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

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

Aug 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000noao.prop...36g&link_type=abstract

NOAO Proposal ID #2000B-0036

Physics

Scientific paper

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 (≳30 ksec) galactic fields (b ≲10°) 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 10^-15 erg/s and thus CVs or qLMXBs with Lx=10^31 erg/s out to ~7 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 Hα excess as ``blue'' objects in the R vs. (Hα - 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.

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