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1. Euclid preparation: XXXVIII. Spectroscopy of active galactic nuclei with NISP.

Author

Euclid Collaboration, Lusso, E., Fotopoulou, S., Selwood, M., Allevato, V., Calderone, G., Mancini, C., Mignoli, M., Scodeggio, M., Bisigello, L., Feltre, A., Ricci, F., La Franca, F., Vergani, D., Gabarra, L., Le Brun, V., Maiorano, E., Palazzi, E., Moresco, M., and Zamorani, G.

Subjects
DISTRIBUTION (Probability theory), BLACK holes, ACTIVE galactic nuclei, REDSHIFT, SUPERMASSIVE black holes, ASTROPHYSICS, SPECTROMETRY, GALAXY clusters
Abstract

The statistical distribution and evolution of key properties of active galactic nuclei (AGN), such as their accretion rate, mass, and spin, remains a subject of open debate in astrophysics. The ESA Euclid space mission, launched on July 1 2023, promises a breakthrough in this field. We create detailed mock catalogues of AGN spectra from the rest-frame near-infrared down to the ultraviolet – including emission lines – to simulate what Euclid will observe for both obscured (type 2) and unobscured (type 1) AGN. We concentrate on the red grisms of the NISP instrument, which will be used for the wide-field survey, opening a new window for spectroscopic AGN studies in the near-infrared. We quantify the efficiency in the redshift determination as well as in retrieving the emission line flux of the Hα+[N II] complex, as Euclid is mainly focused on this emission line, given that it is expected to be the brightest one in the probed redshift range. Spectroscopic redshifts are measured for 83% of the simulated AGN in the interval where the Hα is visible (i.e. 0.89 <  z <  1.83 at a line flux of > 2 × 10−16 erg s−1 cm−2, encompassing the peak of AGN activity at z ≃ 1 − 1.5) within the spectral coverage of the red grism. Outside this redshift range, the measurement efficiency decreases significantly. Overall, a spectroscopic redshift iscorrectly determined for about 90% of type 2 AGN down to an emission line flux of roughly 3 × 10−16 erg s−1 cm−2, and for type 1 AGN down to 8.5 × 10−16 erg s−1 cm−2. Recovered values for black hole mass show a small offset with respect to the input values by about 10%, but the agreement is good overall. With such a high spectroscopic coverage at z <  2, we will be able to measure AGN demography, scaling relations, and clustering from the epoch of the peak of AGN activity down to the present-day Universe for hundreds of thousands of AGN with homogeneous spectroscopic information. [ABSTRACT FROM AUTHOR]

Published
2024
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2. The VVDS Data‐Reduction Pipeline: Introducing VIPGI, the VIMOS Interactive Pipeline and Graphical Interface

Author

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

Published
2005
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3. The VIMOS Integral Field Unit: Data‐Reduction Methods and Quality Assessment

Author

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

Published
2005
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4. The Very Large Telescope Visible Multi‐Object Spectrograph Mask Preparation Software

Author

Bottini, D., Garilli, B., Maccagni, D., Tresse, L., Le Brun, V., Le Fèvre, O., Picat, J. P., Scaramella, R., Scodeggio, M., Vettolani, G., Zanichelli, A., Adami, C., Arnaboldi, M., Arnouts, S., Bardelli, S., Bolzonella, M., Cappi, A., Charlot, S., Ciliegi, P., Contini, T., Foucaud, S., Franzetti, P., Guzzo, L., Ilbert, O., Iovino, A., McCracken, H. J., Marano, B., Marinoni, C., Mathez, G., Mazure, A., Meneux, B., Merighi, R., Paltani, S., Pollo, A., Pozzetti, L., Radovich, M., Zamorani, G., and Zucca, E.

Published
2005
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5. A test of the nature of cosmic acceleration using galaxy redshift distortions

Author

Guzzo, L., Pierleoni, M., Meneux, B., Branchini, E., Le Fevre, O., Marinoni, C., Garilli, B., Blaizot, J., De Lucia, G., Pollo, A., McCracken, H. J., Bottini, D., Le Brun, V., Maccagni, D., Picat, J. P., Scaramella, R., Scodeggio, M., Tresse, L., Vettolani, G., Zanichelli, A., Adami, C., Arnouts, S., Bardelli, S., Bolzonella, M., Bongiorno, A., Cappi, A., Charlot, S., Ciliegi, P., Contini, T., Cucciati, O., de la Torre, S., Dolag, K., Foucaud, S., Franzetti, P., Gavignaud, I., Ilbert, O., Iovino, A., Lamareille, F., Marano, B., Mazure, A., Memeo, P., Merighi, R., Moscardini, L., Paltani, S., Pello, R., Perez-Montero, E., Pozzetti, L., Radovich, M., Vergani, D., Zamorani, G., and Zucca, E.

Subjects
Red shift -- Research -- Observations, Expanding universe -- Observations -- Research, Environmental issues, Science and technology, Zoology and wildlife conservation, Observations, Research
Abstract

Author(s): L. Guzzo (corresponding author) [1, 2, 3, 4]; M. Pierleoni [3]; B. Meneux [5]; E. Branchini [6]; O. Le Fèvre [7]; C. Marinoni [8]; B. Garilli [5]; J. Blaizot [...]

Published
2008
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6. Clinical spectrum, prognosis and estimated prevalence of DNAJB11-kidney disease

Author

Huynh, V.T., Audrézet, M.-P., Sayer, J.A., Ong, A.C., Lefevre, S., Le Brun, V., Després, A., Senum, S.R., Chebib, F., Barroso-Gil, M., Patel, C., Mallett, A.J., Goel, H., Mallawaarachchi, A.C., Van Eerde, A.M., Ponlot, E., Kribs, M., Le Meur, Y., Harris, P.C., and Cornec-Le Gall, E.

Abstract

Monoallelic mutations of DNAJB11 were recently described in seven pedigrees with atypical clinical presentations of autosomal dominant polycystic kidney disease. DNAJB11 encodes one of the main cofactors of the endoplasmic reticulum chaperon BiP, a heat-shock protein required for efficient protein folding and trafficking. Here we conducted an international collaborative study to better characterize the DNAJB11-associated phenotype. Thirteen different loss-of-function variants were identified in 20 new pedigrees (54 affected individuals) by targeted next-generation sequencing, whole-exome sequencing or whole-genome sequencing. Amongst the 77 patients (27 pedigrees) now in total reported, 32 reached end stage kidney disease (range, 55-89 years, median age 75); without a significant difference between males and females. While a majority of patients presented with non-enlarged polycystic kidneys, renal cysts were inconsistently identified in patients under age 45. Vascular phenotypes, including intracranial aneurysms, dilatation of the thoracic aorta and dissection of a carotid artery were present in four pedigrees. We accessed Genomics England 100,000 genomes project data, and identified pathogenic variants of DNAJB11 in nine of 3934 probands with various kidney and urinary tract disorders. The clinical diagnosis was cystic kidney disease for eight probands and nephrocalcinosis for one proband. No additional pathogenic variants likely explaining the kidney disease were identified. Using the publicly available GnomAD database, DNAJB11 genetic prevalence was calculated at 0.85/10.000 individuals. Thus, establishing a precise diagnosis in atypical cystic or interstitial kidney disease is crucial, with important implications in terms of follow-up, genetic counseling, prognostic evaluation, therapeutic management, and for selection of living kidney donors.

Published
2020

8. Estimating the galaxy two-point correlation function using a split random catalog

Author

Gargiulo, A., Cucciati, O., Garilli, B., Scodeggio, M., Bolzonella, M., Zamorani, G., De Lucia, G., Krywult, J., Guzzo, L., Granett, B. R., de la Torre, S., Abbas, U., Adami, C., Arnouts, S., Bottini, D., Cappi, A., Franzetti, P., Fritz, A., Haines, C., Hawken, A. J., Iovino, A., Le Brun, V., Le Fèvre, O., Maccagni, D., Małek, K., Marulli, F., Moutard, T., Polletta, M., Pollo, A., Tasca, L. A. M., Tojeiro, R., Vergani, D., Zanichelli, A., Bel, J., Branchini, E., Coupon, J., Ilbert, O., Moscardini, L., Peacock, J. A., Gargiulo, A., Cucciati, O., Garilli, B., Scodeggio, M., Bolzonella, M., Zamorani, G., De Lucia, G., Krywult, J., Guzzo, L., Granett, B. R., de la Torre, S., Abbas, U., Adami, C., Arnouts, S., Bottini, D., Cappi, A., Franzetti, P., Fritz, A., Haines, C., Hawken, A. J., Iovino, A., Le Brun, V., Le Fèvre, O., Maccagni, D., Małek, K., Marulli, F., Moutard, T., Polletta, M., Pollo, A., Tasca, L. A. M., Tojeiro, R., Vergani, D., Zanichelli, A., Bel, J., Branchini, E., Coupon, J., Ilbert, O., Moscardini, L., and Peacock, J. A.

Subjects
formation [galaxies], galaxies: evolution, galaxies: formation, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, evolution [galaxies]
Abstract

We use the unparalleled statistics of the VIPERS survey to investigate the relation between the surface mean stellar mass density Sigma = M/(2 pi R-e(2)) of massive passive galaxies (MPGs, M >= 10(11) M-circle dot) and their local environment in the redshift range 0.5 2 x 10(11) M-circle dot, we find an excess of MPGs with low Sigma and a deficit of high-Sigma MPGs in the densest regions with respect to other environments. We interpret this result as due to the migration of some high-Sigma MPGs (= 0.8 migrate to the MPG population. Here, we investigate the Sigma-delta relation of MSFGs at z >= 0.8 and find that it is consistent within 1 sigma with that of low-Sigma MPGs at z = 0.8 are consistent in terms of number and environment with being the progenitors of low-Sigma MPGs at z < 0.8.

Published
2019

9. Obscured AGN at 1.5 < z < 3.0 from the zCOSMOS-deep Survey

Author

Mignoli, M., Feltre, A., Bongiorno, A., Calura, F., Gilli, R., Vignali, C., Zamorani, G., Lilly, S. J., Le Fèvre, O., Bardelli, S., Bolzonella, M., Bordoloi, R., Le Brun, V., Caputi, K. I., Cimatti, A., Diener, C., Garilli, B., Koekemoer, A. M., Maier, C., Mainieri, V., Peng, Y., Pérez Montero, E., Silverman, J. D., Zucca, E., Mignoli, M., Feltre, A., Bongiorno, A., Calura, F., Gilli, R., Vignali, C., Zamorani, G., Lilly, S. J., Le Fèvre, O., Bardelli, S., Bolzonella, M., Bordoloi, R., Le Brun, V., Caputi, K. I., Cimatti, A., Diener, C., Garilli, B., Koekemoer, A. M., Maier, C., Mainieri, V., Peng, Y., Pérez Montero, E., Silverman, J. D., and Zucca, E.

Subjects
galaxies: active, line: formation, galaxies: evolution, galaxies: fundamental parameter, quasars: emission line, X-rays: galaxie
Abstract

Context. The physics and demographics of high-redshift obscured active galactic nuclei (AGN) is still scarcely investigated. New samples of such objects, selected with different techniques, can provide useful insights into their physical properties.Aims. With the goal to determine the properties of the gas in the emitting region of type 2 AGN, in particular, the gas metal content, we exploit predictions from photoionization models, including new parameterizations for the distance of gas distribution from the central source and internal microturbulence in the emitting clouds, to interpret rest-frame UV spectral data.Methods. We selected a sample of 90 obscured (type 2) AGN with 1.45

Published
2019

10. The VIMOS Public Extragalactic Redshift Survey (VIPERS)

Author

Gargiulo, A., Cucciati, O., Garilli, B., Scodeggio, M., Bolzonella, M., Zamorani, G., De Lucia, G., Krywult, J., Guzzo, L., Granett, B. R., de la Torre, S., Abbas, U., Adami, C., Arnouts, S., Bottini, D., Cappi, A., Franzetti, P., Fritz, A., Haines, C., Hawken, A. J., Iovino, A., Le Brun, V., Le Fèvre, O., Maccagni, D., Małek, K., Marulli, F., Moutard, T., Polletta, M., Pollo, A., Tasca, L. A. M., Tojeiro, R., Vergani, D., Zanichelli, A., Bel, J., Branchini, E., Coupon, J., Ilbert, O., Moscardini, L., Peacock, J. A., Gargiulo, A., Cucciati, O., Garilli, B., Scodeggio, M., Bolzonella, M., Zamorani, G., De Lucia, G., Krywult, J., Guzzo, L., Granett, B. R., de la Torre, S., Abbas, U., Adami, C., Arnouts, S., Bottini, D., Cappi, A., Franzetti, P., Fritz, A., Haines, C., Hawken, A. J., Iovino, A., Le Brun, V., Le Fèvre, O., Maccagni, D., Małek, K., Marulli, F., Moutard, T., Polletta, M., Pollo, A., Tasca, L. A. M., Tojeiro, R., Vergani, D., Zanichelli, A., Bel, J., Branchini, E., Coupon, J., Ilbert, O., Moscardini, L., and Peacock, J. A.

Subjects
formation [galaxies], Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, evolution [galaxies]
Abstract

We use the unparalleled statistics of the VIPERS survey to investigate the relation between the surface mean stellar mass density Sigma = M/(2 pi R-e(2)) of massive passive galaxies (MPGs, M >= 10(11) M-circle dot) and their local environment in the redshift range 0.5 2 x 10(11) M-circle dot, we find an excess of MPGs with low Sigma and a deficit of high-Sigma MPGs in the densest regions with respect to other environments. We interpret this result as due to the migration of some high-Sigma MPGs (= 0.8 migrate to the MPG population. Here, we investigate the Sigma-delta relation of MSFGs at z >= 0.8 and find that it is consistent within 1 sigma with that of low-Sigma MPGs at z = 0.8 are consistent in terms of number and environment with being the progenitors of low-Sigma MPGs at z < 0.8.

