NATIONAL OPTICAL ASTRONOMY OBSERVATORIES

NATIONAL OPTICAL ASTRONOMY OBSERVATORIES

Cerro Tololo Inter-American Observatory Kitt Peak National Observatory National Solar Observatory

La Serena, Chile Tucson, Arizona 85726 Sunspot, New Mexico 88349

ANNUAL REPORT October 1993 - September 1994

November 10, 1994

TABLE OF CONTENTS

I. INTRODUCTION n. AURA BOARD m. SCIENTIFIC PROGRAM

Cerro Tololo Inter-American Observatory (CTIO) 1. A Hubble Diagram of Distant Type la Supernovae 2. The Stellar Populations of the Carina Dwarf Galaxy 3 3. Observations of the Collision ofComet Shoemaker-Levy 9 and Jupiter 4

B. Kitt Peak National Observatory (KPNO) 5 1. Faint Galaxy Halo Could Trace Dark Matter 5 2. Young Stellar Objects in Bok Globules 5 3. A New Tool for Stellar Population Studies 6

C. National Solar Observatory (NSO) 7 1. New Observations of IR Coronal Emission Lines 7 2. High Resolution Infrared Spectroscopy of the Carbon Monoxide Molecule 7 3. Subsurface Magnetic Flux Tubes 8

IV. DIVISION OPERATIONS 9

A. Cerro Tololo Inter-American Observatory 9 1. 4-m Telescope Image Quality Improvements 9 2. Infrared Instrumentation 10 3. Arcon CCD Controllers 10 4. Other Projects 11

B. Kitt Peak National Observatory 11 1. New KPNO Programs in FY 1994 11 2. KPNO Facilities Improvements in FY 1994 13 3. KPNO Instrumentation 14

C. National Solar Observatory 17 1. Image Quality Improvement Program for NSO Telescopes 17 2. Sac Peak Instrumentation 18 3. Tucson Instrumentation 20

D. US Gemini Program 21

E. NOAO Instrumentation Program 22 V. MAJOR PROJECTS 23

A. Global Oscillation Network Group Project 23 B. The Precision Solar Photometric Telescope Project (PSPT) 25 C. SWATH Mission 26 D. WIYN 26 E. Partnerships in Progress at CTIO 28 1. 2MASS Survey 28 2. Sao Paulo Telescope 29 3. Southern Spectroscopic Survey Telescope 29 4. SOAR 29

VI. CENTRAL COMPUTER SERVICES 29

VII. SCIENTIFIC STAFF 30

A. CTIO Scientific Staff Changes 30 B. KPNO Scientific Staff Changes 31 C. NSO Scientific Staff Changes 31

Vm. DIRECTOR'S OFFICE 32

IX. NOAO STATISTICS 33

A. CTIO Statistics 33 B. KPNO Statistics 33 C. NSO Statistics 34 D. NOAO Central Computer Services Statistics 34 E. NOAO Tucson Headquarters Building Statistics 34

APPENDICES

Appendix A: NOAO Technical Reports List Appendix B: CTIO Publications List Appendix C: KPNO Publications List Appendix D: NSO Publications List

n I. INTRODUCTION

This report covers the period 1 July 1993 - 30 June 1994.

The National Optical Astronomy Observatories (NOAO) are operated for the National Science Foundation by the Association of Universities for Research in Astronomy. The four divisions of the NOAO are: the Cerro Tololo Inter-American Observatory (CTIO), in northern Chile; the Kitt Peak National Observatory (KPNO), near Tucson; the National Solar Observatory (NSO), with facilities on Kitt Peak and at Sacramento Peak, New Mexico; and the US Gemini Program (USGP), based in Tucson. NOAO observing and data reduction facilities are available to the entire astronomical community. The NOAO Home Page contains on-line information about NOAO services, including telescope schedules and instrument availability, and information about how to apply for telescope time. The NOAO Home Page can be accessed through the World Wide Web at http://www.noao.edu/.

II. AURA BOARD

NOAO is managed by the Association of Universities for Research in Astronomy, Inc. (AURA). There are twenty-six AURA member universities, including three international institutions. Each member university appoints one individual to serve on the AURA Board, which also includes the President of the Corporation and twelve Directors-at-Large. AURA also operates the Space Telescope Science Institute under contract with the National Aeronautics and Space Administration, and the Gemini 8-m Telescopes Project for the NSF.

III. SCIENTIFIC PROGRAM

A. Cerro TololoInter-American Observatory (CTIO)

1. A Hubble Diagram ofDistant Type la Supernovae

Since the discovery by Edwin Hubble in 1929 that the Universe is expanding, one of the outstanding problems in observational cosmology has been the determination of the Hubble constant, Ho, which measures the rate of expansion in the neighborhood of the Milky Way. Knowledge of Ho is of special importance since it provides a limit to the age of the Universe. In the 65 years since Hubble's discovery, debate has raged over the precise value of Ho, with astronomers currently dividing into two main camps: those who argue for a "short" distance scale with Ho -70-90 km s' Mpc"1, and those who favor a "long" distance scale with Ho -50 km s1 Mpc'1. The short distance scale is supported by several different techniques for measuring distances to galaxies, but a persistent thorn in the side has been the results based on Type la Supernovae (SNe la) which have consistently favored the long distance scale. Indeed, recent distance measurements to the host galaxies of two SNe la using Cepheid variable stars discovered with the Hubble Space Telescope have yielded values of Ho between 50-55 km s'1 Mpc"1. Since several of the distance indicators which support the short distance scale are also based on Cepheid distances for calibration, this disagreement is particularly perplexing.

Recent work by a team of investigators at CTIO and the University of Chile at Cerro Calan led by Mario Hamuy (CTIO) and Jose Maza (U. of Chile) provides a possible resolution to this conflict. From 1990-1993, Hamuy and Maza carried out a supernova search using the Michigan Curtis Schmidt telescope at CTIO with the goal of discovering and observing a sample of distant SNe la which could then be used to study the Hubble diagram of these objects. The first Hubble diagram for SNe la, which was published by Charles Kowal in 1968, yielded a relatively small dispersion (0.6 mag) in the peak brightnesses of SNe la, revealing the potential utility of these objects as extragalactic distance indicators. More modern studies have found a scatter of 0.3-0.5 mag, but two major observational complications have hampered the determination of the intrinsic spread in the peak luminositiesof these objects:

1) These Hubble diagrams are based nearly entirely on nearby objects (z < 0.02). At such low redshifts, the peculiar motions of individual galaxies introduce significant scatter in the velocity field associated with the general expansion of the Universe.

2) Most historical SNe la light curves consist of fragmentary observations, more often than not obtained from photographic plates. With photographic plates, it is difficult to subtract accurately the bright galaxy background light on which the supernovae are often projected. The lack of a precise definition of the photographic band introduces an additional problem when comparing observations obtained from different observers and emulsions. Not surprisingly, even for bright supernovae with frequent observations, large discrepancies (-1 mag) often appear among photometry from different sources.

Since supernovae aretransitory objects, visible typically foronly a few months, they cannot simply be re- observed to improve the data quality. Hence, Hamuy and Maza organized the Calan/Tololo search which led to the discovery of 50 new SNe during the three-year period that it was carried out. Follow-up spectroscopic observations obtained mostly with the CTIO 1.5-m and 4.0-m telescopes revealed that a significant fraction (-60%) of these objects were members of the Type la class, and thatnearly all were at redshifts between 0.02 and 0.1. Thanks to the generous collaboration of many visiting astronomers and CTIO staffmembers, BVRI photometry was secured with CCD detectors for most of these supernovae. So far, light curves have been completely reduced for 13 SNe la (i.e., roughly halfthe complete sample), and the analysis of these data forms the subject of a paper to be published by Hamuy et al. in the January 1995 issue of the Astronomical Journal.

The Hubble diagrams in B and V for these 13 SNe la show clear evidence for a distance-dependent dispersion. Although some of the scatter could be due to the peculiar velocities of the host galaxies or to uncorrected dust absorption in the host galaxies,Hamuy and collaborators argue that the dominant source is an intrinsic dispersion in the peak absolute magnitudes of SNe la amounting to -0.8 mag in MB and -0.5 mag in Mv. The data also confirm, in general terms, the recent finding by Phillips from an independent sample of well-observed nearby SNela that the absolute B and V magnitudes are correlated with the initial decline rate of the B light curve. The sense of this correlation is that the most slowly declining events tend to be intrinsically the most luminous. In addition, Hamuy et al. find rather unexpectedly that galaxieshaving a youngerstellar populationappear to host the most luminous SNe la.

It is these two effects-the dependence of the absolute luminosity on decline rate and host galaxy morphology-that provide the clues to understanding the small value of the Hubble constant derived by Sandage and collaborators from Cepheid distances to the host galaxies of SN 1937C and SN 1972E. As shown by Hamuy et al. from the published photometry of SN 1972E, this supernova was a slow- declining event and, therefore, probably more luminous than average. Using the peak luminosity-decline rate relations derived from either the Phillips or Calan/Tololo samples of SNe la, Hamuy et al. derive a Hubble constant in the range Ho = 62-67 km s' Mpc"1, which is -15% larger than the value that would be obtained if the peak luminosity-decline rate relation were to be ignored. Recent remeasurements by Pierce and Jacoby (KPNO) of the photographic plates obtained by Zwicky and Baade of SN 1937C indicate that this supernova was also an unusually slow-declining event, and so this supernova was probably also more luminous than average. Taken together, the results for these two supernovae imply a Hubble constant of 65-75 km s"1 Mpc'1, favoring the shorter of the two distance scales. Although it is somewhat surprising at first sightthat bothSNe la with Cepheid distances would happen to be unusually luminous events, this is consistent with the fact that both host galaxies, NGC 5253 and IC 4182, show considerable evidence for having experienced significant bursts of recent star formation.

2. The Stellar Populations ofthe Carina Dwarf Galaxy

There are9 known dwarfspheroidal galaxies (dSph) nearthe Milky Way galaxy. Theirrelative proximity allows us to study their properties in detail, shedding light on their stellar populations and galactic evolution. In particular, some dSphs appear to consist of a single, old population like Galactic globular clusters, while others appear to have experienced multiple episodes of star formation. What causes this dichotomy, and further, why are dSphs today devoid of gas, while similar-mass galaxies (the dwarf irregulars) still possess considerable gas? Supernova-driven winds have been suggested as a means for halting star formation and for clearing the gas from dSphs, but it is not clear how some dSphs managed to undergo a second epochof star formation. Massive dark halos, as inferred from the large mass-to-light ratios of most dSphs, may play animportant role in maintaining or acquiring new gas, and must certainly help to keep the stellar systems intact after large episodes of gas loss.

Carina may be an example of a dSph with two different-aged populations of stars. Previous work has shown that the helium core-burning stars in this galaxy form a "red clump" in a color-magnitude diagram, yet RR Lyrae variables, which indicate a bluer horizontal branch population, have been observed. Another study has suggested that there are 2 populations in Carina with different ages; however, the result was barely significant. There has also been disagreement on the distance to Carina. Clearly, this galaxy is a strong candidate for further study.

T. Smecker-Hane, P. Stetson, J. Hesser (Dominion Astrophysical Obs.), and M. Lehnert (Lawrence Livermore National Lab.) have used the CTIO 1.5-m telescope to obtain direct images of Carina in B and I filters, from which they constructed a color-magnitude diagram of the brighter sequences of the dSph (1994, AJ, 108, 507). Their frames covered nearly half of the area of the galaxy, providing them with photometry for over 11,000 stars. They were therefore able to detect sparsely- populated sequences not previously observed in this galaxy. In particular, they found two distinct horizontal branch (HB) populations (stars burning helium in their cores): one population spread in color over the HB, and a second, larger population forming a "red clump" near the red giant branch. Comparing these HBs with other stellar systems of known age and abundance, they inferred that the former is an old, metal-poor population like that of the globular cluster M15, whereas the latter is a younger, but still metal-poor, population. They see these two populations echoed in a color-spread of the red giant branch. The spatial distributions of the two HB populations are identical, suggesting that the star formation episodes which produced them covered similar spatial distributions (since the dynamical relaxation timescale is much longer than the age of the universe). This places constraints on galactic evolution models, particularly with regard to mechanisms for retarding star formation in the interval between the formation of the two stellar populations.

From the color of the red giant branch, they determined that the old, bluer-HB population has an abundance [Fe/H] —2.2 dex, while the red-clump population is slightly more metal-rich, at -2.0 dex. From the magnitudes of the HB stars, and of the red giant branch tip, they estimated a distance modulus of 20.09 ± 0.06 mag, which is about 0.3 mag fainter than the value usually adopted. Employing previously determined main sequence turn-off magnitudes, along with their new abundances, they derive preliminary age estimates of > 10 billion years and > 6 billion years for the bluer-HB and red-clump populations, respectively. They also derive new values for Carina's integrated magnitude and mass-to- light ratio, based on their updated values.

In November 1993, the group obtained deeper images with the CTIO 4-m telescope. A preliminary, unpublished color-magnitude diagram shows two clearly distinct main sequence tumoffs feeding into the one red giant branch described above. This confirms the claim for two populations of different age. The group also plans to obtain spectroscopy for a large number of Carina giants, in order to confirm the abundance estimates obtained from the color of the red giant branch. This will provide the observational data needed to form a comprehensive picture of the star formation history of Carina.

3. Observations of the Collision of Comet Shoemaker-Levy 9 and Jupiter

The much anticipated collision of comet Shoemaker-Levy 9 with Jupiter disappointed no one. The effects, which many astronomers expected to be negligible, were spectacular and very well-observed, thanks to an unprecedented global observational campaign.

The sequence of observable events for the larger impacts, gathered from many observatories, went something like this: As the nuclei approached Jupiter, the clouds of dust which surrounded them and made them visible were stretched out towards Jupiter by tidal forces, and the previous anti-sunward tails, produced by solar radiation pressure on the dust, disappeared. The actual impacts produced rather faint 30-second flashes at 0.95 microns, seen by the Galileo spacecraft, but visible-wavelength flashes reflected off the satellites have not been confirmed at the time of this writing. Within a couple of minutes, "fireballs" developed which were big enough to rise above Jupiter's limb and be seen directly from Earth; some of these were incredibly bright, brighter than Jupiter, between 2 and 10 microns. Spectra revealed emission lines due to CO and other species. These fireballs faded over tens of minutes, by which time a cloud at theimpact site began to rotate into view. The clouds were very large, more than ten thousand km across even when new, and were probably generated in situ by the effectsof the fireball as it spread laterally, predominantly to the south of the impact point. The largest impacts showed spectacular rings spreading out from the impact point in the first hour after impact, presumably atmospheric shock waves of some sort. Many of the impact-generated clouds lasted several weeks. They were dark at visible wavelengths, very conspicuous visually, and very bright against the dark planet at wavelengths absorbed bymethane, indicating a very high altitude, above most of the methane absorption: residual CH, absorption can be used to estimate cloud altitudes. HSTand groundbased images revealed a complex dark core andanextended crescent-shaped halo to thesouth of each impact site.

Not all of the 20impacts produced such dramatic effects. Several of the fragments seen in the pre-impact images produced no observable effects at all, while others of similar pre-impact brightness were spectacular. Intriguingly, most of the fragments which "fizzled" were displaced away from the linear alignment of the other fragments in pre-impact images.

CTIO playedan important part in this campaign, despite bad luck with both the weather and the faintness of the impacts that were visible from there. Wide-field CCD imaging on the Curtis Schmidt telescope by P. Seitzer (U. of Michigan) was used to obtain final astrometry of the comet fragments just days before the impacts began. J. Spencer (Lowell Obs.), D. Depoy (Ohio State U.), J. Frogel (Ohio State U.), and N. Schneider (U. of Colorado), using the OSIRIS camera atthe 4-m, obtained some of the first images of the persistent cloud at the first impact site in the hours after the impact at 2.3 microns, and continued to image the development of the clouds as they accumulated over the following week. OSIRIS also obtained 1 - 2.5 micron spectra with a resolution of 500 of several of the impact sites: these show CH4 absorption above the clouds and will provide estimates of cloud altitude. S.-J. Kim (U. of Maryland), C. Dumas (CalTech), J. Elias (CTIO), and R. Elston (CTIO) used the IRS 1-5 micron spectrometer at the 1.5-m telescope, and among other things detected CH4 emission from the A impact site, which will constrain physical conditions at this site in the hours after impact. IRS 5-micron spectra of the D site showed very strong continuum emission and several molecular species, and many other spectra were obtained. CCD imaging by B. Schaefer (Yale U.) and F. Ringwald (Keele U.) at the 0.9-m and C. Ford (Lowell Obs.) at the Lowell 24-inch showed the development of the dark impact clouds in the visible, and the 16-inch provided spectacular visual views of the impact sites.

B. Kitt Peak National Observatory (KPNO)

1. Faint Galaxy Halo Could Trace Dark Matter

The high rotation speeds of gas and stars in the outermost regions of spiral galaxy disks have implied the existence of massive halos of dark matter. These extended halos are postulated to create gravitational potentials adequate to support and stabilize the disk rotation, but they had not been directly detected. P.D. Sackett (Inst, for Advanced Study), H.L. Morrison (Hubble Fellow at KPNO), P. Harding (Steward Obs.), and T.A. Boroson (USGP/NOAO) report in a Letter to Nature in August the detection of a faint light halo in an edge-on spiral galaxy. The properties of that halo suggest that it might trace the distribution of the dark matter, and may give clues to the nature of the dark matter itself.

The group's imaging observation of the spiral galaxy NGC 5907 in red light was performed with the KPNO 0.9-m telescope and Tektronix 2048 x 2048 CCD. By taking 3 hours of exposure on the galaxy and 7.5 hours of exposure on the dark sky, they were able to define the night sky brightness level to an accuracy of 0.01% and the detector small-scale response to 0.02%. They detected extended light associated with the galaxy at a level of 1% of the night sky brightness, a detection with high confidence because of the high accuracy of the measurement. The best fitting profile is that of a flattened spheroid, with an axial ratio of about 2:1 and a luminosity density that falls off as the inverse square of the distance from the center. For comparison, the observed field stars and globular clusters in the halos of our Galaxy and M 31 fall off as the cube or fourth power of the radius. Dynamical modeling of the rotation curve of NGC 5907 requires a halo mass profile similar to the light profile observed, and suggests a mass-to-red- light ratio about 400 times that of the Sun for the average contributing star. That value is similar to the ratio for metal-poor M dwarf stars in the Milky Way halo, and is almost an order of magnitude lower than that inferred for brown dwarfs near the hydrogen-burning limit. The dark matter halo in NGC 5907 could therefore be composed of metal-poor lower main sequence stars. Observations in other color bands can confirm the nature of the stars contributing to the faint light profile of the galaxy.

2. Young Stellar Objects in Bok Globules

A class of astronomical objects, identified by Bart Bok in the 1940s, consists of isolated, nearly round patches of obscuration seen against the dense field of stars observed near the Galactic plane. They are now known to be nearby, small, dark clouds of cold gas and dust, often containing dense compact cores as small as 0.1 parsec. The smaller globules may be the sites of formation of individual or very small groups of stars. J.L. Yun (U. of Lisbon) and D.P. Clemens (Boston U.) used the SQIID near-infrared imager on the KPNO 1.3-m in combination with other telescopes and IRAS mid-infrared data to perform a detailed survey of 34 sites with candidate Young Stellar Objects (YSOs).

They found that the ratio of 12-micron to 25-micron mid-infrared flux in the satellite data serves as a very good predictor of the near-infrared and optical properties of the globules, and that an ordered sequence of those ratios is probably an evolutionary sequence for the YSOs. The objects with stronger 25-micron fluxes tend to have molecular outflows detected in carbon monoxide and near-infrared nebulae imaged with SQIID that are brighter at the redder near-infrared wavelength of 2.2 microns than at 1.1 microns. The objects with stronger 12-micron fluxes tend not to have molecular outflows, to have near- infrared nebulae brighter at shorter wavelengths, and to show optical nebulae not visible in the redder objects. The morphologies of the associated nebulae are well matched by theoretical models that have a small disk plus infalling envelope with evacuated cavity. The interpretation is that the redder objects are younger, more deeply embedded in their natal clouds, and show strong molecular outflows as part of early star formation. The bluer objects have apparently dissipated more of their associated obscuring material, allowing greater visibility for the reflection nebulae at shorter wavelengths, including optical light.

3. A New Tool for Stellar Population Studies

A major problem in extragalactic studies is untangling the combined effects of ages and metallicities of the stellar populations that determine a galaxy's integrated color and brightness. In visible light, the integrated properties are often dominated by dwarf stars near the main sequence turn-off, or by younger, more recently formed luminous massive stars. Inredder light, there is uncertainty asto whether the signal is produced by the numerous lower-mass main sequence stars or by the more rare but much more luminous red giants and supergiants. E.A. Ajhar (KPNO) and J.L. Tonry (MIT) have applied the technique of surface brightness fluctuation (SBF) measurement to globular clusters in order to address this question. Their results appeared in a report in theJuly 1994 Astrophysical Journal.

In mathematical terms, the integrated light and colors of a galaxy are measurements of the sum of the brightnesses of all the stars, while the surface brightness fluctuations arise from a sum of the squares of the brightnesses of individual stars, divided by the integrated light. That technique emphasizes the contribution of the most luminous stars, the red giants and supergiants. Ajhar and Tonry used the KPNO and CTIO 4-m telescopes to take prime focus images of 19 globular clusters and apply the SBF methods. The globular cluster stars are generally a population of single age and mctallicity, and allow a check on calibrations applied to the more complex mixed populations of entire galaxies. The calibrations are critical to determinations ofthe extragalactic distance scale, because the absolute brightness ofthe typical contributing stellar type makes a standard candle with low apparent scatter. The absolute fluctuation magnitude for the globular clusters in the near-infrared I band is brighter than that found for galaxies, while the galaxy results disagree with theoretical predictions. The interpretation rests on the form of the spectra ofthe luminous giant stars as a function ofthe content ofheavy elements intheir atmospheres. As the heavy element fraction increases, molecules tend to blanket the luminous output of the star, first in visible wavelengths, then in the near infrared. The effect is to dim the brightness ofa giant star ofa given mass, and make its visible to near-infrared flux ratio decrease. The globular clusters show bluer fluctuation colors and more luminous mean fluctuation luminosities than do the much more metal- enriched galaxies, consistent with this interpretation. Further work in the near-ultraviolet may provide a discriminant for age as well. C. National Solar Observatory (NSO)

1. New Observations ofIR Coronal Emission Lines

New ground-based coronagraph observations have been obtained at NSO/Sac Peak. The first ground- based measurement of the 1430 nm [Si X] coronal emission line was made, and accurate wavelength and intensities were recorded (Perm and Kuhn, ApJ, 20 Oct 94). New, more accurate measurements of the [Fe XIII] line pair wavelengths have also been made. The search for other coronal emission lines in the near-infrared spectrum continued with a search for lines observed by Olsen et al. (Solar Physics, 1971). Their observations were not repeatable, and upper limits have been set for coronal emission from [S IX] at 1266 nm (less than 4 x 106Bo) and from [Cr XI] at 1523 nm (less than 3 x lO'BJ. A coronal spectral scan from 1165 to 1261 nm detected no coronal emission lines brighter than the [Fe XIII] 1075 nm emission (less than 3x 106Bo) nor any prominence lines brighter than 3x 106Bo, although He I 1083 nm emission was seen at an intensity of about 100 x 10 6Bo. A more complete study of the coronal spectrum from about 1000 nm to 1400 nm will be done during the November 1994 total eclipse in Chile; the sensitivity of these observations should be an order of magnitude better than coronagraphic studies.

