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NATIONAL OPTICAL ASTRONOMY OBSERVATORIES FY 1993 PROVISIONAL PROGRAM PLAN July 15,1992 TABLE OF CONTENTS I. INTRODUCTION AND PLAN OVERVIEW 1 II. SCIENTIFIC PROGRAM 3 A. Cerro Tololo Inter-American Observatory 3 B. Kitt Peak National Observatory 10 C. National Solar Observatory 19 III. MAJOR PROJECTS 24 A. Global Oscillation Network Group (GONG) 24 B. Gemini Project Office 26 C. 3.5-m Mirror Project 27 D. WIYN 28 E. SOAR 29 F. Other Telescopes at CTIO 30 IV. INSTRUMENTATION 30 A. Cerro Tololo Inter-American Observatory 30 B. Kitt Peak National Observatory 32 1. KPNO O/UV 32 2. KPNO Infrared 35 C. National Solar Observatory 38 1. Sacramento Peak 39 2. Kitt Peak 41 D. Central Computer Services 44 V. TELESCOPE OPERATIONS AND USER SUPPORT 45 A. Cerro Tololo Inter-American Observatory 45 B. Kitt Peak National Observatory 45 C. National Solar Observatory 46 1. Kitt Peak 46 2. Sacramento Peak 46 VI. OPERATIONS AND FACILITIES MAINTENANCE 46 A. Cerro Tololo 47 B. Kitt Peak 48 C. NSO/Sacramento Peak 48 D. Tucson Headquarters 49 VII. SCIENTIHC STAFF AND SUPPORT 49 A. CTIO 49 B. KPNO 50 C. NSO 50 VIII. PROGRAM SUPPORT 50 A. Director's Office 51 B. Central Administrative Services 51 C. Central Computer Services 52 D. Central Facilities Operations 52 E. Engineering and Technical Services 52 F. Publications and Information Resources 53 IX. BUDGET 53 Appendix 1 - NOAO Organizational Chart Appendix 2 - NOAO Management Appendix 3 - NOAO Scientific Staff List Appendix 4 - Scientific Staff Primary Fields of Interest and 1991 Publications CTIO KPNO NSO Appendix 5 - User Statistics, FY 1991 CTIO (Visitor Telescope Usage) KPNO (Visitor Telescope Usage) NSO (Visitor Telescope Usage) CCS Facilities (Visitor Reduction Facilities Usage) Appendix 6 - Budget Tables I. INTRODUCTION AND PLAN OVERVIEW The next decade will present unparalleled opportunities for making qualitatively new kinds ofastronomical observations from the ground. The revolution in infrared array detectors makes it possible to address a host of new problems ranging from the analysis of magnetic structures on the Sun to the study of the evolution of galaxies. The availability oflarger format optical CCDs, more powerful computers for handling massive quantities of data, and efficient fibers for multiple object spectroscopy will dramatically increase the scientific productivity of existing optical telescopes. Adaptive optics will find important applications in both solar and nighttime astronomy. In order to respond to these opportunities, NOAO has prepared a long range plan for building major new facilities and for upgrading its existing telescopes. In nighttime astronomy, the centerpiece of the program is the construction of the Gemini 8-m telescopes, one to be located on Mauna Kea and the other in Chile. The plan also calls for construction of new 4-m class telescopes in collaboration with universities. These telescopes would be located at KPNO and CTIO. In solar astronomy, the GONG project is already in progress. The sites have been selected, the prototype instrument is in operation, and construction of the equipment for the sites is well underway. Work on adaptive optics is continuing at Sacramento Peak, and new instrumentation for infrared solar astronomy has been made available at the McMath telescope. Overall, the NOAO plan is consistent with, and indeed in several areas has anticipated, many of the recommendations of the Astronomy and Astrophysics Survey Committee (AASC) for the next decade. The planned NOAO 8-m telescopes will provide the scientific capabilities recommended in that report. Adaptive optics was cited as a high priority moderate program. The emphasis on infrared astronomy at NOAO is designed to take advantage ofthe revolution in technology highlighted by the AASC. Initiatives with universities respond directly to the need for additional 4-m class telescopes. A new budget category is included in the program plan for FY 1993. NOAO has assumed responsibility for the support activities required in the US by the Gemini project. These activities include working with the community to formulate the US input into the scientific requirements for the telescopes, working directiy with project staff to review particular technical approaches, preparing proposals for work packages to be carried out within NOAO, and identifying potential US bidders outside NOAO for additional work packages. In addition to summarizing the work that will be carried out for major new facilities in FY 1993, this program plan also outlines the projects and scientific research that the divisions of NOAO plan to undertake in order to continue their support of the astronomical community. Highlights of the program for FY 1993 include the following: • Completion of the components for the field instruments and field-station shelters for GONG. • Integration and testing of the first two field stations. • Installation