NATIONAL OPTICAL ASTRONOMY OBSERVATORIES

NATIONAL OPTICAL ASTRONOMY OBSERVATORIES

QUARTERLY REPORT

APRIL-JUNE 1993

August 15,1993 TABLE OF CONTENTS

I. INTRODUCTION 1

II. SCIENTIFIC HIGHLIGHTS 1 A. Cerro Tololo Inter-American Observatory 1 1. Halo Masses of Spiral Galaxies 1 2. Detection of [Fe II] Emission in the Galactic Center 2 3. Southern Spectrophotometry Standards 2 B. Kitt Peak National Observatory 3 1. Primordial Lithium in Very Old, Very Metal Poor Stars 3 2. NGC 6611: A New Star Cluster Caught in the Act of Formation 3 3. Dusty Emission Filaments in M87: Probing the History of the Intracluster Medium ... 4 C. National Solar Observatory 5 1. Solar Oscillations and Atmospheric Structures 5 2. Flare-like Phenomena in High Coronal Loops 6 3. Research in Local Helioseismology 6

III. PERSONNEL AND BUDGET STATISTICS, NOAO 7 A. Visiting Scientists 7

B. New Hires 7 C. Change in Status 8

D. Terminations 8

E. Summer Research Assistants 8 F. Gemini 8-m Telescopes Project 8

G. Chilean Economic Statistics 9 H. NSF Foreign Travel Fund 9

Appendices Appendix A: Telescope Usage Statistics Appendix B: Observational Programs I. INTRODUCTION

This document covers scientific highlights and personnel changes for the period 1 April - 30 June 1993. Highlights emphasize concluded projects rather than work in progress. The NOAO Newsletter No. 35 (September 1993) contains information on major projects, new instrumentation, and operations. The appendices to this report summarize telescope usage statistics and observational programs.

II. SCIENTIFIC HIGHLIGHTS

A. Cerro Tololo Inter-American Observatory

1. Halo Masses of Spiral Galaxies

Galaxy formation is an essential test of any cosmological theory. Despite many efforts to investigate the subject over the past decade, it remains very poorly understood. The cosmological theory that has received the most attention in the last several years is the cold dark matter (CDM) model, which assumes that most of the mass in the Universe is made of nonluminous matter. Great support for this assumption comes from the study of galactic rotation curves, which indicate that spiral galaxies are embedded in massive dark halos. Rotation curves, however, can probe the halo mass distribution only out to the maximum radius of luminous material (stars and ionized gas) in a galaxy. It is clear that the dark matter extends further out than this, but how far is unknown. A rough estimate that this distance was relatively small (-50 kpc) with a commensurably small mass (2 x 1011 solar masses) was made based upon analyses of ten satellite galaxies around the Milky Way; this estimate was corroborated by less extensive studies of several nearby spiral galaxies. Such truncated halos would be difficult to reconcile with the standard CDM model. The discovery of several new satellites of the Galaxy caused the mass estimate for the Milky Way to go up by a factor offive, contributing to mounting evidence from independent methods that the Galaxy is indeed surrounded by a massive halo.

In order to extend greatly the radius and accuracy at which halos of galaxies like the Milky Way can be probed directly, D. Zaritsky (Steward Obs./Carnegie Inst, of Washington), R. Smith (U. of Wales, UK), C. Frenk (U. of Durham, UK) and S. White (U. of Cambridge, UK) surveyed satellite galaxies around a homogeneous set of spiral galaxies (1993, ApJ, 405, 464). They took most of their data with the CTIO 4-m telescope and the Argus multifiber spectrograph, with additional data taken with the Steward Observatory 2.3-m, AAT, WHT, and from published catalogues, in order to determine radial velocities of faint galaxies around isolated bright spirals. This enabled them to separate true satellites from coincidental pairings. Isolated spirals of similar absolute magnitude, morphology, and distance were used as targets for the study in order to avoid complicating effects from the gravity of neighboring large galaxies and to minimize variations in supposed halo structure with galaxy characteristics (which are suggested by rotation curve studies). Thirty-five new satellite galaxies were discovered, over half of them resulting from CTIO data. Treating the sample of satellites as an ensemble around a typical spiral galaxy, it is found that the more diffuse satellites tend to be at larger separations from their primaries, as though tidal effects extend only out to a certain distance. Their result indicates that halos of galaxies like the Milky Way characteristically extend out to -200 kpc, with total masses of 2 x 1012 solar masses, and is the first evidence that typical spiral galaxies have massive extended dark halos. 2. Detection of [Fe II] Emission in the Galactic Center

The center of our own Galaxy provides a unique opportunity to study the dynamics and physical conditions of the region around a galactic nucleus in detail. However, due to the vast amounts of dust and gas between us and the Galactic center, optical radiation from the center cannot reach us. Studies at other wavelengths, particularly in the infrared and radio, have revealed a highly complex environment. Some studies have produced evidence for high velocity gas and stellar motions, supporting the idea that there may be a massive compact object, such as a black hole, buried in the center of our Galaxy. Other studies have found evidence of gas streamers, which may be indicative of shocks and other violent processes. While radio studies have measured electron temperatures from 7000 K to 40,000 K, no complementary electron density measurements have been available to complete the picture.

Using the CTIO 1.5-m telescope and CTIO's infrared spectrometer (IRS), D. DePoy (now at Ohio State U.) obtained spectra of the Galactic center covering the emission of ionized iron, [Fe II] at 1.64 and 1.53 u.m, as well as the infrared emission from hydrogen, Bry, at 2.17 (im. [Fe II] emission has been widely used as a tracer of shocked gas. The ratio of the two [Fe II] lines can be used to derive electron densities. DePoy found emission from both of the [Fe II] lines (1992, ApJ, 398, 512). The measured ratio of [Fe II] 1.64 (im to Bry is similar to that seen in galaxies with active nuclei. This result is intriguing, as it may point to a similarity between the center of our supposedly "normal" Galaxy and the centers of active galaxies. With the detection of both [Fe II] lines, DePoy was able to derive a density of > 10 cm"3, a density much greater than that of 10 to 100 cm"3 found in the disk of our galaxy. DePoy found that the source of the [Fe II] emission could be either shock excitation or photoionization by nonthermal radiation, such as that produced by accretion onto compact objects. Observation of additional lines of [Fe II] may provide information to clarify this ambiguity and give additional information about the centers of active galaxies, where we cannot see the details we can see in the center of our own Galaxy.

3. Southern Spectrophotometric Standards

Standard stars with accurate energy fluxes are essential for the absolute determination of fluxes, temperatures, luminosities and surface gravities of celestial objects. The primary (defining) standard for calibrations is the bright star Vega in the northern hemisphere. Several observers have transferred the flux calibration of Vega to a set of secondary spectrophotometric standards, most of which are bright stars in the northern hemisphere. These bright stars are generally too bright for modern detectors on large telescopes, so a tertiary set of standard stars has been in wide use for the past decade. The Stone-Baldwin spectrophotometric standards, measured at CTIO in the early 1980s, have been the standards of choice in the southern hemisphere.

Recent advances in detector technology (charge coupled devices or CCDs) have made more accurate calibrations possible. In addition, an updated fundamental calibration of Vega was published by Hayes in 1985. For these reasons, CTIO staff members M. Hamuy, A. Walker, N. Suntzeff, P. Gigoux, S. Heathcote, and M. Phillips (1992, PASP, 104, 533 for first results) have been working for the past six years on a revision of the calibration of the Stone-Baldwin spectrophotometric standards. These new measurements cover almost all optical wavelengths observable from the ground (3300 to 10,000 A) at moderate (50 A) steps. The calibrations are accurate to better than 1%, allowing accurate spectrophotometry of program objects for southern hemisphere observers. Ten of the bright secondary standards have also been recalibrated based on the newfundamental calibrationand sampledat sufficiently small regular intervals (16 A) to be useful for high-dispersion spectroscopy. Both ofthese sets ofstandards will be of great use for a wide variety of spectroscopic observing programs done from the southern hemisphere.

B. Kitt Peak National Observatory

1. Primordial Lithium in Very Old, Very Metal Poor Stars

The abundances of the light elements D, 3He, 4He, Li, Be, and B provide one of the few direct, observational tests of cosmological models. The amounts of these elements produced in the Big Bang not only test the consistency of the standard model for primordial nucleosynthesis, but also may constrain the cosmic baryon to photon ratio, the mass density of baryons in the Universe, and the number of lepton families permitted in particle physics. The determination of the abundances of these species is, however, a difficult observational problem. Many of the species (D, Li, Be, and B) are easily destroyed in the hot, dense environment of a stellar interior; other species (3He and 4He) can be observed only in hot stars. All of these species (except D) may also be produced through spallation or fusion reactions in the interstellar medium, in normal stars undergoing main sequence hydrogen burning or double shell burning, or in supemovae. The determination of the primordial light element abundances from stars usually requires substantial interpretation to remove the contributions of element synthesis. One exception is observations of lithium in very old, very metal poor stars whose surfaces may still reflect the original composition of the material from which the stars formed. Such stars may provide an almost unique opportunity to measure directly the primordial abundance of an element produced in the Big Bang.

J. Thorburn (U. of Chicago/Yerkes Obs.) recently completed aseries ofobservations ofthe6707 Alithium feature in extremely metal poor main sequence stars for her thesis. Spectra were obtained primarily on two telescopes at KPNO: the 2.1-m telescope with the Coude" spectrograph and the 4-m telescope and echelle spectrograph. The mean lithium abundance of the extremely metal poor subdwarfs (i.e., those more metal poor than [Fe/H]=-2.2 compared to the Sun) is N(Li) = 12 + log(Li/H) = 2.32 ± 0.02, nearly a factor of 10 below the solar system value. The data also show a larger dispersion in the lithium abundance than can be explained simply as observational uncertainty. The observations may suggest a slight decline in the abundance of lithium with declining temperature, even among the warmest subdwarfs previously thought to demonstrate a more or less constant lithium abundance with temperature. Furthermore, the data suggest a trend of declining lithium abundance in the most metal poor stars of the sample, which may indicate some contribution of Galactic production of lithium even in the oldest stars observed in the Galaxy. The abundance of lithium actually produced in the Big Bang may be estimated from these observations to be N(Li) = 2.2 ± 0.2.

