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Sidney C Wolff NOAO/DIR NATIONAL OPTICAL ASTRONOMY OBSERVATORIES NATIONAL OPTICAL ASTRONOMY OBSERVATORIES Cerro Tololo Inter-American Observatory Kitt Peak National Observatory National Solar Observatory La Serena, Chile Tucson, Arizona 85726 Sunspot, New Mexico 88349 ANNUAL REPORT October 1996 - September 1997 October 30,1997 TABLE OF CONTENTS L INTRODUCTION IL AURA BOARD m. SCffiNTDJIC PROGRAM A. Cerro Tololo Inter-American Observatory (CTIO) 1. The Search for High Z Supernovae 2. Nearby Stars and Planets 2 B. Kitt Peak National Observatory (KPNO) 3 1. The History of Star Formation in Distant Galaxies 3 2. Oxygen Abundance and the Age of the Universe 4 3. The Age of Elliptical Galaxies - Is There Enough Time? 5 C. National Solar Observatory (NSO) 5 1. Results from GONG 5 2. High-Resolution Images of Solar Magnetic Fields 6 3. Active Optics Control Loop Closed at the Sac Peak Vacuum Tower Telescope 7 IV. DIVISION OPERATIONS 7 A. CTIO 7 Telescope Upgrades and Instrumentation 7 1. 4-m Upgrades 8 2. Major Instrumentation Efforts 9 3. SOAR 4-m Telescope Project 9 4. CCD Implementation and ARCON Controller Development 10 5. Existing Small General-User Telescopes on Cerro Tololo 10 6. New "Tenant" Installations and Upgrades 10 7. Other 11 B. KPNO 12 1. Image Quality Improvements 12 2. WTYN Queue Observing Experiment 12 3. WTYN 13 4. KPNO Instrumentation Improvements 14 5. Burrell-Schmidt 14 C. NSO 15 1. Kitt Peak 15 2. Sacramento Peak 17 3. Digital Library Development 21 D. USGP/ScOpe 21 E. NOAO Instrumentation 25 1. CCD Mosaic Imager 26 2. Phoenix 26 3. Hydra for CTIO 26 4. SQIID Upgrade 27 5. Gemini IR Array Controllers 27 6. Gemini Near-IR Spectrometer 27 7. High-Efficiency Spectrograph 28 V. MAJOR PROJECTS 28 A. GONG 28 B. RISE/PSPT 30 C. SOLIS 32 D. CLEAR 33 E. SOAR 34 VI. CENTRAL COMPUTER SERVICES 34 A. Tucson 34 B. Mountain Programming Group 35 C. CTIO - La Serena 35 D. CTIO -Communications 36 E. NSO-Sunspot 36 Vn. SCIENTIFIC STAFF 36 A. Hired 36 B. Completed Employment 37 C. Changed Status '. 37 Vffl. DIRECTOR'S OFFICE „ 37 EX. NOAO STATISTICS , 38 A. CTIO 38 B. KPNO 39 C. NSO '40 D. NOAO Tucson Headquarters Building 41 APPENDICES Appendix A NOAO Technical Reports List Appendix B CTIO Publications List Appendix C KPNO Publications List Appendix D NSO Publications List L INTRODUCTION This report covers the period 1 October 1996 - 30 September 1997. The National Optical Astronomy Observatories (NOAO) are operated by the Association of Universities for Research in Astronomy, Inc. (AURA), for the National Science Foundation (NSF). The four divisions of the NOAO are: the Cerro Tololo Inter-American Observatory (CTIO) in northern Chile; the Kitt Peak National Observatory (KPNO) near Tucson; the National Solar Observatory (NSO) with facilities on Kitt Peak and at Sacramento Peak, New Mexico; and the US Gemini Program (USGP) based in Tucson. NOAO observing and data reduction facilities are available to the entire astronomical community. The NOAO Home Page contains on-line information about NOAO services, including telescope schedules and instrument availability, and information about how to apply for telescope time. The NOAO Home Page can be accessed through the World Wide Web at http://www.noao.edu/. IL AURA BOARD AURA is a private, non-profit corporation that operates world-class astronomical observatories through its "operating centers." NOAO is an operating center managed by AURA, under cooperative agreement with NSF. There are thirty-one AURA member institutions, including four international affiliates. The member institutional representatives elect a governing Board of Directors: thirteen members, including the President, ex-officio. In addition to NOAO, AURA operates and manages the Space Telescope Science Institute under contract with NASA, and the International Gemini Project under cooperative agreement with the NSF on behalf of six partner countries. m. SCIENTIFIC PROGRAM Several hundred papers are published each year based on data from NOAO. A sample of recent work is described in this section of the report. A. Cerro Tololo Inter-American Observatory (CTIO) 1. The Search for High Z Supernovae It has long been known that modeling the observed Hubble Diagram (the magnitude- redshift relation) could lead to the determination of cosmological parameters if "standard candles" of sufficient luminosity could be found and calibrated for use at large redshift (z - 0.3 - 0.6). The recent work of M. Hamuy (U. of Arizona) and collaborators (carried out with CTIO telescopes and reported in the December 1996 Astronomical Journal) establishes the type la supernova as such a calibrated standard candle. After an initial find of a single object by a Danish group at ESO in 1989 and with standard candle in hand, two groups have made extensive use of CTIO facilities in the past year to carry out searches for high z supernovae