National Optical Astronomy Observatories
National Optical Astronomy Observatories
Quarterly Report
October - December 1989
National Optical Astronomy Observatories
Quarterly Report
October - December 1989
TABLE OF CONTENTS
I. INTRODUCTION 1
II. SCIENTIFIC HIGHLIGHTS 2
A. The Brightest Hydrogen Emission Region in the Small Magellanic Qoud . . 2 B. Measurements of Stratospheric Hydrogen-Fluoride (HF) 2 C. Rotation of Solar Active Regions 3 D. Reduction of the South Pole Data 3 E. The Effect of Large-Scale Flows on Oscillation Ring Diagrams 3 F. The Kinematics of Very Low Mass Galaxies: Is Dark Matter Ubiquitous? . . 4 G. Outflows in YSOs: Dynamics Revealed by New Technology 4
III. PERSONNEL 6
A. Visiting Scientists 6
IV. INSTRUMENTATION, NEW PROJECTS AND OBSERVATORY ACTIVITIES 7
A. Future Telescope Technology Program (FTT) 7 B. Global Oscillation Network Group (GONG) 7 C. Instrumentation Projects 9 D. Observatory Activities 13
V. PROGRAM SUPPORT 15
A. Director's Office 15 B. 8-M Office 18 C. Central Administrative Services 18 D. Central Computer Services 18 E. Central Facilities Operations 19 F. Engineering and Technical Services 20 G. Publications and Information Resources 20
Appendices
Appendix A Telescope Usage Statistics Appendix B Observational Programs Appendix C Annual Safety Report
I. INTRODUCTION
This quarterly report covers scientific highlights for the period of October - December 1989, as well as personnel changes for the period. Highlights emphasize concluded projects rather than work, in progress. The report also discusses new technology for telescopes and instrumentation, GONG, instrumentation projects, and observatory activities. The Engineering and Technical Services division now submits reports for the instrumentation projects, with contributions from program scientists, if necessary. The Associate Directors for CTIO and NSO continue to provide the information of efforts at La Serena/Cerro Tololo and Sacramento Peak. Activities of the NOAO units are included, and the appendices list telescope usage statistics, observational programs, and the NOAO annual safety report.
H. SCIENTIFIC HIGHLIGHTS
A. The Brightest Hydrogen Emission Region in the Small Magellanic Cloud.
The most prominent and strikingly beautiful feature of the Small Magellanic Cloud is a large, bright (H II) region of hydrogen emission, designated as NGC 346, found in the northern part of this nearby galaxy. The source of ionizing radiation has long been suspected to be luminous stars with extremely high photospheric temperatures. In 1978 CTIO staff astronomer N.R. Walbom found, with the CTIO 4-m telescope, two such stars near the center of NGC 346. One of the stars, designated as NGC 346-1, was so hot and luminous (spectral type 04 III) that it was spectroscopically similar to Zeta Puppis, which is suspected to be one of the most luminous galactic stars known. However, as Walbom recognized, NGC 346-1 by itself could not produce the required ionizing radiation. This star was, however, part of a cluster of luminous stars. Indeed Walbom, who by 1986 had become a staff member at the Space Telescope Science Inst, and his collaborator J.C. Blades (European Space Agency) found, with the Anglo-Australian 3.9-m telescope, another extraordinarily luminous star in that cluster. Designated as NGC 346-3, the contribution of this new star (of spectral type 03 III) appeared to be comparable to that of NGC 346-1, but Walbom and Blades concluded that an assessment of their role in the total required ionization had to await further studies.
Recently, P. Massey (KPNO), collaborating with J.W. Parker and CD. Garmany (U. of Colorado), reobserved at CTIO the central cluster in NGC 346. Photometry with the 0.9-m telescope and spectroscopy with the 4-m telescope of 42 cluster members identified 33 hot, luminous (0 type) stars, doubling the total number of such stars previously known in the Small Magellanic Cloud. The total ionizing flux of all the hot stars now known to exist within NGC 346 is consistent with the brightness of the hydrogen H n emission regioa Furthermore, and astrophysically more interesting, is the fact that the cluster contains very young bright stars estimated to fall in the mass range 40 to 85 solar masses~at the upper known limit of stellar masses. Thus this group of stars shows how extremely massive stars may be distributed in a star forming region and confirms their existence in significant numbers in the Small Magellanic Cloud. In addition, there is a group of somewhat older less massive stars; five of them are probably red supergiants and two are blue supergiants with masses estimated at about 15 solar masses. The presence of the evolved stars together with the more massive stars is not only an example of how massive stars evolve, but is evidence that one can not always assume, as is usually taken for granted, that all members of a star cluster field are coeval.
B. Measurements of Stratospheric Hydrogen-Fluoride (HF).
The molecule hydrogen-fluoride is one of several end products from a series of chemical reactions originating from the industrial release of fluorocarbons. Not found near ground level nor in the troposphere, HF appears confined to the stratosphere. Its presence is therefore not measured by normal gas sampling schemes. Thanks to a suggestion of C. Rinsland (NASA/Langley), L. Wallace (KPNO) and W. Livingston (NSO/T) have measured the strength of the HF feature at 24752.05 A in the 'Stokes' archives 1979-1985. HF is found to have doubled in strength over this time interval. New FTS data show the trend continues.
The eruption of Mt. Redoubt in Alaska may also cause new increases of HF. Jet streams in December brought volcanic ash to Arizona for a short time. NSO is presently attempting to monitor HF using the 13.5-m vertical spectrograph. C. Rotation of Solar Active Regions.
R. Howard (NSO/T) has examined the rotation of solar active regions using data from Mt. Wilson. He finds generally good agreement with some previous studies of plage and active region rotation characteristics, although the rates are slightly slower than those found previously for magnetic fields and faculae. Reversed polarity regions show little if any differential rotation, and the scatter in their rotation rates is larger than for regions showing normal polarity orientation. Larger regions rotate more slowly than smaller regions. There is a correlation of rotation rate with activity cycle phase that is similar in nature to that found in sunspot data. Leading and following portions of regions show very similar rotation rates, unlike spot groups, where the leading portions rotate more rapidly than the following portions. Active regions with polarity orientations nearest the normal orientation tend to show rotation rates nearest the mean values. In general these results support the notion that older, weaker magnetic fields at the solar surface have evolved different subsurface connections from the time that they were a part of sunspots or plages. It seems possible that they are connected at a shallower layer than are sunspot or plage fields.
D. Reduction of the South Pole Data.
S. Jefferies (Bartol/NSO/T) has continued work on the analysis of the 1981 and 1987 South Pole data sets. To address the issue of possible temporal variations in the mode frequencies due to changing solar activity, the differences in the mode frequencies from the two data sets (taken at times of high and low solar activity respectively), were computed for the frequency range 2.4 < v < 4.8 mHz and the degree range 3 < / < 98. It was found that the differences appeared to be independent of v and / over these ranges, with a mean difference (v„81 - v19g7) of 224 ± 19 nHz. This result is consistent with reports of increasing frequency with increasing solar activity.
The line width measurements from the two data sets showed the same variation with frequency as that previously reported by K. Libbrecht (Big Bear Solar Obs.), an increase with degree (/) and with solar activity. Investigations are continuing into the line width measurements and their apparent variation with solar cycle.
The 1987 data set was also used to make measurements of the rotational splittings of the sectoral modes (m = ± I) in the range (3 < / < 15). The measurements showed no indication of a dependence on the depth of the lower turning points of the modes.
E. The Effect of Large-Scale Flows on Oscillation Ring Diagrams.
F. Hill (NSO/T) has continued his development of the oscillation ring diagrams as a tool for mapping convection zone flows by theoretically computing the effects of large-scale flows on the ring diagrams. To do this, Hill has analyzed the forward problem, wherein a large-scale velocity field as a function of depth is assumed, the corresponding depth-weighted velocity for a given ring is computed, a dispersion relation is assumed, a set of artificial rings is generated, the artificial rings are fitted with ellipses, and the artificial ellipse parameters are compared with those obtained from the data. The computed results are sensitive to the choice of parameters in the assumed dispersion relation, and point out the need for more accurate determinations of these quantities. The chosen parameters minimize the rms deviation between the calculated ellipses using the velocity curves actually determined from the data, and the observed ellipses. These same dispersion relation parameters were then used to investigate the effect of different velocity curves on the rings. It was found that velocity curves with a local maximum were much better fits to the data than curves that varied monotonically. This is consistent with the velocity curve actually inferred from the data. F. The Kinematics of Very Low Mass Galaxies: Is Dark Matter Ubiquitous?
Over a decade ago, work by V. Rubin (Dept. of Terrestrial Magnetism) and others on the rotation curves of spiral galaxies began to provide definite evidence for some amounts of non luminous matter in large spiral galaxies. This evidence came in the form of rotation curves which remained flat out to the observed limit of the optical emission, thus implying the presence of significant amounts of mass beyond this point. Spurred in part by theoretical models which required an exactly closed universe, other observations of various galaxies have also produced evidence for dark matter, to the point where it is now often assumed that all galaxies have dark halos. However, observational evidence for enough matter to precisely close the universe has not yet been attained. The nature of this dark matter has been the subject of a great deal of attention, and insight into this question can be obtained by seeing if there is a lower limit on the mass of a galaxy which can form a dark matter halo, since some of the dark matter candidate particles are quite energetic and easily trapped only by large gravitational potentials.
A new limit may now be available from recent observations of a dwarf irregular galaxy known as GR8. Using the VLA, the Mont Megantic Obs. in Quebec and the KPNO #1 0.9-m telescope, C. Carignan (Montreal), S. Beaulieu (Montreal), and K.C. Freeman (Mt. Stromlo) have mapped the optical and H I distribution of this galaxy. GR 8 is an outlying member of the Local Group with an absolute B magnitude of -10.7, which makes it one of the faintest known irregular galaxies. In addition, one of its H II regions has been determined to have an oxygen abundance of 0.024 solar masses, which is equal to the lowest oxygen abundance ever measured in an extragalactic H II region. Carignan et al. derive the total mass distribution from the H I kinematics, and the surface photometry allows determination of the mass contribution of the luminous stellar disk. They find the H I mass to be 2 x 106 solar masses, the B luminosity to be 2.5 x 106 solar masses, and obtain a derived stellar mass of 1.2 x 10*solar masses. However, the H I kinematics show the total mass out to 500 pc to be 3.9 x 107 solar masses, more than ten times the "luminous" mass. Hence these results show that even the faintest of dwarf galaxies have massive dark halos, and they lend support to the idea that it is the dark matter which is kinematically important, not the luminous material. In addition, dark matter particle candidates must now be sufficiently "cold" that they can form in aggregates of a few times 107 solar masses.
G. Outflows in YSOs: Dynamics Revealed by New Technology.
It has been known for some time that young stellar objects (YSOs) are often associated with bipolar outflows which possess high velocities and large mass flux. A fundamental problem associated with these objects is the determination of the mechanism that drives the outflow. Knowledge of this not only allows modeling of the outflow itself, but also is essential to understanding the evolution of young stellar objects and protostars and ultimately to the process of star-formation itself. One class of these objects, called the low excitation objects, exhibits enigmatic dynamic behavior. The radial velocities and line profiles of these objects indicate shock velocities of the order of 100 km/s. However, their spectra show oxygen and sulfur lines which are characteristic of shock velocities more like 10-30 km/s.
In principle this drastic change in velocity could come about through molecular cooling, and in fact H2 line emission is seen from these objects. However, the H2 emission could just as well be coming from weak oblique shocks that are spatially and dynamically unrelated to the optical line regions. Until now this question was impossible to answer because of the poor resolution of near IR detectors. However, the situation changed dramatically with the introduction of high-resolution two-dimensional IR arrays at Kitt Peak. P. Hartigan, S. Curiel, and J. Raymond, all of the Center for Astrophysics, have used the KPNO 2.1-m telescope with the 58 x 62 IR array and the TI2 CCD camera to obtain H2 and optical images of Herbig Haro objects 7 through 11. These HH objects are prototypical low excitation YSOs. The observations produced images in H2, S I, [S II], and Ha for each of these objects. With the exception of HH 11, all the regions with bright H2 emission have optical counterparts, which indicates that in fact molecular cooling is critically important in the outflow dynamics and is a principle energy loss mechanism in decelerating the outflow. Thus a significant advance in our understanding of these objects has been made possible by new technology being put into operation at the telescopes. m. PERSONNEL
During the October 1 - December 31, 1989 quarter there were no hires, terminations, or changes of status in the scientific and professional staff.
