The VVDS-VLA deep field

Bardelli, S.; Zucca, E.; Bolzonella, M.; Ciliegi, P.; Gregorini, L.; Zamorani, G.; Bondì, M.; Zanichelli, A.; Tresse, L.; Vergani, D.; Gavignaud, I.; Bongiorno, A.; Bottini, D.; Garilli, B.; Brun, V. Le; Fèvre, O. Le; Maccagni, D.; Scaramella, R.; Scodeggio, M.; Vettolani, G.; Adami, C.; Arnouts, S.; Cappi, A.; Charlot, S.; Contini, T.; Foucaud, Sylvie; Franzetti, P.; Guzzo, L.; Ilbert, O.; Iovino, A.; Lamareille, F.; McCracken, H. J.; Marinoni, C.; Mazure, A.; Meneux, B.; Merighi, R.; Paltani, S.; Pelló, R.; Pollo, A.; Pozzetti, L.; Radovich, M.; Abbas, U.; Brinchmann, Jarle; Cucciati, O.; Torre, S. de la; Ravel, L. de; Memeo, P.; Pérez-Montero, E.; Mellier, Y.; Merluzzi, P.; Temporin, S.; Ruiter, H. R. de; Parma, P.

doi:10.1051/0004-6361:200810567

Cited by 12 publications

(19 citation statements)

References 52 publications

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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%

“…The fraction of AGN that have log(SSFR) < −10.5 is ∼60%. A similar percentage of star forming excess was found in the AGN sample defined by Bardelli et al (2009), where a spectrophotometric division was adopted. The apparently large difference between our own and the Smolčic et al (2008) method is largely due to the fact that optical AGN and composite galaxies are included in the AGN sample in Smolčic et al (2008) and not in our scheme.…”

Section: Comparison With Other Classificationsmentioning

confidence: 61%

“…Bardelli et al 2009;Smolčic et al 2009a,b), the aim is to count the total number of AGN (or star-forming galaxies) and for these studies it is correct to consider all objects exhibiting AGN (SF) activity, regardless of its relative contribution to the radio flux. For density studies, the situation is slightly different.…”

Section: Agn Versus Star Forming Galaxies In Environmental Studiesmentioning

confidence: 99%

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Properties and environment of radio-emitting galaxies in the VLA-zCOSMOS survey

Bardelli¹,

Schinnerer

Smolčić

et al. 2010

A&A

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Aims. We investigate the properties and the environment of radio sources with optical counterparts from the combined VLA-COSMOS and zCOSMOS samples. The advantage of this sample is the availability of optical spectroscopic informations, high quality redshifts, and accurate density determination. Methods. By comparing the star formation rates estimated from the optical spectral energy distribution with those based on the radio luminosity, we divide the radio sources in to three families passive AGN, non-passive AGN, and star-forming galaxies. These families occupy specific regions of the 8.0−4.5 μm infrared color-specific star-formation plane, from which we extract the corresponding control samples. Results. Only the passive AGN have a significantly different environmental distribution from their control sample. The fraction of radio-loud passive AGN increases from ∼2% in underdense regions to ∼15% for overdensities (1 + δ) greater than 10. This trend is also present as a function of richness of the groups hosting the radio sources. Passive AGN in overdensities tend to have higher radio luminosities than those in lower density environments. Since the black hole mass distribution is similar in both environments, we speculate that, for low radio luminosities, the radio emission is controlled (by fuel availability or confinement of the radio jet by local gas pressure) by the interstellar medium of the host galaxy, while in other cases it is determined by the structure (group or cluster) in which the galaxy resides.

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Section: Spectral Differences Between Radio-loud and Control Samplessupporting

confidence: 84%

Section: Stellar Mass Distributionssupporting

confidence: 77%

Section: Comparison With Other Classificationsmentioning

confidence: 61%

Section: Agn Versus Star Forming Galaxies In Environmental Studiesmentioning

confidence: 99%

See 2 more Smart Citations

Properties and environment of radio-emitting galaxies in the VLA-zCOSMOS survey

Bardelli¹,

Schinnerer

Smolčić

et al. 2010

A&A

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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%

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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The Role of the Environment on Galaxy Evolution

Boselli

2011

A Panchromatic View of Galaxies

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Esame finale anno 2016A Milena "Che fai tu, Luna, in ciel? Dimmi, che fai, silenziosa Luna?" -Giacomo Leopardi, Canto notturno di un pastore errante dell'Asia A B S T R A C TAlthough the general picture of how galaxies have formed and evolved through cosmic time is already in place, still many details are missing. An example is represented by a quantitative characterization of the role that environment plays during the evolution of galaxies in determining their observed properties in the local Universe. Local galaxy environment has been thoroughly explored through observations at low redshift and it has recently started to being investigated also in the distant Universe. Moreover, general attention has been increasingly focused on the relation between galaxy evolution and galaxy positions with respect to the large-scale structures of the cosmic web.This work explores how environment (defined both in terms of local overdensities on the Mpc scale around galaxies, as well as in terms of the distribution of galaxy distances from ∼ 10 2 Mpc long cosmic filaments) is observationally related to galaxy properties such as their stellar mass, their star-formation activity, or the presence of Active Galactic Nucleus phenomena. The analysis reported here is performed in a large redshift range, going from the local Universe (z 0.2) to intermediate (z ∼ 0.7) and high-redshifts (z 3). To perform this study, both spectroscopic redshift data sets as well as photometric redshift surveys have been deployed and (particularly for the photometric redshift data sets) a thorough analysis of the effect of their observational issues on the measurement of local and global environment has been executed.The picture that emerges is that high-density environments are favoured places for galaxy evolution, showing an enhanced fraction of massive galaxies which have stopped forming stars and belong to the quiescent population. Galaxies in high-density environments have an increased probability of hosting radio-AGNs (belonging to the ensemble of processes that turn off the star-formation in massive galaxies) and these effects are visible since the start of the decline in the cosmic star-formation history. Large-scale structures, such as the filaments of the cosmic web, have also a role in shaping galaxy evolution and they may represent key places for the pre-processing of galaxies before they enter higher density regions such as the cluster or group environment.As an increasing amount of observational evidence on the relation between the evolution of galaxies and their environment is gathered, a complete solution to the problem of how the local galaxy population has evolved approaches, and the history of galaxies from their formation at the dawn of time to the present day gets closer to being traced. Figure 2 Growth of structures . . . . . . . . . . . . . . . 7 Figure 3 Evolution of the global SFR density . . . . . . . 8 Figure 4 Colour-density relation for VVDS galaxies . . 11 Figure 5 Fraction of M * contained in galaxies as a function sSFR ....

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The VVDS-VLA deep field

Cited by 12 publications

References 52 publications

Properties and environment of radio-emitting galaxies in the VLA-zCOSMOS survey

Properties and environment of radio-emitting galaxies in the VLA-zCOSMOS survey

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

The Role of the Environment on Galaxy Evolution

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