NATIONAL OPTICAL ASTRONOMY OBSERVATORIES

NATIONAL OPTICAL ASTRONOMY OBSERVATORIES

QUARTERLY REPORT

JULY - SEPTEMBER 1993

November 11,1993 TABLE OF CONTENTS

I. INTRODUCTION 1

II. SCIENTIFIC HIGHLIGHTS 1 A. Cerro Tololo Inter-American Observatory 1 1. The Self-Enrichment History of 1 2. The Optical and X-ray Eclipse of the LMC Binary CAL 87 2 3. The Warped Disk of A in the Near- 2 B. Kitt Peak National Observatory 3 1. What Determines the Rate at Which Young Rotate? 3 2. Dark Matter in Elliptical 4

3. Butcher-Oemler Effect Found in the Coma Ouster 5 C. National Solar Observatory 6

1. Flows in Quiescent Prominences 6 2. Spatial Scales of Solar Magnetic Structures 6 3. GONG Site Survey Network Observations of Mt. Pinatubo Dust Qoud 7 D. US Gemini Project Office 7

III. PERSONNEL AND BUDGET STATISTICS, NOAO 8 A. Visiting Scientists 8

B. New Hires 8

C. Terminations 9

D. Summer Research Assistants 9

E. Chilean Economic Statistics 9 F. 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 July - 30 September 1993. Highlights emphasize concluded projects rather than work in progress. The NOAO Newsletter Number 36 (December 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. The Self-Enrichment History of Omega Centauri

Globular clusters were among the first objects to form in our , and as such, they hold valuable clues to the formation and early evolution of the Galaxy's halo. In particular, the abundance ratios of the different elements observed today in the stars reflect the types of stars responsible for the pre-enrichment of the clusters. For example, Type II supernovae (SN II) produce a different ratio of O to Fe than Type I supernovae. The heavy element (e.g., Fe) abundance of most globular clusters is single- valued, whereas some -to-star variations of the lighter elements (e.g., N, Al, Na) are seen within many clusters. The globular cluster Omega Centauri is unique in this respect. Its stars span a range of nearly 2 orders of in Fe abundance. Presumably, Omega Centauri managed to retain and self-enrich its primordial gas, unlike the other clusters. Thus, Omega Centauri stands as a point of comparison between the other globular clusters, the Galactic halo field stars, and even the dwarf elliptical galaxies.

In an effort to shed light on this matter, J. Brown and G. Wallerstein (U. of Washington) have obtained very high resolution spectra of six stars (spanning a range in Fe abundance) in the globular cluster Omega Centauri using the Echelle Spectrograph on the CTIO 4-m telescope. They have supplemented their data with information on other stars taken from the literature and have found that the abundances of O and the alpha-elements (Mg, Si, Ca, and Ti) appear to increase at a constant rate with the Fe abundance, as expected if all were produced by SN II. In contrast, the C+N abundance increases more rapidly than Fe, as if another source, in addition to SN II, was producing C and N. The authors note that winds from massive Wolf-Rayet stars or M supergiants could have provided this enrichment. Finally, the authors observed an excess of Na and Al relative to Fe along with a real star-to-star scatter in the abundances of these elements of a factor of 10. The authors note that both Na and Al can be produced above the burning shell in massive evolving stars, such that it can later be released into the interstellar medium via stellar winds in the Wolf-Rayet or M supergiant evolutionary phases. The relatively low-speed winds from these stars might result in localized enrichments of N, Na and Al within the proto- cluster cloud, which manifest themselves today as the large star-to-star scatter in the abundances of these elements. Also, these slower winds would be more easily captured and incorporated into a subsequent generation of stars (or lower-mass proto stars) in the dense cluster environments, whereas the gas could more easily escape from star-forming regions in the field. The authors offer this as the explanation as to why N, Na and Al are enhanced in globular cluster stars relative to field stars of the same Fe abundance. Finally, they note that the story does not end here. The abundance ratios of the most metal-rich stars in Omega Centauri, yet to be determined because of the stars' fainter , will tell whether the period of cluster formation lasted long enough for Type I SN to begin altering the O/Fe ratio or for Asymptotic Giant Branch stars to begin altering the relative abundances of s-process elements.

2. The Optical and X-ray Eclipse of the LMC Binary CAL 87

CAL 87 is one of only three known low-mass X-ray binaries (LMXBs) in the Large Magellanic Cloud (LMC). Such binary systems are thought to be composed of a massive stellar remnant, such as a neutron star or , in orbit with a smaller companion star which is transferring material to the more massive component. Because of the presence of an eclipse, CAL 87 presents the potential for determining many physical parameters of the system, such as orbital period and mass, to better constrain the models of LMXB systems.

A. Cowley, P. Schmidtke (Arizona State U.), D. Crampton, and J. Hutchings (Dominion Astrophys. Obs.) obtained simultaneous spectroscopic and photometric observations of this eclipsing X-ray binary system with the CTIO 4-m and 1.5-m telescopes in December 1988. From the photometric observations, they found an orbital period of 10.624 hours. With the spectroscopic observations, they followed the orbital velocity of the system to determine a velocity amplitude of 80 km/s. Both the photometric and spectroscopic data indicate that the majority of the optical light from this system is coming from a luminous disk. Combining the orbital period and velocity, they find that the compact remnant at the center of the accretion disk is likely to be a black hole with a mass greater than 6 M0.

To probe the structure of the inner regions of the accretion disk and better understand the system, P. Schmidtke, T. McGrath, A. Cowley, and L. Frattare (Arizona State U.) obtained ROSAT PSPC data on the system together with further optical using the CTIO 0.9-m. They found that the low X-ray of the system was consistent with the presence of a thick accretion disk which prevents the observer from viewing the X-ray source directly. The X-ray light curve showed a shallow dip which corresponds to the deep minimum in the optical light curve. The investigators interpreted this as an indication that the X-rays seen from the system come from an extended accretion-disk corona partially eclipsed by the orbiting companion star. Thus, from the combination of ROSAT X-ray and CTIO optical data, a picture of the binary system can be derived, consisting of a small companion star (mass approximately 1 MJ orbiting a massive compact object, most likely a black hole (mass > 6 MQ), which is encircled by a thick luminous accretion disk with a hot extended corona.

3. The Warped Disk of Centaurus A in the Near-Infrared

Centaurus A (Cen A), the nearest giant , provides a unique opportunity to study in detail the structure and dynamics of a candidate system formed by the merger of a small gas-rich spiral galaxy with a larger . Its prominent gas disk and dust lane are strong evidence for merger activity. In addition, it possesses shell structure, which is a prediction of simulations. Mergers are thought to affect the evolution of many galaxies in rich clusters. Therefore, Cen A is a key object of study for understanding this important aspect of galaxy evolution.

The gas kinematics of Cen A are well-modeled by a warped disk composed of connected rings of gas undergoing circular motion. Folds in the disk correspond to the edges of the dust lane observed at optical wavelengths. At near-infrared wavelengths, it is possible to view through the outer fold into the inner region of the disk. A. Quillen (California Inst, ofTech.), J. Graham (U. California, Berkeley) and J. Frogel (Ohio State U.) observed Cen A with the IR imager on the CTIO 1.5-m telescope to produce a large-scale mosaic in the J, H and K bands. Using a model of the gas distribution, they integrated the light distribution of the galaxy through an absorptive warped disk and were able to reproduce successfully the morphology and colors seen in the data. The deduced disk geometry is consistent with the kinematics from published CO and Ha data.

