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1. Multifrequency JVLA observations of the X-shaped radio galaxy in Abell 3670

Author: Luca Bruno, L. Gregorini, Myriam Gitti, Alessandra Zanichelli, Bruno L., Gitti M., Zanichelli A., Gregorini L., and ITA
Subjects: Physics, Spectral index, 010308 nuclear & particles physics, Radio galaxy, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Galaxies: evolution, Astronomy and Astrophysics, Context (language use), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxies: active, Astrophysics - Astrophysics of Galaxies, 01 natural sciences, Galaxy, Radio continuum: galaxies, Jansky, X-shaped radio galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Radiative transfer, Brightest cluster galaxy, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: Context. X-shaped radio galaxies (XRGs) exhibit a pair of bright primary lobes and a pair of weak secondary lobes (wings), which are oriented with an angle that gives the structure a cross-like shape. Though several theoretical models have been proposed to explain their origin, there is currently not a general consensus on a formation scenario. Aims. We analysed new multifrequency Karl G. Jansky Very Large Array (JVLA) radio data at 1.5, 5.5, 6, and 9 GHz of the candidate XRG in Abell 3670 (A3670) in order to characterise and classify it for the first time and to investigate its origin. Methods. We produced flux, spectral index, and radiative age maps of A3670 by means of the new radio data. We investigated the connection between the radio galaxy and its host, a brightest cluster galaxy (BCG) with two optical nuclei classified as a dumbbell galaxy. Finally we discussed the literature models and compared them to the observed properties of A3670. Results. We classify A3670 as a Fanaroff-Riley I-type XRG and measured a 1.4 GHz radio power of 1.7 x 10^25 W Hz-1. By estimating the radiative age of the various source components, we find that the wings are 20 Myr older than the lobes. We verified that the lobes and wings are aligned with the major and minor axes of the optical galaxy, respectively, and we estimated a black hole mass of 10^9 Msun , which is in agreement with the typical properties of the XRGs. Conclusions. Among the discussed scenarios, the jet-shell interaction model may best reproduce the observed properties of A3670. The gas of a stellar shell is responsible for the deflection of the jets, thus forming the wings. The presence of stellar shells in A3670 is plausible, but it needs further optical observations to be confirmed., Comment: 11 pages, 19 figures grouped in 8, in press on Astronomy&Astrophysics
Published: 2019

2. Observations of the galaxy cluster CIZA J2242.8+5301 with the Sardinia Radio Telescope

Author: F. de Gasperin, Gabriele Giovannini, Andrea Melis, G. Valente, Torsten A. Enßlin, Fabio Gastaldello, Matteo Murgia, Raimondo Concu, F. Loi, Walter Boschin, Chiara Ferrari, Sergio Poppi, L. Gregorini, H. Junklewitz, P. Parma, Luigina Feretti, Emanuela Orrú, Melanie Johnston-Hollitt, Federica Govoni, Ettore Carretti, S. Colafrancesco, Rosita Paladino, Franco Vazza, G. B. Taylor, Tracy E. Clarke, V. Vacca, Richard A. Perley, Marisa Girardi, Joseph Louis LAGRANGE (LAGRANGE), 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), Joseph Louis LAGRANGE ( LAGRANGE ), Université Nice Sophia Antipolis ( UNS ), Université Côte d'Azur ( UCA ) -Université Côte d'Azur ( UCA ) -Observatoire de la Côte d'Azur, Université Côte d'Azur ( UCA ) -Centre National de la Recherche Scientifique ( CNRS ), Loi, F., Murgia, M., Govoni, F., Vacca, V., Feretti, L., Giovannini, g., Carretti, E., Gastaldello, F., Girardi, M., Vazza, F., Concu, R., Melis, A., Paladino, R., Poppi, S., Valente, G., Boschin, W., Clarke, T. E., Colafrancesco, S., Enßlin, T., Ferrari, C., de Gasperin, F., Gregorini, L., Johnston-Hollitt, M., Junklewitz, H., Orrù, E., Parma, P., Perley, R., Taylor, G. B., 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), and 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)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), galaxies: clusters: intracluster medium, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], FOS: Physical sciences, magnetic field, Astrophysics, magnetic fields, 01 natural sciences, Power law, Radio spectrum, Radio telescope, symbols.namesake, 0103 physical sciences, Faraday effect, 010303 astronomy & astrophysics, acceleration of particle, acceleration of particles, Physics, Spectral index, 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Magnetic field, Radio halo, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), symbols, clusters: intracluster medium. [galaxies], magnetic fields – galaxies: clusters: intracluster medium, galaxies: clusters: intracluster medium – magnetic fields – acceleration of parti- cles, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We observed the galaxy cluster CIZA J2242.8+5301 with the Sardinia Radio Telescope to provide new constraints on its spectral properties at high frequency. We conducted observations in three frequency bands centred at 1.4 GHz, 6.6 GHz and 19 GHz, resulting in beam resolutions of 14$^{\prime}$, 2.9$^{\prime}$ and 1$^{\prime}$ respectively. These single-dish data were also combined with archival interferometric observations at 1.4 and 1.7 GHz. From the combined images, we measured a flux density of ${\rm S_{1.4GHz}=(158.3\pm9.6)\,mJy}$ for the central radio halo and ${\rm S_{1.4GHz}=(126\pm8)\,mJy}$ and ${\rm S_{1.4GHz}=(11.7\pm0.7)\,mJy}$ for the northern and the southern relic respectively. After the spectral modelling of the discrete sources, we measured at 6.6 GHz ${\rm S_{6.6GHz}=(17.1\pm1.2)\,mJy}$ and ${\rm S_{6.6GHz}=(0.6\pm0.3)\,mJy}$ for the northern and southern relic respectively. Assuming simple diffusive shock acceleration, we interpret measurements of the northern relic with a continuous injection model represented by a broken power-law. This yields an injection spectral index ${\rm \alpha_{inj}=0.7\pm0.1}$ and a Mach number ${\rm M=3.3\pm0.9}$, consistent with recent X-ray estimates. Unlike other studies of the same object, no significant steepening of the relic radio emission is seen in data up to 8.35 GHz. By fitting the southern relic spectrum with a simple power-law (${\rm S_{\nu}\propto\nu^{-\alpha}}$) we obtained a spectral index ${\rm \alpha\approx1.9}$ corresponding to a Mach number (${\rm M\approx1.8}$) in agreement with X-ray estimates. Finally, we evaluated the rotation measure of the northern relic at 6.6 GHz. These results provide new insights on the magnetic structure of the relic, but further observations are needed to clarify the nature of the observed Faraday rotation., Comment: 20 pages, 11 figures. Accepted by MNRAS
Published: 2017
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3. Sardinia Radio Telescope observations of Abell 194. The intra-cluster magnetic field power spectrum

Author: Franco Vazza, Matteo Murgia, Gianni Bernardi, F. de Gasperin, Melanie Johnston-Hollitt, Raimondo Concu, Federica Govoni, M. Rossetti, Torsten A. Ensslin, Luigina Feretti, Tracy E. Clarke, Richard A. Perley, Rosita Paladino, Chiara Ferrari, M. Brienza, Marisa Girardi, G. B. Taylor, G. Giovannini, F. Gastaldello, H. Junklewitz, V. Vacca, W. Boschin, L. Gregorini, P. Parma, Sergio Poppi, Ettore Carretti, Emanuela Orrú, G. Valente, Annalisa Bonafede, S. Colafrancesco, Dominique Eckert, F. Loi, Andrea Melis, Astronomy, Joseph Louis LAGRANGE (LAGRANGE), 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), Govoni, F., Murgia, M., Vacca, V., Loi, F., Girardi, M., Gastaldello, F., Giovannini, G., Feretti, L., Paladino, R., Carretti, E., Concu, R., Melis, A., Poppi, S., Valente, G., Bernardi, G., Bonafede, A., Boschin, W., Brienza, M., Clarke, T. E., Colafrancesco, S., De Gasperin, F., Eckert, D., Enã lin, T. A., Ferrari, C., Gregorini, L., Johnston-Hollitt, M., Junklewitz, H., Orrã¹, E., Parma, P., Perley, R., Rossetti, M., B Taylor, G., Vazza, F., Joseph Louis LAGRANGE ( LAGRANGE ), Université Nice Sophia Antipolis ( UNS ), Université Côte d'Azur ( UCA ) -Université Côte d'Azur ( UCA ) -Observatoire de la Côte d'Azur, Université Côte d'Azur ( UCA ) -Centre National de la Recherche Scientifique ( CNRS ), 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), Enßlin, T. A., and Orrù, E.
Subjects: VELOCITY DISPERSIONS, Electron density, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Large-scale structure of Universe, Radio galaxy, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], FOS: Physical sciences, REPRESENTATIVE SAMPLE, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, clusters: general [Galaxies], magnetic fields, 01 natural sciences, Power law, Radio telescope, 0103 physical sciences, FARADAY-ROTATION MAPS, 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, galaxies: clusters: individual: Abell 194, VLA OBSERVATIONS, Physics, 010308 nuclear & particles physics, SCALE-INDEPENDENT METHOD, Spectral density, RICH CLUSTERS, Astronomy and Astrophysics, Astronomy and Astrophysic, Polarization (waves), Astrophysics - Astrophysics of Galaxies, clusters: individual: Abell 194 [Galaxies], Magnetic field, Space and Planetary Science, galaxies: clusters: general, Astrophysics of Galaxies (astro-ph.GA), ALL-SKY SURVEY, X-RAY, large-scale structure of Universe, HYDRA-A CLUSTER, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], GALAXY CLUSTERS, Galaxies: clusters: general, Galaxies: clusters: individual: Abell 194, Magnetic fields, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We study the intra-cluster magnetic field in the poor galaxy cluster Abell 194 by complementing radio data, at different frequencies, with data in the optical and X-ray bands. We analyze new total intensity and polarization observations of Abell 194 obtained with the Sardinia Radio Telescope (SRT). We use the SRT data in combination with archival Very Large Array observations to derive both the spectral aging and Rotation Measure (RM) images of the radio galaxies 3C40A and 3C40B embedded in Abell 194. The optical analysis indicates that Abell 194 does not show a major and recent cluster merger, but rather agrees with a scenario of accretion of small groups. Under the minimum energy assumption, the lifetimes of synchrotron electrons in 3C40B measured from the spectral break are found to be 157 Myrs. The break frequency image and the electron density profile inferred from the X-ray emission are used in combination with the RM data to constrain the intra-cluster magnetic field power spectrum. By assuming a Kolmogorov power law power spectrum, we find that the RM data in Abell 194 are well described by a magnetic field with a maximum scale of fluctuations of Lambda_max=64 kpc and a central magnetic field strength of =1.5 microG. Further out, the field decreases with the radius following the gas density to the power of eta=1.1. Comparing Abell 194 with a small sample of galaxy clusters, there is a hint of a trend between central electron densities and magnetic field strengths., Comment: Accepted by Astronomy and Astrophysics, 29 pages, 15 figures. Abstract abridged. A pdf version with high-quality figures can be downloaded from http://erg.oa-cagliari.inaf.it/preprints/a194_paper.pdf
Published: 2017
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4. Highlights from the VIMOS VLT Deep Survey

Author: O. . Fevre, B. Garilli, V. . Brun, D. Maccagni, R. Scaramella, M. Scodeggio, L. Tresse, G. Vettolani, A. Zanichelli, C. Adami, S. Arnouts, S. Bardelli, M. Bolzonella, D. Bottini, A. Cappi, S. Charlot, P. Ciliegi, T. Contini, S. Foucaud, P. Franzetti, I. Gavignaud, L. Guzzo, O. Ilbert, A. Iovino, F. Lamareille, H. J. McCracken, B. Marano, C. Marinoni, A. Mazure, B. Meneux, R. Merighi, S. Paltani, R. Pello, A. Pollo, L. Pozzetti, M. Radovich, D. Vergani, G. Zamorani, E. Zucca, M. Bondi, A. Bongiorno, J. Brinchmann, S. . La, L. . Ravel, L. Gregorini, E. Perez Montero, Y. Mellier, P. Merluzzi, S. Temporin, C. J. Walcher, CUCCIATI, OLGA, O. . Fevre, B. Garilli, V. . Brun, D. Maccagni, R. Scaramella, M. Scodeggio, L. Tresse, G. Vettolani, A. Zanichelli, C. Adami, S. Arnout, S. Bardelli, M. Bolzonella, D. Bottini, A. Cappi, S. Charlot, P. Ciliegi, T. Contini, S. Foucaud, P. Franzetti, I. Gavignaud, L. Guzzo, O. Ilbert, A. Iovino, F. Lamareille, H. J. McCracken, B. Marano, C. Marinoni, A. Mazure, B. Meneux, R. Merighi, S. Paltani, R. Pello, A. Pollo, L. Pozzetti, M. Radovich, D. Vergani, G. Zamorani, E. Zucca, M. Bondi, A. Bongiorno, J. Brinchmann, O. Cucciati, S. . La, L. . Ravel, L. Gregorini, E. Perez-Montero, Y. Mellier, P. Merluzzi, S. Temporin, and C. J. Walcher
Subjects: Galaxy group, cluster, Characteristics and properties of external galaxies and extragalactic objects, and superclusters, large scale structure of the Universe
Abstract: Taking advantage of the efficient VIMOS multi-slit spectrograph on the VLT, we are conducting the VIMOS VLT Deep Survey (VVDS), aimed to trace the evolution of galaxies and large-scale structures over more than 90% of the life of the Universe. The VVDS is made of three magnitude selected surveys: the wide survey at IAB = 22.5, the deep survey at IAB = 24, and the ultra-deep survey at IAB = 24.75. To date, the VVDS has assembled more than 45000 redshifts in the range 0 < z ≤ 5. A number of results have been obtained, including a comprehensive view of the luminosity and stellar mass evolution as a function of galaxy type over 0 < z ≤ 2, a detailed look at the evolution of the clustering of galaxies as a function of type and environment, and a complete census of the actively star-forming galaxy population for 1.5 < z ≤ 5. This paper focuses on current highlights and on-going work from the VVDS.
Published: 2007

5. The VIMOS VLT Deep Survey. The assembly history of the stellar mass in galaxies: from the young to the old universe

Author: O. Ilbert, R. Pello, E. Zucca, Sylvie Foucaud, Thierry Contini, F. Lamareille, C. Adami, I. Gavignaud, Paolo Ciliegi, Paola Merluzzi, P. Franzetti, A. Pollo, Roberto Scaramella, A. Mazure, S. Temporin, M. Radovich, Olga Cucciati, R. Merighi, Laurence Tresse, D. Maccagni, A. Zanichelli, Stéphane Arnouts, Bianca Garilli, V. Le Brun, Stéphane Paltani, A. Iovino, Angela Bongiorno, C. J. Walcher, S. Bardelli, J. P. Picat, Yannick Mellier, D. Bottini, B. Meneux, M. Scodeggio, A. Cappi, Micol Bolzonella, M. Bondi, Bruno Marano, Daniela Vergani, Luigi Guzzo, Christian Marinoni, Stephane Charlot, O. Le Fevre, Lucia Pozzetti, S. de la Torre, Jarle Brinchmann, G. Zamorani, Gianpaolo Vettolani, H. J. McCracken, L. Gregorini, INAF-Osservatorio Astronomico di Bologna (OABO), 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), 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), Istituto di Astrofisica Spaziale e Fisica Cosmica (IASF-Milano), 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, Institute for Astronomy, University of Hawaii, 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), Centro de Astrofisica da Universidade do Porto (CAUP), 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), Dipartimento di Astronomia, Università di Bologna, 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, Astronomical Observatory, Jagiellonia University, INAF-Osservatorio Astronomico di Capodimonte (INAF-OAC), Dipartimento di Fisica, Università di Bologna, AUTRES, Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées (LATT), 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), Observatoire de Paris - Site de Paris (OP), 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), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Services communs OMP (UMS 831), Axe 1 : procédés céramiques, Science des Procédés Céramiques et de Traitements de Surface (SPCTS), Université de Limoges (UNILIM)-Ecole Nationale Supérieure de Céramique Industrielle (ENSCI)-Institut des Procédés Appliqués aux Matériaux (IPAM), Université de Limoges (UNILIM)-Université de Limoges (UNILIM)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)-Université de Limoges (UNILIM)-Ecole Nationale Supérieure de Céramique Industrielle (ENSCI)-Institut des Procédés Appliqués aux Matériaux (IPAM), Université de Limoges (UNILIM)-Université de Limoges (UNILIM)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), European Southern Observatory (ESO), Beaussier, Catherine, 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 Pierre et Marie Curie - Paris 6 (UPMC), École normale supérieure - Paris (ENS Paris), L. Pozzetti, M. Bolzonella, F. Lamareille, G. Zamorani, P. Franzetti, O. Le Fèvre, A. Iovino, S. Temporin, O. Ilbert, S. Arnout, S. Charlot, J. Brinchmann, E. Zucca, L. Tresse, M. Scodeggio, L. Guzzo, D. Bottini, B. Garilli, V. Le Brun, D. Maccagni, J. P. Picat, R. Scaramella, G. Vettolani, A. Zanichelli, C. Adami, S. Bardelli, A. Cappi, P. Ciliegi, T. Contini, S. Foucaud, I. Gavignaud, H. J. McCracken, B. Marano, C. Marinoni, A. Mazure, B. Meneux, R. Merighi, S. Paltani, R. Pellò, A. Pollo, M. Radovich, M. Bondi, A. Bongiorno, O. Cucciati, S. de la Torre, L. Gregorini, Y. Mellier, P. Merluzzi, D. Vergani, and C. J. Walcher
Subjects: Stellar mass, Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph], 01 natural sciences, Photometry (optics), [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, education.field_of_study, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Star formation, Astrophysics (astro-ph), Astronomy and Astrophysics, Galaxy, Redshift, Stars, Space and Planetary Science, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], VIMOS-VLT Deep Survey
Abstract: We present a detailed analysis of the Galaxy Stellar Mass Function of galaxies up to z=2.5 as obtained from the VVDS. We estimate the stellar mass from broad-band photometry using 2 different assumptions on the galaxy star formation history and show that the addition of secondary bursts to a continuous star formation history produces systematically higher (up to 40%) stellar masses. At low redshift (z=0.2) we find a substantial population of low-mass galaxies (10^8 Msun at z=1), and a mild mass-dependent average evolution (`mass-downsizing'). In particular our data are consistent with mild/negligible (6x10^10 Msun). For less massive systems the no-evolution scenario is excluded. A large fraction (>=50%) of massive galaxies have been already assembled and converted most of their gas into stars at z=1, ruling out the `dry mergers' as the major mechanism of their assembly history below z=1. This fraction decreases to 33% at z=2. Low-mass systems have decreased continuously in number and mass density (by a factor up to 4) from the present age to z=2, consistently with a prolonged mass assembly also at z, 20 pages with 12 encapsulated figures. Version accepted by A&A
Published: 2007

