NATIONAL OPTICAL ASTRONOMY OBSERVATORIES
NATIONAL OPTICAL ASTRONOMY OBSERVATORIES
QUARTERLY REPORT
OCTOBER - DECEMBER 1995
July 16,1996
TABLE OF CONTENTS
I. INTRODUCTION 1
II. SCIENTIFIC HIGHLIGHTS 1
A. Cerro Tololo Inter-American Observatory 1
1. The Faintest Known White Dwarf 1 2. Evidence for a Black Hole in the X-ray Nova GRO J1655-40 2 3. The Stellar Metallicity Distribution in Omega Centauri 3
B. Kitt Peak National Observatory 3 1. Infrared Colors and Pre-Main-Sequence Evolution 3 2. Bargain Redshifts for Faint Galaxies 4 3. Weighing the Dwarf Spheroidal Companions to the Milky Way 5
C. National Solar Observatory 6 1. Fine Dark Threads and the Temperature of the Solar Corona 6 2. An Objective Test of Magnetic Shear as a Flare Predictor 7 3. Solar Particle Dynamics 7
D. US Gemini Program 8
m. PERSONNEL AND BUDGET STATISTICS, NOAO 9
A. Visiting Scientists 9
B. Hired 9 C. Completed Employment 9 D. Changed Status 9 E. Gemini 8-mTelescopes Project 10
F. Chilean Economic Statistics 10 G. NSFForeign Travel Fund 10
Appendices
Appendix A: Telescope Usage Statistics Appendix B: Observational Programs Appendix C: US Sites Safety Report
I. INTRODUCTION
This document covers scientific highlights and personnel changes for the period 1 October - 31 December 1995. Highlights emphasize concluded projects rather than work in progress. The March 1996 NOAO Newsletter Number 45 contains information on major projects, new instrumentation, and operations. The appendices to this report summarize telescope usagestatistics and observational programs.
II. SCIENTIFIC HIGHLIGHTS
A. Cerro Tololo Inter-American Observatory
1. The Faintest Known White Dwarf
The white dwarf luminosity function incorporates information on the age and star formation history of the Galactic disk which is independent of other techniques. In particular, the least luminous white dwarfs set lower limits on the disk age, and thus the age of the Universe. The faintest known white dwarfs have Mv ~ 16.2. Age estimates for these stars are in the range 6.5-11 Gyr, with the variation largely due to uncertainty in the core composition. The white dwarf luminosity function declines abruptly at this absolute magnitude, and this decline has been interpreted as beingdue to the age of the Galactic disk. The question remains, do even less luminous and older white dwarfs—however rare—exist? The search for very low luminosity white dwarfs is still very active.
A concerted effort has been carried out for a number of years by Maria Teresa Ruiz and her colleagues at Cerro Calan Observatory (U. of Chile). Selection of promising candidates is done with a classic technique, blinking plate pairs from the ESO Schmidt telescope to identify faint stars with substantial proper motion. The magnitude limit is about mR ~ 21 and motions as small as 0.1 arcsec yr"1 are detectable with a few years' time base. Followup observations at CTIO and other facilities in Chile help winnow the most interesting objects out of the hundreds found on a plate pair.
One such object is the cold DC type white dwarf ESO 439-26. Following its initial discovery in 1988, preliminary spectroscopic and astrometric data suggested it to be of very low luminosity. Several years' subsequent investigation at CTIO have now established this definitively. This result is based on another classic technique, the determination of trigonometric parallax, applied with modern CCD detectors in a program led by Claudio Anguita (U. of Chile). Observations were carried out on the CTIO 1.5-m telescope overa five-year period, using initially a 312 x 508 RCA CCDand morerecently a Tek IK device. With 0.3 arcsec pixels and seeing at 1.2 arcsec or better, 40 frames yield a parallax of 0.024± 0.003 arcsec, or Mv = 17.4—more than one magnitude fainter than the faintest previously known white dwarfs. The existence of such an extreme low-luminosity white dwarf may imply a very large value for the age of the local Galactic disk.
Alternatively, the low luminosity of ESO439-26 couldbe accounted for if it is a massive whitedwarfwith a correspondingly small radius—also a rare beast, but not one implying greatage. Onlya detailed comparison of the observed absolute flux distribution with theoretical models can resolve the ambiguity. Ruiz and Anguita, together withS. K. Leggett (IRTF) and P. Bergeron (U. of Montreal), haveused BVRIphotometry obtained on the CTIO 1.5-m and 0.9-m telescopes and model atmosphere calculations by Bergeron and colleagues to make this comparison. They find the high mass interpretation to be the correct one, independent of details of atmospheric composition. The best fit to the photometiy gives Teff=4560 K, log g = 9.0, and M= 1.2 M solar masses—twice that of a typical white dwarf. Comparison with carbon core evolutionary models yields an upper age limit of 6.4 Gyr for the best fit solution. More complex interiors models would tend to reduce the age significantly, but are not yet available at appropriately cool temperatures.
Infrared JHK photometry, in progress, will help constrain the atmospheric composition. Interestingly, spectroscopy does not. Even though Ha can be detected in low mass white dwarfs of comparable effective temperature, the large surface gravity of this small, massive object collisionally broadens hydrogen lines to the level of undetectability. Although not of great age, the high mass of ESO 439-26 makes it unique in one respect. Comparison withmodel isochrones indicate it is in an advanced stateof crystallization.
2. Evidence for a Black Hole in the X-ray Nova GRO J1655-40
X-ray novae are binary systems in which a compact object accretes gas from a companion star. The observed velocity of the secondary starcan be used to determine the minimum mass of thecompact object. In six cases to date, the mass function of the compact object has been found to exceed 3 solar masses, confirming thepresence of black holes in these systems. These black hole X-ray novae (orBHXNs) provide a unique opportunity to study black holes, since one can observe both thesecondary starvia the absorption lines and the accretion disk surrounding the black hole via the emission lines.
The unusual X-ray nova GRO J1655-40 is the newest and one of the most interesting of the BHXNs. Following its discovery in August 1994 by the Compton Gamma-Ray Observatory, Charles Bailyn (Yale U.) and collaborators located the optical counterpart using the CTIO 0.9-m telescope. Soon after, superluminal radio jets were discovered by Tingay et al. (1995, Nature, 374, 141) and Hjellming et al. (1995, Nature, 375, 464), making GRO J1655-40 the only galactic superluminal source which can be observed optically. The jet ejection, at 92% of the speed of light, appears to be episodic and asymmetric, and is so rapid that distinct motions can be seen from one hour to the next.
Bailyn and collaborators returned to CTIO in 1995 to make further optical photometric and spectroscopic measurements of GRO J1655-40. Photometry was obtained on 18-25 March and 5-24 April with the 0.9-m telescope and CCD imager, and on 28 March to 2 April with the CTIO 1.5-m telescope and CCD imager. In addition, spectra were obtained with the RC spectrograph on the CTIO 4-m telescope on the nights of 30 April and 2-4 May. As the photometric data were obtained, it became clear that the light curve showed eclipses and was periodic on a timescale of approximately three days. The overall light curve shape was found to consist of a broad triangular primary minimum, and a shorter secondary minimum displaced by about 0.5 in phase from the primary minimum. By analogy with the eclipsing X-ray binary CAL87, it seems likely that aneclipse of a large accretion disk by the secondary staris responsible for theprimary minimum, and an eclipse of the secondary star by the disk explains the secondaryminimum.
The spectra of GRO J1655-40 obtained by Bailyn et al. had less prominent Balmer emission lines and stronger high-excitation lines than X-ray novae in quiescence, presumably because the outburst was still underway. Nevertheless, it became immediately apparent from the individual spectra that a stellar F-type absorption spectrum was present. Cross-correlating the spectra against an F5 subgiant of known radial velocity revealed sinusoidal radial velocity variations with a period of 2.6days and a semi-amplitude of 227 km s"1. These parameters yield a minimum possible mass of the compact object of 3.16 ±0.15 solar masses. The maximum stable mass of a neutron star is 3 solarmasses for all possible equations of state, and below 2.5 solar masses for most plausible equations of state. Thus, in the absence of exotic matter and/or non-Einsteinian gravity, a mass function above 3 solarmasses requires thecompact object in GRO J1655-40 to be a black hole. The eclipsing geometry of GRO J1655-40 allows the possibility of using eclipse mapping techniques to explore the geometry of the system in further detail. Changes in the flux and spectral line shape during eclipse can be used to map the inner regions of the accretion disk. Hence, a multiwavelength campaign involving GRO, ROSAT, ASCA, XTE, and a variety of ground-based optical and radio observations (including 0.9-m time at CTIO) was organized for March 1996. One of the primary goals of this campaign was to use the eclipses to map the high-energy, optical, and radio emission. When successful, these observations allow the emission geometry near an accreting, jet-producing black hole to be explored in unprecendented detail.
3. The Stellar Metallicity Distribution in Omega Centauri
Suntzeff (CTIO) and Kraft (UCO/Lick) have finished a project on stellar abundances and radial velocities for giant stars in the Galactic globular cluster co Centauri based on the Call infrared triplet. Two samples of stars were observed: 234 stars at Mv ~+ 1.25 on the lower giant branch at radial distances between 8' and 23', and 145 stars at Mv — 1.3 at radial distances between 3' and 22'. They found 199 and 144 radial velocity members, respectively, in the two samples. These samples were corrected for evolutionary effects to provide an unbiased distribution of the underlying stellar metallicity. They found a mean cluster velocity of
Previous metallicity studies found a non-gaussian metallicity distribution containing a tail of metal-rich stars. Suntzeff and Kraft have confirmed these results except that the unbiased cluster metallicity distributions were found to be significantly narrower. The abundance distributions contain the following key features: (1) No very metal-poor stars, (2) a sudden rise in the metal-poor distribution to a modal [Fe/H] value of -1.70 consistent with a homogeneous metallicity unresolved at the 0.07 dex level, (3) a tail to higher metallicities with more stars than predicted by simple chemical evolution models, and (4) a weak correlation between metallicity and radius such that the most metal-rich stars are concentrated to the cluster core. The unresolved metal-weak tail implies that the gas out of which co Cen formed was well-mixed up to the modal metallicity of the cluster. Therefore, co Cen like other Galactic globular clusters, seems to have formed in a pre-enriched and homogenized (up to the modal metallicity) environment.
