NATIONAL OPTICAL ASTRONOMY OBSERVATORIES
NATIONAL OPTICAL ASTRONOMY OBSERVATORIES
FY 1998 PROVISIONAL PROGRAM PLAN
July 31,1997
TABLE OF CONTENTS
I. INTRODUCTION AND OVERVIEW 1
II. THE DEVELOPMENT PROGRAM: MILESTONES PAST AND FUTURE 2
A. Milestones for FY 1998 3 B. Milestones for FY 1997 4 m. NIGHTTIME PROGRAM 6
A. SOAR 6 B. Access to the Hobby-Eberly Telescope and to the MMT 7 C. Joint Nighttime Instrumentation Program 8 1. Overview 8 2. Description of Individual Major Projects 9 D. USGP 13 E. Telescope Operations and User Support 13 1. Telescope Upgrades at CTIO 13 2. Instrumentation Improvements at CTIO 17 3. Telescope Improvements at KPNO 20 4. Changes in User Services at KPNO 26
IV. NATIONAL SOLAR OBSERVATORY 27
A. Major Projects 27 1. Global Oscillation Network Group 27 2. RISE/PSPT Program 29 3. FY 1998 Program Plan Contribution for CLEAR Study 30 B. Instrumentation Program 31 1. NSO/Sacramento Peak 32 2. NSO/KittPeak 33
V. THE SCIENTIFIC STAFF 36
VI. EDUCATIONAL OUTREACH 37
VH. COMPUTER SERVICES 37
A. NOAO-Tucson 37 B. KPNO - Kitt Peak 38 C. CTIO - Cerro Tololo 39 D. CTIO Communications 40 E. NSO/Sacramento Peak 41 1. Main Lab Plan for FY 1998 41 2. Telescope Computers 42 F. NSO/Tucson 42 G. NSO/KittPeak 43 H. IRAF 44 VIH. FACILITIES MAINTENANCE. 46
A. CerroTololo 46 1. Fire Prevention and Fire Fighting 47 2. Renovation of the Vehicle Fleet 47 3. Improvement of the Main Access Road 47 4. Repainting 4-m Blanco Telescope 47 5. Cerro Tololo Power House 48 6. Water System - Cerro Tololo Pipeline 48 7. Control of Light Pollution 48 8. Enclosure for the TELOPS Cable Car 48 9. Bulldozer for Cerro Tololo 48 B. KPNO 48 C. Tucson: Central Facilities and Operations 50 D. NSO 51 1. Sac Peak 51 2. KittPeak 52
IX. CENTRAL SERVICES 53
A. NOAO Director's Office 53 B. Central Administrative Services 53 C. Tucson Facilities 53
X. THE BUDGET 54
A. KPNO Operations 54 B. USGP 56 C. Instrumentation Program 57 D. Budget Details 58
Appendix 1 - NOAO Organizational Chart Appendix 2 - NOAO Management Appendix 3 - Scientific Staff: Research Interests and Service Roles CTIO i KPNO xiii USGP xxviii INSTRUMENTATION DIVISION xxxv NSO xli Appendix 4 - User Statistics, FY 1996 Appendix 5 - Budget Tables Appendix 6 - KPNO and USGP Staffing Models I. INTRODUCTION AND OVERVIEW
AURA has recently submitted a long range plan for NOAO for the time interval 1998-2002. That long range plan defines the program for a critical phase in the evolution of NOAO: the nighttime program will complete the transition from an earlier generation of telescopes and instruments to an almost completely new suite of facilities; and the solar program will be redefined, with the primary goal being initiation of construction of the first large-aperture solar telescope to be built in this country in nearly 40 years. The program plan for FY 1998, which is described in this current submission, provides more detail on the specific activities that will be undertaken during the first of the five years covered by the long range plan. To place the program plan in context, we summarize here the long-term goals of NOAO.
Gemini South is currently scheduled to begin scientific operations in 2002. This milestone will mark the completion of an effort to replace essentially the entire complement of telescopes offered by NOAO to the community with the exception of the Blanco and Mayall 4-m telescopes, which will remain in operation. The construction that remains to be completed includes the 4-m SOAR telescope, for which it now appears that funding is available from Brazil, the University of North Carolina, and Michigan State University, and the 2.4-m wide-field O/IR imaging telescopes, which we believe are essential for supporting Gemini observations. Funding for these two telescopes has not yet been identified.
During this same period, we expect to complete several major instruments, including 8K x 8K mosaic CCD imagers for both CTIO and KPNO; a multi-fiber spectrograph for the Blanco telescope, which will match the capability of the Hydra spectrograph already at WIYN; medium resolution IR spectrometers for both CTIO and KPNO, with the CTIO instrument being a clone of the Gemini IRS and the KPNO spectrograph being a simpler device with more limited capability; wide-field IR imagers for both sites, with one being a single channel device with a lKx IK detector and the other being the multi-channel SQITD, upgraded to 500 x 500 arrays; a single high resolution (R = 100,000) spectrometer to be shared by both sites and with Gemini; and possibly a very high throughput single object optical spectrometer. A high resolution IR imager will be shared between CTIO and Gemini South during commissioning. We expect to provide a low-order natural- guide-star adaptive optics system at WIYN.
At the end of this time period, NOAO will be the only organization that offers observing time in both hemispheres, on telescopes with a range of apertures, and with a broad complement of infrared and optical instrumentation. In order to take advantage of this uniqueness, we must learn how to use this suite of telescopes in an optimum fashion. How do we match complex observing programs to telescopes in order to maximize the scientific output? How do we inform the community most effectively about options for their programs? How do we best support programs that require the use of more than one facility? What kinds of supporting infrastructure are required in order to use the time on Gemini and the large telescopes at the independent observatories most effectively? The long range plan outlined steps that we propose to take to develop answers to these questions and to provide user support that is unified across all of the facilities accessed through NOAO.
The changes in the nighttime offerings of NOAO, including access to Gemini and some of the independent observatories through the NSF instrumentation program, represent a qualitative change in what we offer the community. There will be fewer (by about a factor of 2) individual nights available, but the throughput of photons per unit time will in some cases be literally orders of magnitude higher than it was two decades earlier. It is almost certainly true that we will support fewer users than we have in the past, but this higher throughput will enable new types of science, including much larger sample sizes for programs ranging from the study of stellar activity levels in nearby open clusters to the analysis of the dynamics of distant clusters of galaxies. The use of new observing modes, such as queue scheduling, can potentially increase efficiencies still further and enable studies, that have up until now been impossible, of variable objects and targets of opportunity. During the period covered by this long range plan, we will re-examine the way we schedule the telescopes and experiment with a variety of modes of observing (queue, remote, and service, in addition to conventional observing with the astronomer present) so that we can understand what strategies will best support the diverse science proposed by the large community served by NOAO.
NOAO continues to look beyond 2002 in its long range planning. The crucial question is whether major gains in sensitivity and angular resolution beyond what is provided by the 8- to 10-m class telescopes linked to satellite telescopes for interferometry can be achieved most cost effectively in space or on the ground. We are working with a variety of groups and committees, including most notably ACCORD (the council of directors of major US observatories), to evaluate this issue. We also continue to work on the development of interferometry techniques through our participation in CHARA, which is building an interferometry on Mt. Wilson.
The issues that will be addressed by NSO during the next five years are very different from the issues confronting the nighttime program. It has been nearly forty years since a large-aperture solar telescope was built by NSO. In that same period of time, the nighttime program has built two generations of facilities: the Mayall and Blanco telescopes, followed by new technology telescopes in the form of WIYN, SOAR, and Gemini. The GONG project is an excellent example of how new techniques can yield fundamental advances in our understanding of solar structure. Application of modern technologies to the construction of a large-aperture solar telescope for studies of the solar disk and atmosphere can be expected to lead to equally profound advances in our understanding of the nature, variability, and origin of solar activity.
During the next five years, the central effort in the solar program will be to define the scientific requirements for a large-aperture telescope, establish the technical feasibility of building a telescope that will meet those requirements, identify the best possible site, and prepare and submit a proposal for such a telescope to the NSF.
The remainder of the NSO program is well defined and includes the continuation of GONG for at least one 11-year solar cycle; the preparation of a proposal to upgrade the spatial resolution of the GONG cameras by a factor of 4; the construction by the time of the next solar maximum of SOLIS, which is a suite of instruments designed to support Synoptic Optical Long-term Investigations of the Sun; completion of the construction and the operation of the PSPT (Precision Solar Photometric Telescopes) to study irradiance variations; demonstration and use of a low-order adaptive optics system at the NSO/SP Vacuum Tower Telescope; and the continuation of the infrared program at the McMath-Pierce Telescope with upgraded cameras based on the IK x IK InSb arrays.
IL THE DEVELOPMENT PROGRAM: MILESTONES PAST AND FUTURE
The primary component of the NOAO program is the continued operation of observing facilities for the user community at all three sites. In addition to operations, NOAO conducts an ongoing development program for both telescopes and instruments in order to ensure that what we offer to the community is competitive with the best facilities available worldwide. In this section, we list new milestones for FY 1998 and summarize the status of progress toward milestones included in the plan for FY 1997.
A. Milestones for FY 1998
• SOAR: Hire project team; select site; initiate design; complete agreement among partners.
• SOLIS: Complete definition and detailed engineering of the SOLIS instrumentation. Procure the long lead time items.
• Gemini Work Packages: Conclude the competition to design and build Gemini Mid-IR Imager; develop work scope for CCD controllers and initiate work; complete IR array procurement.
• GONG: Continue operation of the network and the pipeline processing and distribution of data; continue development of data reduction and management software; complete proof- of-concept high-resolution breadboard instrument; submit proposal for upgrade to high resolution cameras.
• Flagship Solar Telescope: Complete the feasibility study of CLEAR. Carry out a program of community outreach leading to AURA sponsored workshop concerning the science requirements for the telescope. Prioritize the science drivers and set the technical requirements. Continue the seeing tests and expand the site survey to include cloud-cover, coronal sky, and IR characterization.
• RISE: Complete deployment of the Mauna Loa and NSO/SP Precision Photometric Telescopes; establish routine operation of the network by the end of FY 1998.
• CCD Mosaic Imager: Upgrade the eight detectors to thinned science-grade SITe CCDs, and re-commission the upgraded instrument for scientific use by visiting astronomers.
• CCD Mosaic Imager II: Complete fabrication of mechanical parts.
• Hydra/CTIO: Complete fabrication of this multi-fiber positioner for the Blanco 4-m and its associated corrector and atmospheric dispersion compensator. Complete the testing in Tucson of its positioning performance and prepare for shipment to CTIO.
• CTIO Blanco Telescope: Complete commissioning and implementation of the f/14 tip/tilt system for use with the COB IR imager and the newly-converted IR spectrometer. Improve tracking and guiding system, including the addition of acceleration feedback in the servo loop and upgrade guide cameras to permit faster readout of subrasters; complete substantial fraction of work required to modify the telescope to allow installation of the Mosaic CCD Imager.
• KPNO Mayall Telescope: Install dome ventilation system; increase cooling capacity of mirror cooling; optimize use of Mayall thermal control system both for scientific performance and for improved energy efficiency; ventilate volume above the primary mirror; complete analysis of gains from active primary mirror support and secondary collimation systems.
« GNIRS: Carry out the Critical Design Review for the Gemini Near-IR Spectrograph. Maintain the fabrication schedule required to meet the planned delivery date.
• SQIID: Upgrade this near-IR imager with the installation of at least three ALADDIN arrays and a customized NOAO/Gemini Controller.
• Phoenix: Transfer this high-resolution IR spectrometer to CTIO and commission it at the Blanco 4-m telescope.
• Next Major IR Instrument: Develop a scientific definition and conceptual design for the next planned IR instrument: the Wide-Field-of-View IR Imager.
• Telescope Proposal Process: Unify proposal process for KPNO, CTIO; merge HET, MMT, and Gemini into proposal submission/review system as these telescopes come on line.
• HET and MMT: Complete Memoranda of Understanding for how program of public access to the Hobby-Eberly Telescope and the MMT will be managed.
• NIM 2: Complete commissioning of filter-based Near-Infrared Magnetograph.
• Solar Adaptive Optics: Initiate 3-year program to develop 20 Zernike Fast Adaptive Optics System for Sac Peak Vacuum Tower Telescope.
• Kitt Peak Solar Vacuum Telescope: Complete TCS upgrade.
• McMath-Pierce Facility: Install ALADDIN 1024 x 1024 InSb array and controller.
Bo Milestones for FY 1997
A similar list of milestones was included in the program plan for FY 1997. Their status as we approach the end of the fiscal year is as follows:
• GONG: Submit full scale papers on initial results to archival journals; continue network operations and distribution of reduced data to the community; prepare proposal to NSF for operation of GONG with upgraded cameras through a solar cycle. The 6-station GONG will have been in operation for nearly two years at the start of FY 1998; the first science results were published in May 1996. The pipeline processing and distribution of data continues. The feasibility study for continued observations for a full 11-year solar cycle and for upgrading the detectors has been completed, and preparation of a proposal for the upgrade is in progress.
• SOAR: Initiate design of this 4-m telescope, which is being constructed through a partnership involving Brazil, the University of North Carolina, Michigan State University, and NOAO. The Science and Operations Working Groups have completed planning documents for SOAR, and an external review, chaired by lerry Nelson, will be conducted on July 7 and 8. Tom Sebring, who was the project manager for the HET, has been hired as project manager for SOAR.
RISE: Deploy two Precision Solar Photometric Telescopes (PSPT) at field sites. The Italian PSPT telescope was deployed and now generates daily solar precision photometric data. A letter agreement with NOAA and HAO for deploying a second PSPT on Mauna Loa is being developed. Deploymentof the Mauna Loa instrument will be completed by the end of FY 1997.
• Phoenix: Complete commissioning of the high resolution 1-5 micron spectrometer at KPNO. Phoenix has been commissioned and will be used for 14 science runs on the KPNO 2.1-m telescope during the 1997 spring semester. One of the highlights was a study of the chemical composition of comet Hale-Bopp. During the summer, some upgrade work will occur in the areas of image quality and the speed with which the spectrograph configuration can be changed. Phoenix will be scheduled on both the 4-m and 2.1-m telescopes during the 1997 fall semester.
Optical Mosaic: Complete commissioning of this 8K x 8K mosaic of eight CCDs at KPNO. The CCD Mosaic Imager will be used for four runs on the KPNO 4-m and 0.9-m telescopes by visiting astronomers in June. The final commissioning items, including final software development and filter procurement, should be complete before the end of FY 1997. The next phase in this effort is upgrading the engineering-grade CCDs to science grade.
Cryogenic Optical Bench: Complete modifications and upgrades to this instrument, install a 512 x 512 ALADDIN array, and commission the instrument at CTIO. This infrared imager was successfully upgraded and tested in Tucson. It was then transferred to CTIO, interfaced to the tip/tilt secondary system on the Blanco telescope and commissioned. Its first use for science by a visiting astronomer occurred on 19 May 1997.
• NIM2: Commission filter-based Near Infrared Magnetograph. The instrument has been assembled and installed at the telescope, and test data have been taken with it. However, commissioning will extend through the first quarter of FY 1998.
Solar Cameras: Commission 2K x 2K CCD camera and data acquisition system. Xedar fast solar 2K x 2K cameras are now being used at the VTT and other NSO/SP telescopes.
Solar adaptive optics: Experimentally validate wavefront sensing concept. A Shack- Hartmann solar wavefront sensor was successfully demonstrated and incorporated into a slow adaptive optics system ("active optics"). It allowed for the first time the operation of the NSO/SP VTT as a diffraction-limited telescope.
KPNO Mayall 4-m Telescope: Complete work on cooling of primary mirror and develop an algorithm for using the cooling to improve image quality; design system for improved ventilation of dome; undertake package of smaller improvements based on CTIO program to improve image quality. The primary mirror cooling system has been installed and is in regular operation, with the performance currently being evaluated. The design for installing vents for natural ventilation in the dome is complete. A dome air mixing fan has been installed. Other desirable smaller improvements have not been completed because of lack of resources.
• CTIO Blanco 4-m Telescope: Install f/14 IR secondary; begin commissioning tip/tilt capability. The IR secondary has been installed. Commissioning of the tip/tilt capability is in progress as this is being written (June 1997), and the optical performance of the mirror is being verified as part of this commissioning activity.
• Kitt Peak Vacuum Telescope: Complete telescope control system upgrades. Substantial progress has been made on the new telescope control system, but bad weather and technical challenges have caused a delay in completion of the project. Completion should occur during the first quarter of FY 1998.
• SQIID: Upgrade this imager with the installation of at least three ALADDIN arrays; demonstrate the performance of the prototype Gemini IR-array controller. This has been postponed by one year. The reasons are: 1) no arrays were available from the ALADDIN development program; and 2) given the need for resources to complete higher priority projects (Phoenix, Cryogenic Optical Bench, Gemini IR Array Controllers), insufficient resources remained to accomplish the SQIID work.
• GRASP: Work out arrangement with OSU for construction and deployment of at least a three-channel IR/Imager Spectrometer; complete preliminary design review. OSU has recently made commitments to several other projects (LBT, MDM, and 1-m with Portugal and Yale in the south) and determined that they could not build an instrument as complicated and ambitious as GRASP. We are continuing to explore the feasibility of a more modest project, which would involve the modification of their dewar/optical bench to accomplish spectroscopy with a resolution near 5000.
• Gemini Work Packages: Complete Preliminary Design Review for Gemini IRS; deliver controller to Gemini by 15 July, 1997. The Gemini IRS project successfully passed its Preliminary Design Review in October 1996. The instrument team spent the remainder of FY 1997 doing detailed design work in preparation for the Critical Design Review, planned for October 1997. After reviewing the detailed requirements for the Gemini IR controllers, and taking into account engineering staff vacancies which we have been unable to fill in this competitive market, NOAO determined that it could not meet the requested delivery date of 15 July 1997. Working with Gemini and Hawaii, NOAO arranged for a staged delivery that would not impact the Hawaii schedule for the imager. A software simulator and test hardware (a fully functional array mount with cables and connectors) have been delivered according to the agreed schedule. Final delivery of the controller and test dewar is now scheduled for October 1997.
IIL NIGHTTIME PROGRAM
A. SOAR
The primary initiative currently in progress in the nighttime program is the SOAR project, which has as its goal the construction of a 4-m class telescope with superb image quality. The telescope is being designed to complement the Blanco 4-m telescope, which offers a wide field of view and has been retrofitted to provide very good image quality (median FWHM - 0.9 arcsec), but whose ultimate performance is limited by the technology with which it was built. The partners in the SOAR project are Brazil, the University of North Carolina, Michigan State University, and NOAO. The intention is that the financial contributions of the partners to construction, commissioning, instrumentation, and operations be such that NOAO and Brazil will each receive 30 percent of the observing time, UNC and MSU will receive 15 percent each, and the remaining 10 percent will be allocated to Chilean astronomers in accord with the agreement under which AURA operates in Chile. Letters of intent for sufficient funds to complete the SOAR project have been signed by the person in each of participating organizations who is authorized to commit funds.
An interim agreement was signed by the SOAR partners to cover preliminary design, which was funded at a level of $200,000, with equal amounts being provided by each of the partners. This phase of the project was led by Gerald Cecil from UNC. The Science Working Group (SWG) has prepared a document that summarizes the scientific and technical issues associated with the trades between an off-axis low-scattered light telescope and an on-axis telescope. The trades between equatorial and alt-azimuth designs have also been considered. The trade studies and the recommendations of the SWG will be evaluated by an external review board chaired by Jerry Nelson in July 1997. Based on that evaluation and the input of the SWG, the SOAR Interim Board, which is chaired by Sidney Wolff, will meet in mid-August to determine the optical configuration of the telescope. At that time, the Board also expects to select a site (Pachon or Tololo) for the telescope.
The external review board will also be asked to make a critical assessment of the report of the Operations Working Group, which has developed a cost model for the operations phase of the telescope.
Assuming that the summer reviews go well, the Board will then authorize the expenditure of several hundred thousand dollars to support the design phase of the project and to enable the hiring of the project team. We expect to complete this detailed design and planning stage by the spring of 1998, at which time the Board will be asked to authorize construction.
All future agreements with the partners will require AURA and NSF approval, and they will be forwarded for review as soon as they are drafted.
B. Access to the Hobby-Eberly Telescope and to the MMT
The NSF has funded instruments for the Hobby-Eberly Telescope and for the upgraded (6.5-m) MMT. In return, approximately 7 percent of the time on each will be available to the community for six years. Agreements in principle have been worked out with both the HET and MMT for how this access is to be managed, and NOAO now has the responsibility for drafting the MOUs that will describe the process; when we have mutually agreed, these MOUs will be forwarded to the NSF for approval. In the case of the HET, we have decided that the open access will be handled in such a way as to make NOAO look to the HET like a single user. That is, proposals for open access on the HET will be received by NOAO on our standard proposal form and reviewed by an NOAO TAC. The successful proposers will be asked to fill out a second form, which is required by the HET queue program, describing their planned observations in detail. NOAO will then forward those forms to the HET and receive the data for distribution to the community. NOAO will also establish a mirror site so that access to HET documentation is obtained directly from NOAO. This approach has the advantage that the HET will not have to provide any support beyond that which they provide to their own users. It does mean that NOAO will have to find the resources necessary to provide whatever assistance is required by the community. We do not yet have enough information to estimate how much time will be required.
The MMT will support conventional—astronomer at the telescope—observing. Again, the proposals for open access will be received and evaluated by NOAO. Depending on the program and the experience of the observer, we will then work with the MMT to determine whether their usual level of support is adequate or whether NOAO must supplement that support.
C. Joint Nighttime Instrumentation Program
1. Overview
NOAO must provide the national community of users with facilities that enable them to carry out observations competitive on an international level. That charge alone is sufficient to compel a substantial ongoing investment in new and upgraded focal plane instrumentation. Advances in detector performance, delivered image quality, and in user expectations all drive the development of new capabilities. International competition also forces an extremely focused investment that plays to the strengths of the telescopes and sites, exploits new detector and optical technology to maximum advantage, and manages resources with extreme diligence.
The existing facilities at CTIO and KPNO will be essential in providing observations that support and complement observations with the Gemini telescopes. We intend to exploit the one-degree fields of view of the 4-m telescopes for deep optical imaging and fiber-coupled spectroscopy. The new technology telescopes, WIYN and SOAR, will deliver image quality nearly undegraded relative to that provided by the atmosphere. These telescopes can also support image compensation systems (adaptive optics) that will enable both imaging and spectroscopy at higher angular resolution than offered by the older 4-m telescopes. The problems of star formation and evolution of galaxies at intermediate and high redshifts depend for their resolution on observations made in the near-IR. Both 4-m telescopes and SOAR will be equipped with imagers and spectrographs to tackle these challenging IR investigations.
Rapid advances in both optical and near-IR detector technology have created opportunities and strong user demand for new instrumentation. NOAO will continue to exploit the revolution in near-IR indium antimonide arrays that it has helped create by deploying a suite of new and upgraded instruments designed around IK x IK and larger formats. These will include multi-color and wide-field imagers, and two new slit spectrographs. The development of 2K x 4K, three-side buttable CCDs, driven in part by NOAO and its Gemini partners, enables very large format optical imaging. Mosaic imagers with 8K square format will be deployed for the prime foci of both 4-m telescopes, and mini-mosaics will be created for WIYN and SOAR. NOAO is developing new array controller hardware and software for Gemini that will be adapted for NOAO instruments as well. The Gemini telescopes will take on the proposals based on multi-object optical spectroscopy of the faintest objects. The niche for the national 4-m telescopes will be fiber-coupled wide-field spectroscopy and very high efficiency limited-field beam-fed spectroscopy. New holographic grating technology holds the promise of offering very high efficiencies for new instruments for SOAR and at Kitt Peak. Managing the instrumentation resources efficiently and in a manner that is satisfactory to both sites is crucial to the success of our program. The Instrument Projects Advisory Committee (IPAC) provides scientific prioritization to the Instrument Projects Group. Its current members are Taft Armandroff (NOAO-Opt. Instr.), Todd Boroson (USGP), Dave De Young (KPNO), Jay Elias (GNIRS Project), Richard Green (NOAO-Chair), Brooke Gregory (CTIO), and Bob Schommer (CTIO). IPAC meets with the instrumentation engineering managers once each month to review priorities, schedules, and budgets. They develop the scientific content of the long range plan on the basis of input from the users through the Users' Committee and personal contact, the WIYN and SOAR partners, and the Gemini advisory structure through the USGP. Every instrument under development has an instrument scientist from the NOAO scientific staff. We believe that this arrangement is essential for successful development: each instrument must have an intellectual champion to see that the project meets its scientific performance goals. IPAC provides a venue where the interests of each site are fairly represented. Concurrent with the establishment of IPAC, we put into place a revised system of project management. It places greater emphasis on initial design and planning and on overall accountability and resource tracking.
The CCD Mosaic imager entered shared risk use in the spring semester of 1997. It is an excellent example of the current project approach. The imager hardware design phase was extensive, with strict external review. The hardware was completed on schedule and functioned fully in every major aspect on its first engineering run at the telescope. Innovative design aspects included an articulated filter transport and a pneumatically driven blade shutter for high-precision exposure timing over the large array format. The multiplexed ARCON controller was produced by CTIO in this fully collaborative effort. Neil Gaughan, the IPG Program Manager, worked with the CTIO technical team to develop project planning tools and methods for resource tracking.
2. Description of Individual Major Projects
CCD Mosaic Imagers: The major instrument currently in commissioning is the CCD Mosaic Imager, to be deployed at KPNO, then cloned for CTIO. IPG has produced an imager with 8096 x 8096 format that has an active imaging area of over 12-cm on a side. The Mosaic currently contains eight 2K x 4K three-side buttable CCDs from Loral, but they are engineering grade. Scientific grade CCDs have been ordered for two Mosaic imagers, through a consortium purchase with Carnegie Observatories. The controller is a multiplexed quadruple version of the ARCON, developed and produced at CTIO. The first Mosaic Imager will be made available for shared risk observing on KPNO telescopes in June 1997. The second Mosaic is scheduled for completion in FY 1999, with deployment at CTIO in the first half of the calendar year.
Hydra for CTIO: The next project in the queue is building a version of the Hydra fiber positioner for the CTIO 4-m telescope. In the area of wide-field multi-fiber spectroscopy, the existing 4-m telescopes can and should complement the capabilities of the Gemini telescopes. The present multi-fiber instrument at CTIO is Argus, which was designed almost a decade ago. It is capable of observing 24 objects at a time, which puts it at a factor of four disadvantage compared with more modern instruments such as KPNO's Hydra. The new multi-fiber system is being built in Tucson and is based largely on the design of Hydra, but new motor controllers, a new gripper, and new fiber cables are being produced for the system for CTIO, along with a new wide-field corrector with atmospheric dispersion compensating prisms. This instrument will be located at the f/8 Ritchey-Chretien focus and will take advantage of the excellent image quality by using fibers of smaller on-sky diameter than those of Argus. Delivery and first commissioning activities are planned for October 1998. The new motors and motor controllers will provide a much more rapid positioning time than is currently achieved with Hydra on WIYN. The new technology will then be retrofitted as an improvement to WIYN Hydra.
Gemini IRS: The major instrument under production for Gemini is the Near-IR Spectrograph (GNIRS). This project is the largest IR instrument ever undertaken by NOAO. The dewar will be 2 meters in length, and the instrument weighs some 2000 kg, including electronics. It will provide long-slit capabilities with a range of dispersions through selectable gratings, covering the wavelength region from 0.9 to 5.5 microns at two pixel scales by means of four interchangeable cameras, which feed a single 1024 square ALADDIN-type InSb detector. Fabrication will begin after the Critical Design Review in early FY 1998, with delivery to the Mauna Kea site planned for late calendar 1999.
SQIID Upgrade: A high priority for the users, as expressed through the Users' Committee, is wide-field near-IR imaging. The first realization of that capability will be in the upgrade of SQUD, the four-color near-IR imager. The 256 square PtSi arrays will be upgraded to 512 square InSb arrays with a customized NOAO/Gemini Controller. That instrument will be available for shared risk user observations on Kitt Peak in fall semester 1998.
OSU IR Instrument: The next instrument after the SQUD Upgrade may be produced in collaboration with the astronomy department of the Ohio State University, which is exploring the feasibility of modifying their existing dewar/optical bench design to accommodate spectroscopy with a resolution near 5000 and a slit width appropriate to the Mayall 4-m image scale. If that is the case, NOAO would supply the ALADDIN detector, some capital, and probably the controller. Deployment would be planned for fall semester 1999.
WFOV IR Imager: To meet the needs for wider field imaging, the major instrument produced within the IPG will be an imager that addresses a large-format near-IR detector, probably 2K x 2K. That imager will be used on both the Mayall 4-m and the new 2.4-m imaging telescope. It is listed in Table 1 as WFOV IR imager, and is scheduled to be completed in FY 2000. The deployment of that imager is part of the integrated plan for supporting both CTIO and KPNO as well as Gemini. When WFOV is completed, SQUD can be sent to CTIO to support near-IR imaging programs while COB is used to commission Gemini South.
Adaptive Optics Imager: An extremely high priority for the entire WIYN partnership is the implementation of a low-order, natural guide star adaptive optics imager for the WIYN telescope. A general description of the capability is given in the KPNO section of this program plan. NOAO's participation in the project is listed in Table 1 under WIYN instrument upgrades. If this AO system proves effective, it could be replicated at other NOAO telescopes in both northern and southern hemispheres. There are currently no plans to implement high order systems with laser guide stars because of their excessive cost. However, should such a system be developed for Gemini South, NOAO would have an opportunity to evaluate its effectiveness at that time.
10 High-Efficiency Spectrograph: Studies are currently underway to define a new-generation moderate-resolution spectrograph for the 4-m telescopes. Scientific performance tradeoffs are being investigated to identify the most effective combination of field of view, spectral dispersion, and wavelength coverage. A key goal is to use the new generation of large- format CCDs with smaller slits and adequate pixel sampling in order to exploit the expected improvement in delivered image quality. In addition, the use of holographic volume phase gratings, coupled with the highest performance anti-reflection coatings on all optical surfaces, should allow a significant increase in throughput. Conceptual optical designs for the red and blue channels that meet the scientific performance goals will be undertaken in FY 1998.
A summary of the overall program, including manpower and costs, is given in Table 1. Detailed project plans are available on request. Neither expenditures nor reimbursements for the Gemini IRS are shown since this work is effectively done on a cost-recovery basis for direct costs.
11 Table 1 NOAO FY 1998 Instrumentation Projects
Project PI Labor Payroll Capital Total (MM) ($K) ($K) ($K) Operations & Maintenance IRO&M Merrill 26 146 50 196 OUVO&M Armandroff 21 117 20 137 Subtotal 47 263 70 333
KP Upgrades ARCON Upgrades Armandroff 18.5 104 7 111
KPNO Support 15.5 87 — 87 Gold Cam II Jannuzi 10 56 5 61 WIYN Instrument Upgrades Jacoby 16 _90 20 110 Subtotal 60 336 32 368
Research and Development Infrared Array Development Gatley 33 185 48 233 OUV CCD Development Armandroff 27 151 20 171 Fiber R&D Barden 2 _n _1 M Subtotal 62 347 69 416
Major Instruments CCD Mosaic Imager Boroson 4 22 5 27 High Efficiency Spectrograph Armandroff 7 39 1 40 CCD Mosaic Imager II Armandroff 60 336 120 456 Hydra for CTIO Barden 45 252 29 281 SQIID Upgrade Merrill 30 168 37 205
WFOV IR Imager Merrill 10 56 — 56 ALADDIN Controller Electronics Merrill 15 84 125 209
Gemini IR Array Controllers Merrill 20 112 — 112
IR Lab Array Controller Merrill 10 56 ~ 56
Solar IR Array Controller Merrill 5 28 — 28
OSU Instruments Green — — 235 235 Subtotal 206 1154 552 1706
Total IPG Labor/Capital Required 375 2100 723 2823
IPG Budget 375 2100 431 2531 Capital Recovery from KPNO 32 32 Capital Recovery from Gemini IR Array Controllers 210 210 Capital Recovery from Solar IR Arrav Controller 50 50
12 D. USGP
In FY 1998, the USGP will begin planning and implementing its support of US access to Gemini in the operations phase, while continuing to manage the procurement of the US- assigned Gemini instruments and to act as scientific liaison between the US community and the international Gemini Project. In addition, the USGP is beginning its expanded role within NOAO, taking on responsibility for the "before and after" activities that are common to all the telescopes to which NOAO does or will provide access. The goal is to unify these processes so that users in the community can work with a single interface and a single set of rules for getting information about the facilities, applying for telescope time, preparing for observing runs, and reducing and analyzing their data.
Specific activities to be undertaken by the USGP in FY 1998
• The form and the process for telescope time allocation will be unified so that proposers use identical procedures for KPNO and CTIO.
• The USGP will hold a workshop on capabilities required to support efficient use of the 6.5- 10-m telescopes now coming on-line. The goal is to identify and quantify the needs for smaller telescopes, instruments, surveys, and software in a community-wide forum using a science-based approach.
• The information available to the community about the facilities which NOAO provides will be organized into a coherent internet Web site. This Web site will incorporate telescope proposal information, telescope and instrument capability information (including software for predicting exposure times), and contact information for user support.
• Work will continue on a number of Gemini work packages that are in progress, including the Near-IR Spectrograph, the Near-IR arrays and controllers, and the CCDs and CCD controllers.
• The USGP will select a group to design and build the Gemini Mid-IR Imager through a competitive procurement.
• The USGP will begin work on procurement of instruments for the ongoing Gemini development program. Early activities will include developing cost estimates and establishing community interest for those instruments that will receive early consideration.
E. Telescope Operations and User Support
1. Telescope Upgrades at CTIO
a. Background
CTIO's program for the coming years focuses on upgrading and instrumenting NOAO's southern telescopes so that they remain scientifically productive in an era of modern 4-m and 8-m apertures. The Gemini 8-m project is well advanced on Cerro Pachon, and it will have a modern 4-m companion in the SOAR telescope. These projects will be coming on-line in the next 3-5 years, and we anticipate that CTIO ETS
13 resources will be used extensively in the SOAR (and possibly Gemini) instrumentation and commissioning. The combination of SOAR and the Blanco 4-m and their instruments will be configured as far as possible—through sharing arrangements between the 4-m telescopes—as a complementary observing system in support of work with Gemini.
In FY 1997, CTIO accomplished the following:
• Began commissioning of the F/14 tip-tilt system on the Blanco, for use with COB and the IR spectrograph (IRS), including a fast (100 Hz) guide camera and GUI interface
• Conversion of the IRS to f/14 (from the old f/30 system)
• Successful deployment of COB with a 512 x 512 InSb array
• Installation of a new 4-m thermal control system
• Implementation of dome ventilation doors for the 1.5-m telescope
• Commissioning and successful scientific use of an optical mosaic imager (the BTC, 4K x 4K thinned CCDs) at the Blanco PF, an instrument provided by T. Tyson (Lucent Technologies) and G. Bernstein (U. of Michigan)
• Installation of a modern TCS on the 1.5-m telescope (a copy of our 4-m system)
A major feature of the program for FY 1998 continues to be preparation for new instruments which are due to arrive in 1998-1999. In collaboration with the Tucson IPG effort, we will be equipping the Blanco 4-m with: a) an NOAO 8K Mosaic imager at prime focus; b) the Phoenix high resolution IR spectrometer; and c) the Hydra/CTIO multi-fiber spectrograph. Within two years we should have, for infrared work, a well- instrumented 4-m telescope with excellent image quality over a small field at f/14, mainly for near-IR imaging and spectroscopy. At the same time, in the optical, the wide-field aspects are being emphasized with the Mosaic imager and Hydra spectrograph; the telescope will be able to deliver good image quality at f/8 on a routine basis over a 45-arcminute field.
One main focus in FY 1998 continues to be on further improving the performance and general maintainability of the 4-m telescope. The addition of active optics, an image analyzer, and thermal controls over the past several years has proven highly successful, and delivered image performance has improved significantly. In FY 1998 we will be continuing the analysis and tuning of the servo and guiding system, including a major upgrade of the servo controller hardware and software; we also plan continued upgrades of the thermal control for the R-C and PF cages.
14 b. Prime Focus Pedestal Upgrade/Mosaic Installation
The existing Prime Focus Pedestal is not strong enough to support the NOAO Mosaic Imager, and during FY 1998 we will modify and strengthen this assembly. The pedestal for the 4-m Mayall telescope was modified in FY 1996 for the same reason, but due to differences in corrector design it is not possible to simply copy the KPNO system. We will also take the opportunity to install new focus motors, and provide lateral and tilt adjustment for the PF corrector. This latter facility will greatly simplify procedures for collimating the telescope. The PF cage will be prepared to accept this instrument through modification of the entrance doors and removal of internal structures. c. 4-m Control System Improvements
During FY 1996, the antiquated 4-m telescope control logic was replaced with a modern programmable logic controller based system, following the upgrades made to the KPNO 4-m several years ago. With the improvement of the optical quality of the telescope, tracking and guiding performance have become limiting factors on delivered image quality.
During FY 1997 and continuing into FY 1998, effort is therefore being devoted to improving the servo system's performance. Initially this involves careful tuning of the existing servo system and the addition of acceleration feedback in the servo loop. We will also begin a project to replace the actual servo system to provide a modern and maintainable level of performance. The current model, still under evaluation, is to replace the servo controllers with Delta-Tau systems, analogous to the Gemini telescopes. d. 4-m Guide Camera Upgrades
We will upgrade the guide cameras at the R-C and Prime foci of the Blanco telescope to allow faster readouts (-10 hz) of subrasters to permit better guiding performance with our new servo system. Most of the development work has already taken place for the very fast (100 Hz) tip-tilt camera system for f/14, and these changes will be ported to three additional cameras (the f/8 and prime + a spare). As time and resources permit, we will also upgrade the guide cameras on the 1.5-m and 0.9-m to more modern systems in order to eliminate dependence on aging leaky-guider hardware. e. 4-m Thermal Control
The present 4-m primary mirror cover, when open, forms a 2-m deep cylindrical enclosure above the mirror which can trap air and thus degrade the seeing. We plan to replace the mirror cover with a two-component folding cover, which will provide a completely clear path in the N-S direction to the level of the primary, and thus ensure that flushing is rapid and efficient.
An air extraction system for the prime focus cage has been designed in order to remove the thermal load introduced by the electronics and machinery of the prime focus imagers. Although this load is not large, any air at non-ambient temperature escaping from the cage passes across the telescope input beam and thus will degrade the seeing. Analysis of the data produced by the many temperature probes installed on the
15 telescope and dome interior show that there is still significant heating of the dome air by the building interior, of particular importance in low wind conditions when little natural flushing of the dome air occurs. The NOAO 10-micron camera system will be used to help in diagnosing which building surfaces are responsible for the heating, followed by installation of extra insulation or air conditioning, where appropriate. f. 1.5-m Telescope Upgrades
Our second largest telescope, the 1.5-m, suffers from a poor thermal environment and several optical problems with the secondary mirrors. It is also being run with a hybrid control system.
