National Optical Astronomy Observatories
National Optical Astronomy Observatories
Quarterly Report
July - September 1988
TABLE OF CONTENTS
I. INTRODUCTION 1
II. SCIENTIFIC HIGHLIGHTS 2
A. Dwarf Elliptical Galaxies in Fornax and Centaurus Clusters 2 B. Montreal-Cambridge Survey 2 C. Metallicity of the Globular Clusters 3 D. Spatial Structure in the Lyman Alpha Forest 4 E. Emission Line Nebulae in Cooling Flows: Fundamental Indicators? 4 F. Large-Scale Magnetic Fields 5 G. An Inhomogeneous Model of the Solar Atmosphere 6
III. PERSONNEL 7
A. Visiting Scientists 7 B. New Appointees 7 C. Terminations 8 D. Change of Status 8 E. Summer Research Assistants 8
IV. INSTRUMENTATION, NEW PROJECTS AND OBSERVATORY ACTIVITIES ... 9
A. Advanced Development Program 9 B. GONG 11 C. Instrumentation Projects 13 D. Observatory Activities 18
V. PROGRAM SUPPORT 20
A. Director's Office 20 B. Publications and Information Resources 20 C. Central Computer Services 20 D. Central Administrative Services 21 E. Central Facilities Operations 21
Appendices A. Telescope Usage Statistics 22 B. Observational Programs 23
I. INTRODUCTION
The National Optical Astronomy Observatories applied for supplemental funding for the NSF's Research Experiences for Undergraduates Site Program at the end of September. NOAO hopes to accommodate 18 students during the summer of 1989 and through the fall. Students participating in the REU program will have access to the facilities in Tucson, on Kitt Peak, and in Sunspot.
Work was begun on the NOAO annual report for the period July 1987 - June 1988. The AURA Executive Committee met September 7 - 9, 1988 in Sunspot, New Mexico. The meeting was held at the National Solar Observatory/Sac Peak Community Center. Agenda items included: report of the NOAO Director; MOU with the U. of Hawaii; report of the ST Scl Director; report of IVC/ST Scl; and the AURA President's Report. Issues covered were: update on impacts of NOAO budget cuts; action on interim WIN agreement; NOAO plans for 8-m telescopes; status of AURA advocacy group; and mirror polishing.
The Advanced Development Program was formally dissolved as a NOAO division at the end of FY 1988. Those ADP activities that will be continued and the ADP scientific staff were transferred to the KPNO division. J. Beckers, Director of ADP, departed NOAO at the end of July 1988 to join the European Southern Observatory and to participate in their Very Large Telescope project in Chile. In August, P. Osmer agreed to serve as the acting project scientist for the NOAO 8-m Telescopes Project. NSF foreign travel funds expended this quarter amounted to $82.64. A total of $19,991.82 was spent in FY 1988.
II. SCIENTIFIC HIGHLIGHTS
A. Dwarf Elliptical Galaxies in Fornax and Centaurus Clusters.
N. Caldwell (Whipple Obs.) and G. Bothun (U. of Michigan) have been using the CTIO 1.5-m telescope to obtain CCD images of a number of dwarf elliptical galaxies in the Fornax and Centaurus clusters. The data will be used to investigate the structure, stellar populations, and luminosity functions of these galaxies, and to derive independent distances relative to the Virgo cluster, for which similar data exists.
Caldwell and Bothun have shown that a strong relation exists between the surface brightnesses and luminosities of dwarf elliptical galaxies. This is in contrast to the classical ellipticals which show very little correlation between those parameters, outside of the nucleus. The dispersion in the relation for the dwarf ellipticals is about 0.6 mag, making the relation a viable candidate for determining relative distances to clusters of galaxies, where these dwarfs tend to reside. The relation between central or isophotal surface brightness and luminosity is linear (in logarithmic units), thus the error in determining magnitude zero-point shifts between clusters can be made to be as small as that found for the IR Tully-Fisher relation, if many dwarfs are measured.
Caldwell and Bothun have obtained images for some 30 - 40 dwarfs in the Fornax and Centaurus clusters. From these, surface brightness profiles are extracted, which give total and isophotal magnitudes and central surface brightnesses. These data will provide a differential distance of Centaurus to Fornax.
The Centaurus cluster is a particularly interesting target. Recently, the uniformity of the universal expansion has come into question with the contention by Dressier (Mt. Wilson and Las Campanas Obs.) and collaborators that several large clusters of galaxies have relative redshifts that are not in accord with their relative distances, as determined from a variant of the Faber-Jackson relation. In particular, the Hydra and Centaurus clusters have discrepant velocities that indicate a motion in an opposite direction from us, which Dressier et al. attribute to a large, as yet unidentified mass that is attracting the clusters. Clearly, supporting evidence of such findings is of utmost importance. The independent distance determined by Caldwell and Bothun will help to resolve this discrepancy.
B. Montreal-Cambridge Survey. The Montreal-Cambridge Survey, initiated in October 1984, is nearing completion of the photographic phase. The survey is an on-going project to discover blue stellar objects with B < 17 in the South Galactic Pole region. The survey is patterned after the highly- successful Palomar-Green survey in the Northern hemisphere. The specific goal of this project is to provide a statistically complete sample of blue southern subluminous degenerate stars without regard to space motion. It is a collaborative effort between groups at the U. of Montreal (S. Demers, G. Fontaine, F. Wesemael, R. Lamontagne) and the Inst, of Astronomy in Cambridge (M. Irwin). Extensive use has been made of the Curtis-Schmidt telescope at CTIO, with follow-up observations of interesting candidates on the CTIO 1-m and 1.5-m telescopes. The Montreal-Cambridge survey has the following distinct advantages over previous surveys for ultraviolet-excess objects: 1) a modest limiting magnitude of B ~ 17.3, exposure times of 7.5 min for B and 60 min for U are used on the Schmidt telescope; 2) the survey yields a homogeneous sample of blue subluminous stars down to a completeness limit of B = 16.5; 3) the plates are measured with the APM facility in Cambridge, and the analysis to produce the color-magnitude diagrams, the lists of candidates and the finding charts is done almost completely automatically; and 4) follow up spectroscopic observations of the candidates showing the strongest ultraviolet excess have been done during two runs at the CTIO 1.5-m telescope. The first run to obtain Stromgren photometry of newly-discovered white dwarfs with the CTIO 1.5- m was recently successfully completed.
C. Metallicity of the Globular Clusters.
J. Claria and D. Minniti (Obs. Astron. de C6rdoba, Argentina) have used the CTIO 1-m and 0.6-m telescopes to obtain observations in the Washington and DDO photometric systems of red giants in globular clusters whose fundamental properties suggest extreme metal deficiency. Much effort has been devoted recently to accurately determining the upper limit of metallicity for the globular cluster system of the Galaxy. However, less observational importance has been assigned to the lower limit of metallicity for the globular clusters. This limit has not been precisely established due to limitations imposed by the techniques so far employed. Many of the existing metallicity values are based on integrated properties (spectroscopic or photometric) which can be affected by stochastic effects or by the contribution of the horizontal branch to integrated light. Methods based on individual photometry of red giants, such as the Washington system, have been shown to be very reliable.
Based on Washington and DDO photoelectric observations at the CTIO 1-m and 0.6-m telescopes, Claria and Minniti have found that the globular clusters M30 and M68 appear to have a metal abundance even lower than -2.4 dex, the traditional lower metallicity limit for Galactic globular clusters. They are currently investigating other very metal-poor candidates. If indeed there are more metal-poor globular clusters, then important conclusions related to their formation will be derived. For example, the distribution function for the metallicities of the globular clusters will be sensibly modified, affecting previous conclusions about the origin of the metal-poor stars belonging to the galactic halo. Several authors have compared the distribution of metallicities for both samples, globular clusters and metal-poor halo stars, to establish whether or not they have a common origin. Recent studies have uncovered differences between halo and globular cluster giants, but this picture may change if the distribution of metallicities for the globular clusters changes. Also, the most important observational argument favoring the theory of formation of globulars during the collapse of the protogalaxy, as presented by Fall (St Scl) and Rees (Inst, of Astronomy, Cambridge), is the similarity between these two populations. The possible existence of very metal-poor, [Fe/H] < -2.4, globular clusters has crucial importance for the metal enrichment history of the Galaxy. Another motivation for the investigation of globular cluster metal abundances is brought about by the recent revolution in the ability to obtain accurate main-sequence photometry for these objects. Now that beautiful CCD color-magnitude diagrams are becoming available for more and more globular clusters, the study of their ages has greatly improved. However, reliable age determination requires an accurate and independent knowledge of the metallicity, reddening and distance. In fact, the age determination has a strong metallicity dependence. For example, an overestimation of the metal content of M68 by 0.5 dex would lead to an error in the age of the order of 3 Gyr. Clearly, more accurate abundance determinations are required.
D. Spatial Structure in the Lyman Alpha Forest.
A long standing and intriguing feature in QSO spectra is the extremely high density of absorption lines due to Lyman alpha absorption by hydrogen atoms. This "forest" of absorption lines lies at redshifts well below that of the quasar, and it is presumed to arise from gaseous matter in extremely distant galaxies or protogalaxies. A knowledge of the spatial distribution of these clouds would yield significant information about the large scale structure of the universe at early epochs, as well as providing insight into the process of galaxy formation itself. An obvious way to probe this structure is to search for clustering in the absorption lines as a function of wavelength. This velocity clustering analysis will be unambiguous only if the effect is large enough not to be contaminated by internal, perhaps systematic, motions within the individual clouds. Unfortunately, for the hydrogen-only systems this has not been the case, and only weak clustering has been suggested on scales of less than about 300 km/sec.
Another technique for examining this problem would be to search for angular correlations in the absorption line systems. This method avoids the ambiguities due to internal motions of the clouds, but it requires a search for very closely spaced, bright quasars to illuminate the absorption line systems. The few cases of adjacent high redshift QSOs studied so far show only a marginal effect at scales less than about 2 Mpc. However, A. Crotts (U. Texas) has recently used the KPNO 4-m telescope to further this effort. He has found four closely spaced, high redshift QSOs located in an area only 440 arcsec in diameter, and he has studied 276 absorption lines in these objects. These data allow an unprecedented analysis of high redshift, large scale structure in the neutral hydrogen distribution at early epochs. The analysis by Crotts finds some evidence for voids in this distribution on a scale comparable to that found in the voids of galaxy distributions at low redshift. For example, he finds a deficiency of absorbers at a redshift of 2.38 which is about 30 Mpc in size. The presence of such large scale clustering at high redshift is of critical importance in constraining models for the evolution of the universe. In most of these models, large scale structure is a slowly evolving feature which does not become evident until later times. These new observations will clearly require some revision of current models.
