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108 results on '"J.-P. Kneib"'

1. Potential scientific synergies in weak lensing studies between the CSST and Euclid space probes

Author: D. Z. Liu, X. M. Meng, X. Z. Er, Z. H. Fan, M. Kilbinger, G. L. Li, R. Li, T. Schrabback, D. Scognamiglio, H. Y. Shan, C. Tao, Y. S. Ting, J. Zhang, S. H. Cheng, S. Farrens, L. P. Fu, H. Hildebrandt, X. Kang, J. P. Kneib, X. K. Liu, Y. Mellier, R. Nakajima, P. Schneider, J. L. Starck, C. L. Wei, A. H. Wright, H. Zhan, HEP, INSPIRE, 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), 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), 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 Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut d'Astrophysique de Paris (IAP), and Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)
Subjects: large-scale structure of universe, photometric redshifts, spectroscopy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), hyper suprime-cam, gravitational lensing, FOS: Physical sciences, weak, Astronomy and Astrophysics, telescopes, telescope, dark matter, gravitational lensing: weak, surveys, Space and Planetary Science, cfhtlens, galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], dark energy, constraints, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], cosmology, dark energy survey, cosmic shear, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Aims. With the next generation of large surveys poised to join the ranks of observational cosmology in the near future, it is important to explore their potential synergies and to maximize their scientific outcomes. In this study, we aim to investigate the complementarity of two upcoming space missions: Euclid and the China Space Station Telescope (CSST), both of which will be focused on weak gravitational lensing for cosmology. In particular, we analyze the photometric redshift (photo-z) measurements by combining NUV, 2006;gy bands from CSST with the VIS, Y,2006;J,2006;H bands from Euclid, and other optical bands from the ground-based Vera C. Rubin Observatory Legacy Survey of Space and Time (LSST) and Dark Energy Survey. We also consider the advantages of combining the two space observational data in simplifying image deblending. For Euclid, weak lensing measurements use the broad optical wavelength range of 550-900 nm, for which chromatic point-spread function (PSF) effects are significant. For this purpose, the CSST narrow-band data in the optical can provide valuable information for Euclid to obtain more accurate PSF measurements and to calibrate the color and color-gradient biases for galaxy shear measurements., Methods. We created image simulations, using the Hubble Deep UV data as the input catalog, for different surveys and quantified the photo-z performance using the EAZY template fitting code. For the blending analyses, we employed high-resolution HST-ACS CANDELS F606W and F814W data to synthesize mock simulated data for Euclid, CSST, and an LSST-like survey. We analyzed the blending fraction for different cases as well as the blending effects on galaxy photometric measurements. Furthermore, we demonstrated that CSST can provide a large enough number of high signal-to-noise ratio multi-band galaxy images to calibrate the color-gradient biases for Euclid., Results. The sky coverage of Euclid lies entirely within the CSST footprint. The combination of Euclid with the CSST data can thus be done more uniformly than with the various ground-based data that are part of the Euclid survey. Our studies show that by combining Euclid and CSST, we can reach a photo-z precision of sigma(NMAD)0.04 and an outlier fraction of eta 2.4% at the nominal depth of the Euclid Wide Survey (VIS24.5 AB mag). For CSST, including the Euclid Y,& 2006;J,& 2006;H bands reduces the overall photo-z outlier fraction from similar to 8.5% to 2.4%. For z & 2004;>& 2004;1, the improvements are even more significant. Because of the similarly high resolutions, the data combination of Euclid and CSST can be relatively straightforward for photometry measurements. On the other hand, to include ground-based data, sophisticated deblending utilizing priors from high-resolution space observations are required. The multi-band data from CSST are very helpful in controlling the chromatic PSF effect for Euclid VIS shear measurements. The color-gradient bias for Euclid galaxies with different bulge-to-total flux ratio at different redshifts can be well calibrated to the level of 0.1% using galaxies from the CSST deep survey.
Published: 2023
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2. Lightweight HI source finding for next generation radio surveys

Author: E. Tolley, D. Korber, A. Galan, A. Peel, M.T. Sargent, J.-P. Kneib, F. Courbin, and J.-L. Starck
Subjects: Space and Planetary Science, data analysis, galaxies, FOS: Physical sciences, Astronomy and Astrophysics, techniques, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), methods, image processing, Computer Science Applications
Abstract: Future deep HI surveys will be essential for understanding the nature of galaxies and the content of the Universe. However, the large volume of these data will require distributed and automated processing techniques. We introduce LiSA, a set of python modules for the denoising, detection and characterization of HI sources in 3D spectral data. LiSA was developed and tested on the Square Kilometer Array Science Data Challenge 2 dataset, and contains modules and pipelines for easy domain decomposition and parallel execution. LiSA contains algorithms for 2D-1D wavelet denoising using the starlet transform and flexible source finding using null-hypothesis testing. These algorithms are lightweight and portable, needing only a few user-defined parameters reflecting the resolution of the data. LiSA also includes two convolutional neural networks developed to analyse data cubes which separate HI sources from artifacts and predict the HI source properties. All of these components are designed to be as modular as possible, allowing users to mix and match different components to create their ideal pipeline. We demonstrate the performance of the different components of LiSA on the SDC2 dataset, which is able to find 95% of HI sources with SNR > 3 and accurately predict their properties., 18 pages, 16 figures
Published: 2022
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3. CODEX Weak Lensing Mass Catalogue and implications on the mass-richness relation

Author: Lance Miller, N Cibirka, J. Valiviita, L. van Waerbeke, P. Spinelli, Eduardo Rozo, Nicolas Clerc, J. Patrick Henry, R. A. Dupke, M. Costanzi, K. Kiiveri, Alexis Finoguenov, C. C. Kirkpatrick, Eduardo Serra Cypriano, Eli S. Rykoff, Jochen Weller, Ghassem Gozaliasl, Steffen Hagstotz, J. P. Kneib, Thomas Erben, Huanyuan Shan, Daniel Gruen, 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 de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Helsinki Institute of Physics, Department of Physics, Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), University of Helsinki, Helsinki Institute of Physics, University of Helsinki, Department of Physics, Kiiveri, K., Gruen, D., Finoguenov, A., Erben, T., van Waerbeke, L., Rykoff, E., Miller, L., Hagstotz, S., Dupke, R., Henry, J. Patrick, Kneib, J. -P., Gozaliasl, G., Kirkpatrick, C. C., Cibirka, N., Clerc, N., Costanzi, M., Cypriano, E. S., Rozo, E., Shan, H., Spinelli, P., Valiviita, J., and Weller, J.
Subjects: COSMOLOGICAL CONSTRAINTS, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Lambda, PROFILE, 01 natural sciences, 114 Physical sciences, gravitational lensing: weak, MAXBCG, weak [gravitational lensing], 0103 physical sciences, LARGE-SCALE STRUCTURE, clusters: general [galaxies], PROBE, 010303 astronomy & astrophysics, Weak gravitational lensing, Galaxy cluster, LOCUSS, Physics, TEMPERATURE RELATION, 010308 nuclear & particles physics, Astronomy and Astrophysics, observations [cosmology], Redshift, REDUCTION, Space and Planetary Science, galaxies: clusters: general, cosmology: observations, GIANTS, GALAXY CLUSTERS, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The COnstrain Dark Energy with X-ray clusters (CODEX) sample contains the largest flux limited sample of X-ray clusters at $0.35 < z < 0.65$. It was selected from ROSAT data in the 10,000 square degrees of overlap with BOSS, mapping a total number of 2770 high-z galaxy clusters. We present here the full results of the CFHT CODEX program on cluster mass measurement, including a reanalysis of CFHTLS Wide data, with 25 individual lensing-constrained cluster masses. We employ $lensfit$ shape measurement and perform a conservative colour-space selection and weighting of background galaxies. Using the combination of shape noise and an analytic covariance for intrinsic variations of cluster profiles at fixed mass due to large scale structure, miscentring, and variations in concentration and ellipticity, we determine the likelihood of the observed shear signal as a function of true mass for each cluster. We combine 25 individual cluster mass likelihoods in a Bayesian hierarchical scheme with the inclusion of optical and X-ray selection functions to derive constraints on the slope $\alpha$, normalization $\beta$, and scatter $\sigma_{\ln \lambda | \mu}$ of our richness-mass scaling relation model in log-space: $\left = \alpha \mu + \beta$, with $\mu = \ln (M_{200c}/M_{\mathrm{piv}})$, and $M_{\mathrm{piv}} = 10^{14.81} M_{\odot}$. We find a slope $\alpha = 0.49^{+0.20}_{-0.15}$, normalization $ \exp(\beta) = 84.0^{+9.2}_{-14.8}$ and $\sigma_{\ln \lambda | \mu} = 0.17^{+0.13}_{-0.09}$ using CFHT richness estimates. In comparison to other weak lensing richness-mass relations, we find the normalization of the richness statistically agreeing with the normalization of other scaling relations from a broad redshift range ($0.0, Comment: 37 pages, 12 figures
Published: 2021
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4. CODEX clusters. The Survey, the Catalog, and Cosmology of the X-ray Luminosity Function

Author: Nicolas Clerc, J. Patrick Henry, L. van Waerbeke, Florian Kaefer, Eli S. Rykoff, M. Costanzi, K. Kiiveri, Alexis Finoguenov, R. A. Dupke, Eduardo Rozo, Johan Comparat, Steffen Hagstotz, S. Damsted, Jochen Weller, V. Lindholm, G. Erfanianfar, C. C. Kirkpatrick, R. Capasso, J. P. Kneib, J. Ider Chitham, 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), 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), Department of Physics, Helsinki Institute of Physics, Particle Physics and Astrophysics, Finoguenov, A., Rykoff, E., Clerc, N., Costanzi, M., Hagstotz, S., Ider Chitham, J., Kiiveri, K., Kirkpatrick, C. C., Capasso, R., Comparat, J., Damsted, S., Dupke, R., Erfanianfar, G., Patrick Henry, J., Kaefer, F., Kneib, J. -P., Lindholm, V., Rozo, E., Van Waerbeke, L., and Weller, J.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Large-scale structure of Universe, Astrophysics::High Energy Astrophysical Phenomena, Population, rosat, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Surveys, 01 natural sciences, Cosmology, Galaxy group, galaxies, 0103 physical sciences, ROSAT, Galaxy formation and evolution, spiders spectroscopy, education, 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, Luminosity function (astronomy), Physics, education.field_of_study, 010308 nuclear & particles physics, Astronomy and Astrophysics, 115 Astronomy, Space science, Redshift, sky survey, Space and Planetary Science, Catalogs, mass calibration, Catalog, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Large area catalogs of galaxy clusters constructed from ROSAT All Sky Survey provide the base for our knowledge on the population of clusters thanks to the long-term multiwavelength efforts on their follow-up. Advent of large area photometric surveys superseding in depth previous all-sky data allows us to revisit the construction of X-ray cluster catalogs, extending the study to lower cluster masses and to higher redshifts and to provide the modelling of the selection function. We perform a wavelet detection of X-ray sources and make extensive simulations of the detection of clusters in the RASS data. We assign an optical richness to each of the 24,788 detected X-ray sources in the 10,382 square degrees of SDSS BOSS area, using redMaPPer version 5.2. We name this survey COnstrain Dark Energy with X-ray (CODEX) clusters. We show that there is no obvious separation of sources on galaxy clusters and AGN, based on distribution of systems on their richness. This is a combination of increasing number of galaxy groups and their selection as identification of an X-ray sources either by chance or due to groups hosting an AGN. To clean the sample, we use a cut on the optical richness at the level corresponding to the 10\% completeness of the survey and include it into the modelling of cluster selection function. We present the X-ray catalog extending to a redshift of 0.6 down to X-ray fluxes of $10^{-13}$ ergs s$^{-1}$ cm$^{-2}$. We provide the modelling of the sample selection and discuss the redshift evolution of the high end of the X-ray luminosity function (XLF). Our results on $z, Comment: 10 pages, 11 figures, A&A in press, part of SDSS DR16 data release
Published: 2020
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5. Herschel deep far-infrared counts through Abell 2218 cluster-lens

Author: G. Rodighiero, Ángel Bongiovanni, Roberto Maiolino, Raanan Nordon, Albrecht Poglitsch, I. Valtchanov, Ekkehard Wieprecht, P. Popesso, Bruno Altieri, Dieter Lutz, J. Cepa, Johan Richard, Eckhard Sturm, Antonio Cava, E. Daddi, P. Andreani, H. Dominguez, A. Cimatti, A. M. Pérez García, J. P. Kneib, Reinhard Genzel, Lijing Shao, Laure Ciesla, D. Elbaz, S. Berta, M. Wetzstein, M. Sánchez-Portal, Carlotta Gruppioni, L. Riguccini, Georgios E. Magdis, Linda J. Tacconi, Francesca Pozzi, H. Aussel, L. Metcalfe, P. Santini, Amelie Saintonge, N. M. Förster Schreiber, Benjamin Magnelli, XMM-Newton Science Operations Centre, European Space Agency (ESA), AUTRES, Max-Planck-Institut für Extraterrestrische Physik (MPE), 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)), 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), Station de Pathologie Végétale [Angers], Institut National de la Recherche Agronomique (INRA), Max Planck Institute for Extraterrestrial Physics (MPE), Max-Planck-Gesellschaft, Department of Physics [Berkeley], University of California [Berkeley], University of California-University of California, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-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-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Mecanique des Fluides et d'Acoustique (LMFA), École Centrale de Lyon (ECL), Université de Lyon-Université de Lyon-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-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), 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), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), B. Altieri, S. Berta, D. Lutz, J.-P. Kneib, L. Metcalfe, P. Andreani, H. Aussel, A. Bongiovanni, A. Cava, J. Cepa, L. Ciesla, A. Cimatti, E. Daddi, H. Dominguez, D. Elbaz, N.M. Forster Schreiber, R. Genzel, C. Gruppioni, B. Magnelli, G. Magdi, R. Maiolino, R. Nordon, A.M. Perez Garcia, A. Poglitsch, P. Popesso, F. Pozzi, J. Richard, L. Riguccini, G. Rodighiero, A. Saintonge, P. Santini, M. Sanchez-Portal, L. Shao, E. Sturm, L.J. Tacconi, I. Valtchanov, M. Wetzstein, E. Wieprecht, Agence Spatiale Européenne = European Space Agency (ESA), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), and École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Strong gravitational lensing, Population, FOS: Physical sciences, Astrophysics, 01 natural sciences, infrared: galaxies, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], surveys, galaxies: high-redshift, Cosmic infrared background, 0103 physical sciences, Source counts, Surface brightness, education, 010303 astronomy & astrophysics, Galaxy cluster, Physics, Luminous infrared galaxy, Galaxy: evolution, education.field_of_study, 010308 nuclear & particles physics, gravitational lensing: strong, Astronomy and Astrophysics, Gravitational lens, Space and Planetary Science, galaxies: clusters: general, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Gravitational lensing by massive galaxy clusters allows study of the population of intrinsically faint infrared galaxies that lie below the sensitivity and confusion limits of current infrared and submillimeter telescopes. We present ultra-deep PACS 100 and 160 microns observations toward the cluster lens Abell 2218, to penetrate the Herschel confusion limit. We derive source counts down to a flux density of 1 mJy at 100 microns and 2 mJy at 160 microns, aided by strong gravitational lensing. At these levels, source densities are 20 and 10 beams/source in the two bands, approaching source density confusion at 160 microns. The slope of the counts below the turnover of the Euclidean-normalized differential curve is constrained in both bands and is consistent with most of the recent backwards evolutionary models. By integrating number counts over the flux range accessed by Abell 2218 lensing (0.94-35 mJy at 100 microns and 1.47-35 mJy at 160 microns, we retrieve a cosmic infrared background (CIB) surface brightness of ~8.0 and ~9.9 nW m^-2 sr^-1, in the respective bands. These values correspond to 55% (+/- 24%) and 77% (+/- 31%) of DIRBE direct measurements. Combining Abell 2218 results with wider/shallower fields, these figures increase to 62% (+/- 25%) and 88% (+/- 32%) CIB total fractions, resolved at 100 and 160 microns, disregarding the high uncertainties of DIRBE absolute values., Accepted for publication on the A&A Herschel Special Issue, final version
Published: 2016
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6. A gravitationally boosted MUSE survey for emission-line galaxies at z ≳ 5 behind the massive cluster RCS 0224

Author: Richard Massey, J. P. Kneib, Ian Smail, Renske Smit, A. M. Swinbank, Johan Richard, Centre de Recherche Astrophysique de Lyon (CRAL), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), 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), 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), 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 de Recherche Astrophysique de Lyon ( CRAL ), École normale supérieure - Lyon ( ENS 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 ), Laboratoire d'Astrophysique de Marseille ( LAM ), Aix Marseille Université ( AMU ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National d'Etudes Spatiales ( CNES ) -Centre National de la Recherche Scientifique ( CNRS ), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Advanced Camera for Surveys, galaxies: high-redshift, 0103 physical sciences, galaxies: formation, Emission spectrum, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Very Large Telescope, 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, Multi Unit Spectroscopic Explorer, Astrophysics - Astrophysics of Galaxies, Galaxy, Space and Planetary Science, Outflow, Halo, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Wide Field Camera 3, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a VLT/MUSE survey of lensed high-redshift galaxies behind the z=0.77 cluster RCS0224-0002. We study the detailed internal properties of a highly magnified ({\mu}~29) z=4.88 galaxy seen through the cluster. We detect wide-spread nebular CIV{\lambda}{\lambda}1548,1551{\AA} emission from this galaxy as well as a bright Ly{\alpha} halo with a spatially-uniform wind and absorption profile across 12 kpc in the image plane. Blueshifted high- and low-ionisation interstellar absorption indicate the presence of a high-velocity outflow ({\Delta}v~300 km/s) from the galaxy. Unlike similar observations of galaxies at z=2-3, the Ly{\alpha} emission from the halo emerges close to the systemic velocity - an order of magnitude lower in velocity offset than predicted in "shell"-like outflow models. To explain these observations we favour a model of an outflow with a strong velocity gradient, which changes the effective column density seen by the Ly{\alpha} photons. We also search for high-redshift Ly{\alpha} emitters and identify 14 candidates between z=4.8-6.6, including an over-density at z=4.88, of which only one has a detected counterpart in HST/ACS+WFC3 imaging., Comment: 21 pages, 16 figures, MNRAS, in press
Published: 2017
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7. The Colors of Central and Satellite Galaxies in zCOSMOS out to z ~ 0.8 and Implications for Quenching

