NOAO >   Observing Info >   Approved Programs >   2000B-0036

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Program Information for 2000B-0036


PI: Jonathan E Grindlay, Harvard-Smithsonian Center for Astrophysics, josh@head.cfa.harvard.edu
Address: 60 Garden St., Cambridge, MA 02138 USA

CoI: Peter D Edmonds, Harvard-Smithsonian Center for Astrophysics
CoI: Jeffrey E McClintock, Harvard-Smithsonian Center for Astrophysics
CoI: Ping Zhao, Harvard-Smithsonian Center for Astrophysics
CoI: Michael R Garcia, Harvard-Smithsonian Center for Astrophysics
CoI: Adrienne M Cool, San Francisco State U.
CoI: Stefanie Wachter, IPAC
CoI: Donald W Hoard, IPAC
CoI: Paul J Green, Harvard-Smithsonian Center for Astrophysics
CoI: Belinda Wilkes, Harvard-Smithsonian Center for Astrophysics
CoI: Andrew J Drake, Harvard-Smithsonian Center for Astrophysics
CoI: Vinay Kashyap, Harvard-Smithsonian Center for Astrophysics
CoI: Charles D Bailyn, Yale U.
CoI: Haldan Cohn, Indiana U.
CoI: Maureen Van Den Berg, Harvard-Smithsonian Center for Astrophysics
CoI: Jeroen Homan, MIT
CoI: Silas Laycock, Harvard-Smithsonian Center for Astrophysics

Title: ChaMPlane: Measuring the Faint X-ray Binary and Stellar X-ray Content of the Galaxy

Abstract: We propose to conduct the Chandra Multiwavelength Plane (ChaMPlane) Survey to identify a large sample of serendipitous x-ray sources located to arcsec precision in the deep (\gsim30 ksec) galactic fields (b \lsim10\deg) imaged by the Chandra X-ray Observatory. Our primary goal is to identify cataclysmic variables (CVs) and quiescent Low Mass X-ray Binaries (qLMXBs), primarily black hole x-ray novae in quiescence, in order to constrain and ultimately measure the luminosity functions of each. Secondary objectives are to determine the Be x-ray binary content and stellar coronal source distributions in the Galaxy. The deep Chandra galactic fields will detect 2-6 keV fluxes (allowing for low energy absorption) of \Fx(2-6 keV) = 2 \X ^$ erg/s and thus CVs or qLMXBs with \Lx = 10$^$ erg/s out to $\sim kpc. Thus most CVs and qLMXBs in the Galaxy can be reached, and the ChaMPlane survey offers the best chance for constraining their formation/evolution and the stellar BH content of the Galaxy. CVs and qLMXBs will be identified by their ubiquitous \Halpha excess as ``blue'' objects in the R vs. (\Halpha - R) plane down to R \about 24. We have demonstrated this technique for crowded fields with our HST discovery of the first CVs in globular cluster cores and have now conducted a successful pilot ChaMPlane survey at CTIO.

Program Type: Survey

Scheduled Nights:
Run 1 (2002A):  CT-4m/MOSAIC -- 5n on May 13 - May 17 2002
Run 1 (2003A):  CT-4m/MOSAIC -- 5n on Jun 02 - Jun 06 2003
Run 1 (2004A):  CT-4m/MOSAIC -- 5n on May 16 - May 20 2004
Run 1 (2005A):  CT-4m/MOSAIC -- 5n on Jun 07 - Jun 11 2005
Run 2 (2001A):  CT-4m/MOSAIC -- 2.5n on May 13 - May 17 2001
Run 2 (2002B):  KP-4m/MOSA -- 2n on Dec 07 - Dec 08 2002
Run 2 (2003B):  KP-4m/MOSA -- 2n on Jan 30 - Jan 31 2004
Run 2 (2004B):  KP-4m/MOSA -- 2n on Jan 11 - Jan 12 2005
Run 3 (2000B):  KP-4m/MOSA -- 1n on Dec 05 - Dec 06 2000
Run 3 (2001B):  KP-4m/MOSA -- 0.5n on Oct 25 2001


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