A. Visiting Scientists.
The following visitors arrived at NOAO facilities for periods of one month or more during the quarter.
date NOAO facilitv arrived name institution visited
10/1/89 Schelte Bus Lowell Obs., Arizona CTIO 10/1/89 Jean Marc Conan Ecole Superieure D'Optique, France NSO/SP 10/1/89 Serge Koutchmy Institut D'Astrophysique, France NSO/SP 10/1/89 Malcolm Northcott Inst, for Astronomy, Hawaii 8-m 10/1/89 Sergio Restaino New Jersey Inst, of Technology NSO/SP 10/1/89 Francois Roddier Inst, for Astronomy, Hawaii 8-m 10/1/89 Don York U. of Chicago NSO/SP 10/13/89 Michael Grady U. of Arizona KPNO 10/16/89 Paul Hintzen NASA Goddard, Maryland CCS 10/20/89 Pat Seitzer ST Scl, Maryland CTIO 11/1/89 Wendy Hagen Bauer Steward Obs., Arizona CCS 11/22/89 Craig Wheeler U. of Texas CTIO 11/28/89 Stephen Warren Steward Obs., Arizona KPNO 12/1/89 Lyman Neuschaefer Arizona State U. CCS
IV. INSTRUMENTATION, NEW PROJECTS AND OBSERVATORY ACTIVITIES
A. Future Telescope Technology Program (FTT).
The 3.5-m Mirror Project. Calibration of the 1024 thermal sensors was finished in October and 960 of them were installed in the mirror. Software to provide isothermal contour plots and temperature versus time plots from the thermal data were completed. In November, 30 of the thermal sensors were damaged by static electricity generated when polyethylene sheeting was dragged over the surface of the mirror blank during installation of a splash shield around the mirror. The sensors will be replaced the next time the mirror is removed from the polishing table.
Work on the polishing support was completed late in October. Grinding with 80 grit was started the first week in November and more than one millimeter of glass was removed from the mirror surface. By the end of December grinding with 220 grit had been completed, and we were about half through grinding with 25 Jim aluminum oxide grit. The radius of curvature is accurate to a few millimeters out of 12.3 meters (about 1 part in 3000).
Writing of the software for reduction of subaperture Hartmann test data was completed and integrated into the testing system on the Hewlett Packard computer. Simulations indicate this new form of the Hartmann test will make it possible to measure print-through of the hexagonal core structure if it exists on the 3.5-m mirror. This will allow verification of the measurements made with the scatterplate interferometer.
Finite-element stress analysis of a localized section of the 3.5-m mirror structure under two different loading situations was performed. A case that represented the maximum stress region from a three-point support was examined, and the maximum tensile stress was 168 psi, compared to a safe limit of 1000 psi. A second case was run to model the stresses produced by application of active forces. For the maximum force of 250 pounds, the highest stress was 79 psi.
A decision was made to proceed with design and fabrication of the telescope mirror cell this year (originally planned for FY 1991). A mockup of 1/12 of the cell was designed to use in testing prototype ventilation systems.
Fabrication of the parts for the support mechanisms is continuing. Most of the parts are now in hand.
The new 1000 x 1024 Photometries CCD camera has been received and is working as specified under computer control.
Division Support. FTT staff worked on design studies for an infrared-optimized 8-m telescope; some of these designs include collimators and cameras that show promise of producing excellent image quality. Recalibrated thermal sensors for the mirror mockup experiment at Apache Point Obs. were delivered and installed in the telescope early in January.
B. Global Oscillation Network Group (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 exploit 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.
This will be a watershed year for the project in many important respects. The development work on the breadboard instrument is now complete, and the results are most gratifying. The prototype field station will be operational in March and producing data on a more or less ongoing basis. Delivery has been made on the first batch of critical optical components for the network field stations. Field station construction efforts will grow to become a major aspect of project activity by year end, and selection of the network field sites will be completed by this fall. Furthermore, the success of these various efforts will be validated by separate external reviews conducted on the reduction and analysis software development effort, the prototype instrument design, and the project as a whole. These reviews will be completed before the Annual GONG Meeting in late March.
The efforts leading to the instrument and software reviews were meshed together in a very synergetic way. The instrument Prototype Design Review (PDR), scheduled for February 21 - 23, represents the conclusion of the breadboard development. This is a review focused on validating the prototype design with actual solar observations taken with the breadboard system. Of course, this necessarily demands that those data be reduced to meaningful product data sets. So, the data reduction group has focused their development efforts over the last several months on producing "prototypes" of essential pipeline reduction routines, which has required implementing many of the important GONG processing concepts.
The instrument development group has taken several days of solar data, both imaged and in the calibration mode. These data have been reduced and they reveal that, even though there are some correctable shortcomings, the GONG breadboard clearly produced outstanding velocity images at this spatial resolution. Contrary to some expectations for an imaged device, modes were observed well above the noise all the way down to / = 0, and these were seen in only a 12.8 hour (single day) run! The clarity of the /-v diagrams obtained from these short runs was surprisingly good and, among other things, clearly showed temporal aliasing of high frequency modes which indicates that the cadence must be moved from 75 sec to 60 sec or less.
A detailed document describing the design of the instrument, both as a breadboard and as it has been adapted for the prototype, is in preparation and will be presented to the instrument PDR panel for their review. This material will include performance analyses based on the solar observations obtained during the past summer and fall. The review panel is chaired by K. Libbrecht (CalTech/Big Bear Solar Obs.) and includes T. Brown (High Altitude Obs.), D. Elmore (High Altitude Obs.), B. Gault (High Altitude Obs./WIND II), J. Hall (JILA), and A. Title (Lockheed Palo Alto Research Lab.).
With some pangs of mourning for an old friend, a necessary "casualty" of the instrument milestone has been the breadboard itself. This optical system has been dismantled to make room for the acceptance testing of the field station optics. Four complete sets of the 1 A Lyot filter optical components have been received from the vendor. We view these as "proof sets to demonstrate the vendor's ability to produce these critical elements, including the very thin ADP pieces. As will be the case with the subsequent deliveries, these first sets will be examined exhaustively to assure that they meet GONG requirements. The initial tests are encouraging.
The data reduction review, which was conducted on January 15 - 17, was combined with a joint meeting of the Data Reduction and Analysis, Steady Flows, and Low Frequency science teams. The "teams" aspect of this meeting included addressing a variety of significant issues relating to the design of the production GONG pipeline. Particular emphasis was placed on the strategy and tactics of data quality assurance and merging, and how these might differ for low temporal and spatial frequencies vis-a-vis medium and high frequencies.
The software review was conducted by a panel chaired by D. Hathaway (NASA-Marshall Space Flight Ctr.) and included R. Bogart (Stanford), J. Kuhn (Michigan State), and R. Stebbins (JILA). This review dealt with the overall software development strategy, and in particular, the operational examples provided by the prototype pipeline software. This software was developed and used in the IRAF environment ultimately intended for helioseismic analysis packages. This provided the panel an opportunity to examine the GRASP (GONG Reduction and Analysis Software Package) effort as well. As these activities have occurred just at our press deadline; a more complete and detailed report will be deferred to a later report.
The Site Survey group has completed the most recent enhancement of the analysis software, and they are in the process of performing a comprehensive analysis of all of the site survey data from the beginning of that program. It is expected that the observational statistics will be ready for discussion at the annual meeting. The previous analysis of this data, reported two years ago, suggested that many of the potential networks had remarkably similar performance. Consequently, it may well be that some decisions will be driven by other considerations, such as logistics and infrastructure. These will be more difficult factors to evaluate and consequently actual site selection probably will not be made until sometime this summer or fall.
The NSF has scheduled an overall project review which will take place March 8-9. This study will assess the scientific imperatives, the technical progress, the management, the project plan for production and deployment, and the future of the GONG budget. Needless to say, the NSF panel will have the results of the software and instrument design reviews as points of departure for those aspects of their activities.
If the NSF project review is positive, the FY 1990 GONG budget will be S1.9M. A detailed review of the project time line, in view of both the shift from the "buy" to "make" philosophy and realistic funding level options, is presently under way and will be presented to the NSF at their March program review.
C. Instrumentation Projects.
Two projects were completed at CTIO during the last quarter, while other projects also made progress.
A closed-cycle cryocooler was installed in the IR Imager. This is the same type of cooler already in use in the IR Spectrometer, so that the compressors and high-pressure helium lines at the telescope serve both instruments. The cryocooler replaces liquid helium as the means of cooling the detector. The installation is operationally convenient, in that it eliminates the need for twice-daily liquid helium transfers, which was an inefficient process. In addition, the cost saving is significant, close to $20,000 annually in direct costs, plus the savings in wear on CTIO's ancient and fragile helium liquifier.
A number of improvements were made to the CTIO 4-m autoguider hardware and software, which considerably enhance its efficiency and versatility: the image dissector has been replaced by an RCA ISIT camera, which is much more sensitive and easier to set up for guiding. A variety of routines have been implemented to speed acquisition of guide stars and make precision offsets. Finding and setting up on guide stars with the spectrographs, once a tedious and time-consuming process, is now almost painless. The offset guider is also now, for the first time, a useful tool with the IR instruments. The added sensitivity allows usable stars to be found in the smaller field at f/30, and the software now supports use of the guider while making grids with the imager or beam-switching with the single-channel instruments. It is also now possible to input user-supplied catalogs in floppy disk to the telescope control program. Other improvements, such as making the ST Guide Star Catalog available on-line, are scheduled for the near future.
The CCD TV camera system is now in routine use on the CTIO 4-m telescope for acquisition with the R-C instruments. CTIO is gearing up for full production of the final version, which will differ in some respects from the version now in use-some additional features will be added, and the circuit boards will be printed circuits rather than wired by hand. The first of these cameras is now in production.
The new gratings were installed and tested in the IR spectrometer at Cerro Tololo. Stray radiation has been reduced by another order of magnitude, to the point where it is comparable to the array dark current, and well below sky background at most wavelengths and resolutions. Operating parameters of the detector are still being improved.
Following the successful operation of a 5 cm-aperture superpolished-Si-mirror coronograph constructed at Sacramento Peak, a 15-cm instrument consisting of a superpolished Zerodur primary objective mirror in a special mount having fine motorized control in tilt and a second mount with motor-control of an occulting mirror, was constructed by the Institut d'Astrophysique and a French engineering company. It features rejection outside the telescope of heat from the solar disk, a novel concept for ground-based coronagraphs.
This "breadboard" instrument is being used primarily to explore and optimize design concepts for a larger, research-quality reflecting coronagraph of 35- to 50-cm aperture. Mirror samples collected for this larger instrument have yielded rms variations over the surface as small as 1.9 A, thus promising extremely low scatter from the mirror surface, a previously-unmet requirement for reflecting coronagraphs. The ultimate instrument will feature video-rate rejection of dust streaks, a significant background contribution to the coronal image.
In parallel with this effort, S. Restaino (New Jersey Inst, of Technology), currently a long-term visitor to NSO/SP, has carried out a preliminary ray-tracing analysis of such reflecting coronagraphs to explore designs for the secondary optical system that minimize the aberrations of a tilted optical system. It has been found that a special field-flattener can markedly reduce the field curvature. Ultimately, designs will be explored that also minimize instrumental polarization.
Development of such an instrument is being pursued in hopes of achieving true achromatic imaging of the corona, either over a broad wavelength range ("white light") or over widely-spread emission lines from the UV into the IR, and yielding high temporal, spatial, and spectral resolution, including observations of polarization. Such observations are demanded to support new concepts of coronal heating, prominence formation, small-scale solar-wind generation, and initiation of coronal mass ejections.
K-line Filter. Significant progress was made during this quarter in the construction of the stellar K-line filter. The end windows and insulation package were ordered. The machining of the actual filter housing and the fabrication of the insulation shell were completed. The fabrication of the temperature controller, with its associated electronics, is nearing completion. The optics for the filter were tested at Sac Peak and subsequently returned to the vendor because they did not meet specifications. The mechanical fabrication of the filter has progressed as far as currently possible in the absence of the optical elements. Once acceptable optics are received from Kappler Crystal (which is anticipated during the second quarter) then the instrument can be completed.
10 Infrared Magnetograph. The infrared magnetograph project made significant progress. Laboratory space was cleared and organized. Precision rail tables for scanning the solar image were received, assembled, and operated successfully in the lab under computer control. A multiple-frame video acquisition board was installed in its host computer and used to acquire infrared images with the newly arrived infrared vidicon. Optical components (polarizers and retarders) began arriving late in the quarter, testing and characterization are now underway.
New grating at the McMath. NSO has recently aquired a new grating 16.5 inch x 12.5 inch from Milton-Roy Co. (successor to Bauch & Lomb Co. grating division) to replace the present 10 x 6 inch grating, which was ruled by H. Babcock at the offices of the Mt. Wilson Obs. 30 years ago, in the main spectrograph of the McMath Solar Telescope. In spite of the poor blaze and bright zero order, the new grating is twice as efficient as the old, representing a four-fold gain in double pass. Drawings are now being prepared which will allow us, when converted to hardware, to install this grating in a tandem mounting with a second 18.5 inch x 14.5 inch IR grating. Thus in a few minutes we can flip from one grating to the other, thus covering the spectral range 3000 A to 15 u.m.