Measurement of the ratio of the two [Fe XIII] lines is important for determining the coronal electron density. The new 256 x 256 HgCdTe IR array provides good sensitivity at these wavelengths; exposures of 2 seconds on the 40-cm coronagraph and Littrow spectrograph provide high signal-to-noise spectra. The calculations of Flower and Pineau des Forets (Astron. and Astrophys., 1973) are applied to NSO/Sac Peak data as well as to data from the 1991 total eclipse taken on Mauna Kea. Emission from the [Fe XIII] 1079.8 nm line and the [Si X] emission line is correlated with the coronal electron density as determined from the [Fe XIII] tine ratio. The intensity does not appear to vary as Ne2 as expected; rather the observed line intensity varies as Ne°'5. Models of the optically thin corona where the electron density varies along the line of sight reproduce this spurious line intensity behavior, but nonetheless give accurate Ne measurements from the line ratio technique (Perm and Kuhn, NSO/SP 1994 Workshop Proceedings). More advanced modeling that includes temperature variations will be required to explain the line emission as well as the continuum emission from the corona.

The search for bright coronal emission lines at IR wavelengths is driven by the possibility of measuring the coronal magnetic field. Using a Wollaston prism to measure both circular polarizations simultaneously, polarization data of the [Fe XIII] 1075 nm emission line was taken using the NSO/SP 40-cm coronagraph and Littrow spectrograph. By measuring both polarizations simultaneously and then switching the polarizations on the array, the data are relatively free from seeing effects and completely insensitive to gain variations on the detector. A slit-averaged spectrum showed Zeeman splitting consistent with a 40 Gauss coronal magnetic field (Kuhn, NSO/SP 1994 Workshop Proceedings). As the Zeeman splitting becomes more favorable with increasing wavelength, emission lines at longer wavelengths, such as the expected [Fe XII] line at 2217 nm (Chang, NSO/SP 1994 Workshop Proceedings), may provide a direct window on the coronal magnetic fields.

2. High Resolution Infrared Spectroscopy ofthe Carbon Monoxide Molecule

Carbon monoxide (CO) in the solar atmosphere is thought to exist primarily in highly structured and anomalously cool clouds in the high photosphere and low chromosphere. The temperature in these structures can be as low as -3,700 K, significantly colder than the "typical" photospheric temperature (-6,000 K). Several explanations have been proposed for this apparent thermal bifurcation. For example, radiative cooling by COitselfmay trigger a thermal instability. Alternatively, thedominant effect may be the quasi-adiabatic cooling of gas lofted into the mid-photosphere by the overshoot of granular convection. If several mechanisms are at work, their relative importance is probably modulated by the presence of concentrated magnetic fields. We want to understand where, when, and why CO exists in order to understand how the solar photosphere departs from simple one-dimensional models in hydrostatic equilibrium andhow this complex structure is related to theexistence of thechromosphere.

During 1993-1994, two infrared experiments at the 1.5-m McMath-Pierce Telescope probed the spatial and temporal distribution of CO in the atmosphere. The fundamental vibration-rotation bands of CO near 4.67 mm are excellent temperature diagnostics because radiative transfer models have demonstrated that these lines form nearly in LTE.

A team led by Alan Clark (U. Calgary) used the McMath-Pierce 13.7-m vertical spectrograph and an infrared array camera to obtain high resolution spectra of more than a dozen CO lines during the partial solar eclipse of 10 May 1994. It is particularly difficult to study the vertical distribution of CO because the layer in which it forms is only about one arcsec thick. Eclipse observations can use the distant "knife- edge" of the lunar limb to achieve an effective angular resolution of about 0.1 arcsec, ten times better than is possible with conventional observations degraded by atmospheric turbulence and telescope diffraction. Initial analysis of the eclipse data reveals that emission from the strong 12CO 3-2 R14 line extends about 0.55 arcsec beyond the continuum limb, while the weaker 12CO 6-5 R47 line emission extends to about 0.38 arcsec and the 13CO 4-3 R43 emission reaches only to 0.15 arcsec. These extensions are significantly smaller than have been inferred from existing non-eclipse data and will require modifications to the models proposed to interpret those observations. NSO/T staff members participating in the eclipse observations included P. Hartmann, D. Jaksha, C. Lindsey, W. Livingston, C. Plymate, and D. Rabin. NOAO senior programmer K. Gillies provided special-purpose software; NSO REU student S. Keilholz (U. Missouri) assisted withdata analysis.

H. Uitcnbroek and R. Noyes (Harvard-Smithsonian CfA) and D. Rabin (NSO/T) exploited the imaging capability of the infrared array camera to analyze spatially and temporally resolved CO spectra in active and quiet regions on the solar disk (ApJ 423, L67). The observations show that, in the quiet Sun, spatial variations in CO intensity are largely dynamical in nature, supporting the theoretical suggestion that dynamical effects play a key role in the formation of the dark CO line cores. Bright, isolated network elements appear to dominate the thermal structure at the height of formation of 12CO 7-6 R68; higher in the atmosphere, the stronger 12CO 3-2 R14 line shows a different topology that is consistent with hydrodynamic perturbations giving rise to isolated low-temperature spots (200-300 K below average). Time sequences of resolved spectra exhibit mainly 3-minute power in line-core intensity but mainly 5- minute power in Doppler shift. This constrains models of CO line formation to those in which the cores form high enough in the atmosphere to sample the 3-minute oscillations with the observed amplitudes.

3. Subsurface Magnetic Flux Tubes

S. D'Silva has studied the interaction ofacoustic waves with the magnetic flux tube that forms a sunspot, in an attempt to decipher the subsurface structure of sunspots. Acoustic waves are known to be absorbed by sunspots. In addition, he found that a sunspotwith a monolithic flux tube structure would have to mix modes; it would reflect the incoming acoustic modes into modes with a completely different horizontal wave length, which we call mode-mixing. He found mode-mixing to be sensitive to the subsurface structure of the flux tube, and the scattered modes carry information of the subsurface geometry. Time- distance helioseismology was found to be a potential tool to decipher this information, and as a first step D'Silva studied the signatures of various flux tube geometries through the acoustic modes scattered by them.

In another attempt to understand the subsurface connection of sunspots, D'Silva studied the dynamics of flux tubes rising from the base of the convection zone, which are believed to produce the sunspots we see. Sunspots are known to exhibit longitudinal and latitudinal velocities which are correlated. It was believed that this velocity correlation was due to the Reynolds stresses of the turbulent plasma in which these sunspot-flux tubes are anchored. He found an alternative explanation-the Coriolis force acting on the rising flux tubes could easily explain the velocity correlations; Coriolis force pushes the faster rotating spots equatorward and slower rotating spot poleward. These attempts to understand the subsurface connection of sunspots have also led to a possible unification of the origin of plages and spots, with the density stratification of the lower layers of the convection zone. These studies indicate a need to try alternate prescriptions of mixing-length theories in the solar model calculations.

IV. DIVISION OPERATIONS

A. Cerro Tololo Inter-American Observatory

Over a several year period CTIO is concentrating its instrumentation and ETS resources in three primary areas: improvements to the 4-m telescope; new or upgraded IR instrumentation; and getting Arcon CCD controllers into use on the telescopes. Good progress was made in all of these areas during FY 1994.

1. 4-m Telescope Image Quality Improvements

Using the sub-arcsecond performance standard now expected from all new telescopes, CTIO has continued its program aimed at improving the image quality delivered by the 4-m telescope. In the past the telescope's performance has been limited both by seeing and by its optics. A multi-year program of improvements to the telescope's thermalenvironment, aimed at decreasing the dome seeing, was finished during the past year. One of the final steps was to install a cooling system for the primary mirror; the system is run during the day in order to slightly overcool the mirror in preparation for the night's observing. A new building to house the Telescope Operations group was also completed; when it is occupied early in FY 1995, it will remove further extraneous activity from the 4-m building and, more importantly, allow the removal of the machine shop that is a major heat source in the 1.5-m dome.

A major effort has gone this year into improving the telescope's optics. The figure of the f/7.8 secondary mirror was significantly improved through ion polishing by Kodak. Previously this mirror had an incorrect conic constant, which caused severe spherical aberration, and also had high frequency ripples on its surface. Reinstallation of the improved mirror immediately resulted in images in the 0.7-0.8 arcsec FWHM range, an improvement of 0.2-0.3 arcsec over the previous best-case images. While the secondary was being repolished, a new collimation system for the mirror was built. This provides precise computer control of collimation and focus, which fits into the overall active optics approach described below.

The 4-m primary mirror is of very high quality but the original support system was not capable of highly accurate support of the mirror. The major effect is astigmatism in certain parts of the sky; trefoil aberration is also detected. Since the axial support of the mirror consists of 33 "air bags" (pneumatic pistons), the system lends itself to an active optics approach, in which each air bag would be controlled individually in order to bend the mirror in its eigenmode shapes, to counteract the existing aberrations. This system was installed on the telescope during a month-long shutdown in August/September, and is presently being tested. It has so far been demonstrated that the mirror can be bent into the various modal shapes without problems, and that the astigmatism previously present can be removed to good accuracy. The system should go into routine use sometime in early calendar 1995.

The overall active optics scheme is to correct coma by tilting the secondary mirror using the new collimation system, while all of the other low-order aberrations are removed with the primary mirror control system. The other necessary ingredient is an image analyzer to measure the aberrations that need to be corrected. A Hartmann screen is presently being used, but this requires dedicated engineering nights, and prevents on-line use or frequent checking of the telescope's performance. A Shack-Hartmann system is under construction; it will be mounted on the existing Cassegrain offset guider probe and will be used at the f/8 focus. This will provide real-time diagnostic capability, though it is expected that most of the time the active corrections will be driven from look-up tables.

2. Infrared Instrumentation

The newest CTIO infrared instrument, put into service in 1994, is a direct imager that uses a 256 x 256 NICMOS array. All of the mechanical parts including the dewar were designed and built at CTIO, representing a substantial effort for the ETS group in Chile. The detector and Wildfire controller were provided by the NOAO infrared group in Tucson.

CTIO's infrared group also made a major upgrade to the infrared spectrometer (IRS) this year. A 256 x 256 InSb array was installed in the spectrometer, which had previously had a 58 x 62 array. Much of this effort was provided by NOAO staff in Tucson, who characterized the detector and provided a Wildfire controller.

The installation of the new detector into the IRS and the commissioning of the new direct imager are excellentexamples of NOAO-wide effort. R. Elston and M. Lazo (CTIO) traveled to Tucson to install the new IRS detector, then both instruments were brought to Chile. They were commissioned at CTIO in July and August with theparticipation of J. Heim (NOAO-EEL) andN. Buchholz (NOAO-CCS).

The CTIO infrared group is in the design stage of building a new f/14 tip-tilt secondary. Modeling the servo loop for the system and planning how to light-weight the mirror blank were carried out this year. The mirror will be polished in the NOAO optical shop in Tucson, and CTIO will build the mirror cell, collimation and tip-tilt control units, and the tip-tilt detector system. The new secondary will enable CTIO to share infrared instruments with KPNO (who have recently switched to f/15) and Gemini (f/16). In addition the tip-tilt system will complement CTIO's program to improve theimage quality at the4-m. The f/14 focus will be used forinfrared imaging and spectroscopy and for optical imaging.

3. Arcon CCD Controllers

CTIO's program to design and build new state-of-the-art CCD controllers has now moved into a mature phase; large numbers ofthese units are being put into routine use on telescopes. The goal is to replace all VEB CCD controllers by the end of FY 1995. Four new Arcon controllers are now in routine use at the Observatory; two more are inthe process of being mated to CCDs. In addition, one laboratory Arcon and

10 one for the WIYN telescope have been produced. An additional 2-3 Arcons are needed to support existing CCDs on Cerro Tololo, and more are needed for projects such as the mosaic and mini-mosaic imagers. The Arcons are very popular with CTIO's users, who appreciate the combination of fast multi- quadrant readout and low noise. Astronomers and technical staff alike are also very pleased with the great improvement in reliability over the 15 year-old VEB controllers.

4. Other Projects

A long-term project which continued through FY 1994 is the construction of "Smart Motor Controllers." These are built around Standard Bus components and are connected to the computer network by RS-485 lines. They are replacing Camac crates plus a hodgepodge of home-built multiplexers.

An historic moment was realized when CTIO's "Tolnet" computer system was finally turned off forever. This network of ancient Data General Eclipses had at one time run all of the instruments on the mountain top, but had gradually been superseded until it was used only with an infrared photometer and for passing coordinate information to a few instruments. Since the Tolnet system had become a major maintenance headache, it was decided to retire the elderly IR photometer, and Tolnet along with it.

CTIO staff have become involved in scientific, technical and administrative activity in support of Gemini South, located on nearby Cerro Pach6n. In particular, work on the site preparation for the southern telescope is now under way. The site has been leveled to form a platform at the 2715-m contour. Work is proceeding on the realignment and upgrade of the access road and installation of the commercial power line to the summit area; the new access road from the summit already reaches the general area where the dormitory buildings will be sited. Paul Gillett, Gemini Site Engineer for Cerro Pach6n, has arrived in La Serena with his family; he is the first member of the international Gemini Project to arrive in Chile. The Gilletts have taken up residence in the CTIO Observatory compound.

B. Kitt Peak National Observatory

Kitt Peak National Observatory has achieved several important technical goals and milestones during this reporting period.

1. New KPNO Programs in FY 1994

During FY 1994 construction of the new WIYN Observatory was completed and the commissioning phase began. Operations are expected to start in March 1995, with a period of "shared risk" observing during the final shakedown of the telescope and instrumentation. Forty-five proposals were received by the September 30 deadline. NOAO will get 40% of the time on the WIYN telescope; most observations will be obtained via queue scheduling. The decision to implement queue scheduling on WIYN is motivated by the desire both to provide new science opportunities to the community and to develop new observing protocols applicable to the Gemini Telescopes. KPNO support staff have been identified to carry out the WIYN observing program for NOAO. Two facility instruments will be available on the WIYN telescope: the Hydra fiber positioner and bench spectrograph (moved from the Mayall 4-m Telescope) and a CCD imaging camera.

11 In spring of 1994, new proposal submission procedures were initiated for telescope time at KPNO. For the first time proposals, including figures, were accepted via e-mail. A new proposal form in LaTeX, modeled on the AASTeX style adopted by the AAS for the submission of journal articles and meeting abstracts, was used. Seventy-eight percent of the proposals for the spring 1995 semester were received electronically. CTIO has also adoptedthe new proposal submissionproceduresdeveloped by KPNO.

KPNO has initiated a program whereby large observing projects with broad implications can be supported at Kitt Peak (i.e. key projects). This program builds on our existing program of "long term status" in which observers can propose for and receive a commitment of telescope time over several semesters. The purpose of this program is not only to provide a wider variety of scientific opportunities to the community, but also to develop expertise within NOAO to review, allocate, and support large programs. Key projects can be awarded up to 20 nights per semester for up to three years. KPNO also supports, on a competitive basis, small workshops for teams to meet together to prepare key project proposals. Key Project Proposals are reviewed by the Telescope Allocation Committee. Criteria in addition to scientific merit for reviewing Key Projects will include: (1) is access to significant amounts of telescope time necessary to make progress on the scientific problem; (2) will KPNO telescope time comprise most of the observing for the project; (3) will the projects selected be distributed among several KPNO telescopes, and not be concentrated on the 4-m; and (4) will the large body of data collected will be made available to the community? Two Key Projects were approved and scheduled for the fall 1994 semester. While neither involved long term status, both received larger blocks of telescope time, including 4-m time, than are usually scheduled.

Since July 1993, KPNO has been routinely saving raw CCD images taken with our telescopes. During FY 1994 CCD spectra from the Solar-Stellar Synoptic Program at the McMath-Pierce SolarTelescope as well as images from IR arrays in use at KPNO telescopes were added to the archive. The rate of data collection will exceed half a terabyte each year when the WIYN telescope becomes fully instrumented and operational. While the data are not generally available to the community, the archive has already proven scientifically useful. Long term observing programs monitoring solar system and extragalactic objects have been organized that rely on images contributed by observers. The archive simplifies such ad hoc scientific collaborations by avoiding data chasing headaches: an observer who finds herself with a convenient hour angle window need only snap the requested picture and e-mail a unique image identifier to the Pi-no fuss, no tapes, no FTP. The archive is also useful for observatory operations, allowing us to monitor image quality anddetector performance at KPNO telescopes. Anatlas of CCD problem frames is being compiled in a similar way to assist observers in recognizing and identifying problems in theirdata. Finally, the archive has allowed us to recover for observers over 15 nights of data that would have been lost due to tape errors, reduction mishaps, and theft.

KPNO has taken significant steps in the last year to improve its electronic presence in the community. Announcements of important opportunities are sent to users via e-mail, and a variety of KPNO documentation and information are now on-line via Mosaic and anonymous FTP. Many instrument manuals have been put on-line, and the "Users Handbook", which is distributed each semester to all principalinvestigators awarded telescope time, is also available.

In January 1994, KPNO staff sponsored a "Town Meeting" at the 183rd Meeting of the American Astronomical Society in Crystal City. This meeting was an experiment to open a dialog directly with the community. A questionnaire was distributed to users in October 1993 to evaluate how the needs of the astronomical community can best be met. The questionnaire was sent via e-mail to 520 proposal applicants from recent years; 166 replies were received. The most significant results of the survey are

12 listed below. On the issue of what should be KPNO's highest priority, the questionnaire results were very clear: KPNO users' highest priority is to keep the telescopes open.

28% of the respondents reported that their observing runs exceeded a 90% success rate, while 52% reported a success rate exceeding 70%. The reason most cited for lack of success was weather (55%).

95% of the respondents having experience at other observatories described KPNO telescopes as comparable or superior to those used elsewhere.

The primary reason for using KPNO is to gain access to reliable instrumentation.

The response to problems at the telescope was at least adequate 95% of the time and excellent 72% of the time.

91% felt the TAC process was fair most of the time; 81% felt the TAC comments they received on denied proposals were useful.

IRAF is used as a primary system by 85% of our users, 92% find it sufficient for quick-look reductions at the telescope, and 90% were happy with the ICE control system for CCDs.

65% of KPNO users are from universities, distributed nearly equally from graduate students to full professors.

69% of KPNO users paid for their recent runs with funding from either NSF or NASA, while 12% found their observing plans hampered by not having funding.

Our users prefer that observing runs at the 4-m should be kept to an average of length of 3 nights.

2. KPNO Facilities Improvements in FY 1994

As described elsewhere in this report, the construction of the 3.5-m WIYN telescope was completed in FY 1994, and the commissioning phase was begun. NOAO is responsible for 40% of the costs of the commissioning phase, and has been providing engineering, operations, and software support to the new facility, including telescope operators, as it comes on line.

As part of a long term program to improve the image quality delivered by the 4-m Mayall telescope, the KPNO Engineering Group installed a system developed at CTIO for cooling the oil for the telescope bearings. The relatively high temperature of the oil has been a major source of heat affecting the image quality of the 4-m.

Also at the 4-m, the electronic and mechanical systems in the guider and instrument rotator were refurbished, the secondary flip mechanism was repaired, oil drain lines from the hydrostatic bearings were replaced, the primary mirror was re-aluminized, the primary mirror support system was refurbished, the computers were upgraded, the upgrade of the control system was completed, a damaged axial bearing was repaired, and the mount for the declination encoder to improve pointing accuracy was replaced.

A cryogenic cooler for infrared instrumentation was installed at the 2.1-m telescope and successfully tested with the multi-color SQIID infrared imager. The cryo-cooler is used in place of liquid helium to

13 cool infrared detectors and instruments. All new IR instruments are designed to work with cryo-coolers for improved reliability and lower operations costs.

Of greatest significance to observers at the 0.9-m telescope is the installation of vents in the dome to improve air flushing in the telescope enclosure. This modification has already yielded a substantial improvement in seeing at the 0.9-m telescope. A new secondary mirror cell and mercury band were also designed for the 0.9-m telescope to improve optical alignment and collimation of the secondaries. The new cell will be installed in the telescope early in FY 1995.

The IR Instrumentation Group has completed an electronics upgrade for IRIM and CRSP so that both instruments arein routine service with the Wildfire array controls andobserving interface.

Following the 1994 summer shutdown, the observers' workstations at the KPNO telescopes were permanently switched overto X-windows. IRAF has been updated to version 2.10.3 to support the new wiring required by xgterm and ximtool. ICE itself has also been updated (to version 1.6), including a few more features that are described in the ICE manual.

3. KPNO Instrumentation

The KPNO instrumentation groups continued their emphasis on the production and upgrading of major focal plane instruments, detector research and development, and exploration of high-resolution imaging. Substantial improvements in performance were achieved at all KPNO telescopes in FY 1994 through a variety of improvement projects.

Infrared Instrumentation Group The ALADDIN array development program is a joint effort among Hughes Santa Barbara Research Corp., NOAO, and the US Naval Observatory in Flagstaff. The goal is to produce high performance 1024 x 1024 InSb arrays for astronomical use. These detectors will be valuable for Phoenix, SQIID, COB, and all the planned near IR instruments for NOAO and Gemini. The silicon readout array architecture was designed and fabricated with apparently initial success. Cold testing of several 512x512 quadrants indicated that the bare readout was performing nominally. Afirst device is being prepared for mating the InSb detector material to the readout. An infrared dewar isbeing modified to accommodate camera optics and a chip carrier suitable for testing the first large-format device onthe telescope.

