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NOAO Newsletter NOAO-NSO Newsletter Issue 82 June 2005 Science Highlights Cerro Tololo Inter-American Observatory Low-Luminosity, Compact Accretion Sources SOAR Update .......................................................................................24 in the Galaxy.. .....................................................................................3 Virtual Observing ...............................................................................25 Gemini Observations of the Two Intrinsically Other Happenings at CTIO ...............................................................27 Brightest Minor Planets.. ..................................................................5 Th e Sun’s New Neighbors .....................................................................7 Kitt Peak National Observatory Magnetic Field Changes during Solar Flares ....................................8 Tohono O’odham Dispute Process of VERITAS Th e Spatial Distribution of Sodium on Mercury ..............................9 Site Selection on Kitt Peak .............................................................28 Community Time Off ered on Calypso 1.2-Meter Telescope.. .....29 Director’s Offi ce More Details Emerge on the NSF Senior Review.. .........................11 National Solar Observatory/GONG New Partnership Opportunities at NOAO.. ....................................13 A Time of Transitions .........................................................................30 Q&A with Tom Matheson ..................................................................14 Austin Keith Pierce 1918–2005 ..........................................................32 ATST Project Developments.. ............................................................33 NOAO Gemini Science Center SOLIS .....................................................................................................35 Th e Gemini Rapid Response Mode.. ................................................16 Instrumentation for Nighttime Use at the NIRI and Altair: Report from a Successful McMath-Pierce Solar Telescope ....................................................36 Observing Run .................................................................................17 GONG ....................................................................................................38 Phoenix in Classical Mode.. ...............................................................18 Following the Aspen Process: Presentations Public Aff airs & Educational Outreach and Reviews ......................................................................................18 Astrobiology Weekend at the NGSC Instrumentation Program Update .......................................20 McMath-Pierce Solar Telescope ....................................................41 2005 CTIO REU/PIA PROGRAM ....................................................41 Observational Programs Th e Sky is the Limit—Student Light Pollution Surveys 2005B Proposal Process Update.. ......................................................21 in Both Hemispheres.. .....................................................................43 2005B Instrument Request Statistics by Telescope ........................21 FunFest 2005 ........................................................................................44 2005B TAC Members ..........................................................................23 “World Year of Physics” Celebrated at Kitt Peak.. ..........................44 On the Cover Th e dynamic solar chromosphere on 18 January 2005 is seen in this false color image. Daily images like this one, made with the new SOLIS vector spectromagnetograph, have been obtained with various instruments on Kitt Peak for 31 years. Shown is the strength of the He I absorption line at 1083 nanometers; dark is increasing line absorption. Unique among lines accessible from the ground, helium line strength is controlled in part by the intensity of emission from the overlying corona and also has negligible strength in the cool photosphere. Th is allows mapping of the bases of coronal features like holes, fi lament channels, and streamers. Such features are important in forecasting space weather. Image Credit: NSO/AURA/NSF The NOAO-NSO Newsletter is published quarterly by the National Optical Astronomy Observatory P.O. Box 26732, Tucson, AZ 85726 [email protected] —Governor—Governor JanetJanet NNapolitanoapolitano issuedissued thisthis letterletter toto thethe AArizonarizona HouseHouse ooff RepresentativesRepresentatives followingfollowing herher secondsecond vetoveto thisthis yearyear ofof legislationlegislation thatthat wouldwould hhaveave oopenedpened tthehe ddooroor Douglas Isbell, Editor for further development of illuminated billboards and fl ashing signs across the state.state. TheThe