Author: "Le Fevre, O" / Topic: astrophysics::cosmology and extragalactic astrophysics - Searchworks@Jio Institute Digital Library Search Results

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74 results on '"Le Fevre, O"'

1. The ALPINE-ALMA [CII] survey The contribution of major mergers to the galaxy mass assembly at z similar to 5

Author: Romano, M., Cassata, P., Morselli, L., Jones, G. C., Ginolfi, M., Zanella, A., Bethermin, M., Capak, P., Faisst, A., Le Fevre, O., Schaerer, D., Silverman, J. D., Yan, L., Bardelli, S., Boquien, M., Cimatti, A., Dessauges-Zavadsky, M., Enia, A., Fujimoto, S., Gruppioni, C., Hathi, N. P., Ibar, E., Koekemoer, A. M., Lemaux, B. C., Rodighiero, G., Vergani, D., Zamorani, G., and Zucca, E.
Subjects: C II SURVEY, formation [galaxies], DISTANT GALAXIES, POST-STARBURST GALAXIES, Astrophysics::Cosmology and Extragalactic Astrophysics, VLT DEEP SURVEY, early Universe, GAS ACCRETION, STAR-FORMATION, COSMOS FIELD, LUMINOSITY FUNCTION, kinematics and dynamics [galaxies], ILLUSTRIS SIMULATION, PHOTOMETRIC REDSHIFTS, Astrophysics::Galaxy Astrophysics, evolution [galaxies], high-redshift [galaxies]
Abstract: Context. Galaxy mergers are thought to be one of the main mechanisms of the mass assembly of galaxies in the Universe, but there is still little direct observational evidence of how frequent they are at z greater than or similar to 4. Recently, many works have suggested a possible increase in the fraction of major mergers in the early Universe, reviving the debate on which processes (e.g., cold accretion, star formation, mergers) most contribute to the mass build-up of galaxies through cosmic time.Aims. To estimate the importance of major mergers in this context, we make use of the new data collected by the ALMA Large Program to INvestigate [CII] at Early times (ALPINE) survey, which attempted to observe the [CII] 158 mu m emission line from a sample of 75 main-sequence star-forming galaxies at 4.4 < z < 5.9.Methods. We used, for the first time, the morpho-kinematic information provided by the [CII] emission, along with archival multiwavelength data to obtain the fraction of major mergers (f(MM)) at z similar to 5. By combining the results from ALPINE with those at lower redshifts from the literature, we also studied the evolution of the merger fraction through cosmic time. We then used different redshift-evolving merger timescales (T-MM) to convert this fraction into the merger rate per galaxy (R-MM) and in the volume-averaged merger rate (Gamma(MM)).Results. We find a merger fraction of f(MM) similar to 0.44 (0.34) at z similar to 4.5 (5.5) from ALPINE. By combining our results with those at lower redshifts, we computed the cosmic evolution of the merger fraction which is described by a rapid increase from the local Universe to higher redshifts, a peak at z similar to 3, and a slow decrease toward earlier epochs. Depending on the timescale prescription used, this fraction translates into a merger rate ranging between similar to 0.1 and similar to 4.0 Gyr(-1) at z similar to 5, which in turn corresponds to an average number of major mergers per galaxy between 1 and 8 in similar to 12.5 yr (from z = 6 to the local Universe). When convolved with the galaxy number density at different epochs, the merger rate density becomes approximately constant over time at 1 < z < 4, including values from 10(-4) to 10(-3) Gyr(-1) Mpc(-3), depending on the assumed T-MM. We finally compare the specific star formation and star-formation rate density with the analogous quantities from major mergers, finding a good agreement at z > 4 if we assume a merger timescale that quickly decreases with increasing redshift.Conclusions. Our new constraints on the merger fraction from the ALPINE survey at z similar to 5 reveal the presence of a significant merging activity in the early Universe. Whether this population of mergers can provide a relevant contribution to the galaxy mass assembly at these redshifts and through the cosmic epochs is strongly dependent on the assumption of the merger timescale. However, our results show that an evolving T-MM proportional to (1 + z)(-2) agrees well with state-of-the-art cosmological simulations, suggesting a considerable role of mergers in the build-up of galaxies at early times.
Published: 2021
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2. The ALPINE-ALMA [CII] survey:The nature, luminosity function, and star formation history of dusty galaxies up to z similar or equal to 6

Author: Gruppioni, C., Bethermin, M., Loiacono, F., Le Fevre, O., Capak, P., Cassata, P., Faisst, A. L., Schaerer, D., Silverman, J., Yan, L., Bardelli, S., Boquien, M., Carraro, R., Cimatti, A., Dessauges-Zavadsky, M., Ginolfi, M., Fujimoto, S., Hathi, N. P., Jones, G. C., Khusanova, Y., Koekemoer, A. M., Lagache, G., Lemaux, B. C., Oesch, P. A., Pozzi, F., Riechers, D. A., Rodighiero, G., Romano, M., Talia, M., Vallini, L., Vergani, D., Zamorani, G., and Zucca, E.
Subjects: REDSHIFT SURVEY, SPECTROSCOPIC SURVEY, FORMING GALAXIES, MU-M, galaxies [submillimeter], MASSIVE GALAXIES, Astrophysics::Cosmology and Extragalactic Astrophysics, observations [cosmology], FORMATION RATES, MOLECULAR GAS, mass function, QUIESCENT GALAXY, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, DEEP FIELD-SOUTH, FORMATION RATE DENSITY, Astrophysics::Galaxy Astrophysics, evolution [galaxies], high-redshift [galaxies], luminosity function [galaxies]
Abstract: Aims. We present the detailed characterisation of a sample of 56 sources serendipitously detected in ALMA band 7 as part of the ALMA Large Program to INvestigate CII at Early Times (ALPINE). These sources, detected in COSMOS and ECDFS, have been used to derive the total infrared luminosity function (LF) and to estimate the cosmic star formation rate density (SFRD) up to z similar or equal to 6.Methods. We looked for counterparts of the ALMA sources in all the available multi-wavelength (from HST to VLA) and photometric redshift catalogues. We also made use of deeper UltraVISTA and Spitzer source lists and maps to identify optically dark sources with no matches in the public catalogues. We used the sources with estimated redshifts to derive the 250 mu m rest-frame and total infrared (8-1000 mu m) LFs from z similar or equal to 0.5 to 6.Results. Our ALMA blind survey (860 mu m flux density range: similar to 0.3-12.5 mJy) allows us to further push the study of the nature and evolution of dusty galaxies at high-z, identifying luminous and massive sources to redshifts and faint luminosities never probed before by any far-infrared surveys. The ALPINE data are the first ones to sample the faint end of the infrared LF, showing little evolution from z similar or equal to 2.5 to z similar or equal to 6, and a "flat" slope up to the highest redshifts (i.e. 4.5 3.
Published: 2020
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3. The ALPINE-ALMA [CII] survey:Dust attenuation properties and obscured star formation at z similar to 4.4-5.8

Author: Fudamoto, Y., Oesch, P. A., Faisst, A., Bethermin, M., Ginolfi, M., Khusanova, Y., Loiacono, F., Le Fevre, O., Capak, P., Schaerer, D., Silverman, J. D., Cassata, P., Yan, L., Amorin, R., Bardelli, S., Boquien, M., Cimatti, A., Dessauges-Zavadsky, M., Fujimoto, S., Gruppioni, C., Hathi, N. P., Ibar, E., Jones, G. C., Koekemoer, A. M., Lagache, G., Lemaux, B. C., Maiolino, R., Narayanan, D., Pozzi, F., Riechers, D. A., Rodighiero, G., Talia, M., Toft, S., Vallini, L., Vergani, D., Zamorani, G., and Zucca, E.
Subjects: LEGACY SURVEY, CALIBRATION, ISM [galaxies], FORMING GALAXIES, extinction, ULTRAVIOLET, Astrophysics::Cosmology and Extragalactic Astrophysics, EVOLUTION, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, dust, HIGH-REDSHIFT, FIELD, STELLAR MASS, Astrophysics::Galaxy Astrophysics, high-redshift [galaxies], POPULATION
Abstract: We present dust attenuation properties of spectroscopically confirmed star forming galaxies on the main sequence at a redshift of similar to 4.4-5.8. Our analyses are based on the far infrared continuum observations of 118 galaxies at rest-frame 158 mu m obtained with the Atacama Large Millimeter Array (ALMA) Large Program to INvestigate [CII] at Early times (ALPINE). We study the connection between the ultraviolet (UV) spectral slope (beta), stellar mass (M-star), and infrared excess (IRX = L-IR/L-UV). Twenty-three galaxies are individually detected in the continuum at > 3.5 sigma significance. We perform a stacking analysis using both detections and nondetections to study the average dust attenuation properties at z similar to 4.4-5.8. The individual detections and stacks show that the IRX-beta relation at z similar to 5 is consistent with a steeper dust attenuation curve than typically found at lower redshifts (z 4. Similarly, we find that our galaxies have lower IRX values, up to 1 dex on average, at a fixed mass compared to previously studied IRX-M-star relations at z less than or similar to 4, albeit with significant scatter. This implies a lower obscured fraction of star formation than at lower redshifts. Our results suggest that dust properties of UV-selected star forming galaxies at z greater than or similar to 4 are characterised by (i) a steeper attenuation curve than at z less than or similar to 4, and (ii) a rapidly decreasing dust obscured fraction of star formation as a function of redshift. Nevertheless, even among this UV-selected sample, massive galaxies (log M-star/M-circle dot> 10) at z similar to 5-6 already exhibit an obscured fraction of star formation of similar to 45%, indicating a rapid build-up of dust during the epoch of reionization.
Published: 2020
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4. The VLA‐COSMOS 3 GHz Large Project: The infrared‐radio correlation of star‐ forming galaxies and AGN to z less than or similar to 6

Author: Delhaize, J., Smolcic, V., Delvecchio, I., Novak, M., Sargent, M., Baran, N., Magnelli, B., Zamorani, G., Schinnerer, E., Murphy, E. J., Aravena, M., Berta, S., Bondi, M., Capak, P., Carilli, C., Ciliegi, P., Civano, F., Ilbert, O., Karim, A., Laigle, C., Le Fevre, O., Marchesi, S., McCracken, H. J., Salvato, M., Seymour, N., Tasca, L., 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: [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: International audience; We examine the behaviour of the infrared‐radio correlation (IRRC) over the range 0 < z less than or similar to 6 using new, highly sensitive 3 GHz observations with the Karl G. Jansky Very Large Array (VLA) and infrared data from the Herschel Space Observatory in the 2 deg(2) COSMOS field. We distinguish between objects where emission is believed to arise solely from star‐formation, and those where an active galactic nucleus (AGN) is thought to be present. We account for non‐detections in the radio or in the infrared using a doublycensored survival analysis. We find that the IRRC of star‐forming galaxies, quantified by the infrared‐to‐1.4 GHz radio luminosity ratio (qTIR), decreases with increasing redshift: q(TIR)(z) = (2.88 +/‐ 0.03)(1 + z)(‐0.19 +/‐ 0.01). This is consistent with several previous results from the literature. Moderate‐to‐high radiative luminosity AGN do not follow the same q(TIR)(z) trend as star‐forming galaxies, having a lower normalisation and steeper decrease with redshift. We cannot rule out the possibility that unidentified AGN contributions only to the radio regime may be steepening the observed q(TIR)(z) trend of the star‐forming galaxy population. We demonstrate that the choice of the average radio spectral index directly affects the normalisation, as well as the derived trend with redshift of the IRRC. An increasing fractional contribution to the observed 3 GHz flux by free‐free emission of star‐forming galaxies may also affect the derived evolution. However, we find that the standard (M82‐based) assumption of the typical radio spectral energy distribution (SED) for star‐forming galaxies is inconsistent with our results. This suggests a more complex shape of the typical radio SED for star‐forming galaxies, and that imperfect K corrections in the radio may govern the derived trend of decreasing q(TIR) with increasing redshift. A more detailed understanding of the radio spectrum is therefore required for robust K corrections in the radio and to fully understand the cosmic evolution of the IRRC. Lastly, we present a redshift‐dependent relation between rest‐frame 1.4 GHz radio luminosity and star formation rate taking the derived redshift trend into account.
Published: 2017
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5. The VLA‐COSMOS 3 GHz Large Project: AGN and host‐galaxy properties out to z less than or similar to 6

Author: Delvecchio, I., Smolcic, V., Zamorani, G., Lagos, C. Del P., Berta, S., Delhaize, J., Baran, N., Alexander, D. M., Rosario, D. J., Gonzalez‐Perez, V., Ilbert, O., Lacey, C. G., Le Fevre, O., Miettinen, O., Aravena, M., Bondi, M., Carilli, C., Ciliegi, P., Mooley, K., Novak, M., Schinnerer, E., Capak, P., Civano, F., Fanidakis, N., Ruiz, N. Herrera, Karim, A., Laigle, C., Marchesi, S., McCracken, H. J., Middleberg, E., Salvato, M., Tasca, L., 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: [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: International audience; We explore the multiwavelength properties of AGN host galaxies for different classes of radio‐selected AGN out to z less than or similar to 6 via a multiwavelength analysis of about 7700 radio sources in the COSMOS field. The sources were selected with the Very Large Array (VLA) at 3 GHz (10 cm) within the VLA‐COSMOS 3 GHz Large Project, and cross‐matched with multiwavelength ancillary data. This is the largest sample of high‐redshift (z less than or similar to 6) radio sources with exquisite photometric coverage and redshift measurements available. We constructed a sample of moderate‐to‐high radiative luminosity AGN (HLAGN) via spectral energy distribution decomposition combined with standard X‐ray and mid‐infrared diagnostics. Within the remainder of the sample we further identified low‐to‐moderate radiative luminosity AGN (MLAGN) via excess in radio emission relative to the star formation rates in their host galaxies. We show that at each redshift our HLAGN have systematically higher radiative luminosities than MLAGN and that their AGN power occurs predominantly in radiative form, while MLAGN display a substantial mechanical AGN luminosity component. We found significant differences in the host properties of the two AGN classes, as a function of redshift. At z < 1 : 5, MLAGN appear to reside in significantly more massive and less star‐forming galaxies compared to HLAGN. At z > 1., we observed a reversal in the behaviour of the stellar mass distributions with the HLAGN populating the higher stellar mass tail. We interpret this finding as a possible hint of the downsizing of galaxies hosting HLAGN, with the most massive galaxies triggering AGN activity earlier than less massive galaxies, and then fading to MLAGN at lower redshifts. Our conclusion is that HLAGN and MLAGN samples trace two distinct galaxy and AGN populations in a wide range of redshifts, possibly resembling the radio AGN types often referred to as radiative‐and jet‐mode (or high‐and low‐excitation), respectively, whose properties might depend on the different availability of cold gas supplies.
Published: 2017
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6. The VLA‐COSMOS 3 GHz Large Project: Cosmic star formation history since z similar to 5

