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J/A+AS/58/39 1412 MHz catalogue of Westerbork survey. II (Windhorst+, 1984)
The following files can be converted to FITS (extension .fit .fgz or .fiZ)
table1.dat table4a.dat table4b.dat notes.dat
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Beginning of ReadMe :J/A+AS/58/39 1412 MHz catalogue of Westerbork survey. II (Windhorst+, 1984)
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A deep Westerbork survey of areas with multicolor Mayall 4 m plates.
II. Optical identifications.
Windhorst R.A., Kron R.G., Koo D.C.
<Astron. Astrophys. Suppl. Ser. 58, 39 (1984)>
=1984A&AS...58...39W
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ADC_Keywords: Radio sources ; Surveys ; Cross identifications
Keywords: radio sources: general - astrometry - galaxies: radio - cosmology
Abstract:
A deep multicolor optical identification program is presented for a
complete sample of 302 radio sources that were observed with the
Westerbork Synthesis Radio Telescope within 5.52deg^2^ down to
S_1.4GHz_> 0.6mJy (5sigma). Optical identifications are made from
multicolor prime focus plates taken with the Kitt Peak 4 meter
telescope in the passbands U,J,F and N with approximate respective
limiting magnitudes of 23.3, 23.7, 22.7 and 21.1. The astrometry
has systematic errors smaller than 0.2"-0.3", while the random errors
are of order 0.4". The agreement between the radio and optical
coordinate frames is on average better than 0.25". Identifications are
based on positional coincidence using the likelihood ratio method. For
171 out of the 302 radio sources likely identifications are proposed
with an a posteriori identification percentage of 53%, 14 expected
spurious objects (or 5% of all radio sources), while not more than 4
identifications have been missed. The sample reliability is 92% and
its completeness 98%. About 20% of the identifications are stellar
objects, the remaining have extended images or are too faint to be
classified. About 15% of the identifications appear in possible
clusters. The identification statistics are roughly constant from
field to field, except for the Hercules 2 field which has an
unusually high identification fraction (74%). The identification
fraction is presented as a function of 21 cm flux density and limiting
magnitude, and amounts to 15% for 1< S_1.4GHz_< 100mJy down to the
Palomar Sky Survey limit and 29% down to the effective 48" Schmidt
limit. For S_1.4_< 100mJy the identification fraction remains roughly
constant with flux density, contrary to the prediction of higher
fractions by some models for cosmological evolution. The magnitude
distributions for galaxies plus objects of unknown type generally
increase towards fainter magnitudes; the quasar magnitude
distributions are also increasing but not as steeply as for the radio
galaxies.