E. Emission Line Nebulae in Cooling Flows: Fundamental Indicators?
As has been known for some time, the x-ray emitting gas at the centers of many rich clusters of galaxies has a cooling time less than the Hubble time; hence the gas should cool and fall inward. Such cooling flows in clusters are the source of some controversy, for if the infall rates inferred are correct, serious problems arise as to the final disposition of the gas. Converting it to stars does not work, for any normal stellar population would provide more light than is seen. Considerably more exotic mechanisms have been suggested, none of which have been confirmed. Hence any additional information about the physical characteristics of such flows is of considerable importance. As the temperature of the flows drops to around 100,000 degrees, optical and UV emission lines become the dominant coolant, and observations of such emission line regions can yield important information about the density, temperature, and velocity structure of the flows. Such clouds are in fact seen, but a major dilemma arises in that their emissivity is greater than that expected from simple cooling of the Mailing gas. Hence some additional heating mechanism is required. Observations which address all these issues have recently been made with the KPNO 4-m and 2.1-m telescopes by T. Heckman and S. Baum (U. of Maryland), W. van Breugel and P. McCarthy (U. of California, Berkeley). They examined emission line regions associated with the dominant galaxy in nine clusters of galaxies thought to have cooling flows. An interesting kinematic result that emerges from the observations is that there is little evidence for shearing motion or coherent rotation in the emission line gas. This would imply that the intracluster medium (ICM) from which the clouds coalesce has little angular momentum. Moreover, the line widths decrease with increasing distance from the galaxy in a manner consistent with free fall into the galaxy gravitational potential. If this is the case, the mass accretion rates are consistent with those estimated from the x-ray data. However, this interpretation is not unique; increasing turbulence in the flow near the center could also produce the line broadening. Electron number densities in the central regions are typically a few hundred per cubic centimeter, and this results in pressures there which are up to ten times greater than those inferred from the x-ray data over slightly larger scales. Some insight is gained about the elusive heating mechanism. Shock heating seems unlikely, and photoionization by an active galaxy nucleus is clearly ruled out. Heating by x-rays from the ICM is possible, and is perhaps the most likely mechanism. Thus these new observations provide several important results: the ICM probably has very little angular momentum, which in turn reflects upon the dynamics of the primordial cloud from which the cluster evolved; mass infall rates may be as high as those suggested by the x-ray data; and a mechanism for heating the emission line clouds may at last have been found.
F. Large-Scale Magnetic Fields.
As part of an investigation funded by the Office of Naval Research, R. Howard, J. Harvey, and S. Forgach (NSO/T) continued the analysis of Solar Vacuum/KP magnetograph data during this quarter. Various instrumental and ephemeris corrections have been generated and tested. A correlation method of determining rotation and meridional drift of small magnetic elements has been worked out and tested on a small sample of data. Preparation is underway to reduce a large number of magnetograms in an analysis of rotation, meridional flow, giant cells, and any other large-scale velocity fields that may be present. This will be the first time that such velocity fields have been examined using small magnetic field structures as tracers. They expect during the next quarter to begin large-scale reduction of many years of data. It is necessary to use a large data base for this type of analysis in order to detect a weak signal against a strong background of noise from oscillations, supergranulation, active-region associated velocity fields and other large-scale noise sources.
Howard has initiated a program of analysis of Mt. Wilson synoptic magnetic data for the purpose of examining the gross properties of active region magnetic fields. He is using the "coarse array" data to identify magnetic regions from day to day and study properties such as region size, total and net magnetic flux, magnetic complexity, separation of magnetic polarities, polarity orientation, maximum magnetic field strength, rotation rate, meridional flow, and other parameters. Early results include correlations between average region size and phase in the activity cycle and between region growth and decay rates and phase in the activity cycle. Active regions are the fundamental elements of the visible activity cycle-the manifestations of the eruption of magnetic flux at the solar surface, and the maximum phase of the cycle is characterized both by more active regions per unit time and by larger active regions. Decay rates for the magnetic fields of active regions average 25-30% of the region flux per day. Flux growth rates are significantly higher than flux decay rates.
G. An Inhomogeneous Model of the Solar Atmosphere.
During this quarter, J. Jefferies (NSO/T) completed an analytical program for interpreting airborne infrared data, obtained at the March 1988 total eclipse, in terms of an inhomogeneous model of the solar atmosphere. The computer program calculates the profile of the solar limb, as observed during an eclipse, for a given wavelength and a specified model, for comparison with experimental data. The theoretical approach is based on a novel statistical formulation of the transfer of radiation through an inhomogeneous medium, which was recently completed by Jefferies and C. Lindsey (U. of Hawaii) and is to be published in December 1988 in the Astrophysical Journal. The program, which calculates the expected value and the variance of the emerging radiation, has been extensively tested. Comparison of the computations with the observational data, which spans the range from 30 to 800 ^m is to begin in the immediate future. The objective is to infer a single inhomogeneous model of the Sun's atmosphere which will be consistent with these observations of this hitherto unstudied region of the solar spectrum while simultaneously accounting for the extensive data on more readily accessible regions of the solar spectrum.
In a collaborative program with B. Lites and A. Skumanich (High Altitude Obs.), Jefferies has worked extensively on the transfer of spectral line radiation through a gas permeated by a magnetic field. The equations governing the propagation of the polarized line radiation for this situation were re-derived from first principles using classical theory and their forms discussed for the limiting case where the magnetic field is 'weak' in the sense that the Zeeman splitting is smaller than the line width arising from the thermal motion of the atoms (the Doppler width). This class of cases, in fact, typically includes fields up to 1000 Gauss. Some new procedures were developed during this theoretical study which generally clarify and extend approximate methods developed previously for inferring the characteristics of the field directly and simply from the observed spectra. This work is essentially complete and is to be submitted in October 1988 for publication. Extended testing of the new procedures using data obtained from existing solar polarimeters is planned for the immediate future.
III. PERSONNEL
Visiting Scientists.
The following visitors arrived at NOAO facilities for periods of one month or more during the July 1 - September 30, 1988 quarter.
date NOAO facility arrived name institution visited
7/01/88 Mark Abrams U. of California, Berkeley NSO 7/01/88 Domenico Bonaccini Inst, de Astronomia, Italy NSO 7/01/88 Serge Koutchmy Centre National de la Recherche Scientific, France NSO 7/01/88 Tomas Rimelle Kiepenheuer Institut fur Sonnenphysik, Germany NSO 7/01/88 Al Schultz U. of Nevada, Las Vegas CCS 7/01/88 Motohide Tamura U. of Massachusetts, Amherst ADP 7/01/88 Tokio Tsubaki Shiga U., Japan NSO 7/05/88 Edigio Landi Osservatorio di Arcetri, Italy NSO 7/08/88 Drew Phillips U. of Washington, Seattle CCS 7/25/88 Franz Deubner Inst. Astronomie und Astrophysik, Germany NSO 7/28/88 Christian Nitschelm Institute d'Astrophysique, France NSO 8/01/88 Christopher Pritchet U. of Victoria, Canada CTIO 8/07/88 Liu Jinming Progress in Astronomy, China KPNO 8/15/88 Phillip Lu Western Connecticut State U. CTIO 8/15/88 Abdulrahman Sa'ad King Abdul Aziz City for Science Al Khashlan & Technology, Saudi Arabia KPNO 8/18/88 Julia Lutz Washington State U. CTIO 8/18/88 Thomas Lutz Washington State U. CTIO 8/22/88 Robert Schommer Rutgers U. CTIO 8/30/88 Huisong Tan Yunnan Obs., China KPNO 8/31/88 Lois Kieffaber Whitworth Coll., Washington NSO 8/31/88 Alan Peterson Utah State U., Utah NSO
B. New Appointees.
The table below shows details of new appointments made to NOAO during the July 1 September 30, 1988 quarter. date of appointment name position NOAO division
7/15/88 Timothy Ellis Senior Engineer ETS 8/16/88 Carol Neese Research Associate NOAO 9/09/88 Richard Elston Research Associate KPNO 9/26/88 John Dunlop Manager, CFO NOAO C. Terminations.
date name position NOAO division
7/09/88 De Wayne Graham Manager, CFO NOAO 8/02/88 Francois Roddier Astronomer ADP 8/05/88 Leonard Sitongia Scientific Programmer I NSO 8/05/88 Charles Miller Scientific Programmer I NSO 9/02/88 Myron Smith Astronomer NSO 9/16/88 Oskar von der Luhe Assoc. Scientist NSO
D. Change of Status.
date name position NOAO division
8/03/88 Lonnie Cole Transfer from Sunspot to Tucson NSO 8/04/88 Ronald Probst Asst. Astronomer to Assoc. Astronomer KPNO 8/15/88 Brice Boxum Transfer from Sunspot to Tucson NSO
E. Summer Research Assistants.
date NOAO facility arrived name institution visited
7/11/88 Kimberly Leka Yale Coll., Connecticut NSO 7/18/88 Steven Chidester Michigan State U. NSO 7/25/88 Bernard Fleck U. of Wurzburg, Germany NSO IV. INSTRUMENTATION, NEW PROJECTS AND OBSERVATORY ACTIVITIES
A. Advanced Development Program.
1. ADP functions transferred to KPNO. As announced previously, the Advanced Development Program was dissolved as an NOAO division at the end of FY 1988. All of the remaining ADP scientific staff have been transferred to KPNO, and various projects are continuing as follows:
• 8-m Telescopes Project —Completion of the proposal to build two 8-m telescopes continues to be of highest priority for NOAO. The engineering staff in the New Telescope Technology program will continue to prepare for the polishing of a 3.5-m mirror and to develop the design of the 8-m telescopes.
• Adaptive optics —Support will continue for implementation of the prototype adaptive optics system on Kitt Peak. This work is expected to have both short-term and long-term payoffs (for existing and 8-m telescopes).
• Distributed array telescope - Fabrication of a prototype array will not be continued. NOAO continues to provide some organizational support for the "Interferometry Working Group"--formed in 1987 and made up of individuals in the field of interferometry.
• Coatings and gratings - Operation of the coatings laboratory will be transferred to NOAO's Engineering and Technical Services division and will be supervised by L. Daggert. The gratings laboratory has been closed.
2. 8-m proposal draft to be circulated. All three of the major sections of the 8-m telescope proposal have now been drafted: the scientific justification, the description of the first complement of instruments, and the description of the telescopes themselves. The first draft has been circulated for review within NOAO.
3. Optical designs for 8-m instruments. Optical design work has proceeded on several of the instruments to be included in the 8-m telescope proposal:
• Nasmyth beam-fed instruments - To eliminate the need for correctors or relay optics, a third secondary mirror option (f/12) will be added specifically for Nasmyth use. (The other two are f/6.6 for Cassegrain and fiber-fed Nasmyth instruments, and f/35 for infrared Cassegrain.) With the f/12 secondary, the Nasmyth focus will be moved another 2 m beyond the f/6.6 position. This brings it to an accessible point well outside the altitude journal of the telescope.
• Infrared focal reducer ~ For use at the f/35 Cassegrain focus an IR focal reducer has been designed to work in the 5 to 15 (im band. It has a 9 mm diameter pupil and terminates with an f/4 camera that gives an image spread over the detector of 24 (im (for the entire 5 - 15 |im wavelength range). The detector is assumed to have a diagonal radius of just under 1 arcmin. • Cassegrain wide-field imaging - The wide-field corrector design has now been effectively "frozen." For a special application using a mosaic of CCDs, the fused silica "dummy" window can be replaced by two 20 mm thick fused silica meniscus lenses that provide a plane focal surface. In this configuration the field of view is -22 arcmin in diameter, with a computed image quality of better than 0.15 arcsec in the spectral region from 0.365 to 1 }im. In the normal configuration (with windows instead of lenses) the field of view is slightly curved and has a diameter of 45 arcmin.