Phoenix, a high-resolution infrared spectrograph offering spectral resolutions of 67,000 to 100,000, reached the stage of fabrication and assembly inFY 1994. The spectrograph is intended for use in the 1-5 micron, near-infrared wavelength range. The detector will be an InSb array, probably a 1024 x (<1024) format array resulting from the Aladdin project. Since the spectrograph is intended for use into the thermal infrared, the instrument must be both light-tight and cryogenically cooled. Completion of the instrument is expected by early FY 1996. FY 1994 saw Phoenix progress from the early design phase, through the detailed design phase, and into the construction phase. All the optics required were either ordered or acquired in FY 1994. The grating consists of a silicon substrate with a Milton-Roy replica grating on the front surface. The silicon substrate was received, optically tested, and sent on to Milton-Roy. The finished grating was received back from Milton-Roy and the first of several tests performed. The collimator/camera assembly is an 8-inch Ritchey-Chretien telescope. The primary and secondary were received from a vendor who had diamond turned the approximate figures from silicon blanks. These have been sent to a second vendor who has been undertaking the final polishing. Two

14 order-sorting interference filters were also ordered in FY 1994. Fabrication of the collimator/camera assembly was well underway by the end of the year. This assembly consists of four 1 x 3 foot aluminum plates with a large amount of structural detail. These plates have been rough cut and heat treated. The other elements of the collimator/camera have been fabricated and assembled. These include the secondary support and focus mechanism, the grating holder and tip assembly, and the primary support and baffle. Fabrication has started on the foreoptics wheel assemblies. A number of fixed parts in the foreoptics assembly have been ordered from a commercial shop.

The Cryogenic Optical Bench (COB) was commissioned during FY 1994 and released for shared risk observing by KPNO users. COB is an IR imager/grism spectrometer equipped with a variety of analytical optics for infrared observations. A detent mechanism was added on the filter wheels to provide repeatable filter positions. The Cryogenic Optical Bench was fitted with a 256 x 256 InSb array, and the controller was upgraded to the Wildfire electronics and software.

Following this initial service, a new, higher spatial resolution camera was designed and built for COB, capable of diffraction-limited imaging at the 4-m telescope using a shift-and-add approach. Thermal emission of the atmosphere in the L' band (3.5-4.1 microns) requires high speed operation (50- millisecond integrations) to avoid saturation, and the KPNO Wildfire electronics have this capability. This is also fast enough to "freeze" the atmospheric seeing in this band, which together with the long wavelength can produce excellent image quality. In speckle terms, a point source image often has a single dominant speckle. To get the highest resolution available on Kitt Peak, the instrument, known as DLIRIM (Diffraction-Limited Infrared Imager) was used at the 4-m telescope (3.8 meters effective aperture), known from wavefront curvature analysis to have high quality surface figure. An appropriately bright point source in each image provides a peak (or brightest speckle) for shifting and adding the short exposures together digitally. The high magnification optics produce a scale of O.l'Vpixel at the detector. DLIRIM on the 4-m clearly produced diffraction limited cores on point sources in the L' band. Segments of the Airy rings could be seen in the raw single frames on bright stars, and a uniform point source core FWHM was achieved across the full 25-arcsec field with the reference source in one comer. Limited data in the K band showed more of the core-halo image structure predicted for adaptive optics systems at shorter wavelengths. Interestingly, these results were obtained in very unstable atmospheric conditions with rapidly varying low clouds plus high cirrus. Following the experiment, COB is being returned to its original configuration and returned to service at KPNO. We are evaluating whether COB should be dedicated permanently in its diffraction-limited configuration or maintained in its original state.

A second high angular resolution experiment (FTAS) was also completed at the 2.1-m in November 1993. This experiment involved a simple camera with an IR detector and dichroic to provide a visible light error signal. A commercial CCD provided the error signal to the f/15 chopping secondary to compensate for fast image motions. A considerable improvement over the time-integrated seeing was achieved, limited ultimately by the 2.1-m optical quality.

The infrared spectrometer CRSP, used at the 4-m, the 2.1-m and the 1.3-m telescopes, was upgraded with a new 256 x 256 InSb array detector. User response has been enthusiastic. The 30-micron pixels (vs. 76 for the old array) provide much improved sampling of both the slit and spatial field. This has resulted in an improved ability to remove telluric features, as well as somewhat higher spectral resolution. The dark current was reduced from 50 e/s to 2 e/s and the readnoise was reduced to 35 e for a single read, yielding a larger dynamic range and increased sensitivity on long exposures with the high resolution grating.

15 Due to the improved performance and larger spectral coverage of the 256 x 256 InSb array in CRSP, the instrument now provides complete coverage of a given spectral band with a single grating setting. To take advantage of this new capability, a new grating 4, a 200 lines/mm ruling blazed at 3 microns, was installed. This new grating is also used in the J and H bands to improve CRSP's capabilities at those wavelengths.

The Optical/UV Instrumentation Program The Optical/UV group was engaged in developing two major instruments. The first is the conversion of the Hydra multifiber positioner from use at the Cassegrain focus of the Mayall 4-m to use at the Nasmyth focus of the WIYN telescope. The change from horizontal to vertical positioning, and the stronger curve of the WIYN focal surface, dictated a completely new design for the mounting surface of the fiber buttons and the robotic stages to reposition the fibers. The mechanical design of the vacuum bending surface and the new gripper were completed and fabricated, and the reassembled Hydra fiber positioner was installed at WIYN. The Bench Spectrograph, which is fed by the Hydra fibers, was also relocated from the Mayall to the WIYN dome. A new SITe 2048 x 2048 CCD was evaluated and installed in a dewar for use on the Bench. Remaining are installation and commissioning on the WIYN, scheduled to be mostly completed by the end of calendar 1994, and completion of an all-refractive spectrograph camera,whichis expectedto improve the system throughputsignificantly.

The other major project was the continuing design of the CCD mosaic imager. The goal is to produce an imager with 8192 x 8192 format that has an activeimaging area of over 12 cm on a side. The mechanical design of the dewar and filter tray was completed for an external design review held in mid-August. The large shutter assembly was fabricated and tested. Two more lots of 2048 x 2048 CCDs were produced by Loral, but the final yield was modest, through a combination of both the fabrication and thinning processes. Initial specifications for the data handling system were defined. Designs were investigated for a prime focus corrector for the Mayall 4-m to accommodate the wide-field format and back-focal distance. Fabrication of thedewar will proceed after successful completion of Hydra. The first successful production of two-side buttable 2048 square devices will populate the mini-mosaic prototype imager, destined for direct imaging at the WIYN telescope. Further yield will be used for the mosaic imager itself; if the number of such devices is limited, the planned development of 2048 x 4096 three-side buttable devices may provide the needed detectors.

The Optical/UV Instrumentation Group fabricated parts for four new CCD dewars (including one for the Bench Spectrograph at the WIYN Telescope, and onefor the WIYN mini-mosaic detector), and the CCD development project continued with testing of new devices from SITe (formerly Tektronix), STIS, and the Loral foundry run.

In 1986 a scan-table was implemented for the Prime Focus CCD camera that allowed much "flatter" (more uniform) images to be obtained. In this mode, a scanning table on which the CCD is mounted is stepped by a few rows while the charge is shifted simultaneously by the same number of rows; the procedure is continued until the requested number of rows and total integration time have been achieved. Since agiven point inthe resulting image has actually been observed with a number ofdifferent pixels of the detector, the non-uniformities in the chip have been effectively averaged in producing the final image. The flat-fielding accuracy is therefore improved, since the data are intrinsically much flatter. In FY 1994 4-m Prime Focus CCD Camera was upgraded to work with the large Tektronix 2048 x 2048 devices and to make it considerably easier for users to both obtain and reduce their data. In addition to updating the

16 instrument hardware and software, the IRAF reduction codes were modified to check for and process scanned images.

The performance of the detectors in the 4-m Cryogenic Camera and the 2.1-m Goldcam CCD spectrograph have been improved. In CryoCam, the detector is a thinned Ford 800 x 1200 CCD with 15-micron pixels. The chip has been coated with an AR coating which peaks at 6000 A. This choice of coating has the dual effect of reducing the fringing in the far red and lowering the QE shortwards of 4000 A. The advantage in the red is dramatic. Fringing has been reduced at 9000 A from about 25% amplitude peak-to-peak on a chip with no coating or a blue-optimized coating to less than 5% amplitude peak-to-peak. This facilitates sky subtraction and accurate fluxing of faint objects. The Loral CCD installed in the 2.1-m Goldcam spectrograph was re-coated to move the peak response somewhat further to the red and reduce the fringing by about a factor of three.

A Loral IK x 3K CCD (F3KB) was deployed for use on the Coude' Spectrograph. The new detector is quite good cosmetically, and has excellent charge transfer characteristics, high quantum efficiency, and good linearity and dynamic range.

Since its inception, the Schmidt CCD system has used a sliding filter bolt containing 2-inch x 2-inch slots and a small shutter, all recycled from the original 4-m prime focus CCD system. The comers of the 2048 x 2048 CCD (S2KA), the workhorse detector at the Schmidt, were vignetted by the filter and shutter assemblies. In addition, because there were no mechanical stops (i.e. detents), filter positioning was not as repeatable as desired, which occasionally resulted in low-level flat fielding problems. To overcome these difficulties, a new 4-inch x 4-inch filter wheel and shutter have been built for the Schmidt CCD system. These are slight modifications of the filter wheel and shutter in use at the 4-m and 0.9-m telescopes.

C. National Solar Observatory

1. Image Quality Improvement Program For NSO Telescopes

Most of the important astrophysical processes observable at visible and infrared wavelengths on the Sun occur on sub-arcsecond scales. Sometimes the seeing at both NSO sites (Kitt Peak and Sac Peak) allow observations at these small scales, provided that the telescopes and their instrumentation are of sufficient quality to give the required resolution. Because of the large energy input from solar radiation into the telescopes, the latter is not an easy condition to fulfill. The NSO solar telescopes suffer from image quality deterioration due to a variety of effects including: (1) optical distortion by solar heating (e.g. the- McMath-Pierce [McM-P] mirrors and the Sac Peak Vacuum Tower Telescope [VTT] window), (2) seeing caused by the heating of the telescope mirrors (e.g. the McM-P and the Kitt Peak Vacuum Telescope [KPVT] mirrors), (3) seeing present in the large and long McM-P telescope tube, and (4) rapid image motion from a variety of effects. A number of experiments are underway to evaluate these telescope effects, with the aim of reducing or eliminating them.

An array of sensors incorporated into the Kitt Peak McM-P telescope are expected to provide a "seeing budget" for that telescope that will be consistent with the final image quality. The sensors include a seeing meter at the telescope entrance to measure the external seeing, thermal sensors on the mirrors which will estimate mirror seeing, micro-thermal sensors in the telescope tube to measure seeing in the tube, and a "Brandt" limb-motion meter in the final image to measure image shake and quality. Mirror

17 seeing is likely to be a major contributor because of the 1 to 2 degree heating of at least two of the three mirrors. Its control may therefore be essential. The measurements will tell! In addition to the McM-P telescope seeing improvement, the results will be important for the design of future infrared telescopes, which cannot use evacuated airpaths. At Sac Peak, the VTT window introduced about one wave of optical aberration. Remounting it and improving its thermal control is expected to reduce those aberrations to acceptable levels. First observations have already resulted in occasional 0.25 arcsec quality images at the VTT. Further improvements are anticipated.

To correct for any image vibration and to eliminate image motion due to atmospheric seeing, NSO is constructing a second generation correlation tracker. The first generation tracker was re-commissioned at the Sac Peak VTT this year by combining functioning components of the two oldertrackers of the NSO and theKiepenheuer Institute (Germany). Thesecond generation tracker willfollow the same fast Fourier transform techniques, but with commercial rather than custom-made hardware (see below). When ready it will be tested both on the Kitt Peak and Sac Peak telescopes. We are currently exploring the possibility of using this image position sensor with a tip-tilt mirror developed at the Kiepenheuer Institute. This tip-tilt correction system will do particularly well in the seeing regime where D/ro is < 4, which is the case (for good seeing conditions) at the Sac Peak VTT in the red and for the Kitt Peak McM-P telescope in the infrared. The NSO adaptive optics system, which is under development (described in the following section), will further improve the image quality at shorter wavelengths and under worse seeing conditions.

2. Sac Peak Instrumentation

Mark II Correlation Tracker About two years ago, the NSO copy ofthe correlation tracker, which was developed jointly during the 1980s with the Kiepenheuer Institut fur Sonnenphysik (KIS) in Freiburg, Germany, quit working because ofahardware failure. This correlation tracker was based on custom-built hardware components. Asecond copy had been built for KIS for use at the German VTT at the Canary Islands. Since KIS is currently completing a Mark II correlation tracker in conjunction with the Instituto de Astrofisica de Canarias, the Institute has lent its copy ofthe original tracker to NSO on a temporary basis. This unit is frequently used at the VTT/SP, effectively without spares or backup. This high risk situation has led to efforts here for NSO/SP to develop its own Mark II tracker.

Astudy has been performed to compare different tracking algorithms. In particular, the performance of the "absolute difference algorithm" and the "FFT cross correlation algorithm" were compared via computer simulation using data taken at the VTT/SP under different and varying seeing conditions. The simulations clearly show a performance advantage for the FFT cross correlation algorithm in conditions where the image contrast is low. The ability to track low contrast images is important to a user-friendly system. It also bears on possible use of a tracker in a Shack-Hartmann type wavefront sensor. Based on the results of the simulation studies, it was decided to design and build a Mark II correlation tracker system by implementing the FFT cross correlation algorithm. The initial design has been completed and is based purely on commercially available hardware components. Therefore the system should be easily maintainable and can be cloned for use at other NSO sites. First engineering runs are projected to occur early next year.

18 Fast CCD-Camera system, Data channel The Kiepenheuer Institut fur Sonnenphysik and NSO have signed an MOU concerning the development of a high-speed data acquisition system using a 10 frame/second IK x IK Thomson CCD camera. The system will be capable of recording up to 3 frames/second, storing the data on hard disk. The data acquisition system is camera-independent and can be configured for other cameras. Preliminary tests performed with the IK x IK Thomson camera of the RISE project demonstrated good S/N ratio. There were no fringes visible in narrow-band filtergrams recorded with the camera. Initially a fast CCD system will be implemented at Sac Peak using the RISE IK x IK camera. The camera system will be well suited for high time-resolution spectral filtergrams and good seeing frame selection and in the near future will supplement the Multiple-Diode-Array (MDA) system at the VTT/SP. Unlike the MDA system, the fast CCD system will be portable and can be reproduced for use at all NSO sites. KIS will buy the development system, which will stay at NSO/SP. A copy of the working system will be purchased and the software copied to the system for KIS. Both NSO and KIS will profit from this collaboration sharing the development cost.

Adaptive Optics The development and installation of an Adaptive Optics (AO) system continues to be one of NSO's highest priority projects. The AO program closely follows the plan outlined in the LEST (Large Earthborne Solar Telescope) proposal, but at a reduced rate due to funding limitations.

Most of the effort this year has been spent on the "Digital Reconstructor" for computing the mirror actuator positions, and on the development of the Sac Peak 61-actuator, continuous-face-plate mirror. Considerable effort was spent by R. Dunn and W. Hull on characterizing the servoed piezoelectric actuators. Tests were devised for determining linearity, drift, tilt, resonances, preload, etc., and measurements were made on all 75 actuators. Thirteen of the questionable actuators were returned to the manufacturer for evaluation and confirmation of our results. We anticipate that the actuators will have to be disassembled and reassembled before they can be used in the 61-actuator mirror.

Other technical problem areas include finding a cement that keeps the steel buttons that are cemented to the face plate from showing in the interferogram. G. Streander is completing the flattening of the face plate itself.

The twelve best actuators were set up on a 5-inch-apcrture prototype adaptive mirror with a Dyson-white- light interferometer as a wavefront sensor. S. Doinidis determined both analytically and experimentally the influence functions and the value of the weight tables similar to those that will be loaded into the "Digital Reconstructor". About three iterations are needed to bring the mirror back to flat from a several- fringe error in the wavefront.

The Lockheed AO system, which operated successfully at the VTT/SP in July 1992, will eventually come back to Sac Peak for another run. It is currently being used by S. Acton (Lockheed) in the Canary Islands for about a year.

19 3. Tucson Instrumentation

He 10830 A VideoFiltergraphlMagnetograph A new instrument for high spatial and temporal resolution imaging of solar active regions and flares in the 10830 Aline of He I is being developed for use at the NSO/Kitt Peak Vacuum Telescope (KPVT) under a Memorandum of Agreement between AURA and NASA/GSFC. The instrument will be used simultaneously with the spectromagnetograph. Nearly two decades of full-disk observations in the 10830 A line at the KPVT show a wide range of solar phenomena, such as coronal holes, filament channels associated with coronal mass ejections, long-duration flares, and analogues to X-ray bright points, which are otherwise viewed on the disk only from spacecraft. The filtergraph will provide a new view of transient phenomena in solar active regions, with temporal and spatial resolution that cannot be obtained from the spectromagnetograph, where data images are built by scanning the telescope's solar image across a long entrance slit. The new data will be particularly timely for comparisons with observations from the SOHO spacecraft (to be launched in the summer of 1995), which promise to resolve long-standing controversies on how the formation of the line depends upon external EUV radiation from the corona and low-temperature transition region.

The instrument is built around a conventional but cleverly packaged five-element Lyot filter. Ferroelectric liquid crystals modulate bandpass response and polarization at video rates. Subtracting accumulated observations in three possible pairs of filter transmission modes provides active-region imagery of 10830 A equivalent width, line-of-sight velocity, or longitudinal magnetic field, with time cadence of a few seconds. J. Harvey provided the basic concept and optical design, NASA/GSFC provided the detailed design and drawings, and the instrument was fabricated in NOAO shops using calcite birefringent crystals obtained from the GONG project. H. Jones developed the concept for the data system and coordinated the GSFC design work. Non-payroll costs were financed from peer-reviewed proposals through NASA's Solar Physics Office under terms of the Memorandum of Agreement. The filter has been tested and tuned, the optical assembly has been installed at the KPVT, and satisfactory video images have been obtained with the filter in its four-element, centrally tuned mode. All hardware for the filtergraph and its data system are on hand and the basic software for differential accumulation of images has been written and tested. In the remainder ofcalendar year 94, we expect to install the liquid crystal modulators, connect the data system, experiment with flat-fielding techniques, obtain demonstration data, andbegin development of a graphical userinterface for routine control.

South Pole '94Helioseismology Ajoint project between Bartol Research Institute, NASA and NSO/T started in 1993. The goal is to make solar oscillation observations from the geographic South Pole during the 1994-1995 austral summer. The observations will complement those from GONG and the Solar Oscillations Imager to be launched onthe SOHO spacecraft in 1995. Unlike previous observations, these will concentrate on high-frequency oscillations measured simultaneously at two heights in the solar atmosphere. Not only will information be gleaned about the solar interior, but unique data about how waves propagate in the solar atmosphere will be provided by this project. During testing of the instrument in Tucson in summer 1994, results showed that oscillation frequencies near the acoustic cutoff frequency of the atmosphere (5 mHz) are unusually sensitive to the amount of solar activity. In addition, newly erupting magnetic flux and about- to-erupt solar filaments are easily detected in the observations. The instrument was built at NSO/T using components from earlier experiments and new equipment provided by an NSF grant to Bartol. The principal investigator is S. Jefferies (Bartol). Co-investigators include T. Duvall (NASA), J. Harvey (NSO) and A. Jones (Bartol).

20 D. US Gemini Program

The US Gemini Program, formerly known as the US Gemini Project Office, serves as a liaison between the international Gemini Project Office and the US community. The Gemini Project is an international consortium formed to build two 8-meter telescopes, one on Mauna Kea, Hawaii, and one on Cerro Pach6n, Chile, in which the US maintains a 50% share. The USGP was established in 1993 as a fourth division of NOAO with a status which is on par with Kitt Peak National Observatory, Cerro Tololo Inter- American Observatory, and the National Solar Observatory. The USGP is led by the US Gemini Project Scientist, and currently includes an Associate US Gemini Project Scientist and a Technical Administrator. Efforts are underway to hire a Project Engineer.

The USGP is responsible for monitoring the technical developments within the project and for the dissemination of current information on the scientific goals, technical design, schedule, and other information to the US scientific community and industry. Both the US Gemini Project Scientist and the Associate US Gemini Project Scientist serve on the Gemini Science Committee (GSC) and represent there the views of the US scientific community. In addition to taking part in the GSC and weekly project scientist team teleconferences, they have formal input through participation in reviews and working group meetings organized by the project. During the past year, such reviews and meetings included:

IR Sky Noise Working Group Telescope CDR Secondary System CoDR Secondary Mirror PDR Acquisition and Guiding functional requirements meeting Michelle optical design review Instrument Support Structure PDR AO Functional Requirements Meeting Enclosure Design Reviews AO/A&G Science Working Group IR Instrumentation Science Working Group Optical Instrumentation Science Working Group Systems Review #1 Telescope Baffles CoDR Silver Coating Development meetings

The USGP also solicits membership for US participants in these reviews and meetings and organizes the US participation in the GSC.

In a less formal sense, the USGP personnel interact frequently and directly 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 for critical systems and components.

On the community side, the USGP provides information to and solicits opinions from the US community in a number of ways. In 1993, USGP and NOAO personnel gave approximately 20 colloquia on the Gemini Project at astronomy departments of US universities. These colloquia serve as a valuable conduit for community feedback as well. Also, the USGP prepares a display for each AAS meeting highlighting

21 the status of the Gemini Project and the activities of the USGP. Forthe upcoming meeting in Tucson, an interactive lunchtime meeting is planned. A new mechanism which has been initiated this year is an electronic mail distribution which allows the USGP to inform a broad segment of the US scientific community of issues in a timely manner. Since March, 1994, information about Gemini and USGP activities has been circulated to about 120 astronomers around the US via e-mail every three weeks on average. Articles written by USGP personnel for the NOAO and Gemini Newsletters reach a larger number of astronomers four times per year.

The advisory body to the USGP is the US Science Advisory Committee (US SAC), which meets a week or two before each GSC meeting to review issues which will be brought to the GSC. The emphasis of these discussions during the past yearhas been the instrumentation program, but the scientific drivers for operations will make up an increasing fraction of the discussions in the future. The US SAC is also polled at irregular intervals between meetings when the development of a consensus on a critical issueis required.