2. NGC 6611: A New Star Cluster Caught in the Act of Formation

Much effort has gone into the characterization of the numbers of massive stars contained in young associations of stars in the Milky Way and in the Magellanic Clouds in order to begin to understand the relative fraction of stars of different mass which might be formed in different astrophysical environments (i.e., the initial mass function). Despite the difference in overall metal abundance between the Milky Way and the more metal poor Magellanic Clouds, the highest mass stars seen in each region all have about the same mass, about 80 solar masses. Evidence also suggests that not all stars in a given association of massive stars are strictly coeval, but rather that star formation may have occurred over some period of time.

The youngest Galactic clusters of stars still contain stars young enough to retain circumstellar disks left from the process of star formation. Such disks around the more massive young stars contain more mass, are larger in size, accrete material more rapidly, and dissipate more quickly than disks around less massive stars. Recent thesis work by L. Hillenbrand (U. of Massachusetts) has concentrated on understanding the role that disks play in star formation and the evolution of circumstellar disks in young stars. These efforts were recently combined in a definitive study of the young cluster NGC 6611, part of the Ser OBI Association, using optical and infrared photometry and spectroscopy with the KPNO 0.9-m telescope and a Tektronix 2040 x 2048 CCD, the KPNO 1.3-m telescope and the Simultaneous Quad-color Infrared Imaging Device (SQIID), and the KPNO 4-m telescope with the Hydra fiber positioner and multi-object spectrograph. The physical HR Diagram (luminosity versus temperature) of the cluster shows a strong population of high mass stars and an age of roughly two million years. The cluster also contains a significant number of intermediate mass stars (3-8 solar masses) still in the stage of formation, with ages from possibly as young as 0.25 million years to at least one million years of age. Many of the stars show emission lines similar to the classical Be/Ae stars. Hillenbrand, Massey, S. Strom (U. of Massachusetts) and K.M. Merrill (NOAO) conjecture that these may be young stars whose circumstellar disks may have become optically thin, rather than slightly evolved stars undergoing mass loss (the traditional interpretation). They also find a number of stars that appear to be surrounded by optically thick circumstellar accretion disks. Such objects are rare, and their observations imply that the disk survival times around intermediate and higher mass stars are much shorter that those around lower mass stars. The combination of a population of massive stars with intermediate mass stars still in the late stages of star formation in a single cluster provides a rare and detailed glimpse at the process of star formation itself.

3. Dusty Emission Filaments in M87: Probing the History of the Intracluster Medium

Optical emission line filaments have been known to occur in the cores of clusters of galaxies for many years. The connection between these optical emission line systems and the surrounding intracluster medium (ICM), however, is still poorly understood. Initially, the observed optical filaments were believed to be condensing out of the surrounding hot, X-ray emitting gas, perhaps as the result of thermal instabilities in a "cooling flow," which X-ray observations have implied to exist in many cluster cores. If this proposed origin is correct, these systems provide an opportunity to constrain the evolution of the ICM and establish the end products of the material which X-ray observations imply are cooling in these objects. Alternatively, these emission line systems may represent the remnants of past stripping or merger events among the constituent cluster galaxies; in which case, their properties can provide insight into the efficiency and history of such processes in the cluster. Finally, many of the central galaxies in clusters contain strong sources of nuclear activity and this activity has been suggested as a possible excitation mechanism for the observed optical emission from the filaments. Consequently, these filament systems may yield clues to the interaction between non-thermal nuclear processes and the surrounding ICM.

The proximity of M87, which exhibits a strong optically emitting filament system to the Galaxy, makes it an ideal object to investigate these questions in detail. Numerous studies at a variety of wavelengths have been undertaken. One such study has recently been completed by W.B. Sparks (STScI), H.C. Ford (Johns Hopkins U.), and A.L. Kinney (STScI). Using the narrow-band imaging and spectroscopy obtained with the KPNO 4-m telescope, as well as continuum imaging from the ESO 3.6-m, these investigators have studied the dust contents of the optical filament system in M87. Constraining the dust content in these systems is important since the existence and persistence of dust has strong implications for both the origin and physical state of the gas in the filaments. Sparks and collaborators confirm that the observed emission line gas is dusty and estimate that the dust-to-gas ratio is consistent with, or slightly higherthan, typical galactic values. Analysis of the velocity field indicates that the optical line emission from material near the nucleus is outflowing, while emission from material farther out from the nucleus is apparently inflowing. The authors advance the idea that the observed optical filament system represents the remnant of the capture of a small, dusty, gas-rich dwarf galaxy. Alternatively, if the filaments represent the products of cooling in the hot, X-ray emitting plasma, then cooling must have proceeded to the point where dust has been able to form. Although this project cannot definitely rule out either scenario, such observations, both for M87 and other opticalfilament systems, providean importantmeans of probingthe environment in cluster cores.

C. National Solar Observatory

1. Solar Oscillations and Atmospheric Structures

L. November (NSO/SP) is completing a study of the spatial distribution of power and phase of solar oscillations from a high-resolution Vacuum Tower Telescope data set. A four-hour time series of quiet Sun at disk center in a 3 arcminute, 2D field was obtained with 1-minute temporal sampling, using the UBF and branch filters. The data contain intensity measurements in three continuum windows, in Fe I 5576 A, Fe I 5434 A, Mg B2 5173 A, Na D2 5890 A, the CN band head 3883 A, the Ca K core, and in Ha, as well as Doppler velocity in four lines (Fe I 5576 A, FeI 5434 A, Mg B2 5173 A) and in Ha, and longitudinal magnetic field from Ca I 6102 A. The sampling resolution was 0.3 arcsecond and the data were correlation tracked to remove the average image motion. Fourier analysis in time at each spatial location was applied to study the spatial distribution of the power and phase in the range of frequencies DC to 7 mHz. The power and phase differences were smoothed in frequency by convolution with a 1 mHz Gaussian window. This new method, which allows us to distinguish atmospheric phenomena from wave- mode interference effects, has given a reliable way to understand the relation between the wave modes and structures in the solar atmosphere. The spatial maps of power and phase difference give the following results:

1) A decrease of power above 3 mHz is seen in the network magnetic points at all heights. In the photosphere the relative power decrease is small, < 10%, but at the temperature minimum and above it is quite large, > 80%. The effect is interpreted as due to absorption of p-mode energy at the magnetic field elements, which is consistent with what is seen in sunspots. The area of regions of decreased power increases substantially with height as we would expect for the spreading of magnetic field with height in the atmosphere. The strong height variation of the attenuation indicates that p-mode absorption by magnetic fields must be mainly a chromospheric phenomenon.

2) The frequency-smoothed intensity-velocity phase difference above 3 mHz shows that intensity and velocity are approximately in phase in the magnetic points at all heights, and intensity leads velocity by about 90° outside the magnetic points. At higher frequencies the p-modes become more in-phase at all heights and at all spatial positions. The phase difference seen in quiet Sun above 3 mHz indicates that these p-modes are upwardly propagating adiabatic modes. The wave character is substantially modified in magnetic regions, consistent with nonadiabatic modes. The high-frequency modes may not be sufficiently resolved in phase to permit a valid interpretation of those phase differences. 3) Rings of increased power appear around the magnetic points which are strongly attenuated at the temperature minimum above 5 mHz. There is an associated phase difference of intensity leading velocity by about 90° in the bright rings. The bright rings are interpreted to be direct evidence for scattering of p-modes by magnetic flux tubes.

4) There is a large relative excess of power in Ha at frequencies below 3 mHz around the network magnetic points with a 90° intensity-velocity phase lead. This observation rules out the possibility that the enhanced low-frequency power is due to a mechanical motion of the fibrils. November interprets this as evidence for adiabatic waves of magnetic or g-mode type in magnetic points in the chromosphere.

2. Flare-like Phenomena in High Coronal Loops

Localized interactions of coronal loops have been recorded in the emission of the Fe XIV line at 5303 A, and the emission of the Fe X line at 6374 A by R. Smartt (NSO/SP) and colleagues. The interactions are evident as transient brightenings in the emission where two loops came into contact. The observations are interpreted as a process of localized loop coalescence involving partial magnetic reconnection. The heating and subsequent cooling of the plasma in the region of interaction appears to have flare-like characteristics. Cooling of the plasma as observed in the green-line emission (characteristic temperature -2 x 106 K) results in a delay in the observed maximum brightness of the red-line emission (characteristic temperature -1 x 10 ), following a maximum in the green-line emission, by about 9 minutes on average. Key plasma processes involved in such interactions remain uncertain without complementary radio and short- wavelength data. However, X-Q. Li (Purple Mountain Obs., Nanjing, China), Z. Zhang (Dept. of Astronomy, Nanjing U., Nanjing, China) and Smartt have investigated the phenomenon in terms of the interaction between the magnetohydrodynamic and high frequency plasma waves, and the instability associated with an electromagnetic solitary wave in a current sheet. It is shown that there is a resistive instability, which eventually turns into an eruptive instability at the onset of the magnetic field reconnection. The numerical results are found to be consistent with typical times for these events as recorded in the observations.

3. Research in Local Helioseismology

C. Lindsey (NSO/T/SPRC) is carrying out a program in "local helioseismology," with collaborators D. Braun (coming to NSO from Hawaii) and S. Jefferies (working at NSO through the Bartol Research Institute at the U. of Delaware). The project grew out of the discovery by Braun, Duvall and LaBonte that sunspots absorb acoustic waves. This result raised the possibility, suggested by Lindsey and Braun, that sunspots could produce acoustic deficits at their antipodes that would allow them to be detected on the far-side surface.