in order to determine or constrain the cosmological parameters Q.M (the mean matter density parameter) and Q.A (the vacuum energy density parameter). The high z searches will help to place limits on these parameters for certain cosmologies and may eventually answer the long standing question about the type of universe we inhabit: is it open, closed, or flat? The two groups involved are: S. Perlmutter (Lawrence Berkeley Labs.) and collaborators, collectively known as the Supernova Cosmology Project (SCP), and B. Schmidt (Mt. Stromolo Obs., Australia), N. Suntzeff (CTIO), and collaborators. The primary problem with using the type la supernovae as cosmological probes (aside from understanding their characteristics as standard candles) is that they are random events which last only a relatively short time. Finding them is a statistical process which requires covering a large area of sky down to faint limiting magnitudes. Both groups have been successful in large part due to the image quality at the CTIO 4-m combined with the large areal coverage and sensitivity provided by the Big Throughput Camera (BTC). The BTC is a visitor instrument currently available for use at CTIO. It was developed by A. Tyson (Bell Labs., Lucent Technologies) and G. Bernstein (U. of Michigan) and employs a mosaic of four 2048 x 2048 CCDs covering 0.25 sq. degrees in a single exposure. Both supernova groups employ a number of other telescopes (including the MMT, CFHT, HST, WIYN, and Keck) in the post-discovery phase to track the light curves (necessary to obtain the intrinsic luminosity of a given supernova) and obtainspectra(necessary to distinguish the type la's from other typesand obtainthe redshift). The SCP and Schmidt, et al. groups have so far each found roughly 30 type la's in the required redshift range. Preliminary results suggest a near critical value of the density parameter for a universe with no vacuum energy density (see Perlmutter, et al. in the July 1997 issue of the Astrophysical Journal) and that the local and global values of the Hubble constant (H0, the present expansion rate of the universe) do not differ by more than about 10% in a flat or zero vacuum energy density universe (see Kim, et al. in the February 1997 issue of the Astrophysical Journal). 2. Nearby Stars and Planets Several groups are currently utilizing CTIO telescopes to search for objects at the other end of the astrophysical luminosity scale from type la supernovae. These are the on going programs designed to find new solar neighbors within 10 pc, the Research Consortium on Nearby Stars (RECONS) project, and the Probing Lensing Anomalies NETwork (PLANET) collaboration which is doing follow-on monitoring of microlensing events towardthe Galactic bulge. a. RECONS, a project of T. Henry (STScI) and collaborators, is searching a volume of space 10 pc in radius for as yet undiscovered solar neighbors. They estimate an additional 130 systems have yet to be found in this volume if the density of stellar systems is the same as that in the volume out to 5 pc radius from the Sun. RECONS is systematically characterizing the coolest (M type) dwarfs in the nearby sample with new JHK photometry, red spectroscopy, and speckle images designed to detect companions. The cool dwarf stars contribute as much as 70% of the Galaxy's stars by number, about 50% by mass. In addition to seeking new members of the solar neighborhood, the RECONS project plans to obtain good infrared photometry for the entire sample of nearby stars (combined with optical photometry from the literature) and spectra for all the faintest (Mv > 8.0) M dwarfs to determine the local mass and luminosity functions to a very high degree of accuracy. These data can be used to study the transition between stellar and sub-stellar objects, Galactic structure, and the star-formation process through a better knowledge of observed stellar multiplicity. Much of the near infrared photometry and red spectroscopy have been carried out on the CTIO 1.5-m telescope with the facility infrared imager, CIRIM, and on the CTIO 4-m Blanco telescope using the R-C spectrograph. This includes work done on LHS 1565, which RECONS has established as the 20th nearest stellar system to the Sun (see their article in the July 1997 issue of the Astronomical Journal). The most recent CTIO observing session for RECONS promises exciting results for the future: they have identified a number of new solar neighbors as well as new "ultra cool dwarfs," including several likely brown dwarfs. b. The PLANET collaboration, organized by P. Sackett (Kapteyn Lab.), began extensive monitoring of Galactic bulge microlensing events this year at CTIO using the 0.9-m telescope. The collaboration makes use of telescopes throughout the southern hemisphere to follow the events 24 hours per day. Microlens hunting collaborations monitor millions of stars toward the bulge each night during the southern winter.