In FY 1997, we conducted a TCS software upgrade, converting to the system we are currently running on the 4-m. We designed more stable secondary mirror mounts, with encoders to permit reliable collimation runs, and we plan to install these, as time and resources permit, in FY 1998. We have also included an effort to provide a field (coma) corrector for the f/13.5 focus.
In FY 1997, we completed the dome ventilation system and in FY 1998 we will continue to improve the dome thermal environment by improving the insulation on the main floor, replacing the main transformers which are dumping heat into the space below the observing floor, and installing air conditioning units in the building. g. Collaborative and Guest Facilities
The following is a brief summary of facilities likely to be under construction or in operation at CTIO during FY 1998 which involve a variety of new collaborative, shared and/or contractual arrangements with other institutions or organizations. Where NOAO has agreed to provide supporting services to programs in which it is not a direct partner, such services will be made available on a strict, at-cost, aperture-priority basis; for example, smaller facilities that encounter problems during a weekend may not get help until the following Monday.
• Gemini South 8-m Telescope. Work on construction of the Gemini South telescope on Cerro Pachon is described at http://www.gemini.edu/. CTIO staff are likely to continue to serve on a variety of Gemini committees, both for the international and US parts of this effort. Importation of Gemini hardware into Chile will continue to be supported by AURA's CTIO offices in Santiago and La Serena. During FY 1998, the major work on Cerro Pachon will be the construction of the dome for the Gemini South telescope.
• SOAR 4-m Telescope. Planning for the SOAR telescope is described at http://www.pa.msu.edu/soar/. CTIO staff members have been involved in major aspects of optical design and in planning for operations of SOAR. As NOAO is a major partner in SOAR, involvement by staff from CTIO will continue in FY 1998 and increase in subsequent years. The SOAR project was discussed in more detail in Section HI.A.
16 • 2MASS-South, 1.3-m IR Survey Telescope. A description of work on the construction and operation of this facility can be found at: http://pegasus.phast.umass.edu/GradProg/2mass.html. The southern part of this survey is expected to start in FY 1998. NOAO/CTIO will provide specially contracted operators for the telescope, as well as limited maintenance under the terms of an MOU signed with the UMASS consortium.
• Revival of the 1-m Telescope by a Yale-led International Consortium. During FY 1998, the Yale 1-m telescope, closed in FY 1997 for lack of funding, is expected to re-open on the basis of funding received from Yale (30%), Ohio State University (30%), the University of Lisbon (Portugal) (30%), and NOAO (10%) (see articles in recent issues of the NOAO Newsletter). The Yale 1-m telescope is expected to be used primarily with a simultaneous Optical/TR imager for synoptic observations, which are difficult to schedule on the existing CTIO telescopes. As a minor partner, CTIO's primary contribution in FY 1998 will be in the form of operations infrastructure.
• GONG-CTIO station. A description of the Global Oscillation Network Group (GONG) program in Solar Seismology appears at: http://www.gong.noao.edu/ index.html. Further information is given in Section IV.A.l. of this Program Plan. Impact on the operations group at CTIO has been small as a result of the high quality of engineering and maintenance of the station by GONG staff, sent down at carefully-planned intervals from the US.
• United States Naval Observatory's 20-cm Astrographic Survey Telescope. A new astrometric survey of the Southern hemisphere will be in progress during FY 1998, using the USNO 8-inch CCD astrograph mounted in the current 16-inch dome. (The 16-inch telescope is obsolete and will be removed.) More details can be found at http://aries.usno.navy.mil/ad/ucac/ucac-s.html.
• Swarthmore 3-cm Robotic H-alpha Survey. Described briefly in the March NOAO Newsletter and at: http://www.noao.edu/noao/noaontvJs/mar97/node2.html, the Survey, which is expected to start in FY 1997, will continue throughout FY 1998. Limited maintenance will be provided under terms of an MOU signed with the Swarthmore group.
• The MACHO Program on the CTIO 0.9-m Telescope. This highly successful program, involving a 15% share of the 0.9-m telescope, is expected to continue through at least part of FY 1998. CTIO provides telescope operator support in a cost-sharing arrangement with the MACHO consortium.
2. Instrumentation Improvements at CTIO
a. Hydra Corrector/ADC Mounting and Installation
In order to obtain high quality images over the entire 4-m R-C field, an ADC corrector has been designed as part of the Hydra/CTIO project for the Blanco 4-m. This corrector should permit fibers as small as 1 arcsec to be used efficiently. In FY 1997 we began a project to design and construct the mounting cell and rotation subsystem for the
17 ADC/wide-field corrector, based upon our experience with the prime focus ADC. Fabrication and installation will carry over into FY 1998. The corrector will be installed in the 4-m chimney and feature a motor drive to flip the elements in or out of the beam to accommodate other instruments, particularly in the IR. b. Hydra Spectrograph
In order to accept the 130+ fiber spectra that Hydra will produce, CTIO began in FY 1997 a project to modify the Argus bench spectrograph. Among other things, this entails changing the focal ratio by installing a new camera. The number of fibers which can be accommodated also has to be increased and the optical path changed. Fabrication of the optics for a new camera was finished in FY 1997. During FY 1998 we will increase the size of the spectrograph by installing a second optical bench, implementing the new camera, and changing the optical path. We will then mechanically modify the system to increase its fiber capacity and implement remote controls at least for focus, filter changes, and grating tilt. With the arrival of Hydra, the new collimator will be installed. This effort also includes a calibration lamp assembly. c. CCD Controllers
We intend to begin retrofitting the existing ARCONs on CTIO with the final versions of three controller electronics cards (Video, VTT, and ADC), which have been developed over the past two years. These printed circuit cards will provide increased reliability and a cleaner video path. New functionality includes remote configuration of bias and clock voltages and full telemetry. d. Spectrograph Motor Controllers
The R-C (low-dispersion) spectrograph on the 4-m has a number of functions that are remotely controlled by a convoluted patchwork of Camac and 25-year-old stepping motors, only some of which still work. During FY 1998, we will continue the process of converting spectrograph control to our new generation of standard, self-contained "Smart" Motor Controllers (SMCs). This will involve changing the control of functions of the R-C spectrograph and implementing remote control of some of the movements of the Argus/Hydra and echelle spectrographs—all of which at present are operated manually.
This process is part of a more general conversion of much of the old motor control at the observatory to a more modern, robust, and standard system. e. Implement Two CCD Systems
We expect to bring up two additional CCD systems on an ARCON controller during FY 1998. These conceivably would be a SITe or EEV 2048 x 4096 for 4-m spectroscopy, and a pair in a mini-Mosaic dewar for direct imaging. Our main needs at this point would be a lower noise, faster readout CCD to replace the LORAL 3K x IK in our 4-m R-C spectrograph, and a replacement for a SITe 2K imager which failed. The capital costs include an estimate for the purchase of a single 2K x 4K (80K).
18 f. Telescopes and Instruments at CTIO
A complete list of telescope and instrument combinations available at CTIO is given in Table 2. Estimates of the manpower required for the improvements projects described here are given in Table 3.
Table 2
CTIO Telescope Instrument Combinations
Blanco 4-m Telescope: Argus Prime-Focus Fiber-Fed Spectrograph + Blue Air Schmidt (BAS) Camera + Loral 3K CCD R-C Spectrograph + Blue Air Schmidt (BAS) Camera + Loral 3K CCD Echelle Spectrograph + Blue Air Schmidt (BAS) Camera + Loral 3K CCD Echelle Spectrograph + Folded Schmidt + Tek IK Echelle Spectrograph + Long Cameras + Tek 2K Prime Focus Camera + BTC (4K x 4K Tyson/Bernstein CCD Mosaic) Prime Focus Camera + Tek 2K CCD Prime Focus Camera + Photographic Plates Cass Direct + Tek 2K Rutgers Imaging Fabry-Perot + Tek 1K Cryogenic Optical Bench + 512 InSb CTIO IR Imager + 256 HgCdTe CTIO IR Spectrometer + 256 InSb
1.5-m Telescope: Cass Direct + Tek IK and Tek 2K CCDs Cass Spectrograph + Loral 1200 x 800 CCD Bench-Mounted Echelle Spectrograph + BME camera + Tek 2K Rutgers Imaging Fabry-Perot + Tek IK CTIO IR Imager + 256 HgCdTe ASCAP Photometer
2MASS 1.3-m: Scheduled to open for dedicated 2 micron survey work in mid-1998
1-m Telescope: Closed. To re-open in March 1998 as a consortium under Yale U., Ohio State U., U. de Lisbon, and NOAO partnership.
0.9-m Telescope: Cass Direct + Tek 2K
Curtis Schmidt: STIS 2K CCD (Direct or Prism)
19 Table 3
FY 1998 Projects (Labor Estimates in Manweeks)
Project ME MD MF OE EE ED EF CS $K 4-m Servo Replacement 46 1 12 27 20 Hydra Spectrograph 24 55 81 15 9 8 14 67 Hydra Corrector Mount+Ins 12 12 84 4 1 2 11 25 PF Pedestal + Mosaic Inst. 25 41 83 30 4-m Primary Cover/Thermal 10 15 30 4 10 4-m Guide camera upgrades 2 20 5 8 28 6 CCD controller retrofits 50 2 53 19 20 Spectro. Motor Control 10 12 10 17 1 12 30 1.5-m Tel. Upgrades 4 2 10 10 Implement 2 CCDs 2 4 6 14 6 4 2 _80 Total 87 141 304 16 166 25 99 142 $258K
Columns headed ME, MD, MF are Mechanical Engineering, Design, and Fabrication estimates; OE is Optical Engineer; EE, ED, and EF are Electronics Engineering, Drafting and Fabrication; CS is Computer Software; all in manweeks. Column $K lists non-payroll expenses in units of $1000.
3. Telescope Improvements at KPNO
The primary focus for KPNO telescope improvements in FY 1998 will again be the two largest telescopes: at the Mayall 4-m, improvements will continue to address the delivered image quality; work at WIYN will primarily address telescope performance and operations efficiency. The proposed modifications reflect the reality that improvements begin as soon as commissioning ends and continue throughout the lifetime of a telescope as new scientific demands and expectations are made upon it.
We will continue to upgrade the CCDs in use at the KPNO telescopes as improved devices become available. 2K x 4K SITe CCDs with 15-micron pixels are on order to form the 4K x 4K "mini-Mosaic" for the WIYN telescope. KPNO scientific staff will be heavily involved in commissioning of this significant new capability for the WIYN. We also continue to evaluate alternatives for the R-C and Echelle spectrographs that will allow better sampling than the Tektronics CCD now used.
a. Progress on Work Proposed for FY 1997
Systematic measurements of delivered image quality at the Mayall 4-m to form a baseline against which future improvements to the image quality could be assessed have been taken for the past year, generally one measurement per night. The average DIQ is 1.1 arcsec, with 0.9 arcsec or better 25% of the time. We have begun to correlate DIQ with various dome environmental variables. As expected, the seeing is degraded by a warm mirror. In addition, when the temperature differential between the inside and the outside of the dome exceeds more than a few degrees C, the DIQ is significantly degraded, a condition which will be addressed by dome ventilation. On nights when the seeing is approximately 1 arcsec and we cannot attribute degradation
20 to local temperature effects, the Mayall produces image quality comparable to that at WIYN, indicating generally good optics at the 4-m and proving that local seeing effects are still the limiting factor in determining the DIQ.
Design of the Mayall dome ventilation system has been completed. Installation began in late spring 1997, with major effort to be taken during Summer Shutdown 1997 and completion projected in FY 1998. Based on the need to achieve thermal equilibrium with the outside air, simple studies in the literature suggested several dozen flushes per hour would be sufficient, a result which is difficult to model or test. The starting performance requirements for the Mayall ventilation system were to produce a minimum of a hundred dome flushes per hour in a 10 mi/hr wind with a minimum of dead-air space (i.e., vents distributed mainly away from the dome slit but also forward of 90 degrees from the slit). The final design will deliver some 200 flushes per hour in a 10 mi/hr wind from twenty-two 6 ft. wide by 22 ft. high panels, the same ventilation rate as that achieved with the CTIO 4-m (c.f. WIYN delivers some 675 flushes per hour in a 10 mi/hr wind; the Mayall site is significantly windier than either WIYN or the CTIO 4-m). We were not able to copy the CTIO system because of significant differences in the designs of the two domes.
Thermal control of the mirror, floor, and telescope oil was achieved in FY 1997, as was installation of a dome air mixing fan to promote thermal equilibrium during the daytime.
Two projects related to Mayall image improvements, encoding of the f/8 secondary and mirror heating, proposed in the FY 1997 Program Plan, were not undertaken because of lack of resources. The analysis required to evaluate the usefulness of active control of the primary and f/8 secondary will be carried out in the next few months. b. Proposed Upgrades to Telescopes and Instruments for FY 1998
Improvements for FY 1998 will again primarily address image quality at the Mayall 4-m. The goal of this work is to reduce average DIQ to 0.9 arcsec and to increase the percentage of nights when excellent images are achieved (0.6-0.7 arcsec images are observed at the 4-m when atmospheric conditions are just right).
Mayall 4-m • Optimal use of the Mayall thermal control system: Now that the hardware and basic software for the mirror and floor cooling and the temperature control of the telescope oil have been completed with a unified control system, we must learn to use this system each day to respond to local weather conditions in a manner which will maximize the potential improvement of the thermal conditions, at the same time doing nothing which would degrade the seeing conditions at night (e.g., cooling the mirror and floor too much). The system must be thoroughly characterized and operating procedures developed to respond to typical and atypical weather conditions. In particular, we must plan to increase the amount of cooling capacity of the current mirror system, which now only offsets heat gained during the daytime.
21 • Installation of the Mayall dome ventilation system: Construction on this project began in the third quarter of FY 1997, will take the entire six week Summer Shutdown period for this calendar year, and is not expected to be completed until at least the second quarter of FY 1998. Upon completion of the vent installation, time must be taken to characterize the system to develop operating procedures that maximize the benefit of vents but do not contribute to image degradation, e.g., by wind buffeting the telescope structure.
• Completion of the f/8 secondary motion and wavefront analysis system (begun in FY 1997 but not completed due to resource limitations).
• Completion of the analysis of the necessity for active primary mirror supports: If found to be an important source of image degradation, design work will begin in FY 1998 with possible installation during Summer Shutdown 1998 when the mirror is next out for aluminization.
• Ventilation of the volume immediately above the mirror: This volume is a potential source of stagnant air where convective currents can be established with resulting image degradation. Experiments more than a decade ago with simple mirrors in the laboratory indicate that fans can disrupt the currents. Modern telescope designs like WIYN and Gemini use the wind blowing through the dome. More active measures must be taken at the Mayall, which has its mirror at the bottom of a relatively deep cavity.
• Mirror heating system: We continue to follow Gemini's development of a system for heating the surfaces of the primary mirror. The proposed operating procedure is to cool the bulk of the mirror during the daytime to well below the anticipated nighttime temperature, and then to heat the mirror surface to achieve thermal equilibrium of the reflective surface of the mirror. This improvement has potentially larger gains in thick mirrors, such as the Mayall 4-m, than in the Gemini telescopes, as many nights exist when the mirror temperature is significantly different from ambient because of the long thermal time constant of a massive mirror.
WIYN • The partners of the WIYN Observatory have approved a two-year special assessment totaling $400K to upgrade many telescope systems. Safety of personnel and equipment is foremost in the upgrade plan. Additional upgrades will bring the telescope within original specifications, enhance its operational efficiency, minimize maintenance, and provide documentation. Tasks ordered in decreasing priority for the first year are listed in Table 4. Definition of the projects to be completed during the second year of the special assessment (FY 1998) will begin in July 1997.
• The Observatory Scientist and the WITN Science Advisory Committee are responsible for preparing a development plan extending beyond the two-year special assessment period. It appears likely that the next new instrument will be a low order (19 elements) adaptive optics camera capable of producing near- diffraction limited (0.1") images in the long-wavelength optical or very near-IR
22 over a relatively narrow field of view (15"). It will allow for operation at lower orders or tip/tilt only when bright natural guide stars (V < 14) are unavailable or when a wider corrected field (60") is desired. A wide-field imager (10') also will be available using a 4K x 4K CCD mosaic, but with no atmospheric correction. The AO system would be permanently mounted, and a switch between the different modes of operation would be easily possible. Laser guide stars are not under consideration at this time due to their significant operational costs. If a laser guide star system is installed at Gemini South, then NOAO will be able to see if such systems are feasible for deployment at NOAO telescopes at CTIO or KPNO.
Other instrument concepts are also under consideration, such as a high efficiency spectrograph, infrared camera, a very wide-field imager (20'), and an infrared multi-object fiber spectrograph. These concepts will be reviewed in the larger context of NOAO's instrumentation capabilities at other telescopes in order to define a coherent set of tools for visiting astronomers as well as the WIYN partners without unnecessarily duplicating existing or planned instrumentation. A long- range planning workshop for WIYN is being scheduled during the summer of FY 1997 in order to devise a strategy for developing WIYN's capabilities.
FY 1997 Project List: Table 4 contains the projects that are expected to be completed during the first year of the WIYN special assessment.
Manpower estimates are given in months of effort for Kitt Peak Mechanical Engineering (KPME), Kitt Peak Electronics Engineering (KPEE), Mountain Programming Group software (MPG), Facilities (FAC), and miscellaneous resources (Other). A full-time equivalent (FTE) is considered to provide 10 months of effort, after vacation, sick leave, and training.
23 Table 4 Expected Project Completion During Year One - WIYN Special Assessment
Description KPME KPEE MPG FAC Other
Manual brake release system 3.0 Install intercom 0.25 Hardwired speed limits versus altitude 0.75 Install Azimuth hardware limit 0.15 0.25 Elevation hard-stop upgrade 0.25 Lower overspeed limits 0.15 Servo/encoder inhibit brake release 1.00+ Global Software Watchdog 0.50 Documentation 4.50 3.00 4.50 E-Stop upgrade/delay reduction 1.50+
Limit upgrades 0.90 3.25 Instrument elevator interlock 0.15 0.30 OSSCS runaway 0.50 IAS cable wrap 0.90 IAS chiller 0.25 Secondary Resonance 0.25 3.25 Hydra guider upgrades 0.25 Telemetry enhancements 0.75 Add new telemetry to EDS 0.15 Battery charger spare 1.50 IAS motor control 0.30 0.45 High pressure brake system 0.40 0.50 Move OSSCS power supplies 0.50 3.50 PMS Manager 0.50 MPG router upgrades 2.00 Wind breakaway 0.25 1.25 Hoist modifications 1.00 Secondary vane guides 0.55 Tertiary air bag 0.70
Drive motor rework 0.55 PMS tuning 1.15 IAS power supply ventilation 0.80 CS Electronics Rack Ventilation 2.00 Real-time image quality estimator 0.25 EDS tools enhancement 1.00 VSIO hang fix 1.00
PMS overpressure valves 0.15 Dome hatches for snow removal 0.70 Exhaust duct louvers 0.25 0.15 Secondary mirror control system upgrades 0.25 0.25 Totals (man-months) 13.40 25.15 10.40 2.65 1.50 Grand Total 50.3 months (5.0 FTEs)
24 c. Instrument Improvements
The KPNO Users' Committee has given high priority to providing a new camera for the 2.1-m GoldCam Spectrograph. The new camera will achieve low to moderate spectral resolution of point and extended objects with improved performance and efficiency over the wide spectral range possible with the 3K x IK Loral CCD. The existing camera was not designed to provide good image quality over such a large area in the focal plan. This project has been a high priority for the users for the last two years but has been delayed because of lack of resources. The intention is to complete the camera in FY 1998 and to begin commissioning in spring of that year.
We also plan to replace the leaky guider systems. The "leaky" memory guide electronics—integrators with time-weighted history to feed correction pulses to the telescope servo control—are based on commercial circuit boards that are no longer available and cannot be readily repaired at the component level. A design study will be initiated in FY 1998 to select a replacement. One option is a commercial frame-grabber unit similar to that at WITN. Other designs using PC-based components will be considered.
The year 2000 has unknown consequences for the computer systems on the mountain. So that operations do not grind to a halt on 1 January 2000 or put us back to 1900, we plan in FY 1998 to determine all of the century dependencies in our software and to make changes in early FY 1999, well before the millennium arrives.
Table 5 summarizes the telescopes and instruments to be offered at KPNO during FY 1998.
25 Table 5
KPNO Telescopes-Instrument Combinations for FY 1998
Mayall 4-m Telescope R-C Spectrograph + CCD (T2KB) Cryocam Spectrometer (with 800 x 1200 Loral CCD) Echelle + UVFast, Red Long and Blue Long cameras + CCD (T2KB) Prime Focus Direct Camera + CCD (T2KB) CCD Mosaic Imager (shared risk observing beginning in fall 1997) IR Cryogenic Spectrograph (CRSP) IR Imager (IRIM) High-resolution Near-IR Spectrometer (Phoenix) Ohio State - NOAO Imaging Spectrometer
WIYN Telescope Hydra + Bench Spectrometer (T2KC) CCD Imager (S2KB)
2.1-m Telescope Direct Camera + CCD (T1KA) GoldCam CCD Spectrograph (F3KA) IR Cryogenic Spectrograph (CRSP) IR Imager (IRIM) High-resolution Near-IR Spectrometer (Phoenix) Ohio State - NOAO Imaging Spectrometer
Coude Feed Telescope Coude Spectrograph + Cameras 5 and 6 + CCD (F3KB) NICMASS HgCdTe IR Array, no new programs accepted)
0.9-m Telescope Direct Camera + CCD (T2KA) CCD Mosaic Imager (shared risk observing beginning in fall 1997) CCDPhotometer (CCDPHOT) (T5HA), no new programs accepted
4. Changes in User Services at KPNO
Driven by decreases in budget and the transfer of resources to the USGP and other programs, we continue to shrink operations on Kitt Peak. Specifically, KPNO has made arrangements to transfer the responsibility for operation of the Burrell Schmidt telescope back to Case Western Reserve University, which owns the telescope. NOAO users will no longer be scheduled after 1 October 1997. The scientific rationale for this closure is that the mosaic CCD imager at the 0.9-m telescope offers better sampling of the point spread function and is therefore better suited to more than 90 percent of the science currently supported at the Schmidt. We will consider purchasing time from Case for the one ongoing program that cannot be transferred.
26 The Coude Feed is unique in offering resolutions of 200,000 for spectroscopy. It is, for example, the only telescope in the US that can test the claim that the radial velocity variations in 51 Peg are due to changes in line shape rather than the result of reflex motion caused by an orbiting planet. However, the Feed has an aperture of only 1 meter, and therefore is limited to the very brightest stars. We are currently exploring the feasibility of moving the spectrograph optics to the 4-m dome and feeding them with a fiber in order to extend the limiting magnitude. In the meantime, we have restricted the number of programs supported at the Feed so that only one new setup per week is required.
If the budget permits, we will continue to operate the 2.1-m and the 0.9-m telescopes until they are replaced with the proposed 2.4-m telescope. The only work planned for the 2.1-m is the replacement of the motors on the guider. The goal is to lower the maintenance effort; the existing motors are of low torque and stall at times with consequent loss of observing efficiency. If funds can be found, a commercial TCS will be considered for the 0.9-m telescope in FY 1998 to bring lower maintenance costs and higher reliability with the overall goal of lowering the complexity of maintenance and response on the mountain. This telescope, in combination with the mosaic CCD offers a powerful new capability to the community.
Sometime in the next few months, we will ask the community for proposals to restore operation of the 1.3-telescope.
IV. NATIONAL SOLAR OBSERVATORY
A. Major Projects
1. Global Oscillation Network Group
The Global Oscillation Network Group (GONG) is an international project conducting a detailed study of the internal structure and dynamics of the closest star by measuring resonating waves that propagate throughout the solar interior. To overcome the limitations imposed by the day-night cycle at a single observatory, GONG has developed and deployed a six-station network of extremely sensitive and stable solar velocity mappers located around the Earth to obtain nearly continuous observations of the "five-minute" pressure oscillations. To accomplish its objectives, GONG has also established a distributed data reduction and analysis system to facilitate the coordinated analysis of these data. The primary data analysis is being carried out by a half-dozen or so scientific teams, each focusing on a few specific categories of problems. Membership in these teams is open to all qualified researchers.
The network commenced observing in October 1995, and the performance and reliability are excellent, with an equipment downtime of less than 2%. The scientific duty cycle routinely exceeds 90% and the daily sidelobes are virtually invisible. Routine servicing of the field stations has proceeded since the deployment according to plan, with the intention of assuring satisfactory operation over an eleven-year solar cycle. Development of engineering data-analysis software is continuing to facilitate the review and analysis of the functioning of the remote instruments, including fault diagnosis and long-term trend analysis.
27 Sixteen months of data have been processed by the project's data management group and have been made available to the research community for scientific analysis. A number of improvements have been made in the data reduction processes and a planned reprocessing of earlier data has begun.
The results to date demonstrate that an eleven-year data run, combined with a smaller camera pixel size, can produce very significant payoffs in our knowledge of the Sun, at a relatively small cost compared to the overall investment in the program. Accordingly, it is the advice of the GONG Scientific Advisory Committee that the project should continue the observing run for an eleven-year solar cycle and pursue the installation of higher- resolution detectors in the instruments on a three-year timescale, to catch the rising slope to the next solar maximum.
The GONG group has explored the feasibility of retrofitting a higher-resolution, square- pixel camera to the existing observing stations. At least one suitable 1024 x 1024 camera model has been identified that has excellent characteristics. This camera could be installed with the existing optical and telescope control systems. A seeing-effects study indicates that the current optics and the image sampling rate are satisfactory for the larger format system. This new detector will provide spatial resolution comparable to the optical system resolution, thus eliminating the spatial aliasing in the current system, as well as overcoming some inherent problems with the current rectangular pixels. Increasing the detector scale would provide significantly improved helioseismic resolution in the near-surface regions that are the home of the intense magnetic fields that seem to cause many of the more dramatic aspects of solar activity, extend all aspects of "local helioseismology" dramatically, and enable many non-helioseismic, diachronic solar measurements.
The project will continue this new-camera effort with the development of a proof-of- concept breadboard instrument during FY 1998. A proposal for funding the new camera system will be presented to the NSF. a. Recent Accomplishments
Operation of the network and activities with the host sites Software developed for engineering analysis of instrument functions Routine operation of the prototype instrument Routine preventative and emergency service of the field stations Continued development of modifications to the current system Reduction and delivery of network data to the community Developed data reduction and distribution of software enhancements Coordination of science team research efforts • Completion of the feasibility study for continued observations for a full 11-year solar cycle and upgrading the detectors b. Specific FY 1998 Tasks
• Operate the network and coordinate activities with the host sites • Continue software development for analysis of instrument functions » Continue routine operation of the prototype instrument
28 Continue routine preventative and emergency service of the field stations Reduce network data and deliver it to the community Continue development of data management software enhancements Coordinate and facilitate science team research efforts Develop proof-of-concept high-resolution breadboard instrument
Table 6
Anticipated Long-term Funding Requirements (in FY 1998 dollars)
Fiscal Year 1998 1999 2000 2001 2002 Base Budget 1,850 1,850 1,850 2,000 2,000 New Cameras 402 835 574 Annual Total 2,252 2,685 2,424 2,000 2,000
2. RISE/PSPT Program
Status The Italian PSPT telescope was deployed and now generates daily solar precision photometric data. A letter agreement with NOAA and HAO for deploying a second PSPT on Mauna Loa is being developed, and we expect to complete the deployment of the Mauna Loa and NSO/SP instruments in FY 1998. Routine operation of the photometric network should begin by the end of FY 1998.
These instruments will allow, for the first time, full-disk photometric measurements of the differential surface brightness of the Sun with an accuracy which is comparable to the precision of absolute bolometric measurements from space. To minimize NSO/NOAO operation expenses, our partner institutions (the Osservatorio Astronomico di Roma and the High Altitude Observatory) will operate two of the facilities. The third site at NSO/SP must be operated by NSO.
The PSPT operations have been descoped from the original 1992 plan. Nevertheless, with the proposed configuration, we will achieve daily measurements of solar photometric variability. Occasional higher cadence observations will be possible (for example to support space experiments or brief periods of exceptional solar activity) depending on the availability of support from our partner institutions. In this configuration we expect to be able to satisfy the data needs of up to 10 research groups, but much of the higher level data processing beyond the lowest level instrument calibration will be the responsibility of our scientific collaborators. A small operation at NSO/SP, consisting of a postdoc and the instrument specialist, will be responsible for maintaining all of the instruments and performing low-level quality assurance and calibration of the daily data. NSO scientists H. Lin and J.R. Kuhn will have overall responsibility for the scientific performance of the PSPT network.
29 FY 1998 Capital Budget
Completion of M. Loa and NSO/SP PSPT Telescope $180K
Operations Budget (per year):
M. Loa Operations Contribution 5K Travel (OAR and M. Loa) 5K Data/medium costs 7K Instrument Specialist + NSO/SP labor pool 75K Postdoc 45K Telescope network Hardware Maintenance 15K
Total NSO/SP site and network maintenance $152K/year
3. FY 1998 Program Plan Contribution for CLEAR Study
The technical and budgetary feasibility study of a design for a large solar telescope, the Coronagraphic and Low Emissivity Astronomical Reflector (CLEAR), is nearing completion. This 4-m aperture solar telescope aims at doing very high angular resolution observations of the Sun at all visible and infrared wavelengths transmitted by the earth's atmosphere. Its design will allow accurate polarimetry in solar spectral lines and continuum radiation. It will include adaptive optics initially designed for 1.6 microns. Care is taken to minimize scattered light to the extent that coronal observations become possible. The cost model will consider various options, including a descoping in size/aperture, relaxed requirements on scattered light, and several different sites. We expect to finish the report on the feasibility study in FY 1998.
CLEAR was initially planned to go to an existing NSO site. However, the first results of the site survey now underway show that, at least where high angular resolution is concerned, better sites do exist. The survey strongly confirms earlier indications that lake sites offer superior conditions for good seeing over long durations. We intend to continue this survey, extending it to several lake sites in the southwest US. As a result we expect to understand better the conditions needed for best seeing, leading ultimately to a recommendation for the telescope siting. It may turn out, of course, that it will be impossible to identify a site on which all conditions for solar observations (good seeing, IR transparency, low cloud cover, and coronagraphic skies) are simultaneously satisfied. In that case the scientific goals of the large facility must drive the site selection. Depending on the outcome of such site selection procedures, several options will exist concerning the location of most of the NSO operations. Transfer of these to the flagship site with concomitant installation of robotic operations at other sites is one possibility; on the other hand if the flagship facility is located at an extremely remote site, then the most viable option may be retention of some combination of the current facilities with largely remote operation of the flagship facility. There are obviously many options that lie between these two extreme cases.
FY 1998 will see extensive testing of telescope seeing and dust control measures using the 1/7 scale mock-up now mounted on the Sacramento Peak large 28 foot spar.
30 CLEAR is one of the options for the large future "Flagship Telescope" for solar physics. The last AURA Observatory Visiting Committee strongly endorsed the NSO/NOAO plans for such a telescope. As a result of this strong endorsement the NSO scientific staff is now intensely engaged in various aspects of the Flagship Telescope study, all aimed at developing a proposal for its construction which, at intermediate stages, will be presented to and reviewed by two major National Academy committees, the current one on groundbased solar astronomy (the Parker Committee) and the decadal study which is expected to start in FY 1998. These activities are expected to sharpen the science focus for the large telescope and broaden community participation and consensus.
The CLEAR resources carried forward from FY 1997 should suffice to complete the feasibility study and to fund the modest seeing site survey now underway. Therefore no new FY 1998 resources are currently assigned to this feasibility study.
B. Instrumentation Program
Tables 7 and 8 summarize the NSO instrumentation program.
Table 7
NSO/Sacramento Peak FY 1998 Instrumentation Projects
Non-Pavroll ($K) Project Priority Payroll (MM) NSF USAF Adaptive Optics 1 37 31 TBD Detector Upgrades 2 11 24 Spectroheliograph CCD 3 6 15 CLEAR Mock-Up 4 _ Total 54 zs TBD
Table 8
NSO/Kitt Peak FY 1998 Instrumentation Projects
Non-Pavroll ($K) Project Priority Payroll (MM) NSF USAF Near IR Magnetograph 1 4 7 KPVT Upgrade 2 20 25 IR Array & Controller 3 10 60 McMath Piece Control 4 9 KPVT Post-Focus Upgrades 5 11 30 Image Quality Improvement 6 1 2 Refurbish CSIRO Filter 7 2 2 Total 52 2£ M
Total All NSO 111 166
31 1. NSO/Sacramento Peak
Adaptive Optics Two years ago the Sacramento Peak image quality improvement program was restructured in a major way. In the new program, a step-by-step approach is being followed, which will lead in 3 years to a full-up adaptive optics system in which atmospheric wavefront distortions at the Sac Peak Vacuum Tower Telescopes will be corrected up to 20 Zernike terms. This new program was designed to produce increasingly better imaging as it progresses, and this improved image quality will be used for new science programs during the course of the three-year program. The development effort will also allow staff to learn about the technology involved gradually.
Milestones and Status
• Improve Telescope Optics (Window T-Control, Mirror) DONE
• MARK II Correlation Tracker (CT using commercial components) DONE
• Full-Up Tip-Tilt System (with German KIS collaboration) DONE
• Image Selection Observations Using CT & Tip-Tilt DONE
• Explore Wave-Front Sensor (WFS) Options (LCD, S- H) DONE
• Demonstrate Solar Shack-Hartmann WFS Sensor DONE
• Build & Demonstrate Active Optics Using Commercial Components & Solar WFS DONE
• Combine Active Optics & Image Selection (longer exposure time, larger isoplanatic patch, more often) FY 1998
• Speed Up System Using Parallel Processing and USAF/SOR or Commercial Reconstructor Aiming at 20 Zernike Adaptive Optics System FY 1999
As intermediate results of this systematic approach to solar adaptive optics we have achieved: (1) a rapid solar tip-tilt system (or 2 Zernike adaptive optics system), (2) the best (diffraction-limited) images of the Sun ever obtained (1/8 arcsec resolution) using image selection techniques, and (3) full correction of the residual aberrations of the VTT by means of active optics. The next step, image selection using the aberration-free telescope, is expected to lead to even better quality imaging (more frequently, larger isoplanatic patch and longer exposure times).
The budget listed above is by itself inadequate to accomplish the goal of the 20 Zernike system. This project benefits very much from the synergism created by the partnership with USAF/Phillips Lab solar group at Sac Peak. In addition to contributing payroll and non- payroll resources (the Xynetics 97-element adaptive mirror procurement was only possible by their contribution), this collaboration provides an important link to the Phillips Lab
32 Starfire Optical Range expertise in adaptive optics. In addition to benefiting from USAF/PL collaborations, this project has the highest priority for the assignment of FY 1997 year-end resources.
Benefits of the development of this solar adaptive optics system extend well beyond the Sac Peak VTT. It provides the know-how essential for the implementation of a large- aperture solar telescope. The prime requirement for that 2- to 4-m telescope is diffraction- limited resolution. The availability of a functioning solar adaptive optics system is crucial for the successful pursuit of the funding for such a telescope (PI: Rimmele; Radick, USAF/PL).
Detector Upgrades Because of the rapid development of array detectors, all NSO telescopes/instruments require continuous upgrading of their Visible and IR detectors to remain state-of-the-art. At Sac Peak, this implies the implementation of blue sensitive CCDs and the further coupling of the IR HgCdTe NICMOS detector and the Xedar fast 2K x 2K CCD (developed under the RISE/PSPT program) to the various telescopes/instruments (PI: Hegwer).
Spectroheliograph CCD The daily Sac Peak spectroheliograph images are among the data most used by the solar community. These images are still obtained with photographic detectors, which seriously inhibit their quality and usability. The addition of a 2048 CCD array and associated optics adjustments will result in fully digital imaging (PI: Varsik).
CLEAR Mock-Up A 1/7 scale mock-up of the CLEAR telescope mounted on the JESF 28 feet spar will be used to explore the conditions needed to control seeing and dust in an open telescope under solar illumination conditions. Thermal control of the primary mirror and prime focus heat stop and airflow are the variable instrumental parameters; micro-thermal and dust sensors are the evaluation tools. As is the case for solar adaptive optics, the results of this project will be essential for any future windowless solar telescopes, not just CLEAR. Funding for this project will come from FY 1997 CLEAR carry-over funds (Pis: Beckers and Varsik).
2. NSO/KittPeak
Near Infrared Magnetograph, NIM-2 Completion of the NIM-2 instrument (an imaging vector magnetograph using a Fabry-Perot and 256x256 InSb detector in the 1.565 micron line) is expected early in FY 1998. Weather and unexpected instrumentation problems caused a delay of the commissioning, expected initially in FY 1997 (PI: Rabin).
KPVT Upgrade FY 1998 is the last year in the program to upgrade the KP Vacuum Telescope Control System. Completion, initially planned for FY 1997, is now anticipated by the end of Calendar Year 1997. We refer to the FY 1997 program plan for a detailed description (PI: Harvey).
IR Array & Controller FY 1997 year end funds will be transferred to NOAO-ETS to construct and deliver an IR ALADDIN array controller and its 1024 x 1024 InSb array to the McMath-Pierce telescope
33 by late FY 1998. It will take full advantage of NOAO's major investment in the ALADDIN array development project.
This infrared camera will make the McMath-Pierce the most powerful infrared solar telescope in existence. It will have 16 times more pixels than the 256 x 256 NICMOS arrays used elsewhere and it will make use of the fact that the McMath-Pierce facility is the only large windowless solar telescope, thus giving it unique access to the important spectral region between 2.5 and 5 microns. The lower dark current, lower read-out-noise, higher quantum efficiency, and increased immunity from electronic interference will make it superior to the 256 x 256 Amber Engineering camera used in recent years. The ALADDIN camera will be used with the NIM-2 magnetograph as well in other imaging and spectroscopic applications. No single instrumentation event at NSO/KP in recent years will have a larger impact on its capabilities than this one (PI: Rabin).
McMath-Pierce Control With the completion of the KPVT TCS upgrade, attention will be directed to the McMath- Pierce telescope control system. Priority will go to the implementation of a modern guiding system for the three telescopes that are part of this facility. There is currently no permanent, general guiding system on this telescope (PI: Wagner).
KPVT Post-Focus Upgrades This project is also referred to as the KPVT Data Systems Upgrade. Included in it will be the continued improvement of the He 1083 nm Polarization Modulator and the High Spatial Resolution Spectromagnetograph. The budget for this project comes from funding generated by our NASA/GSFC partners at NSO/KP (PI Jones/NASA/GSFC).
Image Quality Improvement This year will see the beginning of the transfer of the image quality techniques developed at NSO/SP to the Kitt Peak solar facilities (PI: Keller).
Refurbish CSIRO Filter Recently NSO acquired a number of H-alpha Lyot filters from the discontinued solar physics program at CSIRO in Australia. These filters will be used as instrumental components at NSO's existing telescopes as well as at SOLIS. In FY 1998 we will start refurbishing these filters, supplying them, for example, with modern temperature controllers (PI: Harvey).