CCD Development. The OUV Lab SUN installation has been completed and is being used for display and analysis. Spare parts were used to build an 11/73 CCD controller for the downtown Tucson lab, which permitted sending a full CCD system to the Burrell Schmidt telescope for permanent installation. A new TV pickoff mirror for the 4-m prime has been completed. This will provide less vignetting when the 2048 CCD is used. The #1 0.9-m guider was also modified for less vignetting. KPNO completed a second filter wheel for the 4 x 4 filter assembly to reduce the handling requirement for the large filters. Discussions with Tektronix revealed an anticipated delivery time for 1024 x 1024 thinned backside treated AR coated to be delivered first or second quarter of 1990. They have agreed to change our order to purchase three of the above mentioned devices instead of the seven 512 x 512 devices we had previously ordered. A proposal is being prepared to join with Steward Obs. to develop a CCD optimized for spectroscopic work. RCA3 has been taken out of service to free up a test dewar. The (STIS) 1024 Tektronix device has been installed and preliminary tests conducted.
Kitt Peak Fiber Actuator Device (FAD). Efforts during this quarter focused on software development and construction of the fiber cable and "test" fiber/button assemblies. During October the computer interface to the instrument was modified to use two serial (RS232) lines. Code was written and debugged to run repetitive testing of the positioner with the two serial lines. This has proved to be more efficient than the previous coding (which used one serial port). Code was also written and tested to place buttons on the three focal plane plate levels, and to allow rotation of the fiber button during movement. Astrometry routines were begun. A borrowed Sun workstation was installed in the fiber lab for development work on the instrument. This has proved to be beneficial because the communications with the positioner do not have to be timeshared. The red fiber cable has been assembled and moved to the fiber lab. Work was begun on the cable ends. Six "test fibers" were constructed (6 feet or so lengths of fiber) to use for the February 2-4 T&E time and to practice construction techniques and experiment with various epoxies. The gripping function of the instrument was mechanically optimized and the control circuit for the gripper motor modified to allow for adjustment of the grip positions. Several additional cable supports were constructed. Formal electronic documentation of the instrument was continued and largely completed.
Bench Fiber-Fed Spectrograph (BFFS). Much of the actual fabrication of spectrograph modules was completed during this quarter. Both collimator mounts were assembled and tested in the Tucson optics shop. The focal surface module was fabricated and assembled and most of the grating module was completed. Work began on the locator sub-module. The design for the camera-axis mount was finished, a design review performed, and fabrication initiated. Also, the design for the
11 mount to hold the Simmons' camera was finished. All of these efforts are focused to provide an operational minimum "first-light" configuration within next quarter. One of the FY 1990 goals for the spectrograph is to have it automated sometime after "first-light." An overall plan was formulated to accomplish this. Specific functions for all the spectrograph modules (current and future) were defined and approved. Necessary parts were identified, purchased, and construction is well under way. In addition, software concerns have been addressed. Since the bench spectrograph may serve as a model for future instrument user interfaces, a meeting was convened to formalize the system environment and functions of each component (instrument control unit, workstation, and "dumb" or development terminals). It is an observatory-wide goal to eventually control all instruments via some use of X-windows on the console workstations. A list of desired spectrograph status/control commands was made. J. Simmons (NOAO) released a study of a refractive dedicated spectrograph camera. Some concerns have been raised by the scientific staff regarding this design and these are currently being analyzed. Quotations for optical glass have been acquired with current prices and availability.
Next Generation CCD Controller. The OUV Sun computer "libra" was brought on line; the Inmos BOH Transputer/VME interface card (which is the standard CTIO/Tucson host computer interface for the transputer systems) was installed and successfully tested. The IR Sun computer "omega" had its disk cross-mounted to "libra" in order to have access to the Transputer code from either machine. The decision was made to use a simpler (lower-power and cost) communications link for the transputers (from the host computer to the remote transputer controller) than the "TAXI" interface which had been under development here. The "TAXI" fiber optic interface R&D efforts were documented and distributed. Construction was begun on a second of the new compact power supplies. Design and board layout was begun for a new quad Analogic A/D card (parallel conversion). The new (Eurocard format) dual channel video processor card was constructed. Adaptor frames were constructed and wired to patch the new dual video processor and quad Burr- Brown A/D cards into the existing systems (Eurocard to 86/44 pin adapters) for testing. Some R&D efforts were continued with the simple "Sequencer" card constructed earlier in the year. A meeting was held with CTIO personnel; they believe they will have a prototype controller running by March 1990.
KPTT/HRIS Progress Report. Early this quarter the KPCA Time-Tag (KPTT) was used at the KPNO 4-m telescope for the second time. A new WWV absolute time synchronization was implemented for the first time; data were successfully acquired using this new accessory.
STIS. The new dewar has been received from Infrared Labs and is being wired to accommodate virtually any CCD device with an extremely quick tum-around. The adaptor cards have been reworked and sockets modified.
Infrared Research & Development Program. Telescope and laboratory testing of the new noise reduction algorithm is complete. KPNO was able to reduce the read-noise in the SBRC-InSb arrays to 50 electrons. The technique is extremely useful in the spectrometer and for narrow band imaging. The Infrared group's paper "Status of the NOAO Evaluation of the Hughes 20x64 Si:As Impurity Band Conduction Array" has been approved for presentation and publication by the Air Force Weapons Laboratory. It will be presented at the February SPIE meeting in Tucson. Based on KPNO and CTIO's experience with the TAXI chips KPNO has decided to change its approach to that used by CTIO. We will use fibers for the data transmission and opto-isolated twisted pair for control signals for advanced instrumentation control. We will be including enough memory in the controller to contain the entire program rather than continuously download code in operation. When the new digital engineer arrives we will begin system definition, which will take into account the data processing as well as the control needs of present and future IR instrumentation. The first lot of PV-Ge arrays has high dark current which was measured during wafer probe. It is thought
12 that there was some processing problem. A second lot is now in wafer test and the results of those tests will determine whether they will be hybridized. If these tests are successful we can expect that the arrays will go into hybrid testing in March. The first lot of astronomy PtSi arrays was a decided failure. Several arrays made from different wafers all showed most unusual low background performance. It is thought that there is trapping or other surface related effects due to a processing error. If it were not for the cavity tuning, these devices could be considered for delivery. The cavity mismatch results in a lower than acceptable quantum efficiency. A second lot has been started and we can expect to see devices in March. We are using this time to improve our testing procedures and speed.
An 0.3-m telescope, left over from the rocket program days, is being modified for use as a coating test bed. Emissivity measurements of the sky and the KPNO 1.3-m and 2.1-m telescopes are being made using the CRSP and the IRIM over a long time period. The test telescope will be left in the dome to simulate actual conditions and its emissivity will be measured and compared to the 1.3-m and 2.1-m results. We expect the first tests with the new test telescope to be made in late January. The plan for the FY 1990 effort on the cryogenic echelle spectrometer project has been completed. We will finish the collimator mirrors and design and test the grating and collimator mounts. After the tests are complete the detail conceptual design of the remainder of the instrument will be started. We hope to complete the conceptual work in FY 1990 and begin detail design and fabrication in FY 1991. The polishing of collimator mirror Ml is continuing and progress is much slower than expected. M2 has been generated but polishing will not begin until Ml is completed. The new noise reduction code has been generated in an R&D version for testing over the coming semester at the telescope. The user version of the code will appear later this year. CRSP has been used at the telescope with great success during the fall semester. The detail mechanical design of the simultaneous quad-color infrared imaging device is 80% complete and the electrical design is 95% complete. An outside source was used to design the PC cards and generate documentation for the boards from our rough schematics. This has proved to be cost effective and has resulted in our getting the design done in a timely manner. We received the dewar housing and coolers for the camera. The silicon mirrors were received but it was necessary to reject them; the vendor has agreed to redo them to our requirements. All the optics are expected during the first quarter of 1990. Software to operate the instrument is now being coded. Although the project is behind schedule we expect to get to the telescope in May and do extensive testing during the summer shutdown.
D. Observatory Activities.
During the period October - December 1989 the continued shutdown and major overhaul of the KPNO 2.1-m telescope was the largest and most difficult project underway at the observatory. After the last period, where the bulk of the rework was accomplished, all the testing and evaluation remained. Most of the testing has been completed. While a few difficulties remain to be worked out regarding the optical quality of the telescope, its refurbishment is considered a large success. Several of the improvements, such as the new mirror support system and the telescope control software, are considered to be significant advances in our capability of operating and maintaining first rate telescopes. This period also saw a number of smaller safety and telescope improvements by KPNO, such as a new drive system for the #2 mirror mast at the Vacuum telescope, safety equipment and procedures for handling large optics during aluminization at the McMath telescope, and completion of the KPNO portion of the public visitor walkway to the 4-m telescope. Continuing progress was made in a number of mountain programming projects. There was an increased emphasis in getting the user interface code at the Vacuum telescope in place; improvements in operations of the various IR arrays were made through changes in the controller microcode; the first SQUID application software was written for use with the laboratory (R&D) system; and additional software was written to control Fiborg, the fiber optic positioner for the 4-m
13 telescope. In an effort to conserve water on Kitt Peak, new low water use toilets were ordered for the public visitors area. A study will be necessary to determine if the mountain sewer system is capable of handling low water use devices of this type. This is being done on the heels of the driest year on record at Kitt Peak. Average rainfall and snowfall for Kitt Peak are 25.36 and 25.44 inches. This year we received 14.73 inches of rain and 5 inches of snow. To remain in compliance with the latest EPA regulations, two five-hundred and two one-thousand gallon fuel tanks were removed from the ground in preparation for installation of one new two-thousand gallon tank with the required leak detection capability.
The SN 1987A database in Tucson continues to grow. At present, the following CTIO data sets are available in machine-readable form:
1. 2D-Frutti spectra, days 1-180 2. CCD spectra, days 198 - 805 3. UBVRI photometry, days 1 - 813.
The SN 1987A database can be accessed through the Internet and SPAN computer networks. The second set of 12 positioners has been added to Argus, the CTIO multi-fiber-fed spectrograph. It now has a total of 48 fibers on 24 positioners, which is its final configuration. The CTIO 4-m telescope control program (TCP) and associated hardware are now permanently installed on the 4-m telescope. The new program provides better pointing and tracking, and has also enabled us to begin implementing a variety of improvements. The final optical design for the CTIO 4-m prime focus corrector/atmospheric dispersion corrector (PFC/ADC) was completed and orders have been placed for the glass and for fabrication of the optical elements. Work has started on the mechanical design; work has begun on the design of the new 4-m PFCCD unit; and work is proceeding on the La Serena-Tololo microwave link.
CTIO's Chilean economic statistics, FY 1990:
Month %Change Cum, change Avr. monthly
Oct 2.9 2.9 308.07 Nov 1.7 4.7 312.91 Dec 2.1 6.9 311.99
14 V. PROGRAM SUPPORT
A. Director's Office.
1. Visitors/Tour Groups. Individuals and groups from Arizona Precision Industries, Cole Optical, Congressman Kolbe's office, Kirtland Air Force Base, the U. of Arizona, and Valley National Bank, visited the NOAO large optics polishing facility, in October. The Director's office arranged a tour for the Science Club of Amphitheater High School in November. The group consisted of 14 students and one teacher. The students, looking for ideas for projects to submit to the annual science and engineering fair, visited the GONG lab, the NOAO mirror lab, and the optics shop. A. Hiller and E. Hardesty provided postcards and NOAO stickers as mementos of their visit In December, NOAO Tucson was visited by seventh and eighth graders from Miles Junior High School. The group of 16 toured the optics shop with G. Poczulp and were also provided with mementos by the PIR office.
Earlier in the year, program assistants from NSF's Division of Astronomical Sciences visited. They toured the downtown Tucson offices, the UA Mirror Lab., Kitt Peak, and Sacramento Peak. There were several visits to the NOAO large optics polishing facility and these visits are continuing. Groups came from the Cranfield Inst, of Technology, Indiana U., Ohio State U., Schott Glass Technologies, Inc., the U. of Hawaii, Yale U., and of course, the National Science Foundation. Foreign visitors included groups from ESO, Imperial College, Italy, and the U. College of London. The Director's office arranged a tour for the High Altitude Observatory's Summer Colloquium Group. This group of 25 started with a visit to Kitt Peak. Their downtown Tucson visit included a talk by R. Angel of the U. of Arizona on "Very Large Optics," and tours of the UA mirror casting facilities given by E. Mannery and B. Martin. Lunch was served at NOAO followed by an overview of the national observatories by S. Wolff, a demonstration of KPNO CCD development by R. Green, a tour of the GONG lab with S. Chidester, and a visit to the optics shop accompanied by P. Kupczewski. The group also visited the NSO facilities at Sacramento Peak.
CTIO entertained six groups in October, totalling 113 people. They were visited by the Corporacion del Cobre, Ninos Cantores de Vina del Mar (a primary school), a Rotary Club, and la Universidad del Norte, Coquimbo. Two schools, and a public medical clinic visited in November. During this month, seven groups took a tour of Cerro Tololo, totalling 186 people. This included Escuela Diaguitas (a primary school), Nido de Aguilas (a high school), and Consultorio P. Aguirre Cerda (a public medical clinic). IBM also visited. Two tours were conducted in December, totalling 58 people. One primary school and Los Carabineros de Chile.
