0.00 24.00 157.00

1039 487 L Gilliam, National Solar Observatory/Sac Peak s/H008-White Light Sunspot Drawing Hilltop Dome/SP 0.00 0.00 92.00 76.00

1226 487 L Goad, National Optical Astronomy Observatories T/Adaptive Optics McMath East 9.00 24.00 0.00 0.00 Executed Proposals 10/01/87 - 12/31/87 Page 4 Tue Jan 26 12:44:22 1988

into Aon Nights Hours Days Hours luoo 4 8 7 L Goldberg, National Optical Astronomy Observatories T/Radial Velocity Variations of alpha Ori and Two other--- McMath Main 10.00 21.50 0.00 0.00

1292 487 J Harvey, National Solar Observatory/Tucson T/Solar Vacuum-NASA/GSFC Rocket Support Solar Vacuum 0.00 0.00 3.00 17.00

3790 487 J Harvey, National Solar Observatory/Tucson T/Vacuum Synoptic Program: Daily Solar Vacuum 0.00 0.00 90.00 367.00

1221 487 R Holt, Swarthmore College T/Chromospheric Velocity Fields at Hel Dark Points McMath Main 0.00 0.00 3.00 16.00

1207 487 S Keil, Sacramento Peak Observatory S/T258-Tests of Agile Mirror on ESG VT 0.00 0.00 8.00 42.00

1305 487 S Koutchmy, National Solar Observatory/Sac Peak S/B205-Spectroheliograms, CaK H\(*a Evans Solar Facility/SP 0.00 0.00 1.00 2.00

1326 487 S Koutchmy, National Solar Observatory/Sac Peak S/T298-Photospheric vs. Chromospheric Network.... VT 0.oo 0.00 1.00 5.00

1240 487 S Koutchmy, National Solar Observatory/Sac Peak S/T281-PHotospheric True White-light Structures VT 0.00 0.00 8.00 45.00 Executed Proposals 10/01/87 - 12/31/87 Page 6 Tue Jan 26 12:44:22 1988

Nights Hours Days Hours 1150 487 H Neckel, Hamburger Sternwarte T/Limb Darkening McMath Main 0.00 0.00 3.00 0.00

1316 487 L November, Sacramento Peak Observatory S/H022 - Proper Motion Tests Hilltop Dome/SP 0.00 0.00 13.00 55.00

1339 487 L November, Sacramento Peak Observatory S/B216-CaK spectroheliograms Evans Solar Facility/SP 0.00 0.00 2.00 3.00

1290 487 G Peters, University of Southern California T/Synoptic observations of Rapid Variable Be Star Androm.. McMath Main 6.00 24.00 0.00 0.00

1235 487 A Pierce, National Solar Observatory/Tucson T/Solar Gravitational Redshift McMath Main 0.00 0.00 10.00 42.00

1223 487 A Potter, NASA Johnson Space Flight Center T/Spatial Distribution of Sodium & Potasium in Atmosphere.. McMath Main 0.00 0.00 4.00 17.50

1298 487 D Rabin, National Solar Observatory/Tucson T/Magnetograms in the Mgl 818 cm-1 Solar Emission •••• McMath Main 0.00 0.00 2.00 18.00

1222 487 C Rinsland, NASA Langley Research Center T/Monitoring of Long Term Trends in Concentrations of Atmos McMath FTS Lab 4.00 10.00 4.00 10.00 Executed Proposals 10/01/87 - 12/31/87 Page 5 Tue Jan 26 12:44:22 1988

Nights Hours Days Hours 1269 487 * S Koutchmy, National Solar Observatory/Sac Peak S/H023-Polar Faculae Hilltop Dome/SP 0.00 0.00 6.00 54.00

1310 487 S Koutchmy, National Solar Observatory/Sac Peak S/T291-Measurements of Small Scale Magnetic Fields and ... VT 0.00 0.00 10.00 57.00

1149 487 W Livingston, National Solar Observatory/Tucson T/Solar Irrandiance Line Bisectors McMath Main 0.00 0.00 1.00 8.00

1209 487 W Livingston, National Solar Observatory/Tucson T/Spectrum Irradiance Variability of Sun McMath East 0.00 0.00 3.00 28.00

5877 487 >, Edinboro University of PJ ravitational Redshift McMath Main 0.00 0.00 3.00 14.00

1135 487 P Mcintosh, National Oceanic & Atmospheric Admin., Boulder S/H001-NOAA Monitoring Program Evans Solar Facility/SP 0.00 0.00 91.00 135.00

1211 487 W Mitchell, Jr., Ohio State University T/Changes in Solar Flux Fraunhofer Spectrum from Solar ••• McMath FTS Lab 3.00 5.50 3.00 5.50

1136 487 H Neckel, Hamburger Sternwarte T/FTS Spectra McMath Main 0.00 0.00 5.00 5.00 Executed Proposals 10/01/87 - 12/31/87 Page 7 Tue Jan 26 12:44:22 1988