6. The VVDS type-1 AGN sample: the faint end of the luminosity function

Author: A. Bongiorno, G. Zamorani, I. Gavignaud, B. Marano, S. Paltani, G. Mathez, P. Møller, J. P. Picat, M. Cirasuolo, F. Lamareille, D. Bottini, B. Garilli, V. Le Brun, O. Le Fèvre, D. Maccagni, R. Scaramella, M. Scodeggio, L. Tresse, G. Vettolani, A. Zanichelli, C. Adami, S. Arnouts, S. Bardelli, M. Bolzonella, A. Cappi, S. Charlot, P. Ciliegi, T. Contini, S. Foucaud, P. Franzetti, L. Guzzo, O. Ilbert, A. Iovino, H. J. McCracken, C. Marinoni, A. Mazure, B. Meneux, R. Merighi, R. Pellò, A. Pollo, L. Pozzetti, M. Radovich, E. Zucca, E. Hatziminaoglou, M. Polletta, M. Bondi, J. Brinchmann, O. Cucciati, S. de la Torre, L. Gregorini, Y. Mellier, P. Merluzzi, S. Temporin, D. Vergani, C. J. Walcher, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), INAF-Osservatorio Astronomico di Bologna (OABO), Astrophysikalisches Institut Potsdam (AIP), INTEGRAL Science Data Centre, 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), European Southern Observatory (ESO), University of Edinburgh, Istituto di Astrofisica Spaziale e Fisica Cosmica (IASF-Milano), 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), IRA-INAF, Bologna, 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, INAF-Osservatorio Astronomico di Brera, Institute for Astronomy, University of Hawaii, 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), Astronomical Observatory, Jagiellonia University, INAF-Osservatorio Astronomico di Capodimonte (INAF-OAC), Center for Astrophysics and Space Sciences, University of California, San Diego, Centro de Astrofisica da Universidade do Porto (CAUP), AUTRES, Services communs OMP (UMS 831), 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 l'Observatoire Midi-Pyrénées (LATT), Observatoire de Paris - Site de Paris (OP), 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), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), École normale supérieure - Paris (ENS Paris), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), 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 Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), A. Bongiorno, G. Zamorani, I. Gavignaud, B. Marano, S. Paltani, G. Mathez, J.P. Picat, M. Cirasuolo, F. Lamareille, D. Bottini, B. Garilli, V. Le Brun, O. Le Fevre, D. Maccagni, R. Scaramella, M. Scodeggio, L. Tresse, G. Vettolani, A. Zanichelli, C. Adami, S. Arnout, S. Bardelli, M. Bolzonella, A. Cappi, S. Charlot, P. Ciliegi, T. Contini, S. Foucaud, P. Franzetti, L. Guzzo, O. Ilbert, A. Iovino, H.J. McCracken, C. Marinon, A. Mazure, B. Meneux, R. Merighi, R. Pello', A. Pollo, L. Pozzetti, M. Radovich, E. Zucca, E. Hatziminaoglou, M. Polletta, M. Bondi, J. Brinchmann, O. Cucciati, S. de la Torre, L. Gregorini, Y. Mellier, P. Merluzzi, S. Temporin, D. Vergani, and C.J. Walcher
Subjects: Physics, Active galactic nucleus, COSMIC cancer database, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Spectral line, Redshift, Luminosity, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Space and Planetary Science, 0103 physical sciences, Magnitude (astronomy), Range (statistics), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Luminosity function (astronomy)
Abstract: In a previous paper (Gavignaud et al. 2006), we presented the type-1 Active Galactic Nuclei (AGN) sample obtained from the first epoch data of the VIMOS-VLT Deep Survey (VVDS). The sample consists of 130 faint, broad-line AGN with redshift up to z=5 and 17.5< I, 13 pages, 10 figures, submitted to A&A
Published: 2007
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7. The molecular environment of the Galactic star forming region G19.61–0.23

Author: L. Gregorini, G. Santangelo, Frederic Schuller, Silvia Leurini, Sergio Molinari, Luca Olmi, C. M. Walmsley, Leonardo Bronfman, Alberto Noriega-Crespo, Karl M. Menten, R. Cesaroni, Sean Carey, Leonardo Testi, Santangelo G., Testi L., Leurini S., Walmsley C. M., Cesaroni R., Bronfman L., Carey S., Gregorini L., Menten K. M., Molinari S., and Noriega-Crespo A., Olmi L., Schuller F.
Subjects: Physics, education.field_of_study, Spiral galaxy, RADIO CONTINUUM, Star formation, Molecular cloud, ISM: STAR: FORMATION, Population, FOS: Physical sciences, Astronomy and Astrophysics, ISM:INDIVIDUAL OBJECT:G19.61-0.23, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galactic plane, Astrophysics - Astrophysics of Galaxies, ISM:MOLECULES, Stars, Star cluster, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, education, Astrophysics::Galaxy Astrophysics, Dwarf galaxy
Abstract: We present single-dish (sub)millimeter observations of gas and dust in the Galactic high-mass star-forming region G19.61-0.23, with the aim of studying the large-scale properties and physical conditions of the molecular gas across the region. The final aim is to compare the large-scale (about 100 pc) properties with the small-scale (about 3 pc) properties and to consider possible implications for extragalactic studies. We have mapped CO isotopologues in the J=1-0 transition using the FCRAO-14m telescope and the J=2-1 transition using the IRAM-30m telescope. We have also used data from the ATLASGAL survey and from the BU-FCRAO Galactic Ring Survey, as well as the Spitzer infrared Galactic plane surveys GLIMPSE and MIPSGAL to characterize the star-formation activity within the molecular clouds. We reveal a population of molecular clumps in the 13CO(1-0) emission. Our analysis of the 13CO suggests that the virial parameter (ratio of kinetic to gravitational energy) varies over an order of magnitude between clumps that are unbound and some that are apparently "unstable". This conclusion is independent of whether they show evidence of ongoing star formation. We find that the majority of ATLASGAL sources have MIPSGAL counterparts with luminosities in the range 10^4 - 5 10^4 Lsun and are presumably forming relatively massive stars. We compare our results with previous extragalactic studies of the nearby spiral galaxies M31 and M33; and the blue compact dwarf galaxy Henize2-10. We find that the main giant molecular cloud surrounding G19.61-0.23 has physical properties typical for Galactic GMCs and which are comparable to the GMCs in M31 and M33. However, the GMC studied here shows smaller surface densities and masses than the clouds identified in Henize2-10 and associated with super star cluster formation., Accepted for publication in Astronomy & Astrophysics
Published: 2010

8. The VIMOS VLT Deep Survey. Evolution of the major merger rate since z ~ 1 from spectroscopically confirmed galaxy pairs

Author: S. Temporin, D. Maccagni, B. Meneux, Paola Merluzzi, O. Cucciati, T. Contini, S. de la Torre, E. Zucca, Stéphane Charlot, Sylvie Foucaud, O. Le Fevre, L. Gregorini, R. Pello, L. Tresse, S. Paltani, Roberto Scaramella, L. de Ravel, Yannick Mellier, Mario Radovich, D. Bottini, R. Merighi, G. Vettolani, A. Pollo, Marco Scodeggio, H. J. McCracken, V. Le Brun, O. Ilbert, S. Bardelli, Alain Mazure, P. Franzetti, Enrique Perez-Montero, Angela Bongiorno, Jarle Brinchmann, A. Zanichelli, A. Iovino, I. Gavignaud, M. Bondi, Paolo Ciliegi, Bruno Marano, Stephane Arnouts, M. Bolzonella, Lucia Pozzetti, A. Cappi, Luigi Guzzo, G. Zamorani, Christian Marinoni, D. Vergani, F. Lamareille, B. Garilli, P. Memeo, C. Adami, 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, Istituto Nazionale di Astrofisica (INAF), INAF - Osservatorio Astronomico di Bologna (OABO), Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Laboratoire 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), Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), 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), Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto, de Ravel L., Le Fèvre O., Tresse L., Bottini D., Garilli B., Le Brun V., Maccagni D., Scaramella R., Scodeggio M., Vettolani G., Zanichelli A., Adami C., Arnouts S., Bardelli S., Bolzonella M., Cappi A., Charlot S., Ciliegi P., Contini T., Foucaud S., Franzetti P., Gavignaud I., Guzzo L., Ilbert O., Iovino A., Lamareille F., McCracken H. J., Marano B., Marinoni C., Mazure A., Meneux B., Merighi R., Paltani S., Pellò R., Pollo A., Pozzetti L., Radovich M., Vergani D., Zamorani G., Zucca E., Bondi M., Bongiorno A., Brinchmann J., Cucciati O., de La Torre S., Gregorini L., Memeo P., Perez-Montero E., Mellier Y., Merluzzi P., Temporin S., Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université de la Méditerranée - Aix-Marseille 2-Université de Provence - Aix-Marseille 1-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), and Universidade do Porto = University of Porto
Subjects: Physics, Stellar mass, 010308 nuclear & particles physics, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Galaxy, Space and Planetary Science, 0103 physical sciences, galaxies: interactions, Astrophysics::Solar and Stellar Astrophysics, galaxies: formation, Astrophysics::Earth and Planetary Astrophysics, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], 10. No inequality, galaxies: evolution, 010303 astronomy & astrophysics, VIMOS-VLT Deep Survey, Astrophysics::Galaxy Astrophysics
Abstract: From the VIMOS VLT Deep Survey we use a sample of 6447 galaxies with I_{AB} < 24 to identify 251 pairs of galaxies, each member with a secure spectroscopic redshift, which are close in both projected separation and in velocity. We find that at z ~ 0.9, 10.9 +/- 3.2 % of galaxies with M_B(z) < -18-Qz are in pairs with separations dr < 20 kpc/h, dv < 500 km/s, and with dM_B < 1.5, significantly larger than 3.76 +/- 1.71 % at z ~ 0.5; we find that the pair fraction evolves as (1+z)^m with m = 2.49 +/- 0.56. For brighter galaxies with M_B(z=0) < -18.77, the pair fraction is higher and its evolution with redshift is somewhat flatter with m=1.88 \pm 0.40, a property also observed for galaxies with increasing stellar masses. Early type, dry mergers, pairs increase their relative fraction from 3 % at z ~ 0.9 to 12 % at z ~ 0.5. We find that the merger rate evolves as N_{mg}=(9.05 +/- 3.76) * 10^{-4}) * (1+z)^{2.43 +/- 0.76}. We find that the merger rate of galaxies with M_B(z) < -18-Qz has significantly evolved since z ~ 1. The merger rate is increasing more rapidly with redshift for galaxies with decreasing luminosities, indicating that the flat evolution found for bright samples is not universal. The merger rate is also strongly dependent on the spectral type of galaxies involved, late type mergers being more frequent in the past, while early type mergers are more frequent today, contributing to the rise in the local density of early type galaxies. About 20 % of the stellar mass in present day galaxies with log(M/M_{sun}) > 9.5 has been accreted through major merging events since z ~ 1, indicating that major mergers have contributed significantly to the growth in stellar mass density of bright galaxies over the last half of the life of the Universe., 22 pages, 19 figures, accepted in A&A
Published: 2009
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9. The VVDS-VLA deep field. IV. Radio-optical properties

Author: Daniela Vergani, P. Parma, Laurence Tresse, Jarle Brinchmann, S. Temporin, Sylvie Foucaud, D. Maccagni, P. Memeo, Agnieszka Pollo, Stéphane Paltani, R. Pello, S. de la Torre, D. Bottini, Angela Bongiorno, Roberto Scaramella, A. Mazure, Bianca Garilli, E. Zucca, B. Meneux, L. Gregorini, F. Lamareille, R. Merighi, Stéphane Arnouts, Giampaolo Vettolani, O. Le Fevre, Paola Merluzzi, H. R. de Ruiter, Ummi Abbas, Lucia Pozzetti, H. J. McCracken, A. Iovino, C. Adami, P. Franzetti, L. de Ravel, Olga Cucciati, A. Zanichelli, Stephane Charlot, Christian Marinoni, Paolo Ciliegi, M. Radovich, Yannick Mellier, Enrique Pérez-Montero, A. Cappi, Micol Bolzonella, Bruno Marano, Luigi Guzzo, M. Bondi, V. Le Brun, S. Bardelli, O. Ilbert, Thierry Contini, I. Gavignaud, G. Zamorani, M. Scodeggio, INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Laboratoire 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'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Bardelli S., Zucca E., Bolzonella M., Ciliegi P., Gregorini L., Zamorani G., Bondi M., Zanichelli A., Tresse L., Vergani D., Gavignaud I., Bongiorno A., Bottini D., Garilli B., Le Brun V., Le Fèvre O., Maccagni D., Scaramella R., Scodeggio M., Vettolani G., Adami C., Arnouts S., Cappi A., Charlot S., Contini T., Foucaud S., Franzetti P., Guzzo L., Ilbert O., Iovino A., Lamareille F., McCracken H. J., Marano B., Marinoni C., Mazure A., Meneux B., Merighi R., Paltani S., Pellò R., Pollo A., Pozzetti L., Radovich M., Abbas U., Brinchmann J., Cucciati O., de La Torre S., de Ravel L., Memeo P., Perez-Montero E., Mellier Y., Merluzzi P., Temporin S., de Ruiter H. R., Parma P., Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), 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 École normale supérieure - Paris (ENS-PSL)
Subjects: Hubble Deep Field, Astrophysics::High Energy Astrophysical Phenomena, Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, GALASSIE: RADIO, Photometry (optics), GALASSIE: SURVEY, 0103 physical sciences, fundamental parameters [galaxies], Astrophysics::Solar and Stellar Astrophysics, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, radio continuum: galaxies, education.field_of_study, 010308 nuclear & particles physics, Star formation, Astrophysics (astro-ph), Astronomy and Astrophysics, galaxies: fundamental parameters, Rest frame, luminosity function, mass function [galaxies], galaxies: general, galaxies [radio continuum], Redshift, Galaxy, galaxies: luminosity function, Space and Planetary Science, mass function, QUIET, GALASSIE: PROPRIETÀ RADIO-OTTICHE, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], general [galaxies]
Abstract: (abridged) We use the 1.4 GHz VIMOS-VLA Deep Survey and the optical VVDS and the CFHT-LS to compare the properties of radio loud galaxies with respect to the whole population of optical galaxies. The availability of multiband photometry and high quality photometric redshifts allows to derive rest frame colors and radio luminosity functions down to a limit of a B rest-frame magnitude of M=-20. Galaxy properties and luminosity functions (LFs) are estimated up to z~1 for radio loud and radio quiet early and late type galaxies. Radio loud late type galaxies are redder than radio quiet objects of the same class and this is an effect related to the presence of more dust in stronger star forming galaxies. Moreover, we estimate optical LFs, stellar masses and star formation rate distributions for radio sources and compare them with those derived for a well defined control sample, finding that the probability for a galaxy to be a radio emitter significantly increases at high values of these parameters. Radio loud early type galaxies show luminosity evolution of their bivariate radio-optical LF, due to an evolution in the radio-optical ratio. The lack of evolution of the mass function of radio loud early type galaxies means that no new AGN are formed at z0.7. This evolution is the direct effect of the strong optical evolution of this class and no significant change with redshift of the radio-optical ratio is required. With the knowledge of the radio-optical ratio and the optical and radio LFs for late type galaxies, we estimated the star formation history of the Universe up to z~1.5, using optical galaxies as tracers of the global radio emission., 17 pages, A&A in press
Published: 2009
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10. Resolving the molecular environment of super star clusters in Henize 2-10

Author: G. Santangelo, Silvia Leurini, Leonardo Testi, David J. Wilner, C. M. Walmsley, L. Gregorini, Leonardo Vanzi, Santangelo G., Testi L., Gregorini L., Leurini S., Vanzi L., Walmsley C.M., and Wilner D.J.
Subjects: Physics, Star formation, Molecular cloud, GALAXIES: STARBURST, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, GALAXIES: INDIVIDUAL: HENIZE 2-10, GALAXIES: DWARF, Submillimeter Array, Astrophysics - Astrophysics of Galaxies, Galaxy, Stars, Star cluster, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Irregular galaxy, Dwarf galaxy
Abstract: The rate of star formation both in the Galaxy and in external galaxies should be related to the physical properties of the molecular clouds from which stars form. This is expected for the starbursts found both in irregular galaxies and in some mergers. The dwarf galaxy Henize 2-10 is particularly interesting in this context as it shows a number of newly formed Super Star Clusters (SSCs) associated with a very rich molecular environment. We present a high angular resolution study of the molecular gas associated with the SSCs with the aim of deriving the physical properties of the parent molecular clouds. The final goal is to test the expectation that the formation of SSCs requires exceptionally dense and massive clouds. We have used the Submillimeter Array with an angular resolution of 1.9 X 1.3 to map the J=2-1 transition of CO in Henize 2-10. Supplementary measurements of HCN(J=1-0), 13CO(J=2-1) and millimeter continuum were obtained with the APEX, IRAM-30m and SEST single dish telescopes. Our single dish observations confirm the association of the newly formed SSCs in Henize 2-10 with dense molecular gas. Our interferometric observations resolve the CO(2-1) emission in several giant molecular clouds. Overall the molecular gas accounts for approximately half of the mass in the central regions of Henize 2-10. Although we find indications that the molecular clouds associated with the formation of SSCs in Henize 2-10 are massive and dense, the tracer we used (CO) and the linear resolution of our observations (60 X 80 pc) are still not adequate to test the expectation that exceptionally dense and massive cores are required for SSCs formation., Comment: 10 pages, 7 figures, 3 tables; Accepted for publication in Astronomy and Astrophysics
Published: 2009