Several schools visited our Sacramento Peak site. In October four different school groups visited; Alamogordo Elementary School, group of 20; Alamogordo Junior High School, group of 25; El Paso Senior High School, group of 22; El Paso Community College, group of 34. The four schools totalled 101 people. Two New Mexico junior high schools toured the mountain in November. One school sent 20 people; the other, 25.
2. Safety Report. The major accomplishments/highlights of the NOAO Safety and Health Program for each U.S. site are as follows:
KPNO. Additional first aid stations were installed and the existing ones, upgraded. An ice shield awning was installed over the entrance to the 4-m telescope building to protect staff members and vehicles from ice which builds up on and falls from the dome. First responder training, a higher level of
15 industrial first aid training, was given to new employees and as a refresher to existing employees. An in-depth review of the dining facility operation resulted in several improvements including routine inspections by the County Health Agency. The water system operation was audited and found to be in compliance with EPA regulations. The audit included a backup bacteriological analysis of the water, as well as an analysis for parasites which were thought to be a potential problem. The results of the analyses were negative.Telescope and other maintenance activities were extensively reviewed for potential personal fall hazards. The review resulted in identifying and reporting many such hazards along with providing recommendations for the use of personal protective equipment and other preventive measures. Regarding personal fall protection equipment, a demonstration of full body harnesses, lanyards and retractable lifelines was given.
NSO/SP. A program was established to prevent the exposure to elemental mercury-approximately seven tons-used in the Vacuum Tower telescope for bearing support and as a vacuum seal. The program included notification of the hazards of exposure, the minimum allowable levels of exposure, the recommended administrative and engineering controls for preventing exposure, and the appropriate documentation concerning the controls for handling mercury. An extensive fire protection survey was conducted. The survey included inspection of all the facilities with an emphasis on forest fire hazards, adequacy of fire detection/alarm systems, LPG hazards, adequacy of fire brigade facilities, as well as a general review of the facilities and practices along with recommended improvements in all areas. Major recommended improvements were replacing the existing antiquated fire detection/alarm systems, incorporating fire detection/alarm in facilities not currently covered, providing Halon automatic extinguishing systems for computer installations and automatic water fog protection for the LPG storage tanks. A comprehensive forest fire response plan was prepared. The plan provides a comprehensive program to cope with this exposure; i.e., a means to familiarize all persons involved with what to expect and how to react in such a crisis. Several modifications for the safety of operation of the Vacuum Tower telescope elevator were completed. The elevator was also thoroughly inspected and serviced. The power distribution transformers which were identified as contaminated with PCBs were removed from service, retrofitted with non-PCB oil, then put back into service. An extensive operations/maintenance effort to clean up and repair friable asbestos containing pipe insulation in the mechanical rooms was completed. The Tucson Safety Officer assisted the NSO/SP Safety Officer with a general safety review. The review resulted in recommendations for improvements in the areas of general emergency procedures, metal cleaning/anodizing operations, high voltage work procedures, crane inspection/testing, personal fall protection and confined space entry. Other areas that were reviewed such as water and sewage treatment operations were noted as meeting all safety or EPA requirements.
Tucson. Prior to etching the 3.5-m WIN mirror with hydrofluoric acid, the hazards of this operation were extensively reviewed. Following the review, the appropriate personal protective equipment and engineering controls were provided and the project was successfully completed without incident. Automatic fire detection equipment was selected and purchased for protecting personnel and adjacent facilities not presently protected. Installation of this equipment, which is scheduled for the next quarter, will include connecting the equipment via phone lines to a 24 hour/day central reporting station. A major house cleaning effort resulted in reducing fuel loads, providing safety cabinets for flammables, and a separate fire protected records storage building. The safety library was extensively augmented and updated with new safety references, codes and regulations. Several new sections for the NOAO Safety and Health manual were completed and are currently in the process of being reviewed. The manual itself is expected to be released during the next quarter. A final response to the AURA safety committee's review of all sites was prepared. All 35 of the recommendations have been addressed. Many of the recommendations have been implemented and those that remain are in the process of being implemented. The Earth First environmental group's
16 activities on the UA campus and elsewhere prompted a review of security procedures. As a consequence, existing procedures were tightened, additional security procedures were implemented, and Tucson and KPNO staff were given guidelines for various situations likely to be faced.
All Sites. A new NOAO safety footwear policy was put into effect. The policy identifies the particular work activities requiring such protection and the means for employees to obtain their footwear. Approximately 70 persons at the three sites were provided with protective footwear. As required, a total of 15 underground fuel storage tanks (USTs) were leak/tightness tested at the three sites. All were found to be in compliance. Three USTs at the KPNO site and one at the Tucson site were identified, based on their age, as requiring upgrading or replacement to meet new leak detection requirements by the end of 1989. As a result of this requirement, along with cost considerations and other factors, the process of closing and replacing these tanks was begun. Personnel at all sites were notified of a potential problem with Carpal Tunnel Syndrome (CTS), a repetitive motion disorder involving the wrists and associated with PC/VDT operators. The notification included an explanation of the disorder, the causes and symptoms, and specific preventive measures including information relative to workstation design.
3. General. NOAO's proposal to participate in the 1990 REU program was mailed to the NSF in early October, and we were informed in December that the award had been given. The Final Report from the summer of 1989 program was submitted to the NSF in October. NOAO agreed to participate again in the National Comparative R&D Laboratory Project (NCRDP). This is a continuation of the 1987 NCRDP study appointed by the National Research Council to continue to profile the United States R&D system, for a Technology and Information Policy Program.
A progress report on the People's Republic of China Scientist Supplement Program was sent to the NSF in November. The July 1988 - June 1989 Annual Report was submitted to the NSF in November, and to the Bulletin of the American Astronomical Association, for publication.
NOAO has agreed to participate in the 36* annual southern Arizona regional science and engineering fair. Support includes providing judges from the Tucson scientific staff, and awards. In December, the Director's office created a flyer and sent it to all junior and high schools in the southern Arizona region, encouraging students to participate in the fair and to consider a project in astronomy. During this quarter, the Director's office received the Report of the IRAF Users' Committee which met in Tucson in September. The Report was published in the December issue of the NOAO Newsletter.
A total of $4,650.96 was paid out of the NSF Foreign Travel Fund account this quarter. Sites and institutions visited were Chile, Las Campanas, UKTRT and Tenerife.
17 B. 8-M Office.
8-m Telescope Design Studies. A 1/40 scale model of the 8-m telescopes was constructed this quarter. L. Barr (retired employee) designed the model and enclosure, and fabricated the telescope model. Arizona Plastics built the enclosure of clear acrylic plastic. R. Harris designed shipping boxes for the telescope and enclosure, which were made by J. Ventura with some special fixtures made by L. Macomber and L. Junco. J. Richardson made scale model mirrors for the telescope, which were coated for us by D. Kucera. All are NOAO staff members in the ETS division. The model was assembled during the first week in January, and sent to the AAS Meeting in Washington, D.C.
The model will be used for displays at scientific and technical meetings as well as for public information. Because it permits an excellent visualization of the design concepts involved in the telescope, it will also be useful in future development of the project
Preliminary water tunnel tests were performed on scale models of four different proposed 8-m enclosures at the U. of Washington this quarter. During these preliminary tests W.-Y. Wong and F. Forbes (NOAO) were active in helping U. of Washington personnel develop new equipment and procedures to make sure the tests were complete and were well documented by two video cameras. Final tests were performed January 8-16. The purpose of the tests is to aid in selecting a final design for the enclosure.
Other Activities. P. Osmer (NOAO) attended the meeting of the Joint Working Group on Ground-Based Astronomy held in Waimea, Hawaii, on November 27, 1989. On the same trip he visited the proposed site of the 8-m telescope at the Mauna Kea Observatories and gave a talk on the 8-m project at the Inst, for Astronomy, U. of Hawaii.
C. Central Administrative Services.
During the quarter ending December 31, 1989, CAS was primarily involved in the following:
1) The FY 1989 audit by Coopers & Lybrand was completed, and draft reports of the financial statements and report to management were issued. The final reports are expected in late January or early February.
2) New rental rates for NOAO housing were calculated in accordance with OMB Circular A-45, and policies and procedures for charging rent at Kitt Peak and Sunspot were developed. A schedule for implementing the new rates will be set after approval is received from the NSF.
3) Proposed changes to NOAO's employee benefits were prepared and submitted to the Personnel Policies Committee. Approval is pending.
4) The AURA overtime pay policy was revised to agree with federal legislation and the NSF Cooperative Agreement.
D. Central Computer Services.
The NOAO-Tucson Scientist Workstation Network reached its initial operational configuration, with a total of 10 SPARCstation-1 desktop workstations and a powerful Sun-4/370 server.
18 Members of the NOAO IRAF group, STSDAS (Space Telescope Science Inst.), and PROS (the ROSAT software project at the Center for Astrophysics), the three main groups currently producing and supporting IRAF software, met in Baltimore to discuss technical issues and to plan for IRAF release 2.9 in coordination with HST and ROSAT launches.
A new VOS (IRAF programming environment) interface, providing general system support for linear and nonlinear world coordinate systems (WCS), including the astronomical sky projections, has been written and will be included in the V2.9 release. Although the new interface addresses the general WCS problem at the systems level, full integration of WCS support into the IRAF system and application tasks will take some time. A new graphics kemel (written by Z. Levay of the Space Telescope Science Inst.) has been added to the system. This new graphics kernel, called the IMD kemel, allows plots to be directed to the image display device.
A first release of the SAOimage image display server for XI1 (the X-window system), written by M. VanHilst at the Center for Astrophysics, is now available for distribution for several host systems. These include the VAX running Ultrix 3.1, the VAXstation running VMS and DECwindows, the DECstation, and all Sun architectures running SunOS4.
Several new applications packages have been made available to the user community in the last few months as add-on packages to V2.8. These include a beta release of TESTPHOT, the IRAF version of DAOPHOT, prepared by L. Davis in collaboration with D. Crabtree (Dominion Astrophysical Obs. and now at ST Scl) and P. Stetson (DAO) with much help from P. Massey (KPNO); a test release of RV, the radial velocity analysis package that is available to users for testing and evaluation; and a test release of NEWIMRED, a suite of instrument packages for streamlined reductions of various KPNO and CTIO instruments such as Argus (CTIO), Coude" (KPNO), Echelle (generic), Goldcam (KPNO stellar longslit), Nessie (KPNO), Slitlets (KPNO), and Specred (CTIO stellar longslit).
Two personal workstations were acquired for the use of the IRAF group. These were funded from the new NASA grant for IRAF systems development, and were purchased with substantial vendor discounts.
Substantial progress was made in the implementation of new telescope computer systems and software. In coordination with the general overhaul of the KPNO 2.1-m telescope, the new telescope control program was installed, as well as software control for the telescope console and drive servos. Pointing and open loop tracking are good. The user interface was also installed and is working well.
A new algorithm for IR array readout was implemented, resulting in a reduction of detector read- noise by a factor as large as 6 for the InSb imager and spectrometer.
E. Central Facilities Operations.
Central Facilities Operations continues its efforts to upgrade and maintain the Tucson facility. Architectural/engineering support of the various departments' programs and facilities is also being increased.
In early December, a major leak developed within the existing east wing boiler which required immediate replacement with the new boiler purchased in FY 1989. The earlier modification of the HVAC system (September 1989) was able to maintain environmental control within the computer room for the week required to remove and replace the boiler. Monitoring of the Tucson facility power system was also initiated during this quarter along with a program to repair/repaint the
19 exterior overhead soffits damaged from roof leaks over the past few years. Relocation of the accounting records is approximately 90% complete and the necessary modifications have been completed for a centralized, secure, excess equipment storage area. In an effort to increase employee safety, handrails were installed at exterior entrance stairs and the emergency exit maps within the Tucson facility were updated.
Architectural/engineering design/drawings have been completed for replacement of the underground fuel storage tanks and exterior landscape modifications. This work is scheduled to commence in the second quarter. An architectural rendering of the WEN telescope was completed as part of the ongoing program support.
F. Engineering and Technical Services.
The computer software for the "Subaperture Hartmann Optical Test (SHOT) was completed and debugged using simulated data generated by the computer. The real data for testing will proceed when the 3.5-m mirror is polished to a sphere (projected to be the first quarter of 1990).
G. Publications and Information Resources Office.
Publications and Information Resources dealt with the typical load of media contact and referrals as well as the annual tourist-inspired influx of queries. Photographic sales continue from the Photo Collection. A monthly break-out of major activities for PIR follows:
6 October - Press release on Dr. M. Belton. Details of the launch were given a local twist with the disclosure of Dr. Belton's position as Lead Scientist of the Imaging Team for the Galileo satellite set in orbit after the shuttle launch of 17 October.
10 October - PIR created and underwrote an advertisement that appeared in the Tohono O'dham Rodeo Program, Fall 1989.
20 October - Drs. Balzano, Higgins, and Smoot guest-observe through arrangements facilitated by A. Hiller and Dr. J. Graham's (Department of Terrestrial Magnetism - observer on the Burrel- Schmidt that evening) extension of professional courtesy.
23 October - Photographer for National Geographic, T. Ives, escorted for a telescope photographic session at the 50-inch by A. Hiller.