One explanation for warped gas disks considers gas stripped from a smaller galaxy merging with a larger one. The stripped gas is assumed to accumulate on a plane that is misaligned with the larger galaxy's principal axis. Differential precession then causes a twist, or warp, in the gas surface. Eventually, the gas will settle onto a principal plane of the galaxy. The merger in Cen A, however, was too recent for this to have occurred. Moreover, Quillen, Graham and Frogel find that the disk inclination as a function of radius is inconsistent with precession from an initially planar system.

Quillen, Graham and Frogel propose that the process of the merger determines the details of the warp structure; tidally stripped gas from a small Mailing spiral galaxy forms rings with varying radius and orientation, which precess in the nonspherical gravitational field of the elliptical galaxy. If the gas- stripping takes place over time, a smoothly connected system of rings forms, producing a warp. The geometry of a gas warp can provide clues about the process of a previous merger. In galaxies containing active nuclei, gas is observed to be nonplanar and misaligned with the host galaxy axes, similar to that in Cen A. This scenario suggests a dynamic, relatively short timescale explanation for such a phenomenon, which is the direct result of merger activity.

B. Kitt Peak National Observatory

1. What Determines the Rate at Which Young Stars Rotate?

Young main sequence stars in newly formed clusters often spin very rapidly and exhibit a range of rotation rates even within a narrow range of in a single cluster. Comparison of rates among otherwise similar clusters of comparable age may show marked differences in average rotation speed at the same mass or temperature. Our current understanding of the processes of suggest that the ultimate mass and angular momentum with which a star arrives on the main sequence is determined in the earliest stellar evolutionary phases, while the new star is still embedded in an accretion disk of material from the surrounding interstellar medium. The accretion of high angular momentum material by the star from the disk should increase the rotation rate of the young star to roughly half the break-up velocity, around a few hundred kilometers per second at the equator. Young, low mass stars are thought to be fully convective; as they contract to the main sequence, angular momentum should be preserved more or less as if the stars rotate like solid bodies. That is, the rotation rate should increase proportionally as the radius of the star decreases. Observations suggest, however, that the rotation velocities of classical T Tauri stars surrounded by accretion disks remain small, typically less than about 20 km s"1, or only 1% of the breakup velocity. Somehow the young stars must be shedding angular momentum during the disk accretion phase, perhaps through magnetized winds or a magnetic coupling between the star and the more slowly rotating outer portions of the disk. If this is the case, then the stellar angular momentum actually decreases as the star contracts toward the main sequence (the total angular momentum of the star-disk-wind system must, of course, be conserved). Once accretion stops and the disk dissipates, the star itself must conserve angular momentum as it contracts and the rotation rate should increase. S. Edwards (U. of Massachusetts) and her colleagues have recently completed a study comparing rotation in young T Tauri stars with and without accretion disks. They identified a sample of thirty-four T Tauri stars in a fully convective state with rotation periods determined from the modulation in a star's brightness due to starspots on the surface rotating across the disk. This approach provides a true measure of the star's rotation rate, free of projection effects if the axis of rotation does not lie in the plane of the sky. The presence or absence of an accretion disk for each star was determined using the criteria of optical/uv continuum excess (veiling), [0 I] emission due to accretion-related winds, and an IR excess from the disk itself. Optical and IR magnitudes and colors were derived primarily from CCD images obtained with the KPNO 0.9-m telescope and IR array data obtained with SQIID on the KPNO 1.3-m. Spectroscopy to identify the presence of [O I] was obtained with the Hydra fiber positioner and spectrograph on the KPNO 4-m telescope, supplemented with spectra from the 4-m R-C spectrograph. Stars with accretion disks all have rotation periods longer than four days, with a most probable period of about 8.5 days. Stars with no accretion disks have rotation periods between 1.5 and 16 days with a significant number of stars having rotation periods less than four days. The two samples are otherwise identical in terms of age and mass. The presence of an accretion disk apparently prevents stars from spinning up as they contract to the main sequence and accounts for the relatively low rotation rates of pre-main sequence stars. The accretion disk holds the stellar rotation rate to a fixed value until the disk dissipates. At that point, the star continues to contract and to spin up with the angular momentum it happens to possess at the time the disk dissipates. This mechanism naturally accounts for the wide spread in angular momentum observed in young, low mass stars in clusters such as a Persei.

2. Dark Matter in Elliptical Galaxies

Studies of the rotation rates of spiral galaxies as a function of distance from the galaxy's center have provided compelling evidence for the presence of unseen, non-luminous matter that affects, or even dominates, the gravitational potentials of galaxies. Rotation curves for spiral galaxies are determined from studies of 21 cm hydrogen emission, but elliptical galaxies, lacking significant amounts of neutral hydrogen, are more difficult to study. Rotation curves for the inner parts of elliptical galaxies can be determined from the integrated stellar absorption spectrum, but such measurements are limited to the brighter central regions. The outer portions of elliptical galaxies, from which the presence of dark matter might be inferred, are virtually unexplored. The dynamics of the outer regions of elliptical galaxies are more easily measured using discrete sources such as globular clusters or planetary nebulae associated with the galaxy. The usefulness of globular clusters for this purpose is limited to a few galaxies since, the clusters are hard to distinguish from faint foreground stars and background galaxies, some elliptical galaxies have few globular clusters, and these faint continuum sources are difficult to observe. Emission line objects such as planetary nebulae offer a useful alternative; they can be easily distinguished even at great distances and their radial velocities can be more easily measured.

R. CiarduUo (Pennsylvania State U.), G. Jacoby (NOAO), and H. Dejonghe (Universiteit Gent) have recently reported the results of their investigation of the radial velocities of planetary nebulae in the elliptical galaxy NGC 3379. This galaxy is an ideal target for a dynamical study for the following reasons: it is one of the nearest normal elliptical galaxies; excellent surface photometry data are available; the dynamics of the inner portion have been well-studied with both high quality rotation curves and velocity dispersion profiles; and the distance is well-determined. CiarduUo et al. obtained radial velocities for twenty-nine planetary nebulae associated with NGC 3379 using the KPNO 4-m telescope and the "Nessie" multifiber spectrograph, a prototype of the Hydra fiber positioner. This study extends three times further into the halo of NGC 3379 than earlier dynamical studies. Analysis of these data suggests that stellar orbits in the galaxy are isotropic and not affected by the presence of dark matter. The dynamics of the planetary nebulae are consistent with the observed mass of the galaxy and are consistent with no dark matter existing within 3.5 effective radii of the nucleus of NGC 3379.

While some elliptical galaxies (e.g., M87) seem to contain substantial amounts of dark matter, evidence that at least some ellipticals do not contain dark matter is strong. In the case of NGC 3379, either its dark matter halo was stripped off during past galactic encounters or dark matter is not as important for the dynamics of ellipticals as it seems to be for spiral galaxies.