11. The Vimos VLT Deep Survey. Stellar mass segregation and large-scale galaxy environment in the redshift range 0.2 < z < 1.4

Author: E. Zucca, Paolo Ciliegi, C. J. Walcher, V. Le Brun, Bianca Garilli, Ummi Abbas, Laurence Tresse, C. Adami, S. Temporin, M. Radovich, A. Iovino, L. Gregorini, Sylvie Foucaud, Giampaolo Vettolani, D. Maccagni, D. Vergani, Stéphane Paltani, Roberto Scaramella, A. Mazure, D. Bottini, R. Merighi, R. Pello, Angela Bongiorno, L. de Ravel, H. J. McCracken, Luigi Guzzo, S. Bardelli, Yannick Mellier, Lucia Pozzetti, O. Le Fèvre, A. Cappi, P. Franzetti, Olga Cucciati, F. Lamareille, A. Zanichelli, Bruno Marano, M. Bondi, S. Arnouts, Stephane Charlot, Enrique Pérez-Montero, B. Meneux, M. Scodeggio, Thierry Contini, I. Gavignaud, G. Zamorani, Jarle Brinchmann, P. Memeo, Christian Marinoni, S. de la Torre, Agnieszka Pollo, M. Bolzonella, O. Ilbert, Istituto di Astrofisica Spaziale e Fisica Cosmica (IASF-Milano), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), INAF-Osservatorio Astronomico di Brera, Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), INAF-Osservatorio Astronomico di Bologna (OABO), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), INAF-Osservatorio Astrofisico di Torino (INAF-OATo), Centre de Physique Théorique - UMR 7332 (CPT), Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), IRA-INAF, Bologna, Canada-France-Hawaii Telescope Corporation (CFHT), National Research Council of Canada (NRC)-Centre National de la Recherche Scientifique (CNRS)-University of Hawai'i [Honolulu] (UH), 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), Max-Planck-Institut für Astrophysik (MPA), School of Physics and Astronomy, University of Nottingham, Astrophysikalisches Institut Potsdam (AIP), Institute for Astronomy, University of Hawaii, 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), Max-Planck-Institut für Extraterrestriche Physik (MPE), INTEGRAL Science Data Centre, The Andrzej Soltan Institute for Nuclear Studies, INAF-Osservatorio Astronomico di Capodimonte (INAF-OAC), Centro de Astrofisica da Universidade do Porto (CAUP), Institut für Astro- und Teilchenphysik, Leopold-Franzens-Universität Innsbruck, Scodeggio M., Vergani D., Cucciati O., Iovino A., Franzetti P., Garilli B., Lamareille F., Bolzonella M., Pozzetti L., Abbas U., Marinoni C., Contini T., Bottini D., Le Brun V., Le Fèvre O., Maccagni D., Scaramella R., Tresse L., Vettolani G., Zanichelli A., Adami C., Arnouts S., Bardelli S., Cappi A., Charlot S., Ciliegi P., Foucaud S., Gavignaud I., Guzzo L., Ilbert O., McCracken H. J., Marano B., Mazure A., Meneux B., Merighi R., Paltani S., Pellò R., Pollo A., Radovich M., Zamorani G., Zucca E., Bondi M., Bongiorno A., Brinchmann J., de La Torre S., de Ravel L., Gregorini L., Memeo P., Perez-Montero E., Mellier Y., Temporin S., and Walcher C. J.
Subjects: Physics, education.field_of_study, Stellar mass, Population, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Redshift, Galaxy, COSMOLOGIA: GALASSIE, Dark matter halo, Space and Planetary Science, Range (statistics), Galaxy formation and evolution, Astrophysics::Earth and Planetary Astrophysics, COSMOLOGIA: REDSHIFT SURVEYS, Halo, education, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Hierarchical models of galaxy formation predict that the properties of a dark matter halo depend on the large-scale environment surrounding the halo. As a result of this correlation, we expect massive haloes to be present in larger number in overdense regions than in underdense ones. Given that a correlation exists between a galaxy stellar mass and the hosting dark matter halo mass, the segregation in dark matter halo mass should then result in a segregation in the distribution of stellar mass in the galaxy population. In this work we study the distribution of galaxy stellar mass and rest-frame optical color as a function of the large-scale galaxy distribution using the VLT VIMOS Deep Survey sample, in order to verify the presence of segregation in the properties of the galaxy population. We use the VVDS redshift measurements and multi-band photometric data to derive estimates of the stellar mass, rest-frame optical color, and of the large-scale galaxy density, on a scale of approximately 8 Mpc, for a sample of 5619 galaxies in the redshift range 0.20.7. However, when we consider only galaxies in narrow bins of stellar mass, in order to exclude the effects of the stellar mass segregation on the galaxy properties, we do not observe any more any significant color segregation., Comment: 7 pages, 5 figures; accepted for publication in Astronomy and Astrophysics
Published: 2009
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12. Eddington ratios of faint AGN at intermediate redshift: evidence for a population of half-starved black holes

Author: Roberto Scaramella, A. Mazure, Christian Marinoni, Vincenzo Ripepi, R. Merighi, Yannick Mellier, M. Radovich, Stéphane Arnouts, Laurence Tresse, G. Zamorani, B. Husemann, Angela Bongiorno, V. Le Brun, Paolo Ciliegi, P. Franzetti, E. Zucca, D. Rizzo, Thierry Contini, Paola Merluzzi, A. Cappi, A. Zanichelli, Daniela Vergani, B. Meneux, Sylvie Foucaud, I. Gavignaud, Lucia Pozzetti, Bruno Marano, M. Scodeggio, Lutz Wisotzki, Magda Arnaboldi, Giampaolo Vettolani, Luigi Guzzo, Bianca Garilli, A. Pollo, Palle Møller, M. Bolzonella, R. Pello, M. Bondi, M. Schramm, Stephane Charlot, D. Bottini, F. Lamareille, A. Iovino, S. Bardelli, O. Cucciati, O. Ilbert, G. Busarello, S. de la Torre, D. Maccagni, Stéphane Paltani, O. Le Fevre, H. J. McCracken, L. Gregorini, C. Adami, European Southern Observatory (ESO), 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), 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), Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, 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), 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), INAF- Milano, Istituto Nazionale di Astrofisica (INAF), 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 Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-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), Gavignaud I., Wisotzki L., Bongiorno A., Paltani S., Zamorani G., Møller P., Le Brun V., Husemann B., Lamareille F., Schramm M., Le Fèvre O., Bottini D., Garilli B., Maccagni D., Scaramella R., Scodeggio M., Tresse L., Vettolani G., Zanichelli A., Adami C., Arnaboldi M., Arnouts S., Bardelli S., Bolzonella M., Cappi A., Charlot S., Ciliegi P., Contini T., Foucaud S., Franzetti P., Guzzo L., Ilbert O., Iovino A., McCracken H. J., Marano B., Marinoni C., Mazure A., Meneux B., Merighi R., Pellò R., Pollo A., Pozzetti L., Radovich M., Zucca E., Bondi M., Busarello G., Cucciati O., de La Torre S., Gregorini L., Mellier Y., Merluzzi P., Ripepi V., Rizzo D., and Vergani D.
Subjects: ACTIVE GALACTIC NUCLEI, Active galactic nucleus, Astrophysique (Planète et Univers), Astrophysics::High Energy Astrophysical Phenomena, Population, galaxies: active, enquête, EXTRAGALACTIC SURVEYS, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Virial theorem, symbols.namesake, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, BLACK HOLES, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Line (formation), Physics, Electronic appendix, education.field_of_study, 010308 nuclear & particles physics, galaxie, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Redshift, galaxies: Seyfert, Space and Planetary Science, COSMOLOGY, Eddington luminosity, symbols, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], catalogue, galaxies: nuclei, VIMOS-VLT Deep Survey, catalogs, surveys, quasars:general
Abstract: We use one of the deepest spectroscopic samples of broad line active galactic nuclei (AGN) currently available, extracted from the VIMOS VLT Deep Survey (VVDS), to compute MgII and CIV virial masses estimate of 120 super-massive black holes in the redshift range 1.0, Comment: accepted for publication in Astronomy & Astrophysics
Published: 2008
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13. The VIMOS VLT Deep Survey. Testing the gravitational instability paradigm at z ~ 1

Author: C. Marinoni, L. Guzzo, A. Cappi, O. Le Fèvre, A. Mazure, B. Meneux, A. Pollo, A. Iovino, H. J. McCracken, R. Scaramella, S. de la Torre, J. M. Virey, D. Bottini, B. Garilli, V. Le Brun, D. Maccagni, J. P. Picat, 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, F. Lamareille, B. Marano, G. Mathez, R. Merighi, S. Paltani, R. Pellò, L. Pozzetti, M. Radovich, D. Vergani, G. Zamorani, E. Zucca, U. Abbas, M. Bondi, A. Bongiorno, J. Brinchmann, A. Buzzi, O. Cucciati, L. de Ravel, L. Gregorini, Y. Mellier, P. Merluzzi, E. Perez-Montero, P. Taxil, S. Temporin, C. J. Walcher, 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), INAF- Milano, Istituto Nazionale di Astrofisica (INAF), Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), INAF - Osservatorio Astronomico di Brera (OAB), Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Laboratoire 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), European Southern Observatory (ESO), INAF - Osservatorio Astronomico di Capodimonte (OAC), Istituto di Radioastronomia [Bologna] (IRA), Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto, Bernardo, Elizabeth, AUTRES, Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Université de la Méditerranée - Aix-Marseille 2-Université de Provence - Aix-Marseille 1-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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, Marinoni C., Guzzo L., Cappi A., Le Fèvre O., Mazure A., Meneux B., Pollo A., Iovino A., McCracken H. J., Scaramella R., de La Torre S., Virey J. M., Bottini D., Garilli B., Le Brun V., Maccagni D., Picat J. P., Scodeggio M., Tresse L., Vettolani G., Zanichelli A., Adami C., Arnouts S., Bardelli S., Bolzonella M., Charlot S., Ciliegi P., Contini T., Foucaud S., Franzetti P., Gavignaud I., Ilbert O., Lamareille F., Marano B., Mathez G., Merighi R., Paltani S., Pellò R., Pozzetti L., Radovich M., Vergani D., Zamorani G., Zucca E., Abbas U., Bondi M., Bongiorno A., Brinchmann J., Buzzi A., Cucciati O., de Ravel L., Gregorini L., Mellier Y., Merluzzi P., Perez-Montero E., Taxil P., Temporin S., and Walcher C. J.
Subjects: statistics [galaxies], Distribution (number theory), Field (physics), FOS: Physical sciences, Probability density function, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph], 01 natural sciences, Measure (mathematics), GALASSIE, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], GRAVITAZIONE, galaxies: high-redshift, cosmology: theory, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, galaxies: statistics, Physics, large-scale structure of Universe [cosmology], Galaxy: evolution, theory [cosmology], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics (astro-ph), Astronomy and Astrophysics, COSMOLOGIA, COSMOLOGIA OSSERVATIVA, cosmology: large-scale structure of Universe, Redshift, Galaxy, SURVEY, Space and Planetary Science, Skewness, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], evolution [galaxy], Perturbation theory (quantum mechanics), [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], high-redshift [galaxies]
Abstract: We have reconstructed the three-dimensional density fluctuation maps to z ~ 1.5 using the distribution of galaxies observed in the VVDS-Deep survey. We use this overdensity field to measure the evolution of the probability distribution function and its lower-order moments over the redshift interval 0.7, Comment: 14 pages, 5 figures, A&A in Press
Published: 2008
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14. The VIMOS VLT Deep Survey. Tracing the galaxy stellar mass assembly history over the last 8 Gyr

Author: D. Vergani, M. Scodeggio, L. Pozzetti, A. Iovino, P. Franzetti, B. Garilli, G. Zamorani, D. Maccagni, F. Lamareille, O. Le Fèvre, S. Charlot, T. Contini, L. Guzzo, D. Bottini, V. Le Brun, J. P. Picat, R. Scaramella, L. Tresse, G. Vettolani, A. Zanichelli, C. Adami, S. Arnouts, S. Bardelli, M. Bolzonella, A. Cappi, P. Ciliegi, S. Foucaud, I. Gavignaud, O. Ilbert, H. J. McCracken, B. Marano, C. Marinoni, A. Mazure, B. Meneux, R. Merighi, S. Paltani, R. Pellò, A. Pollo, M. Radovich, E. Zucca, M. Bondi, A. Bongiorno, J. Brinchmann, O. Cucciati, S. de la Torre, L. Gregorini, E. Perez-Montero, Y. Mellier, P. Merluzzi, S. Temporin, INAF- Milano, Istituto Nazionale di Astrofisica (INAF), INAF - Osservatorio Astronomico di Bologna (OABO), INAF - Osservatorio Astronomico di Brera (OAB), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, 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), 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), Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), Centre de Physique Théorique - UMR 6207 (CPT), Université de la Méditerranée - Aix-Marseille 2-Université de Provence - Aix-Marseille 1-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Centre de Physique Théorique - UMR 7332 (CPT), Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Capodimonte (OAC), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto = University of Porto, 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), AUTRES, 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, Observatoire de Paris - Site de Paris (OP), 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), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Services communs OMP (UMS 831), 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), European Southern Observatory (ESO), École normale supérieure - Paris (ENS Paris), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Centre National de la Recherche Scientifique (CNRS)-Université de Toulon (UTLN)-Université de Provence - Aix-Marseille 1-Université de la Méditerranée - Aix-Marseille 2, Università di Bologna, Dipartimento di Astronomia, Universidade do Porto, Beaussier, Catherine, Vergani D., Scodeggio M., Pozzetti L., Iovino A., Franzetti P., Garilli B., Zamorani G., Maccagni D., Lamareille F., Le Fèvre O., Charlot S., Contini T., Guzzo L., Bottini D., Le Brun V., Picat J. P., Scaramella R., Tresse L., Vettolani G., Zanichelli A., Adami C., Arnouts S., Bardelli S., Bolzonella M., Cappi A., Ciliegi P., Foucaud S., Gavignaud I., Ilbert O., McCracken H. J., Marano B., Marinoni C., Mazure A., Meneux B., Merighi R., Paltani S., Pellò R., Pollo A., Radovich M., Zucca E., Bondi M., Bongiorno A., Brinchmann J., Cucciati O., de La Torre S., Gregorini L., Perez-Montero E., Mellier Y., Merluzzi P., and Temporin S.
Subjects: Stellar mass, formation [galaxies], Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies: fundamental, [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph], 01 natural sciences, GALASSIE, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], symbols.namesake, 0103 physical sciences, Galaxy formation and evolution, fundamental parameters [galaxies], Astrophysics::Solar and Stellar Astrophysics, galaxies: formation, education, 010303 astronomy & astrophysics, evolution [galaxies], Astrophysics::Galaxy Astrophysics, Physics, parameters, SPETTROGRAFIA, education.field_of_study, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], EVOLUZIONE, 010308 nuclear & particles physics, Star formation, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, Balmer series, Astronomy and Astrophysics, COSMOLOGIA, luminosity function, mass function [galaxies], Galaxy, Redshift, observations [cosmology], Stars, galaxies: luminosity function, Space and Planetary Science, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], mass function, cosmology: observations, symbols, Astrophysics::Earth and Planetary Astrophysics, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], galaxies: evolution
Abstract: We selected a mass-limited sample of 4048 objects from the VIMOS VLT Deep Survey in the redshift interval 0.5, Comment: Accepted for pubblication in A&A, 14 pages, 5 figures
Published: 2008
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15. The Vimos VLT Deep Survey: Global properties of 20000 galaxies in the I_AB<=22.5 WIDE survey

