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. =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 (). File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file atesp.dat 87 3370 Full radio catalog table3.dat 86 16 Main parameters for the 16 final mosaics fits/* . 16 Individual fits images -------------------------------------------------------------------------------- See also: http://www.ira.bo.cnr.it/atesp/ : The ATESP survey home page J/A+AS/130/323 : ESO Slice Project (Vettolani+ 1998) J/A+A/457/517 : ATESP 5 GHz radio survey. I. (Prandoni+, 2006) Nomenclature Notes: The ATESP acronym was pre-registered at IAU. Byte-by-byte Description of file: atesp.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 5 A5 --- --- [ATESP] 7- 21 A15 --- ATESP Source IAU name (ATESP JHHMMSS+DDMMSSA) (1) 24- 25 I2 h RAh Right ascension (J2000) 27- 28 I2 min RAm Right ascension (J2000) 30- 34 F5.2 s RAs Right ascension (J2000) 36 A1 --- DE- Declination sign (J2000) 37- 38 I2 deg DEd Declination (J2000) 40- 41 I2 arcmin DEm Declination (J2000) 43- 46 F4.1 arcsec DEs Declination (J2000) 48- 54 F7.2 mJy Fpeak Source peak flux (1400MHz) 57- 62 F6.2 mJy Fint Source integrated flux (1400MHz) 66- 71 F6.2 arcsec FWHMa Intrinsic source angular size, major axis (2) 74- 78 F5.2 arcsec FWHMb ? Intrinsic source angular size, minor axis (2) 80- 84 F5.1 deg PA [-90/90]? Source Position Angle (measured from N through East) for the major axis 86- 87 A2 --- Flag [EMS* ] Fitting procedure flag (3) -------------------------------------------------------------------------------- Note (1): The name is based on J2000 coordinates. Different components of multiple sources are labeled "A", "B", etc. Note (2): Intrinsic = deconvolved from the beam. Zero values refer unresolved sources. Note (3): Flags indicating fitting procedure and parametrization adopted: S: gaussian fitting S*: poor gaussian fitting E: non gaussian source M: multiple source -------------------------------------------------------------------------------- Byte-by-byte Description of file: table3.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 9 A9 --- Field Mosaic field (1) 10 A1 --- n_Field [d] d: reported values for Smin and noise refer to masked mosaic (see text) 12 I1 --- Nx Number of columns 13 A1 --- --- [x] 14 I1 --- Ny Number of rows 16- 17 I2 h RAh Right ascension of tangent point (J2000) 19- 20 I2 min RAm Right ascension of tangent point (J2000) 22- 26 F5.2 s RAs Right ascension of tangent point (J2000) 28 A1 --- DE- Declination sign of tangent point (J2000) 29- 30 I2 deg DEd Declination of tangent point (J2000) 32- 33 I2 arcmin DEm Declination of tangent point (J2000) 35- 38 F4.1 arcsec DEs Declination of tangent point (J2000) 40- 42 F3.1 arcsec bmin Minor axis of synthesized beam 44- 47 F4.1 arcsec bmaj Major axis of synthesized beam 49- 51 I3 deg PA [] Position angle of synthesized beam (from North through East) 53- 57 F5.2 mJy Smin Minimum (negative) flux recorded on the image (2) 59- 62 F4.1 uJy/beam rmsFit Noise level 64- 67 F4.1 uJy/beam Standard deviation of the average flux in several source-free sub-regions of the mosaic 69- 71 F3.1 uJy/beam e_ rms uncertainty on 73- 86 A14 --- FileName Name of the fits image in subdirectory fits -------------------------------------------------------------------------------- Note (1): fldXtoY, X and Y refer to the first and last field columns composing the mosaic. Note (2): typically |S_min| is of the order of 0.5mJy, corresponding to the value at which we have stopped the cleaning. -------------------------------------------------------------------------------- History: * 07-Jul-2000 : Copied from http://www.ira.bo.cnr.it/atesp * 06-Sep-2018 : Table3 and fits images from by Isabella Prandoni, via Heinz Andernach (heinz(at)astro.ugto.mx) References: Prandoni et al., Paper I, 2000A&AS..146...31P ================================================================================ (End) James Marcout, Patricia Bauer [CDS] 05-Dec-2000