Author: E. Zucca, T. J. Bschorr, J. F. Le Borgne, Daniela Vergani, Andrea Cimatti, Masayuki Tanaka, Christian Maier, Anton M. Koekemoer, P. Kampczyk, Angela Bongiorno, Bianca Garilli, C. López-Sanjuan, Lucia Pozzetti, H. J. McCracken, R. Pello, E. Perez Montero, Graziano Coppa, Niraj Welikala, P. Franzetti, O. Le Fèvre, Olga Cucciati, F. Lamareille, S. de la Torre, Michele Moresco, Simon J. Lilly, Lidia Tasca, C. M. Carollo, S. Bardelli, A. Iovino, V. Presotto, Luke A. Barnes, Laurence Tresse, Karina Caputi, C. Knobel, Gianni Zamorani, L. de Ravel, Alvio Renzini, J. P. Kneib, M. Mignoli, A. Cappi, Preethi Nair, V. Mainieri, M. Bolzonella, John D. Silverman, Rongmon Bordoloi, V. Le Brun, Thierry Contini, Yingjie Peng, K. Kovac, M. Scodeggio, C. Knobel, S. J. Lilly, K. Kovac, Y. Peng, T. J. Bschorr, C. M. Carollo, T. Contini, J.-P. Kneib, O. Le Fevre, V. Mainieri, A. Renzini, M. Scodeggio, G. Zamorani, S. Bardelli, M. Bolzonella, A. Bongiorno, K. Caputi, O. Cucciati, S. de la Torre, L. de Ravel, P. Franzetti, B. Garilli, A. Iovino, P. Kampczyk, F. Lamareille, J.-F. Le Borgne, V. Le Brun, C. Maier, M. Mignoli, R. Pello', E. Perez Montero, V. Presotto, J. Silverman, M. Tanaka, L. Tasca, L. Tresse, D. Vergani, E. Zucca, L. Barne, R. Bordoloi, A. Cappi, A. Cimatti, G. Coppa, A. M. Koekemoer, C. Lopez-Sanjuan, H. J. McCracken, M. Moresco, P. Nair, L. Pozzetti, N. Welikala, Kapteyn Astronomical Institute, C., Knobel, S. J., Lilly, K., Kovač, Y., Peng, T. J., Bschorr, C. M., Carollo, T., Contini, J. P., Kneib, O., Le Fevre, V., Mainieri, A., Renzini, M., Scodeggio, G., Zamorani, S., Bardelli, M., Bolzonella, A., Bongiorno, K., Caputi, O., Cucciati, S., de la Torre, L., de Ravel, P., Franzetti, B., Garilli, A., Iovino, P., Kampczyk, F., Lamareille, J. F., Le Borgne, V., Le Brun, C., Maier, M., Mignoli, R., Pello, E., Perez Montero, Presotto, Valentina, J., Silverman, M., Tanaka, L., Tasca, L., Tresse, D., Vergani, E., Zucca, L., Barne, R., Bordoloi, A., Cappi, A., Cimatti, G., Coppa, A. M., Koekemoer, C., López Sanjuan, H. J., Mccracken, M., Moresco, P., Nair, L., Pozzetti, and N., Welikala
Subjects: GALAXIES: EVOLUTION, statistics [galaxies], Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, media_common.quotation_subject, COSMOLOGY: OBSERVATIONS, GALAXIES: STATISTICS, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, STAR-FORMATION, COSMOS SURVEY, 0103 physical sciences, Satellite galaxy, Astrophysics::Solar and Stellar Astrophysics, GALAXIES: LUMINOSITY FUNCTION, 10. No inequality, 010303 astronomy & astrophysics, RED SEQUENCE, evolution [galaxies], Astrophysics::Galaxy Astrophysics, luminosity function [galaxies], media_common, Physics, Quenching, REDSHIFT SURVEY, MASS FUNCTION, groups: general [galaxies], 010308 nuclear & particles physics, Astronomy and Astrophysics, GROUP CATALOG, cosmology: observations, galaxies: evolution, galaxies: groups: general, galaxies: luminosity function, mass function, galaxies: statistics, Redshift, EVOLUTION, Space and Planetary Science, Sky, galaxies: luminosity function, mass function, SPECTROSCOPIC SAMPLE, Physics::Space Physics, STELLAR MASS FUNCTION, DIGITAL SKY SURVEY, Satellite, QUIESCENT GALAXIES, GALAXIES: GROUPS: GENERAL, Astrophysics - Cosmology and Nongalactic Astrophysics, observation [cosmology]
Abstract: We examine the red fraction of central and satellite galaxies in the large zCOSMOS group catalog out to z ~ 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., 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 when the universe was about a half its present age, as it is today., Comment: 11 pages, 6 figures, published in ApJ
Published: 2012
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8. The SDSS-IV eBOSS: emission line galaxy catalogues at z ≈ 0.8 and study of systematic errors in the angular clustering

Author: J. R. Brownstein, Johan Comparat, Xu Zhou, Kyle S. Dawson, Guangtun Zhu, Jeffrey A. Newman, D. P. Schneider, F. B. Abdalla, Ashley J. Ross, Adam D. Myers, Stephanie Jouvel, J. P. Kneib, Francisco Prada, E. Jullo, C. Yeche, Will J. Percival, Timothée Delubac, Hu Zou, Zhimin Zhou, A. Raichoor, Département de Physique des Particules (ex SPP) (DPP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, 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), Département de Physique des Particules (ex SPP) (DPhP), Département de Physique des Particules (ex SPP) ( DPP ), Institut de Recherches sur les lois Fondamentales de l'Univers ( IRFU ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay, Laboratoire d'Astrophysique de Marseille ( LAM ), Aix Marseille Université ( AMU ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National d'Etudes Spatiales ( CNES ) -Centre National de la Recherche Scientifique ( CNRS ), 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: Cosmology and Gravitation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), astro-ph.GA, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], media_common.quotation_subject, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Photometry (optics), 0103 physical sciences, data analysis [methods], Cluster analysis, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, catalogues, media_common, Physics, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Linear discriminant analysis, Redshift survey, Astrophysics - Astrophysics of Galaxies, galaxies: general, methods: data analysis, observations [cosmology], Galaxy, Weighting, galaxies: photometry, Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA), cosmology: observations, astro-ph.CO, photometry [galaxies], distances and redshifts [galaxies], Baryon acoustic oscillations, galaxies: distances and redshifts, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], general [galaxies], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present two wide-field catalogs of photometrically-selected emission line galaxies (ELGs) at z=0.8 covering about 2800 deg^2 over the south galactic cap. The catalogs were obtained using a Fisher discriminant technique described in a companion paper. The two catalogs differ by the imaging used to define the Fisher discriminant: the first catalog includes imaging from the Sloan Digital Sky Survey and the Wide-Field Infrared Survey Explorer, the second also includes information from the South Galactic Cap U-band Sky Survey (SCUSS). Containing respectively 560,045 and 615,601 objects, they represent the largest ELG catalogs available today and were designed for the ELG programme of the extended Baryon Oscillation Spectroscopic Survey (eBOSS). We study potential sources of systematic variation in the angular distribution of the selected ELGs due to fluctuations of the observational parameters. We model the influence of the observational parameters using a multivariate regression and implement a weighting scheme that allows effective removal of all of the systematic errors induced by the observational parameters. We show that fluctuations in the imaging zero-points of the photometric bands have minor impact on the angular distribution of objects in our catalogs. We compute the angular clustering of both catalogs and show that our weighting procedure effectively removes spurious clustering on large scales. We fit a model to the small scale angular clustering, showing that the selections have similar biases of 1.35/D_a(z) and 1.28/D_a(z). Both catalogs are publicly available., Accepted for publication in MNRAS. 16 pages, 12 figures
Published: 2017
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9. SDSS-IV eBOSS emission-line galaxy pilot survey

Author: J. Comparat, T. Delubac, S. Jouvel, A. Raichoor, J-P. Kneib, C. Yèche, F. B. Abdalla, C. Le Cras, C. Maraston, D. M. Wilkinson, G. Zhu, E. Jullo, F. Prada, D. Schlegel, Z. Xu, H. Zou, J. Bautista, D. Bizyaev, A. Bolton, J. R. Brownstein, K. S. Dawson, S. Escoffier, P. Gaulme, K. Kinemuchi, E. Malanushenko, V. Malanushenko, V. Mariappan, J. A. Newman, D. Oravetz, K. Pan, W. J. Percival, A. Prakash, D. P. Schneider, A. Simmons, T. M. C. Abbott, S. Allam, M. Banerji, A. Benoit-Lévy, E. Bertin, D. Brooks, D. Capozzi, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, F. J. Castander, C. E. Cunha, L. N. da Costa, S. Desai, P. Doel, T. F. Eifler, J. Estrada, B. Flaugher, P. Fosalba, J. Frieman, E. Gaztanaga, D. W. Gerdes, D. Gruen, R. A. Gruendl, G. Gutierrez, K. Honscheid, D. J. James, K. Kuehn, N. Kuropatkin, O. Lahav, M. Lima, M. A. G. Maia, M. March, J. L. Marshall, R. Miquel, A. A. Plazas, K. Reil, N. Roe, A. K. Romer, A. Roodman, E. S. Rykoff, M. Sako, E. Sanchez, V. Scarpine, I. Sevilla-Noarbe, M. Soares-Santos, F. Sobreira, E. Suchyta, M. E. C. Swanson, G. Tarle, J. Thaler, D. Thomas, A. R. Walker, Y. Zhang, Massachusetts Institute of Technology (MIT), Departamento de FisicaTeorica e IFT-UAM/CSIC, Universidad Autonoma de Madrid (UAM), EPFL Laboratoire d’astrophysique, Ecole Polytechnique Fédérale de Lausanne (EPFL), Institut de Ciencies de l'Espai [Barcelona] (ICE-CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), University College of London [London] (UCL), Département de Physique des Particules (ex SPP) (DPP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Services communs OMP (UMS 831), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institute of Cosmology and Gravitation (Institute of Cosmology and Gravitation), University of Portsmouth, Instituto de Física Teórica UAM/CSIC (IFT), Universidad Autonoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Lawrence Berkeley National Laboratory [Berkeley] (LBNL), Institute of Oceanology [China], Key Laboratory of of Optical Astronomy, Chinese Academy of Sciences [Changchun Branch] (CAS)-National Astronomical Observatories of China, 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), Laboratoire Hippolyte Fizeau (FIZEAU), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Chimie du solide et de l'énergie (CSE), Collège de France (CdF (institution))-Institut de Chimie du CNRS (INC)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), CSIR (CSIR), CSIR, European Centre for Medium-Range Weather Forecasts (ECMWF), Equipe Circuit Instrumentation et Modélisation Electronique (ECIME), Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Ecole Nationale Supérieure de l'Electronique et de ses Applications, 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), Laboratoire Interdisciplinaire de Physique [Saint Martin d’Hères] (LIPhy), Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Institut de Física d’Altes Energies [Barcelone] (IFAE), Universitat Autònoma de Barcelona (UAB), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Physique et mécanique des milieux hétérogenes (UMR 7636) (PMMH), Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Universidad Simon Bolivar (USB), Scotland's Rural College (SRUC), Universidad de Castilla-La Mancha (UCLM), UAM. Departamento de Física Teórica, Universidad Autónoma de Madrid (UAM), Département de Physique des Particules (ex SPP) (DPhP), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Universidad Autónoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Chinese Academy of Sciences [Beijing] (CAS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), and Universidad de Castilla-La Mancha = University of Castilla-La Mancha (UCLM)
Subjects: Galaxies: general, spectroscopy, Cosmology and Gravitation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Large-scale structure of Universe, astro-ph.GA, media_common.quotation_subject, observational [methods], FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, 01 natural sciences, Photometry (optics), Methods: observational, 0103 physical sciences, survey, Emission spectrum, 010303 astronomy & astrophysics, Selection algorithm, Spectrograph, STFC, Astrophysics::Galaxy Astrophysics, QB, media_common, Physics, 010308 nuclear & particles physics, Standard ruler, Astrophysics::Instrumentation and Methods for Astrophysics, RCUK, Física, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA), astro-ph.CO, galaxy, large-scale structure of Universe, emission lines, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], cosmology, Astronomical and Space Sciences, Astrophysics - Cosmology and Nongalactic Astrophysics, general [galaxies]
Abstract: Artículo escrito por un elevado número de autores, solo se referencian el que aparece en primer lugar, el nombre del grupo de colaboración, si le hubiere, y los autores pertenecientes a la UAM, Astronomy and Astrophysics 592 (2016): A121reproduced with permission from Astronomy & Astrophysics, The Sloan Digital Sky Survey IV extended Baryonic Oscillation Spectroscopic Survey (SDSS-IV/eBOSS) will observe 195 000 emission-line galaxies (ELGs) to measure the baryonic acoustic oscillation (BAO) standard ruler at redshift 0.9. To test different ELG selection algorithms, 9000 spectra were observed with the SDSS spectrograph as a pilot survey based on data from several imaging surveys. First, using visual inspection and redshift quality flags, we show that the automated spectroscopic redshifts assigned by the pipeline meet the quality requirements for a reliable BAO measurement. We also show the correlations between sky emission, signal-to-noise ratio in the emission lines, and redshift error. Then we provide a detailed description of each target selection algorithm we tested and compare them with the requirements of the eBOSS experiment. As a result, we provide reliable redshift distributions for the different target selection schemes we tested. Finally, we determine an target selection algorithms that is best suited to be applied on DECam photometry because they fulfill the eBOSS survey efficiency requirements, J.C .and F.P. acknowledge support from the Spanish MICINNs Consolider-Ingenio 2010 Programme under grant MultiDark CSD2009-00064, MINECO Centro de Excelencia Severo Ochoa Programme under the grants SEV-2012-0249, FPA2012-34694, and the projects AYA2014- 60641-C2-1-P and AYA2012-31101. F.P. acknowledges the spanish MEC Salvador de Madariaga program, Ref. PRX14/00444. T.D. and J.P.K. acknowledge support from the LIDA ERC advanced grant. AR acknowledges funding from the P2IO LabEx (ANR-10-LABX-0038) in the framework Investissements d’Avenir (ANR- 11-IDEX-0003-01) managed by the French National Research Agency (ANR). The DES data management system is supported by the National Science Foundation under Grant Number AST-1138766. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2012-39559, ESP2013- 48274, FPA2013-47986, and Centro de Excelencia Severo Ochoa SEV-2012- 0234. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Programme (FP7/2007−2013) including ERC grant agreements 240672, 291329, and 306478
Published: 2016
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10. Comparison of star formation rates from Hα and infrared luminosity as seen byHerschel

Author: H. Domínguez Sánchez, M. Mignoli, F. Pozzi, F. Calura, A. Cimatti, C. Gruppioni, J. Cepa, M. Sánchez Portal, G. Zamorani, S. Berta, D. Elbaz, E. Le Floc'h, G. L. Granato, D. Lutz, R. Maiolino, F. Matteucci, P. Nair, R. Nordon, L. Pozzetti, L. Silva, J. Silverman, S. Wuyts, C. M. Carollo, T. Contini, J.-P. Kneib, O. Le Fèvre, S. J. Lilly, V. Mainieri, A. Renzini, M. Scodeggio, S. Bardelli, M. Bolzonella, A. Bongiorno, K. Caputi, G. Coppa, O. Cucciati, S. de la Torre, L. de Ravel, P. Franzetti, B. Garilli, A. Iovino, P. Kampczyk, C. Knobel, K. Kovač, F. Lamareille, J.-F. Le Borgne, V. Le Brun, C. Maier, B. Magnelli, R. Pelló, Y. Peng, E. Perez-Montero, E. Ricciardelli, L. Riguccini, M. Tanaka, L. A. M. Tasca, L. Tresse, D. Vergani, and E. Zucca
Subjects: Physics, Spiral galaxy, 010504 meteorology & atmospheric sciences, Star formation, Metallicity, Extinction (astronomy), Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Redshift, Galaxy, Luminosity, Space and Planetary Science, 0103 physical sciences, Emission spectrum, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract: We empirically test the relation between the SFR(LIR) derived from the infrared luminosity, LIR, and the SFR(Ha) derived from the Ha emission line luminosity using simple conversion relations. We use a sample of 474 galaxies at z = 0.06 - 0.46 with both Ha detection (from 20k zCOSMOS survey) and new far-IR Herschel data (100 and 160 {\mu}m). We derive SFR(Ha) from the Ha extinction corrected emission line luminosity. We find a very clear trend between E(B - V) and LIR that allows to estimate extinction values for each galaxy even if the Ha emission line measurement is not reliable. We calculate the LIR by integrating from 8 up to 1000 {\mu}m the SED that is best fitting our data. We compare SFR(Ha) with the SFR(LIR). We find a very good agreement between the two SFR estimates, with a slope of m = 1.01 \pm 0.03 in the SFR(LIR) vs SFR(Ha) diagram, a normalization constant of a = -0.08 \pm 0.03 and a dispersion of sigma = 0.28 dex.We study the effect of some intrinsic properties of the galaxies in the SFR(LIR)-SFR(Ha) relation, such as the redshift, the mass, the SSFR or the metallicity. The metallicity is the parameter that affects most the SFR comparison. The mean ratio of the two SFR estimators log[SFR(LIR)/SFR(Ha)] varies by approx. 0.6 dex from metal-poor to metal-rich galaxies (8.1 < log(O/H) + 12 < 9.2). This effect is consistent with the prediction of a theoretical model for the dust evolution in spiral galaxies. Considering different morphological types, we find a very good agreement between the two SFR indicators for the Sa, Sb and Sc morphologically classified galaxies, both in slope and normalization. For the Sd, irregular sample (Sd/Irr), the formal best-fit slope becomes much steeper (m = 1.62 \pm 0.43), but it is still consistent with 1 at the 1.5 sigma level, because of the reduced statistics of this sub-sample.
Published: 2012
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11. The evolution of quiescent galaxies at high redshifts (z≥ 1.4)