The month of October also entailed detailed legwork to coordinate for the upcoming shoot with astronaut N. Armstrong scheduled in November.
11 November - Research Corporation Technologies conference attendees tour of Kitt Peak and the Steward Obs. 92-inch coordinated by Visitor Center staffer A. Cramer and A. Hiller.
12 and 13 November -- Two day video shoot located at Kitt Peak to celebrate the Twentieth Anniversary of the Apollo Moon Landing produced by Japan Television Workshop. The shoot was facilitated through the cooperation of telescope operator G. Will, S. Bulau (engineer on the 13th), the large Japanese crew, N. Armstrong, and many of the mountain personnel. Arranged and escorted by A. Hiller and E. Hardesty. Shown in Japan on 10 December a VHS video is available for viewing either from PIR or at K. Cramer's office on Kitt Peak.
19 November - Overflight and videotaping of Kitt Peak for an UA promotional tape arranged for Dr. P. Franken through the cooperation of mountain personnel and A. Hiller.
20 10 December - BBC video crew escorted to the mountain by Dr. D. Crawford for interviews and early evening "sky glow" shots to complete a special on "Light Pollution."
Other major projects for December were the re-issue of the in-house printed Kitt Peak brochure which will available the second week of January. PIR also did a mailing to encourage media coverage of the upcoming Astrophysics with Infrared Arrays conference in February.
Materials and historic pictures were collected, and interviews arranged for R. Bliss, who is organizing a year-long exhibit of the historic impact on the state of Arizona's astronomers (S. Wolff and H. Abt are among those featured) and observatories. The exhibit is entitled "Arizona's Astronomers" and will open 26 January in the Arizona Hall of Fame at the State Capitol Museum in downtown Phoenix.
21
TELESCOPE USAGE STATISTICS
October - December 1989 Appendix A
Astronomical Observations Scheduled Maintenance, Engineering, Hours Instrument Tests, Scheduled Hours Used Hours Lost Equipment Changes, etc. Telescope Visitors Staff Weather Failure
4-m 855.0 626.3 132.8 34.0 17.9 44.0
1.5-m 848.7 563.0 105.2 73.3 25.2 82.0
1-m 678.3 555.4 22.5 65.7 8.0 26.7
CTIO 0.9-m 814.5 588.8 120.7 59.6 6.9 38.5
*0.6/0.9-m 221.3 82.7 20.5 26.0 0 92.1
0.6-m 143.8 141.8 0 0 2.0 0
4-m 1083.01 590.69 173.82 250.0 30.0 38.5
2.1-m 0 0 0 0 0 0
CF 996.0 654.51 56.99 233.5 32.0 19.0
KPNO 1.3-m 983.25 473.71 146.29 284.25 43.0 36.0
#1-0.9-m 1025.75 586.25 143.5 287.25 7.75 1.0
#2-0.9-m 977.5 555.0 44.5 339.25 21.25 17.5
Schmidt 273.5 122.3 25.7 115.5 2.0 8.0
Hilltop 1753.0 1451.0 0 291.0 11.0 0
Vac Tower 806.0 115.0 273.0 195.0 79.0 144.0
Evans Fac 1659.0 675.0 372.0 462.0 118.0 32.0
NSO **FTS Lab 518.0 315.0 0 99.0 0 104.0
**McMath 1117.0 514.0 221.0 353.0 29.0 0
Vacuum 687.0 332.0 4.0 261.5 89.5 0
Fourier 627.0 535.0 0 77.0 15.0 0
Note: Scheduled hours are calculated according to the ephemerides for CTIO: October - 9.9 hours/night; November - 8.9 hours/night; December 8.2 hours/night * Use restricted to dark of the moon. ** Totals include both day and night hours. (All others are day only.)
CERRO TOLOLO INTER-AMERICAN OBSERVATORY OBSERVATIONAL PROGRAMS
APPENDIX "B"
October-November-December: Individual Telescope assignments are listed below. Graduate Students are indicated by an asterisk after their names. Nights assigned (hours worked), and telescope used are indicated. Service Observing programs are denoted by S.O. instead of nights assigned.
C. Anguita, M.T. Ruiz, U. de Chile: "CCD Parallaxes for Faint High Proper Motion Stars," 3(ll)1.5-m.
B. Anthony-Twarog, CTIO: "Standard Fields for CCD uvby," 4(33)0.9-m.
J. Baldwin, CTIO: "Monitoring QSOs for Variability," l(10)0.9-m.
R. Bell, U. of Maryland, J. Hesser, U. of Victoria, and G.H. Smith, Mt. Stromlo Observ.: "C and N Abundances Among 47 Tuc Main-Sequence Stars" 3(29)4-m.
M. Berrios, M. Maldini, J. Fernandez, and M. Guzman, U. de La Serena: "Activity and Rotational Modulation in RSCV„ Stars," 5(41)0.6-m.
E. Bica, UFRGS, Brazil, J. Claria, U. Nacional de Cordoba, Argentina, H. Dottori, and L. Grondin, UFRGS, Brazil: "Integrated UBV Photometry of LMC Clusters," 8(66)0.6-m.
H. Bond, Space Telescope Science Inst.: "CCD Photometric Monitoring of Planetary Nuclei," 5(44)0.9-m.
N. Caldwell, Whipple Observ., R. Kennicutt, U. of Arizona, and R. Schommer, Rutgers U.: "H II Regions in SO Galaxies," 3(28)4-m, 4(35)1.5-m.
A. Campbell, DTM, and R.A.W. Elson, Institute for Advanced Study: "A Search for Low-Mass Stars in 30 Doradus," 3(27)1.5-m.
B. Carney and J. Sturm*, U. of North Carolina: "Distance and Age of 47 Tuc," 4(43)4-m.
G. Cecil, Institute for Advanced Study, S. Heathcote and D. DePoy, CTIO: "Imaging Spectrophotometry of HH 34 and HH 46/47," 3(27)4-m.
G. Cecil, Institute for Advanced Study, and J. Bland, Rice U.: "Imaging Spectrophotometry of Ionized Filaments in the Galactic Wind of NGC 253," 3(28)4-m.
K. Chambers and P. Seitzer, Space Telescope Science Inst.: "Lyman a Emission from Primeval Galaxies," 3(28)4-m.
R. CiarduUo and G. Jacoby, KPNO, and H. Ford, Space Telescope Science Inst.: "Planetary Nebulae as Standard Candles: The Fornax Cluster," 4(24)4-m, 2(18)MS.
A. Cowley and P. Schmidtke, Arizona State U., D. Crampton and J. Hutchings, Dominion Astrophysical Observ.: "Direct Determination of Neutron Star Masses in Low-Mass X-ray Binaries," 4(36)4-m, 9(84)0.9-m.
A. Crotts, Goddard Space Flight Center, and S. Heathcote, CTIO: "The Dynamics and Morphology of the Emission-line Nebula Surrounding SN1987A," 2(19)4-m, 3(26)1.5-m. G. Da Costa, Yale U.: "The History of Star Formation in the LMC," 4(30)4-m.
G. Da Costa, Yale U.: "A Search for LMC Ousters with 3 < age < 12 Gyr," 6(59)1.5-m.
M. Davis, K. Fisher*, and M. Strauss, U. of California, Berkeley, A. Yahil, SUNY, Stony Brook, and J. Huchra, Haravard-Smithsonian Center for Astrophys.: "A Deep Redshift Survey of IRAS Galaxies," 6(63)1.5-m.
R. de Carvalho, Observatorio Nacional, Brasil, M. Franz, Harvard-Smithsonian Center for Astrophys., M. Strauss, U. of California, Berkeley, S. Djorgovski, and D. Thompsion, Caltech: "A New Distance-Indicator Relation for Elliptical Galaxies, and its Application," 10(81)0.9-m.
S. Demers, U. of Montreal, M. Irwin, U. of Cambridge, W. Kunkel, The Carnegie Observatories, and L. Grondin, U. of Montreal: "Investigation of Radial Velocities of Blue Stars Between the SMC and LMC," 3(34)l-m.
J. Elias, CTIO, G. Neugebauer, D. Sanders, B. Soifer, and P. Hacking, Caltech, and J.R. Houck, Cornell U.: "Cosmic Evolution of Infrared-Luminous Galaxies," 4(31)4-m, 4(33)0.9-m.
E. Fitzpatrick, Princeton U., and B. Bohannan, U. of Colorado: "High-Resolution Spectroscopy of OB Supergiants," 3(25)4-m.
E. Fitzpatrick, Princeton U.: "Metallicity Variations Among LMC B-type Supergiants," 7(55)l-m.
C. Folz, U. of Arizona, P. Hewett, Cambridge U., C. Hagen and F. Chaffee, U. of Arizona: "A Search for a Supercluster at High Redshift," 3(30)4-m.
G. Fontaine, F. Wesemael, S. Demers, R. Lamontagne, U. de Montreal, and M.J. Irwin, U. of Cambridge: "Follow-up Spectroscopic Observations of Blue Objects in the MCT Survey," 4(42)4-m, 4(38)1.5-m.
J.C. Forte and S. Cellone*, IAFE, Argentina, and D. Geisler, CTIO: "Washington Photometry of Low Surface Brightness Galaxies in Fornax," 2(20)1.5-m, 4(40)0.9-m.
L. French, Hanscom AFB, K. Russell, UK Schmidt, Siding Spring Observ., E. Bowell and S. Bus, Lowell Observ., and L. Shoemaker, U.S. Geological Survey: "A Search for L5 Trojan Asteroids, Recovery of New Asteroids and Search for Horseshoe Orbits," 11(83)MS, 3(22)0.6-m.
J. Graham, DTM, D. Geisler, N. Suntzeff, and T. Ingerson, CTIO, and M. Mateo, The Carnegie Observatories: "Abundances of Red Giants in Large Magellanic Cloud Clusters," 2(16)0.9-m.
S. Heathcote, CTIO, and B. Reipurth, ESO: "High Dispersion Spectroscopy of Jets from Young Stars," 4(33)4-m.
P. Hodge and E. Wilcots*, U. of Washington: "Faint HII Regions in the MCs," 5(47)0.9-m.
R. Humphreys, U. of Minnesota, D. Temdrup, CTIO, R. Pennington and S. Odewahn, U. of Minnesota: "Calibration Sequences for Galactic Structure Studies in the Bulge and Halo," 5(45)0.9-m.
D. Koo, U. of California, Santa Cruz, and D. Bennett, Princeton U.: "Multicolor Imaging of Twin Galaxies," S.O.(8)4-m. T. Lauer and M. Postman, Princeton U.: "The Motion of the Local Group with Respect to Nearby Abell Clusters," 4(36)1.5-m.
P. Lu, Western Connecticut State U.: "Faint Dwarf F-stars at South Galactic Pole," 9(88)l-m, 10(94)0.9-m.
P. Massey, KPNO, K. Garmany and J. Parker*, U. of Colorado: "The Massive Star Content of the Magellanic Clouds," 2(14)4-m, 3(27)1.5-m.
P. Massey, KPNO, and P. Conti, U. of Colorado: "The Spectra of Magellenic Qoud Wolf-Rayet Stars in the Near-IR," 4(34)1.5-m.
J. Maza, C. Anguita, and M.T. Ruiz, U. de Chile: "Proper Motion of the LMC," 3(26)1.5-m.
H. McAlister, W. Hartkopf, W. Bagnuolo, and J. Sowell, Georgia State U., and O. Franz, Lowell Observ.: "Binary Star Speckle Interferometry and Photometry," 5(48)4-m.
P. McCarthy, The Carnegie Observatories, H. Spinrad, W. van Breugel, and M. Dickson*, U. of California, Berkeley: "Spectroscopy of High Redshift Southern Radio Galaxies," 2(21)4-m.
A. McWilliam and D. Geisler, CTIO, L. Pasquini and J. Melnick, ESO: "Age-Composition Study of LMC M Supergiants," 3(23)4-m, 2(21)1.5-m.
J. Mould, Caltech, G. Bothun, U. of Michigan, J. Elias, CTIO, and N. Reid, Caltech: "Carbon Stars at the South Galactic Pole," l(10)1.5-m.
B. Penprase* and J.C. Blades, STScI: "Optical Spectroscopy of High Latitude Molecular Clouds," 3(8)1.5-m, 4(34)l-m.
R. Peterson, Tucson, AZ, and N. Caldwell, Whipple Observ.: "Stellar Velocity Dispersions for the Nuclei of Dwarf Galaxies in Fornax," 3(28)4-m.
M. Phillips, A. G6mez, M. Hamuy, S. Heathcote, J. Elias, G. Martin, M. Navarrete, N. Suntzeff, D. Temdrup, L. Wells, and R. Williams, CTIO: "Continuing Optical and Infrared Observations of SN 1987A in the LMC," 4(43)1.5-m, 5(23)l-m, 5(41)0.9-m.
R. Remillard and H. Bradt, MTT: "X-ray and Optical Study of Prototype HEAO-1 Sources," 6(58)1.5-m.
J. Rose and R. Agostinho*, U. of North Carolina: "The Vertical Struture of Our Galaxy," 2(17)1.5-m, 3(13)0.6-m.
M.T. Ruiz, J. Maza, and C. Anguita, U. de Chile: "Search and Study of Faint Nearby Stars," 4(27)4-m.
