THE SWIRE/CHANDRA SURVEY: THE X-RAY SOURCES

We report a moderate-depth (70 ks), contiguous 0.7 deg(2) Chandra survey in the Lockman Hole Field of the Spitzer/SWIRE Legacy Survey coincident with a completed, ultra-deep VLA survey with deep optical and near-infrared imaging in-hand. The primary motivation is to distinguish starburst galaxies and active galactic nuclei (AGNs), including the significant, highly obscured (log N(H) > 23) subset. Chandra has detected 775 X-ray sources to a limiting broadband (0.3-8 keV) flux similar to 4 x 10(-16) erg cm(-2) s(-1). We present the X-ray catalog, fluxes, hardness ratios, and multi-wavelength fluxes. The log N versus log S agrees with those of previous surveys covering similar flux ranges. The Chandra and Spitzer flux limits are well matched: 771 (99%) of the X-ray sources have infrared (IR) or optical counterparts, and 333 have MIPS 24 mu m detections. There are four optical-only X-ray sources and four with no visible optical/IR counterpart. The very deep (similar to 2.7 mu Jy rms) VLA data yield 251 (>4 sigma) radio counterparts, 44% of the X-ray sources in the field. We confirm that the tendency for lower X-ray flux sources to be harder is primarily due to absorption. As expected, there is no correlation between observed IR and X-ray fluxes. Optically bright, type 1, and red AGNs lie in distinct regions of the IR versus X-ray flux plots, demonstrating the wide range of spectral energy distributions in this sample and providing the potential for classification/source selection. Many optically bright sources, which lie outside the AGN region in the optical versus X-ray plots (f(r)/f(x) > 10), lie inside the region predicted for red AGNs in IR versus X-ray plots, consistent with the presence of an active nucleus. More than 40% of the X-ray sources in the VLA field are radio-loud using the classical definition, R(L). The majority of these are red and relatively faint in the optical so that the use of R(L) to select those AGNs with the strongest radio emission becomes questionable. Using the 24 mu m to radio flux ratio (q(24)) instead results in 13 of the 147 AGNs with sufficient data being classified as radio-loud, in good agreement with the similar to 10% expected for broad-lined AGNs based on optical surveys. We conclude that q(24) is a more reliable indicator of radio-loudness. Use of R(L) should be confined to the optically selected type 1 AGN.