The VIRMOS deep imaging survey

McCracken, H. J.; Radovich, M.; Bertin, E.; Mellier, Y.; Dantel-Fort, M.; Fèvre, O. Le; Cuillandre, Jean-Charles; Gwyn, Stephen; Foucaud, Sylvie; Zamorani, G.

doi:10.1051/0004-6361:20031081

Cited by 158 publications

(214 citation statements)

References 51 publications

(49 reference statements)

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“…The VDIS and CFHTLS photometric catalogues reach limiting magnitudes (80% completeness for point-like sources) of 24.6, 26.2, 25.9, 25.4, 25.1, 24.6 respectively for I, u * , g , r , i , z bands (see McCracken et al 2003;Goranova et al 2009). When computing the magnitude counts in the VVDS data, we carefully excluded stars using colour-colour diagrams following McCracken et al (2003). We first compare the I-band galaxy counts in the VDIS field with published measurements from large and deep photometric surveys.…”

Section: Magnitude Countsmentioning

confidence: 97%

Comparison of the VIMOS-VLT Deep Survey with the Munich semi-analytical model

Torre

Meneux

Lucia

et al. 2010

A&A

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Aims. This paper presents a detailed comparison between high-redshift observations from the VIMOS-VLT Deep Survey (VVDS) and predictions from the Munich semi-analytical model of galaxy formation. In particular, we focus this analysis on the magnitude, redshift, and colour distributions of galaxies, as well as their clustering properties. Methods. We constructed 100 quasi-independent mock catalogues, using the output of the semi-analytical model presented in De Lucia & Blaizot (2007, MNRAS, 375, 2). We then applied the same observational selection function of the VVDS-Deep survey, so as to carry out a fair comparison between models and observations. Results. We find that the semi-analytical model reproduces well the magnitude counts in the optical bands. It tends, however, to overpredict the abundance of faint red galaxies, in particular in the i and z bands. Model galaxies exhibit a colour bimodality that is only in qualitative agreement with the data. In particular, we find that the model tends to overpredict the number of red galaxies at low redshift and of blue galaxies at all redshifts probed by VVDS-Deep observations, although a large fraction of the bluest observed galaxies is absent from the model. In addition, the model overpredicts by about 14 per cent the number of galaxies observed at 0.2 < z < 1 with I AB < 24. When comparing the galaxy clustering properties, we find that model galaxies are more strongly clustered than observed ones at all redshift from z = 0.2 to z = 2, with the difference being less significant above z 1. When splitting the samples into red and blue galaxies, we find that the observed clustering of blue galaxies is well reproduced by the model, while red model galaxies are much more clustered than observed ones, being principally responsible for the strong global clustering found in the model. Conclusions. Our results show that the discrepancies between Munich semi-analytical model predictions and VVDS-Deep observations, particularly in the galaxy colour distribution and clustering, can be explained to a large extend by an overabundance of satellite galaxies, mostly located in the red peak of the colour bimodality predicted by the model.

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Section: Magnitude Countsmentioning

confidence: 97%

Comparison of the VIMOS-VLT Deep Survey with the Munich semi-analytical model

Torre

Meneux

Lucia

et al. 2010

A&A

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“…It consists of a wide survey (Garilli et al 2008), spread over three fields, with an effective area of 4.5 deg 2 for 17.5 < IAB < 22.5 and a deep survey (Le Fevre et al 2005), spread over two fields, with an effective area of 0.62 deg 2 for 17.5 < IAB < 24.0. The I-band imaging has been designed to be complete to much fainter magnitudes than these limits, with limiting magnitudes of IAB = 24.8 and IAB = 25.3 at 5σ in the wide and the deep fields, respectively (McCracken et al 2003;Le Fèvre et al 2004). Targets have been nearly randomly selected for spectroscopy with the VIMOS multi-object spectrograph on the Very Large Telescope (VLT).…”

Section: The Vvdsmentioning

confidence: 99%

The cosmic growth of the active black hole population at 1 <z <2 in zCOSMOS, VVDS and SDSS

