The VIMOS-VLT deep survey

Ilbert, O.; Tresse, L.; Zucca, E.; Bardelli, S.; Arnouts, S.; Zamorani, G.; Pozzetti, L.; Bottini, D.; Garilli, B.; Brun, V. Le; Fèvre, O. Le; Maccagni, D.; Picat, J. P.; Scaramella, R.; Scodeggio, M.; Vettolani, G.; Zanichelli, A.; Adami, C.; Arnaboldi, M.; Bolzonella, M.; Cappi, A.; Charlot, S.; Contini, T.; Foucaud, S.; Franzetti, P.; Gavignaud, I.; Guzzo, L.; Iovino, A.; McCracken, H. J.; Marano, B.; Marinoni, C.; Mathez, G.; Mazure, A.; Meneux, B.; Merighi, R.; Paltani, S.; Pelló, R.; Pollo, A.; Radovich, M.; Bondì, M.; Bongiorno, A.; Busarello, G.; Ciliegi, P.; Lamareille, F.; Mellier, Y.; Merluzzi, P.; Ripepi, V.; Rizzo, D.

doi:10.1051/0004-6361:20041961

Cited by 234 publications

(366 citation statements)

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“…The TSR is the number of targets that were allocated a slit for spectroscopic observation divided by the number of photometric targets down to an apparent magnitude limit. The TSR depends on RA, DEC, magnitudes and for VVDS on the size of the galaxy along the spatial dimension of the slit (see Ilbert et al 2005). The SSR is the fraction of spectroscopic targets for which the redshift was successfully determined.…”

Section: Sampling Rate Correctionsmentioning

confidence: 99%

“…Furthermore, we bin the data in narrow redshift bins, and therefore, we neglect the variation of TSR with galaxy size. VVDS-Deep TSR and SSR are provided through their data base (see Ilbert et al 2005, for more details). For the VVDS-Wide and DEEP2, we compute them as follows.…”

Section: Sampling Rate Correctionsmentioning

confidence: 99%

“…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%

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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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Section: Sampling Rate Correctionsmentioning

confidence: 99%

Section: Sampling Rate Correctionsmentioning

confidence: 99%

Section: Datamentioning

confidence: 99%

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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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“…Absolute magnitudes are computed following the method described in the Appendix of Ilbert et al (2005). The K-correction is computed using a set of templates and all the multi-band photometry data available.…”

Section: Stellar Masses and Absolute Magnitudes Estimatementioning

confidence: 99%

The zCOSMOS redshift survey: the role of environment and stellar mass in shaping the rise of the morphology-density relation from z ~ 1

Tasca

Kneib²,

Iovino

et al. 2009

A&A

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152

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Context. For more than two decades we have known that galaxy morphological segregation is present in the Local Universe. It is important to see how this relation evolves with cosmic time. Aims. To investigate how galaxy assembly took place with cosmic time, we explore the evolution of the morphology-density relation up to redshift z ∼ 1 using about 10 000 galaxies drawn from the zCOSMOS Galaxy Redshift Survey. Taking advantage of accurate HST/ACS morphologies from the COSMOS survey, of the well-characterised zCOSMOS 3D environment, and of a large sample of galaxies with spectroscopic redshift, we want to study here the evolution of the morphology-density relation up to z ∼ 1 and its dependence on galaxy luminosity and stellar mass. The multi-wavelength coverage of the field also allows a first study of the galaxy morphological segregation dependence on colour. We further attempt to disentangle between processes that occurred early in the history of the Universe or late in the life of galaxies. Methods. The zCOSMOS field benefits of high-resolution imaging in the F814W filter from the Advanced Camera for Survey (ACS). We use standard morphology classifiers, optimised for being robust against band-shifting and surface brightness dimming, and a new, objective, and automated method to convert morphological parameters into early, spiral, and irregular types. We use about 10 000 galaxies down to I AB = 22.5 with a spectroscopic sampling rate of 33% to characterise the environment of galaxies up to z ∼ 1 from the 100 kpc scales of galaxy groups up to the 100 Mpc scales of the cosmic web. The evolution of the morphology-density relation in different environments is then studied for luminosity and stellar-mass selected, volume-limited samples of galaxies. The trends are described and related to the various physical processes that could play a relevant role in the build-up of the morphology-density relation. Results. We confirm that the morphological segregation is present up to z ∼ 1 for luminosity-selected, volume-limited samples. The behaviour of the morphology-density relation gets flatter at fixed masses expecially above 10 10.6 M . We suggest the existence of a critical mass above which the physical processes governing galaxy stellar mass also determine the shaping of the galaxy more than its environment. We finally show that at a fixed morphology there is still a residual variation in galaxy colours with density. Conclusions. The observed evolution with redshift of the morphology-density relation offers an opportunity to trace the effect of nature and nurture as a function of environment. Even though it is based mainly on a biased view, the environmental dependence of the morphological evolution for luminosity-selected, volume-limited samples seems to indicate that nurture is in play. On the other hand, the lack of evolution observed for earlytype and spiral galaxies that are more massive than 10 10.8 M independents of the environment indicates that nature has imprinted these properties early in the life of...

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“…The LFs are computed using the "Algorithm for Luminosity Function" (ALF, Ilbert et al 2005). Ilbert et al (2004) demonstrated that the estimate of the global LF can be biased when the band used to compute the LF strongly differs from the rest-frame band in which the galaxies are selected.…”

Section: Resultsmentioning

confidence: 99%

Where is the Light? Tracing the Evolution of Bulges and Disks since z ~ 0.8

Tasca

Tresse

2010

Proc. IAU

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Abstract. The chronology of galactic bulge and disk formation is studied by analysing the relative contributions of these components to the B band rest-frame luminosity density (LD) at two different cosmological epochs. The luminosity function (LF) of the bulge and disk components at z ∼ 0.8 is computed on a galaxy subsample of the final zCOSMOS "bright" catalogue of roughly 20,000 objects with spectroscopic redshift in the COSMOS field. The comparison is then performed on galaxies in the local universe. Our preliminary results show that the LD in the disk component strongly decreases from ∼ 80% at z ∼ 0.8 to ∼ 50% at z = 0, the bulges having a specular behaviour. The observational constraints provided in this work are aimed to discriminate among competing scenarios of galaxy formation and evolution. An appropriate comparison with hydrodynamical semianalytical models will be considered in a future study to understand further the formation and evolution of galaxies.

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The VIMOS-VLT deep survey

Cited by 234 publications

References 32 publications

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

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

The zCOSMOS redshift survey: the role of environment and stellar mass in shaping the rise of the morphology-density relation from z ~ 1

Where is the Light? Tracing the Evolution of Bulges and Disks since z ~ 0.8

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