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1. The MUSE second-generation VLT instrument

Author: R., Bacon, M., Accardo, L., Adjali, H., Anwand, S., Bauer, I., Biswas, J., Blaizot, D., Boudon, S., Brau-Nogue, J., Brinchmann, P., Caillier, L., Capoani, M., Carollo C., T., Contini, P., Couderc, E., Daguise, S., Deiries, B., Delabre, S., Dreizler, P., Dubois J., M., Dupieux, C., Dupuy, E., Emsellem, T., Fechner, A., Fleischmann, M., Francois, G., Gallou, T., Gharsa, A., Glindemann, D., Gojak, B., Guiderdoni, G., Hansali, T., Hahn, A., Jarno, A., Kelz, C., Koehler, J., Kosmalski, F., Laurent, M., Le Floch, J., Lilly S., -L., Lizon J., M., Loupias, A., Manescau, C., Monstein, H., Nicklas, J-C, Olaya, L., Pares, L., Pasquini, A., Pecontal-Rousset, R., Pello, C., Petit, E., Popow, R., Reiss, A., Remillieux, E., Renault, M., Roth, G., Rupprecht, D., Serre, J., Schaye, G., Soucail, M., Steinmetz, O., Streicher, R., Stuik, H., Valentin, J., Vernet, P., Weilbacher, L., Wisotzki, and N, Yerle
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The Multi Unit Spectroscopic Explorer (MUSE) is a second-generation VLT panoramic integral-field spectrograph currently in manufacturing, assembly and integration phase. MUSE has a field of 1x1 arcmin2 sampled at 0.2x0.2 arcsec2 and is assisted by the VLT ground layer adaptive optics ESO facility using four laser guide stars. The instrument is a large assembly of 24 identical high performance integral field units, each one composed of an advanced image slicer, a spectrograph and a 4kx4k detector. In this paper we review the progress of the manufacturing and report the performance achieved with the first integral field unit., Comment: 10 pages, 5 figures
Published: 2022
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2. Euclid preparation: XI. Mean redshift determination from galaxy redshift probabilities for cosmic shear tomography

Author: C. Colodro-Conde, Marco Baldi, K. Pedersen, F. Sureau, Sebastiano Ligori, M. Fabricius, F. Torradeflot, Chiara Sirignano, L. Whittaker, Michele Moresco, J. Valiviita, Sandrine Pires, Christopher J. Conselice, Andrea Zacchei, Natalia Auricchio, A. Renzi, Peter Schneider, M. Tenti, E. Romelli, Elisabetta Maiorano, P. Tallada Crespa, A. Ealet, Eric Jullo, Yu Wang, Marco Castellano, Hendrik Hildebrandt, S. Paltani, K. Markovic, Fabio Pasian, Hélène M. Courtois, E. Franceschi, Enzo Branchini, A. Secroun, N. Martinet, Mark Cropper, Stein Vidar Hagfors Haugan, Adam Amara, Ghassem Gozaliasl, D. Masters, Martin Kunz, G. Seidel, Ismael Tereno, A. Cappi, Leonardo Corcione, Emanuel Rossetti, Ralf Bender, Pedro G. Ferreira, Giuseppe Riccio, Massimo Brescia, D. Di Ferdinando, G. Zamorani, Stefano Borgani, D. Bonino, X. Dupac, Lauro Moscardini, C. Baccigalupi, B. Morin, Rafael Toledo-Moreo, Federico Marulli, C. Padilla, A. Boucaud, Jason Rhodes, F. Dubath, Javier Graciá-Carpio, Remi A. Cabanac, S. Casas, Roberto P. Saglia, F. Grupp, S. Galeotta, Enrico Bozzo, V. Scottez, Luca Valenziano, B. Gillis, Alina Kiessling, L. Popa, R. Cledassou, V. Capobianco, L. Patrizii, Julien Zoubian, Iary Davidzon, Carlo Burigana, Hannu Kurki-Suonio, Jean Coupon, L. Conversi, H. J. McCracken, Lucia Pozzetti, T. Vassallo, Edwin A. Valentijn, G. Sirri, Jean-Gabriel Cuby, N. Welikala, S. Dusini, R. Nakajima, Matteo Maturi, H. Degaudenzi, P. Franzetti, A. Balestra, Stefano Cavuoti, Ole Marggraf, C. S. Carvalho, S. Bardelli, Ruyman Azzollini, W. Gillard, E. Keihänen, A. Da Silva, R. Benton Metcalf, G. Polenta, Gianluca Castignani, S. Maurogordato, M. Poncet, O. Ilbert, Stefano Andreon, Richard Massey, Knud Jahnke, E. Zucca, E. Medinaceli, Mauro Roncarelli, S. Farrens, C. A. J. Duncan, C. Neissner, Doug Potter, Andrea Tramacere, Jochen Weller, Sotiria Fotopoulou, F. J. Castander, J. Carretero, S. Serrano, Pablo Fosalba, Andrea Cimatti, E. Munari, R. Pello, Anne Costille, Tim Schrabback, Stefano Camera, Y. Copin, L. Stanco, W. A. Holmes, Domenico Sapone, I. Lloro, Harry I. Teplitz, B. Garilli, Clotilde Laigle, Ariel G. Sánchez, Luigi Guzzo, F. Raison, N. Mauri, P. B. Lilje, C. Bodendorf, A. Balaguera-Antolínez, Valeria Pettorino, Carmelita Carbone, Fabio Finelli, Andrea Biviano, Angus H. Wright, J. Nightingale, S. de la Torre, S. Niemi, Carlo Giocoli, G. Congedo, S. Kermiche, C. C. Kirkpatrick, Davide Maino, Felix Hormuth, Simona Mei, Astronomy, 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), University of New South Wales [Sydney] (UNSW), 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), California Institute of Technology (CALTECH), University of Copenhagen = Københavns Universitet (KU), INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), AstroParticule et Cosmologie (APC (UMR_7164)), 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)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - 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Paris 7 (UPD7), Fondation FondaMental [Créteil], Université Paris-Sorbonne - Paris 4 - École des hautes études en sciences de l'information et de la communication (UP4 CELSA), Université Paris-Sorbonne (UP4), Laboratoire Européen Performance Santé Altitude (LEPSA), Université de Perpignan Via Domitia (UPVD), Wuhan University [China], Euclid Collaboration, Department of Physics, Research Program in Systems Oncology, Helsinki Institute of Physics, Ilbert, O., De La Torre, S., Martinet, N., Wright, A. H., Paltani, S., Laigle, C., Davidzon, I., Jullo, E., Hildebrandt, H., Masters, D. C., Amara, A., Conselice, C. J., Andreon, S., Auricchio, N., Azzollini, R., Baccigalupi, C., Balaguera-Antolinez, A., Baldi, M., Balestra, A., Bardelli, S., Bender, R., Biviano, A., Bodendorf, C., Bonino, D., Borgani, S., Boucaud, A., Bozzo, E., Branchini, E., Brescia, M., Burigana, C., Cabanac, R., Camera, S., Capobianco, V., Cappi, A., Carbone, C., Carretero, J., Carvalho, C. S., Casas, S., Castander, F. J., Castellano, M., Castignani, G., Cavuoti, S., Cimatti, A., Cledassou, R., Colodro-Conde, C., Congedo, G., Conversi, L., Copin, Y., Corcione, L., Costille, A., Coupon, J., Courtois, H. M., Cropper, M., Cuby, J., Da Silva, A., Degaudenzi, H., Di Ferdinando, D., Dubath, F., Duncan, C., Dupac, X., Dusini, S., Ealet, A., Fabricius, M., Farrens, S., Ferreira, P. G., Finelli, F., Fosalba, P., Fotopoulou, S., Franceschi, E., Franzetti, P., Galeotta, S., Garilli, B., Gillard, W., Gillis, B., Giocoli, C., Gozaliasl, G., Gracia-Carpio, J., Grupp, F., Guzzo, L., Haugan, S. V. H., Holmes, W., Hormuth, F., Jahnke, K., Keihanen, E., Kermiche, S., Kiessling, A., Kirkpatrick, C. C., Kunz, M., Kurki-Suonio, H., Ligori, S., Lilje, P. B., Lloro, I., Maino, D., Maiorano, E., Marggraf, O., Markovic, K., Marulli, F., Massey, R., Maturi, M., Mauri, N., Maurogordato, S., Mccracken, H. J., Medinaceli, E., Mei, S., Benton Metcalf, R., Moresco, M., Morin, B., Moscardini, L., Munari, E., Nakajima, R., Neissner, C., Niemi, S., Nightingale, J., Padilla, C., Pasian, F., Patrizii, L., Pedersen, K., Pello, R., Pettorino, V., Pires, S., Polenta, G., Poncet, M., Popa, L., Potter, D., Pozzetti, L., Raison, F., Renzi, A., Rhodes, J., Riccio, G., Romelli, E., Roncarelli, M., Rossetti, E., Saglia, R., Sanchez, A. G., Sapone, D., Schneider, P., Schrabback, T., Scottez, V., Secroun, A., Seidel, G., Serrano, S., Sirignano, C., Sirri, G., Stanco, L., Sureau, F., Tallada Crespa, P., Tenti, M., Teplitz, H. I., Tereno, I., Toledo-Moreo, R., Torradeflot, F., Tramacere, A., Valentijn, E. A., Valenziano, L., Valiviita, J., Vassallo, T., Wang, Y., Welikala, N., Weller, J., Whittaker, L., Zacchei, A., Zamorani, G., Zoubian, J., Zucca, E., Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), University of Copenhagen = Københavns Universitet (UCPH), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), 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), 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)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), 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 Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université de Genève = University of Geneva (UNIGE), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères (LERMA (UMR_8112)), 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), University of Zurich, Ilbert, O, Ilbert O., De La Torre S., Martinet N., Wright A.H., Paltani S., Laigle C., Davidzon I., Jullo E., Hildebrandt H., Masters D.C., Amara A., Conselice C.J., Andreon S., Auricchio N., Azzollini R., Baccigalupi C., Balaguera-Antolinez A., Baldi M., Balestra A., Bardelli S., Bender R., Biviano A., Bodendorf C., Bonino D., Borgani S., Boucaud A., Bozzo E., Branchini E., Brescia M., Burigana C., Cabanac R., Camera S., Capobianco V., Cappi A., Carbone C., Carretero J., Carvalho C.S., Casas S., Castander F.J., Castellano M., Castignani G., Cavuoti S., Cimatti A., Cledassou R., Colodro-Conde C., Congedo G., Conversi L., Copin Y., Corcione L., Costille A., Coupon J., Courtois H.M., Cropper M., Cuby J., Da Silva A., Degaudenzi H., Di Ferdinando D., Dubath F., Duncan C., Dupac X., Dusini S., Ealet A., Fabricius M., Farrens S., Ferreira P.G., Finelli F., Fosalba P., Fotopoulou S., Franceschi E., Franzetti P., Galeotta S., Garilli B., Gillard W., Gillis B., Giocoli C., Gozaliasl G., Gracia-Carpio J., Grupp F., Guzzo L., Haugan S.V.H., Holmes W., Hormuth F., Jahnke K., Keihanen E., Kermiche S., Kiessling A., Kirkpatrick C.C., Kunz M., Kurki-Suonio H., Ligori S., Lilje P.B., Lloro I., Maino D., Maiorano E., Marggraf O., Markovic K., Marulli F., Massey R., Maturi M., Mauri N., Maurogordato S., McCracken H.J., Medinaceli E., Mei S., Benton Metcalf R., Moresco M., Morin B., Moscardini L., Munari E., Nakajima R., Neissner C., Niemi S., Nightingale J., Padilla C., Pasian F., Patrizii L., Pedersen K., Pello R., Pettorino V., Pires S., Polenta G., Poncet M., Popa L., Potter D., Pozzetti L., Raison F., Renzi A., Rhodes J., Riccio G., Romelli E., Roncarelli M., Rossetti E., Saglia R., Sanchez A.G., Sapone D., Schneider P., Schrabback T., Scottez V., Secroun A., Seidel G., Serrano S., Sirignano C., Sirri G., Stanco L., Sureau F., Tallada Crespa P., Tenti M., Teplitz H.I., Tereno I., Toledo-Moreo R., Torradeflot F., Tramacere A., Valentijn E.A., Valenziano L., Valiviita J., Vassallo T., Wang Y., Welikala N., Weller J., Whittaker L., Zacchei A., Zamorani G., Zoubian J., Zucca E., German Research Foundation, European Commission, Centre National D'Etudes Spatiales (France), and Duncan, C
Subjects: statistical [Methods], IMPACT, UNIVERSE, Astrophysics, 01 natural sciences, Dark energy, Galaxies: distances and redshift, dark energy, PHOTOMETRIC REDSHIFTS, 010303 astronomy & astrophysics, Weak gravitational lensing, Photometric redshift, media_common, Physics, distances and redshift [Galaxies], Galaxies: distances and redshifts, Methods: statistical, SIMULATION, astro-ph.CO, 3103 Astronomy and Astrophysics, Probability distribution, Spectral energy distribution, galaxies: distances and redshifts, Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 530 Physics, astro-ph.GA, media_common.quotation_subject, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 1912 Space and Planetary Science, 0103 physical sciences, distances and redshifts [Galaxies], DISTRIBUTIONS, methods: statistical, 010308 nuclear & particles physics, Astronomy and Astrophysics, PERFORMANCE, 115 Astronomy, Space science, Astrophysics - Astrophysics of Galaxies, EVOLUTION, Galaxy, Universe, Redshift, STELLAR, RESOLUTION, Space and Planetary Science, 10231 Institute for Computational Science, Astrophysics of Galaxies (astro-ph.GA), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: Ilbert, O., et al. (Euclid Collaboration), The analysis of weak gravitational lensing in wide-field imaging surveys is considered to be a major cosmological probe of dark energy. Our capacity to constrain the dark energy equation of state relies on an accurate knowledge of the galaxy mean redshift ⟨ z⟩. We investigate the possibility of measuring ⟨ z»with an accuracy better than 0.002(1 + z) in ten tomographic bins spanning the redshift interval 0.2 99.8%. The zPDF approach can also be successful if the zPDF is de-biased using a spectroscopic training sample. This approach requires deep imaging data but is weakly sensitive to spectroscopic redshift failures in the training sample. We improve the de-biasing method and confirm our finding by applying it to real-world weak-lensing datasets (COSMOS and KiDS+VIKING-450)., H. Hildebrandt is supported by a Heisenberg grant of the Deutsche Forschungsgemeinschaft (Hi 1495/5-1) as well as an ERC Consolidator Grant (No. 770935). A.H. Wright is supported by the ERC Consolidator Grant (No. 770935). This work relied on the HPC resources of CINES (Jade) under the allocation 2013047012 and c2014047012 made by GENCI and on the Horizon Cluster hosted by Institut d’Astrophysique de Paris. ID acknowledges that he received funding from the European Union’s Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement No. 896225. We warmly thank S. Rouberol for running the cluster on which the simulation was post-processed. This research is also partly supported by the Centre National d’Etudes Spatiales (CNES). We would also like to recognise the contributions from all of the members of the COSMOS team who helped in obtaining and reducing the large amount of multi-wavelength and spectroscopic data. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme IDs 177.A-3016, 177.A-3017, 177.A-3018, 179.A-2004, and on data products produced by the KiDS consortium. The KiDS production team acknowledges support from: Deutsche Forschungsgemeinschaft, ERC, NOVA and NWO-M grants; Target; the University of Padova, and the University Federico II (Naples). SA thank the support PRIN MIUR2015 “Cosmology and Fundamental Physics: Illuminating the Dark Universe with Euclid”.
Published: 2021

