The extended Chandra Deep Field-South survey:: Chandra point-source catalogs

We present Chandra point-source catalogs for the Extended Chandra Deep Field - South (E-CDF-S) survey. The E-CDF-S consists of four contiguous 250 ks Chandra observations covering an approximately square region of total solid angle approximate to 0.3 deg(2), which flank the existing approximate to 1 Ms Chandra Deep Field - South (CDF-S). The survey reaches sensitivity limits of approximate to 1.1 x 10(-16) and approximate to 6.7 x 10(-16) ergs cm(-2) s(-1) for the 0.5 - 2.0 and 2 - 8 keV bands, respectively. We detect 762 distinct X-ray point sources within the E-CDF-S exposure; 589 of these sources are new (i.e., not previously detected in the approximate to 1 Ms CDF-S). This brings the total number of X-ray point sources detected in the E-CDF-S region to 915 ( via the E-CDF-S and approximate to 1 Ms CDF-S observations). Source positions are determined using matched-filter and centroiding techniques; the median positional uncertainty is approximate to 0.'' 35. The basic X-ray and optical properties of these sources indicate a variety of source types, although absorbed active galactic nuclei (AGNs) seem to dominate. In addition to our main Chandra catalog, we constructed a supplementary source catalog containing 33 lower significance X-ray point sources that have bright optical counterparts ( R < 23). These sources generally have X-ray - to - optical flux ratios expected for normal and starburst galaxies, which lack a strong AGN component. We present basic number-count results for our main Chandra catalog and find good agreement with the approximate to 1 Ms CDF-S for sources with 0.5 - 2.0 and 2 - 8 keV fluxes greater than 3 x 10(-16) and 1 x 10(-15) ergs cm(-2) s(-1), respectively. Furthermore, three extended sources are detected in the 0.5 - 2.0 keV band, which are found to be likely associated with galaxy groups or poor clusters at z approximate to 0.1-0.7; these have typical rest-frame 0.5 - 2.0 keV luminosities of (1-5) x 10(42) ergs s(-1).