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

Overview

In Simpson et al. (2006, MNRAS, 372, 741, hereafter Paper I, available at the HEASARC as the VLASXDF1P4 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 deg² 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.

Catalog Bibcode

2012MNRAS.421.3060S

References

Radio imaging of the Subaru/XMM-Newton Deep Field.
III. Evolution of the radio luminosity function beyond z= 1.
    Simpson C., Rawlings S., Ivison R., Akiyama M., Almaini O., Bradshaw E.,
    Chapman S., Chuter R., Croom S., Dunlop J., Foucaud S., Hartley W.
   <Mon. Not. R. Astron. Soc., 421, 3060-3083 (2012)>
   =2012MNRAS.421.3060S
Radio imaging of the Subaru/XMM-Newton Deep Field.
I. The 100-{mu}Jy catalogue, optical identifications, and the nature of the
faint radio source population.
    Simpson C., Martinez-Sansigre A., Rawlings S., Ivison R., Akiyama M.,
    Sekiguchi K., Takata T., Ueda Y., Watson M.
   <Mon. Not. R. Astron. Soc., 372, 741-757 (2006)>
   =2006MNRAS.372..741S

Provenance

This table was created by the HEASARC in August 2013 based on CDS Catalog J/MNRAS/421/3060 file table1.dat.

Parameters

Source_Number
A unique identification number for each VLA 1.4-GHz source in the catalog, in order of decreasing 1.4-GHz flux density as first listed in Paper I of the series.

Name
The name for the radio source suggested by the Dictionary of Nomenclature of Celestial Objects, using the prefix '[SMR2006]' for Simpson, Martinez-Sansigre, Rawlings 2006 (Paper I) and the source number, e.g., '[SMR2006] 1'.

RA
The Right Ascension of the UKIRT DR3 counterpart to the radio source (or, in cases where there was no such counterpart detected, the radio source position or the location of the Paper I optical counterpart) in the selected equinox. This was given in J2000 equatorial coordinates and to a precision of 0.01 seconds of time in the original source table.

Dec
The Declination of the UKIRT DR3 counterpart to the radio source (or, in cases where there was no such counterpart detected, the radio source position or the location of the Paper I optical counterpart) in the selected equinox. This was given in J2000 equatorial coordinates and to a precision of 0.1 arcseconds in the original source table.

LII
The Galactic Longitude of the UKIRT DR3 counterpart to the radio source (or, in cases where there was no such counterpart detected, the radio source position or the location of the Paper I optical counterpart).

BII
The Galactic Latitude of the UKIRT DR3 counterpart to the radio source (or, in cases where there was no such counterpart detected, the radio source position or the location of the Paper I optical counterpart).

Kmag_Limit
This limit parameter is set to '>' if the corresponding kmag value is an upper limit rather than a detection.

Kmag
The K magnitude of the counterpart to the radio source in the UKIRT Deep Survey if within its footprint, else from 2MASS, using a 4-arcsec diameter aperture.

Kmag_Error
The uncertainty in the K magnitude of the counterpart to the radio source.

Phot_Redshift
The probability-weighted mean photometric redshift of the counterpart to the radio source.

Phot_Redshift_Min
The 68%-Confidence interval minimum value for the probability-weighted mean photometric redshift of the counterpart to the radio source.

Phot_Redshift_Max
The 68%-Confidence interval maximum value for the probability-weighted mean photometric redshift of the counterpart to the radio source.

Redshift
The spectroscopic redshift of the counterpart to the radio source. If this value is blank, as well as redshift_flag, no spectroscopic observation was obtained. If this value is blank, and the redshift_flag is set to '?', a spectrum was taken with VIMOS but no plausible redshift could be determined.

Redshift_Flag
If this parameter is set to '?', a spectrum was taken with VIMOS but no plausible redshift could be determined.

Broad_Type
The source classification, as described in Section 2.3 of Paper III: a "Cont" in this column indicates that the detection of continuum emission and that the spectrum is therefore presented in Fig. A1 of paper III. The codes for the source classes are:

    BLAGN = Broad-line Active Galaxy Nucleus
    NLAGN = Narrow-line Active Galaxy Nucleus
      Abs = Absorption-line galaxy (no emission line)
     Cont = Detection of continuum emission
            (the spectrum is therefore presented in Fig. A1)
       SB = Starburst galaxy
   Strong = Strong emitter (equivalent width of [OII] > 15 Angstroms)
     Weak = Weak emitter (equivalent width of [OII] < 15 Angstroms)
     Star = Stellar spectrum

Ref_Spectroscopy
The reference code for the spectroscopy, as follows:

     1 = this work
     2 = Paper II, Vardoulaki et al. (2008, MNRAS, 387, 505)
     3 = Geach et al. (2007, MNRAS, 381, 1369)
     4 = van Breukelen et al. (2009, MNRAS, 395, 11)
     5 = Smail et al. (2008, MNRAS, 389, 407)
     6 = Akiyama et al. (in preparation)
     7 = S. Chapman (private communication)
     8 = S. Croom (private communication)
     9 = UDSz/VIMOS (Chuter 2011, PhD thesis, University of Nottingham)
    10 = UDSz/FORS2 (Pearce et al., in preparation)

Comments
Comments concerning the identification of the counterpart to the radio source.

Class
The HEASARC Browse object classification, based on the broad_type parameter value.

Contact Person

Questions regarding the VLASXDFOID database table can be addressed to the HEASARC Help Desk.

Page Author: Browse Software Development Team
Last Modified: Monday, 16-Sep-2024 17:36:30 EDT