Author: Novak, M., Smolcic, V., Delhaize, J., Delvecchio, I., Zamorani, G., Baran, N., Bondi, M., Capak, P., Carilli, C. L., Ciliegi, P., Civano, F., Ilbert, O., Karim, A., Laigle, C., Le Fevre, O., Marchesi, S., Mccracken, H., Miettinen, O., Salvato, M., Sargent, M., Schinnerer, E., Tasca, L., 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), 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), 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 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: [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: International audience; We make use of the deep Karl G. Jansky Very Large Array (VLA) COSMOS radio observations at 3 GHz to infer radio luminosity functions of star‐forming galaxies up to redshifts of z similar to 5 based on approximately 6000 detections with reliable optical counterparts. This is currently the largest radio‐selected sample available out to z similar to 5 across an area of 2 square degrees with a sensitivity of rms approximate to 2.3 mu Jy beam(‐1). By fixing the faint and bright end shape of the radio luminosity function to the local values, we find a strong redshift trend that can be fitted with a pure luminosity evolution L‐1.4 (GHz) proportional to /(1 + z)((3.16 +/‐ 0.2)‐(0.32 +/‐ 0.07)z). We estimate star formation rates (SFRs) from our radio luminosities using an infrared (IR)‐radio correlation that is redshift dependent. By integrating the parametric fits of the evolved luminosity function we calculate the cosmic SFR density (SFRD) history since z similar to 5. Our data suggest that the SFRD history peaks between 2 < z < 3 and that the ultraluminous infrared galaxies (100 M‐circle dot yr(‐1) < SFR < 1000 M‐circle dot yr(‐1)) contribute up to similar to 25% to the total SFRD in the same redshift range. Hyperluminous infrared galaxies (SFR > 1000 M fi yr 1) contribute an additional less than or similar to 2% in the entire observed redshift range. We find evidence of a potential underestimation of SFRD based on ultraviolet (UV) rest‐frame observations of Lyman break galaxies at high redshifts (z greater than or similar to 4) on the order of 15‐20%, owing to appreciable star formation in highly dust‐obscured galaxies, which might remain undetected in such UV observations.
Published: 2017
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7. Size evolution of star-forming galaxies with 2 \textless z \textless 4.5 in the VIMOS Ultra-Deep Survey

Author: Ribeiro, B., Le Fevre, O., Tasca, L. A. M., Lemaux, B. C., Cassata, P., Garilli, B., Maccagni, D., Zamorani, G., Zucca, E., Amorín, R., Bardelli, S., Fontana, A., Giavalisco, M., Hathi, N. P., Koekemoer, A., Pforr, J., Tresse, L., Dunlop, J., 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), AUTRES, Istituto Nazionale di Astrofisica (INAF), Oncology Institute of Southern Switzerland, INAF - Osservatorio Astronomico di Roma (OAR), INAF - Osservatorio Astronomico di Bologna (OABO), Department of Astronomy [Amherst], University of Massachusetts [Amherst] (UMass Amherst), University of Massachusetts System (UMASS)-University of Massachusetts System (UMASS), Space Telescope Science Institute (STSci), Institute of cosmology and gravitation, University of Portsmouth, SUPA, Institute for Astronomy, University of Edinburgh, 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: Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics
Abstract: International audience; Context. The size of a galaxy encapsulates the signature of the different physical processes driving its evolution. The distribution of galaxy sizes in the Universe as a function of cosmic time is therefore a key to understand galaxy evolution. Aims. We aim to measure the average sizes and size distributions of galaxies as they are assembling before the peak in the comoving star formation rate density of the Universe to better understand the evolution of galaxies across cosmic time. Methods. We used a sample of similar to 1200 galaxies in the COSMOS and ECDFS fields with confirmed spectroscopic redshifts 2 \textless= z(spec) \textless= 4 : 5 in the VIMOS Ultra Deep Survey (VUDS), representative of star-forming galaxies with i(AB) \textless= 25. We first derived galaxy sizes by applying a classical parametric profile-fitting method using GALFIT. We then measured the total pixel area covered by a galaxy above a given surface brightness threshold, which overcomes the difficulty of measuring sizes of galaxies with irregular shapes. We then compared the results obtained for the equivalent circularized radius enclosing 100% of the measured galaxy light r(T)(100) to those obtained with the effective radius re; circ measured with GALFIT. Results. We find that the sizes of galaxies computed with our non-parametric approach span a wide range but remain roughly constant on average with a median value r(T)(100) similar to 2 : 2 kpc for galaxies with 2 \textless z \textless 4 : 5. This is in stark contrast with the strong downward evolution of r(e) with increasing redshift, down to sizes of \textless 1 kpc at z similar to 4 : 5. We analyze the difference and find that parametric fitting of complex, asymmetric, multicomponent galaxies is severely underestimating their sizes. By comparing r(T)(100) with physical parameters obtained through fitting the spectral energy distribution we find that the star-forming galaxies that are the largest at any redshift are, on average, more massive and form more stars. We discover that galaxies present more concentrated light profiles with increasing redshifts. We interpret these results as the signature of several, possibly different, evolutionary paths of galaxies in their early stages of assembly, including major and minor merging or star formation in multiple bright regions.
Published: 2016
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8. A COHERENT STUDY OF EMISSION LINES FROM BROADBAND PHOTOMETRY: SPECIFIC STAR FORMATION RATES AND [O III]/H beta RATIO AT 3 \textless z \textless 6

Author: Faisst, A. L., Capak, P., Hsieh, B. C., Laigle, C., Salvato, M., Tasca, L., Cassata, P., Davidzon, I., Ilbert, O., Le Fevre, O., Masters, D., McCracken, H. J., Steinhardt, C., Silverman, J. D., Barros, S., Hasinger, G., Scoville, N. Z., Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Centre de résonance magnétique biologique et médicale (CRMBM), Aix Marseille Université (AMU)-Assistance Publique - Hôpitaux de Marseille (APHM)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Extraterrestrische Physik (MPE), Excellence Cluster Universe, excellence cluster centre, 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), 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), AUTRES, Institute for Astronomy [Honolulu], University of Hawai‘i [Mānoa] (UHM), California Institute of Technology (CALTECH), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-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), 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: Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics
Abstract: International audience; We measure the H alpha and [O III] emission line properties as well as specific star formation rates (sSFRs) of spectroscopically confirmed 3 \textless z \textless 6 galaxies in COSMOS from their observed colors versus redshift evolution. Our model describes consistently the ensemble of galaxies including intrinsic properties (age, metallicity, star formation history), dust attenuation, and optical emission lines. We forward-model the measured Ha. equivalent widths (EW) to obtain the sSFR out to z similar to 6 without stellar mass fitting. We find a strongly increasing rest-frame Ha. EW that is flattening off above z similar to 2.5 with average EWs of 300-600 angstrom at z similar to 6. The sSFR is increasing proportionally to (1 + z)(2.4) at z \textless 2.2 and to (1 + z)(1.5) at higher redshifts, indicative of a fast build-up of mass in high-z galaxies within e-folding times of 100-200 Myr at z similar to 6. The redshift evolution at z \textgreater 3 cannot be fully explained in a picture of growth driven by cold accretion. We find a progressively increasing [O III]lambda 5007/H beta ratio out to z similar to 6, consistent with the ratios in local galaxies selected by increasing H alpha EW (i.e., sSFR). This demonstrates the potential of using “local high-z analogs” to investigate the spectroscopic properties and relations of galaxies in the re-ionization epoch.
Published: 2016
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9. 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

10. 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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11. 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

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

Author: Amorín, R., Perez-Montero, F., Contini, T., Vílchez, 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., Renzini, A., Scodeggio, M., Bardelli, S., Bongiorno, A., Caputi, K., Cucciati, O., Torre, S., Ravel, L., Franzetti, P., Garilli, B., Iovino, A., 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., INAF - Osservatorio Astronomico di Roma (OAR), Istituto Nazionale di Astrofisica (INAF), 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), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), 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 Vienna [Vienna], University of Chicago, Ecole Polytechnique Fédérale de Lausanne (EPFL), European Southern Observatory (ESO), INAF- Milano, INAF - Osservatorio Astronomico di Bologna (OABO), College of Computing (GATECH), Georgia Institute of Technology [Atlanta], Hunan Normal University (HNU), Università degli studi di Trieste = University of Trieste, INAF - Osservatorio Astronomico di Trieste (OAT), INAF - Osservatorio Astrofisico di Arcetri (OAA), Oncology Institute of Southern Switzerland, European Project: 312725,EC:FP7:SPA,FP7-SPACE-2012-1,ASTRODEEP(2013), 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), 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), Hunan Normal University, and Università degli studi di Trieste
Subjects: Galaxies: fundamental parameters, Galaxies: star formation, Galaxies: abundances, Astrophysics::Solar and Stellar Astrophysics, Galaxies: evolution, Galaxies: irregular, Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Galaxies: starburst, Astrophysics::Galaxy Astrophysics
Abstract: International audience; 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 \textless= z \textless= 0.93 selected from the 20k zCOSMOS bright survey because of their unusually large emission line equivalent widths. 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 (\textless0.1 Z(circle dot)) EELGs. While similar to 80% of the EELGs show non-axisymmetric morphologies, including clumpy and cometary or tadpole galaxies, we find that similar to 29% of them show additional low-surface-brightness features, which strongly suggests recent or ongoing interactions. As star-forming dwarfs in the local Universe, EELGs are most often found in relative isolation. While only very few EELGs belong to compact groups, almost one third of them are found in spectroscopically confirmed loose pairs or triplets. 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
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13. Probing the galaxy-halo connection in UltraVISTA to z similar to 2

Author: McCracken, H. J., Wolk, M., Colombi, S., Kilbinger, M., Ilbert, O., Peirani, S., Coupon, J., Dunlop, J., Milvang-Jensen, B., Caputi, K., Aussel, H., Bethermin, M., Le Fevre, O., 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), AUTRES, 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), SUPA, Institute for Astronomy, University of Edinburgh, Dark Cosmology Centre (DARK), Niels Bohr Institute [Copenhagen] (NBI), Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU)-Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), European Project: 312725,EC:FP7:SPA,FP7-SPACE-2012-1,ASTRODEEP(2013), Astronomy, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), 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 Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH)-Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)
Subjects: LESS-THAN 2, Large-scale structure of Universe, Galaxies: evolution, VLT DEEP SURVEY, SPECTRAL ENERGY-DISTRIBUTIONS, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxies: formation, REDSHIFT SURVEY VIPERS, LARGE-SCALE STRUCTURE, DARK-MATTER, OCCUPATION DISTRIBUTION, LUMINOSITY DEPENDENCE, STELLAR MASS, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], PHOTOMETRIC REDSHIFTS, Astrophysics::Galaxy Astrophysics, Methods: statistical
Abstract: International audience; We use percent-level precision photometric redshifts in the UltraVISTA-DR1 near-infrared survey to investigate the changing relationship between galaxy stellar mass and the dark matter haloes hosting them to z similar to 2. We achieve this by measuring the clustering properties and abundances of a series of volume-limited galaxy samples selected by stellar mass and star formation activity. We interpret these results in the framework of a phenomenological halo model and numerical simulations. Our measurements span a uniquely large range in stellar mass and redshift and reach below the characteristic stellar mass to z similar to 2. Our results are: (1) at fixed redshift and scale, clustering amplitude depends monotonically on sample stellar mass threshold; (2) at fixed angular scale, the projected clustering amplitude decreases with redshift but the comoving correlation length remains constant; (3) characteristic halo masses and galaxy bias increase with increasing median stellar mass of the sample; (4) the slope of these relationships is modified in lower mass haloes; (5) concerning the passive galaxy population, characteristic halo masses are consistent with a simply less-abundant version of the full galaxy sample, but at lower redshifts the fraction of satellite galaxies in the passive population is very different from the full galaxy sample; (6) finally, we find that the ratio between the characteristic halo mass and median stellar mass at each redshift bin reaches a peak at log (Mh/M-circle dot) similar to 12.2 and the position of this peak remains constant out to z similar to 2. The behaviour of the full and passively evolving galaxy samples can be understood qualitatively by considering the slow evolution of the characteristic stellar mass in the redshift range probed by our survey.
Published: 2015
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14. 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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15. 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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16. The XMM-Newton Wide-Field Survey in the COSMOS field (XMM-COSMOS): demography and multiwavelength properties of obscured and unobscured luminous AGN

Author: BRUSA, MARCELLA, LUSSO, ELISABETA, VIGNALI, CRISTIAN, Civano F., Comastri A., Miyaji T., Salvato M., Zamorani G., Cappelluti N., Fiore F., Hasinger G., Mainieri V., Merloni A., Bongiorno A., Capak P., Elvis M., Gilli R., Hao H., Jahnke K., Koekemoer A. M., Ilbert O., Le Floc'h E., Mignoli M., Schinnerer E., Silverman J. D., Treister E., Trump J. D., Zamojski M., Aldcroft T., Aussel H., Bardelli S., Bolzonella M., Cappi A., Caputi K., Contini T., Finoguenov A., Fruscione A., Garilli B., Impey C. D., Iovino A., Iwasawa K., Kampczyk P., Kartaltepe J., Kneib J. P., Knobel C., Kovac K., Lamareille F., Leborgne J. F., Le Brun V., Le Fevre O., Lilly S. J., Maier C., McCracken H. J., Pello R., Peng Y. J, Perez Montero E., de Ravel L., Sanders D., Scodeggio M., Scoville N. Z., Tanaka M., Taniguchi Y., Tasca L., de la Torre S., Tresse L., Vergani D., Zucca E., Brusa M., Civano F., Comastri A., Miyaji T., Salvato M., Zamorani G., Cappelluti N., Fiore F., Hasinger G., Mainieri V., Merloni A., Bongiorno A., Capak P., Elvis M., Gilli R., Hao H., Jahnke K., Koekemoer A. M., Ilbert O., Le Floc'h E., Lusso E., Mignoli M., Schinnerer E., Silverman J. D., Treister E., Trump J. D., Vignali C., Zamojski M., Aldcroft T., Aussel H., Bardelli S., Bolzonella M., Cappi A., Caputi K., Contini T., Finoguenov A., Fruscione A., Garilli B., Impey C. D., Iovino A., Iwasawa K., Kampczyk P., Kartaltepe J., Kneib J. P., Knobel C., Kovac K., Lamareille F., Leborgne J.-F., Le Brun V., Le Fevre O., Lilly S. J., Maier C., McCracken H. J., Pello R., Peng Y-J, Perez-Montero E., de Ravel L., Sanders D., Scodeggio M., Scoville N. Z., Tanaka M., Taniguchi Y., Tasca L., de la Torre S., Tresse L., Vergani D., and Zucca E.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, galaxies: active – surveys – X-rays: diffuse background – X-rays: galaxies – X-rays: general, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We report the final optical identifications of the medium-depth (~60 ksec), contiguous (2 deg^2) XMM-Newton survey of the COSMOS field. XMM-Newton has detected ~800 X-ray sources down to limiting fluxes of ~5x10^{-16}, ~3x10^{-15}, and ~7x10^{-15} erg/cm2/s in the 0.5-2 keV, 2-10 keV and 5-10 keV bands, respectively. The work is complemented by an extensive collection of multi-wavelength data from 24 micron to UV, available from the COSMOS survey, for each of the X-ray sources, including spectroscopic redshifts for ~50% of the sample, and high-quality photometric redshifts for the rest. The XMM and multiwavelength flux limits are well matched: 1760 (98%) of the X-ray sources have optical counterparts, 1711 (~95%) have IRAC counterparts, and 1394 (~78%) have MIPS 24micron detections. Thanks to the redshift completeness (almost 100%) we were able to constrain the high-luminosity tail of the X-ray luminosity function confirming that the peak of the number density of logL_X>44.5 AGN is at z~2. Spectroscopically-identified obscured and unobscured AGN, as well as normal and starforming galaxies, present well-defined optical and infrared properties. We devised a robust method to identify a sample of ~150 high redshift (z>1), obscured AGN candidates for which optical spectroscopy is not available. We were able to determine that the fraction of the obscured AGN population at the highest (L_X>10^{44} erg s^{-1}) X-ray luminosity is ~15-30% when selection effects are taken into account, providing an important observational constraint for X-ray background synthesis. We studied in detail the optical spectrum and the overall spectral energy distribution of a prototypical Type 2 QSO, caught in a stage transitioning from being starburst dominated to AGN dominated, which was possible to isolate only thanks to the combination of X-ray and infrared observations., ApJ, in press. 59 pages, 14 figures, 2 Tables. A few typos corrected and a reference added. Table 2 is also available at http://www.mpe.mpg.de/XMMCosmos/xmm53_release ; a version of the paper in ApJ format (27 pages) is available at http://www.mpe.mpg.de/XMMCosmos/xmm53_release/brusa_xmmcosmos_optid.pdf
Published: 2010
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17. LATE-STAGE GALAXY MERGERS IN COSMOS TO z similar to 1