Author: Enrique Perez-Montero, P. Kampczyk, F. Lamareille, J. F. Le Borgne, Francesca Pozzi, Graziano Coppa, Y. Peng, Mara Salvato, H. Domínguez Sánchez, Angela Bongiorno, L. A. M. Tasca, H. J. McCracken, T. Contini, Vincenzo Mainieri, R. Pello, John D. Silverman, Christian Maier, M. Mignoli, E. Ricciardelli, Peter Capak, O. Cucciati, L. Tresse, A. Iovino, S. de la Torre, Alvio Renzini, Mikito Tanaka, D. Vergani, C. M. Carollo, G. Zamorani, L. de Ravel, E. Zucca, A. Cimatti, P. Franzetti, J. P. Kneib, O. Le Fevre, Marco Scodeggio, C. Knobel, K. Caputi, Lucia Pozzetti, M. Bolzonella, B. Garilli, E. Le Floc'h, Katarina Kovac, S. Bardelli, Carlotta Gruppioni, S. J. Lilly, V. Le Brun, and O. Ilbert
Subjects: Physics, education.field_of_study, Stellar mass, 010308 nuclear & particles physics, Star formation, Population, Extinction (astronomy), Theoretical models, Sigma, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Galaxy, Redshift, Space and Planetary Science, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We have studied the evolution of high redshift quiescent galaxies over an effective area of ~1.7 deg^2 in the COSMOS field. Galaxies have been divided according to their star-formation activity and the evolution of the different populations has been investigated in detail. We have studied an IRAC (mag_3.6 1.4 with multi-wavelength coverage. We have derived accurate photometric redshifts (sigma=0.06) and other important physical parameters through a SED-fitting procedure. We have divided our sample into actively star-forming, intermediate and quiescent galaxies depending on their specific star formation rate. We have computed the galaxy stellar mass function of the total sample and the different populations at z=1.4-3.0. We have studied the properties of high redshift quiescent galaxies finding that they are old (1-4 Gyr), massive (log(M/M_sun)~10.65), weakly star forming stellar populations with low dust extinction (E(B-V) 11, while the quiescent population increases from 10% to 50% at the same redshift and mass intervals. We compare the fraction of quiescent galaxies derived with that predicted by theoretical models and find that the Kitzbichler & White (2007) model is the one that better reproduces the data. Finally, we calculate the stellar mass density of the star-forming and quiescent populations finding that there is already a significant number of quiescent galaxies at z > 2.5 (rho~6.0 MsunMpc^-3).
Published: 2011
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12. Understanding the shape of the galaxy two-point correlation function at z ≃ 1 in the COSMOS field

Author: Thierry Contini, E. Zucca, Preethi Nair, G. Zamorani, Olivier Ilbert, C. Knobel, A. Iovino, N. Z. Scoville, L. de Ravel, V. Mainieri, J. F. Le Borgne, S. Bardelli, Daniela Vergani, J. P. Kneib, M. Scodeggio, Andrea Cimatti, O. Le Fèvre, Lidia Tasca, P. Kampczyk, P. Memeo, V. Le Brun, Paolo Cassata, Graziano Coppa, R. Pello, Olga Cucciati, D. Bottini, David S Sanders, Y. Peng, Simon J. Lilly, Karina Caputi, Masayuki Tanaka, Enrique Pérez-Montero, Roberto Scaramella, K. Kovac, A. Cappi, Micol Bolzonella, Alvio Renzini, Pascal Oesch, S. de la Torre, Laurence Tresse, Lucia Pozzetti, C. M. Carollo, Ummi Abbas, Angela Bongiorno, Anton M. Koekemoer, Luigi Guzzo, V. Presotto, E. Ricciardelli, Niraj Welikala, John D. Silverman, F. Lamareille, H. J. McCracken, Bianca Garilli, B. Meneux, P. Franzetti, D. Maccagni, M. Mignoli, M. Fumana, Cristiano Porciani, Christian Maier, Christian Marinoni, and Alexie Leauthaud
Subjects: Physics, Field (physics), 010308 nuclear & particles physics, Dark matter, Astronomy and Astrophysics, Probability density function, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Galaxy, Redshift, Correlation function, Space and Planetary Science, 0103 physical sciences, Halo, Density contrast, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We investigate how the shape of the galaxy two-point correlation function as measured in the zCOSMOS survey depends on local environment, quantified in terms of the density contrast on scales of 5 Mpc/h. We show that the flat shape previously observed at redshifts between z=0.6 and z=1 can be explained by this volume being simply 10% over-abundant in high-density environments, with respect to a Universal density probability distribution function. When galaxies corresponding to the top 10% tail of the distribution are excluded, the measured w_p(r_p) steepens and becomes indistinguishable from LCDM predictions on all scales. This is the same effect recognised by Abbas & Sheth in the SDSS data at z~0 and explained as a natural consequence of halo-environment correlations in a hierarchical scenario. Galaxies living in high-density regions trace dark matter halos with typically higher masses, which are more correlated. If the density probability distribution function of the sample is particularly rich in high-density regions because of the variance introduced by its finite size, this produces a distorted two-point correlation function. We argue that this is the dominant effect responsible for the observed "peculiar" clustering in the COSMOS field.
Published: 2010
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13. Bars in early- and late-type discs in COSMOS

Author: Monique Aller, T. J. Bschorr, Y. Taniguchi, Pascal Oesch, Nick Scoville, Kartik Sheth, E. Le Floc'h, A. Leauthaud, P. Cerulo, Anton M. Koekemoer, O. Ilbert, S. J. Lilly, C. M. Carollo, Richard Massey, Jason Rhodes, Mara Salvato, David R. Thompson, Ewan Cameron, Peter Capak, D. B. Sanders, H. Aussel, H. J. McCracken, and J. P. Kneib
Subjects: Physics, 010308 nuclear & particles physics, Bar (music), media_common.quotation_subject, Late type, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Redshift, Universe, Galaxy, Hubble sequence, symbols.namesake, Barred spiral galaxy, Space and Planetary Science, 0103 physical sciences, symbols, Cosmos (category theory), Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common
Abstract: We investigate the (large-scale) bar fraction in a mass-complete sample of M > 10^10.5 Msun disk galaxies at 0.2 10^11 Msun), where the fraction of bars in early-type disks becomes significantly lower, at all redshifts, than that in late-type disks. The bar fractions for galaxies with low and high SSFRs closely follow those of the morphologically-selected early-type and late-type populations, respectively. This indicates a close correspondence between morphology and SSFR in disk galaxies at these earlier epochs. Interestingly, the total bar fraction in 10^10.5 10^11 Msun disks it remains roughly constant. This indicates that, already by z ~ 0.6, spectral and morphological transformations in the most massive disk galaxies have largely converged to the familiar Hubble sequence that we observe in the local Universe, while for intermediate mass disks this convergence is ongoing until at least z ~ 0.2. Moreover, these results highlight the importance of employing mass-limited samples for quantifying the evolution of barred galaxies. Finally, the evolution of the barred galaxy populations investigated does not depend on the large-scale environmental density (at least, on the scales which can be probed with the available photometric redshifts).
Published: 2010
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14. A spectacular giant arc in the massive cluster lens MACS J1206.2−0847

Author: J. F. Le Borgne, Harald Ebeling, C. J. Ma, Alastair C. Edge, N. J. D. Courtney, E. Barrett, J. P. Kneib, Eric Jullo, Institute for Astronomy [Honolulu], University of Hawai‘i [Mānoa] (UHM), 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), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), 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: Astrophysics::High Energy Astrophysical Phenomena, gravitational lensing, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Virial theorem, galaxies: clusters: individual: MACSJ1206.2-0847, Luminosity, Galaxy group, 0103 physical sciences, Cluster (physics), Brightest cluster galaxy, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Galaxy cluster, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Galaxy, Redshift, galaxies: clusters: general, Space and Planetary Science, X-rays: galaxies: clusters, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Astrophysics - High Energy Astrophysical Phenomena
Abstract: We discuss the X-ray and optical properties of the massive galaxy cluster MACSJ1206.2-0847 (z=0.4385), discovered in the Massive Cluster Survey (MACS). Our Chandra observation of the system yields a total X-ray luminosity of 2.4 x 10^45 erg/s (0.1-2.4 keV) and a global gas temperature of (11.6 +/- 0.7) keV, very high values typical of MACS clusters. In both optical and X-ray images MACSJ1206 appears close to relaxed in projection, with a pronounced X-ray peak at the location of the brightest cluster galaxy (BCG); we interpret this feature as the remnant of a cold core. A spectacular giant gravitational arc, 15" in length, bright (V~21) and unusually red (R-K=4.3), is seen 20" west of the BCG; we measure a redshift of z=1.036 for the lensed galaxy. From our HST image of the cluster we identify the giant arc and its counter image as a seven-fold imaged system. An excess of X-ray emission in the direction of the arc coincides with a mild galaxy overdensity and could be the remnant of a minor merger with a group of galaxies. We derive estimates of the total cluster mass as well as of the mass of the cluster core using X-ray, dynamical, and gravitational-lensing techniques. For the mass enclosed by the giant arc (r, 13 pages, 14 figures, accepted for publication in MNRAS
Published: 2009
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15. SPACE: the spectroscopic all-sky cosmic explorer

Author: A. Cimatti, M. Robberto, C. Baugh, S. V. W. Beckwith, R. Content, E. Daddi, G. De Lucia, B. Garilli, L. Guzzo, G. Kauffmann, M. Lehnert, D. Maccagni, A. Martínez-Sansigre, F. Pasian, I. N. Reid, P. Rosati, R. Salvaterra, M. Stiavelli, Y. Wang, M. Zapatero Osorio, M. Balcells, M. Bersanelli, F. Bertoldi, J. Blaizot, D. Bottini, R. Bower, A. Bulgarelli, A. Burgasser, C. Burigana, R. C. Butler, S. Casertano, B. Ciardi, M. Cirasuolo, M. Clampin, S. Cole, A. Comastri, S. Cristiani, J.-G. Cuby, F. Cuttaia, A. De Rosa, A. Diaz Sanchez, M. Di Capua, J. Dunlop, X. Fan, A. Ferrara, F. Finelli, A. Franceschini, M. Franx, P. Franzetti, C. Frenk, Jonathan P. Gardner, F. Gianotti, R. Grange, C. Gruppioni, A. Gruppuso, F. Hammer, L. Hillenbrand, A. Jacobsen, M. Jarvis, R. Kennicutt, R. Kimble, M. Kriek, J. Kurk, J.-P. Kneib, O. Le Fevre, D. Macchetto, J. MacKenty, P. Madau, M. Magliocchetti, D. Maino, N. Mandolesi, N. Masetti, R. McLure, A. Mennella, M. Meyer, M. Mignoli, B. Mobasher, E. Molinari, G. Morgante, S. Morris, L. Nicastro, E. Oliva, P. Padovani, E. Palazzi, F. Paresce, A. Perez Garrido, E. Pian, L. Popa, M. Postman, L. Pozzetti, J. Rayner, R. Rebolo, A. Renzini, H. Röttgering, E. Schinnerer, M. Scodeggio, M. Saisse, T. Shanks, A. Shapley, R. Sharples, H. Shea, J. Silk, I. Smail, P. Spanó, J. Steinacker, L. Stringhetti, A. Szalay, L. Tresse, M. Trifoglio, M. Urry, L. Valenziano, F. Villa, I. Villo Perez, F. Walter, M. Ward, R. White, S. White, E. Wright, R. Wyse, G. Zamorani, A. Zacchei, W. W. Zeilinger, F. Zerbi, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Space Telescope Science Institute (STScI), Institute for Computational Cosmology, Department of Physics, Durham University, Durham (ICC), Centre for Advanced Instrumentation, Department of Physics, Durham University (CfAI), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Max-Planck-Institut für Astrophysik (MPA), Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano (IASF-MI), Istituto Nazionale di Astrofisica (INAF), Brera, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Physique des Galaxies et Cosmologie, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-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), Max-Planck-Institut für Astronomie (MPIA), INAF-Osservatorio Astronomico di Trieste (INAF-OATs), European Southern Observatory (ESO), Università di Milano, University of Oklahoma, Instituto de Astrofísica de Canarias (IAC), Rheinische Friedrich-Wilhelms-Universität Bonn, Istituto di Astrofisica Spaziale e Fisica Cosmica (IASF-Bologna), Department of Earth Atmospheric and Planetary Sciences, MIT, The Royal Observatory (ROE), Goddard Space Flight Center, NASA, Astrophysics Science Division, INAF-Osservatorio Astronomico di Bologna (OABO), 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), Universidad Politecnica de Cartagena (UPCT), University of Maryland, University of Arizona, Scuola Internazionale Superiore di Studi Avanzati (SISSA), Università degli Studi di Padova = University of Padua (Unipd), University of Leiden, California Institute of Technology, Department of Astronomy (CALTECH), OpSys Project Consulting, University of Hertfordshire [Hatfield] (UH), Institute of Astronomy, University of Cambridge (IoA), Research and Scientific Support Department, ESA-ESTEC (RSSD), University of California, Santa Cruz (UCSC), Steward Observatory, University of Arizona, UC Riverside, INAF-Osservatorio Astrofisico di Arcetri (INAF-OAA), University of Bucharest, Institute for Astronomy, University of Hawaii, INAF-Osservatorio Astronomico di Padova, Princeton, Ecole Polytechnique Fédérale de Lausanne (EPFL), University of Oxford, Johns Hopkins University (JHU), Yale University, University of California, Los Angeles (UCLA), University of Vienna, Cimatti A., Robberto M., Baugh C., Beckwith S. V. W., Content R., Daddi E., De Lucia G., Garilli B., Guzzo L., Kauffmann G., Lehnert M., Maccagni D., Martínez-Sansigre A., Pasian F., Reid I. N., Rosati P., Salvaterra R., Stiavelli M., Wang Y., Osorio M. Zapatero, Balcells M., Bersanelli M., Bertoldi F., Blaizot J., Bottini D., Bower R., Bulgarelli A., Burgasser A., Burigana C., Butler R. C., Casertano S., Ciardi B., Cirasuolo M., Clampin M., Cole S., Comastri A., Cristiani S., Cuby J.-G., Cuttaia F., de Rosa A., Sanchez A. Diaz, di Capua M., Dunlop J., Fan X., Ferrara A., Finelli F., Franceschini A., Franx M., Franzetti P., Frenk C., Gardner Jonathan P., Gianotti F., Grange R., Gruppioni C., Gruppuso A., Hammer F., Hillenbrand L., Jacobsen A., Jarvis M., Kennicutt R., Kimble R., Kriek M., Kurk J., Kneib J.-P., Le Fevre O., Macchetto D., MacKenty J., Madau P., Magliocchetti M., Maino D., Mandolesi N., Masetti N., McLure R., Mennella A., Meyer M., Mignoli M., Mobasher B., Molinari E., Morgante G., Morris S., Nicastro L., Oliva E., Padovani P., Palazzi E., Paresce F., Garrido A. Perez, Pian E., Popa L., Postman M., Pozzetti L., Rayner J., Rebolo R., Renzini A., Röttgering H., Schinnerer E., Scodeggio M., Saisse M., Shanks T., Shapley A., Sharples R., Shea H., Silk J., Smail I., Spanó P., Steinacker J., Stringhetti L., Szalay A., Tresse L., Trifoglio M., Urry M., Valenziano L., Villa F., Perez I. Villo, Walter F., Ward M., White R., White S., Wright E., Wyse R., Zamorani G., Zacchei A., Zeilinger W., Zerbi F., Cimatti, A., Robberto, M., Baugh, C., Beckwith, S. V. W., Content, R., Daddi, E., De, Lucia, G., Garilli, B., Guzzo, L., Kauffmann, Ferrara, Andrea, and 113, Coauthors
Subjects: Observational cosmology, media_common.quotation_subject, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Space (mathematics), law.invention, Telescope, law, Dark energy, Spectral resolution, media_common, Physics, COSMIC cancer database, Astronomical and space-research instrumentation, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Billion years, Galaxy, Redshift, Space and Planetary Science, Sky, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: We describe the scientific motivations, the mission concept and the instrumentation of SPACE, a class-M mission proposed for concept study at the first call of the ESA Cosmic-Vision 2015-2025 planning cycle. SPACE aims to produce the largest three-dimensional evolutionary map of the Universe over the past 10 billion years by taking near-IR spectra and measuring redshifts for more than half a billion galaxies at 0, Comment: 27 pages, Experimental Astronomy, in press. The SPACE team complete list is available at http://urania.bo.astro.it/cimatti/space . The article with full resolution figures is available at http://urania.bo.astro.it/cimatti/space/publications.htm
Published: 2008
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16. The Hα Luminosity Function and Star Formation Rate atz≈ 0.24 in the COSMOS 2 Square Degree Field