Author: O. Cucciati, G. Vettolani, G. Zamorani, S. de la Torre, H. J. McCracken, C. Adami, B. Garilli, Marco Scodeggio, A. Cappi, Paolo Ciliegi, L. Tresse, A. Pollo, D. Maccagni, E. Zucca, T. Contini, J. Blaizot, S. Bardelli, R. Scaramella, M. Radovich, A. Iovino, L. Gregorini, V. Le Brun, O. Ilbert, C. Marinoni, M. Bolzonella, F. Lamareille, Luigi Guzzo, P. Franzetti, D. Bottini, A. Zanichelli, Alain Mazure, R. Pello, O. Le Fevre, I. Gavignaud, Bruno Marano, C. Moreau, S. Paltani, R. Merighi, Yannick Mellier, L. Paioro, Sylvie Foucaud, Stephane Arnouts, D. Vergani, Lucia Pozzetti, B. Meneux, Stéphane Charlot, Angela Bongiorno, Centre de Physique Théorique - UMR 6207 (CPT), Université de la Méditerranée - Aix-Marseille 2-Université de Provence - Aix-Marseille 1-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Centre de Physique Théorique - UMR 7332 (CPT), Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université de Toulon (UTLN)-Université de Provence - Aix-Marseille 1-Université de la Méditerranée - Aix-Marseille 2, INAF- Milano, Istituto Nazionale di Astrofisica (INAF), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Brera (OAB), Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, 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), 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), European Southern Observatory (ESO), Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), INAF - Osservatorio Astronomico di Bologna (OABO), INAF - Osservatorio Astronomico di Capodimonte (OAC), 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 National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Centre National de la Recherche Scientifique (CNRS)-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 di Bologna, Dipartimento di Astronomia, École normale supérieure - Paris (ENS Paris), Garilli B., Le Fèvre O., Guzzo L., Maccagni D., Le Brun V., de La Torre S., Meneux B., Tresse L., Franzetti P., Zamorani G., Zanichelli A., Gregorini L., Vergani D., Bottini D., Scaramella R., Scodeggio M., Vettolani G., Adami C., Arnouts S., Bardelli S., Bolzonella M., Cappi A., Charlot S., Ciliegi P., Contini T., Foucaud S., Gavignaud I., Ilbert O., Iovino A., Lamareille F., McCracken H. J., Marano B., Marinoni C., Mazure A., Merighi R., Paltani S., Pellò R., Pollo A., Pozzetti L., Radovich M., Zucca E., Blaizot J., Bongiorno A., Cucciati O., Mellier Y., Moreau C., and Paioro L.
Subjects: Field (physics), REDSHIFT, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Correlation function (astronomy), 01 natural sciences, GALASSIE, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, 010303 astronomy & astrophysics, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astronomy and Astrophysics, galaxies: fundamental parameters, Cosmic variance, COSMOLOGIA OSSERVATIVA, cosmology: large-scale structure of Universe, SURVEY, Galaxy, Redshift, Stars, Space and Planetary Science, Limiting magnitude, cosmology: observations, Magnitude (astronomy), [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], catalogs
Abstract: The VVDS-Wide survey has been designed with the general aim of tracing the large-scale distribution of galaxies at z~1 on comoving scales reaching ~100Mpc/h, while providing a good control of cosmic variance over areas as large as a few square degrees. This is achieved by measuring redshifts with VIMOS at the ESO VLT to a limiting magnitude I_AB=22.5, targeting four independent fields with size up to 4 sq.deg. each. The whole survey covers 8.6 sq.deg., here we present the general properties of the current redshift sample. This includes 32734 spectra in the four regions (19977 galaxies, 304 type I AGNs, and 9913 stars), covering a total area of 6.1 sq.deg, with a sampling rate of 22 to 24%. The redshift success rate is above 90% independently of magnitude. It is the currently largest area coverage among redshift surveys reaching z~1. We give the mean N(z) distribution averaged over 6.1 sq.deg. Comparing galaxy densities from the four fields shows that in a redshift bin Deltaz=0.1 at z~1 one still has factor-of-two variations over areas as large as ~0.25 sq.deg. This level of cosmic variance agrees with that obtained by integrating the galaxy two-point correlation function estimated from the F22 field alone, and is also in fairly good statistical agreement with that predicted by the Millennium mocks. The variance estimated over the survey fields shows explicitly how clustering results from deep surveys of even ~1 sq.deg. size should be interpreted with caution. This paper accompanies the public release of the first 18143 redshifts of the VVDS-Wide survey from the 4 sq.deg. contiguous area of the F22 field at RA=22h, publicly available at http://cencosw.oamp.fr, Comment: Accepted for publication on Astronomy & Astrophysics
Published: 2008
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16. The VVDS-VLA deep field. III. GMRT observations at 610 MHz and the radio spectral index properties of the sub-mJy population

Author: R. Athreya, L. Gregorini, Thierry Contini, E. Zucca, Daniela Vergani, O. Le Fevre, Paolo Ciliegi, S. Bardelli, Daniele Dallacasa, A. Iovino, Bianca Garilli, M. Bondi, S. Temporin, A. Zanichelli, Tiziana Venturi, Bondi M., Ciliegi P., Venturi T., Dallacasa D., Bardelli S., Zucca E., Athreya R. M., Gregorini L., Zanichelli A., Le Fèvre O., Contini T., Garilli B., Iovino A., Temporin S., Vergani D., Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), and Beaussier, Catherine
Subjects: Physics, QSOS, education.field_of_study, Spectral index, Hubble Deep Field, Astrophysics (astro-ph), Population, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Low frequency, Galaxy, Luminosity, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Space and Planetary Science, Source counts, education
Abstract: We present the low frequency (610 MHz) radio source counts of the VVDS-VLA field and investigate the radio spectral index properties of the sub-mJy population. We use new deep (r.m.s.$\simeq 50$ $\mu$Jy/beam) observations of the VVDS-VLA field obtained at 610 MHz with the GMRT and matched in resolution (6 arcsec) with already available VLA data at 1.4 GHz on the same field. We find evidence of a change of the dominant population of radio sources below 0.5 mJy (at 1.4 GHz): between 0.15 and 0.5 mJy the median spectral index is significantly flatter ($\alpha=-0.46\pm 0.03$) than that of brighter sources ($\alpha=-0.67\pm 0.05$). A relevant contribution below 0.5 mJy from a population of flat spectrum low luminosity compact AGNs and radio quiet QSOs could explain this effect. At even fainter flux density, between 0.10 and 0.15 mJy at 1.4 GHz, the median spectral index steepens again ($\alpha=-0.61\pm 0.04$) suggesting that the contribution of starburst galaxies becomes important below $\sim 0.2$ mJy. Finally we present a sample of 58 candidate ultra-steep sources with radio flux density from one to two orders of magnitude lower than any other sample of such objects., Comment: Accepted for publication in Astronomy & Astrophysics
Published: 2007

17. The VIMOS VLT Deep Survey - Evolution of the luminosity functions by galaxy type up to z=1.5 from first epoch data

Author: G. Zamorani, Stéphane Charlot, J. P. Picat, O. Le Fevre, A. Cappi, S. Paltani, E. Zucca, D. Rizzo, O. Cucciati, D. Bottini, A. Pollo, Roberto Scaramella, R. Merighi, Stephane Arnouts, G. Busarello, Yannick Mellier, L. Gregorini, Lucia Pozzetti, Sylvie Foucaud, D. Maccagni, Paolo Ciliegi, M. Bolzonella, S. Bardelli, B. Garilli, V. Ripepi, Bruno Marano, M. Bondi, G. Vettolani, C. Adami, Magda Arnaboldi, T. Contini, H. J. McCracken, B. Meneux, F. Lamareille, R. Pello, Paola Merluzzi, Christian Marinoni, Mario Radovich, A. Iovino, G. Mathez, I. Gavignaud, Angela Bongiorno, Marco Scodeggio, P. Franzetti, L. Tresse, A. Zanichelli, Alain Mazure, V. Le Brun, O. Ilbert, Luigi Guzzo, 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 Bologna (OABO), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'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), Istituto di Astrofisica Spaziale e Fisica Cosmica (IASF-Milano), 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), Istituto di Radioastronomia, Bologna, INAF-Osservatorio Astronomico di Capodimonte (INAF-OAC), Max-Planck-Institut für Astrophysik (MPA), European Southern Observatory (ESO), INAF-Osservatorio Astronomico di Brera, 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), Zucca E., Ilbert O., Bardelli S., Tresse L., Zamorani G., Arnouts S., Pozzetti L., Bolzonella M., McCracken H. J., Bottini D., Garilli B., Le Brun V., Le Fevre O., Maccagni D., Picat J.P., Scaramella R., Scodeggio M., Vettolani G., Zanichelli A., Adami C., Arnaboldi M., Cappi A., Charlot S., Ciliegi P., Contini T., Foucaud S., Franzetti P., Gavignaud I., Guzzo L., Iovino A., Marano B., Marinoni C., Mazure A., Meneux B., Merighi R., Paltani S., Pello' R., Pollo A., Radovich M., Bondi M., Bongiorno A., Busarello G., Cucciati O., Gregorini L., Lamareille F., Mathez G., Mellier Y., Merluzzi P., Ripepi V., and Rizzo D.
Subjects: Physics, 010308 nuclear & particles physics, Epoch (astronomy), Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Rest frame, Stellar classification, 01 natural sciences, Redshift, Galaxy, Luminosity, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Space and Planetary Science, [SDU]Sciences of the Universe [physics], 0103 physical sciences, Magnitude (astronomy), 10. No inequality, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Luminosity function (astronomy)
Abstract: From the first epoch observations of the VVDS up to z=1.5 we have derived luminosity functions (LF) of different spectral type galaxies. The VVDS data, covering ~70% of the life of the Universe, allow for the first time to study from the same sample and with good statistical accuracy the evolution of the LFs by galaxy type in several rest frame bands from a purely magnitude selected sample. The magnitude limit of the VVDS allows the determination of the faint end slope of the LF with unprecedented accuracy. Galaxies have been classified in four spectral classes, using their colours and redshift, and LFs have been derived in the U, B, V, R and I rest frame bands from z=0.05 to z=1.5. We find a significant steepening of the LF going from early to late types. The M* parameter is significantly fainter for late type galaxies and this difference increases in the redder bands. Within each of the galaxy spectral types we find a brightening of M* with increasing redshift, ranging from =< 0.5 mag for early type galaxies to ~1 mag for the latest type galaxies, while the slope of the LF of each spectral type is consistent with being constant with redshift. The LF of early type galaxies is consistent with passive evolution up to z~1.1, while the number of bright early type galaxies has decreased by ~40% from z~0.3 to z~1.1. We also find a strong evolution in the normalization of the LF of latest type galaxies, with an increase of more than a factor 2 from z~0.3 to z~1.3: the density of bright late type galaxies in the same redshift range increases of a factor ~6.6. These results indicate a strong type-dependent evolution and identifies the latest spectral types as responsible for most of the evolution of the UV-optical luminosity function out to z=1.5., 18 pages with encapsulated figures, revised version after referee's comments, accepted for publication in A&A
Published: 2006
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18. The VIMOS VLT Deep Survey: the build-up of the colour-density relation

Author: V. Le Brun, O. Ilbert, C. Adami, G. Zamorani, G. Busarello, Marco Scodeggio, Gianpaolo Vettolani, H. J. McCracken, D. Maccagni, Paola Merluzzi, Stéphane Paltani, I. Gavignaud, E. Zucca, D. Rizzo, B. Garilli, M. Bolzonella, Christian Marinoni, Angela Bongiorno, A. Cappi, Luigi Guzzo, T. Contini, D. Vergani, R. Pello, L. Gregorini, G. Mathez, L. Tresse, Magda Arnaboldi, Mario Radovich, F. Lamareille, Stéphane Charlot, G. Temporin, A. Pollo, S. Bardelli, Stephane Arnouts, A. Zanichelli, Lucia Pozzetti, Paolo Ciliegi, V. Ripepi, Yannick Mellier, Alain Mazure, D. Bottini, O. Le Fevre, P. Franzetti, M. Bondi, J. P. Picat, Sylvie Foucaud, O. Cucciati, S. de la Torre, Bruno Marano, Roberto Scaramella, A. Iovino, R. Merighi, B. Meneux, INAF-Osservatorio Astronomico di Brera, Centre de Physique Théorique - UMR 7332 (CPT), Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), 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 Bologna (OABO), Istituto di Astrofisica Spaziale e Fisica Cosmica (IASF-Milano), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'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), IRA-INAF, Bologna, Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), INAF-Osservatorio Astronomico di Capodimonte (INAF-OAC), Max-Planck-Institut für Astrophysik (MPA), European Southern Observatory (ESO), INTEGRAL Science Data Centre, 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, 010504 meteorology & atmospheric sciences, Star formation, Diagram, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Function (mathematics), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Rest frame, 01 natural sciences, Redshift, Bin, Galaxy, Luminosity, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Space and Planetary Science, 0103 physical sciences, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences
Abstract: We investigate the redshift and luminosity evolution of the galaxy colour-density relation using the data from the First Epoch VIMOS-VLT Deep Survey (VVDS). The size (6582 galaxies), depth (I_AB, 17 pages, 10 figures, figures added, accepted by A&A
Published: 2006
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19. The VIMOS-VLT Deep Survey. The evolution of galaxy clustering per spectral type to z ~= 1.5

Author: Christian Marinoni, T. Contini, Luigi Guzzo, Paolo Ciliegi, G. Zamorani, A. Cappi, O. Cucciati, Angela Bongiorno, L. Tresse, Stephane Arnouts, Lucia Pozzetti, Yannick Mellier, V. Ripepi, E. Zucca, D. Rizzo, V. LeBrun, S. Paltani, Roberto Scaramella, Stéphane Charlot, G. Mathez, O. LeFevre, R. Merighi, I. Gavignaud, A. Zanichelli, M. Bondi, B. Meneux, D. Bottini, Alain Mazure, G. Vettolani, J. P. Picat, M. Bolzonella, A. Iovino, R. Pello, M. Arnaboldi, G. Busarello, B. Garilli, Marco Scodeggio, C. Adami, L. Gregorini, Mario Radovich, F. Lamareille, P. Franzetti, Paola Merluzzi, O. Ilbert, Bruno Marano, D. Maccagni, H. J. McCracken, Sylvie Foucaud, A. Pollo, S. Bardelli, 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 (INAF-OAB), INAF-Osservatorio Astronomico di Bologna (OABO), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), INAF-Osservatorio Astronomico di Brera, 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), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Istituto di Astrofisica Spaziale e Fisica Cosmica (IASF-Milano), Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), INAF-Osservatorio Astronomico di Roma (INAF-OAR), IRA-INAF, Bologna, INAF-Osservatorio Astronomico di Capodimonte (INAF-OAC), Max-Planck-Institut für Astrophysik (MPA), School of Physics and Astronomy, University of Nottingham, European Southern Observatory (ESO), INTEGRAL Science Data Centre, 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), Meneux B., Le Fèvre O., Guzzo L., Pollo A., Cappi A., Ilbert O., Iovino A., Marinoni C., McCracken H. J., Bottini D., Garilli B., Le Brun V., Maccagni D., Picat J.P., Scaramella R., Scodeggio M., Tresse L., Vettolani G., Zanichelli A., Adami C., Arnouts S., Arnaboldi M., Bardelli S., Bolzonella M., Charlot S., Ciliegi P., Contini T., Foucaud S., Franzetti P., Gavignaud I., Marano B., Mazure A., Merighi R., Paltani S., Pello' R., Pozzetti L., Radovich M., Zamorani G., Zucca E., Bondi M., Bongiorno A., Busarello G., Cucciati O., Gregorini L., Lamareille F., Mathez G., Mellier Y., Merluzzi P., Ripepi V., and Rizzo D.
Subjects: Population, Dark matter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Type (model theory), Stellar classification, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, 10. No inequality, education, Cluster analysis, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, education.field_of_study, 010308 nuclear & particles physics, Star formation, Astrophysics (astro-ph), Astronomy and Astrophysics, Galaxy, Space and Planetary Science, Halo, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: We measure the evolution of clustering for galaxies with different spectral types from 6495 galaxies with 17.51.2, due to the growth in clustering of the star-forming population. We find similar results when splitting the sample into `red' and `blue' galaxies using the observed color bi-modality. When compared to the expected linear growth of mass fluctuations, a natural interpretation of these observations is that: (a) the assembly of massive early type galaxies is already mostly complete in the densest dark matter halos at z~=1; (b) luminous late-type galaxies are located in higher-density, more clustered regions of the Universe at z~=1.5 than at present, indicating that star formation activity is progressively increasing, going back in time, in the higher-density peaks that today are mostly dominated by old galaxies., 12 pages, Accepted on 11-Feb-06 for publication in Astronomy and Astrophysics
Published: 2006
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20. Accurate photometric redshifts for the CFHT Legacy Survey calibrated using the VIMOS VLT Deep Survey

Author: Paolo Ciliegi, G. Busarello, R. Pello, Mario Radovich, A. Pollo, V. Ripepi, A. Iovino, V. Le Brun, O. Ilbert, T. Contini, C. Adami, L. Tresse, S. Bardelli, M. Bondi, Christian Marinoni, O. Le Fevre, D. Vergani, I. Gavignaud, Marco Scodeggio, B. Garilli, D. Maccagni, E. Zucca, D. Rizzo, Stéphane Paltani, Gianpaolo Vettolani, H. J. McCracken, P. Franzetti, Bruno Marano, Alain Mazure, M. Bolzonella, Yannick Mellier, Sylvie Foucaud, Roberto Scaramella, R. Merighi, D. Bottini, A. Cappi, Luigi Guzzo, O. Cucciati, S. de la Torre, L. Gregorini, J. P. Picat, E. Bertin, B. Meneux, G. Mathez, Paola Merluzzi, Angela Bongiorno, Stéphane Charlot, Stephane Arnouts, Lucia Pozzetti, G. Zamorani, F. Lamareille, A. Zanichelli, 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), Ilbert O., Arnouts S., McCracken H. J., Bolzonella M., Bertin E., Le Fèvre O., Mellier Y., Zamorani G., Pellò R., Iovino A., Tresse L., Le Brun V., Bottini D., Garilli B., Maccagni D., Picat J. P., Scaramella R., Scodeggio M., Vettolani G., Zanichelli A., Adami C., Bardelli S., Cappi A., Charlot S., Ciliegi P., Contini T., Cucciati O., Foucaud S., Franzetti P., Gavignaud I., Guzzo L., Marano B., Marinoni C., Mazure A., Meneux B., Merighi R., Paltani S., Pollo A., Pozzetti L., Radovich M., Zucca E., Bondi M., Bongiorno A., Busarello G., de La Torre S., Gregorini L., Lamareille F., Mathez G., Merluzzi P., Ripepi V., Rizzo D., Vergani D., Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'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), 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), INAF-Osservatorio Astronomico di Brera, Istituto di Astrofisica Spaziale e Fisica Cosmica (IASF-Milano), INAF-Osservatorio Astronomico di Roma (INAF-OAR), IRA-INAF, Bologna, School of Physics and Astronomy, University of Nottingham, European Southern Observatory (ESO), 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 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: FOS: Physical sciences, METHODS: DATA ANALYSIS, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Extended Groth Strip, 0103 physical sciences, Calibration, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Photometric redshift, Physics, 010308 nuclear & particles physics, Astrophysics (astro-ph), Sigma, Astronomy and Astrophysics, GALAXIES: PHOTOMETRY, Cosmic variance, Galaxy, Redshift, Cover (topology), 13. Climate action, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], GALAXIES: DISTANCES AND REDSHIFTS
Abstract: We present photometric redshifts for an uniquely large and deep sample of 522286 objects with i'_{AB}, Comment: 19 pages, 17 figures, submitted to A&A. The photometric redshifts described in this paper will be made publicly available from 1st may 2006 at http://terapix.iap.fr and http://cencosw.oamp.fr/
Published: 2006
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21. The VIMOS-VLT Deep Survey: Luminosity dependence of clustering at z~1