• Prime focus corrector - Although not finished to the level of the Cassegrain correctors, the prime focus corrector has been shown to be feasible and its design is ready for completion. The performance is 1/3 arcsec imaging (inevitably of lower quality than the Cassegrain imaging) over a field of 14 arcmin diameter, for 0.365 to 1 u.m. The final focal ratio is f/2.
4. Analysis of meniscus mirror supports. The meniscus mirror option for the 8-m telescopes has been analyzed and a support designed. So far, the analysis verifies the feasibility of this option as a means of achieving the 0.25 arcsec imaging specified for the 8-m telescopes. The next step in the analysis will be a rigorous treatment of the structural effects of the cooling channels. The elasticity relations in spherical coordinates are written in a finite-difference format and then solved with a stiffness-equilibrium algorithm. Such a solution is complementary to the finite-element approach and also to the analytical (thick-shell) analysis done at the European Southern Obs. The results indicate a solution similar to that found at ESO. The number of axial and transverse support units is 162 (compared with 152 in the ESO analysis). The NOAO supports are less complex (a counterweight replaces four of the bellows units) and the active force system is for error correction only.
5. Enclosures and control facilities for 8-m telescopes. During this quarter we investigated options for the telescope enclosure design and the separate control building for an 8-m telescope. After site visits to telescopes with different types of enclosures, we specified the enclosure requirements and sent the request for proposal to three companies with applicable experience. By the end of September, two firms had responded with proposals. We plan to consider three possible building shapes: dome-shaped, rectangular, and cylindrical.
Site development plans were begun for locations on the summit ridge of Mauna Kea (Hawaii) and on Cerro Pachon (a possible site in Chile). In addition to the telescope enclosure itself, supporting facilities comprise a control building (with computers, shops, and offices) and an 8-m recoating chamber. The architectural layouts include elevators for moving the primary mirror to and from the recoating chamber, and for exchange of the wide-field and infrared secondary mirrors. 6. Polishing and testing honeycomb mirrors. As the new driven-lap polisher at NOAO has been repolishing the 1.8-m prototype honeycomb mirror, a CCD camera and the Roddier FFT analysis technique have been used to measure the diminishing level of quilting over the honeycomb pockets. The amplitude of the quilting has now been reduced to 1/32 of a wave. We are encouraged to find that our optical measurements are sensitive down to this level of precision, which will be required for an 8-m telescope capable of producing 0.25 arcsec (FWHM) images. The Roddier method is what has made it routinely possible to do this quality of testing on timescales of just a few minutes. Only a few years ago, it took typically several days to test at the level of 1/10 wave.
10 We are continuing our analysis, design and prototyping of supports for a 3.5-m borosilicate glass blank. A system of 24 lateral supports (170 pounds per support) along with 66 active axial forces meets the imaging goal while keeping the stress level in the glass acceptably low. The prototype lateral support mechanism has been designed and built.
7. Adaptive optics at NOAO. An article in the August 9 issue of IAU Today reported on the adaptive optics projects at NOAO and other observatories. It summarized the August 6 tutorial in Baltimore, sponsored by Commission 9 (Instruments and Techniques) of the IAU. Here are some excerpts from the article entitled "Astronomers Adapt to New Optics," by Ronald A. Schorn:
- "Larry Goad (National Optical Astronomy Obs.) presented a survey of the field. The basic aim of using adaptive optics is to correct distortions in an incoming stellar wavefront that are produced by the Earth's atmosphere. Most systems now in development perform the corrections with a mirror whose surface can be warped in a precisely controlled manner. Several types of reflectors have been considered: segmented, continuous thin plates, "monolithic" (one variety uses a ceramic originally developed for capacitors), and the membrane or pellicle kind, which uses electrostatic deformation. In addition, the wavefront must be sensed in order to determine just what warping must be done, and sensor development is a vital part of all programs, such as the NOAO one Goad described. Alan Wirth (Adaptive Optics Associates) covered developments by his company, including some surprisingly compact configurations."
- "By popular demand, Fred Forbes (Kitt Peak National Obs.) gave a repeat performance of his talk on "bimorph" mirrors, which are made of piezoelectric lead titanate. One reflector under development at KPNO is segmented, with a diameter of 23 millimeters but a thickness of only 1 mm. A voice from the crowd informed the audience that many persons in the room could begin research on these mirrors immediately. If you have a digital alarm watch, just take it apart - there's a bimorph plate inside!"
B. GONG.
The Global Oscillation Network Group (GONG) is a community-based project to conduct a detailed study of solar internal structure and dynamics using helioseismology. In order to expoit this new technique, GONG is developing a six-station network of extremely sensitive, and stable solar velocity imagers located around the Earth to obtain nearly continuous observations of the Sun's "five-minute" oscillations, or pulsations. GONG is also establishing a major distributed data reduction and analysis system to facilitate the coordinated scientific investigation of the measurements.
Tests of the GONG prototype shelter's air conditioning and power backup systems were completed in August during Tucson's hottest summer on record. The shelter is now ready for installation at its test "field site." The site which was finally selected is adjacent to the U. of Arizona's track and field facility, located two km from the NOAO office in Tucson. The Arizona Board of Regents has given its final approval to the plan and the official ground breaking should occur early in the fall. In early August, the prototype lightfeed turret was removed from its position near the Hilltop facility on Sacramento Peak, disassembled, and shipped to Tucson for final testing
11 prior to integration into the prototype field station. L. Cole, B. Boxum, and A. Boxum (NSO) also made the trip west, where they have now joined the balance of the GONG instrument development team in Tucson.
Most of the instrument development activity continues to center around the Doppler analyzer breadboard, where the most critical elements of the GONG instrument are being tested. Integrated Sun tests have been completed and detailed evaluation of Texas Instrument's TC-241 virtual-phase CCD has begun. Tests of dynamic range, stability and noise all indicate satisfactory performance. There are still some questions about the linearity of the camera, and about photometric corrections which are required because of ac coupling early in the camera signal processing and because no shutter is used while the image is transferred for readout.
The balance of the breadboard activity has been carried out primarily by the opticians. F. Vaughn (NOAO) has assembled a second solid Michelson cube incorporating new mirror materials with the result that the temperature sensitivity has been reduced by a factor of 5. Vaughn has also produced an excellent single-element low-order quartz wave plate to establish the feasibility of making thin wave plates.
The analysis of the site survey has been updated to include data up to June 20, 1988. The performance of the GONG site survey network over a period of 588 days from November 10, 1986 to June 20, 1988 continues to be excellent; and in fact it has increased slightly since the last analysis of 407 days in April 1988. The range of duty cycles for the 12 possible networks is now 93.20 to 94.00%, up from 93.03 to 93.67% in April. The signal-to-noise ratio for the first daily harmonic now ranges from about 30,000 to 51,000 to 1, compared with the 19,000 to 29,000 to 1 obtained in April. The longest length of continuous clear time obtained remains at 418.58 hours, but the longest length of continuous dark time has increased to 12.82 hours, up from 10.22 hours in April. One site enjoyed 32 consecutive days of virtually unbroken sunshine. An interesting sidelight is that a periodicity of 1.653 u.Hz is becoming noticeable in the power spectra of the windows, and is now actually comparable in magnitude to the second daily harmonic. This new peak corresponds to a period of a week, and most probably reflects a periodicity in human society, rather than in the Sun or the Earth's atmosphere.
On the GONG data reduction and analysis front, some progress has been made on the artificial data project. This activity is designed primarily to produce realistic data sets which can be used to test and evaluate reduction pipeline software. Early this year, D. Hathaway (Marshall Space Flight Ctr.) generated two artificial images with steady flow velocity fields and oscillations and with ephemeris velocity effects for Sac Peak and for Haleakala. These were subsequently distorted with atmosphere effects and converted to phase intensities by F. Hill (NSO), B. Andersen (European Space Agency), and T. Brown (High Altitude Obs.). These images have been converted back to velocity, intensity, and modulation images and corrected for Earth-Sun ephemeris velocity. The next step will be to correct for atmospheric effects so that the two contemporaneous images can be merged.
A recent teleconference of the Artificial Data Science Team discussed the current status of the project. This included a review of how the artificial images were generated, a discussion of future direction for the correction and merge problem, an initial attempt to begin defining image quality both for the initial editing of the raw data and as a means of determining relative weighting for the merge of contemporaneous images, and a discussion
12 of how to proceed with the generation of artificial time series for the appraisal of mode frequency identification algorithms.
Another major activity of the GONG data reduction and analysis group is the development of a field tape reader system. Tests are underway to establish the performance and reliability of the Exabytes drives and media (Sony 8 mm camcorder and cartridge technology). To date, it appears that the Exabytes can provide the data density and performance needed for GONG data acquisition at an affordable price. However, some questions regarding reliability have appeared. The failure rate while writing full cartridges is approaching 30%. Hopefully, tape certification prior to use will eliminate all marginal 8 mm cartridges. Also, it is possible that future improvements to the Exabyte drive and to the quality of Sony 8 mm cartridges may alleviate this problem.
A symposium addressing the "Seismology of the Sun and Sun-like Stars" was held on Tenerife in the Canary Islands during the last week of September. In addition to their specific research presentations, GONG project staff members presented three poster papers detailing the current status of the major aspects of the project. F. Hill reported on the site survey effort, J. Harvey presented the GONG instrument design, and J. Pintar reported on the data reduction and analysis activity. J. Leibacher also presented a brief oral summary of all three papers to the assembled helioseismology community. These papers will be appearing in the meeting's "Proceedings" in the near future.
C. Instrumentation Projects.
During the last quarter, three major projects have entered the final stages of testing at CTIO; Argus and two prototype projects. Argus, the 4-m multifiber spectrograph, is fed from the CTIO 4-m prime focus by a head which currently has 12 positioners. Argus has been successfully tested on the telescope, and is now scheduled for visitor use on a limited basis. Test results indicate that the overall efficiency per fiber is roughly half that of the RC Spectrograph + Air Schmidt Camera; this value is what would be predicted by calculations of light losses in the optical fibers. Software and hardware developed for Argus permit auto-centering of the individual fibers on objects to be observed. This allows one to correct for error in the model of the 4-m prime focus field and errors in astronomers' object positions and thereby maximize throughput. A fiber-bundle "periscope" allows one to view the field of any fiber and manually adjust its position. Argus was designed to use a total of 24 fiber positioners. Now that it has been fully tested, the second set of 12 positioners is being fabricated, and will be added some time in 1989. Argus has the distinction of being the largest mechanical project undertaken at CTIO in recent years, and its success is in part a tribute to the excellence of the CTIO ETS staff.
A prototype television camera based on a cooled GEC TV-grade CCD has been constructed.
The CCD camera is conceptually rather similar to the Lick system, although designed from scratch (as recommended by L. Robinson, Lick Obs.) at CTIO. The camera head itself uses a thermoelectric cooler to cool the chip in order to permit long integrations; its small size permits it to be used in all applications where currently the RCA or Quantex cameras were used, as well as some where these cameras will not fit (specifically the CTIO 4-m autoguider; some repackaging to further decrease size will need to be done).
13 A prototype preprocessor for the infrared imager has been built and tested at CTIO and demonstrated in Tucson. At long wavelengths, ER arrays saturate very quickly (millisec) so normal procedure is to read out the array and co-add many frames on-line. For the shortest exposures our present data acquisition computers cannot accept the data and co- add it fast enough, so the solution is a dedicated preprocessor to do this. The device CTIO is using is an Inmos transputer. CTIO is presently completing interfacing of the preprocessor to the data acquisition computers for general use (as opposed to demonstration purposes). This should permit 5 (im imaging with the ER imagers, and is also serving as a conceptual basis for the new ER array controllers.
