========================================================================== J/ApJS/180/102 AEGIS-X: Chandra deep survey (Laird+, 2009) The following files can be converted to FITS (extension .fit or fit.gz) table9.dat table10.dat table11.dat ========================================================================== Query from: http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=J/ApJS/180/102 ==========================================================================
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Beginning of ReadMe : J/ApJS/180/102 AEGIS-X: Chandra deep survey (Laird+, 2009) ================================================================================ AEGIS-X: the Chandra Deep Survey of the Extended Groth Strip. Laird E.S., Nandra K., Georgakakis A., Aird J.A., Barmby P., Conselice C.J., Coil A.L., Davis M., Faber S.M., Fazio G.G., Guhathakurta P., Koo D.C., Sarajedini V., Willmer C.N.A. <Astrophys. J. Suppl. Ser., 180, 102-116 (2009)> =2009ApJS..180..102L ================================================================================ ADC_Keywords: X-ray sources ; Surveys ; Cross identifications ; Photometry Keywords: galaxies: active - galaxies: nuclei - surveys - X-rays: galaxies Abstract: We present the EGIS-X survey, a series of deep Chandra ACIS-I observations of the Extended Groth Strip. The survey comprises pointings at eight separate positions, each with nominal exposure of 200ks, covering a total area of approximately 0.67deg^2^ in a strip of length 2 degrees. We describe in detail an updated version of our data reduction and point-source-detection algorithms used to analyze these data. A total of 1325 band-merged sources have been found to a Poisson probability limit of 4x10^-6^, with limiting fluxes of 5.3x10^-21^W/m2 in the soft (0.5-2keV) band and 3.8x10^-19^W/m2 in the hard (2-10keV) band. We present simulations verifying the validity of our source-detection procedure and showing a very small, <1.5%, contamination rate from spurious sources. Optical/NIR counterparts have been identified from the DEEP2, CFHTLS, and Spitzer/Infrared Array Camera (IRAC) surveys of the same region. Using a likelihood ratio method, we find optical counterparts for 76% of our sources, complete to R_AB_=24.1, and, of the 66% of the sources that have IRAC coverage, 94% have a counterpart to a limit of 0.9uJy at 3.6um (m_AB_=23.8). After accounting for (small) positional offsets in the eight Chandra fields, the astrometric accuracy of Chandra positions is found to be 0"8rms; however, this number depends both on the off-axis angle and the number of detected counts for a given source. All data products described in this paper are made available via a public Web site. Description: The data used in this paper were obtained during two Chandra observation cycles. An initial Chandra observation in the EGS region was taken in 2002 August during Cycle 3. These observations of the "Groth-Westphal Strip" (GWS) region have been reported by Nandra et al. (2005, Cat. J/MNRAS/356/568). The majority of the AEGIS-X data were obtained over the period 2005 March-December as part of Chandra Cycle 6.