Nights Hours Days Hours 1123 487 S Saar, Harvard-Smithsonian Center for Astrophysics T/Synoptic Observations of Stellar Magnetic Fields on ... McMath Main 21.00 135.50 0.00 0.00

1057 487 S Saar, Harvard-Smithsonian Center for Astrophysics T/A Survey of Magnetic Fields on Late Type Stars McMath Main 3.00 20.00 0.00 0.00

1253 487 C Schrijver, Observatory S/B193 - Cak Spectroheliograms Evans Solar Facility/SP 0.00 0.00 27.00 37.00

1251 487 E Seykora, East Carolina University S/B191 Investigation of Very Low Contrast White Solar .... Evans Solar Facility/SP 0.00 0.00 38.00 69.00

1027 487 E Seykora, East Carolina University S/B113-Differential Photometry Limb Darkening Evans Solar Facility/SP 0.00 0.00 1.00 8.00

1131 487 E Seykora, East Carolina University S/B174-Ca K, H\ (*a Spectroheliograms Evans Solar Facility/SP 0.00 0.00 15.00 13.00

1282 487 G Simon, USAFGL S/T286-Chromospheric Structures & Photospheric Magnetic... VT 0.00 0.00 4.00 18.00

1337 487 R Smartt, National Solar Observatory/Sac Peak S/B214-Line Profield analysis in Coronal Enhancement Evans Solar Facility/SP 0.00 0.00 8.00 19.00 Executed Proposals 10/01/87 - 12/31/87 Page 8 Tue Jan 26 12:44:22 1988

Nights Hours Days Hours 1263 487 M Smith, National Optical Astronomy Observatories T/Nonradial Pulsation/Outburst Interactions in Lambda Erid McMath Main 34.00 117.50 0.00 0.00

1295 487 M Smith, National Optical Astronomy Observatories T/Spectroscopic Search for Non-radial Pulsations in McMath Main 6.00 53.50 0.00 0.00

1209 487 M Steffen, Kiel University T/Spectrum Irrandiance Variability of Sun McMath West 0.00 0.00 1.00 3.00

1347 487 G Stellmacher, Institut d'Astrophysique de Paris S/T297-Effectivce Temperature in Sunspots VT 0.00 0.00 16.00 78.00

1044 487 R Toth, Jet Propulsion Laboratory T/Laboratory Spectroscopy/Support of Atmospheric Remote See McMath FTS Lab 3.00 26.00 3.00 26.00

1209 487 L Wallace, Kitt Peak National Observatory T/Spectrum Irradiance Variability of Sun McMath Main 0.00 0.00 6.00 41.00

1264 487 H Wang, California Institute of Technology T/Relation between Super Granual Velocity & .... Solar Vacuum 0.00 0.00 2.00 17.00

1267 487 D Webb, ASE, Inc. S/B203-Small Scale Structure/Bright Point Rocket Coll. Evans Solar Facility/SP 0.00 0.00 1.00 1.00 Executed Proposals 10/01/87 - 12/31/87 Page 9 Tue Jan 26 12:4.4:22 1988

Nights Hours Days Hours 1210 487 0 White, High Altitude Observatory T/Sun as a Star: Ca II Profile Measurements McMath Main 0.00 0.00 3.00 21.00

5883 487 E Worden, Lawrence Livermore Laboratory T/Measurement of Frequencies & Intensities of Emission McMath FTS Lab 3.00 8.00 3.00 8.00

1024 487 S Worden, OSUDRE/ADEW S/B044-Solar Rotation 3898-3954A Evans Solar Facility/SP 0.00 0.00 90.00 219.00

1081 487 H Yoshimura, University of Tokyo S/H017-Birth&Evolution of Sunspots Hilltop Dome/SP 0.00 0.00 6.00 33.00

1268 487 J Zirker, National Solar Observatory/Sac Peak S/B204-Coronal Hole Line Profiles Evans Solar Facility/SP 0.00 0.00 15.00 22.00

APPENDIX C

NOAO Annual Safety Report

The following is a summary of recordable occupational injuries for the KPNO, SPO and Tucson sites, as reported on the OSHA 200 log. As required, the respective data will be posted at each site by February 1, 1988.

KPNO SPO Tucson Total

Deaths 0 0 0 0

Injuries involving days off or days of restricted work activity or both 3 2 0 5

Injury involving days off 3 2 0 5

Days off from work 12 42 0 54

Days of restricted work activity 0 40 0 40

Injuries without lost workdays 3 1 4 8

There were no occupational illnesses recorded at either site.

CTIO Recordable Occupational Injuries: January - December 1987

Jan/Mar Apr/Jun Jul/Sep Oct/Dec

Deaths 0 0 0 0

Injuries involving days off or days of restricted work activities or both 0 0 2 0

Injury involving days off 0 0 2 0

Days off from work 0 0 41 0

Days of restricted work activity 0 0 0 0

Injuries without lost workdays 4 9 12 1

There were no occupational illnesses recorded at CTIO.