3. Butcher-Oemler Effect Found in the Coma Cluster

Fifteen ago at Kitt Peak, H. Butcher and G. Oemler using the 2.1-m telescope, discovered that many galaxies in moderate clusters (i.e., z > 0.1) show evidence of enhanced star formation, while a similar effect in nearby clusters of galaxies had not been observed. Specifically, they found that blue spiral galaxies comprised about a quarter of all galaxies in compact clusters at greater than about z = 0.5. For nearby, centrally compact clusters, the fraction of blue galaxies is only a few percent or less. The rate of star formation appeared to have decayed rapidly with advancing , even, to some extent, independent of galaxy environment. An explanation of the Butcher-Oemler effect has remained elusive. The great distances of the clusters showing the Butcher-Oemler effect, and the poor spatial resolution that can be obtained for the individual galaxies in the clusters, have stymied efforts to find an answer. The relatively nearby Coma cluster (z = 0.02) has often been used for comparison to more distant clusters; the central galaxies of the Coma cluster show little or no evidence for recent star formation.

N. Caldwell (Smithsonian Inst.) and his collaborators recently completed a study to search for evidence of variations in age and between galaxies in the inner and outer portions of the Coma cluster. They found the surprising result that roughly a third of the Coma galaxies in a field some 40 arcmin southwest of the cluster center show abnormal spectra very reminiscent of those found for Butcher-Oemler cluster galaxies. If the abnormal spectra indeed result from the same cause, observations of Coma cluster galaxies may well lead to an explanation of the Butcher-Oemler effect. The galaxies in the Coma cluster can be observed with ten times the spatial resolution than more distant cluster galaxies. Further studies of Coma galaxies should provide a much more detailed understanding ofenvironmental effects on galaxies than can be obtained from more distant clusters.

The spectra were obtained with the Hydra fiber positioner and bench spectrograph on the KPNO 4-m telescope. Caldwell et al. selected early type galaxies (E and SO) in two regions of the Coma cluster; one centered on the cluster core (with seventy-four galaxies observed) and one centered 40 arcmin southwest (with fifty-one galaxies observed). Of the whole sample, fifteen galaxies have enhanced Balmer absorption lines suggesting recent star formation, three have emission lines characteristic of active galactic nuclei, and two more have emission lines indicative of ongoing star formation. All but five of these unusual galaxies are found in the southwest field. It is not yet clear whether the southwest field is unique in the Coma cluster or whether fields at similar distances but different directions from the cluster center would show a similar effect. Observations of additional fields are clearly important. The abnormal galaxies are, however, concentrated in a region near a secondary peak in the cluster X-ray emission discovered with ROSAT. This same region shows an enhanced density of galaxies; the number of galaxies in the southwest field is about twice the number in the corresponding northwest field. This enhancement may represent a gravitationally bound substructure falling to the center of the Coma cluster. C. National Solar Observatory

1. Flows in Quiescent Prominences

Under good seeing conditions, prominences at the solar limb display narrow vertical threads that most observers claim are streaming downwards. On the solar disk, the same type of object (now called a filament) will often show both upward and downward motions in predominantly horizontal threads. At this time, the geometrical relationship between the horizontal threads (at low altitudes) and vertical threads (at high altitudes) is unknown. The thread structure presumably provides clues to the overall magnetic configuration of quiescent prominences, which is fundamental to an understanding of their equilibrium.

In an attempt to sort out the relationship between horizontal and vertical threads in prominences, O. Engvold, Zhang Yi (Inst, of Theoretical Astrophys., Oslo) and J. Zirker (NSO/SP) reanalyzed several superb prominence movies obtained by R. Dunn (NSO/SP) in the mid-1950s. They reasoned that the motions of the fine structure might give some clues to the connectivity of the magnetic field.

The original films were digitized at Oslo and a local correlation algorithm was applied to the threads to derive their motions transverse to the line of sight (i.e., horizontally and vertically). One prominence showed stationary downward flows in the lower half and upward and horizontal flows in the upper half. The average speeds were 3-5 km/sec, with a maximum of 20 km/sec. Another prominence showed predominantly upward flows with similar speeds. Neither of these prominences was in the process of erupting. The persistent upward and downward flows imply photospheric sources and coronal sinks of mass.

What can we conclude? Contrary to most opinions in the literature, upward flows are common in prominence threads and their speeds are consistent with those observed on the solar disk in filaments. The connectivity of horizontal and vertical thread structure remains obscure, however, and the study ofmotions does not seem to help clarify it.

2. Spatial Scales of Solar Magnetic Structures

R. Komm (NSO/T, Office of Naval Research) analyzed the spatial scales ofsolar magnetic structures with the wavelet transform using orthogonal Daubechies wavelets. The wavelet transform is "local" in physical space in contrast to the "non-local" Fourier transform and, thus, provides information not only about spatial scales but also about positions. Komm applied this method to magnetograms, which were obtained with the NSO Kitt Peak Vacuum Telescope during the years 1985 and 1988, focusing on the structure and evolution of magnetic flux outside of active regions. The global spectra, power as a function of length scale, show that the power is mainly in structures with length scales of about 46 Mm (supergranulation) and smaller, with a maximum at about 12 Mm (mesogranulation). The local spectra, power as a function of length scale and position, show that at all length scales about 25% of the positions contain about 80% of the power, which illustrates the intermittent distribution of magnetic flux on the solar surface. Furthermore, Komm used the locality of the wavelet transform to define a global measure of intermittency, intermittency as a function of length scale. The global intermittency measure increases with decreasing length scale, which shows that smaller magnetic structures are more intermittent, less space-filling, than larger structures. 3. GONG Site Survey Network Observations of Mt. Pinatubo Dust Cloud

This summer, Lance Lones (NSO Summer Research Assistant, U. of California, San Diego), funded by GONG, studied the Mt. Pinatubo dust cloud that was observed by some of the stations in the Site Survey Network. The cloud was observed at Haleakala, Mauna Loa, Izana, Learmonth, Cerro Tololo, Tucson, and Big Bear. Lones formed weekly averages of the coefficient derived from the site survey data and then fitted the temporal variation. Three of the sites (Izana, Learmonth, and Tucson) displayed an annual periodic component of the extinction. This was removed and the residual signal fitted with a sum of two exponentials reflecting the rise and decay of the cloud component. The cloud was observed to rise with an e-folding time of 0.97 to 20.0 weeks; reached a maximum 4.3 to 47.5 weeks after the eruption; increased the pre-emption extinction by factors of 1.4 to 2.7; and is decaying with e-folding times of 0.8 to 44.6 years. The onset of maximum extinction at the different geographical sites is consistent with the movements of the cloud derived from satellite data. The time constant of the rise in the extinction, as a function of the time elapsed between the eruption and the maximum increase in extinction, is well- represented by an exponential, demonstrating that diffusion is the dominant transport process governing the aerosol dispersal to higher latitudes. A paper describing this study will be submitted to Geophysical Research Letters.

D. US Gemini Project Office

The US 50% share in the Gemini telescopes will constitute the US National 8-m Telescopes. Each of the Gemini partners has set up a National Project Office to act as a focus for national scientific and technical interests within their countries. The US Gemini Project Office (USGPO) works closely with the international Gemini Project Office. The US Gemini Project Scientist is responsible for formulating the views of the US scientific community into a set of priorities for discussion by the GSC and for the guidance of the Project. The USGPO reports to NOAO as a division on the same level as CTIO, KPNO, and NSO.

The US SAC, including some US members of the Gemini Board and Gemini Oversight Committee, met in Tucson on 15-16 June. The next meeting of the US SAC was 19-20 October 1993. There have been two Gemini Science Committee meetings in 1993, one in Victoria, BC, in March 1993, one in Tucson in July. A third GSC meeting was held on 27-28 October. Final reports of the Instrument Working Groups were available for the US SAC and GSC meetings. The GSC's instrumentation plan is to be presented to the Gemini board next May.