The existence of a weak metallicity gradient supports the idea that co Cen self-enriched, with the enriched gas sinkingto the cluster center due to gas dissipation processes. Suntzeffand Kraft also note, however, that the metal-rich stars are more massive than the bulk of the stars in the cluster, and could also have sunk to the center by dynamical mass segregation over the lifetime of the cluster.
B. Kitt Peak National Observatory
1. Infrared Colors and Pre-Main-Sequence Evolution
The picture of star formation from core ignition until arrival on the main sequence is gradually taking shape as more sophisticated theory is confronted with increasingly informative observations. The general picture envisions several stages in the pre-main-sequence phase. The star may begin life while heavily enshrouded in dust during a period of maximum mass accretion and ejection. As the shroud is cleared away, the system shows strong excess emission in the ultraviolet and in emission lines from the accretion disk and associated materials, along with a continuing infrared excess from hot dust. The stage immediately preceding the main sequence shows a decreased infrared emission and the fading of the material producing the thermal disk and emission lines.
A substantial multi-wavelength survey reported by S.J. Kenyon and L. Hartmann (Smithsonian Astrophysical Obs.) in the November 1995, Astrophysical Journal Supplements confirms the general picture of pre-main-sequence evolution. They combined observations of the Taurus-Auriga molecular cloud region from several telescopes, including the IRAS satellite, and the KPNO 1.3-m with the near-IR photometer, Imager, and SQITD four-color imager. More than half the stars in the region show excess near-IR emission, and that emission correlates with other measures of activity, such as atomic hydrogen emission, ultraviolet excess, millimeter continuum emission, reflection nebulae and molecular outflows. The fraction of the total energy of a pre-main-sequence staremitted in the far infrared shows a smoothly decreasing progression from the most heavily embedded stars to the bluest accretion-disk objects with high rates of mass flow. Since the ER colors are consistent with an Mailing dusty envelope model, the amount of envelope emission must decrease as the star develops.
A gap in the mid-infrared diagram of stellar colors suggests that there is an abrupt transition from the phase of strong accretion mass flow producing a thick accretion disk to that of weaker flow with a thin disk. The distribution of inferred disk energy distributions is consistent with flared disks rather than geometrically flat ones. The Hertzsprung Russell Diagram and the derived luminosity function in the near-infrared 1.0 \x.m and 2.2 |^m bands indicate that the molecular cloud complex has formed stars steadily over the past 1 to 2 million years. A comparison of the prediction of theoretical evolutionary tracks with the observed locations of objects in the near-infrared color-magnitude diagram allow inferences about the initial mass function (IMF). That relative distribution of masses is more like an empirically constructed IMF for the solar neighborhood by Miller and Scalo than a pure power-law in mass formulated by Salpeter. There seems to be littleevidence for evolution in the total luminous output of sources as they move from dust-enshrouded to exposed high accretion rate objects. The last finding contradicts theoretical expectations, and enforces the concept ofprogress in understanding.
2. Bargain Redshifts for Faint Galaxies
Deep images of the sky present large numbers of very faint galaxies, which hold the key to defining the evolutionary history of each modern galaxy type. Even the largest telescopes cannot obtain detailed spectra of the faintest objects, and very large amounts of time must be committed to redshift surveys to trace large-scale structures at substantial redshifts. These difficulties have continually motivated astronomers to find a way to determine redshifts from the much lower resolution measurement of spectral energy distributions provided by broad-band photometry.
A recent mathematical exploration of a promising technique was described in the December 1995, Astronomical Journal by A. Connolly, I. Csabai, and A. Szalay (Johns Hopkins U.), D. Koo (UCSC), R. Kron (Fermilab), and J. Munn (U. Chicago). They had measured a large sample of galaxies from their photographic survey taken over years on the Kitt Peak Mayall 4-metertelescope. Plates had been taken in ultraviolet (U), blue (Bj), red (RF), and near-infrared (IN). The first question is the amount of independent information contained in the fluxes recorded in the different colors, and how that information can be correlated with spectroscopically measured redshifts. They used a measure of that information, the fractal dimensionality, to show that galaxies occupy roughly a two-dimensional planar surface in four- dimensional color space, that slowly twists with increasing redshift. The position of a galaxy within that space is determinedby its redshift, luminosity and spectral type. The authors then devised combinations of the brightness measurements through the color filters, essentially rotating the coordinate frame to better align with this surface of galaxy measurements. They were able to define a set of four orthogonal coordinates: the first correlates with redshift, the second with flux, the third with spectral energy distribution, and the fourth is normal to the "plane" of galaxies. The existence of a data plane is consistent with yet a third type of analysis, principal component analysis, which reveals the variables that contain most of the correlated power. The first component contains 98% of the power, the second 2%, and the third 0.04%. When the principal component directions in multi color space are compared to the orthogonal components derived to maximize the dependence on single physical variables, the agreement was found to be very good. The first component corresponded to flux, the second correlated most strongly with redshift, and the third with spectral energy distribution shape.
With this mathematical construction in place, it was possible to test the accuracy with which redshifts could be determined from a slightly curved (quadratic) representation of the data surface in galaxy multicolor space. The authors found that they could estimate redshifts to an accuracy of 0.05 for blue magnitudes brighter than 22.5 from the combined color measurements alone. Experiments with exclusion of various passbands confirmed that the blanketing break that produces the depression of the spectral energy distribution at wavelengths shorter than 4000A provides most of the power in the redshift determination.
The authors then used model spectral energy distributions and simulated counts with lower measurement uncertainties than those provided by the photographic data to suggest that the redshift uncertainty could be decreased to as low as 0.02. The ultimate limit is the "warping" of the data plane as the weak-featured near-ultraviolet energy distribution occupies more of the optical passband at higher redshifts. With the assumption of no evolution, that limit occurs at z ~ 0.8. The combination of that effect and galaxy color evolution will provide the ultimate limits to the technique until evolutionary sequences are very well defined. For lower redshift systems, the technique is powerful in assigning redshifts for large, faint samples of galaxies.
3. Weighing the Dwarf Spheroidal Companions to the Milky Way
The puzzle of Dark Matter has long been manifest in the dwarf spheroidal galaxies in the Local Group. Early measurements of the velocities of a few stars in each galaxy suggested that there was a considerable unseen mass producing the apparent velocity dispersion. The results remained open to question because of three concerns: were the uncertainties quoted for the velocities of individual stars reliable? Did the velocities reflect a large contribution from the orbital motion of binary stars? Were dynamical conditions in the galaxies appropriate for the application of the virial theorem of energy equilibrium as a valid means for deriving total gravitational mass?
The advent of multifiber spectroscopy enabled a new global attack on the velocity dispersion problem. T.E. Armandroff (KPNO), E.W. Olszewski (U. of Arizona), and C. Pryor (Rutgers U.) report in the November 1995, Astronomical Journal on their measurements of individual stellar velocities in the Draco and Ursa Minor Dwarf Spheroidal galaxies. They used the Hydra multifiber positioner and bench spectrograph on the KPNO Mayall 4-meter telescope to measure velocities in 762 stellar spectra of 94 stars in Ursa Minor, 91 stars in Draco and many foreground objects. They took extreme care in calibration and in error simulation to determine the median uncertainty in individual velocity measurements of 4 km/s. The stability of the Hydra - bench spectrograph combination was clearly demonstrated in the year-to-year repeatability of the measurements. Binary stars were straightforwardly identified in the repeated measurements. The authors were also able to obtain detailed comparisons with systematics of previously published velocities of other groups. Armandroff et al. found that the distribution of velocity members of the Ursa Minor and Draco dwarf spheroidals was not as modeled by a simple isothermal distribution. They found that about two times more stars were found outside the ellipses predicted to contain 90% of the population than predicted by the model. A possible explanation is that the radius at which the Milky Way truncates the population of the satellite galaxy, the tidal radius, has been calculated to be too small, and that the stellar distribution is telling us more about the dynamics of the tidal encounter.
Theoriginal stellarvelocity probes were chosen to be Carbon Stars, because of the strong velocity signal from their sharp carbon absorption bands. The new velocity survey allowed discovery of additional members of this population and allowed an inference about their nature. Since the bulk of the Carbon Stars in Ursa Minor and Draco are significantly less luminous than stars at the tip of the red giant branch in the Hertzsprung-Russell diagram, they cannot be the products of dredging up carbon in intermediate- mass single-stars. They must be the result of the transfer of material in binaries.
The major finding is that of the dynamics of the galaxies. Ursa Minor shows a slow rotation of about 3 km/s, while Draco shows no evidence of rotation. The velocity dispersion in Ursa Minor is 10.4 ± 0.9 km/s, while that of Draco is 10.7 ± 0.9 km/s. If extreme velocity objects are excluded, the values drop to 8.8 ± 0.8 and 8.5 ± 0.7 km/s, respectively. Simple dynamical models predictcorresponding mass to light ratios between about 60 and 90. These are the largest valuesfor any measured dwarf spheroidals, and are much larger than those found for any star cluster or the old stellar population of any luminous galaxy. The result confirms and provides strengthened evidence for the presence of dark matter as providing much of the gravitational potential of these dwarf spheroidal systems. Further work on the spatial distribution of the dark matter will provide another step toward unraveling its enigmatic role in galaxy formation.