3. An atlas of MUSE observations towards twelve massive lensing clusters

Author: Jean-Paul Kneib, Michael V. Maseda, W. Mercier, Franz E. Bauer, Johan Richard, Peter M. Weilbacher, Geoffroy de la Vieuville, Vera Patrício, Lutz Wisotzki, Guillaume Mahler, Andrei Variu, Kasper B. Schmidt, Roland Bacon, David Carton, J. Martinez, Lucia Guaita, Harald Ebeling, Themiya Nanayakkara, Benjamin Clément, R. Pello, Gonzalo Prieto Lyon, D. Lagattuta, Amélie Tamone, Genevieve Soucail, Nicolas Bouché, Adélaïde Claeyssens, Rychard Bouwens, 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), Durham University, 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), 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), Ecole Polytechnique Fédérale de Lausanne (EPFL), Leibniz-Institut für Astrophysik Potsdam (AIP), 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), 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), 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: Point source, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics - astrophysics of galaxies, FOS: Physical sciences, Context (language use), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, galaxies: high-redshift, 0103 physical sciences, Cluster (physics), galaxies: formation, 010303 astronomy & astrophysics, Galaxy cluster, Physics, 010308 nuclear & particles physics, gravitational lensing: strong, Astronomy and Astrophysics, Multi Unit Spectroscopic Explorer, Galaxy, Redshift, Supernova, Space and Planetary Science, techniques: imaging spectroscopy, galaxies: clusters: general, Astrophysics of Galaxies (astro-ph.GA), galaxies: distances and redshifts
Abstract: Spectroscopic surveys of massive galaxy clusters reveal the properties of faint background galaxies, thanks to the magnification provided by strong gravitational lensing. We present a systematic analysis of integral-field-spectroscopy observations of 12 massive clusters, conducted with the Multi Unit Spectroscopic Explorer (MUSE). All data were taken under very good seeing conditions (0.6") in effective exposure times between two and 15 hrs per pointing, for a total of 125 hrs. Our observations cover a total solid angle of ~23 arcmin$^2$ in the direction of clusters, many of which were previously studied by the MACS, Frontier Fields, GLASS and CLASH programs. The achieved emission line detection limit at 5$\sigma$ for a point source varies between (0.77--1.5)$\times$10$^{-18}$ erg\,s$^{-1}$\,cm$^{-2}$ at 7000\AA. We present our developed strategy to reduce these observational data, detect sources and determine their redshifts. We construct robust mass models for each cluster to further confirm our redshift measurements using strong-lensing constraints, and identify a total of 312 strongly lensed sources producing 939 multiple images. The final redshift catalogs contain more than 3300 robust redshifts, of which 40\% are for cluster members and $\sim$30\% for lensed Lyman-$\alpha$ emitters. 14\% of all sources are line emitters not seen in the available HST images, even at the depth of the FFs ($\sim29$ AB). We find that the magnification distribution of the lensed sources in the high-magnification regime ($\mu{=}$ 2--25) follows the theoretical expectation of $N(z)\propto\mu^{-2}$. The quality of this dataset, number of lensed sources, and number of strong-lensing constraints enables detailed studies of the physical properties of both the lensing cluster and the background galaxies. The full data products from this work are made available to the community. [abridged], Comment: 47 pages, 13 figures, 18 tables. Accepted for publication in A&A. Data Release products available on CDS and at https://cral-perso.univ-lyon1.fr/labo/perso/johan.richard/MUSE_data_release
Published: 2021

4. ALMA 1.3 mm survey of lensed submillimeter galaxies selected by Herschel

Author: Ian Smail, Miroslava Dessauges-Zavadsky, Eiichi Egami, Pablo G. Pérez-González, Kimihiko Nakajima, Francoise Combes, Gregory Walth, T. D. Rawle, Scott Chapman, Ivan Valtchanov, Fengwu Sun, Alexis Finoguenov, Harald Ebeling, Antonio Cava, Frédéric Boone, Bruno Altieri, Paul van der Werf, R. Pello, Johan Richard, B. Clement, Daniel Schaerer, Wiphu Rujopakarn, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Department of Physics, Sun, F. [0000-0002-4622-6617], Rawle, T. D. [0000-0002-7028-5588], Walth, G. L. [0000-0002-6313-6808], Smail, I. [0000-0003-3037-257X], Dessauges-Zavadsky, M. [0000-0003-0348-2917], Pérez González, P. G. [0000-0003-4528-5639], Richard, J. [0000-0001-5492-1049], Combes, F. [0000-0003-2658-7893], Ebeling, H. [0000-0001-8249-2739], Pelló, R. [0000-0003-0858-6109], Werf, P. V. [0000-0001-5434-5942], Altieri, B. [0000-0003-3936-0284], Cava, A. [0000-0002-4821-1275], Finoguenov, A. [0000-0002-4606-5403], Nakajima, K. [0000-0003-2965-5070], Rujopakarn, W. [0000-0002-0303-499X], Schaerer, D. [0000-0001-7144-7182], Valtchanov, I. [0000-0001-9930-7886], Science and Technology Facilities Council (STFC), and National Aeronautics and Space Administration (NASA)
Subjects: Infrared galaxies, Astrophysics - astrophysics of galaxies, Continuum (design consultancy), FOS: Physical sciences, Starburst galaxies, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, High redshift galaxies, 01 natural sciences, Submillimetre astronomy, 734, 1570, 790, 594, 1647, Galaxy evolution, 0103 physical sciences, Galaxy formation and evolution, Astrophysics::Solar and Stellar Astrophysics, Surface brightness, 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, Luminous infrared galaxy, Physics, [PHYS]Physics [physics], 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, 115 Astronomy, Space science, Galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), High-redshift galaxies, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Submillimeter astronomy
Abstract: We present an ALMA 1.3 mm (Band 6) continuum survey of lensed submillimeter galaxies (SMGs) at $z=1.0\sim3.2$ with an angular resolution of $\sim0.2$". These galaxies were uncovered by the Herschel Lensing Survey (HLS), and feature exceptionally bright far-infrared continuum emission ($S_\mathrm{peak} \gtrsim 90$ mJy) owing to their lensing magnification. We detect 29 sources in 20 fields of massive galaxy clusters with ALMA. Using both the Spitzer/IRAC (3.6/4.5 $\mathrm{\mu m}$) and ALMA data, we have successfully modeled the surface brightness profiles of 26 sources in the rest-frame near- and far-infrared. Similar to previous studies, we find the median dust-to-stellar continuum size ratio to be small ($R_\mathrm{e,dust}/R_\mathrm{e,star} = 0.38\pm0.14$) for the observed SMGs, indicating that star formation is centrally concentrated. This is, however, not the case for two spatially extended main-sequence SMGs with a low surface brightness at 1.3 mm ($\lesssim 0.1$ mJy arcsec$^{-2}$), in which the star formation is distributed over the entire galaxy ($R_\mathrm{e,dust}/R_\mathrm{e,star}>1$). As a whole, our SMG sample shows a tight anti-correlation between ($R_\mathrm{e,dust}/R_\mathrm{e,star}$) and far-infrared surface brightness ($\Sigma_\mathrm{IR}$) over a factor of $\simeq$ 1000 in $\Sigma_\mathrm{IR}$. This indicates that SMGs with less vigorous star formation (i.e., lower $\Sigma_\mathrm{IR}$) lack central starburst and are likely to retain a broader spatial distribution of star formation over the whole galaxies (i.e., larger $R_\mathrm{e,dust}/R_\mathrm{e,star}$). The same trend can be reproduced with cosmological simulations as a result of central starburst and potentially subsequent "inside-out" quenching, which likely accounts for the emergence of compact quiescent galaxies at $z\sim2$., Comment: 32 pages, 18 figures, 4 tables. Accepted for publication in ApJ
Published: 2021

5. Maunakea Spectroscopic Explorer Low Moderate Resolution Spectrograph: paths toward the Preliminary Design Phase

Author: Eric Prieto, R. Pello, Nicolas Flagey, Alexis Hill, Laurence Tresse, Kjetil Dohlen, C. Yeche, P. H. Carton, Alexandre Jeanneau, S. Brau-Nogué, 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), 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), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, 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), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), and Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Physics, Resolution (electron density), Dark matter, Astrophysics, Status report, 01 natural sciences, law.invention, 010309 optics, Telescope, Design phase, law, 0103 physical sciences, Instrumentation and Methods for Astrophysics, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Neutrino, Spectral resolution, 010303 astronomy & astrophysics, Spectrograph
Abstract: International audience; The Maunakea Spectroscopic Explorer (MSE) is a 10m-class, wide-field (1.5 sq. degree) and high-multiplex (< 3000 fibers) spectroscopic facility that will replace the 3.6m Canada-France-Hawaii Telescope. With backend spectrographs operating at low (R ~ 3000), moderate (R ~ 6000) and high (R ~ 20/40 k) spectral resolution across the 0.36 – 1.8 µm range, MSE will be poised to address a variety of science questions among which the nature of dark matter, the origin of the elements in the periodic table, the mass of the neutrino, whilst enabling a new era of rapid-response and time-domain astronomy. This paper is a status report of the MSE Low Moderate Resolution spectrograph design, from the Conceptual Design Review (CoDR) towards the Preliminary Design Phase (PDP).
Published: 2020

6. MUSE observations towards the lensing cluster A2744: Intersection between the LBG and LAE populations at z ∼ 3–7

Author: Daniel Schaerer, G. de La Vieuville, Lucia Guaita, T. Contini, D. Lagattuta, Guillaume Mahler, Anne Verhamme, J. Richard, R. Pello, Michael V. Maseda, J. Blaizot, L. Lévêque, Nicolas Laporte, J. Martinez, Kasper B. Schmidt, Haruka Kusakabe, Franz E. Bauer, 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 Ergonomie et Sciences Cognitives pour les Transports (TS2-LESCOT ), Université Gustave Eiffel, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Université de Genève = University of Geneva (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), Université de Genève (UNIGE), Laporte, Nicolas [0000-0001-7459-6335], and Apollo - University of Cambridge Repository
Subjects: media_common.quotation_subject, Population, first stars, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, galaxies: high-redshift, 0103 physical sciences, dark ages, reionization, first stars, dark ages, education, 010303 astronomy & astrophysics, Reionization, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, media_common, Physics, education.field_of_study, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, gravitational lensing: strong, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Universe, Stars, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Dark Ages, reionization, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: We present a study of the intersection between the populations of star forming galaxies selected as either Lyman break galaxies (LBGs) or Lyman-alpha emitters (LAEs) in the redshift range 2.9 − 6.7 and within the same volume of universe sampled by the Multi-Unit Spectroscopic Explorer (MUSE) behind the Hubble Frontier Fields lensing cluster A2744. We define three samples of star-forming galaxies: LBG galaxies with an LAE counterpart (92 galaxies), LBG galaxies without an LAE counterpart (408 galaxies), and LAE galaxies without an LBG counterpart (46 galaxies). All these galaxies are intrinsically faint because of the lensing nature of the sample (M1500 ≥ −20.5). The fraction of LAEs among all selected star-forming galaxies increases with redshift up to z ∼ 6 and decreases for higher redshifts, in agreement with previous findings. The evolution of LAE/LBG populations with UV magnitude and Lyα luminosity shows that the LAE selection is able to identify intrinsically UV faint galaxies with M1500 ≥ −15 that are typically missed in the deepest lensing photometric surveys. The LBG population seems to fairly represent the total population of star-forming galaxies down to M1500 ∼ −15. Galaxies with M1500 Lyα uv, whereas the opposite trend is observed within our sample for faint galaxies with M1500 > −17, including galaxies only detected by their Lyα emission, with a large scatter. These trends, previously observed in other samples of star-forming galaxies at high-z, are seen here for very faint M1500 ∼ −15 galaxies; that is, much fainter than in previous studies. The present results show no clear evidence for an intrinsic difference between the properties of the two populations selected as LBG and/or LAE. The observed trends could be explained by a combination of several phenomena, like the existence of different star-formation regimes, the dust content, the relative distribution and morphology of dust and stars, or the stellar populations.
Published: 2020

7. The 2175 Å Dust Feature in Star-forming Galaxies at 1.3 ≤ z ≤ 1.8: The Dependence on Stellar Mass and Specific Star Formation Rate

Author: Alvio Renzini, S. Bardelli, E. Zucca, Emanuele Daddi, Yingjie Peng, John D. Silverman, O. Cucciati, Simon J. Lilly, David B. Sanders, Daichi Kashino, Vincenzo Mainieri, R. Pello, and Jeyhan S. Kartaltepe
Subjects: Physics, Stellar mass, Star formation, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Star (graph theory), Astrophysics - Astrophysics of Galaxies, Galaxy, Interstellar medium, Space and Planetary Science, Feature (computer vision), Galaxy formation and evolution, Astrophysics::Galaxy Astrophysics, Cosmic dust
Abstract: We present direct spectroscopic measurements of the broad 2175~{\AA} absorption feature in 505 star-forming main-sequence galaxies at $1.3\le z\le 1.8$ using individual and stacked spectra from the zCOSMOS-deep survey. Significant 2175~{\AA} excess absorption features of moderate strength are measured, especially in the composite spectra. The excess absorption is well described by a Drude profile. The bump amplitude expressed in units of $k(\lambda)=A(\lambda)/E(B-V)$, relative to the featureless Calzetti et al. law, has a range $B_k\approx0.2\textrm{--}0.8$. The bump amplitude decreases with the specific star formation rate (sSFR), while it increases moderately with the stellar mass. However, a comparison with local "starburst" galaxies shows that the high-redshift main-sequence galaxies have stronger bump features, despite having a higher sSFR than the local sample. Plotting the bump strength against the $\Delta\log\mathrm{sSFR}\equiv \log \left( \mathrm{SFR}/\mathrm{SFR_{MS}}\right)$ relative to the main sequence, however, brings the two samples into much better concordance. This may indicate that it is the recent star formation history of the galaxies that determines the bump strength through the destruction of small carbonaceous grains by supernovae and intense radiation fields coupled with the time delay of $\sim1~\mathrm{Gyr}$ in the appearance of carbon-rich asymptotic giant branch stars., Comment: Published in ApJ on 2021 March 19
Published: 2021

8. Kinematics, turbulence, and star formation of z ∼ 1 strongly lensed galaxies seen with MUSE

Author: Michael V. Maseda, D. Lagattuta, Franz E. Bauer, Nicolas Bouché, Lutz Wisotzki, Peter M. Weilbacher, Johan Richard, G. Soucail, Guillaume Mahler, Davor Krajnović, J. Martinez, Jarle Brinchmann, Benoît Epinat, David Carton, R. Pello, Vera Patrício, B. Clement, Joseph Caruana, Thierry Contini, H. Finley, Kasper B. Schmidt, 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), 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), 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), Deutsches Zentrum für Luft- und Raumfahrt (DLR), Astrophysikalisches Institut Potsdam (AIP), Departamento de Astronomía y Astrofísica [Santiago], Pontificia Universidad Católica de Chile (UC), Techniques of Informatics and Microelectronics for integrated systems Architecture (TIMA), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), 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), 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), Techniques de l'Informatique et de la Microélectronique pour l'Architecture des systèmes intégrés (TIMA), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), 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), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), and Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Physics, 010308 nuclear & particles physics, Star formation, Turbulence, Attenuation, Metallicity, Extinction (astronomy), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Galaxy, Spectral line, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Emission spectrum, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We analyse a sample of 8 highly magnified galaxies at redshift 0.6, Comment: 22 pages, 9 Figures (plus appendices). Accepted for publication in MNRAS
Published: 2018

9. The WIRCam Ultra Deep Survey (WUDS)

Author: Nicolas Laporte, Marc Balcells, Frédéric Boone, Mercedes Prieto, R. Pello, Daniel Schaerer, P. Hudelot, Johan Richard, Yannick Mellier, Jean-Gabriel Cuby, J. F. Le Borgne, Nicolás Cardiel, Matthew Hayes, Rafael Guzman, Jesús Gallego, H. J. McCracken, Francisco Garzón, K. Disseau, Laurence Tresse, Stéphane Arnouts, Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Department of Chemistry, RIDER UNIVERSITY, Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), AGROCAMPUS OUEST, Institut national d'enseignement supérieur pour l'agriculture, l'alimentation et l'environnement (Institut Agro), 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), Galaxies, Etoiles, Physique, Instrumentation (GEPI), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris
Subjects: Population, first stars, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, surveys, galaxies: high-redshift, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, dark ages, education, 010303 astronomy & astrophysics, Reionization, Astrophysics::Galaxy Astrophysics, Luminosity function (astronomy), Physics, education.field_of_study, 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), reionization, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Lyman-break galaxy
Abstract: The aim of this paper is to introduce the WIRCam Ultra Deep Survey (WUDS), a near-IR photometric public survey carried out at the CFH Telescope in the field of the CFHTLS-D3 field (Groth Strip). WUDS includes four near-IR bands (Y, J, H and K_s) over a field of view of ~400 arcmin^2. The typical depth of WUDS data reaches between ~26.8 in Y and J, and ~26 in H and K_s (AB, 3 sigma in 1.3 arcsec aperture). The area and depth of this survey were specifically tailored to set strong constraints on the cosmic star formation rate and the luminosity function brighter or around L* in the z~6-10 redshift domain, although these data are also useful for a variety of extragalactic projects.This first paper is intended to present the properties of WUDS: catalog building, completeness and depth, number counts, photometric redshifts, and global properties of the galaxy population. We have also concentrated on the study of galaxy samples at z~[4.5-7] in this field. UV luminosity functions were derived at z~5 and z~6 taking advantage from the fact that WUDS covers a particularly interesting regime at intermediate luminosities, which allows a combined determination of M* and Phi* with increased accuracy. Our results on the luminosity function are consistent with a small evolution of both M* and Phi* between z=5 and z=6, irrespective of the method used to derive them, either photometric redshifts applied to blindly-selected dropout samples or the classical Lyman Break Galaxy color-preselected samples. Our results lend support to higher Phi* determinations at z=6 than usually reported. The selection and combined analysis of different galaxy samples at z>7 will be presented in a forthcoming paper. WUDS is intended to provide a robust database in the near-IR for the selection of targets for detailed spectroscopic studies, in particular for the EMIR/GTC GOYA Survey (Abridged), Accepted for publication in Astronomy & Astrophysics. 17 pages, 11 figures
Published: 2018
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10. Optimal CYFRA 21-1 cut-off in patients with suspected malignancy