Author: A. Leauthaud, A. Nakajima, Nick Scoville, J. P. Kneib, Takashi Murayama, Y. Taniguchi, Richard Massey, Eva Schinnerer, S. J. Lilly, Patrick L. Shopbell, S. Mihara, D. B. Sanders, Masaru Ajiki, G. Hasinger, Alvio Renzini, M. Giavalisco, Jason Rhodes, H. Aussel, M. I. Takahashi, S. S. Sasaki, Y. Shioya, Y. Ideue, M. Rich, Chris Impey, Bahram Mobasher, Luigi Guzzo, Tohru Nagao, and O. LeFevre
Subjects: Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics, Correlation function (quantum field theory), Lambda, 01 natural sciences, Power law, Redshift, Galaxy, Luminosity, Square degree, Space and Planetary Science, 0103 physical sciences, 010303 astronomy & astrophysics, Luminosity function (astronomy)
Abstract: To derive a new H$\alpha$ luminosity function and to understand the clustering properties of star-forming galaxies at $z \approx 0.24$, we have made a narrow-band imaging survey for H$\alpha$ emitting galaxies in the HST COSMOS 2 square degree field. We used the narrow-band filter NB816 ($\lambda_c = 8150$ \AA, $\Delta \lambda = 120$ \AA) and sampled H$\alpha$ emitters with $EW_{\rm obs}(\rm H\alpha + [N\textsc{ii}]) > 12$ \AA in a redshift range between $z=0.233$ and $z=0.251$ corresponding to a depth of 70 Mpc. We obtained 980 H$\alpha$ emitting galaxies in a sky area of 5540 arcmin$^2$, corresponding to a survey volume of $3.1 \times 10^4 {\rm Mpc^3}$. We derive a H$\alpha$ luminosity function with a best-fit Schechter function parameter set of $\alpha = -1.35^{+0.11}_{-0.13}$, $\log\phi_* = -2.65^{+0.27}_{-0.38}$, and $\log L_* ({\rm erg s^{-1}}) = 41.94^{+0.38}_{-0.23}$. The H$\alpha$ luminosity density is $2.7^{+0.7}_{-0.6} \times 10^{39}$ ergs s$^{-1}$ Mpc$^{-3}$. After subtracting the AGN contribution (15 %) to the H$\alpha$ luminosity density, the star formation rate density is evaluated as $1.8^{+0.7}_{-0.4} \times 10^{-2}$ $M_{\sun}$ yr$^{-1}$ Mpc$^{-3}$. The angular two-point correlation function of H$\alpha$ emitting galaxies of $\log L({\rm H\alpha}) > 39.8$ is well fit by a power law form of $w(\theta) = 0.013^{+0.002}_{-0.001} \theta^{-0.88 \pm 0.03}$, corresponding to the correlation function of $\xi(r) = (r/1.9{\rm Mpc})^{-1.88}$. We also find that the H$\alpha$ emitters with higher H$\alpha$ luminosity are more strongly clustered than those with lower luminosity.
Published: 2008
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17. Separating Baryons and Dark Matter in Cluster Cores: A Full Two‐dimensional Lensing and Dynamic Analysis of Abell 383 and MS 2137−23

Author: J. P. Kneib, David J. Sand, Richard S. Ellis, Graham P. Smith, and Tommaso Treu
Subjects: Physics, Dark matter, Velocity dispersion, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy, Gravitational lens, Space and Planetary Science, Stellar dynamics, Cluster (physics), Halo, Brightest cluster galaxy, Astrophysics::Galaxy Astrophysics
Abstract: We utilize existing data for the galaxy clusters MS 2137–23 and Abell 383 to present improved measures of the distribution of dark and baryonic material in the clusters' central regions. Our method, based on the combination of gravitational lensing and dynamical data, is uniquely capable of separating the distribution of dark and baryonic components at scales below 100 kpc. Our mass models include pseudoelliptical generalized NFW profiles for constraining the inner dark matter slope. We find that a variety of strong-lensing models fit the available data, including some with dark matter profiles as steep as expected from recent simulations. However, when combined with stellar velocity dispersion data for the brightest member, shallower inner slopes than predicted by numerical simulations are preferred, in general agreement with our earlier work in these clusters. For Abell 383, the preferred shallow inner slopes are statistically a good fit only when the multiple-image position uncertainties associated with our lens model are assumed to be 0.5", to account for unknown substructure. No statistically satisfactory fit was obtained matching both the multiple-image lensing data and the velocity dispersion profile of the brightest cluster galaxy in MS 2137–23. This suggests that the mass model we are using, which comprises a pseudoelliptical generalized NFW profile and a brightest cluster galaxy component, may inadequately represent the inner cluster regions. This may arise due to halo triaxiality or by the gravitational interaction of baryons and dark matter in cluster cores. The progress made via this detailed study highlights the key role that complementary observations of lensed features and stellar dynamics offer in understanding the interaction between dark and baryonic matter on nonlinear scales in the central regions of clusters.
Published: 2008
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18. The SDSS-IV extended Baryon Oscillation Spectroscopic Survey: selecting emission line galaxies using the Fisher discriminant

Author: A. Raichoor, J. Comparat, T. Delubac, J.-P. Kneib, Ch. Yèche, H. Zou, F. B. Abdalla, K. Dawson, A. de la Macorra, X. Fan, Z. Fan, Z. Jiang, Y. Jing, S. Jouvel, D. Lang, M. Lesser, C. Li, J. Ma, J. A. Newman, J. Nie, N. Palanque-Delabrouille, W. J. Percival, F. Prada, S. Shen, J. Wang, Z. Wu, T. Zhang, X. Zhou, Z. Zhou, Département de Physique des Particules (ex SPP) (DPP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Instituto de Física Teórica UAM/CSIC (IFT), Universidad Autonoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), EPFL Laboratoire d’astrophysique, Ecole Polytechnique Fédérale de Lausanne (EPFL), 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), Key Laboratory of of Optical Astronomy, Chinese Academy of Sciences [Changchun Branch] (CAS)-National Astronomical Observatories of China, A.R. acknowledges funding from the P2IO LabEx (ANR-10-LABX-0038) in the framework 'Investissements d’Avenir' (ANR-11-IDEX-0003-01) managed by the French National Research Agency (ANR), European Project: 290975,EC:FP7:ERC,ERC-2011-ADG_20110209,LIDA(2012), Département de Physique des Particules (ex SPP) (DPhP), Universidad Autónoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), and Chinese Academy of Sciences [Beijing] (CAS)
Subjects: astro-ph.GA, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmology, Photometry (optics), 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Emission spectrum, Linear combination, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Linear discriminant analysis, Astrophysics - Astrophysics of Galaxies, galaxies: general, methods: data analysis, Redshift, Galaxy, Baryon, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies: star formation, galaxies: stellar content, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: We present a new selection technique of producing spectroscopic target catalogues for massive spectroscopic surveys for cosmology. This work was conducted in the context of the extended Baryon Oscillation Spectroscopic Survey (eBOSS), which will use ~200 000 emission line galaxies (ELGs) at 0.6, Comment: Version published in A&A
Published: 2016
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19. The Red Radio Ring: a gravitationally lensed hyperluminous infrared radio galaxy at z=2.553 discovered through the citizen science project SPACE WARPS

Author: E Paget, Grant W. Wilson, Christine Jordan, Gopal Narayanan, Robert Beswick, David H. Hughes, J. P. Kneib, Raúl Mújica, M Parrish, A. More, Y-T. Lin, Stuart Lynn, C Snyder, Eli S. Rykoff, Claude Cornen, Marco Viero, M. S. Yun, Amit Kapadia, David Sánchez-Arguelles, James E. Geach, Alexie Leauthaud, R. Simpson, Chris Lintott, P. A. Harrison, Matthias Tecza, Thomas Erben, Masamune Oguri, B E Cox, D Ó Briain, Philip J. Marshall, Rob Ivison, F. P. Schloerb, Aprajita Verma, T. W. B. Muxlow, Elisabeth Baeten, Julianne K. Wilcox, Miguel Chavez, Grant Miller, Milagros Zeballos, P-E Belles, Nicholas P. Ross, W-H Wang, Cristian Rusu, L. van Waerbeke, Eduardo Rozo, N. J. Jackson, Alfredo Montaña, N J Erickson, Christine Macmillan, Tim O'Brien, Kevin Harrington, Simon Garrington, M Makler, Royal Observatory Edinburgh (ROE), University of Edinburgh, Jodrell Bank Centre for Astrophysics (JBCA), University of Manchester [Manchester], California Institute of Technology (CALTECH), Ecole Polytechnique Fédérale de Lausanne (EPFL), KIPAC, Stanford (KIPAC), Stanford University-SLAC National Accelerator Laboratory (SLAC), Stanford University, 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), Computing and Mathematical Sciences [Pasadena]], AUTRES, Department of Physics, Durham University, 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), Oxford Astrophysics, University of Oxford, Jodrell Bank Centre for Astrophysics, Jodrell Bank Observatory, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), 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 University of Oxford [Oxford]
Subjects: Einstein ring, Radio galaxy, Astrophysics::High Energy Astrophysical Phenomena, Doubly ionized oxygen, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, symbols.namesake, X-shaped radio galaxy, galaxies: high-redshift, 0103 physical sciences, Emission spectrum, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, Quasar, Galaxy, Redshift, Space and Planetary Science, methods: miscellaneous, symbols, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: International audience; We report the discovery of a gravitationally lensed hyperluminous infrared galaxy (intrinsic L-IR approximate to 10(13) L-circle dot) with strong radio emission (intrinsic L-1.4 GHz approximate to 10(25) WHz(-1)) at z = 2.553. The source was identified in the citizen science project SPACE WARPS through the visual inspection of tens of thousands of iJK(s) colour composite images of luminous red galaxies (LRGs), groups and clusters of galaxies and quasars. Appearing as a partial Einstein ring (r(e) approximate to 3 arcsec) around an LRG at z = 0.2, the galaxy is extremely bright in the sub-millimetre for a cosmological source, with the thermal dust emission approaching 1 Jy at peak. The redshift of the lensed galaxy is determined through the detection of the CO(3 -\textgreater 2) molecular emission line with the Large Millimetre Telescope's Redshift Search Receiver and through [O III] and Ha line detections in the near-infrared from Subaru/Infrared Camera and Spectrograph. We have resolved the radio emission with high-resolution (300-400 mas) eMERLIN L-band and Very Large Array C-band imaging. These observations are used in combination with the near-infrared imaging to construct a lens model, which indicates a lensing magnification of mu approximate to 10. The source reconstruction appears to support a radio morphology comprised of a compact (\textless250 pc) core and more extended component, perhaps indicative of an active nucleus and jet or lobe.
Published: 2015
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20. The cosmic evolution of oxygen and nitrogen abundances in star-forming galaxies over the past 10 Gyr

Author: G. Zamorani, Y. Peng, L. de Ravel, E. Ricciardelli, Alvio Renzini, E. Zucca, V. Presotto, J. F. Le Borgne, P. Kampczyk, J. P. Kneib, T. Contini, Marco Scodeggio, John D. Silverman, Mikito Tanaka, P. Franzetti, Enrique Perez-Montero, L. A. M. Tasca, Angela Bongiorno, L. Tresse, O. Cucciati, S. de la Torre, C. M. Carollo, O. Le Fevre, K. Caputi, R. Pello, V. Mainieiri, M. Mignoli, A. Iovino, V. Le Brun, S. J. Lilly, B. Garilli, C. Knobel, Christian Maier, F. Lamareille, D. Vergani, S. Bardelli, M. Bolzonella, Katarina Kovac, 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), E. Pérez-Montero, T. Contini, F. Lamareille, C. Maier, C. M. Carollo, J.-P. Kneib, O. Le Fèvre, S. Lilly, V. Mainieri, A. Renzini, M. Scodeggio, G. Zamorani, S. Bardelli, M. Bolzonella, A. Bongiorno, K. Caputi, O. Cucciati, S. de la Torre, L. de Ravel, P. Franzetti, B. Garilli, A. Iovino, P. Kampczyk, C. Knobel, K. Kovač, J.-F. Le Borgne, V. Le Brun, M. Mignoli, R. Pellò, Y. Peng, V. Presotto, E. Ricciardelli, J. D. Silverman, M. Tanaka, L. A. M. Tasca, L. Tresse, D. Vergani, E. Zucca, 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: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, Metallicity, MASS-METALLICITY RELATION, chemistry.chemical_element, FOS: Physical sciences, PHYSICAL-PROPERTIES, galaxies: starburst, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, COSMOLOGICAL HYDRODYNAMIC SIMULATIONS, 01 natural sciences, Physical cosmology, H-II REGIONS, galaxies: abundance, EMISSION-LINE GALAXIES, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, galaxies: fundamental parameter, Astrophysics::Galaxy Astrophysics, SIMILAR-TO 1.4, Chemical content, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, galaxies: fundamental parameters, VLT DEEP SURVEY, CHEMICAL ABUNDANCES, Nitrogen, Redshift, Galaxy, chemistry, Space and Planetary Science, DIGITAL SKY SURVEY, galaxies: abundances, galaxies: evolution, STELLAR MASS, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The chemical evolution of galaxies on a cosmological timescale is still a matter of debate despite the increasing number of available data provided by spectroscopic surveys of star-forming galaxies at different redshifts. The fundamental relations involving metallicity, such as the mass-metallicity relation (MZR) or the fundamental-metallicity relation, give controversial results about the reality of evolution of the chemical content of galaxies at a given stellar mass. In this work we shed some light on this issue using the completeness reached by the 20k bright sample of the zCOSMOS survey and using for the first time the nitrogen-to-oxygen ratio (N/O) as a tracer of the gas phase chemical evolution of galaxies that is independent of the star formation rate. Emission-line galaxies both in the SDSS and 20k zCOSMOS bright survey were used to study the evolution from the local Universe of the $MZR up to a redshift of 1.32 and the relation between stellar mass and nitrogen-to-oxygen ratio (MNOR) up to a redshift of 0.42 using the N2S2 parameter. All the physical properties derived from stellar continuum and gas emission-lines, including stellar mass, star formation rates, metallicity and N/O, were calculated in a self-consistent way over the full redshift range. We confirm the trend to find lower metallicities in galaxies of a given stellar mass in a younger Universe. This trend is even observed when taking possible selection effects into account that are due to the observed larger median star formation rates for galaxies at higher redshifts. We also find a significant evolution of the MNOR up to z = 0.4. Taking the slope of the O/H vs. N/O relation into account for the secondary-nitrogen production regime, the observed evolution of the MNOR is consistent with the trends found for both the MZR and its equivalent relation using new expressions to reduce its dependence on SFR., Comment: 15 pages, 13 figures. Accepted for publication in Astronomy & Astrophysics. Replaced to match published version and references corrected
Published: 2013
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21. Proto-groups at 1.8<z<3 in the zCOSMOS-deep sample

Author: C. Diener, S. J. Lilly, C. Knobel, G. Zamorani, G. Lemson, P. Kampczyk, N. Scoville, C. M. Carollo, T. Contini, J. P. Kneib, O. Le Fevre, V. Mainieri, A. Renzini, M. Scodeggio, S. Bardelli, M. Bolzonella, A. Bongiorno, K. Caputi, S. de la Torre, L. de Ravel, P. Franzetti, B. Garilli, A. Iovino, K. Kovac, F. Lamareille, J. F. Le Borgne, V. Le Brun, C. Maier, M. Mignoli, R. Pello', Y. Peng, E. Perez Montero, V. Presotto, J. Silverman, M. Tanaka, L. Tasca, L. Tresse, D. Vergani, E. Zucca, R. Bordoloi, A. Cappi, G. Coppa, A. M. Koekemoer, C. Lopez Sanjuan, H. J. McCracken, P. Nair, L. Pozzetti, N. Welikala, CUCCIATI, OLGA, CIMATTI, ANDREA, MORESCO, MICHELE ENNIO MARIA, C. Diener, S. J. Lilly, C. Knobel, G. Zamorani, G. Lemson, P. Kampczyk, N. Scoville, C. M. Carollo, T. Contini, J.-P. Kneib, O. Le Fevre, V. Mainieri, A. Renzini, M. Scodeggio, S. Bardelli, M. Bolzonella, A. Bongiorno, K. Caputi, O. Cucciati, S. de la Torre, L. de Ravel, P. Franzetti, B. Garilli, A. Iovino, K. Kovac, F. Lamareille, J.-F. Le Borgne, V. Le Brun, C. Maier, M. Mignoli, R. Pello', Y. Peng, E. Perez Montero, V. Presotto, J. Silverman, M. Tanaka, L. Tasca, L. Tresse, D. Vergani, E. Zucca, R. Bordoloi, A. Cappi, A. Cimatti, G. Coppa, A. M. Koekemoer, C. Lopez-Sanjuan, H. J. McCracken, M. Moresco, P. Nair, L. Pozzetti, and N. Welikala
Subjects: CATALOGS, GALAXIES: GROUPS: GENERAL, GALAXIES: HIGH-REDSHIFT, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We identify 42 "candidate groups" lying between 1.8 < z < 3.0 from a sample of 3502 galaxies with spectroscopic redshifts in the zCOSMOS-deep redshift survey within this same redshift interval. These systems contain three to five spectroscopic galaxies that lie within 500 kpc in projected distance (in physical space) and within 700 km s–1 in velocity. Based on extensive analysis of mock catalogs that have been generated from the Millennium simulation, we examine the likely nature of these systems at the time of observation, and what they will evolve into down to the present epoch. Although few of the "member" galaxies are likely to reside in the same halo at the epoch we observe them, 50% of the systems will have, by the present epoch, all of the member galaxies in the same halo, and almost all (93%) will have at least some of the potential members in the same halo. Most of the candidate groups can therefore be described as "proto-groups." A crude estimate of the overdensities of these structures is also consistent with the idea that these systems are being seen as they assemble. We also examine present-day halos and ask whether their progenitors would have been seen among our candidate groups. For present-day halos between 1014 and 1015 M ⊙ h –1, 35% should have appeared among our candidate groups, and this would have risen to 70% if our survey had been fully sampled, so we can conclude that our sample can be taken as representative of a large fraction of such systems. There is a clear excess of massive galaxies above 1010 M ⊙ around the locations of the candidate groups in a large independent COSMOS photo-z sample, but we see no evidence in this latter data for any color differentiation with respect to the field. This is, however, consistent with the idea that such differentiation arises in satellite galaxies, as indicated at z < 1, if the candidate groups are indeed only starting to be assembled.
Published: 2012