A number of minor projects associated with the ER imager include fabrication of spare electronic boards, installation of a new 12-position filter wheel, installation of new data acquisition software, and electronics modifications. This work has made the instrument more "user-friendly" and has also increased efficiency by up to a factor of 2 overall. A remotely controlled and more reliable slit mechanism was installed on the CTIO 1-m spectrograph. The Folded Schmidt Camera + 4-m 2-D Frutti detector system is now functional. This provides greater throughput with the 2-D Frutti than the old Singer camera. The Folded Schmidt is likely to see substantial future use with CTIO's regular CCD dewars (mainly TI 800 x 800 or Thomson 1024 x 1024).
The adaptive optics prototype instrument was brought to downtown Tucson and the mounts are being extensively modified and adapted to improve the alignment capabilities. Simple repairs to the electronic system were accomplished to eliminate noise problems that had previously limited system performance. Noise in the analog to digital converter may require redesign of this portion of the circuit.
A fiber optic cable was installed at the KPNO 2.1-m telescope, and baseline measurements of its performance as a data link were made. A Sun 3 computer was received for use in the ER development lab. It will be used to operate the 10 p.m arrays presently in hand for test, and to develop the control systems needed for transputer-based, fiber-linked instruments. Testing was completed on the detector mount to be used with the 10 (im arrays, and final wiring is proceeding. Various new control microcodes for the SBRC arrays have been developed and tried at the telescope. Successes were achieved in high speed applications for speckle observing and 5 |im operation. A germanium diode array, on loan from Hughes Aircraft Company, was tested but proved unsuitable for astronomical use. Fowler and Joyce (KPNO) visited the Air Force AMOS facility on Haleakala in Hawaii to study their use of closed cycle coolers for telescope instrumentation.
The KPNO ER Imager was used for ER speckle observing at the KPNO 4-m. Electronic and software modifications made for this run worked well and improved the data rate to a reasonable level. This instrument is now considered to be fully commissioned and the project is closed.
The Cryogenic Spectrometer was used for an operationally successful, scientifically productive observing run on the KPNO 4-m. Following this, the annual shutdown period in July-August was used for internal refurbishment. Problems identified during the spring test and evaluation observing runs were addressed, including vacuum leaks, grating control and readout, and additional filters. The instrument was back on the KPNO 1.3-m
14 telescope in September, where it suffered minor internal mechanical damage from a slippage of the grating mount while observing. There remain a number of performance and operational issues to be resolved before the instrument can be released for general use.
Our new mechanical engineer, T. Ellis, reported to work on July 15. His efforts have produced considerable progress in the mechanical and thermal design of the Cryogenic Optical Bench and the Cryogenic Echelle, our "second generation" infrared array instruments. These instruments will have a great commonality of design in the mechanical/thermal areas. In the CryoBench project, the instrument passed its final optical review. We will use ZnS rather than the standard ZnSe for lens elements. This material is somewhat experimental, but promises improved performance at 1.25 p.m and below. Operation on the KPNO 4-m telescope was a subject of considerable design effort and discussion; this telescope is optically incompatible with the 1.3-m and 2.1-m focal ratios. It was decided to press for fabrication of a new, f/15 secondary for the 4-m. The major hardware components and an unfinished blank are on hand from the original fabrication of the 4-m. Optical Coatings Labs, Inc. (OCLI) has been contracted to produce linearly wedged Fabry-Perot etalons for this instrument. The 2 |im linear variable filters received from OCLI were tested and perform well. The cryogenic test chamber was finished, and initial tests performed on the closed cycle cooler and mechanical sliders for the linear filters.
The optical design of the Cryogenic Echelle passed an internal review; the design is sufficiently complex and expensive that an external reviewer is being sought prior to commencement of fabrication. It was decided to use zerodur rather than diamond-turned aluminum as the optical substrate. The grating blank has been polished and delivered to the grating vendor for completion. T. Ellis has analyzed the dewar design for rigidity, and confirmed that a common basic design for CryoBench and CryoEchelle will perform well. Ellis has been in contact with D. Toomey, project engineer for the U. Hawaii cryogenic echelle. Communication between the two groups promises to conserve considerable effort.
Finally, a new guider for use with IR array instruments is being fabricated as a small project. In conjunction with an existing guider recently modified by mountain support personnel, this will equip us to operate multiple instruments simultaneously at our different telescopes. Improvements continue to be made on the KPCA during this quarter. Bringing the KPCA on line and keeping it on line is a lot less labor intensive in its upgraded state. Packaging of the user panel has also been finalized. During a test sequence the high voltage power supply for the micro channel plate (MCP) lost regulation and resulted in defects in two small areas on the MCP. We have positioned the detector such that the effects are minimized. The spare MCP has been received and prepared for tests. The mounting fixture for the long focus camera on the echelle spectrograph has been completed and tested. Static tests revealed some flexure and problem areas are to be reinforced to reduce the possibility of problems during the run in December.
When the UV enhancement technique was tried in testing TEK #2, there was no apparent improvement in the blue response. This is not all bad because the unenhanced blue response is comparable to the enhanced response of TEK #1. The UV enhancement did have a very strange effect on the device. It actually improved the horizontal charge
15 transfer efficiency (CTE), specifically the low level CTE (100 e' region). Using the bias overscan method with 100 e' charge the first pixel in the overscan contained an average of 2 e" when enhanced, compared to 20 e" for the same conditions unenhanced. This compares to 6 e" in TEK #1, which is considered to have excellent horizontal CTE. The enhanced condition lasts only as long as the dewar remains cold. Long-term tests have not yet been attempted. The results have been consistent on at least six iterations of the enhancement cycle. Combined with the other attributes, this device TEK #2 is an excellent CCD with only slightly higher readout noise (11 e) than TEK #1.
During the summer shutdown period all the dewars were cycled to perform routine maintenance and to make two specific improvements. First, all the shutter assemblies were modified so any dewar could be operated with the new 4-in mechanical interface. Second, we retested the quantum efficiency (QE) of all the dewars and extended the test range down to 240 nm. Using a newly acquired UV enhanced and calibrated diode we were able to make more accurate measurements. The results show improved blue response shortward of 400 nm and we are now in agreement with other facilities which have implemented UV enhancement.
The bad area on TI3 has been, at least for now, eliminated. The probable problem was a gate-to-gate high impedance short that leaked charge resulting in an area that bloomed with time and wreaked havoc with the bias overscan. During the shutdown, we removed TI3 from its clean dewar environment and plunged it into a dark hostile environment (a locker). Presumably, this four week vacation permitted an oxide growth which, for the present, will hold off (insulate) the gate-to-gate voltages without significant leakage. The results of two weeks testing downtown of two hour darks showed no detrimental effects and the device was restored to normal service. Coincident with the above, the device became completely discharged with virtually no blue response below 400 nm. After three iterations of UV enhancement the blue response had still not reached its pre-vacation high (by 3 to 5%).
The X-Y stages, auxiliary X-bearing, and Servo motors with electronic controls for the multi-fiber system for KPNO were received and testing was performed to verify operation. By the end of September the instrument mounting plate was constructed. The X-Y stages were coupled and affixed to it to allow preliminary software development. Technician support for the project was initiated for the construction of electronic interface cabling and rack-mounting/construction of additional electronic control hardware. Design concepts for the overall instrument housing and fiber plate and support were produced. After trips to Lawrence Livermore Labs and Durham U. to see their Fiber Actuating instruments and fiber button pickup heads, the decision was made to commit to an internal design of a mechanical gripper. The concept being currently developed allows for on-axis viewing of the fiber and sky. Specifications were developed and conceptual design begun. Additional magnet samples were obtained and prototype fiber buttons and fiber optic cable support schemes were examined. Initial tests of fibers with the right-angle prisms obtained earlier in the year were performed.
Completion of the conceptual design of the KPNO Bench Spectrograph and the ordering of parts and materials was completed during this quarter. However, lack of a dedicated" mechanical designer has prevented completion of the detailed design.
16 During July, the first interference filter bids were received. These were later evaluated and modified on the basis of scientific merit by the staff. Also, the Echelle (high resolution) operating configuration was analyzed and determined. This enabled required filter pass-bands to be more accurately specified and subsequent bids were prepared.
The two collimator blanks were received and inspected. Plans for short and long term collimator use on the spectrograph were formulated. A simple paraboloid will suffice for the larger blank. The smaller one will have two interchangeable surfaces, a sphere (for possibly a "Schmidt-Type" design) and a paraboloid. Prints were made and checked and both collimators entered the optical shop during the fourth quarter of FY 1988. Afterward, J. Simmons spent available remaining time laying the groundwork for a dedicated Bench Spectrograph camera.
During this period, the 5'x 8' optical table was received and inspected. The basic spectrograph room structure was also finished. This left only detail work to be done before the optical table could be moved in and prepared for optical/mechanical modules. A method for integrating the spectrograph with the existing and future 4-m cabling arrangements was devised, checked, and implemented. Involved scientists, instrumentation, and mountain personnel were given opportunities to make additions and modifications to the spectrograph operating system (spectrograph/BFFS Room/4-m structure). In addition, safety personnel have reviewed the system layout and action items were addressed.
A similar review process was undertaken with the design of the spectrograph components (or modules). Engineering, scientific, and instrumentation revisions were integrated into the layout and prepared for a mechanical designer. This included the addition of several calibration functions. Equipment was ordered and received for the 8-in Collimator Mount, the Focal Surface Module, and the Camera-Axis Sector Module. Available designer time allowed for the completion and manufacture of the 8-in Collimator Stand and start of the Focal Surface Module design. Discussions were continued with possible vendors for the grating rotary stage.
Ensuing discussions with T. Ingerson (CTIO) indicated that CTIO was going ahead full speed with the transputer technology development for the next generation CCD Controller/Instrument Controller/CTIO ER Controller/Processor. At this point in time the CCD controller development at KPNO is very closely coupled to the CTIO schedule, and KPNO's progress is directly dependent on CTIO's progress. KPNO has designed, prototyped and tested a power supply assembly that can be used with the new controller configuration. It was designed with high efficiency in mind and contains all the right voltages to drive any current CCD.
During this quarter, routine full disk observations of the Sun continued at the Vacuum Telescope at Kitt Peak with the new 11/73 computer. The capability to do area scan observations was further developed but still has some bugs. Nevertheless, the ancient Varian computer was finally retired from service. Reduction programs were certified and have now entered production with considerably improved results. Thanks to the efforts of L. Ramirez, a research assistant funded by the NSF REU-Minorities program, considerable progress has been made in reducing the four-year backlog of unreduced helium observations. Improvements to the magnetogram reduction algorithms have also been made and the past four years of those data should be rereduced when personnel are
17 available. A substantial number of routine requests for data from the synoptic archive arrived and were serviced. A capability for producing 4x4 inch prints on a nearly real time basis still awaits programmer availability.
D. Observatory Activities.
For the spring 1989 observing semester, KPNO received 212 observing proposals. This figure is down somewhat from the prior semester's total of 252. A five-year average for spring proposals received is 232. Beginning with this proposal deadline, astronomers were asked to send in 15 copies of each telescope proposal submitted to KPNO. At least 75% of astronomers who submitted proposals complied with this new procedure.