Author: Gayo, S. Garcia-Valdecasas, primary, Ruiz-Alvarez, M.J., additional, Lietor, E. Marquez, additional, Gay, D. Gonzalez, additional, De La ViÑa, A. De Lozar, additional, Corral, R. Ramos, additional, Del Arco, N. Del Amo, additional, Gutierrez, R. Pello, additional, Carballo, B. Ortega, additional, Santos, R. Guillen, additional, and Valenciano, F. Cava, additional
Published: 2019
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11. Mass and Environment as Drivers of Galaxy Evolution in SDSS and zCOSMOS and the Origin of the Schechter Function

Author: Anton M. Koekemoer, Pascal Oesch, P. Kampczyk, A. Cappi, Paolo Cassata, Lucia Pozzetti, Angela Bongiorno, E. Zucca, Marco Scodeggio, P. Nair, G. Zamorani, A. Leauthaud, D. Bottini, David B. Sanders, Jean-Paul Kneib, J. F. Le Borgne, Christian Maier, Christian Marinoni, S. Bardelli, Simon J. Lilly, O. Le Fevre, P. Memeo, D. Maccagni, R. Pello, D. Vergani, John D. Silverman, T. Contini, Olga Cucciati, M. Mignoli, G. Hasinger, V. Presotto, Alvio Renzini, B. Meneux, C. Knobel, Graziano Coppa, Olivier Ilbert, Rongmon Bordoloi, Niraj Welikala, V. Le Brun, L. A. M. Tasca, Cristiano Porciani, A. Cimatti, Katarina Kovac, H. J. McCracken, Vincenzo Mainieri, M. Bolzonella, Masaomi Tanaka, Luke A. Barnes, Roberto Scaramella, C. M. Carollo, F. Lamareille, S. de la Torre, P. Franzetti, M. Fumana, E. Ricciardelli, A. Iovino, L. de Ravel, Yingjie Peng, E. Perez Montero, Karina Caputi, U. Abbas, L. Tresse, B. Garilli, Nick Scoville, 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), Y. Peng, S.J. Lilly, K. Kovac, M. Bolzonella, L. Pozzetti, A. Renzini, G. Zamorani, O. Ilbert, C. Knobel, A. Iovino, C. Maier, O. Cucciati, L. Tasca, C. M. Carollo, J. Silverman, P. Kampczyk, L. de Ravel, D. Sander, N. Scoville, T. Contini, V. Mainieri, M. Scodeggio, J.-P. Kneib, O. Le Fevre, S. Bardelli, A. Bongiorno, K. Caputi, G. Coppa, S. de la Torre, P. Franzetti, B. Garilli, F. Lamareille, J.-F. Le Borgne, V. Le Brun, M. Mignoli, E. Perez Montero, R. Pello, E. Ricciardelli, M. Tanaka, L. Tresse, D. Vergani, N. Welikala, E. Zucca, P. Oesch, U. Abba, L. Barne, R. Bordoloi, D. Bottini, A. Cappi, P. Cassata, A. Cimatti, M. Fumana, G. Hasinger, A.M. Koekemoer, A. Leauthaud, D. Maccagni, C. Marinoni, H.J. McCracken, P. Memeo, B. Meneux, P. Nair, C. Porciani, V. Presotto, R. Scaramella, and Astronomy
Subjects: ACTIVE GALACTIC NUCLEI, Cosmology: observations, Galaxies: active, Galaxies: distances and redshifts, Galaxies: evolution, Astronomy and Astrophysics, Space and Planetary Science, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, galaxies: active, FOS: Physical sciences, High density, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, SIMILAR-TO 1, 1ST EPOCH DATA, 0103 physical sciences, Galaxy formation and evolution, [INFO]Computer Science [cs], 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, Physics, REDSHIFT SURVEY, FORMING GALAXIES, 010308 nuclear & particles physics, DIGITAL-SKY-SURVEY, VLT DEEP SURVEY, STAR-FORMATION HISTORY, Differential effects, Galaxy, LUMINOSITY FUNCTION, cosmology: observations, galaxies: distances and redshifts, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], galaxies: evolution, STELLAR MASS, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We explore the inter-relationships between mass, star-formation rate and environment in the SDSS, zCOSMOS and other surveys. The differential effects of mass and environment are completely separable to z ~ 1, indicating that two distinct processes are operating, "mass-quenching" and "environment-quenching". Environment-quenching, at fixed over-density, evidently does not change with epoch to z ~ 1, suggesting that it occurs as large-scale structure develops in the Universe. The observed constancy of the mass-function shape for star-forming galaxies, demands that the mass-quenching of galaxies around and above M*, must be proportional to their star-formation rates at all z < 2. We postulate that this simple mass-quenching law also holds over a much broader range of stellar mass and epoch. These two simple quenching processes, plus some additional quenching due to merging, then naturally produce (a) a quasi-static Schechter mass function for star-forming galaxies with a value of M* that is set by the proportionality between the star-formation and mass-quenching rates, (b) a double Schechter function for passive galaxies with two components: the dominant one is produced by mass-quenching and has exactly the same M* as the star-forming galaxies but an alpha shallower by +1, while the other is produced by environment effects and has the same M* and alpha as the star-forming galaxies, and is larger in high density environments. Subsequent merging of quenched galaxies modifies these predictions somewhat in the denser environments, slightly increasing M* and making alpha more negative. All of these detailed quantitative relationships between the Schechter parameters are indeed seen in the SDSS, lending strong support to our simple empirically-based model. The model naturally produces for passive galaxies the "anti-hierarchical" run of mean ages and alpha-element abundances with mass., 66 pages, 19 figures, 1 movie, accepted for publication in ApJ. The movie is also available at http://www.exp-astro.phys.ethz.ch/zCOSMOS/MF_simulation_d1_d4.mov
Published: 2010

12. THE 10k zCOSMOS: MORPHOLOGICAL TRANSFORMATION OF GALAXIES IN THE GROUP ENVIRONMENT SINCEz∼1

Author: E. Ricciardelli, A. Cappi, Lucia Pozzetti, Micol Bolzonella, Daniela Vergani, Thierry Contini, C. M. Carollo, Alvio Renzini, Laurence Tresse, Y. Peng, A. Iovino, Luigi Guzzo, Angela Bongiorno, John D. Silverman, V. Mainieri, E. Zucca, J. F. Le Borgne, Alexis Finoguenov, Graziano Coppa, Claudia Scarlata, V. Le Brun, Paolo Cassata, P. Oesch, Anton M. Koekemoer, Mark Sargent, L. de Ravel, F. Lamareille, Lidia Tasca, S. Bardelli, P. Memeo, S. J. Lilly, P. Kampczyk, Bianca Garilli, N. Z. Scoville, C. Knobel, Jean-Paul Kneib, Ummi Abbas, O. Le Fèvre, D. Maccagni, R. Pello, Karina Caputi, D. Bottini, G. Zamorani, H. J. McCracken, M. Scodeggio, P. Franzetti, Olga Cucciati, Alessandro Cimatti, Masayuki Tanaka, B. Meneux, E. Perez Montero, S. de la Torre, M. Mignoli, Christian Maier, Christian Marinoni, M. Fumana, Cristiano Porciani, Alexie Leauthaud, Roberto Scaramella, K. Kovac, AUTRES, Università di Bologna, Dipartimento di Astronomia, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), University of Chicago, Dipartimento di Fisica, Università degli Studi di Milano-Bicocca [Milano] (UNIMIB)-Università degli Studi di Milano [Milano] (UNIMI), INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), INAF- Milano, Institute of Astronomy [ETH Zürich], Department of Physics [ETH Zürich] (D-PHYS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), INAF - Osservatorio Astronomico di Brera (OAB), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées (LATT), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Glycosciences Laboratory, Imperial College School of Medicine, Tokai University, INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), Space Telescope Science Institute (STSci), Centre de Physique Théorique - UMR 6207 (CPT), Centre National de la Recherche Scientifique (CNRS)-Université de Toulon (UTLN)-Université de Provence - Aix-Marseille 1-Université de la Méditerranée - Aix-Marseille 2, Centre de Physique Théorique - UMR 7332 (CPT), Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), California Institute of Technology (CALTECH), K. Kovac, S. J. Lilly, C. Knobel, M.Bolzonella, A. Iovino, C.M. Carollo, C. Scarlata, M. Sargent, O. Cucciati, G. Zamorani, L. Pozzetti, L.A.M. Tasca, M. Scodeggio, P. Kampczyk, Y. Peng, P. Oesch, E. Zucca, A. Finoguenov, T. Contini, J.-P. Kneib, O. Le Fevre, V. Mainieri, A. Renzini, S. Bardelli, A. Bongiorno, K. Caputi, G. Coppa, S. de la Torre, L. de Ravel, P. Franzetti, B. Garilli, F. Lamareille, J.-F. Le Borgne, V. Le Brun, C. Maier, M. Mignoli, R. Pello, E. Perez Montero, E. Ricciardelli, J.D. Silverman, M. Tanaka, L. Tresse, D. Vergani, U. Abba, D. Bottini, A. Cappi, P. Cassata, A. Cimatti, M. Fumana, L. Guzzo, A.M. Koekemoer, A. Leauthaud, D. Maccagni, C. Marinoni, H. J. McCracken, P. Memeo, B. Meneux, C. Porciani, R. Scaramella, N.Z. Scoville, Università degli Studi di Milano-Bicocca = University of Milano-Bicocca (UNIMIB)-Università degli Studi di Milano = University of Milan (UNIMI), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université de la Méditerranée - Aix-Marseille 2-Université de Provence - Aix-Marseille 1-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and Astronomy
Subjects: Galaxies: Structure, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010504 meteorology & atmospheric sciences, Stellar mass, Population, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Luminosity, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Galaxies: Evolution, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, education.field_of_study, COSMIC cancer database, Group (mathematics), Star formation, Galaxies: High-redshift, Astronomy and Astrophysics, Redshift survey, Galaxy, Space and Planetary Science, Mass function, Galaxies: Clusters: General, Galaxies: Luminosity function, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We study the evolution of galaxies inside and outside of the group environment since z=1 using a large well defined set of groups and galaxies from the zCOSMOS-bright redshift survey in the COSMOS field. The fraction of galaxies with early-type morphologies increases monotonically with M_B luminosity and stellar mass and with cosmic epoch. It is higher in the groups than elsewhere, especially at later epochs. The emerging environmental effect is superposed on a strong global mass-driven evolution, and at z~0.5 and log(M*/Msol)~10.2, the "effect" of group environment is equivalent to (only) about 0.2 dex in stellar mass or 2 Gyr in time. The stellar mass function of galaxies in groups is enriched in massive galaxies. We directly determine the transformation rates from late to early morphologies, and for transformations involving colour and star formation indicators. The transformation rates are systematically about twice as high in the groups as outside, or up to 3-4 times higher correcting for infall and the appearance of new groups. The rates reach values, for masses around the crossing mass 10^10.5 Msol, as high as (0.3-0.7)/Gyr in the groups, implying transformation timescales of 1.4-3 Gyr, compared with less than 0.2/Gyr, i.e. timescales >5 Gyr, outside of groups. All three transformation rates decrease at higher stellar masses, and must decrease also at the lower masses below 10^10 Msol which we cannot well probe. The rates involving colour and star formation are consistently higher than those for morphology, by a factor of about 50%. Our conclusion is that the transformations which drive the evolution of the overall galaxy population since z~1 must occur at a rate 2-4 times higher in groups than outside of them., 21 pages, 13 figures, submitted to ApJ
Published: 2010

13. Extremely Red Galaxies in Abell 1835

Author: Daniel Schaerer, A. Hempel, Eiichi Egami, Johan Richard, and R. Pello
Subjects: Physics, Luminous infrared galaxy, Space and Planetary Science, Radio galaxy, Galaxy group, Elliptical galaxy, Astronomy, Astronomy and Astrophysics, Quasar, Astrophysics, Galaxy merger, Disc, Peculiar galaxy
Abstract: We use multi-colour data of the gravitational lensing cluster Abell 1835 to search for high-z candidates (Richard et al. 2006) and extremely red galaxies.Applying a colour criteria of R-K ≥ 5.6 we have selected 12 EROs, of which 10(9) have no R(I)-band detection. Two of these sources posses multiple detections in the ACS z850 band, possibly gravitationally bound objects.Using the method of Pozzetti and Mannucci (2000) to classify an ERO either as evolved elliptical or dusty starburst, we find that two thirds of all objects have colours assigned to evolved ellipticals. One of the remaining 4 sources is the known sub-mm source SMMJ14009+0252.The spectral energy distributions of sources with no optical detection show strong similarities to the SED of the high-z object of Mobasher et al. (2005), i.e. a degeneracy between a low- and high-z solution. However, for objects we accept the low-z solution as the better fit.A detailed analyses of the colour properties and spectral energy distribution will be published in two forthcoming papers (Schaerer et al., Hempel et al.).
Published: 2017

14. Strong lensing analysis of Abell 2744 with MUSE and Hubble Frontier Fields images

Author: Guillaume Mahler, Vera Patrício, Marcella Carollo, Roland Bacon, Lutz Wisotzki, B. Clement, G. Soucail, Rychard Bouwens, Floriane Leclercq, J. Martinez, Johan Richard, D. Lagattuta, Michael V. Maseda, R. Pello, Hanae Inami, Kasper B. Schmidt, 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: galaxies: high redshift, Dark matter, Continuum (design consultancy), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, dark matter, Data cube, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, Cluster (physics), 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Remote sensing, Line (formation), Physics, 010308 nuclear & particles physics, galaxies: clusters: individual: Abell 2744, gravitational lensing: strong, Astronomy and Astrophysics, Image plane, Astrophysics - Astrophysics of Galaxies, Redshift, Abell 2744, Space and Planetary Science, techniques: imaging spectroscopy, Astrophysics of Galaxies (astro-ph.GA)
Abstract: We present an analysis of MUSE observations obtained on the massive Frontier Fields cluster Abell 2744. This new dataset covers the entire multiply-imaged region around the cluster core. We measure spectroscopic redshifts for HST-selected continuum sources together with line emitters blindly detected in the datacube. The combined catalog consists of 514 spectroscopic redshifts (with 414 new identifications), including 156 cluster members and 326 magnified background sources. We use this redshift information to perform a strong-lensing analysis of all multiple images previously found in the deep Frontier Field images, and add three new MUSE-detected multiply-imaged systems with no obvious HST counterpart. The combined strong lensing constraints include a total of 60 systems producing 188 images altogether, out of which 29 systems and 83 images are spectroscopically confirmed, making Abell 2744 one of the most well-constrained clusters to date. A parametric mass model including two cluster-scale components in the core and several group-scale substructures at larger radii accurately reproduces all the spectroscopic multiple systems, reaching an rms of 0.67" in the image plane. Overall, the large number of spectroscopic redshifts gives us a robust model and we estimate the systematics on the mass density and magnification within the cluster core to be typically ~9%., 34 pages, 20 figures. Accepted for publication in MNRAS. Full high resolution pdf and other data are available at http://muse-vlt.eu/science/a2744/
Published: 2017

15. The ALMA Frontier Fields Survey - II. Multiwavelength Photometric analysis of 1.1mm continuum sources in Abell 2744, MACSJ0416.1-2403 and MACSJ1149.5+2223

Author: P. Troncoso-Iribarren, Larry Bradley, G. Brammer, Xingxing Huang, N. Padilla, Edo Ibar, Hugo Messias, R. Kneissl, C. Romero-Cañizales, Nicolas Laporte, Leopoldo Infante, Franz E. Bauer, Timo Anguita, Richard S. Ellis, R. Demarco, R. Pello, A. M. Muñoz Arancibia, Adi Zitrin, Harold Francke, Neil M. Nagar, W. Zheng, Anton M. Koekemoer, Manuel Aravena, J. González-López, M. Carrasco, Holland C. Ford, Marc Postman, D. Quénard, Ezequiel Treister, E. Villard, Seock-Sam Kim, R. J. Bouwens, L. F. Barrientos, R. Carvajal, Dan Coe, 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), 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: submillimeter: galaxies, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, infrared: galaxies, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Photometry (optics), Spitzer Space Telescope, galaxies: high-redshift, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, Photometric redshift, radio continuum: galaxies, Luminous infrared galaxy, Physics, Very Large Telescope, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, galaxies: photometry, Abell 2744, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics, galaxies: distances and redshifts
Abstract: [abridged] The Hubble and Spitzer Space Telescope surveys of the Frontier Fields (FF) provide extremely deep images around six massive, strong-lensing clusters of galaxies. The ALMA FF survey aims to cover the same fields at 1.1mm, with maps reaching (unlensed) sensitivities of $$5$\sigma$) sources in the first three FF clusters observed by ALMA, based on data from Hubble and Spitzer, the VLT and Herschel. We measure the total photometry in all available bands and determine the photometric redshifts and the physical properties of the counterparts via SED-fitting. In particular, we carefully estimate the FIR photometry using 1.1mm priors to limit the misidentification of blended FIR counterparts, which strongly affect some flux estimates in previous FIR catalogs. We identify robust near-infrared (NIR) counterparts for all 11 sources with K$_s$ detection, the majority of which are quite red, with eight having $F814W-K_s\gtrsim 4$ and five having $F160W-[4.5]\gtrsim3$. From the FIR point of view, all our objects have $z_{phot}$$\sim$1--3, whereas based on the optical SED one object prefers a high-$z$ solution ($z\geq\ $7). Five objects among our sample have spectroscopic redshifts from the GLASS survey for which we can reproduce their SEDs with existing templates. This verification confirms the validity of our photometric redshift methodology. The mean redshift of our sample is $z_{phot}$=1.99$\pm$0.27. All 1.1mm selected objects are massive (10.0$ \approx$1.6) and high dust contents (8.1 $, Comment: 18 pages, 11 figures, accepted for publication in A&A
Published: 2017
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16. The MUSE Hubble Ultra Deep Field Survey VI: The Faint-End of the Ly$\alpha$ Luminosity Function at $2.91 < z < 6.64$ and Implications for Reionisation

