NATIONAL OPTICAL ASTRONOMY OBSERVATORIES

NATIONAL OPTICAL ASTRONOMY OBSERVATORIES

QUARTERLY REPORT

OCTOBER - DECEMBER 1994

March 6, 1995 TABLE OF CONTENTS

I. INTRODUCTION 1

II. SCIENTIFIC HIGHLIGHTS 1

A. Cerro Tololo Inter-American Observatory 1

1. CN and CH Abundance Variations in Globular Cluster Turnoff and Implications for Stellar Evolution and Formation 1

2. Detection ofLens Candidates for the Double Quasar Q2345+007 2

3. The Lithium Abundance in M67 and Implications for Stellar Evolution and Cosmology 2

B. Kitt Peak National Observatory 3

1. Color Evolution of 3

2. Kinematics ofBrightest Cluster Galaxies 4

3. Evolution ofthe Infrared Spectrum of an ONeMgNova 5

C. National Solar Observatory 6

1. High Temperature Coronal Regions Follow Solar Ring Current 6

2. Scattering ofP-Modes by Localized Inhomogeneities 7

3. Detection of Intrinsically Weak Solar Disk Magnetism 8

III. US GEMINI PROGRAM 9

IV. PERSONNEL AND BUDGET STATISTICS, NOAO 10

A. Visiting Scientists 10

B. Hired 10

C. Completed Employment 10

D. Changed Status 10

E. Gemini 8-m Telescopes Project 11

F. Chilean Economic Statistics 11

G. NSF Foreign Travel Fund 11

Appendices

Appendix A: Telescope Usage Statistics Appendix B: Observational Programs Appendix C: Safety Report I. INTRODUCTION

This document covers scientific highlights and personnel changes for the period 1 October - 31 December 1994. Highlights emphasize concluded projects rather than work in progress. The NOAO Newsletter Number 41 (March 1995) contains information on major projects, new instrumentation, and operations. The appendices to this report summarize telescope usage statistics and observational programs.

H. SCIENTIFIC HIGHLIGHTS

A. Cerro Tololo Inter-American Observatory

1. CN and CH Abundance Variations in Globular Cluster Turnoff Stars and Implications for Stellar Evolution and Star Formation

Globular clusters are typically characterized by a single abundance of heavy metals: the fraction of heavy elements compared to hydrogen is constant from star to star. This suggests that the cluster formation was rapid, occurring in less than the characteristic time for heavy metal enrichment by Type II supernovae. (In fact, the energetics of these supernovae may have been responsible for clearing the gas from the early clusters, thus ending the star formation process in these systems.) It has long been known, however, that the abundances of light elements, such as carbon (C) and nitrogen (N), vary substantially from star to star within a cluster. These results are based on observations of the bright red giant stars in these clusters. Two scenarios have been put forward to explain these variations. The first involves deep convection, in which material processed by the nuclear reactions near the core of a star is dredged up to the star's surface; the activity of this process varies from star to star, resulting in the light-element abundance variations in stars' spectra. The second possible explanation invokes a "primordial" cause, such as enrichment of the intra-cluster gas and later-forming stars by the stellar winds of the earliest-formed, high-mass stars. Enrichment would have occurred before a cluster was swept clean of gas by detonations.

Aluminum (Al) and sodium (Na) abundances also are observed to vary from star to star in some clusters. This was taken as strong evidence for a primordial cause until Langer et al. (1993) showed that nuclear reactions involving Al and Na can take place in the hydrogen-burning shells of some red giant stars. Thus observations of less-evolved stars are required to determine which of the two processes are responsible for the observed C and N variations. During the 1980's, several studies were made of the CN and CH features of main sequence turnoff (MSTO) stars in the nearby globular cluster 47 Tuc. These studies employedsingle-slit spectrographs, however, so the numbers of stars in the samples were small. The studies showed that CN and CH variations do appear at the MSTO, but did not reveal whether the proportions of CN-strong and CN-weak stars mimic those seen among the red giants.

M.M. Briley (U. of Texas, Austin), J.E. Hesser (Dominion Astrophys. Obs.), R.A. Bell (U. of Maryland), M. Bolte, and G.H. Smith (UC Santa Cruz) used the Argus multi-fiber spectrograph at the CTIO 4-m telescope to observe 24 stars near the MSTO in 47 Tuc. The work is published in the December, 1994, issue of the Astronomical Journal. The observers obtained spectral indices for the CN feature at 3839 A and for the CH feature at 4300 A. They found a broad range in CN and CH strengths at a given stellar temperature, thus confirming previous studies of MSTO stars. Bycomparing their observed indices with those derived from model atmospheres, they determined that the observed range in CN strengths was larger than could be produced by dredge-up of processed material with C > N, and that a large fraction of the atmosphere must have undergone O > N cycling as well. The range of observed CH strengths also mimics that seen in the red giants, and the dwarf stars show a CN-CH anti-correlation, as do the giants. The observers therefore argue that at least some component of the abundance variations on the giant branch cannot be explained by processes occurring during the giant branch evolutionary phase. They were able to rule out several scenarios for explaining the observed variations: surface accretion of N-rich material ejected from higher-mass cluster members in the past, mass transfer from other more-massive cluster stars during stellar interactions, and mixing via meridional circulation in the stellar interior. They conclude that the abundance variations are most easily explained as having existed from near the time of cluster formation. Perhaps gas enhanced in N and depleted in C was expelled from more- massive stars into the interstellar medium, and then condensed into new stars before the cluster gas was swept out by the first supernovae.

2. Detection of Lens Candidates for the Double Quasar Q2345+007

The object called Q2345+007 AB is actually a pair of quasars that appear to lie about 7" apart on the sky. The two components (A and B) have very similar spectra and redshifts (z = 2.15), raising the possibility that the pair is part of a gravitationally lensed system. Such a system would consist of a single quasar that appears double (or multiple) because an object between Earth and the quasar causes the light from the quasar to be bent. Deep searches have failed to detect the object responsible for the lensing of Q2345+007, however. If the system is not part of a gravitational lens, then the presence of two physically associated quasars at high redshift may indicate that clustering was occurring at this .

P. Fischer, J.A. Tyson (Bell Labs), G.M. Bernstein (U. of Arizona), and P. Guhathakurta (STScI) combined images from the CTIO 4-m Prime Focus CCD with images from other telescopes to produce a B-band image of over 13 hours integration time, and an R-band image of nearly 9 hours integration time. They used point-spread- function fitting routines to subtract the light of the quasar pair, and found a faint (B = 25 mag) about 1.5 arcsec from the B image, nearly on a line between the A and B images. They also detected a large number of faint galaxies scattered over the rest of the image. There were several enhancements in the surface density distribution of these galaxies, one of which lay near the quasar pair. The authors suspect that the latter represents a cluster of galaxies, perhaps at z = 1.5, the redshift at which absorption-line systems are seen in the spectra of the quasars.

Assuming that Q2345+007 is a lensing system, Fischer et al. constructed lensing models involving the faint galaxy near component B and the suspected cluster. Though the solution was not uniquely determined, they found several combinations of parameters which reproduced the positions and relative brightnesses of the two quasar components. Thus they suggest that Q2345+007 is an example of a gravitationally lensed system. They further suggest that the slight color difference between components A and B (0.13 mag; a lensing event should be achromatic) might be due to differential reddening along the lines of sight, or to variability of the quasar compounded by the timedelay along the two different light paths. The authors point out that presence of a large cluster (the lens models indicate a mass of 1013 solar masses) at z = 1.5 is less likely in dark matter (Q. = 1) models of the Universe than in open (£2 = 0.2) models. The work is published in the August 20, 1994, issue of the Astrophysical Journal Letters. 3. The Lithium Abundance in M67 and Implications for Stellar Evolution and Cosmology

An accurate determination of the primordial abundance of lithium (Li) places important constraints on models of Big Bang nucleosynthesis and on the baryon density of the Universe. Determinations from meteorites suggest A(Li) = 3.31 (on a logarithmic scale where A(hydrogen) = 12), yet observations in stars indicate the primordial value may be lower. Li can be produced or depleted in a variety of ways. In particular, if surface convection in a star is deep enough, Li will be mixed down to a layer where it is burned, and the surface abundance of Li will appear low in that star. Studies of star clusters of different age show that Li is conserved in a narrow range of effective temperatures, thus forming the "Li peak." The Li abundance in stars within the peak slowly drops with age: A(Li) = 3.1 in the Pleiades (80 Myr), 2.9 in the Hyades (700 Myr), and 2.5 in M67 (5 Gyr). In halo dwarfs, the Li peak lies at A(Li) = 2.5 as well.

Standard stellar models cannot reproduce this behavior, yet models which include rotationally-induced mixing are more successful. This mixing is strongly supported during the time when a star is spinning down, during its late pre-main sequence and early main sequence life. Another way to test the rotationally-mixed models is to measure Li abundances of stars which are not expected to undergo spin down: short-period, tidally-locked binaries (SPTLBs).

C.P. Deliyannis (U. of Hawaii), J.R. King (U. of Texas), A.M. Boesgaard (U. of Hawaii), and S.G. Ryan (Anglo-Australian Observatory) used the CTIO 4-m telescope with the echelle spectrograph to observe the weak Liline at 6708 A in a SPTLB in M67. Both components ofthis binary system have temperatures coincident with the Li peak. The observers find A(Li) = 2.9-3.0 for both components, significantly larger than the Li abundances of the single stars in the cluster. They take this as strong evidence that the rotationally-mixed stellar models are on the right track. They note that even SPTLBs may not preserve their initial Li abundances intact. Some spin-up or spin-down may occur as the stars' orbits are circularized, with the consequent mixing and Li depletion. Thus, the initial Li abundance for M67 was at least 3.0. Galactic Li enrichment places another roadblock in the path of determining the primordial Li abundance via stellar Li abundances. The material that later formed M67 might have been enhanced in Li over its primordial Li abundance. Thus the observers stress the need to find and measure the Li abundance of SPTLBs in the Galactic halo, where the history of the pre-stellar interstellar medium is shorter. The work appeared in the October 20, 1994, issue of the Astrophysical Journal Letters.