The surplus and used film processors for the Tucson photo lab have arrived, and a darkroom has been refurbished to accommodate them. These processors give us the ability to better process most black and white film. KPNO now has the ability to also process Ektachrome, 35-mm slides, make prints from slides and process, but not print, color negatives.
The summer shutdown on Kitt Peak proved to be very successful. This scheduled period permitted major accomplishments in the areas of maintenance, installation of new telescope improvements, and investigation of various telescope-related problems. Most of the summer shutdown work was focused on the 4-m, 2.1-m, #l-0.9-m, Coude feed, and McMath telescopes. Between these five telescopes, six large mirror surfaces were realuminized, numerous preventative maintenance activities were completed, and many mechanical and electronic systems were upgraded. These efforts will improve overall reliability, and facilitate maintenance on the telescope. Without this shutdown time, it would not have been possible to accomplish most of this work. No proposals requesting only the Intensified Image Dissector Scanner were received by the September 30 deadline. Therefore, this 2.1-m instrument will be retired immediately. It is replaced by the Gold Camera, a CCD spectrometer for low-to-moderate resolution spectroscopy, that has been tremendously popular among observers.
New Telescope Control Program Software (TCP) called VxWorks arrived and has been installed in the development VME system. A Sun workstation was ordered to use with VxWorks. This combination will provide a very strong development environment, and one identical with that being used by GONG. An object-oriented parser for the TCP command language was written and tested. Interface specifications for the Dome control module were written, and coding begun. The design of TCP is such that rather rapid code writing is expected for much of the rest of the system, particularly now that an object-oriented programming approach has been adopted.
New pointing maps were made for the 4-m Cassegrain and prime foci, the 2.1-m Cassegrain focus, and the 1.3-m and #2 36-in telescopes. These maps are now in use: further work on the large telescopes is still required. Pointing improvements were also made at the McMath.
During this quarter, M. Giampapa (NSO/T) assumed the role of Project Scientist for the McMath nighttime program of stellar spectroscopy, in addition to his present Observatory responsibilities. The new duties include the supervision of the entire nighttime program of synoptic and visitor observations, and the data reduction and archiving program.
18 Planning of instrument upgrades and modifications is also an integral part of the role of Project Scientist for this program. During this quarter, the DTI-221 video guider was installed and tested at the McMath. This effort has been led by D. Jaksha (NSO/T). The new guider extends our tracking and acquisition capabilities at the McMath for faint (V > 11.0) stars and thus represents a substantial improvement over our previous system.
CTIO's Chilean economic statistics, FY 1988:
Month %Change Cum. Change Avr. Monthly
Jul 0.1 10.0 278.98 Aug 0.8 10.9 280.46 Sep 0.9 12.0 285.06
19
V. PROGRAM SUPPORT
A. Director's Office.
The NOAO Computer Advisory Committee met on July 28 in Tucson. Agenda items discussed were: CCS long range plan, GONG computers, and ERAF. A summary of the major points raised and conclusions reached during the Executive session were reported to the NOAO Director on September 16, 1988.
Dear Colleague letter number three was reviewed by the AURA Board; an AURA safety team reviewed safety activities at Kitt Peak and Sac Peak in September; and E. Bloch, NSF, held a meeting in July that included representatives from Keck, Magellan, Columbus, the U. of Arizona, the MMT Upgrade, and NOAO. P. Bautz scheduled a followup meeting on July 23 in Tucson to discuss and plan for the U.S. program in optical ground-based astronomy.
The National Science Board sent people to Tucson, September 29 - 30, to review AURA's five-year contract renewal proposal for NOAO. A new centralized system for collecting publications information for the NOAO annual report was implemented. Four scientific staff members departed during this quarter; J. Beckers, R. Davies, J. Frogel, and M. Smith.
At the end of September, the maintenance contract for Hughes Calihan's NBI system was allowed to expire. The administrative offices of NOAO, at all three sites, are moving to PCs and various software packages, most notably WordPerfect.
B. Publications and Information Resources.
Summer saw a decline in the number of contacts and visits by media, film, and photographic visitors to Kitt Peak. During the July 1 - September 30, 1988 quarter there were two major efforts involving the media and Kitt Peak. The first was for a book on Arizona Historical sites. The second involved a local TV station filming a segment of their program "Beyond Bestsellers."
Other activities included: continued efforts toward the revising and updating of the AURA brochure and the Kitt Peak Walking Tour brochure, including contracting with a new printer and supervising the various phases required to obtain a final print of the brochure; considerable progress was made on a smaller informational brochure on Kitt Peak; established priorities, policies, and procedures concerning reprographics activities at NOAO/Tucson; finalizing arrangements for the AURA/NOAO exhibits at the AAS and IAU meetings; arranging for the discontinuation of NOAO's involvement in the NSF film loan program.
Normal activities for the office included filling photo/slide orders; answering a continual stream of public inquiries about NOAO and astronomy in general; and organizing a new semester of the Public Evening program, including developing and implementing new procedures for ticket sales.
C. Central Computer Services.
A Sun 386/i was ordered (with NASA grant funds) to allow an ERAF port to this
20 increasingly popular machine. Also, Apollo Computer Inc. has agreed to an indefinite loan of an Apollo DN3500 workstation to the ERAF group for the purposes of porting and supporting ERAF on the Apollo.
NOAO sponsored a visit by D. Phillips (U. of Washington, Seattle) to Tucson to work on a point-spread-function matching algorithm, to be included with the ERAF registration and mosaicing package.
The Varian computer era on Kitt Peak came to an end. The replacement program began in 1980, following the selection of the DEC 11/23 (later 11/24) for telescope and instrument control. The replacement program was planned to extend over three to four years, but owing to budget reductions was eventually stretched to nine years. The next generation control system is already under development.
A Sun 3/260 for the KPNO 1.3-m telescope was ordered, as were three small workstations for use in programming the telescope control system that will be first used at the KPNO 2.1-m next year.
The contract to complete the basic Kitt Peak optical fiber network was let. This will extend the existing net to reach the McMath complex and the KPNO #2 0.9-m telescope.
D. Central Administrative Services.
During this quarter CAS was involved in Addendum A to the FY 1988 Program Plan, the annual property inventory, a draft of an AURA Policies and Procedures Manual, an audit on contract compliance, and several employee programs. The NSF auditors also reviewed FY 1987 activity; no report has yet been issued.
G. Blevins attended an AURA-sponsored administrative retreat; J. Tracy attended meetings in Washington, D.C. to discuss preliminary results of an insurance review; and J. Ruffino attended a Tucson Urban League Employer Advisory Board meeting as well as two local seminars dealing with personnel issues.
The Personnel Office submitted the FY 1989 salary range recommendations to AURA; held affirmative action meetings for managers and supervisors in Tucson, at Kitt Peak, and at Sac Peak; issued summary annual reports of all benefit plans; and began the recruitment process for post-doctoral appointments. Additionally, they arranged several employee programs including membership for the Employees' Association in the Industrial Relations Council of Southern Arizona. Personnel also arranged an incentive program for Weightwatchers, and a health screening program by the Pima County Health Department.
E. Central Facilities Operations.
The prototype GONG shelter has been completed. This laboratory-style building will serve as the model for six additional identical buildings for the GONG Project. The effort required to build six more shelters is being reviewed. A decision on whether to fabricate these in-house or contract out the work will be forthcoming shortly. Bids were received for the roofing of the east wing of the NOAO headquarters building.
21 TELESCOPE USAGE STATISTICS Appendix A
Astronomica Observations Scheduled Maintenance, Engineering, Hours Instrument Tests, Scheduled Hours Used Hours Lost Equipment Changes, etc. Telescope Visitors Staff Weather Failure 4-m 1067.7 570.4 70.3 205.7 26.7 194.6
1.5-m 1064.2 413.9 132.9 367.3 24.8 125.3
1-m 671.8 307.7 88.3 193.7 4.9 77.2
CTIO 0.9-m 1019.0 499.2 144.1 331.7 5.2 38.8
*0.6/0.9-m 268.7 170.8 31.0 65.9 1.0 0.0
0.6-m 638.1 327.7 20.0 290.4 0.0 0.0
4-m 691.75 293.0 63.5 251.0 30.5 53.75
2.1-m 666.76 207.62 125.14 237.0 10.5 86.5
CF 353.0 105.3 81.2 84.0 12.0 70.5
KPNO 1.3-m 486.0 157.2 56.3 179.0 59.5 34.0
#l-0.9-m 426.75 191.0 93.5 88.5 12.25 41.5
#2-0.9-m 392.75 175.75 17.0 177.0 20.0 3.0
Schmidt 82.5 66.5 0 8.5 4.5 3.0
Hilltop 2472.0 989.0 435.0 903.0 145.0 0
Vac. Tower 1044.0 618.0 84.0 334.0 8.0 0
Evans Fac. 2133.0 611.0 295.0 1166.0 61.0 0
NSO **FTS Lab 925.0 128.0 0 5.0 0 792.0
**McMath 3146.5 150.0 89.0 442.0 41.5 2424.0
Vacuum 849.0 470.0 2.0 367.0 10.0 0
Note: Scheduled hours are calculated according to the ephemerides for CTIO: July - 12.3 hours/night; August - 11.8 hours/night; September - 10.9 hours/night. * Use restricted to dark of the moon. ** Totals include both day and night hours. (All others are day only.)
22
OBSERVATIONAL PROGRAMS APPENDIX B Cerro Tololo Inter-American Observatory
July-August-September: Individual telescope assignments are listed below. Graduate Students are indicated by an asterisk after their names. Nights assigned, (hours worked), and telescope used are included. Service Observing is denoted by S.O. instead of nights assigned.
C. Anguita and M.T. Ruiz, U. de Chile: "CCD Parallaxes for Faint High Proper Motion Stars", 3(29)1.5-m.
B. Anthony-Twarog, U. of Kansas: "Standard Fields for CCD uvby Observations", 4(44)0.9-m.
N. Caldwell, Whipple Obs., and R.A. Schommer, U. of Arizona: "A Search for Lyman a Emission from High Redshift Galaxies", 3(32)4-m.
L. Campusano, U. de Chile: "The QSO Redshift Distribution on the SGP Field", l(10)4-m.
M.T. Carini*, Georgia State U.: "An Investigation of Possible Short-Term Variations in Pks 2155-304 and Pks 1514-240", 7(63)0.9-m.
G. Cecil, Princeton U., J. Bland, U. of Hawaii, and D. DePoy, ADP: "Imaging Spectrophotometry of Ionized Filaments in the Galactic Wind of NGC 253", 3(ll)4-m.
S.G. Djorgovski, Caltech: a) "A Rich Cluster in Saggitarius?" b) "A Search for Obscured Globular Clusters", 3(37)4-m, 5(34)1.5-m, l(9)0.9-m.
O.J. Eggen, CTIO: "Intermediate Band and RI Photometry", 7(2)1.5-m
J.H. Elias, CTIO, G. Neugebauer, D.B. Sanders, B.T. Soifer, and P. Hacking, Caltech, and J.R. Houck, Cornell U.: "Cosmic Evolution of Infrared- Luminous Galaxies", 4(48)4-m, 4(27)0.9-m.