In the past year, a major focus within the USGP has been the instrumentation for the Gemini telescopes. Theinternational agreement states: "Because of their high degree of intellectual content, instruments will be allocated separately, in proportion of the contribution of the Partners." As a result of responses to a "Dear Colleague" letter mailed in 1993, the USGP was able to acquire the allocation of the Near-IR Spectrograph, Near-IR Arrays, IR controllers, and CCDs and Optical Detectors to the US, in addition to the Near-IR Imager which was separately allocated to the University of Hawaii. The Near-IR Spectrograph has been the first ofthese instruments for which the procurement was arranged. As a result of community opinion, and in accordance with the wishes of the NSF, a competitive selection was defined. This process is now under way, and is expected to result in the selection of a builder for this instrument by the end of 1994. Following this, procurement processes will be initiated for the other IR instruments and subsystems. After the instrument selection and contract negotiation phases are completed, the USGP will assist the Gemini Project Office in the management of the contracts for the US-built instruments.

The USGP has a special role in the procurement of the CCDs and optical detectors. The Gemini Board has requested the USGP to assemble an international consortium to procure these devices, preferably through collaborative foundry runs. The intent of this approach is to provide additional detectors to the astronomical communities of the partner countries. This activity has just begun with the formation of the international consortium and the initiation of discussions with CCD vendors to arrive at a workable arrangement to provide these arrays. The next area offocus for the USGP is operations. Because the Gemini telescopes are being designed to exploit the best delivered environmental conditions at two excellent observing sites, they cannot be effectively scheduled in the "classical" way, assigning specific nights to specific observing programs. Instead, amix ofremote observing and queue scheduled service observing will be needed to fully achieve the gains that Gemini can provide. Determining the right mix of these and other observing modes and learning how to run telescopes in this innovative way is an activity which is just now beginning.

E. NOAO Instrumentation Program

Plans were made near the end of the reporting period to dedicate the former KPNO IR and O/UV resources to an NOAO nighttime instrumentation group. A growing gap in capability of the instrumentation provided at KPNO vs. CTIO, particularly in the infrared, is one factor that prompted the

22 formation of the new group: recent funding cuts have reduced the technical group available for instrument development in La Serena below the critical mass required to produce major instruments on reasonable timescales. At the same time, NOAO expects a growing involvement in development and support of instrumentation for the Gemini telescopes. The combined group will produce major focal plane instruments and detector systems for KPNO, CTIO and Gemini. A steering committee of scientific staff from both sites will set the priorities for the program, and the NOAO Deputy Director will have overall charge. NOAO will hire an instrumentation manager for the combined group. The goal is to increase the efficiency of production of major instruments once a mature design concept has been approved. A series of reviews will be required for major projects to receive allocated manpower. Project teams that include mechanical, electrical and software technical talent will be formed to produce integrated designs, with early and thorough trade-off studies. The level of reliability, maintainability, and documentation must be high for instruments produced in one site and used at three. The new organization is intended to achieve those goals, while maintaining the current close interaction between astronomers and technical staff required for best performance and the sense of pride in accomplishment that has characterized the current IR and O/UV groups. Future reports will feature a section dedicated to the accomplishments of the NOAO instrumentation program.

V. MAJOR PROJECTS

A. Global Oscillation Network Group

The Global Oscillation Network Group (GONG) is an international, community-based project formed to conduct a detailed study of the internal structure and dynamics of the closest star by measuring resonating waves that penetrate throughout the solar interior. To overcome the limitations of current observations imposed by the day-night cycle at a single observatory, GONG is deploying a six-station network of extremely sensitive and stable solar velocity mappers located around the Earth to obtain nearly continuous observations of the "five-minute" pressure oscillations for at least three years. GONG is also establishing a distributed data reduction and analysis system to facilitate the coordinated analysis of these data. GONG data will be available to any qualified investigator whose proposal has been accepted, however active membership in a GONG Scientific Team will allow early access to the data and to the collaborative scientific analysis that the Teams have already initiated. The GONG Newsletter provides status reports on all aspects of the project and related helioseismic science.

GONG continues to make good progress towards full scientific operations. With the FY 1994 budget uncertainties resolved, production of the six field stations and spares is nearing completion, data from the prototype instrument continues to be acquired, site preparations are well underway, and data processing capability is on track for full network operations in FY 1995. Observations have now established convincingly that the solar internal structure and dynamics, as measured by the p-mode frequencies that GONG will utilize, vary significantly during the solar activity cycle, and the Project and the community are beginning to look more seriously at the technical and scientific milestones leading up to a decision on whether to pursue GONG operations beyond the baseline of three years.

A Scientific Advisory Committee consisting of P. Gilman (Nat. Center for Atmospheric Research), R. Noyes (Harvard-Smithsonian Center for Astrophys.), A. Title (Lockheed Palo Alto Research Lab.), J. Toomre (U. of Colorado, Chair), and R. Ulrich (U. of California, Los Angeles)-continues to provide overall scientific guidance to the Project, and a Data Management and Analysis Center Users Committee- consisting of T. Brown (High Altitude Obs.), D. Hathaway (NASA/MSFC, chair), J.T. Hoeksema

23 (Stanford U.), S. Korzennik (Harvard-Smithsonian Center for Astrophys.) and M. Thomson (Queen Mary and Westfield College, London), provides important community input in the development of this critical part of the Project.

The Annual GONG Meeting, organized this year by UCLA and USC, was held in Los Angeles in May with 140 participants. In addition to meetings of all of the GONG Scientific Teams, the Data Management and Analysis Center Users Committee, the site representatives, and presentations of the status of the development of the instrument and analysis systems, there were 129 scientific papers in a well-filled, week-long get together. The proceedings will be published by the Astronomical Society of the Pacific. Next year's meeting will take place at Asilomar, California.

Work is underway in preparing the sites at CalTech's Big Bear Solar Observatory in California, the High Altitude Observatory's site on Mauna Loa in Hawaii, the Learmonth Solar Observatory in Western Australia, the Udaipur Solar Observatory in India, the Observatorio del Teide on Tenerife in the Canary Islands, and the Cerro Tololo Inter-American Observatory in Chile. Grading is underway at Mauna Loa and Udaipur, permitting is concluding at Big Bear, and the foundations have been poured at Learmonth and Tenerife. Representatives from the sites participated in a separate meeting following the Annual Meeting, and we have had several-month-long scientific visitors from three of the sites participating in the development of analysis techniques in Tucson. A well attended workshop entitled "Helio- and Astroseismology" was held at the University of Sydney (Australia) in June to encourage research in helioseismology.

The Data Management and Analysis Center (DMAC) Team has continued to develop the pipeline processing and data access and distribution systems. During the past year, the DMAC reduced 66 days of data recorded by the prototype instrument to 1-v spectra and four-minute averages in support of the development of the instrument. These data included a nearly-continuous sequence from 11 June through 5July. The Data Storage and Distribution System (DSDS) has expanded its library ofarchived cartridges to over six hundred volumes. There arc currently fifty members of the GONG scientific community who have accounts on the DSDS users' machine (UM) and the number of 'ftp' and 'rlogin' accesses to the UM by non-project users has recently averaged about ten accesses per day. The GONG project now has a Mosaic/World-Wide-Web home page including links to sample images, documentation regarding GONG membership, and generalinformation about the project.

Last fall, the Data Storage and Distribution System (DSDS) embarked on a major project to upgrade its computer systems and software. This effort was completed as planned in June. The DSDS now consists of two SUN SPARClOs running SOLARIS 2.3 using ORACLE'S database management system with a new design for the file catalog. The anonymous ftp disk area and space available for network distributions of data products on the users' machine was increased significantly. The users' machine will soon be upgraded to a SPARC20. The database on the SPARClOs that supports the cartridge volume and file catalogs was converted from Ingres to ORACLE. The redesign of the file catalog provided a significant increase in performance beyond that derived from the workstation upgrade. At this point the DSDS is operational. Future software activities will be maintenance and minor enhancements primarily to support the orderly reduction of the network data. The project anticipates that during the next year, as the community increases its use of the DSDS for obtaining data products, additional enhancements and modifications may be required.

The development of the data reduction Pipeline is proceeding and the project anticipates that most components of the Pipeline should be in place early next year, early in the deployment phase. The effort

24 to develop the project's multi-site merging capability has recently focused on a modeling exercise that includes realistic atmospheric and instrumental effects. This exercise indicates that a relatively simple merging technique will be effective. Later this fall, the merge development effort will have multi- instrument, common-site data samples which will be generated from tests of the production instruments.

Instrument production activities are winding down as the field instruments are undergoing integration and testing prior to shipping. All of the major systems have been produced, and are currently being integrated at the Farm site in Tucson.

With all of the usual budgetary caveats, the deployment will begin with the Big Bear instrument being brought on-line in Tucson in the fall of 1994, and the Tenerife and Learmonth stations being shipped late in 1994, and becoming operational early in 1995. The Udaipur, Mauna Loa, and Cerro Tololo stations would be deployed during the Spring of 1995, and finally the Big Bear instrument would be relocated from Tucson to BBSO. Two primary installation teams, composed of GONG staff members, have been named to do the bulk of the actual field station setup. Each group of five people will install three stations and serve as a backup to the other group. One team will install the Tenerife, Cerro Tololo, and Udaipur stations, while the other will handle Learmonth, Mauna Loa, and Big Bear. Currently, these groups are actively engaged in the integration and testing of "their" respective stations at the Farm in Tucson. In addition, another team has been handling the preparation of the land and foundations at the various sites, while a fourth group of experts is in the wings ready to do the final certifications of the stations once they are installed in the field. All of these efforts will lead to the commencement of preliminary science-grade operations with a "mini" network of three stations, spaced at 120° longitude intervals ("Big Bear" at Tucson, Tenerife, and Learmonth), near the end of March 1995, with the interleaving longitudes filled in, and Big Bear relocated, in July 1995.

B. The Precision Solar Photometric Telescope Project (PSPT)

The PSPT program is part of the NSF RISE project, which is devoted to understanding the mechanisms of solar luminosity variations. NSO began development in FY 1994 of a small network of photometric telescopes to measure solar surface brightness variations. The instruments are designed around a 6-inch objective, a 2K x 2K CCD, and fast frame-selection electronics. Full-disk surface photometry with 0.1%/pixel accuracy with a one-hour cadence will be obtained.

Highlights from this year include: 1) demonstration of the frame selection technique using measurements of atmospheric scintillation; 2) development of the DSP hardware and software systems using a prototype IK x IK Thomson 10 Mpixs CCD; 3) identification and testing of stable ion-assisted interference filters for Ca II K line imaging; 4) design and testing of several piezo and magnetostrictive fast tilt-mirror systems; and 5) completion of system optical design and fabrication and testing of the telescope objective.

Recently informal arrangements were completed for the development of the 2K x 2K instrument camera with a company from Boulder now heavily involved in high dynamic range medical imaging. The new camera will use a deep-well Thomson 2K x 2K CCD with a 1/4-sec frame rate, yielding a read noise of less than 50 electrons. NSO will make our DSP data acquisition hardware and software available to this company in exchange for sharing the camera development costs with NSO.

25 The project is actively working to minimize development costs by seeking other scientific partners interested in the PSPT hardware. For example, the Kiepenheuer Institut fur Sonnenphysik is currently duplicating the lKx IK prototype camera for their observatory, and we expect to share the complete PSPT instrument package with the Osservatorio Astronomico di Roma. The new camera will be useful for a broad range of high-spatial, and photometric dynamic range problems, and we expect the instrument/camera development effortto decrease in cost as additional partners are identified.

C. SWATH Mission

The Space Weather and Terrestrial Hazards (SWATH) satellite mission is a small, lightweight and inexpensive payload comprising a set of instmments for measurements concerned with the overall problem of space hazards affecting satellites in low-Earth orbit. The instrumentation includes a high resolution solar X-ray/optical imager, a full-disk XUV imager, and a white-light coronagraph. Mission goals include early detection of solar flares and coronal mass ejections, development of solar forecasting techniques, and detection and analysis of space debris in the sub-cm size range. The Smithsonian Astrophysical Observatory (SAO) has the primary contract for this mission (L. Golub, PI). NSO/SP (R. Smartt, PI)has a sub-contract to design, construct and test the small coronagraph. However, SWATH has been officially on hold for approximately twelve months, starting soon after the Preliminary Design Review ofSeptember, 1993. Nevertheless, funding for the coronagraph has allowed the development ofa detailed design as well as the construction of some basic components. Further engineering, concerned primarily with analysis and measurements of the stray-light characteristics of the design, has also been carried out. A contract has beenlet for the advanced CCD Detection System.

D. WIYN

During 1994, the WIYN Consortium, Inc., completed construction of the new 3.5-m WIYN telescope on Kitt Peak. The WIYN Consortium is comprised of the University of Wisconsin, Indiana University, and Yale University together with the National Optical Astronomy Observatories. The WIYN telescope makes use of a 3.5-m, spin-cast lightweight mirror produced at the Steward Observatory Mirror Lab. Commissioning of the telescope began in July 1994, and the operations phase is expected to begin in March 1995. Observing time will be split in accordance with the contributions of each member of the Consortium toward both construction and operations: Wisconsin 26%, Indiana 17%, Yale 17%, and NOAO 40%.

The telescope achieved "first light" during the summer of 1994 after the major subsystems, including the optics, primary mirror supports, thermal control system, control system, and commissioning instrumentation, were installed on the telescope. The quality of the images produced by the WIYN telescope has been extraordinary, and the WIYN telescope is now routinely producing the best images on Kitt Peak. Images are commonly 0.6-0.7 arcsec at telescope elevations greater than 20 degrees for short (10-20 s) exposure times in R-band images using the current "open loop" optical system look-up tables.

Optics Early in FY 1994 the 3.5-m Primary Mirror Group prepared the mirror cell and support systems for mating ofthe mirror to the cell in preparation for testing. All parts of the new axial support mechanisms were delivered and the units assembled. The 66 axial units and the modified 24 lateral supports were mounted to the cell and connected with stainless steel tubing to form the hydraulically connected lateral support system and the 3 axial support zones. In addition, the primary mirror control electronics were

26 updated and additional diagnostic software written. New LVDT units which sense the mirror position in the cell were fabricated and mounted near the outer edge of the mirror to provide better access and greater sensitivity.

The 3.5-m Mirror Group completed the laboratory assembly of the active mirror support system, and then connected the mirror to the supports and installed the whole assembly under the optical tower for testing. Interferometric tests using the same null lens used for polishing demonstrated that the redesigned active axial supports perform extremely well when pointed towards the zenith, the only orientation that can be tested. The rms figure ofthe finished, supported mirror is 0.04 waves (at 6328 A), producing images with a mere 0.033 arcsec FWHM, about a factor of 4 better than specified for the mirror operating in the telescope under varying thermal conditions and elevation angles. The support system and mirror cell were shipped to Kitt Peak in early February of 1994. The mirror was aluminized in the 4-m vacuum chamber, and the cell was "fit" to the telescope structure before the primary mirror was installed.

The primary mirror cell was installed in the telescope in March, mechanically aligned to center the optical axis of the mirror in the Optic Support Structure, and squared to the elevation axis. The NOAO WIYN mirror group tested the active supports for various elevations and reported that the on-telescope hardware is working correctly.

Contraves polished the 1.2-m secondary mirror for WIYN. The mirror was tested interferometrically over its full aperture using NOAO's 100-inch test sphere and a null lens. The surface figure of the mirror is 0.030 waves RMS and meets WIYN's secondary mirror image error budget of 0.05 arcsec. The secondary mirror cell was fabricated at NOAO. Kodak completed the tertiary mirror to WIYN's specifications. The secondary and tertiary mirrors were assembled in their cells and tested in the laboratory. Both mirrors were aluminized at the mountain solar telescope coating facility. The tertiary mirror assembly which allows the mirror to rotate to three focal stations and also to flip out of the beam was mounted on the primary mirror cell and installed in the telescope.

Once the secondary and tertiary mirrors were installed and mechanically aligned, a cooled science grade STIS CCD was mounted at one WIYN Nasmyth port and optical collimation was completed. With the assistance of Claude Roddier (Hawaii), wave front curvature (WFC) mapping was then initiated to tune the primary mirror support actuators. A more extensive WFC mapping effort lead by N. Roddier (NOAO) ultimately lead to the construction of "open loop" lookup tables to control the primary mirror shape, secondary tilt, and system focus as a function of elevation. These initial look-up tables appear to be encouragingly stable and repeatable, reflecting the stability of the WIYN active optics system. This stability will be tested regularly over the next year, and the tables will be updated as necessary.

Based on the analysis of WFC data, it was apparent that the primary and secondary were well-matched, e.g. the total system spherical aberration could be set to zero by spacing the two mirrors properly. To assess the secondary mirror high frequency quality, high resolution, high signal-to-noise out of focus stellar images were acquired with the secondary at its nominal position and then with the secondary rotated 90 degree in its cell. The before and after images were essentially identical, indicating that any residual high frequency optical features are associated with the primary. These features are quite small and should have no impact on the ultimate optical performance of the WIYN. When compared to other telescopes tested in a similar manner by the Roddiers, the WIYN optical system appears to be at least as good if not better than any other 4-m class telescope in the world.

27 Concurrent with this optical work, the installation of the primary mirror active thermal control system was completed. The thermal system has been active during all subsequent nighttime operations. It is quite common to maintain the primary mirror temperature within ± 0.2 degree C of the ambient temperature all night long, starting shortly after sunset.

Two 0.5-m diameter fused silica blanks for the 1 degree wide field corrector were obtained and ground at Rayleigh Optical in Tucson; the corrector cell was fabricated outside as well. The lenses are being-anti- reflection coated and assembled into their cell for installation in the telescope.

Enclosure Thermal testing of the enclosure was accomplished using the KPNO 10-micron infrared camera and thermocouple probes throughout the structure. In nighttime tests with the dome vents opened up, the air temperature within the telescope chamber tracked the outside temperature to 0.13°C RMS. Surface temperatures within the chamber generally tracked the air except for those surfaces exposed to the night sky which cooled below the air temperature. Reflective coatings will be used to control surfaces where this is a problem. No major sources of heat were apparent in the telescope chamber even while the telescope and dome drives were operating.

Control System Installation of the WIYN Control System, designed and fabricated at the University of Wisconsin began late in 1993 and continued throughout FY 1994. NOAO undertook to write a graphical user interface for the control system as part of the control system hand-off from the UW Controls Group. NOAO involvement assures that the WIYN GUI is reasonably consistent with those at other NOAO telescopes, and that operators and observers will find WIYN operations to be familiar.

General Operations The WIYN Site Manager, an employee of the University of Wisconsin, was hired at the beginning of the fiscal year, and assumed responsibility for site operations for WIYN on Kitt Peak. Preparations for facility instrumentation installation and commissioning are nearing completion. Delivery of major instrument components has begun, and instrument commissioning activities should ramp up to full effort by mid-October.

The detailed design of the Instrument Adapter ("guider box") is nearing completion and fabrication is underway. Longlead timeitems such as the guidecameras and integrating CCD for the wavefront sensor havebeenordered and somepartsof the guiderbox are currently beingfabricated.

E. Partnerships in Progress at CTIO

1. 2MASS Survey

Work on this project, an all-sky near-infrared survey, is expected to pick up speed during FY 1995. The observations will be carried out by two 1.3-m dedicated telescopes, one on Mt. Hopkins in Arizona, and one on Cerro Tololo. Rae Stiening has been appointed as Project Manager at the University of Massachusetts, and discussions are underway to work out details of telescope siting, construction, and operations. Preliminary investigations by CTIO staffleadus toprefer a location just below the summit of the mountain on the northwest side. Airflow should be favorable under prevailing conditions and a moderate-sized dome can be constructed there without interfering with existing or planned telescopes. The nominal location is roughly 60 m west-northwest of the GONG site. The bulk of the dome

28 constmction should take place starting in 1996, with survey operations beginning in early 1998 and terminating in 1999.

2. Sao Paulo Telescope

IAGE astronomers continue to show interest in locating a 1.8-m, actively supported, metal-mirror telescope at CTIO. CTIO has forwarded a preliminary set of cost estimates for provision of basic services for this telescope and Malcolm Smith has visited Sao Paulo to discuss this and other possible Brazilian initiatives at Cerro Tololo/Cerro Pach6n.

3. Southern Spectroscopic Survey Telescope

Very preliminary discussions have been held with astronomers from the University of Texas about the possibility of locating a southern version of the SST at CTIO.

4. SOAR

Columbia University has withdrawn from this project to build a 4-m class telescope with excellent imaging on Cerro Pach6n. Brazil has expressed interest in joining the consortium with the University of North Carolina and CTIO/NOAO. The University of North Carolina is continuing its fund-raising efforts. Until fund-raising efforts have stabilized, we will not present further milestone tables.

VI. CENTRAL COMPUTER SERVICES

Central Computer Services consists of three groups: The Mountain Programming Group, which handles programming tasks for KPNO and NSO/Tucson, the IRAF (Image Reduction and Analysis Facility) group, and the Tucson computing support group.

A major project for the Mountain Programming Group for the past year was the ongoing renovation of the 4-m telescope, including a set of graphical user interfaces for the various components of the telescope. The 4-m began regular operation, on schedule, in October 1993. Work continued, at a lower level, for the rest of the year.

The MPG contributed heavily to the ongoing effort to commission the WIYN telescope: constmction of the GUI used to operate the telescope, understanding the control system, building software for the Hydra MOS and the H/ARCON CCD controllers and so on.

MPG staff members worked on the design of the Gemini Observatory Control System and participated in the Preliminary Design Review. We expect that much of this software will find its way into NOAO telescopes.

As it was last year, the major systems software effort for the IRAF group during the year was the development of a general graphics user interface (GUI) capability for IRAF applications. The new facilities are programmable at a high level, making it much easier to develop custom GUIs for applications than has been the case in the past. The GUI toolkit includes not only all the standard window system toolkit facilities, but also modules specifically designed for science applications. Chief among

29 these is a graphics and imaging module which provides a sophisticated graphics and image display capabihty for the visualization and display of 2D astronomical data. Early versions of the XIMTOOL image display server and the XGTERM color graphics terminal emulator were released. The new GUI system level facilities are also being used to develop the first IRAF science applications with integrated GUIs.

An intemal prerelease of IRAF version 2.10.3 was made during the year anticipating a Beta release of 2.10.3 (for SunOS 4.1.x and Solaris 2.x) made in August 1994. This release included the XI1 support utilities described above. A full release to the community for all supported platforms (including DEC Alphas running OSF/1) called 2.11 should be released by the end of calendar year 1994. The V2.ll release will include support for the XI1 support package, a FITS image kernel (developed in collaboration with STScI), a new version of the DAOPHOT crowded-field photometry package incorporating the DAOPHOT-II algorithms, andfurther enhancements to the spectroscopic packages.

The IRAF Mail Network began during the year; it consists of many interrelated network services, including classic services such as the FTP archive, the IRAF Hotline and IRAF sitemail plus a number of new services such as network news, a World Wide Web server, a Mosaic interface and a scheme for remotely executing IRAF over the network.

