^a Effective exposure time after cleaning bad aspect interval and high background intervals (about 8800 s are lost due to high background).
^b Count rates on four ACIS-I CCD (0.57 keV).

   X-ray Catalogue

To detect sources in the Chandra Deep Field South we ran a modified version of the SExtractor algorithm (Bertin & Arnouts 1996) on the 0.57 keV image. This modified detection algorithm is several orders of magnitude faster than the wavelet algorithm of Rosati et al. (1995) or WAVDETECT in the CIAO software (Dobrzycki et al. 1999; Freeman et al. 2002). Detection parameters (e.g., threshold, characteristic object size, and ultimately the signal-to-noise) were chosen to find very faint sources, while limiting the number of spurious sources to 10, or approximately 3% of the total sample.
The number of fake sources as a function of the algorithms' parameters was determined via extensive simulations as described in Tozzi et al. (2001).  For a detailed desrcption of the detection procedure see Giacconi et al. (2002).

1 Msec Catalogue

  LogN-LogS

Rosati et al. (2002)
log N-log S in the soft (0.52 keV), hard (210 keV), and very hard (510 keV) bands from the 1 Ms observations of the CDF-S. The shaded areas indicate uncertainties due to the Poisson statistics (1 ) and the choice of the conversion factor (corresponding to a power law spectrum with = 1.4 ± 0.3). Dashed lines are previous measurements: ROSAT deep surveys in the 0.52 keV band (Hasinger et al. 1998), ASCA surveys in the 210 keV band (Cagnoni et al. 1998; Della Ceca et al. 1999), and the recent XMM Lockman Hole observation in the 510 keV band (Hasinger et al. 2001). Solid lines are predictions from model B by Gilli et al. (2001) (see text for details). The three top panels show the likelihood contours for the best-fit normalization and slope of the faint end in the three bands from the CDF-S (solid line) and CDF-N (dashed line) data. Data points refer to the best-fit values of Tozzi et al. (2001) (300 ks; filled circles) and the Lynx field (190 ks; Stern et al. 2002; open circles).



                            
 

                             Log N - Log S : ASCII files

Soft [0.5-2 keV]

Hard [2-10 keV]

Very hard [5-10 keV]

    Sky coverage


Giacconi et al. (2002)
The sky coverage (area covered vs. flux limit) for the soft image (solid line) and the hard image (dashed line). The sky coverage is plotted against the 210 keV energy flux which is actually used in the catalog.
  

                            Sky coverage : ASCII files

Soft [0.5-2 keV]

Hard [2-10 keV]

Very hard [5-10 keV]

 

  X-ray images

Detection band [0.5-7] keV...................... FITS

Soft band [0.5-2] keV............................... FITS

Hard band [2-10] keV............................. FITS

Adaptive smooth [0.5-7] keV.................. FITS ........ GIF

 

  Exposure maps

Exposure maps are computed in the soft (0.5-2) and hard (2-7 keV) bands for a typical power law spectrum with Gamma = 1.4 (which is the average spectrum of the XRB and therefore of the sources detected in the CDFS).
The units are [sec *cm2].
By dividing the expmaps by the total exposure time (935965.6 sec) we obtained the areamap (in cm2), while dividing the expamp by the maximum effective area in each band, we obtained the timemaps (in sec), which give the effective exposure time. By dividing the net detected counts by the exptime (as given by the Timemaps), one can obtain the net count rate corrected for vignetting.

Exposure map [0.5-2] keV...................... FITS

Exposure map [2-7] keV...................... FITS

Area map [0.5-2] keV...................... FITS

Area map [2-7] keV...................... FITS

Time map [0.5-2] keV...................... FITS

Time map [2-7] keV...................... FITS