R. Schommer, Rutgers U., G. Bothun, U. of Michigan, T. Williams, Rutgers U., and J. Mould, Caltech: "Large Scale Motions and Deviations from Hubble Flow," l(9)0.9-m.
R. Samec, Butler U.: "Continuing Photometric Study of Very Short Period Eclipsing Binaries," 7(40)1-m.
P. Seitzer, STScI: "The Masses of LMC Globular Clusters," 4(36)4-m, 2(18)0.9-m. M. Shara and H. Ford, SCScI, R. Williams, CTIO, R. Qardullo, KPNO, and S. Winkelman*, U. of Michigan: "Recovery of Novae and Detection of Dwarf Novae in the Magellanic Clouds," 2(18)4-m.
M. Shara, R. Burg, C. Sturch, and L. Siciliano, STScI: "The Second Guide Star Photometric Catalog," 3(30)0.9-m.
S. Shawl, U. of Kansas, and D. Bord, U. of Michigan: "A Spectroscopic Search for Companions to Southern Long-Period Variable Stars," 5(43)l-m.
V. Smith and D. Lambert, U. of Texas: "Enhanced Lithium and s-Process Abundances in Magellanic Qoud AGB Stars," 5(48)4-m.
N. Suntzeff, CTIO, and J. Nemec, U. of British Columbia: "A Proper Motion Survey of the Sculptor Dwarf Galaxy," 3(19)4-m.
B. Twarog and B. Anthony-Twarog, CTIO, and J. Laird, Bowling Green State U.: "Extension and Expansion of the uvby Photometric System," 19(129)l-m.
Wakamatsu, K., Gifu U., and M. Nishida, Kobe Women's U.: "Seyfert Nuclei Survey for Ring Galaxies of Arp-Madore Catalogue," 4(36)1.5-m, 4(40)0.9-m.
N. Walbom, STScI, and E. Fitzpatrick, Princeton U.: "Digital Spectroscopy of Three Exceptional OB Ousters in the Southern Milky Way," 3(26) 1-m.
A. Walker, CTIO, G. Jacoby and R. CiarduUo, KPNO: "Magellanic Qoud Planetary Nebulae Luminosity Functions," 7(46)0.9-m.
B. Welsh, STScI, J. Vallerga and P. Vedder, U. of California, Berkeley: "High Resolution Sodium Absorption Studies Towards Very Low Reddened Stars," 4(34)1.5-m.
L. Wells, CTIO: "The Search for ELGs in the Pisces-Cetus Void," 1(5)MS.
T. Williams, Rutgers U., and M. Weinberg, Inst, for Advanced Study: "Kinematic Maps of the Stars and Gas in Barred Spiral Galaxies," 3(28)4-m.
D. York, U. of Chicago, A. Crotts, Goddard Space Flight Or., D. Koo, U. of California, Santa Cruz, and R. Green, KPNO: "Mg II Absorbers in a Cone at the South Galactic Pole," 3(31)4-m.
YALE PROGRAMS
A. Layden* and R. Zinn: "Metallicities and Kinematics of Field RR-Lyrae Stars," 13(108)l-m. KITT PEAK NATIONAL OBSERVATORY OBSERVATIONAL PROGRAMS Executed Proposals 10/01/89 - 12/31/89 Page 1 Mon Jan 15 08:04:01 1990 APPENDIX B
Nights Hours Days Hours 7879 9 f89 M Abbott, J Hoessel, University of Wisconsin Cluster-Cluster Correlations and the Large-Scale Structure 4 meter 3.00 30.50 0.00 0.00
7615 2 f89 H Abt, N Morrell, National Optical Astronomy Observatories Binary Frequency in the alpha Persei Cluster Coude Feed 5.00 28.50 0.00 0.00
7977 4 f89 M Allen, T Snow, Jr., University of Colorado CH+ Column Densities in Spectra of Reddened Stars Coude Feed 3.00 22.50 0.00 0.00
7950 2 f89 C Ambruster, C Ready, D Steelman, Villanova University A Hull, Perkin-Elmer Corportion Determining the First Rotation Periods of Fully Convective Nr. 2 0.9 meter 8.00 80.00 0.00 0.00
7929 8 f89 T Armandroff, National Optical Astronomy Observatories P Seitzer, Space Telescope Science Institute The Globular Clusters in the M31 Halo 4 meter 3.00 34.50 0.00 0.00
7881 4 f89 B Balick, E Wilcots, G Gonzalez, University of Washington I Gatley, National Optical Astronomy Observatories T Hasegawa, Nobeyama Radio Observatory B Zuckerman, University of California, Los Angeles Molecular Excitation in the Molecular Clouds of Planetary 1.3 meter 5.00 36.00 0.00 0.00 Executed Proposals 10/01/89 - 12/31/89 Page 2 Mon Jan 15 08:04:01 1990
Nights Hours Days Hours 7949 9 f89 M Bershady, M Hereld, University of Chicago R Kron, J Munn, University of Chicago, Yerkes Obs. K Bank Imaging of Distant Galaxies: Post-Main-Sequence 4 meter 4.00 43.00 0.00 0.00
7919 2 f89 H Bond, Space Telescope Science Institute R CiarduUo, National Optical Astronomy Observatories CCD Photometric Monitoring of Nuclei of Planetary Nebulae Nr. 1 0.9 meter 10.00 112.25 0.00 0.00
7983 2 f89 R Boyle, Dickinson College J Ready, Los Alamos National Laboratory D Jennings, G Wiedemann, NASA Goddard Space Flight Center S Ridgway, National Optical Astronomy Observatories
Spectroscopy of C3, Methylene, and Vinyl in Heavily 4 meter 0.00 0.00 9.00 44.25
7864 5 f89 A Brown, F Walter, A Hayden, University of Colorado F Vrba, U.S. Naval Observatory, Flagstaff UBVRI Survey and Monitoring of Naked T Tauri Stars in Orion Nr. 2 0.9 meter 12.00 54.50 0.00 0.00
7886 2 f89 J Brown, University of Washington H Johnson, Indiana University K Hinkle, National Optical Astronomy Observatories 10830 in MS/S Stars 4 meter 1.00 12.00 1.00 2.00
7876 8 f89 H Bushouse, Northwestern University Spectral Properties of Interacting Galaxies Nr. 2 0.9 meter 6.00 22.50 0.00 0.00 Executed Proposals 10/01/89 - 12/31/89 Page 3 Mon Jan 15 08:04:01 1990
Nights Hours Days Hours 7847 7 f89 M Carini, H Miller, J Wilson, Georgia State University B Goodrich, National Optical Astronomy Observatories An Investigation of Short-Term Variability for Selected BL Nr. 1 0.9 meter 6.00 69.50 0.00 0.00
7827 2 f89 M Castelaz, J Stein, T Persinger, Allegheny Observatory Continued Intermediate-band Photometry for Determination Nr. 2 0.9 meter 6.50 56.50 0.00 0.00
7931 1 f89 C Chapman, D Davis, S Weidenschilling, D Levy, M Magee, D Spaute, S Howell, Planetary Science Institute Photometric Geodesy of Main-Belt Asteroids Nr. 2 0.9 meter 5.00 25.00 0.00 0.00
7421 8 f89 R CiarduUo, National Optical Astronomy Observatories H alpha Observations of Novae in Local Group Galaxies Nr. 1 0.9 meter 2.00 24.00 0.00 0.00
7846 8 f89 R CiarduUo, G Jacoby, National Optical Astronomy Observatories W Harris, McMaster University Planetary Nebulae as Standard Candles: The NGC 1023 Group 4 meter 3.00 24.00 0.00 0.00
7844 8 f89 R Davies, D Axon, A Pedlar, Nuffield Radio Astronomy Laboratories E Hummel, M Shaw, University of Manchester L Staveley-Smith, Anglo-Australian Observatory Structure and Evolution of Dwarf Galaxies Nr. 1 0.9 meter 5.00 32.00 0.00 0.00 Executed Proposals 10/01/89 - 12/31/89 Page 4 Mon Jan 15 08:04:01 1990
Nights Hours Days Hours 7853 8 f89 R Elston, National Optical Astronomy Observatories D Zaritsky, University of Arizona M Cornell, University of Texas, Austin CCD Atlas of Large Spiral Galaxies Burrell Schmidt 5.00 30.00 0.00 0.00
7855 7 f89 R Elston, National Optical Astronomy Observatories P Maloney, Leiden University Molecular Gas in Nearby AGNs 4 meter 4.00 43.00 0.00 0.00
7831 2 f89 F Fekel, Vanderbilt University G Henry, Tennessee State University Spectroscopy of Binary and Multiple Stars Coude Feed 7.00 81.00 0.00 0.00
7992 2 f89 H Ford, University of Michigan R CiarduUo, G Jacoby, National Optical Astronomy Observatories X Hui, Johns Hopkins University Dynamics of M31's Stellar Halo 4 meter 4.00 39.00 0.00 0.00
7933 2 f89 W Forrest, University of Rochester M Skrutskie, University of Massachusetts J Stauffer, NASA Ames Research Center R Joyce, R Probst, National Optical Astronomy Observatories J Lunine, University of Arizona M Shure, University of Hawaii Infrared Spectroscopy of Very Low Mass Objects 4 meter 3.00 14.50 0.00 0.00
8003 4 f89 P Frisch, University of Chicago J Fowler, Apache Point Observatory Nearby Interstellar Clouds Coude Feed 3.00 0.00 0.00 0.00 Executed Proposals 10/01/89 - 12/31/89 Page 5 Mon Jan 15 08:04:01 1990
Nights Hours Days Hours 7869 8 f89 J Frogel, Ohio State University R Davies, University of Oxford D Terndrup, Cerro Tololo Interamerican Observatory The Stellar Content of the Bulge of M31 4 meter 3.00 22.00 0.00 0.00
7890 9 f89 A Fruchter, Carnegie Institution of Washington G Bothun, University of Michigan T Lauer, Princeton University Peculiar Velocities: Real or Reflection of Systematic Error 4 meter 4.00 28.00 0.00 0.00
7820 7 f89 R Garden, D Grolemund, M Burton, University of California, Irvine M Yates, University of California, Berkeley Simultaneous Optical and Infrared Spectroscopy of High Red 4 meter 3.00 12.00 0.00 0.00
7922 2 f89 D Gies, J Sowell, Georgia State University H Henrichs, University of Amsterdam H Ellis, Ball Aerospace Pulsation and Stellar Wind Variations in O-Type Stars Coude Feed 6.00 54.00 0.00 0.00
7790 5 f89 J Graham, Carnegie Institution of Washington Faint Emission-Line Stars in Orion Burrell Schmidt 3.00 9.00 0.00 0.00
7775 2 f89 A Grauer, University of Arkansas Time-Series Photometry of Hot Evolved Stars 1.3 meter 8.00 36.00 0.00 0.00
7878 3 f89 P Green, B Margon, University of Washington Distant Halo Carbon Stars as Tracers of the Galactic Potent Nr. 1 0.9 meter 4.00 46.00 0.00 0.00 Executed Proposals 10/01/89 - 12/31/89 Page 6 Mon Jan 15 08:04:01 1990
Nights Hours Days Hours 9098 0 f89 L Hobbs, University of Chicago, Yerkes Obs. B Penprase, B Bhattacharya, Space Telescope Science Institute Survey of High Latitude Molecular Clouds Nr. 2 0.9 meter 3.50 0.00 0.00 0.00
7991 6 f89 K Home, T Marsh, H Bond, Space Telescope Science Institute F Verbunt, G Hassinger, Max Planck Institute K Mitsuda, ISAS Simultaneous X-ray and Optical Observations of Cyg X-2 4 meter 2.00 16.00 0.00 0.00 Nr. 1 0.9 meter 3.00 22.50 0.00 0.00
7859 2 f89 D Huenemoerder, L Ramsey, D Buzasi, Pennsylvania State University UX Ari at High Resolution: Mass Transfer and Other Activity Coude Feed 5.00 60.00 0.00 0.00
7871 2 f89 S Hulbert, Case Western Reserve University CNO Abundances in OB Runaways Coude Feed 5.00 24.50 0.00 0.00
7851 2 f89 K Janes, T Liu, T Bania, Boston University Radial Velocities of Young Open Clusters Coude Feed 7.00 66.00 0.00 0.00
7940 2 f89 T Jarrett, R Dickman, University of Massachusetts W Herbst, Wesleyan University Optical/Infrared Study of Faint End of Stellar Luminosity Nr. 1 0.9 meter 7.00 64.00 0.00 0.00
7984 7 f89 V Junkkarinen, T Barlow, University of California, San Diego Photometric Monitoring of Broad Absorption Line QSOs Nr. 1 0.9 meter 8.00 31.50 0.00 0.00 Executed Proposals 10/01/89 - 12/31/89 Page 7 Mon Jan 15 08:04:01 1990
Nights Hours Days Hours 7781 2 f89 J Kaluzny, Warsaw University Observatory S Rucinski, David Dunlap Observatory Searching for Orbital Eccentricity in Old Novae Nr. 1 0.9 meter 7.00 74.00 0.00 0.00
7785 2 f89 J Kaluzny, Space Telescope Science Institute S Rucinski, York University Photometric Study of Distant Anticenter Clusters Nr. 1 0.9 meter 6.00 68.00 0.00 0.00
7887 5 f89 S Kenyon, L Hartmann, Harvard-Smithsonian Center for Astrophysics S Strom, K Strom, University of Massachusetts Infrared Spectra of Luminous Pre-Main Sequence Stars 1.3 meter 4.00 35.00 0.00 0.00