The instrument and telescope combinations available at the NSO are listed in Table 9.
34 Table 9 Telescopes/Instruments Available to the Community Vacuum Tower Telescope (SP) Echelle Spectrograph Universal Spectrograph Horizontal Spectrograph Universal Birefringent Filter Fabry-Perot Filter System Advanced Stokes Polarimeter Slit-Jaw Camera System Correlation Tracker Branch Feed Camera System Horizontal and Vertical Optical Benches for visitor equipment Optical Test Room Evans Solar Facility (SP) 40-cm Coronagraphs (2) 30-cm Coelostat 40-cm Telescope Littrow Spectrograph Universal Spectrograph Spectroheliograph Coronal Photometer Dual Camera System Hilltop Dome Facility (SP) Ha Flare Monitor White-Light Telescope 20-cm Full-Limb Coronagraph White-Light Flare-Patrol Telescope (Mk II) Sunspot Telescope Fabry-Perot Etalon Vector Magnetograph Mirror-Objective Coronagraph (5 cm) Mirror-Objective Coronagraph (15 cm) McMath-Pierce Solar Telescope Facility (KP) 160-cm Main Unobstructed Telescope 76-cm East Auxiliary Telescope 76-cm West Auxiliary Telescope Vertical Spectrograph: IR and visible gratings Infrared Imager Near Infrared Magnetograph CCD cameras 1-m Fourier Transform Spectrometer 3 semi-permanent observing stations for visitor equipment Vacuum Telescope (KP) Spectromagnetograph ' High-1 Helioseismograph 1083-nm Video Filtergraph Razdow (KP) Ha patrol instrument
35 THE SCIENTIFIC STAFF
The roles, responsibilities, and terms and conditions of employment of the scientific staff were described in the renewal proposal. We have adopted the philosophy that the size of the scientific staff should be determined by functional responsibilities. Over the past several years, however, the functional responsibilities of the staff have increased while its size has declined (by about 30 percent over the past decade). The increased responsibilities have come about because of new program requirements: 1) support of US involvement with, and US use of, the Gemini telescopes; 2) the development of consortium telescope projects (WIYN and SOAR); 3) leadership of the GONG project; 4) responsibility for several major instrumentation projects for Gemini; and soon, 5) the construction of SOLIS and SOAR; and 6) access to the MMT and HET.
Because NOAO believes that direct involvement of scientific staff in defining requirements for, and evaluating the implementation of, major new projects is crucial to the success of those projects, each initiative has a project scientist assigned to it. Because none of the initiatives listed above has brought with it support for the scientific staff, the staff responsibilities have grown to the point that there is very little time for research. According to AURA policy, tenured and tenure track staff should have 50 percent of their time available for research, and scientists should be able to devote about 25 percent of their time to research. It is uniform throughout the organization that the staff estimates that they are spending only about 15 percent of their time on research. Attempts to date to ameliorate this situation, including reducing the workload by reducing services offered to users and by re-organizing the way work is carried out, have led to greater efficiencies in some parts of the program, but these efficiencies have been insufficient to compensate for the workload increases associated with the new programs that are being undertaken.
The staff has responded to this situation by taking sabbaticals, thereby increasing the burdens on those who are not on sabbatical. The problem of understaffing, which is a consequence of the budgetary stringency under which we operate, has been further aggravated by our failure to fill some of the vacant positions that do exist. CTIO and KPNO each had two vacant positions this year, and each observatory filled only one. The problem is that NOAO requires staff who have some capability with, or willingness to learn about, building, commissioning, and maintaining very sophisticated instrumentation. Unfortunately, few astronomers coming out of US graduate programs have these skills, and the competition for such individuals is intense.
We also noted in last year's program plan that scientific staff salaries seriously lag (by about 15 percent) salaries computed on an 11-month basis at comparable institutions. We are currently collecting new comparison data, but given the meager salary increases that we provided last year, it is unlikely that we have improved our competitive position.
Key staff changes this year include the recruitment of Hao-Sheng Lin to NSO/SP, Abi Saha to Kitt Peak, and Bob Blum to CTIO. Tom Kinman has become an emeritus astronomer. Dave Silva left KPNO to take a position with the VLT project at ESO in Garching. One position remains vacant at each of KPNO and CTIO, and a new recruitment will be undertaken during the next academic year.
Appendix 3 lists the members of the scientific staff research plans for the coming year, and their functional responsibilities.
36 VI. EDUCATIONAL OUTREACH
Staffing of the NOAO Educational Outreach Program will remain stable with a full-time Education Officer, a half-time Program Coordinator funded by the Astronomical Society of the Pacific's Project ASTRO, and a less than half-time undergraduate student worker funded through the NASA Arizona Space Grant Consortium. In addition, funds recently made available through the NSF EHR Teacher Enhancement Program can be used to provide a quarter to half-time salary for an observing technician, whose services will be required to support the program.
Project ASTRO, which facilitates ongoing partnerships between astronomers and teachers in local schools and community organizations, expanded to Tucson in the fall of 1996 with NOAO as the lead institution. Twenty-three pairs of astronomers and teachers were matched in 1996/97 and a similar number of partnerships are being formed for 1997/98. This will bring the total number of Project ASTRO-Tucson participants who have received training, materials, and support to approximately one hundred by the end of FY 1998.
"The Use of Astronomy in Research Based Science Education" is a four year Teacher Enhancement program that offers a research experience to middle and high school teachers during summer workshops at NOAO, and the extension of this experience to their classrooms during the academic year. This effort is funded through the NSF Directorate for Education and Human Resources. A pilot program involving twelve teachers from Tucson begins in the summer of 1997; in 1998 and each subsequent year, we will accept twenty-four teachers from around the nation.
A third program area of Educational Outreach at NOAO is that of Instructional Materials, and to date we have developed a small suite of informational and educational products such as brochures of classroom activities, a slide set and caption booklet, and informational pamphlets. We expect production of these materials to continue as resources allow, possibly supplemented with NASA IDEA Grant funds. The NOAO Outreach Advisory Board will continue with membership remaining at 15 local teachers. As vacancies occur on the original board of middle and high school teachers, they will be preferentially replaced with elementary teachers. It is our goal to broaden and diversify this advisory board, which has proven to be mutually beneficial to participants and NOAO.
VII. COMPUTER SERVICES
A. NOAO-Tucson
The computer facilities in the Tucson office complex serve several general needs for NOAO- Tucson: data reduction and analysis for the scientific staff and visitors, general computing for all staff members, infrastructure for dedicated computers and for PCs and workstations on staff members' desks, administrative computing, and IRAF development and support. Our distributed computing strategy for Tucson implements a combination of central, shared facilities (provided and maintained by Central Computer Services—CCS) and a variety of desktop facilities including workstations, PCs, and X-terminals (provided and maintained by the individual observatories or departments). Computing systems are networked and linked to the computers on Kitt Peak and to the worldwide Internet.
The central facilities maintained by CCS must provide an environment for data reduction and analysis of data taken at Kitt Peak by visitors and staff members. As the scientific workstation
37 revolution of the past decade has proceeded and powerful computers have appeared on almost every scientist's desk, it is no surprise that fewer visitors and staff members utilize the CCS facilities. Nevertheless, a significant number still use these facilities to reduce and analyze their data in Tucson, especially for the largest and most challenging datasets. Moreover, with the arrival of new instruments such as the 8K x 8K mosaic and the IK x IK IR arrays on Kitt Peak, again outstripping individual workstation capabilities, CCS needs to keep up by upgrading the central facilities devoted to data reduction and analysis. Thus, during FY 1998, we will add disk space and high capacity tape drives to the "visitor" machine Ursa and add disk space and a faster CPU card to the machine Gemini which hosts the Scientist Workstation Network. These upgrades should cost $20K.
An academic and scientific institution such as NOAO-Tucson must provide a set of computing services to its staff such as e-mail, document processing, scientific plotting packages, etc. These needs are met by providing sufficient servers and the necessary infrastructure to connect these servers to several hundred terminals, X-terminals, PCs, and workstations on staff members' desktops. Upgrading the infrastructure is ongoing as more and more computers are attached to the network, as more and more scientists and engineers need access to the computer facilities from their home computers, and as servers need to be updated and upgraded to handle the load of more and faster systems utilizing their services. During FY 1998, we plan to upgrade our "timesharing" machine, Orion, at a cost of $10K, and BigX, the host for our network of X-Terminals, at a cost of $17K. We will continue to upgrade the network infrastructure in the building with the goal of providing a 100 Mbps Fast Ethernet connection to every scientist's desk by the end of FY 1999. The FY 1998 portion of the cost will be $35K.
NOAO is firmly committed to distribute information and interact with our users through the World Wide Web over the Internet. Internal uses of the Web to increase efficiency and share information also abound. During FY 1998, a project to accept telescope proposals from scientists through the Web should reach fruition.
A staff of 5 FTE (3.5 from CCS, 1 from ETS, and 0.5 from KPNO Mountain Electronics) maintains approximately 150 Suns and other workstations, approximately 35 X-Terminals, and approximately 100 PC and Macintosh systems in downtown Tucson and on Kitt Peak.
B. KPNO-Kitt Peak
Computers on Kitt Peak serve three broad (but overlapping) functions: real-time control of the telescopes and instrumentation, data taking (including data reduction and initial analysis), and support for observing and operations of the Observatory. Continuing replacement and upgrading of these computers is required for three reasons: obsolescence, which implies high maintenance costs and lack of functionality (for example, the telescope control system at the 0.9-m telescope is over 15 years old); new technology and improved techniques (for example, the 8K x 8K mosaic imager being developed by the NOAO Instrumentation Group will result in nightly datasets of the order of 30 GB); and changes in standards and approaches (for example, the gradual adoption of Gemini software and standards at KPNO). Furthermore, we strive to provide scientific computing facilities in our domes for visiting astronomers that are comparable in speed and sophistication to those at their home institutions.
The various locations on Kitt Peak (including tenant facilities) are networked together by two fiber-optic rings which are equipped with electronics to emulate 10 Mbps Ethernets. Tenant facilities on the West Ridge are connected to the mountain network via copper connections.
38 The mountain network is connected to the network in the NOAO-Tucson building (and hence to the Internet) via a T-l line running at 1.5 Mbps. No changes in the network infrastructure are planned for FY 1998.
At the 4-m telescope, new instrumentation (new controllers for both IR arrays and CCDs) and new standards (the Gemini OCS, in particular) are slowly converging to mandate a future major revamping of the computer systems. In the short term, during FY 1998, incremental improvements are planned. These include replacing old disk drives that can no longer be maintained ($3K), replacing the current DAT drive with a DDS-2 unit ($1K), equipping the Sun named Khaki to accept data from the NOAO Mosaic Imager ($2K), continuing the project to eliminate CAMAC from the Cassegrain cage, tying dome functions controlled by the PLC (Programmable Logic Controller) into the TCS (Telescope Control System), replacing the leaky guider with a VME board embedded in the TCS computer system ($15K), and improving the GUI display programs used to control the TCS.
At the other telescopes, incremental improvements will take place in FY 1998 to improve reliability and maintainability. Old Exabyte 8200 drives will be replaced by Exabyte 8505 drives ($5K) and old HP DDS-1 DAT drives will be replaced by Seagate DDS-2 DAT drives ($6K). Disk drives older than five years will be replaced with newer, higher capacity drives ($4K). In specific cases: the leaky guider at the 2.1-m will be replaced by a VME board embedded in the TCS computer system ($10K); the Sun called Royal (used for IR data taking) at the 2.1-m will be upgraded to duplicate the similar Sun at the 4-m ($7K); a Fast Ethernet subnet will be installed at the 2.1-m ($3K); and the Sun named Taupe at the 0.9-m will be upgraded to host the NOAO Mosaic Imager ($9K). Spare peripherals and network cards will be purchased for Mountain Electronics ($4K).
The administrative facilities on Kitt Peak (supporting both KPNO and NSO) include computer systems for staff and visitors not scheduled at a telescope dome, the mountain-wide data archiving system ("Save the Bits"), and communications facilities that link the mountain network with NOAO-Tucson. During FY 1998, we plan to upgrade the Sun used for data archiving.
C. CTIO-Cerro Tololo
Data acquisition at CTIO's telescopes is supported by a network of Sun computers located in the various domes. The primary data acquisition machine at each telescope (currently a SPARCstation 10-41) is directly connected to the optical CCD (ARCON) and IR (Wildfire) controllers and is used for the collection, reduction, and initial analysis of the data delivered by these devices. These machines typically have 10-11 GB of disk storage and are equipped with both Exabyte and DAT tape drives. An ancillary machine is also available at the 4-m, 1.5-m, and 0.9-m domes. These machines are older VME bus-based computers and now serve as little more than an extra terminal for use when more than one observer is present. In FY 1997-98 we will purchase a dual processor UltraSPARC workstation to serve as the acquisition machine for optical data at the 4-m telescope at a cost of approximately $40K. This upgrade is necessary in order to adequately support the CCD mosaic imagers (BTC, in service now, and the NOAO mosaic scheduled for deployment in mid 1998). This machine will also be used to run the existing optical CCDs. The existing SPARC 10-41 will then be used exclusively for the acquisition of IR data. The old VME bus ancillary machine will then be retired. At the end of FY 1998 a similar upgrade and rearrangement is planned for the 1.5-m telescope, although in this case a cheaper (approximately $20K) UltraSPARC will suffice to run the optical detectors.
39 In addition to the machines distributed in the domes, two low-end SPARCStations and a number of PCs are located around the mountaintop and in the Tololo library in order to provide network access and limited data reduction capabilities for visitors without telescopes.
Two mid-level workstations and a number of PCs are used by the Cerro Tololo Support staff for data reduction and general computing. An additional SPARCstation 10-41 fully equipped for data acquisition with ARCON is located in the Cerro Tololo electronics laboratory. This machine is used for test and maintenance work on the optical CCD systems and is also available as a hot spare for the data acquisition computers.
Cerro Tololo is the host for an increasing number of tenants. The MACHO collaboration, the Swarthmore robotic telescope, and GONG all currently have machines connected to the mountaintop network. The 2MASS project and the consortium which has taken over operation of the 1-m telescope will be connecting during FY 1998.
The mountaintop machines are connected to one another via a conventional Ethernet, to the USA by a satellite link, and to La Serena by a microwave link (see the communications discussion below). At the end of FY 1996 a separate sub-net was established for all the computers at the 4-m telescope. This was necessary for operation of the BTC mosaic imager, which makes heavy use of the network. During FY 1997-98, this sub-net will be upgraded to 100 Mbps Ethernet and a similar subnet will be installed at the 1.5-m telescope for a total cost of approximately $20K.
There are two rather different telescope control systems in use on Cerro Tololo. The 4-m telescope is controlled by a VME bus-based processor running software based on the VxWorks operating system. During FY 1997 the software at the 1.5-m telescope is being upgraded to make it compatible with the 4-m system to the maximum possible extent. At both telescopes an associated low-end SPARCstation presents the telescope operator with a graphical user interface derived from that in use at KPNO. At the 4-m telescope, the complexity of this GUI has increased with the introduction of adaptive optics and of the tip-tilt secondary. Further demands will be made by the need to interface to the Hydra multi-object spectrograph and the NOAO mosaic imager. Consequently, during FY 1998 a mid-level SPARCstation will be purchased to serve as the operator's console at a cost of approximately $5K. A major project during FY 1998 will be the replacement of the servo system at the 4-m telescope with a modern commercial controller; however the VME bus hardware has already been upgraded in anticipation of this.
The 0.9-m telescopes are operated by an aging and obsolete commercial TCS, which is a serious maintenance headache. We are currently investigating possible commercial replacements for this system in collaboration with the consortium which will take over operation of the 1-m telescope. Expected costs are in the region of approximately $50K; however, at present funding levels it is not clear whether CTIO will be able to purchase such a system for the 0.9-m during FY 1998.
D. CTIO Communications
The networks in La Serena and on Cerro Tololo are joined via a commercial microwave link with backup and maintenance provided by the contractor. At present one of the four available El Channels (2Mbps) is used for network connections and another for voice lines. During FY
40 1998, we plan to install ATM routers in La Serenaand on Cerro Tololo and begin to use ATM on the link between the two sites. The computer networks in both locations will be connected to the switches along with the existing telephone plants. ISDN boards will be installed in both telephone plants along with ATM trunk line equipment. This will immediately increase the maximum speed of data transfer between La Serena and Cerro Tololo from the current 2 Mbps (El) to 8 Mbps (E2) at no additional recurring cost. It will also permit videoconferencing between CTIO and any ISDN-compatible location worldwide, once ISDN service charges within Chile fall to an affordable level. The total cost of this upgrade is around $70K.
The systemconnectivity to the outside world is currently throttled by a 56Kbps satellite link to the US, supplied by NASA. A higher speed connection is a prerequisite for remote/queue scheduled observing and will be essential before the turn of the century. Fortunately, a transition to the use of terrestrial fiber links for telecommunications is taking place in Chile. Fiber connections already exist between Santiago and La Serena and to the USA via Argentina and Brazil. Direct connections from Chile to the US west coast are being installed. As a result it is likely that a higher speed connection between CTIO and the US will be commercially available, at affordable cost, within the next few years. The ATM switch in La Serena can be connected directly to such a terrestrial fiber optic link to provide a high bandwidth connection to the US Internet. However, it must be recognized that rental and traffic costs for this connection will need to be paid from CTIO's budget, while the present satellite connection is paid for by NASA.
At the end of FY 1996 a 64Kbps terrestrial link between La Serena and Cerro Calan Observatory in Santiago (and thence to the Chilean Internet) was implemented in partnership with Universidad de Chile. This allows for more efficient communication between CTIO and the Chilean astronomical community and the other observatories in Chile. It also serves as a backup Internet connection.
E. NSO/Sacramento Peak
The computer facilities at NSO/SP are in four areas; Main Lab (ML), Evans Solar Facility (ESF), Hill Top (HT), and the Vacuum Tower Telescope (VTT). The ESF, HT, and VTT computer systems are mainly used for telescope control and data collection with limited data analysis. The ML facility is used for data reduction, analysis, and general computing for local staff and visitors.
1. Main Lab Plan for FY 1998
• Upgrade the NSO/SP network backbone to 100Base (100 Mbps) Ethernet with the capability to link telescope sites with an ATM or Gigabit Ethernet backbone in the future. The first phase would allow all servers and each telescope building to be connected at 100Base Ethernet. Most workstations would continue to use lOBase (10 Mbps) Ethernet but would allow workstations to move to 100Base Ethernet if necessary. This upgrade would also allow our old Galactica switch to be used in our network but would give us a quick replacement path if it should die. This project will require the following equipment; total cost $25K:
° One 12 port 10/100Base Ethernet switch at the ML to connect our servers to 100BASE speed.
41 ° Two 24 port lOBase with one 100Base port Ethernet switch at the ML to replace the aging Galactica switch.
° Three 12 port lOBase with one 100Base port Ethernet switch at each of the telescope sites.
« Upgrade aging workstations, NFS server, and computer servers. NSO/SP has many workstations that are over six years old, are very slow, and are becoming unproductive. These old units need to be replaced as soon as possible.
0 Upgrade 7 SS1, IPC, SS2 workstations to SS5 workstations: $20K
° Upgrade 1 NFS server to an Ultra 1 1 x 200MHz cpu plus one 24GB multi pack disk unit: $17K
° Upgrade 2 SS 10 computer servers to one Ultra2 2 x 200MHz host: $25K
• Purchase software that will centralize system administration of hardware and software on the NSO/SP LAN. With the increase of local staff for new projects comes the increase of new hardware and software on the network. To continue to administer more hardware and software on our network with the same number of people, software is needed to allow the one system administrator to manage the network from a centralized remote location: $5K
• Purchase a Windows NT server with X Windows software to allow Windows, Windows 95, and Windows NT software to run on a Windows NT server and be displayed on UNIX workstations, X-terminal, or PCs: $10K
2. Telescope Computers
The NSO/SP Telescope Computers plan for FY 1998 is as follows:
« 2 xDLT 7000 (35GB) tape drives: $12K
• Purchase 100 DLT tapes: $10K
• HP Laser Printer for the VTT to replace an aging SPARC printer: $2.5K
• Upgrade SS10 to a dual Ultra: $20K
F. NSO/Tucson
The development of the,NSO Digital Library is well underway, motivated by the heavy demand for data from the NSO Tucson anonymous FTP archive. The currently available data products consist of the daily KPVT images, FTS atlases, and FTS data archives. During the previous year FTP accesses exceeded 34,000 file acquisitions, while WWW interrogations for the KPVT web pages exceeded 41,000 hits. The NSO Digital Library is now moving all data to three CD-
42 ROM jukeboxes with a total capacity of 300 discs. Currently, 55 CDs (35 GB) of data are on line for FTP access, and a prototype Internet user interface and search tool has been installed. A CCD digitizer has been installed at NSO/Sac Peak to migrate the daily H-alpha and Ca K images from film to disk. Funding has been obtained from the NSF Space Weather Program and NASA to support the NSO Digital Library development. In the next year we expect to complete the user interface development, purchase a multi CD-ROM writer, substantially increase the amount of KPVT data in the Library, and begin migration of the daily NSO/SP spectroheliograms.
Administrative and support staff computers used at NSO/Tucson will continue to be Macintosh based. The Macintosh platform is fully integrated into NSO operations. It is used not only for administrative tasks, but observing support at the mountain. NTM is a fully Mac-based instrument, as is NTM2, the new Fabry-Perot based imaging magnetograph. In addition, LabView is being used for quick instrument development and in support of the seeing project at the McMath-Pierce. We will support the standard Microsoft software suite adopted by NOAO (Word, Excel, PowerPoint, and Access) with the exception of Access. Access is not a cross platform database. We have adopted FileMaker as our database of choice, because it is a more capable database and is supported in both Windows and Mac environments. Since most of our Macs run soft windows, we can run the few applications, such as CHAOS, that are not Mac- based. In addition, we have had requests by staff to install MAE (Apple's Macintosh Application Environment) on their Sun workstations. This would allow them to run the same applications used by the administration and support staff. We plan on purchasing a couple of Mac-based laptops to be checked out by NSO staff during travel. We have upgraded two of our current Mac systems to RISC PowerPC architecture to be used by the programming staff for development.
NSO is keeping pace with new developments in Sun workstations. Recent upgrades have typically been from Sun Sparc 20 to Sun Ultra 2 machines. The transition from SunOS 4 to Solaris is now underway.
G. NSO/KittPeak
Computers at the NSO facilities on Kitt Peak serve similar, yet very custom requirements. The Telescope Control Program (TCP) systems in the KPVT work on an auxiliary image, as opposed to the McMath-Pierce, which controls the main image. The KPVT control system is designed for smooth image scanning, the McMath-Pierce for stationary operation. Yet the McMath-Pierce is now being used for scanning in the IR regions not available to the KPVT. Both telescopes are in need of upgrades. The project to upgrade away from a PDP- 11/FORTH/CAMAC system as the telescope control system at the KPVT is currently in the early implementation stages with ETS. This upgrade will bring the TCP systems in line with upgraded systems used on other NOAO telescopes.
The KPVT data acquisition and reduction computers are in relatively good shape.
The FTS has recently been upgraded with a new A/D converter using commercial audio CD technology. This upgrade will greatly improve the maintainability of the system, and has allowed the use of sophisticated filtering software running on a newly purchased Pentium- based PC.
43 The McMath-Pierce has three major areas of computer usage. First is the TCP, which is still based on the PDP-11/FORTH/CAMAC model that has long been supplanted by more modern systems at most other NOAO facilities. A preliminary proposal has been written to upgrade this system. It is premature to specify any computer hardware at this time, except to say that it would most likely conform to hardware used at the new telescopes on Kitt Peak.
The Stellar-Spectrograph is the application that most closely reflects the systems used at other sites on Kitt Peak. With the 800 x 800 TI-4 CCD, we anticipate no changes to Pacifico (the ICE Sun) used for SSG observations.
The third system that is badly outdated is the grating control system for the main spectrograph. This is also a PDP-11 based system, still using 9-track tape. This is an area that needs immediate attention, because of the disappearance of 9-track capability. This is being addressed in the proposal to upgrade the McMath-Pierce TCP. The plan is to upgrade the spectrograph control to a VME-based system in parallel with the KPVT spectrograph upgrade. Hardware has already been purchased, and the plan is in the early stages of implementation.
H„ IRAF
IRAF is the Image Reduction and Analysis Facility developed and distributed by NOAO and used to process and analyze data from NOAO and other astronomical observatories. IRAF is estimated to be used by over 5000 astronomers at over 1500 sites throughout the world. IRAF is heavily used within both the groundbased and NASA space astrophysics communities and is freely available via the Internet from sites in the US, England, Germany, Japan, and India.
IRAF is a portable software system for astronomical data acquisition, reduction, and analysis. It provides tools for general image processing, graphics, and visualization of small or large datasets, as well as instrument specific data reduction software for a wide range of astronomical instruments, including all NOAO instrumentation. Additionally, optional IRAF packages developed by sources outside NOAO are available to provide data reduction support for non- NOAO instruments such as those on the Hubble Space Telescope.
NOAO receives support from NASA in the form of grants and subcontracts to help fund collaborations with NASA sites, making IRAF suitable for the needs of the wider astronomical community. This funding pays mainly for general system software improvements that benefit both the NOAO and NASA communities.
IRAF is one of NOAO's most scientifically productive and visible "facilities," with over 25% of all groundbased observational papers in the major astronomical journals relying on IRAF to some degree. It also serves as the basis for CCD data acquisition and quick-look assessment at NOAO telescopes, and as the image analysis package for most NOAO staff science.
1. Major Developments in IRAF Projects During FY 1997
• Open IRAF: The main goal of this project is to support NASA projects (HST, AXAF) that are developing or releasing software based on the Open IRAF prototypes. For FY 1997 in particular, the STSDAS release in July 1997 is needed to support STIS and NICMOS reductions, and NOAO IRAF support for this release will be completed in June.
44 Science Applications: New astrometry tasks have been incorporated into the general IMAGES package, including the ability to perform complete astrometric solutions. Progress in collaboration with the radio community has been made toward a revised coordinate standard for FITS. A user-contributed infrared package has been added to the available software collection. A vastly improved version of the image display task, XEVITOOL, has been released.
CCD Mosaic Support: System work has concentrated on the data capture agent for data acquisition and on the development of the underlying technology (message bus, distributed shared objects) on which the subsequent data handling system and real-time display and analysis tools will be based.
• Gemini Support: A set of generalized image header definitions has been developed to unify NOAO and Gemini data. A new image file structure that will serve Gemini and is consistent with the FITS standard is now in use with the CCD Mosaic.
• Updated Platform Support: All XI1 IRAF products have been released for all supported IRAF platforms.
• Version 2.11: A preliminary release of Version 2.11 was distributed within NOAO and to selected IRAF sites, including STScI. The final version will be released in June.
2. Major Efforts in IRAF During FY 1998
• Data Handling System for the CCD Mosaic 0 Data capture agent ° Data reduction agent ° Automated pipeline data reductions ° Real-time display for analysis of data during readout
• Open IRAF to improve integration of IRAF and non-IRAF software via 0 Multi-language programming support (e.g., C, FORTRAN) 0 Host callable IRAF libraries ° Distributed applications and network access to IRAF tasks ° Direct access to standard data formats (FITS, PC image formats)
• Plug-In Extensible Image Server ° Powerful stand-alone image browser ° Plug-in capability for dynamically extending browser 0 Message bus and distributed object support ° Implement prototype plug-in extensible image server
45 New science applications/upgrades ° Astrometry package, world coordinate system support ° Data reduction support for CCD mosaics ° Error vector support ° Pixel mask support for image processing ° Infrared data reductions
Data archive support ° Data archiving and data distribution system ° Network access to archival data
• Support for Gemini and NOAO observers ° NOAO/Gemini unified image headers 0 Support for quick-look interaction with data at the telescope ° Polaris transparency monitor to gauge photometric conditions
• Updated platform support (e.g., PCs running Linux, FreeBSD, and Solaris; Macintosh systems running MkLinux; upgrade all supported IRAF platforms).
In addition, support and other interaction with users around the world will continue to occupy about 25% of the IRAF group's effort.
Vffl. FACILITIES MAINTENANCE
A. Cerro Tololo
The Administrative-Operations Program Plan involves the upgrade, improvement, and development of the Observatory's critical infrastructures; such attention to observatory infrastructure was highlighted as a top priority for groundbased astronomy in the most recent NAS decadal review (the "Bahcall" report).
The following topics are detailed below: In$lJSK LRP(Syr) PP(FY 1998) 1. Fire Prevention and Fire Fighting 40 40 2. Renovation of the Vehicle Fleet 50 50 3. Improvement of the Main Access Road 300 50 4. Repainting of the 4-m Blanco Telescope 20 20 5. Cerro Tololo Power House 25 25 6. Water System - Cerro Tololo Pipeline 25 25 7. Control of Light Pollution 22 22
8. Enclosure for the TELOPS building Cable Car 19 -
9. Bulldozer for Cerro Tololo 200 - Total 701 232
46 /. Fire Prevention and Fire Fighting During the last two years, we have been able successfully to install, and bring into operation, an early fire detection and control at CTIO. The fire detection system is currently in full operation at the 4-m Blanco Telescope on Cerro Tololo. However, in order to carry this project to completion, it will be necessary to purchase and install an automatic fire fighting station to cover the more vulnerable areas of the telescope enclosure. Therefore, we plan to spend US$40K to purchase of a "Protection Chemetron Fire System FM200" fire fighting station or a similar substitute.
2. Renovation ofthe Vehicle Fleet Funds will also be spent to modernize the aging CTIO vehicle fleet and further cut expenses on maintenance and repair costs.
Recent Chilean legislation passed a law forbidding the use of public roads by trucks with more than 20 years of use. The aim is to exercise a more rigid control over revamped vehicle emission norms in Chile.
Our only two trucks with a load capability in excess of 8 tons are 29 years old! In addition, it is becoming increasingly difficult to find spares to keep them in reasonable operating shape, as their fabrication was long ago discontinued. These trucks are currently used in the maintenance of the 23-mile unpaved road to the Observatory, for hauling water to the Cerro Pachon installations where the Gemini Project is currently under development, and a score of other tasks that are essential to the operation of the Observatory. The current estimated cost of a truck of the noted capacity is in the range of $95K.
Passenger transportation vehicles are necessary to provide safe transportation for visitors, scientists, technical and operations staff, as well as for instruments that are moved between La Serena and the Observatory sites.
A minimum of $50K is required to continue with our renovation program, which aims to provide a modern, safe and low-maintenance fleet of vehicles.
3. Improvement ofthe Main Access Road Despite the previous funding effort that has been funneled towards the Observatory access road, this crucial area of our operations still presents significant safety hazards. The road is mostly unpaved, and there are some sharp gradients and curves, with less than 5% of the estimated total desirable guardrail protection installed. For example, a recent accident involved a CTIO worker and two foreign press correspondents, whose vehicle skidded off the Observatory road on a curve, and rolled over down a steep embankment.
In order to continue with the CTIO road improvement project, we require funds in a similar amount to those requested during previous fiscal LRP exercises, i.e., $300K—the amount necessary for the purchasing and installation of additional guardrail to protect a length of 10.2 km of the road. Since such a large sum is not available, we will continue to make gradual progress as resources permit.
4. Repainting 4-m Blanco Telescope We plan to proceed with the ongoing repainting of the 4-m Blanco telescope enclosure.
47 5. Cerro Tololo Power House We will expend $25K for the replacement of outdated and obsolete switching gear for the Power House on Cerro Tololo. This equipment has been in use for more than 25 years and is beginning to show symptoms of alarming decay.
6. Water System - Cerro Tololo Pipeline The water line serving the facilities at Cerro Tololo has been in continuous operation for more than 20 years, and we must plan for its prompt, methodical renewal. We will start the first stage of the progressive replacement of this vital facility. Some of the water that is pumped up to Tololo via this pipeline is used for activities on Cerro Pachon.
7. Control ofLight Pollution A disciplined effort aiming to eradicate every conceivable source of nighttime light pollution from Cerro Tololo has already proven successful. One of the measures that has produced most efficient results has been the installation of "electrical rolling shutters" in light emission areas, namely the TELOPS and Electronic Lab building, where we installed these screens with satisfactory results.
We will continue with the installation of these rolling shutters in the buildings used to lodge astronomers and CTIO workers who must stay overnight at the mountain facilities.
8. Enclosurefor the TELOPS Cable Car We would like to be able to completely enclose the TELOPS cable car that links the TELOPS and Electronic Lab building with the telescopes area. The reason for this requirement stems from the fact that during foul weather, the snow accumulates on its track, completely obstructing the carriage and driving cables and preventing the normal operation of this lift. No funds are currently available.
9. Bulldozerfor Cerro Tololo The Caterpillar D-8H Bulldozer has been in continuous operation since 1964 on Cerro Tololo. This equipment has been devoted mostly to the maintenance requirements of the main access road. In addition, since 1988 this equipment has been further committed to the construction, upkeep, and improvement of the road to Cerro Pachon. Our bulldozer has proven to be a critical asset for the operation of Cerro Tololo, especially during wintertime snowstorms, when it has been used to clear the road to bring operations back to normal. The rough nature of the work conditions that this equipment must endure on its day-to-day operation has caused extensive wear on its frame and other mechanical components. As a result, maintenance costs have soared, particularly on account of the age of the equipment, as it is becoming increasingly difficult to obtain spare parts, either in Chile or the USA.
A total of $200K would be required for the replacement of the Caterpillar bulldozer. These funds are not currently available.
B. KPNO
A single management structure was put in place in 1996 for KPNO and Tucson Facilities, and the techniques used successfully to lower utility and telecommunications costs in Tucson are now being applied on the mountain. The resultant annual savings will be invested in future years' infrastructure improvements on Kitt Peak, thereby lowering overall maintenance costs.
48 One large cost item removed from the project list provided in earlier years is the $350K microwave communications equipment intended for use between Tucson and Kitt Peak. We were successful in negotiating a major reduction (58%) in the operating costs for T-l telecommunications service with the Tohono O'Odham Utility Authority (TOUA). Consequently, we no longer need to provide independent microwave service. We will be able to add bandwidth, sufficient for at least the next five years, at a very affordable cost.
Our original intention was to replace our bus in FY 1998. However, because there are approximately 300,000 miles on it, we decided to accelerate the replacement to late FY 1997, provided sufficient funds are available. With a downsized staff, a smaller (27 passenger) bus will be adequate for our needs. Current estimates are that the bus will cost approximately $100K as compared to the original $120-130K range previously estimated for the larger staff.
Summary: Projects for (FY 1998) Estimated Cost
1. Telecommunications Upgrades and Wiring Repairs $20K 2. Fuel Tank Monitoring 7K 3. Energy Management 25K 4. Propane System 15K 5. General Building Repairs 25K 6. Building Ground Systems 20K 7. Water System 10K 8. Road Repairs 15K Total $137K
The procurement of the bus in FY 1997 alters our five year plan slightly and allows us to start on later year projects earlier than expected. However, higher cost estimates on projects such as the propane system and road repair offset this gain somewhat. In addition, we have reduced the estimate of the funds available for FY 1998 projects.
Our AT&T telephone system will continue to require periodic upgrades to maintain state-of- the-art capability. Even though this system was originally purchased in 1984, it is in excellent condition. However, the underground telecommunications wiring on Kitt Peak is not in good condition and is repeatedly in need of repair. We intend to begin correcting the problem this year.
EPA standards require us to install automatic fuel tank monitoring equipment on all our underground fuel storage tanks this year.
Preliminary studies indicate the potential for significant electrical energy savings on Kitt Peak. We are therefore beginning a multi-year energy conservation program aimed at substantially reducing our electrical costs. We have recently received a proposal from our local electric utility, Tucson Electric Power (TEP), and Johnson Controls to upgrade our 4-m telescope electrical facilities at their expense. The agreement requires that we pay them back with the energy savings over a number of years. There are several considerations here, including whether it is cheaper over the long term to carry out the program ourselves. Thus, we are carefully evaluating the proposal.
Our propane system was found to be in worse condition than originally expected. Accordingly, we altered the priority for the repairs and completed the first phase ahead of schedule. We must
49 now continue with the second phase of furnace and water heater replacements. Some of this equipment is original installation.
Work will continue on our general building repairs. This is an ongoing project to repair, paint, and roof all our facilities on a five-to-seven year rotational basis.
One new project for this year is work on our building ground systems. Every year, we expend considerable material and labor repairing lightning damage to our electronic equipment. We are hiring a consultant to evaluate and make recommendations on how to improve the grounding grid for all our telescopes and support buildings. If funds are available, we will begin implementing the recommended changes this year.
In FY 1997, cracks in the water catchment basins were repaired. This has reduced the water loss by a large margin. The intent this year is to seal coat the basins and limit losses to evaporation only.
The roadways on Kitt Peak are continually in need of repair due to harsh weather. The work done in FY 1998 will be in preparation for the major chip-sealing to be performed in FY 1999.
C. Tucson: Central Facilities and Operations
The administration of Central Facilities Operations (CFO) and Kitt Peak Facilities Operations is provided under a single management structure. This unified oversight has strengthened both departments and provided better backup in critical skill areas. A number of ongoing projects are common to both Tucson and Kitt Peak. In addition, CFO provides limited architectural and civil engineering support to KPNO and NSO/Sac Peak as required.
Summary: Projects for (FY 1998) Estimated Cost
1. Tucson Telecommunications $15K 2. Energy Management Control Systems 10K 3. Fuel Tank Monitoring 7K 4. Shuttle Vehicle Replacement 30K 5. Alternate Fuel Storage Facilities 10K 6. Chiller/heating Pipe Replacements 10K 7. Warehouse Alarm System 5K Total $87K
The Tucson facility AT&T telephone system was upgraded in FY 1997, but additional work remains. Specifically, we will purchase port cards to allow for new extensions and rewire portions of the building to accommodate conversions from analog to digital.
The Tucson facilities energy management program will continue in FY 1998 but at a reduced pace relative to prior years because most of the short payback improvements have been made.
EPA standards require us to install automatic fuel tank monitoring equipment on all our underground fuel storage tanks this year.
50 To maintain safe highway vehicles, each year we purchase, on average, three shuttle vehicles for the transportation of staff and visitors to/from Kitt Peak. If a waiver is not granted to us on alternate fuel vehicles, two of the three vehicles will require this more expensive option.
The latest EPA alternate fuel vehicle regulations will force us to consider the installation of some form of alternate fuel station unless a pending waiver request is granted. Alternate fuel is available off-site, but as more of our shuttle fleet is converted, refueling in this manner will not be cost-effective. If a waiver is granted, these funds will be diverted to further energy management improvements.
We have lost, due to corrosion, one of the original construction cast iron heating pipes in the northwest side of the headquarters building. The construction of the building is such that replacement of the pipe will be awkward and expensive. Prior to replacement, all other pipes in the area will be inspected and replaced as needed. Without repair, it is not possible to provide heat to this area of the building.
In FY 1997, we installed fire/intruder alarms in the Central Administrative Services area and GONG DMAC building. In FY 1998, we will extend this alarm coverage to include the warehouse building, optical coating lab and carpenter shop. We will also replace our main alarm panel.
