National Optical Astronomy Observatories

National Optical Astronomy Observatories

Quarterly Report

October - December 1990

TABLE OF CONTENTS

I. INTRODUCTION 1

II. SCIENTIFIC HIGHLIGHTS 1

A. Cosmis Voids 1 B. Chiron 2 C. Surface Dynamics 2 D. South Pole Observations 3 E. Effect of Active Regions on Intermediate-Degree Solar Oscillations 3 F. Resolved Images of High Redshift QSOs: A First Look 4 G. Astrophysical Jets: More Robust than Previously Thought? 4 H. Sub-Arcsecond Structure of R Aquarii: An Accretion Disk Revealed 5

III. PERSONNEL 6

A. Visiting Scientists 6 B. New Hires 6 C. Terminations 6 D. Change in Status 6

IV. INSTRUMENTATION, NEW PROJECTS, AND OBSERVATORY ACTIVITIES . . 7

A. 8-M Project 7 B. Advanced Optical Telescope Technology Program (AOTT) 8 C. Global Oscillation Network Group (GONG) 9 D. WIYN Project 10 E. Instrumentation Projects 11 F. Observatory Activities 16

V. PROGRAM SUPPORT 17

A. Director's Office 17 B. Central Administrative Services 19 C. Central Computer Services 19 D. Central Facilities Operations 20 E. Engineering and Technical Services 21 F. Publications and Information Resources 21

Appendices

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

I. INTRODUCTION

This quarterly report covers scientific highlights for the period of October through December 1990, as well as personnel changes for the period. The report also discusses progress on the 8-m telescopes, GONG, WIYN, and instrumentation projects. The appendices list telescope usage statistics and observational programs.

II. SCIENTIFIC HIGHLIGHTS

A. Cosmic Voids

The observed smoothness of the cosmic background radiation leads one to expect that at a sufficiently large scale the universe should be homogenous. To test this expectation the space distribution of galaxies must be determined over the largest possible sky areas and, if redshifts are used as distance indicators, they must be determined for the faintest possible galaxies. However, properly done, this is such an enormous task that available surveys have been necessarily limited to finite sky areas and to galaxies brighter than convenient limits. A prime example is the on-going survey being carried out by Harvard Smithsonian Center for Astrophysics (CfA) astronomers J.P. Huchra, M. Geller, and collaborators. In this survey, galaxies brighter than about magnitude 15.5 are surveyed in sky areas consisting of strips a few degrees wide in declination but extending over a wide range of right ascension. This survey has shown extensive sheet-like concentrations of galaxies including the so- called "Great Wall." Since the sky strips are not necessarily contiguous and only relatively bright galaxies are observed, the CfA survey is not ideal for the study of what appears to be extensive voids surrounded by concentrations of galaxies. A survey adapted to the study of possible voids was undertaken by R.P. Kirshner (Harvard U.), A. Oemler (Yale U.), P.L. Schechter (Massachusetts Inst, of Tech.), and S.A. Shectman (Carnegie Obs.). Galaxies brighter than about magnitude 17 located within a set of small sample regions near the galactic north pole were included. The extremely large number of galaxies in the extensive sky area that had to be surveyed in order to delineate a possible void, made it necessary to limit the study to such sample regions. Observations obtained in 1987 with the Palomar 5-m telescope and with the KPNO 4-m telescope resulted in the finding of an apparent void toward the constellation of Bootes. With a 106 Mpc3 volume, the so-called Bootes void is a statistically significant low density region for normal galaxies.

A similar survey has now been completed in the southern hemisphere. With spectroscopic observations obtained with the Las Campanas 2.5-m telescope and photometric observations obtained with the CTIO 1.5-m telescope, Kirshner, Oemler, Schechter, and Shectman have found evidence of a possible void toward the constellation of Phoenix. This survey included 150 galaxies brighter than magnitude 17.6. Again, numerous sample regions were selected. These spread over a 25 degree diameter area. The observed galaxies show a significant low density region between redshifts 11,600 and 15,400 km/sec. The apparent Phoenix void is, however, not as clearly defined as the one in Bo5tes.

A search for the galaxies that might have been missed in the 25 degree area covered by the sample region shows, at a redshift of 14,500 km/sec, a clustering of galaxies. Also, three compact bright galaxies within the region have radial velocities that place them within the suspected void. Independent surveys by other investigators show that additional galaxies, near the periphery of the apparent low-density region, have radial velocities within the range mentioned earlier. Prudently, Kirshner, Oemler, Schechter, and Shectman consider the possibility that the Phoenix "void" may be spurious, but conclude that it probably is an underdense region. So far, existing surveys of distant galaxies show no evidence of homogeneity in the universe. The smoothness of the cosmic background radiation remains a challenging fact for observational cosmologists.

B. Chiron

In February 1988, when observing at Mauna Kea, astronomers D.J. Tholen, W.K. Hartmann, and D.P. Cruikshank (U. of Hawaii) found that asteroid No. 2060 (Chiron) was 0.7 magnitudes brighter than expected from predictions based on its position in space and its well-known rotational brightness variations. Chiron's bright outburst was found to persist past 31 October when Lowell Observatory astronomers S.J. Bus and E. Boswell, in collaboration with L. French (Massachusetts Inst, of Tech.), observed it with the CTIO 0.9-m telescope. On this occasion, Chiron's rotational light variations showed an unexpected decrease in amplitude. As it turned out, this was the first indication that Chiron was surrounded by a coma.

Chiron's orbit with a semi-major axis of 13.7 A.U. places it, even at perihelion, well beyond Jupiter: far away from the asteroid belt. This unique orbit for an asteroid caused numerous speculations about Chiron's origin. Was it perhaps an escaped satellite from one of the outer major planets, or possibly a comet captured by the gravitational attraction of those planets? At first, Chiron's brightness outburst resembled frequently observed episodic cometary activity at large heliocentric distances. This led astronomer K. Meech (U. of Hawaii) to include Chiron in a program of comet observations to be carried out at CTIO in collaboration with KPNO astronomer M. Belton. An aim of the program was to search for a coma surrounding Chiron. Formation of a comet-like coma as Chiron approaches its perihelion could explain its unusual brightness outburst. Observations were made in January 1989 with the CTIO 0.9-m telescope and continued in April 1989 with the KPNO 4-m telescope. On 10 April a 5 arcsec coma surrounding Chiron was detected in KPNO direct CCD images. By its reflectivity, the coma could explain the brightness outburst and why its rotational light variations had been partly masked during the earlier CTIO observations.

Further analysis of the observations suggests that the coma is caused by dust particles gravitationally bound to Chiron rather than ejected into space, as in comets. This would explain why its brightness outburst has lasted much longer than those typical of comets. Drs. Meech and Belton suggest that the dust particles may be thrown outward by gas escaping from regions of activity on Chiron's surface. Although its origin remains unknown, Chiron certainly will be carefully monitored as it approaches its 1996 perihelion.

C. Surface Dynamics

G. Simon, A. Title (Lockheed), and N. Weiss (U. of Cambridge), have been working on the modeling of mesogranules and exploders on the solar surface. Correlation tracking of high-resolution observations reveals a horizontal flow field containing both the supergranulation pattern and a much smaller pattern corresponding to mesogranulation. Exploding granules (exploders) occur preferentially near the centers of mesogranules. This raises the question, Are mesogranules just collections of exploders? Radial outflow in exploders and mesogranules can be modeled by superposing gaussian source functions. Simon, Title, and Weiss use this model to explore the relationship between mesogranules and exploders. Although they demonstrate that there is mathematical equivalence between mesogranules and exploders distributed normally about the mesogranules center, their results indicate that the observed mesogranular velocity pattern is not consistent with a flow pattern generated by exploders dropped randomly on the solar surface. Detailed comparison with observations suggests that the averaged mesogranular velocity is produced by a combination of a persistent outflow from a source together with exploders distributed randomly about its center. Similar analysis shows that supergranules are not the result of random occurrences of mesogranules.

D. South Pole Observations

The high-degree helioseismometer was shipped to the South Pole in mid-September with the goal of obtaining observations of solar oscillations uninterrupted by the day-night cycle. A field party consisting of T. Duvall (NASA), J. Harvey, S. Jefferies (Bartol), D. Neff, and M. Pomerantz (Bartol) departed from the United States on 22 October and arrived at the South Pole on 31 October. Since the camera system has 2 arcsec pixels, they were particularly interested in getting observations of high-degree oscillations at a time of high solar activity. The polar solar observatory site was activated in early November and, after the equipment arrived, the instrument was set up. An initial problem with the high speed guider was located and fixed. First observations were made on 9 November. After a few days of observing, the weather became cloudy and unusually windy. Two storms produced massive snow drifts around the instrument. However, starting on 23 November relatively good weather prevailed for two weeks and a large amount of data was obtained. Measurements of seeing quality were also obtained during this period. It was confirmed that daytime seeing at the South Pole can be quite good. Team members Duvall, Harvey, Jefferies, and Pomerantz returned to the United States at various times from 25 November to 11 December leaving D. Neff to run the instrument alone until the arrival of R. Aikens (Photometries, Ltd.) on 29 December. The weather was poor during Neffs solo and an electronic problem developed that he was able to repair. About 30 Exabyte data tapes have been returned to Tucson. Each tape contains one day of data in compressed form, which represents about 3 gigabytes when uncompressed. Calibrations and a few images have been read from the tapes with good results. Duvall has prepared a reduction pipeline to reduce the enormous set of data. He is investigating a new method of suppressing low temporal frequency noise and signals in an effort to speed-up the pipeline. Harvey is studying the details of the calibration images to ensure that the early stages of the pipeline are done properly.

E. Effect of Active Regions on Intermediate-Degree Solar Oscillations

In collaboration with D. Haber (Colorado College), Hill has simulated the effects of active regions on intermediate-degree solar oscillations. The simulation was performed by masking quiet-sun data and comparing the power spectra of the original data and the masked data. The masks were created by digitizing an Ha photograph of the Sun when four large active regions were present on the disk. Within these regions, the observed velocities in the quiet-sun data were attenuated by a random number with a mean of 0.7, simulating the known suppression of the oscillatory velocities within active regions. Comparison of the quiet and "active" power spectra showed that the power of the global intermediate-degree oscillations was reduced by up to 25%, in agreement with observations. The spectral line shapes of the oscillations did not change substantially, suggesting that frequencies measured from the "active" spectra will not be substantially altered. However, helioseismology requires high precision measurements of the oscillation frequencies. There may be small, yet significant, shifts caused by the presence of active regions. The next steps are to measure the frequencies from the quiet and "active" spectra, to vary the simulated active region parameters and investigate the changes in the frequencies, and to attempt the development of a deconvolution method based on the spectrum of the active region. F. Resolved Images of High Redshift QSOs: A First Look

Soon after their discovery, quasi-stellar objects were so named because their optical images were unresolved and stellar in appearance. These objects have become familiar over the years, but in many ways they remain as enigmatic as ever. They form the class of the most distant objects in the Universe, and they also produce the most energetic and explosive events ever seen. These two properties make an understanding of their nature essential to cosmology, to general relativity, and to high energy physics. Until recently the only spatially resolved features associated with QSOs were the regions of extended radio emission associated with a subset of these objects, and these radio features were remarkably similar in nature to the less powerful radio emission arising from some elliptical galaxies. This similarity provided a tantalizing possible link between galaxies and QSOs, but their pointlike optical appearance seemed to preclude QSOs from being a special form of galaxy.

This situation has now changed, largely due to the remarkable increase in sensitivity provided by state of the art detectors used at the KPNO telescopes. Using the KPNO 4-m telescope and a UV flooded 800 x 800 pixel CCD detector at the prime focus, T. Heckman (Johns Hopkins U.) M. Lehnert (Johns Hopkins U.), W. van Breugel (LLL), and G. Miley (Leiden) have obtained spatially resolved images of 15 QSOs, all lying at redshifts greater than or equal to 2.0. The resolved images are all seen in Lyman alpha emission, with a typical size of 100 kpc and a typical luminosity of 1044 ergs/sec. All of these QSOs are associated with radio emission. The optical nebulae are usually asymmetric or elongated; the axis of elongation is aligned with the radio emission. In this regard, these objects are very similar to the population of high redshift radio galaxies that have been discovered recently. Photoionization arguments suggest that the emission arises from small dense clouds, and the production and confinement of such clouds implies a gas cloud around the QSOs which contains up to 101 solar masses of gas. In six of the QSOs, the UV continuum is also resolved, with diameters of 40 to 80 kpc. This UV emission could arise from starlight in a host galaxy or from scattered QSO light Although the mechanism that gives rise to the QSO emission may be unique and still obscure, these observations strongly suggest that the underlying parent object may be a system of stars. In turn, this provides very strong boundary conditions on models for the "central engine" in QSOs, since they must evolve out of a gravitationally bound stellar system.

G. Astrophysical Jets: More Robust than Previously Thought?

Jetlike structures are observed in astronomy over scales which span seven orders of magnitude, from the line emitting jets emanating from young stellar objects at a few hundred kilometers per second to the immense megaparsec scale radio jets associated with wide-angle tail radio galaxies in clusters. These latter jets are the largest single objects yet seen in the Universe. While of interest in themselves, an understanding of the characteristics of the jets (i.e., density and velocity) would provide invaluable boundary conditions on the energy output from the nucleus of the galaxy or QSO. These constraints then determine which models of the nucleus are viable. Knowledge of the jet character can come from an understanding of the interaction of the jet with its surroundings, provided that the nature of those surroundings is known. This approach has been used to study the nature of jets seen in the hot intracluster medium around galaxies, where the jets are smoothly bent, and of jets with sudden bends and hot spots, where they are supposed to have encountered dense clouds.