Published
2019

15. A large population of galaxies 9 to 12 billion years back in the history of the Universe

Author

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

Published
2005

18. The VIMOS Ultra Deep Survey: The role of HI kinematics and HI column density on the escape of Lyα photons in star-forming galaxies at 2 < z < 4

Author

Guaita, L, Talia, M, Pentericci, L, Verhamme, A, Cassata, P, Lemaux, BC, Orlitova, I, Ribeiro, B, Schaerer, D, Zamorani, G, Garilli, B, Le Brun, V, Le Fèvre, O, MacCagni, D, Tasca, LAM, Thomas, R, Vanzella, E, Zucca, E, Amorin, R, Bardelli, S, Castellano, M, Grazian, A, Hathi, NP, Koekemoer, A, and Marchi, F

Subjects
ISM: kinematics and dynamics, techniques: imaging spectroscopy, galaxies: high-redshift, galaxies: star formation, scattering
Abstract

© 2017 ESO. Aims. We wish to assess the role of kinematics and neutral hydrogen column density in the escape and distribution of Lya photons. Methods. We selected a sample of 76 Lya emitting galaxies from the VIMOS Ultra Deep Survey (VUDS) at 2 = z = 4. We estimated the velocity of the neutral gas flowing out of the interstellar medium as the velocity offset, δv, between the systemic redshift (zsys) and the center of low-ionization absorption line systems (LIS). To increase the S/N of VUDS spectra, we stacked subsamples defined based on median values of their photometric and spectroscopic properties. We measured the systemic redshift from the rest-frame UV spectroscopic data using the CIII]1908 nebular emission line, and we considered SiII1526 as the highest signal-to-noise LIS line. We calculated the Lya peak shift with respect to the zsys, the EW(Lya), and the Lya spatial extension, Ext(Lya-C), from the in the 2D stacked spectra. Results. The galaxies that are faint in the rest-frame UV continuum, strong in Lya and CIII] , with compact UV morphology, and localized in an underdense environment are characterized by outflow velocities of the order of a few hundreds of km s -1 . The subsamples with smaller δv are characterized by larger Lya peak shifts, larger Ext(Lya-C), and smaller EW(Lya). In general we find that EW(Lya) anti-correlates with Ext(Lya-C) and Lya peak shift. Conclusions. We interpret these trends using a radiative-transfer shell model. The model predicts that an HI gas with a column density larger than 1020 cm -2 is able to produce Lya peak shifts larger than > 300 km s -1 . An ISM with this value of NHI would favour a large amount of scattering events, especially when the medium is static, so it can explain large values of Ext(Lya-C) and small EW(Lya). On the contrary, an ISM with a lower NHI, but large velocity outflows would lead to a Lya spatial profile peaked at the galaxy center (i.e. low values of Ext(Lya-C)) and to a large EW(Lya), as we see in our data. Our results and their interpretation via radiative-transfer models tell us that it is possible to use Lya to study the properties of the HI gas. Also, the fact that Lya emitters are characterized by large δv could give hints about their stage of evolution in the sense that they could be experiencing short bursts of star formation that push strong outflows., This work is supported by funding from the European Research Council Advanced Grant ERC–2010–AdG–268107–EARLY and by INAF Grants PRIN 2010, PRIN 2012, and PICS 2013. This work is based on data products made available at the CESAM data center, Laboratoire d’Astrophysique de Marseille, France. R.A. acknowledges support from the ERC Advanced Grant 695671 “QUENCH” and I.O. from the Czech Science Foundation grant 17-06217Y.

Published
2017
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19. The zCOSMOS survey

Author

Zucca E., Bardelli S., Bolzonella M., Zamorani G., Ilbert O., Pozzetti L., Mignoli M., Kova, #269, Lilly S., Tresse L., Tasca L., Cassata P., Halliday C., Vergani D., Caputi K., Carollo C. M., Contini T., Kneib J. P., Le Fèvre O., Mainieri V., Renzini A., Scodeggio M., Bongiorno A., Coppa G., de La Torre S., de Ravel L., Franzetti P., Garilli B., Iovino A., Kampczyk P., Knobel C., Lamareille F., Le Borgne J. F., Le Brun V., Maier C., Pellò R., Peng Y., Perez Montero E., Ricciardelli E., Silverman J. D., Tanaka M., Abbas U., Bottini D., Cappi A., Guzzo L., Koekemoer A. M., Leauthaud A., Maccagni D., Marinoni C., McCracken H. J., Meme, P., Meneux B., Oesch P., Porciani C., Scaramella R., Arnouts S., Aussel H., Capak P., Kartaltepe J., Salvato M., Sanders D., Scoville N., Taniguchi Y., Thompson D., CUCCIATI, OLGA, CIMATTI, ANDREA, MORESCO, MICHELE ENNIO MARIA, INAF - Osservatorio Astronomico di Brera (OAB), Istituto Nazionale di Astrofisica (INAF), INAF - Osservatorio Astronomico di Bologna (OABO), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), AUTRES, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astrofisico di Arcetri (OAA), University of Chicago, Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), INAF- Milano, Dipartimento di Fisica, Università degli Studi di Milano-Bicocca = University of Milano-Bicocca (UNIMIB)-Università degli Studi di Milano = University of Milan (UNIMI), Institute of Astronomy [ETH Zürich], Department of Physics [ETH Zürich] (D-PHYS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Tokai University, Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), Space Telescope Science Institute (STSci), Centre de Physique Théorique - UMR 6207 (CPT), Université de la Méditerranée - Aix-Marseille 2-Université de Provence - Aix-Marseille 1-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Centre de Physique Théorique - UMR 7332 (CPT), Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Materials & Process technology, Boeing Company [Chicago], California Institute of Technology (CALTECH), Sea Mammal Research Unit, St Andrews, Astronomy, Zucca E., Bardelli S., Bolzonella M., Zamorani G., Ilbert O., Pozzetti L., Mignoli M., Kova&#269, K., Lilly S., Tresse L., Tasca L., Cassata P., Halliday C., Vergani D., Caputi K., Carollo C. M., Contini T., Kneib J.-P., Le Fèvre O., Mainieri V., Renzini A., Scodeggio M., Bongiorno A., Coppa G., Cucciati O., de La Torre S., de Ravel L., Franzetti P., Garilli B., Iovino A., Kampczyk P., Knobel C., Lamareille F., Le Borgne J.-F., Le Brun V., Maier C., Pellò R., Peng Y., Perez-Montero E., Ricciardelli E., Silverman J. D., Tanaka M., Abbas U., Bottini D., Cappi A., Cimatti A., Guzzo L., Koekemoer A. M., Leauthaud A., Maccagni D., Marinoni C., McCracken H. J., Meme, P., Meneux B., Moresco M., Oesch P., Porciani C., Scaramella R., Arnouts S., Aussel H., Capak P., Kartaltepe J., Salvato M., Sanders D., Scoville N., Taniguchi Y., Thompson D., Università di Bologna, Dipartimento di Astronomia, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Università degli Studi di Milano-Bicocca [Milano] (UNIMIB)-Università degli Studi di Milano [Milano] (UNIMI), Centre National de la Recherche Scientifique (CNRS)-Université de Toulon (UTLN)-Université de Provence - Aix-Marseille 1-Université de la Méditerranée - Aix-Marseille 2, and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)

Subjects
Normalization (statistics), Cosmology and Nongalactic Astrophysics (astro-ph.CO), High density, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Surveys, 01 natural sciences, Luminosity, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], MORPHOLOGICAL CLASSIFICATION, 1ST EPOCH DATA, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Density field, FIELD, 10. No inequality, 010303 astronomy & astrophysics, PHOTOMETRIC REDSHIFTS, Astrophysics::Galaxy Astrophysics, galaxies: statistics, Luminosity function (astronomy), Physics, REDSHIFT SURVEY, LEGACY SURVEY, 010308 nuclear & particles physics, Galaxies: evolution, Galaxies: luminosity function, mass function, Galaxies: statistics, Astronomy and Astrophysics, Space and Planetary Science, VLT DEEP SURVEY, B band, Galaxy, galaxies: luminosity function, mass function, COLOR-DENSITY RELATION, galaxies: luminosity function, mass function, DIGITAL SKY SURVEY, galaxies: evolution, Cosmic time, SURVEY COSMOS, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

(Abridged) We studied the evolution in the B band luminosity function to z~1 in the zCOSMOS 10k sample, for which both accurate galaxy classifications and a detailed description of the local density field are available. The global LF exhibits a brightening of ~0.7 mag in M* from z~0.2 to z~0.9. At low z, late types dominate at faint magnitudes, while the bright end is populated mainly by early types. At higher z, late-type galaxies evolve significantly and, at z~1, the contribution from the various types to the bright end of the LF is comparable. The evolution for early types is in both luminosity and normalization. A similar behaviour is exhibited by late types, but with an opposite trend for the normalization. Studying the role of the environment, we find that the global LF of galaxies in overdense regions has always a brighter M* and a flatter slope. In low density environments, the main contribution to the LF is from blue galaxies, while for high density environments there is an important contribution from red galaxies to the bright end. The differences between the global LF in the two environments are not due to only a difference in the relative numbers of red and blue galaxies, but also to their relative luminosity distributions: the value of M* for both types in underdense regions is always fainter than in overdense environments. The "specular" evolution of late- and early-type galaxies is consistent with a scenario where a part of blue galaxies is transformed in red galaxies with increasing cosmic time, without significant changes in the fraction of intermediate-type galaxies. The bulk of this tranformation in overdense regions probably happened before z~1, while it is still ongoing at lower z in underdense environments., Comment: 18 pages, 10 figures, A&A in press

Published
2009
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22. The VIMOS Public Extragalactic Redshift Survey

Author

Granett, B. R., Branchini, ENZO FRANCO, Guzzo, L., Abbas, U., Adami, C., Arnouts, S., Bel, J., Bolzonella, M., Bottini, D., Cappi, A., Coupon, J., Cucciati, O., Davidzon, I., De Lucia, G., de la Torre, S., Fritz, A., Franzetti, P., Fumana, M., Garilli, B., Ilbert, O., Iovino, A., Krywult, J., Le Brun, V., Le Fèvre, O., Maccagni, D., Małek, K., Marulli, F., Mccracken, H. J., Polletta, M., Pollo, A., Scodeggio, M., Tasca, L. A. M., Tojeiro, R., Vergani, D., Zanichelli, A., Burden, A., Di Porto, C., Marchetti, A., Marinoni, C., Mellier, Y., Moutard, T., Moscardini, L., Nichol, R. C., Peacock, J. A., Percival, W. J., Zamorani, G., Granett, B. R., Branchini, ENZO FRANCO, Guzzo, L., Abbas, U., Adami, C., Arnouts, S., Bel, J., Bolzonella, M., Bottini, D., Cappi, A., Coupon, J., Cucciati, O., Davidzon, I., De Lucia, G., de la Torre, S., Fritz, A., Franzetti, P., Fumana, M., Garilli, B., Ilbert, O., Iovino, A., Krywult, J., Le Brun, V., Le Fèvre, O., Maccagni, D., Małek, K., Marulli, F., Mccracken, H. J., Polletta, M., Pollo, A., Scodeggio, M., Tasca, L. A. M., Tojeiro, R., Vergani, D., Zanichelli, A., Burden, A., Di Porto, C., Marchetti, A., Marinoni, C., Mellier, Y., Moutard, T., Moscardini, L., Nichol, R. C., Peacock, J. A., Percival, W. J., and Zamorani, G.

Subjects
methods: statistical, large-scale structure of Universe, cosmology: observations, galaxies: statistics, cosmological parameters, methods: data analysis, observations, galaxies: statistics, cosmological parameters, methods: statistical, methods: data analysis [large-scale structure of Universe, cosmology], Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

Aims: Using the VIMOS Public Extragalactic Redshift Survey (VIPERS) we aim to jointly estimate the keyparameters that describe the galaxy density field and its spatial correlations in redshift space. Methods: We use the Bayesian formalism to jointly reconstruct the redshift-space galaxy density field, power spectrum, galaxy bias and galaxy luminosity function given the observations and survey selection function. The high-dimensional posterior distribution is explored using the Wiener filter within a Gibbs sampler. We validate the analysis using simulated catalogues and apply it to VIPERS data taking into consideration the inhomogeneous selection function. Results: We present joint constraints on the anisotropic power spectrum, and the bias and number density of red and blue galaxy classes in luminosity and redshift bins as well as the measurement covariances of these quantities. We find that the inferred galaxy bias and number density parameters are strongly correlated although they are only weakly correlated with the galaxy power spectrum. The power spectrum and redshift-space distortion parameters are in agreement with previous VIPERS results with the value of the growth rate fσ8 = 0.38 with 18% uncertainty at redshift 0.7.