7588 2 f89 T Kinman, National Optical Astronomy Observatories Visual and I.R. photometry of nearby RR Lyrae stars 1.3 meter 7.00 56.50 0.00 0.00
7811 2 f89 T Kinman, N Sharp, National Optical Astronomy Observatories Visual and Infrared Photometry of Nearby RR Lyrae Stars Nr. 2 0.9 meter 5.00 37.50 0.00 0.00 Nr. 1 0.9 meter 3.00 17.00 0.00 0.00
7806 2 f89 R Kirshner, E Schlegel, Harvard-Smithsonian Center for Astrophysics CCD Photometry of Supernovae 4 meter 1.00 4.50 0.00 0.00
7807 6 f89 R Kirshner, Harvard-Smithsonian Center for Astrophysics R Smith, Center for Astrophysics K Long, W Blair, Johns Hopkins University P Winkler, Middlebury College Search for Supernova Remnants in M33 4 meter 3.00 2.50 0.00 0.00 Executed Proposals 10/01/89 - 12/31/89 Page 8 Mon Jan 15 08:04:01 1990
Nights Hours Days Hours 7968 2 f89 S Kleinmann, University of Massachusetts M Tamura, R Joyce, National Optical Astronomy Observatories Extremely Red IRAS Variables 1.3 meter 3.00 12.00 0.00 0.00
7979 7 f89 S Kleinmann, University of Massachusetts M Tamura, R Joyce, National Optical Astronomy Observatories N Scoville, California Institute of Technology Near-Infrared Spectroscopy of AGNs and Starburst Galaxies 4 meter 3.00 24.00 0.00 0.00
7988 9 f89 D Koo, University of California, Santa Cruz R Kron, S Majewski, J Munn, University of Chicago, Yerkes Obs. J Tyson, Bell Laboratories U-Band Imaging of Very Faint Field Galaxies 4 meter 1.00 11.50 0.00 0.00
7735 7 f89 R Kron, S Majewski, J Munn, University of Chicago, Yerkes Obs. M Bershady, University of Chicago Complete Survey of Quasars to B - 22.5 4 meter 2.00 24.00 0.00 0.00
7783 10 f89 A Landolt, Louisiana State University Broad-band Monitoring of Space Telescope Spectrophotometric 1.3 meter 4.00 18.00 0.00 0.00
7838 9 f89 T Lauer, M Postman, Princeton University S Wallington, University of Arizona The Motion of the Local Group With Respect to Nearby Abell 4 meter 3.00 14.25 0.00 0.00 Executed Proposals 10/01/89 - 12/31/89 Page 9 Mon Jan 15 08:04:01 1990
Nights Hours Days Hours 7874 5 f89 R Lee, University of Wisconsin, Madison R Mathieu, University of Wisconsin F Walter, University of Colorado A Welty, University of Massachusetts Spectrophotometric Studies of Double-Lined Pre-Main Sequenc 4 meter 3.00 36.00 0.00 0.00 Nr. 2 0.9 meter 7.00 86.00 0.00 0.00
7974 5 f89 P Lena, Observatoire de Paris C Dugados, Observatoire de Paris - Meudon S Ridgway, National Optical Astronomy Observatories J Christou, NOAO-ADP IRc2 in the BN-KL Complex of Orion 4 meter 3.00 37.50 0.00 0.00
8002 4 f89 S Lord, NASA Ames Research Center M Burton, University of California, Irvine B Smith, University of Texas, Austin The Excitation of the Interstellar Medium in Galaxies 1.3 meter 4.00 38.00 0.00 0.00
7780 2 f89 R Luck, Case Western Reserve University Chemical Abundances in Normal A and Early F Stars Coude Feed 6.00 55.00 0.00 0.00
7896 5 f89 M Margulis, University of Massachusetts U Sofia, University of Wisconsin Luminosity Evolution of Young Stellar Objects in Orions 1.3 meter 6.00 23.50 0.00 0.00
7917 4 f89 D Massa, Applied Research Corporation E Fitzpatrick, Washburn Observatory G Clayton, NASA Headquarters J Cardelli, University of Wisconsin A Study of Interstellar Extinction in the NIR and Optical 1.3 meter 7.00 12.00 0.00 0.00 Nr. 2 0.9 meter 5.50 58.00 0.00 0.00 Executed Proposals 10/01/89 - 12/31/89 Page 10 Mon Jan 15 08:04:01 1990
Nights Hours Days Hours 7952 2 f89 R Mathieu, University of Wisconsin S Levine, University of Wisconsin, Madison J Morse, University of North Carolina The Internal Kinematics of OB Associations Coude Feed 6.00 72.00 0.00 0.00
7823 4 f89 D Meyer, Northwestern University High Resolution Observations of Interstellar CN Toward Zeta Coude Feed 4.00 38.00 0.00 0.00
7936 4 f89 D Meyer, Northwestern University M Womack, Arizona State University The Excitation of Interstellar CH Toward Zeta Persei Coude Feed 4.00 36.50 0.00 0.00
7814 2 f89 T Meylan, Georgia State University Abundance Survey of Solar Neighborhood Solar-like Stars Coude Feed 5.00 48.00 0.00 0.00
8006 1 f89 M Mumma, A Storrs, S Hoban, D Reuter, D Glenar, F Espenak, NASA Goddard Space Flight Center H Weaver, Space Telescope Science Institute H Larson, University of Arizona Investigation of the Hydrocarbon Composition of Comets 1.3 meter 3.00 39.00 0.00 0.00
7812 2 f89 C Neese, T Armandroff, P Massey, National Optical Astronomy Observatories Spectroscopy of Ha Emission-Line Stars in M33 4 meter 2.00 21.00 0.00 0.00
7892 2 f89 T Oswalt, S Penton, L Roberts, Florida Institute of Technology P Hintzen, NASA Goddard Space Flight Center E Sion, Villanova University Spectroscopy of Faint Luyten White Dwarf Binaries 4 meter 3.00 0.00 0.00 0.00 Executed Proposals 10/01/89 - 12/31/89 Page 11 Mon Jan 15 08:04:01 1990
Nights Hours Days Hours 7953 2 f89 J Patterson, M Eracleous, E Gotthelf, Columbia University Orbital Dips in Dwarf Novae: The Little Dippers Nr. 2 0.9 meter 11.50 90.00 0.00 0.00
7935 4 f89 B Penprase, J Blades, Space Telescope Science Institute Optical Spectroscopy of High Latitude Molecular Cloud Cores Coude Feed 6.00 4 9.00 0.00 0.00
7857 2 f89 C Pilachowski, National Optical Astronomy Observatories D Bruning, University of Louisville R Milkey, Space Telescope Science Institute The Rotation of 40 Eri B Coude Feed 2.00 3.00 0.00 0.00
7889 2 f89 C Pilachowski, J Booth, National Optical Astronomy Observatories C Sneden, University of Texas, Austin Lithium Dilution in Halo Subgiants Coude Feed 3.50 41.00 0.00 0.00
8000 8 f89 A Porter, National Optical Astronomy Observatories T Tripp, summer student Isophotometry of Large cD Halos Burrell Schmidt 2.00 0.00 0.00 0.00
8007 6 f89 R Remillard, Massachusetts Institute of Technology W Roberts, Harvard-Smithsonian Center for Astrophysics Completion of the Catalog of X-Ray Sources from HEAO-1 Burrell Schmidt 5.00 47.00 0.00 0.00 Executed Proposals 10/01/89 - 12/31/89 Page 12 Mon Jan 15 08:04:01 1990
Nights Hours Days Hours 7924 2 f89 R Sahai, University of Goteborg K Hinkle, National Optical Astronomy Observatories Infrared Spectroscopy of the Binary Carbon Star V Hydrae 4 meter 0.00 0.00 4.00 17.50
7921 8 f89 J Salzer, Arecibo Observatory R Elston, National Optical Astronomy Observatories Distributions of Young & Old Stellar Populations in Dwarf 1.3 meter 5.00 41.00 0.00 0.00 Nr. 1 0.9 meter 4.00 39.00 0.00 0.00
7818 1 f89 B Schaefer, M Schaefer, NASA Goddard Space Flight Center Reflectance Curves for the Outer Jovian Satellites Nr. 1 0.9 meter 4.00 38.00 0.00 0.00
7843 2 f89 P Schmidtke, Arizona State University J Africano, National Optical Astronomy Observatories Lunar Occultations of Double Stars Nr. 2 0.9 meter 2.00 14.00 0.00 0.00
7875 8 f89 P Seitzer, Space Telescope Science Institute T Armandroff, National Optical Astronomy Observatories C Caldwell, Smithsonian Whipple Observatory G Da Costa, Yale University The Dwarf Spheroidal Companions of M31 Burrell Schmidt 6.00 62.00 0.00 0.00
7893 5 f89 M Simon, SUNY at Stony Brook W Chen, State University of New York A Search for Wide Binaries Among the Young Stars in Taurus 1.3 meter 3.00 30.00 0.00 0.00 Executed Proposals 10/01/89 - 12/31/89 Page 13 Mon Jan 15 08:04:01 1990
Nights Hours Days Hours 7826 2 f89 T Simon, S Balachandran, University of Hawaii Rotation Periods of Young Stars Nr. 2 0.9 meter 7.00 14.00 0.00 0.00
7777 2 f89 A Slettebak, Perkins Observatory Balmer Emission Decrements in Be Stars Coude Feed 6.00 32.50 0.00 0.00
7779 2 f89 J Sowell, J Wilson, H McAlister, Georgia State University All-Sky Stromgren Photometry of Speckle Binaries Nr. 2 0.9 meter 7.00 61.50 0.00 0.00
7833 8 f89 A Stanford, A Code, University of Wisconsin Probing Obscured Star-Forming Regions in Colliding Galaxies 1.3 meter 4.00 24.00 0.00 0.00
7860 2 f89 J Stauffer, NASA Ames Research Center R Probst, National Optical Astronomy Observatories The Time Spread of Star Formation in the Pleiades Nr. 1 0.9 meter 5.00 19.00 0.00 0.00
7803 5 f89 K Strom, M Margulis, S Strom, University of Massachusetts The Star-forming History of the L1641 Molecular cloud 1.3 meter 4.00 46.50 0.00 0.00
7903 5 f89 S Strom, K Strom, J Fleischman, A Welty, L Allen, University of Massachusetts S Edwards, Smith College Constraints on Evolutionary Timescales from YSO Binary 4 meter 3.00 37 .50 0.00 0..00 1.3 meter 2.00 21 .50 0.00 0..00 Nr. 1 0.9 meter 2.00 0..00 0.00 0..00 Executed Proposals 10/01/89 - 12/31/89 Page 14 Mon Jan 15 08:04:01 1990
Nights Hours Days Hours 7801 2 f89 P Szkody, University of Washington S Howell, Planetary Science Institute Blue and Near IR Spectroscopy of Two Ultra-short Period 4 meter 2.00 23.50 0.00 0.00
7971 4 f89 M Tamura, National Optical Astronomy Observatories S Kleinmann, University of Massachusetts S Sato, Tokyo Astronomical Observatory T Yamashita, M Sekiguchi, Kyoto University H Suto, University of Hawaii Infrared Polarization Mapping of Mass Outflows Protostars 1.3 meter 6.00 67.00 0.00 0.00
7791 8 f89 T Thuan, University of Virginia H Loose, University of Gottingen Near-Infrared Imaging of Blue Compact Dwarf Galaxies 1.3 meter 6.00 13.00 0.00 0.00
7868 7 f89 E Turner, Princeton University J Hewitt, Princeton University Observatory B Burke, Massachusetts Institute of Technology D Schneider, Institute for Advanced Study CCD Observations of VLA Gravitational Lens Candidates 4 meter 4.00 30.00 0.00 0.00
7882 4 f89 W Waller, M Lee, University of Washington D DePoy, R Joyce, M Tamura, National Optical Astronomy Observatories M Ward, Institute of Astronomy Ionized and Molecular Hydrogen in Extragalactic Starbursts 1.3 meter 6.00 71.00 0.00 0.00
7863 5 f89 F Walter, A Brown, University of Colorado S Barden, National Optical Astronomy Observatories R Mathieu, University of Wisconsin F Vrba, U.S. Naval Observatory, Flagstaff The Initial Mass Function in Star Forming Regions 4 meter 4.00 32.50 0.00 0.00 Executed Proposals 10/01/89 - 12/31/89 Page 15 Mon Jan 15 08:04:01 1990
Nights Hours Days Hours 7930 9 f89 S Warren, University of Arizona P Osmer, National Optical Astronomy Observatories A Search for Young Galaxies Using Narrow-Band Filters 4 meter 2.00 13.50 0.00 0.00
7913 8 f89 B Whitmore, S Zepf, Space Telescope Science Institute How is the Dark Matter Stripped from Cluster Spirals? Nr. 1 0.9 meter 4.00 40.00 0.00 0.00