Author: Lackner, C. N., Silverman, J. D., Salvato, M., Kampczyk, P., Kartaltepe, J. S., Sanders, D., Capak, P., Civano, F., Halliday, C., Ilbert, O., Jahnke, K., Koekemoer, A. M., Lee, N., Le Fevre, O., Liu, C. T., Scoville, N., Sheth, K., Toft, S., 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: [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: International audience; The role of major mergers in galaxy and black hole formation is not well-constrained. To help address this, we develop an automated method to identify late-stage galaxy mergers before coalescence of the galactic cores. The resulting sample of mergers is distinct from those obtained using pair-finding and morphological indicators. Our method relies on median-filtering of high-resolution images to distinguish two concentrated galaxy nuclei at small separations. This method does not rely on low surface brightness features to identify mergers, and is therefore reliable to high redshift. Using mock images, we derive statistical contamination and incompleteness corrections for the fraction of late-stage mergers. The mock images show that our method returns an uncontaminated (\textless10%) sample of mergers with projected separations between 2.2 and 8 kpc out to z similar to 1. We apply our new method to a magnitude-limited (m(FW 814) \textless 23) sample of 44,164 galaxies from the COSMOS HST/ACS catalog. Using a mass-complete sample with log M-*/M-circle dot \textgreater 10.6 and 0.25 \textless z \textless= 1.00, we find similar to 5% of systems are late-stage mergers. Correcting for incompleteness and contamination, the fractional merger rate increases strongly with redshift as R-merge proportional to (1 + z)(3.8 +/- 0.9), in agreement both with earlier studies and with dark matter halo merger rates. Separating the sample into star-forming and quiescent galaxies shows that the merger rate for star-forming galaxies increases strongly with redshift, (1 + z)(4.5 +/- 1.3), while the merger rate for quiescent galaxies is consistent with no evolution, (1 + z)(1.1 +/- 1.2). The merger rate also becomes steeper with decreasing stellar mass. Limiting our sample to galaxies with spectroscopic redshifts from zCOSMOS, we find that the star formation rates and X-ray selected active galactic nucleus (AGN) activity in likely late-stage mergers are higher by factors of similar to 2 relative to those of a control sample. Combining our sample with more widely separated pairs, we find that 8 +/- 5% of star formation and 20 +/- 8% of AGN activity are triggered by close encounters (\textless143 kpc) or mergers, providing additional evidence that major mergers are not the only channels for star formation and black hole growth.
Published: 2014
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18. Redshift-space distortions as a probe of dark energy

Author: Guzzo L., Pierleoni M., Meneux B., 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., Foucaud S., Franzetti P., Gavignaud I., Ilbert O., Iovino A., Lamareille F., Marano B., Mazure A., Memeo P., Mellier Y., Merighi R., Moscardini L., Paltani S., Pello R., Pozzetti L., Radovich M., Vergani D., Zamorani G., Zucca E., BRANCHINI, ENZO FRANCO, L. Guzzo, M. Pierleoni, B. Meneux, E. Branchini, O. . Fevre, C. Marinoni, B. Garilli, J. Blaizot, G. . Lucia, A. Pollo, H. J. McCracken, D. Bottini, V. . Brun, D. Maccagni, J. P. Picat, R. Scaramella, M. Scodeggio, L. Tresse, G. Vettolani, A. Zanichelli, C. Adami, S. Arnout, S. Bardelli, M. Bolzonella, A. Bongiorno, A. Cappi, S. Charlot, P. Ciliegi, T. Contini, O. Cucciati, S. . La, S. Foucaud, P. Franzetti, I. Gavignaud, O. Ilbert, A. Iovino, F. Lamareille, B. Marano, A. Mazure, P. Memeo, Y. Mellier, R. Merighi, L. Moscardini, S. Paltani, R. Pello, L. Pozzetti, M. Radovich, D. Vergani, G. Zamorani, E. Zucca, Guzzo, L., Pierleoni, M., Meneux, B., Branchini, ENZO FRANCO, 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., Foucaud, S., Franzetti, P., Gavignaud, I., Ilbert, O., Iovino, A., Lamareille, F., Marano, B., Mazure, A., Memeo, P., Mellier, Y., Merighi, R., Moscardini, L., Paltani, S., Pello, R., Pozzetti, L., Radovich, M., Vergani, D., Zamorani, G., and Zucca, E.
Subjects: pancake, etc.) – Origin and formation of the Universe, great wall, Astrophysics::Cosmology and Extragalactic Astrophysics, Dark energy. – Superclusters, large-scale structure of the Universe (including void
Abstract: Measurements of the growth rate of structure f at different redshifts can discriminate the origin of cosmic acceleration. Coupled to estimates of the expansion rate H(z) as provided by Type-la supernovae or Baryonic Acoustic Oscillations, accurate measurements of f(z) are able to distinguish "dark energy" models from theories with modified gravity, as, e.g., braneworld models. These two classes are degenerate when considering the expansion history alone. We have recently shown (Nature, 451 (2008) 541) that redshift-space distortions in the clustering pattern of galaxies measured from large redshift surveys represent an extremely promising technique to trace f (z) back in time. We have measured the distortion parameter beta at z similar to 0.8 using the currently largest field of the VVDS-Wide survey, that includes more than 10000 galaxy redshifts to I(AB) = 22.5 over 4 deg(2). We obtain 0 - 0.70 +/- 0.26, corresponding to a growth rate f = 0.91 +/- 0.36, consistent with the simplest cosmological-constant scenario. Error bars are still large compared with the difference among models. However, next-generation deep surveys with N > 100000 redshifts over similar to 100deg(2) or larger, will be able to use this test as an accurate probe of the origin of cosmic acceleration.
Published: 2007

19. Tracing the cosmic growth of supermassive black holes to z similar to 3 with Herschel*

Author: Delvecchio, I., Gruppioni, C., Pozzi, F., Berta, S., Zamorani, G., Cimatti, Alessandro, Lutz, D., Scott, D., Vignali, C., Cresci, G., Feltre, A., Cooray, A., Vaccari, M., Fritz, J., Le Floc'H, E., Magnelli, B., Popesso, P., Oliver, S., Bock, J., Carollo, M., Contini, T., Le Fevre, O., Lilly, S., Mainieri, V., Renzini, A., Scodeggio, M., Commissariat à l'énergie atomique et aux énergies alternatives (CEA), 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), 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), 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), 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: [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Solar and Stellar Astrophysics, Galaxies: evolution, Astrophysics::Cosmology and Extragalactic Astrophysics, Infrared: galaxies, Astrophysics::Galaxy Astrophysics, Galaxies: nuclei
Abstract: International audience; We study a sample of Herschel selected galaxies within the Great Observatories Origins Deep Survey-South and the Cosmic Evolution Survey fields in the framework of the Photodetector Array Camera and Spectrometer (PACS) Evolutionary Probe project. Starting from the rich multiwavelength photometric data sets available in both fields, we perform a broad-band spectral energy distribution decomposition to disentangle the possible active galactic nucleus (AGN) contribution from that related to the host galaxy. We find that 37 per cent of the Herschel-selected sample shows signatures of nuclear activity at the 99 per cent confidence level. The probability of revealing AGN activity increases for bright (L1-1000 \textgreater 10(11) L-circle dot) star-forming galaxies at z \textgreater 0.3, becoming about 80 per cent for the brightest (L1-1000 \textgreater 10(12) L-circle dot) infrared (IR) galaxies at z \textgreater= 1. Finally, we reconstruct the AGN bolometric luminosity function and the supermassive black hole growth rate across cosmic time up to z similar to 3 from a far-IR perspective. This work shows general agreement with most of the panchromatic estimates from the literature, with the global black hole growth peaking at z ~ 2 and reproducing the observed local black hole mass density with consistent values of the radiative efficiency epsilon(rad) (~ 0.07).
Published: 2014
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20. Mass assembly in quiescent and star-forming galaxies since z similar or equal to 4 from UltraVISTA

Author: Ilbert, O., McCracken, H. J., Le Fevre, O., Capak, P., Dunlop, J., Karim, A., Renzini, M. A., Caputi, K., Boissier, S., Arnouts, S., Aussel, H., Comparat, J., Guo, Q., Hudelot, P., Kartaltepe, J., Kneib, J. P., Krogager, J. K., Le Floc'h, E., Lilly, S., Mellier, Y., Milvang-Jensen, B., Moutard, T., Onodera, M., Richard, J., Salvato, M., Sanders, D. B., Scoville, N., Silverman, J. D., Taniguchi, Y., Tasca, L., Thomas, Rajat, Toft, S., Tresse, L., Vergani, D., Wolk, M., Zirm, A., and Astronomy
Subjects: ACTIVE GALACTIC NUCLEI, FORMATION HISTORY, Astrophysics::Cosmology and Extragalactic Astrophysics, VLT DEEP SURVEY, SPECTRAL ENERGY-DISTRIBUTIONS, COSMOS FIELD, STELLAR POPULATION SYNTHESIS, LUMINOSITY FUNCTION, galaxies: star formation, KECK SPECTROSCOPY, galaxies: stellar content, Astrophysics::Solar and Stellar Astrophysics, galaxies: formation, galaxies: distances and redshifts, galaxies: evolution, RED SEQUENCE, PHOTOMETRIC REDSHIFTS, Astrophysics::Galaxy Astrophysics
Abstract: We estimate the galaxy stellar mass function and stellar mass density for star-forming and quiescent galaxies with 0.2 1.5 consistent with the expected uncertainties. We also develop a new method to infer the specific star formation rate from the mass function of star-forming galaxies. We find that the specific star formation rate of 10(10-10.5) M-circle dot galaxies increases continuously in the redshift range 1
Published: 2013

21. THE COLORS OF CENTRAL AND SA℡LITE GALAXIES IN zCOSMOS OUT TO z similar or equal to 0.8 AND IMPLICATIONS FOR QUENCHING

Author: Knobel, C., Lilly, S. J., Kovac, K., Peng, Y., Bschorr, T. J., Carollo, C. M., Contini, T., Kneib, J. -P., Le Fevre, O., Mainieri, V., Renzini, A., Scodeggio, M., Zamorani, G., Bardelli, S., Bolzonella, M., Bongiorno, A., Caputi, K., Cucciati, O., Torre, S., Ravel, L., Franzetti, P., Garilli, B., Iovino, A., Kampczyk, P., Lamareille, F., Le Borgne, J. -F., Le Brun, V., Maier, C., Mignoli, M., Pello, R., 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., Koekemoer, A. M., Lopez-Sanjuan, C., McCracken, H. J., Moresco, M., Nair, P., Pozzetti, L., Welikala, N., 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: [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Physics::Space Physics, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: International audience; We examine the red fraction of central and satellite galaxies in the large zCOSMOS group catalog out to z similar or equal to 0.8, correcting for both the incompleteness in stellar mass and for the less than perfect purities of the central and satellite samples. We show that at all masses and at all redshifts, the fraction of satellite galaxies that have been quenched, i.e., that are red, is systematically higher than that of centrals, as seen locally in the Sloan Digital Sky Survey (SDSS). The satellite quenching efficiency, which is the probability that a satellite is quenched because it is a satellite rather than a central, is, as locally, independent of stellar mass. Furthermore, the average value is about 0.5, which is also very similar to that seen in the SDSS. We also construct the mass functions of blue and red centrals and satellites and show that these broadly follow the predictions of the Peng et al. analysis of the SDSS groups. Together, these results indicate that the effect of the group environment in quenching satellite galaxies was very similar to what it is today when the universe was about half its present age.
Published: 2013
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22. The VIMOS VLT Deep Survey: the redshift distribution N(z) of magnitude-limited samples down to iAB=24.75 and KsAB=22

Author: Le Fevre, O., Cassata, P., Cucciati, O., La Torre, S., Garilli, B., Ilbert, O., Le Brun, V., Maccagni, D., Tresse, L., Zamorani, G., Bardelli, S., Bolzonella, M., Contini, T., Iovino, A., Lopez-Sanjuan, C., Mccracken, H. J., Pollo, A., Pozzetti, L., Scodeggio, M., Tasca, L., Vergani, D., Alessandra Zanichelli, and Zucca, E.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We measure and analyse the redshift distribution N(z) of magnitude-selected samples using spectroscopic redshift measurement from the magnitude-selected VIMOS VLT Deep Survey (VVDS) with 172. Down to iAB2 than in colour-colour selected samples, and we use the magnitude-selected VVDS to emphasize the large uncertainties associated to other surveys using colour or colour-colour selected samples. Our results further demonstrate that semi-analytical models on dark matter simulations have yet to find the right balance of physical processes and time-scales to properly reproduce a fundamental galaxy population property like the observed N(z)., Comment: Submitted to Astronomy and Astrophysics
Published: 2013
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23. Discovery of bright z similar or equal to 7 galaxies in the UltraVISTA survey

Author: Bowler, R. A. A., Dunlop, J. S., McLure, R. J., McCracken, H. J., Milvang-Jensen, B., Furusawa, H., Fynbo, J. P. U., Le Fevre, O., Holt, J., Ideue, Y., Ihara, Y., Rogers, A. B., Taniguchi, Y., 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: [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: International audience; We have exploited the new, deep, near-infrared UltraVISTA imaging of the Cosmological Evolution Survey (COSMOS) field, in tandem with deep optical and mid-infrared imaging, to conduct a new search for luminous galaxies at redshifts z similar or equal to 7. The year-one UltraVISTA data provide contiguous Y, J, H, Ks imaging over 1.5 deg(2), reaching a 5 sigma detection limit of Y + J similar or equal to 25 (AB mag, 2-arcsec-diameter aperture). The central similar or equal to 1 deg(2) of this imaging coincides with the final deep optical (u*, g, r, i) data provided by the Canada-France-Hawaii Telescope (CFHT) Legacy Survey and new deep Subaru/Suprime-Cam z'-band imaging obtained specifically to enable full exploitation of UltraVISTA. It also lies within the Hubble Space Telescope (HST) I-814 band and Spitzer/Infrared Array Camera imaging obtained as part of the COSMOS survey. We have utilized this unique multiwavelength dataset to select galaxy candidates at redshifts z \textgreater 6.5 by searching first for Y + J-detected objects which are undetected in the CFHT and HST optical data. This sample was then refined using a photometric redshift fitting code, enabling the rejection of lower redshift galaxy contaminants and cool galactic M, L, T dwarf stars. The final result of this process is a small sample of (at most) 10 credible galaxy candidates at z \textgreater 6.5 (from over 200 000 galaxies detected in the year-one UltraVISTA data) which we present in this paper. The first four of these appear to be robust galaxies at z \textgreater 6.5, and fitting to their stacked spectral energy distribution yields z(phot) = 6.98 +/- 0.05 with a stellar mass M* similar or equal to 5 x 10 M-circle dot and rest-frame ultraviolet (UV) spectral slope beta similar or equal to -2.0 +/- 0.2 (where f lambda proportional to lambda(beta)). The next three are also good candidates for z \textgreater 6.5 galaxies, but the possibility that they are dwarf stars cannot be completely excluded. Our final subset of three additional candidates is afflicted not only by potential dwarf star contamination, but also contains objects likely to lie at redshifts just below z = 6.5. We show that the three even-brighter z greater than or similar to 7 galaxy candidates reported in the COSMOS field by Capak et al. are in fact all lower redshift galaxies at z similar or equal to 1.5-3.5. Consequently the new z similar or equal to 7 galaxies reported here are the first credible z ? 7 Lyman-break galaxies discovered in the COSMOS field and, as the most UV luminous discovered to date at these redshifts, are prime targets for deep follow-up spectroscopy. We explore their physical properties, and briefly consider the implications of their inferred number density for the form of the galaxy luminosity function at z ?similar or equal to 7.
Published: 2012
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24. MASSIV: Mass Assembly Survey with SINFONI in VVDS IV. Fundamental relations of star-forming galaxies at 1 \textless z \textless 1.6

