Transcript
National
Optical Astronomy Observatories
NATIONAL OPTICAL ASTRONOMY OBSERVATORIES
FY 1989 PROGRAM PLAN
REVISION I
March 1, 1989
National
Optical ASTronomy
950 ncnmv Ave
Ohc£ir\mirW\C±Q
P^ Box 26732 Tucson An/ono 857;'6 6::-?
UUOCI VUlUlltJo Kitl Peak National Observatory
•
(602)327-5511 Telex 0666-484 Auia Noon fu,'
Cerro Tololo Inter-American Observatory
•
National Solar Observatory
•
Advanced Development Program
March 1, 1989
Dr. Kurt Riegel, Head Astronomy Centers Section National Science Foundation
1800 G Street, N.W.
Washington, D. C. 20550
Dear Dr. Riegel:
Enclosed are ten copies of Revision I to NOAO's FY 1989 Program Plan incorporating the changes requested in Mr. Asrael's letter of January 9, 1989. The revision consists of the following pages: NEW - Section III.C, Research Experience for Undergraduates, pp. 34a - 34e
REVISED - Funding Schedule for Instrumentation, pp. 41a - 41b NEW - Section VIII, Non-NSF Projects, pp. 64a - 64d REVISED - Appendix 4, FY 1988 User Statistics REVISED - Appendix 5, Budget Tables The revised Plan reflects the following actions which were necessary to achieve the reduction in FY 1989 funds:
GONG hardware acquisitions deferred and program stretched out
$300,000
Reductions in personnel costs including deferred hiring for open positions
$240,000
The balance of the reduction was taken in the Director's Reserve, essentially exhausting that account. Sincerely,
^ptC^ (3^^U,
'/?
Sidney # Wolff Director sjp enclosures xc: G. Oertel OAC Members Associate Directors
Deputy Directors Unit Heads
Operated by the Association of Universities for Research in Astronomy, Inc. (AURA) under contract with the National Science Foundation
NATIONAL OPTICAL ASTRONOMY OBSERVATORIES
FY 1989 PROGRAM PLAN
REVISION I
March 1, 1989
III.
C. Research Experience for Undergraduates.
In December 1986 the National Science Foundation (NSF) announced a new program to attract talented students into research careers in the fields of mathematics, science and engineering. NOAO was invited to submit proposals both as an REU participation site and also as a supplement to a current program supporting research experience for minority students. Competitive proposals were submitted and based upon the merits of the proposals, awards were made. NOAO is very pleased to participate in the REU program. Our past experience in working with students-both through the
minority program and through the summer research assistant program—coupled with the experience of working with the students from the summer of 1988, testifies to the continued need for support of such programs.
The NSF award of $81,458 for the 1989 Summer Research Experiences Program will be used to fund 18 research assistants; 12 in Tucson, Arizona and six in Sunspot, New Mexico. This award will cover salary for 14 weeks, as well as travel and fringe benefits-with the possibility of extension through the fall. Of the 18 students, seven will be assigned to work with KPNO staff; four with NSO Tucson staff; six with NSO Sunspot staff and one with a CCS staff member.
Applications were submitted to the Personnel Office by February 15; selections should be made by the end of March or early April. Some of the proposed research work for the summer of 1989 follows.
The student will be involved in research into dynamical phenomena in the atmosphere of Jupiter. The project, which utilizes a combination of ground-based telescopic data and data from the
Voyager mission, is aimed at understanding the large-scale meteorological phenomena occurring at the northern edge of the equatorial zone (a region of the atmosphere of special interest since this is where the Galileo atmospheric probe will be inserted in 1995). Of particular interest is the generation and evolution of equatorial plumes, currently thought to be analogous to the Wave-CISK
interaction that occurs in the Earth's tropical atmosphere, but which causes updrafts and patches of turbulence on Jupiter larger than the Earth itself.
Most of the massive O-type stars in our Galaxy and the Magellanic Clouds are found in OB
associations. These complexes are 50-100 pc large, and are more sparsely populated than open clusters. A study of the OB associations in the Magellanic Clouds has been conducted, using CCD UBV data to select the hottest stars, and then obtaining spectroscopy on the Tololo 4-m telescope. These data allow us to accurately place the massive stars in the "theoretical" H-R diagram, and provide the means to study both the star formation rate (SFR) and initial mass function (IMF) of newly bom massive stars in these nearby galaxies.
Our studies so far has shown that star formation is not coeval on the time scale of 107 years. In the two OB associations LH117 and LH118 we see clear evidence that while most of the massive stars
formed at the same time (within 1-2 million years) a few high mass stars formed roughly 8-10 million years earlier (Massey et el., AJ, in press). Blaauw (1864 Ann Rev. Astron. Astrophys. 2, 213), in his early studies of OB associations in our own Milky Way, found spatial variations in the time of star formation, with various subgroups forming at different times. This is unlike what we are finding in the Magellanic Clouds, however, as the older high mass stars are not spatially segregated from their younger companions. It is time to re-examine this issue for galactic OB associations, as there have been significant improvements on the observational side (e.g., Humphreys and McElroy's 1984 [Ap.J. 284, 565] catalog of spectral types and photometry of stars in OB associations) and on the theoretical side (mass-loss evolutionary tracks).