Recent results suggest that the rough estimates of jet parameters so obtained in the past may need to be changed by factors of 10 or more. In a series of three-dimensional time dependent numerical simulations, D. De Young (KPNO) has modeled the off axis encounter of jets with dense clouds as well as the interaction of jets with the intracluster medium. One basic result is that jets cannot easily be deflected by dense clouds in a coherent way, contrary to earlier speculations. Instead, a jet is essentially stopped by a cloud for a brief period, after which time the shock heating and continuous momentum transfer by the jet destroys the cloud, allowing the jet to resume propagation in the original direction. Coherent deflection for over 107 years, necessary to explain the observed radio morphology, requires clouds as massive as dwarf galaxies. Such objects are not seen in and around such deflected jets. On the other hand, the calculations show that jets associated with galaxies moving through an intracluster medium are much more easily deflected than estimated. Earlier estimates ignored the transfer of momentum from the jet to the ambient medium and the resultant jet deceleration. Recent results show jet density or velocity estimates to be in error by factors of 10, and agreement with observations can be obtained if the total energy flux of the jets is increased accordingly. This in turn places even greater requirements on the energy output of the nuclear machine which creates the jets.

H. Sub-Arcsecond Structure of R Aquarii: An Accretion Disk Revealed

Accretion disks have been hypothesized as attendant structures around many astronomical objects, from young stars to galactic nuclei to quasars. They have been used to collimate bipolar outflows and possibly jets, to provide a source of fuel for active galactic nuclei, and to act as the birthplace for planetary systems. Although accretion disks have never been directiy observed, spectral signatures that could be produced by such disks have been seen. The interpretation of these observations is still somewhat ambiguous, and it would be reassuring to obtain direct images of an accretion disk.

This goal may have been attained recently. Using the Steward Observatory speckle camera on the KPNO 4-m telescope, K. Hege, C. Allen, and W.J. Cocke (all at U. of Arizona) have obtained H-alpha images of R Aqr with a resolution of 45 milliarcsec. They find a bright H-alpha source clearly separated by 0'.'124 from the long period variable star, together with a smaller emission feature even further from the primary star. These observations clearly detect a binary system, and the images obtained strongly suggest that the bright H-alpha component arises from an accretion disk which surrounds a hot companion in orbit around the long period variable star. If so, these are the first ground based observations of an accretion disk, and this object is clearly a candidate for further study from space. ffl. PERSONNEL

A. Visiting Scientists

The following visitors arrived at NOAO facilities for periods of one month or more during the 1 October - 31 December 1990 quarter. date NOAO facility arrived name institution visited

10/1/90 Pat Hall University of Arizona, Tucson 8-M 10/10/90 Luca Bertello University of Florence, Italy NSO/Sac Peak 10/15/90 Craig Wheeler University of Texas, Austin KPNO 10/29/90 Luigi Smaldone University of Naples, Italy NSO/Sac Peak 11/15/90 Ruth Peterson University of Arizona KPNO 11/23/90 Ying Wang Urumqi Astronomical Observatory, China NSO/Tucson 11/30/90 Marcos Diaz Universidad de Sao Paulo, Brazil CTIO

B. New Hires

The table below shows details of new appointments made to NOAO during the 1 October - 31 December 1990 quarter. date of appointment name position NOAO division

10/1/90 Greg Kopp Research Associate KPNO 11/14/90 David Silva Research Associate KPNO 12/3/90 Dan Blanco Senior Engineer WIYN 12/13/90 Dick Fredericksen Engineering Programmer KPNO

C. Terminations

date name position NOAO division

10/12/90 John Fox Engineer NOAO 11/30/90 John Africano Manager, Telescope Support KPNO

D. Change in Status date name position NOAO division

10/1/90 Mark Phillips Astronomer/Tenure to Assistant Director, CTIO CTIO 11/16/90 Nicolas Roddier Assistant Engineer to Engineer NOAO

IV. INSTRUMENTATION, NEW PROJECTS AND OBSERVATORY ACTIVITIES

A. 8-M Project

U.K. 10 join partnership. The Science and Engineering Research Council of the U.K. voted at its 19 December meeting to join with the U.S. and Canada to build two 8-m telescopes. Although the SERC will not provide funding immediately, it is committing to a 25% participation in the project, consistent with the original plan for the U.S. to have a 50% share and Canada and the U.K. 25% each. We were delighted with the outcome, as the U.K. had been considering a European option as well. We believe that ihe U.K. decision is a crucial step that will lead soon to an agreement by all three countries to establish the partnership. The Canadians are continuing to make progress on the project within their own funding system.

Project funding. The FY 1991 budget contains $4M for initial work on the 8-m project. The money will be used to hire project staff, provide space and equipment, begin design work, and purchase material for the first mirror blank.

Search for project manager. Recruitment for the project manager, a key position in getting the project staned, began last September. More than 100 applications were received and reviewed. Following telephone interviews with the 11 most highly ranked applicants, four candidates were invited to Tucson in December. The candidates will be interviewed in Washington, D.C., by a committee with representatives from AURA, NOAO, NSF, Canada, and the U.K. We expect to be able to make an offer by the end of January and hope to have the person on board within two months.

Building space. The principal 8-m project office will be located in Tucson and will build up to a staff of about 30 people. Space for the staff is not available in the NOAO buildings. After consideration of various alternatives, plans are being made to locate modular buildings on the roof of the East wing. We believe this offers the best combination of proximity to ongoing activities, least impact on parking spaces, and suitable working conditions. The East wing had been designed for additional stories in the future and therefore provides the structural base and access to utilities needed for the modular buildings. Stairs to the roof already exist. The view will certainly be better than from the parking lot by the engineering wing!

Science Advisory Committee. An ad-hoc Science Advisory Committee met in Oxford in November to work on the Science Requirements Document for the 8-m project. This will be the basic document from which the project team will produce the telescope design. P. Osmer, R. Green, F. Gillett, and R. Schommer represented NOAO. Drafts of this document have been circulating for comment among NOAO staff. The updated version from the Oxford meeting will be coming out soon and will also be circulated for comments.

The project scientists and other scientists will meet in Tucson on 28 January to work on the document, which needs to be finished by the time the project manager arrives.

International Steering Committee. Representatives from all three countries will meet in Tucson at NOAO on 29 and 30 January. The International Steering Committee is serving as the management board for the project until such Board is established by the signing of an agreement by all three countries. A main agenda topic for the meeting will be the draft Memorandum of Understanding that is now in its second version. The intention is to have the three countries sign the MOU early in 1991; then more detailed plans will be drawn up for the partnership.

The meeting will also discuss the work planned for the project in its early phases.

B. Advanced Optical Telescope Technology Program (AOTT)

8-m Telescope Design Studies. Optical design of IR instruments for the 8-m telescopes has continued. Efforts have focused on evaluating the feasibility of high resolution imaging in the near infrared, and on evaluating the effect of the choice of secondary f/ratio on the performance of the instruments.

NOAO and Dominion Astrophysical Observatory collaborated in writing a statement of work for a study of 8-m telescope pier and foundation designs. The contract for this study has been awarded to KPA Engineering Ltd., a Canadian engineering firm.

3.5-m Mirror Project. The 3.5-m mirror was shipped to Kitt Peak on 3 October. During the first week of December the mirror was aluminized in the 4-m coating chamber. The resulting coating is quite satisfactory.

The main weldment of the mirror cell arrived on 16 October. It was fabricated by L & F Industries, and despite its size (14 feet across) and weight (7700 pounds), it is a precisely machined structure. Heavy steel legs have been fabricated to support the mirror cell on the 4-m polishing machine table for testing.

During this quarter, much effort has gone into preparing the components of the mirror cell assembly. These include thermal sensors, blowers, air plenums, heat exchangers and piping for the thermal control system, support mechanisms, hydraulic tubing, cabling, junction boxes, position sensors and fluid level control units for the mirror support system, earthquake pads, position-defining linkages, and removable access panels.

Design of a water chiller that uses thermal electric coolers to control the temperature of the water supplied to the mirror cell was completed. Heat exchanger plates for this chiller are being fabricated by an outside shop on a CNC milling machine.

Testing of manufactured prototypes of the circuit boards that will control the active optics system were performed. A noise problem in the A-to-D converter circuitry required a slight change in the circuit board design. Tests of the second generation prototype boards were successful, and the full quantity of 70+ boards is currently being fabricated by an outside shop.

Hot and cold temperature testing of one of the axial support mechanisms was successfully completed. Active optics components were exercised repeatedly at both cold and hot temperatures without problems.

A new Hartmann screen was designed for testing the 3.5-m mirror. C. Global Oscillation Network Group (GONG)

The Global Oscillation Network Group (GONG) is a community-based project to conduct a detailed study of solar internal structure and dynamics using helioseismology. In order to exploit this new technique, GONG 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 the measurements.

There has been much activity this quarter concerning the selection of the sites for the GONG Network. A panel has been appointed to oversee and review the selection process. This process will culminate in the announcement of the sites at the upcoming annual GONG meeting in April. The membership of the panel is as follows: T. Stebbins (JILA, U. Colorado, Boulder); J. Peterson (U.S. Geological Survey, Albuquerque); E. Nather (U. Texas, Austin); J. Kennedy (GONG); H. Jones (NASA/GSFC); T. Hoeksema (Stanford); and F. Hill (GONG). The panel met via teleconference on 17 December, during which they were briefed on some of the more intangible aspects of the selection. A variety of scoring and weighting schemes for ranking the networks was discussed. The panel will meet in Tucson on 4 and 5 February, to finalize the recommendation and to prepare a draft report for the selection announcement.

The method of computing the scores is itself an interesting question. An infinite number of scoring and weighting schemes can be devised, but which is the most "reliable?" A statistical technique known as Principal ComponentAnalysis is being investigated. This technique first computes the cross-correlations among many realizations of a set of measures. The eigenvalues and vectors of the matrix of cross-correlations are then calculated, and the vector components corresponding to the largest eigenvalues are used as weights in computing scores for the networks. This technique is quite promising, and allows the evaluation of the relative weights of the measures. It is expected that this technique, or something similar, will be used to make the final ranking of the networks.

In mid-October, the data reduction and analysis group began the downstream processing of three days of Mount Wilson magneto-optical Dopplergrams that were graciously provided by E. Rhodes. The processing began with registered, calibrated, velocity images, data similar to what NSO may receive as part of NASA's Solar Oscillations Investigation. The objective of this exercise was to obtain experience with 10242 images. They are 16 times larger than the GONG images previously processed. Since this was the first attempt at processing 10242 images, numerous software problems and a few computer resource problems were expected. It was surprising to discover that these data cannot be processed (using any reasonable definition of the word) on GONG workstations. MIPS and MFLOPS appeared to be sufficient, but memory capacity, disk capacity, disk I/O rates, and Exabyte I/O rates are clearly not adequate. This can be remedied by newer workstations with more memory and disk space.

During the past three months, the instrument team has shifted its emphasis away from instrument verification to purely engineering aspects of the development. Every major component of the Doppler analyzer has been removed from the optical table at the prototype site and returned to the shops. There they have been undergoing stand-alone testing and a variety of other upgrades. The Lyot filter oven has been taken out of service to replace the old Zeiss elements with the new temperature- compensated ENRAD crystals built to GONG's specifications. The calibration assembly has had new elements added to it and is undergoing extensive testing and balancing. Even the electronics racks have been stripped clean to facilitate testing and upgrading of many of the cards that were in service last summer. At this writing, these activities are near completion. With the long clear days of the spring season just ahead, attention is beginning to shift back to solar data collection.

INRAD has now delivered all the crystals for ten Lyot filters. This will meet the needs of the prototype, equip all six field stations, and leave three complete sets of spares. Although the most recent shipment has not yet been acceptance tested, virtually all the elements tested so far are within project specifications. One of the narrow-band filter elements has been assembled and tested and the results are very good. The wide-field requirements were met as evidenced by a maximum 0.03-A wavelength shift across the 2 degree field of this, the thickest element. The ADP crystals are doing their job as well; the thermal coefficient of the assembled element was measured to be -0.0103 A/C. This represents a factor of 40 improvement over calcite alone. The uniformity of birefringence is ±0.01 wave over the central 85% of the crystal dimension, and the fringe contrast is about 200:1. The isochromatic fringes in the wide-field pattern appear almost perfectly round. No special attention was paid to orienting the individual crystals beyond just indexing to the manufacturers flat sides. This result further confirms INRAD's ability to orient and cut the crystals properly.

D. WIYN Project

Enclosure design studies. M3 Engineering in Tucson, has been contracted for the architectural design and engineering of the WIYN enclosure and control building. A kick-off meeting with M3 was held at NOAO on 4 December. The proposed "octagon" conceptual design for the enclosure developed by the WIYN Project was discussed. M3 is now developing the design.

WIYN site. A survey of the site was performed to determine contours and locate existing buildings, roads, and utilities at the WIYN site. The results of the survey were provided to M3 as input for the building design. Soils tests will be scheduled once the building footprints and locations are determined.

Secondary mirror design studies. L. Goble and M. Johns visited a number of optics companies in October to discuss mirror blanks and methods for fabrication and testing of convex secondary mirrors. Designs have been produced for several lightweighted mirrors with core geometries optimized for the various fabrication methods currently available. These are being provided to the manufacturers for evaluation of technical feasibility and estimates of costs and delivery times. A similar process has also been started for the tertiary mirror.

