Radio-loud AGN in the XMM-LSS field. I. Optical identification and sample selection

Details Radio-loud AGN in the XMM-LSS field. I. Optical identification and sample selection Radio-loud AGN in the XMM-LSS field. I. Optical identification and sample selection

Nov 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008a%26a...490..879t&link_type=abstract

Astronomy and Astrophysics, Volume 490, Issue 3, 2008, pp.879-891

Astronomy and Astrophysics

Astrophysics

5

Methods: Observational, Techniques: Photometric, Galaxies: Active, Galaxies: Fundamental Parameters, Cosmology: Observations, Radio Continuum: Galaxies

Scientific paper

The XMM-Large Scale Structure survey field (XMM-LSS) is an extragalactic window surveyed in the X-ray with the XMM-Newton satellite. It has also been observed in the optical with the Canada-France Hawaï Telescope (CFHTLS survey), and in the infrared with the Spitzer Space Telescope (SWIRE survey). These surveys have been carried out to study the structure and evolution of both baryonic and dark matter on cosmological scales. In two previous papers, we presented deep low frequency radio surveys of the XMM-LSS field, with limiting flux density levels of ~4 and ~1.5 mJy/beam at 325 and 610 MHz respectively (5σ). These radio surveys were motivated by the need to understand the various connections between the host galaxies of radio sources and their environments. In this paper, we identify optical counterparts to the low frequency radio sources, using the CFHTLS optical catalogue and images, that have an i-band limiting magnitude of i_AB˜ 25. We use a likelihood ratio method and estimate that ~75% of the radio sources have a detected optical counterpart. Using the CFHTLS and SWIRE data, we derive photometric redshifts for the galaxies that are identified with a radio source, as well as for those that are not; we demonstrate the reliability of these photometric redshifts by deriving the stellar mass function for galaxies at different redshifts, and showing that it is consistent with previous determinations. We classify the radio sources as type-1 AGN, radio galaxies, or star-forming galaxies, and show that the radio luminosity function of the radio galaxies agrees with previous measurements.
Appendices D and E are only available in electronic form at http///www.aanda.org

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