C. National Solar Observatory
1. Fine Dark Threads and the Temperature of the Solar Corona
L. November (NSO) and S. Koutchmy (Institute of Astrophysics, Paris, France) have identified very fine "dark and bright threads" in the solar corona from high spatial resolution, white-light coronal observations obtained during the eclipse of 11 July 1991, using the 3.6-meter Canada-France-Hawaii Telescope on Mauna Kea in Hawaii. These are the highest resolution observations of the solar corona ever made because of the unique opportunity of observing the totally eclipsed Sun with a large-aperture telescope. After dividing out the average radial variation from the white-light photographic observations, relatively dark and bright fine threads can be identified. Spatial filtering reveals clearly the thread-like loop structures, which are as small as 1 arcsec or 720 km. The main feature is an "arcade" of concentric dark and bright threads which extends above a small prominence just above the solar limb. The threads appear to be unchanging, though the time series is too short to get a good determination of their lifetimes.
The relative electron density depletion required to explain the observed dark-thread contrast, assuming that they are isolated, cylindrically symmetric structures, is found to be 100%, which indicates that the fine dark threads are fully evacuated. Only an unphysically large temperature enhancement could produce the degree of evacuation that is measured in the dark threads, and a temperature one half the ambient is required to produce the density enhancements seen in the bright threads. But the scale-height temperature in the bright threads is found to be within 15% of the ambient. On the other hand, pressure fluctuations necessary to produce the measured density fluctuations are produced by an approximately 1-gauss non-force-free magnetic field. Such a picture is consistent, as the threads appear to follow the 6 magnetic field. Dark and bright threads appear to have a preferential organization, probably lying on current sheets that separate normal potential magnetic regions, which is consistent with a widely-held theoretical model for the solar coronal magnetic field.
The most significant aspect of the discovery of dark threads may be that steady non-force-free magnetic fields can play a direct role in defining the coronal temperature structure. If evacuated threads exist within a few arcseconds of the solar surface, then forces that constrain their expansion radially would also impose a constant pressure region and a corresponding sharp radial density drop at the level where the magnetic energy density in the threads becomes comparable to the surrounding gas pressure, effectively acting to "hold down" the whole surrounding solar atmosphere. Such a sharp radial density drop would produce, according to thermodynamic arguments, a corresponding temperature discontinuity which can lead to a very hot corona. This is an attractive possibility, as it avoids the difficulties encountered in traditional models that have been generally unsuccessful in providing the necessary direct heating to explain the 1-5 million degree coronal temperature.
2. An Objective Test of Magnetic Shear as a Flare Predictor
D. Neidig (PL/GPSS, stationed at NSO/Sac Peak), in collaboration with J.B. Smith and members of the NASA Marshall Space Flight Center magnetograph group, completed a preliminary study of magnetic shear as a flare predictor. The study was based on a statistical analysis and classification of 57 active- region-days, using Multivariate Discriminant Analysis (MVDA) as an objective means of deriving relationships between preflare variables and flare outcomes. A total of 51 preflare variables, including 23 based on shear (defined as the angular deviation of the active region magnetic field from a potential field) were used in the analysis. Classifications of flare outcomes were derived both with and without incorporation of variables based on shear. It was found that variables based on shear and on the strength of the transverse magnetic field, while they were able to classify tomorrow's flare outcomes as well as or better than conventional region indices or variables based on longitudinal fields, did not produce improved classification scores when used in combination with the remaining variables. As in previous studies using MVDA, past and present flare activity, i.e., persistence, was found to be the most significant variable in classifying tomorrow's flare activity. Further, when persistence was used in addition to other variables, absolutely no reduction in classification scores was observed when the shear variables were removed. These somewhat surprising results should be considered as preliminary, as the sample was relatively small and did not include large (X-class) flares. Further studies, using a larger sample and including large flares, are under consideration. The results of this study were presented at the Sixteenth NSO/Sac Peak International Workshop, "Solar Drivers of Interplanetary and Terrestrial Disturbances."
3. Solar Particle Dynamics
Two major mysteries of the Sun involve the dynamics of the upper solar atmosphere. The solar wind, a particle flow with a speed of 400-1000 km/sec, is accelerated somewhere in the solar atmosphere by a process that remains unobserved. Solar flares, events that have direct terrestrial consequences, involve reconfigurations of the magnetic fields of the solar atmosphere; and yet direct measurements of the magnetic field changes in solar flares have not been made. New observations in the near-infrared spectrum of the Sun aim to address these mysteries. Several important absorption lines are now being observed in the 1000-2000 nm region of the solar spectrum, and new information about solar physics is being squeezed from the data. Daily observations of the solar disk in the Helium I absorption line at 1083 nm at the NSO/KP Vacuum Telescope provide the only ground-based measurement of coronal holes. The 1083-nm line is formed after photo-ionized helium recombines with free electrons, and in a coronal hole there is less X-ray radiation to ionize helium atoms, and thus less 1083-nm absorption. The daily 1083-nm maps show the position and extent of coronal holes on the Sun, and when combined with solar wind observations, prove that the fast streams of the solar wind originate in coronal holes. New observations from the NSO/KP Vacuum Telescope by M. Penn and H. Jones (Goddard SpaceFlightCenter, stationed at NSO) have also shown that the 1083-nm line widths in coronal holes differ from the surrounding quiet-Sun regions. The narrower line widths they observe in the coronal holes may reflect a thermal difference or may be caused by a change in velocities of gas flow.
The magnetic field in the solar atmosphere can be probed by measuring the polarization of the 1083-nm helium line. Observations by Penn and Kuhn at the NSO/SP Vacuum Tower Telescope measured magnetic fields in the hot emission kernels of a small flare in 1993. These data illustrated the events in the later stages of the flare, but lacked the valuable pre-flare observations that a dedicated instrument can obtain. For this purpose, a new video-rate filtergraph/magnetograph, using the 1083-nm line, is almost on-line at the NSO/KP Vacuum Telescope. Jones, Harvey and Penn are now working on this instrument, which will measure the 1083-nm polarization in solar active regions in a systematic way, obtaining important pre-flare measurements for all events. The exploitation of the 1083-nm polarization by this instrument will be a valuable tool in the study of solar flares during the next solar activity cycle beginning around 1997.
D. US Gemini Program
The US Gemini Program is a division of NOAO which serves as a liaison between the US community and the international Gemini Project. Personnel in this office include Todd Boroson, the US Gemini Project Scientist, Kathy Wood, Technical Administrator, and Mark Trueblood, Project Engineer. Efforts began this quarter to hire another astronomer into the USGP to assist with the development and implementation of operations and instrumentation activities.
This quarter saw the completion of the first Gemini mirror blank at the Corning plant in Canton, New York. The blank was delivered on schedule and has been transported to Reosc Optique in France for polishing. The hexagonal segments for the second blank arecomplete and will be fused in early 1996.
Excavation and concrete work has proceeded on schedule at both north and south Gemini sites. The USGP collaborated with IGP personnel in the placement of a video camera, mounted on a railing of the nearby Canada-France-Hawaii Telescope, that continuously views the Gemini construction on Mauna Kea. Images from this camera are transmitted back to Tucson and can be viewed on the World-Wide Web at the Gemini website.
The USGP organized andcarried out a successful Gemini workshop at the VHI Latin American Regional Astronomy Meeting in Montevideo, Uruguay. This was done in collaboration with the national Gemini Project offices of the South American Gemini partners, Argentina, Brazil, and Chile. In addition to general participation in the meeting by the USGP staff, some IGP personnel, and some US members of the Gemini Board, a two-hour session on Gemini was presented to the 300 Latin American astronomers at the meeting. This session comprised three short presentations on different aspects of the Gemini program followed by a lively question and answer session. During this quarter, the USGP devised a procurement plan for the Gemini Mid-IR Imager. The procurement will involve two competitive selections, the first to produce a concept, and the second to complete the design and fabricate the instrument. This two-stage approach is motivated by the limited funding available initially and by the desire to facilitate participation by a number of instrument groups. The announcement of opportunity for the first competition was released at the end of the quarter.
IV. PERSONNEL AND BUDGET STATISTICS, NOAO
A. Visiting Scientists (visitors who arrived this quarter for a stay of one month or more).
NOAO Facility Arrived Name Institution Visited 02/14/95 Duflia de Mello U. de Sao Paulo CTIO 11/1/95 H. M. Antia Tata institute of Fur NSO/Tucson 12/18/95 Jinghao Sun Beijing Astronomic NSO/Tucson
B. Hired
Date Name Position NOAO Division 10/9/95 John Varsik Research Associate NSO/Sunspot 10/9/95 Dan Vukobratovich Senior Engineer NOAO 10/27/95 Arjun Dey Research Associate KPNO
C. Completed Employment
Date Name Position NOAO Division 11/17/95 Stephane Chariot Research Associate KPNO 11/30/95 David Crawford Astronomer/Tenure KPNO 12/19/95 Paola Sartoretti Research Associate KPNO 12/30/95 Hector Duarte Main. Man. 4 CTIO-Santiago 12/31/95 Helmut Abt Astronomer/Tenure KPNO 12/31/95 Lloyd Wallace Astronomer/Tenure KPNO 12/31/95 Jack Zirker Astronomer/Tenure NSO/Sunspot
D. Changed Status
Date Name Position NOAO Division 10/1/95 Jay Elias Promotion from Associate Astronomer/Tenure CTIO to Astronomer/Tenure 10/1/95 Richard Elston Promotion from Assistant Astronomer CTIO to Associate Astronomer 10/1/95 Tod Lauer Promotion from Assistant Astronomer KPNO to Associate Astronomer 10/1/95 Philip Massey Promotion from Assistant Astronomer/ KPNO Tenure to Astronomer/Tenure 10/1/95 Alistair Walker Promotion from Associate Astronomer/ CTIO Tenure to Astronomer/Tenure 12/1/95 Fred Gillett Promotion and transfer from Astronomer/Tenure NOAO to 8-m Project Scientist
E. Gemini 8-m Telescopes Project
Changed Status
Date Name Position 12/1/95 Fred Gillett Promotion and transfer from NOAO Astronomer/Tenure to 8-m Project Scientist
F. Chilean Economic Statistics FY 1996
%Change Cum. Change Avr. monthly Month inCPI in CPI Pesos/Dollars October 0.8 0.8 414.15 November 0.1 0.8 415.14 December 0.3 1.1 407.02
G. NSF Foreign Travel Fund
For the quarter 1 October through 31 December 1995, a total of $4,503.90 was paid out of the NSF Foreign Travel account for visits to the following site and institutions:
Anglo-Australian Telescope, Mt. Stromlo and Siding Spring Observatory, Australia Las Campanas Observatory, OCIW, Chile
10 APPENDIX A
Telescope Usage Statistics
October - December 1995
Astronomical Observations Scheduled Maintenance,
Hours Used Hours Lost Instrument Tests,
Hours Visitors Staff Weather Equipment Equipment Changes,
Telescope Scheduled Engineering, etc.