G. Fontaine, F. Wesemael, S. Demers, and R. Lamontagne, U. de Montreal, and M. Irwin, U. of Cambridge: "Follow-up Spectroscopic Observations of Blue Objects in the MC Survey", 3(30)4-m, 4(44) 1.5-m.
W.L. Freedman, MWLCO, I. Horowitz, J. Mould, and B.F. Madore, Caltech, J. Graham, Dept. of Terrestrial Magnetism, R. Schommer, Rutgers U., and N. Caldwell, Whipple Obs.: "Cepheid Distances to Sculptor Group Galaxies", S.O.(10)4-m.
L.M. French, MIT, S.J. Bus, Lowell Obs., and L.A. Lebofsky, U. of Arizona: "Shapes and Surface Properties of L5 Trojan Asteroids", 4(22)0.9-m. L.M. French, MIT, K. Russell, Siding Spring Obs., E. Bowell and S.J. Bus, Lowell Obs.: "A Search for L5 Trojan Asteroids", 6(35)MS.
D. Geisler, CTIO, and M.G. Lee*, U. of Washington: "Washington CCD Photometry of Galactic Globular Clusters", 4(33)0.9-m.
D. Geisler and A. McWilliam, CTIO: "Abundance Analysis of Very Strong Lined Giants", 2(18)1.5-m, 3(20)0.6-m.
M. Gregg, U. of North Carolina: a) "Integrated Light of Globular Clusters", b) "Red Spectra of Elliptical Galaxies", 3(31)4-m, 4(21)l-m, 301.5-m.
S.R. Heathcote and W.G. Weller, CTIO: "The Formation, Dynamics, and Excitation of Planetary Nebulae", 4(26)1.5-m, 3(14)MS.
J.P. Huchra, Smithsonian Astrophys. Obs., H. Corwin, U. of Texas at Austin, and R.P. Olowin, St. Mary's Coll.: "Redshifts of Southern Abell Clusters", 4(21)4-m.
S.O. Kepler, UFRGS, Brazil, F. Wesemael, S. Demers, and R. Lamontagne, U. of Montreal, and M. Irwin, U. of Cambridge, England: "Strbmgren Photometry of Hot Subdwarfs and White Dwarfs in the MC Survey", 4(22) 1.5-m, 3(29)1-m.
C.H. Lacey, U. of Arkansas: "Apsidal Motion in Eclipsing Binaries",ll(51)0.6-m.
D.L. Lambert, U. of Texas: "Spectroscopy of Field and Cluster Horizontal Branch A Stars", 3(37)4-m.
A.U. Landolt and R. Light, Louisiana State U.: 1) "UBVRI Photometric Sequences. I.", 2) "UBVRI Photometric Sequences. II.", ll(76)1.5-m. R. Light, Louisiana State U.: "Abundance Variations and Gradients in Sculptor and Fornax", 2(22)1.5-m, 3(33)0.9-m.
P.K. Lu, Western Connecticut State U.: "Photometry and Radial Velocity Observations of Faint Main-Sequence F-Stars to Determine the Galactic Gravitational Force K(z) Law", 7(39)l-m, 3(12)0.9-m, 3(19)MS. G. Madejski, NASA/Goddard, M. Urry and H. Bond, ST Scl: "Multiwave Variability Studies of x-ray Bright BL Lac Objects", 6(45)0.9-m.
M.A. Malkan and L. Spinoglio, U. of California, Los Angeles: "The Unbiased Bolometric Luminosity Function of Galaxies", 7(40)1.5-m.
J. Maza, U. de Chile, F. Mirabel, IAFE Argentina, and M.T. Ruiz, U. de Chile: "Determination of Systematic Velocities of a Sample of Seyfert Galaxies", 3(24)4-m. P.J. McCarthy, W. van Breugel, and H. Spinrad, U. of California, Berkeley, J.A. Peacock and J.S. Dunlop, Royal Obs. Edinburgh: "Spectroscopy of High Redshift Southern Radio Galaxies, 3(32)4-m.
B. McNamara, New Mexico State U., A. Mantegazza, Italy, Moore and Candy, Australia, M. Pena, U. Nacional de Mexico, A. Cox and W. Pesnell, New Mexico State U.: " A Photoelectric World-Campaign on 8 Scuti", 12(94)0.6-m.
A. McWilliam and D. Geisler, CTIO, "Abundance Analysis of HR1614 Group Stars", 2(18)1.5-m.
K.J. Meech, U. of Hawaii: "CCD Observations of Comets Active at Large Heliocentric Distances", 3(12)1.5-m, 3(17)MS.
C. Neese, KPNO: "The Velocity Dispersion-Age Relationship in the Inner Galactic Disk", 4(15)1.5-m, 5(61)0.9-m.
P. Nisenson, M. Karovska, C. Papaliolios, and C. Standley, Harvard- Smithsonian, and S. Heathcote, CTIO: "Speckle Imaging of SN1987A", l(ll)4-m.
P.S. Osmer, NOAO, S.J. Warren* and P.C. Hewett, U. of Cambridge, England: "The Space Density of Quasars with 3 T.D. Oswalt, Florida Inst, of Technology, P. Hintzen, NASA/Goddard SFC, E. Sion, Villanova U., and J. Liebert, U. of Arizona: "Spectroscopy of Faint White Dwarf Binaries", 4(22)4-m. C. Pennypacker, Lawrence Berkeley Lab., J. Middleditch, Los Alamos Nat. Lab., R. Muller, S. Perlmutter, J. Sasseen, P. Beard, L.-P. Wang, S. Yang, C. Smith, and F. Crawford: "Search for Pulsations from SN1987A and Other Objects, 2(12)4-m. B. Penprase* and L. Hobbs, U. of Chicago: "A Survey of Neutral Interstellar Gas in the Galactic Halo", 7(67)1.5-m. C.L. Perry, Louisiana State U.: "Interstellar Reddening of the Solar Neighborhood. II. The Southern Hemisphere", 31(151)9.6-m. R.C. Peterson, Whipple Obs.: "Oxygen Abundances in the Globulars 47 Tuc and NGC 6752", 4(47)4-m. M. Phillips, B. Gregory, M. Hamuy, S. Heathcote, J. Elias, M. Navarrete, N. Suntzeff, L. Wells, and R. Williams, CTIO: "Optical and Infrared Observations of SN1987A in the LMC", 4(31)1.5-m, 7(71)l-m. H. Quintana, A. Ramirez, and G. Herding, U. Catolica de Chile: "Survey of a Complete Sample of Dumb-Bell Galaxies", 5(41)l-m. M. Rao* and A.U. Landolt, Louisiana State U.: "A Study of Selected Open Star Clusters", 7(10)0.9-m. J.A. Rose, U. of North Carolina: "The Vertical Structure of our Galaxy", 10(101)MS. M. Roth and M.T. Ruiz, U. de Chile, M. Tapia, ESO and UNAM, P. Persi and M. Ferrari, Inst. Astrof. Spaziale: "IR and Visual Imaging of Bright IRAS Sources Associated with HII Regions", 2.5(20)1.5-m, 5(24)0.9-m. M.T. Ruiz, J. Maza, and M. Roth, U. de Chile: "IR Photometry of New Faint High Proper Motion Stars", 2.5(20)1.5-m. R. Schommer, Rutgers U., M. Suntzeff and T. Ingerson, CTIO, and E. Olszewski, U. of Arizona: "Accurate Radial Velocities with ARGUS", 2(22)4-m. J.C. Schields* and A. Filippenko, U. of California, Berkeley: "Narrow-Band Imaging of High-Inclination and Active Galaxies", 3(29)1.5-m, 4(46)0.9-m. G. Smith, ST Scl: "A Search for Ca II K Line Chromospheric Emission Among Globular Cluster Giants", 3(7)4-m. H.A. Smith, Michigan State U.: "Photometry of RR Lyrae Stars in the Metal-Rich Globular NGC 6388", S.O.(10)4-m. V.V. Smith and D.L. Lambert, U. of Texas: "High-Resolution Spectroscopy and Abundances of Bulge Giants in Baade's Window", 3(35)4-m. N.B. Suntzeff, M. Phillips, S. Heathcote, M. Hamuy, and A.R. Walker, CTIO: "Southern Spectrophotometric Standards", 2(23)4-m, 2(23)0.9-m. D. Terndrup, CTIO: "New Photometry Standards for CCD Observations", 4(17)0.9-m. J.R. Thorstensen, Dartmouth College, and P.A. Charles, Oxford U.: "Periods and Light Curves of Low-Mass x-ray Binaries", 8(100)0.9-m. B. Twarog and B.J. Anthony-Twarog, U. of Kansas, and J. Laird, Bowling Green State U.: 7(37)l-m, 5(32)0.6-m. J.A. Tyson, AT&T Bell Labs, S. Majewski*, Yerkes Obs., and R. Guhathakurka*, Princeton U.: "Primeval Galaxies: U-band Counts", 4(39)4-m. W. van Breugel and K. Ebneter, U. of California, Berkeley, E. Falmont, NRAO, and S. Heathcote, CTIO: "Spectroscopy of a Peculiar Depolarized Region in the West Lobe of Fornax A", S.O.(5)4-m. G. Wallerstein, U. of Washington: "Abundances of Key Elements in Globular Cluster Red Giants", 4(39)4-m. D.A. Weintraub*, U. of California, Los Angeles: "An Infrared Camera/Coronagraph Study of Nearby Circumstellar Disks", 3(20)4-m. R.E. Williams, CTIO: "Search for Line Huctuations in Old Novae", 5(18)l-m. YALE PROGRAMS: A. Sarajedini* and G. Da Costa: "Search for Blue Stragglers in Globular Clusters", 6(56)0.9-m. C. Heller: "Photometry of the Rapidly Oscillating Ap Star HD203932", 7(73)1-m. P.K. Lu: "A Program to Determine the Galactic Force Law Using Faint Main Sequence F-Stars", 15(107)l-m, 7(20)0.9-m. OBSERVATIONAL PROGRAMS - APPENDIX B - KITT PEAK NATIONAL OBSERVATORY Executed Proposals 07/01/88 - 09/30/88 Page 1 Mon Oct 10 14:43:15 1988 Nights Hours Days Hours 6708 f88 H Abt, National Optical Astronomy Observatories Improved study of Duplicity among F9-G1 Dwarfs. Coude Feed 4.00 15.00 0.00 0.00 9071 f88 J Africano, B Goodrich, National Optical Astronomy Observatories E Halbedel, Corralitos Observatory Sample of IRAS Sources Nr. 2 0.9 meter 5.00 0.00 0.00 0.00 7431 s88 f88 T Armandroff, C Pilachowski, National Optical Astronomy Observatories Kinematics as a Function of Age in the Galactic Halo 2.1 meter 6.00 14.00 0.00 0.00 7408 f88 B Balick, University of Washington I Gatley, National Optical Astronomy Observatories B Zuckerman, University of California, Los Angeles What Shapes the Envelopes of Planetary Nebulae? 