B. Kitt Peak National Observatory

1. Color Evolution of Galaxies

The color of a galaxy, observed by measuring the galaxy's spectrum, is the sum of the colors of the individual stars in the galaxy. A recent burst of active star formation produces a subpopulation of massive blue stars that dominate the blue and near-ultraviolet light of the integrated spectrum. An initial burst of global star formation followed by a long period of passive evolution of the stellar population produces a spectrum dominated by stars onthe redgiantbranch andthemain-sequence turn-off. A series of intermediate-age bursts will produce a mixed stellar population, with properties interpreted through model spectral synthesis. By observing many galaxies at different redshifts, we can study the history of star formation in galaxies, since looking back to higher redshifts means observing galaxies as they were in the past. The study of the color evolution of galaxies, or change in color with time, can also provide information about the ages and metal content of galaxies. In order to study the rate and nature of color evolution of distant galaxies, K. Rakos (U. of Vienna) and J.M. Schombert (IPAC) carried out an imaging program for ten clusters of galaxies using the KPNO 4-meter telescope and the Prime Focus CCD Camera. Their results are reported in the Astrophysical Journal of Jan. 20, 1995. In order to measure the spectra of galaxies in the clusters, the researchers used an extensive set of filters constructed to mimic the Stromgren intermediate band system in the rest frame of each redshifted cluster. By observing the galaxies' colors with the redshifted filters, Rakos and Schombert were able to observe each galaxy at the same rest wavelengths, so that the spectra of the galaxies could be compared. Those filters measure the Balmer continuum (uz), the Paschen continuum in blue and green (bz and yz), and the absorption-rich region just longward of the blanketing break, centered at 4100 A (vz). The filters avoid all strong emission lines. The sample of galaxy clusters was chosen from the Gunn-Hoessel-Oke catalog of distant clusters, identified from photographic plates by their surface density contrast, and confirmed by spectroscopic redshifts.

The major phenomenon Rakos and Schombert measured was the Butcher-Oemler effect, the increasing fraction of blue cluster galaxies with increasing cosmic look-back time, or redshift. That fraction was consistently defined by application of the bz-yz or vz-yz indices to identify objects bluer than the E/SO restframe colors. They found that the blue fraction increases from about 20% at z = 0.4 to 80% at z = 0.9. This strong trend suggests that all galaxies with disks or high gaseous surface densities were involved in star formation at redshifts around z= 1. The colors of the Butcher-Oemler population suggest ongoing star formation or post-starburst populations (E+A galaxy spectral type). Interpreting the colors with spectral synthesis models points to a formation epoch for the blue population around z = 2 or 3.

The interpretation of the blue population is problematic, because the fraction of blue galaxies at high redshift is much greater than that observed now. The blue galaxies cannot be converted to red galaxy types, such as ellipticals or SOs, and do not share the latter's morphological properties. The authors propose that the population of Butcher-Oemler (blue) objects consists of low surface brightness galaxies undergoing episodes of pressure- induced star formation as they undergo infall into their clusters. This population fades with time, and is later destroyed by the cluster tidal field while the older, more massive systems survive.

The colors of the red galaxies are consistent with initial burst and quiet evolution of ellipticals, including a red color peak at z~0.4. The vz-yz metallicity index is bluer than the models predict, suggesting the need for including more metal-poor stars in the old population in galaxy models. The oldest (reddest) galaxies seem to have formation redshifts of z~10. That early epoch is a challenge to structure formation theories. Since the mean colors suggest an epoch of formation of z~5, ellipticals in clusters were probably not formed at the same time as the other galaxies.

The combination of imaging from HST with high angular resolution, intermediate-band imaging as in this paper, and selected spectroscopy with very large aperture ground-based telescopes holds the promise for progress in understandingthe complex problem of the evolution of galaxies and their stellar populations. 2. Kinematics of Brightest Cluster Galaxies

Many rich clusters of galaxies contain a brightest cluster galaxy (BCG), an elliptical galaxy that is larger and brighter both than other galaxies within the cluster and any galaxies found outside of clusters. A variety of formation mechanisms have been proposed for brightest cluster galaxies. One model assumes continuing mergers that lead to a progressive build-up of the central galaxy in a cluster as smaller galaxies are tidally disrupted. An alternative involves some merging, but depends primarily on formation during cluster collapse, with little subsequent evolution. A third possibility is mass accretion from x-ray cooling flows, which are observed to occur in many clusters; the accumulation in the central potential would build up the mass of the central brightest cluster galaxy with time.

To discriminate among the formation models, detailed information about the motions of stars in the brightest cluster galaxies is needed. D. Fisher and G. Illingworth (Lick Obs.) and M. Franx (U. of Groningen) have obtained and analyzed long-slit spectra of a sample of 13 brightest cluster galaxies, and compared them to a larger sample of less luminous ellipticals. They reported their results in the 10 January 1995 Astrophysical Journal. The spectra were obtained mostly with the Cryogenic Camera on the KPNO 4-m telescope. The authors used a Fourier fitting technique to derive spatially resolved velocity centroids and dispersions by use of a normalized stellar template.

They found that, with one previously-observed exception, the velocity dispersions decreased outward from the centers of the galaxies with a shallow gradient, similarly to other bright ellipticals. Taken in conjunction with the finding that brightest cluster galaxies fit relations among other physical properties for normal ellipticals (the "fundamental plane"), the authors suggest that BCGs and ellipticals share similar histories.

Only two of the 13 brightest cluster galaxies showed appreciable central rotation. The BCG sample continued a trend indicated in the larger sample of normal ellipticals: the higher the intrinsic luminosity, the lower the rotational velocities measured for the galaxy. The two galaxies in the sample with well established rotation were at the low luminosity end, and fell within the locus of the normal ellipticals. Similarly, the brightest cluster galaxies with the lowest level of rotational relative to random velocities lie in the clusters with the highest cluster velocity dispersions. The latter result should not be surprising given the strong correlation between absolute luminosity of the brightest cluster galaxy and cluster velocity dispersion. In general, the brightest cluster galaxies were not consistent with being rotationally flattened prolate or oblate spheroids, suggesting that further investigations of the degree of triaxiality would be profitable.

The unique aspects of these BCGs relative to other ellipticals are therefore their extremely low level of rotational support, and the extent of their extremely extended stellar envelopes. The derived mass-to-light ratios showed a large scatter when plotted against quantities such as the dispersion gradient, the degree of rotational support, the absolute luminosity or the cluster mass accretion rate inferred from x-ray cooling flows. Other studies have indicated evidence for increasing M/L with increasing mass accretion rate, a trend consistent with but not confirmed by the data presented in this paper. If verified, that trend would indicate a significant coupling between mass inflow and the dynamical and physical properties of the brightest central galaxies.

Ongoing mergers in the central potential of a cluster are expected from the density of galaxies in a cluster. The existenceof a counter-rotating core observed in NGC 4073 further supports the idea that mergers play a role in the development of BCGs. Further work in this area will push the observations of the extended envelopes of BCGs to determine the dynamical state of the extended stellar component. 3. Evolution of the Infrared Spectrum of an ONeMg

Nova explosions are the result of a thermonuclear runaway reaction on the surface of a that is accreting material from a close companion star. After the detonation, a shell expands from the white dwarf. The shell is optically thick, and appears as an expanding pseudo-photosphere. As the shell becomes optically thin, the nova spectrum becomes dominated by free-free continuum emission and recombination lines of hydrogen and helium, which diminish in intensity as the shell evolves. After this period, many novae exhibit a coronal line phase, with emission of near-infrared forbidden line features from heavy elements.

The nature of the coronal spectrum depends partially on the composition of the accreted material and partially on the composition of the white dwarf. The composition of the white dwarf depends on the degree of processing of material during the helium flash phase of the progenitor star. White dwarfs can therefore be made of helium, if the processing stops after helium formation, or of iron, if processing continues as far as possible. In the case of an intermediate stage of processing, the white dwarf will contain a mixture of oxygen (O), neon (Ne), and magnesium (Mg). The spectra of ONeMg novae are unique in showing strong permitted magnesium emission, along with forbidden neon lines. Abundance analyses of their ejecta typically show enhancements of oxygen, neon, aluminum and magnesium over their solar ratios relative to hydrogen. Observational monitoring of novae is required to identify the thermonuclear processes at work in the explosion, the composition of the white dwarf primaries, and the physical conditions in the ejecta and the nova environment into which the material expands.

In the 10 January 1995, issue of the Astrophysical Journal, C.E. Woodward (U. of Wyoming) and colleagues, including R.R.Joyce (KPNO), report on near-infrared spectroscopy of Nova Cygni 1992. The spectra were obtained primarily with the Cryogenic Spectrometer (CRSP) on the KPNO 2.1-m telescope. The nova outburst occurred on 19 February 1992; the KPNO spectra were obtained from March 1992, through June 1993. The nova showed spectral similarities to QU Vulpeculae, the archetype of the ONeMg novae. It faded slowly while producing little dust, making it suitable for an extended spectral monitoring program.

The spectral lines observed in the nova included hydrogen and helium recombination lines; permitted lines of oxygen and nitrogen; and infrared coronal lines of [Al VI], [Al VIII], [Ca IV], [Mg VIII], and newly-identified features of [S FX] and [Ca FX]. By using ratios of strengths of features from successive ionization states in the same element (for example, forbidden Si VI and VII), the authors determined the temperature and density of the emitting gas. With ranges for those parameters, abundance ratios were then derived. They found that the Al/Si ratio is about five times the solar abundance ratio, while the Mg/Si ratio is at least three times solar. At the same time, there were only upper limits on the strength of certain forbidden sodium (Na) features. The Al-to-Na ratio is a sensitive function of the peak temperature in the thermonuclear runaway, the white dwarf envelope composition, and the mass of the white dwarf. The observed chemical abundance pattern deduced from the coronal spectrum of the ejecta suggests that the ONeMg nova was produced on an intermediate mass (~1 solar mass) white dwarf, and that the initial accreted envelope of material was close to solar abundance.

The hydrogen recombination lines wereusedto set limits on the density of the material in the pre-coronal phase. The line ratios suggest that the density exceeded 109 atoms per cubic cm on day 23.5, and 10 atoms per cubic cm on day 203. Permitted oxygen lines were observed that were probably excited by Bowen fluorescence (hydrogen Lyman p pumping). On the other hand, other oxygen line ratios were inconsistent with that mechanism, and arose within regions where both hydrogen and oxygen were neutral. Higher dispersion spectra of the line profiles suggested several discrete components contributing to individual lines. The most consistent modelis that of high density clumps embedded in a hottersubstrate. The complexity of the nuclear processes and the hydrodynamics of the nova explosion can be slowly unraveled through exploitation of relative abundance diagnostics. C. National Solar Observatory

1. High-Temperature Coronal Regions Follow Solar Ring Current

R. Altrock (USAF/PL/GPSS and NSO/SP) collaborated with P. Hick and B.V. Jackson (UCSD), J.T. Hoeksema and X.P. Zhao (Stanford U.) and G. Slater (Lockheed) to study the large-scale structure of the solar corona. They used large-scale "synoptic" Carrington-rotation maps produced from NSO/SP coronal data, Yohkoh/SXT (Soft X-ray Telescope) satellite data, and Wilcox Solar Observatory (WSO) "source surface" maps of the large- scale solar magnetic field.

