J/MNRAS/421/3060 Subaru/XMM Deep Field radio imaging. III. (Simpson+, 2012)
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 2012MNRAS.421.3060S
ADC_Keywords: Surveys ; Radio sources ; Active gal. nuclei ; Redshifts
Keywords: surveys - galaxies: active - galaxies: distances and redshifts -
galaxies: evolution - radio continuum: galaxies
Abstract:
We present spectroscopic and 11-band photometric redshifts for
galaxies in the 100-uJy Subaru/XMM-Newton Deep Field radio source
sample. We find good agreement between our redshift distribution and
that predicted by the Square Kilometre Array (SKA) Simulated Skies
project. We find no correlation between K-band magnitude and radio
flux, but show that sources with 1.4-GHz flux densities below ∼1mJy
are fainter in the near-infrared than brighter radio sources at the
same redshift, and we discuss the implications of this result for
spectroscopically incomplete samples where the K-z relation has been
used to estimate redshifts. We use the infrared-radio correlation to
separate our 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.
Description:
Many of the spectra presented here were obtained as part of the
European Southern Observatory (ESO) programme P074.A-0333, undertaken
using the Visible Multi-Object Spectrograph (VIMOS) instrument on
UT3/Melipal, VIMOS.
Several observational campaigns have obtained spectra of objects
within the Subaru/XMM-Newton Deep Field (SXDF), and Paper II
(Vardoulaki et al., 2008MNRAS.387..505V 2008MNRAS.387..505V) 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.
The optical data in the UDS come from the SXDF, which comprises five
separate Suprime-Cam pointings.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 115 505 Photometric and (where available) spectroscopic
redshifts of all 505 SXDF radio sources
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See also:
J/MNRAS/372/741 : SXDF 100µJy catalogue (Simpson+, 2006)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 3 A3 --- --- [VLA]
5- 7 I3 --- Seq [1/505] Name, <[SMR2006] NNN> in Simbad
9- 10 I2 h RAh UKIRT right ascension (J2000.0)
12- 13 I2 min RAm UKIRT right ascension (J2000.0)
15- 19 F5.2 s RAs UKIRT right ascension (J2000.0)
21 A1 --- DE- UKIRT declination sign (J2000.0)
22- 23 I2 deg DEd UKIRT declination (J2000.0)
25- 26 I2 arcmin DEm UKIRT declination (J2000.0)
28- 31 F4.1 arcsec DEs UKIRT declination (J2000.0)
33 A1 --- l_Kmag Limit flag on Kmag
34- 38 F5.2 mag Kmag ? UKIRT K magnitude made in 4"-diameter aperture
40- 43 F4.2 mag e_Kmag ? rms uncertainty on Kmag
45- 48 F4.2 --- zph ? Probability-weighted mean photometric redshift
50- 53 F4.2 --- b_zph ? Photometric redshift 68% confidence interval
54 A1 --- --- [-]
55- 58 F4.2 --- B_zph ? Photometric redshift 68% confidence interval
60- 65 F6.4 --- zsp ? spectroscopic redshift
66 A1 --- n_zsp [?] ? indicates a spectrum taken with VIMOS but
no plausible redshift could be determined
68- 73 A6 --- Type Source classification (1)
75- 76 I2 --- Ref [1/10]? Reference for the spectroscopy (2)
78-115 A38 --- Com Comments
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Note (1): Spectral classification, described in Section 2.3:
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] > 15Å)
Weak = weak emitter (equivalent width of [OII] < 15Å)
Star = stellar spectrum
Note (2): References for the spectroscopy are as follows:
1 = this work
2 = Paper II, Vardoulaki et al. (2008MNRAS.387..505V 2008MNRAS.387..505V)
3 = Geach et al. (2007, Cat. J/MNRAS/381/1369)
4 = van Breukelen et al. (2009MNRAS.395...11V 2009MNRAS.395...11V)
5 = Smail et al. (2008MNRAS.389..407S 2008MNRAS.389..407S)
6 = Akiyama et al. (in prep)
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)
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History:
From electronic version of the journal
References:
Simpson et al., Paper I 2006MNRAS.372..741S 2006MNRAS.372..741S, Cat. J/MNRAS/372/741
Vardoulaki et al., Paper II 2008MNRAS.387..505V 2008MNRAS.387..505V
(End) Patricia Vannier [CDS] 08-Mar-2013