Author: R. Pello, Lutz Wisotzki, Simon Conseil, Raffaella Anna Marino, Peter M. Weilbacher, Jeremy Blaizot, Hanae Inami, Takuya Hashimoto, Thierry Contini, Guillaume Mahler, Roland Bacon, E. Ventou, J. Lewis, Joseph Caruana, Floriane Leclercq, Thibault Garel, Johan Richard, Edmund Christian Herenz, Anne Verhamme, Alyssa B. Drake, B. Guiderdoni, Joop Schaye, 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), 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), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - 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), 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 ), Institut de recherche en astrophysique et planétologie ( IRAP ), and Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS )
Subjects: [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, first stars, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Parameter space, 01 natural sciences, 0103 physical sciences, galaxies: formation, dark ages, 010303 astronomy & astrophysics, Reionization, Astrophysics::Galaxy Astrophysics, Physics, COSMIC cancer database, 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, early Universe, Hubble Ultra-Deep Field, Redshift, Galaxy, galaxies: luminosity function, Space and Planetary Science, mass function, Dark Ages, reionization, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present the deepest study to date of the Lya luminosity function (LF) in a blank field using blind integral field spectroscopy from MUSE. We constructed a sample of 604 Lya emitters (LAEs) across the redshift range 2.91 < z < 6.64 using automatic detection software in the Hubble Ultra Deep Field. We calculate accurate total Lya fluxes capturing low surface brightness extended Lya emission now known to be a generic property of high-redshift star-forming galaxies. We simulated realistic extended LAEs to characterise the selection function of our samples, and performed flux-recovery experiments to test and correct for bias in our determination of total Lya fluxes. We find an accurate completeness correction accounting for extended emission reveals a very steep faint-end slope of the LF, alpha, down to luminosities of log10 L erg s^-1< 41.5, applying both the 1/Vmax and maximum likelihood estimators. Splitting the sample into three broad redshift bins, we see the faint-end slope increasing from -2.03+1.42-inf at z ~ 3.44 to -2.86+0.76-inf at z ~ 5.48, however no strong evolution is seen between the 68% confidence regions in L*-alpha parameter space. Using the Lya line flux as a proxy for star formation activity, and integrating the observed LFs, we find that LAEs' contribution to the cosmic SFRD rises with redshift until it is comparable to that from continuum-selected samples by z ~ 6. This implies that LAEs may contribute more to the star-formation activity of the early Universe than previously thought - any additional interglactic medium correction would act to further boost the Lya luminosities. Finally, assuming fiducial values for the escape of Lya and LyC radiation, and the clumpiness of the IGM, we integrated the maximum likelihood LF at 5.00 < z < 6.64 and find we require only a small extrapolation beyond the data (< 1 dex in L) for LAEs alone to maintain an ionised IGM at z ~ 6., Comment: 16 pages, 10 figures. Accepted for publication in A&A special issue: "The MUSE Hubble Ultra Deep Field Survey" (MUSE UDF Series Paper VI)
Published: 2017

17. Lens modelling Abell 370: crowning the final frontier field with MUSE

Author: Kasper B. Schmidt, J. Martinez, Johan Richard, D. Bina, Lutz Wisotzki, G. Soucail, R. Pello, Guillaume Mahler, D. Lagattuta, B. Clement, Vera Patrício, 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), 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: Dark matter, FOS: Physical sciences, Scale (descriptive set theory), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, dark matter, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], galaxies: high-redshift, 0103 physical sciences, Cluster (physics), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, galaxies: clusters: individual: Abell 370, Physics, Mass distribution, 010308 nuclear & particles physics, Astronomy, gravitational lensing: strong, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Abell 2744, Space and Planetary Science, techniques: imaging spectroscopy, Astrophysics of Galaxies (astro-ph.GA), Halo
Abstract: We present a strong lensing analysis on the massive cluster Abell 370 (A370; z = 0.375), using a combination of deep multi-band Hubble Space Telescope (HST) imaging and Multi-Unit Spectroscopic Explorer (MUSE) spectroscopy. From only two hours of MUSE data, we are able to measure 120 redshifts in the Southern BCG area, including several multiply-imaged lens systems. In total, we increase the number of multiply-imaged systems with a secure redshift from 4 to 15, nine of which are newly discovered. Of these, eight are located at z > 3, greatly extending the redshift range of spectroscopically-confirmed systems over previous work. Using these systems as constraints, we update a parametric lens model of A370, probing the mass distribution from cluster to galaxy scales. Overall, we find that a model with only two cluster- scale dark matter halos (one for each BCG) does a poor job of fitting these new image constraints. Instead, two additional mass clumps -- a central "bar" of mass located between the BCGs, and another clump located within a "crown" of galaxies in the Northern part of the cluster field -- provide significant improvements to the fit. Additional physical evidence suggests these clumps are indeed real features of the system, but with relatively few image constraints in the crown region, this claim is difficult to evaluate from a modeling perspective. Additional MUSE observations of A370 covering the entire strong-lensing region will greatly help these efforts, further improving our understanding of this intriguing cluster., 20 pages, 13 figures, submitted to MNRAS
Published: 2017

18. Optimal CYFRA 21-1 cut-off in patients with suspected malignancy

Author: S. Garcia-Valdecasas Gayo, M.J. Ruiz-Alvarez, E. Marquez Lietor, D. Gonzalez Gay, A. De Lozar De La ViÑa, R. Ramos Corral, N. Del Amo Del Arco, R. Pello Gutierrez, B. Ortega Carballo, R. Guillen Santos, and F. Cava Valenciano
Subjects: medicine.medical_specialty, business.industry, Biochemistry (medical), Clinical Biochemistry, Suspected malignancy, Medicine, In patient, General Medicine, Radiology, CYFRA 21-1, business, Biochemistry
Published: 2019

19. 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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20. 3D kinematics of high-z galaxies as seen through the gravitational telescope

Author: T. Contini, M. Lemoine-Busserolle, R. Pello, Andrew Bunker, Jean-Paul Kneib, Markus Kissler-Patig, and Sebastián F. Sánchez
Subjects: Luminous infrared galaxy, Physics, Radio galaxy, Galaxy group, Elliptical galaxy, Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Brightest cluster galaxy, Disc, Astrophysics::Galaxy Astrophysics, Galaxy cluster, Peculiar galaxy
Abstract: The study of the physical properties of high-redshift galaxies has become one of the major goals of extragalactic astronomy. In particular the massassembly histories of galaxies have been the focus of many studies at redshifts 1 to 3. In the purpose of probing the dynamics of intermediate and high-redshift galaxies, we have designed a research program to carry out a near-infrared spectroscopic follow up of spatially resolved distant galaxies. Here, we present the results for A370-A5 (z=1.341), an arc behind the lens cluster Abell 370 (z=0.374), observed in the case of science verification programme of SINFONI/VLT. The natural magni fication due to massive galaxy clusters allows to spatially resolve and constrain the dynamics of young star forming galaxies 1 to 3 magnitudes fainter than those selected in blank fields. Thus, the study of lensed galaxies allows to probe a low mass regime of galaxies not accessible in standard observation. In this particular case, we found that the gas distribution and kinematics are consistent with a bipolar outflow with a range of velocities of v ∼ 100km/s. © 2007 Springer-Verlag Berlin Heidelberg.
Published: 2016

21. Multi-wavelength characterisation of z ~ 2 clustered, dusty star-forming galaxies discovered by Planck

Author: Guilaine Lagache, E. Le Floc'h, Herve Dole, L. Montier, Genevieve Soucail, D. Pierini, D. Guery, I. Flores-Cacho, R. Pello, R. Cañameras, Nicole P. H. Nesvadba, Etienne Pointecouteau, 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 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 National d’Études Spatiales [Paris] (CNES), Institut Universitaire de France (IUF), Ministère de l'Education nationale, de l’Enseignement supérieur et de la Recherche (M.E.N.E.S.R.), 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), I.F.C., L.M. and E.P. acknowledge the support from grant ANR-11-BD56-015. DP acknowledges the financial support from Labex OCEVU. This work has been carried out thanks to the support of the OCEVU Labex (ANR-11-LABX-0060) and the A*MIDEX project (ANR-11-IDEX-0001-02), funded by the 'Investissements d’Avenir' French government program managed by the ANR., ANR-11-IDEX-0001,Amidex,INITIATIVE D'EXCELLENCE AIX MARSEILLE UNIVERSITE(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), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Sud - Paris 11 (UP11), 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), Université Fédérale Toulouse Midi-Pyrénées-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), ANR-11-IDEX-0001-02/11-LABX-0060,OCEVU,Origines, Constituants et EVolution de l'Univers(2011), and ANR-11-IDEX-0001-02/11-IDEX-0001,AMIDEX,AMIDEX(2011)
Subjects: submillimeter: galaxies, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, law.invention, Telescope, symbols.namesake, law, galaxies: high-redshift, 0103 physical sciences, Planck, Spectroscopy, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Photometric redshift, Physics, 010308 nuclear & particles physics, Near-infrared spectroscopy, Astronomy and Astrophysics, Radius, Astrophysics - Astrophysics of Galaxies, Galaxy, Space and Planetary Science, galaxies: clusters: general, Astrophysics of Galaxies (astro-ph.GA), cosmology: observations, galaxies: star formation, symbols, Substructure, Astrophysics::Earth and Planetary Astrophysics, large-scale structure of Universe, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: (abridged) We report the discovery of PHz G95.5-61.6, a complex structure detected in emission in the Planck all-sky survey that corresponds to two over-densities of high-redshift galaxies. This is the first source from the Planck catalogue of high-z candidates that has been completely characterised with follow-up observations from the optical to the sub-millimetre domain. Herschel/SPIRE observations at 250, 350 and 500 microns reveal the existence of five sources producing a 500 microns emission excess that spatially corresponds to the candidate proto-clusters discovered by Planck. Further observations at CFHT in the optical bands (g and i) and in the near infrared (J, H and K_s), plus mid infrared observations with IRAC/Spitzer (at 3.6 and 4.5 microns) confirm that the sub-mm red excess is associated with an over-density of colour-selected galaxies. Follow-up spectroscopy of 13 galaxies with VLT/X-Shooter establishes the existence of two high-z structures: one at z~1.7 (three confirmed member galaxies), the other at z~2.0 (six confirmed members). This double structure is also seen in the photometric redshift analysis of a sample of 127 galaxies located inside a circular region of 1'-radius containing the five Herschel/SPIRE sources, where we found a double-peaked excess of galaxies at z~1.7 and z~2.0 with respect to the surrounding region. These results suggest that PHz G95.5-61.6 corresponds to two accreting nodes, not physically linked to one another, embedded in the large scale structure of the Universe at z~2 and along the same line-of-sight. In conclusion, the data, methods and results illustrated in this pilot project confirm that Planck data can be used to detect the emission from clustered, dusty star forming galaxies at high-z, and, thus, to pierce through the early growth of cluster-scale structures., Comment: 15 pages, 13 figures. Accepted for publication in Astronomy and Astrophysics
Published: 2016

22. MUSE observations of the lensing cluster Abell 1689

Author: Joel Vernet, J. Lewis, Johan Richard, R. Pello, Jean-Gabriel Cuby, G. Soucail, Anne Verhamme, Benjamin Clément, David J. Lagattuta, Lutz Wisotzki, Peter M. Weilbacher, Roland Bacon, Kurt T. Soto, Sebastiano Cantalupo, D. Bina, Edmund Christian Herenz, V. Patrício, 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), Bina, D, Pello, R, Richard, J, Lewis, J, Patricio, V, Cantalupo, S, Herenz, E, Soto, K, Weilbacher, P, Bacon, R, Vernet, J, Wisotzki, L, Clement, B, Cuby, J, Lagattuta, D, Soucail, G, Verhamme, A, 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: Physics, Very Large Telescope, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Gravitational lensing: strong, Galaxies: high-redshift, FOS: Physical sciences, Astronomy and Astrophysics, Context (language use), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Multi Unit Spectroscopic Explorer, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Galaxies: clusters: individual: Abell 1689, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Spectral resolution, 010306 general physics, 010303 astronomy & astrophysics, Reionization, Astrophysics::Galaxy Astrophysics, Luminosity function (astronomy)
Abstract: We present the results obtained with MUSE on the core of the lensing cluster A1689. Integral-field observations with MUSE provide a unique view of the central region, allowing us to conduct a complete census on both cluster galaxies and lensed background sources, identified based on their spectral features without preselection. We investigate the multiple-image configuration for all known sources in the field. Previous to our survey, 28 different lensed galaxies displaying 46 multiple images were known in the MUSE field of view, most of them based on photometric redshifts and lensing considerations. Among them, we spectroscopically confirm 12 images based on their emission-lines, corresponding to 7 different lensed galaxies between z = 0.95 and 5.0. In addition, 14 new galaxies have been spectroscopically identified in this area, with redshifts ranging between 0.8 and 6.2. All background sources within the MUSE field of view correspond to multiple-imaged systems lensed by A1689. 17 sources in total are found at z > 3 based on their Lyman-alpha emission, with Lyman-alpha luminosities ranging between 40.5 < log(Ly{\alpha}) < 42.5 after correction for magnification. This sample is particularly sensitive to the slope of the LF toward the faintest-end. The density of sources obtained in this survey is consistent with a steep value of {\alpha} < -1.5, although this result still needs further investigation. These results illustrate the efficiency of MUSE in the characterization of lensing clusters on one hand, and the study of faint and distant populations of galaxies on the other hand. In particular, our current survey of lensing clusters should provide a unique census of sources responsible for the reionization in a representative volume at z ~ 4-7., Comment: 12 pages, 11 figures
Published: 2016
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23. The COSMOS density field: a reconstruction using both weak lensing and galaxy distributions

Author: Graziano Coppa, Jean-Paul Kneib, Alvio Renzini, S. Lilly, O. Le Fèvre, C. M. Carollo, M. Mignoli, C. López-Sanjuan, E. Zucca, A. Iovino, Jeffrey M. Silverman, Niraj Welikala, F. Lamareille, J. F. Le Borgne, Masayuki Tanaka, Angela Bongiorno, A. Koekoemoer, Karina Caputi, S. de la Torre, H. J. McCracken, K. Kovac, P. Kampczyk, Olga Cucciati, Rongmon Bordoloi, Richard Massey, Bianca Garilli, R. Pello, Preethi Nair, P. Franzetti, A. Cappi, Micol Bolzonella, Andrea Cimatti, V. Mainieri, Adam Amara, S. Bardelli, E. Perez Montero, Christian Maier, Luke A. Barnes, C. Knobel, Thierry Contini, G. Zamorani, Michele Moresco, Lidia Tasca, M. Scodeggio, Lucia Pozzetti, Daniela Vergani, V. Presotto, L. de Ravel, Laurence Tresse, Y. Peng, V. Le Brun, and Jason Rhodes
Subjects: Physics, 010308 nuclear & particles physics, Dark matter, Gaussian blur, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Redshift, Galaxy, symbols.namesake, Space and Planetary Science, 0103 physical sciences, symbols, Entropy (information theory), 010303 astronomy & astrophysics, Scaling, Weak gravitational lensing, Smoothing
Abstract: The COSMOS field has been the subject of a wide range of observations, with a number of studies focusing on reconstructing the 3D dark matter density field. Typically, these studies have focused on one given method or tracer. In this paper, we reconstruct the distribution of mass in the COSMOS field out to a redshift z=1 by combining Hubble Space Telescope weak lensing measurements with zCOSMOS spectroscopic measurements of galaxy clustering. The distribution of galaxies traces the distribution of mass with high resolution (particularly in redshift, which is not possible with lensing), and the lensing data empirically calibrates the mass normalisation (bypassing the need for theoretical models). Two steps are needed to convert a galaxy survey into a density field. The first step is to create a smooth field from the galaxy positions, which is a point field. We investigate four possible methods for this: (i) Gaussian smoothing, (ii) convolution with truncated isothermal sphere, (iii) fifth nearest neighbour smoothing and (iv) a muliti-scale entropy method. The second step is to rescale this density field using a bias prescription. We calculate the optimal bias scaling for each method by comparing predictions from the smoothed density field with the measured weak lensing data, on a galaxy-by-galaxy basis. In general, we find scale-independent bias for all the smoothing schemes, to a precision of 10%. For the nearest neighbour smoothing case, we find the bias to be 2.51\pm 0.25. We also find evidence for a strongly evolving bias, increasing by a factor of ~3.5 between redshifts 0
Published: 2012