They found that the NSO/SP Fe XIV 5303 A data are an excellent proxy for smoothed Yohkoh/SXT data. Isolated emission features and large-scale structures are nearly identical in SXT and Fe XJV data. In addition, coronal holes and other low-emission regions are very similar. The two-dimensional cross-correlation coefficients for such pairs of maps are in the range 0.8 to 0.9. This indicates that the Fe XIV data are sensitive to the same physical processes as the soft x-ray data and could be very useful in studies of the large-scale structure of the solar corona during pre- and post-Yohkoh epochs.

Observations in Fe XFV 5303 A and Fe X 6374 A can be used to calculate the temperature of the emitting plasma. Synoptic temperature maps, calculated from the NSO/SP Fe X/Fe XIV ratio, show a tendency for the high temperatures to occur where the large-scale solar magnetic fields change polarity at high latitudes. These regions of enhanced temperature generally follow the heliospheric current sheet (HCS) as defined by the WSO maps. The HCS is the locus of an inferred large-scale current system circling the Sun at a height of one million kilometers. The observers hypothesize that this association is due to heating associated with current dissipation within the HCS. If true, this is an important, previously unknown, source of heating of the solar corona that must be taken into account by theories of coronal global structure and energy balance, including sources of dynamic phenomena (e.g., coronal mass ejections). Although this structure appears to overlie the "polar crown" prominence region, the cause of the excess temperature over those prominences, and not over prominences at lower latitudes, is not understood. The coronal features associated with all of these lower-lying features are mostly referred to as "streamers." This study also confirms previous findings that quiet regions in the corona and "coronal holes" (open-field regions that are the source of the steady-state solar wind) are significantly cooler (by up to 500,000 K) than the hottest regions. It seems very likely that this phenomenon is revealing properties of the large-scale distribution of magnetoconvective energy that are not currently accounted for by models of the solar cycle. Revisions in our concept of how the Sun produces activity appear to be required from these findings. In particular, it has never been recognized by any accepted model that heating due to current dissipation plays any role in the temperature structure of the corona.

The group also found that most strong solar active regions have a very complex overlying temperature distribution, with temperatures ranging from 1 to 6 million K. Temperatures on the low end were previously not included in models of active regions but must be now.

These results are reported in "Solar Coronal Structure: a Comparison of NSO/SP Ground-Based Coronal Emission Line Intensities and Temperatures with Yohkoh SXT and WSO Magnetic Data" by R. C. Altrock, P. Hick, B. V. Jackson, J. T. Hoeksema, X. P. Zhao, G. Slater and T. W. Henry, submitted to Adv. in Space Res. 2. Scattering of P -Modes by Localized Inhomogeneities

Recent observational studies have shown that sunspots scatter intermediate and high-degree p-modes. It is found that sunspots absorb up to about 50% of the acoustic energy flux that is incident upon them, and furthermore they produce a shift in phase between the in-going and out-going waves of individual modes. In the past year at NSO, D. Braun (NSO/SPRC) has discovered that sunspots scatter a measurable amount of incoming p -mode waves into outgoing modes of the same temporal frequency but different radial orders (a process termed mode- coupling). This wealth of observational information on the interaction between p-modes and sunspots offers the possibility that suitable models of scattering may yield important clues about the subsurface structure and evolution of solar activity.

A considerable amount of theoretical effort has been devoted to understanding the physical mechanisms of p- mode absorption by sunspots, with limited success. Recently, work by Y. Fan, D.-Y. Chou (National Tsing-Hua U., Taiwan), and Braun has shown that the p-mode phase shifts may be modeled by localized changes in the acoustic properties of the medium within the volume occupied by the sunspot. Fan, Braun and Chou are carrying out a study of scattering of p-modes by localized inhomogeneities in wave speed, pressure and density in an adiabatically stratified polytropic atmosphere. The solution of the scattered waves is obtained by solving the inhomogeneous wave equation under the simplification of the Born approximation, i.e. in the limit of weak scattering. It is found that the variation of the observed phase shifts with mode degree, I, and frequency, v, (or radial order, r\) can be reproduced if the characteristic depth of the inhomogeneity is shallow (-1000 km). The observed magnitude of the p-mode phase shifts requires an effective wave speed enhancement over this depth (which is determined largely by the ratio of the magnetic pressure to external gas pressure) within the sunspot of roughly a factor of two.

The current model is a simplified one which assumes an isotropic increase of wave speed. This represents an idealized addition of the magnetic pressure to the total restoring force for acoustic waves. Thus, the model does not include the effect of magnetic tension which introduces anisotropy into the medium. Future research will incorporate the effects of the Lorentz force into the equation for the scattered waves (following work by Rosenthal) and hence produce a more realistic model of the magnetic fields. The formalism developed by Fan, Braun and Chou may also be extended from the simple polytropic atmosphere to a more realistic solar model and to more complicated sunspot structures. The technique offers a significant step forward in probing acoustic inhomogeneities produced by sunspots. It is expected that these techniques will play an important role in interpreting "sunspot seismology" observations planned in the upcoming GONG and SOHO projects.

3. Detection of Intrinsically Weak Solar Disk Magnetism

First, a bit of history: Babcock's 1953 invention of the photoelectric magnetograph revealed non-sunspot fields down to a few Gauss, but could not discriminate between intrinsically weak fields of, say, 10 G over 2 arcsec, and 1000 G occupying 0.2 arcsec. Low-resolution observations with the Stenflo line-ratio method (Fe 5250.2 A, g = 3 vs. Fe 5247.1 A, g = 2), as well as select high-resolution data indicate that plage and network fields actually have kG field strengths. But what about the intra-network fields which have low values of flux? Until recently, the field strengths of these regions have not been measurable. Recently in separate studies, S. Martin (Caltech), C. Keller (NSO/T) and collaborators, and H. Lin (CfA) have suggested that there is an important component of solar surface magnetism which lies below 500 G in field strength. To explore this question further, W. Livingston (NSO/T) has put together a single channel Babcock-type system utilizing the favorable g = 3 line at 15648 A. More sensitive than Fe 5250, the Fe 15648 line allows the deduction of field strengths down to about 400 G. The experimental setup is as follows: On the 13.5-m spectrograph of the McMath-Pierce, light input from the 80-cm image feeds a 2 x 2 arcsec image sheer behind the NIM liquid crystal modulator, which is driven at 20Hz. A 0.2 A exit slit can besetto various fixed positions along the line profile (AX = 0.0 A, 0.05 A, 0.10 A, ...) on the 15648 line (0.5A FWHM). Output from the "Babo" InSb diode detector is fed to a lock-in amplifier set to a time constant of 3 sec. It is possible to scan slowly at 0.1 arcsec/sec along the solar disk N-S meridian. Seeing-induced Stokes I-V cross-talk is ameliorated by the 20 Hz chopping rate; telescope polarization I-V cross-talk is eliminated by nulling the lock-in signal with a tilted glass plate in front of the NFM modulator.

Results: Center-to-limb scans are made at exit slit positions from A^= 0.0 to 0.5 A (the last value being appropriate for strong fields). With the exit slit at 0.1 A from line center we have a noise level of 0.02% polarization. The scan gives (presumed magnetic) signals of typical amplitude 0.7% which are 3 to 4 arcsec wide and spaced at an average of 5 arcsec intervals across the entire disk. A comparison with high sensitivity magnetograms shows that these signals represent mostly intra-network elements. As observed by Martin, they persist right out to the limb and this needs further study. At a slit position of 0.5 A, the number of signal elements detected is much less than near line core, as expected if most are weak fields. S. Solanki (ETH) is modeling signal statistics vs. slit position to deduce field strengths. His preliminary finding is 400 to 500 G as an upper limit.

Problem: Because our method is statistical, we cannot distinguish in detail between plage (or network) and intra-network features. An imaging system would be necessary to separate the two.

III. US GEMINI PROGRAM

The US Gemini Program is a division of NOAO which serves as a liaison between the US community and the international Gemini Project. Personnel in this office include Todd Boroson, the US Gemini Project Scientist, Fred Gillett, the Associate US Gemini Project Scientist, Kathy Wood, Technical Administrator, and Mark Trueblood, Project Engineer. During this quarter, Fred Gillett was assigned to the international Gemini Project to fill in as interim Project Scientist for approximately one year.

This quarter saw the initiation of construction activities at both Gemini sites. The USGP was represented at the ground-breaking at Gemini North on Mauna Kea, Hawaii, and the laying of the foundation stone at Gemini South on Cerro Pachon, Chile. The USGP worked with the NSF and AURA on a press announcement for the two events. The southern ceremony was held immediately after the Gemini Science Committee meeting, which took place in La Serena, Chile. This meeting saw the beginning of discussions of the scientific aspects of operations. The USGP held a meeting of its advisory committee, the US SAC, in Tucson in mid-October.

The selection of a supplier for the near-IR Spectrograph was completed during this quarter. This US-allocated Gemini instrument was the subject of a community-wide competition. As part of a process defined by the USGP and approved by AURA and the NSF, a panel appointed by the NSF evaluated proposals and made a recommendation to the international project office. As a result, the international project office has begun negotiations with NOAO to supply this instrument.

The USGP participated in a number of technical reviews including conceptual review of the coating related activities, a preliminary design review of the acquisition and guiding assembly, and a meeting to discuss design tradeoffs for the near-IR imager being built by the University of Hawaii. Outreach activities of th USGPO this quarter centered on preparations for the American Astronomical Society meeting in Tucson in January. Work continued on the new version of the Gemini brochure and its translation into Spanish and French, with printing expected early in the next quarter.

