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Sub-millijansky 1.4 GHz source counts and multicolor studies of weak radio galaxy populations
Windhorst, R. A.; Miley, G. K.; Owen, F. N.; Kron, R. G.; Koo, D. C.
AA(Mount Wilson and Las Campanas Observatoires, Pasadena, CA; Leiden, Rijksuniversiteit, Sterrewacht, Leiden, Netherlands; Kitt Peak National Observatory, Tucson, AZ), AB(Leiden, Rijksuniversiteit, Sterrewacht, Leiden, Netherlands), AC(National Radio Astronomy Observatory, Socorro, NM), AD(Yerkes Observatory, Williams Bay, WI; Kitt Peak National Observatory, Tucson, AZ), AE(Carnegie Institution of Washington, Washington, DC; Kitt Peak National Observatory, Tucson, AZ)
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 289, Feb. 15, 1985, p. 494-513. Sponsorship: Nederlandse Organisatie voor Zuiver-Wetenschappelijk Onderzoek. (ApJ Homepage)
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NASA/STI Keywords:
Astronomical Catalogs, Astronomical Photometry, Extragalactic Radio Sources, Radiant Flux Density, Radio Galaxies, Centimeter Waves, Cosmology, Functions (Mathematics), Seyfert Galaxies, Spiral Galaxies, Visible Spectrum
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A deep survey has been carried out with the VLA at 21 cm to a noise level of 45 muJy. The region chosen was the Leiden-Berkeley Deep Survey (LBDS) area Lynx.2, known to be devoid of radio sources stronger than 10 mJy. A catalog of 124 sources is presented, of which 93 form a sample complete to the 5 sigma level. The normalized differential source counts show a flattening below 5 mJy. Optical data are used to probe the nature of the sub-millijansky radio source population. Deep identifications and calibrated photometry are made on prime-focus plates obtained in four bands with the Kitt Peak 4 m Mayall telescope. In the complete sample 41 radio sources are reliably identified. It is shown that for radio sources with 1 < S1.4 < 10 mJy a blue radio galaxy population becomes increasingly important; these often have a peculiar optical morphology indicative of interacting or merging galaxies. Below 1 mJy the VLA sources consist of some red galaxies, but the majority are faint blue galaxies mostly fainter than V ≈ 20.

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