Details

Autor(en) / Beteiligte

• Ibar, Edo
• Cirasuolo, Michele
• Ivison, Rob
• Best, Philip
• Smail, Ian
• Biggs, Andy
• Simpson, Chris
• Dunlop, Jim
• Almaini, Omar
• McLure, Ross
• Foucaud, Sebastien
• Rawlings, Steve

Titel

Exploring the infrared/radio correlation at high redshift

Ist Teil von

• Monthly notices of the Royal Astronomical Society, 2008-05, Vol.386 (2), p.953-962

Ort / Verlag

Oxford, UK: Blackwell Publishing Ltd

Erscheinungsjahr

2008

Quelle

Wiley Online Library - AutoHoldings Journals

Beschreibungen/Notizen

• We have analysed the 24-μm properties of a radio-selected sample in the Subaru–XMM–Newton Deep Field in order to explore the behaviour of the far-infrared/radio (FIR/radio) relation at high redshifts. Statistically, the correlation is described by q24, the ratio between the observed flux densities at 24 μm and 1.4 GHz, respectively. Using 24-μm data results in considerably more scatter in the correlation than previous work using data at 60–70 μm. Nevertheless, we do observe a steady correlation as a function of redshift, up to z≈ 3.5, suggesting its validity back to primeval times. We find q24= 0.30 ± 0.56 for the observed and q24= 0.71 ± 0.47 for the k-corrected radio sample, based on sources with 300 μJy < S1.4 GHz < 3.2 mJy and 24-μm detections. A suitable k-correction given by a M82-like mid-infrared (mid-IR) template suggests no extreme silicate absorption in the bulk of our radio sample. Using thresholds in q24 to identify radio-excess sources, we have been able to characterize the transition from radio-loud active galactic nuclei (AGN) to star-forming galaxies and radio-quiet AGN at faint (≲1 mJy) radio-flux densities. Our results are in broad agreement with previous studies which show a dominant radio-loud AGN population at >1 mJy. The rest-frame U−B colours of the expected radio-excess population have a redder distribution than those that follow the correlation. This is therefore a promising way to select obscured type 2 AGN, with a radio-loud nature, missed by deep X-ray observations. Spectroscopic follow-up of these sources is required to fully test this method.