Published
2015

23. VizieR Online Data Catalog: COSMOS photometric redshift catalog (Ilbert+, 2009)

Author

Ilbert, O., Capak, P., Salvato, M., Aussel, H., Mccracken, H. J., Sanders, D. B., Scoville, N., Kartaltepe, J., Arnouts, S., Le Floc H, E., Mobasher, B., Taniguchi, Y., Lamareille, F., Leauthaud, A., Sasaki, S., Thompson, D., Zamojski, M., Zamorani, G., Bardelli, S., Bolzonella, M., Angela Bongiorno, Brusa, M., Caputi, K. I., Carollo, C. M., Contini, T., Cook, R., Coppa, G., Cucciati, O., La Torre, S., Ravel, L., Franzetti, P., Garilli, B., Hasinger, G., Iovino, A., Kampczyk, P., Kneib, J. -P, Knobel, C., Kovac, K., Le Borgne, J. F., Le Brun, V., Fevre, O. L., Lilly, S., Looper, D., Maier, C., Mainieri, V., Mellier, Y., Mignoli, M., Murayama, T., Pello, R., Peng, Y., Perez-Montero, E., Renzini, A., Ricciardelli, E., Schiminovich, D., Scodeggio, M., Shioya, Y., Silverman, J., Surace, J., Tanaka, M., Tasca, L., Tresse, L., Vergani, D., Zucca, E., Laboratoire d'Astrophysique de Marseille (LAM), and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Photometry, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Redshifts, Surveys, Galaxy catalogs
Published
2017

24. The VIMOS Public Extragalactic Redshift Survey (VIPERS): The growth of structure at 0.5 < z < 1.2 from redshift-space distortions in the clustering of the PDR-2 final sample

Author

Pezzotta , A., De La Torre , S., Bel , J., Granett , B.R., Guzzo , L., Peacock , J.A., Garilli , B., Scodeggio , M., Bolzonella , M., Abbas , U., Adami , C., Bottini , D., Cappi , A., Cucciati , O., Davidzon , I., Franzetti , P., Fritz , A., Iovino , A., Krywult , J., Le Brun , V., Fèvre , O., Maccagni , D., Małek , K., Marulli , F., Polletta , M., Pollo , A., Tasca , L.A.M., Tojeiro , R., Vergani , D., Zanichelli , A., Arnouts , S., Branchini , E., Coupon , J., De Lucia , G., Koda , J., Ilbert , O., Moutard , T., Moscardini , L., Laboratoire d'Astrophysique de Marseille ( LAM ), Aix Marseille Université ( AMU ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National d'Etudes Spatiales ( CNES ) -Centre National de la Recherche Scientifique ( CNRS ), Centre de Physique Théorique - UMR 7332 ( CPT ), Aix Marseille Université ( AMU ) -Université de Toulon ( UTLN ) -Centre National de la Recherche Scientifique ( CNRS ), Joseph Louis LAGRANGE ( LAGRANGE ), Université Nice Sophia Antipolis ( UNS ), Université Côte d'Azur ( UCA ) -Université Côte d'Azur ( UCA ) -Observatoire de la Côte d'Azur, Université Côte d'Azur ( UCA ) -Centre National de la Recherche Scientifique ( CNRS ), Université de la Méditerranée - Aix-Marseille 2, Institut de recherche en astrophysique et planétologie ( IRAP ), and Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS )

Subjects
galaxies: high-redshift, cosmology: observations, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], large-scale structure of Universe, galaxies: statistics
Abstract

International audience; We present measurements of the growth rate of cosmological structure from the modelling of the anisotropic galaxy clustering measured in the final data release of the VIPERS survey. The analysis is carried out in configuration space and based on measurements of the first two even multipole moments of the anisotropic galaxy auto-correlation function, in two redshift bins spanning the range 0.5

Published
2017
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25. The VIMOS Public Extragalactic Redshift Survey (VIPERS) Omega(m0) from the galaxy clustering ratio measured at z similar to 1

Author

Bel J., Marinoni C., Granett B. R., Guzzo L., Peacock J. A., Cucciati O., de la Torre S., Iovino A., Percival W. J., Steigerwald H., Abbas U., Adami C., Arnouts S., Bolzonella M., Bottini D., Cappi A., Coupon J., Davidzon I., De Lucia G., Fritz A., Franzetti P., Fumana M., Garilli B., Ilbert O., Krywult J., Le Brun V., Le Fevre O., Maccagni D., Malek K., Marulli F., McCracken H. J., Paioro L., Polletta M., Pollo A., Schlagenhaufer H., Scodeggio M., Tasca L. A. M., Tojeiro R., Vergani D., Zanichelli A., Burden A., Di Porto C., Marchetti A., Mellier Y., Moscardini L., Nichol R. C., Phleps S., Wolk M., Zamorani G., BRANCHINI, ENZO FRANCO, Bel, J., Marinoni, C., Granett, B. R., Guzzo, L., Peacock, J. A., Branchini, ENZO FRANCO, Cucciati, O., de la Torre, S., Iovino, A., Percival, W. J., Steigerwald, H., Abbas, U., Adami, C., Arnouts, S., Bolzonella, M., Bottini, D., Cappi, A., Coupon, J., Davidzon, I., De Lucia, G., Fritz, A., Franzetti, P., Fumana, M., Garilli, B., Ilbert, O., Krywult, J., Le Brun, V., Le Fevre, O., Maccagni, D., Malek, K., Marulli, F., Mccracken, H. J., Paioro, L., Polletta, M., Pollo, A., Schlagenhaufer, H., Scodeggio, M., Tasca, L. A. M., Tojeiro, R., Vergani, D., Zanichelli, A., Burden, A., Di Porto, C., Marchetti, A., Mellier, Y., Moscardini, L., Nichol, R. C., Phleps, S., Wolk, M., and Zamorani, G.

Published
2014

26. Measuring Large-Scale Structure atz∼ 1 with the VIPERS galaxy survey

Author

GUZZO, Luigi, Abbas, U., Adami, Christophe, Arnouts, Stephane, Bel, Julien, Bolzonella, M., Bottini, D., Branchini, Enzo Franco, Burden, Angela, Cappi, A., Coupon, Jean, Cucciati, O., Davidzon, Iary, de la Torre, Silvain, De Lucia, G., Di Porto, Cinzia, Franzetti, P., Fritz, Alexander, Fumana, M., GARILLI, BIANCA MARIA ROSA, Granett, B. R., Guennou, L., Hawken, A., Ilbert, O., Iovino, A., Krywult, J., Le Brun, V., Le Fevre, O., Maccagni, D., Malek, K., Marchetti, A., Marinoni, C., Marulli, F., McCracken, H. J., Mellier, Y., Moscardini, L., Nichol, R. C., Paioro, L., Peacock, J. A., Percival, W. J., Phleps, S., POLLETTA, MARIA DEL CARMEN, Pollo, A., Rota, S., Schlagenhaufer, H., SCODEGGIO, MARCO, Solarz, A., Tasca, L. A. M., Tojeiro, R., VERGANI, DANIELA, Wolk, M., Zamorani, G., and ZANICHELLI, Alessandra

Subjects
Physics, Space and Planetary Science, Scale structure, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics, Galaxy
Abstract

The VIMOS Public Extragalactic Redshift Survey (VIPERS) is the largest redshift survey ever conducted with the ESO telescopes. It has used the Very Large Telescope to collect nearly 100,000 redshifts from the general galaxy population at 0.5

Published
2016

27. The evolving star formation rate: M-star relation and sSFR since z similar or equal to 5 from the VUDS spectroscopic survey

Author

Tasca, L. A. M., Le Fevre, O., Hathi, N. P., Schaerer, D., Ilbert, O., Zamorani, G., Lemaux, B. C., Cassata, P., Garilli, B., Le Brun, V., Maccagni, D., Pentericci, L., Thomas, R., Vanzella, E., Zucca, E., Amorín, R., Bardelli, S., Cassara, L. P., Castellano, M., Cimatti, Alessandro, Cucciati, O., Durkalec, A., Fontana, A., Giavalisco, M., Grazian, A., Paltani, S., Ribeiro, B., Scodeggio, M., Sommariva, V., Talia, M., Tresse, L., Vergani, D., Capak, P., Charlot, S., Contini, T., Torre, S., Dunlop, J., Fotopoulou, S., Koekemoer, A., Lopez-Sanjuan, C., Mellier, Y., Pforr, J., Salvato, M., Scoville, N., Taniguchi, Y., Wang, P. W., Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Istituto Nazionale di Astrofisica (INAF), INAF - Osservatorio Astronomico di Roma (OAR), Oncology Institute of Southern Switzerland, INAF - Osservatorio Astronomico di Bologna (OABO), University of Bologna/Università di Bologna, Department of Astronomy [Amherst], University of Massachusetts [Amherst] (UMass Amherst), University of Massachusetts System (UMASS)-University of Massachusetts System (UMASS), ISDC Data Centre for Astrophysics, Université de Genève = University of Geneva (UNIGE), INAF- Milano, INAF - Osservatorio Astrofisico di Arcetri (OAA), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), SUPA, Institute for Astronomy, University of Edinburgh, Aristotle University of Thessaloniki, Space Telescope Science Institute (STSci), Institute of cosmology and gravitation, University of Portsmouth, Max-Planck-Institut für Extraterrestrische Physik (MPE), Excellence Cluster Universe, excellence cluster centre, California Institute of Technology (CALTECH), European Project: 268107,EC:FP7:ERC,ERC-2010-AdG_20100224,EARLY(2011), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), University of Bologna, and University of Geneva [Switzerland]

Subjects
Galaxies: star formation, Galaxies: high-redshift, Galaxies: evolution, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxies: formation, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics
Abstract

International audience; We study the evolution of the star formation rate (SFR) - stellar mass (M-star) relation and specific star formation rate (sSFR) of star-forming galaxies (SFGs) since a redshift z similar or equal to 5.5 using 2435 (4531) galaxies with highly reliable spectroscopic redshifts in the VIMOS Ultra-Deep Survey (VUDS). It is the first time that these relations can be followed over such a large redshift range from a single homogeneously selected sample of galaxies with spectroscopic redshifts. The log(SFR) - log(M-star) relation for SFGs remains roughly linear all the way up to z = 5, but the SFR steadily increases at fixed mass with increasing redshift. We find that for stellar masses M-star \textgreater= 3.2 x 10(9) M-circle dot the SFR increases by a factor of similar to 13 between z = 0.4 and z = 2.3. We extend this relation up to z = 5, finding an additional increase in SFR by a factor of 1.7 from z = 2.3 to z = 4.8 for masses M-star = 1010 M-circle dot. We observe a turn-off in the SFR-M-star relation at the highest mass end up to a redshift z similar to 3.5. We interpret this turn-off as the signature of a strong on-going quenching mechanism and rapid mass growth. The sSFR increases strongly up to z similar to 2, but it grows much less rapidly in 2 \textless z \textless 5. We find that the shape of the sSFR evolution is not well reproduced by cold gas accretion-driven models or the latest hydrodynamical models. Below z similar to 2 these models have a flatter evolution (1+z)(Phi) with Phi = 2-2.25 compared to the data which evolves more rapidly with Phi = 2.8 +/- 0.2. Above z similar to 2, the reverse is happening with the data evolving more slowly with Phi = 1.2 +/- 0.1. The observed sSFR evolution over a large redshift range 0 \textless z \textless 5 and our finding of a non-linear main sequence at high mass both indicate that the evolution of SFR and M-star is not solely driven by gas accretion. The results presented in this paper emphasize the need to invoke a more complex mix of physical processes including major and minor merging to further understand the co-evolution of the SFR and stellar mass growth.

Published
2015
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28. Extreme emission-line galaxies out to z similar to 1 in zCOSMOS I. Sample and characterization of global properties

Author

Amorin, R., Perez-Montero, F., Contini, T., Vilchez, J. M., Bolzonella, M., Tasca, L. A. M., Lamareille, F., Zamorani, G., Maier, C., Carollo, C. M., Kneib, J. -P., Le Fevre, O., Lilly, S., Mainieri, V., Renzinis, A., Scodeggio, M., Bardelli, S., Bongiorno, A., Caputi, K., Cucciati, O., de la Torre, S., de Ravel, L., Franzetti, P., Garilli, B., Iovino, A., Kampczyk, P., Knobel, C., Kovac, K., Le Borgne, J. -F., Le Brun, V., Mignoli, M., Pello, R., Peng, Y., Presotto, V., Ricciardelli, E., Silverman, J. D., Tanaka, M., Tresse, L., Vergani, D., Zucca, E., and Kapteyn Astronomical Institute

Subjects
ACTIVE GALACTIC NUCLEI, galaxies: irregular galaxies: star formation, ULTRA DEEP FIELD, METAL-POOR GALAXIES, galaxies: fundamental parameters, galaxies: starburst, Astrophysics::Cosmology and Extragalactic Astrophysics, LYMAN BREAK GALAXIES, LY-ALPHA EMITTERS, LUMINOSITY-METALLICITY RELATION, COMPACT DWARF GALAXIES, STAR-FORMING GALAXIES, Astrophysics::Solar and Stellar Astrophysics, DIGITAL SKY SURVEY, galaxies: abundances, Astrophysics::Earth and Planetary Astrophysics, GREEN PEA GALAXIES, galaxies: evolution, Astrophysics::Galaxy Astrophysics
Abstract

Context. The study of large and representative samples of low-metallicity star-forming galaxies at different cosmic epochs is of great interest to the detailed understanding of the assembly history and evolution of low-mass galaxies. Aims. We present a thorough characterization of a large sample of 183 extreme emission-line galaxies (EELGs) at redshift 0.11 Methods. We use multiwavelength COSMOS photometry, HST-ACS I-band imaging, and optical zCOSMOS spectroscopy to derive the main global properties of star-forming EELGs, such as sizes, stellar masses, star formation rates (SFR), and reliable oxygen abundances using both "direct" and "strong-line" methods. Results. The EELGs are extremely compact (r(50) similar to 1.3 kpc), low-mass (M-* similar to 10(7)-10(10) M-circle dot) galaxies forming stars at unusually high specific star formation rates (sSFR equivalent to SFR/M-star up to 10(-7) yr(-1)) compared to main sequence star-forming galaxies of the same stellar mass and redshift. At rest-frame UV wavelengths, the EELGs are luminous and show high surface brightness and include strong Ly alpha emitters, as revealed by GALEX spectroscopy. We show that zCOSMOS EELGs are high-ionization, low-metallicity systems, with median 12+log(O/H) = 8.16 +/- 0.21 (0.2 Z(circle dot)) including a handful of extremely metal-deficient ( Conclusions. The zCOSMOS EELGs are galaxies caught in a transient and probably early period of their evolution, where they are efficiently building up a significant fraction of their present-day stellar mass in an ongoing, galaxy-wide starburst. Therefore, the EELGs constitute an ideal benchmark for comparison studies between low- and high-redshift low-mass star-forming galaxies.