This work is well suited to an undergraduate with some astronomy and physics background. We will be reducing more photometry of OB associations in the Clouds, and using the existing data on galactic OB associations to study the length of time over which star formation proceeds in OB associations.
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The student would be involved in the study of the kinematics in the galactic disk. This project involves the determination of radial velocities, distances, and ages of large numbers of F stars in the galactic disk both in the Southern and Northern hemispheres to investigate the relationship between velocity dispersion and age at various distances from the galactic center. This relationship is known for stars near the Sun, but the observed galactocentric gradient of velocity dispersion as well as the observed distribution of molecular cloud complexes, which are believed to influence
stellar kinematics, suggest that the velocity dispersion-age relationship could be quite different in the inner and outer disk. Knowledge of the structure of this relationship will constrain the models for kinematic heating of the galactic disk and shed light on the kinematic history of the galaxy. This project has a number of possibilities for student participation, including the reduction and analysis of both photometric and spectroscopic data and actual observation at the telescope.
IRAF (Image Reduction and Analysis Facility) is an ongoing project for the development of high quality reduction and analysis software for distribution to the astronomical community. A large part of the development effort involves testing the software prior to release for numerical accuracy and in understanding the role of both the algorithm and the host computer in determining the achievable accuracy of a given procedure. The student would help to develop and execute procedures for testing numerical software. Duties would include creating artificial data, designing test procedures, writing simple tasks, evaluating, analyzing, and writing up the results.
The candidate student should have good analytic skills, a solid background in scientific data reduction and analysis techniques and familiarity with scientific computing. Familiarity with astronomical reduction techniques is desirable but not essential.
One project for a summer student would be to work on the atlas of mixed morphology double galaxies. The observational part of this project has been completed. The student would be involved in some simple data reduction of CCD images. Much of the work would involve production of annotated photographic mosaics, and of considerable tabular data, in a form suitable for publication.
A second project which would be quite timely for the summer of 1989 involves work for a
projected review for a forthcoming IAU Colloquium. It would be principally a literature search involving location and checking of references, following of cross references, and perhaps, depending on the student's interests and abilities, summaries of the contents of the papers so located.
Finally, the student would assist with the adaptation and operation of image processing software. This last affords the greatest opportunity for independent study and research by a student.
Observations of emission in the core of the Ca U K-line is a valuable indicator of magnetic activity on the Sun and other stars. Regular measurements of K-line emission strength are made for the full-disk Sun at both National Solar Observatory sites, Kitt Peak and Sacramento Peak. Differences
in location and weather mean that these two data sets, which both cover more than ten years, are not redundant. The student would carefully compare the two sets and determine scaling factors that will allow one to use the full, combined data set from both sites.
The REU student will be involved in the reduction and analysis of high resolution spectroscopic data obtained with the NSO/McMath Solar-Stellar Spectrograph and CCD detector system. The research project(s) will concern the investigation of analogues of solar activity as they occur on other stars. This includes spectroscopic manifestations of spots, flares, active regions and other phenomena associated with emergent magnetic fields in stars. In this way, we can gain insights on the nature of both the dynamo mechanism responsible for the generation of magnetic fields and the
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associated atmospheric heating processes that give rise to chromospheres and coronae in the Sun and stars.
Through this research the student will necessarily become "computer conversant" while simultaneously becoming familiar with the sophisticated reduction and analysis methods that are applied to astronomical data obtained with modern detector systems.
This project involves studying the interaction of five-minute acoustic waves with intense magnetic fields on the Sun. In order to use solar five-minute oscillations as accurate probes of sub-surface velocities it is necessary to separate out any magnetic field effects on the wave frequencies. Mapping out the wavenumber dependence of changes in the oscillation frequencies over magnetic fields may also in future be used to infer the depth to which magnetic fibrils penetrate. Theoretical calculations by Bogdan and Zweibel (1987) and Bogdan (1987) have also shown that sunspot models composed of many magnetic flux tubes can act as scatterers of acoustic oscillations. Measuring the properties of such scattering may help determine the interior makeup of the spots, e.g. whether they are composed of random collections of many fibrils or simply large-scale magnetic fields.
Observations have been obtained in a magnetically insensitive Fe I line using a single diffraction grating spectrograph at the Vacuum Tower Telescope (VTT) at Sacramento Peak. A CCD chip, sampling wavelength in one dimension and latitude in the other, was scanned parallel to the solar equator from limb to limb across an active region at 23 degrees south latitude. Since this data has information on the oscillations over both quiet and active regions, it should be useful for addressing the scientific questions mentioned above. The REU student will participate in any further observations taken with the VTT at Sacramento Peak during the summer of 1989. He or she will reduce the present spectral data into radial Doppler velocities and help generate the diagnostic power diagrams used in determining the frequencies of the oscillations and the power in these waves.