Primary mirror progress. Good progress is being made on the 3.5-m primary mirror system under the direction of L. Stepp. The primary mirror has been polished to a sphere and was shipped to Kitt Peak on 3 October for aluminization. A successful coating was achieved on the first attempt. The main weldment for the primary mirror cell was received from L&F Industries in October. Activity for the latter part of the quarter centered around preparing the cell, mirror supports, and thermal controls for assembly. The plan is to install the primary mirror in the assembled cell early in 1991 and commence approximately six months of testing of the supports and thermal controls. At the conclusion of the tests, the mirror will be re-generated and polished to the hyperboloid required in the Ritchey-Chretien optical design of the WIYN telescope.

10 Telescope mount L&F Industries has been contracted for a second round of preliminary design studies to concentrate on various subsystems of the telescope. The first will look at options and produce a preliminary design for the azimuth and altitude drives.

New staff. D. Blanco, previously with the Multiple Mirror Telescope, has joined WIYN as lead mechanical engineer on the project. G. Duffek, already part of the NOAO engineering staff, is moving to WIYN to work on the mechanical design. Recruitment is still underway for a controls engineer.

Other activity. WIYN is now official. The agreement establishing the WIYN consortium was accepted at the October meeting of the interim board. A corporation named the WIYN Consortium, Inc., was established shortly thereafter to manage the affairs of the consortium, principally the construction of the WIYN 3.5-m Observatory. The management organization of the corporation was substantially completed during the quarter. A board was duly constituted and corporation bylaws adopted. Incorporation papers and tax forms were filed with the appropriate authorities. WIYN has contracted with NOAO for the financial management of the corporation. An accounting system to manage the income, expenses, liabilities and assets of the corporation was established under the direction of G. Blevins and has been reviewed by outside auditors. Arrangements were also made for liability, property loss, and directors and officers insurance.

E. Instrumentation Projects

KPNO During the October-December 1990 quarter, the Telescope Allocation Committee met to review the 236 telescope proposals received for observing at Kitt Peak in the Spring 1991 semester. The number of proposals received was 8% smaller than the previous Spring semester. However, there is one less telescope on Kitt Peak with the merger of the 0.9-m telescopes.

A major effort continued in this period to complete the Gold Guider upgrade at the 0.9-m telescope. The project is on schedule and should be completed by the middle of February. This project is a carryover from last year of the #1 and #2 0.9-m telescopes merger.

Most of the parts for the new CCD universal dewars have been completed by the subcontractor and received by KPNO. A number of detail parts still have not been completed by the vendor due to material shortages and manufacturing problems. Two dewar tanks have been completed and leak tested, and one of the tanks has already been pressed into service as a replacement part for a failed tank in an existing dewar.

At the 2.1-m telescope, dome truck realignment work was started and is still in progress. This project was undertaken in order to reduce the high maintenance effort required on the truck guide rollers and to reduce the drive motor current loadings.

At the Vacuum Telescope, the #1 and #2 mirrors were realuminized and the vacuum tank entrance window was cleaned. A new azimuth drive gear box for the #2 mirror mount was also installed.

At the McMath Telescope, the fabrication and installation of a redesigned control chassis for the FTS servo was completed.

11 A new office was built in the maintenance area for the Assistant Mountain Manager. The reason for the change was to provide a more suitable geographical location for coordinating the work between the various facility support groups.

In December, one of the new Intensified Lens-coupled System (DLS) TV cameras was installed in place of the aging south image-dissector tube (IDT) guider at the 4-m. The chief advantage of this new camera is that the limiting magnitude for guiding is approximately two magnitudes fainter than with the old IDT system. The increased efficiency in finding guide stars should contribute directly to making better use of the observing time at the 4-m. A temporary disadvantage of the ILS camera is that it is not yet able to autoguide at non-orthogonal slit position angles, such as is needed for long-slit spectroscopy on galaxies. This will be corrected by a future edition of the telescope control software program. Two of these guider-cameras are now in operation on the mountain. The other one is in use at the 0.9-m.

At the NSO telescopes, code is being developed for the spectromagnetograph so that data acquisition can proceed in parallel with the EUCLID processor which does real-time flat-field corrections. The user interface was improved with the addition of the capability to select regions on the sun by specification of heliocentric coordinates and epoch. Magnetograms can now be displayed both in black and white, and in pseudocolor. At the main spectrograph, the MULTI program can now accept control signals from an optical scanning device.

Regarding IR software, along with the usual microcode changes and other laboratory and mountain support work, considerable progress was made on the Fast IR Electronics (FIRE) project. With the basic design done and the detailed design mostly completed, actual coding has started. Two part-time programmers were hired to help the project meet its fall operation date. Of the 20 major subsections, three have been written, and the project appears on schedule.

After more work on the Fiborg collision software for the fiber positioner for optical spectroscopy, the routines now appear to be solid. New code was written to support additional modes of operation of the Compumotor servos, including more detailed diagnostics. Flexure and graphics routines have been refined, and the astrometry calculations now give the expected results.

Optical & Ultraviolet Program CCD Development. The hardware to run the CCD controller/data acquisition system with the Steward software under the IRAF environment has been built and tested.

The 3rd TEK 1024 CCD was delivered and sent directly to CTIO without testing.

A dewar and associated electronics for operation of a Metachrome II-coated STIS 2048 CCD were prepared. This device is on permanent loan and adds significantly to KPNO capabilities.

The results from the Ford foundry run have been, in a single word, "outstanding". Preliminary test results indicate a significant yield of the 3K x IK devices. One 3K x IK front-side device has been packaged and tested. First tests indicate good cosmetic quality, < 10 e" rms read noise, almost perfect CTE, and above normal QE (for a frontside device), with all four amplifiers usable. Thinning, packaging and testing will continue.

12 HYDRA. After long delays in procurement, the necessary components arrived for the redesigned dual X-drive stages. Precision-grade twin 24" lead screws were received and sent back to the vendor because they did not meet specifications. Acceptable lead screws were finally delivered in early November, allowing assembly of the new X-drive modules. These drive modules incorporate new low-profile hnear bearing stages. The redesigned Y-stage was assembled with multi-axis flex pivots so motion along the X-axis would not be over-constrained.

The HYDRA rack control electronics were modified to drive the additional X-stage. Mechanical limit switches were installed and fault detection circuitry for the dual drives was interfaced back to the controlling indexer. A method for dealing with potential X-stage misalignments was discussed and arranged. A system using dual rotary encoders to detect axis misalignment errors was designed and construction was initiated.

The upgraded positioner was assembled and aligned prior to the scheduled instrument T&E night at the 4-m telescope in November. The primary accomplishment of this evaluation run was to verify and test the new dual X-drive system. X & Y profiles and flexure effects were measured on the telescope as well. A preliminary flexure model was then incorporated from the data taken. The positioning control system was tested and positioning errors were measured. In December, a position maintenance mode was incorporated into this system to compensate for indexer/drive/encoder feedback problems. This allows for more precise positioning accuracy by constantly monitoring the encoders and compensating for movement overshoot.

Bench Spectrograph. An investigation was made to determine if plans to design and build a rear "blue" module for the Bench Spectrograph Camera (BSC) in FY 1991 should proceed. Performance measurements with the Simmons camera support the conclusion not to proceed with the "blue" module. Progress was made manufacturing the BSC optical components by an outside vendor. Design specifications for the BSC shutter were reviewed.

The preliminary design specifications for the low-level software was finished and released for review. Construction proceeded with the grating hoist and a number of modifications were incorporated into the R-C Sub-Cell (for gratings).

Next Generation CCD Controller. In collaboration with CTIO, the Tucson O/UV group has taken the responsibility for getting the first PC card for the design to a vendor. The various details and interactions about the design were worked out between the Texas-based vendor (CAE/D Systems) and NOAO. The "sequencer" PC card was fully designed from NOAO CAD-generated schematics. A vendor in Arizona (Avanti) was selected to fabricate an initial run of four cards. The completed artwork package was sent to them in December.

With the prototype hardware, the fiber optic link for serial communication between the host Gab) Sun computer's plug-in transputer board and the remote prototype sequencer unit (or controller) was successfully debugged and installed.

Work continued with the checkout and interfacing of the wire-wrapped version of the sequencer card prototype design. Data were taken from the remote sequencer unit over the fiber optic link and stored into the Sun as an IRAF image. These data represented a "bias" reading of the video processor and 16-bit A/D converter, which were clocked by waveforms simulating the readout of a CCD. Programs to derive the waveforms needed to read a CCD were also coded and upgraded using a "micro-code"

13 type of waveform definition language developed at CTIO. There was continued interaction with the CTIO programming group about the functions of the software package being used with the new transputer-based design.

CCD Mosaic. We have been awaiting results of the Ford 3K x IK run prior to plunging into this project. With the encouraging results, we are in the process of putting together a request for bid for another foundry run to provide the device to be used in the Mosaic.

STIS. Three of the 2048s have received the Metachrome II coating. Two of these will go to Goddard and one has been put into routine service at KPNO, as mentioned above. Testing of the STIS IK AR-coated devices has continued on a low priority basis. So far none have been acceptable for use at Kitt Peak.

Infrared Research & Development Program Research and development. Testing continued on 256 x 256 PtSi arrays as the vendor grappled with performance anomalies which are proving quite difficult to solve. The root cause is thought to be known, and individual devices which do not suffer from these anomalies have been fabricated. Fabrication was begun on small parts needed to test an Amber Electronics 128 x 128 pixel InSb array, on loan to NOAO for evaluation.

Cryogenic Echelle. The most significant activity in this quarter was a major change in the optical design concept for this very high resolution (R = 100,000) infrared spectrometer. The original design called for large, steep, very well corrected off-axis reflective elements. Mechanical design and tolerance analysis indicated that maintaining the optical elements in alignment was going to be a very tough design problem.

The proposed new optical design uses a Cassegrain-type collimator/camera. This design uses axially symmetric optics which are known to be straightforward to fabricate commercially. The axial symmetry and other features of the Cassegrain design greatly ease the mechanical design problem. The existing concept for the dewar, using designs and technologies already proven on other instruments, remains unchanged. Compromises in instrumental performance include some loss in slit length and throughput, and some degradation of the modulation transfer function. However, the basic high spectral resolution and high quality imaging capabilities are retained.

Fast Infrared Electronics (FIRE). The second generation fast IR electronics achieved the status of a project. Project engineers developed a schedule, and electronics design and fabrication proceeded largely as planned. A commercial source is being used to fabricate PC cards from the designs; this has proven efficient in both time and cost. The software effort slipped somewhat due to a manpower shortage, which was alleviated at the end of the quarter by approval of a temporary position by the Director.

Cryogenic Optical Bench (COB). The cryogenic optical bench passed a conceptual design review at the end of the quarter. Optical designers provided assistance with slight revisions to the original design and worked out a firm design for the grisms. A revised design for the filter sliders was cryogenically tested with great success.

Simultaneous Quad-Color Infrared Imaging Device (SOUP). The multichannel IR camera was used at the 1.3-m telescope for further technical evaluation and for scientific observing by staff. Achieving a

14 common alignment and focus of the four channels has proven tractable to a high degree, and very good photometric performance was demonstrated. The instrument was disassembled for internal modifications, cleaning, and optical adjustment prior to receiving its final suite of detectors.

Software. The new user software, incorporating an algorithm for dramatically reducing read noise, was telescope tested and proved to have some bugs which are both serious and subtle. Data are occasionally lost to these errors, and a diagnosis is proceeding as manpower is available. Despite the problems, the read noise advantage is so pronounced for use with the cryogenic spectrometer that the code has been regularly used with this instrument.

Facility instruments. Problems with the filter wheel drive in the infrared imager IRIM were solved by polishing the shaft and bearing surfaces, much worn after several years of use. Defective component mounts on the electronics boards used by IRIM and the spectrometer CRSP were identified; these may account for the occasional low level electrical oscillations seen in the output of these instruments. Both instruments continue to be heavily subscribed at several KPNO and NSO telescopes.

NSO

Stellar K-line Filter. Tests of the optical stack revealed an unexpected sidelobe and on-band performance that was outside of the specified operating temperature range. The optical stack for the Stellar K-line Filter was sent to R. Dunn at NSO Sacramento Peak for further tests. A preliminary examination suggests that one of the optical elements may not be natural quartz, but may instead contain some impurities. Thus, its index would not meet specifications and may explain the unexpected test results. Further tests by R. Dunn at Sacramento Peak will continue. The stack will then be returned to NSO Tucson and taken to the McMath for measurement of total transmission characteristics at the K-line.

Spectromagnetograph. A simplified version of the desired real-time spectral analysis software for the Spectromagnetograph was written and installed for testing. Two key features of the package are a simplified convolution kernel for locating line centers and the use of the Euclid board as a slave to do flat-fielding, rather than as an independent parallel master to execute the entire analysis algorithm as originally intended. In off-line tests, magnetograms appear to be free of residual systematic patterns which are visible when the data are reduced with the Diode Array Magnetograph algorithm. However, the random noise, which is significantly reduced in the full spectral analysis algorithm, is about the same (7 Gauss) as the Diode Array Magnetograph at its best. Thus, the simplified version achieves the design goal of no added noise but is not optimum. Real-time performance under observing conditions has yet to be demonstrated.