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

Author: R. Amorín, E. Pérez-Montero, T. Contini, J. M. Vílchez, M. Bolzonella, L. A. M. Tasca, F. Lamareille, G. Zamorani, C. Maier, C. M. Carollo, J.-P. Kneib, O. Le Fèvre, S. Lilly, V. Mainieri, A. Renzini, M. Scodeggio, S. Bardelli, A. Bongiorno, K. Caputi, O. Cucciati, S. de la Torre, L. de Ravel, P. Franzetti, B. Garilli, A. Iovino, P. Kampczyk, C. Knobel, K. Kovač, J.-F. Le Borgne, V. Le Brun, M. Mignoli, R. Pellò, Y. Peng, V. Presotto, E. Ricciardelli, J. D. Silverman, M. Tanaka, L. Tresse, D. Vergani, and E. Zucca
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, Star formation, FOS: Physical sciences, Astronomy and Astrophysics, Context (language use), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Photometry (optics), Stars, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Solar and Stellar Astrophysics, Surface brightness, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a thorough characterization of a large sample of 183 extreme emission-line galaxies (EELGs) at redshift 0.11 < z < 0.93 selected from the 20k zCOSMOS Bright Survey because of their unusually large emission line equivalent widths. We use multiwavelength COSMOS photometry, HST-ACS I-band imaging and optical zCOSMOS spectroscopy to derive the main global properties of EELGs, such as sizes, masses, SFRs, reliable metallicities from both "direct" and "strong-line" methods. The EELGs are compact (R_50 ~ 1.3 kpc), low-mass (log(M*/Msol)~7-10) galaxies forming stars at unusually high specific SFR (log(sSFR/yr) up to ~ -7) compared to main sequence SFGs of the same stellar mass and redshift. At UV wavelengths, the EELGs are luminous and show high surface brightness and include strong Ly$��$ 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, including a handful of extremely metal-deficient galaxies (, Accepted in A&A. Final replacement to match the version in press. It includes a minor change in the title and a new figure
Published: 2015

23. The nature of faint submillimetre-selected galaxies

Author: Ian Smail, J. P. Kneib, Rob Ivison, and Andrew Blain
Subjects: Physics, education.field_of_study, Astrophysics::High Energy Astrophysical Phenomena, Early universe, Population, Gravitational lensing, Astrophysics::Instrumentation and Methods for Astrophysics, Formation, Lens (geology), Starburst, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, evolution [Galaxies], Galaxy, Cosmology, Space and Planetary Science, Galaxy formation and evolution, education, Observations, Astrophysics::Galaxy Astrophysics
Abstract: We present the source catalogue for the SCUBA Lens Survey. We summarise the results of extensive multi-wavelength observations of the 15 submillimetre-selected galaxies in the catalogue, from X-rays to radio. We discuss the main observational characteristics of faint submillimetre galaxies as a population, and consider their interpretation within the framework of our understanding of galaxy formation and evolution.
Published: 2002
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24. Disentangling a group of lensed submm galaxies at z\xa0 2.9

Author: T. P. MacKenzie, D. Scott, I. Smail, E. L. Chapin, S. C. Chapman, A. Conley, A. Cooray, J. S. Dunlop, D. Farrah, M. Fich, A. G. Gibb, W. S. Holland, R. J. Ivison, T. Jenness, J.-P. Kneib, G. Marsden, J. Richard, E. I. Robson, I. Valtchanov, and J. L. Wardlow
Published: 2014

25. Evidence for major mergers of galaxies at 2 \u2272 z < 4 in the VVDS and VUDS surveys

Author: L. A. M. Tasca, O. Le Fxe8vre, C. Lxf3pez-Sanjuan, P.-W. Wang, P. Cassata, B. Garilli, O. Ilbert, V. Le Brun, B. C. Lemaux, D. Maccagni, L. Tresse, S. Bardelli, T. Contini, S. Charlot, O. Cucciati, A. Fontana, M. Giavalisco, J.-P. Kneib, M. Salvato, Y. Taniguchi, D. Vergani, G. Zamorani and E. Zucca
Published: 2014

26. [C II] and ^(12)CO(1-0) Emission Maps in HLSJ091828.6+514223: A Strongly Lensed Interacting System at z=5.24

Author: Ian Smail, J. P. Kneib, Giovanni G. Fazio, Andrew Blain, I. Valtchanov, Frédéric Boone, R. S. Bussmann, A. L. R. Danielson, Rob Ivison, P. van der Werf, Johan Richard, Gregory Walth, Miroslava Dessauges-Zavadsky, M. Rex, T. A. Jones, Daniel Schaerer, A. M. Swinbank, Michael Zemcov, Bruno Altieri, M. Zamojski, Pablo G. Pérez-González, Francoise Combes, Mark Gurwell, Eiichi Egami, T. D. Rawle, A. C. Edge, Benjamin Clément, Alain Omont, Steward Observatory, University of Arizona, AUTRES, Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University [Cambridge]-Smithsonian Institution, Royal Observatory Edinburgh (ROE), University of Edinburgh, Alfred-Wegener-Institut, Helmholtz-Zentrum für Polar- und Meeresforschung (AWI), 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), Institute for Computational Cosmology (ICC), Durham University, Department of Physics, Herschel Science Centre, European Space Agency (ESA), Department of Physics and Astronomy [Leicester], University of Leicester, Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), 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), Departamento de Física y Astronomía, Universidad Complutense de Madrid = Complutense University of Madrid [Madrid] (UCM), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), California Institute of Technology (CALTECH), Harvard University-Smithsonian Institution, 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), Agence Spatiale Européenne = European Space Agency (ESA), Université de Genève = University of Geneva (UNIGE), 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 Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), 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: Astrofísica, submillimeter: galaxies, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Continuum (design consultancy), FOS: Physical sciences, Astrophysics, Submillimeter Array, star formation [Galaxies], Spectral line, Luminosity, high-redshift [Galaxies], [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], galaxies: high-redshift, Physics, galaxies. [Submillimeter], Star formation, Astronomy and Astrophysics, Galaxy, Interstellar medium, Astronomía, Stars, 13. Climate action, Space and Planetary Science, galaxies: star formation, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present Submillimeter Array (SMA) [CII] 158um and Jansky Very Large Array (JVLA) $^{12}$CO(1-0) line emission maps for the bright, lensed, submillimeter source at $z=5.2430$ behind Abell 773: HLSJ091828.6+514223 (HLS0918). We combine these measurements with previously reported line profiles, including multiple $^{12}$CO rotational transitions, [CI], water and [NII], providing some of the best constraints on the properties of the interstellar medium (ISM) in a galaxy at $z>5$. HLS0918 has a total far-infrared (FIR) luminosity L_FIR(8-1000um) = (1.6$\pm$0.1)x10^14 L_sun/mu, where the total magnification mu_total = 8.9$\pm$1.9, via a new lens model from the [CII] and continuum maps. Despite a HyLIRG luminosity, the FIR continuum shape resembles that of a local LIRG. We simultaneously fit all of the observed spectral line profiles, finding four components which correspond cleanly to discrete spatial structures identified in the maps. The two most redshifted spectral components occupy the nucleus of a massive galaxy, with a source plane separation, 28 pages, 9 figures, accepted in ApJ
Published: 2014
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27. Detection of an Iron Emission Feature from the Lensed Broad Absorption Line QSO H1413+117 at [CLC][ITAL]z[/ITAL][/CLC] = 2.56

Author: K. Futamoto, Kazuhisa Mitsuda, K. Mori, N. Iyomoto, Naomi Ota, J. M. Miralles, Yasushi Ikebe, Makoto Hattori, Ryuichi Fujimoto, T. Oshima, and J. P. Kneib
Subjects: QSOS, Physics, Astrophysics::High Energy Astrophysical Phenomena, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Rest frame, Redshift, Space and Planetary Science, Emission spectrum, Continuum (set theory), Advanced CCD Imaging Spectrometer, Equivalent width, Line (formation)
Abstract: We present the X-ray energy spectrum of the lensed BAL QSO H1413+117 (the Cloverleaf) at z=2.56 observed with the Chandra X-ray observatory. We detected 293 photons in a 40 ks Advanced CCD Imaging Spectrometer (ACIS-S) observation. The X-ray image consists of four lensed image components, thus the photons are from the lensed QSO itself. The overall spectrum can be described with a power-law function heavily absorbed by neutral matter at a redshift consistent with the QSO redshift. This supports the idea that intrinsic absorption is significant for BAL QSOs. The spectral fit significantly (99% confidence) improves when we include an emission line. The centroid energy and intrinsic width (Gaussian \sigma) of the line are 6.21 \pm 0.16 keV and 220 ^{+270}_{-130} eV (90% errors), respectively, in the QSO rest frame, assuming the absorbed power-law as the continuum. The equivalent width of the line in the QSO rest frame is 960 ^{+1400}_{-480} eV. We suggest that the large equivalent width, the centroid energy, and the line broadness can be explained by iron K emission arising from X-ray reprocessing in the BAL flow, assuming it has a conical thin-sheet structure.
Published: 2001
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28. Detection of an Iron Emission Feature from the Lensed Broad Absorption Line QSO H1413+117 at z = 2.56

Author: Oshima, Tai, Mitsuda, Kazuhisa, Fujimoto, Ryuichi, Iyomoto, Naoko, Futamoto, Kazuo, Hattori, M., Ota, Naomi, Mori, K., Ikebe, Y., J., M. Miralles, and J.-P., Kneib
Abstract: 著者人数：11名, Accepted: 2001-11-13, 資料番号: SA1001388000
Published: 2001

29. [Untitled]

Author: R. Pelló, M. Bolzonella, L. E. Campusano, M. Dantel-Fort, B. Fort, J.-P. Kneib, J.-F. Le Borgne, Y. Mellier, R.S. Ellis, and I. Smail
Subjects: Gravitation, Physics, Wavelength, Space and Planetary Science, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Redshift, Galaxy
Abstract: We discuss the first results obtained on the study of a sample of high-z galaxies (2 < z < 7), using the gravitational amplification effect in the core of lensing clusters. Sources are located close to the critical lines in clusters with well constrained mass distributions, and selected through photometric redshifts, computed on a large wavelength domain, and lens inversion techniques.
Published: 2001
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30. Faint Submillimeter Galaxies: [ITAL]Hubble Space Telescope[/ITAL] Morphologies and Colors

Author: Ian Smail, Rob Ivison, Andrew Blain, and J. P. Kneib
Subjects: Physics, education.field_of_study, Star formation, media_common.quotation_subject, Population, Continuum (design consultancy), Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy, Universe, Redshift, Space and Planetary Science, Galaxy formation and evolution, education, Astrophysics::Galaxy Astrophysics, media_common
Abstract: We present optical morphologies obtained from deep HST and ground-based images for galaxies selected from the first sub-millimeter survey of the distant Universe. Our sample comprises galaxies detected in deep 850-micron continuum maps of seven massive clusters, obtained using SCUBA, the new bolometer camera on the JCMT. The survey covers a total area of 0.01 square degrees to 1-sigma noise levels of about 2 mJy/beam. We detect a total of 25 sources at 850 microns, of which 17 and 10 are brighter than the respective 50% and 80% completeness limits. Optical counterparts are identified for 14 of the 16 sources in the f(50%) sample and for 9 of the 10 sources in the f(80%) sample that lie within our optical fields. The morphologies of those galaxies for which we have HST imaging fall into three broad categories: faint disturbed galaxies and interactions; faint galaxies too compact to classify reliably; and dusty, star-forming galaxies at intermediate redshifts. The disturbed and interacting galaxies constitute the largest class, which suggests that interactions remain an important mechanism for triggering star formation and the formation of ultraluminous galaxies in the distant Universe. The faint, compact galaxies may represent a later evolutionary stage in these mergers, or more centrally-concentrated starbursts. It is likely that some of these will host AGN. Analysis of the colors of our sample allow us to estimate a crude redshift distribution: >75% have z 50% lie at z
Published: 1998
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31. Evidence for major mergers of galaxies at 2 â² z < 4 in the VVDS and VUDS surveys

Author: L. A. M. Tasca, O. Le Fèvre, C. López-Sanjuan, P.-W. Wang, P. Cassata, B. Garilli, O. Ilbert, V. Le Brun, B. C. Lemaux, D. Maccagni, L. Tresse, S. Bardelli, T. Contini, S. Charlot, O. Cucciati, A. Fontana, M. Giavalisco, J.-P. Kneib, M. Salvato, Y. Taniguchi, D. Vergani, G. Zamorani, and E. Zucca
Subjects: Physics, Stellar mass, 010308 nuclear & particles physics, Star formation, Galaxies: high-redshift, Context (language use), Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy merger, Mass ratio, Galaxies: formation, Space and Planetary Science, 01 natural sciences, Redshift, Galaxy, Photometry (optics), 0103 physical sciences, 010303 astronomy & 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 redshi fts 2. z< 4 and discuss the impact of major mergers in shaping 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 t he contribution of merging processes to the early mass assembly of galaxies. Methods. We search for galaxy pairs with a transverse separation rp ≤ 25 h −1 kpc and a velocity differencev≤ 500 km s −1 using the VIMOS VLT Deep Survey (VVDS) and early data from the VIMOSUltra Deep Survey (VUDS) that comprise a sample of 1111 galaxies with spectroscopic redshifts measurements at redshifts 1.8≤ z≤ 4 in the COSMOS, ECDFS, and VVDS-02h fields. We analyse their spectra and associated visible and near-infr ared photometry to assess the main properties of merging galaxies that have an average stellar mass M⋆ = 2.3× 10 10 M⊙ at these redshifts. Results. Using the 12 physical pairs found in our sample we obtain a firs t estimate of the merger fraction at these rdshifts, fmerg∼ (15− 20)%. The pair separations indicate that these pairs will merge within 1 Gyr, on average, with each producing a more massive galaxy by the time the cosmic star formation peaks at z∼ 1− 2. From the average mass ratio between galaxies in the pairs, the stellar mass of the resulting galaxy after merging will be∼ 60% larger than the most massive galaxy in the pair before merging. We conclude that major merging of galaxy pairs is on-going at 2. z< 4 and significantly contributing to the major assembly phase of galaxies at this early epoch.
Published: 2014

32. Molecular gas content in strongly-lensed z~1.5-3 star-forming galaxies with low IR luminosities

Author: Andrew Blain, T. Rawle, J. P. Kneib, Daniel Schaerer, A. M. Swinbank, M. Rex, Francoise Combes, J. Richard, Eiichi Egami, Frederic Boone, Panos Sklias, Miroslava Dessauges-Zavadsky, M. Zamojski, Observatoire de Genève, 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'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), 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), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Galaxies et cosmologie, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Steward Observatory, University of Arizona, Institute for Computational Cosmology, Department of Physics, Durham University, Durham (ICC), Centre de Recherche Astrophysique de Lyon (CRAL), 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), European Space Astronomy Centre (ESAC), Agence Spatiale Européenne = European Space Agency (ESA), Ecole Polytechnique Federale de Lausanne (EPFL), 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 Department of Physics & Astronomy, University of Leicester
Subjects: Physics, Stellar mass, Gas depletion, Star formation, Infrared, Plateau de Bure Interferometer, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Luminosity, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: To extend the molecular gas measurements to typical star-forming galaxies (SFGs) with SFR < 40 Msun yr^{-1} and M* < 2.5x10^{10} Msun at z~1.5-3, we have observed CO emission with the IRAM Plateau de Bure Interferometer and 30m telescope for five strongly-lensed galaxies selected from the Herschel Lensing Survey. These observations are combined with a compilation of CO measurements from the literature. We infer the luminosity correction factors r2,1 = 0.81+/-0.20 and r3,1 = 0.57+/-0.15 for the J=2 and J=3 CO transitions, respectively, valid for SFGs at z>1. The combined sample of CO-detected SFGs at z>1 shows a large spread in star formation efficiency (SFE), such that SFE extend beyond the low values of local spirals and overlap the distribution of z>1 sub-mm galaxies. We find that the spread in SFE (or equivalently in molecular gas depletion timescale) is due to primarily the specific star formation rate, but also stellar mass and redshift. Correlations of SFE with the offset from the main-sequence and the compactness of the starburst are less clear. The increase of the molecular gas depletion timescale with M* now revealed by low M* SFGs at z>1 and observed at z=0 is in contrast to the admitted constant molecular gas depletion timescale and the linear Kennicutt-Schmidt relation. We confirm an increase of the molecular gas fraction (fgas) from z~0.2 to z~1.2, followed by a very mild increase toward higher redshifts. At each redshift fgas shows a large dispersion due to the dependence of fgas on M*, producing a gradient of increasing fgas with decreasing M*. We provide the first measure of fgas of z>1 SFGs at the low-M* end (10^{9.4} < M*/Msun < 10^{9.9}), reaching a mean fgas = 0.69+/-0.18, which shows a clear fgas upturn. Finally, we find evidence for a non-universal dust-to-gas ratio among high-redshift SFGs and sub-mm galaxies, local spirals and ULIRGs with near-solar metallicities., 21 pages, 16 figures. Accepted in A&A
Published: 2014
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33. Star formation histories, extinction, and dust properties of strongly lensed z~1.5-3 star-forming galaxies from the Herschel Lensing Survey