Author: Garilli, B., Kissler-Patig, M., Le Fevre, O., Moultaka, J., Paioro, L., Queyrel, J., Lopez-Sanjuan, C., Vergani, D., Epinat, B., Contini, T., Tasca, L., Tresse, L., Amram, P., 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), 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, INAF- Milano, Istituto Nazionale di Astrofisica (INAF), INAF - Osservatorio Astrofisico di Arcetri (OAA), 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), and 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)
Subjects: [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: International audience; Aims. How mass assembly occurs in galaxies and which process(es) contribute to this activity are among the most highly debated questions in galaxy formation and evolution theories. This has motivated our survey MASSIV (Mass Assembly Survey with SINFONI in VVDS) of 0.9 \textless z \textless 1.9 star-forming galaxies selected from the purely flux-limited VVDS redshift survey. Methods. We evaluate the characteristic size and stellar mass of 46 MASSIV galaxies at 1 \textless z \textless 1.6 and use the internal dynamics obtained with the SINFONI integral field spectrograph mounted at the Very Large Telescope, to derive the stellar mass-size-velocity relations. We use the Kennicutt-Schmidt formulation to estimate the gas content and compute its contribution to the total baryonic mass in MASSIV galaxies. Results. For the first time, we derive the relations between galaxy size, mass, and internal velocity, and the baryonic Tully-Fisher relation, from a statistically representative sample of star-forming galaxies at 1 \textless z \textless 1.6. We find a dynamical mass that agrees with those of rotating galaxies containing a gas fraction of similar to 20%, that is perfectly consistent with the content derived using the Kennicutt-Schmidt formulation and corresponds to the expected evolution. Non-rotating galaxies have more compact sizes for their stellar component, and are less massive than rotators, but do not have statistically different sizes for their gas-component. Discs of ionized gas have irregular, clumpy distributions, but the simplistic assumption of exponential profiles is verified. We measure a marginal evolution in the size-stellar mass and size-velocity relations in which discs become evenly smaller with cosmic time at fixed stellar mass or velocity, and are less massive at a given velocity than in the local Universe. This result is inconsistent with previous reports of an abnormal evolution in the galactic spin. The scatter in the Tully-Fisher relation is smaller when we introduce the S 05 index, which we interpret as evidence of an increase in the contribution to galactic kinematics of turbulent motions with cosmic time. We report a persistently large scatter for rotators in our relations, that we suggest is intrinsic, and possibly caused by complex physical mechanism(s) at work in our stellar mass/luminosity regime and redshift range. Conclusions. Our results consistently point towards a mild, net evolution of these relations, comparable to those predicted by cosmological simulations of disc formation. In a conflictual picture where earlier studies reported discrepant results, we place on firmer ground the measurement of a lack of any large evolution of the fundamental relations of star-forming galaxies in at least the past 8 Gyr and evidence that dark halo is strongly coupled with galactic spectrophotometric properties.
Published: 2012
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25. Discovery of bright z ~ 7 galaxies in the UltraVISTA survey

Author: Bowler, R. A. A., Dunlop, J. S., McLure, R. J., McCracken, H. J., Milvang-Jensen, B., Furusawa, H., Fynbo, J. P. U., Le Fevre, O., Holt, J., Ideue, Y., Ihara, Y., Rogers, A. B., and Taniguchi, Y.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), formation [galaxies], FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, evolution [galaxies], high-redshift [galaxies], Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We have exploited the new, deep, near-infrared UltraVISTA imaging of the COSMOS field, in tandem with deep optical and mid-infrared imaging, to conduct a new search for luminous galaxies at redshifts z ~ 7. The unique multi-wavelength dataset provided by VISTA, CFHT, Subaru, HST and Spitzer over a common area of 1 deg^2 has allowed us to select galaxy candidates at z > 6.5 by searching first for Y+J-detected (< 25 AB mag) objects which are undetected in the CFHT+HST optical data. This sample was then refined using a photometric redshift fitting code, enabling the rejection of lower-redshift galaxy contaminants and cool galactic M,L,T dwarf stars.The final result of this process is a small sample of (at most) ten credible galaxy candidates at z > 6.5 which we present in this paper. The first four of these appear to be robust galaxies at z > 6.5, and fitting to their stacked SED yields z = 6.98+-0.05 with a stellar mass M* = 5x10^9 Msun, and rest-frame UV spectral slope beta = -2.0+-0.2. The next three are also good candidates for z > 6.5 galaxies, but the possibility that they are low-redshift galaxies or dwarf stars cannot be excluded. Our final subset of three additional candidates is afflicted not only by potential dwarf-star contamination, but also contains objects likely to lie at redshifts just below z = 6.5. We show that the three even-brighter z > 7 galaxy candidates reported in the COSMOS field by Capak et al. (2011) in fact all lie at z ~ 1.5-3.5. Consequently the new z ~ 7 galaxies reported here are the first credible z ~ 7 Lyman-break galaxies discovered in the COSMOS field and, as the most UV-luminous discovered to date at these redshifts, are prime targets for deep follow-up spectroscopy. We explore their physical properties, and briefly consider the implications of their inferred number density for the form of the galaxy luminosity function at z = 7., Updated to accepted version, MNRAS. 18 pages, 9 figures, 3 tables
Published: 2012
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26. THE ROLE OF GALAXY INTERACTION IN ENVIRONMENTAL DEPENDENCE OF THE STAR FORMATION ACTIVITY AT z similar or equal to 1.2

Author: Ideue, Y., Taniguchi, Y., Nagao, T., Shioya, Y., Kajisawa, M., Trump, J. R., Vergani, D., Iovino, A., Koekemoer, A. M., Le Fevre, O., Ilbert, O., Scoville, N. Z., AUTRES, RIKEN International Frontier Research Group on Earthquakes at Earthquake Prediction Research Center, Tokai University, INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), Space Telescope Science Institute (STSci), 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 California Institute of Technology (CALTECH)
Subjects: [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: International audience; In order to understand environmental effects on star formation in high-redshift galaxies, we investigate the physical relationships between the star formation activity, stellar mass, and environment for z similar or equal to 1.2 galaxies in the 2 deg(2) COSMOS field. We estimate star formation using the [O II]lambda 3727 emission line and environment from the local galaxy density. Our analysis shows that for massive galaxies (M-* greater than or similar to 10(10) M-circle dot), the fraction of [O II] emitters in high-density environments (Sigma(10th) greater than or similar to 3.9 Mpc(-2)) is 1.7 +/- 0.4 times higher than in low-density environments (Sigma(10th) less than or similar to 1.5 Mpc(-2)), while the [O II] emitter fraction does not depend on environment for low-mass M-* less than or similar to 10(10) M-circle dot galaxies. In order to understand what drives these trends, we investigate the role of companion galaxies in our sample. We find that the fraction of [O II] emitters in galaxies with companions is 2.4 +/- 0.5 times as high as that in galaxies without companions at M-* greater than or similar to 10(10) M-circle dot. In addition, massive galaxies are more likely to have companions in high-density environments. However, although the number of star-forming galaxies increases for massive galaxies with close companions and in dense environments, the average star formation rate of star-forming galaxies at a given mass is independent of environment and the presence/absence of a close companion. These results suggest that interactions and/or mergers in a high-density environment could induce star formation in massive galaxies at z similar to 1.2, increasing the fraction of star-forming galaxies with M-* greater than or similar to 10(10) M-circle dot.
Published: 2012
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27. MASSIV: Mass Assemby Survey with SINFONI in VVDS I. Survey description and global properties of the 0.9 \textless z \textless 1.8 galaxy sample

Author: Contini, T., Garilli, B., Le Fevre, O., Kissler-Patig, M., Amram, P., Epinat, B., Moultaka, J., Paioro, L., Queyrel, J., Tasca, L., Tresse, L., Vergani, D., Lopez-Sanjuan, C., Perez-Montero, 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: [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: International audience; Aims. Understanding how galaxies evolve and assemble their mass across cosmic time is still a fundamental, unsolved issue. To get insight into the various processes of galaxy mass assembly, the Mass Assembly Survey with SINFONI in VVDS (MASSIV) aims at probing the kinematical and chemical properties of a significant and representative sample of high-redshift (0.9 \textless= z \textless= 1.8) star-forming galaxies. Methods. This paper presents the selection function, the observing strategy, and the global properties of the MASSIV sample. This sample contains 84 star-forming galaxies, selected from the VIMOS VLT Deep Survey (VVDS) and observed with the SINFONI integral-field spectrograph at the VLT. We present the redshift distribution, and derive the stellar masses and SED-based star formation rates (SFR). Integrated metallicities and the presence of type-2 AGNs are investigated using composite 1D spectra built from VIMOS and SINFONI observations. Results. The MASSIV selection function, based on star formation criteria ([O II]lambda 3727 emission-line strength up to z similar to 1.5 and colors/UV absorption lines at higher redshifts), provides a good representation of “normal” star-forming galaxies with SED-based SFRs between 5 and 400 M-circle dot yr(-1) in the stellar mass regime 10(9)-10(11) M-circle dot. Analysis of typical emission-line ratios performed on composite spectra reveals that the contamination by type-2 AGNs is very low and that the integrated metallicity of the galaxies follows the well-known mass-metallicity relation. Conclusions. The MASSIV sample has been built upon a simple selection function, fully representative of the star-forming galaxy population at 0.9 \textless z \textless 1.8 for S FR \textgreater= 5 M-circle dot yr(-1). Together with the size of the sample, the spatially-resolved SINFONI data therefore enables us to discuss global, volume averaged, galaxy kinematic, and chemical properties across the full mass and SFR range of the survey to derive robust conclusions for galaxy mass assembly on cosmological timescales. All the data published in this paper are publicly available at the time of publication following this link: http://cosmosdb.lambrate.inaf.it/VVDS-SINFONI.
Published: 2012
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28. The zCOSMOS-Bright survey: the clustering of early and late galaxy morphological types since z similar or equal to 1

Author: de la Torre, S., Le Fevre, 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., Kovac, K., Lamareille, F., Le Borgne, J. -F., Le Brun, V., Maier, C., Mignoli, M., Pello, 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., Scaramella, R., and Astronomy
Subjects: REDSHIFT SURVEY, DIGITAL-SKY-SURVEY, 2-POINT CORRELATION-FUNCTION, Astrophysics::Cosmology and Extragalactic Astrophysics, VLT DEEP SURVEY, ENVIRONMENTAL DEPENDENCE, COLD DARK-MATTER, SPECTRAL TYPE, galaxies: high-redshift, cosmology: observations, LARGE-SCALE STRUCTURE, SPECTROSCOPIC SAMPLE, LUMINOSITY DEPENDENCE, large-scale structure of Universe, galaxies: evolution, Astrophysics::Galaxy Astrophysics, galaxies: statistics
Abstract: We measure the spatial clustering of galaxies as a function of their morphological type at z similar or equal to 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 similar or equal to 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 similar or equal to 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 similar or equal to 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

29. The power spectrum from the angular distribution of galaxies in the CFHTLS-Wide fields at redshift ~0.7

Author: Krywult, J., Le Brun, V., Le Fevre, O., Maccagni, D., Malek, K., Marulli, F., Meneux, B., Paioro, L., Polletta, M., Pollo, A., Scodeggio, M., Schlagenhaufer, H., Tasca, L., Tojeiro, R., Vergani, D., Zanichelli, A., Granett, B.~R., Guzzo, L., Coupon, J., Arnouts, S., Hudelot, P., Ilbert, O., McCracken, H.~J., Mellier, Y., Adami, C., Bel, Julien, Bolzonella, M., Bottini, D., Cappi, A., Cucciati, O., Torre, S., Franzetti, P., Fritz, A., Garilli, B., Iovino, A., 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), B. R. Granett, L. Guzzo, J. Coupon, S. Arnout, P. Hudelot, O. Ilbert, H. J. McCracken, Y. Mellier, C. Adami, J. Bel, M. Bolzonella, D. Bottini, A. Cappi, O. Cucciati, S. de la Torre, P. Franzetti, A. Fritz, B. Garilli, A. Iovino, J. Krywult, V. Le Brun, O. Le Fevre, D. Maccagni, K. Malek, F. Marulli, B. Meneux, L. Paioro, M. Polletta, A. Pollo, M. Scodeggio, H. Schlagenhaufer, L. Tasca, R. Tojeiro, D. Vergani, A. Zanichelli, and University of St Andrews. School of Physics and Astronomy
Subjects: Cosmology and Gravitation, statistical [Methods], methods: statistical, cosmology: observation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Large-scale structure of Universe, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, QC Physics, cosmology: observations, QB Astronomy, [INFO]Computer Science [cs], large-scale structure of Universe, observations [Cosmology], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], QC, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, QB, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We measure the real-space galaxy power spectrum on large scales at redshifts 0.5 to 1.2 using optical colour-selected samples from the CFHT Legacy Survey. With the redshift distributions measured with a preliminary ~14000 spectroscopic redshifts from the VIMOS Public Extragalactic Redshift Survey (VIPERS), we deproject the angular distribution and directly estimate the three-dimensional power spectrum. We use a maximum likelihood estimator that is optimal for a Gaussian random field giving well-defined window functions and error estimates. This measurement presents an initial look at the large-scale structure field probed by the VIPERS survey. We measure the galaxy bias of the VIPERS-like sample to be b_g=1.38 +- 0.05 (sigma_8=0.8) on scales k, Comment: Minor changes to match journal version
Published: 2011
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30. The VIMOS-VLT Deep Survey: Dependence of galaxy clustering on stellar mass

Author: Meneux, B., Guzzo, L., Bianca Garilli, Le Fevre, O., Pollo, A., Blaizot, J., Lucia, G., Bolzonella, M., Lamareille, F., Pozzetti, L., Vvds, The Team, 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 Beaussier, Catherine
Subjects: [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We have investigated the dependence of galaxy clustering on their stellar mass at z~1, using the data from the VIMOS-VLT Deep Survey (VVDS). We have measured the projected two-point correlation function of galaxies, wp(rp) for a set of stellar mass selected samples at an effective redshift =0.85. We have control and quantify all effects on galaxy clustering due to the incompleteness of our low mass samples. We find that more massive galaxies are more clustered. When compared to similar results at z~0.1 in the SDSS, we observed no evolution of the projected correlation function for massive galaxies. These objects present a stronger linear bias at z~1 with respect to low mass galaxies. As expected, massive objects at high redshift are found in the highest pics of the dark matter density field., Comment: 4 pages, 2 figures, 43rd Rencontres de Moriond - March 15-22, 2008 - La Thuile (Val d'Aosta, Italy)
Published: 2008