Near Infrared Magnetograph. Activity in the Near Infrared Magnetograph (NIM) project focused on data analysis and on design of the adjustable-height scan platform and nematic liquid crystal retarders. Shortly after his arrival, G. Kopp began to work with D. Jaksha on speeding up the switching of the liquid crystal. Results are encouraging.

A one-year proposal to NASA by D. Rabin and C. Lindsey (U. of Hawaii) to support the development of near-infrared solar imaging and magnetometry was accepted.

15 CTIO During the last quarter, there was continued progress on two major top priority projects, and another major project has been completely finished.

Argus, the multi-fiber-fed spectrograph, has been in use successfully for two years, but work has continued to improve reliability (e.g. wear problems in the fiber probes) and ease of use, and to complete the documentation. This work is now finished. In addition, an echelle mode has now been added, with the purchase of an appropriate large echelle grating and order-sorting filters.

The production of "Revision A" CCD-TV acquisition cameras is now underway, with a batch of four in the final stages of production and testing; a fifth camera has already been produced and is in use on the 4-m telescope, while the prototype is in use on the 1.5-m telescope. The initial set of five production cameras will satisfy urgent needs, while a second batch of four, to be produced later in the year, will include some additional features ("Revision B") and allow older cameras (RCA and Quantex) to be permanently phased out. ESO will also be producing several CCD-TV cameras from the design.

The CCD Controller project continues to make progress, with the prototype now reading out a CCD in the lab with more or less acceptable noise figures. Tests at the telescope are scheduled during the second quarter (calendar year 1991).

In other areas, the ASCAP single-channel photometer is now being controlled by a PC, which also carries out quick look data reduction. This is another major step to eliminating aging (and heat- producing) Eclipse computers; it also allows observers to use the ASCAP at the 0.6-m Lowell telescope.

Progress continues on the PF corrector, two of the elements have been delivered to Tucson with the remainder scheduled for the near future. Once delivery is complete, the optics will be anti-reflection coated and shipped to Chile for mechanical assembly. First tests of the corrector are scheduled for June 1991.

F. Observatory Activities

Evans Solar Facility Coronal Observations. Five months of pre-launch support of a dual solar rocket flight to observe activity in the x-ray and EUV regimes were provided at the Evans Solar Facility. Daily updates of conditions in the solar corona as it rotated onto the solar disk from the East limb were used in determining the appropriate active region to observe. This culminated in successful missions being carried out (by D. Moses, principal investigator) on 21 November 1990, based partly on observations at GL/OLAC of strong activity in Fe XIV and Ca XV on the East limb several days earlier.

Cool Stars Workshop. M. Giampapa established the Scientific Organizing Committee for the Seventh Cambridge Workshop entitled "Cool Stars, Stellar Systems and the Sun," to be hosted by the NSO. The meeting will be held at the Tucson Hilton East in Tucson on 9-12 October 1991. Giampapa and the SOC hope to complete the formulation of the meeting format during the next quarter.

M. Giampapa continued to serve as a Co-Editor for the book The Sun and Time (University of Arizona Press). Nearly all the manuscripts are completed. The book will be submitted to the printers

16 sometime during the next quarter. Giampapa also continued his editorial duties for the journal The Astronomy Quarterly and was promoted to Associate Editor.

Infrared Solar Physics. The IAU accepted a proposal to sponsor a meeting on "Infrared Solar Physics" to be hosted by NSO in Tucson during February 1992. D. Rabin will chair the local organizing committee. In expectation of considerable interest in the meeting worldwide, the IAU requested that the meeting be sponsored as a symposium rather than a colloquium as originally proposed. The scientific organizing committee has agreed and is now readying a first announcement of IAU Symposium 154.

Chilean economic statistics, FY 1991:

%Change Cum. change Avr. monthly Month in CPI in CPI Pesos/Dollars

Oct 3.8 3.8 313.14 Nov 0.9 4.7 326.63 Dec 0.5 5.3 335.55

V. PROGRAM SUPPORT

A. Director's Office

A proposal requesting a three-year award to fund the Research Experiences for Undergraduates Site Program at NOAO was submitted to the NSF in October. The 1990 REU Site Program Final Report was completed and mailed to the NSF in November.

The NOAO Annual Report for the period July 1989 - June 1990 was submitted to the Bulletin of the American Astronomical Society and the NSF in November. The report will appear in Volume 23, Number 1, of the BA.A.S., which is scheduled to be mailed in February 1991.

The Director's Office assisted the NSO division in preparing for their review by the AURA Visiting Committee on 17 and 18 October, and made arrangements for an IRAF User's Committee meeting on 10 December.

A total of $ 5,079.00 was paid out of the NSF Foreign Travel Account for the quarter. The following sites and institutions were visited: European Southern Observatory, Chile; UKTRT, Mauna Kea; and Las Campanas Observatory, Chile.

B. Safety Report

The major accomplishments and highlights of the NOAO Safety and Health Program for the U.S. sites are as follows:

Safety Reviews. Reviews were conducted of the modifications to MIT's ETC building at the KPNO site, and the safety plan for etching the AFWL 3.5-m mirror with hydrochloric and hydrofluoric acid at the University of Arizona Steward Observatory Mirror Lab.

17 Air Quality Control Permits and Emissions Reports. Annual permits required by Pima County were issued following inspection of air polluting equipment and operations at the KPNO and Tucson sites. Emission reports were filed for both sites.

Hazardous Materials Cargo Placarding and Manifests. Department of Transportation requirements for placarding, and new manifests for hazardous materials transported between the Tucson and KPNO sites, were implemented.

Print Shop Chemicals. An extensive review of the chemicals used in the Tucson Print Shop was carried out. As a result, new and revised procedures for minimizing the potentially harmful exposure to perchlorethylene and other chemicals were implemented. Subsequently, printing presses requiring the use of such chemicals were removed from service and replaced by dry contact duplicating equipment.

Lead in Water Coolers. Two Halsey Taylor water coolers at the KPNO site were identified as potential contributors to more than 20ppb of lead in the drinking water. Tests revealed that one of these exceeded the limit and the subject cooler was removed from service.

Lockout-Tagout of Harmful Energy. The specific rules, procedures, and responsibilities for the lockout-tagout of harmful energy were written and are in the process of being implemented at all sites.

Extra Low Frequency (ELF) Electromagnetic Fields (EMFs). Because of the concerns raised over the potential for harmful exposure to ELF/EMFs from sources such as power lines, transformers, and video display terminals, this subject was investigated. While it is the opinion from various sources that we do not have any problems, it is generally recommended that a survey of ELF/EMFs be performed. A survey is planned for the near future.

Mercury Spill - Canada France Telescope (CFT). CFT personnel were provided with a sample procedure and other information to help clean up 5 kg of mercury which spilled from a secondary mirror support bug.

Fall Protection. A policy and procedure for the protection of personnel from a fall from an unguarded elevated work situation was written. Full implementation of the policy and procedure, which will require engineering, installation of fall arrest systems, and training, has been requested for the KPNO site.

Hazardous/Chemical Waste Disposal. Seven PCB contaminated transformers and one contaminated capacitor from the NSO Sacramento Peak site were disposed of properly. Approximately 60 small containers of waste chemicals were collected from the KPNO and Tucson sites and consolidated for future contract disposal.

Safety Training. The following training was accomplished: Safety of operating forklift trucks (Tucson maintenance and Shipping and Receiving); Safe operation of powder actuated fastener tools (Tucson maintenance personnel); Lockout-Tagout of harmful energy (KPNO maintenance and technical personnel).

Underground Fuel Storage Tanks (UFSTs). Because of age and other factors mandated by EPA, a total of ten UFSTs at the three sites were removed. The remaining five UFSTs, which must either be

18 upgraded with leak monitors and spill controls or replaced in the future, were tested for leaks. Leak testing and procedures, for the reconciliation of fuel usage, will be ongoing until these UFSTs are upgraded, replaced, or removed. Three new UFSTs, all having required controls, were installed.

Assessment of Asbestos. An assessment of asbestos in an AURA owned house at the Tucson site was undertaken prior to its demolition. A qualified demolition and asbestos abatement contractor removed and properly disposed of the asbestos.

Fire Alarm Systems. Basic components for a modern fire alarm system were purchased for all sites. The components, planned for installation by NOAO personnel, will replace the antiquated system at NSO Sacramento Peak, provide a new system at KPNO, and protect five buildings adjacent to the main Tucson complex.

Fire Truck Pump. A defective truck pump at NSO Sacramento Peak was rebuilt.

Fire District. The NSO Sacramento Peak site was designated by Otero County as a fir district.

Facilities Cleanup. An extensive, in-depth cleaning of the NSO Sacramento Peak buildings and grounds was accomplished.

Safety Manual. The NOAO Safety Manual was completed and submitted for approval.

Resignation and Replacement of KPNO Safety Officer. J. Cook, KPNO Safety Officer, resigned. H. Marquez, a retired captain from the Tucson Fire Department, was hired as his replacement.

B. Central Administrative Services

Changes in employee benefits were announced to NOAO staff the week of 15 October.

Subsequent to NSF approval and a WIYN Board meeting on 22 and 23 October, the WIYN Consortium was incorporated on 5 November 1990.

The annual audit by Coopers & Lybrand was completed in December and draft financial statements were issued. The final statement will be issued early in the next quarter.

The NOAO Flexible Spending Account (FSA) plan, as approved by the AURA Executive Committee, was submitted to AURA's attorneys for review.

C. Central Computer Services

Ursa, the fast Sun-4/470 representing the Draco (VMS-Vax) replacement, was made operational. This continues a shift in computing activities from VMS to UNIX begun 10 years ago. Several desktop workstations were installed or upgraded.

IRAF A second update for version 2.9 IRAF has been prepared and is now in beta testing, with a release scheduled for February. The primary purpose of this minor release is to support the version 1.0 release of PROS from CfA. Work has concentrated mainly on the QPOE (photon image) and PLIO

19 (image mask) interfaces. Work continues on the next major release of IRAF, version 2.10, due out early in the summer.

In IRAF port news, the HP-UX/IRAF upgrade to IRAF version 2.9.1 for both the Motorola and RISC architectures was completed in early December, and the system is now in distribution. The first phase of the IRAF port to the Silicon Graphics Personal IRIS 2 has been completed and this system is now being tested.

Work on the CCDPHOT (CCD photometer) project is well along. The initial implementation will use the KPNO CCD controller connected directly to a Sun via a parallel interface. Detector control and readout will be done directly by the Sun, rather than by the old CCD Forth systems. This direct-to- Sun interface was developed by S. Schaller and Steward Observatory.

The initial phase of incorporating the CTIO photometric calibration software into IRAF has been completed. The package is now being tested in-house and written documentation is being prepared. A first version of the planned radial velocity package (RVO), is now undergoing intensive testing and should be publicly available in a few months.

Preparation for the astronomical data analysis software conference sponsored by the major IRAF centers (NOAO, STScI, and SAO) to be held in Tucson in November 1991 is well underway. In recent weeks, most of the effort has centered on lining up the invited speakers; further information on the speakers list and conference program should be available shortly. To date, over 100 people have preregistered for the conference.

The IRAF Users Committee met in Tucson in December. A group of KPNO scientists interested in IRAF development met with IRAF staff to discuss scientist participation in software specification and evaluation. The group will continue to meet monthly.

D. Central Facilities Operations

Repair and repainting of the stucco surfaces of both the Engineering and East Wing were completed. A graphic design denoting the size of the 8-m mirror was incorporated in the painting of the Engineering Wing. Outdated leased phones were replaced with new phones in order to make better use of the existing phone system features. Options regarding 8-m office space were investigated and initial efforts were undertaken to procure modular structures for this usage. Current plans are to install these structures on the East Wing roof during the second quarter. The AURA house located on the Martin Avenue property was demolished and the necessary improvements were made to establish the GONG staging yard.

Central Facilities personnel were involved in changing the Print Shop into a high-speed copy center. This involved modifications to the area and the installation of a new HVAC system to replace the existing outdated A/C unit and gas space heaters.

At the request of the Safety Committee, CFO personnel identified all window and door glass not meeting building code specifications within the Tucson and Kitt Peak facilities. All inferior glass will be replaced with safety glass.

20 E. Engineering and Technical Services

Flow visualization data videos taken in September were duplicated and sent to our prospective 8-m telescope partners. The tapes were also studied and graphs generated to compare the flushing times for each enclosure model at all angles of flow. The results indicate that each model type can be vented properly to provide not only adequate but also uniform flushing at all angles. The 4-m dome test results showed venting to be more effective than pumping, and these results were transmitted to CTIO.

Through cooperation with Steward Observatory, arrangements were made to view and copy their Columbus project flow visualization videos. Their data are interesting in terms of flow line behavior for the open base case and the effect of trees.

A guide-alignment figure sensor concept was developed last quarter which was intended to serve as a model for the WIYN telescope control system and possibly for the 8-m telescope design. The technique uses curvature sensing to record extrafocal images simultaneously in a CCD camera. These images are then processed into a combined curvature intensity map and finally into a reconstructed wavefront phase map of the telescope optics. By having no moving parts, the system is inexpensive and simple, and provides all of the information to collimate, focus, and adaptively correct the wavefront. Telescope time was provided by SAO at Mt. Hopkins for the 1.5-m and 1.2-m telescopes to test for alignment, spherical aberrations, and the source of the trifoil aberrations in the 1.5-m. Sufficient data were taken to prove the technique, and a poster paper has been prepared for the January Philadelphia AAS meeting giving the results of this first test.