D. NSO
The current budgets for the National Solar Observatory are insufficient to provide for an optimum maintenance program of the facilities at Sac Peak and Kitt Peak. There are, however, sufficient funds to carry out essential maintenance. Year end funds, to the extent that they become available from vacant positions or indirect charges on grants, are used to supplement this minimum maintenance program.
1. NSO/SacPeak
The FY 1998 NSO/SP budget includes $20K for facility maintenance. These funds will be used to paint the Vacuum Tower Telescope, and the Evans Solar Facility. In addition, the Long Range Plan lists as other maintenance tasks the replacement of the power lines and the reroofing of the Cloudcroft facility/RCA building.
Projects for FY 1998 Estimated Cost
Painting of Telescope Buildings $20K Power Line Replacement *$20K Cloudcroft Facility/RCA Bldg Reroofing *$75K Total 115K
* = from FY 1998 year-end funds if available
The painting of the telescope buildings are part of an ongoing maintenance program of the Sac Peak facilities.
The power lines in the housing area were installed in the 1950's and are beginning to show signs of serious degradation.
51 NASA recently spent over $175K in renovation of the main telescope building at the Cloudcroft Telescope Facility. Other buildings, in particular the RCA building, require roof repair to prevent water damage.
2. NSO/KittPeak
In contrast to NSO/SP where NSO is fully responsible for site and building maintenance, KPNO continues to be responsible for the labor and non-payroll associated with the routine maintenance of the solar telescopes of NSO/KP and the Kitt Peak site and facilities. NSO/KP is responsible, at the level of $30K/year, for non-payroll costs associated with major solar facility maintenance, such as the recent repair of the Kitt Peak Vacuum Telescope clamshell pistons.
The FY 1998 NSO/KP budget includes $15K for facility maintenance. These funds will be used for a number of maintenance items at the McMath-Pierce facility, including: (1) re roofing and sealing, (2) energy management, and (3) fall protection. In addition, the Long Range Plan lists as other maintenance tasks the electrical upgrade and painting of the McMath-Pierce facility.
Projects for FY 1998 Estimated Cost
Re-roofing and Sealing McMath-Pierce $5K Energy Management McMath-Pierce $5K Fall Protection McMath-Pierce $5K Electrical Upgrade McMath-Pierce $30K* Painting McMath-Pierce $15K* Total $15K $45K*
* = from FY 1998 year-end funds if available
Several water leaks in the McMath-Pierce facility, especially those in the main observing room and in the FTS stairwell, require attention.
Improvement of energy management within the McMath-Pierce complex will result in significant cost savings. We plan to upgrade the cooling system to a "closed-loop" operation with the addition of a smart controller and sensors, as well as change the general building lighting.
Access to the east and west auxiliary heliostat drives is difficult and can, under certain circumstances, present a safety hazard. A redesign will allow us to remove the current restriction on access.
Sections of the wiring and electrical components within the main observing room and telescope structure will be replaced to ensure that the facility remains operational.
The exterior of the McMath-Pierce was painted in 1991. Maintenance of the interior surfaces is, however, long overdue. The section of the windscreen just below the top of the pier requires extensive work.
52 IX. CENTRAL SERVICES
NOAO has consolidated in Tucson the types of administrative support that companies normally provide through a "home office." Included are all financial management, the NOAO Director's office, and the space occupied by the above. The cost of this administrative support, as shown in the proposal to renew the cooperative agreement, is low relative to the costs of comparable activities in universities, industry, and federal research centers.
A. NOAO Director's Office
Staffing includes the Director; three administrative assistants; a half-time manuscript specialist, who prepares the NOAO Newsletter and assists with proposals and other long documents; the receptionist in the lobby; and the head of the copy center, who is responsible for all major copying tasks and in-house maintenance of copying machines. The Deputy Director, who heads the joint CTIO/KPNO instrumentation program and is also the Director of KPNO, is funded in the KPNO budget. We have examined the alternative of contracting outside for copying and also for handling outgoing mail; the contract costs were approximately twice what we spend doing the tasks in-house.
B. Central Administrative Services (CAS)
This office provides business management support to all sites, including human resources services for all US hires at all sites, payroll, procurement, contracting, accounts payable and receivable, property management, and general accounting for all actions in the US. In addition, this department handles shipping and receiving for Tucson and expedites shipments to Chile. The Gemini international project has relied on CAS for these same services while the construction team was based in Tucson. However, we expect Gemini to begin providing its own administrative support during FY 1998.
C. Tucson Facilities
The Tucson facilities staff is responsible for maintaining 136,123 square feet of space and for operating the shuttle fleet, which provides transportation and cargo service to and from Kitt Peak. As noted in the proposal to renew the cooperative agreement, we have benchmarked the staffing and costs of this activity against NCAR and against the Best-in-Class in the Benchmark II Report from the International Facilities Manager Association (Cooperative Agreement, Appendix 3-R). In every area, NOAO compares very favorably to these benchmarks, which is especially impressive given that our facilities are more than 30 years old and that the floor area is smaller than that at NCAR. The benchmarks show that certain economies of scale reduce the cost per square foot as the total area maintained increases. We have recently placed both Tucson and Kitt Peak facilities under common management.
In addition, the Tucson Facilities group provides support for all of the activities based in Tucson, including KPNO, Gemini, and NSO. We expect Gemini, however, to leave Tucson entirely during FY 1998.
53 X. THE BUDGET
When NOAO prepared the proposal to renew the cooperative agreement, we established zero-based staffing models for those functions carried out in the nighttime program in Arizona. The models were based primarily on benchmarking with respect to other observatories, and the costs per telescope in the NOAO models were shown in that proposal to be low relative to other international observatories (CFHT, AAO, UKTRT, very low relative to ESO, and comparable to that of the one university observatory (Texas) that was willing to make comparison data available. We have not developed similar detailed models for the solar or CTIO programs, but there has been substantial examination by the NOAO directors of relative staffing levels within the organization, and it is the judgment of the NOAO Director that detailed modeling would show that the NSO program is operating at levels below what is required to maintain operations and facilities at their current level of quality, competitiveness, and repair over a long period of time. The CTIO operations levels are judged not to be significantly different from those in Arizona if the difference in scope of the activities in the two locations is taken into account.
The zero-based models for Arizona operations were designed to provide a long term, stable operation. That is, we identified staffing and funding levels that were judged to be adequate to maintain the facilities in a reasonable state of repair; to continually upgrade telescope performance to modern standards; and to replace instrumentation on a regular schedule. Most other observatories receive special funding at intervals of about five years to make major repairs; since NOAO has never received such special allocations, the annual budget must include all of the necessary support.
In preparing the program plan for FY 1998, we have compared the zero-based models with the current staffing levels, which have changed since the completion of the proposal to renew the cooperative agreement. Specifically, we have compared three of the programs for which the detailed staffing models were presented: KPNO operations, the USGP, and the instrumentation program.
A. KPNO Operations
The original zero-based model for KPNO is given in Appendix 6. Here the entries from that model are summarized by type of function for the case of a three-telescope operation (the Mayall 4-m, WIYN, and a modern 2.4-m telescope) and compared with the current staffing levels.
Table 10
Actual KPNO Staffing Compared with Zero-Based Model for Three-Telescope Operation
Function Zero-Based Current Administration 6 4.67 Scientific Staff 12 7.50 Observing Support 13 14.00 Engineering 22 *20.50 Software 7 5.00 Facilities 18 *18.00 Total 78 69.67
54 * The actual staff has been adjusted to reflect only that fraction devoted to KPNO activities; of the 19 staff in the telescope engineering group, on average 2.5 FTE each year are devoted to NSO maintenance; of the 21 facilities maintenance staff, approximately 3 are committed to maintenance of the NSO complex on Kitt Peak. We have also excluded cooks from this table because some of them are paid for by income from visiting astronomers and observers at tenant facilities.
As this table shows, KPNO is currently operating five telescopes—the Mayall, WIYN, 2.1-m, 0.9-m, and Coude Feed, with staffing that is only 89 percent of what was estimated to be the minimum required for a three-telescope operation. Furthermore, none of these telescopes is a modern, remotely operable telescope, as the 2.4-m telescope was planned to be. And a sixth telescope, the Burrell-Schmidt, was phased out only during the summer of 1997.
Furthermore, we are having exactly the problems that the model would have predicted. The staffing is short in those areas that allow the observatory to move forward. The scientific staff is too small for a multi-telescope facility. Most of their time is required simply to maintain the performance of telescopes and instruments and to support users. Efforts to identify modest changes in instruments that would enhance performance, to experiment with improved observing and calibration techniques, and to develop such capabilities as remote observing are at a standstill.
The engineering staff is only slightly too small, but even at this level the only significant telescope maintenance and improvements projects are occurring at the 4-m and WIYN; and despite this focusing of efforts, the program to improve the image quality at the Mayall will extend over at least four years, solely because of limitations in manpower. The 2.1-m and 0.9-m are being maintained at minimum levels, which are inadequate to ensure long term viability. For example, the 0.9-m telescope control system is still FORTH-based and depends on computers that are no longer available; also, we no longer have programmers with sufficient knowledge of FORTH to make any modifications to the system. Given the emphasis on the 4-m and WIYN, we have insufficient resources to replace the 0.9-m control system.
A second critical problem is that we have fallen critically behind in documentation. Some WrYN systems, including especially the control system, were delivered to NOAO with inadequate documentation. Many of the new procedures, tooling, and procedures for mounting instruments, maintaining optical alignment, and handling mirrors at both WTYN and the 4-m are inadequately documented. We do not have an effective preventive maintenance program and in many cases do not have an adequate supply of spares. Much of the equipment on KPNO is so old that it is no longer manufactured, and major failures often require a complete new design rather than simple replacement. We need to develop a database of critical parts and components, schedule routine maintenance, identify suppliers of equivalent components, and where replacements are no longer available, begin to design new systems to replace those that are beyond their expected lifetime. The 4-m has had two failures recently that closed it for several months, and so there are substantial opportunity costs associated with major mechanical failures.
And finally, software remains the single biggest bottleneck in the observatory. The staff at KPNO is smaller than the model specified, and about one-third of the available staff is devoted to maintenance of the computers and computer-networks and of the user databases, proposal processing, etc., not to new programming. Another third is working on instrumentation
55 projects, because of the inadequate size of that group, leaving very little support for the control systems of the existing telescopes. For example, improvements in software that would have improved the throughput of the WIYN by at least an hour per night took more than two years to implement.
In other words, actual management experience suggests that the models were indeed approximately correct, that KPNO (and by inference NSO and CTIO) remain overextended in the sense that we are devoting most of the budget to current consumption (telescope operations and user support) and too little to future development to ensure that the observatories will remain fully competitive in 5 to 10 years.
How do we plan to deal with these conflicting goals—providing observing opportunities to current users while maintaining some degree of investment in the future? After the turbulence of the past year, including the Web posting, NOAO has reached an accommodation with the users. It is our intention to maintain capabilities but to consolidate those capabilities on fewer telescopes. KPNO is committed to operating four telescopes until the 2.1-m and 0.9-m are replaced by a new wide-field imaging telescope. The Coude Feed will be closed as soon as we have the resources to move the spectrograph to the 4-m, where it will be fed by a fiber. This move is probably about two years away inasmuch as we plan to complete the image quality improvements at the 4-m telescope first. CTIO has already transferred the 1.0-m back to Yale and will continue to operate the 4-m, 1.5-m, and 0.9-m. The Curtis Schmidt will also remain in operation for at least the next two years. The long term goal is to replace the 1.5-m and the 0.9-m with SOAR and a new wide-field imaging telescope. It is NSO's intention to replace its multiple sites with a single site and a major new telescope.
Inasmuch as we are already overextended, all of these intentions depend on maintaining staffing at current levels. Recent data show that salaries are now rising in real terms, and maintaining staffing will therefore either require an increase in the budget or a decrease in compensation relative to the market, which in turn would inevitably mean a deterioration in the quality of the staff. We are also running several of the telescopes into the ground because of inadequate investment in maintenance and upgrades. Replacement of the 2.1-m and 0.9-m at KPNO, of the 1.5-m and 0.9-m at CTIO, and of the VTT and McMath-Pierce at NSO will be required at sometime during the next several years if the type of science that these facilities support is to continue; at current resource levels, we are no longer able to maintain the performance of these telescopes.
Will NOAO remain competitive worldwide? The one mitigating factor is that comparable problems are being faced by other university and international observatories, with the probable exception of ESO. However, the staff can take no pride in seeing operations slide below the level of quality that is possible, demanded by the types of problems that astronomers wish to tackle, and that would have been feasible with the funding levels available only a few years ago.
B„ USGP
The staffing required for the USGP program during Gemini operations is given in a table in Appendix 6. The table below summarizes the current staffing of the USGP, which is beginning to assume responsibility for handling observing proposals for all of the telescopes that can be accessed through NOAO.
56 Table 11
Actual USGP Staffing Compared with Zero-Based Model
Function Zero-Based Current Scientific Staff 6.5 6.0 Administration 1.6 1.0 Technical (Oversight of Gemini Instrumentation 6.2 1.5 in US, User Databases, Data Reduction, Archiving, Remote Observing) Total 14.3 8.5
This program, like KPNO, emphasizes current services to users. A major effort is in progress to facilitate and streamline the electronic submission of proposals to NOAO to use the KPNO, CTIO, Gemini, HET, and MMT facilities. It is important to initiate this work now since we expect the number of proposals at least to double when the Gemini telescopes come on line. We have not identified the technical resources that would allow us to support reduction of data from Gemini instruments, explore the options for cost effective archiving of data, or to begin experiments in remote observing—all of which the community will expect to be available when the Gemini telescopes go on line. However, at this time we place higher priority on maintaining access to a reasonable number of telescopes for the community. This priority will be re examined when some of the facilities now under construction are ready to be scheduled for science observations.
C. Instrumentation Program
In the proposal to renew the cooperative agreement, the instrumentation program was built around the assumption that each major instrument would have a lifetime of about six years; that each of the 4-m telescopes would have two instruments each and that the 2.4-m wide-field imaging telescopes would have one instrument each; and that the WIYN and SOAR partners would pay for new instrumentation in the same proportion as their share of the observing time. Given the typical price of instruments and detectors, this led to an expenditure of approximately $3.2M annually. A comparison of the Zero-Based and current staffing is shown in Table 12 below.
Table 12
Actual Staffing in Instrumentation Program Compared with Zero-Based Model
Activity Zero-Based Current O&M 4.7 4.7 Detector R&D 6.2 6.2 Instrumentation 20.5 18.1 Project Scientists 4J3 5.0 Total 35.4 34.0
Note that the staffing in the instrumentation program is down by nearly 2.5 FTE, or about 12 percent—even though the NSF site visit (Kirshner) committee said that the instrumentation program should not be cut. This reduction in staffing level has been made in order to provide
57 sufficient capital for the program and also to provide pay increases for key staff. Industry is hiring aggressively, and several staff have recently been offered pay increases in excess of $20K (or about 40 percent) by outside organizations. We are also having extreme difficulty recruiting staff to replace those who have left—independent of salary. Therefore, we decided it was mandatory that we provide a more favorable compensation package for current employees who are critical to the program.
The program, even before it was cut, was inadequate to maintain the flow of state-of-the-art instruments. For the first time in several years, the evaluation forms submitted by observers to KPNO note that the some of the instrumentation—particularly for wide-field IR imaging and for low resolution IR spectroscopy-is not competitive with what is available elsewhere. At the current rate of expenditure, and given the focus on bringing the CTIO instrument complement up to world standards, it will be several years before new IR instruments are available at KPNO.
The increase in scientific staff has come about because of work for Gemini—the near IR spectrometer, the IR arrays and controllers, and the integration of the CCDs and controllers. Note that Gemini does not reimburse NOAO for scientific staff time spent on building Gemini instruments.
The non-payroll funding for the instrumentation program in FY 1998 will be $100K below that in the model; this is acceptable in FY 1998 because we do not need to purchase any new detectors at this time. However, the lack of funding for detector purchases will become a critical problem over the next couple of years—and sooner if the first round of the ALADDIN program does not yield at least some additional 512x512 InSb detectors. (The goal of the ALADDIN program is IK x IK detectors, but 512 x 512 detectors could replace the 256 x 256 arrays currently in use in existing instruments.)
D. Budget Details
In formulating the budget for FY 1998, we have taken into account the following changes:
1. We expect that inflation in Chile will continue to run at a six percent rate, and NOAO will continue to cover this inflation in Chilean payroll expenditures. CTIO reduced its staff by about 15 percent two years ago, and is now operating at the minimum viable level. Therefore, NOAO will maintain staffing levels in Chile until Gemini operations begin to ramp up. At that time, sharing of infrastructure costs between NOAO and Gemini may allow some cost containment. Union negotiations will occur this year in Chile, and we have also budgeted a 3 percent merit increase. If this large an increase were actually granted, Chilean salaries would rise by 9 percent in a single year. While we will do our best to minimize the cost impact of the union settlement, there is no question that Chilean salaries are currently rising in real terms—that is, on average compensation is rising at a rate that is faster than the rate of Chilean inflation.
2. In the US-based component of the program we have allowed for approximately a 2 percent increase in salaries and no compensation for non-payroll inflation. However, we do not expect to grant an increase of 2 percent across the board. We will target the increase toward critical staff, mainly engineers and programmers, for whom salaries are currently non competitive and where turnover is significant. At the level of the President's request to Congress, most NOAO employees will receive no increase in base salary. We have been
58 unable to devise a way to operate the telescopes, carry out legally required administrative functions, or maintain basic facilities with fewer staff (and benchmarking indicates that other organizations generally are better staffed than NOAO). In some areas, such as telescope operators, staffing at the current level is required simply to cover the hours. Therefore, rather than reducing staff in order to accommodate pay increases that match or exceed inflation, we have decided to run the risk that we will compromise the quality of employees and our ability to retain them by holding down salaries.
3. We have reorganized the nighttime program in Tucson to reflect more accurately where the funds are actually being spent. The USGP has taken on the responsibility for providing a unified user interface for proposals for all of the telescopes that can be accessed through NOAO. The first step is to unify the application process for CTIO and KPNO, and a new Web-based proposal form that is identicalfor both sites will be used for applications for the spring semester, 1998. We are also developing modern database tools to manage the proposals received. This effort has required considerable oversight by scientific staff and substantial technical support, but the goal is to be able to handle twice as many proposals in the next few years with no increase in staff.
We have also included under the USGP those programs that support scientific staff in more than one division—most notably the library, the photo lab, central computing services, and the IRAF group. It is likely that once the public information programs have been redefined, they will also be moved to this division.
As noted above, the USGP is now at the level of scientific staffing that was specified in the proposal to renew the cooperative agreement. It is not adequately staffed or funded to support such technical efforts as developing archiving capability and remote observing or for providing software for Gemini instruments. However, by placing IRAF in this division, we have made it possible to prioritize the work on IRAF applications for all of the telescopes at CTIO, KPNO, and Gemini, and so presumably some relevant Gemini software will be written, albeit at the expense of software for NOAO instruments.
4. The nighttime scientific staff in Tucson are now budgeted in the department where they have their primary functional responsibilities; that is, they are budgeted in KPNO, the USGP, or the instrumentation program. Formerly, all Tucson nighttime staff were budgeted in KPNO; this transfer is the primary reason for the decrease in the KPNO budget relative to earlier years.
5. One primary change in the budget is the sharp decline in indirect charges on outside grants for which NOAO provides administrative support and space. In fact, we expect this level of support to decline by approximately $1M over about a two year period primarily due to three factors: 1) the departure of Gemini staff from Tucson; 2) the completion of WrYN construction; and 3) the transfer of the office of the Astrophysical Journal to MIT. SOAR has yet to ramp up its staffing but is likely to provide indirect income of only about $100K. The mechanism of indirect charges causes each external project to pay a share of administrative and facilities costs, not the incremental costs. Also, administrative costs do not scale with the size of the program. Therefore, we expect NOAO's own costs of maintaining the building and providing administrative services to drop by only $100-$200K with the departure of these external projects. The new projects coming into NOAO, most notably SOLIS, instrumentation for Gemini, and the teacher enhancement program, by
59 agreement with the NSF do not provide any support for overhead functions. Therefore, we expect the net decrease in funds available to NOAO scientific programs as a result of these program changes (which will force NOAO to pay essentially the entire bill for maintaining the Tucson facilities and for such administrative services as personnel, procurement, accounting, etc.) to be about $700K.
6. The support for GONG operations, now that the network is fully deployed, will be reduced to $1,850K. Work on the higher resolution cameras for network deployment cannot be funded at this level, and the cameras will be built only if a proposal to the NSF is successful.
7. Funding for SOLIS is not shown. A management plan for SOLIS was submitted to the NSF this spring. When funding is made available, we will modify the program plan to show the details of the SOLIS project.
60 APPENDIX 1
NATIONAL OPTICAL ASTRONOMY OBSERVATORIES (NOAO) ORGANIZATIONAL CHART
OBSERVATORIES AURA OBSERVATORIES COUNCIL BOARD OF DIRECTORS VISITING (TBD), Chair B. Margon, Chair COMMITTEE (TBD), Vice Chair R. Kennicutt, Chair
AURA G.Oertel, President H. Feinstein, VP for Admin. R. Malow, VP lor Intl. Programs
NATIONAL OPTICAL ASTRONOMY OBSERVATORIES S. Wolff, Director R. Green, Deputy Director
CERRO TOLOLO INTER-AMERICAN KITT PEAK NATIONAL NATIONAL SOLAR SCIENCE OBSERVATORY OBSERVATORY OBSERVATORY OPERATIONS M. Smith-AD, NOAO R.Green-AD, NOAO J. Beckers-AD, NOAO T. Boroson-AD.NOAO T I 1 TELESCOPE CTIO TELESCOPE KPNO TELESCOPE NSO US GEMINI CENTRAL ALLOCATION USERS' ALLOCATION USERS' ALLOCATION USERS' PROJECT COMPUTER COMMITTEE COMMITTEE COMMITTEE COMMITTEE COMMITTEE COMMITTEE SERVICES S.Grandi, Manager
T CENTRAL CENTRAL PUBLIC ENGINEERING KPNO/CTIO ADMINISTRTIVE FACILITIES INFORMATION &TECHNICAL INSTRUMENTATION SERVICES OPERATIONS OFFICE SERVICES N.Gaughan, Manager G. Blevins, Manager J. Dunlop, Manager Y. Estok, Manager L. Daggert, Manager
July 1997
APPENDLX 2
NOAO Management
Sidney Wolff Director, NOAO
Richard Green Deputy Director, NOAO/Director KPNO
Jacques Beckers Associate Director, NOAO/Director NSO
Todd Boroson Associate Director, NOAO/Director USGP
Malcolm Smith Associate Director, NOAO/Director CTIO
John Leibacher Project Director, GONG
Mark Phillips Assistant Director, CTIO
Robert Barnes Assistant to the Director, KPNO
Glen B levins Manager, Central Administrative Services
Larry Daggert Manager, Engineering and Technical Services
John Dunlop Manager, Central Facilities Operations and Kitt Peak Facilities Operations
Yvette Estok Manager, Public Information Office
Steve Grandi Manager, Central Computer Services
Rob Hubbard Manager, GONG Project
Rex Hunter Administrative Manager, NSO/Sacramento Peak
James Tracy Controller, Central Administrative Services
APPENDLX 3
FY 1998 Provisional Program Plan Appendix
CTIO Scientific Staff: Research Interests and Service Roles
Jack Baldwin
Areas of Interest QSOs and Active Galaxies, HII Regions
Recent Research Results Baldwin spent calendar year 1996 on sabbatical leave at Cambridge University, England. There he worked with G. Ferland, K. Korista, D. Verner, and J. Ferguson (U. of Kentucky) on various aspects of the Locally Optimally-emitting Clouds (LOC) model of QSO broad- and narrow-lined regions. They found that the intensity ratios in AGN emission-line spectra can be understood as being the natural consequence of the variation of the line emissivity in individual BLR and NLR clouds as a function of their densities and radial positions. Baldwin also continued his work with R. Rubin (NASA Ames), Ferland, P. Martin (CITA), and others on studies of the Orion nebula using both HST and the echelle spectrograph on the Blanco telescope. This work showed that the spectrum of the photodissociation region is consistent with a warm, low-density gas, contradicting some previous results, and that the gas- phase iron abundance is consistent with heavy depletion of iron onto grains. Finally, in work still in progress, Baldwin, A. Cooke (Edinburgh), A. Wilson (U. of Maryland), and others studied the Seyfert 2 galaxy NGC 3393 using an extensive set of HST and groundbased data.
Future Research Plans Baldwin is continuing to study the Orion nebula in collaboration with Rubin, Ferland, et al. and will be obtaining further groundbased echelle spectra to complement HST observations. He is also continuing investigations of the LOC models and of QSO luminosity indicators in collaboration with Korista, et al. An immediate effort is to finish up the work on NGC 3393, which is a very detailed study of a case where the NLR consists primarily of bow shocks swept up ahead of a double-lobed radio source.
Service Baldwin is serving as the NOAO representative on the Science Working Group for the SOAR 4-m telescope project.
Olin J. Eggen
Areas of Interest Stellar and Galactic Structure and Kinematics
Recent Research Results The abundance of the oc-process element calcium is smoothly related to the heavy element abundance (Fe/H) by the relation [Ca/H] = 0.88[Fe/H]+0.18. This relation holds for most stars to [Fe/H]~-3 dex. Several features appear to differentiate between old disk and halo stars at a boundary near [Fe/H] -0.9 dex. The most striking differences are (1) the dependence of CN abundance upon temperature, in both dwarfs and giants and (2) a change in the form and progression of the RHB and EAGB stars. The domain of young disk stars in the Bottlinger diagram is unique and forms a void in the distribution of old disk stars. RHB and EAGB stars of the halo population are unaffected by differential line blanketing. Some 70 field, RHB and AGB stars near the sun have been isolated. Calcium abundances of these objects are obtained from the Twarog hk index, P[Ca/H] = [(hk)0OBS - (hk)0COMP]/0326 +0.14, where (hk)0COMP= 1.55 (b-y)0+0.35. Moving groups in the old disk and halo populations are used to fix the luminosity level of the main sequence as a function of heavy element abundance. In summary, Eggen's research is based on the fact that most stellar movement reflects the movement of the gas from which the stars were formed, and therefore provides stellar families, formed under similar original conditions, for study.
Future Research The investigation of moving groups and superclusters, and their application to the astrophysical problems will be the main thrust of Eggen's future research.
Service Olin Eggen serves the Time Assignment Committee when necessary, and supervises the Library.
Brooke Gregory
Areas of Interest Gregory is an instrument physicistworkingprimarily in the area of development of IR Instrumentation.
Recent Research Results Gregory is in the middle of the commissioning and testing of the latest upgrade of the CTIO IR Spectrometer. This upgrade incorporates new fore-optics (to adapt the system to the f/14, tip-tilt secondary on the 4-m telescope) and a new system of mechanical support required by the tip-tilt mechanical interface.
Future Research Plans Gregory plans to be involved in the planning and execution of the next major IR instrumentation effort undertaken at CTIO. He is particularly interested in the prospect of building a simple wide-field imager for the f/14 foci on 4-m and 1.5-m telescopes, to take advantage of the larger format devices (with HgCdTe or Aladdin InSb) that are now available.
Gregory is planning to take sabbatical during calendar year 1998 and will visit a site of development of Adaptive Optics instrumentation in anticipation of the implementation of such facilities on the SOAR and Gemini telescopes.
Service Manager of Engineering and Technical Resources Group at CTIO. Liaison to Gemini in development of plan for sharing technical resources between Gemini and CTIO. Supports users of IR instrumentation generally.
Steve Heathcote
Areas of Interest Star Formation, Herbig-Haro Objects, Supernovae and Novae
Recent Research Results Heathcote's recent research efforts have concentrated on the study of Herbig-Harojets using high spatial resolution images obtained with the Hubble Space Telescope. It is now known that stars in the process of formation blow extremely powerful, often highly collimated winds. The collision of these highly supersonic outflows with gas surrounding the nascent star excites luminous shock waves, which we observe as a Herbig-Haro jet. These jets provide key information about the mechanisms at play in forming a star. In particular it is possible to measure how much mass the star is losing now and how the rate of mass loss has varied over the last few thousand years. Such jets are also valuable astrophysical laboratories for the study of shock physics and chemistry. In two recently completed papers Heathcote and collaborators, B. Reipurth (ESO), R. Schwartz (U. of Missouri), J. Bally (U. of Colorado), J. Morse (U. of Colorado), P. Hartigan (Rice U.), and J. Stone (U. of Maryland) present HST images of two of the finest examples of such jets, HH 46/47 (AJ 112, 1141) and HH 111 (AJin press). These images provide the first clear evidence that shocks within these jets are excited by fluctuations in the velocity and direction of the outflow from the source. At the very high spatial resolution obtained with HST it is possible to study for the first time the structure of the zone behind these shocks. The data also provide new insights into the way in which jets sweep up material in their surroundings, helping to clear away the debris left behind after formation of the star. In a separate project, carried out in collaboration with B. Reipurth (ESO) and A. Raga (UNAM), Heathcote has combined HST images with groundbased high resolution spectroscopy and proper motion measurements to study the structure and kinematics of the HH 80/81 complex. Whereas most HH flows (including HH 46/47 and HH 111) are driven by low luminosity stars with masses similar to that of the Sun, the source of the HH 80/81 outflow is a much more luminous, BO type star. This system thus provides a rare opportunity to study how outflow properties depend on the power of the driving source.
Future Research Plans During the next year Heathcote will re-observe four HH jets already imaged with HST. The velocities of such jets are so high that motion is detectable over periods of only one or two years. Thus these second epoch images will supply crucial information on how the various shock waves move and how they change with time. Heathcote, in collaboration with B. Reipurth (ESO), M. McCaughrean (MPIfR), and H. Zinnecker (Potsdam) will also obtain IR images of two HH jets using both the NICMOS imager on HST and the COB imager plus tip-tilt secondary on the Blanco 4-m telescope. While the optical emission from an HH jet traces the strongest shocks, molecular hydrogen emission in the IR probes the weaker shocks at the periphery of the jet. At IR wavelengths it is also possible to study the sections of the jet closer to the driving source, which is hidden from view in the optical by overlying extinction.
Service Heathcote is responsible for scientific oversight of CTIO's computer system and network and of the CTIO computer programming group. He also supervises the data reduction assistants on Cerro Tololo. During the past two years, Heathcote has been heavily involved in the software side of CTIO's Arcon CCD controllers. He is consequently closely involved with the development of the NOAO CCD mosaic imager, based on these controllers, which will be commissioned during 1997. Heathcote is also project scientist and manager for a multi-year project to upgrade the drives and control system for the Blanco 4-m telescope. Heathcote is a member of the Advisory Committee on Technical Resources at CTIO.
Tom Ingerson
Areas of Interest Astronomical Instrumentation, Optics, Spectroscopy, Fiber Optics, Electronics, Computer Networking
Recent Research Results Ingerson is a Support Scientist whose work consists of developing and improving the instruments CTIO needs to maintain itself as a world-class facility with state-of-the-art equipment. In recent years, he has supervised the design, construction and installation of a fiber-fed, multiple object spectrograph, Argus, and a Prime Focus Atmospheric Dispersion Correction optical system for the Blanco 4-m telescope. He
in has also implemented a bench-mounted echelle spectrograph for the 1.5-m telescope and a new system of stand-alone control for motors and other peripherals, which is gradually replacing the old control systems on all telescopes. For several years, he acted as project manager for the CTIO CCD Control system, Arcon, and is now playing a major role in the thrust to build for CTIO an upgraded version of the second- generation multiple object spectrograph, Hydra, which is now in use at the WIYN telescope on Kitt Peak.
Future Research Plans Currently Ingerson is on sabbatical leave at the Dominion Astrophysical Observatory (DAO), Victoria, BC and is using this opportunity to prepare himself to aid CTIO in integrating itself with the Gemini project. This is the planned thrust of much of his activity for the next few years. While at the DAO, he has participated on Review Committees for the Gemini Multiple Object Spectrograph (GMOS) and the High Resolution Optical Spectrograph (HROS), which are the two primary Gemini optical instruments. He has also been working with the Canadian Astronomical Data Center (CADC) in Victoria, which is writing the Gemini Data Handling System (DHS). This is because of his interest in high speed communications and the smooth flow of astronomical data and commands between observer and telescope. He plans to continue active participation in all these projects as part of the effort to help CTIO make a smooth transition to a well-integrated Tololo-Pachon (Gemini) observatory system.
Service Ingerson's position is primarily one of service to the observatory rather than personal research. His job is to design and support instruments and to teach observers to use them. Observatory-wide, instruments must be integrated into systems that are reliable and maintainable. This is an especially challenging task with the limited resources available today. Old instruments need to be supported and astronomers educated on their use, while they are being replaced, upgraded, or phased out as appropriate. Reliable, well-integrated communication needs to be provided between all systems. All these areas are within Ingerson's expertise and are tasks in which he invests large fractions of his time. Finally, users must have the tools available to leam how to use instruments and prepare themselves as well as possible for an observing run in advance. For this purpose, Ingerson also acts as the supervisor of the CTIO Internet site which is now the primary method by which instruction and documentation is passed to prospective observers.
Michael Keane
Areas of Interest Quasar Absorption Line Systems, High Redshift Galaxies, Stellar Populations, the Extragalactic Distance Scale, Galactic Structure, Astronomical Instrumentation
Recent Research Results Sakurai's Object is a star that recently underwent a sudden, reverse phase in its evolution, changing from a white dwarf back into a giant. Keane, in collaboration with M. Shetrone (ESO) and G. Wallerstein (Washington), has shown the atmosphere of this star possesses a most peculiar composition. The atmosphere is deficient in hydrogen and enriched in several heavier elements; carbon, for example, is 100 times more abundant than in typical stars. The pattern of elemental abundances seen in Sakurai's Object suggests that this star may be related to the class of hydrogen-deficient stars known as R CrB stars.
Future Research Plans Keane is nearing completion of a survey to identify bright quasars behind the Magellanic Clouds. Observations of background quasars in the ultraviolet using HST permit probing interstellar gas in the Clouds via the absorption lines produced by the intervening gas. Because of their large angular extent,
IV the Magellanic Clouds offer one of the few opportunities to investigate the spatial extent and distribution of gas in the halo of an external galaxy.
With Elston (CTIO; Florida), Keane is extending to greater redshifts the range over which the evolution of quasar absorption systems can be studied by moving to the near-infrared in order to observe absorption lines at extreme redshift.
Keane is continuing to monitor Sakuari's Object which also continues to evolve rapidly. The recycling of this star into its present high luminosity state is almost certainly due to the renewal of nuclear reactions within the star. It is possible that the surface abundance of hydrogen will decrease and the over abundances of certain heavier elements will grow as the nuclear burning proceeds towards completion. Another reason for continuing to observe this star is the opportunity to detect short-lived isotopes produced in the nuclear burning shell if these isotopes are convected out to the surface of the star before they can radioactively decay.
Keane is collaborating with M. Shetrone (ESO) on several projects to investigate the role that deep mixing might play in the post-main sequence evolution of metal-poor stars. The signature for the presence of such deep mixing that is being looked for is a specific pattern of elemental and isotopic abundance variations along the giant branch.
Service Keane's primary areas of responsibility are the Cassegrain spectrographs used on CTIO's 4-m and 1.5-m telescopes. He is the primary staff contact for users of these instruments.
In support of visiting observers, Keane writes and maintains manuals for the spectrographs, advises visiting astronomers about instrument configurations, and assists with startup nights. Keane has also written instrument simulators for the spectrographs for planning observations and he also maintains a database of current instrument performance, distributing this information to users via the World Wide Web. Keane also organizes the colloquium series at CTIO.
Mark M. Phillips
Areas of Interest Supernovae, Observational Cosmology
Recent Research Results During the past few years, Phillips has concentrated his research on characterizing the optical spectroscopic and photometric characteristics of Type la (thermonuclear) supernova explosions, and using these events as cosmological standard candles. In collaboration with colleagues at CTIO and the University of Chile, he has recently published an analysis of the Hubble diagram of ~ 30 type la supernovae (SNe la) discovered during the course of the Calan/Tololo SN search, which was carried out at CTIO from 1990-1993. The main results of this study are: 1) confirmation of the dependence of the luminosities of SNe la on the initial rate of decline of the B light curve (an effect discovered by Phillips in 1993 from a smaller sample of nearby SNe la), 2) evidence for significant correlations between the absolute magnitudes (or decline rate of the B light curve) and the morphological type of the host galaxy, and 3) calculation of a Hubble constant in the range H0 = 60-67 km/s/Mpc when the luminosity-decline rate relation is taken into account. Phillips has also worked with Nugent (U. of Oklahoma) and several others in describing a spectroscopic sequence among SNe la based on systematic variation of several features seen in the near-maximum spectrum. This sequence is analogous to the above-described photometric sequence of SNe la, which shows a relationship between the peak brightness of a SN la and the shape of its B light curve. In addition, Phillips, Nugent, and collaborators were able to reproduce the major features of the sequence through a series of theoretical model calculations in which the only parameter varied was the effective temperature. Since the supernova is almost entirely powered by the radioactive decay of Ni56, the temperature differences are likely to be due to the total amount of Ni56 produced in the explosion.
Future Research Plans Phillips intends to focus most of his research over the next three years on two specific aspects of SNe la: determining the luminosity function and using SNe la to measurethe space motion of the Local Group as well as the deceleration parameter q0. These projects will require two different SN searches: 1) a search for SNe la in rich clusters of galaxies in the redshift range 0.03-0.07, and 2) a deeper search for SNe la at redshifts of z ~ 0.5. The cluster search is currently being attempted with the Curtis Schmidt telescope (the same telescope used for the Calan/Tololo search) using CCD detectors instead of photographic plates, which should allow SNe la to be detected to high levels of completeness down to absolute magnitudes as faint as Mv = -18.5 + 51og(Ho/65). Among the questions to be pursued are the relative frequency of low-luminosity events (e.g., SNe 1987A and 1991bg) with respect to the more luminous "normal" SNe la, and the true slope and dispersion of the peak luminosity-decline rate relation. This same sample will also be used to provide an independent measurement of the space motion of the Local Group, which can be compared with the results of Lauer and Postman, who found evidence that the inertial frame of Abell clusters with z < 0.05 is moving en masse at a speed of nearly 700 km/s with respect to the cosmic microwave background. The high-redshift SN search is currently being carried out with the 4-m telescope prime focus CCD camera and has resulted in the discovery of - 60 SNe in the redshift range 0.3 < z < 0.7. During 1997, the primary goal of obtaining spectra and well-observed light curves for a subsample of ~ 30 SNe la in this redshift range should be achieved, which should in principle allow the value of q0 to be determined to a precision of ± 0.1. This will tell us whether the universe is infinite and will continue to expand forever, or whether the expansion will eventually halt and the universe collapse in upon itself.