IV. PERSONNEL AND BUDGET STATISTICS, NOAO

A. Visiting Scientists (visitors who arrived thisquarter for a stay of onemonth or more). NOAO Facility Arrived Name Institution Visited 10/4/94 Damien Burtonclay University of Sydney NSO/Tucson 10/4/94 Xiang-Tao He Beijing Normal University NOAO 10/4/94 Xiaojun Jiang Beijing Normal University NOAO 10/4/94 Keliang Huang Nanjing Normal University NOAO 10/17/94 Olivier Bouchard Paris, France NSO/SP 11/15/94 R. Kariyappa Indian Institute of Astrophysics NSO/SP 11/28/94 Vincent Foresto Max-Planck-Institut fur Astronomie KPNO 11/28/94 Guy Perrin Observatorie de Paris-Section de Meudon - France KPNO

B. Hired

Date Name Position NOAO Division 10/5/94 Brian Pohl Data Reduction Specialist GONG 10/10/94 Carole Leiker Scientific Programmer II NOAO/CCS 10/12/94 Stephane Chariot Research Associate KPNO 10/12/94 Paola Sartoretti Research Associate KPNO 10/27/94 Marguerite Rodriquez Data Reduction Specialist GONG 10/31/94 Neil Gaughan Engineering Manager ETS

C. Completed Employment

Date Name Position NOAO Division 10/27/94 Rudolf Komm Research Associate NSO 11/1/94 John Hughes Scientific Programmer I NOAO/CCS 12/30/94 Douglas Geisler Assistant Scientist CTIO

D. Changed Status

Date Name Position NOAO Division 10/1 /94 Wendy Erdwurm Promotion from Scientific Programmer II to Sr. Scientific Programmer GONG 10/1/94 Jeff Vernon Promotion from Scientific Programmer I to Scientific Programmer II GONG 10/3/94 Daniel Bass Department transfer from ETS

10 to GONG GONG 11/1/94 Jean Goodrich Promotion from Data Reduction Specialist to Scientific Programmer I GONG 12/1/94 Fred Gillett Temporary appointment Acting 8-M Project Scientist NOAO/USGPO 12/19/94 Mark Trueblood Promotion Sr. Scientific Programmer to Sr. Engineer NOAO/USGPO

E. Gemini 8-m Telescopes Project

Changed Status

Date Name Position 12/1/94 Matt Mountain Promotion from 8-M Project Scientist to Director, Gemini

F. Chilean Economic Statistics FY 1995

%Change Cum. Change Avr. monthly Month inCPI inCPI Pesos/Dollars October 0.6 0.6 414.92 November 0.6 1.2 415.19 December 0.3 1.5 403.03

G. NSF Foreign Travel Fund

For the quarter 1 October through 31 December 1994, a total of $1,374.95 was paid out of the NSF Foreign Travel account for visits to the following site and institutions:

Las Campanas Observatory, La Serena, Chile,

11 APPENDIX A Telescope Usage Statistics

October - December 1994

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

4-m 911.5 591.1 116.7 43.5 48.3 111.9

1.5-m 857.6 556.0 99.2 109.4 22.5 70.5

1-m 432.4 295.6 17.0 67.5 12.8 39.5

CTIO 0.9-m 874.1 548.0 153.5 59.6 14.3 98.7

*0.6/0.9-m 416.6 337.3 9.5 49.3 2.5 18.0

0.6-m 182.5 161.5 0.0 19.5 1.5 0.0

4-m 1061.6 571.72 109.28 338.1 19.0 23.5

2.1-m 1041.25 535.89 75.61 329.25 32.5 68.0

Gourde Feed 963.6 519.45 64.5 303.9 14.25 61.5

KPNO 1.3-m 1033.5 436.1 128.5 433.6 28.8 6.5

0.9-m 916.5 450.37 60.13 325.0 13.5 67.5

Schmidt 392.5 217.88 13.62 140.5 13.5 7.0

Hilltop Dome 1703.0 0.0 1135.0 551.0 17.0 0.0

Vac. Tower/SP 791.0 218.0 177.0 315.0 10.0 71.0

Evans Facility 1191.0 287.0 467.0 414.0 23.0 0.0

NSO **FTSLab 520.0 216.0 224.0 0.0 0.0 80.0

**McMath-Pierce 2000.0 921.0 401.0 573.0 75.0 30.0

Vacuum/KP 592.0 31.0 315.0 231.0 15.0 0.0

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

October 9.9 hours/night; November 8.9 hours/night; December 8.2 hours/night.

* Use restricted to dark of the moon.

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

October - November - December 1994: 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 68 programs were carried out during this quarter.

G. Alcaino, W. Liller, E. Wenderoth, F. Alvarado (Instituto Isaac Newton): "Photometry of Globular Cluster Standards". 9(66)1-m

E. Albert (U.S. Naval Academy), K. Roth, J. Blades (STScI): "Interstellar Titanium in the Galactic Halo and the Large Magellanic Cloud". 4(30)4-m

C. Anguita, M.T. Ruiz, P. Loyola (U. de Chile): "CCD Parallaxes for Faint Stars". 2(18)1.5-m

J. Baldwin (CTIO), B. Wills, D. Wills (U. of Texas), R. Carswell (U. of Cambridge, UK), G. Ferland (U. of Kentucky), A. Cooke (Cambridge U., England): "The Inner Regions of Quasars". 3(28)4-m, l(10)0.9-m

T. Barnes III (U. of Texas), T. Moffett (Purdue U.), W. Gieren, M. Gomez* (U. Catolica de Chile): "Independent Distances to LMC/SMC Cepheids". ll(89)0.9-m

C. Beauvais*, G Bothun (U. of Oregon), R. Schommer (CTIO): "Reducing Tully-Fisher Scatter Kinematic Observations". 4(34)1.5-m, 1(6)0.9-m

T. Beers, R. Wilhelm* (Michigan State U.), A. Layden (CTIO): "uUBV Photometry of Halo and Thick-Disk FHB and A-Type Stars". 4(19)1.5-m, 9(51)l-m

L. Campusano (U. de Chile), R. Clowes, M. Graham* (U. Central Lancashire, UK): "Search for Quasar Groups in SGP and ESO/SERC 345 Fields". 4(28)4-m

E. Colbert* (U. of Maryland), J. Mulchaey*, A. Wilson (STScI), T. Storchi-Bergmann (UFRGS, Brazil): "Extended Emission-Line Gas as a Probe of the Nuclear Ionizing Continuum in Active Galaxies". 3(26)4-m

K. Cook (Lawrence Livermore Nat. Lab.), C. Stubbs, M. Pratt (U. of California, Santa Barbara): "Spectroscopy and Photometry of Candidate Lensed Stars and Other Interesting Objects from the MACHO Project". 3(27)4-m

A. Cowley, P. Schmidtke (Arizona State U.), J. Hutchings, D. Crampton (Dominion Astrophys. Obs., Canada): "Spectroscopy of X-Ray Sources in the Magellanic Clouds". 5(50)4-m

A. Crotts, J. Xu* (Columbia U.), S. Heathcote (CTIO): "The Dynamics and Morphology of the Emission-Line Surrounding SN 1987A". 3(35)4-m

S. Djorgovski, R. de Carvalho, L. Yan* (California Inst, of Tech.): "Surface Photometry of Rich Clusters of Galaxies". 9(79)CS

A. Ferguson*, R. Wyse (Johns Hopkins U.), J. Gallagher (U. of Wisconsin-Madison): "Star Formation in the Outer Regions of Disk Galaxies". 2(10)1.5-m

J. Frogel, D. DePoy, R. Pogge, A. Quillen, K. Sellgren, D. Terndrup (Ohio State U.), R. Davies (U. of Oxford, UK): "An Atlas of Galaxies in the Near-Infrared: A Study of Structure and Stellar Content I. Infrared Observations of Spiral Galaxies". 7(45) 1.5-m

J. Frogel, D. DePoy, R. Pogge, A. Quillen, D. Terndrup (Ohio State U.), R. Davies (U. of Oxford): "An Atlas of Galaxies in the Near-Infrared: A Study of Structure and Stellar Content II. Optical Surface Photometry". 6(45)0.9-m

A. Fruchter (STScI), B. Moore (U. of California, Berkeley), C. Steidel (Massachusetts Inst, of Tech.): "Do We All Go Together When We Flow?". 7(46)1.5-m

J. Gardner (U. of Durham, UK), J. Annis (Fermilab): "The Optical and Near-Infrared Luminosity Function of the Rich X-Ray Cluster Abell 496". 5(50)1.5-m

D. Geisler (CTIO), A. Cooke (Cambridge U., England): "Standard Branches in the Washington System: A New Method for Metallicity Determination and its Application to the Sculptor and Fornax dSphs". 5(38)0.9-m

S. Gibson*, K. Nordsieck (U. of Wisconsin): "Faint Reflection Nebulosity Imaging Survey in the Large Magellanic Cloud". 4(24)CS

M. Gregg (Lawrence Livermore Nat. Lab.), M. Drinkwater (Anglo-Australian Obs.): "Multicolor Imaging Survey of the Fornax Cluster of Galaxies". 7(64)CS

S. Hawley (Michigan State U.), I. Reid, J. Gizis (California Inst, of Tech.): "Basic Data for Nearby Stars". 4(37)1.5-m

M. Irwin (Royal Greenwich Obs.), S. Demers (U. de Montreal), W. Kunkel (Las Campanas Obs.): "The Absolute Proper Motion of the Small Magellanic Cloud". 2(19)4-m

K. Johnston, N. Zacharias, M. Zacharias (US Naval Observatory), J. Russell (Naval Research Lab.), Chr. de Vegt (U. of Hamburg, Germany): "Structure Analysis and Precise Positions of Extragalactic Reference Frame Sources". 8(83)0.9-m

C. Joseph, J. Gallagher (U. of Wisconsin), M. Phillips (CTIO): "Spectroscopic Studies of Gravitational Microlenses". 2(22)4-m K. Krisciunas (Joint Astronomy Centre, Hawaii): "Multi-Site Photometry of yDoradus (Continuation)". 10(80)0.6-m

C. Lacy (U. of Arkansas): "Apsidal Motion in Eccentric Eclipsing Binary Stars". 2(15)0.6-m

A. Landolt (Louisiana State U.): "UBVRI Photoelectric Photometric Sequences (Proposal I)". 7(51)1.5-m

A. Landolt (Louisiana State U.): "Intercomparison of UBVRI Photometric Filter Sets". 5(23)1-m

T. Lauer (KPNO), M. Postman (STScI), M. Strauss (Inst, of Advanced Study): "Motion of the Local Group with Respect to Distant Abell Clusters". 4(32) 1.5-m

A. Layden (CTIO): "The Kinematics and Metallicities of Field RR Lyraes at |Z| > 5 kpc from the Galactic Plane". 3(27)4-m, 5(53)0.9-m

J. Loveday (Fermi Nat. Accelerator Lab.), S. Cote, T. Broadhurst (Johns Hopkins U.): "CCD Imaging of Parkes-APM Low Surface-Brightness Galaxies". 4(39)1.5-m

P. Lu (Western Connecticut State U.): "Continuing the Spectral and Photometry Studies for F and G Stars at the SGP". 6(54)1-m, 6(56)0.9-m

M. Luhman*, D. Jaffe, S. Pak* (U. of Texas): "Uv-Excited H2: A New Tool for Forging Molecular Clouds". 4(37)1.5-m

G Mackie (Harvard-Smithsonian), A. Stanford (Infrared Processing & Analysis Center): "A Dynamical Study of Advanced Merger Galaxies: The Fundamental Plane". 3(30)4-m

G. Mackie, P. Fabbiano (Harvard-Smithsonian): "Optical Panoramic Studies of ROSAT/IRAS Observed Large Spirals: Local vs. Global Correlations in FIR, X-Ray, Ha and B, I Emission". 5(42)CS