Acoustic power maps that Lindsey and his colleagues made in various spatial and temporal passbands from the NSO-Bartol-NASA South Pole helioseismic observations of 1987 and 1988 have shown no evidence of antipodal images, as yet. However, they have shown other interesting features suggesting the signature of subsurface magnetic structure interacting with acoustic waves. These include strong halos of high- frequency (=6 mHz) acoustic power in the quiet Sun surrounding all active regions. Less frequently, mainly in the 1987 South Pole observations, they show long filamentary shadows, "fingers," in 3 mHz acoustic-power maps stretching across the solar equator that tend to connect surface magnetic regions in opposing active-region bands. These features persist for days, rotating with the Sun. Lindsey and his colleagues suspect that they are the surface manifestation of wave absorption by subsurface magnetic structures. Similar features are now being reported by other groups.

The trans-equatorial fingers suggest very surprising-if only occasional-instances of global magnetic structures lying only a few thousand kilometers beneath the photosphere that show no evidence of having become wrapped up by differential rotation. This extremely puzzling prospect, if borne out, is certain to be important and could be closely related to the mechanism of the solar dynamo. The general implications of direct subsurface magnetic absorption manifested at the surface would be extremely broad. They include the possibility of straightforward techniques in computational holography that would allow us to extrapolate acoustic power maps thousands of kilometers beneath the surface. The possibility of acoustically examining subsurface structure could make local helioseismology a powerful new field. It may even help us to understand the more general question of how stellar dynamos and activity cycles operate.

III. PERSONNEL AND BUDGET STATISTICS, NOAO

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

NOAO facility arrived name institution visited 4/01/93 Igor Antokhin University of Montreal CTIO 5/01/93 Rob Rutten Sterrekundig Institut NSO/Sunspot 5/15/93 Nick Hoekzema Sterrekundig Institut NSO/Sunspot 6/01/93 Elliotte Harold New Jersey Institute of Technology NSO/Sunspot 6/01/93 Thomas Rimmele New Jersey Institute Of Technology NSO/Sunspot 6/02/93 Victor Afansiev Special Astrophysical Observatory of Russian Academy of Science KPNO 6/02/93 Valeriy Vlassyuk Special Astrophysical Observatory of Russian Academy of Science KPNO 6/03/93 Griet Van de Steene Kapteyn Astronomical Institute KPNO 6/26/93 Iraida Kim Sternberg Astronomical Institute NSO/Sunspot

B. New Hires

date name position NOAO division 4/19/93 Jeff Lewis Scientific Programmer II NOAO

C. Change in Status

date name position NOAO division 5/01/93 Melissa Collier Visitor Center Supervisor to Museum Administrator KPNO 5/24/93 Taft Armandroff Assistant Astronomer to Associate Astronomer KPNO D. Terminations date name position NOAO division 5/04/93 Frank Hegwer Assistant to Director/Director Administrative Services, NSO/SP NSO/Sunspot

E. Summer Research Assistants arrived name institution facility visited

5/17/93 Brent Ballard Miami University NSO/Tucson 5/17/93 Steve Doinidis New Mexico State University NSO/Sunspot 5/18/93 Pamela Baugus Rhodes College NSO/Tucson 5/18/93 Wendy Forrester Smith College KPNO 5/18/93 Jennifer Regan Miami University NSO/Sunspot 5/19/93 Andrew Dombard Haverford College NSO/Sunspot 5/24/93 Anastasia Alexov Wesleyan University KPNO 5/24/93 Tracey Buettgens University of Rochester CCS 5/24/93 Douglas Hott Bradley University NSO/Tucson 5/24/93 Daniel Engfer University of Texas NSO/Sunspot 5/24/93 Amy Lesser Mt. Holyoke College KPNO 5/25/93 Jennifer Heath Whitman College NSO/Tucson 5/27/93 Carlos Cortes Vassar College KPNO 6/01/93 Donald Stanchfield University of Rochester NSO/Tucson 6/02/93 Lynn Weller University of Arizona KPNO 6/02/93 Stephen Gallo State U. of New York, B inghamton NSO/Sunspot 6/07/93 Bernard Reger State U. of New York, Binghamton NSO/Sunspot 6/07/93 Gordon Richards Princeton University NSO/Sunspot 6/16/93 Mark Robison University of Minnesota NSO/Tucson 6/21/93 Lance Lones University of California, San Diego NSO/Tucson 6/22/93 Pietro Bernasconi ETH-Zentrum NSO/Sunspot

F. Gemini 8-m Telescopes Project

Terminations date name position 5/28/93 John Morton Administrative Manager 8-m

Change of Status date name position 6/01/93 Jacobus Oschmann Systems Engineer to Acting 8-m Project Manager G. Chilean Economic Statistics

%Change Avr. monthly FY 1993: Month inCPI Pesos/Dollars April 1.4 203.38 May 1.5 206.35 June 0.5 207.37

H. NSF Foreign Travel Fund

For the quarter 1 April through 30 June 1993, a total of $1,247.00 was paid out of the NSF Foreign Travel account for visits to the following sites and institutions:

Las Campanas Observatory, La Serena, Chile; Canada-France-Hawaii Telescope, Hawaii. APPENDIX A

Telescope Usage Statistics

April - June 1993

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

4-m 1087.9 583.4 121.1 300.7 25.7 57.0

1.5-m 1074.0 607.5 69.0 370.5 -0- 27.0

1-m 890.3 290.8 104.0 447.3 10.6 37.6

CTIO 0.9-m 1072.9 538.8 176.3 291.1 12.7 54.0

*0.6/0.9-m 540.0 219.9 82.6 185.0 28.0 24.5

0.6-m 567.1 247.3 -0- 307.1 12.7 -0-

4-m 712.0 425.47 124.03 65.75 16.25 80.5

2.1-m 841.5 590.53 135.47 66.5 15.5 33.5

Coud6 Feed 744.31 409.68 248.48 70.35 4.5 11.3

KPNO 1.3-m 903.65 519.13 86.82 151.15 23.95 122.6

0.9-m 816.5 478.72 141.33 90.4 43.8 62.25

Schmidt 455.1 268.2 79.3 89.6 18.0 -0-

Hilltop Dome 2099.0 451.0 1223.0 389.0 36.0 -0-

Vac. Tower/SP 1032.0 343.0 402.0 214.0 3.0 70.0

Evans Facility 2109.0 588.0 1015.0 475.0 23.0 8.0

NSO **FTS Lab 260.0 180.0 -0- -0- -0- 80.0

**McMafh-Pierce 2016.0 992.0 456.0 311.0 257.0 -0-

Vacuum/KP 777.0 208.0 418.0 107.0 44.0 -0-

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

April 11.5 hours/night; May 12.1 hours/night; June 12.4 hours/night.

* Use restricted to dark of the moon.

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

Cerro Tololo Inter-American Observatory

January - March 1993: 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. A total of 75 programs were carried out during this quarter.

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

J. Baldwin (CTIO), K. Lanzetta (U. of California, San Diego), D. Bowen (STScI): "The Kinematic Structure of z = 0.5 Galaxy Halos." 2(17)4-m

J. Baldwin (CTIO), B. Wills, D. Wills (U. of Texas), H. Netzer (Tel Aviv U.), G. Feriand (U. of Kentucky): "The Inner Regions of Quasars." 4(44)4-m, l(10)0.9-m

J. Baldwin (CTIO), H. Netzer (Tel Aviv U.), G. Feriand (U. of Kentucky), B. Wills, D. Wills (U. of Texas): "Physics of the Narrow Line Region." 2(20)4-m

H. Bond (STScI), S. Kawaler (Iowa State U.): "A Search for Radial Pulsations of White Dwarfs." 3(28)4-m

N. Caldwell (U. of Arizona), R. Schommer, A. Walker (CTIO), J. Graham (Carnegie Inst, of Washington): "Cepheid Distances to Centaurus Group Galaxies." 2(16)4-m

L. Campusano (U. de Chile), R. Clowes (U. of Central Lancashire, U.K.): "Quasar Groups in the Universe: Last Step for a New Diagnostic on the Largest and More Distant Known Group (~200H"'Mpc at z=1.3). 3(28)4-m

J. Claria\ A. Piatti* (Obs. Astron6mico de Cdrdoba, Argentina), M. Lattanzi (STScI): "UBV and Washington Photometry of Southern Open Ousters." 5(32)l-m, 7(38)0.6-m

W. Craig*, S. Kahn (U. of California, Berkeley), J. Hester (Arizona State U.), J. Raymond (Harvard- Smithsonian): "Emission Line Imaging of the Vela Supernova Remnant." 7(62)1.5-m

A. Crotts, J. Xu* (Columbia U.): "Dynamics and Three-Dimensional Structure of the Interstellar Medium Around SN1987A." 2(16)4-m

R. de Souza, S. dos Anjos, R. de Carvalho (U. de Sao Paulo, Brazil): "Galaxies with Box-Shaped Bulges." 4(30)1.5-m, 4(42)0.9-m

R. Elston (CTIO), P. McCarthy (Carnegie Inst, ofWashington), P. Eisenhardt, N. Lu (Jet Propulsion Lab.): "IR Spectroscopy of High Redshift Radio Galaxies." l(12)4-m Mar#514

D. Forbes (Memorial U., Canada): "Age Spread and Initial Mass Function of Young Open Clusters." 8(77)1-m A. Fullerton (U. of Delaware), R. Prinja (U. Coll. London, U.K.), D. Massa (Applied Research Corp.): "Nonradial Pulsations in B Supergiants: The Seeds of Stellar Wind Variability?. 6(55)1.5-m