31. Testing gravity on large scales. The skewness of the galaxy distribution at z~1

Author: Marinoni, C., Guzzo, L., Cappi, A., Le Fevre, O., Mazure, A., Meneux, B., Pollo, A., Iovino, A., Mccracken, H. J., Roberto Scaramella, La Torre, S., Virey, J. M., Bottini, D., Garilli, B., Le Brun, V., Maccagni, D., Picat, J. P., Scodeggio, M., Tresse, L., Vettolani, G., Zanichelli, A., Adami, C., Arnouts, S., Bardelli, S., Bolzonella, M., Charlot, S., Ciliegi, P., Contini, T., Foucaud, S., Franzetti, P., Gavignaud, I., Ilbert, O., Lamareille, F., Marano, B., Mathez, G., Merighi, R., Paltani, S., Pellò, R., Pozzetti, L., Radovich, M., Vergani, D., Zamorani, G., Zucca, E., Abbas, U., Bondi, M., Bongiorno, A., Brinchmann, J., Buzzi, A., Cucciati, O., Ravel, L., Gregorini, L., Mellier, Y., Merluzzi, P., Perez-Montero, E., Taxil, P., Temporin, S., Walcher, C. J., 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), AUTRES, Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), Istituto Nazionale di Astrofisica (INAF), INAF - Osservatorio Astronomico di Capodimonte (OAC), 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), 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), INAF- Milano, Laboratoire Astrophysique de Toulouse-Tarbes (LATT), 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, 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), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Services communs OMP - UMS 831 (UMS 831), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Toulouse III - Paul Sabatier (UT3), Università di Bologna, Dipartimento di Astronomia, Università di Bologna [Bologna] (UNIBO), Centre d'Economie et de Sociologie Rurales Appliquées à l'Agriculture et aux Espaces Ruraux (CESAER), Institut National de la Recherche Agronomique (INRA)-AgroSup Dijon - Institut National Supérieur des Sciences Agronomiques, de l'Alimentation et de l'Environnement, Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Istituto Nazionale di Astrofisica - Osservatorio Astronomico di Brera (INAF), European Southern Observatory (ESO), Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, INAF - Osservatorio Astronomico di Bologna (OAB), Observatoire de Paris - Site de Paris (OP), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto di Radioastronomia (IRA), Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto [Porto], Dipartimento di Fisica, Università degli studi di Milano [Milano]-Università di Milano-Bicocca, Departement de Radioastronomie Millimétrique (DEMIRM), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Department of Biology, University of Washington [Seattle], 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 National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), 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), 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), Services communs OMP (UMS 831), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Etablissement National d'Enseignement Supérieur Agronomique de Dijon (ENESAD)-Institut National de la Recherche Agronomique (INRA), INAF - Osservatorio Astronomico di Brera (OAB), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Istituto di Radioastronomia [Bologna] (IRA), Universidade do Porto, Università degli Studi di Milano-Bicocca [Milano] (UNIMIB)-Università degli Studi di Milano [Milano] (UNIMI), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Bernardo, Elizabeth, 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), Universidade do Porto = University of Porto, Università degli Studi di Milano-Bicocca = University of Milano-Bicocca (UNIMIB)-Università degli Studi di Milano = University of Milan (UNIMI), and École normale supérieure - Paris (ENS-PSL)
Subjects: [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics
Abstract: We study the evolution of the low-order moments of the galaxy overdensity distribution over the redshift interval 0.7, Comment: To appear in the proceedings of 43rd Rencontres de Moriond on Cosmology (La Thuile, 2008)
Published: 2008

32. Studying the evolution of large-scale structure with the VIMOS-VLT Deep Survey

Author: Guzzo, L., Le Fevre, O., Meneux, B., Pollo, A., Marinoni, Christian, Cappi, A., Cucciati, O., Garilli, B., Iovino, A., McCracken, H. J., Bottini, D., Brun, V. Le, Maccagni, D., Picat, J. P., Scaramella, R., Scodeggio, M., Tresse, L., Vettolani, G., Zanichelli, A., Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), Istituto Nazionale di Astrofisica (INAF), 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 Brera (OAB), AUTRES, 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), Services communs OMP (UMS 831), 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), Istituto di Radioastronomia [Bologna] (IRA), 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)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-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: [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: The VIMOS-VLT Deep Survey (VVDS) currently offers a unique combination of depth, angular size and number of measured galaxies among surveys of the distant Universe: ~ 11,000 spectra over 0.5 deg2 to I_{AB}=24 (VVDS-Deep), 35,000 spectra over ~ 7 deg2 to I_{AB}=22.5 (VVDS-Wide). The current ``First Epoch'' data from VVDS-Deep already allow investigations of galaxy clustering and its dependence on galaxy properties to be extended to redshifts ~1.2-1.5, in addition to measuring accurately evolution in the properties of galaxies up to z~4. This paper concentrates on the main results obtained so far on galaxy clustering. Overall, L* galaxies at z~ 1.5 show a correlation length r_0=3.6\pm 0.7. As a consequence, the linear galaxy bias at fixed luminosity rises over the same range from the value b~1 measured locally, to b=1.5 +/- 0.1. The interplay of galaxy and structure evolution in producing this observation is discussed in some detail. Galaxy clustering is found to depend on galaxy luminosity also at z~ 1, but luminous galaxies at this redshift show a significantly steeper small-scale correlation function than their z=0 counterparts. Finally, red galaxies remain more clustered than blue galaxies out to similar redshifts, with a nearly constant relative bias among the two classes, b_{rel}~1.4, despite the rather dramatic evolution of the color-density relation over the same redshift range., Comment: 14 pages. Extended, combined version of two invited review papers presented at: 1) XXVIth Astrophysics Moriond Meeting: "From Dark Halos to Light", March 2006, proc. edited by L.Tresse, S. Maurogordato and J. Tran Thanh Van (Editions Frontieres); 2) Vulcano Workshop 2006 "Frontier Objects in Astrophysics and Particle Physics", May 2006, proc. edited by F. Giovannelli & G. Mannocchi, Italian Physical Society (Editrice Compositori, Bologna)
Published: 2007

33. Seeing the Nature of the Accelerating Physics: It's a SNAP

Author: Aldering, G., Althouse, W., Amanullah, R., Annis, J., Astier, P., Baltay, C., Barrelet, E., Basa, S., Bebek, C., Bergstrom, L., Bernstein, G., Bester, M., Bigelow, B., Blandford, R., Bohlin, R., Bonissent, A., Bower, C., Brown, M., Campbell, M., Carithers, W., Commins, E., Craig, W., Day, C., Dejongh, F., Deustua, S., Diehl, T., Dodelson, S., Ealet, A., Ellis, R., Emmet, W., Fouchez, D., Frieman, J., Fruchter, A., Gerdes, D., Gladney, L., Goldhaber, G., Goobar, A., Groom, D., Heetderks, H., Hoff, M., Holland, S., Huffer, M., Hui, L., Huterer, D., Jain, B., Jelinsky, P., Karcher, A., Kent, S., Kahn, S., Kim, A., Kolbe, W., Krieger, B., Kushner, G., Kuznetsova, N., Lafever, R., Lamoureux, J., Lampton, M., Le Fevre, O., Levi, M., Limon, P., Lin, H., Linder, E., Loken, S., Lorenzon, W., Malina, R., Marriner, J., Marshall, P., Massey, R., Mazure, A., Mcginnis, B., McKay, T., McKee, S., Miquel, R., Mobqsher, B., Morgan, N., Mörtsell, E., Mostek, N., Mufson, S., Musser, J., Nakajima, R., Nugent, P., Oluseyi, H., Pain, R., Palaio, N., Pankow, D., Peoples, J., Perlmutter, S., Peterson, D., Prieto, E., Rabinowitz, D., Refregier, A., Rhodes, J., Roe, N., Rusin, D., Scarpine, V., Schubnell, M., Seiffert, M., Sholl, M., Shuka, H., Smadja, G., Smith, R.M., Smoot, G., Snyder, J., Spadafora, A., Stabenau, F., Stebbins, A., Stoughton, C., Szymkowiak, A., Tarlé, G., Taylor, K., Tilquin, A., Tomasch, A., Tucker, D., Vincent, D., Von Der Lippe, H., Walder, J.-P., Wang, Gang, Weinstein, A., Wester, W., White, M., Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Nucléaire de Lyon (IPNL), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), SNAP, Flores, Sylvie, Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)
Subjects: [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics (astro-ph), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics
Abstract: For true insight into the nature of dark energy, measurements of the precision and accuracy of the Supernova/Acceleration Probe (SNAP) are required. Precursor or scaled-down experiments are unavoidably limited, even for distinguishing the cosmological constant. This white paper presents an overview of the necessity for SNAP and the role of precursor experiments; accompanying white papers detail the supernovae and weak lensing parts of the experiment., Comment: 14 pages, 4 figures; White paper to the Dark Energy Task Force
Published: 2005
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34. First Results from a Deep Spectroscopic Survey of Faint Red Galaxies - Clues on the Nature of Low Redshift Dwarf Galaxies

Author: Laurence Tresse, Hammer, F., Le Fevre, O., Proust, D., Tresse, Laurence, Departement d'Astrophysique Extragalactique et de Cosmologie (DAEC), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Canada-France-Hawaii Telescope Corporation (CFHT), and National Research Council of Canada (NRC)-Centre National de la Recherche Scientifique (CNRS)-University of Hawai'i [Honolulu] (UH)
Subjects: Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics
Abstract: International audience; Deep multi-object spectroscopy of a sample of 44 faint galaxies selected on deep I band images is presented. The combination of long integration times with careful data reduction has led to a completeness in redshift measurement of 93% to a limiting magnitude I = 22.1. Although we have selected our galaxies from their old stellar content we confirm the existence of an over-abundant population of dwarf galaxies at low redshifts, which are probably responsible for the excess in the blue number counts. Combined with a slight deficiency of high-z galaxies (no galaxies beyond z = 1),our data provide red counts apparently consistent with an absence of luminosity and number evolution. Most of the low redshift dwarf galaxies in our sample are star-forming galaxies which is an indication of a high level of activity at relatively low redshifts. We present the discovery of a dwarf galaxy at z = 0.21, seemingly forming its first generation of population II stars, making it one of the best primordial galaxy candidate. Evidence for galaxy-galaxy interactions in several other dwarfs is presented, especially in the most active ones. We finally stress that differences between red and blue counts result from a complex mixture of effects which will have to be studied from a much larger spectroscopic sample.
Published: 1993

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

Author: Tasca, L. A. M., Le Fevre, 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., and Zucca, E.
Subjects: galaxies: high-redshift, galaxies: formation, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: 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 < 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)

36. Witnessing the build-up of the colour-density relation

Author: Cucciati, O., Iovino, A., Marinoni, C., Ilbert, O., Bardelli, S., Franzetti, P., Le Fevre, O., Pollo, A., Zamorani, G., Cappi, A., Guzzo, L., Mccracken, H. J., Meneux, B., Scaramella, R., Scodeggio, M., Tresse, L., Zucca, E., Bottini, D., Garilli, B., Le Brun, V., Maccagni, D., Picat, J. P., Vettolani, G., Zanichelli, A., Adami, C., Arnaboldi, M., Arnouts, S., Bolzonella, M., Charlot, S., Ciliegi, P., Contini, T., Foucaud, S., Gavignaud, I., Marano, B., Mazure, A., Merighi, R., Paltani, S., Pello, R., Pozzetti, L., Radovich, M., Bondi, M., Bongiorno, A., Busarello, G., La Torre, S., Gregorini, L., Lamareille, F., Mathez, G., Mellier, Y., Paola Merluzzi, Ripepi, V., Rizzo, D., Temporin, G., Vergani, D., 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 L.Tresse, S. Maurogordato and J. Tran Thanh Van
Subjects: [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We investigate the redshift and luminosity evolution of the galaxy colour-density relation using the data from the First Epoch VIMOS-VLT Deep Survey (VVDS) on scales of R=5 h^(-1)Mpc up to redshift z ~ 1.5. While at lower redshift we confirm the existence of a steep colour-density relation, with the fraction of the reddest(/bluest) galaxies of the same luminosity increasing(/decreasing) as a function of density, this trend progressively disappears in the highest redshift bins investigated.Our results suggest the existence of an epoch (more remote for brighter galaxies) characterized by the absence of the colour-density relation on the R=5 h^(-1)Mpc scales investigated. The rest frame u*-g' colour-magnitude diagram shows a bimodal pattern in both low and high density environments up to redshift z ~ 1.5. We find that the bimodal distribution is not universal but strongly depends upon environment. Both the colour-density and colour-magnitude-density relations, on the R=5 h^(-1)Mpc scales, appear to be a transient, cumulative product of genetic and environmental factors that have been operating over at least a period of 9 Gyr. These findings support an evolutionary scenario in which star formation/gas depletion processes are accelerated in more luminous objects and in high density environments: star formation activity is progressively shifting with cosmic time towards lower luminosity galaxies (downsizing), and out of high density environments., Comment: 6 pages, 3 figures, To appear in the proceedings of the XLIst Rencontres de Moriond, XXVIth Astrophysics Moriond Meeting: "From dark halos to light", Eds. L.Tresse, S. Maurogordato and J. Tran Thanh Van (Editions Frontieres)

37. The VIMOS VLT Deep Survey: Public release of 1599 redshifts to IAB<=24 across the Chandra Deep Field South

Author: Le Fevre, O., Vettolani, G., Paltani, S., Laurence Tresse, Zamorani, G., Le Brun, V., Moreau, C., Vimos Vlt Deep Survey Team, 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: [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: {This paper presents the VIMOS VLT Deep Survey around the Chandra Deep Field South (CDFS). We have measured 1599 new redshifts with VIMOS on the European Observatory Very Large Telescope - UT3, in an area 21x21.6 arcmin^2, including 784 redshifts in the Hubble Space Telescope - Advanced Camera for Surveys GOODS area. 30% of all objects with I_AB=24 have been observed independently of magnitude, indicating that the sample is purely magnitude limited. We have reached an unprecedented completeness level of 88% in terms of the ratio of secure measurements vs. observed objects, while 95% of all objects have a redshift measurement. A total of 1452 galaxies, 139 stars, 8 QSOs have a redshift identification, 141 of these being unsecure measurements. The redshift distribution down to I_AB=24 is peaked at a median redshift z=0.73, with a significant high redshift tail extending up to ~4. Several high density peaks in the distribution of galaxies are identified. In particular, the strong peak at z=0.735 contains more than 130 galaxies in a velocity range +/-2000 km/s distributed all across the transverse ~20 h^-1 Mpc of the survey. We are releasing all redshifts to the community, along with the cross identification with HST-ACS GOODS sources on the CENCOS database environment http://cencosw.oamp.fr., Comment: 9 pages, 8 figures (figure 8 is too big to be compressed for astro-ph), submitted to Astronomy and Astrophysics. The uncompressed version can be found on cencosw.oamp.fr

38. Galaxy luminosity function per morphological type up to z=1.2

Author: Ilbert, O., Lauger, S., Tresse, L., Buat, V., Arnout, S., Le Fevre, O., Burgarella, D., Zucca, E., Bardelli, S., Zamorani, G., Bottini, D., Garilli, B., Le Brun, V., Maccagni, D., Picat, J. -P, Scaramella, R., Scodeggio, M., Vettolani, G., Zanichelli, A., Adami, C., Arnaboldi, M., Bolzonella, M., Cappi, A., Charlot, S., Contini, T., Foucaud, S., Franzetti, P., Gavignaud, I., Guzzo, L., Iovino, A., Mccracken, H. J., Marano, B., Marinoni, C., Mathez, G., Mazure, A., Meneux, B., Roberto Merighi, Paltani, S., Pello, R., Pollo, A., Pozzetti, L., Radovich, M., Bondi, M., Bongiorno, A., Busarello, G., Ciliegi, P., Mellier, Y., Merluzzi, P., Ripepi, V., Rizzo, D., 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: [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We have computed the evolution of the rest-frame B-band luminosity function (LF) for bulge and disk-dominated galaxies since z=1.2. We use a sample of 605 spectroscopic redshifts with I_{AB}0.9 and bright galaxies showing a strongly decreasing LF slope \alpha=+0.55 \pm 0.21, and 32% of blue (B-I)_{AB}, Comment: 9 pages, 4 figures, 2 tables, accepted for publication in Astronomy and Astrophysics