J. Maza, M. Wischnjewsky, X. Gomez* (U. de Chile): "UBVRI Photometry of Calan-Tololo Seyfert Galaxies". l(10)4-m, 6(51)0.9-m

J. Maza, P. Ortiz, M. Wischnjewsky (U. de Chile): "Spectroscopy of Calan-Tololo Quasar Candidates". 2(17)4-m, 6(40)CS

P. McCarthy (Carnegie Obs.), W. van Breugel (Lawrence Livermore Nat. Lab.), V. Kapahi (Poone U., India): "Spectroscopy of Southern Hemisphere Radio Galaxies". 4(33)4-m

R. McMillan*, R. Ciardullo (Pennsylvania State U.): "Extragalactic Observations of Supernova Age Indicators". 8(64)0.9-m

R.H. Mendez (Univ. Observatory, Munich), M. Breger, G Hardier (Inst, for Astronomy, Vienna), E. Costa (U. de Chile): "On the Variability of the Central Star of the PN IC 418". 5(32)l-m

P. Ortiz, J. Maza (U. de Chile): "Search for Quasars with Redshift z > 4.0". 3(29)CS

S. Pak*, D. Jaffe, M. Luhman* (U. of Texas): " Extended Molecular Hydrogen Emission from the LMC". 6(45)1.5-m

J. Patterson, A. Shambrook*, J. Kemp, C. Haswell, J. Zimmerman* (Columbia U.): "Superhumps in Cataclysmic Variables". 5(28) 1-m

E. Paunzen, M. Gelbmann (Inst, fuer Astronomie, Austria): "Survey to Detect Pulsation in X Bootis Stars". ll(67)0.6-m

A. Phillips (U. of California, Sta Cruz): "Na D Search for Superwinds in Hotspot Galaxies". l(7)4-m

M. Phillips, N. Suntzeff, A. Walker, J. Elias, M. Navarrete, M. Hamuy (CTIO), D. DePoy (Ohio State U.): "Observations of SN 1987A at Late Epochs". 5(40)4-m, l(10)0.9-m

M. Regan*, S. Vogel, R. Gruendl, P. Teuben (U. of Maryland): "The Gas Kinematics of Barred Spiral Galaxies". 4(40)1.5-m

M. Regan*, S. Vogel, P. Teuben, M. Thornley (U. of Maryland): "The Near Infrared Structure and Extinction in Barred Spiral Galaxies". 3(30)1.5-m

B. Reipurth, (ESO, Chile), J. Bally, D. Devine (U. of Colorado): "Herbig-Haro Objects in LI641 in Orion". 3(27)CS

M.T. Ruiz (U. de Chile), M. Peiia, S. Torres-Peimbert (U. Nac. de Mexico): "A Spectroscopic Study of MC Planetary Nebulae with WR Features and the Changes of N66". 2(19)4-m

M.T. Ruiz (U. de Chile), P. Bergeron (U. de Montreal, Canada), S. Leggett (JAC, Hawaii): "Study of Carbon White Dwarfs". 4(36)4-m, 4(31)0.9-m

D. Schlegel*, M. Davis (U. of California, Berkeley), J. Roth (California Inst, of Tech.), M. Strauss (Inst, for Advanced Study): "Tully-Fisher Observations of IRAS Galaxies". 3(31)4-m, l(6)0.9-m, 2(13)CS

P. Schmidtke, A. Cowley, T. McGrath* (Arizona State U.), J. Hutchings, D. Crampton (Dominion Astrophys. Obs., Canada): "Photometry of X-Ray Sources in the Magellanic Clouds". 8(63)0.9-m

F. Schweizer (Dept. of Terrestrial Magnetism), P. Seitzer (U. of Michigan): "Spectroscopy of Young Globular Clusters in the Merger Remnants NGC 7252 and 1316". 2(14)4-m T. Smecker-Hane, P. Stetson, J. Hesser (Dominion Astrophys. Obs., Canada), D. Geisler (CTIO): "The Stellar Populations of Dwarf Spheroidal Galaxies: III. Photometry of Fornax". 3(24)4-m

H.A. Smith, N. Silbermann (Michigan State U.), A. Walker (CTIO): "CCD Photometry of SMC Variable Stars". 5(25)CS

R.C. Smith (CTIO), F. Winkler (Middlebury College), Y.-H. Chu (U. of Illinois): "An Emission-Line Survey of [Selected Regions of] the Magellanic Clouds". 1(4)CS

R.C. Smith, R. Elston (CTIO): "IR Imaging & Spectroscopy of Supernova Remnants". 7(63)1.5-m

V. Smith, D. Lambert (U. of Texas), N. Suntzeff (CTIO), K. Cuhna (Observatorio Nacional, Brazil): "Chemical Evolution and Globular Clusters". 5(49)4-m

C. Sneden (U. of Texas), G. Preston, A. McWilliam (Carnegie Observatories), J. Cowan (U. of Oklahoma): "An Extremely Metal-Poor Giant with Large Neutron Capture Element Excesses". 4(35)4-m

M. Strauss (Inst, for Advanced Study), T. Lauer (KPNO), M. Postman (STScI): "Velocity Dispersions and Redshifts of Brightest Cluster Galaxies: Bulk Flows to 240 h-1 Mpc". 4(39)4-m

A. Walker (CTIO): "Horizontal Branch Evolution and Pulsation Study". 5(49)0.9-m

F. Walter (State U. of New York), D. Duncan (U. of Chicago), A. Collier-Cameron (U. of Sussex, UK), M. Kuerster (MPE, Germany): "The Atmosphere of AB Dor from the Photosphere through the Corona". 3(32)4-m

T. Williams (Rutgers U.), D. Schiminovich*, J. van Gorkom (Columbia U.), T. van der Hulst (Kapteyn Astron. Inst., The Netherlands): "Sharp Edges in Neutral Hydrogen in Elliptical Shell Galaxies and Spirals: the Result of Photoionization?". 3(27)1.5-m

R. Wing (Ohio State U.), D. MacConnell (STScI): "A Photometric Search for Dwarf Carbon Stars". 8(59)1-m

P. Winkler (Middlebury College), R.C. Smith (CTIO), R. Petre (NASA/GSFC), Y.-H. Chu (U. of Illinois): "New Supernova Remnants in the Magellanic Clouds". 4(32)1.5-m

MACHO (Massive Compact Halo Object) Program: S. Marshall (U. of California, Santa Barbara), D. Bennett (L. Livermore National Lab.), D. Reiss* (U. of Washington): "Real-Time Follow-up of Candidate Microlensing Events". 6(47)0.9-m Executed Proposals 10/01/94 - 12/31/94 Page 1 Tue Jan 31 14:02:33 1995

Nights Hours Days Hours 1525 0 f94 H Abt, D Willmarth, National Optical Astronomy Observatories Binary Search Among Sharp Lined A Stars Coude Feed 4.00 32.50 0.00 0.00

1447 0 f94 S Adelman, The Citadel A Philip, Van Vleck Observatory Elemental Abundances of Field Horizontal Branch Stars IV Coude Feed 3.00 11.95 0.00 0.00

1490 2 f94 G Albright, M Richards, University of Virginia P Koubsky, Astronomical Institute Simultaneous Balmer Line IUE and Radio Continuum Observ Coude Feed 7.00 37.00 0.00 0.00

1609 0 f94 B Andersson, P Wannier, Jet Propulsion Laboratory S Federman, University of Toledo The Envelope of Molecular Cloud B5 II, K I and Na I Lines Coude Feed 7.00 50.00 0.00 0.00

1595 0 f94 J Annis, Fermi National Accelerator Laboratory J Gardner, Durham University K Band Imaging of Low Redshift X-Ray Selected Clusters 1.3 meter 5.00 34.00 0.00 0.00

1622 0 f94 S Baggett, J MacKenty, Space Telescope Science Institute Near-IR Imaging of Edge-On Disk Galaxies 1.3 meter 5.00 30.00 0.00 0.00

1486 2 f94 C Bailyn, J Orosz, Yale University Observations of Black Hole Candidate Nova Per 1992 2.1 meter 3.90 26.00 0.00 0.00 4 meter 3.00 33.50 0.00 0.00 Executed Proposals 10/01/94 - 12/31/94 Page 2 Tue Jan 31 14:02:33 1995

Nights Hours Days Hours 1446 0 f94 J Baldwin, National Optical Astronomy Observatories B Wills, D Wills, M Brotherton, University of Texas, Austin H Netzer, Tel Aviv University The Inner Regions of Quasars 2.1 meter 5.00 51.50 0.00 0.00

1562 0 f94 J Bally, D Devine, R Sutherland, University of Colorado Kinematics & Excitation of Herbig-Haro Objects & Jets.... 4 meter 3.00 31.00 0.00 0.00

1455 0 f94 T Beers, Michigan State University A Search for Extremely Low Metallicity Stars and FHB/A Star Burrell Schmidt 8.00 44.00 0.00 0.00

1630 0 f94 M Bershady, C Gronwall, University of California, Santa Cruz A Stanford, California Institute of Technology Are Faint Blue Galaxies Exploding Dwarfs? 4 meter 3.00 25.00 0.00 0.00

1605 0 f94 H Bond, A Saha, Space Telescope Science Institute Testing Post-AGB A-F Supergiants as Standard Candles in 4 meter 3.00 23.50 0.00 0.00

1570 0 f94 G Bothun, University of Oregon D Silva, National Optical Astronomy Observatories Age Dating Suspected Mergers via AGB Light: Part III 1.3 meter 4.00 40.00 0.00 0.00 Executed Proposals 10/01/94 - 12/31/94 Page 3 Tue Jan 31 14:02:33 1995

Nights Hours Days Hours 1448 0 f94 M Brotherton, B Wills, University of Texas, Austin The Intermediate Line Region of QSOs 2.1 meter 4.00 22.00 0.00 0.00

1516 0 f94 D Calzetti, A Kinney, K McQuade, Space Telescope Science Institute T Storchi-Bergmann, Instituto di Fisica Dust Extinction and Initial Mass Function in Starburst.... 1.3 meter 5.00 20.50 0.00 0.00 0.9 meter 3.00 4.50 0.00 0.00

1618 0 f94 A Connolly, T Broadhurst, G Szokoly, Johns Hopkins University B Mobasher, Imperial College The Local Infrared Luminosity Function of Field Galaxies 1.3 meter 5.00 24.50 0.00 0.00

1454 5 f94 N Devereux, New Mexico State University P Scowen, Arizona State University N Duric, University of New Mexico H Alpha Imaging of Large Nearby Galaxies Burrell Schmidt 3.00 10.50 0.00 0.00