of the GONG Data Management and Analysis Center in the AURA building on Warren Avenue. • Completion of the bar lap polishing tool for the 3.5-m mirror project. • Grinding and polishing the 3.5-m mirror to its aspheric configuration. • Completion of the enclosure for the WIYN telescope on Kitt Peak. • Installation of the WIYN telescope mount on Kitt Peak. • Modification of the Hydra fiber-fed spectrograph for use at the WIYN telescope. • Deployment of imagers with 4x4 mosaics of CCDs at KPNO and CTIO. • Installation of a new prime focus corrector at the CTIO 4-m telescope. • Completion of modifications to the CTIO 4-m building to improve the thermal environment. • Initiation of construction of a wavefront sensor for the CTIO 4-m telescope. • Scientific verification of the performance of the Cryogenic Optical Bench at KPNO. • Implementation of 256 x 256 HgCdTe imagers at both CTIO and KPNO. • Completion of design of a 55-cm All-Reflecting Coronagraph at NSO/SP. • Further progress on adaptive optics at NSO/SP. • Upgrade of the detector used with the Near Infrared Magnetograph at the McMath and bringing the NIM up to full operational status. • Installation of a large format CCD and a cross disperser for stellar observations at the McMath. The budget request submitted to Congress by the President for FY 1993 includes an increase of approximately 3.5 percent relative to the budget initially received in FY 1992. While 3.5 percent is the assumption being used by the federal government for inflation in FY 1993, NOAO's costs are expected to increase by slightly more than $1M beyond the rate of US inflation. The two contributing factors are an increase in the GONG budget ($250,000 as specified in the project plan) and the higher rate of inflation in Chile relative to the US rate of inflation ($800,000 if changes in the peso/dollar ratio continue at the present rate.) The $800,000 is a combination of a $300,000 differential (Chile relative to US) inflation rate in FY 1992, which must be built into the base budget for future years, and an additional $500,000 in FY 1993 if present trends in Chilean costs continue. NSF has provided funds to cover Chilean inflation in each of the past two fiscal years. If the NSF does so again in FY 1993, then the budget problems will be substantially mitigated. II. SCIENTIFIC PROGRAM The scientific staff of NOAO is expected to devote approximately half of their time to service, with the remaining time reserved for research. In accordance with NSF requirements, this section of the program plan summarizes the research that will be undertaken in FY 1993. A list of papers published in calendar year 1991 is contained in Appendix 3. A. Cerro Tololo Inter-American Observatory J. Baldwin has been working in collaboration with G. Williger (CTIO), R. Carswell and A. Cooke (U. of Cambridge, UK), and K. Lanzetta (U. of California, San Diego) on several projects involving echelle spectroscopy of high redshift QSOs. Data have been obtained of the z = 4 absorption spectrum of an intervening galaxy, with the aim ofdetermining chemical abundances and physical conditions in the galaxy of highest known redshift. Other data were gathered of Lya forest lines at lower redshifts. This coming year these spectra will be supplemented by observations redward of the Lya emission line to provide a large sample of redshift systems which can be stacked (co-added) to search for weak metal lines. The goal here is to determine whether or not the Lya forest clouds are composed of primordial material. In another echelle QSO spectroscopy project, Baldwin made observations of Lya forest systems as close as possible to the atmospheric cutoff in order to try to link the statistics ofLya forest systems as observed from the ground to the surprisingly high number of very low-redshift systems seen with HST. Also, molecular hydrogen lines from another intervening galaxy were observed for the purpose of comparing ISM conditions at high redshift to the conditions that are found locally. Analysis of these data will be carried out in FY 1993. Baldwin will continue to work with G. Ferland (Ohio State U.) and P. Martin (Canadian Inst, for Theoretical Astroph., Toronto) on studies of local HII regions. Long slit echelle spectra have been obtained of M17, with the goal of mapping out the three dimensional structure of the ionized gas. A continuing project will make use of the 36-inch telescope for photometric monitoring of a sample of QSOs, which are also being observed with HST in collaboration with B. Wills and D. Wills (U. ofTexas), G. Ferland, H. Netzer (Tel Aviv U.) and I. Browne (U. of Manchester). Finally, Baldwin will work with T. Storchi-Bergmann (Brazil) and A. Wilson (U. of Maryland) on studies of narrow-lined regions (NLRs) in Seyfert galaxies. Data are now coming in from HST for two projects, which will require major effort from Baldwin.
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