J. Gallagher, L. Matthews (U. of Wisconsin), J. Littleton (West Virginia U.): "CCD Photometry of Low Surface Brightness Southern Dwarf Irregular Galaxies." 4(36)0.9-m

J. Gallagher (U. of Wisconsin), D. Hunter (Lowell Obs.): "Search for Giant Ionized Structures in the ISM of Irregular Galaxies." 3(27)1.5-m

D. Geilser (CTIO): "Faint Washington CCD Standard Fields." 8(35)0.9-m

M. Hamuy, N. Suntzeff, M. Phillips (CTIO): "Southern Spectrophotometric Standards." 1(9)1.5-m

W. Harris, J. Seeker* (McMaster U., Canada), D. Geisler (CTIO): "The Globular Cluster System of the cD Galaxy NGC 3311." 2(16)4-m

P. Hartigan (U. of Massachusetts): "Where are the Low Mass Stars in Dark Clouds?." l(5)4-m

W. Hartkopf, H. McAlister, W. Bagnuolo, D. Barry*, B. Mason, N. Turner*, H-H. Fu* (CHARA): "Speckle Interferometry and Photometry of Close Binary Stars." 4(40)4-m

R. Havlen (ASP): "Characteristics of Third Quadrant OB Associations." 3(33)0.9-m

S. Hawley (L. Livermore National Lab.), I. Reid (Caltech): "Basic Data for Nearby Stars." 4(42)1.5-m

S. Hawley (L. Livermore National Lab.), I. Reid (Caltech): "The Magnetic Activity of Low Mass Stars in Open Clusters." 2(21)4-m

J. Hughes, P. Hartigan, S. Strom (U. of Massachusetts): "Disk Accretion in the Lupus and Chamaeleon Dark Clouds." 2(21)4-m

D. Hunter (Lowell Obs.): "Physical Characteristics of Gas Interacting with Massive Stars in the LMC." 4(38)4-m, 4(36)0.9

D. Hunter (Lowell Obs.), J. Gallagher, C. Anderson (U. of Wisconsin): "The Stellar Population of Constellation III: Case Study of A Star Burst." 3(27)0.9-m

S. Johnson (Idaho State U.), M. Joner (Brigham Young U.), M. P6rez, A. Mitchalisianos (NASA, Goddard), P. The' (U. of Amsterdam, The Netherlands): "The Characterization of the Blueing Effect in Massive PMS Stars and Photometric Observations of MWC 560." 8(68)0.6-m

A. Layden (CTIO): "Statistical Parallax of Field RR Lyrae Stars & Field RR Lyrae Near the Galactic Plane." 5(50)1-m

A. Layden, C. Smith (CTIO): "Photometry of RR Lyraes and a Search for Supernovae in Starburst Galaxies." 2(17)0.9-m M. Lehnert, T. Heckman (Johns Hopkins U.): "The Ionization of the Halos of Starburst Galaxies." 3(32)4-m

G. Mackie (Harvard Smithsonian), A. Stanford (U. of California, Berkeley): "A Dynamical Study of Advanced Merger Galaxies: the Fundamental Plane." 2(22)4-m

S. Marchenko (Inst, de Astronomfa, Mexico), A. Moffat, R. Lamontagne, I. Antokhin, J. Bertrand*, J. Matthews (U. of British Columbia, Canada): "An Intense Photometric Study of the Variable Wolf-Rayet Stars of Type WN8." 43(355)0.6-m

J. Maza, M. Wischnjewsky, R. Antezana (U. de Chile), M. Hamuy, N. Suntzeff, M. Phillips, L. Wells, R.C. Smith, M. Navarrete, G. Valladares (CTIO): "A Search for Supernova." 7(64)0.9-m

J. Maza, M. Wischnjewsky (U. de Chile): "Bright Quasars at High Redshift." 6(63)1.5-m, 6(38)CS

J. Maza, M. Wischnjewsky, R. Antezana, P. Lira* (U. de Chile), M. Hamuy, N. Suntzeff, M. Phillips, C. Smith, R. Aviles, M. Navarrete, G. Valladares (CTIO): "A Search for Supernovae." 2(13)4-m, 1(9)1.5-m, 5(49)0.9-m, 13(82)CS

J. McClintock (Harvard Smithsonian), C. Bailyn (Yale U.), R. Remillard (MIT): "Dynamical Studies of Black Hole Binaries." 2(20>4-m

J. Middleditch (Los Alamos National Lab.), T. Sasseen, C. Pennypacker, R. Muller, S. Perlmutter (U. of California, Berkeley), G. Fazio, S. Ranson* (HarvardSmithsonian), W. Kunkel, J. Kristian (Carnegie Inst, of Washington) "Confirmation/Timing of the 2.1 MS Candidate in SN1978A." 2(18)4-m

A. Moffat, N. St-Louis, J. Matthews (U. de Montreal, Canada), N. Walborn (STScI): "Measuring the Masses of the Most Massive Stars." 4(37)4-m

J. Morse (STScI), P. Winkler (Middlebury Coll.), R. Kirshner, J. Raymond (Harvard Smithsonian): "Area Spectrophotometry and Kinematics of Supernova Remnants: Explosions from Massive Stars and Interactions of the Debris with the ISM." 3(28)4-m

J. Mould (Caltech), R. Schommer (CTIO): "An Investigation of the Peculiar Velocities of Clusters of Galaxies." 3(31)1.5-m

B. Patten*, T. Simon (U. of Hawaii): "CCD Photometry of X-ray Sources in IC 2391." 4(44)0.9-m

B. Patten*, T. Simon (U. of Hawaii): "Rotation Periods of Young Spotted Stars in the Chamaeleon I Dark Cloud." 11(84)1-m

J. Patterson, H. Richman*, E. Thomas*, E. Sterner, L. Cantor*, D. Flax* (Columbia U.): "Periodicities from He II." 32(275)1-m, 7(47)0.6-m

B. Penprase (Caltech), E. Albert (US Naval Academy), J. Blades (STScI), B. Welsh (NASA, Headquarters): "Spectroscopic Observations of Nearby High Velocity Clouds." 3(26)1.5-m, 2(19)l-m M. Phillips, R. Williams, N. Suntzeff, J. Elias, M. Hamuy, R.C. Smith, G. Valladares, L. Wells (CTIO): "Spectral and Photometric Evolution of Supernova and Novae." 3(26)4-m, 2(19)1.5-m, 5(40)0.9-m

J. Powell*, M. Joner (Brigham Young U.): "MetallicityGradient in the Disk from uvby-^-Ca Photometry of Supergiant Stars." 10(61)0.6-m

R. Rood (U. of Virginia), R. Peterson (Lick Obs.): "A Dynamical Comparison of Red and Blue Horizontal Branch Stars in NGC 2808." 3(36)4-m

K. Roth, D. Meyer (Northwestern U.): "High Resolution Observations of the QSO 0551-266." 2(17)4-m

M.T. Ruiz (U. de Chile), P. Bergeron (U. de Montreal, Canada), S. Leggett (US. Naval Obs.): "Study of Cold White Dwarfs." 3(28)4-m, 4(38)1.5-m

S. Ryan (U of Texas), C. Deliyannis (U. of Hawaii): "Lithium Abundances in Halo Dwarfs: Comparison with Rotational Models." 4(36)4-m

J. Schachter, M. Elvis, J. Huchra, J. Grindlay (Harvard-Smithsonian): "Broad Band Photometry of Southern Slew Survey Sources, Part 2 of 2." S.O.(8)CS

J. Schachter, M. Elvis, J. Huchra (Harvard-Smithsonian): "Optical Counterparts of Southern High-Latitude Einstein Slew Survey Sources." 5(46)1.5-m

B. Schaefer, D. Palmer, T. Cline (NASA, Goddard), K. Hurley (U. California, Berkeley), J. Laros (Los Alamos National Lab.), J. Fishman, C. Kouveliotou (NASA, Marshall Space Flight Ctr.): "Infrared Counterparts of Gamma Ray Bursts." 4(39)1.5-m

B. Schaefer, D. Palmer, T. Cline (NASA, Goddard), K. Hurley (U. California, Berkeley), J. Laros (Los Alamos National Lab.), J. Fishman, C. Kouveliotou (NASA, Marshall Space Flight Ctr.): "Optical Counterparts of Gamma Ray Bursts." 3(29)0.9-m

E. Schlegel (NASA, Goddard), R. Fesen (Wilder Lab.), M. Phillips, C. Smith (CTIO): "The Optical Recovery of Supernovae 1986G, 1972E, and 1895A." l(7)4-m

P. Schmidtke, A. Cowley (Arizona State U.), J. Hutchings, D. Crampton (Dominion Astrophys. Obs., Canada): "Photometric Identification of LMC X-ray Sources using ROSAT Positions." 4(45)0.9-m

H. Schmitt*, T. Storchi-Bergmann, M. Pastoriza (UFRGS, Brazil): "Spectroscopy and Imaging ofSouthern Active IRAS Galaxies." 3(28)1.5-m, 5(42)1-m

P. Seitzer (U. of Michigan), R. Reijns*, T. de Zeew, R. Le Poole (U. of Leiden, Netherlands), K. Freeman (Mt. Stromlo & Siding Spring Obs., Australia), T. Ingerson (CTIO): "The Kinematics of Omega Centauri." 5(48)4-m A. Smette* (European Southern Obs., Chile), G. Williger (CTIO), J. Surdej (U. de Liege, Belgium), P. Shaver (European Southern Obs., Germany), G. Robertson (U. of Sydney, Australia): "Sizes of Ly-a Clouds." 2(24)4-m

J. Smith*, T. Oswalt (Florida Inst, of Tech.), S. Leggett (US. Naval Lab.): "Photometry of White Dwarfs in Wide Binaries." 4(39)1.5-m, 6(43)0.9-m