1665 0 f94 M Dickinson, Space Telescope Science Institute P Eisenhardt, Jet Propulsion Laboratory Using Radio Galaxies to Find Clusters at z > 1 4 meter 3.80 11.00 0.00 0.00

1477 0 f94 E Ellingson, University of Colorado H Yee, University of Toronto Quasars in Clusters at Z - 1 4 meter 2.65 31.00 0.00 0.00

1566 0 f94 D Elmegreen, Vassar College J Salzer, Wesleyan University Star Forming Complexes in Spiral Galaxies 0.9 meter 5.00 41.50 0.00 0.00 Executed Proposals 10/01/94 - 12/31/94 Page 4 Tue Jan 31 14:02:33 1995

Nights Hours Days Hours 1585 0 f94 D Elmegreen, F Chromey, Vassar College B Elmegreen, IBM Near-Infrared Imaging of Barred Galaxies 1.3 meter 5.00 42.50 0.00 0.00

1608 0 f94 R Elston, National Optical Astronomy Observatories P Eisenhardt, Jet Propulsion Laboratory The Evolution of Early Type Galaxies at Z=l 4 meter 4.00 42.00 0.00 0.00

1459 0 f94 F Fekel, NASA Marshall Space Flight Center J Marshall, Villanova University Spectroscopy of Close Multiple Stars and Speckle Binaries Coude Feed 5.00 41.50 0.00 0.00

1583 0 f94 A Ferguson, R Wyse, Johns Hopkins University J Gallagher, University of Wisconsin, Madison Chemical Abundances in Outer Disks of Galaxies 4 meter 3.00 24.00 0.00 0.00

1590 0 f94 A Fry, B Carney, University of North Carolina T Kinman, National Optical Astronomy Observatories Infrared Photometry and the Cepheid and RR Lyrae Distance.. 2.1 meter 6.00 44.50 0.00 0.00 0.9 meter 6.00 26.50 0.00 0.00

1629 0 f94 G Fuller, National Radio Astronomy Observatory E Lada, University of Maryland at College Park P Myers, Harvard-Smithsonian Center for Astrophysics The Structure of the Extinction in the Dense Core in L1400G 2.1 meter 5.50 33.00 0.00 0.00 Executed Proposals 10/01/94 - 12/31/94 Page 5 Tue Jan 31 14:02:33 1995

Nights Hours Days Hours 1637 0 f94 M Garcia, J McClintock, P Callanan, P Zhao, Harvard-Smithsonian Center for Astrophysics Searching for Black Holes: Mass Function of X-Ray Nova.... 4 meter 3.00 25.00 0.00 0.00

1634 0 f94 M Giavalisco, F Macchetto, Space Telescope Science Institute P Rosati, Johns Hopkins University C Steidel, Massachusetts Institute of Technology A Broad-Band Multi-Color Search for 3 < z < 3.5 Galaxies 4 meter 3.00 0.00 0.00 0.00

1495 0 f94 S Gibson, K Nordsieck, University of Wisconsin, Madison Interstellar Absorption Associated with Pleiades Reflection Coude Feed 7.00 59.00 0.00 0.00

1510 0 f94 R Giovanelli, M Haynes, Cornell University Measurement of Peculiar Velocities of Spiral Galaxies 0.9 meter 12.00 74.50 0.00 0.00

1599 0 f94 R Gonzalez, J Graham, J Najita, A Dey, University of California, Berkeley Deep IR Imaging of Nearby Spirals: Global Morphology and... 1.3 meter 6.00 34.50 0.00 0.00

1670 0 f94 R Green, National Optical Astronomy Observatories R Griffiths, Johns Hopkins University V Sarajedini, University of Arizona The Morphological Evolution of Distant Galaxies 4 meter 4.00 42.00 0.00 0.00 Executed Proposals 10/01/94 - 12/31/94 Page 6 Tue Jan 31 14:02:33 1995

Nights Hours Days Hours 1632 0 f94 M Gregg, Lawrence Livermore Laboratory A Spectral Atlas of M32 Coude Feed 3.00 5.50 0.00 0.00

1671 0 f94 P Hall, University of Arizona R Green, National Optical Astronomy Observatories Associated CIV Absorption and Environments of Radio-Loud... 4 meter 4.00 50.00 0.00 0.00

1661 0 f94 P Harding, A Nelson, University of Arizona A Sarajedini, National Optical Astronomy Observatories I Ferrin, University of the Andes E Alvarez, The M33 Cluster System 0.9 meter 2.00 17.00 0.00 0.00

1606 0 f94 T Heckman, G Meurer, Johns Hopkins University A Galactic Wind from the Nucleus of M31 4 meter 2.90 32.00 0.00 0.00

1658 0 f94 L Hillenbrand, L Allen, S Strom, University of Massachusetts Age Spreads & Mass Functions in Isolated High Mass Star.... 4 meter 4.00 25.50 0.00 0.00

1548 0 f94 K Hinkle, L Wallace, E Hardesty, D Little, D Branston, National Optical Astronomy Observatories M Meyer, University of Massachusetts S Edwards, Smith College V Sarajedini, University of Arizona L and K Band Infrared Spectral Standards 4 meter 0.00 0.00 7.00 28.00 Executed Proposals 10/01/94 - 12/31/94 Page 7 Tue Jan 31 14:02:33 1995

Nights Hours Days Hours 1580 0 f94 K Janes, Boston University E Friel, Maria Mitchell Observatory P Seitzer, University of Michigan Integrated Properties of Galactic Open Clusters Burrell Schmidt 1.00 0.00 0.00 0.00

1616 0 f94 B Jannuzi, Institute for Advanced Study R Green, C Lowe, National Optical Astronomy Observatories R Weymann, Carnegie Observatories, (OCIW) 5 Morris, Dominion Astrophysical Observatory V Sarajedini, University of Arizona Connection Between Low Redshift Lyman-a Absorbers 6 Large.. Burrell Schmidt 6.00 54.50 0.00 0.00 2.1 meter 1.50 5.50 0.00 0.00

1470 0 f94 K Johnston, N Zacharias, U. S. Naval Observatory J Russell, M Zacharias, Naval Research Laboratory C de Vegt, Universitat Hamburg Structure Analysis and Precise Positions of Extragalactic. 0.9 meter 6.50 52.00 0.00 0.00

1507 0 £94 S Kenyon, R Marzke, M Geller, Harvard-Smithsonian Center for Astrophysics The H-Band Luminosity Function of Nearby Galaxies 1.3 meter 5.00 32.50 0.00 0.00

1535 0 f94 S Kenyon, C Lada, J Alves, Harvard-Smithsonian Center for Astrophysics The Luminosity Function of Nearby Protostars 1.3 meter 4.00 17.50 0.00 0.00

1523 0 f94 T Kinman, National Optical Astronomy Observatories Blue Horizontal Branch & RR Lyrae Stars in the Outer Halo 1.3 meter 7.50 51.50 0.00 0.00 Executed Proposals 10/01/94 - 12/31/94 Page 8 Tue Jan 31 14:02:33 1995

Nights Hours Days Hours 1487 0 f94 R Kirshner, B Schmidt, A Riess, Harvard-Smithsonian Center for Astrophysics D Mcintosh, M Walters, University of Arizona L Wells, National Optical Astronomy Observatories P Garnavich, Dominion Astrophysical Observatory Supernova Light Curves 2.1 meter 1.50 5.50 0.00 0.00

1534 0 f94 E Lada, University of Maryland at College Park C Lada, Harvard-Smithsonian Center for Astrophysics R Phelps, Phillips Laboratory Investigations of the Nature of Young Stellar Clusters 1.3 meter 5.00 33.00 0.00 0.00

1469 0 f94 A Landolt, Louisiana State University Broad-Band Standards at +45 Degrees 1.3 meter 8.70 41.10 0.00 0.00

1578 0 f94 T Lanz, NASA Goddard Space Flight Center J Landstreet, University of Western Ontario G Mathys, European Southern Observatory Ap Stars with Magnetically Resolved Lines Coude Feed 6.00 51.00 0.00 0.00

1574 0 f94 T Lauer, National Optical Astronomy Observatories M Postman, Space Telescope Science Institute M Strauss, Institute for Advanced Study Motion of the Local Group with Respect to Distant Abell 2.1 meter 5.00 37.50 0.00 0.00

1517 0 f94 S Lee, Seoul National University B Carney, M Corwin, University of North Carolina The Luminosity/Mass Function for Halo Stars 1.3 meter 6.00 49.50 0.00 0.00 Executed Proposals 10/01/94 - 12/31/94 Page 9 Tue Jan 31 14:02:33 1995

Nights Hours Days Hours 1572 0 f94 M Lehnert, IGPP\Lawrence Livermore Natl. Lab T Heckman, Johns Hopkins University Shock-Heated Gas in Halos of Starburst Galaxies 2.1 meter 5.00 32.00 0.00 0.00

1573 0 f94 M Lehnert, IGPPXLawrence Livermore Natl. Lab T Heckman, Johns Hopkins University Determining the Nature of Diffuse Interstellar Medium in... 0.9 meter 4.00 14.00 0.00 0.00

1503 0 f94 C Martin, R Kennicutt, Jr., University of Arizona Galactic Winds from Dwarf Galaxies 4 meter 2.00 6.00 0.00 0.00

9149 0 f94 P Mason, Case Western Reserve University CCD Photometry of the Unusual Magnetic Cataclysmic Binary.. Burrell Schmidt 2.00 24.00 0.00 0.00

1440 0 f94 P Massey, National Optical Astronomy Observatories Are There Massive Stars in the Andromeda Galaxy? 4 meter 4.00 23.00 0.00 0.00

1496 0 f94 P Massey, C Corson, National Optical Astronomy Observatories S Strom, L Hillenbrand, University of Massachusetts The Star Forming History of h and x Persei Modern Study... 4 meter 2.00 9.00 0.00 0.00 0.9 meter 1.50 20.00 0.00 0.00

1554 0 f94 R Mathieu, University of Wisconsin, Madison A Search for Pre-Main Sequence Eclipsing Binaries 0.9 meter 5.00 56.00 0.00 0.00 Executed Proposals 10/01/94 - 12/31/94 Page 10 Tue Jan 31 14:02:33 1995

Nights Hours Days Hours 1556 0 f94 R McMillan, R Ciardullo, Pennsylvania State University Extragalactic Observations of Supernova Age Indicators 0.9 meter 6.00 53.00 0.00 0.00

1504 0 f94 B McNamara, Harvard-Smithsonian Center for Astrophysics R Elston, M Wise, National Optical Astronomy Observatories B Jannuzi, Institute for Advanced Study C Sarazin, University of Virginia U-Band Polarimetry of Active Central Cluster Galaxies 4 meter 3.00 3.00 0.00 0.00