Author: Miroslava Dessauges-Zavadsky, M. Zamojski, Ian Smail, M. Rex, Eiichi Egami, Bruno Altieri, T. Rawle, P. van der Werf, J. P. Kneib, Johan Richard, Frédéric Boone, Daniel Schaerer, Panos Sklias, J. M. Simpson, Observatoire Astronomique de l'Université de Genève (ObsGE), 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), Steward Observatory, University of Arizona, Alfred-Wegener-Institut, Helmholtz-Zentrum für Polar- und Meeresforschung (AWI), Centre de Recherche Astrophysique de Lyon (CRAL), 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), AUTRES, Institute for Computational Cosmology (ICC), Durham University, Leiden Observatory [Leiden], Universiteit Leiden, Herschel Science Centre, Agence Spatiale Européenne = European Space Agency (ESA), 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), Université de Genève (UNIGE), 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), 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), Universiteit Leiden [Leiden], European Space Agency (ESA), 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: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Extinction, Stellar population, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Extinction (astronomy), FOS: Physical sciences, galaxies: starburst, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, infrared: galaxies, Photometry (optics), high-redshift [Galaxies], [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], galaxies [Infrared], galaxies: high-redshift, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Emission spectrum, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Star formation, extinction, Astronomy and Astrophysics, Dust, Redshift, Galaxy, starburst [Galaxies], 13. Climate action, Space and Planetary Science, dust, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Multi-wavelength, optical to IR/sub-mm observations of 5 strongly lensed galaxies identified by the Herschel Lensing Survey, plus two well-studied lensed galaxies, MS1512-cB58 and the Cosmic Eye, for which we also provide updated Herschel measurements, are used to determine the physical properties of z~1.5-3 star-forming galaxies close to or below the detection limits of blank fields. We constrain their stellar and dust content, determine star formation rates and histories, dust attenuation and extinction laws, and other related properties. We perform SED-fits of the full photometry of each object as well for the optical and infrared parts separately, exploring various parameters, including nebular emission. The IR observations and emission line measurements, where available, are used a posteriori constraints on the models. Besides the various stellar population models we explore, we use the observed IR/UV ratio to estimate the extinction and create "energy conserving models", that constrain most accurately the physical properties of our sources. Our sample has a median lensing-corrected IR luminosity ~ 3e11 Lsun, stellar masses between 2e9 and 2e11 Msun, and IR/UV luminosity ratios spanning a wide range. The dust masses of our galaxies are in the range 2 to 17e7 Msun, extending previous studies at the same redshift down to lower masses. We do not find any particular trend of the dust temperature Tdust with IR luminosity, suggesting an overall warmer dust regime at our redshift regardless of luminosity. Lensing enables us to study the detailed physical properties of individual IR-detected z~1.5-3 galaxies up to a factor ~10 fainter than achieved with deep blank field observations. We demonstrate that multi-wavelength observations combining stellar and dust emission can constrain star formation histories and extinction laws of star-forming galaxies., 27 pages, 19 figures
Published: 2013
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34. Mass assembly in quiescent and star-forming galaxies since

Author: O. Ilbert, H. J. McCracken, O. Le Fxe8vre, P. Capak, J. Dunlop, A. Karim, M. A. Renzini, K. Caputi, S. Boissier, S. Arnouts, H. Aussel, J. Comparat, Q. Guo, P. Hudelot, J. Kartaltepe, J. P. Kneib, J. K. Krogager, E. Le Floc’h, S. Lilly, Y. Mellier, B. Milvang-Jensen, T. Moutard, M. Onodera, J. Richard, M. Salvato, D. B. Sanders, N. Scoville, J. D. Silverman, Y. Taniguchi, L. Tasca, R. Thomas, S. Toft, L. Tresse, D. Vergani, M. Wolk, and A. Zirm
Published: 2013

35. HerMES: A Deficit in the Surface Brightness of the Cosmic Infrared Background due to Galaxy Cluster Gravitational Lensing

Author: M. Zemcov, A. Blain, A. Cooray, M. Béthermin, J. Bock, D. L. Clements, A. Conley, L. Conversi, C. D. Dowell, D. Farrah, J. Glenn, M. Griffin, M. Halpern, E. Jullo, J.-P. Kneib, G. Marsden, H. T. Nguyen, S. J. Oliver, J. Richard, I. G. Roseboom, B. Schulz, Douglas Scott, D. L. Shupe, A. J. Smith, I. Valtchanov, M. Viero, L. Wang, J. Wardlow, California Institute of Technology (CALTECH), Department of Physics and Astronomy [Leicester], University of Leicester, 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), Computing and Mathematical Sciences [Pasadena]], Astrophysics Group, Blackett Laboratory, Imperial College London-Imperial College London, Center for Astrophysics and Space Astronomy [Boulder] (CASA), University of Colorado [Boulder], Herschel Science Center [Madrid], European Space Astronomy Centre (ESAC), Agence Spatiale Européenne = European Space Agency (ESA)-Agence Spatiale Européenne = European Space Agency (ESA), Astronomy Centre, University of Sussex, School of Physics and Astronomy [Cardiff], Cardiff University, Department of Physics and Astronomy [Vancouver], University of British Columbia (UBC), 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 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), AUTRES, Centre de Recherche en Acquisition et Traitement de l'Image pour la Santé (CREATIS), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université Jean Monnet - Saint-Étienne (UJM)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), Department of Astronomy, University of California [Irvine] (UC Irvine), University of California (UC)-University of California (UC), 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 Space Agency (ESA)-European Space Agency (ESA), 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), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Hospices Civils de Lyon (HCL)-Université Jean Monnet [Saint-Étienne] (UJM)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), University of California [Irvine] (UCI), University of California-University of California, 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), Université Jean Monnet [Saint-Étienne] (UJM)-Hospices Civils de Lyon (HCL)-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Université de Lyon-Institut National des Sciences Appliquées (INSA)-Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut National de la Santé et de la Recherche Médicale (INSERM)
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, cosmic background radiation, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Wavelength, Spire, Amplitude, Gravitational lens, Space and Planetary Science, Cosmic infrared background, 0103 physical sciences, Angular resolution, Surface brightness, 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We have observed four massive galaxy clusters with the SPIRE instrument on the Herschel Space Observatory and measure a deficit of surface brightness within their central region after subtracting sources. We simulate the effects of instrumental sensitivity and resolution, the source population, and the lensing effect of the clusters to estimate the shape and amplitude of the deficit. The amplitude of the central deficit is a strong function of the surface density and flux distribution of the background sources. We find that for the current best fitting faint end number counts, and excellent lensing models, the most likely amplitude of the central deficit is the full intensity of the cosmic infrared background (CIB). Our measurement leads to a lower limit to the integrated total intensity of the CIB of I(250 microns) > 0.69_(-0.03)^(+0.03) (stat.)_(-0.06)^(+0.11) (sys.) MJy/sr, with more CIB possible from both low-redshift sources and from sources within the target clusters. It should be possible to observe this effect in existing high angular resolution data at other wavelengths where the CIB is bright, which would allow tests of models of the faint source component of the CIB., 5 pages, 3 figures, replacing with version matching published manuscript
Published: 2013
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36. The role of major mergers in shaping galaxies at 2<z<4 in the VUDS and VVDS surveys

Author: L. A. M. Tasca, O. Le Fevre, C. Lopez-Sanjuan, P.-W. Wang, P. Cassata, B. Garilli, O. Ilbert, V. Le Brun, B. C. Lemaux, D. Maccagni, L. Tresse, S. Bardelli, T. Contini, O. Cucciati, A. Fontana, M. Giavalisco, J.-P. Kneib, M. Salvato, Y. Taniguchi, D. Vergani, G. Zamorani, and E. Zucca
Subjects: Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: 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, Comment: 12 pages, 12 figures, submitted to A&A
Published: 2013

37. Spot the difference - Impact of different selection criteria on observed properties of passive galaxies in zCOSMOS-20k sample

Author: O. Cucciati, S. J. Lilly, Christian Maier, E. Le Floc'h, D. Vergani, John D. Silverman, C. Lopez-Sanjuan, S. de la Torre, Nick Scoville, F. Lamareille, A. Cappi, A. Cimatti, Luke A. Barnes, Y. Peng, Enrique Perez-Montero, Alvio Renzini, Katarina Kovac, P. Kampczyk, C. M. Carollo, L. A. M. Tasca, J. F. Le Borgne, Masaomi Tanaka, Michele Moresco, Angela Bongiorno, A. Iovino, Pradip Nair, L. de Ravel, V. Presotto, Claudia Scarlata, K. Caputi, E. Zucca, S. Bardelli, T. Contini, G. Zamorani, J. P. Kneib, Niraj Welikala, O. Le Fevre, L. Tresse, Anton M. Koekemoer, Marco Scodeggio, C. Knobel, Rongmon Bordoloi, M. Bolzonella, C. Diener, V. Le Brun, Lucia Pozzetti, B. Garilli, P. Franzetti, Vincenzo Mainieri, Pascal Oesch, R. Pello, M. Mignoli, H. J. McCracken, 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), 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), 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), Moresco M., Pozzetti L., Cimatti A., Zamorani G., Bolzonella M., Lamareille F., Mignoli M., Zucca E., Lilly S. J., Carollo C. M., Contini T., Kneib J.-P., Le Fèvre O., Mainieri V., Renzini 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., Maier C., Pelló R., Peng Y., Perez-Montero E., Presotto V., Silverman J. D., Tanaka M., Tasca L., Tresse L., Vergani D., Barnes L., Bordoloi R., Cappi A., Diener C., Koekemoer A. M., Le Floc'h E., López-Sanjuan C., McCracken H. J., Nair P., Oesch P., Scarlata C., Scoville N., Welikala N., and Astronomy
Subjects: ACTIVE GALACTIC NUCLEI, Galaxies: fundamental parameters, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Galaxies: statistics, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Sample (material), Population, FOS: Physical sciences, PHYSICAL-PROPERTIES, SPECTRAL ENERGY-DISTRIBUTIONS, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Surveys, 01 natural sciences, 0103 physical sciences, STAR-FORMING GALAXIES, Astrophysics::Solar and Stellar Astrophysics, Emission spectrum, education, PHOTOMETRIC REDSHIFTS, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Selection (genetic algorithm), REDSHIFT SURVEY, Physics, education.field_of_study, 010308 nuclear & particles physics, Star formation, Cosmology: observations, Galaxies: high-redshift, Galaxies: statistics, Large-scale structure of Universe, Galaxies: evolution, Astronomy and Astrophysics, VLT DEEP SURVEY, Galaxy, 13. Climate action, Space and Planetary Science, Outlier, STELLAR MASS FUNCTION, DIGITAL SKY SURVEY, Spectral energy distribution, 10K-BRIGHT SPECTROSCOPIC SAMPLE, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present the analysis of photometric, spectroscopic, and morphological properties for differently selected samples of passive galaxies up to z=1 extracted from the zCOSMOS-20k spectroscopic survey. This analysis intends to explore the dependence of galaxy properties on the selection criterion adopted, study the degree of contamination due to star-forming outliers, and provide a comparison between different commonly used selection criteria. We extracted from the zCOSMOS-20k catalog six different samples of passive galaxies, based on morphology, optical colors, specific star-formation rate, a best fit to the observed spectral energy distribution, and a criterion that combines morphological, spectroscopic, and photometric information. The morphological sample has the higher percentage of contamination in colors, specific star formation rate and presence of emission lines, while the red & passive ETGs sample is the purest, with properties mostly compatible with no star formation activity; however, it is also the less economic criterion in terms of information used. The best performing among the other criteria are the red SED and the quiescent ones, providing a percentage of contamination only slightly higher than the red & passive ETGs criterion (on average of a factor of ~2) but with absolute values of the properties of contaminants still compatible with a red, passively evolving population. We also provided two revised definitions of early type galaxies based on restframe color-color and color-mass criteria, that better reproduce the observed bimodalities. The analysis of the number densities shows evidences of mass-assembly downsizing, with galaxies at 10.25, Comment: 20 pages, 14 figures, 2 tables, accepted for publication in A\&A
Published: 2013
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38. ENVIRONMENTAL EFFECTS IN THE INTERACTION AND MERGING OF GALAXIES IN zCOSMOS

Author: P. Kampczyk, S. J. Lilly, L. de Ravel, O. Le Fèvre, M. Bolzonella, C. M. Carollo, C. Diener, C. Knobel, K. Kovač, C. Maier, A. Renzini, M. T. Sargent, D. Vergani, U. Abbas, S. Bardelli, A. Bongiorno, R. Bordoloi, K. Caputi, T. Contini, G. Coppa, O. Cucciati, S. de la Torre, P. Franzetti, B. Garilli, A. Iovino, J.-P. Kneib, A. M. Koekemoer, F. Lamareille, J.-F. Le Borgne, V. Le Brun, A. Leauthaud, V. Mainieri, M. Mignoli, R. Pello, Y. Peng, E. Perez Montero, E. Ricciardelli, M. Scodeggio, J. D. Silverman, M. Tanaka, L. Tasca, L. Tresse, G. Zamorani, E. Zucca, D. Bottini, A. Cappi, P. Cassata, A. Cimatti, M. Fumana, L. Guzzo, J. Kartaltepe, C. Marinoni, H. J. McCracken, P. Memeo, B. Meneux, P. Oesch, C. Porciani, L. Pozzetti, R. Scaramella, AUTRES, Institute for Astronomy [Zürich], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), University of Chicago, Laboratoire Léon Brillouin (LLB - UMR 12), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), INAF - Osservatorio Astrofisico di Torino (OATo), College of Computing (GATECH), Georgia Institute of Technology [Atlanta], Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Dipartimento di Fisica, Università degli Studi di Milano-Bicocca = University of Milano-Bicocca (UNIMIB)-Università degli Studi di Milano = University of Milan (UNIMI), Ecole Polytechnique Fédérale de Lausanne (EPFL), Institut de recherche en astrophysique et planétologie (IRAP), California Institute of Technology (CALTECH), European Southern Observatory (ESO), Hunan Normal University (HNU), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), National Optical Astronomy Observatory (NOAO), 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), 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), Astronomy, 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), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS)-Université Paris-Saclay, Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Università degli Studi di Milano-Bicocca [Milano] (UNIMIB)-Università degli Studi di Milano [Milano] (UNIMI), 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), Hunan Normal University, Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre 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), Kampczyk P., Lilly S. J., de Ravel L., Le Fèvre O., Bolzonella M., Carollo C. M., Diener C., Knobel C., Kovac K., Maier C., Renzini A., Sargent M. T., Vergani D., Abbas U., Bardelli S., Bongiorno A., Bordoloi R., Caputi K., Contini T., Coppa G., Cucciati O., de la Torre S., Franzetti P., Garilli B., Iovino A., Kneib J.-P., Koekemoer A. M., Lamareille F., Le Borgne J.-F., Le Brun V., Leauthaud A., Mainieri V., Mignoli M., Pello R., Peng Y., Perez Montero E., Ricciardelli E., Scodeggio M., Silverman J. D., Tanaka M., Tasca L., Tresse L., Zamorani G., Zucca E., Bottini D., Cappi A., Cassata P., Cimatti A., Fumana M., Guzzo L., Kartaltepe J., Marinoni C., McCracken H. J., Memeo P., Meneux B., Oesch P., Porciani C., Pozzetti L., and Scaramella R.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010504 meteorology & atmospheric sciences, Population, FOS: Physical sciences, galaxies: starburst, MORPHOLOGICAL TRANSFORMATION, Astrophysics, Kinematics, Astrophysics::Cosmology and Extragalactic Astrophysics, STAR-FORMATION RATES, MERGER RATE EVOLUTION, 01 natural sciences, SIMILAR-TO 1, galaxies: evolution, galaxies: general, galaxies: interactions, Astronomy and Astrophysics, Space and Planetary Science, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, Fraction (mathematics), education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, QB, Physics, education.field_of_study, FORMATION HISTORY, Star formation, CLOSE PAIRS, Cosmology: observations, Galaxies: high-redshift, Galaxies: statistics, Large-scale structure of Universe, CNOC2 REDSHIFT SURVEY, DISK GALAXIES, Environmental variation, Galaxy, Redshift, COSMOS FIELD, DIGITAL SKY SURVEY, Irregular galaxy, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: (Abridged) We analyze the environments and galactic properties (morphologies and star-formation histories) of a sample of 153 close kinematic pairs in the redshift range 0.2 < z < 1 identified in the zCOSMOS-bright 10k spectroscopic sample of galaxies. Correcting for projection effects, the fraction of close kinematic pairs is three times higher in the top density quartile than in the lowest one. This translates to a three times higher merger rate because the merger timescales are shown, from mock catalogues based on the Millennium simulation, to be largely independent of environment once the same corrections for projection is applied. We then examine the morphologies and stellar populations of galaxies in the pairs, comparing them to control samples that are carefully matched in environment so as to remove as much as possible the well-known effects of environment on the properties of the parent population of galaxies. Once the environment is properly taken into account in this way, we find that the early-late morphology mix is the same as for the parent population, but that the fraction of irregular galaxies is boosted by 50-75%, with a disproportionate increase in the number of irregular-irregular pairs (factor of 4-8 times), due to the disturbance of disk galaxies. Future dry-mergers, involving elliptical galaxies comprise less than 5% of all close kinematic pairs. In the closest pairs, there is a boost in the specific star-formation rates of star-forming galaxies of a factor of 2-4, and there is also evidence for an increased incidence of post star-burst galaxies. Although significant for the galaxies involved, the "excess" star-formation associated with pairs represents only about 5% of the integrated star-formation activity in the parent sample. Although most pair galaxies are in dense environments, the effects of interaction appear to be largest in the lower density environments., 38 pages, 17 figures, submitted to ApJ
Published: 2013
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39. The dominant role of mergers in the size evolution of massive early-type galaxies since z ~ 1