Service Phillips serves as the Assistant Director of CTIO, and hence plays a significant role in the administration and operation of the observatory. He is a member of IPAC, which is the oversight committee for the NOAO Instrumentation and Projects Group (IPG), and also interfaces with the ACTR (Advisory Committee on Technical Resources), which oversees the CTIO ETS instrumentation effort. Phillips is in charge of efforts at CTIO to control light pollution, and also shares support responsibility for the low- dispersion spectrographs on the 4-m and 1.5-m telescopes.
Ronald G. Probst
Areas of Interest Star Forming Regions, Low Mass Stars, Infrared Imaging Instrumentation
Recent Research Results Infrared astronomy has been largely technology driven. Over the past decade, NOAO's deployment of sensitive, large format infrared detector arrays in robust and flexible imaging systems has brought an immense increase in scientific capability to the astronomical community. A part of Probst's research has been to apply this capability to the study of photodissociation regions: the boundary layers between hot, thin, ionized gas and cold, dense, molecular material. These layers are associated with stellar birth, as hot young stars carve holes in their natal dust clouds; and stellar death, when radiation from newly exposed inner portions of a star interacts with material ejected earlier from its outer layers. One of the best techniques for tracing these regions is imaging in the 2.12 mm line of molecular hydrogen. The
VI morphology itself offers insight into the processes at work, and quantitative measurement of radiation at this wavelength is a guide to the energy exchange. While on sabbatical at CTIO, Probst has assembled a special purpose small telescope and coupled it to a facility IR camera equipped with custom filters. This permits imaging of H2 emission over an area the size of the full Moon in a single picture, a unique and powerful capability for mapping extended faint structure. Probst has applied this technique to the molecular cloud in which the Orion Nebula is imbedded in order to trace the complex H2 morphology of this nearby region of massive star formation. He has also extended this work to H2 imaging of star forming regions in the Large Magellanic Cloud with the CTIO 1.5-m telescope. Use of a large telescope on a more distant object enables comparisons at the same linear scales. A surprising result is the complex and extensive H2 morphology of the 30 Dor region, a more energetic region of star formation than Orion which serves as a stepping stone to the starburst phenomenon seen in more distant galaxies.
Future Research Plans Probst plans to follow up this work with additional infrared imaging and spectroscopy of star forming regions in the Large Magellanic Cloud. Higher spatial resolution provided by larger telescopes, together with IR adaptive optics soon to be implemented at CTIO, will improve the morphological understanding of the 30 Dor H2 complex. Imaging in other infrared lines, made possible in part by the deployment of new detectors, will enable determination of dust extinction. This helps to disentangle the actual three- dimensional structure of this star forming region. H2 emission can be induced by the impact of a shock front on neutral material, or as fluorescence caused by radiation of the appropriate wavelength. Infrared spectroscopy will allow discrimination between these much different physical mechanisms by measurement of H2 line strengths. It may also be possible to infer the neutral hydrogen content of the LMC directly, a fundamental and poorly understood parameter for study of the star formation process in an environment much different from our own surroundings in the Galaxy. Together with M. Rubio (U. of Chile) as principal investigator, Probst will use the SEST telescope at ESO for high resolution millimeter wave maps to trace the spatial and density structure of cold molecular gas around 30 Dor.
Service Probst's staff position as a Support Scientist requires him to spend the bulk of his time in service activities. As a member of the KPNO Infrared Group, he has been centrally involved in the development and deployment of infrared imaging systems over the past ten years. This involves close interaction with engineering staff during design and construction, in order to deliver a scientifically capable, technically maintainable, astronomer friendly instrument; and with scientific users at the telescope, so that they may get the most out of an instrument's capabilities. His most recent, multiyear endeavor has been as Project Scientist for the Cryogenic Optical Bench (COB), an advanced imager with multiple spatial and spectral filtering capabilities. After bringing this instrument from conceptual design through construction to deployment at the focal plane as a facility instrument, Probst was Project Scientist for its upgrade to high spatial resolution capability in the Diffraction Limited IR Imager (DLIRIM) project. As part of a rebalancing of instrumental resources between CTIO and KPNO, COB will be upgraded to a larger detector and redeployed permanently at CTIO, where it will serve as the science sensor in a tip-tilt adaptive optics system on the 4-m telescope. Probst will accompany the instrument to Chile, transferring to the CTIO staff for a three year period. He will be responsible for bringing this combination on-line as a user facility. As a part of his continuing support of facility IR instruments, Probst provides assistance to potential observers in the preparation of technically competent proposals and does feasibility review on all IR imaging proposals received in our biannual cycle. In addition to his service in the Infrared Group, Probst recognized the benefits to be gained from a systematic, mountain-wide program of collimation and related optical work on facility telescopes. He therefore created the position of Optics Scientist and served in this role for two years, coordinating engineering and mountain technical staff in the improvement of delivered image quality at all KPNO focal planes. This initial effort led to the creation of a new scientific staff position with enlarged responsibilities, subsequently filled by C. Claver. Finally,
vn while on sabbatical at CTIO, Probst has been working with operations staff to prepare the infrastructure necessary for receipt, maintenance, and operation of COB and other large infrared instruments which will be deployed there.
Robert A. Schommer
Areas of Interest Stellar Populations, Magellanic Clouds, Cosmology
Recent Research Results Schommer is working with the Calan/Tololo supernova group in the study of the Hubble diagram, using SNe la to measure H0. Current best estimates give H0 in the mid-60s, somewhat higher than Sandage's recent result, and thus argue for a somewhat younger universe. Schommer is studying old star clusters in the Large Magellanic Cloudand in M33 with Hubble SpaceTelescope (HST) data. Deep photometry for central clusters is being used to measure the age and search for the oldest population in the LMC. In the local group spiral M33, photometry and horizontal branch morphologies for 10 old clusters are being obtained to evaluate the difference between the halo of this local group spiral and that of our own Galaxy; in particular, the "second parameter" is being examinedto see if these very different halos might have similar formation processes.
Future Research Plans Future work on the old populations of Local Group galaxies will include studies of field populations in the outer regions of the LMC, using photometry, abundances, and velocities, with both groundbased and HST data. A study of NGC 121,an old cluster in the Small Magellanic Cloud, is also being planned. As a memberof the high-zsupernova team, Schommer is searchingfor SNe at redshifts of - 0.5. Over the past 2+ years, more than 35 SNe la at redshifts> 0.3 have been found and confirmed by the group. The record for the highest redshift SNe la has just been established by this group (z = 0.966). HST cycles 6 and 7 time has been granted to provide accurate photometric follow-up for a portion of this sample. The project's goals include a measurement of the deceleration parameter, q0, from these data, and thus a determination of the geometry and age of the universe.
Service Schommer's extensive service activities currently include chair of the CTIO Advisory Committee on Technical Resources (ACTR); he is thus an ex-officio member of NOAO's IPAC (central instrument planning group). Schommer is working on plans to coordinate the CTIO technical and support staff with that expected for the Geminiproject effort in Chile. He is working on operations plans for CTIO with the expected additions of Gemini South and SOAR to the telescope mix. He remains in charge of small telescope improvements, currently focusing on the 0.9-m and 1.5-m. He is the staff contact and coordinator for the MACHO project, which uses time on the CTIO 0.9-m, and for the Yale 1-m collaboration. He has served as CTIO member of several Gemini committees, including the optical instrument working group, and served on the conceptual design review committee for the Gemini multiple object spectrograph (GMOS).
Malcolm Smith
Areas of Interest Quasars, Active Galactic Nuclei, Faint Red Objects at High Galactic Latitude
Vlll Recent Research Results and Future Research Plans Smith has continued observational work on three complementary, collaborative surveys aimed primarily at: 1) Discovery of quasars at redshifts z > 5, and 2) Characterization of the quasar luminosity function in the redshift range 3 < z < 5.
This research has the goal of clarifying the controversial question of the evolution of the luminosity function of quasars at early epochs in the universe; an estimate of the time which elapsed between the big bang and the time when quasars switched on should prove relevant to an understanding of the early formation of galaxies. This is a long-term project involving extensive calibration work, surveys, and data reduction.
Smith is carrying out these surveys as a member of three quite large groups, each able to handle the substantial amount of data involved. Two of these groups are using the newly-available BTC camera (4-shooter CCD optical imager) to survey large areas of sky to different depths with the 4-m Blanco telescope. The first of these 4-m surveys, by Falco, et al., aims to cover ~ 50 square degrees in I, V, and B to search for z > 5 quasars, gravitational lenses, and z > 0.6 clusters of galaxies. Extrapolation of the quasar luminosity function (QLF) for 5 < z < 6 predicts 0.02 (Warren, et al. 1994) to 0.5 (Schmidt, et al. 1995) quasars per sq. deg. to 1 = 22 mag. This survey should thus find between 1-25 z>5 quasars to I = 22. The full 50 sq. deg. are needed to distinguish at the 5-sigma level between QLFs that agree well at z = 4.
The detection or non-detection of the most distant objects in the universe and the characterization of their QLF with this survey is expected to yield important constraints on models of massive galaxy formation and on the ionizing UV background at high redshifts.
The second of the 4-m surveys, by Hall, et al., has as its aim the determination of the shape of the QLF between 3.3 < z < 5.0 and should prove complementary to the work of Falco, et al. at higher redshifts. Observing for this program begins in June 1997.
A third CCD survey for high-z quasars is being carried out by Kennefick, et al. using a Gunn-Thuan z-band filter at the 61 cm Curtis Schmidt telescope in conjunction with the digitized Second Palomar Observatory Sky Survey (DPOSS, Reid and Djorgovski 1993); DPOSS consists of photographic J, F, N data calibrated to the Gunn-Thuan gri system. The g-band data is detection complete to g - 22, allowing selection of quasar candidates with (g-i)>4 to i = 18.0 Such red selection should select almost all quasars at 5.0 < z< 6.0 within the fields selected because these bands cover the Ly-alpha emission and Ly-alpha forest absorption regions of quasars at these redshifts, giving a distinct (g-i) colour. To find the most luminous (and rare) quasars requires a survey covering hundreds of square degrees, which is why Schmidt telescopes are being used for this work. Given the uncertainty in the QLF at high redshifts, the goal of this third survey is better to constrain the degree of decline in the number of quasars at high redshift, as well as possibly provide objects for study at z ~ 5, when the universe was less than 5% of its current age. To date, just over 400 sq. deg. have been covered in this third survey. No quasars have yet been found. If no quasars are discovered, the resulting limits will help rule out some current models postulating that at least the most luminous quasars continue to exist at essentially constant co-moving space density out to redshifts 4 or 5.
Service Director, CTIO; Associate Director, NOAO; representative of AURA in Chile.
Smith has multiple service duties as Director of CTIO. He has been initiating the renewal of CTIO into an international observatory centered around support of the 8-m Gemini South telescope and two
IX complementary 4-m telescopes—the Blanco and SOAR telescopes. In addition, he has initiated and participated in an extensive program to combat light pollution in Chile. He is also introducing a greater degree of privatization in the operation of the smaller telescopes at CTIO. He has worked closely with NOAO Tucson to encourage collaboration in the production of large instruments for Gemini and the NOAO telescopes. Most recently he has been involved in intense activity for AURA as its representative in Chile, particularly with respect to the Gemini project.
Nicholas B. Suntzeff
Areas of Interest Stellar Populations, Globular Clusters, Stellar Chemical Abundances, Galactic Structure, Magellanic Clouds, Supernovae, Large-Scale Structure, Astronomical Site Characteristics
Recent Research Results Suntzeff, in collaboration with Phillips, Schommer, and the rest of the Calan/Tololo supernovae project, has continued his long-term study of supernovae. The first phase of the Calan/Tololo project has been finished, and over 50 supernovae (SNe) were discovered out to z = 0.12. They have used the Type la subsample of these SNe to measure the local structure of the universe. The Tololo group has shown that a Type la event can be used to measure relative distances accurate to about 6%. Of particular interest is the measurement of the local rate of universal expansion (the Hubble constant) with respect to the SNe reference frame. The distant SNe overcome the problem associated with local, non-cosmological flows affecting the perceived expansion rate of the universe. The SNe results, coupled with HST-based distance calibrations to nearby galaxies that have hosted SNe (published by Saha, Sandage, and collaborators), show that the Hubble constant is near 65 km/sec/Mpc with an error dominated by the distance to the local calibrators, not the SNe reference frame. The Calan/Tololo group also finds that the reference frame for the universal expansion is directed towards the dipole defined by the microwave signal measured by the COBE satellite. In stellar astronomy, Suntzeff is working with T.D. Kinman at KPNO to measure the spatial and kinematical structure of the Galactic halo. This study will provide clues as to the origin of the halo, and ultimately, the origin of the Milky Way Galaxy. Suntzeff, in collaboration with Schommer, Walker, and others, is also pursuing a similar project in the Large and Small Magellanic Clouds. They seek to find the original population of the stars in the Clouds to study the age and kinematics of the oldest stars, in order to compare the galaxian formation of these close satellite galaxies with the formation of our Galaxy.
Future Research Plans The future research for Suntzeff will concentrate on using new samples of supernovae to measure physical properties of supernovae explosions and to measure the local geometry of the universe. In collaboration with Phillips, Schommer, and others, he will start a new search for supernovae at CTIO, concentrating on galaxy clusters out to z = 0.1. This search will attempt to find up to 100 SNe to establish the natural population of supernova explosions. These data will be a key to understanding the explosion mechanism for Type la events (which is still unknown) and estimating the intrinsic luminosity spread in the range of Type la explosions. This latter property is extremely important to tie down, since many modern studies of the local rate of expansion and the geometry of the universe rely on a detailed knowledge of the range of SNe luminosities.
Another CTIO collaboration seeks to measure q0, the local geometry of the universe. One of the outstanding questions of cosmology is the local curvature of the universe. The Calan/Tololo team has shown that the Type la SNe are such good standard candles that a simple comparison of SNe events at z = 0.5 with local events can be used to measure the q0 geometry factor to better than 20% if roughly 25 SNe can be discovered. The CTIO group is spearheading an international campaign of astronomers at CfA, University of Washington, the MSSSO in Australia, and in Chile to discover a distant sample of supernovae to measure q0. A by-product of this survey will be a list of variable stars, which Suntzeff will use to continue his Galactic structure studies with Kinman, Cook (LLNL), and Schmidt (MSSSO), with the goal of measuringGalactic structurebased on field stars out to 100kpc.
Service Suntzeff will continue in a multi-faceted program of service to CTIO. He is in charge of the Argus and bench-mounted echelle instruments. He is actively participating in the upgrade of the Argus fiber system to a Hydrasystemsimilarto that at the WIYN telescope, which will increase the number of objects that can be observed by a factor of six. He will work with J. Filhaber to try to bringsignificant improvements in image quality to the smaller telescopes, using the knowledge gained during the 4-m telescope image improvement campaign. Suntzeff will continue to be in charge of the basic site monitoring at CTIO, including the seeing telescope that is now routinely measuring the CTIO site seeing. He will also work with Gemini to begin a permanentmonitoring for the Pachon site, in order to build up environmental and seeing data prior to the inauguration of the Gemini South telescope. Suntzeff will continue to serve on the CTIO TAC and ACTR committees.
Alistair Walker
Areas of Interest Stellar Populations, Magellanic Clouds, Distance Scale, Stellar Photometry
Recent Research Results Walker is a member of a team awarded HST WFPC2 time in Cycle 5 (N. Suntzeff, PI), to determine ages and abundances for several old or probably old clusters in the inner regions of the Large Magellanic Cloud. Data reduction is nearly complete and analysis is underway. All the clusters are found to be as old as galactic globular clusters. This work, together with complementary photometry of MC field stars, will allow the early star formation history of the Magellanic Clouds to be deciphered. The results will bear directly on our ideas on the early formation and subsequent evolution of galaxies in general. Walker, with H. Smith (Michigan State) and N. Silbermann (IPAC), is completing the analysis of CCD photometry of a one-degree square field in the Small Magellanic Cloud, obtained with the Curtis Schmidt telescope. This field contains many short-period Cepheids, and the program is aimed particularly at defining the structure of the faint end of the Cepheid Period-Luminosity relation in the HR diagram.
Walker, with Y-W Lee, S-C Rey (Yonsei, Korea), and S. Baird (Benedictine College) are measuring [Fe/H] abundances for all the RR Lyrae variables in the galactic globular cluster co Centauri. All data have been obtained and reductions are just starting. This work will allow comparison with evolutionary and pulsation models, and further constrain the relative contributions of primordial enrichment and evolutionary mixing to the present-day metallicity distribution of the cluster.
Future Research Plans Walker is PI of a Cycle 6 HST program which will study the oldest Small Magellanic Cloud cluster and two distant field regions, one in each Cloud. Extensive groundbased observations with the CTIO 4-m and 1.5-m telescopes are integral parts of this program, which complements the MC cluster photometry mentioned above.
A collaboration led by D. Terndrup (OSU), with R. Peterson (UCSD), E. Sadler (AAO), and Walker is beginning a search in galactic bulge fields (photometry, spectroscopy) for hot evolved stars in the hope of identifying the origin of the copious UV flux in old, metal-rich populations in other galaxies.
XI P. Seitzer (U. of Michigan), E. Grebel (UCSC), and Walker are beginning a study of the globular cluster systems in two nearby Magellanic Irregulars, in order to test whether their cluster formation is episodic, like in the Large Magellanic Cloud, and to determine the effects of environment on the cluster population.
Service Walker is currently responsible for the Blanco 4-m telescope, and in particular is supervising the on going program of optical and thermal tests, together with managing the upgrades work in these areas.
Walker directs and coordinates CCD operations and upgrades, supervises the operation of the CCD laboratory, and is responsible for optical imaging programs on all telescopes. He is responsible for the Schmidt telescope and has managed the projects that have automated the wide-field imager at that telescope. He is the CTIO scientist who liases with NOAO Tucson on the production of the NOAO 8K x 8K imager and is leading the effort to upgrade the Blanco 4-m telescope so that it is ready for a clone of that instrument, due at CTIO in late 1998. He is project scientist for most projects involving production and implementation of the Arcon CCD controllers. He has organized the long-term visit to CTIO of the Tyson and Bernstein mosaic imager BTC (Big Throughput Camera) and is the responsible CTIO scientist for the instrument.
Walker is a member of ACTR (CTIO Advisory Committee for Technical Resources) and has served as a member of the US Gemini Science Advisory Committee since 1994. On two occasions he has represented the US on the Gemini Science Committee.
xn KPNO Scientific Staff: Research Interests and Service Roles
Helmut A. Abt, Astronomer Emeritus
Areas of Interest Duplicity, Rotation, Spectral Characteristics, and Evolution of Stars; Publication Statistics
Recent Research Results Helmut Abt and his collaborators have been trying to understand how binaries are formed. Because most stars are in binary systems, the mechanism of formation must occur frequently. If they are formed by capture in clusters, one would expect the young binaries to have low-mass companions (because they are so plentiful). Those binaries are then disrupted and gradually the high-mass primaries pair with high- mass companions. That is exactly what those people discovered in studying binaries in clusters of various ages. Thus the capture mechanism replaces the fission mechanism that theoreticians have found not to work for binary formation.
In three-body encounters in clusters, there is a tendency for two stars to form a pair and the third one is kicked away. In some cases the momentum given to the third star is enough to eject it from the cluster. Thus with time we would expect clusters to become rich in binaries and the field outside of clusters to have proportionally fewer binaries. H. Abt and D. Willmarth are collecting data on 100 stars in clusters and 100 similar ones outside of clusters to see if that is true. Because our knowledge of stellar luminosities and ages is based mostly upon cluster stars, we should be aware of whether they represent a fair sample of all stars. Stars in binaries appear to be brighter and their evolutionary stages are different from those of single stars.
Service H. Abt spends his free time on research but is paid half-time (by the AAS) to be Editor-in-Chief of the Astrophysical Journal. That journal is published every 10 days and currently publishes 25,000 pages per year. The editorship is due to be transferred to P. Joss at MrT late in 1997 and the KPNO office will finish its work in early 1998. Abt has arranged to have the Van Biesbroeck Award for outstanding service to astronomy transferred from Tucson control to the AAS in 1997. He is scheduled to become a Guest Professor at Beijing University and at Nanjing Normal University in China.
Michael J. S. Belton
Areas of Interest Planetary Science, Comets, Asteroids, Jupiter System
Recent Research Results With B.E.A. Muller, Belton has obtained observations of comet P/Wirtanen from CTIO with the goal of constraining the rotation state of the the comet's nucleus which is a target of the ESA Rosetta mission. A long time-series covering three months and sampled on 11 nights is currently being analyzed. In earlier work with Muller and N. Samarasinha it was shown from the limited data available, that the large production rate inferred for the comet and its small size that the nucleus would likely be in a state of complex rotation. Whether this is, or is not the case may be discovered in this data set. Belton is also working on the interpretation of Galileo SSI observations of Io in eclipse, and new very high resolution observations of Europa that seem to indicate that a weak liquid, or slush, layer exists a few kilometers below the surface in some regions. The Io data shows patchy Io-glow associated with a few areas. The Europa data shows evidence for geologically recent ice-floe/ice-pack activity in some regions.
Xlll Belton plans to expand his investigations of Io and Europa with the Galileo data. Europa will be the focus of his Galileo SSI team as they plan the observational sequences for the two year extension of the nominal mission to 2000. He also plans to work with Imke dePater (UC Berkeley), to see if the Hat Creek interferometer is sensitive enough to map S02 on Io. The goal is to improve our knowledge of volcanic plume dynamics and to characterize the sources and sinks of the primary atmospheric gas. Belton is also involved in other cometary and Jupiter system projects. Some of these stem from his leadership of the Galileo imaging team and others from participation in Hubble Space Telescope projects already granted time. These include an investigation of the partially gravitationally bound radial structure of Chirons atmosphere (with K. Meech, U. of Hawaii), an investigation of the composition of the Pele plume on Io (with Melissa McGrath, STScI), and an investigation into the development and dissipation of atmospheric features in Jupiters atmosphere (with Reta Beebe, New Mexico State U.).
Service Beltons service activities are primarily in the planetary astronomy community where he is Chair of the NASA IRTF Management and Operational Working Group and Chair of the NASA/Keck Observatory Management and Operations Working Group. In addition he is a member of the NASA Planetary Astronomy Committee, and the NASA Small Bodies Science Working Group. Within NOAO he provides appraisals and advice to the Director on planetary astronomy observing proposals. He has also sponsored two successful IDEA education outreach programs at NOAO.
Bruce Bohannan
Areas of Interest Stellar Spectroscopy, Structure and Evolution of Massive Stars, Astrophysical Instrumentation and Data Reduction
Recent Research Results Bohannan's research centers on observational studies of the evolution of massive stars. Massive stars, through their radiation, mass loss, and supernovae explosions, dominate the chemical element evolution and kinetic energy of their parent galaxies. Because of their high luminosity, such stars are readily observed to great distance in the Milky Way and in other galaxies. The evolution of these stars is poorly understood because models are not readily connected to simple spectral morphology which underlies stellar astrophysics. Bohannan and his colleagues have used the measurement of basic stellar properties (temperature, gravity, mass, mass loss rate, and surface element abundances) to define the evolutionary path of massive stars and to make connections between various stages of massive star evolution, stages most readily observed as morphological differences. For example, P.A. Crowther (University College, London) and Bohannan (1997 A&A 317,532) recently concluded that a direct evolutionary connection may exist between certain hot, massive stars (those classified as 08 Iafpe) and a later stage of stellar evolution (low excitation WN stars) without an intermediate stage of rapid and unstable evolution (commonly known as Luminous Blue Variables), a conclusion which is contrary to current evolutionary theory and suggestive that an additional process (e.g., mixing) brings core processed material to the surface.
Future Research Plans Similar investigations of stars in the Galactic Center and in other galaxies provide critical diagnostics of stellar evolution because they can examine the effect of different stellar environments on stellar evolution. Such studies require infrared observations because of extreme interstellar absorption (e.g., in the Galactic Center) or severe crowding of stellar images (e.g., other galaxies). The IR diagnostics are being developed with Crowther and tested through a set of spectral line profiles recently obtained at CTIO and analyzed with Hillier model atmospheres (Bohannan and Crowther 1997, in preparation). The
xiv next stage will be to analyze a set of Of and WN stars in the Large Magellanic Cloud, to be followed by observations of stars in the Galactic Center thought to be of similar spectral morphology. The final step would be to undertake a similar study of stars in the nearby spiral galaxy, M 33, research which requires a moderate resolution IR spectrometer combined with an image compensation system to provide high spatial resolution (e.g., tip-tilt and fast focus).
The theory of radiatively driven winds provides simple analytical expressions which link the mass, luminosity and effective temperature of a star to the observed mass loss rate and terminal velocity. The analytical expressions use parameters which are related to the number of lines responsible for driving the wind, the opacity of the lines, and the ionization structure of the wind. These parameters are now sufficiently well established that one can use the analytical expressions in an inverse fashion to measure stellar masses from spectroscopic analysis using detailed models which determine the effective temperature, mass loss rate and terminal velocity for stars of known luminosity (i.e., of known distance). Bohannan and Crowther have begun to apply this technique to a group of peculiar stars in the Large Magellanic Cloud which have the characteristics of both hydrogen-burning Of stars and helium-burning WN stars and which have massive circumstellar shells from either a LBV or red supergiant phase. The determination of a stellar mass for these stars is critical in defining the evolutionary path of the stars and defining the origin of the circumstellar shell. The method they are developing is the only way to measure stellar masses as none of these stars are in binary star systems and few are in clusters and associations. Tracks of stellar evolution do not provide reliable masses because of the unknown effect of stellar rotation on luminosity and effective temperature.
Service Service is Bohannan's primary role within NOAO. As KPNO Assistant Director for Operations and Projects, Bohannan has day-to-day and long-range supervisory responsibility for all Kitt Peak-based activities, including electronic and computer maintenance, and instrument and observing support for astronomers using KPNO telescopes. Personnel reporting to him also provide electronic maintenance for the National Solar Observatory site on Kitt Peak. He works with Tucson-based engineering personnel on telescope and instrument improvement projects. Major projects in the past year involve improvement of the optical performance at the Mayall 4-m telescope through cooling of the primary mirror and the design of a dome ventilation system. Major activities for the coming year include continuing work on improving the optical performance of the 4-m telescope (installation of the Mayall dome ventilation is to begin during summer shutdown 1997, to be completed in FY 1998) and implementing a preventative maintenance system for the telescopes and ancillaries.
Charles F. Claver
Areas of Interest Stellar Ages, White Dwarf Structure and Evolution, Stellar Photometry, Optical Instrumentation
Recent Research Results Claver's research focuses on obtaining an independent estimate of the Universe's age, and in doing so, resolving the apparent discrepancy between the expansion age and the main-sequence age of the oldest stars we see—the globular clusters. The age dating technique Claver uses exploits the relatively simple physics found in the cooling remnants of stellar evolution—white dwarf stars. The age of a white dwarf is directly related to its luminosity, and any reasonable estimates for the age of the Universe still allow for the oldest white dwarfs to be visible. Therefore, a census of white dwarfs according to their brightness—called a luminosity function—in any stellar population will show an abrupt cut-off at low luminosities that is dependent on the population's age. Claver has used this fact in observations of white dwarfs in the open clusters Praesepe and NGC 752 to show the white dwarf and main-sequence ages are
xv in good agreement up to 3 billion years old. If the agreement persists at older ages, then we can be confident in the ages of the globular cluster; the current estimate of Hubble's constant would not then allow for a simple inflationary cosmology, and a more complex one would be demanded. Otherwise, if the agreement breaks down beyond ages of 3 billion years, then we must be suspect of the estimates of stellar ages and re-evaluate the state of stellar evolution calculations.
To date, all estimates of the white dwarf luminosity function for the Galaxy's disk suffer from poor statistics at their faint ends, and prevent us from fully utilizing the excellent clocks offered to us by white dwarf stars. Thus, age estimates for the Galactic disk from these luminosity functions range from 8-13 billion years, which is not precise enough to help resolve the age dilemma. As part of Claver's thesis work he developed a method for identifying cool white dwarf candidates from photometry alone. With his technique, Claver has initiated a deep photometric survey to search for cool white dwarfs in the field. To date, Claver's survey has covered enough area to improve the number statistics in the cool part of the disk white dwarf luminosity function by a factor of 3-5 over previous estimates.
Future Research Plans Over the next several observing seasons Claver plans to continue spectroscopic follow-up observations with WIYN Hydra of his cool white dwarf photometric survey. The cool white dwarfs identified will be used to redefine the cool part of the white dwarf luminosity function (WDLF). These data are important not only for estimating the Galaxy's age, but also for placing an observational constraint on the importance of phase separation of a carbon-oxygen mixture in crystallization of white dwarf cores. Phase separation, if it happens, releases additional energy into the white dwarf core further delaying the cooling process beyond the delay caused by the release of latent heat. The exact nature of white dwarf crystallization causes observable features in the WDLF and has a large effect on the inferred white dwarf cooling ages. Claver will also work toward increasing the area of his survey in order to increase the detection sensitivity of older, cooler white dwarfs belonging to the Galactic Halo. He plans to extend his work on calibrating the stellar chronology in star clusters to ages older than 3 billion years. Specifically, in collaboration with Don Winget (U. of Texas), Mike Bolte (Lick Obs.) and Matt Wood (FIT), he plans to search for and identify the oldest white dwarfs in the clusters M67 and NGC 188 in the North and IC4651 and NGC 3680 in the south using both ground- and space-based telescopes. These clusters will extend the calibration to roughly 8 billion years, which is sufficient to constrain the source of the present differences in the Universe's expansion age and its oldest stars.
Service Within the Kitt Peak scientific staff, C.F. Claver holds the title of Imaging Scientist. As part of his service activities he has begun a coherent, comprehensive look at the imaging quality produced by Kitt Peak telescopes with the aim of having all Kitt Peak telescopes deliver the excellent seeing of which the site is capable. To this end Claver has taken on the responsibility of overseeing and maintaining optical alignment of Kitt Peak telescopes, as well as debugging problems. As a member of the 4-m imaging improvement group, Claver is investigating the performance of the 4-m primary support system to determine if and where significant improvements can be made in the delivered image quality of this valuable telescope. Claver has conducted a study of high frequency image motion at WIYN. Analysis of these data by Claver and others is providing essential information for the development of an Adaptive Optics program for WIYN. Claver also serves the Kitt Peak Visitor Center by answering questions and reviewing material for their docent program.
Arjun Dey
Areas of Interest Galaxy Evolution, Observational Cosmology, the High-Redshift Universe, Active Galaxies
xvi Recent Research Results Dey is an NOAO postdoctoral fellow. His primary research interests are the evolution of galaxies and active galactic nuclei, and observational cosmology. He has recently demonstrated that the UV continuum emission from high-redshift radio galaxies is largely non-stellar in origin, and that these radio galaxies harbor hidden quasar nuclei. This result provides strong support for unification theories of AGNs (i.e., that radio galaxies are quasars, whose beamed radiation is directed in the plane of the sky rather than towards us). In addition, he and his collaborators are studying the stellar content and ages of high-redshift galaxies. They have recently discovered two galaxies at redshifts z> 1.4 with ages greater than 3.5 Gyr which provide strong constraints on the age of the Universe.
Future Research Plans During the next two years, Dey will continue to investigate the stellar content of distant galaxies in order to determine the earliest epoch of galaxy formation. Although the observed optical emission from radio galaxies is non-stellar, the infrared radiation is most likely dominated by starlight, and Dey will investigate the infrared properties of high redshift radio galaxies with the aim of utilizing these luminous galaxies as cosmological probes. Dey's future research will also be directed at understanding the formation and evolution of massive galaxies. There is growingevidence that young galaxies may be dust enshrouded, and he will investigate the properties of a newly discovered population of very red galaxies. (Dey received a Hubble fellowship and will be leaving NOAO at the end of CY 1998.)
Service Dey participates in the Observatories' service activities. He helps new visiting observers acquaint themselves with the telescopes and imaging cameras, and aids them in using the facility instruments effectively and efficiently. In collaboration with staff member Buell Jannuzi, Dey is designing and will undertake a public very deep wide-field optical and IR survey of the sky using NOAO telescopes. The primary goals of this survey are to enable the study of the evolution of large scale structure in the redshift range z~l-4, investigate the formation and evolution of distant galaxy populations, and detect luminous and distant star-forming galaxies and quasars. Since such a survey will also prove invaluable for the study of various other scientific issues, the survey data will be made public in a timely manner. The timescale for completion of the proposed survey is two years and therefore samples of faint objects selected from the survey will be available for spectroscopic follow-up using NOAO's 8-m Gemini Telescopes.
Richard F. Green
Areas of Interest Active Galactic Nuclei, Quasar Absorption, Line Systems, Galaxy Nuclear Dynamics
Research Plans Richard Green is a member of the Instrument Definition Team for the Space Telescope Imaging Spectrograph. He leads an Internal Key Project to perform a census of supermassive black holes in the nuclei of early-type galaxies. He is also a member of the "Nuker" proposal team that won a number of orbits in Cycle 7 to perform a complementary survey. The two teams have coordinated their observing approach and will analyze the stellar absorption profiles at the calcium triplet to deduce the presence and mass of any central black hole. An initial success was M84, an elliptical in the Virgo Cluster. Research Associate Gary Bower suggested this object because of its 3C radio source and morphology of emission- line gas near the nucleus. Its central gas disk showed nearly Keplerian motions, suggesting a dark mass of (3 - 8) x IO8 M_.
xvn Green is a member of the Medium Deep Survey team working with the Hubble Space Telescope parallel imaging survey. Early studies have focused on the evolution of galaxy morphological properties as a function of redshift. Current work with Vicki Sarajedini (thesis student at Steward Obs.) concentrates on identifying faint active galactic nuclei as unresolved point sources in the high-resolution Wide Field Camera images. The result will be tracing the incidence of lower level nuclear activity out to redshifts of 0.5 to map the increase of non-thermal power with cosmic lookback time.
Green also collaborates with B. Jannuzi in determining the association of low-redshift Lyman alpha absorption clouds with the large-scale structure of galaxies. They are conducting an imaging and redshift survey to concentrate on the range 0.1 < z < 0.4.
Service Deputy Director, NOAO; Director, KPNO
George Jacoby
Areas of Interest Galaxy Distances, Dynamics, and Chemical Compositions, Planetary Nebulae
Recent Research Results G. Jacoby developed a method based on the brightnesses of planetary nebulae to measure the distances to galaxies. Using the KPNO 4-m telescope, he and collaborators R. Ciardullo and J. Feldmeier (Penn State U.) recently extended this method to four spiral galaxies (M96, M101, NGC 300, and M51) where a comparison to the well-known Cepheid method is possible, and thereby demonstrated that planetary nebulae yield distances accurate to about 7%. His results from recent analyses of nearly 20 galaxies indicate that the Hubble Constant is about 75 km/s/Mpc. In a related project, he has identified 320 planetary nebulae in the giant Virgo elliptical galaxy M87 for the purpose of measuring the motions of several hundred stars. Surprisingly, about half of these PN appear to have no association to M87 or any other galaxy—that is, they are intracluster stars. From these it is possible to map out the three- dimensional distribution of matter in M87 and the Virgo cluster, in general, and identify the presence and location of any dark matter. Motions will be measured in the next few months using the Hydra multifiber spectrometer on the WITN telescope. Prior work on giant ellipticals (Cen A, M86, NGC 1399, NGC 3379) has shown that each galaxy has unique dynamical properties: some have complex rotational and triaxial motions, some have dark matter, and others appear to have simple motions with no evidence for dark matter. A similar project is underway for our own Milky Way Galaxy, where G. Jacoby found 95 new planetary nebulae in its central 500 pc. Velocities have been measured for about 40 of these, and many of the remaining objects will be observed at CTIO shortly with collaborator G. Van de Steene (ESO). G. Jacoby has just completed a survey for planetary nebulae in the Milky Way globular cluster system. Earlier investigators have failed to find any nebulae, but he found one object in NGC 6441, and a probable second nebula in the small cluster Pal 6. An analysis of the abundances in NGC 6441 indicates that the stars in the cluster are deficient in oxygen, an element that controls, to some degree, the rate of burning in the stellar core. The low oxygen abundance implies that the stars in this globular cluster are older than previously thought, perhaps by 2 billion years.
Future Research Plans The observation and analysis of planetary nebula motions in galaxies is of growing interest because there is no better way to measure the stellar velocities. There are many candidate galaxies, and no physical trends have surfaced yet among the few galaxies that have been observed. This technique also applies to the bulges and disks of spiral galaxies. G. Jacoby and collaborators have accumulated velocities for over 800 nebulae in the nearby Andromeda galaxy, and the analysis is underway. Preliminary results show
xvin that the bulge of the galaxy is rotationally supported. Also, there are about 10 times fewer stars in the galaxy halo that produce planetary nebulae than initially thought, possibly evidence for either a very low mass or a very old halo. The observations of the Galactic center nebulae will help define the motions of stars in the central "bar" of our Galaxy, as well as flagging any nebulae that originated in the halo of our Galaxy but are presently passing near the Galactic nucleus; already, two very fast moving candidates have been identified as possible halo visitors. The spectra of the Galactic center nebulae also will allow Jacoby to determine the chemical compositions of the nebulae, from which the composition of their progenitor stars follows. That, in turn, provides an alternative means to measuring the chemical composition in a region of our Galaxy where abundances traditionally have been very hard to measure due to intervening dust. Our Galaxy is not the only difficult place to measure chemical compositions; for decades, there has been suspicion of gradients in the compositions of stars in elliptical galaxies based on the increasing blue color of the integrated light from those stars as one looks outward from the center. There is no direct way to measure those compositions. Planetary nebulae, however, by virtue of concentrating their energy into a few key emission lines, allow measurement of the compositions. The techniques for observing extragalactic nebulae are well known and have been tested recently in the center of the Andromeda galaxy using the Kitt Peak 4-m telescope in a multi-slit configuration. The same approach, using the Gemini telescopes, will allow a direct measurement of the compositions of nebulae (and therefore the stars) in distant elliptical galaxies for the first time.
Service Jacoby's service responsibilities fall into three primary areas. He is the project scientist for the IRAF project, setting priorities and giving scientific direction to the project, interfacing between the programmers and the users, NOAO management, and outside organizations interested in the project (STScI, AXAF, EUVE), and is the PI for the Open IRAF initiative being funded by NASA. Jacoby serves as the telescope scientist for the WIYN telescope, helping to set scientific priorities for continuing work on this new telescope. In addition, he is the project scientist for the new optical correctors recently built for the 4-m and 0.9-m that are required to provide the very wide fields of view (50' and 80', respectively) needed by the NOAO CCD Mosaic camera. Jacoby also serves as a member of the scientific organizing committees for the annual Astronomical Data Analysis and Software Systems conferences, and the LAU Symposia on Planetary Nebulae.
