Optical identifications of $\sim 4000$ radio sources at the 1 mJy level

Details Optical identifications of $\sim 4000$ radio sources at the 1 mJy level Optical identifications of $\sim 4000$ radio sources at the 1 mJy level

2001-06-23

arxiv.org/abs/astro-ph/0106429v1

Mon.Not.Roy.Astron.Soc. 330 (2002) 241

Astronomy and Astrophysics

Astrophysics

11 pages, 13 figures, submitted to MNRAS

Scientific paper

10.1046/j.1365-8711.2002.04954.x

We present an analysis of the properties of optical counterparts of radio sources down to 1 mJy. Optical identifications have been obtained by matching together objects from the APM and FIRST surveys over the region $148.13^\circ\simlt {\rm RA(2000)}\simlt 218.13^\circ$, $-2.77^\circ\simlt {\rm Dec} \simlt 2.25^\circ$. Selecting radio sources down to 1 mJy, and adopting a uniform optical limit of $b_J = 21.5$ we find 3176 have a counterpart in the APM catalogue, corresponding to 13 per cent of the radio sample. For $b_J \le 20.5$ we can divide radio sources into resolved radio galaxies and stellar-like objects (principally QSO). We find the population of radio galaxies to be mainly made by early-type galaxies with very red colours ($b_J-R$ up to $\sim 4$) and a radio-to-optical ratio $10^2\simlt r\simlt 10^4$. The contribution of starbursting objects is negligible. In general QSO show $r\simgt 10^4$ and $0\simlt b_J -R \simlt 1$. On the basis of the $R$ magnitudes, we estimate the sample of radio galaxies to be complete up to $z\simeq 0.3$. We can therefore divide the whole sample of radio sources into a low-z and high-z population. The low-z one includes the objects identified as galaxies in the APM survey, the high-z one includes sources either identified as QSO or with no optical counterpart for $b_J \le 20.5$. We find that radio galaxies are strongly clustered and highly biased tracers of the underlying mass distribution. Models for the angular correlation function $w(\theta)$ show good agreement with the observations if we assume a bias factor $b\simeq 2$ at $z\simeq 0.3$.

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