Chandra Deep Field South: The 1 Ms Catalog

Abstract

In this Paper we present the source catalog obtained from a 942 ks exposure of the Chandra Deep Field South (CDFS), using the Advanced CCD Imaging Spectrometer (ACIS-I) on the Chandra X-ray Observatory. Eleven individual pointings made between October 1999 and December 2000 were combined to generate the final image used for object detection. Catalog generation proceeded simultaneously using two different methods; a method of our own design using a modified version of the SExtractor algorithm, and a wavelet transform technique developed specifically for Chandra observations. The detection threshold has been set in order to have less than 10 spurious sources, as assessed by extensive simulations. We subdivided the catalog into four sections. The primary list consists of objects common to the two detection methods. Two secondary lists contain sources which were detected by: 1) the SExtractor algorithm alone and 2) the wavelet technique alone. The fourth list consists of possible diffuse or extended sources. The flux limits at the aimpoint for the soft (0.5-2 keV) and -2hard (2-10 keV) bands are 5.5×10 −17 erg s −1 cm −2 and 4.5×10 −16 erg s −1 cm −2 respectively. The total number of sources is 346; out of them, 307 were detected in the 0.5-2 keV band, and 251 in the 2-10 keV band.We also present optical identifications for the catalogued sources. Our primary optical data is R band imaging from VLT/FORS1 to a depth of R ∼ 26.5 (Vega). In regions of the field not covered by the VLT/FORS1 deep imaging, we use R-band data obtained with the Wide Field Imager (WFI) on the ESO-MPI 2.2m, as part of the ESO Imaging Survey (EIS), which covers the entire X-ray survey. We found that the FORS1/Chandra offsets are small, ∼ 1 ′′ . Coordinate cross-correlation finds 85% of the Chandra sources covered by FORS1 R to have counterparts within the 3σ error box ( 1.5 ′′ depending on off-axis angle and signal-to-noise). The unidentified fraction of sources, approximately ∼ 10-15%, is close to the limit expected from the observed X-ray flux to R-band ratio distribution for the identified sample.

THE SFR–M* RELATION AND EMPIRICAL STAR FORMATION HISTORIES FROM ZFOURGE AT 0.5 < z < 4*

“…The FourStar Galaxy Evolution Survey (ZFOURGE 16 : Straatman et al 2015) is a deep near-IR survey conducted with the FourStar imager (Persson et al 2013) covering one 11′ × 11′ pointing in each of the three legacy fields CDF-S (Giacconi et al 2002), COSMOS (Capak et al 2007) and UDS (Lawrence et al 2007) reaching depths of ∼26 mag in J 1 , J 2 , J 3 , and ∼25 mag in H s , H l , and K s (5σ in d = 0 6 apertures). The medium-bandwidth filters utilized by this survey offer spectral resolutions λ/Δλ ≈ 10, roughly twice that of their broadband counterparts.…”

Black hole growth and starburst activity atz= 0.6–4 in the Chandra Deep Field South

“…X-ray data: catalogs and multiband identifications X-ray data for a total exposure time of ∼1 Ms in the GOODS field have been obtained by the CDFS consortium and are publicly available. The source catalog has been published by Giacconi et al (2002), including the basic X-ray properties in three different X-ray bands (source counts, fluxes, exposure times). Subsequently, Alexander et al (2003, hereinafter A03) published a re-analysis of the CDFS data that led mainly to an improved astrometry of the X-ray positions with some differences in the number of detected sources at the very faint counts level (see A03 for more details).…”

Supermassive Black Holes in Galaxies

“…The two deepest images of the X-ray sky ever taken are the 2 Ms Chandra Deep Field-North (CDF-N; Alexander et al 2003) and the 1 Ms Chandra Deep Field-South (CDF-S; Giacconi et al 2002). These data resolve greater than 80 to 90% of the 2−8 keV X-ray background (XRB) into discrete sources.…”