Published
2015

29. Stellar mass to halo mass relation from galaxy clustering in VUDS: a high star formation efficiency at z similar or equal to 3

Author

Durkalec, A., Le Fevre, O., Torre, S., Pollo, A., Cassata, P., Garilli, B., Le Brun, V., Lemaux, B. C., Maccagni, D., Pentericci, L., Tasca, L. A. M., Thomas, R., Vanzella, E., Zamorani, G., Zucca, E., Amorín, R., Bardelli, S., Cassara, L. P., Castellano, M., Cimatti, Alessandro, Cucciati, O., Fontana, A., Giavalisco, M., Grazian, A., Hathi, N. P., Ilbert, O., Paltani, S., Ribeiro, B., Schaerer, D., Scodeggio, M., Sommariva, V., Talia, M., Tresse, L., Vereani, D., Capak, P., Charlot, S., Contini, T., Cuby, J. G., Dunlop, J., Fotopoulou, S., Koekemoer, A., Lopez-Sanjuan, C., Mellier, Y., Pforr, J., Salvato, M., Scoville, N., Taniguchi, Y., Wang, P. W., Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Roma (OAR), Istituto Nazionale di Astrofisica (INAF), Oncology Institute of Southern Switzerland, INAF - Osservatorio Astronomico di Bologna (OABO), University of Bologna/Università di Bologna, Department of Astronomy [Amherst], University of Massachusetts [Amherst] (UMass Amherst), University of Massachusetts System (UMASS)-University of Massachusetts System (UMASS), ISDC Data Centre for Astrophysics, Université de Genève = University of Geneva (UNIGE), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), INAF- Milano, Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), SUPA, Institute for Astronomy, University of Edinburgh, Aristotle University of Thessaloniki, Space Telescope Science Institute (STSci), Max-Planck-Institut für Extraterrestrische Physik (MPE), Excellence Cluster Universe, excellence cluster centre, California Institute of Technology (CALTECH), ANR-11-IDEX-0001,Amidex,INITIATIVE D'EXCELLENCE AIX MARSEILLE UNIVERSITE(2011), European Project: 268107,EC:FP7:ERC,ERC-2010-AdG_20100224,EARLY(2011), University of Bologna, University of Geneva [Switzerland], Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), and Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Large-scale structure of Universe, Astrophysics::Solar and Stellar Astrophysics, Galaxies: evolution, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Early Universe, Astrophysics::Galaxy Astrophysics, Methods: statistical
Abstract

International audience; The relation between the galaxy stellar mass M-star and the dark matter halo mass M-h gives important information on the efficiency in forming stars and assembling stellar mass in galaxies. We present measurements of the ratio of stellar mass to halo mass (SMHR) at redshifts 2 \textless z \textless 5, obtained from the VIMOS Ultra Deep Survey. We use halo occupation distribution (HOD) modelling of clustering measurements on similar to 3000 galaxies with spectroscopic redshifts to derive the dark matter halo mass M-h, and spectral energy density fitting over a large set of multi-wavelength data to derive the stellar mass M-star and compute the SMHR = M-star/M-h. We find that the SMHR ranges from 1% to 2.5% for galaxies with M-star = 1.3 x 10(9) M-star to M-star = 7.4 x 10(9) M-circle dot in DM halos with M-h = 1.3 x 10(11) M-circle dot to M-h = 3 x 10(11) M-circle dot. We derive the integrated star formation efficiency (ISFE) of these galaxies and find that the star formation efficiency is a moderate 6-9% for lower mass galaxies, while it is relatively high at 16% for galaxies with the median stellar mass of the sample similar to 7 x 10(9) M-circle dot. The lower ISFE at lower masses may indicate that some efficient means of suppressing star formation is at work (like SNe feedback), while the high ISFE for the average galaxy at z similar to 3 indicates that these galaxies efficiently build up their stellar mass at a key epoch in the mass assembly process. Based on our results, we propose a possible scenario in which the average massive galaxy at z similar to 3 begins to experience truncation of its star formation within a few million years.

Published
2015
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30. Obscured AGN at 1.5 < z < 3.0 from the zCOSMOS-deep Survey: I. Properties of the emitting gas in the narrow-line region.

Author

Mignoli, M., Feltre, A., Bongiorno, A., Calura, F., Gilli, R., Vignali, C., Zamorani, G., Lilly, S. J., Le Fèvre, O., Bardelli, S., Bolzonella, M., Bordoloi, R., Le Brun, V., Caputi, K. I., Cimatti, A., Diener, C., Garilli, B., Koekemoer, A. M., Maier, C., and Mainieri, V.

Subjects
SEYFERT galaxies, STELLAR mass, ACTIVE galactic nuclei, IONIZED gases, GAS distribution, GALAXY spectra
Abstract

Context. The physics and demographics of high-redshift obscured active galactic nuclei (AGN) is still scarcely investigated. New samples of such objects, selected with different techniques, can provide useful insights into their physical properties. Aims. With the goal to determine the properties of the gas in the emitting region of type 2 AGN, in particular, the gas metal content, we exploit predictions from photoionization models, including new parameterizations for the distance of gas distribution from the central source and internal microturbulence in the emitting clouds, to interpret rest-frame UV spectral data. Methods. We selected a sample of 90 obscured (type 2) AGN with 1.45 ≤ z ≤ 3.05 from the zCOSMOS-deep galaxy sample by 5σ detection of the high-ionization C IVλ1549 narrow emission line. This feature in a galaxy spectrum is often associated with nuclear activity, and the selection effectiveness has also been confirmed by diagnostic diagrams based on utraviolet (UV) emission-line ratios. We applied the same selection technique and collected a sample of 102 unobscured (type 1) AGN. Taking advantage of the large amount of multiband data available in the COSMOS field, we investigated the properties of the C IV-selected type 2 AGN, focusing on their host galaxies, X-ray emission, and UV emission lines. Finally, we investigated the physical properties of the ionized gas in the narrow-line region (NLR) of this type 2 AGN sample by combining the analysis of strong UV emission lines with predictions from photoionization models. Results. We find that in order to successfully reproduce the relative intensity of UV emission lines of the selected high-z type 2 AGN, two new ingredients in the photoionization models are fundamental: small inner radii of the NLR (≈90 pc for LAGN = 1045 erg s−1), and the internal dissipative microturbulence of the gas-emitting clouds (with vmicr ≈ 100 km s−1). With these modified models, we compute the gas-phase metallicity of the NLR, and our measurements indicate a statistically significant evolution of the metal content with redshift. Finally, we do not observe a strong relationship between the NLR gas metallicity and the stellar mass of the host galaxy in our C IV-selected type 2 AGN sample. [ABSTRACT FROM AUTHOR]

Published
2019
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31. The COSMOS Density Field: A Reconstruction Using Both Weak Lensing and Galaxy Distributions

Author

Amara, A., Lilly, S., Kovac, K., Rhodes, J., Massey, R., Zamorani, G., Carollo, C. M., Contini, T., Kneib, J-P, Le Fevre, O., Mainieri, V., Renzini, A., Scodeggio, M., Bardelli, S., Bolzonella, M., Bongiorno, A., Caputi, K., Cucciati, O., Torre, S., Ravel, L., Franzetti, P., Garilli, B., Iovino, A., Kampczyk, P., Knobel, C., Lamareille, F., Le Borgne, J-F, Le Brun, V., Maier, C., Mignoli, M., Pello, R., Peng, Y., Perez Montero, E., Presotto, V., Silverman, J., Tanaka, M., Tasca, L., Tresse, L., Vergani, D., Zucca, E., BARNES, L., Bordoloi, R., Cappi, A., Cimatti, Alessandro, Coppa, G., Koekoemoer, A., Lopez-Sanjuan, C., McCracken, H. J., Moresco, M., Nair, P., Pozzetti, L., Welikala, N., Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Amara A., Lilly S., Kovač K., Rhodes J., Massey R., Zamorani G., Carollo C. M., Contini T., Kneib J.-P., Le Fevre O., Mainieri V., Renzini A., Scodeggio M., Bardelli S., Bolzonella M., Bongiorno A., Caputi K., Cucciati O., de la Torre S., de Ravel L., Franzetti P., Garilli B., Iovino A., Kampczyk P., Knobel C., Lamareille F., Le Borgne J.-F., Le Brun V., Maier C., Mignoli M., Pello R., Peng Y., Montero E. Perez, Presotto V., Silverman J., Tanaka M., Tasca L., Tresse L., Vergani D., Zucca E., Barnes L., Bordoloi R., Cappi A., Cimatti A., Coppa G., Koekoemoer A., López-Sanjuan C., McCracken H. J., Moresco M., Nair P., Pozzetti L., Welikala N., Astronomy, and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)

Subjects
SAMPLE, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], DEEP, DATA RELEASE, FOS: Physical sciences, HUBBLE-SPACE-TELESCOPE, Astrophysics::Cosmology and Extragalactic Astrophysics, dark matter, ADVANCED CAMERA, Large-scale structure of Universe, LARGE-SCALE STRUCTURE, DARK-MATTER, Dark matter, DIGITAL SKY SURVEY, dark matter, large-scale structure of Universe, large-scale structure of Universe, CLUSTERS, ZCOSMOS GALAXIES, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The COSMOS field has been the subject of a wide range of observations, with a number of studies focusing on reconstructing the 3D dark matter density field. Typically, these studies have focused on one given method or tracer. In this paper, we reconstruct the distribution of mass in the COSMOS field out to a redshift z=1 by combining Hubble Space Telescope weak lensing measurements with zCOSMOS spectroscopic measurements of galaxy clustering. The distribution of galaxies traces the distribution of mass with high resolution (particularly in redshift, which is not possible with lensing), and the lensing data empirically calibrates the mass normalisation (bypassing the need for theoretical models). Two steps are needed to convert a galaxy survey into a density field. The first step is to create a smooth field from the galaxy positions, which is a point field. We investigate four possible methods for this: (i) Gaussian smoothing, (ii) convolution with truncated isothermal sphere, (iii) fifth nearest neighbour smoothing and (iv) a muliti-scale entropy method. The second step is to rescale this density field using a bias prescription. We calculate the optimal bias scaling for each method by comparing predictions from the smoothed density field with the measured weak lensing data, on a galaxy-by-galaxy basis. In general, we find scale-independent bias for all the smoothing schemes, to a precision of 10%. For the nearest neighbour smoothing case, we find the bias to be 2.51\pm 0.25. We also find evidence for a strongly evolving bias, increasing by a factor of ~3.5 between redshifts 0, Comment: Accepted by MNRAS. 12 pages with 6 Figures

Published
2012
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32. The Nonlinear Biasing of the zCOSMOS Galaxies up to z ~ 1 from the 10k Sample

Author

Kova, #269, Porciani C., Lilly S. J., Marinoni C., Guzzo L., Zamorani G., Iovino A., Oesch P., Bolzonella M., Peng Y., Meneux B., Zucca E., Bardelli S., Carollo C. M., Contini T., Kneib J. P., Le Fèvre O., Mainieri V., Renzini A., Scodeggio M., Bongiorno A., Caputi K., Coppa G., de la Torre S., de Ravel L., Finoguenov A., Franzetti P., Garilli B., Kampczyk P., Knobel C., Lamareille F., Le Borgne J. F., Le Brun V., Maier C., Mignoli M., Pello R., Perez Montero E., Pozzetti L., Ricciardelli E., Silverman J. D., Tanaka M., Tasca L. A. M., Tresse L., Vergani D., Abbas U., Bottini D., Cappi A., Cassata P., Fumana M., Koekemoer A. M., Leauthaud A., Maccagni D., McCracken H. J., Memeo P., Scaramella R., Scoville N. Z., CUCCIATI, OLGA, CIMATTI, ANDREA, Kova&#269, K., Porciani C., Lilly S. J., Marinoni C., Guzzo L., Cucciati O., Zamorani G., Iovino A., Oesch P., Bolzonella M., Peng Y., Meneux B., Zucca E., Bardelli S., Carollo C. M., Contini T., Kneib J.-P., Le Fèvre O., Mainieri V., Renzini A., Scodeggio M., Bongiorno A., Caputi K., Coppa G., de la Torre S., de Ravel L., Finoguenov A., Franzetti P., Garilli B., Kampczyk P., Knobel C., Lamareille F., Le Borgne J.-F., Le Brun V., Maier C., Mignoli M., Pello R., Perez-Montero E., Pozzetti L., Ricciardelli E., Silverman J. D., Tanaka M., Tasca L. A. M., Tresse L., Vergani D., Abbas U., Bottini D., Cappi A., Cassata P., Cimatti A., Fumana M., Koekemoer A. M., Leauthaud A., Maccagni D., McCracken H. J., Memeo P., Scaramella R., and Scoville N. Z.

Subjects
Physics, cosmology: observation, Field (physics), 010308 nuclear & particles physics, Dark matter, Astronomy and Astrophysics, Biasing, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Redshift, Galaxy, Luminosity, Space and Planetary Science, cosmology: observations, 0103 physical sciences, Halo effect, galaxies: evolution, galaxies: statistics, 010303 astronomy & astrophysics, Smoothing, Astrophysics::Galaxy Astrophysics
Abstract

We use the zCOSMOS galaxy overdensity field to study the biasing of galaxies in the COSMOS field. By comparing the probability distribution function of the galaxy density contrast δ g to the lognormal approximation of the mass density contrast δ, we obtain the mean biasing function b(δ, z, R) between the galaxy and matter overdensity fields and its second moments \hat{b} and \tilde{b}. Over the redshift interval 0.4 < z < 1 the conditional mean function langδ g |δrang = b(δ, z, R)δ is of a characteristic shape, requiring nonlinear biasing in the most overdense and underdense regions. Taking into account the uncertainties due to cosmic variance, we do not detect any significant evolution in the langδ g |δrang function, but we do detect a significant redshift evolution in the linear biasing parameter \hat{b} from 1.23 ± 0.11 at z ~ 0.55 to 1.62 ± 0.14 at z ~ 0.75, for a luminosity-complete sample of MB < -20 - z galaxies. The \hat{b} parameter does not change significantly with smoothing scale between 8 and 12 h -1 Mpc, but increases systematically with luminosity (at 2σ-3σ significance between the MB < -20.5 - z and MB < -20 - z samples). The nonlinearity parameter \tilde{b}/ \hat{b} is offset from unity by at most 2%, with an uncertainty of the same order. The \tilde{b}/\hat{b} parameter does not show any significant redshift evolution, dependence on the smoothing scale or on the luminosity. By matching the linear bias of galaxies to the halo bias, we infer that the MB < -20 - z galaxies reside in dark matter halos with a characteristic mass of about (2.6 - 5.6) × 1012 M sun with a small dependence on the adopted bias-mass relation. Our detailed error analysis and comparison with previous studies lead us to conclude that cosmic variance is the main contributor to the differences in the linear bias measured from different surveys. While our results support the general picture of biased galaxy formation up to z ~ 1, the fine-tuning of the galaxy formation models is still limited by the restrictions of the current spectroscopic surveys at these redshifts.

