The VIRMOS deep imaging survey

Radovich, M.; Arnaboldi, M.; Ripepi, V.; Massarotti, M.; McCracken, H. J.; Mellier, Y.; Bertin, E.; Zamorani, G.; Adami, C.; Bardelli, S.; Fèvre, O. Le; Foucaud, Sylvie; Garilli, B.; Scaramella, R.; Vettolani, G.; Zanichelli, A.; Zucca, E.

doi:10.1051/0004-6361:20034458

Cited by 57 publications

(64 citation statements)

References 21 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Photometric redshifts computed by Arnouts et al (2007) are also available in the VVDS database (see also McCracken et al 2003;Radovich et al 2004;Iovino et al 2005). These were estimated using the χ 2 fitting algorithm Le Phare 2 and calibrated with the VVDS first epoch spectroscopic redshifts (providing ∼1500 secure spectra for sources with m AB (3.6 μm) < 21.5) in the same dataset as described in Ilbert et al (2006), which includes the 3.6 μm and 4.5 μm infrared photometry from SWIRE .…”

Section: Vvds-swirementioning

confidence: 99%

Mid- and far-infrared luminosity functions and galaxy evolution from multiwavelengthSpitzerobservations up toz ~ 2.5

Rodighiero¹,

Vaccari²,

Franceschini³

et al. 2010

A&A

Self Cite

156

145

View full text Add to dashboard Cite

Context. Studies of the infrared (IR) emission of cosmic sources have proven essential to constraining the evolutionary history of cosmic star formation and the gravitational accretion of nuclear black holes, because many of these events occur inside heavily dustextinguished environments. Aims. The Spitzer Space Telescope has provided a large amount of data to constrain the nature and cosmological evolution of infrared source populations. In the present paper we exploit a large homogeneous dataset to derive a self-consistent picture of IR emission based on the time-dependent λ eff = 24, 15, 12, and 8 μm monochromatic and bolometric IR luminosity functions (LF) over the full 0 < z < 2.5 redshift range. Methods. Our present analysis is based on a combination of data from deep Spitzer surveys of the VIMOS VLT Deep Survey (VVDS-SWIRE) and GOODS fields. To our limiting flux of S 24 = 400 μJy, our sample derived from VVDS-SWIRE includes 1494 sources, and 666 and 904 sources brighter than S 24 = 80 μJy are catalogued in GOODS-S and GOODS-N, respectively, for a total area of ∼0.9 square degrees. Apart from a few galaxies, we obtain reliable optical identifications and redshifts for all these sources, providing a rich and robust dataset for our luminosity function determination. The final combined reliable sample includes 3029 sources, the fraction with photometric redshifts being 72% over all redshifts and almost all galaxies at z > 1.5. Based on the multiwavelength information available in these areas, we constrain the LFs at 8, 12, 15, and 24 μm. We also infer the total IR luminosities from our best-fit model of the observed SEDs of each source, and use this to derive the bolometric (8−1000 μm) LF and comoving volume emissivity to z ∼ 2.5. Results. In the redshift interval 0 < z < 1, the bolometric IR luminosity density evolves as (1 + z) 3.8±0.4 . Although it is more uncertain at higher-z, our results show a flattening in the IR luminosity density at z > 1. The mean redshift of the peak in the source number density shifts with luminosity: the brightest IR galaxies appear to form stars at earlier cosmic times (z > 1.5), while star formation in the less luminous galaxies continues until more recent epochs (z ∼ 1 for L IR < 10 11 L ), in overall agreement with similar analyses in the literature. Conclusions. Our results are indicative of a rapid increase in the galaxy IR comoving volume emissivity up to z ∼ 1 and a constant average emissivity at z > 1. We also appear to measure a difference in the evolutionary rate of the source number densities as a function of luminosity, which is consistent with the downsizing evolutionary patterns reported for other samples of cosmic sources.

show abstract

Section: Vvds-swirementioning

confidence: 99%

Mid- and far-infrared luminosity functions and galaxy evolution from multiwavelengthSpitzerobservations up toz ~ 2.5

Rodighiero¹,

Vaccari²,

Franceschini³

et al. 2010

A&A

Self Cite

156

145

View full text Add to dashboard Cite

show abstract

“…The survey strategy and goals are described in detail by Le Fèvre et al (2005). The VVDS is complemented by ancillary deep photometric data that have been collected at the CFHT telescope (BVRI, Le Fèvre et al 2004;McCracken et al 2003), at the NTT telescope (JK, Iovino et al 2005;Temporin et al 2008), and at the MPI telescope (U, Radovich et al 2004). In addition, u * , g , r , i , and z'-band data are available as part of the CFHT Legacy Survey.…”