4-m 899.6 587.4 107.2 63.7 32.7 108.6
1.5-m 885.4 670.1 51.8 83.5 8.0 72.0
1-m 607.1 338.5 101.1 122.7 2.5 42.3
CTIO 0.9-m 875.6 697.2 5.0 96.4 12.0 65.0
*0.6/0.9-m 656.0 509.4 27.0 76.4 2.7 40.5
0.6-m 145.5 83.5 0.0 46.5 7.5 8.0
4-m 363.5 205.89 98.11 24.0 24.0 11.0
2.1-m 996.5 702.29 52.21 171.0 30.5 40.5
Coude Feed 1019.5 715.27 113.73 165.75 13.75 11.0
KPNO 1.3-m C L O S E D
0.9-m 941.7 546.26 138.19 234.0 14.25 9.0
Schmidt 404.5 319.0 0.0 81.5 4.0 0.0
Evans Facility 1149.0 339.0 408.0 288.0 46.0 68.0
**FTS Lab 162.0 45.0 111.0 0.0 6.0 0.0
Hilltop Dome 1580.0 0.0 1163.0 348.0 11.0 58.0
NSO * *McMath-Pierce 1664.2 909.0 323.2 331.5 100.5 0.0
Vacuum/KP 790.0 312.0 266.0 158.0 0.0 54.0
Vac. Tower/SP 598.25 0.0 342.5 238.75 17.0 0.0
Note: Scheduled hours are calculated according to the ephemerides for CTIO:
October 9.9 hours/night; November 8.9 hours/night; December 8.2 hours/night.
* Use restricted to dark of the moon. ** Totals include both day and night hours. All others are day only.
APPENDIX B
CERRO TOLOLO INTER-AMERICAN OBSERVATORY
October - November - December 1995: Individual Telescope Assignments are listed below. Graduate students are indicated by an asterisk after their names. Nights assigned (hours worked), and telescope used are indicated. Service Observing programs are denoted by S.O. instead of nights assigned. A total of 67 programs were carried out during this quarter.
T. Barnes III (U. of Texas), T. Moffett (Purdue U.), R. Luck (Case West. Res. U.), W. Gieren (U. Catolica de Chile): "Cepheid Metallicities in the LMC/SMC." 3(32)4-m
F. Barrientos*, S. Lilly (U. of Toronto, Canada): "Precision Photometry of Early Type Galaxies in High Redshift Clusters." 3(26)4-m
D. Bomans, S. Points*, Y. Chu (U. of Illinois): "Self Propagating Star Formation in Supergiant Shells." 5(50)0.9-m
H. Bond (STScI): "Post-AGB Stars in the Magellanic Clouds as Standard Candles." 5(43)1.5-m
L. Campusano, E. Hardy (U. de Chile): "Search for Galaxy Group at z = 0.074." l(9)0.9-m
M. Corbin (KPNO), T. Boroson (U.S. Gemini Project Office): "Spectrophotometry of Low-Redshift Quasars." 2(18)1.5-m
E. Costa, P. Loyola (U. de Chile): "Towards the Definition of a Unified Radio/Optical Reference Frame. CCD Astrometry of Benchmark Compact Extragalactic Radio Sources." 4(33) 1.5-m
N. Craig, J. Dupuis, C. Christian, M. Mathioudakis (U. of California, Berkeley): "The EUVE Optical Identification Campaign II: Southern Sources." 4(35) 1.5-m
S. Demers (U. de Montreal, Canada), M. Mateo (U. of Michigan), W. Kunkel (Las Campanas Obs): "The RR Lyraes as a Probe to the Oldest Population of Fornax." 5(38)1.5-m
D. DePoy (Ohio State U.), J. Elias (CTIO), R. Probst (KPNO): "Infrared Spectroscopy of Protostar Candidates in the LMC." 4(24)4-m
J. Elias, R. Elston (CTIO), P. Seitzer (U. of Michigan): "Near-Infrared Standards for Large Telescopes." 7(58)l-m
P. Fischer (AT&T Bell Labs), K. Gebhardt (U. of Michigan), C. Pryor, T. Williams (Rutgers U.): "Dynamical Mass Functions of Young LMC Clusters." 5(44)4-m
G. Fontaine, F. Wesemael, R. Lamontagne, S. Demers (U. de Montreal, Canada): "Spectroscopy of Blue Subluminous Objects in the MCT Survey." 5(47)1.5-m J. Frogel, A. Quillen, R. Pogge, D. DePoy, D.Terndrup, K. Sellgren (Ohio StateU.), R. Davies (Durham U., UK): "A Multi-color Atlas of Galaxies: A Study of Structure andStellar Content: IR and Optical Surface Photometry." 7(55)1.5-m, 7(56)0.9-m
A. Fruchter, J. Morse (STScI), R. Romani (Stanford U.): "Imaging Spectrophotometry of the Nebula about PSRJ0437-4715."2(10)4-m
K. Gebhardt (U. of Michigan), P. Palunas*, B. Weiner*, T. Williams (Rutgers U.): "Dynamics of Moderate Redshift Clusters of Galaxies." 3(23)4-m
D. Geisler (KPNO), T. Bridges (Royal Greenwich Obs., UK), J. Forte (Obs. La Plata, Argentina), C. Pritchet (U. of Victoria, Canada): "Kinematics and Metallicities of Globular Clusters in NGC 1399." 3(22)4-m M. Gregg (Lawrence Livermore Nat. Lab.), M. Drinkwater (Anglo-Australian Obs., Australia): "Multicolor Imaging Survey of the Fornax Cluster of Galaxies." 6(53)CS
P. Guhathakurta (U. of California, Sta. Cruz), R. Cutri, J. Bernard (California Inst, of Technology, IPAC), F. Boulanger (Inst. d'Ap. Spatiale, France): "Wide Field Optical Imaging of theInfrared Cirrus: Probing the Properties of Interstellar Dust." 4(31)CS
P. Hartigan, C. O'Dell (Rice U.), J. Morse (STScI): "Dynamicsof the OrionNebula."4(36)1.5-m
K. Johnston, N. Zacharias, M. Zacharias (US Naval Obs.), C. de Vegt (U. of Hamburg, Germany): "StructureAnalysisand PrecisePositionsof Extragalactic Reference Frame Sources." 2(14)4-m
M. Joner (BrighamYoung U.): "StandardFields for BVRI CCD Photometry." 7(77)0.9-m
M. Joner (Brigham Young U.), C. Kim (Chonbuk Nat. U., Korea): "Stromgren-(3-Ca Photometry of SX Phoenicis Stars." 15(73)l-m
M. Keane (CTIO): "Bright Quasars Behind the Magellanic Clouds." 3(27)CS
S. Kepler, O. Giovannini* (UFRGS, Brazil): "TheInstability Strip Limits of ZZCeti Stars." 5(48)1.5-m
R. Lamontagne, S. Demers,F. Wesemael, G. Fontaine (U. de Montreal, Canada): "PhotometricCalibration of the Montreal-Cambridge-Tololo Survey Fields." 4(16)0.9-m
A. Landolt(Louisiana State U.): "UBVRI Photometry of Standard and Variable Stars."7(47)1-m
A. Leonardi*, J. Rose (U. of North Carolina): "A New Method of Age-Dating Post-Starburst Events." 5(47)1.5-m
P. Lu (Western Connecticut StateU.), W. Tsay (National Central U., Taiwan): "Continuing the Spectral and Photometric Studies of F and G Stars at SGP." 7(38)0.9-m, 4(31)CS
J. Maza, X. Gomez, M. Wischnjewsky (U. de Chile): "UBVRI Photometry of Calan-Tololo Seyfert Galaxies." 3(32)0.9-m
J. Maza(U. de Chile): "Spectroscopy of Calan-Tololo QuasarCandidates." 3(1 l)4-m A. Moffat, N. St-Louis, J. Bertrand* (U. de Montreal, Canada), N. Walborn (STScI): "Measuring the Masses of the Most Massive Stars." 2(17)4-m, 8(62)0.9-m
P. Morris, P. Conti (U. of Colorado), P. Eenens (Inst. Nac. de Astrofisica, Optica y Electronica, Mexico), R. Schulte-Ladbeck (U. of Pittsburgh): "The Properties of Wolf-Rayet Star Winds Through Infrared Spectroscopy." 4(39)4-m
P. Ortiz, J. Maza (U. de Chile): "Extensive Search for Quasars with Redshift up to z = 5.0." 8(74)CS
S. Pak*, D. Jaffe (U. of Texas): "Extended Near-Infrared H2 Emission from the Magellanic Clouds." 7(47)1.5-m
S. Pak*, D. Jaffe (U. of Texas): "Large-Scale Near-Infrared H2 Emission from Nearby Gas-Rich Galaxies." 2(21)1.5-m
J. Patterson, J. Zimmerman, J. Kemp, R. Patino (Columbia U.): "Superhumps in Cataclysmic Variables." 20(119)l-m, 10(31)0.6-iti
S. Perlmutter, A. Kim*, G. Goldhaber, S. Duestua, M. Kim, L. Hook, R. Pain, D. Groom (Lawrence Berkeley Lab.), G. Bernstein (U. of Michigan), J. Willick (Carnegie Inst, of Washington): "Homogeneity and Rate of High-Redshift Supernovae with Three other Wide-Field Imaging Projects for Cosmology: Gravitational Lens Search, >1-Degree Galaxy Correlation Study, and Very High-Redshift QSO Survey." 5(48)4-m
M. Phillips, A. Walker, J. Elias, N. Suntzeff, M. Hamuy, M. Navarrete (CTIO), D. DePoy, M. Bautista* (Ohio State U.): "Observations of SN 1987A at Late Epochs." 3(26)4-m
S. Points*, Y. Chu, D. Bomans (U. of Illinois): "Probing the Origin of the Hot Gas in the LMC." 5(50)0.9-m M. Postman, C. Sturch, D. Rehner, J. Doggett (STScI), E. Costa (U. de Chile): "The Second Guide Star Photometric Catalog." 9(74)0.9-m
R. Probst (KPNO): "Wide Field Imaging of Molecular Cloud Interfaces in Orion." 5(44)l-m
R. Probst (KPNO), M. Rubio (U. de Chile): "Search for Molecular Hydrogen in LMC Star Forming Regions." 2(18) 1-m
M. Rich, S. Castro* (Columbia U.), J. Truran, J. Larouche* (U. of Chicago): "Iron Abundance and Element Ratios of the Young Globular Cluster Pal 12." 3(33)4-m
M. Ruiz (U. de Chile), P. Bergeron (U. de Montreal, Canada), S. Leggett (U. of Hawaii): "Study of Cool White Dwarfs." 2(20)4-m
