ChaMPlane Galactic Bulge Latitude Survey: Optical Results

Details ChaMPlane Galactic Bulge Latitude Survey: Optical Results ChaMPlane Galactic Bulge Latitude Survey: Optical Results

Feb 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010head...11.4235z&link_type=abstract

American Astronomical Society, HEAD meeting #11, #42.35; Bulletin of the American Astronomical Society, Vol. 41, p.731

Astronomy and Astrophysics

Astronomy

Scientific paper

We present the initial optical result of the Galactic Bulge Latitude Survey (BLS), which is an important component of our ChaMPlane survey (see Grindlay et al.). It extends from +/- 0.2 to +/- 1.5 degrees along the galactic latitude, centered at the SgrA*. The main goal is to measure the radial gradient of the Lx > 1031.5 erg/s source population (primarily CVs and qLMXBs) along latitude vs. longitude in the galactic bulge. We completed the BLS survey in Chandra cycles 7-10, with 36 ACIS-I pointings of 15ks each (see Hong et al.). The survey covers two 1.2 square-degrees region in the "north" (BLS-N)
and "south" (BLS-S) of the galactic plane. The southern tip of the BLS-S is connected with our Chandra observation "Limiting Window", a low extinction window closest to the SgrA* with Av=3.9. We also completed the corresponding optical and IR (see van den Berg et al.) survey to cover the same region. The optical images (V,R,I,H-alpha band) were obtained from CTIO/4m/Mosaic from 2008 to 2009. Six Mosaic images (36'x36') covers all 36 Chandra pointings. Candidate optical counterparts of the X-ray point sources were found from the Mosaic images. Although, due to severe extinction towards the galactic center, most of the real counterparts are in the foreground of the bulge, except in the southern tip of the BLS-S. Spectroscopic follow-ups for the identified optical counterparts were conducted in 2009 using the CTIO/4m/Hydra for classification, to identify the nature of the Chandra sources.

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