An Overview of ChaMPlane Accretion Sources in the Disk, Bulge and Cusp

Details An Overview of ChaMPlane Accretion Sources in the Disk, Bulge and Cusp An Overview of ChaMPlane Accretion Sources in the Disk, Bulge and Cusp

Aug 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004head....8.2510g&link_type=abstract

American Astronomical Society, HEAD meeting #8, #25.10; Bulletin of the American Astronomical Society, Vol. 36, p.955

Astronomy and Astrophysics

Astronomy

Scientific paper

The Chandra Multiwavelength Plane (ChaMPlane) survey is an ongoing effort to survey the accretion source content of the Galaxy. Archived pointings (>30 ksec, b <12deg) on fields without bright point sources or diffuse emission are processed uniformly for source positions, fluxes, colors and variability. Our special interest is in the constraints a 0.5-8keV survey with ACIS can provide for the CV and quiescent X-ray binary (both LMXB and HMXB) numbers in the Galaxy, but stellar coronal sources will be the largest (by far) by product. We describe the survey through Chandra cycles 4-5 and the (l,b) variation of logN-logS counts in the 2-8 keV band, for optimum accretion source sensitivity and minimized absorption effects. We constrain the distribution of hard sources identified with quantile analysis (see Hong et al) and focus here on our deep pointings in the low extinction Baades Window and Stanek Window near the galactic center (see van den Berg et al). These include sources identified with OGLE binaries including an M giant that are likely wind-fed systems containing WDs (or possibly NSs or BHs) and may constrain the hard sources in the central Cusp around SgrA*. The Galactic Bulge source content is also constrained by our deep optical imaging and spectroscopy (see Zhao et al) and now especially by our deep IR photometry of the central Cusp from Magellan (see Laycock et al) for which analysis is in progress.
This work is supported by Chandra grants AR3-4002A, AR4-5003A and GO3-4033A and NSF grant AST-0098683.

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