Section: The Vvds-02h Samplementioning

confidence: 99%

The VIMOS-VLT deep survey: the group catalogue

Cucciati

Marinoni

Iovino³

et al. 2010

A&A

Self Cite

View full text Add to dashboard Cite

Aims. We present a homogeneous and complete catalogue of optical galaxy groups identified in the purely flux-limited (17.5 ≤ I AB ≤ 24.0) VIMOS-VLT deep redshift Survey (VVDS). Methods. We use mock catalogues extracted from the Millennium Simulation, to correct for potential systematics that might affect the overall distribution as well as the individual properties of the identified systems. Simulated samples allow us to forecast the number and properties of groups that can be potentially found in a survey with VVDS-like selection functions. We use them to correct for the expected incompleteness and, to asses in addition, how well galaxy redshifts trace the line-of-sight velocity dispersion of the underlying mass overdensity. In particular, on these mock catalogues we train the adopted group-finding technique i.e., the Voronoi-Delaunay Method (VDM). The goal is to fine-tune its free parameters, recover in a robust and unbiased way the redshift and velocity dispersion distributions of groups (n(z) and n(σ), respectively), and maximize, at the same time, the level of completeness and purity of the group catalogue. Results. We identify 318 VVDS groups with at least 2 members in the range 0.2 ≤ z ≤ 1.0, among which 144 (/30) with at least 3 (/5) members. The sample has an overall completeness of ∼60% and a purity of ∼50%. Nearly 45% of the groups with at least 3 members are still recovered if we run the algorithm with a particular parameter set that maximizes the purity (∼75%) of the resulting catalogue. We use the group sample to explore the redshift evolution of the fraction f b of blue galaxies (U − B ≤ 1) in the redshift range 0.2 ≤ z ≤ 1. We find that the fraction of blue galaxies is significantly lower in groups than in the global population (i.e. in the whole ensemble of galaxies irrespective of their environment). Both of these quantities increase with redshift, the fraction of blue galaxies in groups exhibiting a marginally significant steeper increase. We also investigate the dependence of f b on group richness: not only we confirm that, at any redshift, the blue fraction decreases in systems with increasing richness, but we find that this result continues to hold towards fainter luminosities.

show abstract

“…1, we compare our galaxy number counts with those derived by shallow surveys of large area (SDSS EDR, Yasuda et al 2001) or of similar area (GOYA by Eliche-Moral et al 2006; VVDS-F2 by Radovich et al 2004), and with deep pencil beam surveys (Hawaii HDFN by Capak et al 2004; WHT, HDFN, and HDFS by Metcalfe et al 2001). In particular, the WHT galaxy counts (Metcalfe et al 2001) are based on a 34 h exposure time image reaching U(Vega) = 26.8 but at the much lower 3σ level in the photometric noise and in an area of ∼50 arcmin 2 , while the GOYA survey at the INT telescope is complete at the 50% level at U(Vega) = 24.8.…”

Section: Deep U-band Galaxy Number Countsmentioning

confidence: 99%

Wide and deep near-UV (360 nm) galaxy counts and the extragalactic background light with the Large Binocular Camera

Grazian

Menci

Giallongo

et al. 2009

A&A

Self Cite

View full text Add to dashboard Cite

Context. Deep multicolour surveys are the main tool for exploring the formation and evolution of the very faint galaxies that are beyond the spectroscopic limit of present technology. The photometric properties of these faint galaxies are usually compared with current renditions of semianalytical models to provide constraints on the detailed treatment of the fundamental physical processes involved in galaxy formation and evolution, namely the mass assembly and the star formation. Aims. Galaxy counts over large sky areas in the 360 nm near-UV band are particularly difficult to obtain given the low efficiency of near-UV instrumentation, even at 8 m class telescopes. Observing in the near-UV bands can provide a first assessment of the distribution of star formation activity in distant (up to z ∼ 3) galaxies. A relatively large instrumental field of view helps to minimize the biases caused by cosmic variance. Methods. We obtained deep images in the 360 nm U band provided by the blue channel of the Large Binocular Camera at the prime focus of the Large Binocular Telescope. Over an area of 0.4 sq. deg., we derived the galaxy number counts down to U = 27 in the Vega system (corresponding to U = 27.86 in the AB system) at a completeness level of 30% reaching the faintest current limit for this wavelength and sky area. Results. The shape of the galaxy number counts in the U band can be described by a double power-law, the bright side being consistent with the shape of shallower surveys of comparable or greater areas. The slope bends over significantly at U > 23.5 ensuring the convergence of the contribution by star-forming galaxies to the extragalactic background light in the near-UV band to a value that is more than 70% of the most recent upper limits derived for this band. We jointly compared our near-UV and K band counts collected from the literature with a few selected hierarchical CDM models, concentrating on specific critical issues in the physical description of the galaxy formation and evolution.

show abstract

The VIRMOS deep imaging survey

Cited by 57 publications

References 21 publications

Mid- and far-infrared luminosity functions and galaxy evolution from multiwavelengthSpitzerobservations up toz ~ 2.5

Mid- and far-infrared luminosity functions and galaxy evolution from multiwavelengthSpitzerobservations up toz ~ 2.5

The VIMOS-VLT deep survey: the group catalogue

Wide and deep near-UV (360 nm) galaxy counts and the extragalactic background light with the Large Binocular Camera

Contact Info

Product

Resources

About