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  • Galaxy Data Name Constell

    Galaxy Data Name Constell

    Galaxy Data name constell. quadvel km/s z type width ly starsDist. Satellite Milky Way many many 0 0.0000 SBbc 106K 200M 0 M31 Andromeda NQ1 -301 -0.0010 SA 220K 1T 2.54Mly M32 Andromeda NQ1 -200 -0.0007 cE2 Sat. 5K 2.49Mly M31 M110 Andromeda NQ1 -241 -0.0008 dE 15K 2.69M M31 NGC 404 Andromeda NQ1 -48 -0.0002 SA0 no 10M NGC 891 Andromeda NQ1 528 0.0018 SAb no 27.3M NGC 680 Aries NQ1 2928 0.0098 E pec no 123M NGC 772 Aries NQ1 2472 0.0082 SAb no 130M Segue 2 Aries NQ1 -40 -0.0001 dSph/GC?. 100 5E5 114Kly MW NGC 185 Cassiopeia NQ1 -185 -0.0006dSph/E3 no 2.05Mly M31 Dwingeloo 1 Cassiopeia NQ1 110 0.0004 SBcd 25K 10Mly Dwingeloo 2 Cassiopeia NQ1 94 0.0003Iam no 10Mly Maffei 1 Cassiopeia NQ1 66 0.0002 S0pec E3 75K 9.8Mly Maffei 2 Cassiopeia NQ1 -17 -0.0001 SABbc 25K 9.8Mly IC 1613 Cetus NQ1 -234 -0.0008Irr 10K 2.4M M77 Cetus NQ1 1177 0.0039 SABd 95K 40M NGC 247 Cetus NQ1 0 0.0000SABd 50K 11.1M NGC 908 Cetus NQ1 1509 0.0050Sc 105K 60M NGC 936 Cetus NQ1 1430 0.0048S0 90K 75M NGC 1023 Perseus NQ1 637 0.0021 S0 90K 36M NGC 1058 Perseus NQ1 529 0.0018 SAc no 27.4M NGC 1263 Perseus NQ1 5753 0.0192SB0 no 250M NGC 1275 Perseus NQ1 5264 0.0175cD no 222M M74 Pisces NQ1 857 0.0029 SAc 75K 30M NGC 488 Pisces NQ1 2272 0.0076Sb 145K 95M M33 Triangulum NQ1 -179 -0.0006 SA 60K 40B 2.73Mly NGC 672 Triangulum NQ1 429 0.0014 SBcd no 16M NGC 784 Triangulum NQ1 0 0.0000 SBdm no 26.6M NGC 925 Triangulum NQ1 553 0.0018 SBdm no 30.3M IC 342 Camelopardalis NQ2 31 0.0001 SABcd 50K 10.7Mly NGC 1560 Camelopardalis NQ2 -36 -0.0001Sacd 35K 10Mly NGC 1569 Camelopardalis NQ2 -104 -0.0003Ibm 5K 11Mly NGC 2366 Camelopardalis NQ2 80 0.0003Ibm 30K 10M NGC 2403 Camelopardalis NQ2 131 0.0004Ibm no 8M NGC 2655 Camelopardalis NQ2 1400 0.0047 SABa no 63M Page 1 2/28/2020 Galaxy Data name constell.