24. 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

25. Extragalactic science with the FRESNEL imager

Author: Johan Richard, R. Pello, and Alexandre Maizy
Subjects: Physics, Cosmic Vision, business.industry, media_common.quotation_subject, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy, Universe, Fresnel Imager, Interferometry, Optics, Space and Planetary Science, business, Image resolution, media_common
Abstract: The space Fresnel Interferometric Imager, originally proposed to the ESA Cosmic Vision plan, is an innovative concept providing enhanced capabilities in terms of spatial resolution and dynamical range. In this paper we describe some of the most promising applications of the Fresnel Interferometric Imager concept in extragalactic studies. There are two different topics where the FII could make major progress. The first one is the mapping of star-formation in galaxies, from the local universe to ∼75–85% look back time, based on the first version of FII which is optimized for the UV and optical domains. The second topic is a test case for a subsequent improved version of FII, with a larger collecting area and optimized for the near-IR, focusing on the physical properties of the first galaxies.
Published: 2010

26. 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

27. The role of environment in the morphological transformation of galaxies in 9 rich intermediate redshift clusters

Author: G. Foëx, G. Soucail, R. Pello, Marc Huertas-Company, European Southern Observatory, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), 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 Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Pôle Astronomie du LESIA, 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)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, 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), 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: Physics, education.field_of_study, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Population, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Radius, Astrophysics, Galaxy, Redshift, Morphological transformation, Space and Planetary Science, Cluster (physics), Segregation effect, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], education, Low Mass, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: [abridged] We analyze a sample of 9 massive clusters at 0.49.5). We find that the red sequence is already in place at z~0.5 and it is mainly composed of very massive (log(M/Msol)>11.3) early-type galaxies. These massive galaxies seem to be already formed when they enter the cluster, probably in infalling groups, since the fraction remains constant with the cluster radius. Their presence in the cluster center could be explained by a segregation effect reflecting an early assembly history. Any evolution that takes place in the galaxy cluster population occurs therefore at lower masses (10.3, Comment: A&A in press
Published: 2009

28. A new window of exploration in the mass spectrum: strong lensing by galaxy groups in the SL2S

Author: Tomás Verdugo, Jean-Paul Kneib, Jon Willis, Sherry H. Suyu, G. Soucail, Bernard Fort, Eric Jullo, C. Faure, Anupreeta More, D. Valls-Gabaud, Philip J. Marshall, Raphael Gavazzi, Mark Swinbank, Johan Richard, David Crampton, H. Tu, Veronica Motta, G. Foëx, Karun Thanjavur, Remi A. Cabanac, Marceau Limousin, Yannick Mellier, R. Pello, J.-F. Sygnet, Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), AUTRES, Departamento de Fisica y Astronomia [Valparaiso], Universidad de Valparaiso [Chile], Institute for Computational Cosmology (ICC), Durham University, 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), Département Réseaux, Sécurité et Multimédia (RSM), Université européenne de Bretagne - European University of Brittany (UEB)-Télécom Bretagne-Institut Mines-Télécom [Paris] (IMT), 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), Department of Astronomy, Stanford University, Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), 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 -Institut national des sciences de l'Univers (INSU - CNRS)-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 -Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and 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 -Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Dark-Matter, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Density Profiles, Xmm-Newton, Dark matter, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Environments, 01 natural sciences, Clusters, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], X-Ray-Properties, Galaxy group, Cosmic-Horseshoe, 0103 physical sciences, Group Connection, gravitational lensing: cosmology: large-scale structure of Universe, 010303 astronomy & astrophysics, Mass-to-light ratio, Astrophysics::Galaxy Astrophysics, Weak gravitational lensing, Galaxy cluster, Physics, Sdss, 010308 nuclear & particles physics, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Galaxy, Redshift, Separation Gravitational Lenses, Space and Planetary Science, Elliptical galaxy, Astrophysics::Earth and Planetary Astrophysics
Abstract: The existence of strong lensing systems with Einstein radii (Re) covering the full mass spectrum, from ~1-2" (produced by galaxy scale dark matter haloes) to >10" (produced by galaxy cluster scale haloes) have long been predicted. Many lenses with Re around 1-2" and above 10" have been reported but very few in between. In this article, we present a sample of 13 strong lensing systems with Re in the range 3"- 8", i.e. systems produced by galaxy group scale dark matter haloes, spanning a redshift range from 0.3 to 0.8. This opens a new window of exploration in the mass spectrum, around 10^{13}- 10^{14} M_{sun}, which is a crucial range for understanding the transition between galaxies and galaxy clusters. Our analysis is based on multi-colour CFHTLS images complemented with HST imaging and ground based spectroscopy. Large scale properties are derived from both the light distribution of the elliptical galaxies group members and weak lensing of the faint background galaxy population. On small scales, the strong lensing analysis yields Einstein radii between 2.5" and 8". On larger scales, the strong lenses coincide with the peak of the light distribution, suggesting that mass is traced by light. Most of the luminosity maps have complicated shapes, indicating that these intermediate mass structures are dynamically young. Fitting the reduced shear with a Singular Isothermal Sphere, we find sigma ~ 500 km/s and an upper limit of ~900 km/s for the whole sample. The mass to light ratio for the sample is found to be M/L_i ~ 250 (solar units, corrected for evolution), with an upper limit of 500. This can be compared to mass to light ratios of small groups (with sigma ~ 300 km/s and galaxy clusters with sigma > 1000 km/s, thus bridging the gap between these mass scales., A&A Accepted. Draft with Appendix images can be found at http://www.dark-cosmology.dk/~marceau/groups_sl2s.pdf
Published: 2009

29. Physical properties of galaxies and their evolution in the VIMOS VLT Deep Survey

Author: E. Zucca, Bianca Garilli, M. Scodeggio, C. Adami, A. Cappi, A. Iovino, A. Pollo, Jarle Brinchmann, M. Radovich, Angela Bongiorno, Luca Limatola, S. Bardelli, Thierry Contini, Enrique Pérez-Montero, I. Gavignaud, Daniela Vergani, Sylvie Foucaud, Roberto Scaramella, A. Mazure, R. Merighi, H. J. McCracken, M. Bolzonella, Christian Marinoni, O. Le Fevre, R. Pello, Gianni Zamorani, L. Tresse, Stephane Charlot, Paolo Ciliegi, Bruno Marano, B. Meneux, A. Romano, O. Ilbert, P. Franzetti, V. Le Brun, A. Zanichelli, Giampaolo Vettolani, C.J. Walcher, Aniello Grado, D. Maccagni, Stéphane Paltani, Luigi Guzzo, F. Lamareille, D. Bottini, Lucia Pozzetti, S. Arnouts, 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), INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto, 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), INAF- Milano, Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Universidade do Porto = University of Porto, 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), Lamareille F., Brinchmann J., Contini T., Walcher C. J., Charlot S., Pérez-Montero E., Zamorani G., Pozzetti L., Bolzonella M., Garilli B., Paltani S., Bongiorno A., Le Fèvre O., Bottini D., Le Brun V., Maccagni D., Scaramella R., Scodeggio M., Tresse L., Vettolani G., Zanichelli A., Adami C., Arnouts S., Bardelli S., Cappi A., Ciliegi P., Foucaud S., Franzetti P., Gavignaud I., Guzzo L., Ilbert O., Iovino A., McCracken H. J., Marano B., Marinoni C., Mazure A., Meneux B., Merighi R., Pellò R., Pollo A., Radovich M., Vergani D., Zucca E., Romano A., Grado A., and Limatola L.
Subjects: Active galactic nucleus, Stellar population, Metallicity, FOS: Physical sciences, galaxies: starburst, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Apparent magnitude, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Emission spectrum, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, GALAXIES: STARBUST, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics (astro-ph), Spectral density, galaxies: fundamental parameters, Astronomy and Astrophysics, Redshift, Galaxy, Space and Planetary Science, galaxies: abundances, galaxies: evolution
Abstract: We derive the mass-metallicity relation of star-forming galaxies up to $z\sim0.9$, using data from the VIMOS VLT Deep Survey. Automatic measurement of emission-line fluxes and equivalent widths have been performed on the full spectroscopic sample. This sample is divided into two sub-samples depending on the apparent magnitude selection: wide ($I_{\mathrm{AB}}, 21 pages, revised version submitted to A&A
Published: 2009

30. VVDS-SWIRE

Author: S. Temporin, D. Maccagni, F. Lamareille, Duncan Farrah, Alain Mazure, C. J. Walcher, Paolo Ciliegi, Christian Marinoni, B. Garilli, V. Le Brun, O. Ilbert, D. Vergani, J. P. Picat, Fan Fang, L. Tresse, T. Contini, Angela Bongiorno, Jarle Brinchmann, E. Zucca, P. Franzetti, S. Paltani, Roberto Scaramella, R. Merighi, Stephane Arnouts, R. Pello, O. Le Fevre, Lucia Pozzetti, G. Zamorani, A. Zanichelli, Stéphane Charlot, M. Bondi, Mario Radovich, S. J. Oliver, H. J. McCracken, David L. Shupe, O. Cucciati, Carol J. Lonsdale, S. de la Torre, Yannick Mellier, D. Bottini, Bruno Marano, C. Adami, A. Pollo, I. Gavignaud, S. Bardelli, Paola Merluzzi, Luigi Guzzo, M. Bolzonella, I. Waddington, Marco Scodeggio, G. Vettolani, A. Iovino, Sylvie Foucaud, Jason Surace, B. Meneux, A. Cappi, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), INAF-Osservatorio Astronomico di Brera, Department of Astronomy, Cornell University, Infrared Processing Analysis Center, California Institute of Technology (IPAC), University of Sussex, Observatoire Astronomique de l'Université de Genève, Istituto di Astrofisica Spaziale e Fisica Cosmica (IASF-Milano), Spitzer Science Center, California Institute of Technology (SSC), 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), IRA-INAF, Bologna, INAF-Osservatorio Astronomico di Bologna (OABO), Max-Planck-Institut für Astrophysik (MPA), 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), School of Physics and Astronomy, University of Nottingham, Astrophysikalisches Institut Potsdam (AIP), Institute for Astronomy, University of Hawaii, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), 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), Centre de Physique Théorique - UMR 7332 (CPT), Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), INTEGRAL Science Data Centre, INAF-Osservatorio Astronomico di Capodimonte (INAF-OAC), and Centro de Astrofisica da Universidade do Porto (CAUP)
Subjects: Physics, Star formation, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Correlation function (astronomy), Galaxy, Redshift, Luminosity, Photometry (optics), Stars, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Cluster analysis, Astrophysics::Galaxy Astrophysics
Abstract: International audience; Aims:By combining data from the VIMOS VLT Deep Survey (VVDS) with the Spitzer Wide-area InfraRed Extragalactic survey (SWIRE), we have built the currently largest spectroscopic sample of high redshift galaxies selected in the rest-frame near-infrared. We have obtained 2040 spectroscopic redshifts of galaxies with (m3.6)_AB < 21.5 at 3.6 mu m, and 1255 spectroscopic redshifts of galaxies with (m4.5)_AB < 21. These allow us to investigate the clustering evolution of galaxies selected via their rest-frame near-infrared luminosity in the redshift range 0.2 < z < 2.1. Methods: We use the projected two-point correlation function w_p(r_p) to study the three dimensional clustering properties of galaxies detected at 3.6 mu m and 4.5 mu m with the InfraRed Array Camera (IRAC) in the SWIRE survey with measured spectroscopic redshifts from the first epoch VVDS. We compare these properties to those of a larger sample of 16672 SWIRE galaxies for which we have accurate photometric redshifts in the same field. Results: We find that in the 3.6 mu m and 4.5 mu m flux limited samples, the apparent correlation length does not change from redshift ~2 to the present. The measured correlation lengths have a mean value of r0 ~= 3.9±0.5 h-1 Mpc for the galaxies selected at 3.6 mu m and a mean value of r0 ~= 4.4±0.5 h-1 Mpc for the galaxies selected at 4.5 mu m, across the whole redshift range explored. These values are larger than those typicaly found for I-band selected galaxies at I_AB < 24, for which r0 varies from 2.69 h-1 Mpc to 3.63 h-1 Mpc between z = 0.5 to z = 2.1. We find that the difference in correlation length between I-band and 3.6-4.5 mum selected samples decreases with increasing redshift, becoming comparable at z ~= 1.5. We interpret this as evidence that galaxies with older stellar populations and galaxies actively forming stars reside in comparably over-dense environments at epochs earlier than z ~= 1.5, supporting the recently reported flattening of the color-density relation at high redshift. The increasing difference in correlation length with cosmic time observed between rest-frame UV-optical and near-infrared selected samples could then be an indication that star formation is gradually shifting to lower density regions with decreasing redshift, while the older, passively evolving galaxies remain in the most over-dense peaks.
Published: 2007

31. The VIMOS-VLT deep survey

Author: J. P. Picat, Stéphane Charlot, O. Cucciati, C. Adami, T. Contini, M. Bolzonella, Jarle Brinchmann, D. Bottini, Luigi Guzzo, C. J. Walcher, A. Pollo, I. Gavignaud, E. Zucca, A. Iovino, B. Meneux, S. Bardelli, Sylvie Foucaud, P. Franzetti, A. Zanichelli, Paolo Ciliegi, Marco Scodeggio, H. J. McCracken, A. Cappi, O. Le Fevre, G. Zamorani, F. Lamareille, R. Pello, D. Maccagni, Roberto Scaramella, Stéphane Paltani, A. Mazure, V. Le Brun, O. Ilbert, R. Merighi, Mario Radovich, Bruno Marano, Stephane Arnouts, B. Garilli, Lucia Pozzetti, L. Tresse, G. Vettolani, M. Arnaboldi, Christian Marinoni, D. Vergani, Istituto di Astrofisica Spaziale e Fisica Cosmica (IASF-Milano), INAF-Osservatorio Astronomico di Brera, 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, University of Hawaii, INAF-Osservatorio Astronomico di Bologna (OABO), 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), Centro de Astrofisica da Universidade do Porto (CAUP), 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), Istituto di Radioastronomia, Bologna, School of Physics and Astronomy, University of Nottingham, Astrophysikalisches Institut Potsdam (AIP), 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), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Centre de Physique Théorique - UMR 7332 (CPT), Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), INTEGRAL Science Data Centre, INAF-Osservatorio Astronomico di Capodimonte (INAF-OAC), Authors: Franzetti P., Scodeggio M., Garilli B., Vergani D., Maccagni D., Guzzo L., Tresse L., Ilbert O., Lamareille F., Contini T., Le Fèvre O., Zamorani G., Brinchmann J., Charlot S., Bottini D., Le Brun V., Picat J. P., Scaramella R., Vettolani G., Zanichelli A., Adami C., Arnouts S., Bardelli S., Bolzonella M., Cappi A., Ciliegi P., Foucaud S., Gavignaud I., Iovino A., McCracken H. J., Marano B., Marinoni C., Mazure A., Meneux B., Merighi R., Paltani S., Pellò R., Pollo A., Pozzetti L., Radovich M., Zucca E., Cucciati O., and Walcher C. J.
Subjects: GALAXIES: EVOLUTION, Physics, Astrophysics (astro-ph), COSMOLOGY: OBSERVATIONS, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Rest frame, Stellar classification, Redshift, Galaxy, Bimodality, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Emission spectrum, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], VIMOS-VLT Deep Survey, Equivalent width, Astrophysics::Galaxy Astrophysics
Abstract: In this paper we discuss the mix of star-forming and passive galaxies up to z~2, based on the first epoch VIMOS-VLT Deep Survey (VVDS) data.In agreement with previous works we find that the galaxy rest-frame color distribution follows a bimodal distribution at z, 15 pages, 10 figures, 2 tables, revised version accepted for publication on A&A
Published: 2007

32. zCOSMOS 20k: Satellite galaxies are the main drivers of environmental effects in the galaxy population at least to z~0.7