Author: A. Pollo, L. Guzzo, O. Le Fèvre, B. Meneux, A. Cappi, P. Franzetti, A. Iovino, H. J. McCracken, C. Marinoni, G. Zamorani, D. Bottini, B. Garilli, V. Le 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, I. Gavignaud, O. Ilbert, B. Marano, A. Mazure, R. Merighi, S. Paltani, R. Pellò, L. Pozzetti, M. Radovich, E. Zucca, M. Bondi, A. Bongiorno, G. Busarello, O. Cucciati, L. Gregorini, F. Lamareille, G. Mathez, Y. Mellier, P. Merluzzi, V. Ripepi, D. Rizzo, 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), Pollo A., Guzzo L., Le Fèvre O., Meneux B., Cappi A., Franzetti P., Iovino A., McCracken H. J., Marinoni C., Zamorani G., Bottini D., Garilli B., Le Brun V., Maccagni D., Picat J.P., Scaramella R., Scodeggio M., Tresse L., Vettolani G., Zanichelli A., Adami C., Arnouts S., Bardelli S., Bolzonella M., Charlot S., Ciliegi P., Contini T., Foucaud S., Gavignaud I., Ilbert O., Marano B., Mazure A., Merighi R., Paltani S., Pello R., Pozzetti L., Radovich M., Zucca E., Bondi M., Bongiorno A., Busarello G., Cucciati P., Gregorini L., Lamareille F., Mathez G., Mellier Y., Merluzzi P., Ripepi V., and Rizzo D.
Subjects: Absolute magnitude, statistical [methods], FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], large scale structure of Universe [cosmology], 0103 physical sciences, Cluster analysis, 010303 astronomy & astrophysics, evolution [galaxies], Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Astrophysics (astro-ph), Astronomy and Astrophysics, Galaxy, Redshift, observations [cosmology], Correlation function (statistical mechanics), Space and Planetary Science, Halo, VIMOS-VLT Deep Survey
Abstract: We investigate the dependence of galaxy clustering on the galaxy intrinsic luminosity at high redshift, using the data from the First Epoch VIMOS-VLT Deep Survey (VVDS). The size (6530 galaxies) and depth (I_{AB}=0.9 and median absolute magnitude -19.6< M_B < -21.3. Fitting w_p(r_p) with a single power-law model for the real-space correlation function xi(r)=(r/r_0)^{-gamma}, we measure the relationship of the correlation length r_0 and the slope gamma with the sample median luminosity for the first time at such high redshift. Values from our lower-redshift samples (0.1=-19.6) have a correlation length r_0=2.7^{+0.3}_{-0.3} h^{-1} Mpc, compared to r_0=5.0^{+1.5}_{-1.6} h^{-1} Mpc at =-21.3. Correspondingly the slope of the correlation function is observed to steepen significantly from \gamma=1.6^{+0.1}_{-0.1} to \gamma=2.4^{+0.4}_{-0.2}. This is not observed neither by large local surveys nor in our lower-redshift sample and seems to imply a significant change in the way luminous galaxies trace dark-matter halos at z~1 with respect to z~0. At our effective median redshift z~0.9 this corresponds to a strong difference of the relative bias, from b/b* < 0.7 for galaxies with L < L*, to b/b*~1.4 for galaxies with L > L*., Comment: Accepted for publication in Astronomy and Astrophysics
Published: 2006
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22. The B3 VLA Sample at Low Frequencies: Results from a survey at 74 MHz

Author: R. T. Schilizzi, W. Tschager, L. Gregorini, I. A. G. Snellen, M. Vigotti, K.-H. Mack, Uli Klein, LOBANOV A.P., ZENZUS J.A., CESARSKY C., DIAMOND P.J., Mack K.-H., Vigotti M., Gregorini L., Klein U., Tschager W., Schilizzi R.T., and Snellen I.A.G.
Subjects: Geography, Observatory, business.industry, Library science, Telecommunications, business, Sample (graphics)
Abstract: 1 Istituto di Radioastronomia del CNR, Via P. Gobetti 101, I-40129 Bologna, Italy 2 Radioastronomisches Institut der Universitat Bonn, Auf dem Hugel 71, D-53121 Bonn, Germany 3 Sterrewacht Leiden, PO Box 9513, NL-2300 RA Leiden, The Netherlands 4 Int. SKA Project Office, Postbus 2, NL-7990 AA Dwingeloo, The Netherlands 5 Institute for Astronomy, Royal Observatory, Blackford Hill, Edinburgh, EH9 3HJ, United Kingdom
Published: 2006

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

Author: D. Rizzo, C. Adami, M. Bolzonella, Marco Scodeggio, Roberto Scaramella, A. Mazure, Lucia Pozzetti, A. Zanichelli, Paola Merluzzi, E. Zucca, B. Meneux, R. Merighi, Thierry Contini, O. Ilbert, G. Busarello, Christian Marinoni, V. Le Brun, Sylvie Foucaud, I. Gavignaud, G. Vettolani, G. Mathez, V. Ripepi, J. P. Picat, B. Garilli, R. Pello, D. Maccagni, Stephane Charlot, Mario Radovich, G. Zamorani, Stéphane Paltani, Yannick Mellier, M. Arnaboldi, Bruno Marano, A. Iovino, F. Lamareille, A. Cappi, M. Bondi, Luigi Guzzo, Laurence Tresse, A. Pollo, S. Bardelli, D. Bottini, Stéphane Arnouts, Angela Bongiorno, H. J. McCracken, L. Gregorini, P. Franzetti, O. Le Fevre, Paolo Ciliegi, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), Le Fèvre O., Paltani S., Arnouts S., Charlot S., Foucaud S., Ilbert O., McCracken H. J., Zamorani G., Bottini D., Garilli B., Le Brun V., Maccagni D., Picat J. P., Scaramella R., Scodeggio M., Tresse L., Vettolani G., Zanichelli A., Adami C., Bardelli S., Bolzonella M., Cappi A., Ciliegi P., Contini T., Franzetti P., Gavignaud I., Guzzo L., Iovino A., Marano B., Marinoni C., Mazure A., Meneux B., Merighi R., Pellò R., Pollo A., Pozzetti L., Radovich M., Zucca E., Arnaboldi M., Bondi, M., Bongiorno A., Busarello G., Gregorini L., Lamareille F., Mathez G., Mellier, Y., Merluzzi P., Ripepi V., Rizzo D., 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 Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)
Subjects: 010504 meteorology & atmospheric sciences, Radio galaxy, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Peculiar galaxy, GALASSIE, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, Galaxy formation and evolution, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, Luminous infrared galaxy, Multidisciplinary, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics (astro-ph), Astronomy, Quasar, COSMOLOGIA, Galaxy, Elliptical galaxy
Abstract: To understand the evolution of galaxies, we need to know as accurately as possible how many galaxies were present in the Universe at different epochs. Galaxies in the young Universe have hitherto mainly been identified using their expected optical colours, but this leaves open the possibility that a significant population remains undetected because their colours are the result of a complex mix of stars, gas, dust or active galactic nuclei. Here we report the results of a flux-limited I-band survey of galaxies at look-back times of 9 to 12 billion years. We find 970 galaxies with spectroscopic redshifts between 1.4 and 5. This population is 1.6 to 6.2 times larger than previous estimates, with the difference increasing towards brighter magnitudes. Strong ultraviolet continua (in the rest frame of the galaxies) indicate vigorous star formation rates of more than 10 to 100 solar masses per year. As a consequence, the cosmic star formation rate is higher than previously measured at redshifts of 3 to 4., Comment: Published in Nature, 22 September 2005
Published: 2005
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24. The Vimos-VLT Deep Survey: Results from the First-Epoch Observations

Author: R. Pello, Mario Radovich, B. Meneux, Paolo Ciliegi, Vincenzo Ripepi, Stephane Charlot, H. J. McCracken, M. Bondi, Alain Mazure, C. Adami, G. Busarello, E. Zucca, Marco Scodeggio, D. Rizzo, D. Bottini, V. Le Brun, Bruno Marano, B. Garilli, I. Gavignaud, D. Maccagni, O. Ilbert, Yannick Mellier, C. Marinoni, S. Paltani, Roberto Scaramella, L. Tresse, R. Merighi, Sylvie Foucaud, A. Pollo, T. Contini, L. Gregorini, M. Bolzonella, Paola Merluzzi, Angela Bongiorno, G. Vettolani, Luigi Guzzo, P. Franzetti, G. Mathez, Magda Arnaboldi, A. Cappi, S. Bardelli, O. Le Fevre, J. P. Picat, A. Iovino, G. Zamorani, Stephane Arnouts, Lucia Pozzetti, A. Zanichelli, 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), Yannick Mellier, Georges Meylan, YANNICK MELLIER AND GEORGES MEYLAN, Paltani S., Ilbert O., Le Fèvre O., Marinoni C., Bottini D., Garilli B., Le Brun V., Maccagni D., Picat J.-P., Scaramella R., Scodeggio M., Tresse L., Vettolani G., Zanichelli A., Adami C., Arnaboldi M., Arnouts S., Bardelli S., Bolzonella M., Cappi A., Charlot S., Contini T., Foucaud S., Franzetti P., Gavignaud I., Guzzo L., Iovino A., McCracken H. J., Marano B., Mazure A., Meneux B., Merighi R., Pellò R., Pollo A., Pozzetti L., Radovich M., Zamorani G., Zucca E., Bondi M., Bongiorno A., Busarello G., Ciliegi P., Gregorini L., Mathez G., Mellier Y., Merluzzi P., Ripepi V., Rizzo D, 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, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astronomy, Astronomy and Astrophysics, Function (mathematics), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Redshift survey, Galaxy, Redshift, Spectral line, Luminosity, Space and Planetary Science, Limiting magnitude, Astrophysics::Galaxy Astrophysics, Luminosity function (astronomy)
Abstract: ISBN 0521851963; The Vimos-VLT Deep Survey is a spectroscopic survey aiming at collecting more than 50000 spectra down to a limiting magnitude IAB=24, and 100000 down to IAB=22.5, on a total of about 16 deg2 without any color or morphology preselection. We present the N(z) distribution up to z~ 5, obtained from a purely magnitude-limited sample down to IAB=24, which is an important input to weak-lensing studies. We discuss the evolution of the galaxy luminosity function up to z~ 2, which exhibits a very strong increase in the typical galaxy luminosity Delta M*&simeq; -2.5 in the U band compared to the local value. Surveys like the VVDS also allow to study the galaxy bias as a function of redshift without assumption about its linearity, an assumption that we find to be violated in some cases. A low bias is found, and the linear bias is shown to increase with redshift.
Published: 2005
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25. The VIRMOS deep imaging survey IV: Near-infrared observations

Author: Thierry Contini, I. Gavignaud, G. Zamorani, M. Scodeggio, O. Le Fevre, M. Radovich, G. Mathez, Bianca Garilli, G. Busarello, H. J. McCracken, Stéphane Arnouts, Giampaolo Vettolani, D. Maccagni, Paola Merluzzi, Stéphane Paltani, Stephane Charlot, D. Bottini, L. Gregorini, Paolo Saracco, R. Pello, Bruno Marano, A. Zanichelli, Yannick Mellier, A. Cappi, Emmanuel Bertin, Olivier Ilbert, B. Meneux, A. Iovino, Paolo Ciliegi, Olga Cucciati, A. Pollo, Roberto Scaramella, A. Mazure, Lucia Pozzetti, R. Merighi, S. Bardelli, J. P. Picat, Magda Arnaboldi, Laurence Tresse, M. Bondi, E. Zucca, D. Rizzo, L. Paioro, V. Le Brun, P. Franzetti, Luigi Guzzo, Angela Bongiorno, Vincenzo Ripepi, Sylvie Foucaud, Christian Marinoni, M. Bolzonella, C. Adami, INAF - Osservatorio Astronomico di Brera (OAB), Istituto Nazionale di Astrofisica (INAF), 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), 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), Services communs OMP (UMS 831), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Bologna (OABO), INAF - Osservatorio Astronomico di Capodimonte (OAC), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, European Southern Observatory (ESO), Dipartimento di Fisica, Università degli Studi di Milano-Bicocca = University of Milano-Bicocca (UNIMIB)-Università degli Studi di Milano = University of Milan (UNIMI), 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), Departement de Radioastronomie Millimétrique (DEMIRM), Observatoire de Paris, 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)-Université Pierre et Marie Curie - Paris 6 (UPMC), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), 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), Università di Bologna, Dipartimento di Astronomia, Università degli Studi di Milano-Bicocca [Milano] (UNIMIB)-Università degli Studi di Milano [Milano] (UNIMI), École normale supérieure - Paris (ENS Paris), Iovino A., McCracken H. J., Garilli B., Foucaud S., Le Fèvre O., Maccagni D., Saracco P., Bardelli S., Busarello G., Scodeggio M., Zanichelli A., Paioro L., Bottini D., Le Brun V., Picat J. P., Scaramella R., Tresse L., Vettolani G., Adami C., Arnaboldi M., Arnouts S., Bolzonella M., Cappi A., Charlot S., Ciliegi P., Contini T., Franzetti P., Gavignaud I., Guzzo L., Ilbert O., Marano B., Marinoni C., Mazure A., Meneux B., Merighi R., Paltani S., Pellò R., Pollo A., Pozzetti L., Radovich M., Zamorani G., Zucca E., Bertin E., Bondi M., Bongiorno A., Cucciati O., Gregorini L., Mathez G., Mellier Y., Merluzzi P., Ripepi V., and Rizzo D.
Subjects: FOS: Physical sciences, Magnitude (mathematics), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, GALAXIES: SURVEYS, infrared: galaxies, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], surveys, 0103 physical sciences, Cluster analysis, 010303 astronomy & astrophysics, Scaling, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Astrophysics (astro-ph), Near-infrared spectroscopy, Astronomy and Astrophysics, galaxies: general, cosmology: large-scale structure of Universe, Galaxy, Wavelength, Amplitude, 13. Climate action, Space and Planetary Science, Limiting magnitude
Abstract: In this paper we present a new deep, wide-field near-infrared imaging survey. Our J- and K-band observations in four separate fields complement optical BVRI, ultraviolet and spectroscopic observations undertaken as part of the VIMOS-VLT deep survey (VVDS). In total, our survey spans ~400arcmis^2. Our catalogues are reliable in all fields to at least Kvega~20.75 and Jvega~21.50 (defined as the magnitude where object contamination is less than 10% and completeness greater than 90%). Taken together these four fields represents a unique combination of depth, wavelength coverage and area. We describe the complete data reduction process and outline a comprehensive series of tests carried out to characterise the reliability of the final catalogues. We compare the statistical properties of our catalogues with literature compilations. We find that our J- and K-selected galaxy counts are in good agreement with previously published works, as are our (J-K) versus K colour-magnitude diagrams. Stellar number counts extracted from our fields are consistent with a synthetic model of our galaxy. Using the location of the stellar locus in colour-magnitude space and the measured field-to-field variation in galaxy number counts we demonstrate that the absolute accuracy of our photometric calibration is at the 5% level or better. Finally, an investigation of the angular clustering of K- selected extended sources in our survey displays the expected scaling behaviour with limiting magnitude, with amplitudes in each magnitude bin in broad agreement with literature values., 15 pages, 19 figs, Accepted by A&A
Published: 2005
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26. The VIMOS VLT deep survey. Computing the two point correlation statistics and associated uncertainties

Author: A. Pollo, B. Meneux, L. Guzzo, O. Le Fèvre, J. Blaizot, A. Cappi, A. Iovino, C. Marinoni, H. J. McCracken, D. Bottini, B. Garilli, V. Le Brun, D. Maccagni, J. P. Picat, R. Scaramella, M. Scodeggio, L. Tresse, G. Vettolani, A. Zanichelli, C. Adami, M. Arnaboldi, S. Arnouts, S. Bardelli, M. Bolzonella, S. Charlot, P. Ciliegi, T. Contini, S. Foucaud, P. Franzetti, I. Gavignaud, O. Ilbert, B. Marano, G. Mathez, A. Mazure, R. Merighi, S. Paltani, R. Pellò, L. Pozzetti, M. Radovich, G. Zamorani, E. Zucca, M. Bondi, A. Bongiorno, G. Busarello, L. Gregorini, F. Lamareille, Y. Mellier, P. Merluzzi, V. Ripepi, D. Rizzo, INAF-Osservatorio Astronomico di Brera (INAF-OAB), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), INAF-Osservatorio Astronomico di Bologna (OABO), INAF-Osservatorio Astronomico di Brera, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'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), Istituto di Astrofisica Spaziale e Fisica Cosmica (IASF-Milano), Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), INAF-Osservatorio Astronomico di Roma (INAF-OAR), Istituto di Radioastronomia, Bologna, INAF-Osservatorio Astronomico di Capodimonte (INAF-OAC), Max-Planck-Institut für Astrophysik (MPA), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Pollo A., Meneux B., Guzzo L., Le Fèvre O., Blaizot J., Cappi A., Iovino A., Marinoni C., McCracken H. J., Bottini D., Garilli B., Le Brun V., Maccagni D., Picat J.P., Scaramella R., Scodeggio M., Tresse L., Vettolani G., Zanichelli A., Adami C., Arnaboldi M., Arnouts S., Bardelli S., Bolzonella M., Charlot S., Ciliegi P., Contini T., Foucaud S., Franzetti P., Gavignaud I., Ilbert O., Marano B., Mathez G., Mazure A., Merighi R., Paltani S., Pello R., Pozzetti L., Radovich M., Zamorani G., Zucca E., Bondi M., Bongiorno A., Busarello G., Gregorini L., Lamareille F., Mellier Y., Merluzzi P., Ripepi V., Rizzo D., 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, COSMIC cancer database, 010308 nuclear & particles physics, Epoch (reference date), Astrophysics (astro-ph), FOS: Physical sciences, Sampling (statistics), Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Galaxy, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Correlation function (statistical mechanics), Space and Planetary Science, 0103 physical sciences, Statistics, Galaxy formation and evolution, Cluster analysis, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, VIMOS-VLT Deep Survey
Abstract: We are presenting in this paper a detailed account of the methods used to compute the three-dimensional two-point galaxy correlation function in the VIMOS-VLT deep survey (VVDS). We investigate how instrumental selection effects and observational biases affect the measurements and identify the methods to correct them. We quantify the accuracy of our correction method using an ensemble of fifty mock galaxy surveys generated with the GalICS semi-analytic model of galaxy formation which incorporate the same selection biases and tiling strategy as the real data does. We demonstrate that we are able to recover the real-space two-point correlation function xi(s) to an accuracy better than 10% on scales larger than 1 h^{-1} Mpc, and of about 30% on scales below 1 h^{-1} Mpc, with the sampling strategy used for the first epoch VVDS data. The projected correlation function w_p(r_p) is recovered with an accuracy better than 10% on all scales 0.1, 16 pages, accepted 10-Mar-05 in A&A
Published: 2005
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27. The VVDS-VLA deep field. II. Optical and near infrared identifications of VLA S1.4 GHz > 80 mu Jy sources in the VIMOS VLT deep survey VVDS-02h field