Some projects would be to: 1.
Undertake to obtain and reduce observations of the full solar disk with the vacuum solar
telescope on Kitt Peak. Every day, weather permitting, maps are made of the longitudinal
magnetic field strength and the strength of the helium 10830 A absorption line. These data are used in a wide range of research projects resulting in about 25 papers per year on subjects ranging from basic mechanisms of the sunspot cycle to satellite drag produced by heating of the Earth's upper atmosphere. A specific project of current interest is to produce an accurate daily index of solar activity from these data. 2.
The archive of these data consists of diverse media in several formats. To make it easier to
extract the data, it is planned to transfer the records to modern storage media in a standardized format. A modem data base catalog would be prepared. 3.
It is anticipated that a large amount of solar data will be obtained at the geographic South Pole in November 1988. These data will be used to probe the structure and dynamics of the solar interior using the techniques of helioseismology. A large amount of data reduction will be required before it will be possible to extract new scientific results.
One activity a REU student could help with would be performing a spherical harmonic transform on the Vacuum Telescope magnetograms. This would allow a search for global patterns in the solar magnetic field similar to those seen in solar oscillations, and could help to shed light on the mechanism underlying the solar cycle. The student would be responsible for running the data through the software that performs the computation. He/she would also develop ways to display the resulting power spectra of the magnetic field fluctuations. It is a big job with a potentially exciting but completely unknown payoff, giving a student a good taste of what science is about. The primary scientific goal of this project is to understand and develop models for the processes that lead to the build-up and release of energy in solar active regions. This release of energy
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affects the interplanetary and terrestrial environment and its understanding is of fundamental
importance to our increased use of space. The project coincides with and is part of the planned MAX '91 campaign to increase our understanding of solar and stellar activity. The project is the first systematic attempt to combine data from a large number of sources that address all aspects of the build-up and release of energy in solar active regions. The project addresses the important scientific issues of magnetohydrodynamics in a highly ionized, convective plasma from both observational and theoretical viewpoints. Both solar and other astrophysical data will be combined to develop models of active regions. The development of non-potential magnetic field configurations and sheared magnetic structures in active regions will be observed with measurements of vector magnetic fields, horizontal and vertical flows, and changes in chromospheric and coronal structures. The projects involve the collection, reduction, and analysis of data on solar and stellar magnetic structures, solar atmospheric motions (both convection and waves), and on how the motions and magnetic fields interact. Simultaneously, empirical and theoretical models for the interactions will be developed and used to interpret the data. Numerical codes for computing solar spectra in the presence of convection, waves, and magnetic fields have been written and are being improved by the inclusion of more realistic physical conditions for the
solar atmosphere. These codes will be used to deduce temperature, pressure, density, field strengths and motions from the observations.
The project includes the use of existing instrumentation and will use new instrumentation that will come on-line in the near future. Large-scale, horizontal flows of mesogranulation and
supergranulation will be derived using cross-correlation analysis from our full-disk, white light granulation camera currently in use. We will use a recently developed, narrow-band (20 milliangstrom) filter system to measure intensity and velocity fluctuations as a function of time and three-dimensional space in the solar photosphere and chromosphere. This data will be combined with measurements of the vector magnetic field in the solar atmosphere that will be made at both
high-spatial resolution of selected regions and at a lower resolution of the full solar disk using vector magnetographs currently under development at Sacramento Peak and at the Johns Hopkins
University Applied Physics Laboratory respectively. The latter system is scheduled for delivery to Sac Peak this fall. Data collection will utilize image stabilization systems and speckle imaging techniques to obtain the highest possible spatial resolution. Agile mirrors (tiltable to remove image motions) are presently in use; a correlation tracker for stabilizing arbitrary solar images (i.e. images without a strong reference feature such as a sunspot), and a speckle camera system have all been developed. Fully active mirrors capable of removing image distortion as well as motion are under development.
Several large databases of synoptic-measurements of solar and stellar activity exist, including solar Ca II H & K emissions from NSO/Sac Peak and NSO/Tucson, Mt. Wilson and Lowell Observatory and stellar data from Mt. Wilson and Lowell. The new HAO/Lowell/AFGL data base is unique
because it contains direct solar as well as stellar observations made with the same instrument, and
thus provides the link necessary to intercalibrate these databases. Stellar data should help us develop a more comprehensive picture of how magnetism interacts with other parameters such as
convection which will aid in developing a model of solar and stellar activity.
A major collaborative effort between NASA/MSFC, the University of Alabama, NOAA/SEL, NSO,
and AFGL will begin in 1989 and will seek to establish an empirical model for energy
storage/release in sheared magnetic fields. The objective is to obtain measurements indicative of the
degree to which the magnetic field configuration deviates from that of a potential (minimum
energy) field. Calculated potential fields will be compared with chromospheric fibril geometry and vector field azimuths. Considerable emphasis will be placed on energy storage rates, estimates of total free energy and relaxation of shear in the presence of flare activity. This collaboration will
provide additional data and modelling efforts that complement our internal project and will expose
the REU students to research at several institutions.