Author: Angela Bongiorno, Michele Moresco, G. Zamorani, K. Caputi, E. Pérez Montero, Anton M. Koekemoer, Daniela Vergani, Vincenzo Mainieri, Jean-Paul Kneib, P. Kampczyk, A. Iovino, F. Lamareille, J. F. Le Borgne, Laurence Tresse, John D. Silverman, S. Bardelli, Marco Scodeggio, C. Knobel, V. Presotto, E. Le Floc'h, L. de Ravel, L. A. M. Tasca, E. Zucca, Katarina Kovac, T. J. Bschorr, V. Le Brun, Micol Bolzonella, Alvio Renzini, Pascal Oesch, Yingjie Peng, Lucia Pozzetti, Herve Aussel, P. Franzetti, R. Pello, B. Garilli, O. Le Fevre, M. Mignoli, O. Cucciati, S. de la Torre, Christian Maier, Thierry Contini, C. M. Carollo, Simon J. Lilly, Masayuki Tanaka, 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), Kovač, K, Lilly, S.J., Knobel, C., Bschorr, T.J., Peng, Y., Carollo, C.M., Contini, T., Kneib, J.-P., Le Févre, O., Mainieri, V., Renzini, A., Scodeggio, M., Zamorani, G., Bardelli, S., Bolzonella, M., Bongiorno, A., Caputi, K., Cucciati, O., de la Torre, S., de Ravel, L., Franzetti, P., Garilli, B., Iovino, A., Kampczyk, P., Lamareille, F., Le Borgne, J.-F., Le Brun, V., Maier, C., Mignoli, M., Oesch, P., Pello, R., Perez Montero, E., Presotto, V., Silverman, J., Tanaka, M., Tasca, L., Tresse, L., Vergani, D., Zucca, E., Aussel, H., Koekemoer, A.M., Le Floc'h, E., Moresco, M., Pozzetti, L., Astronomy, Kapteyn Astronomical Institute, K., Kovac, S. J., Lilly, C., Knobel, T. J., Bschorr, Y., Peng, 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, P., Oesch, R., Pello, E. P., Montero, Presotto, Valentina, J., Silverman, M., Tanaka, L., Tasca, L., Tresse, D., Vergani, E., Zucca, H., Aussel, A. M., Koekemoer, E., Le Floc'h, M., Moresco, and L., Pozzetti
Subjects: HUBBLE SEQUENCE, HALO MASS, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmology: observation, Hubble sequence, symbols.namesake, galaxies: groups: general, 0103 physical sciences, Satellite galaxy, statistic [galaxies], education, 010303 astronomy & astrophysics, RED SEQUENCE, evolution [galaxies], Astrophysics::Galaxy Astrophysics, galaxies: statistics, STAR-FORMATION HISTORIES, Physics, REDSHIFT SURVEY, education.field_of_study, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], groups: general [galaxies], 010308 nuclear & particles physics, galaxies: evolution, galaxies: star formation, cosmology: observations, Astronomy, Astronomy and Astrophysics, Redshift survey, observations [cosmology], Galaxy, Redshift, Ram pressure, COSMOS FIELD, RAM PRESSURE, Space and Planetary Science, COLOR-DENSITY RELATION, symbols, DIGITAL SKY SURVEY, STELLAR MASS FUNCTION, star formation [galaxies], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We explore the role of environment in the evolution of galaxies over 0.1, Comment: 22 pages, 19 figures, submitted to MNRAS
Published: 2013
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33. Near Infrared Spectropolarimetry from Dome C

Author: Pascal Petit, J.-F. Donati, C. Catala, Andrew Collier Cameron, Catherine Dougados, Jerome Bouvier, Tim J. Harries, R. Pello, Frédéric Paletou, T. Contini, Francois Menard, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), 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 Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Pôle Astronomie du LESIA, and 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)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris
Subjects: Physics, Star formation, Near-infrared spectroscopy, Astrophysics::Instrumentation and Methods for Astrophysics, General Engineering, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Asteroseismology, Exoplanet, law.invention, Telescope, Interstellar medium, Dome (geology), Space and Planetary Science, law, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics
Abstract: We discuss in this paper the new science perspectives that a near infrared (NIR) spectropolarimeter installed on a 4 m class telescope at Dome C in Antartica would offer to the astrophysics community worldwide, in very diverse research fields such as stellar formation, extra solar planets, stellar magnetism and activity, asteroseismology, circumstellar environments, interstellar medium, galactic and extragalactic physics. We also propose an instrument concept with estimated performances, as well as an example 2-step scenario for the construction of this instrument.
Published: 2005

34. 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

35. Improved constraints on the expansion rate of the Universe up to z similar to 1.1 from the spectroscopic evolution of cosmic chronometers

Author: Piero Rosati, J. F. Le Borgne, C. Knobel, Laurence Tresse, James Dunlop, S. Foucaud, K. Kovac, Angela Bongiorno, Michele Moresco, G. Zamorani, Lidia Tasca, Daniela Vergani, Preethi Nair, Marc Kamionkowski, C. Diener, Olga Cucciati, Graziano Coppa, Lucia Pozzetti, S. Bardelli, Michele Cirasuolo, Anton M. Koekemoer, Ross J. McLure, C. López-Sanjuan, Niraj Welikala, Vincenzo Mainieri, C. M. Carollo, Rongmon Bordoloi, Andrea Cimatti, Raul Jimenez, Licia Verde, John D. Silverman, F. Lamareille, Karina Caputi, H. J. Pearce, Masayuki Tanaka, Luke A. Barnes, A. Iovino, Jean-Paul Kneib, S. de la Torre, William G. Hartley, V. Presotto, Christian Maier, L. de Ravel, E. J. Bradshaw, S. Lilly, Yingjie Peng, Robert Chuter, P. Kampczyk, M. Mignoli, H. J. McCracken, Bianca Garilli, Adam Stanford, Marco Scodeggio, Italo Balestra, P. Franzetti, Omar Almaini, Thierry Contini, R. Pello, Enrique Pérez-Montero, V. Le Brun, Raphael Gobat, A. Cappi, Micol Bolzonella, Alvio Renzini, Daniel Stern, Pascal Oesch, O. Le Fèvre, E. Zucca, Dipartimento di Astronomia, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Department of Chemical Engineering, Columbia University, Columbia University [New York], INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), SUPA, Institute for Astronomy, University of Edinburgh, 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), European Southern Observatory (ESO), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Departament d'Astronomia i Meteorologia [Barcelona], Universitat de Barcelona (UB), INAF - Osservatorio Astronomico di Brera (OAB), University of Chicago, Laboratoire Astrophysique de Toulouse-Tarbes (LATT), 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), Institute for Astronomy [Zürich], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), INAF - Osservatorio Astronomico di Padova (OAPD), INAF- Milano, INAF - Osservatorio Astronomico di Trieste (OAT), 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), College of Computing (GATECH), Georgia Institute of Technology [Atlanta], AUTRES, Dipartimento di Fisica, Università degli Studi di Milano-Bicocca = University of Milano-Bicocca (UNIMIB)-Università degli Studi di Milano = University of Milan (UNIMI), 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), Hunan Normal University (HNU), Università degli studi di Trieste = University of Trieste, INAF - Osservatorio Astrofisico di Arcetri (OAA), 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), Space Telescope Science Institute (STSci), 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), Universitat de Barcelona, 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)-NASA, Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), 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), 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), Università degli Studi di Milano-Bicocca [Milano] (UNIMIB)-Università degli Studi di Milano [Milano] (UNIMI), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS)-Université Paris-Saclay, Hunan Normal University, Università degli studi di Trieste, 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)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Università di Bologna [Bologna] (UNIBO), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Institut de Ciènces del Cosmos (ICC), Universitat de Barcelona (UB)-Universitat de Barcelona (UB), Istituto Nazionale di Astrofisica - Osservatorio Astronomico di Brera (INAF), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), Università degli studi di Milano [Milano]-Università di Milano-Bicocca, Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), M. Moresco, A. Cimatti, R. Jimenez, L. Pozzetti, G. Zamorani, M. Bolzonella, J. Dunlop, F. Lamareille, M. Mignoli, H. Pearce, P. Rosati, D. Stern, L. Verde, E. Zucca, C.M. Carollo, T. Contini, J.-P. Kneib, O. Le Fevre, S.J. Lilly, V. Mainieri, A. Renzini, M. Scodeggio, I. Balestra, R. Gobat, R. McLure, 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. Kovac, J.-F. Le Borgne, V. Le Brun, C. Maier, R. Pello', Y. Peng, E. Perez-Montero, V. Presotto, J.D. Silverman, M. Tanaka, L.A.M. Tasca, L. Tresse, D. Vergani, O. Almaini, L. Barne, R. Bordoloi, E. Bradshaw, A. Cappi, R. Chuter, M. Cirasuolo, G. Coppa, C. Diener, S. Foucaud, W. Hartley, M. Kamionkowski, A.M. Koekemoer, C. Lopez-Sanjuan, H.J. McCracken, P. Nair, P. Oesch, A. Stanford, and N. Welikala
Subjects: Astrofísica, Cosmology and Nongalactic Astrophysics (astro-ph.CO), galaxy survey, dark energy experiments, Stellar population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Expanding universe, 01 natural sciences, symbols.namesake, Expansió de l'univers, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, Galaxies, Billion years, Galaxy, Redshift, Galàxies, symbols, Elliptical galaxy, Hubble's law, Quintessence, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present new improved constraints on the Hubble parameter H(z) in the redshift range 0.15 < z < 1.1, obtained from the differential spectroscopic evolution of early-type galaxies as a function of redshift. We extract a large sample of early-type galaxies (\sim11000) from several spectroscopic surveys, spanning almost 8 billion years of cosmic lookback time (0.15 < z < 1.42). We select the most massive, red elliptical galaxies, passively evolving and without signature of ongoing star formation. Those galaxies can be used as standard cosmic chronometers, as firstly proposed by Jimenez & Loeb (2002), whose differential age evolution as a function of cosmic time directly probes H(z). We analyze the 4000 �� break (D4000) as a function of redshift, use stellar population synthesis models to theoretically calibrate the dependence of the differential age evolution on the differential D4000, and estimate the Hubble parameter taking into account both statistical and systematical errors. We provide 8 new measurements of H(z) (see Tab. 4), and determine its change in H(z) to a precision of 5-12% mapping homogeneously the redshift range up to z \sim 1.1; for the first time, we place a constraint on H(z) at z \neq 0 with a precision comparable with the one achieved for the Hubble constant (about 5-6% at z \sim 0.2), and covered a redshift range (0.5 < z < 0.8) which is crucial to distinguish many different quintessence cosmologies. These measurements have been tested to best match a ��CDM model, clearly providing a statistically robust indication that the Universe is undergoing an accelerated expansion. This method shows the potentiality to open a new avenue in constrain a variety of alternative cosmologies, especially when future surveys (e.g. Euclid) will open the possibility to extend it up to z \sim 2., 34 pages, 15 figures, 6 tables, published in JCAP. It is a companion to Moresco et al. (2012b, http://arxiv.org/abs/1201.6658) and Jimenez et al. (2012, http://arxiv.org/abs/1201.3608). The H(z) data can be downloaded at http://www.physics-astronomy.unibo.it/en/research/areas/astrophysics/cosmology-with-cosmic-chronometers
Published: 2012

36. A GROUP-GALAXY CROSS-CORRELATION FUNCTION ANALYSIS IN zCOSMOS

Author: H. J. McCracken, Lucia Pozzetti, Daniela Vergani, L. de Ravel, Rongmon Bordoloi, A. Iovino, E. Perez Montero, Anton M. Koekemoer, Preethi Nair, C. López-Sanjuan, Olga Cucciati, S. de la Torre, Angela Bongiorno, Simon J. Lilly, C. M. Carollo, E. Zucca, S. Bardelli, Karina Caputi, Andrea Cimatti, P. Kampczyk, M. Scodeggio, P. Franzetti, V. Mainieri, M. Bolzonella, V. Presotto, R. Pello, V. Le Brun, Y. Peng, Thierry Contini, Laurence Tresse, Graziano Coppa, J. F. Le Borgne, G. Zamorani, Michele Moresco, Masayuki Tanaka, O. Le Fèvre, Lidia Tasca, Bianca Garilli, M. Mignoli, John D. Silverman, C. Knobel, K. Kovac, Christian Maier, A. Cappi, Jean-Paul Kneib, Alvio Renzini, Niraj Welikala, F. Lamareille, Luke A. Barnes, AUTRES, 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), 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), Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), Istituto Nazionale di Astrofisica (INAF), Hunan Normal University (HNU), Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Università degli studi di Trieste = University of Trieste, INAF - Osservatorio Astronomico di Trieste (OAT), INAF - Osservatorio Astrofisico di Arcetri (OAA), INAF - Osservatorio Astronomico di Brera (OAB), 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), Dipartimento di Astronomia, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Space Telescope Science Institute (STSci), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Bologna (OABO), Institute for Astronomy [Zürich], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), University of Chicago, European Southern Observatory (ESO), INAF - Osservatorio Astronomico di Padova (OAPD), INAF- Milano, College of Computing (GATECH), Georgia Institute of Technology [Atlanta], Dipartimento di Fisica, Università degli Studi di Milano-Bicocca = University of Milano-Bicocca (UNIMIB)-Università degli Studi di Milano = University of Milan (UNIMI), C. Knobel, S. J. Lilly, 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, 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, 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, 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), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS)-Université Paris-Saclay, Hunan Normal University, 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 Trieste, 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, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), and Università degli Studi di Milano-Bicocca [Milano] (UNIMIB)-Università degli Studi di Milano [Milano] (UNIMI)
Subjects: ANALYTIC MODEL, EXTRAGALACTIC OBJECTS, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Structure formation, Field (physics), FOS: Physical sciences, Astrophysics, STATISTICAL-ANALYSIS, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmology, 010305 fluids & plasmas, galaxies: groups: general, 0103 physical sciences, EQUAL-TO 1, 010303 astronomy & astrophysics, galaxies: statistics, Astrophysics::Galaxy Astrophysics, Physics, large-scale structure of universe, REDSHIFT SURVEY, MASS FUNCTION, COSMIC cancer database, Cross-correlation, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Group (mathematics), Astronomy and Astrophysics, GROUP CATALOG, Redshift, Galaxy, COSMOS FIELD, BIAS, Space and Planetary Science, galaxies: clusters: general, DARK-MATTER HALOES, cosmology: observations, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a group-galaxy cross-correlation analysis using a group catalog produced from the 16,500 spectra from the optical zCOSMOS galaxy survey. Our aim is to perform a consistency test in the redshift range 0.2 < z < 0.8 between the clustering strength of the groups and mass estimates that are based on the richness of the groups. We measure the linear bias of the groups by means of a group-galaxy cross-correlation analysis and convert it into mass using the bias-mass relation for a given cosmology, checking the systematic errors using realistic group and galaxy mock catalogs. The measured bias for the zCOSMOS groups increases with group richness as expected by the theory of cosmic structure formation and yields masses that are reasonably consistent with the masses estimated from the richness directly, considering the scatter that is obtained from the 24 mock catalogs. An exception are the richest groups at high redshift (estimated to be more massive than 10^13.5 M_sun), for which the measured bias is significantly larger than for any of the 24 mock catalogs (corresponding to a 3-sigma effect), which is attributed to the extremely large structure that is present in the COSMOS field at z ~ 0.7. Our results are in general agreement with previous studies that reported unusually strong clustering in the COSMOS field., 13 pages, 9 figures, published in ApJ
Published: 2012

37. Spectroscopy of clusters in the ESO Distant Cluster Survey (EDisCS)

Author: Alfonso Aragón-Salamanca, Bo Milvang-Jensen, R. Pello, C. Halliday, Luc Simard, Bianca M. Poggianti, G. De Lucia, Roberto P. Saglia, G. Rudnick, Simon D. M. White, P. Jablonka, S. Poirier, Julianne J. Dalcanton, D. Clowe, Dennis Zaritsky, INAF-Osservatorio Astronomico di Padova, Max-Planck-Institut für Extraterrestriche Physik (MPE), 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), School of Physics and Astronomy, University of Nottingham, Max-Planck-Institut für Astrophysik (MPA), 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), National Research Council of Canada (NRC), Rheinische Friedrich-Wilhelms-Universität Bonn, Department of Astronomy [Seattle], University of Washington [Seattle], and Steward Observatory, University of Arizona
Subjects: Physics, Velocity dispersion, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy, Redshift, Space and Planetary Science, Cluster (physics), Galaxy formation and evolution, Substructure, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Spectroscopy, Astrophysics::Galaxy Astrophysics, Data reduction
Abstract: International audience; We present spectroscopic observations of galaxies in 4 clusters at z = 0.7-0.8 and in one cluster at z ˜ 0.5 obtained with the FORS2 spectrograph on the VLT as part of the ESO Distant Cluster Survey (EDisCS), a photometric and spectroscopic survey of 20 intermediate to high redshift clusters. We describe our target selection, mask design, observation and data reduction procedures, using these first 5 clusters to demonstrate how our strategies maximise the number of cluster members for which we obtain spectroscopy. We present catalogues containing positions, I-band magnitudes and spectroscopic redshifts for galaxies in the fields of our 5 clusters. These contain 236 cluster members, with the number of members per cluster ranging from 30 to 67. Our spectroscopic success rate, i.e. the fraction of spectroscopic targets which are cluster members, averages 50% and ranges from 30% to 75%. We use a robust biweight estimator to measure cluster velocity dispersions from our spectroscopic redshift samples. We also make a first assessment of substructure within our clusters. The velocity dispersions range from 400 to 1100 km s-1. Some of the redshift distributions are significantly non-Gaussian and we find evidence for significant substructure in two clusters, one at z ˜ 0.79 and the other at z ˜ 0.54. Both have velocity dispersions exceeding 1000 km s-1 but are clearly not fully virialised; their velocity dispersions may thus be a poor indicator of their masses. The properties of these first 5 EDisCS clusters span a wide range in redshift, velocity dispersion, richness and substructure, but are representative of the sample as a whole. Spectroscopy for the full dataset will allow a comprehensive study of galaxy evolution as a function of cluster environment and redshift.
Published: 2004