Published
2011

33. The zCOSMOS-Bright survey: the clustering of early and late galaxy morphological types since z≃ 1

Author

de la Torre S., Le Fèvre O., Porciani C., Guzzo L., Meneux B., Abbas U., Tasca L., Carollo C. M., Contini T., Kneib J. P., Lilly S. J., Mainieri V., Renzini A., Scodeggio M., Zamorani G., Bardelli S., Bolzonella M., Bongiorno A., Caputi K., Coppa G., de Ravel L., Franzetti P., Garilli B., Halliday C., Iovino A., Kampczyk P., Knobel C., Koekemoer A. M., Kova, #269, Lamareille F., Le Borgne J. F., Le Brun V., Maier C., Mignoli M., Pelló R., Peng Y., Perez Montero E., Ricciardelli E., Silverman J., Tanaka M., Tresse L., Vergani D., Zucca E., Bottini D., Cappi A., Cassata P., Leauthaud A., Maccagni D., Marinoni C., McCracken H. J., Memeo P., Oesch P., Pozzetti L., Scaramella R., CUCCIATI, OLGA, CIMATTI, ANDREA, de la Torre S., Le Fèvre O., Porciani C., Guzzo L., Meneux B., Abbas U., Tasca L., Carollo C. M., Contini T., Kneib J.-P., Lilly S. J., Mainieri V., Renzini A., Scodeggio M., Zamorani G., Bardelli S., Bolzonella M., Bongiorno A., Caputi K., Coppa G., Cucciati O., de Ravel L., Franzetti P., Garilli B., Halliday C., Iovino A., Kampczyk P., Knobel C., Koekemoer A. M., Kova&#269, K., Lamareille F., Le Borgne J.-F., Le Brun V., Maier C., Mignoli M., Pelló R., Peng Y., Perez-Montero E., Ricciardelli E., Silverman J., Tanaka M., Tresse L., Vergani D., Zucca E., Bottini D., Cappi A., Cassata P., Cimatti A., Leauthaud A., Maccagni D., Marinoni C., McCracken H. J., Memeo P., Oesch P., Pozzetti L., and Scaramella R.

Subjects
cosmology: observation, galaxies: high-redshift, galaxies: statistic, Astrophysics::Cosmology and Extragalactic Astrophysics, large-scale structure of Universe, galaxies: evolution, Astrophysics::Galaxy Astrophysics
Abstract

We measure the spatial clustering of galaxies as a function of their morphological type at z≃ 0.8, for the first time in a deep redshift survey with full morphological information. This is obtained by combining high-resolution Hubble Space Telescope imaging and Very Large Telescope spectroscopy for about 8500 galaxies to ? with accurate spectroscopic redshifts from the zCOSMOS-Bright redshift survey. At this epoch, early-type galaxies already show a significantly stronger clustering than late-type galaxies on all probed scales. A comparison to the Sloan Digital Sky Survey Data at z≃ 0.1 shows that the relative clustering strength between early and late morphological classes tends to increase with cosmic time at small separations, while on large scales it shows no significant evolution since z≃ 0.8. This suggests that most early-type galaxies had already formed in intermediate and dense environments at this epoch. Our results are consistent with a picture in which the relative clustering of different morphological types between z≃ 1 and 0 reflects the evolving role of environment in the morphological transformation of galaxies, on top of a global evolution driven by mass.

Published
2011

34. The evolution of quiescent galaxies at high redshifts (z≥ 1.4)

Author

Domínguez Sánchez H., Gruppioni C., Ilbert O., Pozzetti L., McCracken H., Capak P., Le Floch E., Salvato M., Zamorani G., Carollo C. M., Contini T., Kneib J. P., Le Fèvre O., Lilly S. J., Mainieri V., Renzini A., Scodeggio M., Bardelli S., Bolzonella M., Bongiorno A., Caputi K., Coppa G., de la Torre S., de Ravel L., Franzetti P., Garilli B., Iovino A., Kampczyk P., Knobel C., Kova, #269, Lamareille F., Le Borgne J. F., Le Brun V., Maier C., Mignoli M., Pelló R., Peng Y., Perez Montero E., Ricciardelli E., Silverman J. D., Tanaka M., Tasca L. A. M., Tresse L., Vergani D., Zucca E., POZZI, FRANCESCA, CIMATTI, ANDREA, CUCCIATI, OLGA, Domínguez Sánchez H., Pozzi F., Gruppioni C., Cimatti A., Ilbert O., Pozzetti L., McCracken H., Capak P., Le Floch E., Salvato M., Zamorani G., Carollo C. M., Contini T., Kneib J.-P., Le Fèvre O., Lilly S. J., Mainieri V., Renzini A., Scodeggio M., Bardelli S., Bolzonella M., Bongiorno A., Caputi K., Coppa G., Cucciati O., de la Torre S., de Ravel L., Franzetti P., Garilli B., Iovino A., Kampczyk P., Knobel C., Kova&#269, K., Lamareille F., Le Borgne J.-F., Le Brun V., Maier C., Mignoli M., Pelló R., Peng Y., Perez-Montero E., Ricciardelli E., Silverman J. D., Tanaka M., Tasca L. A. M., Tresse L., Vergani D., and Zucca E.

Subjects
galaxies: high-redshift, galaxies: star formation, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies: evolution, Astrophysics::Galaxy Astrophysics
Abstract

The goal of this work is to study the evolution of high-redshift (z≥ 1.4) quiescent galaxies over an effective area of ˜1.7 deg2 in the COSMOS field. Galaxies have been divided according to their star formation activity and the evolution of the different populations, in particular of the quiescent galaxies, has been investigated in detail. We have studied an IRAC (mag 3.6 μm < 22.0) selected sample of ˜18 000 galaxies at z≥ 1.4 in the COSMOS field with multiwavelength coverage extending from the U band to the Spitzer 24 μm one. We have derived accurate photometric redshifts (?) through a SED-fitting procedure. Other important physical parameters [masses, ages and star formation rates (SFR)] of the galaxies have been obtained using Maraston models. We have divided our sample into actively star-forming, intermediate and quiescent galaxies depending on their specific star formation rate (SSFR = SFR/M). We have computed the galaxy stellar mass function (GSMF) of the total sample and the different populations at z= 1.4-3.0. We have studied the properties of high-redshift quiescent galaxies finding that they are old (1-4 Gyr), massive (˜ 1010.65 M⊙), weakly star-forming stellar populations with low dust extinction [E(B-V) ≤ 0.15] and small e-folding time-scales (τ˜ 0.1-0.3 Gyr). We observe a significant evolution of the quiescent stellar mass function from 2.5 < z < 3.0 to 1.4 < z < 1.6, increasing by ˜1 dex in this redshift interval. We find that z˜ 1.5 is an epoch of transition of the GSMF: while the GSMF at z≳ 1.5 is dominated by the star-forming galaxies at all stellar masses, at z≲ 1.5 the contribution to the total GSMF of the quiescent galaxies is significant and becomes higher than that of the star-forming population for M≥ 1010.75 M⊙. The fraction of star-forming galaxies decreases from 60-20 per cent from z˜ 2.5-3.0 to 1.4-1.6 for M˜ 1011.0 M⊙, while the quiescent population increases from 10-50 per cent at the same redshift and mass intervals. We compare the fraction of quiescent galaxies derived with that predicted by theoretical models and find that the Kitzbichler & White model, implemented on the Millennium Simulation, is the one that better reproduces the shape of the data. Finally, we calculate the stellar mass density of the star-forming and quiescent populations as a function of redshift and find that there is already a significant number of quiescent galaxies at z > 2.5 (logρ[M⊙ Mpc-3]˜ 6), meaning that efficient star formation had to take place before that time.

Published
2011

35. The bimodality of the 10k zCOSMOS-bright galaxies up to z ~ 1: a new statistical and portable classification based on the optical galaxy properties

Author

Coppa G., Mignoli M., Zamorani G., Bardelli S., Lilly S. J., Bolzonella M., Scodeggio M., Vergani D., Nair P., Pozzetti L., Zucca E., Carollo C. M., Contini T., Le Fèvre O., Renzini A., Mainieri V., Bongiorno A., Caputi K. I., de la Torre S., de Ravel L., Franzetti P., Garilli B., Memeo P., Iovino A., Kampczyk P., Kneib J. P., Knobel C., Koekemoer A. M., Kova, #269, Lamareille F., Le Borgne J. F., Le Brun V., Maier C., Pellò R., Peng Y., Perez Montero E., Ricciardelli E., Scarlata C., Silverman J. D., Tanaka M., Tasca L., Tresse L., Abbas U., Bottini D., Capak P., Cappi A., Cassata P., Fumana M., Guzzo L., Leauthaud A., Maccagni D., Marinoni C., Meneux B., Oesch P., Porciani C., Scaramella R., Scoville N., CIMATTI, ANDREA, CUCCIATI, OLGA, Coppa G., Mignoli M., Zamorani G., Bardelli S., Lilly S. J., Bolzonella M., Scodeggio M., Vergani D., Nair P., Pozzetti L., Cimatti A., Zucca E., Carollo C. M., Contini T., Le Fèvre O., Renzini A., Mainieri V., Bongiorno A., Caputi K. I., Cucciati O., de la Torre S., de Ravel L., Franzetti P., Garilli B., Memeo P., Iovino A., Kampczyk P., Kneib J.-P., Knobel C., Koekemoer A. M., Kova&#269, K., Lamareille F., Le Borgne J.-F., Le Brun V., Maier C., Pellò R., Peng Y., Perez-Montero E., Ricciardelli E., Scarlata C., Silverman J. D., Tanaka M., Tasca L., Tresse L., Abbas U., Bottini D., Capak P., Cappi A., Cassata P., Fumana M., Guzzo L., Leauthaud A., Maccagni D., Marinoni C., Meneux B., Oesch P., Porciani C., Scaramella R., Scoville N., Institute for Astronomy [Zürich], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), INAF - Osservatorio Astronomico di Bologna (OABO), University of Chicago, Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), European Southern Observatory (ESO), College of Computing (GATECH), Georgia Institute of Technology [Atlanta], AUTRES, Dipartimento di Fisica, Università degli Studi di Milano-Bicocca [Milano] (UNIMIB)-Università degli Studi di Milano [Milano] (UNIMI), Ecole Polytechnique Fédérale de Lausanne (EPFL), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Département Informatique pour les Systèmes Coopératifs Ouverts et Décentralisés (ISCOD-ENSMSE), École des Mines de Saint-Étienne (Mines Saint-Étienne MSE), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT)-Institut Henri Fayol, Laboratoire Léon Brillouin (LLB - UMR 12), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS)-Université Paris-Saclay, Hunan Normal University, Spitzer Science Center, California Institute of Technology (CALTECH), Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre de Physique Théorique - UMR 6207 (CPT), Centre National de la Recherche Scientifique (CNRS)-Université de Toulon (UTLN)-Université de Provence - Aix-Marseille 1-Université de la Méditerranée - Aix-Marseille 2, Astronomy, Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Milano-Bicocca = University of Milano-Bicocca (UNIMIB)-Università degli Studi di Milano = University of Milan (UNIMI), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Hunan Normal University (HNU), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), and Université de la Méditerranée - Aix-Marseille 2-Université de Provence - Aix-Marseille 1-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, STAR-FORMATION, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], MORPHOLOGICAL CLASSIFICATION, 0103 physical sciences, Range (statistics), PHOTOMETRIC REDSHIFTS, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Galaxies: evolution, Galaxies: fundamental parameters, Galaxies: general, Astronomy and Astrophysics, Space and Planetary Science, DIGITAL-SKY-SURVEY, 010308 nuclear & particles physics, FORMATION HISTORIES, HUBBLE DEEP FIELD, Order (ring theory), galaxies: fundamental parameters, ENVIRONMENTAL DEPENDENCE, Redshift survey, galaxies: general, Redshift, Galaxy, Bimodality, LUMINOSITY FUNCTION, SPECTROSCOPIC SAMPLE, STELLAR MASS FUNCTION, Cube, galaxies: evolution, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Our goal is to develop a new and reliable statistical method to classify galaxies from large surveys. We probe the reliability of the method by comparing it with a three-dimensional classification cube, using the same set of spectral, photometric and morphological parameters.We applied two different methods of classification to a sample of galaxies extracted from the zCOSMOS redshift survey, in the redshift range 0.5 < z < 1.3. The first method is the combination of three independent classification schemes, while the second method exploits an entirely new approach based on statistical analyses like Principal Component Analysis (PCA) and Unsupervised Fuzzy Partition (UFP) clustering method. The PCA+UFP method has been applied also to a lower redshift sample (z < 0.5), exploiting the same set of data but the spectral ones, replaced by the equivalent width of H$��$. The comparison between the two methods shows fairly good agreement on the definition on the two main clusters, the early-type and the late-type galaxies ones. Our PCA-UFP method of classification is robust, flexible and capable of identifying the two main populations of galaxies as well as the intermediate population. The intermediate galaxy population shows many of the properties of the green valley galaxies, and constitutes a more coherent and homogeneous population. The fairly large redshift range of the studied sample allows us to behold the downsizing effect: galaxies with masses of the order of $3\cdot 10^{10}$ Msun mainly are found in transition from the late type to the early type group at $z>0.5$, while galaxies with lower masses - of the order of $10^{10}$ Msun - are in transition at later epochs; galaxies with $M 5\cdot 10^{10}$ Msun) mostly completed their transition before $z\sim 1$., 16 pages, 14 figures, accepted for publication in A&A

