J/A+A/403/857 VLA-VIRMOS Deep Field (Bondi+, 2003)
The VLA-VIRMOS Deep Field.
I. Radio observations probing the µJy source population.
Bondi M., Ciliegi P., Zamorani G., Gregorini L., Vettolani G., Parma P.,
de Ruiter H., Le Fevre O., Arnaboldi M., Guzzo L., Maccagni D.,
Scaramella R., Adami C., Bardelli S., Bolzonella M., Bottini D., Cappi A.,
Foucaud S., Franzetti P., Garilli B., Gwyn S., Ilbert O., Iovino A.,
Le Brun V., Marano B., Marinoni C., McCracken H.J., Meneux B., Pollo A.,
Pozzetti L., Radovich M., Ripepi V., Rizzo D., Scodeggio M., Tresse L.,
Zanichelli A., Zucca E.
<Astron. Astrophys. 403, 857 (2003)>
=2003A&A...403..857B 2003A&A...403..857B
ADC_Keywords: Surveys ; Radio sources
Keywords: surveys - radio continuum: galaxies - methods: data analysis
Abstract:
We have conducted a deep survey (rms noise ~=17µJy) with the Very
Large Array (VLA) at 1.4GHz, with a resolution of 6arcsec, of a
1°2 region included in the VIRMOS VLT Deep Survey. In the same
field we already have multiband photometry down to IAB=25, and
spectroscopic observations will be obtained during the VIRMOS VLT
survey. The homogeneous sensitivity over the whole field has allowed
to derive a complete sample of 1054 radio sources (5σ limit). We
give a detailed description of the data reduction and of the analysis
of the radio observations, with particular care to the effects of
clean bias and bandwidth smearing, and of the methods used to obtain
the catalogue of radio sources. To estimate the effect of the
resolution bias on our observations we have modelled the effective
angular-size distribution of the sources in our sample and we have
used this distribution to simulate a sample of radio sources. Finally
we present the radio count distribution down to 0.08mJy derived from
the catalogue. Our counts are in good agreement with the best fit
derived from earlier surveys, and are about 50% higher than the counts
in the HDF. The radio count distribution clearly shows, with extremely
good statistics, the change in the slope for the sub-mJy radio
sources.
Description:
The observations were obtained at the Very Large Array (VLA) in
B-configuration for a total time of 56 hours over 9 days from
November 1999 to January 2000.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
catalog.dat 106 1103 Radio catalogue
--------------------------------------------------------------------------------
Byte-by-byte Description of file: catalog.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 12 A12 --- --- [VIRMOS1.4GHz]
14- 27 A14 --- VIRMOS1.4GHz VIRMOS1.4GHz designation (JHHMMSS-DDMMSS)
28 A1 --- m_VIRMOS1.4GHz [ABCDT] Multiplicity index on
VIRMOS1.4GHz (1)
30 I1 h RAh Right ascension (J2000)
32- 33 I2 min RAm Right ascension (J2000)
35- 39 F5.2 s RAs Right ascension (J2000)
41 A1 --- DE- Declination sign (J2000)
42 I1 deg DEd Declination (J2000)
44- 45 I2 arcmin DEm Declination (J2000)
47- 50 F4.1 arcsec DEs Declination (J2000)
52- 55 F4.2 arcsec e_RAs rms uncertainty on RA
57- 60 F4.2 arcsec e_DEs rms uncertainty on DE
62- 67 F6.3 mJy Speak Peak 1.4GHz flux density, in mJy/beam
69- 74 F6.3 mJy e_Speak rms uncertainty on Speak, in mJy/beam
76- 81 F6.3 mJy Stot Total 1.4GHz flux density
83- 88 F6.3 mJy e_Stot rms uncertainty on Stot
90- 93 F4.1 arcsec MajAxis ? Major axis (1)
95- 98 F4.1 arcsec MinAxis ? Minor axis (1)
100-104 F5.1 deg PA [-73/181]? Position angle (2)
-------------------------------------------------------------------------------
Note (1): For each of the 19 sources fitted with multiple components
we list in the catalogue an entry for each of the components,
identified with a trailing letter (A, B, C, ...) in the source name,
and an entry for the whole source, identified with a trailing T in the
source name. In these cases the total flux was calculated using the
task TVSTAT, which allows the integration of the map values over
irregular areas, and the sizes are the largest angular sizes.
Note (2): For the unresolved sources the total flux density is equal to
the peak brightness and the angular size is undetermined.
-------------------------------------------------------------------------------
History:
* 31-Jul-2003: Copied at http://virmo.bo.astro.it/radio/catalog.html
* 23-Feb-2012: units of the error in RA (e_RAs) was corrected from
"s" to "arcsec" (thanks to S.A. Drake)
(End) James Marcout, Patricia Bauer [CDS] 31-Jul-2003