38. ISAAC/VLT observations of a lensed galaxy atz= 10.0

Author: J. F. Le Borgne, Johan Richard, Daniel Schaerer, Jean-Paul Kneib, R. Pello, 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 Astrophysique de Toulouse-Tarbes (LATT), 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 national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-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), and Université Fédérale Toulouse Midi-Pyrénées
Subjects: [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], galaxies: active, Strong gravitational lensing, FOS: Physical sciences, galaxies: starburst, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, active -infrared, 01 natural sciences, infrared: galaxies, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Optical imaging, galaxies: high-redshift, galaxies, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Emission spectrum, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Photometric redshift, high-redshift -galaxies, Physics, 010308 nuclear & particles physics, Astrophysics (astro-ph), Astronomy and Astrophysics, Redshift, Galaxy, evolution -galaxies, Gravitational lens, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution, starburst -galaxies
Abstract: We report the first likely spectroscopic confirmation of a z 10.0 galaxy from our ongoing search for distant galaxies with ISAAC/VLT. Galaxy candidates at z >~ 7 are selected from ultra-deep JHKs images in the core of gravitational lensing clusters for which deep optical imaging is also available, including HST data. The object reported here, found behind Abell 1835, exhibits a faint emission line detected in the J band, leading to z=10.0 when identified as Ly-a, in excellent agreement with the photometric redshift determination. Redshifts z < 7 are very unlikely for various reasons we discuss. The object is located on the critical lines corresponding to z=9 to 11. The magnification factor ��ranges from 25 to 100. For this object we estimate SFR(Ly-a) (0.8-2.2) Msun/yr and SFR(UV) (47-75) Msun/yr, both uncorrected for lensing. The steep UV slope indicates a young object with negligible dust extinction. SED fits with young low-metallicity stellar population models yield (adopting mu=25) a lensing corrected stellar mass of M*~8.e+6 Msun, and luminosities of 2.e+10 Lsun, corresponding to a dark matter halo of a mass of typically M_tot>~ 5.e+8 Msun. In general our observations show that under excellent conditions and using strong gravitational lensing direct observations of galaxies close to the ``dark ages'' are feasible with ground-based 8-10m class telescopes., To be published in A&A, Vol. 416, p. L35. Press release information, additional figures and information available at http://obswww.unige.ch/sfr and http://webast.ast.obs-mip.fr/galaxies
Published: 2004

39. Physical properties of two low-luminosity $\mathsf{{\vec z} \sim 1.9}$ galaxies behind the lensing cluster AC 114

Author: Jean-Paul Kneib, J. F. Le Borgne, Chris Lidman, Thierry Contini, R. Pello, and M. Lemoine-Busserolle
Subjects: Physics, Star formation, Extinction (astronomy), Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Radius, Astrophysics, Galaxy, Virial theorem, Luminosity, Gravitation, Space and Planetary Science, Astrophysics::Galaxy Astrophysics, Line (formation)
Abstract: We present VLT/ISAAC near-infrared spectroscopy of two gravitationally-lensed z ~ 1.9 galaxies, A2 and S2, located behind the cluster AC 114. Thanks to large magnification factors, we have been successful in detecting rest-frame optical emission lines in star-forming galaxies 1 to 2 magnitudes fainter than in previous studies of Lyman break galaxies (LBGs) at z ~ 3. From the Ha luminosity, we estimate star formation rates (SFRs) which are 7 to 15 times higher than those inferred from the UV continuum flux at 1500 ang without dust extinction correction. The behavior of S2 and A2 in terms of O/H and N/O abundance ratios are very different, and they are also different from typical LBGs at z ~ 3. S2 is a low-metallicity object (Z ~ 0.03 Zsun) with a low N/O ratio, similar to those derived in the most metal-poor nearby HII galaxies. In contrast, A2 is a high-metallicity galaxy (Z ~ 1.3 Zsun) with a high N/O abundance ratio, similar to those derived in the most metal-rich starburst nucleus galaxies. The virial masses, derived from emission-line widths, are 0.5 and 2.4 x 10^10 Msun, for S2 and A2 respectively. Thanks to the gravitational amplification, the line profiles of S2 are spatially resolved, leading to a velocity gradient of +- 240 km/s, which yields a dynamical mass of ~ 1.3 x 10^10 Msun within the inner 1 kpc radius. Combining these new data with the sample of LBGs at z ~ 3, we conclude that these three galaxies exhibit different physical properties in terms of SFRs, abundance and mass-to-light ratios, and reddening. High-redshift galaxies of different luminosities could thus have quite different star formation histories (abridged version).
Published: 2003

40. Infrared properties of the SDSS-maxBCG galaxy clusters

Author: Etienne Pointecouteau, M. Giard, L. A. Montier, R. Pello, Mauro Roncarelli, M. Roncarelli, E. Pointecouteau, M. Giard, L. Montier, and R. Pello
Subjects: Luminous infrared galaxy, Physics, education.field_of_study, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Population, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Stellar classification, Galaxy, Redshift, Luminosity, infrared: galaxies, large scale structure of Universe, Space and Planetary Science, galaxies: clusters: general, Intracluster medium, Astrophysics::Solar and Stellar Astrophysics, intergalactic medium, Astrophysics::Earth and Planetary Astrophysics, education, Galaxy cluster, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The physics of galaxy clusters has proven to be influenced by several processes connected with their galactic component which pollutes the ICM with metals, stars and dust. However, it is not clear whether the presence of diffuse dust can play a role in clusters physics since a characterisation of the IR properties of galaxy clusters is yet to be completely achieved. We focus on the recent work of Giard et al. (2008) who performed a stacking analysis of the IRAS data in the direction of several thousands of galaxy clusters, providing a statistical characterisation of their IR luminosity and redshift evolution. We model the IR properties of the galactic population of the SDSS-maxBCG clusters (0.1, Comment: 12 pages, 6 figures, 2 tables. Accepted for publication in A&A
Published: 2010

41. Summary of comparison of realizations of the ITS-90 over the range 83.8058 K to 933.473 K: CCT key comparison CCT-K3

Author: S. Duris, Gregory F. Strouse, Bernd Fellmuth, B. Thiele-Krivoj, J. Gray, A. I. Pokhodun, R. L. Rusby, A G Steele, A. G. Ivanova, G. Sutton, D. R. White, Dieter Heyer, D I Head, Y. Hermier, Y. Qu, W. F. Guthrie, B. W. Mangum, E. Tegeler, N. P. Moiseeva, J. V. Nicholas, Y. Duan, Yong-Doo Kim, J. Connolly, T. D. Dransfield, K. Nara, K. H. Kang, J. F. Dubbeldam, U. Noatsch, E. Renaot, R. Pello, M. J. de Groot, P. Marcarino, K. S. Gam, G. Bonnier, Kenneth D. Hill, and Michael Stock
Subjects: International Temperature Scale of 1990, General Engineering, Key (cryptography), Range (statistics), Statistical physics, Fixed point, Algorithm, Mathematics
Abstract: This is a summary of the Consultative Committee for Thermometry (CCT) Key Comparison CCT-K3, i.e. the comparison of realizations of the fixed points of the International Temperature Scale of 1990 (ITS-90) over the range 83.8058 K to 933.473 K. The differences in the realizations of the various fixed points in this range of the ITS-90 and the uncertainties of those differences are given for the fifteen standards laboratories participating in the comparison.
Published: 2002

42. Weak lensing analysis of MS 1008–1224 with the VLT

Author: Bernard Fort, M. Dantel-Fort, L. van Waerbeke, Yannick Mellier, R. Pello, and R. Athreya
Subjects: Physics, Mass distribution, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Type-cD galaxy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy, Redshift, Gravitational lens, Space and Planetary Science, Cluster (physics), Astrophysics::Galaxy Astrophysics, Galaxy cluster, Weak gravitational lensing
Abstract: We present a gravitational lensing analysis of the cluster of galaxies MS 1008-1224 (z=0.30), based on very deep observations obtained using the VLT with FORS and ISAAC during the science verification phase. We reconstructed the projected mass distribution from B,V,R,I bands using two different methods independently. The mass maps are remarkably similar, which confirm that the PSF correction worked well. The ISAAC and FORS data were combined to measure the photometric redshifts and constrain the redshift distribution of the lensed sources. The total mass inferred from weak shear is 2.3 10^{14} h^{-1} Mo on large scales, in agreement with the X-ray mass. The measured mass profile is well fit by both Navarro, Frenk and White and isothermal sphere with core radius models although the NFW is slightly better. In the inner regions, the lensing mass is about 2 times higher than the X-ray mass, which supports the view that complex physical processes in the innermost parts of clusters are responsible for the X-ray/lensing mass discrepancy. The central part of the cluster is composed of two mass peaks whose the center of mass is 15 arcsecond north of the cD galaxy. This provides an explanation for the 15 arcsecond offset between the cD and the center of the X-ray map reported elsewhere. The optical, X-ray and the mass distributions show that MS 1008-1224 is composed of many subsystems which are probably undergoing a merger. MS 1008-1224 shows a remarkable case of cluster-cluster lensing. The photometric redshifts show an excess of galaxies located 30 arcseconds south-west of the cD galaxy at a redshift of about 0.9 which is lensed by MS 1008-1224. These results show the importance of getting BVRIJK images silmultenously. The VLT is a unique tool to provide such datasets., 22 pages, submitted to A&A, paper with `big' figures available at ftp://ftp.cita.utoronto.ca/pub/waerbeke/ms1008paper/
Published: 2002

43. The MUSEHubbleUltra Deep Field Survey

Author: C. Marcella Carollo, Wolfram Kollatschny, Leindert Boogaard, Roland Bacon, Anne Verhamme, Hanae Inami, Stephane Charlot, Joop Schaye, Michael V. Maseda, N. Bouché, Thierry Contini, R. Pello, Lutz Wisotzki, Johan Richard, Jacopo Chevallard, Jarle Brinchmann, Raffaella Anna Marino, 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), 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), 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), 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), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Université Fédérale Toulouse Midi-Pyrénées-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 ), Institut de recherche en astrophysique et planétologie ( IRAP ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Institut d'Astrophysique de Paris ( IAP ), and Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS )
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Cosmology, Photometry (optics), Integral field spectrograph, galaxies: high-redshift, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Photometric redshift, Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Hubble Ultra-Deep Field, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, techniques: imaging spectroscopy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), cosmology: observations, Intergalactic travel, Astrophysics::Earth and Planetary Astrophysics, galaxies: distances and redshifts, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We tested the performance of photometric redshifts for galaxies in the Hubble Ultra Deep field down to 30th magnitude. We compared photometric redshift estimates from three spectral fitting codes from the literature (EAZY, BPZ and BEAGLE) to high quality redshifts for 1227 galaxies from the MUSE integral field spectrograph. All these codes can return photometric redshifts with bias |Dzn|=|z-z_phot|/(1+z)3 they are systematically biased high by up to Dzn = 0.05, an offset that can in part be explained by adjusting the amount of intergalactic absorption applied. In agreement with previous studies we find little difference in the performance of the different codes, but in contrast to those we find that adding extensive ground-based and IRAC photometry actually can worsen photo-z performance for faint galaxies. We find an outlier fraction, defined through |Dzn|>0.15, of 8% for BPZ and 10% for EAZY and BEAGLE, and show explicitly that this is a strong function of magnitude. While this outlier fraction is high relative to numbers presented in the literature for brighter galaxies, they are very comparable to literature results when the depth of the data is taken into account. Finally, we demonstrate that while a redshift might be of high confidence, the association of a spectrum to the photometric object can be very uncertain and lead to a contamination of a few percent in spectroscopic training samples that do not show up as catastrophic outliers, a problem that must be tackled in order to have sufficiently accurate photometric redshifts for future cosmological surveys., Comment: 24 pages and 25 figures, accepted for A&A
Published: 2017

44. The spatial clustering of X-ray selected AGN in the XMM-COSMOS field

Author: E. Zucca, Andrea Comastri, C. Knobel, O. Le Fèvre, S. de la Torre, N. Z. Scoville, Francesca Civano, Fabrizio Fiore, Alexie Leauthaud, J. F. Le Borgne, Roberto Gilli, Chris Impey, L. de Ravel, M. Mignoli, Alessandro Cimatti, F. Lamareille, M. Bolzonella, Roberto Scaramella, Takamitsu Miyaji, G. Zamorani, Günther Hasinger, J. Walcher, Lidia Tasca, M. Fumana, Jean-Paul Kneib, P. Memeo, V. Le Brun, D. Maccagni, Angela Bongiorno, K. Kovac, S. Bardelli, Christian Maier, M. Scodeggio, Daniela Vergani, Nico Cappelluti, P. Franzetti, Christian Marinoni, H. J. McCracken, D. Bottini, A. Iovino, P. Kampczyk, E. Perez Montero, Olga Cucciati, Laurence Tresse, R. Pello, Jonathan R. Trump, Y. Peng, Luigi Guzzo, E. Ricciardelli, Emanuele Daddi, Cristiano Porciani, Cristian Vignali, Thierry Contini, Mara Salvato, Masayuki Tanaka, Alexis Finoguenov, Graziano Coppa, Paolo Cassata, Lucia Pozzetti, John D. Silverman, Vincenzo Mainieri, Peter Capak, C. M. Carollo, Marcella Brusa, Bianca Garilli, B. Meneux, Simon J. Lilly, Karina Caputi, Alvio Renzini, Pascal Oesch, A. Cappi, U. Abbas, Yoshiaki Taniguchi, Astronomy, California Institute of Technology (CALTECH), Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Laboratoire d'Astrophysique de Marseille (LAM), 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 Physique Théorique - UMR 6207 (CPT), Centre National de la Recherche Scientifique (CNRS)-Université de Toulon (UTLN)-Université de Provence - Aix-Marseille 1-Université de la Méditerranée - Aix-Marseille 2, Centre de Physique Théorique - UMR 7332 (CPT), Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université de la Méditerranée - Aix-Marseille 2-Université de Provence - Aix-Marseille 1-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), R. Gilli, G. Zamorani, T. Miyaji, J. Silverman, M. Brusa, V. Mainieri, N. Cappelluti, E. Daddi, C. Porciani, L. Pozzetti, F. Civano, A. Comastri, A. Finoguenov, F. Fiore, M. Salvato, C. Vignali, G. Hasinger, S. Lilly, C. Impey, J. Trump, P. Capak, H. McCracken, N. Scoville, Y. Taniguchi, C.M. Carollo, T. Contini, J.-P. Kneib, O. LeFevre, A. Renzini, M. Scodeggio, S. Bardelli, M. Bolzonella, A. Bongiorno, K. Caputi, A. Cimatti, G. Coppa, O. Cucciati, S. de la Torre, L. de Ravel, P. Franzetti, B. Garilli, A. Iovino, P. Kampczyk, C. Knobel, K. Kovac, F. Lamareille, J.-F. Le Borgne, V. Le Brun, C. Maier, M. Mignoli, R. Pello', Y. Peng, E. Perez Montero, E. Ricciardelli, M. Tanaka, L. Tasca, L. Tresse, D. Vergani, E. Zucca, U. Abba, D. Bottini, A. Cappi, P. Cassata, M. Fumana, L. Guzzo, A. Leauthaud, D. Maccagni, C. Marinoni, P. Memeo, B. Meneux, P. Oesch, R. Scaramella, and J. Walcher
Subjects: QSOS, ACTIVE GALACTIC NUCLEI, Stellar mass, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, 2-POINT CORRELATION-FUNCTION, Large-scale structure of universe, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Power law, Luminosity, SUPERMASSIVE BLACK-HOLES, GALAXY REDSHIFT SURVEY, 0103 physical sciences, STAR-FORMING GALAXIES, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, Physics, EVOLUTION SURVEY COSMOS, galaxies: active – cosmology: large-scale structure of Universe – cosmology: observations – X-rays: galaxies, 010308 nuclear & particles physics, Cosmology, Cosmology: observations, Galaxies: active, X-rays: galaxies, Astronomy and Astrophysics, Space and Planetary Science, POINT-SOURCE CATALOGS, cosmology: large-scale structure of Universe, Universe, Galaxy, Redshift, Correlation function (statistical mechanics), LUMINOSITY FUNCTION, cosmology: observations, DIGITAL SKY SURVEY, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], ANGULAR-CORRELATION
Abstract: We study the spatial clustering of 538 X-ray selected AGN in the 2 deg^2 XMM-COSMOS field that are spectroscopically identified to I_{AB} 3 x 10^{10} M_sun) at the same redshift. This suggests that AGN at z~1 are preferentially hosted by massive galaxies, as observed both in the local and in the distant (z~2) Universe. (shortened), Comment: 16 pages, 11 figures; accepted for publication in A&A. Language edited version
Published: 2009