defeatdefeat ofof thisthis legislationlegislation waswas aidedaided signifisignifi cantlycantly byby a coalitioncoalition ofof ArizonaAr izona Section Editors observatoryobservatory directorsdirectors andand a streamstream ofof lettersletters fromfrom observatoryobservatory staffstaff members,members, allall Science Highlights promptedprompted byby thethe tirelesstireless effortsefforts ofof MarkMark Mayer,Mayer, whowho representsrepresents thethe interestsinterests ofof a Joan Najita coalition of Tucson neighborhood associations to state and local government. Dave Bell Observational Programs Mia Hartman Observational Programs Nicole S. van der Bliek CTIO Richard Green KPNO Notable Quotes Ken Hinkle NGSC Sally Adams NGSC “It’s“It’s thethe bbestest thingthing ssinceince ttwowo ppiecesieces ofof sslicedliced bbreadread wwereere aassembledssembled ttoo mmake ake John Leibacher NSO Priscilla Piano NSO a sandwich.” Douglas Isbell Public Affairs & —Paul—Paul Ginsparg,Ginsparg, professorprofessor ofof physicsphysics andand informationinformation sciencescience atat CornellCornell University,Univer sity, Educational Outreach describing the capabilities of a new customized Web alert system from the NASA AstrophysicsAstrophysics DDataata SSystemystem ccalledalled ““myADS,”myADS,” qquoteduoted iinn a HHarvard-Smithsonianarvard-Smithsonian CCenterenter for Astrophysics press release, 18 April 2005. Production Staff Stephen Hopkins Managing Editor Mark Hanna Digital Processing Pete Marenfeld Design & Layout Kathie Coil Production Support 2 June 2005 Science Highlights Low-Luminosity, Compact Accretion Sources in the Galaxy Josh Grindlay (Harvard Observatory and CfA) ccretion onto compact stellar objects (white dwarfs, careful treatment of astrometry for optical identifi cations, neutron stars, and black holes) from companions in and derived source fl uxes for a range of model spectra close binaries is the primary beacon for study of the and absorption columns for both the source number-fl ux Aastrophysics of the extreme: from endpoints of stellar and distribution, logN-logS, and X-ray spectral classifi cation. binary evolution, to the physical processes in the extremes of gravity, radiation, or magnetic fi elds. Accretion from the Initial ChaMPlane results were given for logN-logS in several interstellar medium on the presumed still larger population Galactic fi elds (Grindlay et al. 2003, AN, 324, 57), as well as an of isolated compact objects should, at least for relatively early description of the Mosaic imaging identifi cation survey more massive and low-velocity stellar black holes, also be (Zhao et al. 2003, AN, 324, 176). Th e survey has now achieved observable in certain conditions, yet never has been. Given nearly its original goal of ~100 Chandra ACIS-I or ACIS-S the fundamental role that accretion plays in so many key galactic plane fi elds, with in fact 94 now selected (through problems of interest in current astrophysics, it is surprising Chandra cycle 6). Th ese have |b| ≤ 12o, exposure times that the space density and luminosity function(s) of the most ≥12 ksec (most are >20–30 ksec), and are selected to avoid common accretion-powered compact objects—white dwarfs dense clusters or bright diff use optical emission, and accreting from low-mass stellar companions, or cataclysmic (if possible) to have a minimum hydrogen column density in variables (CVs)—has not been measured to better than a order to maximize the detection and subsequent identifi cation factor of ~10 in the solar neighborhood, and they have even of faint point sources. Th ese 94 ACIS fi elds are covered by less well-known spatial distributions in the Galaxy. 59 Mosaic fi elds (36 x 36 arcmin), as shown in fi gure 1. Motivated by these and related questions, we set out in 2000–2001 to conduct a survey of low-luminosity accretion sources in the Galaxy with the newly-launched Chandra X-ray Observatory. We proposed the Chandra Multiwavelength Plane (ChaMPlane) Survey to constrain • CV space density and X-ray luminosity functions (XLFs) in the disk vs. Bulge; • Galactic Bulge source populations; • Populations of quiescent low-mass X-ray binaries (qLMXBs) with neutron star and black hole primaries and isolated BHs; Figure 1. Distribution of 59 Mosaic fi elds to cover 94 distinct • Be-High Mass X-ray binaries (HMXBs); ChaMPlane fi elds (April 2005). Some 15 Mosaic fi elds cover • Stellar coronal XLFs in the disk vs. Bulge. the Galactic Center region, which includes some 40 Chandra 31 ACIS fi elds. Chandra would fi rst detect low-luminosity (e.g., Lx ~10 erg/s at ~8kpc) sources with suffi cient precision (≤1 arcsec) to enable their optical counterpart candidates to be selected In fi gure 2, we show a “typical” resulting color magnitude and then identifi ed with follow-up
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