Author: P. Ciliegi, G. Zamorani, M. Bondi, L. Pozzetti, M. Bolzonella, L. Gregorini, B. Garilli, A. Iovino, H. J. McCracken, Y. Mellier, M. Radovich, H. R. de Ruiter, P. Parma, D. Bottini, V. Le Brun, O. Le Fèvre, D. Maccagni, J. P. Picat, R. Scaramella, M. Scodeggio, L. Tresse, G. Vettolani, A. Zanichelli, C. Adami, M. Arnaboldi, S. Arnouts, S. Bardelli, A. Cappi, S. Charlot, T. Contini, S. Foucaud, P. Franzetti, L. Guzzo, O. Ilbert, B. Marano, C. Marinoni, G. Mathez, A. Mazure, B. Meneux, R. Merighi, P. Merluzzi, S. Paltani, A. Pollo, E. Zucca, A. Bongiorno, G. Busarello, I. Gavignaud, R. Pellò, V. Ripepi, D. Rizzo, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Ciliegi P., Zamorani G., Bondi M., Pozzetti L., Bolzonella M., Gregorini L., Garilli B., Iovino A., McCracken H. J., Mellier Y., Radovich M., de Ruiter H. R., Parma P., Bottini D., Le Brun V., Le Fèvre O., Maccagni D., Picat J. P., Scaramella R., Scodeggio M., Tresse L., Vettolani G., Zanichelli A., Adami C., Arnaboldi M., Arnouts S., Bardelli S., Cappi A., Charlot S., Contini T., Foucaud S., Franzetti P., Guzzo L., Ilbert O., Marano B., Marinoni C., Mathez G., Mazure A., Meneux B., Merighi R., Merluzzi P., Paltani S., Pollo A., Zucca E., Bongiorno A., Busarello G., Gavignaud I., Pellò R., Ripepi V., and Rizzo D.
Subjects: Physics, radio continuum: galaxies, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Hubble Deep Field, Astrophysics::High Energy Astrophysical Phenomena, Near-infrared spectroscopy, Flux, Astronomy and Astrophysics, galaxies: starburst, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, galaxies: general, Galaxy, Redshift, Luminosity, Space and Planetary Science, cosmology: observations, 0103 physical sciences, Magnitude (astronomy), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Photometric redshift
Abstract: In this paper we present the optical and near-infrared identifications of the 1054 radio sources detected in the 20 cm deep radio survey down to a 5sigma flux limit of ~80 muJy obtained with the VLA in the VIMOS VLT Deep Survey VVDS-02h deep field. Using U,B,V,R,I and K data, with limiting magnitudes of UAB~25.4, BAB~26.5, VAB~26.2, RAB~25.9 IAB~25.0, JAB~24.2, KAB~23.9 (50% completeness) we identified 718 radio sources (~74% of the whole sample). The photometric redshift analysis shows that, in each magnitude bin, the radio sample has a higher median photometric redshift than the whole optical sample, while the median (V-I)AB color of the radio sources is redder than the median color of the whole optical sample. These results suggest that radio detection is preferentially selecting galaxies with higher intrinsic optical luminosity. From the analysis of the optical properties of the radio sources as function of the radio flux, we found that while about 35% of the radio sources are optically unidentified in the higher radio flux bin (S> 1.0 mJy), the percentage of unidentified sources decreases to about 25% in the faintest bins (S< 0.5 mJy). The median IAB magnitude for the total sample of radio sources, i.e. including also the unidentified ones, is brighter in the faintest radio bins than in the bin with higher radio flux. This suggests that most of the faintest radio sources are likely to be associated to relatively lower radio luminosity objects at relatively modest redshift, rather than radio-powerful, AGN type objects at high redshift. Using a classification in early-type and late-type galaxies based on the (B-I)AB color and the photometric redshift, we found that the majority of the radio sources below ~0.15 mJy are indeed late-type star forming galaxies. Finally, the radio sources without optical counterpart in our deep imaging have a median radio flux of 0.15 mJy, equal to that of identified sources. Given the very faint optical limits, these unidentified radio sources probably contain a significant fraction of obscured and/or high redshift galaxies.
Published: 2005
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28. The B3-VLA CSS sample . IV. kp-scale polarization properties

Author: M. Vigotti, Matteo Murgia, C. Fanti, L. Gregorini, C. Stanghellini, Daniele Dallacasa, M. Branchesi, R. Fanti, W. D. Cotton, FANTI C., BRANCHESI M., COTTON W.D., DALLACASA D., FANTI R., GREGORINI L., MURGIA M., STANGHELLINI C., and VIGOTTI M.
Subjects: Physics, Brewster's angle, Active galactic nucleus, Radio galaxy, media_common.quotation_subject, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Polarization (waves), Asymmetry, law.invention, symbols.namesake, Wavelength, Space and Planetary Science, law, Faraday effect, symbols, Faraday cage, Astrophysics::Galaxy Astrophysics, media_common
Abstract: We discuss VLA polarization measurements at 8.5, 4.9 and 1.4 GHz for the B3-VLA sample of Compact Steep-spectrum Sources (CSS). The measurements at the two higher frequencies were presented in a previous paper (Fanti et al. [CITE]), while those at 1.4 GHz are from the NVSS. The study of the fractional polarization as a function of wavelength shows a variety of behaviours not always accounted for by the current simple models. In a large fraction of sources the integrated rotation angle appears to follow the $\lambda^2$ law down to 1.4 GHz, although this conclusion has to be treated with some care due to the small number of polarization measurements. For sources resolved at the two higher frequencies we find that a number exhibit asymmetries in the 8.5 GHz fractional polarization, in depolarization and rotation angle. We discuss depolarization effects and rotation of the polarization angle. We find that Faraday depth effects are very strong within 2-3 kpc of the nucleus, as found earlier by Cotton et al. ([CITE]). A simple model for an external Faraday screen is able to account for the gross observed features. We also find that the Rotation Measure and the Faraday Dispersion appear to increase with the source red-shift.
Published: 2004

29. The VLA-VIRMOS Deep Field I. Radio observations probing the microJy source population

Author: M. Bondi, P. Ciliegi, G. Zamorani, L. Gregorini, G. Vettolani, P. Parma, H. de Ruiter, O. Le Fevre, M. Arnaboldi, L. Guzzo, D. Maccagni, R. Scaramella, C. Adami, S. Bardelli, M. Bolzonella, D. Bottini, A. Cappi, S. Foucaud, P. Franzetti, B. Garilli, S. Gwyn, O. Ilbert, A. Iovino, V. Le Brun, B. Marano, C. Marinoni, H. J. McCracken, B. Meneux, A. Pollo, L. Pozzetti, M. Radovich, V. Ripepi, D. Rizzo, M. Scodeggio, L. Tresse, A. Zanichelli, E. Zucca, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES)
Subjects: Count distribution, Hubble Deep Field, Astrophysics::High Energy Astrophysical Phenomena, data analysis, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, radio continuum, Source Population, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], galaxies, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Very large array, 010308 nuclear & particles physics, Astrophysics (astro-ph), Bandwidth (signal processing), Astronomy and Astrophysics, Square degree, astronomy, Space and Planetary Science, Homogeneous, Data reduction
Abstract: We have conducted a deep survey (r.m.s noise 17 microJy) with the Very Large Array (VLA) at 1.4 GHz, with a resolution of 6 arcsec, of a 1 square degree region included in the VIRMOS VLT Deep Survey. In the same field we already have multiband photometry down to I(AB)=25, and spectroscopic observations will be obtained during the VIRMOS VLT survey. The homogeneous sensitivity over the whole field has allowed to derive a complete sample of 1054 radio sources (5 sigma limit). We give a detailed description of the data reduction and of the analysis of the radio observations, with particular care to the effects of clean bias and bandwidth smearing, and of the methods used to obtain the catalogue of radio sources. To estimate the effect of the resolution bias on our observations we have modelled the effective angular-size distribution of the sources in our sample and we have used this distribution to simulate a sample of radio sources. Finally we present the radio count distribution down to 0.08 mJy derived from the catalogue. Our counts are in good agreement with the best fit derived from earlier surveys, and are about 50 % higher than the counts in the HDF. The radio count distribution clearly shows, with extremely good statistics, the change in the slope for the sub-mJy radio sources., Comment: 13 pages, Accepted for publication in Astronomy & Astrophysics
Published: 2003

30. Radio continuum and CO emission in star-forming galaxies

Author: Matteo Murgia, A. Crapsi, L. Gregorini, Luca Moscadelli, and ITA
Subjects: NRAO VLA Sky Survey, Physics, Spiral galaxy, Star formation, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Continuum (design consultancy), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Star (graph theory), Galaxy, Luminosity, Stars, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We combine the radio continuum images from the NRAO VLA Sky Survey with the CO-line observations from the extragalactic CO survey of the Five College Radio Astronomy Observatory to study the relationship between molecular gas and the star formation rate within the disks of 180 spiral galaxies at 45" resolution. We find a tight correlation between these quantities. On average, the ratio between the radio continuum and the CO emission is constant, within a factor of 3, both inside the same galaxy and from galaxy to galaxy. The mean star formation efficiency deduced from the radio continuum corresponds to convert 3.5% of the available molecular gas into stars on a time scale of 10^8 yr and depends weakly on general galaxy properties, such as Hubble type or nuclear activity. A comparison is made with another similar analysis performed using the H_alpha luminosity as star formation indicator. The overall agreement we find between the two studies reinforces the use of the radio luminosity as star formation rate indicator not only on global but also on local scales., 14 pages, 14 ps figures, A&A in press. Changes: x-axis scale in right panels of figs. 2 and 3 corrected
Published: 2002

31. The ATESP Radio Survey I. Survey Description, Observations and Data Reduction

Author: L. Gregorini, H. R. de Ruiter, Mark H. Wieringa, Ronald D. Ekers, G. Vettolani, P. Parma, and Isabella Prandoni
Subjects: Physics, Astrophysics (astro-ph), General Physics and Astronomy, FOS: Physical sciences, Astrophysics, Redshift survey, Galaxy, law.invention, Telescope, law, Optimal combination, Noise level, Remote sensing, Data reduction
Abstract: This paper is the first of a series reporting the results of the Australia Telescope ESO Slice Project (ATESP) radio survey obtained at 1400 MHz with the Australia Telescope Compact Array (ATCA) close to the South Galactic Pole (SGP) over the region covered by the ESO Slice Project (ESP) galaxy redshift survey (decl. ~ -40 degr). The survey consists of 16 radio mosaics with ~8"x14" resolution and uniform sensitivity (1sigma noise level ~79 microJy) over an area of ~26 sq.degrees. Here we present the design of the survey, we describe the mosaic observing technique which was used to obtain an optimal combination of uniform and high sensitivity over the whole area, and the data reduction: the problems encountered and the solutions adopted., 9 pages, 4 Postscript figures and 1 JPEG figure. Accepted for publication in A&A Suppl. Corrected typos and added Journal Reference
Published: 2000

32. Multi-Frequency Study of the B3--VLA Sample. I. 10.6-GHz Data

Author: K.-H. Mack, J. Zoennchen, L. Gregorini, Uli Klein, and M. Vigotti
Subjects: Physics, Spectral database, Quality (physics), Homogeneous, Astrophysics (astro-ph), Continuum (design consultancy), Range (statistics), FOS: Physical sciences, General Physics and Astronomy, Astrophysics, Sample (graphics), Large sample
Abstract: We present radio continuum data for 1050 B3 radio sources at 10.6 GHz. These sources constitute the B3-VLA sample which is complete down to 100 mJy at 408 MHz. The aim is the construction of a homogeneous spectral database for a large sample of radio sources, 10 times fainter than the K"uhr et al. (1981) sample, in the range 151 MHz to 10.6 GHz. Extended and complex radio sources (53) were mapped; the remaining ones were observed with cross-scans. We detected 99 % of the radio sources with a flux density error of about 1 mJy for the fainter ones. The analysis of the quality of the 10.6 GHz data is presented., 13 pages, 6 Postscript figures, 3 additional LaTeX tables, uses epsf.sty and l-aa.sty; accepted for publication in Astron. & Astrophys. Suppl. Series; complete postscript version also available at http://multivac.jb.man.ac.uk:8000/ceres/papers/papers.html
Published: 1998

33. Analysis of Optical Transition Radiation Emitted by a 1 MeV Electron Beam and its Possible Use as Diagnostic Tool

Author: F. Tazzioli, S. Tazzari, Massimo Ferrario, S. Kulinski, M. Minestrini, L. Gregorini, P. Patteri, L. Catani, and M. G. Castellano
Subjects: Physics, Nuclear and High Energy Physics, business.industry, Optical transition, Boundary (topology), Radiation, Low energy, Optics, Cathode ray, Physics::Accelerator Physics, Detectors and Experimental Techniques, business, Instrumentation, Beam (structure)
Abstract: The main features of optical transition radiation (OTR) backward emitted by a 1 MeV electron beam crossing a vacuum-to-metal boundary are presented. The possible use of OTR as a diagnostic tool for such a low energy beam is discussed, and some preliminary experimental data are presented.
Published: 1994
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34. Observations of a nearby filament of galaxy clusters with the Sardinia Radio Telescope

Author: F. de Gasperin, Rosita Paladino, Matteo Murgia, Claudio Gheller, Tracy E. Clarke, Gianni Bernardi, Emanuela Orrú, Sergio Poppi, Gabriele Giovannini, V. Vacca, Luigina Feretti, G. B. Taylor, Melanie Johnston-Hollitt, L. Gregorini, Federica Govoni, Franco Vazza, Chiara Ferrari, M. Brienza, Fabio Gastaldello, H. Junklewitz, Marisa Girardi, Alexis Finoguenov, Raimondo Concu, Richard A. Perley, Ettore Carretti, G. Valente, Torsten A. Enßlin, Walter Boschin, Andrea Melis, P. Parma, F. Loi, S. Colafrancesco, Department of Physics, Joseph Louis LAGRANGE (LAGRANGE), 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), Vacca, V, Murgia, M, Govoni, F, Loi, F, Vazza, F, Finoguenov, A, Carretti, E, Feretti, L, Giovannini, G, Concu, R, Melis, A, Gheller, C, Paladino, R, Poppi, S, Valente, G, Bernardi, G, Boschin, W, Brienza, M, Clarke, T E, Colafrancesco, S, Enßlin, T A, Ferrari, C, de Gasperin, F, Gastaldello, F, Girardi, M, Gregorini, L, Johnston-Hollitt, M, Junklewitz, H, Orrù, E, Parma, P, Perley, R, Taylor, G B, DIP. DI ASTRONOMIA, DIP. DI DISCIPLINE GIURIDICHE DELL'ECONOMIA E DELL'AZIENDA, DIPARTIMENTO DI FISICA E ASTRONOMIA 'AUGUSTO RIGHI', Facolta' di SCIENZE MATEMATICHE FISICHE e NATURALI, Da definire, AREA MIN. 02 - Scienze fisiche, 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), and De gasperin, F
Subjects: Radio galaxy, magnetic field, magnetic fields, 01 natural sciences, VLA SKY SURVEY, 010303 astronomy & astrophysics, acceleration of particle, SCALE, media_common, acceleration of particles, Physics, BARYONS, galaxies: clusters: intracluster medium, cosmology: observations, large-scale structure of Universe, clusters: intracluster medium [galaxies], LOW-FREQUENCY, large-scale structure of Universe, Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, observations, large-scale structure of Universe [cosmology], Astrophysics::Cosmology and Extragalactic Astrophysics, Low frequency, MAGNETIC-FIELDS, COSMIC FILAMENTS, Radio telescope, 0103 physical sciences, Galaxy cluster, Astrophysics::Galaxy Astrophysics, NRAO VLA Sky Survey, SPECTRUM, 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, 115 Astronomy, Space science, Astrophysics - Astrophysics of Galaxies, Galaxy, EVOLUTION, acceleration of particles, magnetic fields, galaxies: clusters: intracluster medium, cosmology: observations, large-scale structure of Universe, Radio halo, Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA), cosmology: observations, galaxies: clusters medium, ABELL, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], EMISSION
Abstract: We report the detection of diffuse radio emission which might be connected to a large-scale filament of the cosmic web covering a 8deg x 8deg area in the sky, likely associated with a z~0.1 over-density traced by nine massive galaxy clusters. In this work, we present radio observations of this region taken with the Sardinia Radio Telescope. Two of the clusters in the field host a powerful radio halo sustained by violent ongoing mergers and provide direct proof of intra-cluster magnetic fields. In order to investigate the presence of large-scale diffuse radio synchrotron emission in and beyond the galaxy clusters in this complex system, we combined the data taken at 1.4 GHz obtained with the Sardinia Radio Telescope with higher resolution data taken with the NRAO VLA Sky Survey. We found 28 candidate new sources with a size larger and X-ray emission fainter than known diffuse large-scale synchrotron cluster sources for a given radio power. This new population is potentially the tip of the iceberg of a class of diffuse large-scale synchrotron sources associated with the filaments of the cosmic web. In addition, we found in the field a candidate new giant radio galaxy., 35 pages, 30 figures, MNRAS Accepted, A high-resolution version of the paper can be found at the link http://erg.oa-cagliari.inaf.it/preprints/paper_filament.pdf
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35. The VIMOS-VLT Deep Survey: evolution in the halo occupation number since z ~ 1

