The VIMOS-VLT deep survey

Franzetti, P.; Scodeggio, M.; Garilli, B.; Vergani, D.; Maccagni, D.; Guzzo, L.; Tresse, L.; Ilbert, O.; Lamareille, F.; Contini, T.; Fèvre, O. Le; Zamorani, G.; Brinchmann, Jarle; Charlot, S.; Bottini, D.; Brun, V. Le; Picat, J. P.; Scaramella, R.; Vettolani, G.; Zanichelli, A.; Adami, C.; Arnouts, S.; Bardelli, S.; Bolzonella, M.; Cappi, A.; Ciliegi, P.; Foucaud, Sylvie; Gavignaud, I.; Iovino, A.; McCracken, H. J.; Marano, B.; Marinoni, C.; Mazure, A.; Meneux, B.; Merighi, R.; Paltani, S.; Pelló, R.; Pollo, A.; Pozzetti, L.; Radovich, M.; Zucca, E.; Cucciati, O.; Walcher, C. J.

doi:10.1051/0004-6361:20065942

Cited by 86 publications

(105 citation statements)

References 55 publications

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“…In that case, when comparing to VVDS-Deep colour distributions, one finds that while in the highest-redshift intervals the predicted and observed colour distributions are quite similar, the lack of blue galaxies in the model is remarkable at z < 1.1. Franzetti et al (2007) show that the fixed apparent magnitude selection of the VVDS-Deep sample can in principle introduce a mild bias in the intrinsic colours, partially displacing rest-frame U − V colours towards the blue at z > 1.2. However, they find that this effect is marginal and cannot be invoked to explain the discrepancies found in the SAM at all probed redshift.…”

Section: Galaxy Luminosity and Intrinsic Colour Distributionsmentioning

confidence: 91%

“…Le Fèvre et al 2005b;Ilbert et al 2005;Zucca et al 2006;Franzetti et al 2007). As a consequence, the clustering of these galaxies should reflect the average clustering of the different galaxy sub-populations at the different redshifts.…”

Section: Colour-dependent Galaxy Clusteringmentioning

confidence: 99%

“…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%

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

Torre

Meneux

Lucia

et al. 2010

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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: Galaxy Luminosity and Intrinsic Colour Distributionsmentioning

confidence: 91%

Section: Colour-dependent Galaxy Clusteringmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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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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“…Surely, as discussed above, the bimodality in many galaxy properties highlights that red galaxies are mostly quiescent and passively evolving; however, a detailed and quantitative estimate of the contamination due to blue/star-forming outliers should be made before doing a one-to-one correspondence. Franzetti et al (2007) pointed out such possible contamination when studying a color-selected sample of ETGs, concluding that selecting galaxies only on the basis of their colors can be misleading in estimating the evolution of old and passively evolving galaxies.…”

Section: Introductionmentioning

confidence: 99%

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Moresco¹,

Pozzetti

Cimatti³

et al. 2013

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Aims. We present the analysis of photometric, spectroscopic, and morphological properties for differently selected samples of passive galaxies up to z = 1 extracted from the zCOSMOS-20k spectroscopic survey. This analysis intends to explore the dependence of galaxy properties on the selection criterion adopted, study the degree of contamination due to star-forming outliers, and provide a comparison between different commonly used selection criteria. This work is a first step to fully investigating the selection effects of passive galaxies for future massive surveys such as Euclid. Methods. We extracted from the zCOSMOS-20k catalog six different samples of passive galaxies, based on morphology (3336 "morphological" early-type galaxies), optical colors (4889 "red-sequence" galaxies and 4882 "red UVJ" galaxies), specific star-formation rate (2937 "quiescent" galaxies), a best fit to the observed spectral energy distribution (2603 "red SED" galaxies), and a criterion that combines morphological, spectroscopic, and photometric information (1530 "red & passive early-type galaxies"). For all the samples, we studied optical and infrared colors, morphological properties, specific star-formation rates (SFRs), and the equivalent widths of the residual emission lines; this analysis was performed as a function of redshift and stellar mass to inspect further possible dependencies. Results. We find that each passive galaxy sample displays a certain level of contamination due to blue/star-forming/nonpassive outliers. The morphological sample is the one that presents the higher percentage of contamination, with ∼12−65% (depending on the mass range) of galaxies not located in the red sequence, ∼25−80% of galaxies with a specific SFR up to ∼25 times higher than the adopted definition of passive, and significant emission lines found in the median stacked spectra, at least for log (M/M ) < 10.25. The red & passive ETGs sample is the purest, with a percentage of contamination in color <10% for stellar masses log (M/M ) > 10.25, very limited tails in sSFR, a median value ∼20% higher than the chosen passive cut, and equivalent widths of emission lines mostly compatible with no star-formation activity. However, it is also the less economic criterion in terms of information used. Among the other criteria, we found that the best performing are the red SED and the quiescent ones, providing a percentage of contamination only slightly higher than the red & passive ETGs criterion (on average of a factor of ∼2) but with absolute values of the properties of contaminants still compatible with a red, passively evolving population. We also find a strong dependence of the contamination on the stellar mass and conclude that, almost irrespective of the adopted selection criteria, a cut at log (M/M ) > 10.75 provides a significantly purer sample in terms of star-forming contaminants. By studying the restframe color-mass and color−color diagrams, we provided two revised definitions of passive galaxies based on these criteria that better reprodu...