1.3 meter 5.00 20.00 0.00 0.00 7465 f88 S Berrick, K Anderson, New Mexico State University Spiral Density Waves and Star Formation Nr. 1 0.9 meter 5.00 52.00 0.00 0.00 7522 f88 M Bershady, R Kron, University of Chicago, Yerkes Obs. K Band Imaging of Distant Galaxies: Post-Main Sequence Evol 4 meter 4.00 43.75 0.00 0.00 7473 f88 R Boyle, D Jennings, G Wiedemann, NASA Goddard Space Flight Center J Keady, Los Alamos National Laboratory Mass Loss From Heavily Obscured Carbon Stars 4 meter 3.00 1.25 3.00 2.50 Executed Proposals 07/01/88 - 09/30/88 Page 2 Mon Oct 10 14:43:15 1988 Nights Hours Days Hours 7350 f88 J Brown, H Johnson, Indiana University K Hinkle, National Optical Astronomy Observatories 10830 in MS/S Stars 4 meter 0.00 0.00 2.00 8.00 7351 f88 H Bushouse, NASA Ames Research Center Optical Photometry of Interacting and Merging Galaxies 1.3 meter 5.00 26.50 0.00 0.00 7529 f88 K Chambers, Johns Hopkins University W van Breugel, University of California, Berkeley G Miley, Space Telescope Science Institute Imaging of High-Redshift Galaxies 4 meter 2.50 16.50 0.00 0.00 7421 f88 R Ciardullo, National Optical Astronomy Observatories H alpha Observations of Novae in Local Group Galaxies Nr. 1 0.9 meter 2.00 22.50 0.00 0.00 7157 s88 D Crabtree, Dominion Astrophysical Observatory C Rogers, P Martin, University of Toronto Distribution of Dust in Circumstellar Envelopes 2.1 meter 4.00 29.00 0.00 0.00 7405 s88 f88 R Dufour, P Mitra, Rice University R Parker, NASA Headquarters J Hester, California Institute of Technology Spectrophotometry of Filaments & Knots in the WR Shell Nr. 2 0.9 meter 12.75 81.00 0.00 0.00 7476 f88 P Eisenhardt, A Chokshi, NASA Ames Research Center S Djorgovski, California Institute of Technology H Spinrad, University of California, Berkeley Infrared Imaging and Photometry of High Redshift Galaxies 4 meter 3.00 30.00 0.00 0.00 Executed Proposals 07/01/88 - 09/30/88 Page 3 Mon Oct 10 14:43:15 1988 Nights Hours Days Hours 7550 f88 J Frogel, R Davies, National Optical Astronomy Observatories Is there a central concentration of late type giants in M31 4 meter 3.00 20.00 0.00 0.00 7411 f88 I Gatley, R Probst, D DePoy, National Optical Astronomy Observatories Massive Star Formation in the Galaxy 1.3 meter 4.00 30.00 0.00 0.00 7286 s88 M Giampapa, National Optical Astronomy Observatories J Bookbinder, University of Colorado A Beasley, University of Sydney The Chromospheres and Coronae of K Dwarf Stars 2.1 meter 1.00 7.50 0.00 0.00 7300 s88 D Hamilton, National Optical Astronomy Observatories Multicolor CCD Photometry of Faint Red Galaxies 2.1 meter 6.00 3.00 0.00 0.00 7491 f88 C Haswell, E Robinson, A Shafter, University of Texas, Austin A Radial Velocity Study of Low-Mass X-ray Binary V1727 Cyg 4 meter 3.00 3.00 0.00 0.00 7485 f88 J Hester, S Kulkarni, California Institute of Technology W Blair, Johns Hopkins University R Fesen, University of Colorado J Raymond, Harvard-Smithsonian Center for Astrophysics Echelle Spectroscopy of CTB 80 4 meter 3.00 14.75 0.00 0.00 Executed Proposals 07/01/88 - 09/30/88 Page 4 Mon Oct 10 14:43:15 1988 Nights Hours Days Hours 7486 f88 J Hester, California Institute of Technology J Raymond, Harvard-Smithsonian Center for Astrophysics D Cox, University of Wisconsin R Braun, National Radio Astronomy Observatory, VLA Echelle Spectroscopy of the Cygnus Loop SNR 4 meter 3.00 19.50 0.00 0.00 7425 f88 P Hodge, University of Washington The HII Regions of IC 1613 2.1 meter 3.50 32.00 0.00 0.00 7518 f88 K Janes, Boston University L Marschall, Harvard-Smithsonian Center for Astrophysics CCD Photometry of Young Open Clusters Nr. 2 0.9 meter 1.00 2.50 0.00 0.00 7240 s88 D Jewitt, J Luu, Massachusetts Institute of Technology Investigation of Planet-Cross Asteroids Nr. 1 0.9 meter 7.00 22.50 0.00 0.00 7458 f88 C Joseph, Princeton University The 3.1 Micron Ice Feature and Anomalous Extinction 1.3 meter 4.00 23.50 0.00 0.00 7384 f88 T Kinman, N Sharp, National Optical Astronomy Observatories CCD Images of the Fields of the Nearer RR Lyrae Stars Nr. 1 0.9 meter 2.00 20.00 0.00 0.00 7210 s88 S Kleinmann, M Tamura, University of Massachusetts I Gatley, National Optical Astronomy Observatories The Stellar Population of the Galactic Center 1.3 meter 6.00 10.50 0.00 0.00 Executed Proposals 07/01/88 - 09/30/88 Page 5 Mon Oct 10 14:43:15 1988 Nights Hours Days Hours 7243 s88 D Koo, Space Telescope Science Institute M Bershady, S Majewski, J Munn, University of Chicago, Yerkes Obs. The Quasar Luminosity Function at Faint Magnitudes and .... 4 meter 3.00 1.50 0.00 0.00 7492 f88 E Lada, N Evans II, University of Texas, Austin I Gatley, D DePoy, National Optical Astronomy Observatories Near-IR Survey of Dense Molecular Cores in the Orion B 1.3 meter 3.00 28.00 0.00 0.00 7137 s88 D Lambert, V Smith, University of Texas, Austin Infrared Spectroscopy of Obscured Late-type Stars Observed. 4 meter 4.00 23.50 4.50 4.50 7079 s88 A Landolt, Louisiana State University Space Telescope Spectrophotometric Standard Stars. 1.3 meter 9.00 25.50 0.00 0.00 9072 f88 A Landolt, M Rao, Louisiana State University UBV Photometry of Stars Useful for Checking Equipment... Nr. 2 0.9 meter 6.00 39.25 0.00 0.00 7516 f88 T Liu, K Janes, Boston University Radial Velocities of Field RR Lyrae Stars 2.1 meter 2.00 21.00 0.00 0.00 7443 f88 E Malumuth, Space Telescope Science Institute (CSC) G Kriss, H Ferguson, W Dixon, Johns Hopkins University The Distribution of Galaxy Orbits in X-ray Bright Clusters. 4 meter 2.75 26.50 0.00 0.00 Executed Proposals 07/01/88 - 09/30/88 Page 6 Mon Oct 10 14:43:15 1988 -men coo Nights Hours Days Hours /Ujy x 8 8 P Massey, Kitt Peak National Observatory T Armandroff, S Barden, National Optical Astronomy Observatories P Conti, University of Colorado The Hot, Massive Stellar Content of Local Group Galaxies. 4 meter 3.00 31.50 0.00 0.00 7060 f88 P Massey, Kitt Peak National Observatory J Barnes, E Anderson, National Optical Astronomy Observatories Faint Spectrophotometric Standards. 2.1 meter 5.00 25.00 0.00 0.00 7324 f88 P Massey, Kitt Peak National Observatory Wolf-Rayet Stars with Compsoite WN/WC Type: Binaries or... 2.1 meter 3.00 24.00 0.00 0.00 Coude Feed 5.00 36.50 0.00 0.00 7346 f88 P Massey, Kitt Peak National Observatory P Conti, University of Colorado Near-Infrared Spectrophotometry of Wolf-Rayet stars 2.1 meter 2.75 26.00 0.00 0.00 6721 f88 H McAlister, W Hartkopf, J Sowell, Georgia State University 0 Franz, Lowell Observatory Binary Star Speckle Interferometry. 4 meter 5.00 33.75 0.00 0.00 9069 f88 C Neese, S Wolff, National Optical Astronomy Observatories B Stars in Anticenter HII Regions Nr. 1 0.9 meter 2.00 23.00 0.00 0.00 7338 f88 M Oliveri, A Witt, University of Toledo Dust Luminescence in Planetary Nebulae 2.1 meter 4.00 38.50 0.00 0.00 Executed Proposals 07/01/88 - 09/30/88 Page 7 Mon Oct 10 14:43:15 1988 Nights Hours Days Hours 9067 s88 1 R Patterson, Southwest Missouri State University Obtain Scans of F, G and K Spectral Class Supergiants Nr. 2 0.9 meter 4.00 3.00 0.00 0.00 6817 f88 C Pilachowski, J Africano, B Goodrich, B Binkert, National Optical Astronomy Observatories Sky Brightness on Kitt Peak Nr. 2 0.9 meter 3.00 9.50 0.00 0.00 9066 s88 A Porter, National Optical Astronomy Observatories Narrow Band Imaging of Parent HII Regions of Extragalactic. Nr. 1 0.9 meter 5.00 28.00 0.00 0.00 9068 s88 A Porter, National Optical Astronomy Observatories Spectroscopy of CaOH in M Dwarfs 2.1 meter 6.00 19.00 0.00 0.00 6637 f88 L Ramsey, D Huenemoerder, Pennsylvania State University S Barden, National Optical Astronomy Observatories Spectroscopic Monitoring of RS CVn and Related Systems. 2.1 meter 5.00 47.00 0.00 0.00 Coude Feed 10.00 90.00 0.00 0.00 7369 f88 M Rao, A Landolt, Louisiana State University A Photometric Study of Selected Galactic Clusters Nr. 1 0.9 meter 3.00 20.00 0.00 0.00 1.3 meter 4.75 37.50 0.00 0.00 7557 f88 R Remillard, Massachusetts Institute of Technology W Roberts, Harvard-Smithsonian Center for Astrophysics Optical Identification of HEAO-1 X-ray Sources Burrell Schmidt 7.75 66.50 0.00 0.00 Executed Proposals 07/01/88 - 09/30/88 Page 8 Mon Oct 10 14:43:15 1988 _,,„„ Nights Hours Days Hours 7447 f88 P Schmidtke, Arizona State University J Africano, National Optical Astronomy Observatories Lunar Occultations of Double Stars Nr. 2 0.9 meter 4.00 15.00 0.00 0.00 7304 s88 M Smith, National Optical Astronomy Observatories R Polidan, University of Arizona The Site of Nonradial Mode Excitation in B Stars: V356 Sgr 2.1 meter 4.00 15.75 0.00 0.00 7139 s88 D Soderblom, Space Telescope Science Institute Testing the Authenticity of Stellar Kinematic Groups Coude Feed 5.00 7.50 0.00 0.00 7422 f88 P Szkody, University of Washington Optical and IR Colors of A Large Sample of Novae Nr. 1 0.9 meter 3.00 25.50 0.00 0.00 1.3 meter 4.00 11.00 0.00 0.00 7424 f88 P Szkody, University of Washington Simultaneous Light Curves with GINGA Nr. 1 0.9 meter 5.75 55.00 0.00 0.00 7119 s88 T Tsuji, Tokyo Astronomical Observatory S Ridgway, K Hinkle, National Optical Astronomy Observatories Spectroscopy of Circumstellar Envelopes of Late-type Giants 4 meter 1.00 12.00 0.50 6.00 7449 f88 E Turner, Princeton University B Burke, S Conner, Massachusetts Institute of Technology D Schneider, Institute for Advanced Study J Hewitt, Haystack Observatory CCD Observations of VLA Gravitational Lens Candidates 4 meter 3.00 20.00 0.00 0.00 Executed Proposals 07/01/88 - 09/30/88 Page 9 Mon Oct 10 14:43:15 1988 7444 f88 Nights Hours Days Hours A Uomoto, Johns Hopkins University Observations of Population I Supernovae 2.1 meter 4.00 31.00 0.00 0.00 7265 s88 G Wahlgren, Space Telescope Science Institute (CSC) Ca II K-Line Emission in RV Tauri and SRd Variables Coude Feed 5.00 37.50 0.00 0.00 7537 f88 W Waller, M Lee, M Ward, University of