The VIMOS VLT Deep Survey

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

doi:10.1051/0004-6361:20048072

Cited by 292 publications

(221 citation statements)

References 12 publications

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“…Thus, we roughly estimate the efficiency of our B-dropout selection to ∼90%. Six of our U-dropouts have been observed spectroscopically in the VVDS (Le Fèvre et al 2004) and one of them also for the GOODS programme (Vanzella et al 2005). Three of them are at z > 3, while the other three are low-redshift interlopers.…”

Section: Observations With Other Telescopesmentioning

confidence: 87%

GaBoDS: the Garching-Bonn Deep Survey

Hildebrandt¹,

Bomans

Erben³

et al. 2005

A&A

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We present first results of our search for high-redshift galaxies in deep CCD mosaic images. As a pilot study for a larger survey, very deep images of the Chandra Deep Field South (CDFS), taken with WFI@MPG/ESO2.2m, are used to select large samples of 1070 U-band and 565 B-band dropouts with the Lyman-break method. The data of these Lyman-break galaxies are made public as an electronic table. These objects are good candidates for galaxies at z ∼ 3 and z ∼ 4 which is supported by their photometric redshifts. The distributions of apparent magnitudes and the clustering properties of the two populations are analysed, and they show good agreement to earlier studies. We see no evolution in the comoving clustering scale length from z ∼ 3 to z ∼ 4. The techniques presented here will be applied to a much larger sample of U-dropouts from the whole survey in near future.

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Section: Observations With Other Telescopesmentioning

confidence: 87%

GaBoDS: the Garching-Bonn Deep Survey

Hildebrandt¹,

Bomans

Erben³

et al. 2005

A&A

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“…In this study we use spectroscopic redshifts coming from a combination of various studies (Cohen et al 2000;Wirth et al 2004;Cowie et al 2004;Le Fèvre et al 2004;Mignoli et al 2005;Vanzella et al 2006;Reddy et al 2006;Barger et al 2008;Cimatti et al 2008;Kurk et al in prep. for GMASS redshifts and finally Stern et al in prep.).…”

Section: Redshiftsmentioning

confidence: 99%

Evolution of the dusty infrared luminosity function fromz = 0toz = 2.3using observations fromSpitzer

Magnelli

Elbaz

Chary

et al. 2011

A&A

352

422

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Aims. We derive the evolution of the infrared luminosity function (LF) over the last 4/5ths of cosmic time using deep 24 and 70 μm imaging of the GOODS North and South fields. Methods. We use an extraction technique based on prior source positions at shorter wavelengths to build the 24 and 70 μm source catalogs. The majority (93%) of the sources have a spectroscopic (39%) or a photometric redshift (54%) and, in our redshift range of interest (i.e., 1.3 < z < 2.3) ∼20% of the sources have a spectroscopic redshift. To extend our study to lower 70 μm luminosities we perform a stacking analysis and we characterize the observed L 24/(1+z) vs. L 70/(1+z) correlation. Using spectral energy distribution (SED) templates which best fit this correlation, we derive the infrared luminosity of individual sources from their 24 and 70 μm luminosities. We then compute the infrared LF at z ∼ 1.55 ± 0.25 and z ∼ 2.05 ± 0.25. Results. We observe the break in the infrared LF up to z ∼ 2.3. The redshift evolution of the infrared LF from z = 1.3 to z = 2.3 is consistent with a luminosity evolution proportional to (1 + z) 1.0±0.9 combined with a density evolution proportional to (1 + z) −1.1±1.5 . At z ∼ 2, luminous infrared galaxies (LIRGs: 10 11 L < L IR < 10 12 L ) are still the main contributors to the total comoving infrared luminosity density of the Universe. At z ∼ 2, LIRGs and ultra-luminous infrared galaxies (ULIRGs: 10 12 L < L IR ) account for ∼49% and ∼17% respectively of the total comoving infrared luminosity density of the Universe. Combined with previous results using the same strategy for galaxies at z < 1.3 and assuming a constant conversion between the infrared luminosity and star-formation rate (SFR) of a galaxy, we study the evolution of the SFR density of the Universe from z = 0 to z = 2.3. We find that the SFR density of the Universe strongly increased with redshift from z = 0 to z = 1.3, but is nearly constant at higher redshift out to z = 2.3. As part of the online material accompanying this article, we present source catalogs at 24 μm and 70 μm for both the GOODS-North and -South fields.

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“…) and GOODS-S (Szokoly et al 2004;Le Fèvre et al 2004;Mignoli et al 2005;Vanzella et al 2005Vanzella et al , 2006Vanzella et al , 2008Ravikumar et al 2007;Popesso et al 2009;Kurk et al 2009;Balestra et al 2010;…”

Section: Goods Sampleunclassified

GOODS-Herschel: the impact of galaxy-galaxy interactions on the far-infrared properties of galaxies

Hwang¹,

Elbaz²,

Dickinson³

et al. 2011

A&A

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Aims. We study the impact of galaxy-galaxy interactions on the far-infrared properties of galaxies and its evolution at 0 < z < 1.2. Methods. Using the high-z galaxies in the fields of Great Observatories Origins Deep Survey (GOODS) observed by the Herschel Space Observatory in the framework of the GOODS-Herschel key program and the local IRAS or AKARI-selected galaxies in the field of Sloan Digital Sky Survey Data Release 7, we investigate the dependence of galaxy properties on the morphology of and the distance to the nearest neighbor galaxy. Results. We find that the star-formation rates (SFRs) and the specific SFRs (SSFRs) of galaxies on average depend on the morphology of and the distance to the nearest neighbor galaxy in this redshift range. When a late-type galaxy has a close neighbor galaxy, the SFR and the SSFR increase as it approaches a late-type neighbor, which is supported by Kolmogorov-Smirnov (K-S) and Monte Carlo (MC) tests with a significance level of >99%. However, the SFR and the SSFR decrease or do not change much as the galaxy approaches an early-type neighbor. The bifurcations of SFRs and SSFRs depending on the neighbor's morphology seem to occur at R n ≈ 0.5r vir,nei (virial radius of the neighbor), which is supported by K-S and MC tests with a significance level of >98%. For all redshift bins, the SSFRs of late-type galaxies interacting with late-type neighbors are increased by factors of about 1.8 ± 0.7 and 4.0 ± 1.2 compared to those of non-interacting galaxies when the pair separation is smaller than 0.5r vir,nei and 0.1r vir,nei , respectively. The dust temperature of both local and high-z late-type galaxies that strongly interact with late-type neighbors (i.e. R n ≤ 0.1r vir,nei ) appears to be higher than that of non-interacting galaxies with a significance level of 96−99%. However, the dust temperature of local late-type galaxies that strongly interact with early-type neighbors seems to be lower than or similar to that of non-interacting galaxies. Conclusions. Our results suggest that galaxy-galaxy interactions and mergers have been strongly affecting the SFR and the dust properties of star-forming galaxies over at least 8 billion years.

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The VIMOS VLT Deep Survey

Cited by 292 publications

References 12 publications

GaBoDS: the Garching-Bonn Deep Survey

GaBoDS: the Garching-Bonn Deep Survey

Evolution of the dusty infrared luminosity function fromz = 0toz = 2.3using observations fromSpitzer

GOODS-Herschel: the impact of galaxy-galaxy interactions on the far-infrared properties of galaxies

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