1614 0 f94 K Merrill, I Gatley, National Optical Astronomy Observatories Ontogeny of the NGC 2024 Nascent Cluster: Near IR Solution 1.3 meter 6.00 57.00 0.00 0.00

1450 0 f94 D Meyer, Northwestern University The Interstellar Lithium Isotope Ratio Toward Omicron Perse Coude Feed 6.00 42.00 0.00 0.00

1651 0 f94 M Meyer, S Strom, L Allen, K Strom, University of Massachusetts S Edwards, Smith College Infrared Spectroscopy of Deeply Embedded Young Clusters 2.1 meter 4.50 52.50 0.00 0.00

9148 0 f94 B Mueller, National Optical Astronomy Observatories I Ferrin, University of the Andes E Alvarez, Activity of Tempel 2 0.9 meter 3.00 24.00 0.00 0.00 Executed Proposals 10/01/94 - 12/31/94 Page 11 Tue Jan 31 14:02:33 1995

Nights Hours Days Hours 1532 0 f94 S Naoumov, B Carney, J Rose, University of North Carolina J Laird, Bowling Green State University The Galaxy's Disk: Two Populations or One? Burrell Schmidt 8.00 60.00 0.00 0.00

1623 0 f94 C O'Dea, S Baum, Space Telescope Science Institute R Gelderman, NASA Goddard Space Flight Center Spectroscopy of Mysterious GHz Peaked Spectrum Radio.... 4 meter 2.80 21.00 0.00 0.00

1460 0 f94 C O'Dell, X Hu, Rice University Physical Properties in the Orion Nebula Near Proplyds.... Coude Feed 7.00 68.50 0.00 0.00

1520 0 f94 F Owen, National Radio Astronomy Observatory W Keel, University of Alabama Evolution of Radio Galaxies to z=l: Optical Imaging 2.1 meter 1.00 10.00 0.00 0.00

1657 0 f94 B Penprase, J Lauer, M Zarins, Pomona College High Resolution Spectroscopy of Absorption Lines Toward.... Coude Feed 4.00 44.00 0.00 0.00

1654 0 f94 S Perlmutter, G Goldhaber, D Groom, R Pain, University of California, Berkeley C Pennypacker, A Kim, Lawrence Berkeley Laboratory D Zaritsky, J Willick, Carnegie Observatories, (OCIW) G Bernstein, University of Arizona B Grossan, Massachusetts Institute of Technology R McMahon, University of Cambridge S Deustua, Lawrence Livermore Laboratory Homogeneity & Rate of High-Redshift Supernovae with .... 4 meter 2.00 20.00 0.00 0.00 2.1 meter 4.00 21.00 0.00 0.00 Executed Proposals 10/01/94 - 12/31/94 Page 12 Tue Jan 31 14:02:33 1995

Nights Hours Days Hours 1652 0 £94 R Peterson, University of California, Santa Cruz R Saffer, Space Telescope Science Institute Rotational Velocities as Population Discriminant for .... 4 meter 3.00 25.50 0.00 0.00

847 2 f94 M Pierce, G Jacoby, J Hedden, S Courteau, National Optical Astronomy Observatories D Crabtree, Dominion Astrophysical Observatory Long-Period Variables: An Alternative to Cepheids? 2.1 meter 2.65 17.50 0.00 0.00 0.9 meter 4.00 35.50 0.00 0.00

1643 0 f94 C Pilachowski, D Rabin, National Optical Astronomy Observatories Magnetic Fields in Metal Poor Stars Coude Feed 6.00 32.00 0.00 0.00

1441 0 f94 C Prosser, Jr., L Hartmann, Harvard-Smithsonian Center for Astrophysics Rotational Velocity Survey Among Pre-Main Sequence K&M .. 4 meter 5.00 29.50 0.00 0.00

1546 0 f94 M Rauch, R Weymann, Carnegie Observatories, (OCIW) R Carswell, University of Cambridge J Webb, University of New South Wales Is There Primordial Gas at Redshift Three? 4 meter 2.85 32.00 0.00 0.00

1587 0 f94 G Rhee, University of Nevada J Stocke, M Harvanek, E Ellingson, University of Colorado A Study of 3C Radio Galaxy Environments at Intermediate z 0.9 meter 2.00 9.50 0.00 0.00 Executed Proposals 10/01/94 - 12/31/94 Page 13 Tue Jan 31 14:02:33 1995

Nights Hours Days Hours 1541 0 f94 D Schade, S Lilly, University of Toronto The Local Density of Star-Forming Galaxies Burrell Schmidt 7.00 38.50 0.00 0.00

1529 0 f94 K Sellgren, T Mailloux, Ohio State University R Smith, ADFA T Brooke, Jet Propulsion Laboratory Search for Interstellar "Diamonds" in Molecular Clouds 2.1 meter 5.70 40.00 0.00 0.00

1628 0 f94 M Skrutskie, M Weinberg, M Meyer, University of Massachusetts A 1.6um Spectral Survey of Evolved Stars Coude Feed 6.00 46.00 0.00 0.00

1640 0 f94 V Smith, University of Texas, Austin K Cunha, Observatorio Nacional High-Resolution Spectroscopy of Low-Mass Orion Association. 4 meter 1.85 0.00 0.00 0.00

1656 0 £94 A Stanford, California Institute of Technology M Dickinson, Space Telescope Science Institute P Eisenhardt, Jet Propulsion Laboratory Galaxy Evolution in High Redshift Clusters 4 meter 3.00 10.00 0.00 0.00 2.1 meter 4.00 35.00 0.00 0.00

1475 0 f94 C Steidel, Massachusetts Institute of Technology M Dickinson, Space Telescope Science Institute M Pettini, Royal Greenwich Observatory The nature of Normal Galaxies at z>l 4 meter 4.90 33.00 0.00 0.00

1449 0 f94 M Strauss, Institute for Advanced Study T Lauer, National Optical Astronomy Observatories M Postman, Space Telescope Science Institute Velocity Dispersions of Brightest Cluster Galaxies: Bulk... 2.1 meter 6.00 59.00 0.00 0.00 Executed Proposals 10/01/94 - 12/31/94 Page 14 Tue Jan 31 14:02:33 1995

Nights Hours Days Hours 1647 0 f94 D Terndrup, M Pinsonneault, S Balachandran, A Krishnamurthi, Ohio State University J Stauffer, Harvard-Smithsonian Center for Astrophysics S Wolff, National Optical Astronomy Observatories M Gagne, University of Colorado A Key Project to Constrain Angular Momentum Evolution of... 4 meter 4.95 45.50 0.00 0.00 0.9 meter 12.00 33.50 0.00 0.00

1435 0 f94 S Veilleux, National Optical Astronomy Observatories D Sanders, University of Hawaii Optical Spectroscopy of a New High Redshift Sample of Ultra 2.1 meter 4.00 2.00 0.00 0.00

1482 0 f94 F Walter, L Matthews, N Adams, SUNY at Stony Brook A Brown, University of Colorado The Deep ROSAT Survey of Orion: Identifying Low Mass Stars 2.1 meter 6.00 48.50 0.00 0.00

1627 0 f94 A Watson, J Gallagher, T Tripp, University of Wisconsin, Madison E de Feijter, Lowell Observatory NIR Hydrogen Recombination Line Mapping of Nearby Nuclear.. 1.3 meter 5.00 25.00 0.00 0.00

1536 0 £94 A Welty, L Ramsey, Pennsylvania State University A Study of T Tauri Star Winds and Accretion Streams 2.1 meter 7.00 68.50 0.00 0.00

1559 0 f94 R White, Smith College B Rachford, University of Wyoming Titanium Abundances in Pre-shock and Shocked Gas Toward Coude Feed 8.00 63.00 0.00 0.00 Executed Proposals 10/01/94 - 12/31/94 Page 15 Tue Jan 31 14:02:33 1995

Nights Hours Days Hours 1537 0 f94 B Whitney, S Kenyon, Harvard-Smithsonian Center for Astrophysics The Near IR Polarization of the Protostars in Taurus 1.3 meter 6.00 31.50 0.00 0.00

1545 0 f94 L van Zee, M Haynes, A Broeils, Cornell University J Salzer, Wesleyan University Imaging of High Hydrogen Mass-to-Luminosity Ratio Galaxies 0.9 meter 5.00 49.00 0.00 0.00

Total number of proposals: 90 Appendix B

NATIONAL SOLAR OBSERVATORY REPORT Quarter Ended: 12/31/94

Nights Hours Days Hours

1023 R Altrock, PL/GPSS Coronal Observations Evans Solar Facility/SP 74 84

1945 R Altrock, PL/GPSS Emission Line Photometer Support Evans Solar Facility/SP 6 34

1937 J Beckers, National Optical Astronomy Observatories T Rimmele, New Jersey Institute of Technology High Resolution Imaging Vacuum Tower/SP 9 50

1911 P Bernasconi, P Steiner, U Egger, Institut fur Astronomie, Zurich C Keller, National Optical Astronomy Observatories Solar Vector Polarimetry McMP 10 77

1940 P Bernasconi, Institut fur Astronomie, Zurich C Keller, National Optical Astronomy Observatories Two-dimensional Solar Vector Polarimetry Vacuum Tower/SP 12 48

1026 T Brown, National Optical Astronomy Observatories Coronagraph Monitor Evans Solar Facility/SP 42 80

1034 T Brown, National Optical Astronomy Observatories K Strand, High Altitude Observatory Flare Patrol (monitoring) Hilltop Dome/SP 91 541

1035 T Brown, National Optical Astronomy Observatories White Light Patrol (monitoring) Hilltop Dome/SP 91 544 2-

Nights Hours Days Hours

1771 J Elrod, B Armstrong, T Brown National Optical Astronomy Observatories Sunspot Drawings - Manual Drawings of Sunspots Evans Solar Facility/SP 91 69

1706 K Cheng, NASA Goddard Space Flight Center J Neff, Pennsylvania State University Search for New Proto-Planetary System Candidates McMP 6 60

1138 D Deming, NASA Goddard Space Flight Center Monitoring Apparent Velocity of Integrated Sunlight McMP 2 16

1741 J Eaton, Center of Excellence in Information Systems Ha Variations in t, Aurigae Binaries and Cool Supergiants McMP 17 26

1807 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 McMP 28 57

1833 M Giampapa, W Livingston, National Optical Astronomy Observatories Stellar Cycles and the Wilson-Bappu Effect McMP 26 68

1888 M Giampapa, National Optical Astronomy Observatories V Andretta, University of Naples Contemporaneous Lambda 5876 and Lambda 10830 Spectra of F and G Dwarfs McMP 3 30