The IRAF group continues to support the ICE IRAF-based data acquisition software currently in use on Kitt Peak. The Kitt Peak "Save the Bits" project, an automated data archiving facility for Kitt Peak data, reached maturity during the year with the collection of approximately 0.36 Terabytes during the first 11 months of operation. The IRAF group is also working with NSO to archive FTS and vacuum magnetograph data.

Members of IRAF and the Mountain Programming Group attended the third annual conference on Astronomical Data Analysis Software and Systems, held in Victoria in October 1993. NOAO is a co-sponsor of this Conference series, which originated in Tucson in 1991 under the sponsorship of NOAO and the IRAF project.

The downtown Tucson computing facilities continued to evolve as older systems were replaced by newer, more cost-effective and easier-to-maintain systems. In particular, a replacement Sun for the system Gemini (which acts as a server for the Scientist Workstation Network) was purchased during the year. Also, several older disk drives on various CCS systems failed during the year and were replaced by more reliable, and also larger, disks. The network infrastructure in the downtown Tucson office building was upgraded with the addition of several special purpose networks.

VII. SCIENTIFIC STAFF

A. CTIO Scientific Staff Changes

Malcolm Smith, formerly Director of the Joint Astronomy Centre in Hawaii, commenced as Director of CTIO in November 1993.

During February 1994, Gerard Williger completed his post-doctoral term at CTIO and left for Heidelberg where he took up a post-doctoral position.

30 Andrew Cooke, a post-doc from Cambridge University, UK arrived at CTIO in January and has been working with Jack Baldwin on quasar spectra.

B. KPNO Scientific Staff Changes

Stephane Courteau , Research Associate, joined KPNO on 19 September 1993.

Alain Porter, Associate in Research at KPNO, passed away on 10 October 1993.

Heather Morrison, formerly a Hubble Fellow and KPNO Research Associate, left Tucson on 8 August 1994 to join the faculty of the Case Western Reserve University.

Michael Wise, formerly a Research Associate, left KPNO on 9 September 1994 to join the AXAF Science Center of the Smithsonian Center for Astrophysics.

C. NSO Scientific Staff Changes

Jacques Beckers took over the directorship of NSO on 1 October 1993.

John Leibachcr changed status from Director of the National Solar Observatory to GONG Project Director/Astronomer/Tenure on 1 October 1993.

Raymond Smartt changed status from Deputy Director of NSO/Sac Peak to Astronomer/Tenure on 1 October 1993.

William Livingston, Astronomer/Tenure at NSO/Tucson, retired on 30 September 1993 and assumed the position of Astronomer Emeritus.

Robert Howard changed status to a half-time Astronomer at NSO/Tucson on 1 October 1993.

James Brault, Physicist/Tenure at NSO/Tucson, retired on 31 January 1994.

Vladimir Airapctian, Research Associate at NSO/Sac Peak, arrived on 1 April 1994, funded by the Los Alamos Scientific Laboratory.

Kurt Bachman, Junior Scientist, joined NSO/T on 6 July 1993 funded through SOI.

John Beck, Research Assistant, joined NSO/Tucson on 8 July 1993 funded through SOI.

Doug Braun, Research Associate at NSO/Tucson, joined the NSO extended staff through the Solar Physics Research Corporation in December 1993.

Sydney D'Silva, Research Associate, began work at NSO/Tucson on 30 November 1993.

Yuhong Fan joined the NSO/Tucson staff on 1 December 1993 as a Research Associate funded through the Office of Naval Research.

31 Yeming Gu, Research Associate at NSO/Tucson, joined the NSO extended scientific staff through the Solar Physics Research Corporation on 1 December 1993.

Andrew Jones began work as a Research Associate at NSO/Tucson on 12 January 1994, funded by the University ofDelaware.

Christoph Keller arrived at NSO/Tucson on 3 January 1994 under a post-doc position funded through the Swiss Science Foundation.

Gregg Kopp's Research Associate appointment at NSO/Tucson endedon 17 September 1993.

Donald Neff resigned from his position at NSO/Tucson as an Assistant Engineering Physicist on 1 July 1993.

Jesus Patron began work as a Research Assistant at NSO/Tucson on 1 October 1993. His appointment ended on 30 April 1994. Jesus, a graduate student partially supported by the NSO grant with NASA for SOI, completed his thesis work at NSO and was awarded a Ph.D. by the University de La Laguna, Tenerife, Spain, in September 1994.

Thomas Rimmele, Research Associate at NSO/SP, arrived in May 1993, funded by the New Jersey Institute of Technology.

VIII. DIRECTOR'S OFFICE

The current management structure for NOAO consists of the following employees: Sidney Wolff, NOAO Director; Richard Green, Acting NOAO Director; Malcolm Smith, CTIO Director/NOAO Associate Director; Mark Phillips, CTIO Assistant Director; Caty Pilachowski, KPNO Acting Director; Bruce Bohannan, KPNO Assistant Director; Robert Barnes, Assistant to the KPNO Director; Jacques Beckers, NSO Director/NOAO Associate Director; Todd Boroson, USGP Scientist/ NOAO Associate Director; Glen Blevins, Controller/Manager, Central Administrative Services; Larry Daggert, Manager, Engineering and Technical Services; John Dunlop, Manager, Central Facilities Operations; Yvette Estok, Public Information Officer; Steve Grandi, Manager, Central Computer Services; Karie Meyers, Publications Editor.

The NOAO Director is responsible for the overall operation of NOAO, which includes providing scientific leadership for NOAO, determining priorities, budget planning, and allocation resources. The Director represents NOAO, and in particular, the four scientific divisions (CTIO, KPNO, NSO, and USGP) to the Association of Universities for Research in Astronomy, the National Science Foundation, and to the scientific community.

32 IX. NOAO STATISTICS NOAO statistics are reported for the period 1 July 1993 - 30 June 1994.

A. CTIO Statistics

During the period of 1 July 1994 through 30 June 1994, a total of 235 separate observing programs involving 444 scientists (238 visitors, 206 collaborators) were carried out at CTIO. Astronomers using CTIO facilities during this period represented 51 US institutions and 26 foreign institutions, including 8 Latin American institutions.

In the same period, 199 papers were published based on the use of Cerro Tololo facilities. The number of nights CTIO scientific staff spent on CTIO during this period was 334. The number of public visitors to CTIO during this same period is estimated to be 7,000.

Breakdown ofCTIO Observational Statistics

(1) The figures in the following table reflect the number of observers/users physically present at the Observatory and do not include multiple visits by a single observer/user. This table does not include NOAO staff. The total number of visits including multiple ones is 361. Visiting astronomers were assigned 90% of the observing time and the remaining 10% was assigned to the staff.

(2) Observers/Users US Latin A. Foreign Total Ph.D.s 121 20 34 175 Graduate Students 49 1 5 55

Technicians & Research Students 8 - 8

Total visitors 170 29 39 238

(3) Collaborators who were not physically present 139 19 48 206

(4) Institutions represented by the above visits 51 77

B. KPNO Statistics

During the period 1 July 1993 through 30 June 1994, a total of 288 observing programs were carried out on NOAO telescopes on Kitt Peak. Associated with these programs were 522 individual scientists, and 53 programs were identified as graduate theses. These programs brought 518 scientific visitors to Kitt Peak, including 376 Ph.D. astronomers, 121 graduate students, and 21 others, with an additional 140 visits by KPNO scientific staff. A total of 70 visiting scientists used the KPNO measuring engines as follows: 61 - Grant Comparator (2-axis), 9 - PDS microdensitometer.

33 Astronomers using Kitt Peak telescopes in this period represented 86 US institutions and 36 foreign institutions. The top five represented are: 1) Space Telescope Science Institute (26); 2) University of California, Berkeley (16); 3) Harvard Smithsonian Center for Astrophysics (15); 4) University of Arizona (15); and 5) University of Massachusetts (12). Thenumber of public visitors to Kitt Peak in this period is estimated to be 100,000.

C. NSO Statistics

The National Solar Observatory had 268 visits from US visiting astronomers, 51 visits from foreign astronomers, and 150 visits from staff.

During the period 24 October 1993 to 20 September 1994, a total of 423 outside users from 204 institutions accessed the main NSO/Tucson data archive and distribution area a total of 2045 times. A total of 14,719 data files were transferred during these accesses. In addition, 23 distributions per observing day are made automatically to outside users, adding approximately 5500 distributions per year for a total of over 20,000 data distributions annually to about 450 users. Note that these statistics are for NSO/Tucson only, and do not include Mosaic/WWW NSO accesses.

D. NOAO Central Computer Services Statistics

During the period 1 July 93 through 30 June 94, a total of 190visiting scientists used the NOAO Tucson computing facilities: 140 US visits and 50 foreign visits.

E. NOAO Tucson Headquarters Building Statistics

A total of 2,009 visitors signed in at the NOAO Tucson headquarters building for the period 1 July 1993 through 30 June 1994.

34 APPENDIX A

National Optical Astronomy Observatories July 1993 to June 1994 Technical Reports

The following papers were published by CCS personnel:

Lytle, D., PASP Conf. Series 61, ed. D.R. Crabtree, R.J. Hanisch, J. Barnes, "An IRAF Solar Data Pipeline into the World Wide Web"

Valdes, F, PASP Conf. Series 61, ed. D.R. Crabtree, R.J. Hanisch, J. Barnes, "Psfmeasure/Starfocus: IRAF PSF Measuring Tasks"

Valdes, F., PASP Conf. Series 61, ed. D.R. Crabtree, R.J. Hanisch, J. Barnes, "Psfmeasure/Starfocus: PSF Measuring Algorithms"

Davis, L.E., PASP Conf. Series 61, ed. D.R. Crabtree, R.J. Hanisch, J. Barnes, "A GUI for an IRAF Aperture Photometry Task"

Fitzpatrick, M., PASP Conf. Series 61, ed. D.R. Crabtree, R.J. Hanisch, J. Barnes, "A GUI for the IRAF Radial Velocity Task FXCOR"

Seaman, R., PASP Conf. Series 61, ed. D.R. Crabtree, R.J. Hanisch, J. Barnes, "NOAO/IRAF's Save the Bits, a Pragmatic Data Archive"

The following papers were published by ETS personnel:

Forbes, F.F., Proc. of ICO-16 Satellite Conference on Active and Adaptive Optics, Garching, Germany, "Large Telescope Alignment using Wavefront Curvature Sensing"

Fowler, A.M., Gatley, I., et al., Proc. of a Conference on Infrared Astronomy with Arrays: The Next Generation, UCLA, "Performance of the Current 256 x 256 SBRC InSb Array and Status of the Next Generation 1024 x 1024 InSb Array"

Fowler, A.M., Gatley, I., et al., SPIE, 2198, "Next Generation in InSb Arrays: Aladdin*, the 1024 x 1024 InSb Focal Plane Array Development Project Status Report"

Fowler, A.M., Bass, D., Heynssens, J., Gatley, I., et al., SPIE, 2268, "Next Generation in InSb Arrays: ALADDIN,* The 1024 x 1024 InSb Focal Plane Array Readout Evaluation Results"

Harmer, C.F.W., Book Review of "Optics in Astronomy," edited by J.V. Wall, Cambridge University Press"

Heim, G.B., Buchholz, N.C., Luce, R.W., SPIE, 2198, "NOAO Wildfire Instrument Controller"

Heynssens, J., Fowler, A.M., Gillett, F.C., Final Report on Contract No. A16850D, "Valley Oaks/Cincinnati Electronics 256 x 256 InSb Array Evaluation"

Hinkle, K.H., Drake, R., Ellis, T, SPIE, 2198, "Cryogenic Single-Crystal Silicon Optics" Poczulp, G., Richardson, J., Wong, W., et al., SPIE, "Fabrication and testing of the 3.5 m, f/1.75 WIYN primary mirror"

Vaughnn, D., SPIE, 2198, "What's Wrong with the Throughput-Resolution Product?" APPENDIX B

Cerro Tololo Inter-American Observatory July 1993 to June 1994 Publications List

Abt, H.A., Morell, N.I. 1993, ASP Conf. 44, ed. M.M. Dworetsky, F. Castelli, R. Faraggiana (ASP), p. 384, "Rotational Velocities for the Brighter A-Type Stars"

Alonso, M.V., et al. 1993, AJ, 106, p. 676, "CCD Calibration of the Magnitude Scale for the Southern Sky Redshift Survey Extension Galaxy Sample"

Angione, R., et al. 1994, ASP Conf. 55, ed. D.M. Pyper, R.J. Angione (ASP), p. 255, "Ground-Based Wide-Field Direct CCD Imaging in Support of the Astro-UIT Space Shuttle Mission"

Anthony-Twarog, B.J., Twarog, B.A. 1994, AJ, 107, p. 1577, "Reddening Estimation for Halo Red Giants Using uvby Photometry"

Anthony-Twarog, B.J., Twarog, B.A., Sheeran, M. 1994, PASP, 106, p. 486, "vbyHfi CCD Photometry of Melotte 66: A Disk Analog of Omega Centauri?"

Antokhin, I., et al. 1994, AJ, 107, p. 2179, "A Unique Period for the WN5 Star EZ CMa"

Bagnuolo, W.G., Gies, D.R., Penny, L. 1994, ASP Conf. 56, ed. A.W. Shatter (ASP), p. 417, "Separation of Composite Spectra of O-Binaries: Physical Properties of Iota Orionis and 29 Canis Majoris"

Bagnuolo, Jr., W.G., et al. 1994, ApJ, 423, p. 446, "Tomographic Separation of Composite Spectra. II. The Components of 29 UW Canis Majoris"

Bailyn, CD. 1993, ApJ, 411, L83, "The Optical Counterpart of the Bright Nearby Millisecond Pulsar PSR J0437 - 4715"

Bailyn, CD., et al. 1993, ASP Conf. 50, ed. S. Djorgovski, G. Meylan (ASP), p. 227, "Ground-Based Photometry of Nearby Cluster Cores"

Bailyn, CD. 1994, AJ, 107, p. 1073, "Gradients in Giant Branch Morphology in the Core of 47 Tucanae"

Balachandran, S., et al. 1993, ApJ, 413, p. 368, "Lithium in the Binary Halo Star HD 89499"

Barstow, M.A., et al. 1994, MNRAS, 267, p. 647, "A New Hot DA White Dwarf in a Region of Exceptionally Low Hi Density"

Bergbusch, P.A. 1993, AJ, 106, p. 1024, "Luminosity Functions for Post-Tumoff Stars in Globular Clusters. I. NGC 288"

Bergbusch, P.A. 1993, ASP Conf. 48, ed. G.H. Smith, J.P. Brodie (ASP), p. 180, "Luminosity Functions of Post-Tumoff Stars in NGC 288 and NGC 7099" Bergeron, P., et al. 1994, ApJ, 423, p. 456, "The Peculiar Cool White Dwarf LHS 1126 Revisited"

Blum, R.D., et al. 1994, ApJ,422, p. Ill, "Radial Velocities of M Giants at 300 Parsec Projected Radius from the Galactic Center"

Bolte, M. 1993, ASP Conf. 48, ed. G.H. Smith, J.P. Brodie (ASP), p. 60, "Do Age Differences Exist Between Galactic Globular Clusters?"

Bolte, M. 1993, ASP Conf. 49, ed. S.R. Majewski (ASP), p. 173, "Measuring Relative Ages of Galactic Globular Clusters"

Bouchet, F.R., et al. 1993, ApJ,417, p. 36, "Moments of the Counts Distribution in the 1.2 Jansky IRAS Galaxy Redshift Survey"

Bouvier, J., et al. 1993, A&AS, 101, p. 485, "COYOTES I. Multisite UBVRI Photometry of 24 Pre-Main- Sequence Stars of the Taurus-Auriga Cloud"

Briley, M.M., et al. 1993, AJ, 106, p. 142, "CN and CH Variations in the Globular Custer M55 i

Brown, J.A., Wallerstein, G. 1993, AJ, 106, p. 133, "High Resolution CCD Spectra of Stars in Globular Clusters. VIII. The Self-Enrichment History of Omega Centauri"

Brown, J.A., Wallerstein, G. 1993, ASP Conf. 48, ed G.H. Smith, J.P. Brodie (ASP), p. 188, "CNO and Metals in Stars in Omega Centauri"

Buckley, D.A.H., et al. 1993, MNRAS, 265, p. 926, "1H0551-819: Discovery of a New Cataclysmic Variable from the HEAO-1 Survey"

Buta, R., Crocker, D.A. 1993, AJ, 106, p. 939, "The Strange "Barred" Spiral Galaxy ESO 235-58: A Case of Morphological Deception"

Chambliss, C.R., et al. 1993, AJ, 106, p. 2058, "A Photometric Investigation ofthe Eclipsing Binary V505 Sagittarii"

Chu, Y.-H., Kennicutt, Jr., R.C. 1994, ApJ, 425, p. 720, "Kinematic Structure of the 30 Doradus Giant H n Region"

Claria\ J.J., et al. 1994, MNRAS, 268, p. 733, "An Abundance Calibration for DDO Photometry of Population II G and K Giants"

Clarid, J.J., Piatti, A.E., Lapasset, E. 1994, PASP, 106, p. 436, "A Revised Effective-Temperature Calibration for the DDO Photometric System"

Clowes, R.G., Campusano, L.E. 1994, MNRAS, 266, p. 317, "Observations of Quasars in ESO/SERC Field 927"

C6te\ P., et al. 1994, ApJS, 90, p. 83, "A Search for Binaries in the Globular Cluster NGC 3201" Cowley, A.P., et al. 1993, ApJ, 418, L63, "Detection, Identification, and Observed Properties of Large Magellanic Coud Supersoft X-Ray Sources"

Da Costa, G.S. 1993, ASP Conf. 48, ed. G.H. Smith, J.P. Brodie (ASP), p. 363, "The Star Ousters of the Magellanic Couds with Age > 1 Gyr"

Da Costa, G.S., et al. 1993, ASP Conf. 50, ed. S.G. Djorgovski, G. Meylan (ASP), p. 81, "The Dynamics of NGC 3201"

Da Costa, L.N., et al. 1994, ApJ, 424, LI, "A Complete Southern Sky Redshift Survey"

Davidson, K., et al. 1993, ApJ, 411, p. 336, "He 3-519: A Peculiar Post-LBV, Pre-WN Star?"

Davis, L.E., Gigoux, P. 1993, ASP Conf. 52, ed. R.J. Hanisch, R.J.V. Brissenden, J. Barnes (ASP), p. 479, "PHOTCAL: The IRAF Photometric Calibration Package"

DeGioia-Eastwood, K., Meyers, R.P., Jones, D.P. 1993, AJ, 106, p. 1005, "Luminosity Functions and Color-Magnitude Diagrams for Three OB Associations in the Large Magellanic Cloud"

Dekel, A., et al. 1993, ApJ, 412, p. 1, "IRAS Galaxies Versus Potent Mass: Density Fields, Biasing, and n-

Diaz, M.P., Steiner, J.E. 1994, ApJ, 425, p. 252, "On the Magnetic Nature of GQ Muscae"

Dickel, J.R., et al. 1994, AJ, 107, p. 1067, "Structure and Extinction of 30 Doradus and the Nearby SNR N157B as Measured by a Comparison of Radio and Optical Images"

Djorgovski, S. 1993, ASP Conf. 50, ed. S.G. Djorgovski, G. Meylan (ASP), p. 373, "Physical Parameters of Galactic Globular Clusters"

Djorgovski, S., Piotto, G. 1993, ASP Conf. 50, ed. S.G. Djorgovski, G. Meylan (ASP), p. 203, "Color and Population Gradients in Globular Ousters"

Drissen, L., et al. 1994, AJ, 107, p. 2172, "A Survey for Highly Variable Objects on the SRC-J Plates. I. Faint New Cataclysmic Variables in the Galactic Halo"

Eggcn, O.J. 1993, AJ, 106, p. 80, "Evolved GK Stars Near the Sun. I. The Old Disk Population"

Eggen, O.J. 1993, AJ, 106, p. 642, "Degenerate Stars in the Hyades Supercluster"

Eggen, O.J. 1994, AJ, 106, p. 1885, "The Low Mass Hyads and the Evaporation of Qusters"

Eggen, O.J. 1994, AJ, 107, p. 594, "Evolved GK Stars Near the Sun. II. The Young Disk Population"

Eggen, O.J. 1994, AJ, 107, p. 1834, "The Very Short Period Cepheid (RR Lyr) Variables. II. Light and Color Curves of Variables in the Solar Vicinity" Eggen, O.J. 1994, AJ, 107, p. 2131, "Post-Main-Sequence and Post Red Giant Branch Variables with Pulsation Periods Less than One Day"

Eggen, O.J. 1994, AJ, 107, p. 2184, "Photometry of F-K Type Bright Giants and Supergiants. III. The Luminosity, Reddening, and Heavy Element Abundance of GK Stars"

Elias, J.H., et al. 1993, ASP Conf. 43, ed. B.T. Soifer (ASP), p. Ill, "Cosmic Evolution of a Sample of Infrared-Luminous Galaxies"

Elston, R., Thompson, K.L., Hill, G.J. 1994, Nature, 367, p. 250, "Detection of Strong Iron Emission from Quasars at Redshift z > 3"

Elston, R., et al. 1994, AJ, 107, p. 910, "The Seyfert II Nature of the IRAS Source FSC 10214+4724"

Eracleous, M., Halpern, J.P. 1993, ApJS, 90, p. 1, "Double-Peaked Emission Lines in Active Galactic Nuclei"

Ferland, G.J. 1993, ApJS, 88, p. 49, "A Masing [Fe XI] Line"

Fisher, K.B., et al. 1994, MNRAS, 266, p. 50, "Qustering in the 1.2-Jy IRAS Galaxy Redshift Survey - I. The Redshift and Real Space Correlation Functions"

Fisher, K.B., et al. 1994, MNRAS, 267, p. 927, "Custering in the 1.2-Jy IRAS Galaxy Redshift Survey - II. Redshift Distortions and ^(rp, ji)"

Forbes, D.A., et al. 1994, AJ, 107, p. 984, "A Nuclear Starburst Ring in the Spiral Galaxy NGC 7552"

Forbes, D.A., et al. 1994, AJ, 107, p. 1713, "A Search for Secondary Nuclei in Shell Galaxies"

Fried, J.W., Illingworth, G.D. 1994, AJ, 107, p. 992, "Kinematics of 12 EUiptical Galaxies"

Frogel, J.A. 1993, ASP Conf. 48, ed. G.H. Smith, J.P. Brodie (ASP), p. 519, "Connections Between Globular Clusters, Halo Stars, and Galaxies as Observed in the Infrared"

Garay, G., et al. 1993, A&A, 274, p. 743, "Molecular Clouds in the 30 Doradus Halo"

Garcfa, B. 1993, ApJS, 87, p. 197, "A Study of Carina OB2 Association. I. Observational Data"

Garilli, B., Maccagni, D., Tarenghi, M. 1993, A&AS, 100, p. 33, "Galaxy Velocities in Eight Southern Clusters"

Gamett, D.R., Chu, Y.-H., Dopita, M.A. 1993, Rev. Mex. Astron. Astrofis., 27, p. 141, "A New Wolf- Rayet Ejecta Shell in the LMC"

Gamett, D.R., Chu, Y.-H. 1994, PASP, 106, p. 626, "A New Ejecta Shell Surrounding a Wolf-Rayet Star in the LMC" Gebhardt, K., et al. 1993, ASP Conf. 50, ed. S.G. Djorgovski, G. Meylan (ASP), p. 77, "The Inner Velocity Structure of M15 Measured with a Fabry-Pcrot"

Gebhardt, K., et al. 1994, AJ, 107, p. 2067, "Fabry-Perot Measurements of the Dynamics of Globular Cluster Cores: M15 (NGC 7078)"

Geisler, D., et al. 1993, ASP Conf. 48, ed. G.H. Smith, J.P. Brodie (ASP), p. 561, "The Metallicity Distribution Functions for Globular Clusters in NGC 1399 and NGC 5128"

Gies, D.R., et al. 1993, AJ, 106, p. 2072, "Binary Star Orbits from Speckle Interferometry. V. A Combined Speckle/Spectroscopic Study of the O Star Binary 15 Monocerotis"

Gilliland, R.L. 1994, ASP Conf. 55, ed. D.M. Pyper, R.J. Angione (ASP), p. 95, "CCD Stellar Ensemble Time Series Photometry - Pursuing Stellar Oscillations at the Micro-Mag Level"

Gregg, M. 1993, ASP Conf. 48, ed. G.H. Smith, J.P. Brodie (ASP), p. 565, "Comparison of Elliptical Galaxy and Metal-Rich Globular Custer Spectra"

Hamann, F., et al. 1994, ApJ, 422, p. 626, "High-Resolution 6450-24500 Spectra of ETA Carinae"

Hamuy, M., et al. 1993, PASP, 105, p. 787, "K Corrections for Type la Supernovae"

Hamuy, M., et al. 1993, 106, p. 2392, "The 1990 Calan/Tololo Supernova Search"

Hamuy, M. et al. 1994, PASP, 106, p. 566, "Southern Spectrophotometric Standards. II."