Published
2010
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36. The VIMOS-VLT Deep Survey: evolution in the halo occupation number since z ~ 1

Author

Abbas, U., Torre, S., Le Fèvre, O., Guzzo, L., Marinoni, C., Meneux, B., Pollo, A., Zamorani, G., Bottini, D., Garilli, B., Le Brun, V., Maccagni, D., Scaramella, R., Scodeggio, M., Tresse, L., Vettolani, G., Zanichelli, A., Adami, C., Arnouts, S., Bardelli, S., Bolzonella, M., Cappi, A., Charlot, S., Ciliegi, P., Contini, T., Foucaud, S., Franzetti, P., Gavignaud, I., Ilbert, O., Iovino, A., Lamareille, F., Mccracken, H.~j., Marano, B., Mazure, A., Merighi, R., Paltani, S., Pellò, R., Pozzetti, L., Radovich, M., Vergani, D., Zucca, E., Bondi, M., Bongiorno, A., Brinchmann, J., Cucciati, O., Ravel, L., Gregorini, L., Perez-Montero, E., Mellier, Y., Merluzzi, P., Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Abbas U., de la Torre S., Le Fèvre O., Guzzo L., Marinoni C., Meneux B., Pollo A., Zamorani G., Bottini D., Garilli B., and Le brun V., Maccagni D., Scaramella R., Scodeggio M., Tresse L., Vettolani G., Zanichelli A., Adami C., Arnouts S., Bardelli S., Bolzonella M., Cappi A., Charlot S., Ciliegi P., Contini T., Foucaud S., Franzetti P., Gavignaud I., Ilbert O., Iovini A., Lamareille F., McCracken H.J., Marano B., Mazure A., Merighi R., Paltani S., Pello' R., Pozzetti L., Radovich M., Vergani D., Zucca E., Bondi M., Bongiorno A., Brinchmann ., Cucciati P., de Ravel L., Gregorini L., Perez-Montero E., Mellier Y., Merluzzi P.

Subjects
methods: statistical, surveys, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], galaxies: high-redshift, [INFO]Computer Science [cs], Astrophysics::Cosmology and Extragalactic Astrophysics, LARGE-SCALE STRUCTURE OF NIVERSE, large-scale structure of Universe, GALAXIES:HIGH-REDSHIFT, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, METHOD: STATISTICAL
Abstract

We model the evolution of the mean galaxy occupation of dark matter haloes over the range 0.1 < z < 1.3, using the data from the VIMOS-VLT Deep Survey. The galaxy projected correlation function wp(rp) was computed for a set of luminosity-limited subsamples and fits to its shape were obtained using two variants of halo occupation distribution (HOD) models. These provide us with a set of best-fitting parameters, from which we obtain the average mass of a halo and average number of galaxies per halo. We find that after accounting for the evolution in luminosity and assuming that we are largely following the same population, the underlying dark matter halo shows a growth in mass with decreasing redshift as expected in a hierarchical structure formation scenario. Using two different HOD models, we see that the halo mass grows by 90 per cent over the redshift interval z = [0.5, 1.0]. This is the first time the evolution in halo mass at high redshifts has been obtained from a single data survey and it follows the simple form seen in N-body simulations with M(z) = M0 e-βz, and β = 1.3 +/- 0.30. This provides evidence for a rapid accretion phase of massive haloes having a present-day mass M0 ~ 1013.5 h-1 Msolar, with a m > 0.1 M0 merger event occurring between redshifts of 0.5 and 1.0. Furthermore, we find that more luminous galaxies are found to occupy more massive haloes irrespective of the redshift. Finally, the average number of galaxies per halo shows little increase from redshift z ~ 1.0 to ~0.5, with a sharp increase by a factor of ~3 from z ~ 0.5 to ~0.1, likely due to the dynamical friction of subhaloes within their host haloes. Based on data obtained with the European Southern Observatory Very Large Telescope, Paranal, Chile, program 070.A-9007(A), and on data obtained at the Canada-France-Hawaii Telescope, operated by the CNRS of France, CNRC in Canada and the University of Hawaii.

Published
2010
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37. Understanding the shape of the galaxy two-point correlation function at z ~= 1 in the COSMOS field

Author

de la Torre S., Guzzo L., Kova, #269, Porciani C., Abbas U., Meneux B., Carollo C. M., Contini T., Kneib J. P., Le Fèvre O., Lilly S. J., Mainieri V., Renzini A., Sanders D., Scodeggio M., Scoville N., Zamorani G., Bardelli S., Bolzonella M., Bongiorno A., Caputi K., Coppa G., de Ravel L., Franzetti P., Garilli B., Iovino A., Kampczyk P., Knobel C., Koekemoer A. M., Lamareille F., Le Borgne J. F., Le Brun V., Maier C., Mignoli M., Pelló R., Peng Y., Perez Montero E., Ricciardelli E., Silverman J., Tanaka M., Tasca L., Tresse L., Vergani D., Welikala N., Zucca E., Bottini D., Cappi A., Cassata P., Fumana M., Ilbert O., Leauthaud A., Maccagni D., Marinoni C., McCracken H. J., Memeo P., Nair P., Oesch P., Pozzetti L., Presotto V., Scaramella R., CUCCIATI, OLGA, CIMATTI, ANDREA, de la Torre S., Guzzo L., Kova&#269, K., Porciani C., Abbas U., Meneux B., Carollo C. M., Contini T., Kneib J. P., Le Fèvre O., Lilly S. J., Mainieri V., Renzini A., Sanders D., Scodeggio M., Scoville N., Zamorani G., Bardelli S., Bolzonella M., Bongiorno A., Caputi K., Coppa G., Cucciati O., de Ravel L., Franzetti P., Garilli B., Iovino A., Kampczyk P., Knobel C., Koekemoer A. M., Lamareille F., Le Borgne J.-F., Le Brun V., Maier C., Mignoli M., Pelló R., Peng Y., Perez-Montero E., Ricciardelli E., Silverman J., Tanaka M., Tasca L., Tresse L., Vergani D., Welikala N., Zucca E., Bottini D., Cappi A., Cassata P., Cimatti A., Fumana M., Ilbert O., Leauthaud A., Maccagni D., Marinoni C., McCracken H. J., Memeo P., Nair P., Oesch P., Pozzetti L., Presotto V., and Scaramella R.

Published
2010

38. The [O iii] emission line luminosity function of optically selected type-2 AGN from zCOSMOS

Author

Bongiorno A., Mignoli M., Zamorani G., Lamareille F., LANZUISI, GIORGIO, Miyaji T., Bolzonella M., Carollo C. M., Contini T., Kneib J. P., Le Fèvre O., Lilly S. J., Mainieri V., Renzini A., Scodeggio M., Bardelli S., Caputi K., Civano F., Coppa G., de La Torre S., de Ravel L., Franzetti P., Garilli B., Halliday C., Hasinger G., Koekemoer A. M., Iovino A., Kampczyk P., Knobel C., Kova, #269, Le Borgne J. F., Le Brun V., Maier C., Merloni A., Nair P., Pello R., Peng Y., Perez Montero E., Ricciardelli E., Salvato M., Silverman J., Tanaka M., Tasca L., Tresse L., Vergani D., Zucca E., Abbas U., Bottini D., Cappi A., Cassata P., Guzzo L., Leauthaud A., Maccagni D., Marinoni C., McCracken H. J., Memeo P., Meneux B., Oesch P., Porciani C., Pozzetti L., Scaramella R., BRUSA, MARCELLA, CUCCIATI, OLGA, CIMATTI, ANDREA, Bongiorno A., Mignoli M., Zamorani G., Lamareille F., Lanzuisi G., Miyaji T., Bolzonella M., Carollo C. M., Contini T., Kneib J. P., Le Fèvre O., Lilly S. J., Mainieri V., Renzini A., Scodeggio M., Bardelli S., Brusa M., Caputi K., Civano F., Coppa G., Cucciati O., de La Torre S., de Ravel L., Franzetti P., Garilli B., Halliday C., Hasinger G., Koekemoer A. M., Iovino A., Kampczyk P., Knobel C., Kova&#269, K., Le Borgne J.-F., Le Brun V., Maier C., Merloni A., Nair P., Pello R., Peng Y., Perez Montero E., Ricciardelli E., Salvato M., Silverman J., Tanaka M., Tasca L., Tresse L., Vergani D., Zucca E., Abbas U., Bottini D., Cappi A., Cassata P., Cimatti A., Guzzo L., Leauthaud A., Maccagni D., Marinoni C., McCracken H. J., Memeo P., Meneux B., Oesch P., Porciani C., Pozzetti L., Scaramella R., Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), and Astronomy

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, Population, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Type (model theory), Surveys, 01 natural sciences, Luminosity, 0103 physical sciences, Galaxies: active, Astronomy and Astrophysics, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Emission spectrum, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Density evolution, 0105 earth and related environmental sciences, Line (formation), Luminosity function (astronomy), Physics, education.field_of_study, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Redshift, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present a catalog of 213 type-2 AGN selected from the zCOSMOS survey. The selected sample covers a wide redshift range (0.15, Comment: 20 pages, 11 figures, accepted for publication in Astronomy and Astrophysics

Published
2010
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39. Tracking the impact of environment on the galaxy stellar mass function up to z ∼ 1 in the 10 k zCOSMOS sample

Author

Bolzonella M., Kova, #269, Pozzetti L., Zucca E., Lilly S. J., Peng Y., Iovino A., Zamorani G., Vergani D., Tasca L. A. M., Lamareille F., Oesch P., Caputi K., Kampczyk P., Bardelli S., Maier C., Abbas U., Knobel C., Scodeggio M., Carollo C. M., Contini T., Kneib J. P., Le Fèvre O., Mainieri V., Renzini A., Bongiorno A., Coppa G., de la Torre S., de Ravel L., Franzetti P., Garilli B., Le Borgne J. F., Le Brun V., Mignoli M., Pelló R., Perez Montero E., Ricciardelli E., Silverman J. D., Tanaka M., Tresse L., Bottini D., Cappi A., Cassata P., Guzzo L., Koekemoer A. M., Leauthaud A., Maccagni D., Marinoni C., McCracken H. J., Memeo P., Meneux B., Porciani C., Scaramella R., Aussel H., Capak P., Halliday C., Ilbert O., Kartaltepe J., Salvato M., Sanders D., Scarlata C., Scoville N., Taniguchi Y., Thompson D., CUCCIATI, OLGA, CIMATTI, ANDREA, Bolzonella M., Kova&#269, K., Pozzetti L., Zucca E., Cucciati O., Lilly S. J., Peng Y., Iovino A., Zamorani G., Vergani D., Tasca L. A. M., Lamareille F., Oesch P., Caputi K., Kampczyk P., Bardelli S., Maier C., Abbas U., Knobel C., Scodeggio M., Carollo C. M., Contini T., Kneib J.-P., Le Fèvre O., Mainieri V., Renzini A., Bongiorno A., Coppa G., de la Torre S., de Ravel L., Franzetti P., Garilli B., Le Borgne J.-F., Le Brun V., Mignoli M., Pelló R., Perez-Montero E., Ricciardelli E., Silverman J. D., Tanaka M., Tresse L., Bottini D., Cappi A., Cassata P., Cimatti A., Guzzo L., Koekemoer A. M., Leauthaud A., Maccagni D., Marinoni C., McCracken H. J., Memeo P., Meneux B., Porciani C., Scaramella R., Aussel H., Capak P., Halliday C., Ilbert O., Kartaltepe J., Salvato M., Sanders D., Scarlata C., Scoville N., Taniguchi Y., Thompson D., INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), AUTRES, INAF- Milano, Institute of Astronomy [ETH Zürich], Department of Physics [ETH Zürich] (D-PHYS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), INAF - Osservatorio Astronomico di Brera (OAB), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), University of Chicago, Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées (LATT), Human Genetics Center, The University of Texas Health Science Center at Houston (UTHealth), School of Biotechnology and Biomolecular Sciences, University of New South Wales [Sydney] (UNSW), Space Telescope Science Institute (STSci), Centre de Physique Théorique - UMR 6207 (CPT), Université de la Méditerranée - Aix-Marseille 2-Université de Provence - Aix-Marseille 1-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Centre de Physique Théorique - UMR 7332 (CPT), Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), California Institute of Technology (CALTECH), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Materials & Process technology, Boeing Company [Chicago], Sea Mammal Research Unit, St Andrews, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université de Toulon (UTLN)-Université de Provence - Aix-Marseille 1-Université de la Méditerranée - Aix-Marseille 2, and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Photometry (optics), [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, Galaxy formation and evolution, Density contrast, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Star formation, galaxies: fundamental parameters, Astronomy and Astrophysics, Redshift, Galaxy, Bimodality, galaxies: luminosity function, mass function, Space and Planetary Science, cosmology: observations, galaxies: evolution, galaxies: luminosity function, mass function, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We study the impact of the environment on the evolution of galaxies in the zCOSMOS 10k sample in the redshift range 0.1, Comment: 17 pages, 11 figures. Version accepted for publication in Astronomy and Astrophysics, including referee's suggestions, a new section with comparison with literature data, and updated references

Published
2010
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40. The Density Field of the 10k zCOSMOS Galaxies