Author: Abbas, U., Torre, S., Le Fèvre, O., Guzzo, L., Marinoni, C., Meneux, B., Pollo, A., Zamorani, G., Bottini, D., Garilli, B., Le Brun, V., Maccagni, D., Scaramella, R., Scodeggio, M., Tresse, L., Vettolani, G., Zanichelli, A., Adami, C., Arnouts, S., Bardelli, S., Bolzonella, M., Cappi, A., Charlot, S., Ciliegi, P., Contini, T., Foucaud, S., Franzetti, P., Gavignaud, I., Ilbert, O., Iovino, A., Lamareille, F., Mccracken, H.~j., Marano, B., Mazure, A., Merighi, R., Paltani, S., Pellò, R., Pozzetti, L., Radovich, M., Vergani, D., Zucca, E., Bondi, M., Bongiorno, A., Brinchmann, J., Cucciati, O., Ravel, L., Gregorini, L., Perez-Montero, E., Mellier, Y., Merluzzi, P., Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Abbas U., de la Torre S., Le Fèvre O., Guzzo L., Marinoni C., Meneux B., Pollo A., Zamorani G., Bottini D., Garilli B., and Le brun V., Maccagni D., Scaramella R., Scodeggio M., Tresse L., Vettolani G., Zanichelli A., Adami C., Arnouts S., Bardelli S., Bolzonella M., Cappi A., Charlot S., Ciliegi P., Contini T., Foucaud S., Franzetti P., Gavignaud I., Ilbert O., Iovini A., Lamareille F., McCracken H.J., Marano B., Mazure A., Merighi R., Paltani S., Pello' R., Pozzetti L., Radovich M., Vergani D., Zucca E., Bondi M., Bongiorno A., Brinchmann ., Cucciati P., de Ravel L., Gregorini L., Perez-Montero E., Mellier Y., Merluzzi P.
Subjects: methods: statistical, surveys, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], galaxies: high-redshift, [INFO]Computer Science [cs], Astrophysics::Cosmology and Extragalactic Astrophysics, LARGE-SCALE STRUCTURE OF NIVERSE, large-scale structure of Universe, GALAXIES:HIGH-REDSHIFT, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, METHOD: STATISTICAL
Abstract: We model the evolution of the mean galaxy occupation of dark matter haloes over the range 0.1 < z < 1.3, using the data from the VIMOS-VLT Deep Survey. The galaxy projected correlation function wp(rp) was computed for a set of luminosity-limited subsamples and fits to its shape were obtained using two variants of halo occupation distribution (HOD) models. These provide us with a set of best-fitting parameters, from which we obtain the average mass of a halo and average number of galaxies per halo. We find that after accounting for the evolution in luminosity and assuming that we are largely following the same population, the underlying dark matter halo shows a growth in mass with decreasing redshift as expected in a hierarchical structure formation scenario. Using two different HOD models, we see that the halo mass grows by 90 per cent over the redshift interval z = [0.5, 1.0]. This is the first time the evolution in halo mass at high redshifts has been obtained from a single data survey and it follows the simple form seen in N-body simulations with M(z) = M0 e-βz, and β = 1.3 +/- 0.30. This provides evidence for a rapid accretion phase of massive haloes having a present-day mass M0 ~ 1013.5 h-1 Msolar, with a m > 0.1 M0 merger event occurring between redshifts of 0.5 and 1.0. Furthermore, we find that more luminous galaxies are found to occupy more massive haloes irrespective of the redshift. Finally, the average number of galaxies per halo shows little increase from redshift z ~ 1.0 to ~0.5, with a sharp increase by a factor of ~3 from z ~ 0.5 to ~0.1, likely due to the dynamical friction of subhaloes within their host haloes. Based on data obtained with the European Southern Observatory Very Large Telescope, Paranal, Chile, program 070.A-9007(A), and on data obtained at the Canada-France-Hawaii Telescope, operated by the CNRS of France, CNRC in Canada and the University of Hawaii.
Published: 2010
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36. Peri-interventional coronary vasomotion.

Author: Gregorini L, Marco J, and Heusch G
Subjects: Angioplasty, Balloon, Coronary, Humans, No-Reflow Phenomenon therapy, Sympathetic Nervous System metabolism, Sympathetic Nervous System physiopathology, Coronary Circulation physiology, No-Reflow Phenomenon physiopathology
Abstract: A percutaneous coronary intervention (PCI) is a unique condition to study the effects of ischemia and reperfusion in patients with severe coronary atherosclerosis when coronary vasomotor function is compromised by loss of endothelial and autoregulatory vasodilation. We studied the effects of intracoronary non-selective α-, as well as selective α(1)- and α(2)-blockade in counteracting the observed vasoconstriction in patients with stable and unstable angina and in patients with acute myocardial infarction. Coronary vasoconstriction in our studies was a diffuse phenomenon and involved not only the culprit lesion but also vessels with angiographically not visible plaques. Post-PCI vasoconstriction was reflected by increased coronary vascular resistance and associated with decreased LV-function. α (1)-Blockade with urapidil dilated epicardial coronary arteries, improved coronary flow reserve and counteracted LV dysfunction. Non-selective α-blockade with phentolamine induced epicardial and microvascular dilation, while selective α(2)-blockade with yohimbine had only minor vasodilator and functional effects. Intracoronary α-blockade also attenuated the no-reflow phenomenon following primary PCI. This article is part of a Special Issue entitled "Coronary Blood Flow"., (Copyright © 2011 Elsevier Ltd. All rights reserved.)
Published: 2012
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37. Non infective severe aortic paravalvular leakage 7 years after surgery: the role of suture technique.

Author: Agrifoglio M, Filippini S, Roberto M, Zanobini M, Gregorini L, and Alamanni F
Subjects: Aortic Valve surgery, Aortic Valve Insufficiency diagnosis, Aortic Valve Insufficiency etiology, Humans, Male, Middle Aged, Reoperation, Aortic Aneurysm, Thoracic surgery, Aortic Valve Insufficiency surgery, Heart Valve Prosthesis, Postoperative Complications surgery, Suture Techniques
Abstract: We report a case of redo aortic prosthesis replacement for a severe paravalvular leak (PVL) in a man operated with continuous suture technique 7 years earlier. The severe aortic regurgitation was due to the rupture of the suture. In spite of operations to replace malfunctioning heart valves are common procedures and performed all over the world from more than 50 years, there is still an open debate about the most suitable suture technique. In this case report, we'll discuss if the suture technique has a role in preventing or leading complications as severe PVL.
Published: 2011
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38. Proteomics reveals novel oxidative and glycolytic mechanisms in type 1 diabetic patients' skin which are normalized by kidney-pancreas transplantation.

Author: Folli F, Guzzi V, Perego L, Coletta DK, Finzi G, Placidi C, La Rosa S, Capella C, Socci C, Lauro D, Tripathy D, Jenkinson C, Paroni R, Orsenigo E, Cighetti G, Gregorini L, Staudacher C, Secchi A, Bachi A, Brownlee M, and Fiorina P
Subjects: Adult, Case-Control Studies, Diabetes Mellitus, Type 1 therapy, Female, Glycolysis, Humans, Kidney Failure, Chronic metabolism, Male, Middle Aged, Spectrometry, Mass, Matrix-Assisted Laser Desorption-Ionization, Diabetes Mellitus, Type 1 metabolism, Gene Expression Regulation, Kidney Transplantation methods, Oxygen chemistry, Pancreas Transplantation methods, Proteomics methods, Skin metabolism
Abstract: Background: In type 1 diabetes (T1D) vascular complications such as accelerated atherosclerosis and diffused macro-/microangiopathy are linked to chronic hyperglycemia with a mechanism that is not yet well understood. End-stage renal disease (ESRD) worsens most diabetic complications, particularly, the risk of morbidity and mortality from cardiovascular disease is increased several fold., Methods and Findings: We evaluated protein regulation and expression in skin biopsies obtained from T1D patients with and without ESRD, to identify pathways of persistent cellular changes linked to diabetic vascular disease. We therefore examined pathways that may be normalized by restoration of normoglycemia with kidney-pancreas (KP) transplantation. Using proteomic and ultrastructural approaches, multiple alterations in the expression of proteins involved in oxidative stress (catalase, superoxide dismutase 1, Hsp27, Hsp60, ATP synthase delta chain, and flavin reductase), aerobic and anaerobic glycolysis (ACBP, pyruvate kinase muscle isozyme, and phosphoglycerate kinase 1), and intracellular signaling (stratifin-14-3-3, S100-calcyclin, cathepsin, and PPI rotamase) as well as endothelial vascular abnormalities were identified in T1D and T1D+ESRD patients. These abnormalities were reversed after KP transplant. Increased plasma levels of malondialdehyde were observed in T1D and T1D+ESRD patients, confirming increased oxidative stress which was normalized after KP transplant., Conclusions: Our data suggests persistent cellular changes of anti-oxidative machinery and of aerobic/anaerobic glycolysis are present in T1D and T1D+ESRD patients, and these abnormalities may play a key role in the pathogenesis of hyperglycemia-related vascular complications. Restoration of normoglycemia and removal of uremia with KP transplant can correct these abnormalities. Some of these identified pathways may become potential therapeutic targets for a new generation of drugs.
Published: 2010
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39. Disproportionate hyperproinsulinemia, beta-cell restricted prohormone convertase 2 deficiency, and cell cycle inhibitors expression by human islets transplanted into athymic nude mice: insights into nonimmune-mediated mechanisms of delayed islet graft failure.

Author: Davalli AM, Perego L, Bertuzzi F, Finzi G, La Rosa S, Blau A, Placidi C, Nano R, Gregorini L, Perego C, Capella C, and Folli F
Subjects: Animals, Autopsy, Humans, Insulin-Secreting Cells cytology, Insulin-Secreting Cells enzymology, Insulin-Secreting Cells pathology, Islets of Langerhans pathology, Islets of Langerhans Transplantation pathology, Male, Mice, Mice, Nude, Pancreas pathology, Proinsulin blood, Reference Values, Treatment Failure, Cell Cycle physiology, Diabetes Mellitus, Experimental surgery, Hyperinsulinism etiology, Islets of Langerhans enzymology, Islets of Langerhans metabolism, Islets of Langerhans Transplantation adverse effects, Proinsulin metabolism, Proprotein Convertase 2 deficiency, Transplantation, Heterologous adverse effects
Abstract: To learn more about nonimmune-mediated islet graft failure, we transplanted different preparations (preps) of isolated human islets under the kidney capsule of streptozotocin (STZ)-diabetic nude mice. One month after the implantation of 1,000 or 2,000 islets, grafts were harvested for morphological, immunohistochemical, and ultrastructural analysis. Only a single islet prep cured the diabetes out of all the recipients, while the remaining preps showed only partial function after the implantation of 2,000 islets. Transplanted mice showed high circulating proinsulin levels but, with the exclusion of those bearing curative grafts, relatively low mature insulin levels. Engrafted beta-cells showed positive carboxypeptidase E (CPE) and prohormone convertase 1 (PC1) staining, while prohormone convertase 2 (PC2) was undetectable. In contrast, PC2 was abundantly expressed by engrafted alpha-cells. Moreover, engrafted beta-cells did not show evidence of replication, and preapoptotic beta-cells, with intra- and extracellular amyloid deposition, were detected with electron microscopy. Cell cycle inhibitors p16(INK4), p21(WAF1), and p27(Kip1) were abundantly expressed in the islet grafts and showed a predominant nuclear localization. In conclusion, diabetic nude mice transplanted with human islets showed disproportionate hyperproinsulinemia and graft evidence of beta-cell restricted PC2 depletion, amyloid deposition and beta-cell death, and lack of beta-cell replication with nuclear translocation of p27(Kip1) and p21(WAF1) that together may contribute to delayed graft failure.
Published: 2008
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40. A large population of galaxies 9 to 12 billion years back in the history of the Universe.

Author: Le Fèvre O, Paltani S, Arnouts S, Charlot S, Foucaud S, Ilbert O, McCracken HJ, Zamorani G, Bottini D, Garilli B, Le Brun V, Maccagni D, Picat JP, Scaramella R, Scodeggio M, Tresse L, Vettolani G, Zanichelli A, Adami C, Bardelli S, Bolzonella M, Cappi A, Ciliegi P, Contini T, Franzetti P, Gavignaud I, Guzzo L, Iovino A, Marano B, Marinoni C, Mazure A, Meneux B, Merighi R, Pellò R, Pollo A, Pozzetti L, Radovich M, Zucca E, Arnaboldi M, Bondi M, Bongiorno A, Busarello G, Gregorini L, Lamareille F, Mathez G, Mellier Y, Merluzzi P, Ripepi V, and Rizzo D
Abstract: To understand the evolution of galaxies, we need to know as accurately as possible how many galaxies were present in the Universe at different epochs. Galaxies in the young Universe have hitherto mainly been identified using their expected optical colours, but this leaves open the possibility that a significant population remains undetected because their colours are the result of a complex mix of stars, gas, dust or active galactic nuclei. Here we report the results of a flux-limited I-band survey of galaxies at look-back times of 9 to 12 billion years. We find 970 galaxies with spectroscopic redshifts between 1.4 and 5. This population is 1.6 to 6.2 times larger than previous estimates, with the difference increasing towards brighter magnitudes. Strong ultraviolet continua (in the rest frame of the galaxies) indicate vigorous star formation rates of more than 10-100 solar masses per year. As a consequence, the cosmic star formation rate representing the volume-averaged production of stars is higher than previously measured at redshifts of 3 to 4.
Published: 2005
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41. Impaired bradykinin response to ischaemia and exercise in patients with mild congestive heart failure during angiotensin-converting enzyme treatment. Relationships with endothelial function, coagulation and inflammation.

Author: Cugno M, Agostoni P, Mari D, Meroni PL, Gregorini L, Bussotti M, Anguissola GB, Donatelli F, and Nussberger J
Subjects: Adult, Biomarkers blood, Blood Coagulation Factors analysis, Brachial Artery diagnostic imaging, Case-Control Studies, Endothelium, Vascular physiopathology, Factor XIIa analysis, Heart Failure physiopathology, Humans, Interleukin-6 blood, Ischemia physiopathology, Male, Middle Aged, Receptors, Tumor Necrosis Factor, Type II blood, Tissue Plasminogen Activator analysis, Ultrasonography, Vasodilation, von Willebrand Factor analysis, Angiotensin-Converting Enzyme Inhibitors therapeutic use, Bradykinin blood, Exercise, Heart Failure blood, Heart Failure drug therapy, Lisinopril therapeutic use
Abstract: Inflammation and endothelial dysfunction play important roles in the pathophysiology of congestive heart failure (CHF), and the peptide bradykinin, generated during inflammation, may act as a defence mechanism by inducing vasodilation. Plasma bradykinin levels are increased in experimental heart failure but low in patients with advanced chronic CHF despite treatment with angiotensin-converting enzyme (ACE) inhibitors. It is not currently known how bradykinin behaves in less severe phases of CHF controlled by long-term ACE inhibitor treatment. We studied 10 male patients with clinically stable chronic CHF [New York Heart Association (NYHA) class II] on long-term ACE inhibitor treatment and 10 normal sex- and age-matched control subjects. High performance liquid chromatography/radioimmunoassay methods were used to evaluate plasma levels of bradykinin in relation to an array of parameters of endothelial function, coagulation and inflammation before and after stimuli of forearm arterial occlusion and physical exercise. CHF patients had higher levels of bradykinin (P = 0.008), activated factor XII (P = 0.049), interleukin-6 (P = 0.050) and tumour necrosis factor receptor II (sTNFRII) (P = 0.026) than controls. Arterial occlusion and exercise significantly increased bradykinin and von Willebrand factor levels in controls but not in CHF patients. The increase in brachial artery diameter after arterial occlusion was less in CHF patients (P = 0.036) and inversely related to baseline plasma levels of bradykinin (r = -0.855, P = 0.002) and sTNFRII (r = -0.780, P = 0.008). NYHA class II CHF patients during long-term treatment with ACE inhibitors have increased bradykinin levels and signs of inflammation. They are unable to respond adequately to stimuli of ischaemia and physical exercise which both require vasodilation.
Published: 2005
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42. Haemostatic and inflammatory biomarkers in advanced chronic heart failure: role of oral anticoagulants and successful heart transplantation.