7954 8 f89 A Wolfe, D Turnshek, L Lu, University of Pittsburgh K Lanzetta, Cambridge University A Survey for the Progenitors of Galactic Disks 4 meter 4.00 47.00 0.00 0.00
7938 3 f89 R Wyse, T Smecker, Johns Hopkins University Galactic Halo Metallicity Gradient 4 meter 4.00 23.00 0.00 0.00
7941 5 f89 J Young, L Allen, S Kleinmann, University of Massachusetts Massive Star Formation Efficiency in Spiral Galaxies Nr. 1 0.9 meter 5.00 33.00 0.00 0.00
Total number of proposals: 94
NATIONAL SOLAR OBSERVATORY REPORT Quarter Ended: 12/31/89
Nights Hours Days Hours
1023 R Altrock, National Optical Astronomy Observatories S/B003-Coronal Observations Evans Solar Facility/SP 84 128
1369 R Altrock, L Gilliam, National Optical Astronomy Observatories S/B224-Daily Solar Activity Reports for Solar Forecasting Evans Solar Facility/SP 3 45
1511 R Altrock, L Gilliam, National Optical Astronomy Observatories H Zirin, California Institute of Technology S/B269-Search for A XIV 4412A Evans Solar Facility/SP 5 13
1212 P Bemath, C Brazier, L O'Brien, D Perera, M Oliphant, M Lee, University of Arizona D Carrick, U.S. Air Force Astronautics Lab T/Spectroscopy of Molecules of Astrophysical Interest FTS 4 64
1373 T Brown, High Altitude Observatory K Streander, National Optical Astronomy Observatories S/H027-J-Sunspots (Hilltop®SP and FT @ Tucson) Fourier Tachometer 74 535
1476 D Bruning, University of Louisville S Saar, Harvard-Smithsonian Center for Astrophysics T/Line Asymmetries in Late-type Dwarfs McMath Main 3 26V2
1382 T Darvann, University of Oslo R Dunn, National Optical Astronomy Observatories S/T317-Adaptive Optics LEST Seeing Test Vacuum Tower/SP 7 56
18:08 an Thundiy Februtiy 8, 1990 »
1089 R Dunn, National Optical Astronomy Observatories S/B230-Tower Engineering Evans Solar Facility/SP 22
1441 J Eaton, Indiana University T/Balmer Lines in Zeta-Aurigae Binaries McMath Main
1423 D Elkins, D Tans, M Hall, M Kitzis, NOAA T/Solar IR Absorption Measurements of Atmospheric Trace... FTS 16
1180 G Elste, University of Michigan S/B183-Limb Darkening Freed from Scattered Light in Telesc. Evans Solar Facility/SP 13 48
1478 Q Fontenla, D Hathaway, NASA/Marshall Space Flight Center D Rabin, National Optical Astronomy Observatories T/P-mode Phase Relations in Mgl X4571 McMath Main 63
1483 P Foukal, Cambridge Research & Instrumentation, Inc. J Moran, Harvard-Smithsonian Center for Astrophysics S/B261-Electric Fields Evans Solar Facility/SP 16 79
1526 B Franklin, National Solar Observatory/Sac Peak S Colley, National Optical Astronomy Observatories S/B271-Coelostat Guider Tests Evans Solar Facility/SP
18:08 an ThuradiyFebnjuy 8, 1990 iquiii:Ail/}ahnson/qtr.inpuiyouipul2 1429 M Giampapa, National Optical Astronomy Observatories T/Synoptic Observations of Ha Profile Variability in ... McMath Main 12 357a
1448 M Giampapa, National Optical Astronomy Observatories T/Synoptic Studies of Ha in "Marginal" BY Draconis Stars McMath Main 62
1461 M Giampapa, National Optical Astronomy Observatories T/Rotational Modulations of the He I D3 Line in Active.... McMath Main 26'/2
1025 L Gilliam, National Optical Astronomy Observatories S/B057-Monitoring:Community Evans Solar Facility/SP 50 104
1026 L Gilliam, National Optical Astronomy Observatories S/B062-Coronagroph Monitor Evans Solar Facility/SP 23 53
1034 L Gilliam, National Optical Astronomy Observatories S/H001-Flare Patrol (Monitoring) Hilltop Dome/SP 92 671
1035 L Gilliam, National Optical Astronomy Observatories S/H002-White Light Patrol (Monitoring) Hilltop Dome/SP 92 632
1036 14 489 L Gilliam, National Optical Astronomy Observatories S/H003-Multiple Bank Polarimeter (Monitoring) Hilltop Dome/SP 65
18:08 an ThurvhyFebruuy 8, 1990 •quila:/u1/johnson/qlr.inpul/oulpul2 1039 L Gilliam, National Optical Astronomy Observatories S/H008-White Light Sunspot Drawing Hilltop Dome/SP 92 83
1463 E Guinan, G McCook, F Maloney, Villanova University M Richards, University of Virginia T/Synoptic Gas Dynamics Accretion Surface Activity .... McMath Main 4 12'/2
1349 S Habbal, Harvard-Smithsonian Center for Astrophysics K Harvey, Solar Physics %NSO R Gonzalez, National Radio Astronomy Observatory T/Multiwavelength Observations of Time-Varying Phenomena... VAC 2 12
1489 D Haber, National Optical Astronomy Observatories S/T338-Public Info Photograph of Tower Vacuum Tower/SP 9 66
1386 J Harvey, National Optical Astronomy Observatories T/General Community Support-Non-Synoptic VAC 11 31
3790 J Harvey, National Optical Astronomy Observatories T/Vacuum Synoptic Program:Daily/Community VAC 92 288
1055 D Jennings, G Wiedemann, D Deming, NASA Goddard Space Flight Center R Boyle, Dickinson College T Hewagama, University of Maryland T/Infrared Spectroscopy of Sun, Stars, & Planets Using.... FTS 11 58
1260 H Jones, NASA Goddard Space Flight Center T/NASA/Flight Mission Support/Max '91 VAC 1 5
18:08 an Thursdiy February 8, 1990 iquila:/ul/jahnson/qti.inpui/ouiput2 -5-
1504 S Keil, National Optical Astronomy Observatories S/T337-Solar Dynamics A Vacuum Tower/SP 6 4
1529 S Keil, National Optical Astronomy Observatories S/T343-Solar Dynamics B Vacuum Tower/SP 9 65
1149 W Livingston, L Wallace, National Optical Astronomy Observatories T/Solar Irradiance Line Bisectors McMath Main 2 16
1209 W Livingston, L Wallace, National Optical Astronomy Observatories M Steffen, Kiel University T/Spectrum Irradiance Variability of Sun McMath Main 6 33
5877 J LoPresto, Edinboro University of Pennylvania C Schrader, Edinboro University of Pennsylvania T/Solar Gravitiational Redshift McMath Main 7 21
1135 P Mcintosh, National Oceanic & Atmospheric Admin.,Boulder D Marquett, California Institute of Technology L Gilliam, National Optical Astronomy Observatories S/B001-NOAA Monitoring Program Evans Solar Facility/SP 88 132
1477 W Mitchell, Jr., Ohio State University T/High resolution Spectra of the Solar Flux FTS 4 23
1488 H Nations, Franklin & Marshall College L Marschall, Gettysburg College T/Synoptic Spectroscopy of X-ray Selected Late-type Binary. McMath Main 18 87>/2
18:08an Thundiy February 8.1990 iquili:Ail/jahn»on/qLr.input/outpui2 -6
1136 H Neckel, Hamburger Stemwarte D Labs, Landesstemwarte Heidelberg D Marquett, California Institute of Technology T/FTS Spectra FTS 3 2
1150 H Neckel, Hamburger Stemwarte D Labs, Landesstemwarte Heidelberg T/Limb Darkening FTS 7 42
1331 JNeff, T/Ca II K Spectral Images of RS CVN Systems McMath Main 3 19'/2
1462 JNeff, S Saar, Harvard-Smithsonian Center for Astrophysics T/TiO Bandhead Measurements of Starspots Area and Temp. McMath Main 6 57lh
1412 D Neidig, Sacramento Peak Observatory A Kiplinger, B Dennis, NASA Goddard Space Flight Center S/T323-Coordinated Optical & SMM Hard Xray Observations.... Vacuum Tower/SP 6 39
1513 D Neidig, Sacramento Peak Observatory S/T342-Simultaneous Three-Wavelength Flare Photomerty ... Vacuum Tower/SP 23 97
1235 A Pierce, National Optical Astronomy Observatories T/Solar Gravitational Redshift McMath Main 14 48
1390 R Radick, National Solar Observatory S/B234-Effect of Activity on Stromgren Color Indices Evans Solar Facility/SP 7 53
18:08 an Thuridiy February 8.1990 «quili:/u:/johnsoa/qu.input/ouipui2 1524 D Restaino, Universita di Firenze S/B265-Wave Behavior in the Photosphere 5434A Evans Solar Facility/SP 14 7g
1222 C Rinsland, J Levine, NASA Langley Research Center T/Monitoring of Long Term Trends in Concentrations of.... m 8 92
1525 D Rust, Johns Hopkins University S/B270-Solar Vector Magnetograph Filter Tests Evans Solar Facility/SP 5 15
1425 S Saar, Harvard-Smithsonian Center for Astrophysics J Linsky, University of Colorado T/A Survey of Magnetic Fields on G and K Stars McMath Main 6 511/2
1426 S Saar, Harvard-Smithsonian Center for Astrophysics J Linsky, University of Colorado M Giampapa, National Optical Astronomy Observatories T/Synoptic Observations of Magnetic Fields on G & K Stars McMath Main 5 28
1131 E Seykora, East Carolina University S/B174-Ca K, Ha Spectroheliograms Evans Solar Facility/SP j j
1251 E Seykora, East Carolina University S/B 191-Investigation of Very Low Contrast White Solar... Evans Solar Facility/SP 2 8
1492 T Simon, S Balachandran, University of Hawaii T/Multisite Continuous Spectroscopy (MUSICOS) McMath Main 9 69
1417 K Sivaraman, Indian Institute of Astrophysics S/T328-Evershed Effect in Bipolar Spots Vacuum Tower/SP 1j 9
18:08 an Thursday February 8, 1990 ., lw.u aquilaJu1/johnson/qlr.inpuiyouipul2 1053 M Smith, CSC/IUE Observatory/NASA T/Radial Velocity Variations of Alpha Ori and Two other.... McMath Main 6 10
1356 K Strassmeier, Vanderbilt University T/Doppler Imaging of Spotted Chromospherically Active Stars McMath Main 8 1972
1512 DTigzanex, Lockheed Missiles and Space Inc. S Acton, Lockheed S/T341-High Frequency Atmosphere Tilt PSD Measurements Vacuum Tower/SP 6 5i
1474 I Tuominen, M Poutanen, University of Helsinki N Piskunov, USSR Academy of Science S Saar, Harvard-Smithsonian Center for Astrophysics T/Surface Imaging of the FK Comae Star HD 199178 McMath Main 5 2672
1210 O White, Lazy FW Ranch T/Sun as a Star: Ca II Profile Measurements McMath Main 3 19
1024 E Worden, Lawrence Livermore Laboratory S Keil, National Optical Astronomy Observatories S/B044-Solar K-line monitoring Evans Solar Facility/SP 55 17°
1509 J Zirker, W Livingston, National Optical Astronomy Observatories S/B267-Coronal Spectra and Images Evans Solar Facility/SP 22 80
Total number of proposals: 63
18:08 mThundiy February 8.1990 aquila:AilflohnK.n/qir.inpu^outpm2 APPENDIX C
NOAO Annual Safety Report
The following is a summary of recordable occupational injuries for the Kitt Peak, Sacramento Peak, and Tucson sites as reported on the OSHA 200 log. This information covers the calendar year 1989. As required, this data will be posted at each site by February 1, 1990.
KPNO Sac Peak Tucson Total Deaths: 0 0 0 0
Injuries involving days off or days of restricted work activity or both: 3 2 1 6
Injuries involving days off: 3 2 0 5
Days off from work: 7 25 0 32
Days of restricted work activity: 0 0 12 12
Injuries without lost workdays: 1 1 2 4
Total recordable injuries: 4 3 3 10
There were no occupational illnesses recorded at Kitt Peak, Sac Peak, or the Tucson site in 1989.
CTIO recordable occupational injuries: January 1989 - December 1989.
Deaths: 0
Injuries involving days off or days of restricted work activity or both: 2
Injuries involving days off: 4
Days off from work: 40
Days of restricted work activity: 11
Injuries without lost workdays: 2
There were no occupational illnesses recorded at CTIO in 1989.