Washington D DePoy, National Optical Astronomy Observatories Ionized and Molecular Hydrogen in Extragalactic Starbursts 1-3 meter 500 %QQ Q^Q QQQ 7427 f88 M Ward, L Bryant, University of Washington CCD Imaging of AGN Observed with the Infrared Camera Nr- 1 0-9 meter 4.00 16.00 0.00 0.00 7204 f88 E Weis, A Upgren, Wesleyan University Photometry of a Complete Sample of Nearby Stars. Nr. 2 0.9 meter 7.00 42.50 0.00 0.00 7250 s88 R Windhorst, Arizona State University Spectroscopy of Primeval Radio Galaxy Candidates 4 meter 5.00 23.00 0.00 0.00 7070 s88 E Wright, University of California, Los Angeles R Joyce, Kitt Peak National Observatory J Katz, Washington University Infrared Spectrometry of Cygnus X-3 4 meter 2.00 15.00 0.00 0.00 Total number of proposals: 62 OBSERVATIONAL PROGRAMS APPENDIX B National Solar Observatory Quarter Ended: 9/30/88 1023 R Altrock, National Optical Astronomy Observatories S/B003-Coronal Observations Evans Solar Facility/SP 1161 R Altrock, National Optical Astronomy Observatories D Sime, High Altitude Observatory S/B181,230-Coronal Transient Patrol Supts SMM Evans Solar Facility/SP 1369 R Altrock, L Gilliam, National Optical Astronomy Observatories S/B224-Daily Solar Activity Report for Solar Forecasting Evans Solar Facility/SP 1212 P Bernath, C Brazier, M Lee, M Oliphant, University of Arizona D Carrick, U.S. Air Force Astronautics Lab T/Spectroscopy of Molecules of Astrophysical Interest McMath FTS Lab 1384 D Bonaccini, Instituto de Astronomia R Falciani, Osservatorio Astrofisico di Arcetri SAT320-2D Spectroscopy Vacuum Tower/SP 1435 D Bonaccini, Instituto de Astronomia L Smaldone, Capodimonte Astronomical Observatory S/B242-Spectra 3550-9000 Evans Solar Facility/SP 1355 B Bopp, P Noah, R Dempsey, University of Toledo T/Doppler "Snapshots" of UX Ari VII Tau and HD 199178 MCMM 1 1382 M Darvann, University of Oslo R Dunn, National Optical Astronomy Observatories SAT317-Adaptive Optics LEST Seeing Test Vacuum Tower/SP 1138 D Deming, NASA Goddard Space Flight Center T/Monitoring Apparent Velocity of Integrated Sunlight MCMM 1380 F Deubner, M Fleck, Institut fur Astronomie und Astrophysik S/T314-Dynamics of the Active Solar Atmosphere (DYNASOARE) Vacuum Tower/SP 1180 G Elste, University of Michigan S/B183-Limb Darkening Freed from Scattered Light in Telescp Evans Solar Facility/SP 1216 O Engvold, D Elgaroy, E Jensen, University of Oslo T/Star Spots on the RS CVn Variable II Pegasi MCMM 1219 M Giampapa, National Optical Astronomy Observatories T/Ha Emission & Rotation in Selected dM Stars MCMM 1353 M Giampapa, S Wolff, National Optical Astronomy Observatories T/Li I A6707 Strength and Activity in F Dwarf Stars MCMM 1387 M Giampapa, National Optical Astronomy Observatories S/B231-Joint Response to Call K and He ID3 Lines to.... Evans Solar Facility/SP 5273 M Giampapa, National Optical Astronomy Observatories T/Simultaneous Call Resonance Line & Infrared H&K ... MCMM 1025 L Gilliam, National Optical Astronomy Observatories S/B057-Monitoring:Community Evans Solar Facility/SP 1026 L Gilliam, National Optical Astronomy Observatories S/B062-Coronagraph Monitor Evans Solar Facility/SP 1034 L Gilliam, National Optical Astronomy Observatories K Strand, High Altitude Observatory S/H001-Flare Patrol (Monitoring) Hilltop Dome/SP 1035 L Gilliam, National Optical Astronomy Observatories S/H002-White Light Patrol (Monitoring) Hilltop Dome/SP 1036 L Gilliam, National Optical Astronomy Observatories S/H003-Multiple Bank Polarimeter (Monitoring) Hilltop Dome/SP 1039 L Gilliam, National Optical Astronomy Observatories S/H008-White Light Sunspot Drawing Hilltop Dome/SP 1126 L Gilliam, National Optical Astronomy Observatories S/BOlO-Hcc Slitjaw Movie Evans Solar Facility/SP 1169 L Gilliam, National Optical Astronomy Observatories S/B007-USG/Disk Activity Program Ha SJC, Spectra... Evans Solar Facility/SP 1349 S Habbal, Harvard-Smithsonian Center for Astrophysics K Harvey, %KPNO R Gonzalez, National Radio Astronomy Observatory T/Multiwavelength Observations of Time-Varying Phenomena... Solar Vacuum 3790 J Harvey, National Optical Astronomy Observatories T/Vacuum Synoptic Program:Daily/Community Solar Vacuum 1432 H Jones, NASA Goddard Space Flight Center T/ISM-International Solar Month Support of Magnetograms Solar Vacuum 1379 R Killen, Rice University T Morgan, NASA Johnson Space Flight Center T/Spatially Resolved Observations of the Saturaian Atmos MCMM 1305 S Koutchmy, C.N.R.S. S/B205-Spectroheliograms, CaK Ha Evans Solar Facility/SP 1436 S Koutchmy, C.N.R.S. S/B243-Coronal Observations in Conjunction with Evans Solar Facility/SP 1437 M Kundu, University of Maryland S/B244-Spectroheliograms Ha, CaK Evans Solar Facility/SP 1381 D Landi, Universita di Firenze S/T316-Investigation on Line of Sight Magnetic Fields... Vacuum Tower/SP 1383 B Lites, D Tomczyk, High Altitude Observatory/NCAR D Elmore, High Altitude Observatory/NCAR S/T318-Lab Measurements for the Advanced Stokes Polarimeter Vacuum Tower/SP 1149 W Livingston, L Wallace, National Optical Astronomy Observatories T/Solar Irradiance Line Bisectors MCMM 1209 W Livingston, L Wallace, National Optical Astronomy Observatories M Steffen, Kiel University T/Spectrum Irradiance Variability of Sun MCMM 1135 P Mcintosh, National Oceanic & Atmospheric Admin.,Boulder L Gilliam, National Optical Astronomy Observatories D Marquett, California Institute of Technology S/B001-NOAA Monitoring Program Evans Solar Facility/SP 1136 H Neckel, Hamburger Sterawarte D Labs, Landessternwarte Heidelberg D Marquett, California Institute of Technology T/FTS Spectra MCME 1150 H Neckel, Hamburger Sterawarte D Labs, Landessternwarte Heidelberg T/Limb Darkening MCMM 1433 D Neidig, Sacramento Peak Observatory S/H032-SMM Backup for Sept Hilltop Dome/SP 1316 L November, National Optical Astronomy Observatories S/H022-Proper Motion Hilltop Dome/SP 1235 A Pierce, National Optical Astronomy Observatories T/Solar Gravitational Redshift MCMM 1223 A Potter, T Morgan, NASA Johnson Space Flight Center T/Spatial Distribution of Sodium & Potassium in Atmos... MCMM 1307 A Potter, T Morgan, NASA Johnson Space Flight Center T/Search for a Sodium and Potassium Atmosphere on the Moon MCMM 1390 R Radick, High Altitude Observatory S/B234-Effect of Activity on Stromgren Color Indices Evans Solar Facility/SP 1057 S Saar, Harvard-Smithsonian Center for Astrophysics J Linsky, University of Colorado T/A Survey of Magnetic Fields on Late Type Stars MCMM 1123 S Saar, Harvard-Smithsonian Center for Astrophysics J Linsky, University of Colorado M Giampapa, National Optical Astronomy Observatories T/Synoptic Observations of Stellar Magnetic Fields ... MCMM 1363 D Schmidt, Kiepenheuer Institut fur Sonnenphysik O von der Luhe, National Optical Astronomy Observatories S/T312-Properties of Solar Granulation in Magnetic... Vacuum Tower/SP 1027 E Seykora, East Carolina University R Smartt, National Optical Astronomy Observatories S/B113-Differential Photometry Limb Darkening Evans Solar Facility/SP 1131 E Seykora, East Carolina University S/B174-CaK, Ha Spectroheliograms Evans Solar Facility/SP 1251 E Seykora, East Carolina University S/B191-Investigation of Very Low Contrast White Solar.... Evans Solar Facility/SP 1434 E Seykora, East Carolina University S/B241-Ha Spectroheliograms from -l.oA to +1.0A 70 -mm Evans Solar Facility/SP 1309 K Sivaraman, S Bagare, Indian Institute of Astrophysics R Mann, National Optical Astronomy Observatories S/T290-Search for the Foot Points of the Sub-arc Second.... Vacuum Tower/SP 1037 R Smartt, National Optical Astronomy Observatories S/H004-Coronal One-Shot (Monitoring) Hilltop Dome/SP 1053 M Smith, B Patten, National Optical Astronomy Observatories T/Radial Velocity Variations of Alpha Ori and Two Other... MCMM 1113 R Smithson, European Southern Observatory S/T239-Solar Fine Structure Observations w/Active Mirror Vacuum Tower/SP 1375 G Stark, Wellesley College T/Spectroscopy of the h20+ A-K system McMath FTS Lab 1374 C Stoker, R Haberle, T Roush, D Freedman, NASA Ames Research Center B Rizk, University of Arizona T/Seasonal Variation of Water Vapor in Southern Hemisphere. McMath FTS Lab 1210 O White, Lazy FW Ranch T/Sun as a Star: Ca II Profile Measurements MCMM 1391 D Wiehr, Universitaetssternwarte S/B235-Emission Lines in Prominences Evans Solar Facility/SP 1024 S Worden, OSUDRE/ADEW S Keil, National Optical Astronomy Observatories S/B044-Solar Rotation 3898-3954 A Evans Solar Facility/SP 1081 H Yoshimura, University of Tokyo S/H017-Birth & Evolution of Sunspots Hilltop Dome/SP 1388 J Zirker, National Optical Astronomy Observatories S/B232-Prominence Formation Evans Solar Facility/SP 1358 O von der Luhe, National Optical Astronomy Observatories D Rimmele, Kiepenheuer Institut fur Sonnenphysik S/T307-Correlation Tracker Tests Vacuum Tower/SP 1422 O von der Luhe, National Optical Astronomy Observatories S/T319-Stokes V Imaging with High Spatial Resolution Vacuum Tower/SP