R. Samec, B. Carrigan, J. Gray* (Millikin U.), D. Terrell (U. of Calgary, Canada), D. Hube (U. of Alberta, Canada): "A Continuing Study of Eclipsing Binaries as Tests of Relativistic Gravity." 8(40) 1-m, 9(53)0.6-m P. Schechter (MIT), M. Metzger (U. of Hawaii), J. Caldwell (SAAO, South Africa): "The Surface Mass Density of the Milky Way's Disk: K-Dwarf/K-Giant Discrimination at the SGP." 8(73)0.9-m B. Schmidt (Mt. Stromlo & Siding Spring Obs, Australia), N. Suntzeff, R. Schommer, M. Phillips, M. Hamuy, A. Clocchiatti (CTIO), C. Smith (U. of Michigan), R. Aviles (ESO, Chile), J. Maza (U. de Chile), A. Riess, R. Kirshner (Harvard U.), J. Spyromilio, B.Leibundgut (ESO, Germany), C. Stubbs, C. Hogan (U. of Washington): "A Pilot Project to Search for Distant Type la Supernovae." 3(30)4-m
P. Schmidtke, A. Cowley (Arizona State U.), J. Hutchings, D. Crampton (Dominion Astrophys. Obs., Canada): "Observational Constraints on Physical Parameters of Supersoft X-Ray Sources: II. Photometry." 7(60)0.9-m M. Shara, D. Wallace (STScI), A. Moffat (U. de Montreal, Canada): "Dwarf Novae in the Magellanic Clouds." 7(73)1.5-m
T. Smecker-Hane, P. Stetson, J. Hesser (Dominion Astrophys. Obs., Canada), D. Geisler (KPNO): "Stellar Populations of DwarfSpheroidal Galaxies: IV. The Star Formation History of the Fornax dSph." 2(19)4-m, 4(39)1.5-m
C. Smith (U. of Michigan), F. Winkler (Middlebury College), Y. Chu (U. of Illinois), R. Kennicutt (U. of Arizona): "An Optical Emission-Line Survey of the Magellanic Clouds." 13(100)CS
M. Smith (CTIO), P. Osmer, J. Kennefick (Ohio State U.): "A Search for Quasars at Redshifts 5 and 6." 3(31)4-m
V. Smith, D. Lambert (U. of Texas), N. Suntzeff (CTIO), K. Cunha (Observatorio Nacional, Brazil): "Chemical Evolution and Nucleosynthesis in the Large Magellanic Cloud." 4(42)4-m
J. Spyromilio, B. Leibundgut (ESO, Germany), M. Phillips, A. Clocchiatti (CTIO): "IR Spectroscopy of Supernovae." 2(20)4-m
T. Steiman-Cameron (NASA/Ames), J. Imamura (U. of Oregon): "High-Speed Photometry of Accreting White Dwarfs." 6(41)l-m
T. Storchi-Bergmann, C. Winge* (UFRGS, Brazil), M. Ward (Oxford U., UK), A. Wilson (U. of Maryland): "IR Emission Line Signatures of Tori in the Nuclei of Seyferts." 3(31)4-m
A. Tyson, P. Fischer, P. Boeshaar (AT&T Bell Labs.): "Dark Matter Distribution in Clusters of Galaxies: A Direct Observation." 4(21)4-m
A. Walker, R. Schommer, N. Suntzeff (CTIO), E. Olszewski (U. of Arizona): "Photometric Investigation of Magellanic Cloud Field Populations." 4(40)4-m, 4(29) 1.5-m
R. Walterbos (New Mexico State U.), G. Bothun (U. of Oregon), R. Schommer (CTIO), E. Smith (NASA/Goddard): "Diffuse Ionized Gas in Spiral Galaxies." 4(40)1.5-m,2(20)0.9-m
M. Way*, R. Flores (U. of Missouri), H. Quintana, L. Infante (U. Catolica de Chile): "A Search for Active Galactic Nuclei in Rich Clusters of Galaxies." 4(40)1.5-m
T. Williams, D. Merritt, B. Tremblay* (Rutgers U.): "The Kinematics of the Planetary Nebulae of NGC 1399."4(33)4-m G. Williger (Max-Planck Institute, Germany), A. Smette (Kapteyn Astron. Inst., The Netherlands), R. Elston (CTIO): "Low z QSO absorbers and their Environments." 4(32)1.5-m
B. Woodgate (NASA/Goddard), P. Francis (Melbourne U., Australia): "Mapping a Supercluster of Proto- Galaxies." l(ll)4-m
D. Zurek, R. Saffer (STScI), J. Hesser (Dominion Astrophys Obs., Canada), D. VandenBerg (U. of Victoria, Canada): "Is Age the Second Parameter? A Unique Test." 4(28)4-m
MACHO Program "Macho Program." K. Cook, D. Alves*. ll(85)0.9-m
Michigan Program (U. of Michigan): "Michigan Program." S. Lemley*, C. Smith, E. Friel, M. Lopez*. 32(220)CS
Executed Proposals 10/01/95 - 12/31/95 Page 1 Mon Jan 29 16:38:18 1996
Nights Hours Days Hours 1960 0 f95 V Andretta, J Doyle, S Bagnulo, Armagh Observatory M Giampapa, National Optical Astronomy Observatories HE I 1.083um Spectra of F and G Dwarfs Coude Feed 6.00 64.00 0.00 0.00
1939 0 f95 J Bally, D Devine, K Yu, University of Colorado B Reipurth, European Southern Observatory Morphology of Parsec Scale "Superjets" 0.9 meter 6.00 58.00 0.00 0.00
l—l 1941 0 f95 H J Bally, D Devine, V Alten, H University of Colorado B Reipurth, European Southern Observatory W The Interclump Medium and Outflow Shock > Statistics in.... Burrell Schmidt 6.00 39.50 0.00 0.00 ^
1681 0 f95 T Beers, S Hawley, Michigan State University M ^ B Anthony-Twarog, B Twarog, University of Kansas O t-r| A Sarajedini, SS =2 National Optical Astronomy Observatories > O Discovery and Analysis of Extremely Metal-Poor f M X Stars in.... 2.1 meter 00 46.00 0.00 0.00 o 0.9 meter 50 82.20 0.00 0.00 td CO C/3 W 1921 0 f95 5 P Bergeron, University of Montreal > M Ruiz, Universidad de Chile S Leggett, University of Hawaii O The Chemical Evolution of Cool White Dwarfs and pa the Age ... 0.9 meter 6.00 33.00 0.00 0.00 >-<
2008 0 f95 D Calzetti, Space Telescope Science Institute T Heckman, G Meurer, Johns Hopkins University Structure & Evolution of Starburst Galaxies: Study with... 2.1 meter 6.00 66.50 0.00 0.00 Executed Proposals 10/01/95 - 12/31/95 Page 2 Mon Jan 29 16:38:18 1996
Nights Hours Days Hours 2063 0 f95 S Courteau, National Optical Astronomy Observatories J Holtzman, Lowell Observatory Dust Extinction & Color Gradients in Spiral Galaxies 4 meter 3.00 24.50 0.00 0.00
1984 0 f95 N Devereux, New Mexico State University P Scowen, Arizona State University N Duric, University of New Mexico H-beta Imaging of Large Nearby Galaxies Burrell Schmidt 7.00 42.00 0.00 0.00
9163 0 f95 A Dey, National Optical Astronomy Observatories J Graham, J Najita, University of California, Berkeley Direct Imaging of Extremely Red Galaxies 4 meter 2.00 9.00 0.00 0.00
2052 0 f95 S Eikenberry, Harvard University G Fazio, Harvard-Smithsonian Center for Astrophysics Locating a Strange Infrared Variable in M15 2.1 meter 4.00 47.00 0.00 0.00
2053 0 f95 R Elston, National Optical Astronomy Observatories P Eisenhardt, Jet Propulsion Laboratory The Evolution of z>l Field Galaxies 4 meter 2.90 28.00 0.00 0.00
1926 0 f95 E Fitzpatrick, Princeton University D Welty, University of Chicago High Resolution Spectroscopy of Interstellar Clouds in Coude Feed 7.00 27.00 0.00 0.00
1973 0 f95 D Geisler, A Sarajedini, T von Hippel, National Optical Astronomy Observatories Stellar Populations in the Local Group Dwarf Elliptical.... 0.9 meter 1.00 3.00 0.00 0.00 Executed Proposals 10/01/95 - 12/31/95 Page 3 Mon Jan 29 16:38:18 1996
Nights Hours Days Hours 1944 0 f95 R Giovanelli, M Haynes, D Dale, Cornell University Measurement of Peculiar Velocities of Spiral Galaxies 0.9 meter 6.90 65.00 0.00 0.00
2107 0 f95 B Greenawalt, R Walterbos, New Mexico State University Emission-Line Imaging of Diffuse Ionized Gas in Nearby.... Burrell Schmidt 5.00 57.50 0.00 0.00
1979 0 f95 R Gupta, R Gulati, Inter-University Centre for Astronomy/Physics L Jones, University of North Carolina F Valdes, National Optical Astronomy Observatories Spectroscopic Library of Stars for Stellar Population Coude Feed 8.00 68.00 0.00 0.00
1991 0 f95 P Harding, University of Arizona A Sarajedini, National Optical Astronomy Observatories The M33 Cluster System 0.9 meter 7.00 63.00 0.00 0.00
1986 0 f95 D Helfand, E Blanton, Columbia University R White, Space Telescope Science Institute Bent Double Radio Galaxies & the Search for Distant Cluster 4 meter 1.00 14.00 0.00 0.00
2118 0 f95 G Hill, McDonald Observatory R Elston, National Optical Astronomy Observatories K Thompson, University of Texas, Austin Survey of Fe II in High Redshift QSOs 4 meter 4.00 41.00 0.00 0.00 Executed Proposals 10/01/95 - 12/31/95 Page 4 Mon Jan 29 16:38:18 1996
Nights Hours Days Hours 2003 0 f95 K Hinkle, R Joyce, National Optical Astronomy Observatories F Fekel, Tennessee State University Infrared Spectroscopy of Binary Miras Coude Feed 6.00 69.00 0.00 0.00
2130 0 f95 B Hrivnak, Valparaiso University S Kwok, W Lu, University of Calgary Near-IR and CCD Photometry & Spectroscopy of Proto 2.1 meter 8.00 85.50 0.00 0.00