R. Smith (CTIO), P. Winkler (Middlebury Coll.): "Imaging and Spectroscopy of "Forgotten" LMC Supernova Remnants." 2(19)4-m

R. Smith (CTIO): "Wide-field Imaging of the Vela Supernova Remnant." 6(63)CS

A. Stanford (U. California, Berkeley), G. Mackie (Harvard-Smithsonian): "Optical Imaging of Merger- Candidate Galaxies." 2(21)0.9-m

M. Strauss (Inst, for Advanced Study), B. Santiago* (U. California, Berkeley), 0. Lahav (U. Cambridge, U.K.), J. Huchra (Harvard-Smithsonian): "A Whole-Sky Redshift Survey of Optically Selected Galaxies." 5(43)1.5-m

N. Suntzeff(CTIO), V. Smith (U. of Texas),P. Bouchet(European Southern Obs., Chile): "TheKapteyn's Star Group: A Disrupted Galactic Globular Cluster?." 4(36)1.5-m

W. Sutherland (U. California, Berkeley), W. Saunders, G. Efstathiou, S. Maddox (Oxford U., U.K.), M. Rowan-Robinson (Queen Mary College, U.K.), C. Frenk (Durham U., U.K.), R. McMahon, S. White (Cambridge U., U.K.): "The IRAS 0.6 Jansky Redshift Survey." 7(68)1.5-m

A. Walker (CTIO): "Horizontal Branch Evolution and Pulsation Study." 4(38)0.9-m

G. Wallerstein, J. Brown (U. of Washington): "Abundances in the Most Distant Open Cluster: Tombaugh 2." 3(25)4-m

E. Wilcots, P. Hodge (U. of Washington): "Evolution of HII Regions in the Large Magellanic Cloud." 5(44)1.5-m, 7(64)l-m, 3(21)0.9-m

P. Winkler, C. Bevin* (Middlebury Coll.), R.C. Smith (CTIO): "Discovering Supernova Remnants in the Magellanic Clouds." 4(37)1.5-m

P. Winkler,G. Hanson (MiddleburyCollege), R. Petre (NASA, Goddard): "Wide-FieldImaging of Puppis A and SN 1006 in Nebular and Coronal Lines." 6(43)CS

S. Zepf (U. of Durham, U.K.), D. Geisler (CTIO), K. Ashman (U. of Toronto, Canada): "Merger Signatures in the Globular Cluster Systems of Ellipticals." l(7)4-m

MICHIGAN PROGRAM

P. Seitzer, R. Pildis* (U. of Michigan): "Michigan Program." 13(113)CS YALE PROGRAM

S. Cersosimo*, R. Zinn, D. Tucker*, G. Oemler, X. Guo*, W. van Altena, B. Chaboyer*, C. Bailyn, R. M6ndez, R. Koopman*, E. Rubenstein, J. Kennedy, P. Demarque. 18(181)0.9-m Executed Proposals 04/01/93 - 06/30/93 Page 1 Fri Jul 16 14:48:50 1993

Nights Hours Days Hours 662 2 s93 H Abt, D Willmarth, National Optical Astronomy Observatories Are All A-Type Slow Rotators Abnormal or Binaries? Coude Feed 6.00 55.00 0.00 0.00

10086 2 s93 H Abt, National Optical Astronomy Observatories The Binaries in the Coma and Praesepe Clusters Coude Feed 6.00 57.50 0.00 0.00

832 2 s93 E Ajhar, National Optical Astronomy Observatories Age and Metallicity from Surface Brightness Fluctuations .. 0.9 meter 2.00 18.00 0.00 0.00

691 8 s93 T Armandroff, National Optical Astronomy Observatories E Olszewski, University of Arizona C Pryor, Rutgers University Structural Parameters of the Draco and Ursa Minor Dwarf.... 0.9 meter 5.50 38.30 0.00 0.00

702 8 s93 T Armandroff, National Optical Astronomy Observatories E Olszewski, University of Arizona C Pryor, Rutgers University M Irwin, University of Cambridge The Mass-to-Light Ratios of the Draco and Ursa Minor.... 4 meter 3.50 30.00 0.00 0.00

727 7 s93 J Baldwin, G Feriand, -, National Optical Astronomy Observatories D Wills, B Wills, University of Texas, Austin H Netzer, Tel Aviv University The Inner Regions of Quasars 2.1 meter 4.00 37.00 0.00 0.00 Executed Proposals 04/01/93 - 06/30/93 Page 2 Fri Jul 16 14:48:50 1993

Nights Hours Days Hours 9129 0 s93 T Boroson, National Optical Astronomy Observatories A Wolfe, University of California, San Diego The HII Extent of Spiral Galaxies Burrell Schmidt 5.00 8.00 0.00 0.00

622 7 s93 M Carini, D Weinstein, NASA Goddard Space Flight Center J Noble, Georgia State University A Search for Microvariability in Selected Seyfert Galaxies 0.9 meter 4.00 29.00 0.00 0.00

747 9 s93 R Ciardullo, J McMillan, Pennsylvania State University G Jacoby, National Optical Astronomy Observatories PN as Standard Candles: Comparison with Other Distance.... 4 meter 3.00 26.50 0.00 0.00

711 4 s93 P Conti, V Robledo-Rella, University of Colorado Galactic HII Regions and the Teff of the Exciting Stars 0.9 meter 5.50 44.75 0.00 0.00

677 2 s93 M Corwin, B Carney, J Fulbright, R Harvey, University of North Carolina D Latham, Harvard-Smithsonian Center for Astrophysics R Jones, Fayetteville State University RR Lyraes and the Structure of Horizontal Branch Stars 1.3 meter 5.00 38.30 0.00 0.00 0.9 meter 6.00 64.50 0.00 0.00

752 2 s93 S Edwards, Smith College K Hinkle, National Optical Astronomy Observatories M Meyer, S Strom, J Carpenter, L Hillenbrand, M Skrutskie, L Ghandour, A Cannon, University of Massachusetts FTS H Band Spectral Classification for Embedded YS0'S 4 meter 3.00 33.00 7.00 23.00 Executed Proposals 04/01/93 - 06/30/93 Page 3 Fri Jul 16 14:48:50 1993

Nights Hours Days Hours 641 2 s93 F Fekel, NASA Marshall Space Flight Center Spectroscopy of Binary and Multiple Stars Coude Feed 5.00 48.00 0.00 0.00

802 8 s93 A Ferguson, R Wyse, Johns Hopkins University J Gallagher, University of Wisconsin The Outer Disks of Galaxies: Stellar Populations 0.9 meter 4.00 32.60 0.00 0.00

770 .1 s93 R French, S Maene, E Mason, C McGhee, Wellesley College E Dunham, NASA Ames Research Center M Buie, Lowell Observatory J Goguen, Jet Propulsion Laboratory 13/14 April 1993 Stellar Occultation by Uranus and Its 2.1 meter 1.00 8.00 0.00 0.00

610 4 s93 G Fuller, National Radio Astronomy Observatory P Myers, E Lada, Harvard-Smithsonian Center for Astrophysics The Internal Structure of the Dense Cores in L673 2.1 meter 4.66 28.50 0.00 0.00

734 4 s93 I Gatley, K Merrill, National Optical Astronomy Observatories J Kastner, Haystack Observatory IR Emission Line Images of Photodissociation Regions in M17 1.3 meter 3.00 15.00 0.00 0.00

735 3 s93 I Gatley, K Merrill, National Optical Astronomy Observatories Molecular Hydrogen Emission Line Images of the Galactic... 1.3 meter 3.00 32.50 0.00 0.00 Executed Proposals 04/01/93 - 06/30/93 Page 4 Fri Jul 16 14:48:50 1993

Nights Hours Days Hours 728 2 s93 A Grauer, University of Arkansas R Green, National Optical Astronomy Observatories Time-Series Photometry of Cool Stars 0.9 meter 4.00 34.00 0.00 0.00

831 4 s93 R Green, National Optical Astronomy Observatories B Jannuzi, D Schneider, J Bahcall, Institute for Advanced Study V Mader, University of Arizona The Connection Between Galaxies & Quasar Absorption Lines 4 meter 2.70 2 6.00 0.00 0.00

794 l9 s93 R Griffiths, Johns Hopkins University R Green, National Optical Astronomy Observatories J MacKenty, K Ratnatunga, Space Telescope Science Institute V Mader, University of Arizona SQIID Observations of HST Medium-Deep Survey Fields 4 meter 2.00 17.00 0.00 0.00

700 4 s93 J Hackwell, D Lynch, R Russell, R Poole, T Tessensohn, Aerospace Corporation E Churchwell, University of Wisconsin, Madison 3 to 13.5 Spatial and Spectral Studies of Compact HII.... 1.3 meter 5.00 54.10 0.00 0.00

624 2 s93 E Halbedel, Corralitos Observatory A Study of H-Alpha Spectra in Ae and a Shell Stars II Coude Feed 5.00 31.00 0.00 0.00

725 4 s93 I Hawkins, N Craig, University of California, Berkeley Probing Shock Models of CH+ Formation Coude Feed 5.00 48.00 0.00 0.00 Executed Proposals 04/01/93 - 06/30/93 Page 5 Fri Jul 16 14:48:50 1993

Nights Hours Days Hours 745 8 s93 P Hickson, C Mendes de Oliveira, University of British Columbia J MacKenty, Space Telescope Science Institute JHK Surface Photometry of Elliptical Galaxies in Compact... 1.3 meter 5.00 57.00 0.00 0.00

738 2 s93 K Hinkle, L Wallace, D Stultz, National Optical Astronomy Observatories G Wiedemann, European Southern Observatory A 1-5 Micron Infrared Atlas of Arcturus 4 meter 3.00 36.00 3.00 2.00