The USGPO approach to US involvement in the Gemini instrumentation program is for NOAO to play a major role in this activity. However, this presents an important management issue to be resolved. NOAO is prepared to deliver instrumentation to Gemini for a fixed price. On the other hand, NOAO cannot promise a fixed price delivery from a university instrumentation group, whether through a partnership, a system subcontract, or a contract management role through the US Gemini Project Office. Is the NSF prepared to underwrite cost overruns from university instrument groups to support the US commitment to Gemini instrumentation? The USGPO is willing to receive guidance from the NSF or to apply its own stringent set of project management qualifications to potential instrument developers to minimize the risk of overruns but does not have the resources to underwrite them.

The Office sponsored displays at meetings of both the American Astronomical Society and Astronomical Society of the Pacific this summer. At the Berkeley AAS meeting, the Office organized a lunchtime session at which the Gemini and the US Gemini Project Scientists presented a technical overview of the project. USGPO personnel along with NOAO staff are giving colloquia about Gemini during the fall to expand the community's understanding of the Gemini Project and its current technical approach.

USGPO personnel interact frequendy and direcdy with the Gemini Project to provide scientific and technical feedback, to identify scientific performance issues and to help define technical solutions to meet the science requirements, to evaluate implementation plans, and to participate in source selection and design reviews for critical systems and components. The national project scientists also participate in assessment committees providing scientific evaluation as input to the Gemini design reviews, including the telescope PDR in December 1992 and the enclosure PDR in May 1993, the control system PDR in September 1993, and the primary mirror PDR in December.

The Gemini Project frequently allocates work package to the partner countries. The US has expressed an interest in many of these packages. Support of work packages allocation has been a major activity of the USGPO. The US project office has taken the lead in obtaining a model of the telescope and enclosure, test optics have been produced for Gemini by the NOAO optics and coatings labs, and emissivity measurements on a variety of mirror samples have also been carried out in support of the project.

The USGPO consists of Fred Gillett, the Acting USGPS, Jay Gallagher, the interim Associate US Gemini Project Scientist and Larry Daggert, the US Gemini Project Engineer. The USGPO is also supported by Richard Green, USGPS prior to January 1993, and Peggy Wiggins, Administrative Assistant. Gillett, Daggert, Green and Wiggins have been supported by NOAO funding. Gallagher's activities are supported by an NSF allocation to the USGPO. A permanent USGPS is currendy being recruited through a nationally advertised search with applications due 15 October 1993.

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 07/03/93 Sydney D'Silva Tata Institute, India NSO/Tucson 07/30/93 Janet Roundtree-Lesh SAIC NSO/Tucson 08/13/93 Peter Brandt Kiepenheuer Institut NSO/Sunspot 08/18/93 Darren DePoy Ohio State University CTIO 08/23/93 Franz Deubner Universitat Wurzburg NSO/Sunspot 08/23/93 Jurgen Hofmann Universitat Wurzburg NSO/Sunspot

B. New Hires

date name position NOAO division 07/1/93 Michael Corbin Research Associate KPNO 07/6/93 Kurt Bachmann Junior Scientist NSO/Tucson C. Terminations

date name position NOAO division 07/01/93 Donald Neff Assoc. Engrg. Physicist NSO/Tucson 09/07/93 Patsy Day Food Services Manager KPNO 09/10/93 Pat Osmer Deputy Director, NOAO NOAO 09/17/93 Greg Kopp Research Associate NSO/Tucson 09/30/93 Warren Ball Engineering Manager GONG

D. Summer Research Assistants

arrived name institution facility visited 07/06/93 Olivier Bouchard Universites de Paris NSO/Sunspot

E. Chilean Economic Statistics

%Change Avr. monthly FY 1993: Month in CPI Pesos/Dollars July 1.0 12.8 411.98 August 2.1 13.6 410.88 September 1.2 12.3 411.28

F. NSF Foreign Travel Fund

For the quarter 1 July through 30 September 1993, a total of $2,873.45 was paid out of the NSF Foreign Travel account for visits to the following sites and institutions:

Las Campanas Observatory, La Serena, Chile, La Palma Observatory, Tenerife, Canary Islands (Spain). APPENDIX A

Telescope Usage Statistics

July - September 1993

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

4-m 1103.8 660.7 83.6 216.6 30.7 112.2

1.5-m 1097.8 713.1 80.0 247.2 15.1 42.4

1-m 627.6 290.4 64.1 220.7 11.3 41.1

CTIO 0.9-m 1037.3 531.3 158.0 225.0 39.2 83.8

*0.6/0.9-m 554.7 340.5 83.5 94.1 10.8 25.8

0.6-m 202.6 136.5 -0- 53.6 4.0 8.5

4-m -0- -0- -0- -0- -0- -0-

2.1-m 666.5 339.2 85.3 166.5 13.5 62.0

Coud6 Feed 513.8 298.6 -0- 210.8 2.9 1.5

KPNO 1.3-m 378.1 147.92 24.42 123.5 15.75 66.5

0.9-m 574.9 157.76 49.24 203.6 11.5 152.8

Schmidt 239.3 132.0 -0- 98.3 -0- 9.0

Hilltop Dome 2129.0 331.0 855.0 838.0 105.0 -0-

Vac. Tower/SP 1044.0 442.0 162.0 344.0 21.0 75.0

Evans Facility 615.0 65.0 282.0 214.0 43.0 11.0

NSO **FTS Lab 299.0 164.0 -0- 6.0 33.0 96.0

**McMath-Pierce 1326.0 372.0 195.0 332.0 15.0 412.0

Vacuum/KP 672.0 56.0 287.0 275.0 28.0 26.0

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

July 12.3 hours/night; August 11.8 hours/night; September - 10.9 hours/night.

* Use restricted to dark of the moon.

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

Cerro Tololo Inter-American Observatory

July - September 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 70 programs were carried out during this quarter.

L. Aller (U. of California, Los Angeles), F. Keenan, P. Dufton, E. Conlon, E. Little, P. Brown (Queen's U., Belfast), W. Feibelman (NASA Goddard): "High Spectral Resolution Observations of the Slow RR Telescopii." 3(25)1.5-m, 2(8)l-m

C. Anguita, M. Ruiz, P. Loyola (U. de Chile): "CCD Parallaxes for Faint Stars." 3(36)1.5-m 155

J. Baldwin (CTIO), B. Wills, D. Wills (U. of Texas), G. Ferland (U. of Kentucky): "The Inner Regions of Quasars." l(12)0.9-m

M. Berrios, M. Maldini, J. Fernandez, S. Char (U. de La Serena): "Activity and Rotational Modulation in RSCVn Stars." 6(63)1.5-m, 15(137)0.6-m

R. Blum*, K. Sellgren, D. Terndrup, J. Carr (Ohio State U.): "Mass Distribution in the Inner Galaxy." 6(44)1.5-m

R. Blum*, K. Sellgren, D. DePoy (Ohio State U.): "Long-Slit Spectral Study of the Stellar Population." 2(25)4-m

D. Bowen, C. Blades (STScI), D. Tytler, K. Lanzetta (U. of California, San Diego): "Redshifts of Galaxies Close to HST Target QSOs." 5(37)1.5-m