Author

Kova, #269, Lilly S. J., Porciani C., Iovino A., Zamorani G., Oesch P., Bolzonella M., Knobel C., Finoguenov A., Peng Y., Carollo C. M., Pozzetti L., Caputi K., Silverman J. D., Tasca L. A. M., Scodeggio M., Vergani D., Scoville N. Z., Capak P., Contini T., Kneib J. P., Le Fèvre O., Mainieri V., Renzini A., Bardelli S., Bongiorno A., Coppa G., de la Torre S., de Ravel L., Franzetti P., Garilli B., Guzzo L., Kampczyk P., Lamareille F., Le Borgne J. F., Le Brun V., Maier C., Mignoli M., Pello R., Perez Montero E., Ricciardelli E., Tanaka M., Tresse L., Zucca E., Abbas U., Bottini D., Cappi A., Cassata P., Fumana M., Koekemoer A. M., Maccagni D., Marinoni C., McCracken H. J., Memeo P., Meneux B., Scaramella R., CUCCIATI, OLGA, CIMATTI, ANDREA, Centre de Physique Théorique - UMR 6207 (CPT), Centre National de la Recherche Scientifique (CNRS)-Université de Toulon (UTLN)-Université de Provence - Aix-Marseille 1-Université de la Méditerranée - Aix-Marseille 2, Centre de Physique Théorique - UMR 7332 (CPT), Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Kova&#269, K., Lilly S. J., Cucciati O., Porciani C., Iovino A., Zamorani G., Oesch P., Bolzonella M., Knobel C., Finoguenov A., Peng Y., Carollo C. M., Pozzetti L.,Caputi K., Silverman J. D., Tasca L. A. M., Scodeggio M., Vergani D., Scoville N. Z., Capak P., Contini T., Kneib J.-P., Le Fèvre O., Mainieri V., Renzini A., Bardelli S., Bongiorno A., Coppa G., de la Torre S., de Ravel L., Franzetti P., Garilli B., Guzzo L., Kampczyk P., Lamareille F., Le Borgne J.-F., Le Brun V., Maier C., Mignoli M., Pello R., Perez Montero E., Ricciardelli E., Tanaka M., Tresse L., Zucca E., Abbas U., Bottini D., Cappi A., Cassata P., Cimatti A., Fumana M., Koekemoer A. M., Maccagni D., Marinoni C., McCracken H. J.,Memeo P., Meneux B., Scaramella R., Astronomy, and Université de la Méditerranée - Aix-Marseille 2-Université de Provence - Aix-Marseille 1-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Field (physics), FOS: Physical sciences, Scale (descriptive set theory), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Spectral line, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], LY-ALPHA EMITTERS, surveys, galaxies: high-redshift, 0103 physical sciences, LARGE-SCALE STRUCTURE, 010303 astronomy & astrophysics, Weak gravitational lensing, Astrophysics::Galaxy Astrophysics, Photometric redshift, Physics, large-scale structure of universe, REDSHIFT SURVEY, 010308 nuclear & particles physics, Shot noise, Astronomy and Astrophysics, VLT DEEP SURVEY, ENVIRONMENTAL DEPENDENCE, Galaxy, Redshift, COSMOS FIELD, Space and Planetary Science, Galaxies: high-redshift, Large-scale structure of universe, Surveys, SMOOTHED PARTICLE HYDRODYNAMICS, LUMINOSITY DEPENDENCE, DIGITAL SKY SURVEY, STELLAR MASS, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We use the current sample of ~10,000 zCOSMOS spectra of sources selected with I(AB) < 22.5 to define the density field out to z~1, with much greater resolution in the radial dimension than has been possible with either photometric redshifts or weak lensing. We apply new algorithms that we have developed (ZADE) to incorporate objects not yet observed spectroscopically by modifying their photometric redshift probability distributions using the spectroscopic redshifts of nearby galaxies. This strategy allows us to probe a broader range of galaxy environments and reduce the Poisson noise in the density field. The reconstructed overdensity field of the 10k zCOSMOS galaxies consists of cluster-like patterns surrounded by void-like regions, extending up to z~1. Some of these structures are very large, spanning the ~50 Mpc/h transverse direction of the COSMOS field and extending up to Delta z~0.05 in redshift. We present the three dimensional overdensity maps and compare the reconstructed overdensity field to the independently identified virialised groups of galaxies and clusters detected in the visible and in X-rays. The distribution of the overdense structures is in general well traced by these virialised structures. A comparison of the large scale structures in the zCOSMOS data and in the mock catalogues reveals an excellent agreement between the fractions of the volume enclosed in structures of all sizes above a given overdensity between the data and the mocks in 0.2, Comment: 35 pages, 20 figures; submitted to ApJ; the high resolution pdf available at http://www.exp-astro.phys.ethz.ch/kovac/public/zCOSMOS

Published
2010
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41. The evolving star formation rate: MBlack star relation and sSFR since z ≃ 5 from the VUDS spectroscopic survey

Author

Tasca, L. A. M., Le Fèvre, O., Hathi, N. P., Schaerer, D., Ilbert, O., Zamorani, G., Lemaux, B. C., Cassata, P., Garilli, B., Le Brun, V., Maccagni, D., Pentericci, L., Thomas, R., Vanzella, E., Zucca, E., Amorin, R., Bardelli, S., Cassarà, L. P., Castellano, M., Cimatti, A., Cucciati, O., Durkalec, A., Fontana, A., Giavalisco, M., Grazian, A., Paltani, S., Ribeiro, B., Scodeggio, M., Sommariva, V., Talia, M., Tresse, L., Vergani, D., Capak, P., Charlot, S., Contini, T., De La Torre, S., Dunlop, J., Fotopoulou, S., Koekemoer, A., López-Sanjuan, C., Mellier, Y., Pforr, J., Salvato, M., Scoville, N., Taniguchi, Y., and Wang, P. W.

Subjects
galaxies: high-redshift, Space and Planetary Science, galaxies: star formation, galaxies: formation, Astronomy and Astrophysics, galaxies: evolution
Published
2015

42. The zCOSMOS Redshift Survey: How group environment alters global downsizing trends

Author

Iovino A., Scodeggio M., Knobel C., Kova, #269, Lilly S., Bolzonella M., Tasca L. A. M., Zamorani G., Zucca E., Caputi K., Pozzetti L., Oesch P., Lamareille F., Halliday C., Bardelli S., Finoguenov A., Guzzo L., Kampczyk P., Maier C., Tanaka M., Vergani D., Carollo C. M., Contini T., Kneib J. P., Le Fèvre O., Mainieri V., Renzini A., Bongiorno A., Coppa G., de La Torre S., de Ravel L., Franzetti P., Garilli B., Le Borgne J. F., Le Brun V., Mignoli M., Pellò R., Peng Y., Perez Montero E., Ricciardelli E., Silverman J. D., Tresse L., Abbas U., Bottini D., Cappi A., Cassata P., Koekemoer A. M., Leauthaud A., Maccagni D., Marinoni C., McCracken H. J., Memeo P., Meneux B., Porciani C., Scaramella R., Schiminovich D., Scoville N., CUCCIATI, OLGA, CIMATTI, ANDREA, AUTRES, Dipartimento di Fisica, Università degli Studi di Milano-Bicocca [Milano] (UNIMIB)-Università degli Studi di Milano [Milano] (UNIMI), INAF- Milano, Istituto Nazionale di Astrofisica (INAF), Università di Bologna, Dipartimento di Astronomia, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), INAF - Osservatorio Astronomico di Brera (OAB), INAF - Osservatorio Astronomico di Bologna (OABO), Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Tokai University, INAF - Osservatorio Astrofisico di Arcetri (OAA), University of Chicago, Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées (LATT), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institute of Astronomy [ETH Zürich], Department of Physics [ETH Zürich] (D-PHYS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), Space Telescope Science Institute (STSci), Centre de Physique Théorique - UMR 6207 (CPT), Centre National de la Recherche Scientifique (CNRS)-Université de Toulon (UTLN)-Université de Provence - Aix-Marseille 1-Université de la Méditerranée - Aix-Marseille 2, Centre de Physique Théorique - UMR 7332 (CPT), Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), California Institute of Technology (CALTECH), Iovino A., Cucciati O., Scodeggio M., Knobel C., Kova&#269, K., Lilly S., Bolzonella M., Tasca L. A. M., Zamorani G., Zucca E., Caputi K., Pozzetti L., Oesch P., Lamareille F., Halliday C., Bardelli S., Finoguenov A., Guzzo L., Kampczyk P., Maier C., Tanaka M., Vergani D., Carollo C. M., Contini T., Kneib J.-P., Le Fèvre O., Mainieri V., Renzini A., Bongiorno A., Coppa G., de La Torre S., de Ravel L., Franzetti P., Garilli B., Le Borgne J.-F., Le Brun V., Mignoli M., Pellò R., Peng Y., Perez-Montero E., Ricciardelli E., Silverman J. D., Tresse L., Abbas U., Bottini D., Cappi A., Cassata P., Cimatti A., Koekemoer A. M., Leauthaud A., Maccagni D., Marinoni C., McCracken H. J., Memeo P., Meneux B., Porciani C., Scaramella R., Schiminovich D., Scoville N., Università degli Studi di Milano-Bicocca = University of Milano-Bicocca (UNIMIB)-Università degli Studi di Milano = University of Milan (UNIMI), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université de la Méditerranée - Aix-Marseille 2-Université de Provence - Aix-Marseille 1-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), and Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Interactions, Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, Clusters, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, Galaxy formation and evolution, Mass segregation, Evolution - Galaxies, Galaxies, General - Galaxies, Astronomy and Astrophysics, Space and Planetary Science, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, education.field_of_study, 010308 nuclear & particles physics, Redshift survey, Galaxy, Redshift, Low Mass, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We took advantage of the wealth of information provided by the first ~10000 galaxies of the zCOSMOS-bright survey and its group catalogue to study the complex interplay between group environment and galaxy properties. The classical indicator F_blue (fraction of blue galaxies) proved to be a simple but powerful diagnostic tool. We studied its variation for different luminosity and mass selected galaxy samples. Using rest-frame B-band selected samples, the groups galaxy population exhibits significant blueing as redshift increases, but maintains a lower F_blue with respect both to the global and the isolated galaxy population. However moving to mass selected samples it becomes apparent that such differences are largely due to the biased view imposed by the B-band luminosity selection, being driven by the population of lower mass, bright blue galaxies for which we miss the redder, equally low mass, counterparts. By focusing the analysis on narrow mass bins such that mass segregation becomes negligible we find that only for the lowest mass bin explored (logMass = 10.8 are already in place at z ~ 1 and do not exhibit any strong environmental dependence, possibly originating from so-called 'nature'/internal mechanisms. In contrast, for lower galaxy masses and redshifts lower than z ~ 1, we observe the emergence in groups of a population of 'nurture' red galaxies: slightly deviating from the trend of the downsizing scenario followed by the global galaxy population, and more so with cosmic time. These galaxies exhibit signatures of group-related secular physical mechanisms directly influencing galaxy evolution., Submitted to A&A, revised version after referee comments

Published
2009
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43. An optical group catalogue to z = 1 from the zCOSMOS 10k sample

Author

Knobel, C., Lilly S. J., Iovino A., Porciani C., Kova, #269, Finoguenov A., Kitzbichler M. G., Carollo C. M., Contini T., Kneib J. P., LeFèvre O., Mainieri V., Renzini A., Scodeggio M., Zamorani G., Bardelli S., Bolzonella M., Bongiorno A., Caputi K., Coppa G., de la Torre S., de Ravel L., Franzetti P., Garilli B., Kampczyk P., Lamareille F., Le Borgne J. F., Le Brun V., Maier C., Mignoli M., Pello R., Peng Y., Montero E. Perez, Ricciardelli E., Silverman J. D., Tanaka M., Tasca L., Tresse L., Vergani D., Zucca E., Abbas U., Bottini D., Cappi A., Cassata P., Fumana M., Guzzo L., Koekemoer A. M., Leauthaud A., Maccagni D., Marinoni C., McCracken H. J., Memeo P., Meneux B., Oesch P., Pozzetti L., Scaramella R., CUCCIATI, OLGA, CIMATTI, ANDREA, Centre de Physique Théorique - UMR 6207 (CPT), Centre National de la Recherche Scientifique (CNRS)-Université de Toulon (UTLN)-Université de Provence - Aix-Marseille 1-Université de la Méditerranée - Aix-Marseille 2, Centre de Physique Théorique - UMR 7332 (CPT), Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), AUTRES, INAF- Milano, INAF - Osservatorio Astrofisico di Arcetri (OAA), Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Université de la Méditerranée - Aix-Marseille 2-Université de Provence - Aix-Marseille 1-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Knobel, C., Lilly S. J., Iovino A., Porciani C., Kova&#269, K., Cucciati O., Finoguenov A., Kitzbichler M. G., Carollo C. M., Contini T., Kneib J.-P., LeFèvre O., Mainieri V., Renzini A., Scodeggio M., Zamorani G., Bardelli S., Bolzonella M., Bongiorno A., Caputi K., Coppa G., de la Torre S., de Ravel L., Franzetti P., Garilli B., Kampczyk P., Lamareille F., Le Borgne J.-F., Le Brun V., Maier C., Mignoli M., Pello R., Peng Y., Montero E. Perez, Ricciardelli E., Silverman J. D., Tanaka M., Tasca L., Tresse L., Vergani D., Zucca E., Abbas U., Bottini D., Cappi A., Cassata P., Cimatti A., Fumana M., Guzzo L., Koekemoer A. M., Leauthaud A., Maccagni D., Marinoni C., McCracken H. J., Memeo P., Meneux B., Oesch P., Pozzetti L., and Scaramella R.