The post-flare relaxation process will be studied in the case of limb flares by analysis of the detailed morphological characteristics of coronal loops as recorded by the 20-cm aperture, three-line patrol coronagraph and the three-line coronal photometer. Further, spectra will be obtained of post-
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flare loop interactions to obtain estimates of temperature, density and energies involved in such transient phenomena. This post flare data will be compared with the energy build-up and content of the active region that existed before the flare occurred.
Aspects of the project that students will be directly involved in include conducting observations; data reduction using techniques that have been developed here as well as standard packages such as IRAF and ZODIAC; data analysis to produce movies of velocity, intensity and magnetic field evolution; and numerical simulations to deduce the physical parameters in the atmosphere.
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IV.
MAJOR PROJECTS AND INSTRUMENTATION
Instrumentation
Payroll
Payroll
Total
KPNO
IR Program IR Detector Research & Dev.
104
67
171
Cryogenic Optical Bench Cryogenic Echelle Observing Instrument. Imprv. IR Spectrometer Instrument IR Operations & Maintenance Adaptive Optics
409 71 25 25 72 _63
60 20 15 2 34 _35
469 91 40 27 106 98
769
233
1,002
O/UV Program Fiber Actuators
83
19
102
Bench-Mounted Spectrometer
30
28
58
KPCA Time Mode
27
7
34
TV Acquisition Cameras
15
12
27
CCD Controllers
34
16
50
76 _71
18 _6
94 _77
336
106
442
63
63 140
CCD Development O/UV Operations KPNO Miscellaneous Projects NSO - Sunspot Adaptive Optics
87
53
CHIRP
6
10
16
36 61 18
14 5 7
50 66 25
208
89
297
Infrared Array Spectromagnetograph Helioseismograph
12 11 40
44
56 11 62
Stellar K-Line Filter
25
3
McMath FTS Servos
_35
Mirror Coronograph Polarization Compensator Multi-Band Patrol Upgrade
NSO - Tucson
22
28
J35
123
69
192
126
CTIO
100
26
IR Controller/Acquisition System
CCD Controllers
70
6
76
4-m Prime Focus Corrector 4-m IR Photometer
20 8
72 6
92 14
f/7.5 Secondary for 1.5-m IR Detectors
4-m Fiber Optics Feed
10
3
13
103
34
137
147
508
_50 361
41a
_50
Central Offices
WIN Telescope
12
12
31
100 55 155
CCS IRAF
100
Computer Implementation 100
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VIII.
NON-NSF FUNDED PROJECTS
Listed below are NOAO programs whose funding derives from sources other than NSF. Funding for some programs may extend beyond the current fiscal year. Principal Projects: In K's
USAF USAF USAF USAF USAF USAF NASA NASA NASA NASA USAF NASA NASA NASA NASA
3.5-m Honeycomb Mirror Development Sacramento Peak Support Adaptive Optics Optical Testing for Large Objects Liquid Crystal Filter Prototype Advanced Reflecting Coronagraph FTS Program for Upper Atmospheric Research Project Galileo Space Telescope Imaging Spectrograph (STIS) Vacuum Telescope Support Upgrade Coronagraph & Polarimeter Infrared Astronomy Satellite (IRAS) Tuneable Wide Field Lyot Filter IRAF Support NASA/RMT-MIT/ETC Projects
$1,938 643 241 300 145 141 117 104 99 76 75 62 59 52 51
Other Projects:
NASA OSD
Solar Optical Telescope (J. Beckers) Interferometric Imaging
21 21
NASA
Stellar Winds in Hot Stars
21
NASA DOE USAF USAF NASA
Photometry and Astronomy of Comet Halley Battelle Terrestrial Monitoring Multilayer UV Mirror Research Video Imaging System Solar Optical Telescope (J. Harvey)
19 17 16 15 14
NASA
T Tauri Stars
10
NASA NASA OSD USAF NASA
X-Ray Emitting Stars Tucson Workshop Multilayer UV Mirror Research Hare Patrol Upgrade Chromospheric Coronal Emissions Miscellaneous projects less than $5K each
9 9 8 8 7 33 $4,331
USAF
Casting & Preparing to Polish a 3.5-m Borosilicate Honeycomb Mirror
NOAO will administer a subcontract between the USAF and the University of Arizona Mirror Lab which will require the UofA to cast a 3.5-m borosilicate honeycomb mirror blank and to begin the design, development, and construction work required to produce polishing facilities that will be used to finish the blank. USAF will monitor the technical work on the project, with all work being completed by the UofA.
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USAF:
Sacramento Peak Support
Under a Memorandum of Understanding between the United States Air Force (USAF) and the National Science Foundation (NSF), the USAF provides funds ($600K) for general support of a group of USAF personnel who are physically located at
Sacramento Peak and who support programs/projects which are of special interest to the USAF. In FY 1989 an additional $43K will support a research assistant in data
reduction ($25K), upgrade the flare patrol photometer ($8K), and provide miscellaneous project support ($10K). USAF
Adaptive Optics
The USAF has provided NSO with funding to continue development of a second generation adaptive mirror. The work includes development of a phase detector system, development of an interferometer to measure fringes from the active mirror
surface, and development of an improved mirror control system with a range several times that of the first generation mirrors.