Vandenberg Air Force Base personnel witnessed the curvature wavefront data gathering session as they have an interest in building such a system to understand their telescope optics and alignment.

F. Publications and Information Resources

Three press releases were issued by the PIR office during this quarter, one on the work of M. Giampapa and W. Livingston concerning solar variability, one on the work of M. Belton on models for Comet Halley, and a third describing the finalization of the WIYN agreement.

Educational and commercial tours of Kitt Peak and downtown facilities were arranged by P. Patterson, as follows:

R.A.I.S. Berlin Television filmed footage and commentary from the top of the McMath telescope for an eight-part German television series called "The Universe." A University of Arizona group, attending astronomy camp for adults, toured the 4-m and the McMath and were able to watch start-up procedures at the 4-m with J. Schombert (U. of Michigan) and K. Rakos (U. of Vienna). D. McCarthy (U. of Arizona) led the tour. A group from Marcos Di Niza High School, Tempe, Arizona, toured Kitt Peak, accompanied by D. Burstein (Arizona State U.). Thirty-two students and three instructors from the Centra de Bachillerato Techologico Industrial y de Servicios #37 in Sonora, Mexico, toured the optical shop and instrument shop at the NOAO headquarters. The Spanish-speaking students and instructors were given a tour (in Spanish) by two ETS staff members, Jorge Simmons and Earl Pearson. A local Tucson television station, KVOA Channel 13, filmed a story on Kitt Peak about how an observatory operates. The story aired locally on the news program "Cover Story." W. Keel (U. of Alabama) was interviewed at the 2.1-m telescope. P. Patterson accompanied the group. A PBS

21 television station, WHYY from Philadelphia, filmed a segment on Kitt Peak for their television series, "Dinosaur," to be aired nationally in 1992. The segment will feature the work of J. Melosh (U. of Arizona Lunar and Planetary Lab.).

Photo Collection. The photo collection net sales for the quarter were $957, down from $2316 the previous quarter. A set of slides from the most recent solar maximum was developed for the photo collection by E. Hardesty. Slides from the set are for sale through the NOAO catalog, and will be sold as a set by the Astronomical Society of the Pacific.

An informational packet about NOAO was developed by E. Hardesty and 1,951 of the packets were distributed.

A slide set with the purpose of describing the 8-m project was developed by the PIR office. The set is to be distributed to AURA board members.

An introductory astronomy class for NOAO employees was organized by the PIR office and given during the third quarter. Approximately twenty-five employees attended the series. Each lecture was given by an NOAO astronomer, and the lectures were taped for use in training Visitor Center guides.

The PIR office arranged for J. Salzer to speak in the Flandreau Planetarium lecture series.

Visitor Center. The Kitt Peak Visitor Center arranged special tours for 33 groups, for a total of 1,019 visitors, in addition to the twice-daily public tours. Three public evening programs were held on the mountain during the quarter. The Visitor Center has added a Macintosh computer to the exhibit area, as well as a viewing area for short video presentations. The video presentations run continuously during business hours.

22 TELESCOPE USAGE STATISTICS

October - December 1990

APPENDIX A

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

4-m 874.9 485.3 188.2 26.9 24.8 149.7

1.5-m 854.2 542.1 171.6 93.3 35.7 11.5

1-m 751.5 514.2 0 100.6 50.6 86.1

CTIO 0.9-m 857.4 654.8 95.4 58.0 6.3 42.9

*0.6/0.9-m 435.2 229.1 98.4 31.5 29.5 46.7

0.6-m 83.4 72.5 0 0 0 10.9

4-m 1115.5 570.07 142.94 322.25 35.25 45.0

2.1-m 1052.0 618.5 66.5 313.25 24.25 29.5

Coude" Feed 999.0 464.25 175.0 319.75 11.5 28.5

KPNO 1.3-m 1027.5 367.65 170.85 377.5 54.0 57.5

0.9-m 1027.5 499.5 118.25 345.0 25.25 39.5

Schmidt 243.0 143.0 0 87.0 0 13.0

Hilltop Dome 1948.0 126.0 1278.0 534.0 10.0 0

Vac. Tower 798.0 361.4 196.6 171.0 13.0 56.0

Evans Fac. 1641.0 528.1 616.9 428.0 68.0 0

NSO **FTS Lab 402.0 253.4 16.6 44.0 0 88.0

**McMath 1112.5 747.0 30.5 236.0 29.0 0

Vacuum/KP 661.5 374.5 0 209.5 77.5 0

294.5 26.0 Fourier Tach. 904.5 584.0 0 0

Note: Scheduled hours are calculated according to the ephemerides for CTIO: October - 9.9 hours/night; November - 8.9 hours/night; December - 8.2 hours/night.

* Use restricted to dark of the moon.

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

CERRO TOLOLO INTER-AMERICAN OBSERVATORY OBSERVATIONAL PROGRAMS APPENDIX B

October-November-December 1990: Individual Telescope Assignments are listed below. Graduate Students are indicated by an asterisk after their names. Nights assigned, (hours worked), and telescope used are indicated. Service Observing programs are denoted by S.O. instead of nights assigned.

C. Anguita, M. Ruiz, U. de Chile: "CCD Parallaxes for Faint Proper Motrion Stars." 3(27)1.5-m.

F. Baganoff*, M. Malkan, U. of California, Los Angeles: "Multi-wavelength Variability of Active Galactic Nuclei." 4(39)1.5-m, 8(61)l-m, 8(71)0.9-m.

J. Baldwin, G. Williger, CTIO, R. Carswell, J. Webb, Cambridge U., England: "High-redshift Absorption Line Systems." 5(40)4-m.

J. Baldwin, CTIO: "Photometric Monitoring of a QSO Sample." l(5)0.9-m.

J. Baldwin, CTIO, G. Ferland, Ohio State U.: "Helium Abundances in Metal-Rich HII Regions." 3(24)1.5-111, 2(18)0.9-m, 2(10)Sch.

M. Bolte, J. Hesser, Dominion Astrophysical Obs., D. VandenBerg, U. of Victoria: " Precise Ages for the Oldest LMC Clusters." 3(27)4-m.

G. Bothun, C. Mihos*, D. Richstone, U. of Michigan: "The Kinematics and Star Forming Properties of Interacting Disk Galaxies." 2(16)1.5-m.

R. Ciardullo, G. Jacoby, KPNO, K. Engle*, Pennsylvania State U.: "Planetary Nebulae as Standard Candles: The Fornax Cluster." 4(36)4-m, 2(12)Sch.

K. Cook, C. Alcock, H. Sook, T. Axelrod, Lawrence Livermore Natl. Lab: "Feasibility Study for a Search for Halo Dark Matter." 6(57)0.9-m.

E. Costa, U. de Chile: "RI Photometry of LMC Carbon Stars." 3(14)1.5-m.

A. Cowley, Arizona State U., F. Hartwick, U. of Victoria: "Kinematics of the SMC Halo." 3(20)4-m.

A. Crotts, NASA Goddard Space Flight Ctr., S. Heathcote, CTIO: "The Dynamics and Morphology of the Emission-line Nebula Surrounding SN 1987A." 4(34)4-m.

G. Da Costa, Anglo Australian Obs.: "A Search for LMC Clusters with 3

L. Da Costa, M. Geller, J. Huchra, D. Latham, Harvard Smithsonian Ctr. for Astrophysics: "Southern Slice Redshift Survey." 10(100)1.5-m.

S. Demers, F. Wesemael, G. Fontaine, U. de Montreal, M. Irwin, Cambridge, U., England: "The Montreal-Cambridge-Tololo Survey." ll(98)Sch. A. Dey*, U. of California, Berkeley, W. van Breugel, Lawrence Livermore Nat. Lab., M. Lehnert*, STScI.: "The Interaction of Radio Sources with Ambient Gas: A Sample of Nearby, Gas-Rich Radio Galaxies." 3(27)0.9-m.

M. Dickinson*, U. of California, Berkeley: "Multi-bandpass Imaging and Photometry of Distant Galaxy Clusters." 2(19)4-m, 4(41)1.5-m.

S. Djorgovski, M. Strauss, D. Thompson*, W. Weir*, California Inst, of Technology, R. de Carvalho, Obs. CNPq, Brazil: "Spectroscopy and Photometry of Southern Elliptical Galaxies." 6(45)0.9-m.

H. Dottori, J. Santos*, E. Bica, UFRGS, Brazil, J. Claria\ Obs. Cfjrdoba, Argentina: "Deep Photometry of LMC Clusters." 10(73)0.6-m.

0. Eggen, CTIO: "Photometry." 4(15)1.5-m.

J. Elias, CTIO, G. Neugebauer, B. Soifer, P. Hacking, California Inst, of Technology: "Cosmic Evolution of Infrared-Luminous Galaxies." 2(19)4-m.

P. Eskridge, Rensselaer Polytech. Inst.: "Density Anomalies in Halo Dwarf Galaxies." 3(30)4-m.

E. Fitzpatrick, Princeton U.: A Survey of Metallicity Variations Among LMC B-type Supergiants." 7(61)1-m.

C. Foltz, F. Chaffee, C. Hogan, U. of Arizona, P. Hewett, Cambridge U., England: "A Search for a Supercluster at High Redshift." 3(30)4-m.

J. Forte, IAFE, Argentina, S. Cellone*, La Plata, Argentina: "Washington Photometry of Low Surface Brightness Galaxies in Fornax." 2(18)1.5-m, 2(15)0.9-m.

M. Franx, Harvard Smithsonian Ctr. for Astrophysics, G. mingworth, U. of California, Santa Cruz: "Structure and Kinematics of SOs." 3(23)0.9-m.

D. Geisler, CTIO, M. Mateo, The Carnegie Observatories, J. Nemec, U. of British Columbia: "Metal Abundance Variations in Dwarf Spheroidal Galaxies." 2(16)4-m.

M. Hamuy, M. Phillips, N. Suntzeff, CTIO, J. Maza, U. de Chile: "A Search for Supemovae." 10(81)Sch.

E. Hardy, U. Laval, N. Suntzeff, CTIO, R. Zinn, Yale U.: "Color-magnitude Diagrams of the Globular Clusters and their Surrounding Fields in the Fornax Dwarf Spheroidal Galaxy." 3(25)4-m.

S. Heathcote, W. Weller, CTIO: "Using the Curtis Schmidt plus CCD as a Tool to Find Pre-main Sequence Stars and Herbig-Haro Objects." 5(23)Sch.

T. Heckman, Johns Hopkins U., M. Lehnert, STScI: "Spatially-Reoslved Images of High Redshift QSOs." 3(27)4-m. G. Jacoby, R. Ciardullo, KPNO, J. Kaler, U. of Illinois: "The Relationship Between Chemical Composition and Core Mass in Planetary Nebulae." 2(17)4-m.

D. Koo, N. Ellman*, U. of California, Santa Cruz, A. Szalay, Johns Hopkins U.: "Is the Universe Periodic on 100+ Mpc Scales?." 4(34)4-m.

D. Koo, U. of California, Santa Cruz, and D. Bennett, Princeton U.: "Multicolor Imaging of Twin Galaxies Caused by Cosmic Strings." S.O.(4)4-m.

R. Lamontagne, S. Demers, F. Wesemael, G. Fontaine, U. de Montreal: "Photometric Calibration of the Montreal-Cambridge-Tololo Survey Fields." 5(49)0.9-m.

A. Landolt, Louisiana State U.: "UBVRI Photometric Sequences I." 5(41)1.5-m, 5(28)l-m.

T. Lauer, KPNO, M. Postman, STScI:" The Motion of the Local Group With Respect to Nearby Abell Clusters." 3(27)1.5-m.

P. Lu, W. Tsay, Western Connecticut State U.: "Continuation of Study to Determine Using Faint Dwarf F-stars at the SCP." 13(76)l-m, l(10)0.9m.

J. Maza, F. Barrientos*, U. de Chile: "Sodium D Absorption in Seyfert 1 Galaxies." 3(24)4-m.

H. McAlister, W. Hartkopf, W. Bagnuolo, Georgia State U., O. Franz, Lowell Obs.: "Binary Star Speckle Interferometry and Photometry." 5(47)4-m.

V. Niemela, IAFE, Argentina: "Spectroscopic Binaries in the Magellanic Clouds." 5(40)1-m.

R. Olowin, Saint Mary's Coll., J. Huchra, Harvard Smithsonian Ctr. for Astrophysics, H. Corwin, U. of Texas: "Mean Cluster Redshifts and Velocity Dispersions for a Sample of Southern Abell Clusters." 3(28)4-m.

M. Pastoriza, E. Bica, H. Dottori, UFRGS, Brazil, M. Maia, L. Da Costa, Obs. CNPq, Brazil: "Environmental Influence on the Star Formation Rate in Spiral Galaxies." 6(58)l-m.

J. Patterson, U. of California, Los Angeles, E. Gotthelf, Columbia U., E. Sterner, Smith Coll.: "New DQ Herculis Stars." 8(58)l-m, 6(48)0.9-m.

M. Phillips, R. Williams, M. Hamuy, CTIO: "Spectral Evolution of Supernovae and Novae." 9(71)1.5-m.

M. Phillips, D. DePoy, J. Elias, B. Gregory, M. Hamuy, S. Heathcote, M. Navarrete, N. Suntzeff, A. Walker, L. Wells, R. Williams, CTIO: "Continuing Optical and Infrared Observations of SN 1987A in the LMC." 8(74)4-m, 6(52)0.9. A. Phillips*, U. of Washington: "HII Regions in Barred Spiral Galaxies." 3(26)1.5-m, 3(30)0.9-m.