M. Briley (U. of Texas), G. Smith (U. of California, Sta. Cruz): "The Onset of Mixing Along the NGC 6397 and 6752 Subgiant Branches." 2(27)4-m

M. Briley (U. of Texas), J. Hesser (Dominion Astrophys. Obs., Canada), R. Bell (U. of Maryland), G. Smith (U. of California, Sta. Cruz): "Argus Observations of CN and CH in 47 Tuc Main Sequence Stars." 3(27)4-m

R. Buta, D. Crocker, G. Purcell* (U. of Alabama): "The Distribution of HII Regions in Early to Intermediate Hubble Type Ringed Galaxies." 4(48)1.5-m

N. Caldwell (Whipple Observatory), J. Rose (U. of North Carolina): "The Stellar Content of Early-Type Galaxies in Dense Clusters." 3(31)4-m

K.P. Cheng (NASA Goddard): Search for New Proto-PIanetary System Candidates." 3(10)1.5-m C. Collins, K. Romer* (U. of Durham, UK), R. Cruddace, J. Wallin (Naval Research Lab.), H. Boehringer, W. Voges (Max-Planck-Institut, Germany), H. MacGillivray (Royal Observatory, UK): "CCD Imaging of Distant Rosat Clusters." 2(26)1.5-m

P. Conti, M. Hansen* (U. of Colorado): "Spectroscopy of Otherwise Obscured OB Stars in the Infra-Red K Band." 2(19)4-m

P. Cote*, P. Fischer, D. Welch (McMaster U., Canada): "A Search for Main Sequence Binaries in M4." 3(18)4-m

R. de Carvalho (U. de Sao Paulo, Brazil), A. Ribeiro (INPE/MCT, Brazil), S. Zepf (U. of Durham, UK): "The Dynamical Evolution of Compact Groups of Galaxies." 3(37)4-m

D. DePoy (Ohio State U.): "Observations of [Fen] and [Felll] in the Galactic Center." 3(13)4-m

M. Donahue (Carnegie Obs.), C. Urry (STScI), J. Stocke (U. of Colorado): "Optical Counterparts of Nearby Lyman-a Absorption Systems." 3(36)1.5-m

R. Elston (CTIO), G. Hill (U. of Texas), O. Kuhn*, M. Elvis (Harvard-Smithsonian), J. Bechtold, R. Cutri, M. Rieke (U. of Arizona), K. Thompson (Naval Research Lab.): "IR Spectroscopy of Luminous High Redshift Quasars." 4(0)4-m, 4(43)1.5-m, 3(22)0.9-m

A. Feinstein, R. Vasquez, N. Morrel (Observatorio Astronomico, Argentina): "NGC 6530: Concerns About its Star Formation History." 2(26)l-m

G. Fontaine, F. Wesemael, R. Lamontagne, P. Bergeron (U. de Montreal, Canada): "Spectroscopy of Blue Subluminous Objects in the MCT Survey." 4(34)1.5-m

P. Francis, S. Veeraraghavan (U. of Arizona): "Confirmation of Two High Redshift Superclusters." 3(32)0.9-m

J. Frogel, D. DePoy, D. Terndrup (Ohio State U.): "The Metallicity Distribution in the Inner Bulge." 5(57)4-m

A. Ghez, D. McCarthy (U, of Arizona): "Multiplicity of T Tauri Stars in the Nearby Southern Star Forming Regions." 3(21)4-m

A. Gould (Inst, for Advanced Study): "Colors for Faint Galactic Stars Discovered Using HST (Completion)." 5(46)0.9-m

M. Hamuy, N. Suntzeff, M. Phillips (CTIO), J. Maza, J. Aparici, R. Aviles (U. de Chile): "Photometric Evolution of Supernovae." 2(22)4-m, 4(37)0.9-m

T. Henry (STScI), D. McCarthy (U. of Arizona): "Infrared Speckle Search for Companions Orbiting Nearby Stars." 3(26)4-m A. Landolt (Louisiana State U.): "Intercomparison of UBVRI Photometric Filter Sets." 7(39)l-m

A. Layden (CTIO): "Statistical Parallax of Field RR Lyrae Stars and Field RR Lyraes Near the Galactic Plane. II.." 5(38)1-m, 2(6)0.9-m, 7(76)CS

A. Layden (CTIO), R. Zinn (Yale U.): "The Kinematics and of Field RR Lyraes in the Inner Halo." 2(ll)l-m, 8(61)0.9-m

A. Layden (CTIO, S. Rosen (Leicester U., UK): "Simultaneous Optical Photometry and the HST Spectroscopy of Ex Hya." 4(41)1-m

M. Malkan, B. Rush (U. of California, Los Angeles): "UBVRI Photometry of Variable Seyfert Galaxies." 2(18)l-m

J. Maza, R. Aviles, M. Wischnjewsky, R. Antezana (U. de Chile), M. Hamuy, N. Suntzeff, M. Phillips, C. Smith, M. Navarrete (CTIO): "A Search for Supernovae." 5(30)0.9-m

J. Maza, M. Ruiz (U. de Chile), J. Baldwin, G. Williger (CTIO), G. Ferland (U. of Kentucky): "The Connection Between Broad-Absorption-Line and Normal QSOs." 4(40)4-m

K. Mighell, R. Rich (Columbia U.): "Stellar Populations in the Fornax ." 2(24)4-m

B. Miller*, P. Hodge (U. of Washington): "A Study of Star Formation Histories of Sculptor Group Dwarf Galaxies." 3(36)4-m, 4(33)1.5-m

J. Mulchaey*, A. Wilson (STScI), Z. Tsvetanov (Johns Hopkins U.): "Cones of Ionizing Radiation in Early Type Seyfert Galaxies." 5(40)1.5-m

P. McCarthy (Carnegie Obs.), R. Elston (CTIO), P. Eisenhardt, N. Lu (Caltech): "IR Spectroscopy of High Redshift Radio Galaxies." 4(46)4-m

T. Nagata, N. Kobayashi (Kyoto U., Japan), S. Sato (Nagoya U., Japan): "1.4 - 4.2 |im Spectro- Polarimetry of Highly Reddened Stars in the Galaxy and in the LMC." 4(38)1.5-m

B. Nichol (Northwestern U.), A. Connolly (Johns Hopkins U.), C. Collins (U. of Durham, UK): "An Investigation of Galactic Extinction using HI Column Densties and Galaxy Counts from a New Objective Galaxy Catalogue." 5(55)0.9-m

B. Patten*, T. Simon (U. of Hawaii): "Rotation Periods and Spectra of Young Spotted Stars in the Lupus 3 and R CrA T Associations." 17(114)l-m

R. Peterson (U. of California, Sta. Cruz), D. Crocker (U. of Alabama): "Rotation, Oxygen, Helium, Age: The Second Parameter Problem in NGC 288." 3(37)4-m

A. Phillips (U. of California, Sta. Cruz): "Survey of Circumnuclear Star Formation in Early-Type Barred Spirals." 4(23)0.9-m

M. Phillips, R. Williams, N. Suntzeff, J. Elias, M. Hamuy, C. Smith, A. Walker, M. Navarrete (CTIO): "Spectral and Photometric Evolution of Supernovae and Novae." l(12)4-m, l(12)1.5-m, l(10)0.9-m

