2008
DOI: 10.1051/0004-6361:200810567
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The VVDS-VLA deep field

Abstract: Aims. The availability of wide angle and deep surveys, both in the optical and the radio band, allows us to explore the evolution of radio sources with optical counterparts up to redshift z ∼ 1.1 in an unbiased way using large numbers of radio sources and well defined control samples of radio-quiet objects. Methods. We use the 1.4 GHz VIMOS-VLA Deep Survey, the optical VIMOS-VLT Deep Survey and the CFHT Legacy Survey to compare the properties of radio-loud galaxies with respect to the whole population of optic… Show more

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Cited by 12 publications
(19 citation statements)
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“…This is confirmed by the continuum of radio-emitting galaxies being redder than the control sample. This is related to the differences in colors already found by Bardelli et al (2009) for VVDS radio galaxies and present also in our VLA-zCOSMOS sample.…”
Section: Spectral Differences Between Radio-loud and Control Samplessupporting
confidence: 84%
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“…This is confirmed by the continuum of radio-emitting galaxies being redder than the control sample. This is related to the differences in colors already found by Bardelli et al (2009) for VVDS radio galaxies and present also in our VLA-zCOSMOS sample.…”
Section: Spectral Differences Between Radio-loud and Control Samplessupporting
confidence: 84%
“…11 indicates that the the two stellar masses distributions are the same for masses higher than 2 × 10 10 M and differ for lower masses, consistent with a similar plot in Bardelli et al (2009).…”
Section: Stellar Mass Distributionssupporting
confidence: 77%
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“…This scenario is also supported by most recent observations of the VIMOS-VLT Deep Survey (VVDS, Le Fèvre et al 2005a), one of the largest spectroscopic surveys of distant galaxies. In particular, the VVDS-Deep sample provides one with a description of the high-redshift Universe from z 0.2 to z 2, where the evolution of the galaxy luminosity function (Ilbert et al 2005;Zucca et al 2006), galaxy stellar mass function (Pozzetti et al 2007), star formation rate (Tresse et al 2007; Bardelli et al 2009), colour bimodality (Franzetti et al 2007), and galaxy clustering (Le Fèvre et al 2005b) cannot be only explained by a simple scenario of hierarchical growth of baryons.…”
Section: Introductionmentioning
confidence: 99%