M. Rubio, F. Barrientos*, U. de Chile, M. Roth, The Carnegie Observatories: "IR Observations of LMC Molecular Clouds." 2(19)4-m.

M. Ruiz, J. Maza, U. de Chile, M Pena, U. Nacional Aut6noma, Mexico: "Helium, Oxygen and Nitrogen Abundances in HII Galaxies." 2(18)4-m.

R. Schommer, CTIO, G. Bothun, U. of Michigan, T. Williams, Rutgers U., J. Mould, California Inst, of Technology: "Large Scale Motions and Deviations from Hubble Flow." 7(48)1.5-m, 4(33)0.9-m.

V. Smith, D. Lambert, U. of Texas: "Enhanced Lithium Abundances in Magellanic Qoud AGB Stars." 6(53)4-m.

N. Suntzeff, M. Phillips, CTIO: "Optical Photometry of Supernovae at Late Epochs." S.O.(6)4-m.

N. Suntzeff, CTIO, E. Hardy, U. Laval, J. Maza, U. Chile: "Kinematics of SMC Carbon Stars." l(10)4-m.

B. Twarog, B. Anthony-Twarog, U. of Kansas, J. Laird, Bowling Green State U.: "Extension and Expansion of the uvby Photometric System." 3(21)1.5-m, 3(25)l-m.

A. Walker, CTIO: "CCD Photometry of the RR Lyraes in the LMC Ousters NGC 1466, 1835 and GLC 0435-59." 4(32)1.5-m.

A. Walker, CTIO: "Magellanic Qoud Cluster RR Lyraes." 2(12) 1.5-m.

A. Walker, CTIO, E. Brocato, European Southem Obs.: "A Critical Comparison Between Evolutionar}' Theory and Observations for the Younger Magellanic Cloud Clusters." 2(16>4-m, 5(44)0.9-m.

G. Wallerstein, J. Brown, U. of Washington.: "Oxygen-To-Iron Ratios in Metal-Poor Clusters." 3(30)1.5-m.

E. Wilcots*, P. Hodge, U. of Washington: "Multi-wavelength Study of the MC Star-forming Regions I." 3(26)1.5-m, 5(44)1-m, 5(46)0.9-m.

R. Wing, Ohio State U., V. Blanco, CTIO: "Narrow-Band Photometry of M-Type Supergiants in the LMC." 6(44)1.5-m.

R. Wing, Ohio State U.: "Recognition and Classification of K-Type Supergiants in the LMC." 13(51)l-m.

F. Winkler, Middlebury Coll.: (a) "Narrow Band Imaging of Supernova Remnants," (b) "A Search for Supernova Remnants in the Magellanic Clouds." 7(57)Sch.

H. Yee, U. of Toronto, E. Ellingson, Dominion Astrophysicsl Obs.: "The Effect of Environment on the Evolution of AGNs." 3(26)0.9-m, 5(28)Sch. YALE PROGRAMS

B. Chaboyer*, P. Vader, Yale U.: "Imaging and Spectroscopy of Galaxies with Peculiar Internal Structures." 2(14)l-m, 7(67)0.9-m.

C. Heisler*, P. Vader, Yale U.: "Ha Imaging of Amorphous Galaxies, and Tying Up Loose Ends." 9(88)0.9-m.

KITT PEAK NATIONAL OBSERVATORY

APPENDIX B Executed Proposals 10/01/90 - 12/31/90 Page 1 Thu Jan 17 09:59:19 1991

Nights Hours Days Hours 8049 2 f90 H Abt, N Morrell, National Optical Astronomy Observatories A Search for Binaries in Two Extreme Clusters Coude Feed 6.00 41.50 0.00 0.00

8527 2 f90 H Abt, National Optical Astronomy Observatories First Radial Velocities of 147 FG Stars in the SBSC Coude Feed 3.00 32.00 0.00 0.00

8405 5 f90 P Appleton, M Lysaght, Iowa State University A Marston, Drake University Near-IR Imaging of Colliding Ring Galaxies 2.1 meter 4.00 38.50 0.00 0.00

8292 2 f90 T Armandroff, C Neese, P Massey, National Optical Astronomy Observatories Spectroscopy of Stellar Ha Sources in M31 4 meter 5.00 54.50 0.00 0.00

8319 2 f90 D Backman, NASA Ames Research Center K Hinkle, National Optical Astronomy Observatories Infrared Spectoscopy of the Epsilon Aurigae System Near 4 meter 0.00 0.00 2.00 0.00

8513 7 f90 F Baganoff, M Malkan, University of California, Los Angeles R Probst, National Optical Astronomy Observatories Multi-wavelength Variability of Ecliptic Pole Active 2.1 meter 0.50 3.00 0.00 0.00

8399 2 f90 S Balachandran, G Fisher, University of Hawaii Understanding Mixing Mechanisms in Solar Type Stars 4 meter 3.00 22.50 0.00 0.00 Executed Proposals 10/01/90 - 12/31/90 Page 2 Thu Jan 17 09:59:19 1991

Nights Hours Days Hours 8290 2 f90 H Bond, Space Telescope Science Institute R Ciardullo, National Optical Astronomy Observatories CCD Photometric Monitoring of Nuclei of Planetary Nebulae Nr. 2 0.9 meter 10.00 106.50 0.00 0.00

8437 8 f90 K Borne, Space Telescope Science Institute J Hoessel, University of Wisconsin M Balcells, Kapteyn Astronomical Institute Internal Dynamics of Tidally-Disturbed Elliptical Galaxies 4 meter 3.00 15.00 0.00 0.00

8415 7 f90 T Boroson, National Optical Astronomy Observatories Spectroscopic Differences Among High Redshift QSRs 2.1 meter 5.00 55.00 0.00 0.00

8315 4 f90 M Burton, X Tielens, Y Pendleton, H Butner, NASA Ames Research Center N Minchin, J Hough, Hatfield Polytechnic D Axon, Nuffield Radio Astronomy Laboratories Determining Grain Scattering Properties from H2 Line Ratios 1.3 meter 5.00 48.00 0.00 0.00

8351 8 f90 H Bushouse, Northwestern University A Stanford, University of Wisconsin Near-Infrared Imaging of the Arp Atlas of Galaxies 1.3 meter 5.00 30.50 0.00 0.00

8411 8 f90 H Bushouse, Northwestern University Spectral Properties of Interacting Galaxies Nr. 2 0.9 meter 7.00 56.00 0.00 0.00 Executed Proposals 10/01/90 - 12/31/90 Page 3 Thu Jan 17 09:59:19 1991

Nights Hours Days Hours 8517 4 f90 H Butner, NASA Ames Research Center E Lada, Harvard-Smithsonian Center for Astrophysics M Werner, Jet Propulsion Laboratory Near Infrared Imaging Polarimetry of NGC 2071 and NGC 2024 1.3 meter 5.00 7.00 0.00 0.00

8278 3 f90 B Carney, J Rose, University of North Carolina J Laird, Bowling Green State University The Galaxy's Thin Disk vs. Its Thick Disk Burrell Schmidt 8.00 33.00 0.00 0.00

8335 7 f90 M Dickinson, University of California, Berkeley Multi-Bandpass Imaging of Clusters around Distant Radio 2.1 meter 4.00 0.00 0.00 0.00

8379 4 f90 R Downes, NASA Goddard Space Flight Center C Keyes, University of California, Los Angeles D Weistrop, Applied Research Corporation A Search for Nova Shells Around Novalike Objects Nr. 2 0.9 meter 5.00 31.00 0.00 0.00

8400 8 f90 J Eder, Carnegie Institution of Washington Star Formation in Gas-Rich SO Galaxies Nr. 2 0.9 meter 5.00 36.00 0.00 0.00

8470 5 f90 S Edwards, Smith College S Strom, University of Massachusetts Mass Infall Signatures in Low Mass Pre-Main Sequence Stars 4 meter 4.00 38.50 0.00 0.00

8481 7 f90 P Eisenhardt, NASA Ames Research Center R Elston, National Optical Astronomy Observatories P McCarthy, Carnegie Observatories, (OCIW) IR Spectroscopy of High Redshift Radio Galaxies 4 meter 2.00 3.50 0.00 0.00 Executed Proposals 10/01/90 - 12/31/90 Page 4 Thu Jan 17 09:59:19 1991

Nights Hours Days Hours 8420 2 f90 F Fekel, Vanderbilt University G Henry, M Busby, Tennessee State University Spectroscopy of Binary and Multiple Stars Coude Feed 3.00 11.00 0.00 0.00

8357 9 f90 M Fitchett, University of Durham W Oegerle, Space Telescope Science Institute J Hill, University of Arizona Do High Velocity Dispersion Clusters Exist? 4 meter 3.00 34.50 0.00 0.00

8317 3 f90 J Frogel, Ohio State University R Davies, University of Oxford D Terndrup, D DePoy, Cerro Tololo Interamerican Observatory L Wells, National Optical Astronomy Observatories The Distribution of Infrared Light in the Bulges of Spiral 2.1 meter 4.00 40.50 0.00 0.00 1.3 meter 6.00 50.00 0.00 0.00

8401 9 f90 A Fruchter, Carnegie Institution of Washington G Bothun, University of Michigan T Lauer, Princeton University Peculiar Velocities or Systematic Errors? Nr. 2 0.9 meter 5.00 53.00 0.00 0.00

8450 2 f90 I Gatley, K Merrill, A Fowler, National Optical Astronomy Observatories F Piche, B Balick, University of Washington J MacKenty, Space Telescope Science Institute The Star Formation History in the Galaxy M33 1.3 meter 4.00 18.50 0.00 0.00

8454 5 f90 I Gatley, K Merrill, A Fowler, National Optical Astronomy Observatories F Piche, B Balick, University of Washington J MacKenty, Space Telescope Science Institute The Luminosity Function in Regions of Massive star 1.3 meter 5.00 43.00 0.00 0.00 Executed Proposals 10/01/90 - 12/31/90 Page 5 Thu Jan 17 09:59:19 1991

Nights Hours Days Hours 9112 0 f90 E Gotthelf, Columbia University Orbital Period Measurements of TT Ari Nr. 2 0.9 meter 4.50 0.00 0.00 0.00

8293 2 f90 A Grauer, University of Arkansas Time-Series Photometry of Hot Evolved Stars 1.3 meter 9.00 42.50 0.00 0.00

8472 3 f90 P Green, B Margon, S Anderson, University of Washington Distant Halo Carbon Stars as Tracers of the Galactic Nr. 2 0.9 meter 6.00 45.00 0.00 0.00 2.1 meter 4.00 18.50 0.00 0.00

8514 7 f90 J Halpern, M Eracleous, Columbia University Reverberation Mapping of an Accretion Disk 2.1 meter 3.00 0.00 0.00 0.00

8381 5 f90 L Hartmann, S Kenyon, M Gomez, Harvard-Smithsonian Center for Astrophysics B Jones, University of California, Santa Cruz J Stauffer, NASA Ames Research Center A Search for Pre-Main Sequence Stars in Taurus 4 meter 3.00 36.00 0.00 0.00

8297 4 f90 I Hawkins, University of California, Berkeley D Meyer, Northwestern University A Possible Resolution of the Local ISM 12C/13C Ratio Coude Feed 5.00 31.00 0.00 0.00

8524 8 f90 T Heckman, R Wyse, Johns Hopkins University Dwarf Galaxy Evolution : Supernova-Driven Winds? 2.1 meter 4.00 40.00 0.00 0.00 Executed Proposals 10/01/90 - 12/31/90 Page 6 Thu Jan 17 09:59:19 1991

Nights Hours Days Hours 8449 7 f90 G Hill, R Goodrich, University of Texas, Austin D DePoy, Cerro Tololo Interamerican Observatory Pa alpha in Radio Galaxies: A Search for Hidden Broad-Line 4 meter 3.00 30.00 0.00 0.00

8507 2 f90 L Hobbs, J Thorburn, University of Chicago, Yerkes Obs. C Deliyannis, M Pinsonneault, Yale University Li/H Dispersion in Hyades G and Early K Stars 2.1 meter 3.00 37.50 0.00 0.00

8369 9 f90 J Hoessel, University of Wisconsin A Saha, Space Telescope Science Institute Variable Stars in Nearby Irregular Galaxies 2.1 meter 4.50 38.00 0.00 0.00

8446 4 f90 G Jacoby, R Ciardullo, National Optical Astronomy Observatories J Kaler, University of Illinois H Ford, Space Telescope Science Institute The Central Star Masses of M31 Planetary Nebulae 4 meter 3.00 28.00 0.00 0.00

8421 2 f90 T Jarrett, R Dickman, University of Massachusetts W Herbst, Wesleyan University Optical Study of the Faint End of the Stellar Luminosity 4 meter 3.00 0.00 0.00 0.00

8302 8 f90 M Joy, A Prestwich, NASA Near Infrared Imaging of X-ray Cooling Flows 1.3 meter 5.00 32.00 0.00 0.00

8312 4 f90 R Joyce, National Optical Astronomy Observatories D Saperstein, J Kaufman, S Metin, IBM Search for Nitrogenated Amorphous Carbons in Interstellar 1.3 meter 2.00 0.00 0.00 0.00 Executed Proposals 10/01/90 - 12/31/90 Page 7 Thu Jan 17 09:59:19 1991

Nights Hours Days Hours 8275 2 f90 J Kaluzny, Warsaw University Observatory Photometric Study of Distant Anticenter Clusters 2.1 meter 2.00 24.00 0.00 0.00