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, galaxies: high-redshift, Galaxy group, 0103 physical sciences, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Group (mathematics), Velocity dispersion, Astronomy and Astrophysics, methods: data analysis, Redshift, Galaxy, Space and Planetary Science, galaxies: clusters: general, Catalogs, Galaxies: clusters: general, Galaxies: high-redshift, Methods: data analysis, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Astrophysics - Instrumentation and Methods for Astrophysics, catalogs, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present a galaxy group catalogue spanning the redshift range 0.1 = 5 spectroscopically confirmed members, with a further ~700 groups with 2, Comment: 20 pages, 19 figures, accepted for publication in ApJ

Published
2009
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44. VizieR Online Data Catalog: VUDS Dicovery of a high-redshift protocluster (Lemaux+, 2014)

Author

Lemaux, B.~C., Cucciati, O., Tasca, L.~A.~M., Le Fevre, O., Zamorani, G., Cassata, P., Garilli, B., Le Brun, V., Maccagni, D., Pentericci, L., Thomas, R., Vanzella, E., Zucca, E., Amorin, R., Bardelli, S., Capak, P., Cassara, L., Castellano, M., Cimatti, Alessandro, Cuby, J.~G., Torre, S., Durkalec, A., Fontana, A., Giavalisco, M., Grazian, A., Hathi, N.~P., Ilbert, O., Moreau, C., Paltani, S., Ribeiro, B., Salvato, M., Schaerer, D., Scodeggio, M., Sommariva, V., Talia, M., Taniguchi, Y., Tresse, L., Vergani, D., Wang, P.~W., Charlot, S., Contini, T., Fotopoulou, S., Gal, R.~R., Kocevski, D.~D., Lopez-Sanjuan, C., Lubin, L.~M., Mellier, Y., Sadibekova, T., Scoville, N., Laboratoire d'Astrophysique de Marseille (LAM), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES)

Subjects
Photometry, Galaxies: optical, Redshifts, [INFO]Computer Science [cs], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], ComputingMilieux_MISCELLANEOUS
Abstract

International audience; no abstract

Published
2014

45. VizieR Online Data Catalog: VUDS extreme emission line 0.2\lt~z\lt~0.9 galaxies (Amorin+, 2014)

Author

Amorin, R., Sommariva, V., Castellano, M., Grazian, A., Tasca, L.~A.~M., Fontana, A., Pentericci, L., Cassata, P., Garilli, B., Le Brun, V., Le Fevre, O., Maccagni, D., Thomas, R., Vanzella, E., Zamorani, G., Zucca, E., Bardelli, S., Capak, P., Cassara, L.~P., Cimatti, Alessandro, Cuby, J.~G., Cucciati, O., Torre, S., Durkalec, A., Giavalisco, M., Hathi, N.~P., Ilbert, O., Lemaux, B.~C., Moreau, C., Paltani, S., Ribeiro, B., Salvato, M., Schaerer, D., Scodeggio, M., Talia, M., Taniguchi, Y., Tresse, L., Vergani, D., Wang, P.~W., Charlot, S., Contini, T., Fotopoulou, S., Lopez-Sanjuan, C., Mellier, Y., Scoville, N., Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Galaxies: spectra, Redshifts, [INFO]Computer Science [cs], Abundances, Surveys, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], ComputingMilieux_MISCELLANEOUS
Abstract

International audience; no abstract

Published
2014

46. Evidence for major mergers of galaxies at 2 less than or similar to z \textless 4 in the VVDS and VUDS surveys

Author

Tasca, L. A. M., Le Fèvre, O., Lopez-Sanjuan, C., Wang, P. -W., Cassata, P., Garilli, B., Ilbert, O., Le Brun, V., Lemaux, B. C., Maccagni, D., Tresse, L., Bardelli, S., Contini, T., Charlot, S., Cucciati, O., Fontana, A., Giavalisco, M., Kneib, J. -P., Salvato, M., Taniguchi, Y., Vergani, D., Zamorani, G., Zucca, E., Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), AUTRES, INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Dipartimento di Fisica, Università degli Studi di Milano-Bicocca [Milano] (UNIMIB)-Università degli Studi di Milano [Milano] (UNIMI), INAF - Osservatorio Astronomico di Roma (OAR), Department of Astronomy [Amherst], University of Massachusetts [Amherst] (UMass Amherst), University of Massachusetts System (UMASS)-University of Massachusetts System (UMASS), Ecole Polytechnique Fédérale de Lausanne (EPFL), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, INAF - Osservatorio Astrofisico di Arcetri (OAA), Oncology Institute of Southern Switzerland, European Project: 268107,EC:FP7:ERC,ERC-2010-AdG_20100224,EARLY(2011), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and Università degli Studi di Milano-Bicocca = University of Milano-Bicocca (UNIMIB)-Università degli Studi di Milano = University of Milan (UNIMI)

Subjects
[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Galaxies: high-redshift, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxies: formation, Astrophysics::Galaxy Astrophysics
Abstract

International audience; Context. The mass assembly of galaxies can proceed through different physical processes. Here we report on the spectroscopic identification of close physical pairs of galaxies at redshifts 2 less than or similar to z \textless 4 and discuss the impact of major mergers in building galaxies at these early cosmological times. Aims. We aim to identify and characterize close physical pairs of galaxies destined to merge and use their properties to infer the contribution of merging processes to the early mass assembly of galaxies. Methods. We searched for galaxy pairs with a transverse separation r(p) \textless= 25 h(-1) kpc and a velocity difference Delta(v) \textless= 500 km s(-1) using early data from the VIMOS Ultra Deep Survey (VUDS) that comprise a sample of 1111 galaxies with spectroscopic redshifts measurements at redshifts 1.8 \textless= z \textless= 4 in the COSMOS. ECDFS, and VVDS-02h fields, combined with VVDS data. We analysed their spectra and associated visible and near-infrared photometry to assess the main properties of merging galaxies that have an average stellar mass M-* = 2.3 x 10(10) M-circle dot at these redshifts. Results. Using the 12 physical pairs found in our sample we obtain a first robust measurement of the major merger fraction at these redshifts, f(MM)= 19.4(-6)(+9)%. These pairs are expected to merge within 1 Gyr on average each producing a more massive galaxy by the time the cosmic star formation peaks at z similar to 1-2. Using the pairs' merging time scales, we derive a merging rate of R-MM = 0.17(-0.05)(+0.08) Gyr(-1). From the average mass ratio between galaxies in the pairs, the stellar mass of the resulting galaxy after merging will be similar to 60% higher than the most massive galaxy in the pair before merging. We conclude that major merging of galaxy pairs is on-going at 2 less than or similar to z \textless 4 and is significantly contributing to the major mass assembly phase of galaxies at this early epoch.

Published
2014
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47. Evidence for major mergers of galaxies at 2<z<4 in the VVDS and VUDS surveys

Author

Tasca, L. A. M., Le Fxe8vre, O., Lxf3pez-Sanjuan, C., Wang, P.-W., Cassata, P., Garilli, B., Ilbert, O., Le Brun, V., Lemaux, B. C., Maccagni, D., Tresse, L., Bardelli, S., Contini, T., Charlot, S., Cucciati, O., Fontana, A., Giavalisco, M., Kneib, J.-P., Salvato, M., Taniguchi, Y., Vergani, D., Zamorani, G., Zucca, E., Tasca, L. A. M., Le Fxe8vre, Lxf3pez-Sanjuan, Wang, P.-W., Cassata, Garilli, Ilbert, Le Brun, Lemaux, B. C., Maccagni, Tresse, Bardelli, Contini, Charlot, Cucciati, Fontana, Giavalisco, Kneib, J.-P., Salvato, Taniguchi, Vergani, Zamorani, and Zucca

Published
2014

48. The zCOSMOS redshift survey: evolution of the light in bulges and discs since z similar to 0.8

Author

Tasca, L. A. M., Tresse, L., Le Fèvre, O., Ilbert, O., Lilly, S. J., Zamorani, G., Lopez-Sanjuan, C., Ho, L. C., Bardelli, S., Cattaneo, A., Cucciati, O., Farrah, D., Iovino, A., Koekemoer, A. M., Liu, C. T., Massey, R., Renzini, A., Taniguchi, Y., Welikala, N., Zucca, E., Carollo, C. M., Contini, T., Kneib, J. -P., Mainieri, V., Scodeggio, M., Bolzonella, M., Bongiorno, A., Caputi, K., Torre, S., Franzetti, P., Garilli, B., Guzzo, L., Kampczyk, P., Knobel, C., Kovac, K., Lamareille, F., Le Borgne, J. -F., Le Brun, V., Maier, C., Mignoli, M., Pello, R., Peng, Y., Perez Montero, E., Rich, Robert Michael, Tanaka, M., Vergani, D., Bordoloi, R., Cappi, A., Cimatti, Alessandro, Coppa, G., Mccracken, H. J., Moresco, M., Pozzetti, L., Sanders, D., Sheth, K., Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institute for Astronomy [Zürich], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Istituto Nazionale di Astrofisica (INAF), Kavli Institute for Astronomy and Astrophysics [Beijing] (KIAA-PKU), Peking University [Beijing], INAF - Osservatorio Astronomico di Bologna (OABO), Dipartimento di Fisica, Università degli Studi di Milano-Bicocca = University of Milano-Bicocca (UNIMIB)-Università degli Studi di Milano = University of Milan (UNIMI), Department of Physics [Blacksburg], Virginia Tech [Blacksburg], INAF - Osservatorio Astronomico di Brera (OAB), Space Telescope Science Institute (STSci), City University of Hong Kong [Hong Kong] (CUHK), Institute for Computational Cosmology (ICC), Durham University, INAF - Osservatorio Astronomico di Padova (OAPD), Research Center for Space and Cosmic Evolution (RCSCE), Ehime University [Matsuyama, Japon], University of Chicago, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Ecole Polytechnique Fédérale de Lausanne (EPFL), European Southern Observatory (ESO), INAF- Milano, Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), Max-Planck-Institut für Extraterrestrische Physik (MPE), Kapteyn Astronomical Institute [Groningen], University of Groningen [Groningen], Institute of Astronomy [ETH Zürich], Department of Physics [ETH Zürich] (D-PHYS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Department of Physics and Astronomy [UCLA Los Angeles], University of California [Los Angeles] (UCLA), University of California (UC)-University of California (UC), National Astronomical Observatory of Japan (NAOJ), INAF - Osservatorio Astrofisico di Arcetri (OAA), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institute for Astronomy [Honolulu], University of Hawai‘i [Mānoa] (UHM), National Radio Astronomy Observatory (NRAO), European Project: 268107,EC:FP7:ERC,ERC-2010-AdG_20100224,EARLY(2011), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), Università degli studi di Milano [Milano]-Università di Milano-Bicocca, Ehime University [Matsuyama], AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich)-Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, University of California-University of California, Osservatorio Astronomico (INAF), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Università degli Studi di Milano-Bicocca [Milano] (UNIMIB)-Università degli Studi di Milano [Milano] (UNIMI), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)

Subjects
Galaxies: bulges, Galaxies: fundamental parameters, Galaxies: distances and redshifts, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Galaxies: luminosity function, Mass function, Galaxies: evolution, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

International audience; We studied the chronology of galactic bulge and disc formation by analysing the relative contributions of these components to the B-band rest-frame luminosity density at different epochs. We present the first estimate of the evolution of the fraction of rest-frame B-band light in galactic bulges and discs since redshift z similar to 0.8. We performed a bulge-to-disc decomposition of HST/ACS images of 3266 galaxies in the zCOSMOS-bright survey with spectroscopic redshifts in the range 0.7 \textless= z \textless= 0.9. We find that the fraction of B-band light in bulges and discs is (26 4)% and (74 4)%, respectively. When compared with rest-frame B-band measurements of galaxies in the local Universe in the same mass range (10(9)M circle dot M10(11.5).M circle dot),we find that the B-band light in discs decreases by -30% from z similar to 0.7-0.9 to z 0, while the light from the bulge increases by -30% over the same period of time. We interpret this evolution as the consequence of star formation and mass assembly processes, as well as morphological transformation, which gradually shift stars formed at half the age of the Universe from star-forming late-type/irregular galaxies to earlier types and ultimately into spheroids.

Published
2014
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49. The VIMOS VLT Deep Survey: Final Public Release of ~ 35 000 Galaxies and Active Galactic Nuclei Covering 13 Billion Years of Evolution

Author

Le Fxe8vre O., Adami C., Arnouts, S., Bardelli, S., Bolzonella, M., Bondi, M., Bongiorno, A., Bottini, D., Cappi, A., Cassata, P., Charlot, S., Ciliegi, P., Contini, T., Cucciati, O., de la Torre, S, Foucaud, S., Franzetti, P., Garilli, B., Gavignaud, I., Guzzo, L., Ilbert, O., Iovino, A., Le Brun, V., Lemaux, B., Lxf3pez-Sanjuan, C., Maccagni, D., McCracken, H. J., Marano, B., Marinoni, C., Mazure, A., Mellier, Y., Merighi, R., Merluzzi, P., Moreau, C., Paltani, S., Pellxf2, R., Pollo, A., Pozzetti, L., Scaramel, Arnouts, Bardelli, Bolzonella, Bondi, Bongiorno, Bottini, Cappi, Cassata, Charlot, Ciliegi, Contini, Cucciati, de la Torre, S, Foucaud, Franzetti, Garilli, Gavignaud, Guzzo, Ilbert, Iovino, Le Brun, Lemaux, Lxf3pez-Sanjuan, Maccagni, McCracken, H. J., Marano, Marinoni, Mazure, Mellier, Merighi, Merluzzi, Moreau, Paltani, Pellxf2, Pollo, and Pozzetti

Published
2014

50. The VIMOS Ultra Deep Survey: 10 000 Galaxies to Study the Early Phases of Galaxy Assembly at 2 \lt z \lt 6+

Author

Le Fèvre, O., Amorin, R., Bardelli, S., Capak, P., Cassara, L., Cassata, P., Castellano, M., Charlot, S., Cimatti, Alessandro, Contini, T., Cuby, J., Cucciati, O., Durkalec, A., Torre, S., Fontana, A., Fotopoulou, S., Garilli, B., Giavalisco, M., Grazian, A., Hathi, N., Ilbert, O., Le Brun, V., Lemaux, B., Lopez-Sanjuan, C., Maccagni, D., Mellier, Y., Moreau, C., Paltani, S., Pentericci, L., Ribeiro, B., Salvato, M., Schaerer, D., Scodeggio, M., Scoville, N., Sommariva, V., Talia, M., Taniguchi, Y., Tasca, L., Thomas, R., Tresse, L., Vanzella, E., Vergani, D., Wang, P., Zamorani, G., Zucca, E., Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES)

Subjects
[INFO]Computer Science [cs], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], ComputingMilieux_MISCELLANEOUS
Abstract

International audience; no abstract

Published
2014

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