825 4 s93 P Hofner, S Kurtz, E Churchwell, S Sadicario, University of Wisconsin, Madison J Hackwell, R Russell, M Chatelain, D Lynch, Aerospace Corporation The Dust Shells Around Newly Formed Massive Stars 1.3 meter 5.00 41.75 0.00 0.00

697 2 s93 B Hufnagel, G Smith, University of California, Santa Cruz Chemical Evolution of the Galactic Open Cluster System 2.1 meter 4.80 41.50 0.00 0.00

790 7 s93 B Jannuzi, Institute for Advanced Study G Schmidt, P Smith, University of Arizona P Stockman, Space Telescope Science Institute R Elston, National Optical Astronomy Observatories Imaging and Spectropolarimetry of High Redshift Radio.... 4 meter 3.00 30.00 0.00 0.00

851 5 s93 S Kenyon, E Lada, M Barsony, Harvard-Smithsonian Center for Astrophysics Young Stars in the Streamers of the Ophiuchus Dark Cloud 1.3 meter 6.80 44.50 0.00 0.00 Executed Proposals 04/01/93 - 06/30/93 Page 6 Fri Jul 16 14:48:50 1993

Nights Hours Days Hours 9004 2 s93 T Kinman, National Optical Astronomy Observatories A Survey for RR Lyrae and BHB Stars in the Outer Galactic. 0.9 meter 2.50 14.30 0.00 0.00

397 6 s93 R Kirshner, B Leibundgut, B Schmidt, Harvard-Smithsonian Center for Astrophysics A Porter, L Wells, National Optical Astronomy Observatories Supernova Light Curves 2.1 meter 1.00 13.00 0.00 0.00

848 10 s93 S Kleinmann, M Skrutskie, M Rudenko, University of Massachusetts F Gillett, National Optical Astronomy Observatories M Lysaght, Iowa State University Prototyping the Two Micron All Sky Survey (2MASS) 1.3 meter 6.00 55.00 0.00 0.00

844 3 s93 J Laird, Bowling Green State University B Carney, J Rose, University of North Carolina The Galaxy's Thin Disk vs. Its Thick Disk Burrell Schmidt 8.00 41.00 0.00 0.00

8805 10 s93 A Landolt, Louisiana State University Broad-Band Standard Stars at Declination +45 Degrees .... 1.3 meter 3.50 16.00 0.00 0.00 0.9 meter 3.50 11.70 0.00 0.00

640 2 s93 T Lanz, NASA Goddard Space Flight Center J Landstreet, University of Western Ontario G Mathys, European Southern Observatory Ap Stars with Resolved Magnetically Split Lines Coude Feed 7.00 59.50 0.00 0.00 Executed Proposals 04/01/93 - 06/30/93 Page 7 Fri Jul 16 14:48:50 1993

Nights Hours Days Hours 620 8 s93 T Lauer, National Optical Astronomy Observatories M Postman, Space Telescope Science Institute Velocity Dispersions of Brightest Cluster Galaxies 2.1 meter 4.00 30.00 0.00 0.00

804 4 s93 M Lehnert, T Heckman, Johns Hopkins University Shock-Heated Gas in the Halos of Starburst Galaxies 2.1 meter 4.00 32.00 0.00 0.00

615 7 s93 L Lu, B Savage, University of Wisconsin, Madison D Meyer, Northwestern University A Search for C IV Absorption in Lyman-Alpha Forest Systems 4 meter 3.00 28.50 0.00 0.00

701 4 s93 D Lynch; J Hackwell, R Russell, S Acosta, Aerospace Corporation P Hofner, University of Wisconsin, Madison 3-13 Spectral Survey of Reflection Nebulae 1.3 meter 5.00 27.50 0.00 0.00

793 7 s93 J MacKenty, Space Telescope Science Institute R Griffiths, Johns Hopkins University V Mader, University of Arizona SQIID Observtions of Nearby Seyfert Galaxies 4 meter 2.00 18.50 0.00 0.00

744 4 s93 P Maloney, NASA Ames Research Center R Elston, Carnegie Observatories, (OCIW) Near IR Spectroscopy of X-Ray Cooling Flows 4 meter 4.00 38.00 0.00 0.00

759 8 s93 P Marcum, J Gallagher, University of Wisconsin Evolution in Groups: A Collective or Stochastic Process? Burrell Schmidt 5.00 55.60 0.00 0.00 Executed Proposals 04/01/93 - 06/30/93 Page 8 Fri Jul 16 14:48:50 1993

Nights Hours Days Hours 768 5 s93 B McNamara, Kapteyn Astronomical Institute R Elston, M Wise, National Optical Astronomy Observatories C Sarazin, University of Virginia B Jannuzi, Institute for Advanced Study U-Band Polarimetry of Active Central Cluster Galaxies 4 meter 3.00 15.00 0.00 0.00

796 3 s93 M Metzger, P Schechter, Massachusetts Institute of Technology JHK Cepheid Photometry and the Galactic Rotation Curve 1.3 meter 8.00 66.00 0.00 0.00

618 7 s93 D Meyer, Northwestern University K Roth, Space Telescope Science Institute B Savage, L Lu, University of Wisconsin, Madison A Sensitive Search for High-Velocity Gas in the Outer 4 meter 3.00 30.00 0.00 0.00

9132 0 s93 D Meyer, Northwestern University K Roth, Space Telescope Science Institute High Resolution Observations of Interstellar Nal Toward.... Coude Feed 3.00 29.00 0.00 0.00

800 4 s93 J Morse, Space Telescope Science Institute R Klein, C McKee, University of California, Berkeley R Oliversen, L Brown, NASA Goddard Space Flight Center J Raymond, Harvard-Smithsonian Center for Astrophysics Shock Induced Cloud Disruption in the Cygnus Loop 2.1 meter 5.00 30.50 0.00 0.00

771 7 s93 P Osmer, R Green, A Porter, National Optical Astronomy Observatories P Hall, University of Arizona S Warren, Oxford University A Deep Multicolor Survey for High Redshift Quasars 4 meter 2.50 26.50 0.00 0.00 Executed Proposals 04/01/93 - 06/30/93 Page 9 Fri Jul 16 14:48:50 1993

Nights Hours Days Hours 638 7 s93 F Owen, National Radio Astronomy Observatory, VLA M Ledlow, University of New Mexico W Keel, University of Alabama Environment and Evolution of Radio Galaxies in Rich 2.1 meter 4.00 39.00 0.00 0.00

639 7 s93 F Owen, National Radio Astronomy Observatory, VLA W Keel, University of Alabama M Ledlow, University of New Mexico Non-Thermal Cores of Radio Galaxies in Rich Clusters 2.1 meter 5.00 46.00 0.00 0.00

713 2 s93 J Patterson, J Halpern, A Shambrook, Columbia University Disk Precession in Ultrashort-Period Cataclysmic Variables 2.1 meter 5.00 25.00 0.00 0.00

847 2 s93 M Pierce, G Jacoby, A Alexov, National Optical Astronomy Observatories D Crabtree, Dominion Astrophysical Observatory Long-Period Variables: An Alternative to Cepheids? 0.9 meter 5.00 32.50 0.00 0.00 2.1 meter 3.00 26.00 0.00 0.00

9133 0 s93 M Pierce, National Optical Astronomy Observatories Narrow Band Photometry of Galactic LPVs & Nearby Galaxies 0.9 meter 1.00 10.50 0.00 0.00

737 2 s93 C Pilachowski, L Weller, National Optical Astronomy Observatories R Kraft, University of California, Santa Cruz H Roe, Green Fields Country Day School C Sneden, University of Texas, Austin Sodium Variations in Globular Clusters Coude Feed 7.00 47.00 0.00 0.00 4 meter 3.00 27.00 0.00 0.00 Executed Proposals 04/01/93 - 06/30/93 Page 10 Fri Jul 16 14:48:50 1993

Nights Hours Days Hours 9128 0 s93 A Porter, A Lesser, National Optical Astronomy Observatories P Hall, University of Arizona Infrared Photometry of Quasars Observed with IUE 1.3 meter 3.00 17.00 0.00 0.00

9131 0 s93 A Porter, L Wells, National Optical Astronomy Observatories Spectroscopic Monitoring of Supernova 1993J Coude Feed 15.00 92.50 0.00 0.00

780 2 s93 T Ramseyer, University of Texas, Austin Infrared Spectroscopy of Cataclysmic Variables 2.1 meter 4.90 44.00 0.00 0.00

664 7 s93 M Rauch, R Weymann, Carnegie Observatories, (OCIW) R Carswell, P Petitjean, Cambridge University K Lanzetta, University of California, San Diego J Webb, University of New South Wales The Physical State of Lyman Alpha Forest Clouds 4 meter 3.00 13.00 0.00 0.00

661 2 s93 M Richards, G Albright, University of Virginia Balmer-line Spectroscopy of Short-period Algols Coude Feed 12.00 107.66 0.00 0.00

761 8 s93 W Romanishin, R Henry, University of Oklahoma Stellar Abundance Gradients in Virgo Spirals from IR Maps 1.3 meter 7.00 62.00 0.00 0.00

714 8 s93 J Rose, A Leonardi, University of North Carolina R Ellis, University of Durham R Sharpies, Durham University C Caldwell, Smithsonian Whipple Observatory The Stellar Content of Early-Type Galaxies in Dense.... 0.9 meter 3.00 22.00 0.00 0.00 Executed Proposals 04/01/93 - 06/30/93 Page 11 Fri Jul 16 14:48:50 1993

Nights Hours Days Hours 750 8 s93 J Rose, L Jones, University of North Carolina Spectral Variations in Low-Luminosity Early-Type Galaxies 0.9 meter 3.00 29.50 0.00 0.00 2.1 meter 4.00 38.00 0.00 0.00