1916 M Giampapa, T Tilleman, National Optical Astronomy Observatories Sun as a Star: GONG line McMP 3 28 -3

Nights Hours Days Hours

1769 J Harvey, National Optical Astronomy Observatories DAWN (RISE Observations) KPVT 11

3790 J Harvey, National Optical Astronomy Observatories Vacuum Synoptic Program: Daily/Community KPVT 86 272

1692 K Harvey, Solar Physics Research Corp. S Tsuneta, University of Tokyo K Strong, Lockheed Missiles & Space Company L Acton, Montana State University Coordinated Observations with YOHKOH KPVT 31

1918 S Hawley, Michigan State University M Giampapa, National Optical Astronomy Observatories Coordinated Satellite and Ground-based Observations of YZ Cmi McMP 11

1934 B Jackson, University of California, San Diego D Gary, California Institute of Technology D Webb, ASE, Inc. H Hudson, University of Hawaii R Altrock, PL/GPSS Temporal and Spatial coronal Temperature Determinations with Height Evans Solar Facility/SP 18 71

1915 D Jennings, P Sada, G McCabe, D Deming, G Bjoraker, NASA Goddard Space Flight Center Continuing Thermal-IR Spectroscopic Observations of Jupiter and Comet Shoemaker-Levy 9 Fragment Collision Sites McMP 10 99 14 86

1942 P Kaufmann, Centro de Radio Astronomia e Applications J Zirker, National Optical Astronomy Observatories Search for Positions of Millisecond radio Bursts Evans Solar Facility/SP 30 Nights Hours Days Hours

1910 C Keller, National Optical Astronomy Observatories J Stenflo, High Altitude Observatory Coherence Effects in Spectral Lines Near the Solar Limb McMP 42

1912 R Kupke, D Mickey, B Graves, F Roddier, University of Hawaii Curvature Sensing-based Wavefront Sensor for Use with Solar Adaptive Optics McMath-Pierce West 56

1852 T Leifsen, P Maltby, M Omang, M Carlsson University of Oslo Solar Oscillations in Infrared Spectral Lines McMP

1848 W Livingston, L Wallace, National Optical Astronomy Observatories Monitoring of Atmospheric Trace Gases McMP 11

1858 W Livingston, National Optical Astronomy Observatories Cycle Variability of the Solar Spectrum McMP 10 96

1860 J LoPresto, Edinboro University of Pennsylvania A Pierce, National Optical Astronomy Observatories Solar Gravitational Redshift McMP 12

1880 S Martin, California Institute of Technology K Harvey, Solar Physics Research Corp. J Zirker, National Optical Astronomy Observatories O Engvold, University of Oslo V Gaizauskas, Herzberg Institute of Astrophysics T Forbes, University of New Hampshire E Priest, University of St. Andrews Filament Formation Evans Solar Facility/SP 16 88 Vacuum Tower/SP 2 18 5-

Nights Hours Days Hours

1135 P Mcintosh, NOAA T Brown, National Optical Astronomy Observatories W Marquett, California Institute of Technology NOAA Monitoring Program Evans Solar Facility/SP 91 55

1892 J Neff, Pennsylvania State University F Walter, SUNY at Stony Brook Mapping the Chromospheric Structure of AR Lac Over a Stellar Cycle McMP 5 38

1935 D Neidig, PL/GPSS Demonstrate Ground-based Coronagraphic Detection of Space Debris Evans Solar Facility/SP 9 26

1938 L November, L Wilkins National Optical Astronomy Observatories O Bouchard, ICP-French Military Service The Magnetic Force-free Condition with Height in the Solar Atmosphere Vacuum Tower/SP 11 63

1569 L O'Brien, Southern Illinois University Laboratory Measurements of Metal Hydrides in the Near-Infrared FTS 3 24 3 24

1863 A Pierce, National Optical Astronomy Observatories J LoPresto, Edinboro University of Pennsylvania The Absolute Value of the Solar Limb Effects for Different Fraunhofer Lines McMP 11 4

1868 A Potter, NASA Johnson Space Flight Center T Morgan, Southwest Research Institute Studies of Exospheric Emission Lines from Mercury and the Moon McMP 1 2 7 46 6-

Nights Hours Days Hours

1866 D Rabin, National Optical Astronomy Observatories True-Field Imaging Magnetometry in the Near Infrared McMP 70

1936 R Radick, PL/GPSS R Dunn, National Optical Astronomy Observatories T Rimmele, New Jersey Institute of Technology Characterization and Upgrade of VTT Optical Performance Vacuum Tower/SP 16 126

1901 T Rimmele, P Goode, New Jersey Institute of Technology R Stebbins, University of Colorado Oscillation Excitation Mechanisms Vacuum Tower/SP 14 40

1939 G Roumeliotis, University of Sydney S Keil, PL/GPSS K Balasubramaniam, National Optical Astronomy Observatories P Sturrock, Stanford University The Vector Magnetic Field below and H-alpha Filament Vacuum Tower/SP 16 50

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 McMP 18 92

1494 F Scherb, University of Wisconsin, Madison Observation of [OIJ6300 Emission from Io McMP

1881 E Seykora, East Carolina University Solar Photospheric Observations with a New Active Unsharp Mask Filter Evans Solar Facility/SP Nights Hours Days Hours

1037 R Smartt, National Optical Astronomy Observatories Coronal One-Shot (monitoring) Hilltop Dome/SP 16 50

1737 M Smith, C Rinsland, NASA Langley Research Center V Devi, College of William and Mary Long-Path Laboratory Measurements of Infrared Spectra of CO and HO FTS 12 84 12 84

1822 M Smith, T Teays, R Wasatonic, Computer Sciences Corp. E Guinan, Villanova University S Baliunas, A Dupree, D Luttermoser, Applied Research Corp. Harvard-Smithsonian Center for Astrophysics K Nordsieck, University of Wisconsin, Madison Radial Velocity Observations of Alpha Ori, Alpha Sco, and Alpha Her McMP 19 24

1884 M Smith, Computer Sciences Corp. Rapid Lambda 6678 Line Profile Variability in Gamma cas McMP 56

1913 J Stauffer, Harvard-Smithsonian Center for Astrophysics H Bond, Space Telescope Science Institute V471 Tau HST Support McMP 11

1356 K Strassmeier, University of Vienna Doppler Imaging of Spotted Chromospherically Active Stars McMP 27 69

1890 G Tagliaferri, Osservatorio Astronomico di Brera T Fleming, University of Arizona R Pallavicini, Osservatorio Astrofisico Arcetri G Cutispoto, Osservatorio Astrofisico di Catania Spectroscopic Study of Cool Stars Serendipitously Discovered in EUV Surveys McMP 46 Nights Hours Days Hours

1823 I Tuominen, T Hackman, J Huovelin, L Jetsu, University of Helsinki N Piskunov, University of Western Ontario SSaar, Harvard-Smithsonian Center for Astrophysics Surface Imaging of Two Active Stars: HD 199178 and HD 82558 McMP 19 59

1862 O White, High Altitude Observatory W Livingston, National Optical Astronomy Observatories The Sun as a Star: Ca II K Variability McMP 3 19

1024 S Worden, OSUDRE/ADEW S Keil, PL/GPSS Solar Rotation 3898-3954A Evans Solar Facility/SP 79 209

Total number of proposals: 54 APPENDIX C

US Sites Safety Report

Following is the summary of recordable occupational injuries and illnesses for the US sites as reported on the respective CY 1994 OSHA 200 logs. As required, the respective data will be posted at each site no later than 1 February.

KPNO NSO/SP Tucson Total

Fatalities

Injuries involving days off or days of restricted work activity or both 2 3 2 7

Injuries involving days off 2 3 2 7

Days off from work 6 71 4 8

Days ofrestricted work activity 0 0 0 0

Injuries without lost workdays 2 0 4 6

Illnesses

Total recordable injuries/illnesses: 14

Mountainwide Fire Alarm Systems: At KPNO, fire alarm systems were installed in all the buildings. A second phase which includes transmitters and a central station receiver and notification system was started and is nearing completion. At NSO/SP, a similar mountainwide system comprised ofindividual fire alarm systems, transmitters and central station receiver was also started and nearing completion.

LPG Tank Farm: At NSO/SP the LPG tank farm was repiped and brought up to current code.

NSO/SP Volunteer Fire Department: Increased their membership to fifteen persons. Because they are a countyfire districtthis increasewill enable state funds for additional equipment. The departmentwas also reclassified from class 10 to class 8 which in effect enable additional state funds for the department.

Permits, Emissions Reports: Various county air pollution permits were renewed and the associated emissions reports filed for the Tucson and KPNO sites. Loss Prevention Reviews: Various reviews were conducted and the resultant recommendations furnished in regards to the following:

8-m telescope at the critical design review state; electrostatic discharge survey ofall the Tucson electronics labs; handling ofdomestic and industrial waste at KPNO; various PC workstations in regards to ergonomically sound principles. followup review ofWIYN building and site; fire inspection ofNSO/SP facilities by the Holloman Air Force Base Fire Marshall's Office; 16" visitor's telescope at KPNO; GONG instrument, shelters and sites; 4-m building for damaged asbestos containing insulation; and, NASA hazard analysis ofexposure to liquid mercury, relative to the future operation ofthe NASA-JSC liquid mercury telescope at NSO Cloudcroft facility.

Training: First responders at the KPNO and NSO/SP site received refresher training in first aid and CPR.

Tucson first responders trained for potential ammonia hydroxide spill.

Maintenance personnel in Tucson were retrained in the proper use ofrespirators for the protection from asbestos, paints and solvents; personnel at NSO/SP received refresher training in minor abatement of asbestos containing materials.

Three Tucson staffattended a seminar on workplace violence.

The NSO/SP site Safety Officer and Maintenance Supervisor attended collateral Safety Officer Training at White Sands Missile Range.

Hazardous Materials/Chemical Waste Disposal: Several drums ofvarious chemical wastes -mainly non- hazardous - were sampled, analyzed and properly disposed. Approximately 300 pounds ofmildly radioactive mirror polishing compound containing ThO which was discovered in the Optics Shop is awaiting proper disposal.

Memberships: NSO/SP became a member ofthe Southwest Federal Safety & Health Council. The NOAO Safety Officer became a member ofthe National Fire Protection Association. APPENDIX C

CTIO Safety Report

CTLORecordable Occupational Injuries: October 1993 - September 1994 (FY 1994)

Fatalities: 0 Injuries involving days off or days of restrictedwork activitiesor both: (

CTLO Recordable Occupational Injuries: October - December 1994

Fatalities: 0 ,„ Injuries involving days off or days of restricted work activities or both: (0o -A - Injuries involving days off: 2 Days off from work: 95 Days of restricted work activity: 0 Injuries without lost workdays: 1

There were no occupational illness recorded at CTIO.