/ftp/cats/8/63/.



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VIII/63             ATESP radio survey. II.                  (Prandoni+, 2000)
The following files can be converted to FITS (extension .fit or fit.gz)
	atesp.dat table3.dat
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Query from: http://vizier.cds.unistra.fr/viz-bin/VizieR?-source=VIII/63
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drwxr-xr-x 112 cats archive 4096 Nov 7 15:27 [Up] drwxr-xr-x 4 cats archive 4096 Jan 13 2023 [TAR file] -rw-r--r-- 1 cats archive 470 Dec 19 2022 .message -r--r--r-- 1 cats archive 7614 Sep 6 2018 ReadMe -rw-r--r-- 1 cats archive 1031 Sep 24 2018 +footg5.gif -rw-r--r-- 1 cats archive 2555 Sep 24 2018 +footg8.gif -r--r--r-- 1 cats archive 296558 Dec 5 2000 atesp.dat [txt] [txt.gz] [fits] [fits.gz] [html] drwxr-xr-x 2 cats archive 4096 Sep 6 2018 fits -r--r--r-- 1 cats ftp 1392 Sep 6 2018 table3.dat [txt] [txt.gz] [fits] [fits.gz] [html]
Beginning of ReadMe : VIII/63 ATESP radio survey. II. (Prandoni+, 2000) ================================================================================ The ATESP radio survey. II. The source catalogue. Prandoni I., Gregorini L., Parma P., De Ruiter H.R., Vettolani G., Wieringa M.H., Ekers R.D. <Astron. Astrophys. Suppl. Ser. 146, 41 (2000)> =2000A&AS..146...41P ================================================================================ ADC_Keywords: Galaxies, radio ; Surveys ; Galaxy catalogs Keywords: surveys - radio continuum: galaxies - catalogs Description: The ATESP survey is a radio survey accomplished with the Australia Telescope Compact Array (ATCA) at 1.4 GHz over a region of 26 square degrees centered at -40 and ranging in RA from 22h30m to 01h15m. The survey consists of 16 radio mosaics with 8x14 arcsec resolution and uniform sensitivity (1 sigma noise = 79 microJy). The final 6 sigmas catalogue contains 2960 sources down to a detection limit of 0.5 mJy. This region is superposed to the redshift survey ESO Slice Project (ESP) and is partly covered by the EIS survey (Patch A; see Cat. J/A+AS/130/323). Table 3 summarizes the main parameters for the final 16 mosaics: for each mosaic are listed the number of fields composing it (columns x rows), the tangent point (sky position used for geometry calculations) and the synthesized beam (size and position angle). The spatial resolution can vary from mosaic to mosaic depending on the particular array (6A, 6C or 6D) used in the observations. The mean value for the synthesized beam is 8"x14". The last three columns of Table 3 show the results of the noise analysis. For each mosaic we report the minimum (negative) flux (S_min) recorded on the image (typically |S_min| is of the order of 0.5 mJy, corresponding to the value at which we have stopped the cleaning) and the noise level. This has been evaluated either as the FWHM of the Gaussian fit to the flux distribution of the pixels (in the range +/-S_min), in order to check for correlated noise (sigma_fit), or as the standard deviation of the average flux in several source-free sub-regions of the mosaics, in order to verify uniformity (<sigma>).