Optical Imaging Survey of Chandra Galactic Fields: Luminosity Function of CVs and LMXBs

Details Optical Imaging Survey of Chandra Galactic Fields: Luminosity Function of CVs and LMXBs Optical Imaging Survey of Chandra Galactic Fields: Luminosity Function of CVs and LMXBs

Feb 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000noao.prop..374g&link_type=abstract

NOAO Proposal ID #2000A-0374

Physics

Scientific paper

We propose a pilot program to begin a survey of galactic fields imaged at high resolution by the Chandra X-ray Observatory. As part of the Chandra Multiwavelength Project (ChaMP), we seek to identify a large sample of serendipitous x-ray sources located to (few) arcsec precision in the deep (≳30 ksec) galactic fields to be observed in the Chandra cycle 1 program. 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. The deep Chandra galactic fields will detect 2-6 keV fluxes (allowing for low energy absorption) of f_min(2-6 keV)=2× 10^-15fcgs and thus CVs or qLMXBs with L_x=10^31 lcgs out to 7 kpc. Thus most CVs and qLMXBs in the Galaxy can be reached, and the combined ChaMP/optical identification survey offers the best chance for establishing their space density and luminosity functions. CVs and qLMXBs will be identified by their ubiquitous Hα excess as ``blue'' objects in the R vs. Hα vs. R plane down to Mv about 23. We have demonstrated the power of this technique, and the crowded-field analysis methods, in our successful HST identifications of the first CVs in globular cluster cores.

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