45. The zCOSMOS redshift survey : evolution of the light in bulges and discs since z ~ 0.8

Author: Luis C. Ho, O. Le Fevre, H. J. McCracken, P. Franzetti, Anton M. Koekemoer, R. Pello, E. Zucca, A. Cappi, A. Cattaneo, Niraj Welikala, A. Iovino, K. Kovavc, Alvio Renzini, J. F. Le Borgne, R. M. Rich, M. Mignoli, B. Garilli, T. Contini, Yoshiaki Taniguchi, Graziano Coppa, Jean-Paul Kneib, Masaomi Tanaka, C. Lopez-Sanjuan, E. Perez Montero, P. Kampczyk, Vincenzo Mainieri, Andrea Cimatti, F. Lamareille, Richard Massey, Marco Scodeggio, Angela Bongiorno, Rongmon Bordoloi, Y. Peng, L. Tresse, L. A. M. Tasca, C. Knobel, S. Bardelli, Duncan Farrah, Kartik Sheth, Christian Maier, D. Vergani, Michele Moresco, O. Cucciati, S. de la Torre, K. Caputi, C. M. Carollo, M. Bolzonella, Lucia Pozzetti, G. Zamorani, C. T. Liu, D. B. Sanders, Simon J. Lilly, Luigi Guzzo, V. Le Brun, O. Ilbert, Astronomy, Tasca, L.A.M., Tresse, L., Le Fèvre, O., Ilbert, O., Lilly, S.J., Zamorani, G., López-Sanjuan, C., Ho, L.C., Bardelli, S., Cattaneo, A., Cucciati, O., Farrah, D., Iovino, A., Koekemoer, A.M., Liu, C.T., Massey, R., Renzini, A., Taniguchi, Y., Welikala, N., Zucca, E., Carollo, C.M., Contini, T., Kneib, J.-P., Mainieri, V., Scodeggio, M., Bolzonella, M., Bongiorno, A., Caputi, K., De La Torre, S., Franzetti, P., Garilli, B., Guzzo, L., Kampczyk, P., Knobel, C., Kovač, K., Lamareille, F., Le Borgne, J.-F., Le Brun, V., Maier, C., Mignoli, M., Pello, R., Peng, Y., Perez Montero, E., Rich, R.M., Tanaka, M., Vergani, D., Bordoloi, R., Cappi, A., Cimatti, A., Coppa, G., Mccracken, H.J., Moresco, M., Pozzetti, L., Sanders, D., and Sheth, K.
Subjects: Galaxies: fundamental parameter, FORMING GALAXY, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, MASS, fundamental parameters. [Galaxies], LUMINOSITY FUNCTIONS, galaxies: bulges, STAR-FORMATION RATE, Luminosity, ADVANCED CAMERA, bulges [Galaxies], Bulge, distances and redshifts [Galaxies], Galaxies: distances and redshift, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Galaxy Astrophysics, Physics, FORMATION HISTORY, Star formation, Astronomy and Astrophysics, galaxies: fundamental parameters, HUBBLE-SPACE-TELESCOPE, VLT DEEP SURVEY, Astronomy and Astrophysic, Redshift survey, evolution [Galaxies], Astrophysics - Astrophysics of Galaxies, luminosity function [Galaxies], Redshift, Galaxy, Stars, galaxies: luminosity function, Space and Planetary Science, mass function, Astrophysics of Galaxies (astro-ph.GA), galaxies: luminosity function, mass function, Astrophysics::Earth and Planetary Astrophysics, GALAXY FORMATION, galaxies: distances and redshifts, Irregular galaxy, galaxies: evolution, Galaxies: bulge, SURVEY COSMOS
Abstract: We studied the chronology of galactic bulge and disc formation by analysing the relative contributions of these components to the B-band rest-frame luminosity density at different epochs. We present the first estimate of the evolution of the fraction of rest-frame B-band light in galactic bulges and discs since redshift z~0.8. We performed a bulge-to-disc decomposition of HST/ACS images of 3266 galaxies in the zCOSMOS-bright survey with spectroscopic redshifts in the range 0.7 < z < 0.9. We find that the fraction of B-band light in bulges and discs is $(26 \pm 4)%$ and $(74 \pm 4)%$, respectively. When compared with rest-frame B-band measurements of galaxies in the local Universe in the same mass range ($10^{9} M_{\odot}\lessapprox M \lessapprox 10^{11.5} M_{\odot}$), we find that the B-band light in discs decreases by ~30% from z~0.7-0.9 to z~0, while the light from the bulge increases by ~30% over the same period of time. We interpret this evolution as the consequence of star formation and mass assembly processes, as well as morphological transformation, which gradually shift stars formed at half the age of the Universe from star-forming late-type/irregular galaxies toearlier types and ultimately into spheroids., Letter to the Editor, 4 pages, 2 figures, accepted for publication in Astronomy and Astrophysics
Published: 2014

46. Characterizing SL2S galaxy groups using the Einstein radius

Author: Remi A. Cabanac, G. Foëx, Marceau Limousin, Jaime E. Forero-Romero, G. Soucail, R. Pello, A. J. Mejía-Narváez, Roberto Munoz, G. Magris, A. More, John P. Blakeslee, Tomás Verdugo, José G. Fernández-Trincado, Veronica Motta, Departamento de Fisica y Astronomia [Valparaiso], Universidad de Valparaiso [Chile], 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), Institut de recherche en astrophysique et planétologie (IRAP), 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), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Universidad de los Andes [Bogota] (UNIANDES), Instituto de Astrofisica [Santiago], Pontificia Universidad Católica de Chile (UC), 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, 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), Niels Bohr Institute [Copenhagen] (NBI), Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU), Kavli Institute for the Physics and Mathematics of the Universe [Tokyo] (Kavli IPMU), The University of Tokyo Institutes for Advanced Study (UTIAS), The University of Tokyo (UTokyo)-The University of Tokyo (UTokyo), 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), NRC Herzberg Institute of Astrophysics, National Research Council of Canada (NRC), Universidad de Los Andes [Venezuela] (ULA), 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)-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 Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH), 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), Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), Université de Franche-Comté (UFC), and Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Gravitational lensing: strong, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Analytical method, Einstein radius, Luminosity, Velocity dispersion, Hubble space telescope, Galaxy group, Singular isothermal sphere profile, Weak lensing, Dispersions, Weak gravitational lensing, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, Physics, Galaxies: groups: generals, Isothermal spheres, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astronomy and Astrophysics, Galaxies, Redshift, Luminance, Space and Planetary Science, Numerical methods, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Hubble space telescopes, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We analyzed the Einstein radius, $\theta_E$, in our sample of SL2S galaxy groups, and compared it with $R_A$ (the distance from the arcs to the center of the lens), using three different approaches: 1.- the velocity dispersion obtained from weak lensing assuming a Singular Isothermal Sphere profile ($\theta_{E,I}$), 2.- a strong lensing analytical method ($\theta_{E,II}$) combined with a velocity dispersion-concentration relation derived from numerical simulations designed to mimic our group sample, 3.- strong lensing modeling ($\theta_{E,III}$) of eleven groups (with four new models presented in this work) using HST and CFHT images. Finally, $R_A$ was analyzed as a function of redshift $z$ to investigate possible correlations with L, N, and the richness-to-luminosity ratio (N/L). We found a correlation between $\theta_{E}$ and $R_A$, but with large scatter. We estimate $\theta_{E,I}$ = (2.2 $\pm$ 0.9) + (0.7 $\pm$ 0.2)$R_A$, $\theta_{E,II}$ = (0.4 $\pm$ 1.5) + (1.1 $\pm$ 0.4)$R_A$, and $\theta_{E,III}$ = (0.4 $\pm$ 1.5) + (0.9 $\pm$ 0.3)$R_A$ for each method respectively. We found a weak evidence of anti-correlation between $R_A$ and $z$, with Log$R_A$ = (0.58$\pm$0.06) - (0.04$\pm$0.1)$z$, suggesting a possible evolution of the Einstein radius with $z$, as reported previously by other authors. Our results also show that $R_A$ is correlated with L and N (more luminous and richer groups have greater $R_A$), and a possible correlation between $R_A$ and the N/L ratio. Our analysis indicates that $R_A$ is correlated with $\theta_E$ in our sample, making $R_A$ useful to characterize properties like L and N (and possible N/L) in galaxy groups. Additionally, we present evidence suggesting that the Einstein radius evolves with $z$., Comment: Accepted for publication in Astronomy & Astrophysics. Typos corrected
Published: 2014
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47. The fundamental plane of EDisCS galaxies (Corrigendum)

Author: Alfonso Aragón-Salamanca, Luc Simard, G. Rudnick, Douglas Clowe, Vandana Desai, Bianca M. Poggianti, T. Valentinuzzi, R. Pello, Patricia Sanchez-Blazquez, Stefan Noll, Pascale Jablonka, Dennis Zaritsky, C. Halliday, G. De Lucia, Ralf Bender, R. P. Saglia, Bo Milvang-Jensen, and Simon D. M. White
Subjects: Physics, 010308 nuclear & particles physics, Astronomy, Velocity dispersion, Astronomy and Astrophysics, Astrophysics, Disc galaxy, 01 natural sciences, Galaxy, Peculiar galaxy, Space and Planetary Science, 0103 physical sciences, Elliptical galaxy, Galaxy formation and evolution, Disc, Fundamental plane (elliptical galaxies), 010303 astronomy & astrophysics
Abstract: We discovered a mistake in Eqs. (7) and (10) of Saglia et al. (2010, A&A, 524, A6), which propagates to Tables 8 and 9 and Fig. 25. We revise the tables, the figure and the affected statements in the paper. As a result, the reduction in the luminosity evolution due to the effects of the size and velocity dispersion evolution is smaller than claimed in Saglia et al. (2010).
Published: 2016

48. [Untitled]

Author: R. Domínguez, Gustavo Bruzual, R. Pello, and R. Vílchez-Gómex
Subjects: Physics, Astronomy, Velocity dispersion, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy merger, Space and Planetary Science, Galaxy group, Elliptical galaxy, Brightest cluster galaxy, Lenticular galaxy, Astrophysics::Galaxy Astrophysics, Galaxy cluster, Dwarf galaxy
Abstract: We have developed model predictions for the morphological distribution of cluster galaxies as a function of the cluster-centric distance and the local galaxy density, using a semi-analytical code. This code allows us to obtain magnitudes and colours for cluster galaxies at different redshifts, and thus to study in detail the evolution of the colour–magnitude relation of specific distant clusters.
Published: 2001

49. The VIMOS-VLT Deep Survey: Mass and light clustering in the Universe during the last 8 billion years

Author: A. Pollo, U. Abbas, B. Meneux, L. Guzzo, O. . Fevre, A. Cappi, H. J. McCracken, A. Iovino, C. Marinoni, D. Bottini, B. Garilli, V. . Brun, D. Maccagni, J. P. Picat, R. Scaramella, M. Scodeggio, L. Tresse, G. Vettolani, A. Zanichelli, C. Adami, S. Arnouts, S. Bardelli, M. Bolzonella, S. Charlot, P. Ciliegi, T. Contini, S. Foucaud, P. Franzetti, I. Gavignaud, O. Ilbert, B. Marano, A. Mazure, R. Merighi, S. Paltani, R. Pello, L. Pozzetti, M. Radovich, G. Zamorani, E. Zucca, M. Bondi, A. Bongiorno, J. Brinchmann, S. . La, F. Lamareille, Y. Mellier, P. Merluzzi, S. Temporin, D. Vergani, C. J. Walcher, CUCCIATI, OLGA, A. Pollo, U. Abba, B. Meneux, L. Guzzo, O. . Fevre, A. Cappi, H. J. McCracken, A. Iovino, C. Marinoni, D. Bottini, B. Garilli, V. . Brun, D. Maccagni, J. P. Picat, R. Scaramella, M. Scodeggio, L. Tresse, G. Vettolani, A. Zanichelli, C. Adami, S. Arnout, S. Bardelli, M. Bolzonella, S. Charlot, P. Ciliegi, T. Contini, S. Foucaud, P. Franzetti, I. Gavignaud, O. Ilbert, B. Marano, A. Mazure, R. Merighi, S. Paltani, R. Pello, L. Pozzetti, M. Radovich, G. Zamorani, E. Zucca, M. Bondi, A. Bongiorno, J. Brinchmann, O. Cucciati, S. . La, F. Lamareille, Y. Mellier, P. Merluzzi, S. Temporin, D. Vergani, and C. J. Walcher
Subjects: pancake, cosmological constant, Observational cosmology (including Hubble constant, Superclusters, large-scale structure of the Universe (including void, great wall, etc.), Astrophysics::Cosmology and Extragalactic Astrophysics, early Universe, distance scale, Astrophysics::Galaxy Astrophysics
Abstract: Using the first-epoch data from the VIMOS-VLT Deep Survey (VVDS), we investigate the evolution of the projected two-point correlation function of galaxies between z ∼ 1 and the present epoch. For the global galaxy population we do not find strong variations of clustering with redshift. However, dependence of clustering on intrinsic luminosities and stellar masses of galaxies evolves significantly during this period. We observe more close pairs for the most luminous and (less distinctly) most massive objects at z ∼ 1 as compared to what is seen locally, resulting in a non–power-law shape of their correlation function, with an upturn on small scales. This effect can be modeled within the framework of the halo occupation distribution models and leads to the conclusion that at z ∼ 1 we are possibly observing a population of luminous and not very massive satellite galaxies that occupy the most massive dark-matter halos—an effect that is not seen locally.
Published: 2007

50. The VIMOS VLT Deep Survey: Star Formation Since z~5 and Mass Assembly from the VVDS-SWIRE Sample

Author: O. . Fevre, S. Arnouts, L. Tresse, O. Ilbert, C. Lonsdale, M. Polletta, M. Rowan Robinson, G. Zamorani, E. Zucca, S. Bardelli, S. Paltani, L. Pozzetti, D. Bottini, B. Garilli, V. . Brun, D. Maccagni, J. P. Picat, R. Scaramella, M. Scodeggio, D. Shupe, J. Surace, G. Vettolani, A. Zanichelli, C. Adami, M. Bolzonella, A. Cappi, S. Charlot, P. Ciliegi, T. Contini, S. Foucaud, P. Franzetti, I. Gavignaud, L. Guzzo, A. Iovino, H. J. McCracken, B. Marano, C. Marinoni, A. Mazure, B. Meneux, R. Merighi, R. Pello, A. Pollo, M. Radovich, M. Bondi, A. Bongiorno, J. Brinchmann, S. . La, F. Lamareille, Y. Mellier, P. Merluzzi, S. Temporin, D. Vergani, C. J. Walcher, CUCCIATI, OLGA, O. . Fevre, S. Arnout, L. Tresse, O. Ilbert, C. Lonsdale, M. Polletta, M. Rowan-Robinson, G. Zamorani, E. Zucca, S. Bardelli, S. Paltani, L. Pozzetti, D. Bottini, B. Garilli, V. . Brun, D. Maccagni, J. P. Picat, R. Scaramella, M. Scodeggio, D. Shupe, J. Surace, G. Vettolani, A. Zanichelli, C. Adami, M. Bolzonella, A. Cappi, S. Charlot, P. Ciliegi, T. Contini, O. Cucciati, S. Foucaud, P. Franzetti, I. Gavignaud, L. Guzzo, A. Iovino, H. J. McCracken, B. Marano, C. Marinoni, A. Mazure, B. Meneux, R. Merighi, R. Pello, A. Pollo, M. Radovich, M. Bondi, A. Bongiorno, J. Brinchmann, S. . La, F. Lamareille, Y. Mellier, P. Merluzzi, S. Temporin, D. Vergani, and C. J. Walcher
Subjects: GALAXY LUMINOSITY FUNCTION, 1ST EPOCH DATA, EVOLUTION, HISTORY, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: The VIMOS VLT Deep Survey is enabling to trace from one single survey the star formation history in the Universe over 12 billion years of evolution. We find that the star formation rate is strongly linked to the different types of galaxies. While the Luminosity Density of irregular-like galaxies decreased by more than a factor 3.5 from z = 1.2 to z = 0.2, the LD for early-type galaxies increased by a factor 1.7. Star formation happened in several phases, strongly luminosity dependent, with star formation gradually shifting from the first massive galaxies to less massive systems. The peak in SFR at z = 3.5 is identified with the end of the mass assembly of the most luminous galaxies (M-AB(1500 angstrom) < -21). We use the SWIRE Spitzer-IRAC observations of the VVDS-02h field to assemble a flux-limited sample at 3.8 mu m of 1500 galaxies with spectroscopic redshifts and more than 22000 galaxies with photometric redshifts up to z = 2 and build the rest-frame K-band luminosity function and stellar mass density. We find that the global stellar mass density has remained relatively constant since z similar to 1, but the epoch 1 < z < 2 has seen an increase of more than a factor 10 in the stellar mass density of red galaxies selected based on the bimodal distribution of (NUV-r) colors, while in the same period blue galaxies have seen only a modest factor 2 increase. We interpret this as the fast build-up of the red sequence of galaxies, essentially complete by z similar to 1.
Published: 2007

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