Hanson, M.M., Conti, PS. 1994, ApJ, 423, L139, "K-Band Spectroscopy of OB Stars: A Preliminary Classification"

Hartigan, P., et al. 1993, ApJ, 414, L121, "Observations of Entrainment and Time Variability in the HH 47 Jet"

Hartigan, P., Strom, K.M., Strom, S.E. 1994, ApJ, 427, p. 961, "Are Wide Pre-Main-Sequence Binaries Coeval?

Hartkopf, W.I., et al. 1993, AJ, 106, p. 352, "ICCD Speckle Observations of Binary Stars. VIII. Measurements during 1989 - 1991 from the Cerro Tololo 4 m Telescope"

Hawley, S.L. 1993, PASP, 105, p. 955, "Magnetic Activity in Low-Mass Stars"

Hazen, M.L. 1993, AJ, 106, p. 1055, "The Variable Stars in the Field of the Globular Custer NGC 6544"

Hazen, M.L. 1994, AJ, 107, p. 1793, "Variable Stars in the Field of the Globular Custer NGC 6541"

Heisler, C.A., Vader, J.P. 1994, AJ, 107, p. 35, "Galaxies with Spectral Energy Distributions Peaking Near 60 urn. II. Optical Broadband Properties" Hibbard, J.E., et al. 1994, AJ, 107, p. 67, "Cold, Warm, and Hot Gas in the Late-Stage Merger NGC 7252"

Hill, G.J., Thompson, K.L., Elston, R. 1993, ApJ, 414, LI, "Optical Lines in High-Redshift Quasi-Stellar Objects: Balmer Lines, [O III], and Fe II"

Hoban, S., et al. 1993, Icarus, 105, p. 548, "Infrared Observations of Methanol in Comet P/Swift-Tuttle"

Hubbard, W.B., et al. 1993, Icarus, 103, p. 215, "The Occultation of 28 Sgr by Saturn: Saturn Pole Position and Astrometry"

Hughes, J.P, Smith, R.C. 1994, AJ, 107, p. 1363, "Discovery of Be/X-Ray Stars in Two Supernova Remnants in the Small Magellanic Coud"

Hui, X., Ford, H.C. 1993, IAU Symp. 155, ed. R. Weinberger, A. Acker (Kluwer), p. 533, "Planetary Nebulae and Halo Dynamics in Early Type Galaxies"

Hui, X., et al. 1993, ApJ, 414, p. 463, "The Planetary Nebula System and Dynamics of NGC 5128. I. Planetary Nebulae as Standard Candles"

Hui, X., et al. 1993, ApJS, 88, p. 423, "The Planetary Nebula System and Dynamics of NGC 5128. II. A Planetary Nebula Catalog"

Hunter, D.A., Hawley, W.N., Gallagher III, J.S. 1993, AJ, 106, p. 1797, "A Survey forExtra-H II Region Ionized Gas Structures in Irregular Galaxies"

Hunter, D.A. 1994, AJ, 107,p. 565, "Imaging and Spectroscopy of Ionized Shells and Supershells in the Large Magellanic Coud"

Imamura, J.N., et al. 1993, ApJ, 419, p. 793, "The Quasi-Periodic Oscillations of VV Puppis"

Jacoby, G.H., Kaler, J.B. 1993, ApJ, 417, p. 209, "Improved Observations of Faint Planetary Nebulae in the Magellanic Clouds"

Jones, B.F., Klemola, A.R., Lin, D.N.C 1994, AJ, 107, p. 1333, "Proper Motion of the Large Magellanic Coud and the Mass of the Galaxy. I. Observational Results"

Jura, M., et al. 1993, ApJ, 418, L37, "Constraints on the Evolution of Remnant Protostellar Dust Debris Around HR 4796"

Keenan, PC 1993, PASP, 105, p. 905, "Revised MK Spectral Classification of the Red Carbon Stars" Kim, Ch., McNamara, D.H., Christensen, CG. 1993, AJ, 106, p. 2493, "A Photometric and Spectrographic Study of SX Phoenicis"

Kirshner, R.P., et al. 1993, ApJ, 415, p. 589, "SN 1992A: Ultraviolet and Optical Studies Based on HST, IUE, and CTIO Observations" Kotilainen, J.K., Ward, M.J., Williger, G.M. 1993, MNRAS, 263, p. 655, "CCD Imaging of Seyfert Galaxies: Deconvolution of the Nuclear and Stellar Components"

Kotilainen, J.K., Ward, M.J. 1994, MNRAS, 266, p. 953, "The Host Galaxies of Seyfert Type 1 Nuclei"

Lauer, T.R., Postman, M. 1993, ASP Conf. 51, ed. G. Chincarini, A. Iovino, T. Maccacaro, D. Maccagni (ASP), p. 171, "The Motion of the Local Group with Respect to the 15,000 km/s Abell Custer Frame"

Lauer, T.R., Postman, M. 1994, ApJ, 425, p. 418, "The Motion of the Local Group with Respect to the 15,000 Kilometer per Second Abell Custer Inertial Frame"

Lee, M.G., Geisler, D. 1993, AJ, 106, p. 493, "Metal Abundances for a Large Sample of Globular Clusters in M87"

Lee, M.G., Geisler, D. 1993, ASP Conf. 48, ed. G.H. Smith, J.P. Brodie (ASP), p. 576, "The Metallicity and Luminosity Functions of the Globular Clusters in M87: Washington CCD Photometry"

Lemm, K., et al. 1993, PASP, 105, p. 1120, "Superhumps in Cataclysmic Variables. I. T. Leonis"

MacMinn, D., et al. 1994, AJ, 107, p. 1806, "Berkeley 20: An Unusual Old Open Cluster"

Mallen-Ornelas, G., Djorgovski, S. 1993, ASP Conf. 50, ed. S.G. Djorgovski, G. Meylan (ASP), p. 313, "Surface Photometry and Structural Parameters of Obscured Globular Clusters"

Marafi6n DiLeo, C, Colombo, E., Ringuelet, A.E. 1994, A&A, 286, p. 160, "(31 Monocerotis: Oscillations and Chromospheric Structure"

Martinez, P., et al. 1993, MNRAS, 263, p. 273, "A Frequency Analysis of the Rapidly Oscillating Ap Star HD 84041 and a Determination of Its Rotation Period"

Matthews, J.M., et al. 1993, ASP Conf. 44, ed. M.M. Dworetsky, F. Castelli, R. Faraggiana (ASP), p. 617, "An Empirical T - t Curve for the roAp Star HR 3831: Atmospheric Structure from Pulsation Amplitudes"

Maza, J., et al. 1994, ApJ, 424, L107, "SN 1992bc and SN 1992bo: Evidence for Intrinsic Differences in Type la Supernova Luminosities"

McAlister, H.A., et al. 1993, AJ, 106, p. 1639, "ICCD Speckle Observations of Binary Stars. X. A Further Survey for Duplicity Among the Bright Stars"

McMillan, R., Ciardullo, R., Jacoby, G.H. 1993, ApJ, 416, p. 62, "Planetary Nebulae as Standard Candles. IX. The Distance to the Fornax Cluster"

McWilliam, A., Rich, R.M. 1993, ApJS, 91, p. 749, "The First Detailed Abundance Analysis of Galactic Bulge K Giants in Baade's Window"

Mereghetti, S., et al. 1994, ApJ, 424, p. 943, "On the Nature of the X-Ray Emission from IE 1024.0- 5732/Wack 2134: The First X-Ray-Selected Wolf-Rayet Star" Meurer, G.R., Mackie, G., Carignan, C 1994, AJ, 107, p. 2021, "Optical Observations of NGC 2915: A Nearby Blue Compact Dwarf Galaxy"

Meyssonier, N., Azzopardi, M. 1993, A&AS, 102,p. 451, "A New Catalogueof Ha Emission-Line Stars and Small Nebulae in the Small Magellanic Coud"

Mihos, J.C, Bothun, G.D., Richstone, D.O. 1993, ApJ, 418, p. 82, "Modeling the Spatial Distribution of Star Formation in Interacting Disk Galaxies"

Minniti, D., et al. 1993, ApJ, 413, p. 548, "High-Dispersion Spectroscopy of Giants in Metal-Poor Globular Clusters. I. Iron Abundances"

Minniti, D., et al. 1993, ASP Conf. 48, ed. G.H. Smith, J.P. Brodie (ASP), p. 210, "Oxygen Abundances for Globular Cluster Giants"

Moreno, H., et al. 1994, PASP, 106, p. 619, "Spectroscopic Observations of the Planetary Nebula Me 2-1"

Morris, P.W., et al. 1993, ApJ, 412, p. 324, "Spectrophotometry of Wolf-Rayet Stars. I. Continuum Energy Distributions"

Morse, J.A., et al. 1993, AJ, 106, p. 1139, "Spectrophotometric Evidence for Velocity Variability in the HH 34 and HH 111 Stellar Jets"

Morse, J.A., et al. 1994, ApJ, 425, p. 738, "Fabry-Perot Observations and New Models of the HH 47A and HH 47D Bow Shocks"

Mould, J.A., et al. 1993, ApJ, 416, p. 582, "The Age of the Large Magellanic Cloud Cluster NGC 1953" Nagata, T., Kobayashi, N., Sato, S. 1994, ApJ, 423, LI13, "Spectropolarimetry of Five Objects Toward the Galactic Center from 1.4 to 4.2 Microns"

Noumaru, J., Ogura, K. 1993, PASP, 105, p. 867, "W 16-185: A Heavily Reddened, Low-Excitation Planetary Nebula"

Olowin, R.P., Huchra, J.P., Corwin, H.G. 1993, ASP Conf. 51, ed. G. Chincarini, A. Iovino, T. Maccacaro, D. Maccagni (ASP), p. 104, "CTIO-Argus Observations of AcoRich Ousters of Galaxies: MeanRedshifts and Velocity Dispersions for a Complete Statistical Sample" Olszewski, E.W., Pryor, C, Schommer, R.A. 1993, ASP Conf. 48, ed. G.H. Smith, J.P. Brodie (ASP), p. 99, "The Velocity Dispersion of the Distant Halo Globular Custer NGC 2419"

Parker, J.W. 1993, AJ, 106, p. 560, "The OB Associations of30 Doradus in the Large Magellanic Coud. I. Stellar Observations and Data Reductions"

Parker, J.W., Garmany, CD. 1993, AJ, 106, p. 1471, "The OB Associations of 30 Doradus in the Large Magellanic Coud. II. Stellar Content and Initial Mass Function" Patterson, J., Moulden, M. 1993, PASP, 105, p. 779, "Rapid Oscillations in Cataclysmic Variables. X. TW Pictoris (=H 0534-581)"

Pena, M., et al. 1994, Rev. Mex. Astron. Astrofis., 28, p. 27, "LM1-64: A High Excitation Planetary Nebula with WR Nucleus in the LMC"

Pena, M., et al. 1994, ApJ, 428, L9, "A Thermal Pulse in Progress in the Nucleus of the LMC Planetary Nebula N66"

Phelps, R.L., Janes, K.A., Montgomery, K.A. 1994, AJ, 107, p. 1079, "Developmentof the Galactic Disk: A Search for the Oldest Open Clusters"

Phillips, M.M. 1993, ApJ, 413, L105, "The Absolute Magnitudes of Type la Supernovae"

Plez, B., Smith, V.V., Lambert, D.L. 1993, ApJ, 418, p. 812, "Lithium Abundances and Other Oues to Envelope Burning in Small Magellanic Coud Asymptotic Giant Branch Stars"

Prinja, R.K., Fullerton, A.W. 1994, ApJ, 426, p. 345, "Low-Velocity Variability in the Stellar Wind of HD 152408 (08: Iafpe)"

Pryor, C, Meylan, G. 1993, ASP Conf. 50, ed. S.G. Djorgovski, G. Meylan (ASP), p. 357, "Velocity Dispersions for Galactic Globular Clusters"

Quillen, A.C., Graham, J.R., Frogel, J.A. 1993, ApJ, 412, p. 550, "The Warped Disk of Centaurus A in the Near-Infrared"

Quintana, H., de Souza, R. 1993, A&AS, 101, p. 475, "Spectroscopic Observations of the Galaxy Cluster A 3571 (SC 1344-325)"

Rao, N.K., Lambert, D.L. 1993, MNRAS, 263, L27, "Optical Emission Bands in the Spectmm of the R CrB Star V854 Cen at Minimum"

Rao, N.K., Giridhar, S., Lambert, D.L. 1993, A&S, 280, p. 201, "The Hot R Coronae Borealis Star DY Centauri: Nebular and Photospheric Lines"

Reed, B.C. 1993, AJ, 106, p. 2291, "UBV Photometry of Luminous Stars Toward the Galactic Center"

Reijns, R., et al. 1993, ASP Conf. 50, ed. S.G. Djorgovski, G. Meylan (ASP), p. 79, "Internal Motions in co Centauri"

Remillard, R.A., et al. 1994, ApJ, 428, p. 785, "The X-Ray Selected Cataclysmic Variables H0459 + 246 and H0857 - 242"

Rose, J.A. 1994, AJ, 107, p. 206, "The Integrated Spectra of M32 and of 47 Tuc: A Comparative Study at High Spectral Resolution" Roth, K.C, Meyer, D.M., Hawkins, I. 1993, ApJ, 413, L67, "Interstellar Cyanogen and the Temperature of the Cosmic Microwave Background Radiation"

Rovero, A.C, Ringuelet, A.E. 1994, MNRAS, 266, p. 203, "3 Puppis: A Peculiar Object with Infrared Excess"

Rubenstein,E.P., Bailyn, CD. 1994, ASP Conf. 53, ed. R.E. Saffer (ASP), p. 173, "SX Phoenicis Variable Stars in the Globular Custer NGC 6397"

Sarajedini, A. 1993, ASP Conf. 48, ed. G.H. Smith, J.P. Brodie (ASP), p. 109, "A Color-Magnitude Diagram of the Galactic Globular Custer IC 4499"

Sarajedini, A. 1993, ASP Conf. 53, ed. R.E. Saffer (ASP), p. 14, "A Survey of Galactic Globular Clusters for Blue Straggler Stars"

Sarajedini, A. 1994, PASP, 106, p. 404, "CCD Photometry of the Galactic Globular Ouster NGC 6535 in the B and V Passbands"

Schaefer, B.E., et al. 1994, ApJ, 422, L71, "Rapid Searches for Counterparts of GRB 930131"

Schaefer, B.E. 1994, ApJ, 426, p. 493, "The Peak Brightness of SN 1937C in IC 4182 and the Hubble Constant"

Schmidt, B.P., et al. 1994, AJ, 107, p. 1444, "The Expanding Photosphere Method Applied to SN 1992am AT cz = 14 600 kms/s1"

Schmidtke, P.C, et al. 1993, PASP, 105, p. 863, "The X-Ray Eclipse of the LMC Binary CAL 87"

Schmitt, H.R., Storchi-Bergmann, T., Baldwin, J.A. 1994, ApJ, 423, p. 237, "Anisotropic High-Excitation Emission and Chemical Abundances in the Seyfert 2 Galaxy NGC 5643"

Schober, H.J., et al. 1994, A&AS, 105, p. 281, "Physical Studies of Asteroids. XXVIII. Lightcurves and Photoelectric Photometry of Asteroids 2, 14, 51, 105, 181, 238, 258, 369, 377, 416, 487, 626, 679, 1048 and 2183"

Schommer, R.A. 1993, ASP Conf. 48, ed. G.H. Smith, J.P. Brodie (ASP), p. 458, "Kinematics of Star Ousters in M33 and Comparisons with the Magellanic Cloud and Milky Way Systems"

Schroder, M.F.S., Pastoriza, M.G., Kepler, S.O. 1994, A&AS, 104, p. 487, "The Distribution of Light in the Barred Spirals NGC 5757 and IC 1091"

Silbermann, N.A., et al. 1994, AJ, 107, p. 1764, "RR Lyrae Stars and Color-Magnitude Diagram of the Globular Cluster NGC 6388"

Silva, D.R., Elston, R. 1994, ApJ, 428, p. 511, "Probing Radial Age/Metallicity Degeneracy in Early-Type Galaxies"

10 Simkin, S.M., et al. 1994, ASP Conf. 54, ed. G.V. Bicknell. M.A. Dopita, P.J. Quinn (ASP), p. 347, "The Stmcture and Kinematics of Pictor A"

Smith, E.P., et al. 1993, ASP Conf. 52, ed. R.J. Hanisch, R.J.V. Brissenden, J. Barnes (ASP), p. 31, "Wide-Field Direct CCD Observations Supporting the Astro-1 Ultraviolet Imaging Telescope"

Smith, H.A., et al. 1993, IAU Colloquium 139, ed. J.M. Nemec, J.M. Matthews (Cambridge U. Press), p. 349, "Fundamental Mode and First Overtone Mode Cepheids in the Small Magellanic Cloud"

Smith, J.D., Thompson, D., Djorgovski, S. 1993, ASP Conf. 43, ed. B.T. Soifer (ASP), p. 189, "A Search for Quasar-Marked Protoclusters"

Smith, R.C, Raymond, J.C, Laming, J.M. 1994, ApJ, 420, p. 286, "High-Resolution Spectroscopy of Baimer-Dominated Shocks in the Large Magellanic Coud"

Stirpe, G.M., et al. 1994, ApJ, 425, p. 609, "Steps Toward Determination of the Size and Stmcture of the Broad-Line Region in Active Galactic Nuclei. VI. Variability of NGC 3783 From Ground-Based Data"

Suntzeff, N.B. 1993, ASP Conf. 48, ed. G.H. Smith, J.P. Brodie (ASP), p. 167, "The Chemical Homogeneity of Stars in Galactic Globular Clusters"

Suntzeff, N.B., et al. 1993, ApJ, 418, p. 208, "Spectroscopy of Giants in the Sextans Dwarf Spheroidal Galaxy"

Terndrup, D.M., Walker, A.R. 1994, AJ, 107, p. 1786, "Blue Horizontal Branch Stars in NGC 6522 and Baade's Window"

Thompson, D., et al. 1993, ASP Conf. 51, ed. G. Chincarini, A. Iovino, T. Maccacaro, D. Maccagni (ASP), p. 310, "Surveys for Protogalaxies and Protoclusters"

Thorburn, J.A. 1994, ApJ, 421, p. 318, "The Primordial Lithium Abundance from Extreme Subdwarfs: New Observations"

Trager, S.G, Djorgovski, S., King, I.R. 1993, ASP Conf. 50, ed S.G. Djorgovski, G. Meylan (ASP), p. 347, "Structural Parameters of Galactic Globular Clusters"

Vader, J.P., et al. 1993, AJ, 106, p. 1743, "Galaxies with Spectral Energy Distributions Peaking Near 60 (xm. I. Optical Spectroscopy, Infrared Photometry, and Radio Continuum Data"

Vijapurkar, J., Drilling, J.S. 1993, ApJS, 89, p. 293, "MK Spectral Types for OB+ Stars in the Southern Milky Way"

Vilas, F, et al. 1993, Icarus, 105,p. 67, "CCD Reflectance Spectra of Selected Asteroids. II. Low-Albedo Asteroid Spectra and Data Extraction Techniques"

Walborn, N.R., et al. 1993, PASP, 105, p. 1240, "Spectroscopyand Photometry of Companion Stars 2 and 3 to Supernova 1987A"

11 Walker, A.R. 1993, IAU Colloquium 136, ed. C.J. Butler, I. Elliott (Cambridge U. Press), p. 278, "Photometry with CCD's"

Walker, A.R. 1993, AJ, 106, p. 999,"AColor-Magnitude Diagram fortheLarge Magellanic Cloud Ouster Hodge 11"

Walker, A.R. 1993, IAU Colloquium 139, ed. J.M. Nemec, J.M. Matthews (Cambridge U. Press), p. 15, "RR Lyraes in the Magallenic Couds"

Wallerstein, G., et al. 1993, PASP, 105, p. 859, "The Spectmm of the Symbiotic Nova AS 296 (=FG Serpentis) from 1988 July to 1992 March"

Wallerstein, G.,et al. 1994, AJ, 107, p. 2211, "The Lithium Content and Other Properties of F2-G5 Giants in the Hertzsprung Gap"

Walter, F.M., et al. 1994, AJ, 107, p. 692, "X-Ray Sources in Regions of Star Formation. V. The Low Mass Stars of the Upper Scorpius Association"

White II, J.C, Honeycutt, R.K., Home, K. 1993, ApJ, 412, p. 278, "CP Puppis: No Ordinary Old Nova" Wilcots, E.M. 1994, AJ, 107, p. 1338, "Cassical H n Regions in the Magellanic Oouds. I. Physical Properties"

Williams, R.E., Phillips, M.M., Hamuy, M. 1993, ApJS, 90, p. 297 , "The Tololo Nova Survey: Spectra of Recent Novae"

Williams, R.E. 1994, ApJ, 426, p. 279, "Extinction, Ejecta Masses, and Radial Velocities of Novae" Williams, T.B., Schommer, R.A. 1993, ApJ, 419, L53, "Diffuse Ha Emission in the Virgo Cluster Associated with the 3C 273 Lyman-Alpha Oouds"

Williger, G.M., et al. 1993, First Light in the Universe: Stars or QSO's?, ed. B. Rocca-Volmerange, B. Guidcrdoni, M. Dennefeld, J. Tran Thanh Van (Editions Frontieres), p. 429, "The Lya Forest of the z = 4.5 QSO 1033-03"

Williger, G.M., et al. 1994, ApJ, 428, p. 574, "Lyman-Alpha Absorption in the Spectmm of the z = 4 5 QSO BR 1033 - 0327"

Zepf, S.E., Whitmore, B.C. 1993, ApJ, 418, p. 72, "The Stmcture and Dynamics ofElliptical Galaxies in Compact Groups" Zheng, W., Malkan, M.A. 1993, ApJ, 415, p. 517, "Does a Luminosity-Dependent Continuum Shape Cause the Baldwin Effect?