Author: C. Lxf3pez-Sanjuan, O. Le Fxe8vre, O. Ilbert, L. A. M. Tasca, C. Bridge, O. Cucciati, P. Kampczyk, L. Pozzetti, C. K. Xu, C. M. Carollo, T. Contini, J.-P. Kneib, S. J. Lilly, V. Mainieri, A. Renzini, D. Sanders, M. Scodeggio, N. Z. Scoville, Y. Taniguchi, G. Zamorani, H. Aussel, S. Bardelli, M. Bolzonella, A. Bongiorno, P. Capak, K. Caputi, S. de la Torre, L. de Ravel, P. Franzetti, B. Garilli, A. Iovino, C. Knobel, K. Kovač, F. Lamareille, J.-F. Le Borgne, V. Le Brun, E. Le Floc'h, C. Maier, H. J. McCracken, and M
Published: 2012

40. The bright end of the luminosity function at z ~ 9

Author: J. F. Le Borgne, Daniel Schaerer, Johan Richard, J. P. Kneib, Matthew Hayes, Frédéric Boone, Francoise Combes, R. Pello, Nicolas Laporte, 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), Centre de Recherche Astrophysique de Lyon (CRAL), 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), 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 d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), 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), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), 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), 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 - Paris (ENS Paris), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), and 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)-Université Fédérale Toulouse Midi-Pyrénées-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: Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], media_common.quotation_subject, first stars, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], galaxies: high-redshift, 0103 physical sciences, dark ages, 010306 general physics, Spectroscopy, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, Luminosity function (astronomy), Physics, Star formation, Astronomy and Astrophysics, Universe, Redshift, Galaxy, Space and Planetary Science, Magnitude (astronomy), reionization, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We report new constraints on the galaxy luminosity function at z~9 based on observations carried out with ESO/VLT FORS2, HAWK-I and X-Shooter around the lensing cluster A2667, as part of our project aimed at selecting z~7-10 candidates accessible to spectroscopy. Only one J-dropout source was selected in this field fulfilling the color and magnitude criteria. This source was recently confirmed as a mid-z interloper based on X-Shooter spectroscopy. The depth and the area covered by our survey are well suited to set strong constraints on the bright-end of the galaxy luminosity function and hence on the star formation history at very high redshift. The non-detection of reliable J-dropout sources over the ~36arcmin2 field of view towards A2667 was used to carefully determine the lens-corrected effective volume and the corresponding upper-limit on the density of sources. The strongest limit is obtained for Phi(M_{1500}=-21.4+/-0.50)-19.7 with fixed alpha=-1.74 and Phi*=1.10x10^{-3}Mpc^{-3}. The corresponding star formation rate density should be rho_{SFR}, 4 pages, 2 figures, accepted for publication in A&A Letters
Published: 2012
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41. A bright z = 5.2 lensed submillimeter galaxy in the field of Abell 773. HLSJ091828.6+514223

Author: Alastair C. Edge, Mark Gurwell, Daniel Schaerer, A. Berciano Alba, François Combes, Alain Omont, Marie Rex, Graham P. Smith, Ian Smail, P. van der Werf, Caitlin M. Casey, Nobuhiro Okabe, Frédéric Boone, Eiichi Egami, T. D. Rawle, Giovanni G. Fazio, R. Pello, Rob Ivison, Johan Richard, Miroslava Dessauges-Zavadsky, J. P. Kneib, A. M. Swinbank, Pablo G. Pérez-González, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), 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), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Alfred-Wegener-Institut, Helmholtz-Zentrum für Polar- und Meeresforschung (AWI), Steward Observatory, University of Arizona, 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), Institute for Computational Cosmology (ICC), Durham University, Centre de Recherche Astrophysique de Lyon (CRAL), 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), Royal Observatory Edinburgh (ROE), University of Edinburgh, Centre for Astronomy, Harvard University, IOA, University of Hawai‘i [Mānoa] (UHM), 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), Netherlands Institute for Radio Astronomy (ASTRON), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève = University of Geneva (UNIGE), Department of Physics, Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University-Smithsonian Institution, 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), Astronomical institute, Tohoku University, Tohoku University [Sendai], Departamento de Física y Astronomía, Universidad Complutense de Madrid = Complutense University of Madrid [Madrid] (UCM), University of Reading (UOR), Leiden Observatory [Leiden], Universiteit Leiden, Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), 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)-Université Fédérale Toulouse Midi-Pyrénées-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), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Harvard University [Cambridge], Université de Genève (UNIGE), Harvard University [Cambridge]-Smithsonian Institution, Universiteit Leiden [Leiden], École normale supérieure - Paris (ENS Paris), 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), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), 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: Astrofísica, submillimeter: galaxies, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Active galactic nucleus, Evolution, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], High-redshift, FOS: Physical sciences, Astrophysics, 01 natural sciences, Luminosity, infrared: galaxies, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], galaxies: high-redshift, 0103 physical sciences, Galaxy formation and evolution, Submillimeter, HLSJ091828.6+514223, 010303 astronomy & astrophysics, ISM, Galaxy cluster, Line (formation), Physics, Luminous infrared galaxy, 010308 nuclear & particles physics, Astronomy and Astrophysics, Galaxies, galaxies: individual: HLSJ091828.6+514223, Galaxy, Redshift, Astronomía, Space and Planetary Science, infrared, galaxies: evolution, galaxies: ISM, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: During our Herschel Lensing Survey (HLS) of massive galaxy clusters, we have discovered an exceptionally bright source behind the z=0.22 cluster Abell 773, which appears to be a strongly lensed submillimeter galaxy (SMG) at z=5.2429. This source is unusual compared to most other lensed sources discovered by Herschel so far, because of its higher submm flux (\sim 200mJy at 500\micron) and its high redshift. The dominant lens is a foreground z=0.63 galaxy, not the cluster itself. The source has a far-infrared (FIR) luminosity of L_FIR= 1.1 10^{14}/\mu Lo, where \mu is the magnification factor, likely \sim 11. We report here the redshift identification through CO lines with the IRAM-30m, and the analysis of the gas excitation, based on CO(7-6), CO(6-5), CO(5-4) detected at IRAM and the CO(2-1) at the EVLA. All lines decompose into a wide and strong red component, and a narrower and weaker blue component, 540\kms apart. Assuming the ultraluminous galaxy (ULIRG) CO-to-H2 conversion ratio, the H2 mass is 5.8 10^{11}/\mu Mo, of which one third is in a cool component. From the CI line we derive a CI/H2 number abundance of 6 10^{-5} similar to that in other ULIRGs. The H2O line is strong only in the red velocity component, with an intensity ratio I(H_2O)/I(CO) \sim 0.5, suggesting a strong local FIR radiation field, possibly from an active nucleus (AGN) component. We detect the [NII]205\mics line for the first time at high-z. It shows comparable blue and red components, with a strikingly broad blue one, suggesting strong ionized gas flows., Comment: 5 pages, 4 figures, to be published in A and A Letters
Published: 2012
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42. Dissecting Photometric Redshift for Active Galactic Nucleus Using XMM- and Chandra-COSMOS Samples

Author: M. Salvato, O. Ilbert, G. Hasinger, A. Rau, F. Civano, G. Zamorani, M. Brusa, M. Elvis, C. Vignali, H. Aussel, A. Comastri, F. Fiore, E. Le Floc'h, V. Mainieri, S. Bardelli, M. Bolzonella, A. Bongiorno, P. Capak, K. Caputi, N. Cappelluti, C. M. Carollo, T. Contini, B. Garilli, A. Iovino, S. Fotopoulou, A. Fruscione, R. Gilli, C. Halliday, J.-P. Kneib, Y. Kakazu, J. S. Kartaltepe, A. M. Koekemoer, K. Kovac, Y. Ideue, H. Ikeda, C. D. Impey, O. Le Fevre, F. Lamareille, G. Lanzuisi, J.-F. Le Borgne, V. Le Brun, S. Lilly, C. Maier, S. Manohar, D. Masters, H. McCracken, H. Messias, M. Mignoli, B. Mobasher, T. Nagao, R. Pello, S. Puccetti, E. Perez-Montero, A. Renzini, M. Sargent, D. B. Sanders, M. Scodeggio, N. Scoville, P. Shopbell, J. Silvermann, Y. Taniguchi, L. Tasca, L. Tresse, J. R. Trump, E. Zucca, Astronomy, Salvato M., Ilbert O., Hasinger G., Rau A., Civano F., Zamorani G., Brusa M., Elvis M., Vignali C., Aussel H., Comastri A., Fiore F., Le Floc'h E., Mainieri V., Bardelli S., Bolzonella M., Bongiorno A., Capak P., Caputi K., Cappelluti N., Carollo C. M., Contini T., Garilli B., Iovino A., Fotopoulou S., Fruscione A., Gilli R., Halliday C., Kneib J.-P., Kakazu Y., Kartaltepe J. S., Koekemoer A. M., Kovac K., Ideue Y., Ikeda H., Impey C. D., Le Fevre O., Lamareille F., Lanzuisi G., Le Borgne J.-F., Le Brun V., Lilly S., Maier C., Manohar S., Masters D., McCracken H., Messias H., Mignoli M., Mobasher B., Nagao T., Pello R., Puccetti S., Perez-Montero E., Renzini A., Sargent M., Sanders D. B., Scodeggio M., Scoville N., Shopbell P., Silvermann J., Taniguchi Y., Tasca L., Tresse L., Trump J. R., Zucca E., Laboratoire d'Astrophysique de Marseille (LAM), and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Active galactic nucleus, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, SPECTRAL ENERGY-DISTRIBUTIONS, 01 natural sciences, Radio spectrum, Photometry (optics), techniques: photometric, S-COSMOS, surveys, 0103 physical sciences, STAR-FORMING GALAXIES, Astrophysics::Solar and Stellar Astrophysics, [INFO]Computer Science [cs], survey, Emission spectrum, DEEP-FIELD, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, Photometric redshift, Physics, LEGACY SURVEY, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Sigma, Astronomy and Astrophysics, methods: data analysis, Redshift, Galaxy, galaxies: distances and redshift, X-rays: galaxies, EXTENDED GROTH STRIP, Space and Planetary Science, LUMINOSITY FUNCTION, MULTICOLOR CLASSIFICATION, DIGITAL SKY SURVEY, galaxies: distances and redshifts, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics, WIDE-FIELD SURVEY
Abstract: With this paper, we release accurate photometric redshifts for 1692 counterparts to Chandra sources in the central square degree of the COSMOS field. The availability of a large training set of spectroscopic redshifts that extends to faint magnitudes enabled photometric redshifts comparable to the highest quality results presently available for normal galaxies. We demonstrate that morphologically extended, faint X-ray sources without optical variability are more accurately described by a library of normal galaxies (corrected for emission lines) than by AGN-dominated templates, even if these sources have AGN-like X-ray luminosities. Preselecting the library on the bases of the source properties allowed us to reach an accuracy sigma_(Delta z/(1+z_spec)) \sim0.015 with a fraction of outliers of 5.8% for the entire Chandra-COSMOS sample. In addition, we release revised photometric redshifts for the 1735 optical counterparts of the XMM-detected sources over the entire 2 sq. deg.of COSMOS. For 248 sources, our updated photometric redshift differs from the previous release by Delta z>0.2. These changes are predominantly due to the inclusion of newly available deep H-band photometry H_AB=24 mag. We illustrate once again the importance of a spectroscopic training sample and how an assumption about the nature of a source together with the number and the depth of the available bands influence the accuracy of the photometric redshifts determined for AGN. These considerations should be kept in mind when defining the observational strategies of upcoming large surveys targeting AGN, such as eROSITA at X-ray energies and ASKAP/EMU in the radio band., ApJ, accepted for publication. Data also available at http://www.ipp.mpg.de/~msalv/PHOTOZ_XCOSMOS
Published: 2011
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43. A Highly Magnified Supernova at z = 1.703 behind the Massive Galaxy Cluster A1689

Author: A. Goobar, Edvard Mörtsell, S. Fabbro, C. Lidman, K. Paech, H. Dahle, B. Milvang-Jensen, Teresa Riehm, Dan M. Watson, J. Nordin, B. Clement, Vallery Stanishev, J. Richard, Rahman Amanullah, J. P. Kneib, Jakob Jonsson, M. Limousin, Jens Hjorth, J. G. Cuby, Tomas Dahlen, Department of Astronomy, Stockholm University, Department of Physics, 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 Oslo (UiO), Niels Bohr Institute [Copenhagen] (NBI), Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH), University of Victoria [Canada] (UVIC), European Southern Observatory (ESO), Centre de Recherche Astrophysique de Lyon (CRAL), 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), Instituto Superior Técnico, Universidade Técnica de Lisboa (IST), 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), University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)
Subjects: Expansion rate, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], gravitational lensing: weak, supernovae: general, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010306 general physics, 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, media_common, Physics, Astronomy and Astrophysics, Galaxy, Redshift, Universe, Supernova, Space and Planetary Science, galaxies: clusters: individual: A1689, Astrophysics::Earth and Planetary Astrophysics, galaxies: distances and redshifts, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Our ability to study the most remote supernova explosions, crucial for the understanding of the evolution of the high-redshift universe and its expansion rate, is limited by the light collection capabilities of telescopes. However, nature offers unique opportunities to look beyond the range within reach of our unaided instruments thanks to the light-focusing power of massive galaxy clusters. Here we report on the discovery of one of the most distant supernovae ever found, at redshift, z=1.703. Due to a lensing magnification factor of 4.3\pm0.3, we are able to measure a lightcurve of the supernova, as well as spectroscopic features of the host galaxy with a precision comparable to what will otherwise only be possible with future generation telescopes., Comment: 19 pages, 4 figures, 1 table, accepted to ApJL
Published: 2011
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44. The BigBOSS Experiment

Author: Timothy M. Heckman, D. H. Weinberg, Saul Perlmutter, Jeffrey A. Newman, S. LeBohec, Peter Nugent, Brice Ménard, D. Eppelle, Jason X. Prochaska, S. R. Majewski, X. Yang., Michael Schubnell, C. Schimd, David Kieda, H. Heetderks, Javier Sánchez, Ch Yèche, M. Azzaro, M. E. Levi, P. Jelinsky, Chong H. Ahn, Nick Mostek, P. Doel, U. Seljak, Alex G. Kim, Antonio D. Montero-Dorta, M. L. Lampton, C. Tao, Natalie A. Roe, Celine Peroux, H. T. Diehl, Sheila G. Bailey, Benjamin C. Bromley, C. Magneville, G. Rudnick, Dragan Huterer, C. Frenk, R. Mccloskey, O. Lahav, Anne Ealet, C. Allende Prieto, N. Palanque-Delabrouille, David J. Schlegel, R. N. Cahn, Anze Slosar, Marla Geha, J. Annis, H. Lim, Thomas Matheson, D. W. Gerdes, S. Becerril, Will J. Percival, I. Morales, Jordi Miralda-Escudé, J. Tinker, M. Liang, Kevin Reil, Alexander S. Szalay, F. B. Abdalla, M. Wood-Vasey, Marina Cortês, M. R. Blanton, C. Li, P. H. Carton, Nadia L. Zakamska, J. Yang, F. Valdes, W. Springer, Éric Aubourg, W. Lin, A. de la Macorra, N. Ross, Arthur Kosowsky, Steve Kent, Inese I. Ivans, C. Baltay, August E. Evrard, I. Park, Pengjie Zhang, Maryam Modjaz, Nikhil Padmanabhan, Mark Dickinson, Dick Joyce, Bruce Grossan, Michael Sholl, Francisco Prada, V. Le Brun, Chris Bebek, O. Ilbert, D. Sawyer, Kyle Dawson, D. S. Smith, John A. Peacock, Martin White, C. Marinoni, Emmanuel Rollinde, Andrew R. Zentner, R. Scoccimaro, L. Faccioli, Vicent J. Martínez, Jeff McMahon, K. Honscheid, K. A. G. Olsen, P. Petitjean, George F. Smoot, Patrick McDonald, Wolfgang Lorenzon, Roger F. Malina, Y. Jing, G. Tarle, Y. Chu, B. A. Weaver, Stephanie Escoffier, Eric Prieto, Hee-Jong Seo, Arjun Dey, Jerry Edelstein, Erin Sheldon, Antonio González-Arroyo, Adam S. Bolton, C. M. Rockosi, A. Roodman, Carlton M. Baugh, Tinggui Wang, J. P. Kneib, R. Nichol, C. Zhai, K. Krishnan, V. Ruhlmann-Kleider, Eric V. Linder, A. Stril, P. Gondolo, Timothy A. McKay, Jorge L. Cervantes-Cota, R. Shulte-Ladbeck, J. Wang, Tony Abraham, A. Tilquin, C. Kim, Shirley Ho, Xu Kong, R. D. Kennedy, E. N. Taylor, APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, 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), 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), Centre de Physique Théorique - UMR 6207 (CPT), Centre National de la Recherche Scientifique (CNRS)-Université de Toulon (UTLN)-Université de Provence - Aix-Marseille 1-Université de la Méditerranée - Aix-Marseille 2, 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), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Université de la Méditerranée - Aix-Marseille 2-Université de Provence - Aix-Marseille 1-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Cristofol, Danielle, Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), and Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU)
Subjects: Physics, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], 010308 nuclear & particles physics, Dark matter, Astronomy, Quasar, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Redshift survey, 01 natural sciences, 7. Clean energy, Redshift, Galaxy, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Redshift-space distortions, [SDU.ASTR.IM] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], 13. Climate action, 0103 physical sciences, Dark energy, Baryon acoustic oscillations, [PHYS.ASTR.IM] Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: This report is based on the BigBOSS proposal submission to NOAO in October 2010, and reflects the project status at that time with minor updates; BigBOSS is a Stage IV ground-based dark energy experiment to study baryon acoustic oscillations (BAO) and the growth of structure with a wide-area galaxy and quasar redshift survey over 14,000 square degrees. It has been conditionally accepted by NOAO in response to a call for major new instrumentation and a high-impact science program for the 4-m Mayall telescope at Kitt Peak. The BigBOSS instrument is a robotically-actuated, fiber-fed spectrograph capable of taking 5000 simultaneous spectra over a wavelength range from 340 nm to 1060 nm, with a resolution R = 3000-4800. Using data from imaging surveys that are already underway, spectroscopic targets are selected that trace the underlying dark matter distribution. In particular, targets include luminous red galaxies (LRGs) up to z = 1.0, extending the BOSS LRG survey in both redshift and survey area. To probe the universe out to even higher redshift, BigBOSS will target bright [OII] emission line galaxies (ELGs) up to z = 1.7. In total, 20 million galaxy redshifts are obtained to measure the BAO feature, trace the matter power spectrum at smaller scales, and detect redshift space distortions. BigBOSS will provide additional constraints on early dark energy and on the curvature of the universe by measuring the Ly-alpha forest in the spectra of over 600,000 2.2 < z < 3.5 quasars. BigBOSS galaxy BAO measurements combined with an analysis of the broadband power, including the Ly-alpha forest in BigBOSS quasar spectra, achieves a FOM of 395 with Planck plus Stage III priors. This FOM is based on conservative assumptions for the analysis of broad band power (kmax = 0.15), and could grow to over 600 if current work allows us to push the analysis to higher wave numbers (kmax = 0.3). BigBOSS will also place constraints on theories of modified gravity and inflation, and will measure the sum of neutrino masses to 0.024 eV accuracy.
Published: 2011