2161 0 f95 B Jannuzi, R Green, National Optical Astronomy Observatories S Morris, Dominion Astrophysical Observatory R Weymann, Carnegie Observatories, (OCIW) Connection Between Low Redshift Ly-a Absorbers & Large.... 4 meter 2.00 22.00 0.00 0.00
2110 0 f95 L Jones, E Perlman, N White, C Scharf, NASA Goddard Space Flight Center I McHardy, University of Southampton G Wegner, Dartmouth College M Malkan, University of California, Los Angeles H Ebeling, University of Cambridge The X-ray Evolution of Poor Clusters of Galaxies 4 meter 1.00 6.00 0.00 0.00
1544 0 f95 J Kastner, Massachusetts Institute of Technology D Weintraub, Vanderbilt University R Probst, National Optical Astronomy Observatories Polarimetric/Coronagraphic Imaging of IRC + 10216 with 2.1 meter 2.70 28.00 0.00 0.00
1943 0 f95 W Keel, R White III, University of Alabama Extinction in Overlapping Galaxies: A Spectroscopic 2.1 meter 3.00 35.00 0.00 0.00 Executed Proposals 10/01/95 - 12/31/95 Page 5 Mon Jan 29 16:38:18 1996
Nights Hours Days Hours 1962 0 f95 S Kenyon, M Geller, Harvard-Smithsonian Center for Astrophysics R Marzke, Dominion Astrophysical Observatory The H-Band Luminosity Function of Nearby Galaxies 2.1 meter 3.85 18.00 0.00 0.00
1951 0 f95 T Kinman, National Optical Astronomy Observatories A Comparison of Two Halo BHB Surveys with a New Technique 0.9 meter 10.00 87.25 0.00 0.00
1917 0 f95 A Landolt, Louisiana State University Broad-Band Standards at Declination +45 Degrees 0.9 meter 14.00 74.00 0.00 0.00
2160 0 f95 K Lanzetta, SUNY at Stony Brook D Meyer, Northwestern University Deep Infrared Imaging of Damped Lya Absorbing Galaxies 2.1 meter 6.00 52.50 0.00 0.00
1980 0 f95 S Lee, Seoul National University B Carney, University of North Carolina R Probst, National Optical Astronomy Observatories The Luminosity/Mass Function for Halo Stars 2.1 meter 4.00 25.50 0.00 0.00
2159 0 f95 M Lysaght, M Skrutskie, M Weinberg, University of Massachusetts A 1.6um Spectral Survey of Evolved Stars Coude Feed 7.00 80.00 0.00 0.00
9153 0 f95 S Majewski, Carnegie Observatories, (OCIW) Completion of Prime Focus Photography 4 meter 3.00 34.00 0.00 0.00 Executed Proposals 10/01/95 - 12/31/95 Page 6 Mon Jan 29 16:38:18 1996
Nights Hours Days Hours 2075 0 f95 M McCall, York University R Buta, University of Alabama Global Properties of Galaxies in IC 342-Maffei Group.... Burrell Schmidt 6.00 63.00 0.00 0.00
1912 0 f95 D Meyer, Northwestern University Probing Small-Scale ISM Structure at Very High Velocity.... Coude Feed 6.00 40.00 0.00 0.00
1915 0 f95 D Meyer, Northwestern University The Interstellar Lithium Isotope Ratio Toward x2 Ori Coude Feed 7.00 63.00 0.00 0.00
2131 0 f95 M Meyer, University of Massachusetts S Kenyon, Harvard-Smithsonian Center for Astrophysics S Edwards, Smith College Infrared Spectroscopy of Protostars in Taurus Dark Cloud 4 meter 2.00 20.00 0.00 0.00
2070 0 f95 A Moffat, University of Montreal M Shara, Space Telescope Science Institute A Complete Search for Wolf-Rayet Stars in M31 0.9 meter 3.00 22.00 0.00 0.00
2037 0 f95 J Moody, P Roming, M Joner, Brigham Young University Possible Gas Outflow Near the Nucleus of M33 Coude Feed 7.00 82.00 0.00 0.00
2014 0 f95 A Noriega-Crespo, California Institute of Technology P Garnavich, Harvard-Smithsonian Center for Astrophysics A Raga, University of Mexico Herbig-Haro Jets Collimation: NIR Imaging with DLIRM 2.1 meter 3.75 17.50 0.00 0.00 Executed Proposals 10/01/95 - 12/31/95 Page 7 Mon Jan 29 16:38:18 1996
Nights Hours Days Hours 2096 0 f95 C O'Dea, S Baum, Space Telescope Science Institute M Lehnert, Lawrence Livermore Laboratory J,H,K Colors of Compact Powerful Radio Galaxies and a 2.1 meter 6.00 52.00 0.00 0.00
2074 0 f95 P Osmer, Ohio State University P Hall, University of Arizona R Green, National Optical Astronomy Observatories The Evolution of Faint Quasars at High Redshift 4 meter 3.00 29.00 0.00 0.00
2011 0 f95 T Oswalt, J Smith, C Daubigny, Florida Institute of Technology Spectroscopy of White Dwarf Candidates in Wide Binaries 2.1 meter 1.00 10.00 0.00 0.00
2134 0 f95 G Peters, University of Southern California Abundances of Moderately Heavy Elements in Ultrasharp.... Coude Feed 3.00 37.00 0.00 0.00
2222 0 f95 C Pilachowski, S Barden, M Giampapa, F Hill, National Optical Astronomy Observatories Asteroseismographic Explorations Coude Feed 5.00 46.00 0.00 0.00
1970 0 f95 M Postman, C Sturch, D Rehner, J Doggett, M Meakes, Space Telescope Science Institute The Second Guide Star Photometric Catalog 0.9 meter 4.00 20.50 0.00 0.00
1932 0 f95 B Rachford, R Canterna, University of Wyoming The Onset of Chromospheric Activity in late A- and Coude Feed 9.00 107.00 0.00 0.00 Executed Proposals 10/01/95 - 12/31/95 Page 8 Mon Jan 29 16:38:18 1996
Nights Hours Days Hours 2068 0 f95 R Saffer, M Livio, Space Telescope Science Institute Double Degenerate Progenitors of Type IA Supernovae 2.1 meter 6.00 43.50 0.00 0.00
2145 0 f95 R Saffer, Space Telescope Science Institute K Mitchell, General Sciences Corporation Establishment of New & Unique Complete Sample of Faint.... 0.9 meter 5.00 32.00 0.00 0.00
2058 0 f95 P Sarre, T Kerr, J Miles, University of Nottingham Intrinsic Fine Structure in Narrow Diffuse Interstellar.... Coude Feed 5.00 39.00 0.00 0.00
1994 0 f95 D Schade, S Lilly, G Mallen-Ornelas, University of Toronto The Local Density of Star-Forming Galaxies Burrell Schmidt 7.00 66.00 0.00 0.00
1928 0 f95 M Scodeggio, Cornell University Redshift Independent Distances to Galaxy Clusters 0.9 meter 2.00 20.00 0.00 0.00
9152 0 f95 N Sharp, D De Young, National Optical Astronomy Observatories Large Scale Outflows from HH & Young Stellar Objects 0.9 meter 1.00 0.00 0.00 0.00
2102 0 f95 D Smith, S Neff, M Fanelli, NASA Goddard Space Flight Center NGC1068: The Influence of an AGN Upon Star Formation 4 meter 1.00 10.00 0.00 0.00 Executed Proposals 10/01/95 - 12/31/95 Page 9 Mon Jan 29 16:38:18 1996
Nights Hours Days Hours 2103 0 f95 D Smith, S Neff, M Fanelli, NASA Goddard Space Flight Center Star Formation Histories of Starbursts and AGN: A Multi.... 2.1 meter 5.00 49.50 0.00 0.00
2036 0 f95 T Spahr, University of Florida C Hergenrother, University of Arizona B Marsden, Harvard-Smithsonian Center for Astrophysics A CCD Survey of Faint Minor Planets & Comets at High.... Burrell Schmidt 6.00 51.00 0.00 0.00
1924 0 f95 J Stocke, T Rector, University of Colorado Radio-Selected BL Lac Objects: Relativistic Jets or 2.1 meter 4.00 48.00 0.00 0.00
1978 0 f95 M Strauss, Institute for Advanced Study T Lauer, National Optical Astronomy Observatories M Postman, Space Telescope Science Institute Velocity Dispersions of Brightest Cluster Galaxies: Bulk... 2.1 meter 6.00 73.00 0.00 0.00
1961 0 f95 D Terndrup, A Krishnamurthi, S Balachandran, M Pinsonneault, K Sellgren, Ohio State University J Stauffer, Harvard-Smithsonian Center for Astrophysics S Wolff, National Optical Astronomy Observatories Completion of a Key Project to Constrain Angular Momentum 0.9 meter 14.50 124.50 0.00 0.00
1959 0 f95 S Veilleux, University of Maryland D Sanders, University of Hawaii Optical Spectroscopy of Unbiased Sample of Ultraluminous... 2.1 meter 5.00 57.00 0.00 0.00 Executed Proposals 10/01/95 - 12/31/95 Page 10 Mon Jan 29 16:38:18 1996
Nights Hours Days Hours 2061 0 f95 D Welty, University of Chicago High Resolution Spectroscopy of Translucent Interstellar .. Coude Feed 6.00 61.00 0.00 0.00
1933 0 f95 R White, Smith College Probing Shock and Pre-shock Gas Near the Pleiades with Coude Feed 5.00 46.00 0.00 0.00
1953 0 f95 P Winkler, B Williams, Middlebury College Spectra and High-Resolutin Imaging of New Candidate 4 meter 2.00 19.50 0.00 0.00
2167 0 f95 E Zirbel, M Dickinson, Space Telescope Science Institute J Allington-Smith, University of Durham A Oemler, Jr., Yale University R Ellis, University of Cambridge Evolution of Morphology-Density Relation: Spectroscopy.... 4 meter 4.65 47.00 0.00 0.00