8530 7 f90 K Kawara, National Astronomical Observatory Y Taniguchi, Kiso Observatory T Nakajima, Harvard-Smithsonian Center for Astrophysics Near-Infrared H2 Emission Lines in Bare Type 1 Seyferts and 4 meter 3.00 0.00 0.00 0.00

8296 8 f90 W Keel, University of Alabama Spin Orientation and Tidal Perturbations in Galaxy 2.1 meter 4.00 31.50 0.00 0.00

8358 2 f90 F Keenan, D Holmgren, P Dufton, Queen's University The Cosmic Abundance of Oxygen Coude Feed 5.00 41.50 0.00 0.00

8380 5 f90 S Kenyon, L Hartmann, M Gomez, Harvard-Smithsonian Center for Astrophysics A Survey of Low Luminosity Sources in the Taurus-Auiga 1.3 meter 3.00 32.50 0.00 0.00

8475 5 f90 S Kenyon, L Hartmann, M Gomez, Harvard-Smithsonian Center for Astrophysics A Search for the Youngest Binary Stars 1.3 meter 2.00 23.00 0.00 0.00

8389 2 f90 T Kinman, L Davis, National Optical Astronomy Observatories Does the Halo Field Star Horizontal Branch Show a Color 1.3 meter 3.00 34.50 0.00 0.00 Nr. 2 0.9 meter 4.00 33.50 0.00 0.00 Executed Proposals 10/01/90 - 12/31/90 Page 8 Thu Jan 17 09:59:19 1991

Nights Hours Days Hours 8338 2 f90 R Kirshner, B Leibundgut, Harvard-Smithsonian Center for Astrophysics A Porter, National Optical Astronomy Observatories A Saha, Space Telescope Science Institute Supernova Light Curves 2.1 meter 1.50 16.00 0.00 0.00

8523 9 f90 D Koo, N Ellman, University of California, Santa Cruz A Szalay, Johns Hopkins University

Are Galaxies in SA68 Also Distributed in a Periodic 4 meter 4.00 34.00 0.00 0.00

8386 2 f90 R Kraft, University of California, Santa Cruz C Prosser, Jr., Lick Observatory An H alpha Emission-Line Survey of the Pleiades Burrell Schmidt 6.00 55.00 0.00 0.00

8346 4 f90 K Kwitter, Williams College R Downes, Applied Research Corporation Y Chu, University of Illinois A Large-Field Survey of Northern Planetary Nebulae for Halo Burrell Schmidt 6.00 55.00 0.00 0.00

3488 5 f90 E Ladd, E Lada, P Myers, Harvard-Smithsonian Center for Astrophysics Near IR Imaging of Intermediate Mass Star Formation in 2.1 meter 4.00 18.50 0.00 0.00

8474 5 f90 P Lena, Observatoire de Paris K Dougados, Observatoire de Paris - Meudon S Ridgway, National Optical Astronomy Observatories J Christou, N0A0-8-meter Project IRc2 in the BN-KL Complex of Orion 4 meter 3.00 35.00 0.00 0.00 Executed Proposals 10/01/90 - 12/31/90 Page 9 Thu Jan 17 09:59:19 1991

Nights Hours Days Hours 8271 2 f90 P Massey, N Morrell, National Optical Astronomy Observatories The Mass-Luminosity Relation for High Mass Stars Coude Feed 5.00 29.00 0.00 0.00

8272 2 f90 P Massey, National Optical Astronomy Observatories C Garmany, University of Colorado The Initial Mass Function of Galactic OB Associations Nr. 2 0.9 meter 5.00 31.50 0.00 0.00

8484 2 f90 R Mathieu, University of Wisconsin J Morse, University of North Carolina Precise Radial Velocity Measurements of Early-Spectral-Type Coude Feed 5.00 61.50 0.00 0.00

7579 2 f90 H McAlister, W Hartkopf, W Bagnuolo, J Sowell, Georgia State University 0 Franz, Lowell Observatory Binary Star Speckle Interferometry and Photometry 4 meter 3.00 12.50 0.00 0.00

8286 4 f90 D Meyer, Northwestern University 1 Hawkins, University of California, Berkeley E Wright, University of California, Los Angeles The Interstellar 7Li/6Li Isotope Ratio Toward Zeta Persei Coude Feed 6.00 55.50 0.00 0.00

8345 4 f90 D Meyer, Northwestern University A Sensitive Search for Interstellar Molecules at Near UV 4 meter 3.00 20.50 0.00 0.00

8469 7 f90 H Miller, M Carini, J Noble, Georgia State University Blazar Variability and the Existence of Accretion Disks Nr. 2 0.9 meter 5.00 46.00 0.00 0.00 Executed Proposals 10/01/90 - 12/31/90 Page 10 Thu Jan 17 09:59:19 1991

Nights Hours Days Hours 8462 2 f90 N Morrell, National Optical Astronomy Observatories N Walborn, Space Telescope Science Institute D Minniti, University of Arizona Spectroscopic Study of Subluminous OB-stars Coude Feed 5.00 6.00 0.00 0.00

8350 7 f90 T Nakajima, N Carleton, Harvard-Smithsonian Center for Astrophysics M Nishida, University of Kyoto Near Infrared Spectroscopy of Active Galactic Nuclei 4 meter 3.00 29.00 0.00 0.00

8300 4 f90 C O'Dell, D Valk, C Miller, Z Wen, Rice University Observations for a Velocity Derived Model of IC 418 Coude Feed 5.00 9.25 0.00 0.00

8496 8 f90 R Oliversen, B Woodgate, L Brown, A Caulet, NASA Goddard Space Flight Center P Hintzen, University of Nevada N Oliversen, IUE Observatory/CSC K Cheng, Catholic University of America Coronal Line Emission in the NGC 1275 & 2A0335+096 Cooling 4 meter 3.00 10.00 0.00 0.00

8536 7 f90 P Osmer, A Porter, R Green, National Optical Astronomy Observatories Infrared Photometry of High Redshift Quasars 2.1 meter 3.00 11.50 0.00 0.00

9113 7 f90 P Osmer, A Porter, R Green, National Optical Astronomy Observatories Colorimetry of High Redshift Quasars Nr. 2 0.9 meter 2.00 0.00 0.00 0.00 Executed Proposals 10/01/90 - 12/31/90 Page 11 Thu Jan 17 09:59:19 1991

Nights Hours Days Hours 8301 2 f90 T Oswalt, L Roberts, Florida Institute of Technology E Sion, Villanova University P Hintzen, University of Nevada K Cheng, Catholic University of America Spectroscopy of Faint Luyten White Dwarf Binaries 4 meter 3.00 36.50 0.00 0.00

8398 8 f90 R Patterson, T Thuan, University of Virginia CCD Photometric Studies of Dwarf Galaxies with Extemely 2.1 meter 4.00 29.00 0.00 0.00

8422 8 f90 R Peletier, M Franx, Harvard-Smithsonian Center for Astrophysics CO-band Gradients in Giant Elliptical Galaxies 2.1 meter 2.00 20.00 0.00 0.00 1.3 meter 3.00 36.00 0.00 0.00

8162 4 f90 B Penprase, J Blades, Space Telescope Science Institute Optical Spectroscopy of High Latitude Molecular Cloud Cores Coude Feed 5.00 56.50 0.00 0.00

8542 8 f90 R Peterson, University of Arizona C Caldwell, Smithsonian Whipple Observatory J Gallagher, AURA, Inc. Rotation & Velocity Dispersion in Local Group Dwarf 4 meter 4.00 48.00 0.00 0.00

8442 2 f90 R Phelps, K Janes, Boston University An Investigation of the Galactic Initial Mass Function Nr. 2 0.9 meter 6.00 33.00 0.00 0.00 Executed Proposals 10/01/90 - 12/31/90 Page 12 Thu Jan 17 09:59:19 1991

Nights Hours Days Hours 8466 2 f90 R Probst, A Fowler, National Optical Astronomy Observatories J Stauffer, NASA Ames Research Center A Deep Infrared Search for Brown Dwarfs in the Pleiades 1.3 meter 5.00 42.00 0.00 0.00

8308 2 f90 L Ramsey, J Hall, R Patterer, D Huenemoerder, Pennsylvania State University Spectroscopic Studies of Surface Activity in Cool Stars 2.1 meter 4.00 44.50 0.00 0.00 Coude Feed 9.00 81.50 0.00 0.00

8274 8 f90 L Reed, G Harris, University of Waterloo W Harris, McMaster University Refined Integrated BVR CCD Photometry of M31 Halo Globular Nr. 2 0.9 meter 4.00 46.25 0.00 0.00

8453 2 f90 R Sahai, University of Goteborg A Wootten, NRAO K Hinkle, National Optical Astronomy Observatories 4.6um CO Observations of Interrupted Mass Loss AGB Giants 4 meter 0.00 0.00 5.00 27.50

8291 3 f90 P Schechter, M Metzger, Massachusetts Institute of Technology Whither the LSR?—Anticenter Carbon Star Velocities 2.1 meter 4.00 45.00 0.00 0.00

8326 2 f90 P Schmidtke, Arizona State University J Africano, National Optical Astronomy Observatories Lunar Occultations of Double Stars Nr. 2 0.9 meter 0.50 0.00 0.00 0.00 Executed Proposals 10/01/90 - 12/31/90 Page 13 Thu Jan 17 09:59:19 1991

Nights Hours Days Hours 8305 8 f90 J Schombert, University of Michigan M Barsony, University of California, Berkeley JHK Observations of cD Galaxies 1.3 meter 6.00 0.00 0.00 0.00

8539 9 f90 J Schombert, University of Michigan K Rakos, Institut fur Astronomie Galaxy Color Evolution in Distant Clusters 4 meter 3.00 30.00 0.00 0.00

8483 8 f90 N Sharp, National Optical Astronomy Observatories Identification of Leading-Arm Spiral Galaxies Nr. 2 0.9 meter 3.00 0.00 0.00 0.00

8344 5 f90 M Simon, SUNY at Stony Brook S Ridgway, National Optical Astronomy Observatories J Christou, N0A0-8-meter Project IR Speckle Interferometry of YSO Binaries in Taurus 4 meter 2.00 26.00 0.00 0.00

8332 7 f90 H Spinrad, M Dickinson, University of California, Berkeley First Observations of the Lyman Limit: A Test of Models for 4 meter 3.00 34.00 0.00 0.00

8371 5 f90 K Strom, J Hughes, S Strom, L Gauvin, University of Massachusetts Spectrophotometric Study of Optically Discovered Members 2.1 meter 4.00 48.50 0.00 0.00 Nr. 2 0.9 meter 5.00 58.00 0.00 0.00

8372 5 f90 S Strom, M Skrutskie, D Dutkevitch, University of Massachusetts S Edwards, Smith College J Stauffer, D Backman, NASA Ames Research Center Timescales for the Evolution of Secondary Disks Surrounding 1.3 meter 5.00 23.00 0.00 0.00 Executed Proposals 10/01/90 - 12/31/90 Page 14 Thu Jan 17 09:59:19 1991

Nights Hours Days Hours 8373 5 f90 S Strom, K Strom, P Hartigan, University of Massachusetts S Edwards, Smith College Constraints on PMS Evolutionary Timescales from YSO Binary 4 meter 3.00 10.00 0.00 0.00

8364 7 f90 J Sulentic, W Zheng, University of Alabama A Search for the Fe II—Fir Correlation Among QSO's 2.1 meter 4.00 36.50 0.00 0.00

8330 2 f90 P Szkody, University of Washington S Howell, D Dobrzycka, Planetary Science Institute Spectroscopy of High Latitude Cataclysmic Variables 2.1 meter 3.00 6.50 0.00 0.00

8533 4 f90 M Tamura, I Gatley, National Optical Astronomy Observatories S Kleinmann, University of Massachusetts S Sato, Tokyo Astronomical Observatory T Yamashita, Kyoto University The 3.08 Micron Ice Feature around Protostars 1.3 meter 5.00 51.50 0.00 0.00

8306 5 f90 F Walter, F Dudish, SUNY at Stony Brook A Brown, University of Colorado R Mathieu, University of Wisconsin F Vrba, U.S. Naval Observatory, Flagstaff The Low Mass Pre-Main Sequence Stellar Population: 2 2.1 meter 5.00 64.50 0.00 0.00

8355 5 f90 F Walter, SUNY at Stony Brook S Barden, National Optical Astronomy Observatories A Brown, University of Colorado R Mathieu, University of Wisconsin F Vrba, U.S. Naval Observatory, Flagstaff Spatial Distribution of Low Mass Pre-Main Sequence Stars in 4 meter 3.00 8.00 0.00 0.00 Executed Proposals 10/01/90 - 12/31/90 Page 15 Thu Jan 17 09:59:19 1991

Nights Hours Days Hours 8419 2 f90 G Wegner, J Dupuis, Dartmouth College J Africano, B Goodrich, National Optical Astronomy Observatories UBV Photometry of Spectroscopically Observed Faint Blue 1.3 meter 4.00 24.50 0.00 0.00

8448 4 f90 D Welty, University of Chicago J Fowler, Apache Point Observatory D York, L Hobbs, University of Chicago, Yerkes Obs. The Structure and Dynamics of Nearby Interstellar Clouds Coude Feed 6.00 64.00 0.00 0.00

8436 7 f90 M Whittle, C Nelson, University of Virginia The Spheroidal Component of Seyfert Galaxies Nr. 2 0.9 meter 4.00 42.00 0.00 0.00