39. The ALPINE−ALMA [C <scp>ii</scp>] Survey: on the nature of an extremely obscured serendipitous galaxy

Author: S. Bardelli, Paolo Cassata, G. C. Jones, Michele Ginolfi, Andreas L. Faisst, L. Morselli, Livia Vallini, Matthieu Béthermin, O. Le Fevre, D. Vergani, Y. Fudamoto, Miroslava Dessauges-Zavadsky, G. Rodighiero, E. Zucca, Edo Ibar, Margherita Talia, John D. Silverman, Dominik Riechers, Brian C. Lemaux, Peter Capak, Daniel Schaerer, Seiji Fujimoto, A. Enia, Médéric Boquien, Lin Yan, Andrea Cimatti, Chiara Mancini, L. Rodríguez-Muñoz, F. Loiacono, G. Zamorani, M. Romano, Nimish P. Hathi, Carlotta Gruppioni, Anton M. Koekemoer, 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), Romano, M., Cassata, P., Morselli, L., Lemaux, B. C., Bethermin, M. M., Capak, P., Faisst, A., Le Fevre, O., Schaerer, D., Silverman, J., Yan, L., Bardelli, S., Boquien, M., Cimatti, A., Dessauges-Zavadsky, M., Enia, A., Fudamoto, Y., Fujimoto, S., Ginolfi, M., Gruppioni, C., Hathi, N. P., Ibar, E., Jones, G. C., Koekemoer, A. M., Loiacono, F., Mancini, C., Riechers, D. A., Rodighiero, G., Rodriguez-Munoz, L., Talia, M., Vallini, L., Vergani, D., Zamorani, G., Zucca, E., Romano M., Cassata P., Morselli L., Lemaux B.C., Bethermin M.M., Capak P., Faisst A., Le Fevre O., Schaerer D., Silverman J., Yan L., Bardelli S., Boquien M., Cimatti A., Dessauges-Zavadsky M., Enia A., Fudamoto Y., Fujimoto S., Ginolfi M., Gruppioni C., Hathi N.P., Ibar E., Jones G.C., Koekemoer A.M., Loiacono F., Mancini C., Riechers D.A., Rodighiero G., Rodriguez-Munoz L., Talia M., Vallini L., Vergani D., Zamorani G., and Zucca E.
Subjects: Stellar mass, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, MASS, 01 natural sciences, Luminosity, Settore FIS/05 - Astronomia e Astrofisica, galaxies: high-redshift, 0103 physical sciences, STAR-FORMING GALAXIES, PHOTOMETRIC REDSHIFTS, 010303 astronomy & astrophysics, Reionization, evolution [galaxies], Astrophysics::Galaxy Astrophysics, COSMOS, Physics, galaxies: evolution, SUBMILLIMETER GALAXIES, INTERSTELLAR-MEDIUM, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, DUST CONTENT, Atacama Large Millimeter Array, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, STELLAR, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Spectral energy distribution, Astrophysics::Earth and Planetary Astrophysics, EMISSION, FAR-INFRARED SPECTROSCOPY, high-redshift [galaxies]
Abstract: We report the serendipitous discovery of a bright galaxy (Gal-A) observed as part of the ALMA Large Program to INvestigate [CII] at Early times (ALPINE). While this galaxy is detected both in line and continuum emission in ALMA Band 7, it is completely dark in UV/optical filters and only presents a marginal detection in the UltraVISTA Ks band. We discuss the nature of the observed ALMA line, i.e. whether the emission comes from [CII] at z~4.6, or from high-J CO transitions at z~2.2. In the first case we find a [CII]-to-FIR luminosity ratio of log(L_[CII]/L_FIR)=-2.5, consistent with the average value for local star-forming galaxies (SFGs); in the second case, instead, the source would lie outside of the empirical relations between L_CO and L_FIR found in the literature. At both redshifts, we derive the star-formation rate (SFR) from the ALMA continuum, and the stellar mass (M*) by using stellar population synthesis models as input for LePHARE spectral energy distribution (SED) fitting. Exploiting our results, we believe that Gal-A is a Main-Sequence (MS), dusty SFG at z=4.6 (i.e. [CII] emitter) with log(SFR/[M/yr])~1.4 and log(M*/M)~9.7. This work underlines the crucial role of the ALPINE survey in making a census of this class of objects, in order to unveil their contribution to the global star-formation rate density (SFRD) of the Universe at the end of the Reionisation epoch., Comment: 13 pages, 6 figures. Submitted to MNRAS
Published: 2020
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40. The ALPINE-ALMA [CII] survey : dust mass budget in the early Universe

Author: John D. Silverman, S. Bardelli, E. Zucca, Y. Khusanova, Roberto Decarli, Roberto Maiolino, M. Romano, Margherita Talia, Dominik A. Riechers, Peter Capak, Nimish P. Hathi, G. Zamorani, G. Rodighiero, Livia Vallini, A. Enia, Matthieu Béthermin, O. Le Fèvre, Anton M. Koekemoer, Y. Fudamoto, Paolo Cassata, Andrea Cimatti, Michele Ginolfi, Andreas L. Faisst, Lin Yan, Daniel Schaerer, Miroslava Dessauges-Zavadsky, Médéric Boquien, Francesca Pozzi, F. Loiacono, G. C. Jones, Carlotta Gruppioni, Desika Narayanan, Brian C. Lemaux, Francesco Calura, Daniela Vergani, Pozzi, F., Calura, F., Fudamoto, Y., Dessauges-Zavadsky, M., Gruppioni, C., Talia, M., Zamorani, G., Bethermin, M., Cimatti, A., Enia, A., Khusanova, Y., Decarli, R., Le Fevre, O., Capak, P., Cassata, P., Faisst, A. L., Yan, L., Schaerer, D., Silverman, J., Bardelli, S., Boquien, M., Narayanan, D., Ginolfi, M., Hathi, N. P., Jones, G. C., Koekemoer, A. M., Lemaux, B. C., Loiacono, F., Maiolino, R., Riechers, D. A., Rodighiero, G., Romano, M., Vallini, L., Vergani, D., Zucca, E., Jones, Gareth [0000-0002-0267-9024], Maiolino, Roberto [0000-0002-4985-3819], Apollo - University of Cambridge Repository, 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), Pozzi F., Calura F., Fudamoto Y., Dessauges-Zavadsky M., Gruppioni C., Talia M., Zamorani G., Bethermin M., Cimatti A., Enia A., Khusanova Y., Decarli R., Le Fevre O., Capak P., Cassata P., Faisst A.L., Yan L., Schaerer D., Silverman J., Bardelli S., Boquien M., Narayanan D., Ginolfi M., Hathi N.P., Jones G.C., Koekemoer A.M., Lemaux B.C., Loiacono F., Maiolino R., Riechers D.A., Rodighiero G., Romano M., Vallini L., Vergani D., and Zucca E.
Subjects: Extinction (astronomy), Continuum (design consultancy), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Disc galaxy, 01 natural sciences, Luminosity, high-redshift [Galaxies], Settore FIS/05 - Astronomia e Astrofisica, galaxies: high-redshift, 0103 physical sciences, ISM [Galaxies], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Luminosity function (astronomy), Physics, 010308 nuclear & particles physics, extinction, Astronomy and Astrophysics, Dust, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Elliptical galaxy, dust, dust, extinction, Astrophysics::Earth and Planetary Astrophysics, galaxies: ISM
Abstract: The dust content of normal galaxies and the dust mass density (DMD) at high-z (z>4) are unconstrained given the source confusion and the sensitivity limitations of previous observations. The ALMA Large Program to INvestigate [CII] at Early Times (ALPINE), which targeted 118 UV-selected star-forming galaxies at 4.4, Comment: 16 pages, 6 figures. Accepted for publication in A&A
Published: 2021
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41. The ALPINE-ALMA [CII] survey:Molecular gas budget in the early Universe as traced by [CII]

Author: Andrea Cimatti, S. Bardelli, Andreas L. Faisst, E. Zucca, G. Rodighiero, Y. Khusanova, Daniel Schaerer, Pascal Oesch, Sune Toft, Paolo Cassata, Livia Vallini, Nimish P. Hathi, Carlotta Gruppioni, M. Romano, Francesca Pozzi, F. Loiacono, G. Zamorani, Michele Ginolfi, Lin Yan, John D. Silverman, Miroslava Dessauges-Zavadsky, Anton M. Koekemoer, Y. Fudamoto, G. C. Jones, Desika Narayanan, Margherita Talia, Brian C. Lemaux, Daniela Vergani, Seiji Fujimoto, Peter Capak, Edo Ibar, Médéric Boquien, Matthieu Béthermin, O. Le Fevre, Ricardo Amorín, 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), Dessauges-Zavadsky M., Ginolfi M., Pozzi F., Bethermin M., Le Fevre O., Fujimoto S., Silverman J.D., Jones G.C., Vallini L., Schaerer D., Faisst A.L., Khusanova Y., Fudamoto Y., Cassata P., Loiacono F., Capak P.L., Yan L., Amorin R., Bardelli S., Boquien M., Cimatti A., Gruppioni C., Hathi N.P., Ibar E., Koekemoer A.M., Lemaux B.C., Narayanan D., Oesch P.A., Rodighiero G., Romano M., Talia M., Toft S., Vergani D., Zamorani G., Zucca E., Dessauges-Zavadsky, M., Ginolfi, M., Pozzi, F., Bethermin, M., Le Fevre, O., Fujimoto, S., Silverman, J. D., Jones, G. C., Vallini, L., Schaerer, D., Faisst, A. L., Khusanova, Y., Fudamoto, Y., Cassata, P., Loiacono, F., Capak, P. L., Yan, L., Amorin, R., Bardelli, S., Boquien, M., Cimatti, A., Gruppioni, C., Hathi, N. P., Ibar, E., Koekemoer, A. M., Lemaux, B. C., Narayanan, D., Oesch, P. A., Rodighiero, G., Romano, M., Talia, M., Toft, S., Vergani, D., Zamorani, G., and Zucca, E.
Subjects: C-II, Stellar mass, MASS-METALLICITY RELATION, FOS: Physical sciences, DUST, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, CONVERSION FACTOR, SCALING RELATIONS, 01 natural sciences, Settore FIS/05 - Astronomia e Astrofisica, galaxies: high-redshift, 0103 physical sciences, STAR-FORMING GALAXIES, Astrophysics::Solar and Stellar Astrophysics, MAIN-SEQUENCE, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, evolution [galaxies], molecules [ISM], Physics, LEGACY SURVEY, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], ISM [galaxies], 010308 nuclear & particles physics, Star formation, Gas depletion, Gas supply, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, ISM: molecules, EVOLUTION, MODEL, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), Halo, galaxies: evolution, Cosmic time, galaxies: ISM, high-redshift [galaxies]
Abstract: The molecular gas content of normal galaxies at z>4 is poorly constrained, because the commonly used molecular gas tracers become hard to detect. We use the [CII]158um luminosity, recently proposed as a molecular gas tracer, to estimate the molecular gas content in a large sample of main-sequence star-forming galaxies at z=4.4-5.9, with a median stellar mass of 10^9.7 Msun, drawn from the ALMA Large Program to INvestigate [CII] at Early times (ALPINE) survey. The agreement between molecular gas masses derived from [CII] luminosity, dynamical mass, and rest-frame 850um luminosity, extrapolated from the rest-frame 158um continuum, supports [CII] as a reliable tracer of molecular gas in our sample. We find a continuous decline of the molecular gas depletion timescale from z=0 to z=5.9, which reaches a mean value of (4.6+/-0.8)x10^8 yr at z~5.5, only a factor of 2-3 shorter than in present-day galaxies. This suggests a mild enhancement of star formation efficiency toward high redshifts, unless the molecular gas fraction significantly increases. Our estimates show that the rise in molecular gas fraction as reported previously, flattens off above z~3.7 to achieve a mean value of 63%+/-3 over z=4.4-5.9. This redshift evolution of the gas fraction is in line with the one of the specific star formation rate. We use multi-epoch abundance matching to follow the gas fraction evolution over cosmic time of progenitors of z=0 Milky Way-like galaxies in 10^13 Msun halos and of more massive z=0 galaxies in 10^14 Msun halos. Interestingly, the former progenitors show a monotonic decrease of the gas fraction with cosmic time, while the latter show a constant gas fraction from z=5.9 to z~2 and a decrease at z, 16 pages, 9 figures, 2 tables. Submitted to Astronomy & Astrophysics
Published: 2020
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42. The ALPINE-ALMA [CII] survey: Dust attenuation properties and obscured star formation at z~4.4-5.8

Author: Anton M. Koekemoer, Margherita Talia, Guilaine Lagache, Ricardo Amorín, Desika Narayanan, G. Rodighiero, Sune Toft, Brian C. Lemaux, G. Zamorani, Miroslava Dessauges-Zavadsky, Livia Vallini, Y. Khusanova, Matthieu Béthermin, Roberto Maiolino, Andrea Cimatti, Lin Yan, Daniela Vergani, Y. Fudamoto, Francesca Pozzi, Nimish P. Hathi, F. Loiacono, Michele Ginolfi, Edo Ibar, Seiji Fujimoto, S. Bardelli, Médéric Boquien, G. C. Jones, Carlotta Gruppioni, Daniel Schaerer, Andreas L. Faisst, O. Le Fèvre, E. Zucca, Dominik A. Riechers, John D. Silverman, Pascal Oesch, Peter Capak, Paolo Cassata, 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), Fudamoto Y., Oesch P.A., Faisst A., Bethermin M., Ginolfi M., Khusanova Y., Loiacono F., Le Fevre O., Capak P., Schaerer D., Silverman J.D., Cassata P., Yan L., Amorin R., Bardelli S., Boquien M., Cimatti A., Dessauges-Zavadsky M., Fujimoto S., Gruppioni C., Hathi N.P., Ibar E., Jones G.C., Koekemoer A.M., Lagache G., Lemaux B.C., Maiolino R., Narayanan D., Pozzi F., Riechers D.A., Rodighiero G., Talia M., Toft S., Vallini L., Vergani D., Zamorani G., Zucca E., Fudamoto, Y., Oesch, P. A., Faisst, A., Bethermin, M., Ginolfi, M., Khusanova, Y., Loiacono, F., Le Fevre, O., Capak, P., Schaerer, D., Silverman, J. D., Cassata, P., Yan, L., Amorin, R., Bardelli, S., Boquien, M., Cimatti, A., Dessauges-Zavadsky, M., Fujimoto, S., Gruppioni, C., Hathi, N. P., Ibar, E., Jones, G. C., Koekemoer, A. M., Lagache, G., Lemaux, B. C., Maiolino, R., Narayanan, D., Pozzi, F., Riechers, D. A., Rodighiero, G., Talia, M., Toft, S., Vallini, L., Vergani, D., Zamorani, G., Zucca, E., Jones, Gareth [0000-0002-0267-9024], Maiolino, Roberto [0000-0002-4985-3819], and Apollo - University of Cambridge Repository
Subjects: Stellar mass, Extinction (astronomy), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, high-redshift [Galaxies], Settore FIS/05 - Astronomia e Astrofisica, galaxies: high-redshift, 0103 physical sciences, ISM [Galaxies], Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Reionization, Astrophysics::Galaxy Astrophysics, Physics, Infrared excess, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Star formation, extinction, Astronomy and Astrophysics, Dust, Extinction, Atacama Large Millimeter Array, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), dust, Astrophysics::Earth and Planetary Astrophysics, galaxies: ISM
Abstract: We present dust attenuation properties of spectroscopically confirmed star forming galaxies on the main sequence at a redshift of ~4.4-5.8. Our analyses are based on the far infrared continuum observations of 118 galaxies at rest-frame 158��m obtained with the Atacama Large Millimeter Array (ALMA) Large Program to INvestigate [CII] at Early times (ALPINE). We study the connection between the ultraviolet (UV) spectral slope ($��$), stellar mass (M_*), and infrared excess (IRX=L_IR/L_UV). Twenty-three galaxies are individually detected in the continuum at >3.5 sigma significance. We perform a stacking analysis using both detections and nondetections to study the average dust attenuation properties at z~4.4-5.8. The individual detections and stacks show that the IRX-$��$ relation at z~5 is consistent with a steeper dust attenuation curve than typically found at lower redshifts (z4. Similarly, we find that our galaxies have lower IRX values, up to 1dex on average, at a fixed mass compared to previously studied IRX-M_* relations at z4 are characterised by (i) a steeper attenuation curve than at z10) at z~5-6 already exhibit an obscured fraction of star formation of ~45%, indicating a rapid build-up of dust during the epoch of reionization., 12 pages, 6 figures. accepted for publication in Astronomy & Astrophysics. Minor revisions
Published: 2020
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43. The ALPINE-ALMA [CII] survey: Survey strategy, observations and sample properties of 118 star-forming galaxies at $4 < z < 6$