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“…Numerous studies have demonstrated that a bimodal population of galaxies exists up to high redshift (e.g., Franzetti et al 2007;Mignoli et al 2009). The first population consists of galaxies that are actively star-forming, gas-rich, rotationally-supported, and morphologically disk-dominated.…”

Section: Introductionmentioning

confidence: 99%

K+a galaxies in the zCOSMOS survey

Vergani

Zamorani

Lilly³

et al. 2009

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Aims. The identities of the main processes triggering and quenching star-formation in galaxies remain unclear. A key stage in evolution, however, appears to be represented by post-starburst galaxies. To investigate the prevalence of these galaxies and their impact on galaxy evolution in general, we initiated a multiwavelength study of galaxies with k + a spectral features in the well-studied COSMOS field. Methods. We examine a mass-selected sample of k + a galaxies in the COSMOS field at z = 0.48−1.2 using the spectroscopic zCOSMOS sample. To classify galaxies in their k + a phase, we use a spectroscopic criterion, based on the amplitude of the Hδ absorption line and the absence of the [OII] emission line. We develop our analysis for a well-defined sample by imposing stringent confidence levels on the spectroscopic redshifts and spectral measurements. We compare our results for two mass-selected samples of star-forming and quiescent galaxies selected using a purely spectral classification scheme from the 10 000 zCOSMOS catalogue (i.e. , based on measurements of 4000 Å break and EW[OII]). Results. In our mass-limited sample, k+a galaxies occupy the brightest tail of the luminosity distribution. They are as massive as quiescent galaxies and populate the green valley in the colour versus luminosity (or stellar mass) distribution. A small percentage (<8%) of these galaxies have radio and/or X-ray counterparts (implying an upper limit to the SFR of ∼8 M yr −1 ). Over the entire redshift range explored, the class of post-starburst galaxies is morphologically a heterogeneous population with a similar incidence of bulge-dominated and disky galaxies. This distribution does not vary with the strength of the Hδ absorption line but instead with stellar mass in a way reminiscent of the well-known mass-morphology relation. The results about the incidence of asymmetries and the concentration of the light distribution derived from HST/ACS images imply that this galaxy population possibly represents an intermediate stage of galaxy evolution. Although k + a galaxies are also found in underdense regions, they appear to reside typically in a similarly rich environment as quiescent galaxies on a physical scale of ∼2-8 Mpc, and in groups they show a morphological early-to-late type ratio similar to the quiescent galaxy class. With the current data set, we do not find evidence of statistical significant evolution in either the number/mass density of k + a galaxies at intermediate redshift with respect to the local values, or the spectral properties, although more solid results on this and other aspects will be obtained following the completion of the survey. Conclusions. Several mechanisms related and unrelated to the environment are at work in quenching star-formation activity in galaxies on short timescales (<1 Gyr). Those galaxies, which are affected by a sudden quenching of their star-formation activity, may increase the stellar mass of the red-sequence by up to a non-negligible level of ∼10%.

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The VIMOS-VLT deep survey

Cited by 86 publications

References 55 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

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K+a galaxies in the zCOSMOS survey

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