667 2 s93 R Samec, M Arruda, Butler University Continuing Study of Very Short Period Solar-Type.... 0.9 meter 6.30 22.50 0.00 0.00

631 2 s93 A Sarajedini, T Armandroff, W Forrester, National Optical Astronomy Observatories Age Differences Between the Galactic Halo and Thick Disk 2.1 meter 3.50 28.00 0.00 0.00

732 2 s93 A Sarajedini, National Optical Astronomy Observatories E Green, University of Arizona The Age Difference Between the Globular Clusters M3 and M13 4 meter 0.90 9.50 0.00 0.00 0.9 meter 5.00 40.50 0.00 0.00

628 6 s93 B Schaefer, S Barthelmy, D Palmer, T Cline, NASA Goddard Space Flight Center K Hurley, University of California, Berkeley J Laros, Los Alamos National Laboratory G Fishman, C Kouveliotou, NASA Marshall Space Flight Center Optical Counterparts of Gamma Ray Bursts 0.9 meter 4.00 28.00 0.00 0.00

656 3 s93 A Schweitzer, University of Wisconsin, Madison K Cudworth, University of Chicago, Yerkes Observatory S Majewski, Carnegie Observatories, (OCIW) Proper Motion Survey of Galactic Satellites: Draco and 4 meter 1.90 16.50 0.00 0.00 Executed Proposals 04/01/93 - 06/30/93 Page 12 Fri Jul 16 14:48:50 1993

Nights Hours Days Hours 855 8 s93 D Silva, R Elston, National Optical Astronomy Observatories UVRJHK Surface Photometry of Virgo Ellipticals 2.1 meter 6.00 57.00 0.00 0.00

645 2 s93 J Smith, T Oswalt, Florida Institute of Technology S Leggett, U.S. Naval Observatory Photometry of White Dwarfs in Wide Binaries 1.3 meter 6.00 41.00 0.00 0.00

859 2 s93 V Smith, D Lambert, University of Texas, Austin K Hinkle, National Optical Astronomy Observatories Nickel Isotopes in Dwarf Stars 4 meter 2.00 23.00 2.00 7.50

834 2 s93 C Sneden, University of Texas, Austin G Bazan, McDonald Observatory K Yoss,' University of Illinois Abundances of Metal-Rich Halo Giants 4 meter 3.50 32.00 0.00 0.00

776 8 s93 A Stanford, M Dickinson, University of California, Berkeley P Eisenhardt, Jet Propulsion Laboratory Near-IR Imaging of Moderate-z Galaxy Clusters 2.1 meter 5.90 57.50 0.00 0.00

626 4 s93 C Steidel, M Dickinson, University of California, Berkeley Absorption Line Selected High Redshift Galaxies 4 meter 3.00 22.00 0.00 0.00

9127 2 s93 D Stickland, Rutherford & Appleton Laboratory D Harmer, National Optical Astronomy Observatories Determination of Fundamental Properties of Evolved Cool Sta Coude Feed 6.00 55.00 0.00 0.00 Executed Proposals 04/01/93 - 06/30/93 Page 13 Fri Jul 16 14:48:50 1993

Nights Hours Days Hours 668 7 s93 J Stocke, New Mexico State University E Perlman, E Ellingson, University of Colorado J Schachter, Harvard-Smithsonian Center for Astrophysics C Urry, Space Telescope Science Institute Discovering New Bright BL Lac Objects 2.1 meter 4.90 40.00 0.00 0.00

663 7 s93 M Strauss, Institute for Advanced Study L Armus, J Mazzarella, T Nakajima, B Soifer, California Institute of Technology Embedded Broad-Line Regions in Infrared-Ultraluminous 4 meter 2.70 19.00 0.00 0.00

779 2 s93 K Swanson, New Mexico State University A Search for Enhanced Mass Loss in Early-Type Binaries Coude Feed 6.00 28.00 0.00 0.00

815 8 s93 T Thuan, University of Virginia V Lipovestky, Academy of Sciences of Russia Y Izotov, Academy of Sciences of Ukraine CCD Imaging of Selected Blue Compact Galaxies from the.... 0.9 meter 5.00 48.00 0.00 0.00

717 2 s93 R Tweedy, J Holberg, J Liebert, University of Arizona K Kwitter, Williams College R Napiwotzki, K Werner, Universitat Sternwarte, Kiel Do Hot.White Dwarfs Evolve in One or Two Channels? Burrell Schmidt 8.00 59.10 0.00 0.00

718 4 s93 R Tweedy, University of Arizona H Marten, Universitat Sternwarte, Kiel Modelling Senile Planetary Nebulae Interacting with the ISM Burrell Schmidt 3.00 33.20 0.00 0.00 Executed Proposals 04/01/93 - 06/30/93 Page 14 Fri Jul 16 14:48:50 1993

Nights Hours Days Hours 767 2 s93 W Vacca, University of California, Berkeley Absolute Optical Spectrophotometry of Galactic 0 Stars 0.9 meter 5.00 36.50 0.00 0.00

807 4 s93 D Van Buren, California Institute of Technology M Greenhouse, Smithsonian Institution C Woodward, University of Wyoming E Churchwell, P Hofner, University of Wisconsin, Madison CRSP Spectroscopy of Cometary Ultracompact HII Regions 2.1 meter 4.00 29.00 0.00 0.00

650 4 s93 G Van de Steene, S Pottasch, Kapteyn Astronomical Institute G Jacoby, National Optical Astronomy Observatories Spectroscopic Observations Of New Galactic Planetary 0.9 meter 3.50 24.50 0.00 0.00

733 8 s93 S Vogel, University of Maryland I Gatley, K Merrill, National Optical Astronomy Observatories IR Images of Spiral Density Wave Induced Star Formation.... 1.3 meter 5.00 28.80 0.00 0.00

819 7 s93 L Wells, C Smith, National Optical Astronomy Observatories A Search for Supernovae in Starburst Nuclei 0.9 meter 3.80 38.40 0.00 0.00

9130 0 s93 L Wells, National Optical Astronomy Observatories T Balonek, N Silvestri, Colgate University R Tweedy, University of Arizona Imaging of Supernova 1993J Burrell Schmidt 17.50 150.60 0.00 0.00 Executed Proposals 04/01/93 - 06/30/93 Page 15 Fri Jul 16 14:48:50 1993

Nights Hours Days Hours 643 3 s93 R Wilhelm, T Beers, Michigan State University Spectroscopy of Field Horizontal-Branch and Main- 2.1 meter 5.00 47.50 0.00 0.00

657 2 s93 J Wood, Keele University R Saffer, Space Telescope Science Institute HW Vir: A Unique Pre-cataclysmic Binary with an sdB 2.1 meter 3.00 28.50 0.00 0.00

742 8 s93 C Woodward, University of Wyoming S Odewahn, University of Minnesota J Bailey, Agnes Scott College Further SQIID Imagery of SBm Galaxies: Bars & Evolution 1.3 meter 2.00 9.50 0.00 0.00

Total number of proposals: 90 Appendix B

NATIONAL SOLAR OBSERVATORY REPORT Quarter Ended: 06/30/93

Nights Hours Days Hours Scheduled Used Scheduled Used

1023 R Altrock, PIVGSS Coronal Observations Evans Solar Facility 91 155

1369 R Altrock, PL/GSS L Gilliam, National Optical Astronomy Observatories Daily Solar Activity Reports for Solar Forecasting Evans Solar Facility 3 45

1212 P Bernath, University of Waterloo C Brazier, D Carrick, Edwards Air Force Base C Jarman, D Perera, L O'Brien, M Lee, M Oliphant, University of Arizona Spectroscopy of Molecules of Astrophysical Interest FTS 4 26 4 26

1661 L Brown, Jet Propulsion Laboratory Laboratory Infrared Spectroscopy FTS 3 32 3 32

1706 K Cheng, NASA Goddard Space Flight Center J Neff, Pennsylvania State University Search for New Proto-Planetary System Candidates McMath-Pierce 6 62

1138 D Deming, NASA Goddard Space Right Center Monitoring Apparent Velocity of Integrated Sunlight McMath-Pierce 2 16

1738 D Deming, D Jennings, T Moran, G McCabe, NASA Goddard Space Flight Center Simultaneous Plage Magnetic Field Measurements at 1.6 and 12 microns McMath-Pierce 4 21 Nights Hours Days Hours Scheduled Used Scheduled Used

1089 R Dunn, National Optical Astronomy Observatories Tower Engineering Evans Solar Facility 10

1732 R Dunn, National Optical Astronomy Observatories S Doinidis, New Mexico State University Adaptive Optics, Scintillation & Telescope Window Vacuum Tower Telescope 72

1441 J Eaton, Center of Excellence in Information Systems Baimer Lines in Zeta-Aurigae Binaries McMath-Pierce 10

1741 J Eaton, Center of Excellence in Information Systems Ha Variations in Zeta-Aurigae Binaries and Cool Supergiants McMath-Pierce 10

1730 O Engvold, University of Oslo J Zirker, National Optical Astronomy Observatories Filament Observations Vacuum Tower Telescope 10 72

1802 O Engvold, University of Oslo J Zirker, National Optical Astronomy Observatories Filament Observations Evans Solar Facility 43 331

1748 P Foukal, B Behr Cambridge Research & Instrumentation, Inc. Electrograph Observations Evans Solar Facility 20 87

1219 M Giampapa, National Optical Astronomy Observatories Ha Emission & Rotation in Selected dM Stars McMath-Pierce -3

Nights Hours Days Hours Scheduled Used Scheduled Used

1603 M Giampapa, National Optical Astronomy Observatories T Fleming, University of Arizona Contemporaneous ROSAT and McMath Observations of M Dwarfs McMath-Pierce

1722 M Giampapa, National Optical Astronomy Observatories G Basri, University of California, Berkeley C Imhoff, Computer Sciences Corporation Comparative Synoptic Study of Two T Tauri Stars McMath-Pierce