Author: M. Bethermin, Carlotta Gruppioni, Shoubaneh Hemmati, Lin Yan, G. Zamorani, Michele Ginolfi, Andreas L. Faisst, E. Zucca, Fabian Walter, G. Lagache, Francesca Pozzi, F. Loiacono, Edo Ibar, Médéric Boquien, Ricardo Amorín, Nick Scoville, Daniel Schaerer, Anton M. Koekemoer, Y. Khusanova, Pascal Oesch, Dominik Riechers, Desika Narayanan, Andrea Cimatti, John D. Silverman, Nimish P. Hathi, Sune Toft, Brian C. Lemaux, Livia Vallini, Chiara Mancini, Miroslava Dessauges-Zavadsky, H. Mendez-Hernandez, R. Thomas, L. Morselli, G. C. Jones, Mauro Giavalisco, L. A. M. Tasca, Paolo Cassata, Roberto Maiolino, Peter Capak, O. Le Fevre, M. Romano, D. Vergani, S. Bardelli, Margherita Talia, Seiji Fujimoto, Y. Fudamoto, 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 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), ALPINE Team, 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), 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), 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), Le Fevre, O., Bethermin, M., Faisst, A., Jones, G. C., Capak, P., Cassata, P., Silverman, J. D., Schaerer, D., Yan, L., Amorin, R., Bardelli, S., Boquien, M., Cimatti, A., Dessauges-Zavadsky, M., Giavalisco, M., Hathi, N. P., Fudamoto, Y., Fujimoto, S., Ginolfi, M., Gruppioni, C., Hemmati, S., Ibar, E., Koekemoer, A., Khusanova, Y., Lagache, G., Lemaux, B. C., Loiacono, F., Maiolino, R., Mancini, C., Narayanan, D., Morselli, L., Mendez-Hernandez, H., Oesch, P. A., Pozzi, F., Romano, M., Riechers, D., Scoville, N., Talia, M., Tasca, L. A. M., Thomas, R., Toft, S., Vallini, L., Vergani, D., Walter, F., Zamorani, G., Zucca, E., Le Fevre O., Bethermin M., Faisst A., Jones G.C., Capak P., Cassata P., Silverman J.D., Schaerer D., Yan L., Amorin R., Bardelli S., Boquien M., Cimatti A., Dessauges-Zavadsky M., Giavalisco M., Hathi N.P., Fudamoto Y., Fujimoto S., Ginolfi M., Gruppioni C., Hemmati S., Ibar E., Koekemoer A., Khusanova Y., Lagache G., Lemaux B.C., Loiacono F., Maiolino R., Mancini C., Narayanan D., Morselli L., Mendez-Hernandez H., Oesch P.A., Pozzi F., Romano M., Riechers D., Scoville N., Talia M., Tasca L.A.M., Thomas R., Toft S., Vallini L., Vergani D., Walter F., Zamorani G., and Zucca E.
Subjects: formation [galaxies], Population, REDSHIFT, BILLION YEARS, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, COOL GAS, Far infrared, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, galaxies: formation, MAIN-SEQUENCE, FIELD, education, 010303 astronomy & astrophysics, Reionization, BLACK-HOLES, evolution [galaxies], Astrophysics::Galaxy Astrophysics, Physics, EVOLUTION SURVEY COSMOS, education.field_of_study, 010308 nuclear & particles physics, James Webb Space Telescope, Astronomy and Astrophysics, FRAMEWORK, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, C II EMISSION, SIMULATIONS, Reference sample, Space and Planetary Science, galaxies: star formation, Spectral energy distribution, Astrophysics::Earth and Planetary Astrophysics, star formation [galaxies], galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The ALMA-ALPINE [CII] survey is aimed at characterizing the properties of a sample of normal star-forming galaxies (SFGs). The ALMA Large Program to INvestigate (ALPINE) features 118 galaxies observed in the [CII]-158$\mu$m line and far infrared (FIR) continuum emission during the period of rapid mass assembly, right after the end of the HI reionization, at redshifts of 45). Based on a visual inspection of the [CII] data cubes together with the large wealth of ancillary data, we find a surprisingly wide range of galaxy types, including 40% that are mergers, 20% extended and dispersion-dominated, 13% compact, and 11% rotating discs, with the remaining 16% too faint to be classified. This diversity indicates that a wide array of physical processes must be at work at this epoch, first and foremost, those of galaxy mergers. This paper sets a reference sample for the gas distribution in normal SFGs at 4, Comment: 20 pages, 13 figures, 1 table, accepted by A&A
Published: 2020
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44. The ALPINE-ALMA [CII] survey: Circumgalactic medium pollution and gas mixing by tidal stripping in a merging system at z ∼4.57

Author: Roberto Maiolino, Andreas L. Faisst, Brian C. Lemaux, John D. Silverman, G. C. Jones, Paolo Cassata, Y. Fudamoto, G. Zamorani, L. Morselli, Matthieu Béthermin, Peter Capak, Carlotta Gruppioni, O. Le Fevre, S. Carniani, Seiji Fujimoto, Nimish P. Hathi, D. Vergani, Michele Ginolfi, Lin Yan, O. Cucciati, Margherita Talia, S. Bardelli, Pascal Oesch, Daniel Schaerer, Lori M. Lubin, Roy R. Gal, Debora Pelliccia, Miroslava Dessauges-Zavadsky, Ginolfi, M., Jones, G. C., Bethermin, M., Faisst, A., Lemaux, B. C., Schaerer, D., Fudamoto, Y., Oesch, P., Dessauges-Zavadsky, M., Fujimoto, S., Carniani, Stefano, Le Fevre, O., Cassata, P., Silverman, J. D., Capak, P., Yan, L., Bardelli, S., Cucciati, O., Gal, R., Gruppioni, C., Hathi, N. P., Lubin, L., Maiolino, R., Morselli, L., Pelliccia, D., Talia, M., Vergani, D., Zamorani, G., 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), Ginolfi M., Jones G.C., Bethermin M., Faisst A., Lemaux B.C., Schaerer D., Fudamoto Y., Oesch P., Dessauges-Zavadsky M., Fujimoto S., Carniani S., Le Fevre O., Cassata P., Silverman J.D., Capak P., Yan L., Bardelli S., Cucciati O., Gal R., Gruppioni C., Hathi N.P., Lubin L., Maiolino R., Morselli L., Pelliccia D., Talia M., Vergani D., and Zamorani G.
Subjects: Stellar mass, REDSHIFT, Continuum (design consultancy), interaction [Galaxies], Flux, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, STAR-FORMATION, Gravitation, high-redshift [Galaxies], C-II LINE, Settore FIS/05 - Astronomia e Astrofisica, galaxies: high-redshift, METAL ENRICHMENT, 0103 physical sciences, ISM [Galaxies], galaxies: interactions, galaxies: formation, 010303 astronomy & astrophysics, MASS-RATIO, Astrophysics::Galaxy Astrophysics, Envelope (waves), Intergalactic medium, Physics, interactions [galaxies], 010308 nuclear & particles physics, Star formation, GALAXY MERGERS, Astronomy and Astrophysics, DUST CONTENT, evolution [Galaxies], formation [Galaxies], MOLECULAR GAS, EVOLUTION, Galaxy, Baryon, Galaxies: interaction, 13. Climate action, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, intergalactic medium, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], LAMBDA-CDM, galaxies: ISM
Abstract: We present ALMA observations of a merging system atz ∼ 4.57, observed as a part of the ALMA Large Program to INvestigate [CII] at Early times (ALPINE) survey. Combining ALMA [CII]158 μm and far-infrared continuum data with multi-wavelength ancillary data, we find that the system is composed of two massive (M⋆ ≳ 1010 M⊙) star-forming galaxies experiencing a major merger (stellar mass ratiormass ≳ 0.9) at close spatial (∼13 kpc; projected) and velocity (Δv < 300 km s−1) separations, and two additional faint narrow [CII]-emitting satellites. The overall system belongs to a larger scale protocluster environment and is coincident to one of its overdensity peaks. Additionally, ALMA reveals the presence of [CII] emission arising from a circumgalactic gas structure, extending up to a diameter-scale of ∼30 kpc. Our morpho-spectral decomposition analysis shows that about 50% of the total flux resides between the individual galaxy components, in a metal-enriched gaseous envelope characterised by a disturbed morphology and complex kinematics. Similarly to observations of shock-excited [CII] emitted from tidal tails in local groups, our results can be interpreted as a possible signature of interstellar gas stripped by strong gravitational interactions, with a possible contribution from material ejected by galactic outflows and emission triggered by star formation in small faint satellites. Our findings suggest that mergers could be an efficient mechanism of gas mixing in the circumgalactic medium around high-zgalaxies, and thus play a key role in the galaxy baryon cycle at early epochs.
Published: 2020
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45. The ALPINE-ALMA [C II] survey : star-formation-driven outflows and circumgalactic enrichment in the early Universe

Author: Michele Ginolfi, G. Rodighiero, Roberto Maiolino, Edo Ibar, Médéric Boquien, D. Vergani, Francesca Pozzi, F. Loiacono, Sune Toft, Carlotta Gruppioni, Lin Yan, Livia Vallini, Matthieu Béthermin, O. Le Fevre, S. Bardelli, G. C. Jones, G. Zamorani, R. Carraro, Andreas L. Faisst, Miroslava Dessauges-Zavadsky, Desika Narayanan, Daniel Schaerer, Brian C. Lemaux, Y. Khusanova, Y. Fudamoto, Pascal Oesch, Margherita Talia, Seiji Fujimoto, Peter Capak, Paolo Cassata, John D. Silverman, Mauro Giavalisco, Ginolfi, M., Jones, G. C., Bethermin, M., Fudamoto, Y., Loiacono, F., Fujimoto, S., Le Fevre, O., Faisst, A., Schaerer, D., Cassata, P., Silverman, J. D., Yan, L., Capak, P., Bardelli, S., Boquien, M., Carraro, R., Dessauges-Zavadsky, M., Giavalisco, M., Gruppioni, C., Ibar, E., Khusanova, Y., Lemaux, B. C., Maiolino, R., Narayanan, D., Oesch, P., Pozzi, F., Rodighiero, G., Talia, M., Toft, S., Vallini, L., Vergani, D., Zamorani, G., Ginolfi, M, Jones, GC, Bethermin, M, Fudamoto, Y, Loiacono, F, Fujimoto, S, Le Fevre, O, Faisst, A, Schaerer, D, Cassata, P, Silverman, JD, Yan, L, Capak, P, Bardelli, S, Boquien, M, Carraro, R, Dessauges-Zavadsky, M, Giavalisco, M, Gruppioni, C, Ibar, E, Khusanova, Y, Lemaux, BC, Maiolino, R, Narayanan, D, Oesch, P, Pozzi, F, Rodighiero, G, Talia, M, Toft, S, Vallini, L, Vergani, D, Zamorani, G, 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), Jones, Gareth [0000-0002-0267-9024], Maiolino, Roberto [0000-0002-4985-3819], and Apollo - University of Cambridge Repository
Subjects: media_common.quotation_subject, astro-ph.GA, Continuum (design consultancy), Stacking, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Computer Science::Computational Geometry, 01 natural sciences, star formation [Galaxies], high-redshift [Galaxies], Settore FIS/05 - Astronomia e Astrofisica, galaxies: high-redshift, 0103 physical sciences, ISM [Galaxies], galaxies: formation, 010303 astronomy & astrophysics, ISM: jets and outflow, Astrophysics::Galaxy Astrophysics, media_common, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Star formation, jets and outflows [ISM], Astronomy and Astrophysics, evolution [Galaxies], Astrophysics - Astrophysics of Galaxies, formation [Galaxies], Universe, Galaxy, Large sample, Baryon, ISM: jets and outflows, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), galaxies: star formation, galaxies: evolution, galaxies: ISM, Outflow
Abstract: We study the efficiency of galactic feedback in the early Universe by stacking the [C II] 158 um emission in a large sample of normal star-forming galaxies at 4 < z < 6 from the ALMA Large Program to INvestigate [C II] at Early times (ALPINE) survey. Searching for typical signatures of outflows in the high-velocity tails of the stacked [C II] profile, we observe (i) deviations from a single-component Gaussian model in the combined residuals and (ii) broad emission in the stacked [C II] spectrum, with velocities of |v| 4. From the stacking analysis of the datacubes, we find that the combined [C II] core emission (|v|< 200 km/s) of the higher-SFR galaxies is extended on physical sizes of ~ 30 kpc (diameter scale), well beyond the analogous [C II] core emission of lower-SFR galaxies and the stacked far-infrared continuum. The detection of such extended metal-enriched gas, likely tracing circumgalactic gas enriched by past outflows, corroborates previous similar studies, confirming that baryon cycle and gas exchanges with the circumgalactic medium are at work in normal star-forming galaxies already at early epochs., Comment: 16 pages, 10 figures. Accepted for publication in A&A
Published: 2020
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46. The ALPINE-ALMA [CII] survey - The nature, luminosity function, and star formation history of dusty galaxies up to z ≃ 6