G. Porto de Mello*, L. da Silva (Observatorio Nacional, Brazil): "Abundance Distributions in Solar-Type Stars in the Solar Neighborhood." 4(31)1.5-m

M. Postman, D. Rehner, L. Siciliano, C. Sturch, M. Shara, B. Lasker (STScI), E. Costa (U. de Chile): "The Second Guide Star Photometric Catalog." 8(34)0.9-m

R. Rich, R. Gal* (Columbia U.), R. Mendez*, W. van Altena (Yale U.): "Abundances and Kinemataics at the Bulge/Halo Transition." 3(35)4-m

J. Rose (U. of North Carolina), R. Agostinho (Portugal), J. Stock (CIDA, Venezuela): "The Vertical Structure of our Galaxy." 3(27)1.5-m, 9(78)CS

R. Samec (Butler U.), D. Hube (U. of Alberta, Canada): "Continuing Photometric, Spectroscopic and Astrometric Study of Compact Solar-Type Field Binaries." 7(60)1-m

A. Sarajedini (KPNO): "Luminosity Function of Globular Cluster Blue Straggler Stars." 4(47)1.5-m

J. Schachter, M. Elvis, J.Huchra (Harvard-Smithsonian): "Optical Counterparts of Einstein Slew Survey Sources." 3(38)1.5-m

J. Schachter, M. Elvis, J. Huchra, J. Grindlay (Harvard-Smithsonian): "Broad Band Photometry of Southern Slew Survey Sources, Part 3." 2(23)CS

P. Seitzer (U. of Michigan), G. da Costa (Anglo Australian Obs., Australia), H. Cohn, P. Lugger (Indiana U.): "Kinematics of Globular Clusters." 3(4)4-m

K. Sellgren, R. Blum*, D. DePoy (Ohio State U.): "A Narrowband Imaging Study of Stellar Populations in the Galactic Center." l(13)4-m

I. Smail, R. Blandford (Caltech), R. Ellis (U. of Durham, UK): "The Large Scale Distribution of Dark and Luminous Matter in Clusters." 4(41)4-m

H.A. Smith, N. Silbermann* (Michigan State U.), A. Walker (CTIO): "CCD Photometry of SMC Variable Stars." 4(11)CS

D. Soderblom, T. Henry (STScI), S. Baliunas (Harvard-Smithsonian): "A Survey of the Ages of Southern Solar-Type Stars." 1(8) 1.5-m

N. Suntzeff (CTIO), D. Lin (U. of California, Sta. Cruz), H. Richer (U. of British Columbia, Canada): "The Velocities and Metal Abundances of the Globular Clusters Arp 2 and Terzan 7." l(ll)4-m, 2(22)0.9-m

N. Suntzeff, R. Schommer (CTIO): "The Velocity of the Dwarf Elliptical Galaxy." l(12)1.5-m

W. Sutherland (U. of California, Berkeley), W. Saunders, G. Efstathiou, S. Maddox (Oxford U., England), R. McMahon (Cambridge U., England), S. White (U. of Arizona): "The IRAS 0.6 Jansky Redshift Survey." 4(24) 1.5-m

D. Terndrup, G. Tiede* (Ohio State U.): "Kinematics and Abundances in the Inner Galaxy." 4(29)4-m

Z. Tsvetanov (Johns Hopkins U.), S. Lipari (STScI), J. Acosta-Pulido (Inst, de Astrofisica de Canarias, Espafia): "The Extended Emision-Line Regions and the Dusty Environments of Luminous IRAS Galaxies." 2(22)1.5-m

N. Tyson, D. Spergel (Princeton U.), R. Rich (Columbia U.): "Kinematics and Metallicity of Bulge K Giants Along the Minor Axis Q = 0°)." 3(33)4-m, 4(42)0.9-m

W. van Altena, X. Guo* (Yale U.): "Galactic Structure , Kinematics and Chemical Abundance from Multi-Color Photometry and Absolute Proper Motions to B ~ 22.5 at the South Galactic Pole." 3(24)4-m

K. Wakamatsu (Gifu U., Japan), T. Hasegawa (U. of Tokyo, Japan), H. Karoji (National Astronomical Obs., Japan), M. Malkan (U. of California, Los Angeles): "A Large Scale Distribution of Galaxies Near the Galactic Center Region: A Possible Link of - Superclusters." 5(48)1.5-m

A. Walker (CTIO): "Horizontal Branch Evolution and Pulsation Study." 7(67)0.9-m

G. Williger, J. Baldwin (CTIO), C. Hazard (U. of Pittburgh): "Superclustering in the Early Universe." l(12)1.5-m, 4(11)CS

C. Wilson, K. Patel* (McMaster U., Canada), P. Massey (KPNO): "Spectroscopy of a Complete Sample of O Stars in the Galaxy NGC 6822." 3(36)4-m

MICHIGAN PROGRAM

P. Seitzer (U. of Michigan): "Michigan Program." 24(226)CS

YALE PROGRAM

W. Sherry*, J. Jayawardhana* (Yale U.): "Yale Program." 20(190)0.9-m APPENDIX B

Executed Proposals 07/01/93 - 09/31/93 Page 1 Thu Oct 21 13:52:46 1993

Nights Hours Days Hours 1027 4 f93 M Allen, Johns Hopkins University Velocity Structure in CH+ Absorption Lines Coude Feed 5.00 0.00 0.00 0.00

670 7 s93 M Ashby, J Houck, Cornell University S Libonate, University of Rochester Spectral Classification of Infrared Galaxies 2.1 meter 5.80 26.00 0.00 0.00

648 2 s93 T Barnes, University of Texas, Austin J Fernley, University College London I Skillen, University of Cambridge Cepheid Distances by the Infrared Flux Method 1.3 meter 11.80 41.25 0.00 0.00

16 0 s93 f93 T Boroson, National Optical Astronomy Observatories Q Observing Program 2.1 meter 14.00 105.00 0.00 0.00 Coude Feed 14.00 27.50 0.00 0.00 0.9 meter 20.00 56.00 0.00 0.00

795 2 s93 T Boroson, R Green, National Optical Astronomy Observatories C Christian, J Depuis, N Craig, University of California, Berkeley Spectroscopic Follow-up to the EUVE All-Sky Survey 2.1 meter 5.80 18.00 0.00 0.00

923 7 f93 D Bowen, J Blades, Science Institute D Tytler, K Lanzetta, X Fan, University of California, San Diego Redshifts of Galaxies Close to HST Target QSOs 2.1 meter 5.00 40.00 0.00 0.00

893 8 f93 J Brown, H Yee, University of Toronto A Deep Imaging Survey of cD Galaxies Burrell Schmidt 6.00 31.50 0.00 0.00 Executed Proposals 07/01/93 - 09/31/93 Page 2 Thu Oct 21 13:52:46 1993

Nights Hours Days Hours 1075 4 f93 S Courteau, Cornell University J Holtzman, Lowell Observatory S Faber, University of California, Santa Cruz The Distribution and Extinction Effects of Dust in Spirals 2.1 meter 6.00 57.00 0.00 0.00

1079 9 f93 M Dickinson, University of California, Berkeley P Eisenhardt, Jet Propulsion Laboratory Using Radio Galaxies fo Find Galaxy : Optical Imaging 2.1 meter 4.90 28.00 0.00 0.00