USAF
Optical Testing for Large Objects
C. Roddier is the principal investigator for this proposal to the USAF's Rome Air Development Center (RADQ for a program of optical test method improvements intended to shorten the time required to test large optics and improve the spatial resolution obtainable. Funds provided are for payroll costs of scientific and engineering staff and for purchase of optical and computer components. USAF
Liquid Crystal Filter
This project for the USAF will develop a Liquid Crystal Filter. Work will include
obtaining a controller system for rapid wavelength tuning of both the liquid crystal device and the universal birefringent filter that will permit acquisition of vector magnetograms, interfacing the controller to filters, and documentation of the controller system.
USAF
Prototype Advanced Reflecting Coronagraph
R. Smartt will serve as principal investigator at NSO/SP on this project with the USAF to fabricate 15 cm super-polished mirrors through a subcontract to an optical
company; to evaluate the scattering properties of these mirrors in laboratory conditions using the optical evaluation facilities of the Evans Solar Facility at SPO; to develop a fast CCD camera and data processing systems for detecting faint objects
rapidly; and to integrate the optics and detector package on the Evans Solar Facility spar. Testing of the system will be conducted during the second year of the project.
NASA
FTS Program for Upper Atmospheric Research
J. Brault is participating in this project as principal investigator. The primary activities are upper atmospheric studies utilizing the FTS at the McMath Telescope.
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NASA
Project Galileo
M. Belton is continuing his work in Project Galileo as the team leader for the Solid
State Imaging System. Funding will be used to support travel to team and project meetings, the cost of consultants to the team, and the development of a "Home Institution Image Processing System" (HIIPS) to be installed at the NOAO Tucson offices.
NASA
Space Telescope Imaging Spectrograph (STIS)
NASA has continued to provide funds to support S. Wolff and R. Green for their participation in the STIS Instrumentation Definition Team. In addition, NOAO will
support the STIS instrument by testing CCD images and serving as technical liaison between the manufacturer, the STIS team, and NASA. In addition, NOAO will
provide technical and scientific assistance in choosing the final flight package device. NASA
Vacuum Telescope Support
NSO has provided the solar physics community with full-disk, high resolution magnetograms and He 10830 spectroheliograms for a number of years using the Vacuum Telescope for synoptic observations. Since 1979, NASA (a primary user of this data) has been providing funding to assist in the operational support and improvement of the telescope. USAF
Upgrade Coronagraph and Polarimeter
The USAF is funding the provision of a dedicated light feed for the coronal photometer at the Evans Solar Facility as well as to up-grade the multiband polarimeter for flare patrol observations. Both projects are in support of the Max '91 campaign of coordinated activity measurements being conducted by the USAF Solar Research Branch.
NASA
Infrared Astronomy Satellite (IRAS)
During FY 1988 F. Gillett worked with scientists at the Lowell Observatory to obtain
a FITS tape of the NGC 6822 infrared maps, obtain H-alpha images of the galaxy, make far-infrared color maps from the IRAS data, and then compare the spatial distribution of the H-alpha emission with that of the far-infrared in order to separate the component of the dust heated by star formation from that heated by the general interstellar radiation field.
NASA
Tuneable Wide Field Lyot Filter
R. Dunn and R. Smartt are principal investigators of this continuing project for the design and fabrication of a tuneable wide field Lyot filter. NASA
IRAF Support
Continuing the work begun in 1982, the NOAO Central Computer Service personnel have again been supported by NASA in the project to develop the Image Reduction and
Analysis Facility (IRAF) Software. This software,
which has
now been
distributed to some 200 users throughout the country, operates on UNIX computers and high-end graphics workstations, provides new network access to remote data
bases, and has developed new hardware interfaces for image display hardware. In addition to NASA-compatible terminals, NOAO provides technical onsite consultation to NASA scientists, sponsor seminars and conferences on IRAF, and assists NASA in
evaluating relevant new technology. This work directly supports the NASA space science astrophysics community, including the Space Telescope Science Institute.
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NASA
NASA/RMT-MIT/ETC Projects B. Teegarden of NASA, in collaboration with G. Ricker of Massachusetts Institute of
Technology (MIT) will be operating the Rapidly Moving Telescope (RMT) and the Explosive Transient Camera (ETC) on Kitt Peak for at least the next four years. NASA funding is provided to refurbish facilities and for support provided by KPNO operations personnel.
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APPENDIX 4
NATIONAL OPTICAL ASTRONOMY OBSERVATORIES USER STATISTICS1 FY 1988
VISITOR TELESCOPE USAGE
CTIO2
Visiting Observers
U.S.
KPNO3
Foreign
U.S.
NSO4
Foreign
U.S.