Total number of proposals: 63 Appendix B National Solar Observatory October - December, 1995
Nights Days Hours
B003 19.2 108
Richard Altrock USAF/PL/GPSS
Three Line Coronal Photometer Evans Facility Sac Peak
B044 25 120
Steven Keil USAF/PL/GPSS Worden USAF
Ca K Solar Rotation Evans Facility Sac Peak
B057 35.65 227
Joe Elrod National Optical Astronomy Observatories
Ceolostat Activity Monitor Evans Facility Sac Peak
B062 48
Todd Brown National Optical Astronomy Observatories Coronagraph Activity Monitor Evans Facility Sac Peak
B321 5.58
Joe Elrod National Optical Astronomy Observatories Brown National Optical Astronomy Observatories
Sunspot Drawings Evans Facility Sac Peak
T333 54
Richard Mann National Optical Astronomy Observatories Hegwer National Optical Astronomy Observatories Stratton National Optical Astronomy Observatories
Maintenance
Vacuum Tower Tel./SP Sac Peak
B335 Jeffrey Kuhn National Optical Astronomy Observatories Coulter National Optical Astronomy Observatories
RISE/PSPT Testing Evans Facility Sac Peak Nights Days Hours
B344 7.4 68 Shadia Habbal Harvard-Smithsonian Center for Astrophysics Altrock USAF/PL/GPSS Brickhouse Harvard-Smithsonian Center for Astrophysics Esser Harvard-Smithsonian Center for Astrophysics Karovska Harvard-Smithsonian Center for Astrophysics Determination of Coronal Temperature Evans Facility Sac Peak
B348 2.5 20 Joe Elrod National Optical Astronomy Observatories Brown National Optical Astronomy Observatories
Maintenance - General Evans Facility Sac Peak
B354 2.6 26 Donald Hassler High Altitude Observatory/NCAR Moran NASA/Goddard Space Flight Center Ulysses/Spartan 201 Collaboration Using the Evans Facility Coronagraph Evans Facility Sac Peak
B358 4.75 38 Fritz Stauffer National Optical Astronomy Observatories Hegwer National Optical Astronomy Observatories Wilkins National Optical Astronomy Observatories Elrod National Optical Astronomy Observatories ESF Improvements Evans Facility Sac Peak
B363 Don Neidig USAF/PL/GPSS Kuhn National Optical Astronomy Observatories Beckers National Optical Astronomy Observatories Coronal Sky Survey for CLEAR Evans Facility Sac Peak
B364 Jeffrey Kuhn National Optical Astronomy Observatories IR Coronal Spectroscopy Evans Facility Sac Peak Nights Days Hours
T422 10.7 100 John Thomas University of Rochester •Lites High Altitude Observatory Bogdan High Altitude Observatory Sunspot and Active Region Seismology
Vacuum Tower Tel./SP Sac Peak
T442 Jacques Beckers National Optical Astronomy Observatories Rimmele National Optical Astronomy Observatories High Resolution Imaging
Vacuum Tower Tel./SP Sac Peak
T446 2.8 28 Thomas Rimmele National Optical Astronomy Observatories Radick Phillips Lab/Solar Research Branch Dunn National Optical Astronomy Observatories High Resolution Imaging, Wavefront Sensor Tests
Vacuum Tower Tel./SP Sac Peak
T447 14.3 Haosheng Lin National Optical Astronomy Observatories Kuhn National Optical Astronomy Observatories IR Observation of Magnetic Field Oscillations of Sunspots
Vacuum Tower Tel./SP Sac Peak
T450 38
Thomas Rimmele National Optical Astronomy Observatories Stebbins University of Colorado Goode New Jersey Institute of Technology
Strous New Jersery Institute of Technology
P-mode Exitation
Vacuum Tower Tel./SP Sac Peak
T460 1.2 Steven Keil USAF/PL/GPSS Balasubramaniam National Optical Astronomy Observatories Gullixson National Optical Astronomy Observatories Testing of the Optical Quality IR Fabry Perot and IR Camera - Engineering Run
Vacuum Tower Tel./SP Sac Peak Nights Days Hours
T462 61 Jan Stenflo ETH- Zurich Lites High Altitude Observatory Vector Polarimetry of the Hanle Effect
Vacuum Tower Tel./SP Sac Peak
T463 12.5 79 Richard Canfield University of Hawaii Pevtsov University of Hawaii Strous New Jersery Institute of Technology Kinetic and Magnetic Helicity in Active Region Photospheres
Vacuum Tower Tel./SP Sac Peak
T464 10.5 82 Thomas Rimmele National Optical Astronomy Observatories Radick Phillips Lab/Solar Research Branch Dunn National Optical Astronomy Observatories High Resolution Imaging, Wavefront Sensor Tests
Vacuum Tower Tel./SP Sac Peak
T467 3.5 Jeffrey Kuhn National Optical Astronomy Observatories Beebe New Mexico State University Varsik National Optical Astronomy Observatories Lin National Optical Astronomy Observatories Support of Jupiter Galileo Probe Entry Mission
Vacuum Tower Tel./SP Sac Peak
T476 43 Larry November National Optical Astronomy Observatories Zirker National Optical Astronomy Observatories Filament Stereo Imaging
Vacuum Tower Tel./SP Sac Peak
1138 Drake Deming NASA/Goddard SpaceFlightCenter Long Term Program: Monitoring the Apparent Velocity of Integrated Sunlight
McMP FTS/Mc-P
1222 0 21 Curtis Rinsland NASA Langley Research Center Monitoring of Long-Term Trends in the Concentrations of Atmospheric Gases from McMath FTS Solar Spectra Mc-P Main FTS/Mc-P Nights Days Hours
1426 12 66.5 Steven Saar Harvard-Smithsonian Center for Astrophysics
Synoptic Observations of Magnetic Fields on G and K Stars Mc-P Main Stellar Spectrograph
1661 42
Linda Brown Jet Propulsion Laboratory Toth Jet Propulsion Laboratory Laboratory Infrared Spectroscopy
FTS Lab
1741 9.5 Joel Eaton Tennessee State University H Alpha Variations in Zeta Aurigae Binaries and Cool Supergiants McMP Stellar Spectrograph
1822 12 15.66 Myron Smith Computer Sciences Corporation Dupree Harvard-Smithsonian Center for Astrophysics Luttermoser Applied Research Corporation Guinan Villanova University Baliunas Center for Astrophysics Radial Velocity Observations of Alpha Ori, Alpha Sco, and Alpha Her McMP Stellar Spectrograph
1858 38 William Livingston National Optical Astronomy Observatories
Cycle Variability of the Solar Spectrum Mc-P Main Main spectrograph
1860 26.2
James LoPresto Edinboro University of Pennsylvania Pierce National Optical Astronomy Observatories Schrader Edinboro University of Pennsylvania
Solar Gravitational Redshift McMP Main spectrograph
1862 Oran White High Altitude Observatory Livingston National Optical Astronomy Observatories
The Sun as a Star: Ca II K Variability Mc-P Main Main spectrograph Nights Days Hours
1863 1.5 Keith Pierce National Optical Astronomy Observatories LoPresto Edinboro University of Pennsylvania
The Absolute Value of the Solar Limb Effects for Different Fraunhofer Lines Mc-P Main Main spectrograph
1866 59 Douslas Rabin National Optical Astronomy Observatories
True-Field Imaging Magnetometry in the Near Infrared McPE Main spectrograph
1868 29 Andrew Potter NASA Johnson Space Flight Center Morgan Southwest Research Institute
Talent Lockheed Martin Studies of Exospheric Emission Lines from Mercury and the Moon McMP Stellar spectrograph
1915 20 145 Donald Jennings NASA/Goddard Space Flight Center Deming NASA/Goddard Space Flight Center Sada NASA Goddard Space Flight Center Bjoraker NASA Goddard Space Flight Center McCabe NASA Goddard Space Flight Center Continuing Thermal-IR Spectroscopic Observations of Jupiter and Comet Shoemaker-Levy 9 Fragment Collision McMP Main spectrograph
1921 14.5 Joel Eaton Tennessee State University
Structure of the Deep Chromosphere of Zeta Aurigae McMP Stellar Spectrograph
1921 14.5 Joel Eaton Tennessee State University
Structure of the Deep Chromosphere of Zeta Aurigae McMP Stellar Spectrograph Nights Days Hours
1922 12 72.5 Ilkka Tuominen University of Helsinki Saar Harvard-Smithsonian Center for Astrophysics Piskunov University of Colorado/JILA
Jetsu University of Helsinki
Hackman University of Helsinki Surface imaging of magnetic structures in late type stars McMP Stellar Spectrograph
1931 15 70 Andrea Dupree Harvard-Smithsonian Center for Astrophysics
Search for Pulsations in Metal Deficient Field Giants Mc-P Main Stellar Spectrograph
1944 11.5 Peter Foukal Cambridge Research and Instrumentation, Inc.
