VLA Subaru/XMM-Newton Deep Field 1.4-GHz Sources Optical/Near-IR Counterparts

Description

In Simpson et al. (2006, MNRAS, 372, 741, hereafter Paper I, available at the HEASARC as the <a href="/W3Browse/radio-catalog/vlasxdf1p4.html">VLASXDF1P4</a> table, the authors presented a catalog of 505 sources with 1.4-GHz peak radio flux densities greater than 100 uJy over a 0.81 deg<sup>2</sup> region of the Subaru/XMM-Newton Deep Field (SXDF) and some of the properties of their optical counterparts. In this study (Simpson et al. 2012, MNRAS, 421, 3060, Paper III in the series) the authors present spectroscopic and 11-band photometric redshifts for galaxies in the 100-uJy Subaru/XMM-Newton Deep Field radio source sample. The authors find good agreement between their redshift distribution and that predicted by the Square Kilometre Array (SKA) Simulated Skies project. They find no correlation between K-band magnitude and radio flux, but show that sources with 1.4-GHz flux densities below ~ 1 mJy are fainter in the near-infrared than brighter radio sources at the same redshift, and they discuss in their paper the implications of this result for spectroscopically incomplete samples where the K-z relation has been used to estimate redshifts. The authors use the infrared-radio correlation to separate their sample into radio-loud and radio-quiet objects and show that only radio-loud hosts have spectral energy distributions consistent with predominantly old stellar populations, although the fraction of objects displaying such properties is a decreasing function of radio luminosity. Many of the spectra presented in this study were obtained as part of the European Southern Observatory (ESO) program P074.A-0333, undertaken using the Visible Multi-Object Spectrograph (VIMOS) instrument on UT3/Melipal. Several observational campaigns have obtained spectra of objects within the SXDF, and Paper II in this series (Vardoulaki et al. 2008, MNRAS, 387, 505) presented spectra for 28 of the brightest 37 radio sources, obtained from a variety of sources. The near-infrared data used here come from the third data release (DR3) of the UKIRT (United Kingdom Infrared telescope) Infrared Deep Sky Survey, while the optical data in the UDS come from the SXDF, which comprises five separate Suprime-Cam pointings. This table was created by the HEASARC in August 2013 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/MNRAS/421/3060">CDS Catalog J/MNRAS/421/3060</a> file table1.dat. This is a service provided by NASA HEASARC .

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Name Format Description Link
5 https://heasarc.gsfc.nasa.gov%2Fxamin%2Fvo%2Fcone%3Fshowoffsets%26table%3Dvlasxdfoid%26
5 https://heasarc.gsfc.nasa.gov%2FW3Browse%2Fall%2Fvlasxdfoid.html
21 vlasxdfoid.html https://heasarc.gsfc.nasa.gov/W3Browse/all/vlasxdfoid.html
5 https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=vlasxdfoid&
21 goods_colDescriptions.html https://irsa.ipac.caltech.edu/data/SPITZER/GOODS/docs/goods_colDescriptions.html
5 https://irsa.ipac.caltech.edu/SCS?table=goodsn_mips24&
21 vlasxdfoid.html https://heasarc.gsfc.nasa.gov/W3Browse/all/vlasxdfoid.html
5 https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=vlasxdfoid&

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