898 2 f93 F Fekel, NASA Marshall Space Flight Center C Ambruster, Villanova University Chrosmospheric Activity of ZAMS K Dwarfs Coude Feed 7.00 67.50 0.00 0.00

1070 8 f93 A Ferguson, R Wyse, Johns Hopkins University J Gallagher, University of Wisconsin, Madison The Outer Disks of Galaxies: Stellar Populations 0.9 meter 5.00 44.00 0.00 0.00

1054 6 f93 R Fesen, Dartmouth College R Downes, D Wallace, Space Telescope Science Institute Studying SNR Shock Emissions Using Wide-Field Schmidt.... Burrell Schmidt 6.00 44.50 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 1.00 7.00 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 1.00 2.50 0.00 0.00 Executed Proposals 07/01/93 - 09/31/93 Page 3 Thu Oct 21 13:52:46 1993

Nights Hours Days Hours 1006 2 f93 D Gies, M Hahula, R Frazin, M Thaller, Georgia State University H Henrichs, University of Amsterdam G Peters, University of Southern California Pulsation and Mass Loss in the Be Stars EW LAC and KY AND Coude Feed 7.00 66.20 0.00 0.00

946 8 f93 R Gonzalez, J Najita, A Dey, J Graham, University of California, Berkeley Deep IR Imaging of Nearby Spirals: Global Morphology 1.3 meter 4.70 27.50 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 2.00 11.50 0.00 0.00

927 6 f93 R Kirshner, P Ruiz-Lapuente, B Schmidt, Harvard-Smithsonian Center for Astrophysics L Wells, A Porter, National Optical Astronomy Observatories B Leibundgut, University of California, Berkeley Light Curves 2.1 meter 1.00 9.00 0.00 0.00

8805 10 s93 A Landolt, Louisiana State University Broad-Band Standard Stars at +45 Degrees.... 0.9 meter 6.60 13.00 0.00 0.00 1.3 meter 3.50 4.50 0.00 0.00

883 2 f93 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 65.50 0.00 0.00 Executed Proposals 07/01/93 - 09/31/93 Page 4 Thu Oct 21 13:52:46 1993

Nights Hours Days Hours 881 9 f93 T Lauer, National Optical Astronomy Observatories M Postman, Space Telescope Science Institute Motion of the Local Group with Respect to Distant Abell 2.1 meter 3.00 27.00 0.00 0.00

911 4 f93 K Lehtinen, K Mattila, University of Helsinki The Distribution and Properties of Dust in Small Globules Burrell Schmidt 3.30 18.00 0.00 0.00

963 2 f93 P Massey, National Optical Astronomy Observatories Hot and Cold Evolved Massive Stars in the Local Group 2.1 meter 5.00 47.50 0.00 0.00

1061 8 f93 D Minard, W Romanishin, University of Oklahoma JHK Surface Photometry of Brightest Cluster Galaxies 1.3 meter 6.90 51.00 0.00 0.00

1126 2 f93 G Peters, University of Southern California The Chemical Compositions of Early B Stars Coude Feed 7.00 4 9.50 0.00 0.00

847 2 f93 M Pierce, G Jacoby, National Optical Astronomy Observatories D Crabtree, Dominion Astrophysical Observatory Long-Period Variables: An Alternative to Cepheids? 0.9 meter 2.00 22.00 0.00 0.00

1111 8 f93 A Porter, National Optical Astronomy Observatories S Van Dyk, Naval Research Laboratory Early Type Supernova Host Galaxies 1.3 meter 5.00 45.50 0.00 0.00 Executed Proposals 07/01/93 - 09/31/93 Page 5 Thu Oct 21 13:52:46 1993

Nights Hours Days Hours 947 2 f93 S Ridgway, National Optical Astronomy Observatories V Coude du Foresto, Observatoire de Meudon J Mariotti, P Lena, Observatoire de Paris Angular Diameters and Effective Temperatures of Late 0.9 meter 6.90 50.00 0.00 0.00

905 2 f93 D Stickland, Rutherford & Appleton Laboratory D Harmer, National Optical Astronomy Observatories An Optical and UV Study of New Composite Binary Stars Coude Feed 2.00 0.00 0.00 0.00

956 5 f93 M Tamura, National Astronomical Observatory K Sugitani, Nagoya University K Ogura, Kokugakuin University IR Study of Star Formation Induced by Radiation-Driven 1.3 meter 1.00 0.10 0.00 0.00

769 4 s93 S Trammell, H Dinerstein, University of Texas, Austin R Goodrich, California Institute of Technology Near Infrared Spectroscopy of Post-Main-Sequence Bipolar... 2.1 meter 3.00 17.00 0.00 0.00

900 4 f93 R Tweedy, University of Arizona Morphology, Shock Structure & Evolution of Senile Burrell Schmidt 4.00 38.00 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 2.1 meter 5.00 27.00 0.00 0.00 Executed Proposals 07/01/93 - 09/31/93 Page 6 Thu Oct 21 13:52:46 1993

Nights Hours Days Hours 819 7 s93 L Wells, C Smith, National Optical Astronomy Observatories A Search for Supernovae in Starburst Nuclei 0.9 meter 2.80 22.00 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 5.00 0.00 0.00 0.00

1123 4 f93 D Welty, University of Chicago High Resolution Observations of Interstellar Absorption.... Coude Feed 2.00 10.90 0.00 0.00

886 3 f93 R Wilhelm, T Beers, Michigan State University Spectroscopy of Field Horizontal-Branch and Main-Sequence.. 2.1 meter 9.50 16.00 0.00 0.00

Total number of proposals: 37 Appendix B

NATIONAL SOLAR OBSERVATORY REPORT Quarter Ended: 09/30/93

Nights Hours Days Hours Scheduled Used Scheduled Used

1023 R Altrock, PL/GSS Coronal Observations Evans Solar Facility 92 43

1161 R Altrock, PL/GSS R Harrison, D Sime, High Altitude Observatory Coronal Transient Patrol Evans Solar Facility 8 13

1369 R Altrock, PL/GSS L Gilliam, National Optical Astronomy Observatories Daily Solar Activity Reports for Solar Forecasting Evans Solar Facility 3 15

1212 P Bernath, University of Waterloo C Brazier, P Carrick, Edwards Air Force Base D Perera, L O'Brien, C Jarman, A Lee, M Oliphant, University of Arizona Spectroscopy of Molecules of Astrophysical Interest FTS 3 24 3 24

1760 K Bocchialini, J Vial, Institut d'Astrophysique Spatiale S Koutchmy, C.N.R.S. Solar Chromospheric Network: Typical Calcium Line Profiles Vacuum Tower Telescope 13 75

1661 L Brown, Jet Propulsion Laboratory Laboratory Infrared Spectroscopy FTS 3 24 3 24

1785 P Byrne, A Lanzafame, Armagh Observatory Coronal Condensations on the RS CVn star, II Peg McMath-Pierce 7 91 -2-

Nights Hours Days Hours Scheduled Used Scheduled Used

1706 K Cheng, NASA Goddard Space Flight Center J Neff, Pennsylvania State University Search for New Proto-PIanetary System Candidates McMath-Pierce 6 29

1814 R Coulter, J Kuhn, National Optical Astronomy Observatories RISE/RSPT Seeing Veto Test Vacuum Tower Telescope 7 36

1796 F Deubner, J Hofmann, Institut fur Astronomie und Astrophysik Non-linearities in Chromospheric Oscillations Vacuum Tower Telescope 15 135