12 APPENDIX C

Kitt Peak National Observatory July 1993 to June 1994 Publications List

Abt, H.A. 1993, PASP, 105, p.794, "Institutional Productivities"

Adelman, S.J., Pyper, D.M. 1993, A&AS, 101, p.393, "Spectrophotometry of Peculiar B and A Stars. XIX. Variability of the Magnetic CP Stars"

Albright, G.E., Richards, M.T. 1994, ASP Conf. 56, ed. A.W. Shatter (ASP), p.360, "Evidence of Mass Transfer in TX Ursae Majoris"

Aldering, G., Humphreys, R.M., Richmond, M. 1994, AJ, 107, p.662, "SN 1993J: The Optical Properties of Its Progenitor"

Allard, F. et al. 1994, AJ, 107, p.1565, "Studies of Hot B Subdwarfs. IX. Cousins BVRI Photometry and the Binary Fraction of Hot, Hydrogen-Rich Subdwarfs in the Palomar-Green Survey"

Allen, M.M. 1994, ApJ, 424, p.754, "CH+ in the Interstellar Medium"

Anthony-Twarog, B.J., Twarog, B.A. 1994, AJ, 107, p. 1577, "Reddening Estimation for Halo Red Giants Using uvby Photometry"

Armandroff, T.E. 1993, ASP Conf. 49, ed. S.R. Majeweski (ASP), p.167, "Globular Clusters of the Outer Halo as Probes of the Galaxy's Stmcture and Early Evolution"

Armandroff, T.E. 1993, ASP Conf. 48, ed. G.H. Smith (ASP), p.48, "The Disk Population of Globular Clusters"

Armandroff, T.E. et al. 1993, AJ, 106, p.986, "The Dwarf Spheroidal Companions to M31: A Color-Magnitude Diagram for And III"

Baffa, C. et al. 1993, A&A, 280, p.20, "Peculiar Motions in Superclusters: Perseus-Pisces"

Bally, J., Devine, D. 1994, ApJ, 428, p.L65, "A Parsec-Scale "Superjet" and Quasi-Periodic Stmcture in the HH 34 Outflow?"

Banfi, M. et al. 1993, A&A, 280, p.373, "H II Regions in Spiral Galaxies: Positions, Luminosity Function and Diameter Distribution"

Barden, S.C. 1994, ASP Conf. 55, ed. D.M. Pyper (ASP), p.130, "The Use and Benefits of Optical Fibers in Spectroscopy"

Barden, S.C. et al. 1994, SPIE, 2198, ed. D.L. Crawford (SPIE), p.87, "Modifying Hydra for the WIYN Telescope - An Optimum Telescope, Fiber MOS Combination"

Bauer, W.H. 1994, PASP, 106, p.244, "Spectroscopic Observations of the 1982 Eclipse of 31 Cygni" Baum, W.A. et al. 1993, IAU Symp. 153, ed. H. Dejonghe (Kluwer), p.289, "Hubble Space Telescope Observations of Baade's Window"

Belton, M.J.S. et al. 1994, Science, 264, p.1112, "Galileo Multispectral Imaging of the North Polar and Eastern Limb Regions of the Moon"

Benson, P.J. et al. 1994, AJ, 107, p.1453, "Light Curves of SN 1993J from the Keck Northeast Astronomy Consortium"

Bernstein, G.M. et al. 1994, ApJ, 426, p.516, "Correlations of Galaxies at z=0.3"

Blair, W.P., Fesen, R.A. 1994, ApJ, 424, p.L103, "The Optical Counterpart to the Luminous X-Ray Supernova Remnant in NGC 6946"

Blanco, D., Johns, M. 1994, SPIE,2199, ed. L.M. Stepp,p.743, "Thermal Design of the WIYN3.5 Meter Telescope Enclosure"

Bohannan, B., Fitzpatrick, E.L. 1993, New Aspects of Magellanic Cloud Research, ed. B. Baschek (Springer), p.294, "Implications of Processed Material in the Atmospheres of LMC B Supergiants"

Bond, H.E., Cardullo, R. 1993, IAU Symp. 155, ed. R. Weinberger (Kluwer), p.489, "A Search for Pulsations in 0 VI Planetary Nuclei"

Bond, H.E., Cardullo, R. 1993, IAU Symp. 158, ed. M.A. Barstow (Kluwer), p.491, "Asteroseismology of Planetary Nuclei"

Bond, H.E., Cardullo, R., Kawalcr, S.D. 1994, Acta Astron, 43, p.425, "Asteroseismology of Planetary Nebula Nuclei"

Bopp, B.W. ct al. 1993, AJ, 106, p.2502, "Extremely Active Long-Period RS CVn Binary HD 12545"

Boroson, T. ct al. 1994, SPIE, 2198, ed. D.L. Crawford (SPIE), p.877, "Development of a 8192 x 8192 CCD Mosaic Imager"

Boroson, T.A., Salzer, J.J., Trotter, A. 1993, ApJ, 412, p.524, "A New Survey for Low-Luminosity Emission-Line Galaxies"

Bowcn, D.V. et al. 1994, ApJ, 420, p.L71, "Interstellar and Intergalactic Magnesium and Sodium Absorption Toward SN 1993J"

Boyle, R.J. et al. 1994, ApJ, 420, p.863, "Observations of 13.5 Micron Rotation-Vibration Lines of SiS in IRC + 10216"

Braun, R. et al. 1994, ApJ, 420, p.558, "Counterrotating Gaseous Disks in NGC 4826" Bryja, C, Humphreys, R.M., Jones, T.J. 1994, AJ, 107, p.246, "The Lowest Mass Stars in the Hyades" Caldwell, N. et al. 1993, AJ, 106, p.473, "Star Formation in Early-Type Galaxies in the Coma Cluster" Carney, B.W. et al. 1994, AJ, 107, p.2240, "A Survey of Proper Motion Stars. XII. An Expanded Sample"

Carswell, R.F., et al. 1994, MNRAS, 268, p.Ll, "Is There Deuterium in the z=3.32 Complex in the Spectmm of 0014+813?"

Casement, L.S. et al. 1994, Infrared Astronomy with Arrays, ed. I. McLean (Kluwer), p.163, "Extended Near-Infrared Nebulosity Around Elias 32 and Elias 33"

Charmandaris, V., Appleton, P.N., Marston, A.P. 1993, ApJ, 414, p.154, "Threshold Star-Formation Effects in the Peculiar Galaxy ARP 10 (=VV 362)"

Chen, J., Jewitt, D. 1994, Icarus, 108, p.265, "On the Rate at Which Comets Split"

Cardullo, R., Bond, H.E. 1993, IAU Symp. 155, ed. R. Weinberger (Kluwer), p.490, "Global Photometric Campaigns on Pulsating Planetary Nuclei"

Cardullo, R., Jacoby, G. 1993, IAU Symp. 155, ed. R. Weinberger (Kluwer), p.570, "The Radial Velocities of Planetary Nebulae in NGC 3379"

Cardullo, R., Jacoby, G.H., Dejonghe, H.B. 1993, ApJ, 414, p.454, "The Radial Velocities of Planetary Nebulae in NGC 3379"

Cardullo, R., Jacoby, G.H., Tonry, J.L. 1993, ApJ, 419, p.479, "A Comparison of the Planetary Nebula Luminosity Function and Surface Brightness Fluctuation Distance Scales"

Collier, J., Hodge, P. 1994, ApJS, 92, p.119, "The H II Regions of NGC 6822. III. A Photometric Atlas"

Courteau, S. et al. 1993, ApJ, 412, p.L51, "Streaming Motions in the Local Universe: Evidence for Large-Scale, Low-Amplitude Density Fluctuations"

Crawford, D.L. 1994, PASP, 106, p.397, "uvby and p Photometry for Stars in the Open Cluster NGC 1502"

Crawford, D.L. 1994, IAU Colloq. 136, ed. J. Butler (Cambridge U. Press), p.244, "GNAT -A Global Network of Automatic Telescopes"

Crawford, D.L. 1994, Precision Photometry, ed. D. Kilkenny (SAAO), p.18, "Thoughts on Precision Photometry"

Crawford, D.L., Craine, E. 1994, SPIE, 2198, ed. D.L. Crawford (SPIE), p.359, "A Global Network of Astronomical Telescopes ~ GNAT"

Demarque, P., Sarajedini, A., Guo, X.-J. 1994, ApJ, 426, p.165, "The Gap in the Color-Magnitude Diagram of NGC 2420: A Test of Convective Overshoot and Ouster Age"

Devereux, N.A., Young, J.S. 1993, AJ, 106, p.948, "The Origin of the Far Infrared Luminosity Within the Spiral Galaxy NGC 6946" Dey, A., van Breugel, W.J.M. 1994, AJ, 107, p.1977, "Blue Optical Continuum Associated with a Radio Knot in 3C346"

Dobrzycka, D., Kenyon, S.J., Mikolajewska, J. 1993, AJ, 106, p.284, "Spectroscopic Observations of V443 Herculis: A Symbiotic Binary with a Low Mass White Dwarf'

Dobrzycka, D., Kenyon, S.J., Mikolajewska, J. 1994, ASP Conf. 56, ed. A.W. Shatter (ASP), p.368, "Spectroscopic Observations of V443 Herculis: A Symbiotic Binary with a Low Mass White Dwarf'

Dorren, J.D., Guinan, E.F. 1994, ApJ, 428, p.805, "HD 129333: The Sun in Its Infancy"

Durrell, P.R., Harris, W.E. 1993, ASP Conf. 48, ed. G.H. Smith (ASP), p.91, "Deep CCD Photometry of the Globular Ouster M15"

Edwards, S. et al. 1993, AJ, 106, p.372, "Angular Momentum Regulation in Low-Mass Young Stars Surrounded by Accretion Disks"

Eggen, O.J. 1994, AJ, 107, p.1834, "The Very Short Period Cepheid (RR Lyr) Variables. II. Light and Color Curves of Variables in the Solar Vicinity"

Eisenhardt, P. et al. 1994, Infrared Astronomy with Arrays, ed. I. McLean (Kluwer), p.543, "RestFrame Optical Spectroscopy of Distant Radio Galaxies"

Elston, R. 1994, Infrared Astronomy with Arrays, ed. I. McLean (Kluwer), p.33, "The Evolution of Early Type Galaxies"

Elston, R.,Maloney, P. 1994, Infrared Astronomy with Arrays, ed. I. McLean (Kluwer), p.169, "Molecular Hydrogen Emission from Central Cluster Galaxies in Cooling Flows"

Elston, R. et al. 1994, AJ, 107, p.910, "The Seyfert II Nature of the IRAS Source FSC 10214+4724"

Eracleous, M., Halpcrn, J.P. 1994, ApJS, 90, p.l, "Double-Peaked Emission Lines in Active Galactic Nuclei"

Famham, T.L., Meech, K.J. 1994, ApJS, 91, p.419, "Comparison of the Plasma Tails of Four Comets: P/Halley, Okazaki-Levy-Rudenko, Austin, and Levy" Fedcrman, S.R. et al. 1994, ApJ, 424, p.772, "Chemical Transitions for Interstellar C2 and CN in Coud Envelopes"

Fekel, F.C et al. 1993, AJ, 106, p.2370, "Chromospherically Active Stars. XI. Giants with Compact Hot Companions and the Barium Star Scenario"

Fekel, F.C, Bopp, B.W. 1993, ApJ, 419, p.L89, "Optical Spectroscopy of the Dusty K5 V Star HD 98800"

Fekel, F.C, Tomkin, J. 1993, AJ, 106, p.l 156, "The Spectroscopic Orbit for Gamma Geminorum and a Search for Its Secondary" Fleming, T.A. et al. 1993, AJ, 106, p.1729, "Three New BL Lacertae Objects in the Palomar-Green Survey"

Ford, CH. et al. 1993, AJ, 106, p.l 101, "CCD Photometry of Three la Supernovae: V, R, and I Light Curves"

Fowler, A.M. et al. 1994, Experimental Astronomy, 3, p.243, "Performance of the Current 256x256 SBRC InSb Array and Status of the Next Generation 1024x1024 InSb Array"

Fowler, A.M. et al. 1994, Infrared Astronomy with Arrays, ed. I. McLean (Kluwer), p.399, "Performance of the Current 256x256 SBRC InSb Array and Status of the Next Generation 1024x1024 InSb Array"

Fowler, A.M. et al. 1994, SPIE, 2198, ed. D.L. Crawford (SPIE), p.623, "Next Generation in InSb Arrays: ALADDIN, the 1024x1024 InSb Focal Plane Array Development Project Status Report"

Franx, M. 1993, PASP, 105, p. 1058, "Constraining Galaxy Evolution and Cosmology from Galaxay Kinematics: First Observations at z=0.18"

Fried, J.W., Illingworth, G.D. 1994, AJ, 107, p.992, "Kinematics of 12 Elliptical Galaxies"

Gallagher, J.S., Gibson, S.J. 1994, Panchromatic View of Galaxies, ed. G. Hensler (Editiones Frontieres), p.207, "Starburst Galaxies"

Gamett, D.R., Kennicutt, Jr., R.C. 1994, ApJ, 426, p.123, "A Very Metal Poor H II Region in the Outer Disk of M101"

Gatley, I., Merrill, K.M. 1993, SPIE, 1946, A.M. Fowler, ed., p.2, "The Impact of Two Dimensional Arrays on Astronomy"

Gatley, I., Merrill, M. 1994, Infrared Astronomy with Arrays, ed. I. McLean (Kluwer), p.551, "The Distribution of Gas and Dust in Galactic HII Regions"

Gelderman, R., Whittle, M. 1994, ApJS, 91, p.491, "An Optical Study of Compact Steep-Spectrum Radio Sources. I. The Spectroscopic Data"

Gelderman, R.F. 1994, Ph.D. Thesis (University of Virginia), "An Optical Study of Compact Steep Spectmm Radio Sources"

Gies, D.R. et al. 1993, AJ, 106, p.2072, "Binary Star Orbits from Speckle Interferometry. V. A Combined Speckle/Spectroscopic Study of the O Star Binary 15 Monocerotis"

Gies, D.R. et al. 1994, ApJ, 422, p.823, "HD 53975: An O-Type Spectroscopic Binary with a Large Mass Ratio"

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Hillenbrand, L.A. et al. 1993, AJ, 106, p.1906, "NGC 6611: A Cluster Caught in the Act"

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Kaitchuck, R.H. et al. 1994, ASP Conf. 56, ed. A.W. Shatter (ASP), p.287, "Doppler Emission Line Tomography of Cataclysmic Variables"

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Kristian, J. et al. 1993, AJ, 106, p.1330, "Imaging of the Gravitational Lens System PB 1115+080 with the Hubble Space Telescope"

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Lauer, T.R., Postman, M. 1994, ApJ, 425, p.418, "The Motion of the Local Group with Respect to the 15,000 Kilometer Per Second Abell Cluster Incrtial Frame"

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10 Morrison, H.L. 1993, AJ, 106, p.578, "The Local Density of Halo Giants"

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Tumshek, D.A. et al. 1994, ApJ, 428, p.93, "The HST Quasar Absorption Line Key Project. IV. HST Faint Object Spectrograph and Ground-Based Observations of the Unusual Low-Redshift Broad Absorption-Line Quasi-Stellar Object PG 0043+039"

Vader, J.P. et al. 1993, AJ, 106, p.1743, "Galaxies with Spectral Energy Distributions Peaking Near 60 u.m. I. Optical Spectroscopy, Infrared Photometry, and Radio Continuum Data"

van Breugel, W.J.M., Dey, A. 1993, ApJ, 414, p.563, "Induced Star Formation in a Radio Lobe of 3C 285?"

van der Hulst, J.M. et al. 1993, AJ, 106, p.548, "Star Formation Thresholds in Low Surface Brightness Galaxies"

Veilleux, S. 1993, RevMexAA, 27, p.65, "Luminous Infrared Galaxies: AGN or Starbursts?"

Veilleux, S., Goodrich, R.W., Hill, G.J. 1994, ASP Conf. 54, ed. G.V. Bicknell (ASP), p.273, "Infrared Spectroscopy of Seyfert 2S: A Look Through the Obscuring Toms?"

Veilluex, S. 1993,PASP, 105, p.1038,"The Line-EmittingGas in Active Galaxies: A Probe of the Nuclear Engine"

Wallerstein, G., Morell, O. 1994, A&A, 281, p.L37, "Evidence for Sudden Moderate Mixing Events in Early M Giants"

Walter, F.M. et al. 1994, AJ, 107, p.692, "X-Ray Sources in Regions of Star Formation. V. The Low Mass Stars of the Upper Scorpius Association"

Walterbros, R.A.M., Braun, R., Kennicutt, Jr., R.C. 1994, AJ, 107, p.184, "The Optical Morphology of the Kinematically Peculiar Galaxy NGC 4826"

Warren, S.J., Hewett, P.C., Osmer, P.S. 1994, 421, p.412, "A Wide-Field Multicolor Survey for High-Redshift Quasars, z > 2.2. III. The Luminosity Function"

Weintraub,D.A. et al. 1994, ApJ, 423, p.674, "Infrared Spectroscopy and Imaging Polarimetry of the Disk Around the T Tauri Star RNO 91"

15 Weintraub, D.A., Kastner, J. 1993, ApJ, 411, p.767, "The Exciting Young Stellar Object for the Molecular Outflow at the Core of L1287"

Weintraub, D.A., Kastner, J.H., Mahesh, A. 1994, ApJ, 420, p.L87, "Discovery of a Deeply Embedded Companion to LkHa 234"

Weis, E.W. 1994, AJ, 107, p.l 135, "Long Term Variability in Dwarf M Stars"

Welty, A.D. et al. 1993, PASP, 105, p.1427, "A Long-Term Study of Ha Line Variations in FK Comae Berenices"

Wesemael, F. et al. 1993, PASP, 105, p.761, "An Atlas of Optical Spectra of White-Dwarf Stars"

Whitney, B.A. et al. 1993, ApJ, 417, p.687, "Spectrum of the "Invisible" Companion of Z Canis Majoris Revealed in Polarized Light"

Wiedemann, G. et al. 1994, ApJ, 423, p.806, "CarbonMonoxide Fundamental Bands in Late-Type Stars. III. Chromosphere or Co-mosphere?"