NOAO TOTALS
Foreign
U.S. Foreign
Toial
Astronomers
96
44
337
29
200
64
633
137
770
Graduate Students
14
3
113
7
2
1
129
11
140
Other (technicians, research assistants, etc.)
0
3
17
0
11
1
28
4
32
110
50
467
36
213
66
790
152
942
51
24
96
19
53
23
200
66
266
Total Visitors
Institutions
1 The figures in these tables reflect the number of observers/users physically present at the Observatory and also include multiple visits by a single observer^ser. These tables do not include NOAO staff.
2 During fiscal year 1988, a total of 219 observing programs were carried out by visitors and the NOAO staff at Cerro Tololo. Visiting astronomers were assigned 77% of the scheduled telescope time and the remaining 23% was assigned to the staff.
3 During fiscal year 1988, a total of 324 observing programs were carried out by visitors and the NOAO staff at Kitt Peak. Visiting astronomers were assigned 77% of the scheduled telescope time and the remaining 23% was assigned to the staff.
During fiscal year 1988, a total of 147 observing programs were carried out by visitors and the NOAO staff at the National Solar Observatory. Visiting astronomers were assigned 74% of the scheduled telescope time and the remaining 26% was assigned to the staff.
VISITOR REDUCTION FACILITIES USAGE NOAO - Tucson
Visiting Scientists
Number of Institutions
Ph.D.
Student
Other
Total*
VAX Computer Systems
85
229
66
15
310
Grant Comparator - 2 axis
16
22
12
16
50
9
21
52
36
109
PDS Microdensitometer
*The numbers reflected above show duplicated usage of NOAO-Tucson reduction facilities by visiting scientists. NOAO staff are not included in these figures.
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NATIONAL OPTICAL ASTRONOMY OBSERVATORIES FY-1989 PROGRAM PLAN -
APPENDIX
5
REVISION I TABLE I
MARCH 1, 1989
FUNDING BY SOURCE
(Aaounts In Thousands)
Scientific
Staff &
Instru-
Operations &
Support
mentation
Maintenance
Management
Fee
TOTAL
FY-1989(1)
TOTAL
FY-1988(3)
TOTAL
FY-1987(3)
NSF FUNDING
Advanced Development Program
$
$
$
164
$
270
Cerro Tololo Inter-American
Observatory Kitt Peak National Observatory
National Solar Observatory Sunspot USAF Support Tucson
1,085
508
3,286
4.879
4,693
4,938
1,857
1,507
4,293
7.657
7,499
7,304
418
297
1,755
2.470
2.432
2,434
(600) 733
192
(600) 1,378
453
(54)
NASA Support
(54)
(600) 1,427
(54)
(600) 1,327
(49)
Global Oscillations Network Group
1,232
1,232
1,011
977
Future Telescope Technology (2)
1,942
1,942
1.751
1,890
345
467
214
206
193
193
174
128
1.320
1.320
1,129
1,251
1.230
1.230
1.322
1,638
711
1.041
1,024
1,279
797
797
541
554
405
405
433
426
405
$24,357
$23,160
4,331
1,765
$28.688
$24,925
461.71
457.96
466.21
7.00
9.75
8.65
468.71
467.71
474.86
Central Offices
Director's Office
ON
Publications & Info.
110
12
Resources
Central Administrative Services
Central Facilities Operations Central Computer Services Central Engineering &
175
155
Technical Services
Management Fee
Total NSF Funding
$4.378
$13.729
NON-NSF FUNDING
Total Funding
$23,973 1,659
STAFFING SCHEDULE
(In Full Time Equivalents) NSF Funded
65.95
78.75
317.01
Non-NSF Funded
Total
1
Includes $23,810k new funds. $466k carryover funds, and $81k new REU funds.
2
Includes $825k new funds for UA mirror development contract.
3
Where possible, comparative amounts for ADP have been redistributed to reflect current organization.