Richard R. Joyce
Areas of Interest Late-type Stars; Mass Loss; Infrared Detector and Instrumentation Development
Recent Research Results Joyce has completed an infrared spectroscopic survey of a sample of faint carbon stars near both Galactic poles. Because carbon giants are very luminous, with sharp optical spectral bands which make radial velocity measurements possible for faint stars, they are excellent candidates for kinematic studies of the outer Galactic halo. A past complication has been the identification of carbon dwarf stars (nearby main- sequence dwarfs which have been enriched with carbon by mass transfer from a now-evolved binary companion) whose optical spectra at modest resolution are sufficiently similar to those of carbon giants to cause confusion between the two. The infrared spectroscopy shows that those stars known to be carbon dwarfs (from their high proper motion) show weak or barely detectable (depending on metallicity) absorption in the first overtone of CO at 2.3 microns, whereas virtually all the other stars in the survey displayed the much stronger CO bands characteristic of giants. These results support the suggestion of Green, et al. (1992, Ap. J. 400. 659) that near-infrared broadband photometry, which is more feasible than infrared spectroscopy or proper-motion measurements for these faint stars, may provide an effective luminosity discriminant.
xix As part of a multi-wavelength collaboration, Joyce has also obtained infrared spectra (0.9-2.5 microns) of the binary object that may be associated with the Soft Gamma-ray Repeater 1900+14. The two heavily- reddened objects, separated by 3 arcsec, have virtually identical energy distributions, suggesting that the extinction must be interstellar and that the two objects are M5 supergiants at a distance of 12 - 15 kpc, on the other side of the Galaxy. While this is highly unusual, it does not by itself connote an association (other than positional coincidence) with the gamma ray emission, which is conventionally believed to result from mass accretion onto a highly-condensed object such as a neutron star or black hole. If such an object lies in proximity to one of the two stars, one might expect to see subtle differences in their spectra. One such anomaly is observed in the moderate-resolution (700) infrared spectra: while the two stars have virtually indistinguishable spectra in the 1.5-1.8 micron range (which includes several atomic lines and the CO second-overtone absorption bands), there is a significant difference in the depth of the CO first- overtone absorption bands at 2.3 microns, possibly the result of hot circumstellar dust filling in the absorption lines in one of the stars. Preliminary observations with the high-resolution LR spectrograph PHOENIX indicate that the two stars have similar radial velocities, and continuing monitoring is planned to search for any velocity changes which might result from a massive component in proximity to one of the two stars.
C. Pilachowski, K. Hinkle, R. Joyce, and C. Sneden (U. of Texas) have used PHOENIX to obtain high signal-to-noise spectra of the first-overtone infrared bands of CO in metal-poor giant stars. These spectra allow the determination of the ratio of I3C to 12C, which is diagnostic of the degree to which material in the outer convective portion of these stars has been mixed with the LC-rich shell within which CN cycle hydrogen burning is taking place. Use of the infrared CO bands, rather than the blue visible CH bands, for isotope ratio determination significantly increases the available sample of stars for study because late- type giants are much brighter at 2 microns and the CO bands themselves are intrinsically strong.
Future Research Plans Future research plans include the use of high-resolution infrared spectroscopy, largely with PHOENIX, for a variety of stellar studies. Three primary factors can dictate the use of infrared spectroscopy as a diagnostic tool: 1) high extinction in the visual may preclude spectroscopy; 2) dynamic events such as mass transfer in binaries may produce visual emission which confuses the optical spectra; or 3) the physical process produces spectral effects only in the infrared. Examples of these follow.
The Soft Gamma Repeater 1900+14, which suffers 19 mag of visual extinction, is much more amenable to radial velocity studies in the infrared, and the manifestation of a thin hot dust shell may be apparent only in the CO absorption lines at 2.3 microns. An example of the second category is a collaborative project involving Joyce, K. Hinkle (NOAO), and F. Fekel (Tennessee State U.) to determine orbits of symbiotic stars from their infrared spectra. These systems are interacting binaries in which one star is a cool giant and the other a hot main sequence star or white dwarf. Orbital determinations from optical spectra have been problematic, since these spectra are often dominated by the continuum from the energetic and irregular mass flows associated with the stellar interaction.
The infrared spectrum, on the other hand, is almost completely that of the cool giant, and an unambiguous velocity determination of one of the stellar components is possible. This project has already been initiated, utilizing the University of Massachusetts NICMASS LR camera to observe the CO bands in the 1.6 micron region. We have already demonstrated that PHOENIX can obtain the same radial velocity accuracy much more efficiently. The results would not only confirm that symbiotics are mass- transfer binaries, but given the constraints on the mass of a white dwarf secondary, could yield accurate masses for cool giants over a range of evolutionary stages.
xx The third category is exemplified by a recently-initiated project involving Joyce, Hinkle, and C. Sneden (U. of Texas) to observe the He I line at 1.083 micron in metal-poor giant stars. These stars may be considered analogs to the red giants in globular clusters. One such star has been reported in the literature to show a 1.083 micron feature indicative of a high-speed (> 90 km/s) wind. Since this velocity exceeds the escape velocity from globular clusters, the presence of such high-speed winds from metal-poor field stars would suggest a mass loss mechanism for globular cluster giants which could expel matter from the cluster itself and plausibly explain the observed low density of the interstellar medium in globular clusters. Results for a number of stars are being prepared for publication.
Service As a Support Scientist, a significant fraction of Joyce's time is spent in providing observing support to visiting observers using the facility instruments CRSP (a low-resolution LR spectrograph), LRLM (LR imager), and PHOENIX (the recently completed high-resolution LR spectrograph), and the LR imaging spectrograph ONIS, which is shared with the MDM Observatory under a cooperative agreement. Service includes direct support such as checking out the instruments after installation, providing instruction to observers, training the Kitt Peak mountain staff in technical issues associated with these instruments, off line support in providing advice to prospective observers, and assistance with data reduction. Joyce is the capability scientist for infrared spectroscopy with CRSP, as well as co-instrument scientist on PHOENIX (which has entered service but is still being optimized), and has initiated the process of concept definition for a next-generation wide-field LR imager for Kitt Peak. He is responsible for the scheduling of the Kitt Peak telescopes and is overseeing the development of the scheduling portion of the new ALPS++ database. Other service areas include serving on the Infrared Group, KPNO Advisory, ALPS++ Definition, and KPNO Safety Committees, and being the editor for the KPNO section of the NOAO Newsletter. He will also be involved with the US Gemini Program in developing similar "user support" mechanisms for community users of IR instrumentation on Gemini.
Tom D. Kinman, Astronomer Emeritus
Areas of Interest Galactic Structure, Galactic Halo, Horizontal Branch Stars
Recent Research Results The oldest stars in the Galaxy are found in the Galactic Halo; it is by studying these stars that we are most likely to discover how the Galaxy was formed. The Horizontal Branch Stars are a relatively uncommon type of Halo star that make excellent tracers of the Halo because they are less easily confused with the more numerous Disk stars than are other Halo stars. Kinman has spent the last few years searching several hundred square degrees of sky to find the brighter horizontal branch stars within a few kiloparsecs of the Sun. These stars were originally identified in various objective-prism surveys with Schmidt telescopes. Kinman has observed these stars in 5 wavebands (using a CCD on the 0.9-m telescope) so as to pick out the stars whose colors make them highly likely to be Horizontal Branch Stars. With N. Suntzeff (CTIO), Kinman has been taking spectra of these stars at the 4-m telescope in order to get their radial velocities, their metallicity, and a final confirmation of their classification. This sample is being used to study the kinematics and space distribution of the Galactic Halo within a few kiloparsecs of the Sun. Last year, it was shown that a "streaming motion" is present among some of the Halo stars near the North Galactic Pole. This year, a few proper motions for these stars have become available from the new GSC2 catalog as a result of collaboration with an Italian consortium (PI, C. Cacciari, STScI). These data allow one to compute the galactic rotation of the halo relative to the extragalactic background, and it is found to be more like 300 km/s rather than the 220 km/s found in the solar neighborhood.
xxi Future Research Plans Kinman hopes to complete the final photometric and spectroscopic observing during the coming year so that we have a relatively complete dataset of nearby halo stars. It is expected that more proper motions from the GSC2 for the North Galactic Cap will become available during the year so that our kinematic analysis can be extended. The advent of the Hipparcos and Tycho data (that should greatly improve our knowledge of the absolute magnitudes of these objects) will be particularly timely. It should be noted that Kinman's photometry is being fed back into the GSC2 system, so that the GSC2 magnitudes should be significantly improved in this area of the sky; many GSC2-related programs should benefit from this. Kinman also has related programs with C. Allen (UNAM, Mexico City) and C. Cacciari (STScI) to study the Horizontal Branch Stars of the solar neighborhood.
Service Kinman provides informal support to the Library and elsewhere in the Observatory on request.
Roger Lynds
Areas of Interest Galaxy Evolution and Cosmology
Recent Research Results Lynds has been engaged in completing an investigation of the star-formation history of VLI-Zw-403, usually classified as a dwarf irregular galaxy. Images obtained with the Hubble Space Telescope resolve the galaxy into individual stars and reveal especially the fact that the young, luminous blue stars that are responsible for the irregular classification occupy the central region of a dwarf elliptical galaxy. The color-magnitude diagram (CMD) derived from the stellar photometry displays a blue plume consisting of young main-sequence and supergiant stars, mostly confined to clusters and H U regions near the center of the galaxy, as well as a red plume of supergiants that are somewhat more dispersed than the blue stars. In addition, the red giant branch (RGB) is abundantly populated by stars that comprise the much larger underlying elliptical galaxy of older stars. But the most noteworthy feature of the CMD is a well developed asymptotic giant branch (AGB) consisting of stars that must have a metallicity at least of the order of 1/20 the solar value and an intermediate age of the order of 1 Gyr. It happens that the location of the RGB is exactly where one would expect to find not only the red giants associated with such an AGB population, but also red giants from a much older, metal-poor (1/100 solar) population. Is then the elevated metallicity of the AGB population due to a precursor low-metallicity population or to some unknown "cosmological" contaminating event? The relationship between the distribution of stars in the CMD and in space seems to give at least a partial answer: the totality of RGB stars are more widely dispersed spatially than are the AGB stars; there was a star-formation event prior to what must have been a spectacular starburst responsible for the AGB population! Even though VLI-Zw-403 is not entirely young, or even of intermediate age, it is tempting to suppose that the galaxy during its "AGB" starburst must have looked much like the blue dwarf galaxies at comparable look-back times that are being revealed by deep imaging with HST. Collaborators in this investigation have been D. Hunter (Lowell Obs.), E. O'Neil (NOAO), and E. Tolstoy (Space Telescope, European Coordinating Facility).
Future Research Plans Lynds' future research will include VLA 21-cm mapping of VLI-Zw-403 and another galaxy as an exemplar of a dynamically induced starburst. In addition, he will continue work on the integrated properties of galaxies in the various HST deep imaging fields.
xxn Service Lynds has been an active member of the observatory Safety Committee and is one of the instrument scientists for the 4-m Prime Focus CCD Camera.
Philip Massey
Areas of Interest Massive Star Evolution, Star Formation, Resolvable Galaxies
Recent Research Results Massey's research is primarily aimed at understanding the formation and evolution of massive (> 10 MQ) stars. Using the best groundbased and space-based instruments, he has been investigating the stellar content of star-forming regions in the Magellanic Clouds, the Milky Way, and the more distant members of the Local Group. This year, Massey produced a catalog of the UV-brightest sources in the Local Group galaxy M33 using images obtained with the Ultraviolet Imaging Telescope, in collaboration with L. Bianchi (STScI) and J. Hutchings (DAO). Spectra obtained with WIYN were then used to probe the massive star content of this nearby spiral. Their survey identified OB stars as early as spectral type 06. Most significant, however, was the discovery of five stars spectroscopically identical to known Luminous Blue Variable stars (LBVs). LBVs are a poorly understood stage in the evolution of massive stars, and previously only four examples were known in M33. In addition, their survey discovered six "Ofpe/WN9" stars, also believed to be related to LBVs.
Future Research Plans Massey, in collaboration with D. Hunter (Lowell Observatory), is using HST to investigate the massive star content of R136, the central cluster in the 30 Droadus Nebula in the Large Magellanic Cloud. Once thought to be a single, supermassive object, groundbased speckle and WFPC images established that R136 is actually even more interesting: a "super star cluster," possibly what all globular clusters looked like when they were only a few million years old. Spectra have now been obtained of the brightest, bluest 50 stars in this cluster, with the surprising result that most of the stars are of type 03—the hottest, most luminous stars known. The data will be combined with HST photometry to determine the initial mass function of this highly intriguing object. In addition, Massey's goal over the next few years is to establish empirically the mass range of objects that evolve to various types of Wolf-Rayet stars (a type of massive star that is in the last stages of its life), and to understand how this changes with metallicity. He plans to determine this by investigating the top of the H-R diagram in coeval populations in the Magellanic Clouds, M33, and M31, for which he has determined the Wolf-Rayet and red supergiant populations. This involves optical spectroscopy with the 4-m and WLYN, plus UBV imaging with the Hubble Space Telescope.
Service Massey is now the Telescope Performance Astronomer. As such, Massey is responsible for seeing that the Kitt Peak telescopes are used to maximum scientific advantage. His responsibilities include the identification of maintenance problems and software issues, overseeing the monthly Testing and Evaluation time scheduled on each telescope, and working towards improving the delivered image quality, particularly at the 4-m. Massey is also involved in user documentation, and has written and continues to update the visitor manuals for the CCD data-taking software ICE, the direct imaging (CCD) manual, the low-to-moderate resolution spectroscopy manual, and the operation manuals for the 0.9-m and Burrell Schmidt telescopes, as well as data reduction guides for crowded field photometry, CCD reductions, and spectroscopic reductions. Massey also wrote and maintains the software for computing the optimal assignment of fibers to objects with the Hydra multi-fiber spectrometer used on the WIYN telescope, and interacts with visitors as needed.
xxiu James Rhoads
Areas of Interest Galactic Structure, Stellar Populations, Gravitational Lenses, Gamma Ray Bursts, Dust
Recent Research Results Rhoads's recent research results include a study of the 2.3 micron CO index in nearby galaxies, whose results indicate that young stellar populations can locally dominate the emission from star forming regions in a galaxy even at near-infrared wavelengths, although their contribution to the total near- infrared light of the galaxy is modest.
In collaboration with W.N. Colley, J.P. Ostriker, O.Y. Gnedin, and D.N. Spergel (Princeton U.), Rhoads has been studying the correlation function of faint sources in the Hubble Deep Field. This work has shown that many close pairs or multiplets of sources in the Hubble Deep Field are most likely star forming regions within a single galaxy that appear as separate sources because of redshift effects. Alternative explanations for the observed correlations (e.g., merger or satellite accretion models) face dynamical difficulties.
S. Malhotra (Infrared Processing and Analysis Center), Rhoads, and E.L. Turner (Princeton U.) have recently shown that radio-selected gravitational lens systems are redder than optically-selected systems, which is possible evidence for dust in lensing galaxies. This suggests that a large fraction (about half) of gravitational lens systems are hidden from optical surveys by dust. Previously published limits on the cosmological constant Lambda based on the statistics of gravitational lenses may have to be relaxed. Rhoads is also a member of a team headed by Turner that has been monitoring gravitational lenses to obtain time delay measurements and hence determine the Hubble constant.
Recently, a radio counterpart to a gamma ray burst has been observed, at about the flux level and time delay predicted by Paczyski and Rhoads (1993). Rhoads has now submitted a paper to the Astrophysical Journal Letters pointing out that the relative frequencies of radio-optical transients and of gamma ray bursts can be used to determine whether gamma ray bursts are strongly beamed or not. The presence or absence of such beaming can change the estimated event rate by several orders of magnitude, affecting what classes of objects are plausible gamma ray burst sources.
Future Research Plans Rhoads plans to spend the summer developing and applying methods for probing the structure of our own Galaxy using the near infrared colors and fluxes of stars, in collaboration with C. DeLoye (REU student). Additionally, Rhoads is working on theoretical aspects of the reddening to extinction ratio for dust in clusters of galaxies, and hopes to obtain [in collaboration with I. Dell'Antonio and G. Kochanski (Lucent Technologies)] a direct measurement of this reddening law. This work may help address discrepant published estimates of the dust abundance in clusters of galaxies. Rhoads also hopes to do further work on Gamma Ray bursts, exploiting the recent observational breakthrough (detection of counterparts at low energies) made possible by the BeppoSAX satellite to learn about the physics of gamma ray bursts and the nature of their environments. Finally, Malhotra and Rhoads plan to do further work on dust in gravitational lens systems. In collaboration with E.L. Turner (Princeton U.), G. Helou, and R. Cutri (Infrared Processing and Analysis Center), they have obtained Infrared Space Observatory mid-infrared spectrophotometry for two bright gravitational lens systems with other evidence for dust. If the data is of sufficient quality, it should be possible to see the 9.8 micron silicate absorption feature in these spectra, which will provide spectroscopic confirmation of the dust. Rhoads and Malhotra further hope to look for
xxiv color differences between different lens components, which should obey a plausible dust reddening law if dust is present in lenses.
Service Rhoads helps new visiting observers acquaint themselves with the telescopes, and assists them in using the facility instruments effectively and efficiently. He will also be among the first shared-risk observers using the CCD Mosaic camera, and will provide feedback to the Mosaic team.
Stephen T. Ridgway
Areas of Interest Stellar Astronomy; Advanced Instrumentation
Recent Research Results S. Ridgway, in collaboration with colleagues from the University of Paris Meudon Observatory and the Harvard-Smithsonian Center for Astrophysics, has deployed the prototype optical fiber detection system FLUOR at the Infrared Optical Telescope Array on Mt. Hopkins. The FLUOR device was developed at KPNO during an earlier phase of this collaboration. With FLUOR, the team has achieved photon-limited accuracy in the measurement of interferometric visibilities, a significant advance in the field of optical interferometry. This capability has been employed to extend the calibration of very cool giant stars to the latest spectral classes. It has been found that the M8 class giants have an effective surface temperature of only 2780 degrees Kelvin. While cool, this is nearly 500 degrees hotter than estimated earlier by less precise techniques. A careful calibration of stellar temperatures is critical in the comparison of computer models with actual stars. The study of individual cool stars is important for advancing our understanding of the physics of the cool atmospheres, which will eventually culminate in useful models of the coolest stars, brown dwarfs, and protoplanets. Though models of individual stars this cool are not yet reliable, the calibration is already very useful in the analysis of galactic evolution. Computer models of galactic evolution predict the mix of stars in a galaxy, and color calibrations must be employed to convert the model to characteristic observable properties.
Future Research Plans NOAO will continue under contract to support the Georgia State University Center for High Angular Resolution Astronomy (CHARA) interferometric array project. Ridgway will continue his role as technical consultant, with emphasis next year on integration of the first telescopes, installation of the delay lines, and design of the vacuum beam transport system. The CHARA Array offers a unique combination of collecting area and angular resolution. When it becomes operational, toward the year 2000, it will supply a rich return of fundamental stellar data, including temperatures, diameters, and masses, and it will be a valuable testbed for the development of interferometric technology.
Service Ridgway provides technical advice to the NOAO/Gemini community on adaptive optics and interferometry. He is a frequent lecturer at NATO summer schools on these topics, and participates in NASA advisory groups on Keck and space interferometry. He assists with test and evaluation of the new Phoenix high resolution infrared spectrometer. Effective in 1997, Ridgway is the NOAO representative on the KPNO Galactic Telescope Allocation Committee.
Paul S. Smith
Areas of Interest Active Galactic Nuclei, Polarimetry
xxv Recent Research Results P. Smith has completed a study of the polarization of two low-redshift, radio quiet active galactic nuclei (AGNs), I Zw 1 and Mrk 486. This study is the first to conclusively show that the non-synchrotron polarization of some radio quiet AGNs can vary on time scales as short as a few years, implying that some of the material that produces the polarized flux by scattering nuclear radiation resides very close to the nuclear continuum source. In the case of Mrk 486, there is additional evidence for the close proximity of the scattering material to the nucleus from the polarization signature observed in its broad, permitted emission lines. The polarization of the spectral lines can best be explained if the this object's broad-line region (BLR) consists of two distinct regions: a true BLR, and an intermediate-line region (LLR). The differing polarizations of the two regions require that the scattering material be, to some degree, intermixed with the line-emitting gas, and therefore be located within a few parsecs of the nucleus. During the past several years, optical and UV spectropolarimetry has proven to be one of the most powerful techniques in the investigation of the structure of AGNs. In particular, polarimetry has advanced the notion that the AGN ionizing flux does not emerge isotropically from the nuclear region, implying that our viewing perspective is an important factor in determining the differences observed between various types of AGNs. An obscuring torus of material prevents direct observation of the inner nuclear regions if the torus intersects our line of sight. For example, the blue ionizing continuum and line emission from the BLR are not apparent in the spectra of Seyfert 2 nuclei, but can be seen in the spectrum of the polarized flux. The nuclear light is believed to be scattered into our line of sight by material distributed around the AGN. That is, if we were able to observe a Seyfert 2 nucleus from a direction in which the torus does not block our view, a Seyfert 1 nucleus would be observed. Smith has been involved in several studies that have extended these ideas to both lower and higher-luminosity classes of AGNs.
Another successful technique used to probe the innermost structure of AGNs is to monitor their emission-line and continuum fluxes. A time delay between the brightening or fading of the ionizing continuum and the response of the line-emitting gas can be interpreted as the light travel time from the central ionizing source to the gas, thereby giving an estimate of the size of the BLR.
Smith and his collaborators have recently completed the first systematic, long-term spectrophotometric monitoring program of a well-defined sample of quasars. This project succeeded in detecting correlated variations between the continuum and emission-line fluxes and produced the first reliable observational estimates of the size of the BLR in quasars, extending previous studies of Seyfert nuclei to higher luminosity. Preliminary results from this program indicate that the size of the BLR roughly scales with the square root of the AGN luminosity as expected from photoionization models.
Future Research Plans Smith continues various observational projects that investigate the blazar class of AGNs. Programs include simultaneous VLBI radio and optical polarimetry of BL Lacertae objects to find correlations between their radio and optical synchrotron continuum emission. A polarization survey of a new sample of BL Lacs will be initiated to study the possibility that radio and X-ray selected BL Lacs have the same parent population. A nearby AGN will be imaged using HST in an attempt to resolve the scattering regions around the nucleus. This particular object, Mrk 231, exhibits many properties similar to broad absorption-line quasars, and gives us an opportunity to resolve some of the nuclear structures that may be present in higher-redshift objects. Smith will continue a long-term project with M. Corbin (U. of Arizona) to monitor the emission-line profiles of quasars with exceptionally broad emission lines.
xxvi Service During 1996-1997, Smith managed and helped execute the WLYN Queue Observing Experiment. This experiment was designed to test observing strategies that most effectively match TAC-approved WLYN observing projects to observing conditions. About 60 programs per year are serviced in this manner by NOAO under the policythat the highest-ranked proposals are given the highest priority within the WLYN Queue. The flexible schedule of the Queue allows for synoptic programs to be pursued, and allows for the ability to match image quality requirements of programs with observing conditions in a dynamic manner. Smith's duties have included general oversight of the WLYN Queue program, maintenance of the program's public Web pages, and observing during roughly one-third of the nights allocated to the WLYN Queue (about 100 nights are allocated to the Queue annually). In early 1997, Smith was named as the Hydra Multi-Object Spectrograph instrument scientist. Hydra is one of the two main instruments permanently mounted on the WLYN telescope. During the last half of 1997, Smith will become the supervisor of observing support with duties that include the training of LTO's and the development of work schedules and personnel assignments required for KPNO to operate the 4-m, 2.1-m, and WIYN telescopes.
Lloyd Wallace, Astronomer Emeritus
Areas of Interest Stellar and Planetary Atmospheres, Minor Constituents in the Earth's Atmosphere, Composition of Sunspots
Recent Research Results Wallace has completed the analysis of the hydrogen chloride line at 3.4168 microns in twenty-five years of solar spectra obtained at the McMath-Pierce telescope. D. Hall (now at Institute for Astronomy, U. of Hawaii) obtained the earliest spectra with a 20-m horizontal spectrograph; most of those from 1979 to the present were obtained by various observers with J. Brault's (now at Aeronomy Lab., National Oceanic and Atmospheric Administration) Fourier transform spectrometer, and from 1993 to the present by W. Livingston with the 13.5-m vertical spectrograph. This line is the result of absorption in the Earth's stratosphere by HC1 that is produced mostly by decomposition of man-made chlorinated compounds in the troposphere. The analysis shows an overall rise in the HC1 amount of a factor of three from 1971 to 1990. However, in subsequent years the rate of increase appears to have decreased by a factor of two, presumably because of the decreased production of these compounds.
Future Research Plans Wallace is in the process of analyzing the spectra of cool stars in the 1.02-1.35 micron region obtained by K. Hinkle with the Fourier transform spectrometer at the 4-m telescope. This spectral region is particularly interesting because of the variety of molecular absorbers that have been identified: vanadium oxide (VO), titanium oxide and sulphide (TiO and TiS), zirconium oxide and sulphide (ZrO and ZrS), cyanogen (CN), and water (H20). We are in the process of finding the agents responsible for the otherwise unidentified features. Wallace is also continuing his analysis of the sunspot spectrum in the red and near infrared. Two new absorption bands have been discovered but the identity of the absorbers is a mystery.
Service Wallace assists in writing the observing schedule for Kitt Peak and serves as special advisor on administrative matters.
xxvn US Gemini Program: Research Interests and Service Roles
Todd Boroson
Areas of Interest AGN Emission Lines, AGN Host Galaxies and Environments, Stellar Populations, Optical Instrumentation
Recent Research Results Together with H. Morrison (CWRU) and P. Harding (Steward), Boroson has continued his work on the structure of disk galaxies through surface photometry of edge-on systems. Early work in this area identified a faint halo with a very shallow fall-off around the galaxy NGC 5907. Although its nature is ambiguous, this halo may trace the dark matter in which this galaxy sits. More recently, efforts have been concentrated on NGC 891, an edge-on Sb galaxy that possesses a thick disk. Differences between the disk structure of NGC 891 and that of the Milky Way argue for in situ heating of a thin disk as the origin of the thick disk. Boroson has continued his work on the emission lines of quasars. Using data from the HST archive supplemented with groundbased spectra, Boroson and Corbin analyzed the combined UV- optical spectra of 48 low-redshift quasars and found new correlations involving line asymmetries and luminosities. With further work, this may distinguish among possible causes for the line asymmetries, including systematic motion of the clouds, shadowing by dense material, geometry of the broad-line region, and gravitational redshifts. With Laor (Technion), Green, and Jannuzi, Boroson has completed a study of the narrow line quasar I Zwicky 1. This object has been recognized as a prototype for the strong Fe U. emitters, and can be studied in detail because of its brightness. Boroson has also explored through modeling different modes of telescope operation. In particular, Monte Carlo analysis of realistic queue scheduling shows substantial gains in the efficiency with which telescope time is used overall, with particularly large gains for observations requiring rare conditions.
Future Research Plans Boroson is beginning a new imaging study of QSO host galaxies using the WLYN telescope. The intent is to study a complete sample of objects by obtaining high spatial resolution images in two line-free bands in order to study morphology, luminosity, and color of the underlying stellar populations. Boroson continues his work with Salzer (Wesleyan), Thuan (Virginia), Moody (BYU), Izotov (Kiev), and Kniazev (Special Astrophysical Obs.) One hundred square degrees have now been imaged with the Burrell- Schmidt both with and without an objective prism, and follow up spectroscopy with the Hydra spectrograph will allow the determination of the luminosity function of emission-line galaxies to very low luminosities and high precision. Boroson will continue his work on telescope operations to maximize science output with plans underway for workshops on capabilities needed to support the large telescopes now coming on-line.
Service Aside from being instrument scientist for the new CCD Mosaic Imager now being commissioned, Boroson's major service duties are associated with his position as US Gemini Project Scientist and Associate Director of NOAO. These duties include heading the office that has scientific and technical liaison responsibilities for the US community's participation in the international Gemini project, as well as participating with the other national project scientists as the Gemini project scientist team. With the restructuring of NOAO now underway, Boroson will provide oversight and leadership for the expanded roles of this division, including the "before and after" activities for all the telescopes to which NOAO provides access. These activities range from proposal and TAC process support, and support of astronomers preparing proposals or observing programs, to data reduction, archives, and scientific outreach.
xxvin David S. De Young
Areas of Interest Active Galaxies, Galaxy Clusters, Galaxy Evolution, Radio Sources, Hydrodynamics
Recent Research Results Much of De Young's research in recent years has revolved around the common theme of astrophysical outflows and their interaction with the environment. This is a basic problem in nonlinear physics, many aspects of which are poorly understood or not understood at all. This is especially true for highly supersonic and relativistic outflows for which there is little or no experimental data. For these flows the only accessible laboratory often lies in distant galaxies, where the interpretation of the data is often ambiguous. Nonetheless, such outflows can reveal characteristics of a large variety of astronomical objects, from protostellar jets and HH Objects to starbursts in galaxies and the creation of megaparsec scale radio sources—the largest single coherent objects in the Universe. De Young's focus has been on the nature of the boundary between the outflow and the environment, for it is here that the momentum and energy is transferred from the flow to the ambient medium, and it is this interaction that can reveal the characteristics of the outflow and hence constrain the nature of the object giving rise to it. Some of the results of this work have been an analytic description for the evolution of large scale structures seen in such boundaries; an explanation of the blue continuum seen in the central regions of some galaxy clusters in terms of jet induced star formation; a formulation of the relation between slow molecular outflows and fast moving collimated jets in proto-stellar and young stellar objects, and a model for the evolution of compact radio sources into large classical double sources that is consistent with observations from the parsec to 100 kiloparsec scale.
Future Research Plans Galaxy Evolution - In collaboration with C. Norman (STScI) De Young plans an investigation of the fate of hot, metal rich gas that is injected into galactic halos by OB associations and supernova remnants. It has been widely conjectured, but never demonstrated, that this debris causes the halo gas to cool and condense into clouds which then settle back into the galactic disk. In order to see if this model has any credibility, one needs a firm calculation which answers the following questions: is the hot debris, when mixed (or not) with the halo gas, thermally unstable? If so, is the instability damped or does it proceed to the nonlinear regime? Does the instability form dense sheets, filaments or clouds? Do these objects then persist and become gravitationally bound? This project requires complex and accurate modeling of the thermal conductivity in the context of time dependent numerical hydrodynamics, and the requisite algorithms are being developed. In a related project with T. Heckman (Johns Hopkins U.) and C. Martin (U.of Arizona) an extended study of mass loss from dwarf galaxies due to starburst activity is being initiated. The issue is that of possible recollapse of an inflated ISM in the galaxy versus complete dispersal of the ISM due to energy injection from the starburst event, and the object is to reproduce the observed low metallicities in these objects together with their observed stellar populations. The solution will require realistic modeling of a two phase ISM with radiative cooling, and the algorithms are now in hand to do this. De Young is also working on a book, entitled "The Physics of Extragalactic Radio Sources," to be published by the University of Chicago Press.
Service De Young's service activities to NOAO include acting as Chairman of the two KPNO telescope Time Allocation Committees, membership on the NOAO LPAC Committee, membership on the NOAO Management Committee, supervisorof the NOAO Tucson library, member or chairman of ad hoc KPNO Personnel and Post Doctoral Selection Committees, Chairman of the AURA Strategic Planning Committee, and membership on various ad hoc NOAO committees. De Young is currently Acting
xxix Deputy Director of NOAO. De Young is carrying out numerical modeling of airflow around and within various telescope structures to assist in evaluation of proposed designs for a new solar telescope for the National Solar Observatory. De Young also serves on the Board of Trustees of the Aspen Center for Physics and on the Executive and Steering Committees of the San Diego Supercomputer Center.
Ian Gatley
Areas of Interest Infrared Astronomy, Planetary Nebulae, Star Formation, the Galactic Center
Recent Research Results and Future Research Plans Gatley, Merrill, J. Kastner (M.I.T.), and D. Weintraub (Vanderbilt) have studied the structure of planetary nebulae by observing infrared emission lines from the hydrogen molecule. These observations directly probe the neutral component of the mass loss envelope, and are crucial in understanding the three dimensional shape of planetaries. Highly symmetric targets like the Ring Nebula seem obviously to be spherical, yet this work has shown it probable that they are actually bipolar and viewed by chance along the axis of symmetry. The construction of Phoenix offers the possibility of further progress in studying the molecular envelopes of planetaries. During the first commissioning run of Phoenix in August 1996, maps of NGC 7027 in both the Brackett Gamma line of atomic hydrogen and the v = 1-0 S(l) line of molecular hydrogen were obtained: these preliminary data are sufficient to demonstrate that the kinematics of the ionized and the molecular gas are totally different, and hint at velocity structure in the molecular toroid. The team plans to pursue this experiment when the instrument is fully operational, with the goal of understanding the origins and excitation of the molecular toroid.
Service Gatley is responsible for Scientific Oversight of the Photo Lab and of the Aladdin Detector Development Program. He coordinated the collaboration between NOAO, the Center for Astrophysical Research in Antarctica (CARA), the University of New South Wales, Australia, the US Naval Observatory, Flagstaff, and Goddard Space Flight Center that will place an Aladdin-array-based camera at the South Pole at the end of 1997. The South Pole confers important natural advantages to astronomy, most notably in the infrared, where background emission from both sky and telescope is intrinsically low, and targets are visible for twenty-four hours per day, continuously at constant elevation. The deployment of a state-of- the-art camera, with a larger format detector and working at longer wavelengths, will focus the science firmly on the natural advantages of the site, while the broader collaboration will move rapidly towards community involvement through shared risk observations. A survey of star formation activity in the Large Magellanic Cloud will highlight the earliest observations.
Buell T. Jannuzi
Areas of Interest Observational Cosmology, Active Galaxies, Quasar Absorption Lines, Instrumentation
Recent Research Results Jannuzi has recently completed the generation of the final catalogue of quasar absorption line systems found during the Hubble Space Telescope Quasar Absorption Line Survey, a Key Project during cycles 1-3 of the HST mission. The survey of 89 bright quasars yielded a large (over 1000 absorption line systems identified) and homogeneous database suitable for the study of the distribution and evolution of gaseous systems in the intermediate and low redshift Universe. Several papers are in progress completing the analysis of the survey data. Collectively the work is the most extensive census of the nearby gaseous Universe made to date.
xxx Future Research Plans Together with Co-PI Arjun Dey, Jannuzi is leading a team of NOAO astronomers in the execution of the NOAO Deep Wide-Field Survey. This ambitious project is a very deep LR and optical (B,R,I,J,H, and K pass-bands) imaging survey of 18 square degrees of the sky. The primary goal is to enable the study of the evolution of large-scale structure from z ~ 1-4. The detection of large-scale structures at z= 1 will provide unique constraints on theories of hierarchical structure formation and the cosmological parameters. In addition, the survey will enable an investigation of the formation and evolution of the red- envelope galaxy population and detect luminous, very distant (z = 4), star-forming galaxies and quasars. This two-year survey will map an unprecedentedly large area to very faint flux limits (B, R, I 26 AB mag. and J, H = 21; K = 21.5 AB mag. 5-sigma detection limits in a 2 arcsec diameter aperture). The survey areas will be two independent 9 square degree fields, one equatorial near the South Galactic Pole and the second near the North Galactic Pole, in regions of the VLA FLRST radio survey. This survey will be invaluable in addressing many other problems, and we are designing its execution and the presentation of the data to the community in a manner that will maximize the scientific return. A major goal of the project is the distribution to the general community of the calibrated data within six months of completion of the first year of observations.
Service Jannuzi was recently transferred to the US Gemini Project Office, which is an expanding division of NOAO with responsibilities that include being the US astronomical community's interface with the observing facilities operated by NOAO and the Gemini telescopes. Despite the transfer, Jannuzi continues to have responsibilities to KPNO. He serves as the instrument scientist for all of the low to moderate spectral resolution spectrographs on Kitt Peak (the GoldCam, R-C, and CryoCam spectrographs). He is the project scientist for GoldCamLI, an upgrade project for the GoldCam spectrograph which includes the fabrication of a new camera and dewar for the instrument as well as the installation of a new CCD detector. Jannuzi is the coordinator for the Tucson based portion of NOAO's NSF funded Research Experience for Undergraduates program. He serves on numerous NOAO and national committees including the KPNO TAC, a HST cycle 7 TAC panel, the US Gemini Science Advisory Committee, and the Gemini Science Committee.
Tod R. Lauer
Areas of Interest Cosmology: Large Scale Structure of the Universe, Distance Scale, Clusters of Galaxies, Deep Surveys; Normal Galaxies: Structure of Galaxies, Central Structure and Black Holes
Current and Near Term Research Tod Lauer, in collaboration with M. Postman (STScI), has recently completed a deep near-IR sky imaging survey with the KPNO 4-m. This survey was designed to detect galaxy clusters out past a redshift of one, and thus serve as a basis for exploring how the largest structures in the universe have evolved since the universe was half its present age. The survey covers 16 square degrees, contains one million galaxies, and is the deepest sampling of the universe over such a large area. Lauer and Postman are now working on understanding the galaxy counts, correlations functions, and galaxy cluster catalogs generated from the survey as diagnostics of evolution of galaxies and structures sampled by the survey.
Closer to home, Lauer is leading a team that includes Postman, J. Tonry (Hawaii), E. Ajhar (NOAO), and J. Holtzman (New Mexico State) for the purpose of measuring the Hubble constant, or expansion rate of the universe at large distances, using the surface brightness fluctuation method with the Hubble Space Telescope. While there has been much work on the Hubble constant in the last few years, a key problem
xxxi is observing the expansion of the universe at large enough distances so that measurement of the expansion rate is not affected by the random motions or bulk flows of the galaxies being studied. Many investigators have used only single galaxy clusters to sample the unbiased expansion pattern of the universe, which raises concerns as to how accurate such calibrations are. Earlier, Lauer and Postman used the brightest galaxy in clusters (BCG) of galaxies to show that at large distances the expansion of the universe is smooth and linear as expected. The new work with HST uses Tonry's SBF method to calibrate this earlier work, giving now an absolute value of the expansion rate. This work is nearing completion at this time and should resolve one of the major uncertainties in the problem of measuring the Hubble constant.
In the coming year, Lauer and Postman, in collaboration with M. Strauss (Princeton), also hope to use NOAO observations of BCG to continue to search for the scale at which large scale galaxy bulk flows terminate. Lauer and Postman earlier used BCG to show that a bulk flow of galaxies appeared to exist on scales larger than would be expected under standard theories of galaxy formation. Bulk flows contain information about the distribution of matter in the universe, thus the implication of the earlier Lauer and Postman work would be that the universe remains inhomogeneous out to far larger distances than would be expected. The new work hopes to refine the earlier bulk flow measurement, as well as extending it deeper into space; the diameter of the volume being explored is about 1.5 billion light years.
Lauer also continues to use HST to study the makeup of nearby galaxies as part of a team effort chaired by D. Richstone (Michigan). Lauer has shown that the central structure of galaxies is very different than expected—the density of stars in the center appears to rise without limit, rather than leveling off at a constant value. This result may mean that black holes are common in the centers of galaxies; indeed a key goal of the Richstone team is to use HST to detect such black holes. To date the team has detected black holes in a number of galaxies, and hopes to use the new STIS on HST to increase their success rate.
Service Lauer is editor of the NOAONewsletter, which is the major organ of communication between NOAO and its community. The Newsletter is published on the NOAO web page as well as by hardcopy. Lauer also chairs selection of NOAO postdocs, and runs the Friday Lunch and joint NOAO/Steward colloquium series. Lauer is also responsible for direct imaging at KPNO.