1025 L Gilliam, National Optical Astronomy Observatories Monitoring: Community Evans Solar Facility 48 218

1026 L Gilliam, National Optical Astronomy Observatories Coronagraph Monitor Evans Solar Facility 19 45

1034 L Gilliam, National Optical Astronomy Observatories Flare Patrol (monitoring) Hilltop Dome 91 851

1035 L Gilliam, National Optical Astronomy Observatories White Light Patrol (monitoring) Hilltop Dome 91 781

1771 L Gilliam, J Elrod, B Armstrong, National Optical Astronomy Observatories Sunspot Drawings - Manual drawings of Sunspots Evans Solar Facility 91 -4

Nights Hours Days Hours Scheduled Used Scheduled Used

1711 A Gleckler, J Angel, D McCarthy, University of Arizona S Ridgway, National Optical Astronomy Observatories Edge-Matched Segmented Mirrors for IR Adaptive Optics McMath-Pierce 6 66

1754 L Golub, Harvard-Smithsonian Center for Astrophysics S Koutchmy, C.N.R.S. T Bastian, National Radio Astronomy Observatory J Zirker, National Optical Astronomy Observatories Microwave, Soft X-ray and Optical Fluctuations of Corona] Bright Points Vacuum Tower Telescope 2 14 Evans Solar Facility , 3 6

1755 S Habbal, R Esser, M Karovska, Harvard-Smithsonian Center for Astrophysics Coordinated Ground- and Space-based Observations of the Solar Wind Streams Evans Solar Facility 3 14

1736 J Harder, G Mount, NOAA P Johnston, National Institute of Water & Atmospheric UV/Vis Absorption Coefficient/Temperature Coefficient for Nitrogen Dioxide McMath-Pierce 3 42

1769 J Harvey, National Optical Astronomy Observatories DAWN (RISE Observations) KPVT 66 71

3790 J Harvey, National Optical Astronomy Observatories Vacuum Synoptic Program: Daily/community KPVT 91 273 Nights Hours Days Hours Scheduled Used Scheduled Used

1710 D Hassler, Harvard-Smithsonian Center for Astrophysics T Moran, NASA Goddard Space Flight Center Broadening of Coronal Emission Line Profiles Above the Limb as a Signature of Hydromagnetic Waves in the Corona Evans Solar Facility 13 69

1742 F Hill, National Optical Astronomy Observatories J Patron, Instituto de Astrofisica de Canarias J Toomre, University of Colorado D Gough, University of Cambridge Synoptic Convection Zone Flow Maps from Solar Oscillation Ring Diagrams KPVT 14 132

1663 H Jones, NASA Goddard Space Right Center In Support of NASA Right Missions KPVT 2 11

1602 S Keil, D Neidig, G Simon, G Ginet, E Cliver, PL/GSS G Cauzzi, L Smaldone, University of Naples J Bookbinder, Harvard-Smithsonian Center for Astrophysics M Kundu, University of Maryland D Rust, Johns Hopkins University Solar Dynamics in Active Regions Vacuum Tower Telescope 17 146

1681 S Keil, K Balasubramaniam, PL/GSS Ha -Ca K Air Force Initiative Evans Solar Facility 12 44

1791 J Kuhn, M Perm National Optical Astronomy Observatories Coronal IR Spectroscopy Evans Solar Facility 8 63

1687 T Leifson, P Maltby, M Omang, University of Oslo Infrared Solar Oscillations McMath-Pierce 10 111 McMath-Pierce East 10 111 -6-

Nights Hours Days Hours Scheduled Used Scheduled Used

1761 H Lin, California Institute of Technology J Kuhn, G Kopp, National Optical Astronomy Observatories Infrared Array Measurement of Sunspot and Active Region Magnetic Fields Vacuum Tower Telescope 9 72

1803 C Lindsey, Solar Physics Research Corp. J Heath, National Optical Astronomy Observatories Helioseismic Halos Surrounding Active Regions KPVT 2 8

1759 B Lites, D Elmore, A Skumanich, S Tomczyk, High Altitude Observatory Active Region Vector Magnetic Field Structure with the Advanced Stokes Polarimeter Vacuum Tower Telescope 6 43

1149 W Livingston, L Wallace, National Optical Astronomy Observatories Solar Irradiance Line Bisectors McMath-Pierce 1 8

1209 W Livingston, L Wallace, National Optical Astronomy Observatories M Steffen, Kiel University Spectrum Irradiance variability of Sun McMath-Pierce 11 112

1453 W Livingston, L Wallace, National Optical Astronomy Observatories J Elkins, NOAA Measurements of Atmospheric Trace Gases McMath-Pierce 1 10

1545 D Luttermoser, Iowa State University Ruorescent Clues to the Shock Structure of Late-type Giant Stars McMath-Pierce 12 85

1774 R Mann, National Optical Astronomy Observatories Check and Align Ha Halle Filter Evans Solar Facility 3 12 Nights Hours Days Hours Scheduled Used Scheduled Used

1495 S Martin, California Institute of Technology K Harvey, SPRC Magnetic & Velocity Full Observation of the Active & Quiet Sun KPVT 26 129

1135 P Mcintosh, NOAA L Gilliam, National Optical Astronomy Observatories D Marquett, California Institute of Technology NOAA Monitoring Program Evans Solar Facility 91 87

1768 N Morrison, University of Toledo The High-Latitude supergiant Pulsating Star UU Herculis McMath-Pierce 26 144

1762 M Perm, National Optical Astronomy Observatories Measurement of the p-mode Transmission Function of a Sunspot Vacuum Tower Telescope 10 82

1790 J Kuhn, M Penn National Optical Astronomy Observatories Density and Magnetic Field Measurements in the Near-Infrared Corona Evans Solar Facility 35

1235 A Pierce, National Optical Astronomy Observatories Solar Gravitational Redshift McMath-Pierce 12 42

1406 A Potter, T Morgan, NASA Johnson Space Right Center Studies of Exospheric Emission Lines in the Lunar Solar System McMath-Pierce 28 30 Nights Hours Days Hours Scheduled Used Scheduled Used

1709 D Rabin, National Optical Astronomy Observatories True-Field Imaging Magnetometry in the Near Infrared McMath-Pierce East 22 93 McMath-Pierce 13 65

1718 M Richards, G Albright, University of Virginia Full-Orbit Ha Spectroscopy of Short-period Algols McMath-Pierce 15 120

1765 I Ruedi, S Solanki, Institut fur Astronomie, Zurich W Livingston, National Optical Astronomy Observatories Chromospheric Magnetic Fields McMath-Pierce 20

1540 D Rust, Johns Hopkins University J O'Byrne, Univ. of Sydney Vector Magnetograph Hilltop Dome 25

1425 S Saar, Harvard-Smithsonian Center for Astrophysics J Linsky, University of Colorado A Survey of Magnetic Fields on G and K and early M Stars McMath-Pierce 40

1426 S Saar, Harvard-Smithsonian Center for Astrophysics J Linsky, University of Colorado M Giampapa, National Optical Astronomy Observatories Synoptic Observations of Magnetic Fields on G & K Stars McMath-Pierce 11 41

1813 R Saffer, Space Telescope Science Institute Test Observations of VW Vulpeculae McMath-Pierce 10 Nights Hours Days Hours Scheduled Used Scheduled Used

1494 F Scherb, University of Wisconsin, Madison 6300 Emission Studies of Io Atmosphere McMath-Pierce 13

1801 G Simon, PIVGSS L November, National Optical Astronomy Observatories P Brandt, Kiepenheuer Institut fur Sonnenphysik G Scharmer, Stockholm Observatory/Royal Swedish Academy Solar Magnetoconvection Vacuum Tower Telescope 24 244

1037 R Smartt, National Optical Astronomy Observatories Coronal One-Shot (monitoring) Hilltop Dome 17

1737 M Smith, C Rinsland, NASA Langley Research Center V Devi, College of William and Mary Long-Path Laboratory Measurements of Infrared Spectra of C02 and H20 FTS 32 32

1053 M Smith, IUE Observatory/CSC Radial Velocity Variations of Alpha Ori and Two Other Red Supergiants McMath-Pierce 10 12

1789 M Smith, IUE Observatory/CSC I Hubeny, Goddard Space Right Center T Lanz, NASA Goddard Space Flight Center An Augmented B Star Sample to Study He I Line Formation in Hot Atmospheres KPVT

1766 S Solanki, Institut fur Astronomie, Zurich W Livingston, National Optical Astronomy Observatories K Muglach, Karl Franzens Universitat Intranetwork Fields McMath-Pierce 20 10-

Nights Hours Days Hours Scheduled Used Scheduled Used

1749 F Stauffer, National Optical Astronomy Observatories PE Replacement Evans Solar Facility 20 168

1356 K Strassmeier, University of Vienna Doppler Imaging of Spotted Chromospherically Active Stars McMath-Pierce

1743 I Tuominen, T Hackman, University of Helsinki N Piskunov, Academy of Science S Saar, Harvard-Smithsonian Center for Astrophysics Surface Imaging of Two Active Stars: HD 199278 & HD 82558 McMath-Pierce 10 43

1752 L Wallace, K Hinkle, W Livingston, National Optical Astronomy Observatories 1-5 Micron Atlas of Arcturus (telluric component) McMath-Pierce 12

1210 O White, High Altitude Observatory Sun as a Star: Ca II Profile Measurements McMath-Pierce 32

1479 B Woodgate, NASA Goddard Space Right Center R Smartt, L Gilliam, National Optical Astronomy Observatories Limb Rares 7080A +/-300A Evans Solar Facility

1024 S Worden, OSUDRE/ADEW S Keil, PL/GSS Solar Rotation 3898-3954 A Evans Solar Facility 57 125

Total number of proposals: 71