Schulze

Bongiorno

Gavignaud

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We present a census of the active black hole population at 1 < z < 2, by constructing the bivariate distribution function of black hole mass and Eddington ratio, employing a maximum likelihood fitting technique. The study of the active black hole mass function (BHMF) and the Eddington ratio distribution function (ERDF) allows us to clearly disentangle the active galactic nuclei (AGN) downsizing phenomenon, present in the AGN luminosity function, into its physical processes of black hole mass downsizing and accretion rate evolution. We are utilizing type-1 AGN samples from three optical surveys (VVDS, zCOSMOS and SDSS), that cover a wide range of 3 dex in luminosity over our redshift interval of interest. We investigate the cosmic evolution of the AGN population as a function of AGN luminosity, black hole mass and accretion rate. Compared to z = 0, we find a distinct change in the shape of the BHMF and the ERDF, consistent with downsizing in black hole mass. The active fraction or duty cycle of type-1 AGN at z ∼ 1.5 is almost flat as a function of black hole mass, while it shows a strong decrease with increasing mass at z = 0. We are witnessing a phase of intense black hole growth, which is largely driven by the onset of AGN activity in massive black holes towards z = 2. We finally compare our results to numerical simulations and semi-empirical models and while we find reasonable agreement over certain parameter ranges, we highlight the need to refine these models in order to match our observations.

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“…The magnitude limits are i = 22.5 and 24.0 and the effective areas covered are 5.8 and 0.6 deg 2 for the wide and the deep, respectively. The targets were chosen using the i magnitude from CFHT observations (McCracken et al 2003;Ilbert et al 2005;Cucciati et al 2012). The VVDS collaboration provides the slit-extracted 1D-spectra and the redshift catalogue based on visual inspection of the spectra.…”

Section: Datamentioning

confidence: 99%

The evolution of the [O ii], H β and [O iii] emission line luminosity functions over the last nine billions years

Comparat

Zhu

González-Pérez

et al. 2016

Mon. Not. R. Astron. Soc.

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Citation for published item:gomp r tD tF nd huD qF nd qonz lezE erezD F nd xor ergD F nd xewm nD tF nd resseD vF nd i h rdD tF nd epesD qF nd unei D tFE F nd i hoorD eF nd r d D pF nd w r stonD gF nd e heD gF nd helu D F nd tulloD iF @PHITA 9 he evolution of the y ss D r nd y sss emission line luminosity fun tions over the l st nine illions ye rsF9D wonthly noti es of the oy l estronomi l o ietyFD RTI @IAF ppF IHUTEIHVUF Further information on publisher's website: Additional information: Use policyThe full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-pro t purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. ABSTRACTEmission line galaxies are one of the main tracers of the large-scale structure to be targeted by the next-generation dark energy surveys. To provide a better understanding of the properties and statistics of these galaxies, we have collected spectroscopic data from the VVDS and DEEP2 deep surveys and estimated the galaxy luminosity functions (LFs) of three distinct emission lines, [O II] (λλ3726, 3729) (0.5 < z < 1.3), Hβ (λ4861) (0.3 < z < 0.8) and [O III] (λ5007) (0.3 < z < 0.8). Our measurements are based on 35 639 emission line galaxies and cover a volume of ∼10 7 Mpc 3 . We present the first measurement of the Hβ LF at these redshifts. We have also compiled LFs from the literature that were based on independent data or covered different redshift ranges, and we fit the entire set over the whole redshift range with analytic Schechter and Saunders models, assuming a natural redshift dependence of the parameters. We find that the characteristic luminosity (L * ) and density (φ * ) of all LFs increase with redshift. Using the Schechter model over the redshift ranges considered, we find that, for [O II] emitters, the characteristic luminosity L * (z = 0.5) = 3.2 × 10 41 erg s −1 increases by a factor of 2.7 ± 0.2 from z = 0.5 to 1.3; for Hβ emitters L * (z = 0.3) = 1.3 × 10 41 erg s −1 increases by a factor of 2.0 ± 0.2 from z = 0.3 to 0.8; and for [O III] emitters L * (z = 0.3) = 7.3 × 10 41 erg s −1 increases by a factor of 3.5 ± 0.4 from z = 0.3 to 0.8.

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The VIRMOS deep imaging survey

Cited by 158 publications

References 51 publications

Comparison of the VIMOS-VLT Deep Survey with the Munich semi-analytical model

Comparison of the VIMOS-VLT Deep Survey with the Munich semi-analytical model

The cosmic growth of the active black hole population at 1 <z <2 in zCOSMOS, VVDS and SDSS

The evolution of the [O ii], H β and [O iii] emission line luminosity functions over the last nine billions years

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