TABLE I-A ADDENDUM TO
FUNDING BY SOURCE TABLE
(Aaounts 1n Thousands)
NSF Funding
Director's Office - Operation & Maintenance
Office of the Director
FY-1989
FY-1988
FY-1987
$
$
$
Visiting Committee Travel Collaborative Projects
432
321
14
4
3
2
256 11
Performance Awards
21
NOAO Director Search Committee
13
Indirect Cost Credits
(125)
Visitor Program-Foreign Travel
Tota1
(251)
21
$
97
345
(211)
20
$
96
10
$
100
TABLE I-B ADDENDUM TO
FUNDING BY SOURCE TABLE
(Aaounts In Thousands)
Research Experience for Undergraduates (REU) Programs
Amounts shown are included in Scientific Staff & Support: Estimated
Carryover r"unds
Kitt Peak National Observatory
$
New Funds
Total Funds
Number of Students
$ 31
$ 31
7
National Solar Observatory Sunspot
3
27
30
7
Tucson
6
18
24
6
5
5
1
$_81
$ 90
Central Computer Services
Total
$9
98
TABLE II
SUMMARY OF NSF FUWDING BY COST CATEGORY
(Aaounts In Thousands)
NSO KPNO
SUNSPOT
TUCSON
$2,841
$5,834
$1,599
$1,142
Supplies & Materials
982
1.151
296
146
Utilities & Communications
284
282
344
Purchased Services
402
(22)
Personnel
Costs
GONG
$
811
113
17
85
130
25
55
48
Foreign Travel
132
46
5
13
Equipment
193
236
88
5
118
$4,879
$7,657
$2,470
$1,378
$1,232
Subtotal
USAF & NASA Support Total NSF Funding
(600)
$4,879
$
170
45
Domestic Travel
S
CENTRAL
CTI0
MANAGEMENT
TOTAL
FTT
OFFICES
760
$3,277
351
428
3,52
472
1.38
831
$1 ,942
FEE
FY-198
$
$16,26
639
405
2,47
72
37
48
24
112
75
$5,048
$
405
(54)
$25,01
(65
$7,657
$5,048
$
405
$24,35
STAFFING SCHEDULE
(In Full Time Equivalents) Scientists
16.00
27.55
Engineers 4 Scientific Programmers Administrators & Supervisors
16.00
19.00
5.00
10.00
6.00
3.00
1.00
Clerical
26.00
9.35
4.10
2.00
37.50
47.30
13.00
7.00
41.00
30.50
9.90
146.50
139.70
39.00
Workers
Technicians
4.00
10.00
10.00
1.00
5.95
64.5
6.00
12.00
68.0
1.00
7.00
13.00
34.0
1.00
29.26
71.7
6.00
10.30
128.1
14.00
95.4
84.51
461.7
Maintenance & Service Workers
Total
20.00
18.00
14.00
TABLE III
SCIENTIFIC STAFF a SUPPORT
(Aaounts In Thousands)
NSO
Personnel
Costs
SUNSPOT
CENTRAL
TOTAL
TOTAL
TUCSON
OFFICES
FY-1989
FY-1988
$ 275
$3,788
$3,651
923
$1 ,547
368
$ 675
24
134
15
24
197
180
Purchased Services
60
28
15
2
105
88
4
65
15
22
53
38
5
10
21
45
Foreign Travel Equipment
o o
KPNO
Supplies & Materials Domestic Travel
Total
$
CTIO
$1,085
$
$1.857
$ 733
10
$ 285
116
79
106
80
66
34
$4,378
$4,112
56.95
57.20
STAFFING SCHEDULE
(In Full Time Equivalents) Scientists
Clerical Workers Technicians
Total
15.00
25.75
4.00
9.00
1.00
2.00
1.50
1.00
3.20
3.50
19.50
27.75
5.50
10.00
3.20
5.50
5.50
3.50
3.50
65.95
66.20
TABLE IV INSTRUMENTATION
(Aaounts In Thousands)
NSO
Personnel Costs
Supplies & Materials Purchased Services
KPNO
SUNSPOT
TUCSON
$361
$1,105
$208
$123
52
341
66
69
65
2
Domestic Travel
Foreign Travel Equipment Total
-
CTIO
6
GONG
$
811
FTT
$
760
CENTRAL
TOTAL
OFFICES
FY-1989
$
102
351
18
1.067
85
831
47
1,030
3
48
57
20
118
217
4 30
49
$508
$3,470
170
4
$297
$192
$1,232
$1,942
$ 167
$5,845
STAFFING SCHEDULE
(In Full Time Equivalents) Scientists
Engineers & Scientific Programmers
5.00
7.00
10.00
Administrators & Supervisors Clerical Workers Technicians Total
1 .00
0.25
1.25
6 00
2.00
30.00
1.00 1.00
1.00 1 00
2.00 44.50
6.50
17.50
6.00
1.50
7.00
6 00
12.50
24.50
6.00
1.50
18.00
14.00
2.25
78.75
TABLE ¥
OPERATIONS 1 MAINTENANCE BY COST CATEGORY
(Aaounts in Thousands)
NSO
CENTRAL
TOTAL
TOTAL
CTIO
KPNO
SUNSPOT
TUCSON
OFFICES
FY-1989
FY-1988
F
$1,557
$3,182
$1,023
$344
$2,900
$ 9,006
$ 8,985
$
906
676
215
53
410
2,260
2,454
284
282
344
277
(52)
Domestic Travel
41
59
Foreign Travel
79
4
Equipment
142
142
Subtotal
$3,286
$4,293
Personnel Costs
Supplies J Materials Utilities S Communications Purchased Services
USAF & NASA Support
1,382
1,396
15
592
930
494
7
33
62
202
174
3
48
134
147
5
112
469
540
$453
$4,596
68
$1,755 (600)
o
Total
472
98
$3,286
$4,293
$1,155
(54)
$399
$14,383 (654)
$4,596
$13,72?