NOAO has recently created a new division, directed by T. Boroson, to support and provide science and observational capabilities for the community with NOAO, and other nationally available facilities. Lauer has been assigned to this division and a major component of his work in the coming year will be in support of this division's activities.
Catherine A. Pilachowski
Areas of Interest Stellar Seismology, Stellar Compositions, Stellar Evolution and Nucleosynthesis, the Origin of the Elements in the Milky Way
Recent Research Results Pilachowski, in collaboration with C. Sneden and R.P. Kraft, has completed the analysis of 4-m Hydra data to examine the variations in the sodium abundance in the globular cluster Ml3. With sodium abundances for over 150 stars in Ml3, they traced the changes in the abundance of sodium along the giant branch and asymptotic branch, and tied these changes to other elements also affected by nucleosynthesis processes in cluster stars. It is clear that all M13 giants are affected to a varying degree by similar processes, and that mixing of nucleosynthesis products to the surface is occurring at a much
xxxn earlier evolutionary phase than previously predicted. They found a wide dispersion in the sodium abundance (and, from Keck data, in the oxygen abundance) well down on the giant branch. The abundance of sodium is correlated with the nitrogen abundance, and anti-correlated with the oxygen (and sometimes magnesium) abundances. They see clear indication of the action of the ON and NeNa cycles in all the stars, and of the MgAl cycle (which requires a little higher temperature) in some of the stars. The action of these cycles will also alter the He abundance in the envelopes of the post-first ascent giants, and they see evidence for differences in the subsequent course of stellar evolution in the AGB phase. This work will go a long way toward clearing up much of the confusion and ambiguity surrounding globular cluster abundances (nature vs. nurture) in the last decade. Research on globular clusters is an area where WLYN and Keck can provide complementary data, to mutual advantage. Time on Keck is too scarce to sample the number of stars needed to understand abundance variations in globulars, but Keck data can follow up on specific targets identified from WLYN data to provide detailed analyses of many important elements. Without the WLYN data, and the large numbers of stars that can be obtained, it is difficult to draw meaningful conclusions from the Keck data.
Pilachowski, T. Beers, C. Sneden, and R. Cavallo are using a new technique, that of low resolution spectroscopy of the O I triplet at 7772A, to determine oxygen abundances in extremely metal-poor stars ([Fe/H] < -2.5) identified in the Preston-Beers survey. Since the lines are closely spaced in wavelength, they can work on the blended feature at lower resolution without significant penalty in precision, and obtain spectra of fainter stars than would be accessible with a high dispersion spectrograph. They are investigating whether the oxygen excess observed at higher metallicity extends (or even increases) to lower metallicity. The composition of the lowest metallicity stars is probably dominated by the production of elements in a small number of supernovae explosions of relatively massive stars. The [O/Fe] ratio is sensitive to the mass of the progenitor supernova. The dispersion in the [O/Fe] ratio in extremely metal-poor stars may well constrain the dispersion (or lower limit) of the masses of supernovae contributing to the chemical enrichment of Milky Way at its earliest phase. Pilachowski, et al. obtained spectra of nearly two dozen metal-poor subdwarfs and turnoff stars, and are working to establish atmospheric parameters for all the stars observed and to complete preliminary analyses of their spectra. In a related effort, R. Cavallo (U. of Maryland student) and Pilachowski analyzed several coude spectra of the O I triplet lines in intermediate metal-poor subgiants. The paper will appear soon in the PASP.
Future Research Plans Pilachowski, in collaboration with S. Barden, M. Giampapa, F. Hill, C. Keller, and J. Harvey, is working to detect and study acoustic oscillations in stars similar to the Sun. It is their hope that this project will develop into a broad, community-based program to coordinate observing runs on large telescopes around the globe to obtain adequate data to characterize fully the oscillation spectrum of stars of astrophysical interest. Stars in clusters are of special interest, and observations on 4-m class telescopes will be needed to obtain sufficient signal to determine oscillation frequencies. A five-week observing run on the Coude Feed telescope was completed in January-February 1997 to conduct a detailed study of the star Procyon: 12,888 spectra were obtained at a 1-minute sampling rate. Analysis of the spectra is underway.
Service Pilachowski serves as Project Scientist for the ALPS++ Project to develop a new database and proposal management system for observing time proposals for both KPNO and CTIO. This effort is important not only to lighten the workload involved in handling proposals, but also to allow us to undertake easily the new tasks facing NOAO, including changing observing styles, telescopes, instrumentation, and public access to independent observatories. In addition, she is responsible for support of the KPNO electronic proposal submission process for KPNO. Pilachowski, with M. Giampapa (NSO), is responsible for the support of high resolution spectroscopy on KPNO telescopes. Pilachowski is also involved with numerous educational outreach projects and serves on the local ASP/Project Astro Coalition. She assists
xxxm students interested in gaining research experience in astronomy, and participates in the University of Arizona's Women in Science and Engineering Program. Pilachowski continues to serve as a member of and Secretary to the WLYN Consortium Board of Directors, and she has recently been elected to the Council of the American Astronomical Society. She is actively involved in the broader community, serving on numerous advisory committees and review boards.
Francisco G. Valdes
Areas of Interest Cosmology, Gravitational Lensing, Stellar Spectroscopy, Astronomical Software
Recent Research Results Recent work has centered on spectroscopy of a very broad sample of stars of various spectral types, temperatures, and abundances. This collection of stellar spectra will form a unique library, since it covers a larger variety of stars at higher resolution than any existing collection; the atlas will be made available to the astronomical community and public at large. The research use of this library will be for modeling stellar populations in galaxies and for developing software that will be able to determine the temperature, mass, and composition of stars from large future spectroscopic surveys.
Future Research Plans The observations and preparation of the library of stellar spectra is a continuing multi-year project. Valdes will participate in the proposed NOAO Wide-Field Survey using the new NOAO CCD Mosaic camera. This survey is an effort by many NOAO scientific staff to utilize the powerful imaging capabilities of the Mosaic camera to provide data over a large region of the sky to the community and for various research programs. Valdes will study this data to measure masses of galaxies and clusters of galaxies which distort the images of distant galaxies by the gravitational bending of the passing light.
Service Valdes is responsible for the development of forefront astronomical software for CCD and spectroscopic astronomical data. This software involves new techniques as well as complex programs to deal with the increasingly complex astronomical data produced by advanced astronomical instruments. The end- product is to extract the maximum astronomical information from the observations made at the telescopes. The software is required by users of NOAO instruments as well as other observatories in the United States and abroad. Support of this software involves assisting astronomers in the application of the programs and consultation about the best methods to use. This assistance is given to many NOAO staff and visitors. Valdes is currently developing the data reduction software for the NOAO CCD Mosaic camera—a new forefront camera being built by NOAO to image a very large region of the sky in a single exposure.
xxxiv Instrumentation Division: Research Interests and Service Roles
Taft Armandroff
Areas of Interest StellarPopulations in the Galaxy and Nearby Galaxies; Globular Clusters; DwarfSpheroidal Galaxies
Recent Research Results Armandroff has been studying the dwarf spheroidal satellite galaxies of M31, in collaboration with Da Costa (Mt. Stromlo), Caldwell (SAO) and Seitzer (Michigan). This was motivated by the opportunity to increase the number of galaxies defining the properties of dwarf spheroidals, and by the fact that the somewhat different environment of the M31 dwarfs compared to those of the Galaxy allows a first look at how dwarf spheroidal properties change with environment. Images were obtained with the HST WFPC2 camera of And I, a dwarf spheroidal (dSph) galaxy located in the outer halo of M31. The resulting color-magnitude diagram reveals for the first time the morphology of the horizontal branch in this system. They find that, in a fashion similar to many of the Galactic dSph companions, the horizontal branch (HB) of And I is predominantly red. Combined with the metal abundance of this dSph, this red HB morphology indicates that And I can be classified as a "second parameter" system in the outer halo of M31. This result then supports the hypothesis that the outer halo of M31 formed in the same extended chaotic manner as is postulated for the outer halo of the Galaxy. In addition to the red HB stars, blue HB and RR Lyrae variable stars are also found in the And I color-magnitude diagram. The presence of these stars indicates that And I contains a minority population whose age is comparable to that of the Galactic globular clusters. They estimate, however, that the bulk of the stellar population in And I is -10 Gyr old. Thus, again like many of the Galactic dSphs, there is clear evidence for an extended epoch of star formation in And I. A radial gradient in the And I HB morphology has also been discovered in the sense that there are relatively more blue HB stars beyond And I's core radius. This may be evidence for more centrally concentrated star formation after the initial episode. Similar HB morphology gradients have also been identified in two of three Galactic dSphs studied. The mean magnitude of the blue HB stars suggests that And I lies along the line-of-sight at the same distance as M31 to within ± 70 kpc.
Future Research Plans Pursuing the theme described above of studying the properties of dwarf spheroidal galaxies as a function of environment represents a significant portion of Armandroff s research agenda for the coming year. WFPC2 observations of two other M31 dwarf spheroidals, And LI and EL, are expected shortly. From these data, he hopes to learn whether these two galaxies resemble their Galactic counterparts as much as And Ldoes. It will also be interesting to see if the radial gradient in HB morphology seen in And I is mirrored in And LI and LTJ. Armandroff will also study dwarf spheroidal galaxies in the M81 group. Based on surface-brightness profiles from groundbased telescopes (especially WLYN and the Burrell-Schmidt), the structural parameters of M81-group dwarf spheroidals will be compared with those of Local Group dwarfs. In addition, based on imaging of two M81 dwarfs from WFPC2 and the resulting color- magnitude diagrams, their stellar populations and metal abundances will be determined and compared with Local Group dwarfs.
Service Armandroff serves as project scientist for the NOAO optical/UV instrumentation program. In this capacity, he coordinates all optical instrumentation development efforts and serves as a member of the Instrument Projects Advisory Committee (LPAC). Armandroff is a member of the team developing and commissioning the 8K x 8K CCD Mosaic Imager for the KPNO 4-m and 0.9-m telescopes, and a copy of this instrument for CTIO. Armandroff also participates in the group building a version of the Hydra
xxxv multi-fiber spectrograph for the CTIO 4-m. He also serves on the "Kitchen Cabinet" for KPNO operations. During the period April through October (while Richard Green is on sabbatical), Armandroff is also serving as Acting Director of the NOAO Instrumentation Program. Ln this capacity, he chairs IPAC and sits on the NOAO Management Committee.
Samuel C. Barden
Areas of Interest Stellar Physics and Dynamics, Binary Stars, Spectroscopic Instrumentation
Recent Research Results Barden has recently focused his scientific activity on the search for binary stars among globular clusters. The determination of the fraction of binary stars in a globular cluster is important for understanding how globular clusters dynamically evolve (e.g., why they don't have collapsed cores). The study of such binary populations will also provide insight into the dynamic evolution of the binaries themselves when in a dense stellar cluster where interactions with neighboring stars are quite frequent. Barden's preliminary results on binaries in M71, in collaboration with T. Armandroff (NOAO) and T. Pryor (Rutgers), suggest a binary fraction comparable in size to that for field stars near the Sun. This is much higher than originally anticipated but is in line with some recent results by other investigators. Barden and collaborators are currently working on the M13 cluster, which has cluster properties significantly different from M71. Expectations suggest a lower M13 binary fraction. Only one of the several required epochs of observations has been obtained so far for the M13 sample. Barden and collaborators are also attempting to do follow-up observations of the M71 binary sample from which they hope to derive binary orbital parameters.
On another front, Barden has joined with C. Pilachowski, M. Giampapa, F. Hill, C. Keller, and J. Harvey (all NOAO) in a concerted effort to search for acoustic (p-mode) oscillations in solar-like stars. This group is using an equivalent width technique in which oscillations should show up with a signal of about 30 parts per million and which appears to be the most promising technique for detecting these elusive oscillations. The detection and evaluation of p-mode oscillations on stars (similar to the 5-minute oscillations of the Sun) are important for constraining stellar evolutionary theory. Most of modern astrophysics, including the distance scale to the galaxies and the ages of stellar clusters, relies on our knowledge of the fundamental parameters of stars. Measurement of the fundamental p-mode oscillations provides significant leverage on the age and mass of stars when coupled with temperature, luminosity, and the star's metallicity. Barden, et al. recently completed an observing campaign on Procyon. Five weeks were allocated during which 27 nights worth of data were obtained. Analysis of the data is still underway.
Barden is also undergoing a collaborative effort with Giampapa and Pilachowski to observe the long- term behavior of absorption line bisectors in the stars recently detected to have possible planetary companions. It is quite possible that line bisector modulations due to stellar pulsations could in some fashion mimic the behavior of an orbiting body when observed at relatively low resolution. Higher resolving powers (R > 100000) than those used to detect the low level radial velocity motions are needed to see if indeed the behavior can be accounted for by modulations in the shape of the absorption lines rather than by true reflex motions of the star.
Future Research Plans Barden will carry forward his study of M13 and M71 binary stars. Detection of binaries in M13 will take 2 to 3 more epochs of observing over the next couple of years, while follow-up observations of the detected binaries may require baseline observations of several years to derive the desired orbital
xxxvi parameters. The search for stellar oscillations (asteroseismology) is a tedious andtime consuming project requiring longruns andextensive dataanalysis. The group, in which Barden is involved, is in the process of organizing a community-wide effort (called Stellar Oscillations Network Group or SONG) to search for and observe p-mode oscillations in solar-type stars. The goals of SONG are to explore and define observing techniques, develop required instrumentation, coordinate observing efforts, and implement a worldwide network not unlike the GONG network currently studying oscillations in the Sun. Such an effort could easily span the next 5-10 years and involve international collaborations.
Service Barden is Project Scientist for Hydra/CTIO—which involves frequent activity working with team members. Hydra is a multi-object spectrograph, which was recently put into operation at the WIYN telescope. The current project is to build a similar instrument for CTIO. Barden serves as co-project scientist with Bob Schommer from CTIO. The CTIO project will require effort over the next two years to finish fabrication and delivery of a working instrument for use on the Blanco 4-meter telescope.
Barden was recently assigned to be the instrument scientist for the Gemini CCD controller project. The goal is to deliver controllers for use on the Gemini optical instruments by mid-FY 1998. He is currently defining user requirements within the context of the expected controller performance. This effort is currently a collaboration between NOAO, B. Leach (SDSU), and N. Dillon (RGO).
Barden serves as the US Community liaison for the optical instruments being fabricated for the Gemini telescopes. In this role, he attends and participates in the design reviews for both GMOS and HROS. He is expected to assist in the integration and testing of these instruments as well as in the on-telescope commissioning.
Barden is involved in the process of preserving the high resolution spectroscopic capabilities of the coude spectrograph that is currently in use with the Coude Feed telescope. That spectrograph is capable of resolving powers approaching 250,000. The instrument is unique, but suffers from a small telescope aperture (0.9 meters) and the threat of closure due to decreasing operational funds at KPNO. Barden has helped to define a future for the instrument in which it will be moved over to the Mayall 4-m telescope where it will be fed by a fiber optic feed. This will enhance the performance of the instrument allowing new thresholds to be reached by the community users.
Barden is involved in some additional instrument development efforts. This currently includes conceptual ideas for a "high efficiency spectrograph," which KPNO is considering as a potential replacement for the aging R-C spectrograph at the Mayall 4-meter. Barden is exploring new technology gratings and optics in an attempt to simplify and enhance the spectrograph's efficiency. He also has the responsibility of assembling the fiber heads for the Hydra/CTIO instrument and recently produced the fiber array currently in use at the WLYN telescope for integral field spectroscopy. Barden also occasionally serves as a consultant for university level instrument development. He has led two conferences on astronomical applications of fiber optics.
Jonathan Elias
Areas of Interest Star Formation and Evolution, Magellanic Clouds
Recent Research Results Elias's most recent research project has been an investigation of stellar mass loss in the Magellanic Clouds. In the later stages of their evolution, stars become red giants and lose mass. As material flows
xxxvn out from the star, it cools and dust forms. The dust is detectable at infrared wavelengths; if there is enough of it, it will also hide the star itself from view. The abundance of dust in the circumstellar material and the rate and velocity of mass loss may all depend on the abundance of heavy elements in the star losing mass—but it is not known in which ways. In order to see what actually happens, it is necessary to compare observations of stars with different heavy element abundances. As stars in the Magellanic Clouds have lower abundances than similar stars in the Galaxy, and since these galaxies are close enough for individual stars to be readily observable, they provide a useful basis for comparison.
Future Research Plans Elias's work to date shows that the data are consistent with the hypothesis that only the amount of dust depends on the heavy element abundance, and that the two are directly proportional, while the overall mass loss rate is insensitive to abundance variations. Other workers suggest, though, that mass loss rates should be lower in stars with lower heavy element abundances. Few Magallanic Cloud mass-losing stars have been identified, especially in the Small Magellanic Cloud, so the evidence does not strongly favor one hypothesis over the other. Elias will be obtaining data from the Infrared Space Observatory (ISO) on selected regions of the Large and Small Magellanic Clouds. The new data will provide much larger samples of mass-losing stars than have been available up to now, and should settle the issue.
Service Elias's primary service activities during the last year have been in several areas. He began serving officially as project scientist for the Gemini Near-Infrared Spectrometer (GNLRS) in March 1995, and transferred from Chile to Tucson in January 1996 as a consequence. This position also entails service on the Gemini Infrared Instrumentation Science Working Group. In addition, he was one of the three scientific staff members responsible for the CTIO infrared program up until his departure. He also acted as the CTIO telescope scheduler, and was a member of the CTIO Time Allocation Committee, the CTIO Advisory Committee on Technical Resources (which provides scientific oversight of the CTIO instrumentation program) and the NOAO Instrument Projects Advisory Committee (which performs similar functions for NOAO as a whole). His membership on LPAC has continued after his transfer to Tucson. He has also been involved with review of CTIO's cost structures.
Kenneth H, Hinkle
Areas of Interest Circumstellar and Interstellar Matter, Molecular Spectroscopy, Peculiar Stars, Instrumentation
Recent Research Results During the past year Hinkle has concentrated most of his effort in developing the high resolution infrared spectrograph Phoenix. Hinkle has had observing runs with this instrument but much of the data are either so recent that it has not been fully reduced or forms parts of incomplete projects. For instance, Hinkle is a co-investigator with B. McCall and T. Oka (U. of Chicago) in a program to measure abundance of the ion H3+ in the interstellar medium. H3+ is formed as cosmic rays ionize molecular hydrogen. H3+ then reacts via a proton hop route to produce the wide variety of complex molecules observed by radio astronomers. H3+ is not easy to detect due to its symmetry, reactivity, and the nature of the spectrum. Hinkle and collaborators obtained spectra in January 1997, reduced these, and found that improvements in the spectrograph were indicated. These changes have been made and they are now waiting for additional observing time in June. Phoenix observing programs that have been completed by Hinkle involve measurement of hot gas, presumably the result of mass loss, around metal-poor AGB stars using the 1.08 micron He I line with R. Joyce (NOAO) and C. Sneden (U. of Texas), measurement of the magnetic field of the M dwarf EV Lac with J. Valenti (U. of Colorado), C. Johns-Krull (U. of Colorado), and R. Joyce, and the determination of carbon isotope ratios from the first overtone CO bands in metal-poor giant stars
xxxvin with C. Pilachowski (NOAO), C. Sneden (U. of Texas), and R. Joyce. Hinkle and L. Wallace (NOAO) also completed an atlas of medium resolution spectra of normal stars in the K band using archival FTS spectra.
Future Research Plans Hinkle has a number of ongoing collaborations. Using the Phoenix spectrograph, Hinkle and P. Bernath (U. of Waterloo) plan to extend their search for previously undetected circumstellar organic molecules. Previous searches indicate that the pure carbon chain C7 should be easily detectable. Symmetric organic molecules of interest in the early solar system, for example ethane and allene, should also be detectable. Hinkle also plans to use the Phoenix spectrograph to explore the velocity structure and ionization structure of the circumstellar shells of post-AGB stars. These shells show considerable spatial structure and are intermediate between the complex spatial structure of planetary nebula and the simple geometry of AGB mass loss. Hinkle also plans to extend his work on interacting late-type binary systems. Visual spectroscopy of interacting binaries is confused by (hot) emission from the accretion disk. The 1.5-2.5 microns infrared is the ideal spectral region to measure the velocity of the red star in these systems. With R. Joyce (NOAO) and F. Fekel (Tennessee State), he has an ongoing project at the Coude Feed telescope to observe about a dozen symbiotic systems with the NICMAS detector. The 1.6 micron spectra of these symbiotics will be observed on a roughly quarterly basis for three years. The first goal is to characterize the nature of the variable star in the system. Typical late-type giants in interacting binaries have orbits of about two years. Systems with Mira variables should have longer orbital periods. Masses for the red giant and white dwarf should ultimately be obtainable. Another motivation of this project is a planned extension of the object list to interesting related objects, e.g. massive binary systems too highly reddened to be observed in the optical. Hinkle is looking forward to extending this work to the southern hemisphere when Phoenix is taken to CTIO. With T. Lebzelter and J. Hron (Vienna), Hinkle is working on a series of papers on pulsation driven velocity changes in Mira, SRa, and SRb variables.
Service Hinkle's main service activity has been as project scientist for the Phoenix spectrograph. This project started in 1991 and has accounted for nearly full-time effort by Hinkle since then. The Phoenix project is a major observatory contribution to the community. Phoenix now allows high resolution (R= 100,000) spectroscopy in the 1-5 microns infrared to much fainter limiting magnitudes than previously possible. Phoenix will ultimately serve a larger community than Kitt Peak. Current plans envisage use of this instrument at CTIO in late 1998 and with Gemini as well as on Kitt Peak. Hinkle has done a large part of the program management for Phoenix, has provided the astronomical input, and has resolved many engineering and optical design issues. Hinkle did the optical assembly and oversaw the mechanical assembly. He is now in charge of bringing the instrument to complete user readiness as well as supporting user runs. He also maintains FTS spectra dating back to 1976 in an archive; spectra are available upon request. Hinkle and collaborators have recently published a number of atlases based on this archive so that the material is more readily available to the community. Hinkle participates in the Gemini infrared instrumentation working group, and is currently preparing a proposal for SOFIA instrumentation.
K. Michael Merrill
Areas of Interest Star Formation, Young Stellar Objects, Interstellar Medium, Circumstellar Envelopes, Infrared Instrumentation, Data Acquisition and Reduction
xxxix Recent Research Results Merrill and Gatley have recently discovered a striking correlation between the results of two very different approaches to the study of the ionized gas in the Galactic center. Specifically, the dynamical model by Lacy, et al. 1991 (ApJ 380, L71), based on observations of the neon 12.8 micron line, isolates a one-armed Keplerian spiral structure that is also prominent in Merrill and Gatley's images of the reddening of the ionized gas, based on KPNO 1.3-m COB Brackett alpha and gamma emission line images. They will deploy capabilities unique to KPNO to study the "central engine" buried within the Galactic center, which is otherwise hidden from conventional optical techniques by massive extinction. Observations at both high angular resolution to get spatial details (provided by the DLLRLM real-time shift and add facility which produces diffraction-limited images at the 4-m telescope) and high spectral resolution to get the kinematics (provided by the Phoenix spectrograph) will be required to extract the truth from the tangle in the Galactic center. These observations (currently scheduled for June 1997) will significantly improve the database for ionized gas kinematics and star counts, providing a stringent test for the "central engine." Furthermore, because the Lacy spiral shows up as a distinct feature at a characteristic value in the extinction map, one can confidently predict that the kinematic profiles at Brackett alpha and Brackett gamma will show differential extinction which will make it possible to tie the kinematic and the imaging experiments together.
Future Research Plans The cosmic interface between "stellar systems engineering" and "practical astrophysics," which conspire to produce a continual supply of new stars, has been the object of continued fascination to astronomers for many decades with each new discovery somehow whetting the appetite for more. Following the SQUD upgrade, Merrill will resume his pioneering study of regions of active star formation which has awaited extension to a significantly wider field of view (4x area) and higher sensitivity (20x) with high relative stability. The unprecedented ability to survey large regions with absolutely registered JHK(L) imaging will give renewed impetus to systematic studies of the more global aspects of the star formation process which had heretofore been stalled by the complexity of the observations and the attendant data reduction which are required to adequately sample the full luminosity range over a FOV measured in tens of arcminutes in the presence of heavy, patchy extinction. Statistically significant star counts, with derived mass and luminosity functions, and the detailed distribution of the attendant gas and dust will all be amenable to careful study for regions of star formation covering a wide range in distance, total mass, and age.
Service As an Infrared Imaging Scientist at KPNO, Merrill oversees the LR imagers and attendant visitor support at KPNO, including instrument set-ups and observer checkouts, and is the point of contact on performance issues for both proposers and the TAC during the proposal cycle. He is project scientist for the KPNO SQLLD upgrade to 512 x 512 InSb and actively involved with the shake-down and deployment of new LR instrumentation. As the responsible scientist for user support of LR data reductions, he advises observers, programs and supports data reduction scripts, and interacts with the LRAFprogramming group to improve and extend LR specific capabilities within LRAF. As package scientist for the next generation Gemini/NOAO Array Controller project and (with I. Gatley) responsible scientist for the ALADDIN InSb 1024 x 1024 LR array R&D effort, Merrill plays a significant role in developing the deploying state- of-the-art LR detection capability to the wider community. Merrill continues as advisor to Gemini on site and enclosure issues and LR instrumentation—detectors, array controllers, limiting performance and observation techniques. Merrill has been an active participant in outreach activities within the local schools, including teaching classes and coaching Science Olympiad teams, and at scientific meetings.
xl NSO Scientific Staff: Research Interests and Service Roles
Jacques Beckers
Areas of Interest Astronomical Telescopes and Instrumentation, Adaptive Optics, Interferometers, Solar Physics
Recent Research Results Beckers is undertaking the feasibility study of a large aperture solar telescope (CLEAR), including a survey of sites for its location.
Future Research Plans Beckers will complete the solar telescope feasibility study. On the basis of the site survey results, he will do research into the physics of daytime seeing at lake sites.
Service Beckers is Director of the National Solar Observatory, Editor of the journal Experimental Astronomy, a member of the USRA Astronomy and Space Science Council, and of the Advisory Board of the Center for Astronomical Research in the Antarctic (CARA).
Michael Dulick
Areas of Interest Molecular Spectroscopy, High-Resolution Fourier Transform Spectrometry, Study of Molecules of Astrophysical Interest
Future Research Plans Dulick plans to use the McMath FTS to record laboratory spectra of these diatomics in the infrared and visible to aid in the assignment of sunspot spectra. A significant portion of the analysis will entail the development of an effective internuclear potential model for the electronic states of transition-metal diatomics in order to utilize information derived from low-temperature laboratory spectra in predicting the high-temperature spectra of sunspots. Dulick will also participate in projects to upgrade the detectors and data collection system for the FTS.
Service Dulick serves as the NSO FTS Instrument Scientist for visiting investigators funded under the NSF Chemistry grant for Laboratory Fourier Transform Spectroscopy, with specific duties that include providing assistance in the experimental design and setup and the instructional use of the instrument.
Richard Dunn
Areas of Interest High Resolution Imaging, Instrumentation
Future Research Plans Dunn plans to continue his work on improving the quality of resolution at the Vacuum Tower Telescope. He will also continue to consult on the upgrade to the Solar Observing Optical Network (SOON).
xli Mark Giampapa
Areas of Interest Stellar Dynamos, Stellar Cycles and Magnetic Activity, Asteroseismology
Recent Research Results Giampapa and his collaborators, C. Prosser (SAO), and T. Fleming (U. of Arizona), have completed a ROSAT X-ray and optical investigation of the young cluster IC 4665. This cluster has an age similar to the Pleiades (about 70-100 Myr) and thus represents an important comparison to other clusters studied with ROSAT. Giampapa and his colleagues find, on the basis of the joint X-ray and optical study, that the evolution of angular momentum among the stars in IC 4665 occurs in a fashion that appears virtually identical among all young clusters with ages less than 100 Myr. Giampapa and his colleagues, S. Baliunas (SAO) and R. Radick (AFRL), have completed an initial survey of chromospheric Ca LI H and K line emission in the numerous solar counterparts in the solar-age and solar-metallicity open cluster M67, using the WLYN telescope with the Hydra multi-object spectrograph. The results will indicate the range of potential amplitudes of the solar cycle. This is critical to know in view of the impact of solar variations on long-term global climate changes. Giampapa and his collaborators expect to submit for publication in early FY 1998 the initial results of this unique solar-stellar program.
Future Research Plans M. Giampapa and his collaborators plan to repeat their initial survey of magnetic activity in the many Suns in M67 in order to begin an investigation of long-term variability analogous to what would be expected from cycle-like modulations of chromospheric activity. In addition, Giampapa and his colleagues in the solar-stellar community will explore the prospects of establishing a long-term program of measurement of cycle properties in solar analogs at a large-aperture telescope. As a member of the Stellar Oscillations Network Group (SONG), Giampapa and his colleagues expect to complete during early FY 1998 the reduction and analysis of the 30-day Procyon observing campaign. A positive result will open a new vista for the experimental study of stellar interiors through the techniques that have been so successfully employed in helioseismolgy as exemplified by the GONG program. S. O'Brien (REU student, U. of Arizona) and Giampapa will submit for publication the results of their long-term monitoring program of spectroscopic variability in T Tauri stars. Their analysis has disclosed persistent, periodic variability in the mass outflow/inflow regions of these precursors to Sun-like stars and solar systems. In collaboration with C. Pilachowski (NOAO), S. Barden (NOAO/KPNO), and D. Deming (NASA/GSFC), Giampapa is leading an effort to measure line bisectors in stars that have been reported to have Jupiter-like companions. The results will illustrate the potential contribution of intrinsic stellar atmospheric motions to apparent Doppler shifts that could be misinterpreted as being due to planetary companions.
Service Giampapa serves as the Science Branch Chief for the Tucson site of the National Solar Observatory. Ln this role, he has overview responsibilities for the scientific and instrument development activities at NSO/Tucson. Giampapa is chairman of the Tucson site Project Review Committee (PRC) and serves as a member of the full NSO PRC. He is a member of the NSO Management Team and also serves on the NSO/Kitt Peak TAC where he advises on proposals for the use of the solar-stellar spectrograph at the McMath-Pierce facility. Should SOLIS be funded, Giampapa expects to take on significant responsibility for the Solar-Stellar Telescope within SOLIS. As a member of the NOAO/KPNO High Resolution Spectroscopy Committee, Giampapa is investigating the scientific and technical case for the establishment of a bench-mounted high-resolution spectrograph to be placed at the NOAO/KPNO Mayall 4-m telescope.
xlii Other activities include educational outreach through participation in the REU program and through teachinga class in LaboratoryAstronomy to non-science majorsat the University of Arizona. In addition, Giampapa serves as a member of the editorial boards for the journals Solar Physics and Vistas in Astronomy.
Jack Harvey
Areas of Interest Solar Magnetic and Velocity Fields, Helioseismology, Instrumentation
Recent Research Results Recent research by J. Harvey has focused on helioseismology as applied to the study of the solar interior and atmosphere, and the solar magnetic field as the main driver of solar activity. The helioseismology work has centered on studies of sources of systematic errors since the new, high-quality data available from several sources now makes previously negligible effects much more important. Before strong claims are made about failures of astrophysical theories and the ramifications of these failures throughout astrophysics, it is necessary to make sure that helioseismic data are free of errors. The areas that have been studied in detail are the background spectrum and how it affects frequency measurements, and effects of observational problems in precise measurements of times in the so-called time-distance helioseismology technique. Harvey has also studied the polar and chromospheric magnetic field of the Sun. These fields are important to the activity of the Sun that sometimes directly affects Earth. A surprise was that the polar field is much more readily observed in the chromosphere of the Sun than lower in its atmosphere. This is contrary to other magnetic fields on the Sun.
Future Research Plans During FY 1998 J. Harvey will concentrate on additional studies of helioseismology data from the GONG network, from previous observing runs at the South Pole, and from the SOI/MDI project on board SOHO. A grant from NASA to help support this work was successfully sought and awarded. Some of this work is in collaboration with S. Jefferies (NSO/T), T. Duvall, Jr. (NASA/Stanford), and Y. Osaki and H. Shibahashi (U. of Tokyo). He will also continue studies of the solar magnetic field using unique data from the spectromagnetograph on Kitt Peak, as the level of solar activity continues its rise to a maximum in 2000. Harvey is the principal investigator of a recently awarded ONR grant. This grant supports a new postdoctoral fellow, J. Worden (NSO/T), and continues a long-standing collaboration with R. Howard (NSO/T) to exploit data from the NSO/KP vacuum telescope. We plan to completely re do the software that is used to prepare synoptic data from that facility. One result will be much more accurate and timely information useful to predict space weather.
Service J. Harvey performs observatory service as Chair of the NSO/KP TAC and NSO Scientific Personnel Committee, Instrument Scientist for the GONG project, Telescope Scientist for the KP Vacuum Telescope, Project Scientist for the 10830 and KPVT TCS upgrade projects, and is Interim Project Scientist for the proposed SOLIS project to replace NSO's existing synoptic observing facilities. He expects to continue with those responsibilities. Ln the outside community he serves on the NASA Solar-B Science Working Group (soon to conclude its work), and on NSF and NASA review panels. He is involved with three proposals for NASA spacecraft missions. He recently concluded his service on the NASA Solar Probe Science Working Group and as a member of the LAU Commission 10 Organizing Committee.
xliii Frank Hill
Areas of Interest Helioseismology, Asteroseismology, the Fluid Dynamics of the Solar Convection Zone, and the Solar Activity Cycle
Recent Research Results In collaboration with the GONG user community, Hill has produced the initial results from the Global Oscillation Network Group (GONG). These results have shown that the settling of heavy elements in the solar interior has been incorrectly treated in current standard solar models; confirmed that the solar rotation rate is constant along radii in the convection zone, thereby invalidating much of recent dynamo theory; and produced estimates of the variation in sound speed (a proxy for temperature) as a function of depth and latitude. Hill has worked with P. Stark (UC Berkeley) R. Komm (NSO/T), Y. Gu (NCR), and S. Jefferies (NSO/T) on advanced methods, such as multi-taper spectral analysis and wavelet denoising, for estimating the temporal frequency of the oscillations, the most important measurement for inferring the physical conditions in the solar interior. Recently, in collaboration with the Tucson-based GONG team, Hill has found substantial differences in the frequencies measured from oscillation spectra obtained from Doppler velocity compared to those obtained simultaneously from total intensity observations. This calls into question the definition of the fundamental helioseismic observable quantity.
Along with his collaborators D. Haber (U. of Colorado), R. Bogart (Stanford), E. Rhodes (USC), and I. Gonzalez (IAC), Hill has applied his local helioseismic ring diagram technique to several datasets obtained from SOHO/MDI, Mt. Wilson, GONG, and the KPVT High-L Helioseismometer. In all cases, the inferred horizontal velocity field within the outer convection zone shows a striking spiral in its azimuthal direction with increasing depth. This behavior is similar to the Ekman spiral observed in the Earth's oceans, and is also seen in numerical models of astrophysical convection. Hill, in collaboration with D. Haber (U. of Colorado), T. Duvall (NASA/Stanford), and J. Schou (Stanford), has found that these results are in agreement with those obtained by the time-distance and global analysis methods. In collaboration with E. Zweibel (U. of Colorado) and D. Haber, Hill has developed a method to infer the magnetic field as a function of depth and location using the ring diagrams.
Along with C. Pilachowski (NOAO), S. Barden (KPNO), M. Giampapa (NSO/T), J. Harvey (NSO/T), and C. Keller (NSO/T), Hill has obtained asteroseismic observations of Eta Bootes, Procyon, and Alpha Triangulum. This group has so far been unable to confirm the p-mode spectrum of Eta Bootes obtained by Kejldsen, et al.
Future Research Plans Hill will continue the development of methods to determine the parameters of the structures (peaks, ridges, rings) that are the signature of the solar oscillations in multi-dimensional power spectra, a fundamental and pervasive problem in helioseismology. Hill will also continue improving the GONG data reduction pipeline to reduce systematic errors resulting from the data processing. In collaboration with S. Ehgamberdiev (Uzbekistan), Hill will combine data from GONG, LRLS, and TON to improve estimates of the internal solar structure. This collaboration is funded by an award from the Civilian Research and Development Foundation (CRDF). Hill plans to continue his local helioseismic studies of the velocity and magnetic fields in the outer solar convection zone using several different datasets. Synoptic observations obtained over the course of a solar cycle will be used to study the temporal evolution of the flows in the outer solar convection zone. Studies of flows associated with magnetic helicity and active longitudes will also be made.
xliv Along with the other NOAO asteroseismology enthusiasts, Hill obtained 35 nights of observations of the spectrum of Procyon. This is currently being reduced, and will be used to search for low-amplitude stellar oscillations. Funded by a NASA SOHO GI proposal, Hill will work with T. Ayres (U. of Colorado) and D. Rabin (NSO/T) to investigate the relationship between the cooling and heating of the solar atmosphere and the acoustic wave energy propagating through it.
Service Hill serves as the GONG Data Scientist, developing algorithms for the reduction and analysis of data for global helioseismology. Hill serves as the NSO Digital Library Scientist, and was awarded a grant from the NSF Space Weather Program to place the NSO KPVT data on-line and make it accessible over the Internet. Hill typically supervises six staff, currently three scientists, two programmers, and one data technician. He is a member of the NOAO Stellar Oscillation Network Group (SONG) Steering Committee, the LAU Commission 12 Organizing Committee, the LRLS helioseismology network Scientific Committee, the NASA Space Physics Data System Solar Physics Discipline Team, and the NSO Telescope Allocation Committee. He developed an educational module on helioseismology for K-3 students, and is a participant in Project ASTRO.
Robert Howard, Astronomer Emeritus
Areas of Interest Observational Study of Surface Active-Region and Sunspot Orientations and Velocities as Diagnostics of Sub-Surface Conditions Related to the Dynamo Process in the Sun
Recent Research Results Studies of the Mount Wilson datasets have shown recently that the surface rotation of the magnetic axes of active regions is directed on average toward the average orientation in each hemisphere (not toward the east-west orientation). The average orientation is a tilt of a few degrees, with the leading portion of the regions equatorward of the following portions. It is not clear why this tendency for motion of the axis toward the average values should exist. It may signal a preferred orientation of the subsurface flux ropes that are the source of the active regions. Earlier theoretical work which explained the average orientation as due to the effect of the Coriolis force on rising flux tubes is now in some doubt.