Author: Pascal Oesch, Paolo Cassata, Dominik A. Riechers, Giulia Rodighiero, Peter Capak, E. Zucca, Nimish P. Hathi, Daniel Schaerer, Andrea Cimatti, G. Zamorani, Andreas L. Faisst, Michele Ginolfi, O. Le Fèvre, Seiji Fujimoto, John D. Silverman, Margherita Talia, G. C. Jones, Carlotta Gruppioni, Guilaine Lagache, Matthieu Béthermin, R. Carraro, Y. Khusanova, M. Romano, S. Bardelli, Livia Vallini, Francesca Pozzi, F. Loiacono, Brian C. Lemaux, Miroslava Dessauges-Zavadsky, Lin Yan, Daniela Vergani, Anton M. Koekemoer, Médéric Boquien, INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), 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), California Institute of Technology (CALTECH), INAF - Osservatorio Astronomico di Padova (OAPD), Université de Genève = University of Geneva (UNIGE), The University of Tokyo (UTokyo), Universidad de Antofagasta, Universidad de Valparaiso [Chile], INAF - Osservatorio Astrofisico di Arcetri (OAA), University of Copenhagen = Københavns Universitet (UCPH), Space Telescope Science Institute (STSci), University of Cambridge [UK] (CAM), University of California (UC), Cornell University [New York], Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Università degli Studi di Padova = University of Padua (Unipd), Leiden Observatory [Leiden], Universiteit Leiden, Gruppioni, C., Bethermin, M., Loiacono, F., Le Fevre, O., Capak, P., Cassata, P., Faisst, A. L., Schaerer, D., Silverman, J., Yan, L., Bardelli, S., Boquien, M., Carraro, R., Cimatti, A., Dessauges-Zavadsky, M., Ginolfi, M., Fujimoto, S., Hathi, N. P., Jones, G. C., Khusanova, Y., Koekemoer, A. M., Lagache, G., Lemaux, B. C., Oesch, P. A., Pozzi, F., Riechers, D. A., Rodighiero, G., Romano, M., Talia, M., Vallini, L., Vergani, D., Zamorani, G., Zucca, E., Université de Genève (UNIGE), University of Copenhagen = Københavns Universitet (KU), University of California, Universita degli Studi di Padova, Universiteit Leiden [Leiden], Gruppioni C., Bethermin M., Loiacono F., Le Fevre O., Capak P., Cassata P., Faisst A.L., Schaerer D., Silverman J., Yan L., Bardelli S., Boquien M., Carraro R., Cimatti A., Dessauges-Zavadsky M., Ginolfi M., Fujimoto S., Hathi N.P., Jones G.C., Khusanova Y., Koekemoer A.M., Lagache G., Lemaux B.C., Oesch P.A., Pozzi F., Riechers D.A., Rodighiero G., Romano M., Talia M., Vallini L., Vergani D., Zamorani G., Zucca E., ITA, USA, FRA, CHL, DNK, JPN, NLD, and CHE
Subjects: submillimeter: galaxies, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, Continuum (design consultancy), FOS: Physical sciences, observation [Cosmology], Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmology: observation, high-redshift [Galaxies], galaxies [Submillimeter], Settore FIS/05 - Astronomia e Astrofisica, galaxies: high-redshift, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Luminosity function (astronomy), Photometric redshift, Physics, 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, evolution [Galaxies], Astrophysics - Astrophysics of Galaxies, luminosity function [Galaxies], Galaxy, Redshift, galaxies: luminosity function, Space and Planetary Science, mass function, Astrophysics of Galaxies (astro-ph.GA), Mass function, cosmology: observations, Dark galaxy, Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present the detailed characterisation of a sample of 56 sources serendipitously detected in ALMA band 7, as part of the ALMA Large Program to INvestigate CII at Early Times (ALPINE) in COSMOS and ECDFS. These sources have been used to derive the total infrared luminosity function (LF) and to estimate the cosmic star formation rate density (SFRD) up to z=6. We have looked for counterparts in all the available multi-wavelength and photometric redshift catalogues, and in deeper near- and mid-IR source lists and maps, to identify optically dark sources with no matches in the public catalogues. Our ALMA blind survey allows us to push further the study of the nature and evolution of dusty galaxies at high-z, identifying luminous and massive sources to redshifts and faint luminosities never probed before by any far-infrared surveys. The ALPINE data are the first ones to sample the faint-end of the infrared LF, showing little evolution from z=2.5 to z=6, and a flat slope up to the highest redshifts. The SFRD obtained by integrating the luminosity function remains almost constant between z=2 and 6, and significantly higher than the optical/UV derivations, showing an important contribution of dusty galaxies and obscured star formation up to high-z. About 14 per cent of the ALPINE serendipitous continuum sources are optically+near-IR dark (six show a counterpart only in the mid-IR and no HST or near-IR identification, while two are detected as [CII] emitters at z=5). The six HST and near-IR dark galaxies with mid-IR counterpart contribute for about 17 per cent of the total SFRD at z=5 and dominate the high-mass end of the stellar mass function at z>3., 26 pages, 18 figures. Accepted for publication in A&A
Published: 2020
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47. The VANDELS ESO public spectroscopic survey

Author: Nimish P. Hathi, Michele Moresco, Jennifer M. Lotz, Seock-Sam Kim, Lidia Tasca, Andrea Grazian, Intae Jung, Adriano Fontana, Casey Papovich, William G. Hartley, Kirpal Nandra, Emanuela Pompei, S. Bardelli, R. Begley, Mauro Giavalisco, Paola Santini, H. C. Ferguson, Andrea Cimatti, J. S. Dunlop, Lucia Guaita, H. Mendez-Hernandez, Christina C. Williams, Giovanni Cresci, A. C. Carnall, A. Saxena, Adriana Gargiulo, Paolo Cassata, A. Iovino, C. Caputi, D. Maccagni, Stephane Charlot, Michele Cirasuolo, Johan P. U. Fynbo, Stefano Cristiani, Fabrizio Fiore, L. Pentericci, Guido Roberts-Borsani, E. Curtis-Lake, M. Longhetti, Manuela Magliocchetti, Matt J. Jarvis, M. Mignoli, Y. Khusanova, Paola Popesso, Annalisa Citro, Mara Salvato, Ricardo Amorín, Lucia Pozzetti, Olga Cucciati, Fergus Cullen, Pascale Hibon, Fernando Buitrago, Daniel P. Stark, Corentin Schreiber, M. Fumana, P. Franzetti, Jairo Méndez-Abreu, E. Zucca, R. C. Thomas, Filippo Mannucci, Ross J. McLure, Mark Dickinson, K. Matsuoka, M. Franco, O. Le Fèvre, Daniel Schaerer, Steve Finkelstein, M. Bolzonella, Fabio Fontanot, David J. Rosario, Eric F. Bell, Marco Castellano, A. Calabrò, Antonis Georgakakis, Mario Nonino, G. Vietri, Maurilio Pannella, G. Brammer, Marcella Brusa, David T. Maltby, Stéphanie Juneau, Bianca Garilli, Anton M. Koekemoer, Angela Bongiorno, Vivienne Wild, Giovanni G. Fazio, David Elbaz, Margherita Talia, D. J. McLeod, M. Scodeggio, Alberto Saldana-Lopez, M. Hamadouche, Italo Balestra, Omar Almaini, G. Zamorani, Eros Vanzella, Rebecca A. A. Bowler, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), 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), 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), Garilli B., McLure R., Pentericci L., Franzetti P., Gargiulo A., Carnall A., Cucciati O., Iovino A., Amorin R., Bolzonella M., Bongiorno A., Castellano M., Cimatti A., Cirasuolo M., Cullen F., Dunlop J., Elbaz D., Finkelstein S., Fontana A., Fontanot F., Fumana M., Guaita L., Hartley W., Jarvis M., Juneau S., Maccagni D., McLeod D., Nandra K., Pompei E., Pozzetti L., Scodeggio M., Talia M., Calabro A., Cresci G., Fynbo J.P.U., Hathi N.P., Hibon P., Koekemoer A.M., Magliocchetti M., Salvato M., Vietri G., Zamorani G., Almaini O., Balestra I., Bardelli S., Begley R., Brammer G., Bell E.F., Bowler R.A.A., Brusa M., Buitrago F., Caputi C., Cassata P., Charlot S., Citro A., Cristiani S., Curtis-Lake E., Dickinson M., Fazio G., Ferguson H.C., Fiore F., Franco M., Georgakakis A., Giavalisco M., Grazian A., Hamadouche M., Jung I., Kim S., Khusanova Y., Le Fevre O., Longhetti M., Lotz J., Mannucci F., Maltby D., Matsuoka K., Mendez-Hernandez H., Mendez-Abreu J., Mignoli M., Moresco M., Nonino M., Pannella M., Papovich C., Popesso P., Roberts-Borsani G., Rosario D.J., Saldana-Lopez A., Santini P., Saxena A., Schaerer D., Schreiber C., Stark D., Tasca L.A.M., Thomas R., Vanzella E., Wild V., Williams C., Zucca E., University of St Andrews. School of Physics and Astronomy, and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)
Subjects: SELECTION, Galaxies: fundamental parameter, Astrophysics, I, Surveys, 01 natural sciences, observations/surveys/catalogs [Cosmology], Cosmology: observation, Cosmology: Observations, Spectral line, statistics [Galaxies], DATA-REDUCTION, QB Astronomy, Galaxies: distances and redshift, Galaxies: Fundamental Parameters, 010303 astronomy & astrophysics, QC, QB, REDSHIFT SURVEY, Physics, observations [cosmology], Catalogs, Cosmology: observations, Galaxies: distances and redshifts, Galaxies: fundamental parameters, Galaxies: statistics, Galaxies: Statistics, fundamental parameters [Galaxies], astro-ph.CO, Catalog, X-RAY-PROPERTIES, Data release, Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), astro-ph.GA, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxies: Distances and Redshifts, surveys, 0103 physical sciences, STAR-FORMING GALAXIES, distances and redshifts [Galaxies], Astrophysics::Galaxy Astrophysics, 010308 nuclear & particles physics, Galaxies: statistic, Astronomy and Astrophysics, DAS, VLT DEEP SURVEY, Astrophysics - Astrophysics of Galaxies, EVOLUTION, STELLAR, QC Physics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), QUIESCENT GALAXIES, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], catalogs
Abstract: VANDELS is an ESO Public Spectroscopic Survey designed to build a sample of high signal to noise, medium resolution spectra of galaxies at redshift between 1 and 6.5. Here we present the final Public Data Release of the VANDELS Survey, comprising 2087 redshift measurements. We give a detailed description of sample selection, observations and data reduction procedures. The final catalogue reaches a target selection completeness of 40% at iAB = 25. The high Signal to Noise ratio of the spectra (above 7 in 80% of the spectra) and the dispersion of 2.5�� allowed us to measure redshifts with high precision, the redshift measurement success rate reaching almost 100%. Together with the redshift catalogue and the reduced spectra, we also provide optical mid-IR photometry and physical parameters derived through SED fitting. The observed galaxy sample comprises both passive and star forming galaxies covering a stellar mass range 8.3< Log(M*/Msolar), 16 pages, 13 figures, accepted for publication in Astronomy & Astrophysics
Published: 2021
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48. Less and more IGM-transmitted galaxies from z ∼ 2.7 to z ∼ 6 from VANDELS and VUDS

Author: E. Zucca, J. P. U. Fynbo, Margherita Talia, Ricardo Amorín, Anton M. Koekemoer, Y. Khusanova, Stefano Cristiani, Pascale Hibon, Laura Pentericci, Marco Castellano, F. Mannucci, Daniel Schaerer, S. Bardelli, V. Le Brun, Andrea Cimatti, R. Thomas, B. Garilli, M. Franco, O. Le Fevre, Adriana Gargiulo, Giovanni Cresci, Fabio Fontanot, Nimish P. Hathi, Brian C. Lemaux, G. Zamorani, 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), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Thomas R., Pentericci L., Le Fevre O., Koekemoer A.M., Castellano M., Cimatti A., Fontanot F., Gargiulo A., Garilli B., Talia M., Amorin R., Bardelli S., Cristiani S., Cresci G., Franco M., Fynbo J.P.U., Hathi N.P., Hibon P., Khusanova Y., Le Brun V., Lemaux B.C., Mannucci F., Schaerer D., Zamorani G., and Zucca E.
Subjects: Physics, 0303 health sciences, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmology: miscellaneou, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Galaxy, 03 medical and health sciences, Space and Planetary Science, galaxies: high-redshift, Intergalactic medium, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, intergalactic medium, cosmology: miscellaneous, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 030304 developmental biology, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Aim. Our aim is to analyse the variance of the Inter-Galactic Medium transmission (IGM) by studying this parameter in the rest-frame UV spectra of a large sample of high redshift galaxies. Method. We make use of the VIMOS Ultra Deep Survey and the VANDELS public survey to have an insight into the far UV spectrum of $2.7, Comment: Accepted for publication on A&A
Published: 2021
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49. UV and Ly$\alpha$ luminosity functions of galaxies and star formation rate density at the end of HI reionization from the VIMOS UltraDeep Survey (VUDS)

Author: Paolo Cassata, F. Marchi, Marco Castellano, Laurence Tresse, Nimish P. Hathi, O. Cucciati, Janine Pforr, O. Le Fevre, Daniel Schaerer, Anton M. Koekemoer, Mauro Giavalisco, L. A. M. Tasca, Y. Khusanova, Ricardo Amorín, S. Bardelli, Laura Pentericci, R. Thomas, B. Ribeiro, D. Maccagni, Brian C. Lemaux, Daniela Vergani, Letizia P. Cassarà, E. Zucca, G. Zamorani, Andrea Cimatti, V. Le Brun, O. Ilbert, B. Garilli, 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 de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-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), Khusanova Y., Le Fevre O., Cassata P., Cucciati O., Lemaux B.C., Tasca L.A.M., Thomas R., Garilli B., Le Brun V., MacCagni D., Pentericci L., Zamorani G., Amorin R., Bardelli S., Castellano M., Cassara L.P., Cimatti A., Giavalisco M., Hathi N.P., Ilbert O., Koekemoer A.M., Marchi F., Pforr J., Ribeiro B., Schaerer D., Tresse L., Vergani D., and Zucca E.
Subjects: galaxies: high-redshift, galaxies: evolution, galaxies: formation, galaxies: star formation, dark ages, reionization, first stars, galaxies: luminosity function, mass function, Population, first stars, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, 0103 physical sciences, Galaxy formation and evolution, Astrophysics::Solar and Stellar Astrophysics, dark ages, education, 010303 astronomy & astrophysics, Reionization, Astrophysics::Galaxy Astrophysics, Luminosity function (astronomy), Physics, education.field_of_study, 010308 nuclear & particles physics, Galaxies: luminosity function, mass function, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Dark ages, reionization, first star, galaxies: luminosity function, Space and Planetary Science, mass function, reionization, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Equivalent width, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We establish a robust statistical description of the star-forming galaxy population at the end of cosmic HI reionization ($5.0\le{}z\le6.6$) from a large sample of 52 galaxies with spectroscopically confirmed redshifts from the VIMOS UltraDeep Survey. We identify galaxies with Ly$\alpha$ either in absorption or in emission, at variance with most spectroscopic samples in the literature where Ly$\alpha$ emitters dominate. We find that star-forming galaxies at these redshifts are distributed along a main sequence in the stellar mass vs. SFR plane. We report a flat evolution of the sSFR(z) in 32. The bright end of the Ly$\alpha$ luminosity function has a high number density, indicating a significant star formation activity concentrated in the brightest Ly$\alpha$ emitters (LAE) at these redshifts. LAE with EW>25\AA ~contribute to about 75\% of the total UV-derived SFRD. While our analysis favors a low dust content in 5.0, Comment: 27 pages, submitted to A&A
Published: 2020
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50. The most massive, passive, and oldest galaxies at 0.5 < z < 2.1: Downsizing signature from galaxies selected from MgUV index

Author: Letizia P. Cassarà, D. Maccagni, Anton M. Koekemoer, O. Le Fèvre, R. C. Thomas, Nimish P. Hathi, Paolo Cassata, Pascale Hibon, Brian C. Lemaux, E. Zucca, G. Zamorani, S. Bardelli, Margherita Talia, Thomas R., Le Fevre O., Zamorani G., Lemaux B.C., Hibon P., Koekemoer A., Hathi N., MacCagni D., Cassata P., Cassara L.P., Bardelli S., Talia M., 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), 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), ITA, USA, FRA, and CHL
Subjects: Index (economics), Extinction (astronomy), Techniques: spectroscopic, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxies: formation, 01 natural sciences, Spectral line, 0103 physical sciences, 10. No inequality, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Epoch (reference date), Star formation, Galaxies: high-redshift, Astronomy and Astrophysics, Techniques: photometric, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Stars, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Aims. We seek is to identify old and massive galaxies at 0.5, Comment: Accepted for publication in A&A
Published: 2019
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