1441 J Eaton, Center of Excellence in Information Systems Balmer Lines in Zeta-Aurigae Binaries McMath-Pierce 6 16

1741 J Eaton, Center of Excellence in Information Systems Ha Variations in Zeta-Aurigae Binaries and Cool Supergiants McMath-Pierce 5 12

1821 O Engvold, University of Oslo J Zirker, National Optical Astronomy Observatories Filament Observations Evans Solar Facility 20 1

1726 P Foukal, B Behr, Cambridge Research & Instrumentation, Inc. Electrograph Observations in the IR McMath-Pierce 5 48

1748 P Foukal, B Behr, Cambridge Research & Instrumentation, Inc. Electrograph Observations Evans Solar Facility 12 33 Nights Hours Days Hours Scheduled Used Scheduled Used

1729 G Gary, Marshall Space Flight Center MSFC Vector Magnetograph Fabry-Perot Filter System Characterization Vacuum Tower Telescope 9 52

1708 D Gezari, F Varosi, NASA Goddard Space Flight Center G Kopp, W Livingston, National Optical Astronomy Observatories J Braatz, University of Maryland Infrared Array Imaging of Solar Active Regions McMath-Pierce 5 26

1787 M Giampapa, National Optical Astronomy Observatories V Andretta, University of Naples Simultaneous He I D3 and X.10830 Observations of Solar Plages McMath-Pierce 3 39

1025 L Gilliam, National Optical Astronomy Observatories Monitoring: Community Evans Solar Facility 67 82

1034 L Gilliam, National Optical Astronomy Observatories K Strand, High Altitude Observatory Flare Patrol (monitoring) Hilltop Dome/SP 92 605

1035 L Gilliam, National Optical Astronomy Observatories White Light Patrol (monitoring) Hilltop Dome/SP 92 540

1771 L Gilliam, B Armstrong, J Elrod National Optical Astronomy Observatories Sunspot Drawings - Manual Drawings of Sunspots Evans Solar Facility 76 28 -4

Nights Hours Days Hours Scheduled Used Scheduled Used

1769 J Harvey, National Optical Astronomy Observatories DAWN (RISE Observations) KPVT 64 45

3790 J Harvey, National Optical Astronomy Observatories Vacuum Synoptic Program: Daily/Community KPVT 190

1692 K Harvey, SPRC S Tsuneta, University of Tokyo K Strong, L Acton, Lockheed Missiles & Space Company Coordinated Observations with YOHKOH KPVT

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 12 93

1663 H Jones, NASA Goddard Space Flight Center In Support of NASA Flight Missions (MAX '91) KPVT

1791 J Kuhn, M Penn, National Optical Astronomy Observatories Coronal IR Spectroscopy Evans Solar Facility 24 50

1797 J Kuhn, M Penn, National Optical Astronomy Observatories IR HSG Observations Vacuum Tower Telescope 39 5-

Nights Hours Days Hours Scheduled Used Scheduled Used

1798 B Lites, V Pillet, High Altitude Observatory G Scharmer, Stockholm Observatory Royal Swedish Academy Active Region Magnetic Field Fine Structure Vacuum Tower Telescope 15 98

1209 W Livingston, L Wallace, National Optical Astronomy Observatories M Steffen, Kiel University Spectrum Irradiance Variability of the McMath-Pierce 12 85

5877 J LoPresto, C Schrader, Edinboro University of Pennsylvania Solar Gravitational Redshift McMath-Pierce 6 16

1774 R Mann, National Optical Astronomy Observatories Check & Align Ha Halle Filter Evans Solar Facility 1 5

1135 P Mcintosh, NOAA L Gilliam, National Optical Astronomy Observatories W Marquett, California Institute of Technology NOAA Monitoring Program Evans Solar Facility 92 21

1768 N Morrison, University of Toledo The High-Latitude Supergiant Pulsating Starr UU Herculis McMath-Pierce 8 29

1569 L O'Brien, T Bauer, C Gates, R Kubicek, Southern Illinois Univ. at Edwardsville Laboratory Measurements of Metal Hydrides in the Near Infrared FTS 3 18 3 18 -6

Nights Hours Days Hours Scheduled Used Scheduled Used

1790 M Penn, J Kuhn, National Optical Astronomy Observatories Density and Magnetic Field Measurements in the Near-Infrared Corona KPVT 2 4

1235 A Pierce, National Optical Astronomy Observatories Solar Gravitational Redshift McMath-Pierce 8 55

1406 A Potter, T Morgan, NASA Johnson Space Flight Center Studies of Exospheric Emission Lines in the Lunar Solar System McMath-Pierce 3 9

1709 D Rabin, National Optical Astronomy Observatories True-Field Imaging Magnetometry in the Near Infrared McMath-Pierce 4 7

1799 S Restaino, New Jersey Institute of Technology R Radick, PL/GSS G Loos, USAF Phillips Laboratory/LIMI Pupil Masking Experiment Vacuum Tower Telescope 4 42

1534 T Rimmele, Kiepenheuer Institut fur Sonnenphysik P Wiborg, PL/GSS Correlation Tracker Test and Application Vacuum Tower Telescope 5 54

1222 C Rinsland, J Levine, NASA Langley Research Center Monitoring of Long Term Trends in Concentrations of Atmospheric Gases from McMath-Pierce FTS Infrared Solar Spectra FTS 3 Nights Hours Days Hours Scheduled Used Scheduled Used

1540 D Rust, Johns Hopkins University Vector Magnetograph Hilltop Dome/SP 8 28

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 5 11

1494 F Scherb, University of Wisconsin, Madison 6300 Emission Studies of lo Atmosphere McMath-Pierce 1

1788 K Sivaraman, Indian Institute of Astrophysics S Gupta, Kodaikanal Observatory W Livingston, National Optical Astronomy Observatories Stokes V-profiles with Fe I 15648A over Plage Regions on the Solar Disc McMath-Pierce 6 48 KPVT 3 4

1037 R Smartt, National Optical Astronomy Observatories Coronal One-Shot (monitoring) Hilltop Dome/SP 6 13

1053 M Smith, IUE Observatory/CSC Variations of Alpha Ori and Two Other Red Supergiants McMath-Pierce 5 6

1789 M Smith, IUE Observatory/CSC I Hubeny, Goddard Space Flight Center T Lanz, NASA Goddard Space Flight Center An Augmented B Star Sample to Study He I Line Formation in Hot Atmospheres McMath-Pierce 7 14 Nights Hours Days Hours Scheduled Used Scheduled Used

1749 F Stauffer, National Optical Astronomy Observatories PE Replacement Evans Solar Facility 9 9

1786 C Tanner, R Rafac, University of Notre Dame Fourier Transform Spectroscopy of Atomic Cesium FTS 2 16 2 16

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 and HD 82558 McMath-Pierce 3 7

1210 O White, High Altitude Observatory Sun as a Star: Ca II Profile Measurements McMath-Pierce 3 19

1024 S Worden, OSUDRE/ADEW S Keil, PL/GSS Solar Rotation 3898-3954 A Evans Solar Facility 66 47

1795 J Zirker, National Optical Astronomy Observatories D Neidig, PL/GSS Transverse Velocity & Magnetic Shear Evolution in Active Regions Vacuum Tower Telescope 11 73

Total number of proposals: 56