Future Research Plans Howard will continue studies of surface characteristics of solar active regions as diagnostics of sub surface flux tube dynamics. This work promises to shed light on the dynamo process that is believed to operate near the base of the solar convection zone. These studies are being carried out in part in collaboration with P. Gilman (HAO, Boulder, CO) and K.R. Sivaraman (Lndian Lnstitute of Astro physics, Bangalore, India). This project involves the analysis of measurements of the positions and areas of all of the sunspots on the daily Kodaikanal (India) white-light, full-disk photographs of the Sun, which started in 1906. Analysis of these data, in conjunction with similar data from Mount Wilson measured several years ago, will continue during the next year. The Kodaikanal and Mount Wilson datasets will be combined into one large dataset. Ln order to do this, optical aberrations in the Kodaikanal dataset must be identified and corrected for. Using the combined dataset, rotation rates and meridional motions of these spots will be examined, and the results from the observations at the two sites will be compared. Other work by Howard utilizes the Mount Wilson sunspot dataset and the Mount Wilson magnetic active region dataset, put together by Howard several years ago. These studies will center on effects, such as the Coriolis force and magnetic tension in the subsurface flux loops, that govern the orientations and motions of the magnetic field lines that emerge to form active regions.
xlv Service Howard provides editorial assistance for all NSO documents (quarterly reports, newsletter input, etc.) As a service to the community, he serves as co-editor of the journal Solar Physics.
Stuart Jefferies
Areas of Interest Solar/Stellar Oscillations, Image Restoration and Reconstruction
Recent Research Results By performing a time-distance analysis of the solar acoustic waves with frequencies above the nominal atmospheric acoustic cut-off frequency (approximately 5.3 mHz), Jefferies, Y. Osaki (U. of Tokyo), H. Shibahashi (U. of Tokyo), T. Duvall (NASA/Stanford), S. D'Silva (U. of Michigan), and J. Harvey have shown that these waves are partially reflected at both the Sun's photosphere and a layer located higher in the atmosphere. The result supports recent reports of chromospheric modes and opens up the possibility of using the high-frequency acoustic waves to produce local three-dimensional maps of the sound speed and magnetic fields in the solar atmosphere.
Along with S. Vorontsov (U. of London), Jefferies has also studied the characteristics of the high- frequency region of the solar oscillation power spectrum to obtain information on the nature of the oscillation source. Measurements from intensity oscillation power spectra obtained at the geographic South Pole suggest that the source of the high-frequency acoustic waves is located at the base of the photosphere and is emitting both dipole and quadrupole radiation in roughly equal amounts.
Jefferies and N. Meunier (Meudon Obs.) have developed a technique to improve the accuracy with which the solar oscillation power spectrum can be modeled. Their research suggests that many of the oscillation measurements reported in the literature to date are likely to be contaminated by systematic offsets. Inversions of these biased data will lead to incorrect inferences about the Sun's internal structure.
Jefferies, N. Kobayashi (Tokyo Inst, of Tech.), and H. Shibahashi (U. of Tokyo), have preliminary results that show that it may be possible to invert solar oscillation time-series data to reproduce maps of the solar surface which identify the surface locations and times of the excitation events that produce the solar acoustic waves.
Jefferies, K. Shibasaki (Nobeyama Radio Observatory), and H. Shibahashi (U. of Tokyo), are studying the Nobeyama radioheliograph data for evidence of solar oscillations.
Jefferies and C. Toner are looking for the signature of solar g-modes by examining the intensity signal observed at the solar limb. This approach differs from the traditional method of using the entire full-disk signal, and hopes to capitalize on the fact that the g-mode signal is predicted to be a maximum at the solar limb. The detection of g-modes would allow a more accurate probing of the deep solar interior.
Jefferies, with A. Cacciani, P-F. Morretti, and V. DiMartino (all U. of Rome) have made simultaneous velocity and magnetic field measurements of a large emerging sunspot in an attempt to detect Alfven waves in the solar atmosphere. These waves are believed to play an important role in the heat loss from sunspots, the heating of coronal loops, and the generation of the solar wind. A preliminary reduction of the data suggests that Alfven waves may have been detected.
Jefferies, J. Christou (Starfire Optical range), K. Hege (U. of Arizona), and M. Cheselka (U. of Arizona) have developed an iterative algorithm to solve the blind deconvolution problem. This is a problem in
xlvi which the observer has incomplete knowledge of both the object of interest and also how the observation has been degraded. Restoration of infrared images of Ml3 and M31, obtained with the Multiple Mirror Telescope on Mt. Graham, have produced data of a quality comparable to data of the same object obtained with the Hubble Space Telescope. In particular, the restored M31 data showed that M31 has a double nucleus; this has only been seen before in the HST data.
Future Research Plans Jefferies plans to continue with the above-mentioned projects until closure.
Service Jefferies coordinates the internal NSO reviewing of papers.
Christoph Keller
Areas of Interest Solar Magnetic Fields (Observations and Interpretation), High-Precision Imaging Polarimetry (Visible and Near-Infrared), Lmage Reconstruction Techniques (Speckle Imaging and Phase-Diversity), Large Telescope Design, Detector Development (Polarimetry, Hyper-Spectral Imager), Asteroseismology
Recent Research Results Extremely precise linear polarization measurements have recently opened a new window to solar research. These techniques, developed by Keller, give new insight into atoms and molecules and their radiation in the solar atmosphere and properties of weak, turbulent magnetic fields. It was found that the turbulent field on the Sun changes in strength by up to a factor of 10, which is completely unexpected. Collaborative observations in the optical range, radio, UV, and X-ray regimes have been analyzed. In the optical range, downflows in magnetic regions have been detected and studied in detail. These observations will provide new hints on the dynamics of the quiet Sun from the photosphere to the corona. The equivalent width method, an observational approach currently favored in asteroseismology, has been tested on the Sun. Unfortunately, the solar observations have failed to support this new method.
Future Research Plans Keller will use the McMath-Pierce telescopes to investigate solar magnetic fields in the quiet Sun, in particular weak and turbulent fields, by using the Zurich Imaging Stokes Polarimeter I and U and the Near-Infrared Magnetographs (NLM) 1 and 2. The new NLM 2 instrument will be used to get extensive vector magnetic field data. Further observations of scattering polarization will be used to deduce spatial and temporal variations of the turbulent magnetic field of the Sun. Apart from solar work, Keller will work on asteroseismology in connection with the Stellar Oscillations Network Group (SONG).
Service Keller is the telescope scientist for the McMath-Pierce telescopes. He provides observing support at the McMath-Pierce facility, is involved in the design and implementation of new instruments such as the Near-Infrared Magnetograph 2 and the Solar Optical Long-term Investigations of the Sun (SOLIS). Keller is a member of the Project Review Committee and the NOAO Exploration of Technology group, and chaired the Large Telescope Advisory Committee.
Jeffrey Kuhn
Areas of Interest Helioseismology, Infrared Solar Physics, Instrumentation, Astrophysics
xlvii Recent Research Results Kuhn, H. Lin, and R. Coulter (NSO/SP), have completed the final version of a precision photometric telescope, which is being deployed in a small network that will allow high-accuracy solar photometric images to be obtained on a nearly continuous basis. These data are needed to understand how changes in the solar irradiance and luminosity are caused. The data from the first telescope in this network are being distributed to various international research groups. With Lin, Kuhn is building a new high dynamic range LR camera for 1-2.5 micron spectrophotometry. Kuhn (working as a co-Investigator of the SOHO/MDI experiment) used satellite data to measure the solar oblateness with an accuracy that had not previously been achieved from groundbased measurements. He also used the astrometric MDI data to show that the solar photosphere is corrugated with a long-lived pattern of surface features with an average vertical extent of about 1 km and a transverse spatial scale of about 6x10 km. With H. Smith and S. Hawley (Michigan State U.), J. Kuhn verified his dynamic galactic tidal interaction model for the Carina and Draco dwarf spheroidal galaxies. These measurements established that these Milky Way satellite galaxies are not in equilibrium, and that present dynamical mass estimates are wildly in error. Kuhn, working with the SOAR consortium astronomers, spent considerable time justifying the technical feasibility and scientific rationale for building a 4-m low-scattered-light, off-axis telescope.
Future Research Plans Kuhn will complete the deployment of the PSPT network at Mauna Loa, Italy, and Sunspot during the next year. Working with R. MacQueen (Rhodes), I. Mann (Max Planck, Lindau), R. Coulter (NSO/SP), H. Lin (NSO/SP), and NCAR scientists, Kuhn will design and construct two infrared experiments (spectroscopy and imaging polarimetry) to fly on an open CI30 aircraft during the February 1998 total solar eclipse. He will complete an analysis of the MDI astrometric data to search for solar g-modes. Kuhn expects to obtain kinematic data from the Draco and Ursa Minor dwarf galaxy stars (with H. Smith and S. Hawley) which may allow an accurate (10%) Milky Way mass estimate. Kuhn will continue to work with the SOAR telescope consortium to help define that telescope configuration and scientific performance.
Service Kuhn will continue to spend one semester per year at MSU. His MDI research program supports a graduate student and a postdoc at the university. He will continue in his role as Science Branch Head at NSO/SP, and as a member of the Telescope Allocation and Priority Review Committees. Kuhn (with H. Lin) continues as the primary scientific contact for LR experiments at NSO/SP. Kuhn serves on approximately 1-2 NSF or NASA review committees per year and on the NSF/AST RISE advisory panel. He will serve on the Big Bear Observatory Advisory Council.
John Leibacher
Areas of Interest Helioseismology and Atmospheric Dynamics
Recent Research Results The first results from GONG are beginning to emerge, ranging from the thermodynamic and kinematic structure of the solar interior, to the effect of spatial inhomogeneities on the p-modes, to the atmospheric response of the resonant and non-resonant sound waves.
Future Research Plans Leibacher will be devoting the majority of his efforts to assuring GONG's technical and scientific success. He will also continue work on techniques of time series analysis and chromospheric oscillations. Ideas about the observational signature of the convective excitation of p-mode oscillations and the
xlviii detection of gravity modes will be pursued with data from GONG as well as the SOI/MDI instrument on board the SOHO spacecraft.
Service Leibacher serves as Director of the Global Oscillation Network Group program. He supervises a PhD candidate, and serves on the editorial board of the journal Solar Physics, on NASA's Space Science Advisory Committee, on the Goddard Space Flight Center's Space Sciences Visiting Committee, and chairs the AAS Solar Physics Division's Hale Prize Committee.
Haosheng Lin
Areas of Interest Solar Irradiance Variations, Infrared Measurements of Solar Magnetic Fields
Future Research Plans H. Lin will continue to work on the construction and implementation of the Precision Solar Photometric Telescope (PSPT) for the RISE project. Lin completed the PSPT prototype, and installed it at Observatory of Rome in Italy in 1996. Daily high photometric precision full-disk data in the Ca LI K wavelength, and in the blue continuum at 4096 A are now available to solar community. Lin expects to implement the second PSPT this year (1997). This is the beginning of the process to build up a database spanning over a solar cycle for the studies of the total solar irradiance variations observed from satellite experiments. In the short term, Lin is interested in using these data for the study of the energy balance of active regions and the continuum contrast of the faculae and network elements; he will also search for brightness structures that may be related to large scale flow on the Sun.
Lin also plans to continue his work on infrared measurements of solar magnetic fields. He constructed a polarization analyzer that is tunable from 1 to 2 microns, and integrated it with the LR array system at Sac Peak. This new LR capability at Sac Peak now allows us to measure solar magnetic field over a broad range of solar features. Lin used this new IR polarimeter to obtain new data on the intra-network magnetic fields, simultaneous photospheric and chromospheric level vector magnetic fields using the Fe I 15648 A and He I 10830 A lines, and filament magnetic field using also the He I 10830 A line. He will continue to explore the potential of this new instrument, including coronal magnetic field measurement using theinfrared Fe XIII line at 10746 A and 10797 A lines.
William Livingston, Astronomer Emeritus
Areas of Interest Solar Magnetic Fields, Solar Rotation, Solar Spectrum Variability with Time (Sun-as-a-Star), LR Spectrum Atlases
Recent Research Results Working with Nadege Meunier (graduate student from Meudon, France), Livingston made high sensitivity magnetic scans of the solar disk using the favorable IR line of Fe at 1.5648 micron. The aim is to detect and measure weak magnetic fields, a project well-suited to solar minimum. They employ a 300 hz polarization modulator which practically eliminates seeing noise. Modeling of the data by Sami Solanki (Zurich) suggests that perhaps over half of the Sun's surface flux goes undetected by ordinary magnetograms. This weak field flux could thus play a role in modulating the solar output by changing the Sun's color slightly.
xlix With Binxun Ye (Beijing), Livingston has devised a new way to measure rotation right at the heliographic poles. The spectrograph slit is positioned about 5 arcsec inside the limb and, with the spectrograph fixed (not turning as is usual to track the heliostat fed image) the Sun's pole is allowed to slide past the slit. They observe the CO fundamental lines at 4.6 microns with a nearby water vapor line as a wavelength reference. CO offers the advantage of sampling only the quiet Sun. By being at the extreme limb, the influence of super granular motions (a confounding noise in Doppler measurements) is suppressed. The object is to search for a predicted solar vortex.
Livingston continues his long-term monitoring of the Sun's irradiance spectrum. In collaboration with O.R. White (HAO/NCAR), they have a continuous record since 1974 of the behavior of chromospheric Calcium H and K, Helium 10830, H-alpha 6562, Calcium 8542, photospheric Carbon 5380, Beryllium 3131, and various Iron lines. Some long-term secular trends have been discovered indicating subtle alterations in the solar output. He also makes 2-3 observations per year with the 1-m FTS. This archive goes back to 1980 and is an attempt to track spectrum line asymmetry arising from the average convective motions of the million plus granules on the disk. It could be that the weak fields mentioned above suppress in a variable way granular convection, possibly another link in the Sun-Climate relation.
Future Research Plans Livingston plans to continue with the above programs, especially the spectrum monitoring.
Service Livingston has been working with the Visitor's Center to coach docents and help with new exhibits. He is also the resource person for phone queries and other requests for solar information.
Douglas Rabin
Areas of Interest Magnetic Fields and Atmospheric Structure
Recent Research Results D. Rabin has been investigating the three-dimensional structure of the solar atmosphere, from the base of the photosphere to the inner corona. The importance of understanding this structure springs from the growing realization that classical one-dimensional models of stellar atmospheres may fail at a basic level because the "average" conditions embodied in the model exist almost nowhere in the actual, highly inhomogeneous atmosphere. Rabin's work with T. Ayres (U. of Colorado) and T.A. Clark (U. of Calgary) supports this concept through direct measurements of the temperature field in the solar chromosphere, using vibration-rotation lines of the carbon monoxide molecule in the infrared near 4.8 microns. Rabin discussed the relationship of these measurements to measurements and theoretical extrapolations of the photospheric magnetic field in a survey paper on the three-dimensional structure of the atmosphere. Rabin was part of a team of NOAO scientists and engineers who successfully demonstrated that NOAO's PHOENIX cryogenic infrared spectrograph can be applied to solar observing. This demonstration was undertaken to validate NSO's plan to base a next-generation solar infrared camera on the large-format Aladdin array incorporated in PHOENLX.
Future Research Plans In the coming year, Rabin plans to continue a program of integrating carbon monoxide spectroscopy with ultraviolet spectroscopy and photospheric velocity measurements from the SUMER and MDI instruments on the SOHO satellite, in collaboration with T. Ayres and F. Hill (NSO). Rabin and C. Keller (NSO) will study weak magnetic fields in the photosphere using the Near Infrared Magnetograph (NLM-1) and active-region fields using the Fabry-Perot-based NLM-2 instrument. Rabin will continue to develop a large-format infrared camerabased on an Aladdin array (resulting from the NOAO/USNO collaboration) and an NOAO-developed array controller.
Service Rabin leads the solar infrared program on Kitt Peak and is PI of the NASA-supported Near Infrared Magnetograph projects. He serves on the NSO/Kitt Peak Telescope Allocation Committee and Project Review Committee. This year he was a member of the NSO Large Telescope Advisory Committee, the organizing committee of the Solar Magnetism Initiative, and the scientific organizing committee of the NSO/Sac Peak Summer Workshop on Synoptic Solar Physics. Next year he expects to work on the SOLIS (Synoptic Optical Long-Term Investigations of the Sun) project and on the scientific case for a large solar telescope.
Thomas Rimmele
Areas of Interest Adaptive Optics, Small-Scale Magnetic Fields, Active Region Dynamics, Helioseismology
Recent Research Results Rimmele has recently published results from high resolution observations of umbral fine structure. He found evidence for oscillatory magnetoconvection in a sunspot light bridge. Oscillatory convection in strong magnetic fields has been predicted by theoretical models but never observed before. Rimmele collaborates with P. Goode and L. Strous (NJIT), and Tuck Stebbins (JLLA) studying the excitation of solar oscillations. Their observations show that acoustic power is generated in intergranular lanes and give a detailed description of the mechanism responsible for the conversion of convective energy into acoustic energy. They are also able to show that the acoustic energy is fed into the resonance modes of the Sun.
Future Research Plans Rimmele is involved in the adaptive optics program at NSO. In particular, he is developing techniques for wavefront sensing for extended objects. Working with the Air Force Phillips Lab, he is developing the active optics system at the VTT/SP, which corrects optical aberrations that vary on slow time scales and also serves as a test bed for further development of adaptive optics. He is planning to build a low-order (~ 20 modes) adaptive optics system within the next two years as an intermediate step toward a full-up adaptive optics system. The low-order AO system will provide diffraction-limited imaging during reasonable seeing conditions. Rimmele will continue his efforts to perform observations at the highest spatial resolution, using frame selection techniques, in order to study the properties and the dynamics of small-scale magnetic elements.
Service In an ongoing effort, Rimmele is working with R. Radick (NSO/SP) and R. Dunn (NSO/SP) on improving optical performance of the VTT/SP. This effort is expected to be completed in FY 1997. Rimmele is developing narrow-band filter capabilities for the VTT using Fabry-Perots and participates in an ongoing effort to upgrade CCD detectors at NSO/SP. Rimmele serves as Chair of the Project Review Committee (PRC) and is co-investigator for the CLEAR design study.
Raymond Smartt
Areas of Interest Coronal and Prominence Dynamics; Coronagraphic Instrumentation and Narrow-Band Tunable Filters Recent Research Results Coronal Loop Interactions (CLI) are observed in the emission of the two visible coronal lines, 530.3 nm (FeXLV; T~2x IO6 K) and 637.5 nm (FeX; T~ IO6 K), the images recorded with the NSO/SP 20-cm Emission-Line Coronagraph. Similar events are also observed with the Soft X-Ray Telescope on YOHKOH, and with the Extreme Ultraviolet Imaging Telescope on SOHO. Together these data provide critical information about certain MHD processes occurring in the solar corona, and the role of CLIs in coronal heating. The visible coronal data are uniquely important because of their relatively high angular resolution. With V. Airapetian (CSC/GSFC) and Z. Zhang (U. of Nanjing), Smartt has investigated the appearance of cool plasma material (H-alpha emission) at a CLI site. It is interpreted as a consequence of a radiative instability that occurs in the optically-thin, confined plasma volume of a CLI, following an initial interaction and subsequent cooling. As the temperature falls, radiative cooling becomes much more efficient than cooling by conduction (initially the conductive cooling time is much shorter than the radiative time), which is the condition for the onset of the instability. This can cause a low-pressure condition, resulting in a plasma inflow from the surface to the site. At still lower temperatures, recombination of hydrogen ions becomes more efficient, producing H-alpha emission, and the radiative instability ceases. The confined plasma volume then tends to an overpressured state, and loses energy most efficiently by plasma flows along field lines back to the surface, which is observed, and with velocities similar to those predicted.
Future Research Plans Apart from further work on CLI analysis, Smartt will investigate the properties of the prominence-corona transition region (PCTR) in the case of quiescent prominences. It is generally thought that the PCTR can be characterized by a thin sheath surrounding such prominences, where the temperature rises abruptly from T ~ 10 Kto~10 Kor more, and some observations support this picture. But other observations suggest that coronal temperatures can be present in the vicinity of the skeletal structure within the prominence, as defined by the complex magnetic field interior to the prominence. The properties of active prominences will also be investigated, especially with regard to their formation. Joint experiments to investigate CLIs in EUV lines are planned with the CDS instrument of SOHO, but these await sufficient solar activity to produce major post-flare-loop systems. Work will continue on the mirror- objective coronagraph (MAC) program, specifically the design and construction of MACLLL, provided additional funding is available for its completion.
Service Smartt is a member of the NSO Scientific Personnel Committee, the core planning group for the Sunspot Visitor Center, with specific responsibility for scientific exhibits, and Chair of the NSO/SP Telescope Allocation Committee. Apart from his role with the further development of MACLLI, he is working on the development of a tunable, narrow-band, liquid-crystal Fabry-Perot etalon (under construction at CSLRO). He is a Co-I on the LASCO instrument of SOHO, as well as on two planned SOHO experiments. Finally, he continues to provide assistance, both directly and as a consultant, on various aspects of optical instrumentation refurbishment and development at NSO/SP.
Clifford Toner
Areas of Interest Global and LocalHelioseismology, and ImageRestoration
Recent Research Results Atmospheric and instrumental effects (seeing/scattering) degrade images recorded by groundbased telescopes. This modifies the spatial power distribution. Because helioseismic studies rely on measurements of time variations at different spatial scales to infer the internal properties of the Sun, any
Hi non-solar phenomenon that modulates or redistributes the spatial power can have an adverse effect on the final results. Toner, S. Jefferies (NSO/T), and T. Duvall, Jr. (NASA/Stanford) have developed a restoration technique that corrects full-disk solar intensity images for the deleterious effects of variable seeing and scattering. Toner has also developed a method for determining the correct alignment of the solar images being recorded by the GONG network. Since it is necessary to combine data from all six GONG sites, it is important that the data are all aligned in the same way, otherwise there could be discontinuities in the time series as sites switch on or off.
Future Research Plans The detection and measurement of solar g-modes is of significant importance in the study of the internal structure of the Sun. The g-mode signal in intensity is predicted to peak very close to the solar limb (T. Toutain). Toner and S. Jefferies are developing a technique which takes the difference of the signal in a narrow annulus very close to the limb from the signal in an adjacent (interior) annulus in order to remove the solar background "noise" signal and thus enhance the probability of detecting g-modes. Toner will also be working on updating algorithms for the proposed GONG extension/upgrade.
Service Toner performs observatory service as Assistant Data Scientist for the GONG project.
John Varsik
Areas of Interest Magnetic Fields, Solar Oscillations, Instrumentation
Recent Research Results J. Varsik has continued a collaboration with P. Wilson (U. of Sydney) on the long-term behavior of the solar polar magnetic fields, using high-resolution magnetograms from the Big Bear Solar Observatory. Measurement of the magnetic knots within the unipolar regions near the poles has led to a new method for measuring the rotation rate of the photosphere near the poles, as well as some new ideas on the configuration of subsurface magnetic fields. J. Varsik has also begun work on a study of the effects of airborne dust at Sacramento Peak and Apache Point Observatory, using data from a laser particle counter, as well as dust on mirror surfaces. Results thus far suggest criteria for operation of telescopes so as to avoid excessive contamination by dust.
Future Research Plans Varsik will operate the CLEAR Mock-Up, a project investigating internal seeing and dust control in large, open (not evacuated) solar telescopes. He will also be working on a project to explore the possiblity of basal chromospheric heating within supergranule cells by the acoustic events observed by P. Goode (NJLT), Rimmele (NSO/SP), and their collaborators. The basal chromosphere is a concept primarily developed by the Utrecht group (Schrijver, Zwann, and others) as a way of reconciling flux- flux relations in late-type stars of varying degrees of chromospheric and coronal activity. The basal chromosphere represents a level of chromospheric heating that would be present even if magnetic heating is absent, as may be the case during a Maunder minimum, for example.
Service J. Varsik has assumed responsibility for arranging colloquia at Sacramento Peak. He will also be participating in Project ASTRO, and has been involved with other school and public outreach programs.
liii
APPENDLX 4
NATIONAL OPTICAL ASTRONOMY OBSERVATORIES FY 1996 USER STATISTICS1
VISITOR TELESCOPE USAGE
CTIO2 KPNO3 NSO4 NOAO Totals
Visiting Observers US Foreign US Foreign US Foreign US Foreign US/Foreign
Astronomers 105 54 243 36 110 35 458 125 583
Graduate Students 41 13 92 6 2 3 135 22 157
Other (technicians, 4 6 28 0 19 2 51 8 59 research assistants, etc.)
Total Visitors 150 73 363 42 131 40 644 155 799
Institutions 63 39 86 28 42 25 191 92 283
1 The figures in this table reflect the number of observers/users physically present at each observatory for the fiscal period. Multiple visits by a single observer/user are counted separately. This table does not include NOAO staff.
2 During the fiscal year 1996 a total of 198 observing programs were carried out by visitors and the NOAO staff at Cerro Tololo. Visiting astronomers were assigned 93.2% of the scheduled telescope time and the remaining 6.8% was assigned to the staff.
3 During fiscal year 1996 a total of 254 observing programs were carried outby visitors and the NOAO staffat Kitt Peak. Visiting astronomers were assigned 83% of the scheduled telescope time and the remaining 17% was assigned to the staff. 4 During fiscal year 1996 a total of 211 observing programs were carried out byvisitors and the NOAO staff at the National Solar Observatory. Visiting astronomers were assigned 33% of the scheduled telescope time and the remaining 67% was assigned to the staff.
Table I FUNDING BY SOURCE (Amounts in Thousands)
Scientific Staff Operations and FY-1998 FY-1997 FY-1996 and Support Instrumentation Maintenance Budget Budget(a) Expense ASTRONOMY DIVISION FUNDING Cerro Tololo Inter-American Observatory 1,836 501 4,989 7,325 7,266 6,959 Kitt Peak National Observatory 1,274 4,160 5,434 6,242 5,779 National Solar Observatory - Sunspot 660 311 1,389 2,360 2,369 2,325 USAF - Phillips Laboratory (535) (535) (535) (530) National Solar Observatory - Tucson 762 464 555 1,780 2,098 1,834
National Aeronautics and Space Administrationl (32) (32) (32) (32) U.S. Gemini Project Office 1,075 241 1,316 861 403 Central Computer Services 45 621 666 646 571
Image Reduction and Analysis Facility 132 225 357 379 335 CTIO/KPNO Instrumentation 424 2,549 2,973 2,744 3,915 Global Oscillations Network Group 1,850 1,850 2,166 1,987 RISE 279 152 SOAR 1,220 Central Offices
Director's Office 571 571 620 598 Indirect Cost -Miscellaneous Credits (250) (250) (466) (1,442) REU and Gemini Fellowships 80 80 143 203 Public Information and Education 213 213 210 215 Central Administrative Services 1,529 1,529 1,547 1,457 Central Facilites Operations 1,355 1,355 1,257 1,244 Central Engineering and Technical Services 688 688 623 598 Management Fee 550 550 550 505 Total Astronomy Division Funding 6,075 5,806 16,349 28,230 30,187 27,076
OTHER NSF FUNDING
Chemistry Division: FTS Project 76 63 ATM Division: Space Weather Project 42 ESIE Division: Teacher Enhancement Program 210
ATM Division: RISE 150 NON-NSF FUNDING 3,606 1,658
Total Budget 28,230 34,122 28,947
STAFFING SCHEDULE (In Full Time Equivalents)
Astronomy Division Funded 399.49 395.39 412.64 Other NSF Division Funded 1.00 2.00 Non-NSF Funded 27.10 23.40
Total Staffing 399.49 423.49 438.04
(a) FY-1997 Program Plan Revision I. Astronomy Division funds consist of $27,701,000 new funds and $2,487,660 carried over from FY-1996. Table II
SUMMARY OF ASTRONOMY DIVISION FUNDING BY COST CATEGORY (Amounts in Thousands)
NSO US Gemini CTIO/KPNO Central FY 1998 FY 1997 FY 1996 CTIO KPNO Sunspot Tucson Project Instrumentation GONG RISE SOAR Offices Budget Budget Expense
Payroll and Benefits 5,270 4,489 1,862 1,503 1,866 2,543 1,268 2,799 21,600 20,832 20,249 Supplies and Service 1,244 292 257 119 255 381 428 823 3,799 6,224 4,043 Utilities and Communications 363 285 196 28 430 1,302 1,325 1,240 Domestic Travel 43 119 23 51 104 16 19 44 419 424 332 Foreign Travel 131 76 3 14 29 3 67 8 331 329 385 Equipment 275 173 19 93 85 30 41 82 795 1,070 884 550 550 505 Management Fee 550 USAF and NASA Support (535) (32) (567) (567) (562)
Astronomy Division Funding 7,325 5,434 1,825 1,748 2,339 2,973 1,850 4,735 28,230 30,187 27,076
STAFFING SCHEDULE (In Full Time Equivalents)
Scientists 13.50 14.00 7.00 7.50 10.00 5.00 1.00 1.00 59.00 58.00 62.50 Engineers / Scientific Programmers 20.00 11.00 4.00 6.00 11.00 12.00 14.25 3.00 81.25 81.25 76.25 Administrators and Supervisors 9.00 6.00 3.00 1.00 2.00 15.00 36.00 37.50 37.25 Clerical Staff 18.50 3.69 3.00 1.00 1.00 1.50 1.00 25.35 55.04 53.04 57.99 Technicial Staff 25.00 20.00 9.00 7.00 2.75 20.50 6.00 1.00 7.60 98.85 96.25 106.50 Maintenance and Service Staff 31.00 22.60 9.00 6.75 69.35 69.35 72.15
117.00 77.29 35.00 22.50 26.75 39.00 22.25 1.00 0.00 58.70 399.49 395.39 412.64 Table III
SCIENTIFIC STAFF AND SUPPORT (Amounts in Thousands)
NSO US Gemini CTIO/KPNO Central FY 1998 FY 1997 FY 1996 CTIO KPNO Sunspot Tucson Project Instrumentation GONG RISE SOAR Offices Budget Budget Expense
Payroll and Benefits 1,508 1,044 630 719 947 424 5,272 4,958 4,271 Supplies and Service 47 101 14 17 35 214 278 173 Utilities and Communications 2 Domestic Travel 6 55 13 15 84 173 166 108 Foreign Travel 56 46 3 10 26 142 142 134
Equipment 219 27 28 274 282 61
Astronomy Division Funding 1,836 1,274 660 762 1,120 424 6,075 5,826 4,749
STAFFING SCHEDULE (In Full Time Equivalents)
Scientists 12.50 12.00 7.00 6.50 8.50 46.50 49.50 52.00 Engineers and Scientific Programmers 1.00 1.00 1.00 1.00 Administrators and Supervisors 1.00 1.00 1.00 1.00 Clerical Staff 0.50 0.69 1.00 1.00 3.19 1.69 1.84
Technicial Staff 1.00 1.00 1.00 0.00 Maintenance and Service Staff 0.00
13.00 12.69 8.00 7.50 11.50 0.00 0.00 0.00 0.00 0.00 52.69 54.19 55.84 Table IV
INSTRUMENTATION (Amounts in Thousands)
NSO US Gemini CTIO/KPNO Central FY 1998 FY 1997 FY 1996 CTIO KPNO Sunspot Tucson Project Instrumentation GONG RISE SOAR Offices Budget Budget Expense
Payroll and Benefits 384 217 317 132 2,119 1,268 4,437 4,581 4,904 Supplies and Service 117 95 66 381 428 1,085 3,006 2,533 Utilities and Communications 28 28 28 29 Domestic Travel 16 19 34 21 50 Foreign Travel 3 67 70 67 111 Equipment 81 30 41 151 402 318
Astronomy Division Funding 501 311 464 132 2,549 1,850 5,806 8,105 7,945
STAFFING SCHEDULE (In Full Time Equivalents)
Scientists 0.70 5.00 1.00 6.70 2.70 3.00 Engineers and Scientific Programmers 8.00 1.00 3.00 1.50 12.00 14.25 39.75 38.75 39.50 Administrators and Supervisors 0.00 1.00 1.00 Clerical Staff 1.50 1.00 2.50 2.50 2.50 Technicial Staff 5.00 3.00 5.00 20.50 6.00 1.00 40.50 40.50 44.00 Maintenance and Service Staff 0.00
13.00 0.00 4.00 8.00 2.20 39.00 22.25 1.00 0.00 0.00 89.45 85.45 90.00 Table V
OPERATIONS AND MAINTENANCE (Amounts in Thousands)
NSO CTIO/KPNO Central FY 1998 FY 1997 FY 1996 CTIO KPNO Sunspot Tucson Project Instrumentation GONG RISE SOAR Offices Budget Budget Expense
Payroll and Benefits 3,378 3,444 1,016 467 787 2,799 11,890 11,292 11,074 Supplies and Service 1,081 191 148 37 220 823 2,500 2,939 1,337 Utilities and Communications 363 285 196 430 1,273 1,297 1,209 Domestic Travel 37 64 10 36 20 44 212 237 174 Foreign Travel 75 29 4 3 8 119 121 140 Equipment 55 145 19 12 57 82 370 386 505 Management Fee 550 550 550 505 USAF and NASA Support (535) (32) (567) (567) (562)
Astronomy Division Funding 4,989 4,160 854 523 1,087 4,735 16,349 16,255 14,382
STAFFING SCHEDULE (In Full Time Equivalents)
Scientists 1.00 2.00 1.00 0.80 1.00 5.80 5.80 7.50 Engineers and Scientific Programmers 12.00 11.00 3.00 3.00 8.50 3.00 40.50 41.50 35.75 Administrators and Supervisors 9.00 6.00 3.00 1.00 1.00 15.00 35.00 35.50 35.25 Clerical Staff 18.00 3.00 2.00 1.00 25.35 49.35 48.85 53.65 Technicial Staff 20.00 20.00 6.00 1.00 2.75 7.60 57.35 54.75 62.50 Maintenance and Service Staff 31.00 22.60 9.00 6.75 69.35 69.35 72.15
91.00 64.60 23.00 7.00 13.05 0.00 0.00 0.00 0.00 58.70 257.35 255.75 266.80 Table VI
OPERATIONS AND MAINTENANCE BY COST CATEGORY (Amounts in Thousands)
NSO US Gemini CTIO/KPNO Central FY 1998 FY 1997 FY 1996 CTIO KPNO Sunspot Tucson Project Instrumentation GONG RISE SOAR Offices Budget Budget Expense
Engineering and Technical Services 1,181 1,098 92 154 688 3,212 3,193 2,922 Telescope Operations 875 1,651 583 153 3,262 3,060 3,012 Mountain Operations 947 1,271 522 2,740 2,590 2,593 Central Facilities - Tucson/La Serena 903 241 1,355 2,498 2,144 2,243 Central Computer Services 621 621 608 530 Image Reduction and Analysis Facility 225 225 213 190 Administration (a) 1,083 141 192 248 1,850 3,513 4,112 2,531 Public Information and Education 213 213 210 215 REU and Gemini Fellowships 80 80 143 203 Management Fee 550 550 550 505 USAF and NASA Support (535) (32) (567) (567) (562)
Astronomy Division Funding 4,989 4,160 854 523 1,087 4,735 16,349 16,255 14,382
STAFFING SCHEDULE (In -ull Time Equivalents)
Engineering and Technical Services 14.00 8.00 1.00 8.00 31.00 42.00 38.25 Telescope Operations 20.00 23.00 8.00 3.00 54.00 54.00 57.40 Mountain Operations 23.00 25.60 9.00 57.60 52.10 62.75 Central Facilities 19.00 1.00 2.75 11.75 34.50 34.50 29.75 Central Computer Services 4.00 2.00 7.00 13.00 7.50 6.50 Image Reduction and Analysis Facility 3.30 3.30 3.30 3.00 Administration (a) 15.00 4.00 4.00 2.00 38.95 63.95 53.75 62.00 Public Information and Education 0.00 8.60 7.15 REU and Gemini Fellowships 0.00
91.00 64.60 23.00 7.00 13.05 0.00 0.00 0.00 0.00 58.70 257.35 255.75 266.80
(a) Includes all Director's Offices (NOAO, KPNO, CTIO, NSO), funds held by Directors not yet distributed to specific programs, recruitment, insurance, administrative services, freight to Chile, committee and observer travel support, and indirect cost and miscellaneous credits. Table VII
NON-NSF FUNDED PROGRAMS (Amounts in Thousands)
NSO US Gemini CTIO/KPNO Central FY 1998 FY 1997 FY 1996 CTIO KPNO Sunspot Tucson Project Instrumentation GONG RISE SOAR Offices Budget Budget Expense
Payroll and Benefits 1,572 636 Supplies and Service 535 32 567 1,864 912
Utilities and Communications 5 21 Domestic Travel 85 54
Foreign Travel 12 7
Equipment 68 26
Total Non-NSF Funding 535 32 567 3,606 1,656
STAFFING SCHEDULE (In Full Time Equivalents)
Scientists 0.00 17.50 12.00 Engineers and Scientific Programmers 0.00 3.00 3.90 Administrators and Supervisors 0.00 Clerical Staff 0.00
Technicial Staff 0.00 6.60 7.50 Maintenance and Service Staff 0.00
0.00 0.00 0.00 0.00 0.00 0.00 0.00 0.00 0.00 0.00 0.00 27.10 23.40
APPENDIX 6 Kitt Peak Zero-Based Staffing Model
Position 1st Tel. 2nd Tel. 3rd Tel. 1st 2nd 3rd Assistant Director 1 110,000 Facilities Engineer 1 1 75,000 65,000 Telescope Operators 3 3 120,000 120,000 Instrument Specialists 3 1 180,000 60,000 Queue Observing 3 150,000 Astronomers/Telescope Ops. 5 3 2 450,000 270,000 180,000 Astronomer/Instrument Design 1 1 90,000 90,000 Astronomer/Community Support/Interface Chief Engineer 1 102,000 Mechanical Engineer 1 80,000 Opto-Mechanical Engineer 1 80,000 Mechanical Designer 1 1 52,000 52,000 Machinist 1 1 1 45,000 45,000 45,000 Telescope Technician 1 1 47,000 47,000 Drafting/Documentation 1 43,000 Electronic Engineer 1 1 80,000 80,000 Detector Maintenance Engineer 1 70,000 Detector Maintenance Tech 1 55,000 Electronics Tech (Mtn) 2 1 1 140,000 70,000 70,000 Electronics Tech (Fab) 1 1 1 50,000 50,000 50,000 Software 3 2 1 180,000 120,000 60,000 Database/User Software Support 1 55,000 Administrative Assistantt/Secretary 3 1 100,000 30,000 Librarian 1 46,000 Millwright 1 45,000 Mechanic 1 51,000 HVAC 1 51,000 General Crafts 3 3 3 120,000 120,000 120,000 Custodians 2 1 1 50,000 25,000 25,000 Cook 1 2 25,000 50,000 TOTAL PAYROLL 41 24 16 2,367,000 1,384,000 835,000
US Gemini Program Operations Phase
Position Scientist Technical Administration Director Community Interface 1.00 Newsletters, Web Pages, Talks, Workshops Proposal Preparation 0.65 Feasibility, Simulation Software, etc. Proposal Evaluation 0.15 0.10 0.50 Users Committee/GSC 0.05 0.10 Data Reduction Support 3.00 Instrument Support 0.50 Archive Access 1.10 Remote Observing 0.75 1.00 0.25 Queue Observing 1.00 US Gemini Instrument Program 0.25 1.00 0.50 4.50 Research Time 2.00 6.50 6.20 1.60 Payroll: 14.3 x $66,000 $943K 25% Non-Payroll $314K $ 1,257K