$14,190
$
(654) $13,536
$
STAFFING SCHEDULE
(In Full Time Equivalents) Scientists
1.00
1.80
Engineers & Scientific Programmers
11.00
12.00
5.00
Administrators & Supervisors
10.00
6.00
3.00
Clerical Workers
24.00
7.35
Technicians
27.50
29.80
41.00
30.50
9.90
114.50
87.45
27.50
1.00
2.50
10.00
38.00
35.00
1.00
13.00
33.00
33.00
2.60
1.00
29.26
64.21
65.21
7.00
5.50
10.30
80.10
86.60
14.00
95.40
93.40
79.06
317.01
320.36
6.30
7.15
Maintenance & Service Workers Total
8.50
3
TABLE VI
OPERATIONS ft MAINTENANCE BY TYPE OF SERVICE
(Aaounts In Thousands)
NS0 CTIO
KPN0
524
$1,160
CENTRAL
TOTAL
TOTAL
TOT
TUCSON
OFFICES
FY-1989
FY-1988
FY-1
221
* 28
* "7
$ 2,730
$ 2,828
$ 2,
252
2.395
2,438
2,
3,083
3,059
3.
1,230
2.024
2.081
2,
711
711
684
1,665
3,247
2,926
193
193
174
$4,596
$14.383
$14.190
SUNSPOT
Engineering 8 Technical Services
$
$
Telescope Operations
600
913
630
Mountain Operations
747
1,615
721
558
236
Central Facilities - Tucson/ La Serena Operations Central Computer Services Administration
857
369
183
173
2.
Publications & Information o
Resources
Subtotal O&M
$3,286
$4,293
USAF & NASA Support Total
O&M
$.1,755 (600)
$3,286
$4.293
$1.155
$453 (54) $399
(654)
$4,596
$13,729
(654)
$13,536
$14.4
(6
$13,8
STAFFING SCHEDULE
(In Full
Time! Equivalents
Engineering & Technical Services
Telescope Operations Mountain Operations Facilities
12.50
16.00
3.00
26.00
19.00
9.00
30.00
36.60
10.50
23.00
5.05
1.00
Central Computer Services Administration
Total
13.50 6.50
] 19.50
5.80 23.00
114.50
45.00
46.90
50.
60.50
60.50
61.
77.10
79.60
79.
48.55
41.55
43.
] 10.05
15.85
16.20
17.
5.00
4.00
2.00
: 36.01
70.01
75.61
73.
87.45
27.50
8.50
79.06
317.01
320.36
325.
TABLE VII
CONSTRUCTION
(Aaounts in Thousands)
NSO CTIO
SUNSPOT
TUCSON
CENTRAL
TOTAL
TOTAL
TOTAL
OFFICES
FY-1989
FY-1988
FY-1987
Supplies & Materials
25
Purchased Services
12
Total
o
KPNO
37
TABLE VIII MANAGEMENT FEE
(Aaounts in Thousands)
NSO CTIO
KPNO
SUNSPOT
TUCSON
CENTRAL
MANAGEMENT
TOTAL
TOTAL
OFFICES
FEE
FY-1989
FY-1988
Purchased Services
L
$
405
$
405
$
433
$
405
$
405
$
433
Total
o
TABLE IX
NON-NSF FUNDING
(Aaounts in Thousands)
NSO CTIO
Personnel Costs
KPNO
$
Supplies & Materials Utilities & Communications
6
$
151
TUCSON $
74
CENTRAL OFFICES $
176
Domestic Travel
Foreign Travel Equipment
$
3
$
TOTAL FY-1989
$
560
TOTAL FY-1988 $
386
282
14
2
304 1
4
142
710
145
2,133
3,131
1,069
29
2
11
27
7
1
16
206
1
Purchased Services
Total
159
SUNSPOT
360
o
$
202
9
51
10
20
5
17
264
72
$2,347
$4,331
$1,765
2 .00
4 .25
1 .75
1..75
25
TO FY
STAFFING SCHEDULE
(In Full Time Equivalents) Scientists
1 .00
Engineers & Scieritif ic Programmers
1 .00
0 .75
1 .00
1..00
1.25
3.00
1.75
1.25
1.00
Administrators & Supervisors Clerical Workers Technicians
Total
0..25
1.00
3,.25
3..50
7.00
9.75
0
8
TABLE X
COMPARISON OF PROGRAM PLAN WITH PRIOR YEARS AND
FY-89 SPENDING PROJECTIONS BY QUARTER
(Aaounts in Thousands)
FY-1987
Scientific Staff and Support Instrumentation
Construction
Operations & Maintenance
USAF & NASA Support Management Fee Total
FY-1988
FY-1989 Program Plan —
Actual Expenses
Actual Expenses Carryover
$ 3,828
$ 4,112
5,873
FY-1989 Spending Projection
2nd Qtr Estimated
3rd Qtr Estimated
965
$ 1.112
$ 1,150
5,845
1.726
1,372
1,436
14,383
3,464
3.656
3.620
New Funds
Total
15
$ 4,363
$ 4,378
5,079
78
5.667
14,190
273
14,110
$
1ST Qtr Actual $
37
14.458
(649)
(654)
(654)
(654)
(164)
(163)
(164)
426
433
405
405
101
101
101
$23.973
$23,160
$23,891
$24,357
$ 6,092
$ 6.078
$ 6,143
466
E
