A deep X-ray survey of the Lockman Hole Northwest

Details A deep X-ray survey of the Lockman Hole Northwest A deep X-ray survey of the Lockman Hole Northwest

Aug 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005phdt.........1y&link_type=abstract

Ph.D. dissertation.United States -- Maryland: University of Maryland, College Park; 2005. Publication Number: AAT 3183544.243 pa

Computer Science

16

Lockman Hole Northwest, Gravitational Lensing, X-Ray Point, Sources

Scientific paper

I present the X-ray analysis of the Chandra Large Area Synoptic X-ray Survey (CLASXS) of the Lockman Hole Northwest field. The contiguous solid angle of the survey is ~0.4 deg 2 and the flux limits are 5 x 10 -16 erg cm -2 s -1 in the 0.4-2 keV band and 3 x 10 -15 erg cm -2 s -1 in the 2-8 keV band.The survey bridges the gap between deep pencil beam surveys; and shallower, larger are a surveys, allowing a better probe of the X-ray sources that contribute most of the 2-10 keV cosmic X-ray background. A total of 525 X-ray point sources and 4 extended sources have been found. The number counts, X-ray spectra evolution, X-ray variability of the X-ray sources are presented. We show 3 of the 4 extended sources are likely galaxy clusters or galaxy groups. We report the discovery of a gravitational lensing arc associated with one of these sources.
I present the spatial correlation function analysis of non-stellar X-ray point sources in the CLASXS and Chandra Deep Field North (CDFN). I calculate both redshift-space and projected correlation functions in comoving coordinates. The correlation function for the CLASXS field over scales of 3 Mpc < s < 200 Mpc can be modeled as a power-law of the form ξ(s) = (s/s0)-γ, with γ = 1.6+0.4-0.3 and s0 = 8.05+1.4-1.5 Mpc. The redshift-space correlation function for CDFN on scales of 1 Mpc < s < 100 Mpc is found to have a similar correlation length, but a shallower slope. The real- space correlation functions are derived from the projected correlation functions. By comparing the real- and redshift-space correlation functions, we are able to estimate the redshift distortion parameter β = 0.4 +/- 0.2 at an effective redshift z = 0.94. We found the clustering does not dependence significantly on X-ray color or luminosity.
A mild evolution in the clustering amplitude is found, indicating a rapid increase of bias with redshift. The typical mass of the dark matter halo derived from the bias estimates show little change with redshift. The average halo mass is found to be log ( Mhalo/ Msun) ~ 12.4.

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