8545 0 f90 S Wolff, National Optical Astronomy Observatories Director's Observing Program Coude Feed 6.00 71.00 0.00 0.00

8497 7 f90 D Womble, E Burbidge, V Junkkarinen, University of California, San Diego Probing Low Ionization Gas in Galaxies with QSO Absorption 4 meter 3.00 32.00 0.00 0.00

8426 3 f90 R Wyse, T Smecker, Johns Hopkins University Galactic Halo Metallicity Gradient 4 meter 4.00 21.00 0.00 0.00

8395 2 f90 A Young, L Rottler, San Diego State University A Skumanich, High Altitude Observatory R Mielbrecht, San Joaquin Delta College External Plasma and Chromospheric Fluorescence in V471 Coude Feed 7.00 48.00 0.00 0.00 Executed Proposals 10/01/90 - 12/31/90 Page 16 Thu Jan 17 09:59:19 1991

Nights Hours Days Hours 8528 2 f90 H Zinnecker, University of Hawaii J Christou, NOAO-8-meter Project S Ridgway, R Probst, National Optical Astronomy Observatories M Haas, Max Planck Institute for Astronomy An IR Speckle Survey for Duplicity among T Tauri Stars 4 meter 3.00 36.50 0.00 0.00

8374 3 f90 T von Hippel, G Bothun, University of Michigan A Search for Cool White Dwarfs 2.1 meter 4.00 18.00 0.00 0.00

Total number of proposals: 100 APPENDIX B

NATIONAL SOLAR OBSERVATORY REPORT Quarter Ended: 12/31/90

Nights Hours Days Hours 1553 S Acton, Lockheed Palo Alto Research Laboratory S/T347-Active Optics Systems 19 Segment Active Mirror VTT/SP 4 96

1023 R Altrock, AFSC/GL S/B003-Coronal Observations Evans Solar Facility/SP 88 131

1369 R Altrock, AFSC/GL L Gilliam, National Optical Astronomy Observatories S/B224-Daily Solar Activity Reports for Solar Forecasting Evans Solar Facility/SP 3 45

1511 R Altrock, AFSC/GL L Gilliam, National Optical Astronomy Observatories H Zirin, California Institute of Technology S/B269-Search for A XIV 4412 A Evans Solar Facility/SP 2 5

1212 P Bcmaih, University of Waterloo C Brazier, L O'Brien, D Perera, M Lee, M Oliphant, University of Arizona D Carrick, U.S. Air Force Astronautics Lab T/Spectroscopy of Molecules of Astrophysical Interest FTS 5 80

1373 T Brown, K Streandcr, High Altitude Observatory National Optical Astronomy Observatories T/&H-027-J-Sunspots (Hilltop @SP and FT @ Tucson) Fourier Tachometer 92 584

1519 D Bruning, University of Louisville T/Balmer Lines in Zeta-Aurigae Binaries McMath Main 5 11 xh 15-d I L Cram, University of Sydney M Giampapa, N;iiional Optical Astronomy Observatories T/Scarch for Non-radial Oscillations in Red Ciianis McMath Main 10 21

1089 R Dunn, National Optical Astronomy Observatories S/B230-Tower Engineering Evans Solar Facility/SP 3 6

1 ISO G Elste, University of Michigan S/R 183-Limb Darkening Freed from Scattered Light In Telescope F\ ans Solar Facility/SP 3 3

1-4S3 P Foukal, T Moran, Cambridge Research & Instrumentation, Inc. S/B261-Electric Fields Evans Solar Facility/SP 21 68

1556 P Foukal, T Moran, Cambridge Research & Instrumentation, Inc. S/B276-Test UV Imaging 3000 A to 3600 A Evans Solar Facility/SP 7 16

1429 M Giampapa, National Optical Astronomy Observatories T/Synoptic Observations of Ha Profile Variability in T Tauri Stars McMath Main 11 2V/i

1448 M Giampapa, National Optical Astronomy Observatories T/Synoptic Studies of Ha in "Marginal" BY Draconis Stars McMath Main 7 14

1564 M Giampapa, National Optical Astronomy Observatories L Cram, University of Sydney T/Mass Motions in "Naked" T Tauri Stars McMath Main 4 lO'A 1025 L Gilliam, National Optical Astronomy Observatories S/B057-Monitoring Community Evans Solar Facility/SP 40 80

1026 L Gilliam, National Optical Astronomy Observatories S/B062-Coronagraph Monitor Evans Solar Facility/SP 54 150

1034 L Gilliam, National Optical Astronomy Observatories S/H001-Flare Patrol (monitoring) Hilltop Dome/SP 92 577

1035 L Gilliam, National Optical Astronomy Observatories S/H002-White Light Patrol (monitoring) Hilltop Dome/SP~ ~ 92 568

1036 L Gilliam, National Optical Astronomy Observatories S/H003-Multiple Bank Polarimeter (monitoring) Hilltop Dome/SP 10 59

1039 L Gilliam, National Optical Astronomy Observatories S/H008-White Light Sunspot Drawing Hilltop Dome/SP 92 67

1126 L Gilliam, National Optical Astronomy Observatories S/BOlO-Ha Slitjaw Movie Evans Solar Facility/SP 7 25

1169 L Gilliam, National Optical Astronomy Observatories S/B007-USG/Disk Activity Program Ha SJC, Spectra 3500-7200 A Evans Solar Facility/SP 2 3

3790 J Harvey, National Optical Astronomy Observatories T/Vacuum Synoptic Program: Daily VT/KP 90 299 V2 1552 D Huencmoerder, Pennsylvania State University T/He I D3 Variability in RS CVn Stars McMath Main 12 35V2

1450 D Jennings, D Deming, NASA Goddard Space Flight Center D Zipoy, T Hewagama, University of Maryland T/Solar Magnetic Field Studies Using the 12-micron Emission Lines McMath Main 14 95

1570 S Keil, AFSC/GL G Cauzzi, Osservatorio Astronomico di Capodimonte S/T359-Solar Dynamics in Active Regions VTT/SP 16 105

1571 J Kuhn, H Lin, Michigan State University L November, National Optical Astronomy Observatories S/T360-High Precision Time Resolved Infrared Photometry VTT/SP 76

1593 J Kuhn, H Lin, Michigan State University S/B279-Infrared Observations Evans Solar Facility/SP 19 90

1543 T Leifson, University of Oslo T/Infrared Solar Oscillations IR FTS 26

1149 W Livingston, L Wallace, National Optical Astronomy Observatories T/Solar Irradiance Line Bisectors FTS 12

1199 W Livingston, National Optical Astronomy Observatories S/B190-Ca K Spectroheliograms Full Disk 0.0 & 0.38 A Evans Solar Facility/SP 1209 W Livingston, L Wallace, National Optical Astronomy Observatories M Steffen, Kiel University T/Spectrum Irradiance Variability of Sun McMath Main 12 76

1453 W Livingston, L Wallace, National Optical Astronomy Observatories D Elkins, NOAA T/FTS Measurements of Atmospheric Trace Gases FTS 4 32

5877 J LoPresto, Edinboro University of Pennsylvania T/Solar Gravitational Redshift McMath Main 7 55

1545 D Luttermoser, Iowa State University T/Flourescent Clues to the Shock of Late-type Giant Stars McMath Main 2 17

1531 C Mahaffey, Kitt Peak National Observatory T/Using the Solar Absorption Lines To Determine Solar Rotation VT/KP 6 36

1495 S Martin, California Institute of Technology K Harvey, SPRC/Tucson T/Magnetic & Velocity Full Observation of the Active & Quiet Sun VT/KP 11 39

1135 P Mcintosh, NOAA L Gilliam, National Optical Astronomy Observatories D Marquett, California Institute of Technology S/B001-NOAA Monitoring Program Evans Solar Facility/SP 89 117

1462 J Neff, S Saar, Harvard-Smithsonian Center for Astrophysics T/TiO Bandhead Measurements of Starspots Area and Temperature McMath Main 6 36 1565 J Neff, T Simon, University of Hawaii B Foing, Laboratorie de Physique Stellaire et Planetaire T/Ca II K Spectral Images of RS CVn System McMath Main 6672

1513 D Neidig, AFSC/GL S/T342-Simultaneous Three-Wavelength Flare Photometry at High Time Resolution VTT/SP 11 73

1235 A Pierce, National Optical Astronomy Observatories T/Solar Gravitational Redshift McMath Main

1406 A Potter, T Morgan, NASA Johnson Space Flight Center T/Studies of Exospheric Emission Lines in the Lunar Solar System FTS McMath Main 78

1596 R Rentschler, National Solar Observatory, Sacramento Peak S/B283-Installation of UPS in Computer Room Evans Solar Facility/SP 32

1515 S Restaino, New Jersey Institute of Technology S/T345-High Resolution Images from Focal Volume Information VTT/SP 12

1524 S Restaino, New Jersey Institute of Technology S/B265-Wave Behavior in the Photosphere 5434 A Evans Solar Facility/SP 16 118

1594 S Restaino, New Jersey Institute of Technology S Saar, Harvard-Smithsonian Center for Astrophysics S/B280-Analysis of the Octal Spectral Integrated Solar Spectrum Evans Solar Facility/SP 40 l.^v M Richards, University of Virginia T/Full-orbit Ha Spectroscopy of Short-period Algol-type Binaries McMath Main 572

1534 T Rimmele, Kiepenheuer Institut fur Sonnenphysik P Wiborg, USAF/GL S/T350-Correlation Tracker Test and Application vnysp 10 53

1572 D Rimmele, Kiepenheuer Institut fur Sonnenphysik S Kcil, AFSC/GL S/T361-Active Region Dynamics VTT/SP 14 92

1222 C Rinsland, J Levine, NASA Langley Research Center 1/Monitoring of Long Term Trends in Concentrations of Atmospheric Gases From McMath FTS Infrared Solar Spectra FfS 36

1573 P Rudawy, Wroclaw University Observatory S/T362-High Resolution Spectral Observations of the Uppermost Parts of Spicules VTT/SP 10 51

1540 D Rust, J O'Byme, Johns Hopkins University S/H034-Vector Magnetograph Hilltop Dome/SP 25 126

1557 S Ryan, University of Victoria C Deliyannis, Yale University T/Probes of Stellar Rotation McMath Main 36

1425 S Saar, Harvard-Smithsonian Center for Astrophysics J Linsky, University of Colorado T/A Survey of Magnetic Fields on G and K Stars McMath Main 61 1426 S Saar, Harvard-Smithsonian Center for Astrophysics J Linsky, University of Colorado M Giampapa, National Optical Astronomy Observatories T/Synoptic Observations of Magnetic Fields on G and K Stars McMath Main 11 5272

1251 E Seykora, East Carolina University S/B 191-Investigation of Very Low Contrast White Solar Structures in Active Regions Evans Solar Facility/SP 6 28

1037 R Smartt, National Optical Astronomy Observatories S/H004-Coronal One-shot (monitoring) Hilltop Dome/SP 4 7

1053 M Smith, National Science Foundation T/Radial Velocity Variations of Alpha Ori and Two Other Red Super Giants McMath Main 3 5

1420 M Smith, National Science Foundation T/Spectral Transients Related to be Activity in XEridan i McMath Main 1 3

1537 M Smith, National Science Foundation R Polidan, University of Arizona T/Monitoring of the Active He 1 6678A Line in Lambda Eridani McMath Main 10 3872

1356 K Strassmeier, University of Vienna T/Doppler Imaging of Spotted Chromospherically Active Stars McMath Main 10 1972 1560 K Strom, University of Massachusetts D Padgett, California Institute of Technology M Giampapa, National Optical Astronomy Observatories T/Doppler Imaging of the Pre-main-sequence Star V410Tau McMath Main 5 21

1474 I Tuominen, M Poutanen, University of Helsinki N Piskunov, USSR Academy of Science S Saar, Harvard-Smithsonian Center for Astrophysics T/Surface Imaging of the FK Comae Star HDl99178 McMath Main 8 32

1210 O White, Lazy FW Ranch T/Sun as a Star: Ca II Profile Measurements McMath Main 5 36

1024 S Worden, OSUDRE/ADEW S Keil, AFSC/GL S/B044-Solar Rotation 3898-3954 A Evans Solar Facility/SP 60 170

1595 J Zirker, National Optical Astronomy Observatories S/B282-Measure Profiles & Transmissions of USG 4 Line Evans Solar Facility/SP 3 11

Total number of proposals: 68

APPENDIX C The following is asummary of recordable occupational injuries for the Kitt Peak, Sacramento Peak and Tucson sites as reported on the OSHA 200 log. This information covers the calendar year 1990 As required, this data will be posted at each site by February 1, 1991.

KPNO Sac Peak Tucson Deaths: Total 0 0 0 0 Injuries involving days offor days of restricted work activity or both: 3 2 2 7

Injuries involving days off: 3 2 2 7

Days off from work: 44 2 8 54

Days of restricted activity: 24 0 19 43

Injuries without lost workdays: 1 1 3 5

Total recordable injuries: 4 3 5 12

There were no occupational illnesses recorded at Kitt Peak, Sac Peak, or the Tucson site in 1990.

CTIO recordable occupational injuries for calendar year 1990.

Deaths: 0 Injuries involving days offor days of restricted work activities or both: 2

Injuries involving days off: 2

Days off from work: 14

Days of restricted work activity: 5

Injuries without lost workdays: 2 There were no occupational illnesses recorded at CTIO in 1990.