Prominence Electric field Measurements in HI Lamda 10.503 micron
Mc-P Main FTS/Mc-P
1948 57
Peter Bernath University of Waterloo Ram Lamb
Huffman
Tinker Laboratory Spectroscopy of Molecules Found in the Sun
Mc-P Main FTS Lab
1955 Deane Peterson SUNY Stony Brook
Obital Parallax of Finsen 342 Mc-P Main Stellar Spectrograph
1958 25.5 Jian Ge Steward Observatory Livingston National Optical Astronomy Observatories Angel Steward Observatory Study the Annual Variation in Column Density of Sodium Atoms above Kitt Peak McMP Main spectrograph Nights Days Hours
1962 53.5 Vincenzo Andretta Armagh Observatory Giampapa National Optical Astronomy Observatories Doyle Armagh Observatory Bagnulo Armagh Observatory He I 587.6 nm Spectra of F and G Dwarfs McMP Stellar spectrograph
1964 48 Rolf Engleman, Jr. University of New Mexico Germanium Hollow Cathode and Other Emission Spectra
FTS Lab
1965 22 61.5 Christopher Johns-Krull University of Texas
Synoptic Study of Accretion Flows in Two T Tauri Stars McMP Stellar spectrograph
1966 39 Alessandro Cacciani Universita "La Sapienza" Jefferies Bartol Research Institute Low-1 Helioseismology and Active Region Doppler/Magnetic Observations McMP Main spectrograph
1967 54 Kwang-Ping Cheng California State University at Fullerton Neff Pennsylvania State University A Search for New Proto-Planetary System Candidates McMP Stellar spectrograph
1968 Gianpiero Tagliaferri Osservatorio Astronomico di Brera Fleming University of Arizona Pallavicini Osservatorio Astrofisico di Arcetri Cutispoto Osservatorio Astrofisico di Catania Spectroscopic Study of Cool Stars Serendipitously Discovered in EUV Surveys McMP Stellar spectrograph
1969 44.34 Mark Giampapa National Optical Astronomy Observatories Basri University of California Imhoff Computer Sciences Corporation Comparative Synoptic Study of Two T Tauri Stars McMP Stellar spectrograph Nights Days Hours
1971 73 Jeff Valenti University of Colorado Gagne University of Colorado Linsky University of Colorado Chromospheric and Coronal Processes in F and G-type Dwarfs McMP Stellar spectrograph
1972 12 29.75 Alan Welty Pennsylvania State University
Radial Velocity Variations of T Tauri McMP Stellar spectrograph
1973 36.5
Deane Peterson SUNY Stony Brook Hummel US Naval Observatory
Resolved Spectroscopic Binaries McMP Stellar spectrograph
1974 25 37.75 Klaus Strassmeier University of Vienna Doppler Imaging of Spotted Chromospherically Active Stars McMP Stellar spectrograph
1976 12 Thomas Ayres University of Colorado, CASA Rabin National Optical Astronomy Observatories A Sensitive Search for Steam in the COmosphere McMP Main spectrograph
1977 63 Jack Margolis ^et Propulsion Laboratory
Infrared Half-widths and Shifts of Methane
FTS Lab
1978 Geoffrey Marcy University of California, Berkeley Butler University of California, Berkeley
FTS Iodine Cell Spectrum
FTS Lab Nights Days Hours
1979 Christoph Keller National Optical Astronomy Observatories Image Quality Improvement Project Engineering McMP Main spectrograph
1983 91 601 Todd Brown National Optical Astronomy Observatories Daily White Light Patrol Hilltop Dome Sac Peak
1984 620 Todd Brown National Optical Astronomy Observatories
Daily Flare Patrol Hilltop Dome Sac Peak
1991 6.15 Ernest Hildner National Oceanic & Atmospheric Administration November National Optical Astronomy Observatories H-Alpha and Ca K Spectroheliograms Evans Facility Sac Peak
3790 90 342.5 John Harvey National Optical Astronomy Observatories Vacuum Synoptic Program: Daily/Community KPVT Spectromagnetograph
Total number of proposals: 6k APPENDIX C
US Sites Safety Report
Following is the summary of recordable occupational injuries and illnesses for the US sites as reported on the respective CY 1995 OSHA 200 logs. As required, the respective data will be posted at each site no later than 1 February.
KPNO NSO/SP Tucson Total
Fatalities 0 0 0 0
Injuries involving days off or days 3 1 2 7 of restricted work activity or both
Injuries involving days off 3 1 2 7
Days off from work 39 8 8 55
Days of restricted work activity 0 0 0 0
Injuries without lost workdays 0 0 0 0
Illnesses 0 0 2 2
Illnesses without lost workdays 0 0 1 1
Total recordable injuries/illnesses: 3 1 4 8
Compared to last year, NOAO experienced a decrease in the number of injuries/illnesses, from 14 to 8. At the same time there was an increase in illnesses, from 1 to 2, and a slight increase in the average lost workdays, from 5.8 to 6.9 per person.
The types of injuries/illnesses broke down as follows:
Sprain/strains 4 Slips/falls 2 Repetitive motion/cumulative trauma 2
KPNO and NSO/SP Mountainwide Fire Alarm Systems: The installation of individual fire alarm systems begun in CY 1994 was completed. Except for the houses at NSO/SP which are protected with stand-alone smoke detectors every major building or complex is equipped with a fire alarm system. Each system includes the appropriate smoke and heat detectors, manual pull stations, audio/visual alarms and transmitter which transmits the trouble or alarm signal to a central station receiver and annunciation system.
NSO/SP Sewage Treatment Plant was upgraded and permitted with the State of New Mexico. NSO/SP Visitor Center - Environmental Impact: Required National Environmental Protection Act approvals were obtained for the future visitor center site.
Tucson Headquarters Fire Alarm System was upgraded with a new digital transmitter for transmitting fire alarm signals over dedicated phone lines to the central station and monitoring the phone lines.
Mandatory Department of Labor/BLS Statistics Survey for 1994 occupational injuries/illnesses for the Tucson and KPNO sites were prepared and sent to the Arizona Industrial Commission.
Loss Prevention Surveys/Reviews: Various surveys/reviews were conducted and the resultant recommendations furnished in regards to the following:
KPNO mountain brush fire danger Fire prevention - KPNO facilities Survey of optics polishing compounds for potentially dangerous levels of radioactivity General survey of Tucson facilities and all work stations in Block 5, bounded by First and Second Streets and Martin and Warren Avenues Removal of 4-m shutter drive system Safety procedures, equipment and ventilation system for the HF-HC1 acid etching of CTIO 4-m secondary mirror Twenty PC workstations to assure ergonomically sound principles WIYN Safety Program Fire safety of KPNO facilities Extra-low frequency electromagnetic fields for high levels and the potential for causing PC monitor flicker 2.1-m ring change with focus on adequacy of personalfall protection Potential displacement of 02 by N2and/or He2in KPNO IR Labs Working alone in KPNO IR lab and optics basement Final review of 16" Visitor's Telescope facility 4-m telescope shutdown with focus on adequacy of personal fall protection Orbital Debris Liquid Mirror Telescope
Training: Several KPNO and NSO/SP EMT's received refresher training and wererecertified.
Two KPNO staffmembers received 160 hours of emergency medical training andcertified as EMTs.
The NSO/SP Safety Officer attended the state of New Mexico's conference on the requirements for underground storage tank.
The KPNO and NOAO Safety Officers attended the Southwest Safety Congress, including various seminars.
Four KPNO staff members completed 40 hours of First Responder Training.
GONG field support staff were trained in first aid and CPR. The NOAO Safety Officer attended ITT Hartford's loss control management course.
KPNO Maintenance operations attended a demo with hands on use of personalfall protection equipment.
KPNO and Tucson maintenance operations staff received refresher training on the use of fire extinguishers.
CTIO Safety Report
CTIO Recordable Occupational Injuries: Calendar Year 1995
Fatalities: 0 Injuries involving days off or days of restricted work activities or both: 1 Days offfrom work: 5 Days off from work due to accident occured endof 1994: 36 Days of restricted work activity: 0 Injuries without lostworkdays: 0
There were no occupational illnesses recorded at CTIO.
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