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

Author: Angela Bongiorno, Roberto Scaramella, E. Zucca, Alvio Renzini, Anton M. Koekemoer, Graziano Coppa, K. Kovac, Thierry Contini, Bianca Garilli, John D. Silverman, O. Le Fèvre, Cristiano Porciani, G. Zamorani, P. Kampczyk, Christian Maier, C. Knobel, V. Mainieri, R. Pello, Christian Marinoni, L. de Ravel, J. F. Le Borgne, P. Franzetti, Enrique Pérez-Montero, M. Scodeggio, Ummi Abbas, Olga Cucciati, J. P. Kneib, Simon J. Lilly, Luigi Guzzo, Y. Peng, C. M. Carollo, Karina Caputi, A. Iovino, F. Lamareille, S. Bardelli, D. Maccagni, H. J. McCracken, Laurence Tresse, Masayuki Tanaka, V. Le Brun, Paolo Cassata, D. Bottini, S. de la Torre, Lidia Tasca, P. Memeo, C. Halliday, Daniela Vergani, M. Mignoli, Alessandro Cimatti, Lucia Pozzetti, Pascal Oesch, A. Cappi, Micol Bolzonella, B. Meneux, E. Ricciardelli, and Alexie Leauthaud
Subjects: Physics, 010308 nuclear & particles physics, Epoch (reference date), Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Redshift survey, 01 natural sciences, Galaxy, Redshift, Morphological transformation, Space and Planetary Science, 0103 physical sciences, Spatial clustering, Cluster analysis, 010303 astronomy & astrophysics, Cosmic time, Astrophysics::Galaxy Astrophysics
Abstract: We measure the spatial clustering of galaxies as a function of their morphological type at z~0.8, for the first time in a deep redshift survey with full morphological information. This is obtained by combining high-resolution HST imaging and VLT spectroscopy for about 8,500 galaxies to I_AB=22.5 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 SDSS at z~0.1, shows that the relative clustering strength between early and late morphological classes tends to increase with cosmic time at small separations, while on large scales it shows no significant evolution since z~0.8. This suggests that most early-type galaxies had already formed in intermediate and dense environments at this epoch. Our results are consistent with a picture in which the relative clustering of different morphological types between z~1 and z~0, reflects the evolving role of environment in the morphological transformation of galaxies, on top of the global mass-driven evolution.
Published: 2011
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46. The WIRCAM Deep Infrared Cluster Survey I: Groups and Clusters at z > 1.1

Author: Masayuki Tanaka, Kirpal Nandra, O. Le Fèvre, Patrick Petitjean, Yannick Mellier, Raghunathan Srianand, Alexis Finoguenov, C. S. Stalin, Olivier Ilbert, P. Hudelot, H. J. McCracken, Chris J. Willott, E. Daddi, R. M. Bielby, and J. P. Kneib
Subjects: Physics, 010308 nuclear & particles physics, Infrared, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, CMB cold spot, Cosmology, Redshift, Determining the number of clusters in a data set, Space and Planetary Science, 0103 physical sciences, Cluster (physics), Range (statistics), 010303 astronomy & astrophysics, Scaling, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We use CFHTLS deep optical data, WIRCam Deep Survey (WIRDS) NIR data and XMM data to identify z>1.1 clusters in the CFHTLS D1 and D4 fields. Counterparts to such clusters can not be identified without deep NIR data and as such the total of =1deg2 of J , H & Ks band imaging provided by WIRDS is an indispensable tool in such work. Using public XMM X-ray data, we identify extended X-ray sources in the two fields. The resulting catalogue of extended X-ray sources was analyzed for optical/NIR counterparts, using a red-sequence algorithm. Redshifts of candidate groups and clusters were estimated using the median photometric redshifts of detected counterparts and where available spectroscopic data. Additionally, we surveyed X-ray point sources for potential group systems at the limit of our detection range in the X-ray data. A catalogue of z > 1.1 cluster candidates in the two fields has been compiled and cluster masses, radii and temperatures have been estimated using the scaling relations. The catalogue consists of 15 z > 1.1 candidates. Three of the detections are previously published extended X-ray sources. Of note is JKSC 041 for which we identify possible structures at z = 0.8, z = 0.96, z = 1.13 and z = 1.49. We also make an independent detection of the massive cluster, XMMXCS J2215.9-1738. We use the z > 1.1 catalogue to compare the cluster number counts in these fields with models based on WMAP 7-year cosmology and find that the models slightly over-predict the observations, whilst at z>1.5 we do not detect any clusters. We note that cluster number counts at z > 1.1 are highly sensitive to the cosmological model, however a significant reduction in present statistical (due to available survey area) and systematic (due to cluster scaling relations) uncertainties is required in order to confidently constrain cosmological parameters using cluster number counts at high redshift., Comment: 22 pages, 22 figures, Accepted 4 August 2010
Published: 2010

47. MACS J1423.8+2404: gravitational lensing by a massive, relaxed cluster of galaxies at z = 0.54

Author: Harald Ebeling, A. C. Edge, J. P. Kneib, M. Limousin, C. J. Ma, P. J. Marshall, Tim Schrabback, Graham P. Smith, A. M. Swinbank, Johan Richard, Mathilde Jauzac, Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institute for Astronomy [Honolulu], University of Hawai‘i [Mānoa] (UHM), Department of Physics, Durham University, University of Alabama at Birmingham [ Birmingham] (UAB), University of Bristol [Bristol], University of Reading (UOR), Centre de Recherche Astrophysique de Lyon (CRAL), 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), Department of Astronomy, Stanford University, Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], gravitational lensing, Gravitational lensing, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Galaxy group, 0103 physical sciences, Cluster (physics), clusters: individual: MACS J1423.8+2404 [Galaxies], 010306 general physics, 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, Physics, Mass distribution, galaxies: clusters: individual: MACS J1423.8+2404, Astronomy and Astrophysics, Type-cD galaxy, Redshift, Gravitational lens, Space and Planetary Science, Substructure, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present results of a gravitational-lensing and optical study of MACS ,J1423.8+2404 (z=0.545, MACS, J1423). Our analysis uses high-resolution images taken with the Hubble Space Telescope in the F555W and F814W passbands, ground based imaging in eight optical and near-infrared filters obtained with Subaru and CFHT, as well as extensive spectroscopic data gathered with the Keck telescopes. At optical wavelengths the cluster exhibits no sign of substructure and is dominated by a cD galaxy that is 2.1 magnitudes (K-band) brighter than the second brightest cluster member, suggesting that MACS, J1423 is close to be fully virialized. Analysis of the redshift distribution of 140 cluster members reveals a Gaussian distribution, mildly disturbed by the presence of a loose galaxy group that may be falling into the cluster along the line of sight. Combining strong-lensing constraints from two spectroscopically confirmed multiple-image systems near the cluster core with a weak-lensing measurement of the gravitational shear on larger scales, we derive a parametric mass model for the mass distribution. All constraints can be satisfied by a uni-modal mass distribution centred on the cD galaxy and exhibiting very little substructure. The derived projected mass of M(, Resubmitted to MNRAS. High resolution available at http://www.dark-cosmology.dk/~marceau/1423mnras.pdf
Published: 2010
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48. The XMM-Newton Wide-field Survey in the Cosmos Field (XMM-COSMOS): Demography and Multiwavelength Properties of Obscured and Unobscured Luminous Active Galactic Nuclei

Author: Yoshi Taniguchi, E. Le Floc'h, M. Bolzonella, G. Hasinger, S. de la Torre, Heng Hao, Katarina Kovac, John D. Silverman, J. P. Kneib, Marco Scodeggio, Nico Cappelluti, Roberto Gilli, L. Tresse, Andrea Comastri, Anton M. Koekemoer, S. Bardelli, Ezequiel Treister, M. Elvis, Angela Bongiorno, S. J. Lilly, Christian Maier, Andrea Merloni, B. Garilli, Y. Peng, H. J. McCracken, Elisabeta Lusso, Nick Scoville, F. Lamareille, Eva Schinnerer, Karina Caputi, D. Vergani, A. Cappi, Mara Salvato, Vincenzo Mainieri, J-F. Leborgne, M. Zamojski, G. Zamorani, Peter Capak, L. de Ravel, E. Zucca, K. Iwasawa, T. Contini, Cristian Vignali, O. Le Fevre, P. Kampczyk, A. Iovino, Marcella Brusa, Antonella Fruscione, D. B. Sanders, Knud Jahnke, Enrique Perez-Montero, L. A. M. Tasca, Fabrizio Fiore, J. Kartaltepe, C. Knobel, Chris Impey, A. Finoguenov, Masaomi Tanaka, Francesca Civano, V. Le Brun, O. Ilbert, H. Aussel, T. Aldcroft, Takamitsu Miyaji, R. Pello, M. Mignoli, J. D. Trump, 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: Infrared, Population, galaxies: active, Galaxies: active, Surveys, X-rays: diffuse background, X-rays: galaxies, X-rays: general, Astrophysics, 01 natural sciences, Luminosity, surveys, 0103 physical sciences, [INFO]Computer Science [cs], Spectroscopy, education, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Luminosity function (astronomy), Physics, education.field_of_study, 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, Redshift, Galaxy, Space and Planetary Science, Spectral energy distribution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
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.
Published: 2010
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49. Ultraluminous X-ray sources out to z ~ 0.3 in the COSMOS field

Author: Angela Bongiorno, O. Le Fèvre, John D. Silverman, N. Z. Scoville, P. Franzetti, Anton M. Koekemoer, Olga Cucciati, E. Zucca, Simonetta Puccetti, C. Knobel, Thierry Contini, S. Bardelli, Bianca Garilli, Giuseppina Fabbiano, G. Zamorani, Antonella Fruscione, L. de Ravel, E. Perez Montero, Jonathan R. Trump, Nico Cappelluti, Andrea Merloni, Mara Salvato, Cristian Vignali, M. Scodeggio, J. P. Kneib, K. Kovac, Alvio Renzini, Lidia Tasca, Y. Peng, S. de la Torre, Peter Capak, Alexis Finoguenov, Graziano Coppa, Francesca Civano, Roberto Gilli, Tom Aldcroft, Fabrizio Fiore, P. Kampczyk, V. Mainieri, F. Lamareille, Monique Aller, Chris Impey, R. Pello, Andrea Comastri, M. Bolzonella, M. Mignoli, Laurence Tresse, Martin Elvis, M. Carollo, Yoshiaki Taniguchi, Simon J. Lilly, Claudia Scarlata, Masayuki Tanaka, Karina Caputi, V. Le Brun, E. Ricciardelli, Christian Maier, Olivier Ilbert, Marcella Brusa, A. Iovino, J. F. Le Borgne, Daniela Vergani, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Astronomy, Mainieri V., Vignali C., Merloni A., Civano F., Puccetti S., Brusa M., Gilli R., Bolzonella M., Comastri A., Zamorani G., Aller M., Carollo M., Scarlata C., Elvis M., Aldcroft T.L., Cappelluti N., Fabbiano G., Finoguenov A., Fiore F., Fruscione A., Koekemoer A.M., Contini T., Kneib J.P., Le Fevre O., Lilly S., Renzini A., Scodeggio M., Bardelli S., Bongiorno A., Caputi K., Coppa G., Cucciati O., de la Torre S., de Ravel L., Franzetti P., Garilli B., Iovino A., Kampczyk P., Knobel C., 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.D., Tanaka M., Tasca L., Tresse L., Vergani D., Zucca E., Capak P., Ilbert O., Impey C., Salvato M., Scoville S., Taniguchi Y., and Trump L.
Subjects: X-rays: galaxies – X-rays: binaries – X-rays: general – surveys, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Field (physics), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, X-rays: general, 01 natural sciences, X-rays: binaries, surveys, 0103 physical sciences, [INFO]Computer Science [cs], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Star formation, X-ray, Astronomy and Astrophysics, Redshift, Galaxy, Early type, X-rays: galaxies, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Using Chandra observations we have identified a sample of seven off-nuclear X-ray sources, in the redshift range z=0.072-0.283, located within optically bright galaxies in the COSMOS Survey. Using the multi-wavelength coverage available in the COSMOS field, we study the properties of the host galaxies of these ULXs. In detail, we derived their star formation rate from H_alpha measurements and their stellar masses using SED fitting techniques with the aim to compute the probability to have an off-nuclear source based on the host galaxy properties. We divide the host galaxies in different morphological classes using the available ACS/HST imaging. We find that our ULXs candidates are located in regions of the SFR versus M$_star$ plane where one or more off-nuclear detectable sources are expected. From a morphological analysis of the ACS imaging and the use of rest-frame colours, we find that our ULXs are hosted both in late and early type galaxies. Finally, we find that the fraction of galaxies hosting a ULX ranges from ~0.5% to ~0.2% going from L[0.5-2 keV]=3 x 10^39 erg s^-1 to L[0.5-2 keV]= 2 x 10^40 erg s^-1., Comment: 10 pages, 9 figures, accepted for publication in Astronomy & Astrophysics
Published: 2010
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50. The buildup of the Hubble sequence in the cosmos field

Author: Anton M. Koekemoer, Claudia Scarlata, C. M. Carollo, Jason Rhodes, Mara Salvato, Richard Massey, S. J. Lilly, Kevin Bundy, T. J. Bschorr, Y. Taniguchi, H. Aussel, Nick Scoville, Alvio Renzini, Kartik Sheth, A. Leauthaud, Oliver Hahn, M. Bolzonella, H. J. McCracken, Peter Capak, David R. Thompson, Lucia Pozzetti, E. Le Floc'h, D. B. Sanders, Robert Feldmann, O. Ilbert, Katarina Kovac, Monique Aller, Pascal Oesch, M. T. Sargent, J. P. Kneib, 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: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Field (physics), Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Hubble sequence, symbols.namesake, Bulge, 0103 physical sciences, Mass scale, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, QB, Physics, education.field_of_study, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Secular evolution, Astronomy and Astrophysics, Galaxy, Space and Planetary Science, symbols, Irregular galaxy, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We use ~8,600 >5e10 Msol COSMOS galaxies to study how the morphological mix of massive ellipticals, bulge-dominated disks, intermediate-bulge disks, bulge-less disks and irregular galaxies evolves from z=0.2 to z=1. The morphological evolution depends strongly on mass. At M>3e11 Msol, no evolution is detected in the morphological mix: ellipticals dominate since z=1, and the Hubble sequence has quantitatively settled down by this epoch. At the 1e11 Msol mass scale, little evolution is detected, which can be entirely explained with major mergers. Most of the morphological evolution from z=1 to z=0.2 takes place at masses 5e10 - 1e11 Msol, where: (i) The fraction of spirals substantially drops and the contribution of early-types increases. This increase is mostly produced by the growth of bulge-dominated disks, which vary their contribution from ~10% at z=1 to >30% at z=0.2 (cf. the elliptical fraction grows from ~15% to ~20%). Thus, at these masses, transformations from late- to early-types result in disk-less elliptical morphologies with a statistical frequency of only 30% - 40%. Otherwise, the processes which are responsible for the transformations either retain or produce a non-negligible disk component. (ii) The bulge-less disk galaxies, which contribute ~15% to the intermediate-mass galaxy population at z=1, virtually disappear by z=0.2. The merger rate since z=1 is too low to account for the disappearance of these massive bulge-less disks, which most likely grow a bulge via secular evolution., 5 pages, 3 figures, submitted to ApJL
Published: 2010
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