Wilson, W.J.F., Milone,E.F., Fry, D.J.I. 1993, PASP, 105,p.809, "Studiesof Large-Amplitude DeltaScuti Variables. I. A Case Study of EH Librae"

Windhorst, R.A. et al. 1994, AJ, 107, p.930, "Hubble Space Telescope Medium Deep Survey. II. Deconvolution of Wide Field Camera Field Galaxy Images in the 13h+43° Field"

Wise, M.W., Sarazin, CL. 1993, ApJ, 415, p.58, "The X-Ray Spectra of Custer Cooling Hows. I. Optically Thin Models"

Yoon, T.S. et al. 1994, PASP, 106, p.239, "Quantitative Spectral Types for 19 Algol Secondaries"

Zepf, S.E., Whitmore, B.C. 1993, ApJ, 418, p.72, "The Stmcture and Dynamics of Elliptical Galaxies in Compact Groups"

16 APPENDIX D

National Solar Observatory July 1993 to June 1994 Publications List

Alissandrakis, C.E., Nindos, A., Kundu, M.R. 1993, Solar Phys., 147, p. 343, "Evidence for Ordinary Mode-Emission from Microwave Bursts"

Altrock, R.C. 1993, Encyclopedia of Astronomy, 2nd Edition, ed. S.P. Parker, J.M. Pasachoff (McGraw- Hill), p. 377, "Solar Corona"

Altrock, R.C, Gilliam, L.B., Henry, T.W. 1994, Solar-Geophysical Data, Part 1 (Prompt Reports), Nos. 583-594, ed. H.E. Coffey, "Sacramento Peak Coronal Line Synoptic Maps, 1993"

Altrock, R.C, Gilliam, L.B., Henry, T.W. 1994, Solar-Geophysical Data Part 1 (Prompt Reports), Nos. 583-594, ed. H.E. Coffey, "Coronal Line Emission (Sacramento Peak), 1993"

Ambmoso, P., et al. 1993, Solar Phys., 141, p. 35, "The Center-to-Limb Variations of Four Ca I Lines in the Photospheric Spectmm at ^6500"

Aschwanden, M.J. 1993, ApJ, 416, p. 857, "Quasi-Periodic Particle Injection into Coronal Loops"

Bachmann, K.T., Brown, T.M. 1993, ApJ, 411, L45-L48, "p-Mode Frequency Variation in Relation to Global Solar Activity"

Bachmann, K.T., Schou, J., Brown, T.M. 1993, ApJ, 412, p. 870, "Observations of Intermediate Degree Solar Oscillations: 1989 April-June"

Bachmann, K.T., White, O.R. 1994, Sol. Phys., 150, p. 347, "Observations of Hysteresis in Solar Cycle Variations Among Seven Solar Activity Indicators"

Badiali, M., et al. 1994, STARS (Seismic Telescope for Astrophysical Research from Space), ESA Science Division Report 94-8, p. 10, "An Investigation of Stellar Suucture and Evolution"

Bame, S.J., et al. 1993, Geophys. Res. Lett., 20, p. 2323, "Ulysses Observations of a Recurrent High Speed Solar Wind Stream and the Heliomagnetic Streamer Belt"

Bastian, T.S., Ewell, M.W., Zirin, H. 1993, ApJ, 418, p. 510, "A Study of Solar Prominences Near 1 = 1 Millimeter"

Beckers, J.M. 1994, NATO Advanced Research Workshop, ed. R.J. Rutten, C.J.Schrijver (Kluwer), p. 501, "Solar Surface Magnetism: Quests for Observations"

Bocchialini, K., Vial, J.C, Koutchmy, S. 1994, ApJ, 423, L67, "Dynamical Properties of the Chromosphere In and Out of the Solar Magnetic Network"

Bogart, R.S., et al. 1993, GONG 1992: Seismic Investigation of the Sun and Stars, ed. T. Brown (Asuonomical Society of the Pacific), p. 429, "Artificial Data for Testing Helioseismology Algorithms" Braun, D.C, et al. 1993, GONG 1992: Seismic Investigation of the Sun and Stars, ed. T. Brown (Astronomical Society of the Pacific), p. 77, "TheP-Mode ScatteringProperties of a Sunspot"

Brosius, J.W., et al. 1993, ApJ, 411, p. 410, "Simultaneous Observations of Solar Plage with the Solar Extreme Ultraviolet Rocket Telescope andSpecuograph (SERTS), theVLA, and the KittPeak Magnetograph"

Bumba, V., et al. 1993, A&A, 276, p. 193, "Evolution, Activity, Magnetic Fields, Line-of-Sight and Proper Motions in the Solar Active Region NOAA 6659 (June 3-16,1991)"

Cauzzi, G.,et al. 1993, Sol.Phys. 146, p. 207, "On theCalibration of Line-of-Sight Magnetograms"

Clark, T.A., et al. 1993, IAU Symposium 154, ed. D.M. Rabin, J.K. Jefferies (Kluwer), p. 173, "Near IR Observations of the 11 July 1991 Total Solar Eclipse from Mauna Kea, Hawaii"

Cook, J.W. 1994, IAU Symposium 154, ed. D.M. Rabin, J.K. Jefferies (Kluwer), p. 287, "Magnetic Fields, Oscillations, and Heating in the Quiet Sun Temperature Minimum Region from Uluaviolet Observations at 1600A"

Coulter, R.L., Kuhn, J.R. 1994, 13th Sacramento Peak Summer Workshop, ed. R.R. Radick, "RISE/PSPT as an Experimentto Study ActiveRegion Irradianceand LuminosityEvolution"

D'Silva, S., Howard, R.F. 1993, Sol. Phys., 148, p. 1, "Limits on the Magnetic Field Suength at the Base of the Solar Convection Zone"

D'Silva, S., Howard, R.F. 1994, Sol. Phys., 151, p. 213, "Sunspot Rotation and the Field Suengths of Subsurface Flux Tubes"

Dara, H.C, Koutchmy, S., Alissandrakis, C.E. 1993, A&A, 277, p. 648, "Photospheric and Chromospheric Magnetic Field Structureof a Bipolar Sunspot Region"

Darvann, T.A. 1994, IAU Symposium 154, ed. D.M. Rabin, J.K. Jefferies (Kluwer), p. 259, "Measurements of Horizontal Flows in 1.6 mm Granulation"

Darvann, T.A., Koutchmy, S. 1994, IAU Symposium 154, ed. D.M. Rabin, J.K. Jefferies (Kluwer), p. 483, "The IRContrast of Magnetic Elements Obtained from High Spatial Resolution Observations at 1.6 mm"

Deming, D., Plymate, C. 1994, ApJ, 426, p. 382, "On the Apparent Velocity ofIntegrated Sunlight. II. 1983-1992 and Comparisons with Magnetograms"

Denker, C, Restaino, S.R., Radick, R.R. 1994, 13th Sacramento Peak Summer Workshop, ed. R.R. Radick, p. 86, "A Comparison of Two Wavefront Sensors"

Donahue, R.A., Restaino, S.R., Keil, S.L. 1994, Sol. Phys., 149, p. 257, "Solar and Stellar Chromospheric Conuast. I. The Disk-Integrated Solar K-Line"

Dowdy, J.F. 1993, ApJ, 411, p. 406, "Observational Evidence for Hotter Transition Region Loops Within the Supergranular Network" Dunn, R.B., Smartt, R.N., Koutchmy, S. 1994, Space 94: The Fourth International Conference and Exposition on Engineering, Constmction, and Operations in Space, ed. R. G. Galloway (American Society of Civil Engineers), "Novel Designs for Space-Borne White-Light Coronagraphs"

Duvall, T.L., et al. 1993, Applications of Time Series in Astronomy and Meteorology, ed. O. Lessi (S.M. Legatoria: Padova), p. 179, "The Frequency Variation of Solar Acoustic Wave Travel Times"

Fontenla, J. , et al. 1994, ApJ, 424, p. 1022, "Time Evolution of a Miniflare as Seen in Ha, UV Lines, and X- Rays"

Georgakilas, A.A., Zachariadis, T.G., Alissandrakis, CE. 1993, Sol. Phys., 146, p. 241, "Evolution of an Active Region and Associated Ha Arch Sttuctures"

Giampapa, M.S. et al. 1993, ApJ Suppl., Ser. 89, p. 321, "A Synoptic Study of Ha Line Profile Variability in the T Tauri Star SU Aurigae"

Grossmann-Doerth, U., et al. 1994, A&A, 285, p. 648, "The Deep Layers of Solar Magnetic Elements"

Guhathakurta, M., Fisher, R.R., Altrock, R.C. 1993, ApJ, 414, L145, "Large-Scale Coronal Temperature and Density Disuibutions"

Guhathakurta, M., Fisher, R.R., Aluock, R.C. 1994, Adv. Space Res, 14, no. 4, p. 49, "The Solar Cycle Variation of Coronal Temperature and Density During Cycle 21 - 22"

Gurman, J.B. 1993, ApJ, 412, p. 865, "The Sunspot Transition Region: Where are the Bright Plumes and the Downflows?"

Harmon, R., et al. 1993, ApJ, 417, L83, "The Coronal Suucture Above Sunspots and Pores"

Harrison, R.A., et al. 1993, A&A, 274, L9, "An Active Solar Prominence in 1.3 mm Radiation"

Harvey, J., et al. 1993, GONG 1992: Seismic Investigation of the Sun and Stars, ed. T. Brown (Astronomical Society of the Pacific), p. 397, "GONG Project Update"

Harvey, J.W., et al. 1993, GONG 1992: Seismic Investigation of the Sun and Stars, ed. T. Brown (Asuonomical Society of the Pacific), p. Ill, "Chromospheric Oscillations and the Background Spectrum"

Harvey, J.W., Livingston, W.C. 1994, IAU Symposium 154, ed. D.M. Rabin, J.K. Jefferies (Kluwer), p. 59, "Variability of the Solar HeI 10830 ATriplet"

Harvey, K.L. 1993, PhD Thesis (University of Utrecht), "Magnetic Bipoles on the Sun"

Harvey, K.L. 1993, IAU Colloquium 141, ed. H. Zirin, Q. Ai, H. Wang (Kluwer), p. 48, "Properties of Emerging Bipolar Active Regions"

Harvey, K.L. 1994, IAU Symposium 154, ed. D.M. Rabin, J.K. Jefferies (Kluwer), p. 71, "Observations of Dynamic Events in He I X10830"

Harvey, K.L. 1994, NATO ASI Workshop, ed. R.J. Rutten, C.J. Schrijver (Kluwer), p. 347, "The Magnetic Cycle" Harvey, K.L., et al. 1993, Adv. SpaceRes., 13,no. 9, p. 27, "Lifetimes and Distribution of Coronal Bright Points Observed with Yohkoh"

Harvey, K.L., Zwaan, C. 1993, Sol. Phys., 148, p. 85, "Properties and Emergence Patterns of Bipolar Active Regions. I. Size Distribution and Emergence Frequency"

Howard, R.F. 1993, Sol.Phys., 147, p. 1, "Some Factors Affecting the Growth and Decay of Plages"

Howard, R.F. 1993, IAU Colloquium 141, ed. H. Zirin, Q. Ai, H. Wang (Kluwer), "The Development of Sunspot Groups"

Howard, R.F. 1994, Sol. Phys., 149, p. 23, "APossible Coriolis-Force Contribution to the Tilt-Angle Rotation of Sunspot Groups"

Howard, R.F. 1994, Solar Magnetic Fields, ed. M. Schuessler, W. Schmidt (Cambridge Univ. Press), "Polarity Separation in Active Regions"

Howard, R.F. 1994, NATO ASI Workshop, ed. R.J. Rutten, C.J. Schrijver (Kluwer), p. 297, "Average East-West Inclinations of Surface Magnetic Field Lines"

Jaksha, D., etal. 1994, IAU Symposium 154, ed. D.M. Rabin, J.K. Jefferies (Kluwer), "A Magnetic Field Strength vs. Temperature Relation in Sunspots"

Jefferies, S.M., Christou, J.C. 1993, ApJ, 415, p. 862, "Restoration of Astronomical Images by Iterative Blind Deconvolution"

Jones, H.P. 1993, IAU Colloquium 141, ed. H. Zirin, Q. Ai, H. Wang (Kluwer), "Spectrometer-Based Magnetographs"

Jones, H.P. 1994, IAU Symposium 154, ed. D.M. Rabin, J.K. Jefferies (Kluwer), "Interpreting Recent Observations of He I 10830 A"

Kariyappa, R., Sivaraman, K.R., Anadaram, M.N. 1994, Sol. Phys., 151, p. 243, "Heating of the Quiet Solar Chromosphere I. Roleof theInnerNetwork Bright Points" Keil, S.L. 1993, Encyclopedia ofAstronomy, 2nd Edition, ed. S.P. Parker, J.M. Pasachoff (McGraw-Hill), p. 316, "Photosphere"

Keil, S.L., et al. 1994, IAU Symposium 154, ed. D.M. Rabin, J.K. Jefferies (Kluwer), p. 251, "Simultaneous IR and Visible Light Measurements of the Solar Granulation"

Keller, C.U., et al. 1994, A&A, 286, p. 626, "On theSuength of Solar Intra-Network Fields"

Kennedy, J.R., Jefferies, S.M., Hill, F. 1993, GONG 1992: Seismic Investigation of the Sun and Stars, ed. T. Brown (Astronomical Society ofthe Pacific), p. 273, "Solar g-Mode Signatures in p-Mode Signals" Komm, R.W. 1994, Sol. Phys., 149, p. 417, "Meridional Flow and Rotation ofActive Regions"

Komm, R.W., Harvey, J.W., Howard, R.F. 1993, GONG 1992: Seismic Investigation of the Sun and Stars, ed. T. Brown (Astron. Soc. Pac), p. 269, "Torsional Oscillations and Internal Rotation" Komm, R.W., Howard, R.F., Harvey, J.W. 1993, Sol. Phys., 147, p. 207, "Meridional Flow of Small Photospheric Magnetic Features"

Komm, R.W., Howard, R.F., Harvey, J.W. 1994, Sol. Phys., 151, p. 15, "The Covariance of Latitudinal and Longitudinal Motions of Small Magnetic Features"

Komm, R.W., Howard, R.F., Harvey, J.W. 1994, Solar Magnetic Fields, ed. M. Schuessler, W. Schmidt (Cambridge Univ. Press), "Solar Non-Rotational Motions"

Kopp, G., Rabin, D.M. 1994, IAU Symposium 154, ed. D.M. Rabin, J.K. Jefferies (Kluwer), p. 477, "A Magnetic Field Suength vs. Temperature Relation in Sunspots"

Kotov, V.A., Koutchmy, S. 1994, IAU Symposium 154, ed. D.M. Rabin, J.K. Jefferies (Kluwer), "On Sunspot and Facular ConUast Variations Near 2 and 4 Microns"

Koutchmy, S. 1994, IAU Symposium 154, ed. D.M. Rabin, J.K.Jefferies (Kluwer), p. 239, "The Infrared Granulation Observations"

Koutchmy, S., et al. 1994, A&A, 281, p. 249, "CFHT Eclipse Observation of the Very Fine-Scale Solar Corona"

Koutchmy, S., Restaino, S.R. 1994, 13th Sacramento Peak Summer Workshop, ed. R.R. Radick, "Toward High- Spatial Resolution IR Solar Observations"

Kuhn, J.R. 1994, GONG 1992: Seismic Investigation of the Sun and Stars, ed. T. Brown (Asuonomical Society of the Pacific), p. 27, "What Causes Cycle-Related Global Solar Changes?"

Kuhn, J.R., et al. 1994, IAU Symposium 154, ed. D.M. Rabin, J.K. Jefferies (Kluwer), p. 185, "IR Observations of the K and F Corona During the 1991 Eclipse"

Kumar, P., et al. 1994, ApJ, 422, L29, "Limits on Coronal Reflection Using High-Frequency Solar Oscillations"

Kundu, M.R., et al. 1994, ApJ, 427, L59, "Nonthermal Processes in Flaring X-Ray Bright Points"

Lang, K.R., et al. 1994, ApJ, 419, p. 398, "Magnetospheres of Solar Active Regions Inferred from SpecUal- Polarization Observations with High Spatial Resolution"

Latushko, S. 1993, Sol. Phys., 146, p. 401, "The Relationship Between Meridional Drift and Rotation of the Large-Scale Solar Magnetic Field"

Latushko, S. 1994, Sol. Phys., 149, p. 231, "Meridional Drift in the Large-Scale Solar Magnetic Field Pattern"

Lawrence, J.K., Topka, K.P., Jones, H.P. 1993, J. Geophys. Res., 98, p. 18911, "Conuast of Faculae Near the Disk Center and Solar Variability"

Lazrek, M., Hill, F. 1993, A&A, 280, p. 704, "Temporal Window Effects and Their Deconvolution from Solar Oscillation SpecUa"

Lazrek, M., Hill, F. 1993, GONG 1992: Seismic Investigation of the Sun and Stars, ed. T. Brown (Asuonomical Society of the Pacific), p. 449, "The Deconvolution of Temporal Window Effects from Solar Oscillation SpecUa" Le Blanc, R.B., White, J.B., Bernath, P.F. 1994, J. Mol. SpecU., 164, p. 574, "High-Resolution Infrared Emission Specua of HC1 and HFX"

Lindsey, CA. 1994, IAU Symposium 154, ed. D.M. Rabin, J.K. Jefferies (Kluwer), "The Sun in Submillimeter Radiation"

Lindsey, C.A., Braun, D.C, Jefferies, S.M. 1993, GONG 1992: Seismic Investigation of the Sun and Stars, ed. T. Brown, (Asuonomical Society ofthe Pacific), p. 81, "Local Helioseismology of Subsurface Structure"

Lites, B.W., et al. 1993, ApJ, 418, p. 928, "Stokes Profile Analysis and Vector Magnetic Fields. VI. Fine Scale SUucture of a Sunspot"

Lites, B.W., Rutten, R.J., Thomas, J.H. 1994, NATO ASI Workshop,ed. R.J. Rutten, C.J. Schrijver (Kluwer), p. 159, "Chromospheric Oscillations"

Livingston, W.C. 1993, NATO Advanced Research Series, ed. E. Ribes (Springer-Verlag), "Surrogates for Total Solar Irradiance"

Livingston, W.C. 1994, IAU Symposium 154, ed. D.M. Rabin, J.K. Jefferies (Kluwer), p. 589, "A 4-Meter McMath Telescope for die Infrared"

LoPresto, J.C, Kraus, P.M., Pierce, A.K. 1994, Sol. Phys., 149, p. 243, "Observations of the Limb Effects in Potassium a7699"

Loucif, M.L. 1994, A&A, 281, p. 95, "Giant Macrospicules as Possible Sources ofthe Fast SolarWind"

Milford, P.N., Hill, F., Tarbell, T.D. 1993, GONG 1992: Seismic Investigation of the Sun and Stars, ed. T. Brown (AsuonomicalSociety of thePacific), p. 85, "Subsurface TransverseFlows Near an Active Region"

Muglach, K., Solanki, S.K., Livingston, W.C. 1994, NATO Advanced Research Workshop, ed. R.J. Rutten, C.J.Schrijver (Kluwer), p.127, "Preliminary Properties of Pores Derived From 1.56 Micron Lines"

Nave, G., Johansson, S. 1993, A&A, 274, p. 961, "Highly-Excited Levels of Fe I Obtained from Laboratory and Solar Fourier Transform and Grating SpecUa"

Neff, J.E., O'Neal, D., Saar, S.H. 1993, IAU Colloquium 137, ed. W.W. Weiss, A. Baglin, "Absolute Measurements of Starspot Areas and Temperatures"

Neidig, D.F. 1993, Adv. Space Res., 13, no. 9, p. 317, "Consequences of Chromospheric Irradiation in White- Light Flares: an Observer's Point of View"

Neidig, D.F., et al. 1994, 1994 Space Surveillance Workshop, ed. K.P. Schwan (Lincoln Laboratory, M.I.T.), p. 147, "Prospects for Observing SpaceDebriswith SolarCoronagraphs"

Nesme-Ribes, E., Ferreira, E.N., Mein, P. 1993, A&A, 274, p. 563, "Solar Dynamics Over Solar Cycle 21 Using Sunspots as Tracers"

November, L.J. 1994, 13th Sacramento Peak Summer Workshop, ed. R.R. Radick, "Local-Coherence Averaging for Nonisoplanatic Imaging" November, L.J. 1994, SPIE 2010, ed. S.Fineschi, p. 192, "Design of Precise Uluaviolet Imaging Polarimeters that Rely on In Situ Calibration"

Pation, J., et al. 1993, GONG 1992: Seismic Investigation of the Sun and Stars, ed. T. Brown (Asuonomical Society of the Pacific),p. 437, "RingDiagram Analysis of Mt.Wilson Data"

Penn, M.J., Kuhn, J.R. 1994, Sol. Phys., 151, p. 51, "How Bright is the [Si-X] 1431 nm Coronal Emission Line?"

Penn, M.J., LaBonte, B.J. 1993, ApJ, 415, p. 383, "The Source of Five-Minute Period Photospheric Umbral Oscillations"

Pillet, V.M., et al. 1994, ApJ, 425, LI 13, "Evidence for Supersonic Downflows in the Photosphere of a Delta Sunspot"

Prasad, C.V., Bemath, P.F. 1994, ApJ, 426, p. 812, "Fourier Transform Specuoscopy of the Swan (d 3) System of the Jet-Cooled C2 Molecule"

Quatieri,T.F., Dunn, R.B., Hanna, T.E. 1994,ICASSP "Scale Modification of Complex Acoustic Signals"

Quinet, P., et al. 1993, Phys. Rev. A , 49, p. 2446, "New Energy Levels in Ar II"

Rabin, D.M. 1994, IAU Symposium 154, ed. D.M. Rabin, J.K. Jefferies (Kluwer),p. 449, "Near Infrared Imaging Magnetometry"

Ram, R.S., Bernath, P.F. 1994, J. Mol. SpecU., 165, p. 97, "Fourier Transform Emission Specuoscopy of the A'l+ -X'Z+System of YN"

Ram, R.S., Bemath, P.F. 1994, J. Opt. Soc. Am., 11, p. 225, "High-Resolution Fourier-Transform Emission Specuoscopy of the A4n-X4S" System of WN"

Randich, S., Giampapa, M.S., Pallavicini, R. 1993, A&A, 283, p. 893, "Lithium in RS CVn Binaries and Related Chromospherically ActiveStars. III. Northern RS CVn Systems"

Restaino, S.R., et al. 1993, SPIE 2019, Infrared Spaceborne Remote Sensing Workshop, ed. M.S. Scholl, p. 390, "Image Deconvolution from Pupil Masking Experiment"

Restaino, S.R., Radick, R.R., Loos, G.C. 1994, IAU Symposium 158, ed. J. Davis, R. Ekers, (Kluwer), p. 370, "First Experimental Results from Pupil Masking on a Solar Telescope"

Restaino, S.R., et al. 1994, Applied Optics, 33, p. 4143, "A Validation of Interferomeuic Imaging from a Pupil Masking Experiment on a Solar Telescope"

Rhodes, E.J., et al. 1993, GONG 1992: Seismic Investigation of the Sun and Stars, ed. T. Brown (Asuonomical Society of thePacific), p. 477, "Plans for Mt. Wilson - Crimean Observatory High-Degree Helioscismology Network"

Rimmele, T., Kentischer, T., Wiborg, P.H. 1994, 13th Sacramento Peak Summer Workshop, ed. R.R. Radick, "High-Resolution Observations with the NSO/KIS Correlation Tracker" Rust, D.M. 1994, 13th Sacramento Peak Summer Workshop, ed. R.R. Radick, "A Biologically-Inspired Image Position Sensor"

Saar, S.H. 1994, IAUSymposium 154, ed. D.M. Rabin, J.K. Jefferies (Kluwer), p.437, "Infrared Measurements of Stellar Magnetic Fields"

Saar, S.H. 1994, IAU Symposium 154, ed. D.M. Rabin, J.K. Jefferies (Kluwer), p. 493, "New Infrared Measurements of Magnetic Fields on Cool Stars"

Salucci, G., et al. 1994, A&A, 285, p. 322, "The Height Dependence of Intensity and Velocity Structures in the Solar Photosphere"

Schmieder, B., et al. 1994, Sol. Phys., 150, p. 199, "Relationship Between Magnetic Field Evolution and Flaring Sites in AR 6659 in June 1991"

Schrijver, C.J., Harvey, K.L. 1994, Sol. Phys., 150, p. 1, "The Photospheric Magnetic Flux Budget" Simon, G.W. 1993, Encyclopedia of Asuonomy, 2nd Edition, ed. S.P. Parker, J.M. Pasachoff (McGraw-Hill), p. 448, "Supergranulation"

Simon, G.W., et al. 1994, Solar Surface Magnetism Workshop, ed. R.J. Rutten, C.J. Schrijver (Kluwer), p. 261, "Large-Scale Photospheric Motions: First Results from an Exffaordinary Eleven-Hour Granulation Observation" Simon, G.W., et al. 1994, Solar Magnetic Fields Symposium, ed. M. Schuessler, W. Schmidt (Cambridge Univ. Press), p. 276, "KinematicModelingof Magnetoconvection"

Singh, J„ Jain, S.K., Venkatakrishnan, P. 1994, ApJ, 150, p. 49, "Time Variability of the He I 10830 A Line Profile"

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