Author: Cugno M, Mari D, Meroni PL, Gronda E, Vicari F, Frigerio M, Coppola R, Bottasso B, Borghi MO, and Gregorini L
Subjects: Adult, Aged, Antithrombin III analysis, Biomarkers blood, Carrier Proteins blood, Case-Control Studies, Female, Fibrin Fibrinogen Degradation Products analysis, Fibrinogen analysis, Heart Failure therapy, Humans, Intercellular Adhesion Molecule-1 blood, Interleukin-6 blood, Male, Middle Aged, Peptide Hydrolases analysis, Plasminogen Activator Inhibitor 1 analysis, Postoperative Period, TNF Receptor-Associated Factor 2, Thrombomodulin analysis, Tissue Plasminogen Activator analysis, Tumor Necrosis Factor-alpha analysis, Vascular Cell Adhesion Molecule-1 blood, von Willebrand Factor analysis, Anticoagulants therapeutic use, Heart Failure blood, Heart Failure immunology, Heart Transplantation, Tumor Necrosis Factor Receptor-Associated Peptides and Proteins
Abstract: Advanced chronic heart failure (CHF) is associated with abnormal haemostasis and inflammation, but it is not known how these abnormalities are related, whether they are modified by oral anticoagulants (OAT), or if they persist after successful heart transplantation. We studied 25 patients with CHF (New York Heart Association class IV, 10 of whom underwent heart transplantation) and 25 age- and sex-matched healthy controls by measuring their plasma levels of prothrombin fragment 1 + 2 (F1 + 2), thrombin-antithrombin (TAT) complexes, tissue plasminogen activator (t-PA), plasminogen activator inhibitor-1 (PAI-1), D-dimer, factor VII (FVII), fibrinogen, von Willebrand factor (VWF), tumour necrosis factor (TNF), soluble TNF receptor II (sTNFRII), interleukin 6 (IL-6), soluble intercellular adhesion molecule-1 (sICAM-1), soluble vascular cell adhesion molecule-1 (sVCAM-1), endothelial-selectin (E-selectin) and thrombomodulin. CHF patients had higher plasma levels of TAT, D-dimer, t-PA, fibrinogen, VWF, TNF, IL-6, sTNFRII, sVCAM-1 (P = 0.0001), sICAM-1 (P = 0.003) and thrombomodulin (P = 0.007) than controls. There were significant correlations (r = 0.414-0.595) between coagulation, fibrinolysis, endothelial dysfunction and inflammation parameters, which were lower in those patients treated with OATs. Heart transplantation led to reductions in fibrinogen (P = 0.001), VWF (P = 0.05), D-dimer (P = 0.05) and IL-6 levels (P = 0.05), but all the parameters remained significantly higher (P = 0.01-0.0001) than in the controls. Advanced CHF is associated with coagulation activation, endothelial dysfunction and increased proinflammatory cytokine levels. Most of these abnormalities parallel each other, tend to normalize in patients treated with OATs and, although reduced, persist in patients undergoing successful heart transplantation, despite the absence of clinical signs of CHF.
Published: 2004
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43. The alpha1-adrenergic blocker urapidil improves contractile function in patients 3 months after coronary stenting: a randomized, double-blinded study.

Author: Kozàkovà M, Marco J, Heusch G, Bernies M, Bossi IM, Palombo C, Anguissola GB, Donatelli F, Laurent JP, and Gregorini L
Subjects: Adrenergic alpha-Antagonists pharmacology, Adult, Aged, Angina Pectoris drug therapy, Angina Pectoris physiopathology, Angioplasty, Balloon, Coronary, Double-Blind Method, Female, Humans, Male, Middle Aged, Myocardial Contraction drug effects, Piperazines pharmacology, Ventricular Dysfunction, Left drug therapy, Adrenergic alpha-Antagonists therapeutic use, Angina Pectoris therapy, Piperazines therapeutic use, Stents, Stroke Volume drug effects
Abstract: Background: The recovery of left ventricular function (LVF) after revascularization takes time. alpha-Adrenergic blockade acutely improves coronary blood flow and LVF, whereas the effects of more prolonged alpha-adrenergic blockade on LVF recovery after stenting are unknown., Methods: In 32 patients (age 58 +/- 12 y) with an 82% +/- 6% stenosis, ejection fraction (EF) and systolic thickening (%Th) were measured by transthoracic echocardiography before and 30 minutes to 2 hours after revascularization. In a double-blinded protocol, either 200 microg/kg urapidil or placebo was given intravenously, and LVF was measured 10 minutes later. Two hours later, oral treatment with 30 mg/d drug or placebo was started, and LVF measured again after 24 hours and 3 months., Results: Before revascularization, EF was 49.4% +/- 8.5% (+/-SD) and 51.3% +/- 8.8% in the urapidil-treated and the placebo groups, respectively. Thirty minutes to 2 hours after coronary stenting, EF was unchanged. After intravenous drug administration, EF increased to 56.5% +/- 9.7%). At 24 hours and 3 months after revascularization, EF became 59.5% +/- 7.9% and 59.6% +/- 8.2% in the urapidil-treated group, respectively, whereas EF in the placebo group did not change (50.4% +/- 5.7% and 49.7% +/- 4.9%, respectively). Revascularization did not acutely improve %Th. Intravenous urapidil improved %Th from 31.4% +/- 17.6% to 44.2% +/- 11.6%, whereas there was no change in the placebo group. At 3 months, %Th was 49.5% +/- 12.9% in the urapidil-treated group and 39.7% +/- 8.9% in the placebo group., Conclusions: These data suggest that long-term alpha-adrenergic blockade might improve LVF at midterm after coronary revascularization.
Published: 2004
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44. Effects of selective alpha1- and alpha2-adrenergic blockade on coronary flow reserve after coronary stenting.

Author: Gregorini L, Marco J, Farah B, Bernies M, Palombo C, Kozàkovà M, Bossi IM, Cassagneau B, Fajadet J, Di Mario C, Albiero R, Cugno M, Grossi A, and Heusch G
Subjects: Adenosine adverse effects, Blood Flow Velocity drug effects, Blood Pressure drug effects, Coronary Angiography, Coronary Disease diagnostic imaging, Coronary Disease physiopathology, Coronary Disease surgery, Coronary Vessels physiopathology, Coronary Vessels surgery, Female, Heart Rate drug effects, Humans, Male, Middle Aged, Piperazines pharmacology, Vascular Patency drug effects, Yohimbine pharmacology, Adrenergic alpha-1 Receptor Antagonists, Adrenergic alpha-2 Receptor Antagonists, Adrenergic alpha-Antagonists pharmacology, Coronary Circulation drug effects, Coronary Vessels drug effects, Stents
Abstract: Background: Coronary flow reserve (CFR) is not normalized shortly after coronary stenting. We hypothesized that alpha-adrenergic coronary vasoconstriction acts to limit CFR., Methods and Results: We assessed flow velocity by Doppler wires and cross-sectional area by angiography in 46 patients undergoing coronary culprit lesion stenting (81+/-4% stenosis). Hyperemia was induced by adenosine (24 micro g IC or 140 micro g/kg per minute IV) before and after stenting. Finally, either the alpha(1)-antagonist urapidil (10 mg IC) or the alpha(2)-antagonist yohimbine (3 mg IC) was randomly combined with adenosine. In 8 subjects with angiographically normal coronary arteries, CFR was increased from 3.21+/-0.30 to 3.74+/-0.43 by yohimbine and to 4.58+/-0.65 by urapidil, respectively (P=0.0001). Patients were divided according to the cutoff of CFR > or =3.0 (n=18) or <2.5 (n=28). Revascularization per se did not change CFR. However, 15 minutes after stenting, CFR decreased to 2.05+/-0.55 from CFR 3.64+/-0.58, whereas in patients with CFR 2.39+/-0.51, it remained unchanged. Yohimbine improved CFR to 3.26+/-0.42 and to 3.41+/-0.58 in patients with >3.0 and <2.05+/-0.55 baseline CFR, respectively. Urapidil improved CFR to 3.52+/-0.30 and 3.98+/-1.07, respectively., Conclusions: Urapidil and yohimbine attenuated the CFR impairment occurring after revascularization by increasing both the epicardial vasodilator effect of adenosine and the blood flow velocity, thus suggesting that the adrenergic system plays an important role in limiting the capacity of the coronary circulation to dilate.
Published: 2002
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45. Limitation of coronary reserve after successful angioplasty is prevented by oral pretreatment with an alpha1-adrenergic antagonist.

Author: Rimoldi O, Spyrou N, Foale R, Hackett DR, Gregorini L, and Camici PG
Subjects: Administration, Oral, Adult, Aged, Double-Blind Method, Female, Humans, Male, Middle Aged, Adrenergic alpha-1 Receptor Antagonists, Adrenergic alpha-Antagonists pharmacology, Angioplasty, Balloon, Coronary, Coronary Circulation drug effects, Doxazosin pharmacology
Abstract: Coronary vasoconstriction that occurs after percutaneous transluminal coronary angioplasty (PTCA) is abolished by intracoronary phentolamine. An impairment of coronary vasodilator reserve (CVR) has been observed < or = 7 days after successful PTCA. To ascertain whether pretreatment with the alpha1-adrenergic receptor blocker doxazosin could prevent the limitation of CVR after PTCA, we carried out a randomised, double-blind, controlled study on 26 patients with significant (> 75%) single vessel disease undergoing PTCA. Twelve patients received doxazosin 4 mg daily in addition to their standard treatment, while 14 patients received matching placebo, starting 11 days before PTCA. Myocardial blood flow (MBF) at baseline and after i.v. dipyridamole (0.56 mg/kg) was measured within 5 days after PTCA using positron emission tomography (PET) with oxygen-15-labelled water. Angioplasty was successful in all patients with a residual stenosis < or = 35%. At PET scanning, hemodynamic parameters were comparable in the two groups. In the territory subtended by the dilated artery, CVR was significantly higher in patients treated with doxazosin compared with those receiving placebo (2.78 +/- 0.1.21 vs. 1.95 +/- 0.68; p < 0.01). Conversely, CVR in the remote territories subtended by angiographically normal arteries was similar in the two groups (2.53 +/- 0.92 and 2.48 +/- 0.80, respectively; p = NS). Treatment with oral doxazosin in addition to standard antianginal therapy can prevent the impairment of CVR frequently observed despite successful PTCA.
Published: 2000
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46. Coronary vasodilator capacity and epicardial vessel remodeling in physiological and hypertensive hypertrophy.

Author: Kozàkovà M, Galetta F, Gregorini L, Bigalli G, Franzoni F, Giusti C, and Palombo C
Subjects: Adult, Aged, Aging physiology, Analysis of Variance, Bicycling physiology, Blood Flow Velocity, Blood Pressure physiology, Coronary Vessels anatomy & histology, Coronary Vessels drug effects, Dipyridamole, Echocardiography, Transesophageal, Humans, Hypertrophy, Left Ventricular diagnostic imaging, Male, Middle Aged, Running physiology, Swimming physiology, Ultrasonography, Doppler, Color, Vasodilator Agents, Coronary Circulation physiology, Coronary Vessels physiology, Hypertrophy, Left Ventricular physiopathology, Physical Endurance physiology, Sports physiology
Abstract: The aim of this study was to compare resting coronary flow velocity, determinants of myocardial oxygen demand, and coronary vasodilator capacity in subjects with physiological, exercise-induced, and hypertensive left ventricular hypertrophy. Sixteen healthy sedentary men, 16 endurance athletes, and 16 hypertensive subjects (mean+/-SEM for left ventricular mass index: 94.9+/-5.5, 184.6+/-8.4, 154.4+/-9.5 g/m(2), respectively) were studied by transesophageal and transthoracic Doppler echocardiography. Coronary flow velocity in left anterior descending artery and cross-sectional area of left main artery were assessed at rest and during dipyridamole-induced vasodilation. Myocardial oxygen demand was estimated through rate-pressure product, left ventricular wall stress, and inotropic function. Coronary flow reserve and minimum coronary resistance were comparable to those of sedentary men in athletes (mean+/-SEM: 3. 23+/-0.16 versus 3.60+/-0.18 and 0.96+/-0.06 versus 1.04+/-0.04 mm Hg. s. cm(-1)), while in hypertensive subjects they were decreased and increased, respectively (mean+/-SEM: 2.31+/-0.08 and 1.21+/-0.10 mm Hg. s. cm(-1); P:<0.05 for both). Resting flow velocity was directly related to rate-pressure product in sedentary men and athletes and also to wall stress in athletes, while these correlations were absent in hypertensives. Dilation of left main artery after dipyridamole was significantly higher in athletes than in sedentary men and hypertensive subjects (mean+/-SEM for area change: 32.9+/-3.7% versus 12.8+/-2.5% and 6.4+/-3.3%; P:<0.05 and 0.01). These data indicate that vasodilator capacity of coronary microcirculation is not impaired in athletes with physiological hypertrophy, in contrast to hypertensive patients. The relationship between resting flow velocity and determinants of oxygen demand is preserved in physiological hypertrophy but missing in hypertensive hypertrophy. Furthermore, the vasodilator capacity of coronary macrocirculation is also enhanced in exercise-trained subjects.
Published: 2000
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47. Effect of aspirin and ticlopidine on plasma tissue factor levels in stable and unstable angina pectoris.

Author: Marco J, Ariëns RA, Fajadet J, Bossi IM, Marco I, Bernies M, Romano SM, Donatelli F, Brambilla GM, Somalvico F, Mari D, and Gregorini L
Subjects: Angina Pectoris blood, Angina Pectoris therapy, Angina, Unstable blood, Angina, Unstable therapy, Angioplasty, Balloon, Coronary, Antithrombin III metabolism, Aspirin administration & dosage, Atherectomy, Coronary, Drug Therapy, Combination, Female, Humans, Male, Middle Aged, Peptide Hydrolases metabolism, Platelet Aggregation Inhibitors administration & dosage, Premedication, Stents, Thromboplastin drug effects, Ticlopidine administration & dosage, Time Factors, Angina Pectoris drug therapy, Angina, Unstable drug therapy, Aspirin therapeutic use, Platelet Aggregation Inhibitors therapeutic use, Thromboplastin metabolism, Ticlopidine therapeutic use
Abstract: Patients with unstable angina have an increased activation of the coagulation system. Aspirin and ticlopidine given in combination may potentiate each other by the combination of different action mechanisms and may reduce the risk of coronary occlusion and clinical instability. Plasma tissue factor (TF) levels collected into the stenotic coronary artery may be an index of TF expression within the vasculature. In 160 patients undergoing angioplasty for a 81+/-5% coronary lesion, we measured TF in blood samples collected from a vein and from the coronary ostium. Immediately after and 10 minutes after the dilation procedures the samples were withdrawn also beyond the lesion. Heparin 150 U/kg was given as an anticoagulant. All patients were pretreated with 250 mg/day of aspirin. One hundred twenty patients were randomly assigned to receive 24, 48, or 72 hours of ticlopidine treatment (250 mg/twice daily). TF levels did not increase during angioplasty but there was a significantly higher TF expression in unstable than in stable patients, irrespective of the invasiveness of debulking procedures. When ticlopidine was given for 72 hours, TF levels were similar to normal laboratory values both in stable and unstable patients. This combined antiplatelet pretreatment may be of benefit in unstable angina patients, with a favorable cost/benefit ratio.
Published: 2000
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48. alpha-adrenergic coronary vasoconstriction and myocardial ischemia in humans.

Author: Heusch G, Baumgart D, Camici P, Chilian W, Gregorini L, Hess O, Indolfi C, and Rimoldi O
Subjects: Humans, Coronary Vessels physiopathology, Myocardial Ischemia physiopathology, Receptors, Adrenergic, alpha physiology, Vasoconstriction
Abstract: The use of quantitative coronary angiography, combined with Doppler and PET, has recently been directed at the study of alpha-adrenergic coronary vasomotion in humans. Confirming prior animal experiments, there is no evidence of alpha-adrenergic coronary constrictor tone at rest. Again confirming prior experiments, responses to alpha-adrenoceptor activation are augmented in the presence of coronary endothelial dysfunction and atherosclerosis, involving both alpha(1)- and alpha(2)-adrenoceptors in epicardial conduit arteries and microvessels. Such augmented alpha-adrenergic coronary constriction is observed during exercise and coronary interventions, and it is powerful enough to induce myocardial ischemia and limit myocardial function. Recent studies indicate a genetic determination of alpha(2)-adrenergic coronary constriction.
Published: 2000
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49. Alpha-adrenergic blockade improves recovery of myocardial perfusion and function after coronary stenting in patients with acute myocardial infarction.

Author: Gregorini L, Marco J, Kozàkovà M, Palombo C, Anguissola GB, Marco I, Bernies M, Cassagneau B, Distante A, Bossi IM, Fajadet J, and Heusch G
Subjects: Adrenergic beta-Antagonists therapeutic use, Aged, Blood Flow Velocity drug effects, Coronary Angiography, Coronary Vessels drug effects, Female, Humans, Male, Middle Aged, Myocardial Infarction diagnostic imaging, Myocardial Infarction physiopathology, Myocardial Infarction surgery, Receptors, Adrenergic, alpha drug effects, Vasoconstriction drug effects, Adrenergic alpha-Antagonists therapeutic use, Coronary Circulation drug effects, Coronary Vessels physiopathology, Myocardial Infarction drug therapy, Phentolamine therapeutic use, Piperazines therapeutic use, Stents, Ventricular Function, Left drug effects
Abstract: Background: AMI reperfusion by thrombolysis does not improve TIMI flow and LV function. The role of infarct-related artery (IRA) stenosis and superimposed changes in coronary vasomotor tone in maintaining LV dysfunction must be elucidated., Methods and Results: Forty patients underwent diagnostic angiography 24 hours after thrombolysis. Seventy-two hours after thrombolysis, the culprit lesion was dilated with coronary stenting. During angioplasty, LV function was monitored by transesophageal echocardiography. Percent regional systolic thickening was quantitatively assessed before PTCA, soon after stenting, 15 minutes after stenting, and after phentolamine 12 microg/kg IC (n=10), the alpha1-blocker urapidil 600 microg/kg IV (n=10), or saline (n=10). Ten patients pretreated with beta-blockers received urapidil 10 mg IC. Coronary stenting significantly improved thickening in IRA-dependent and in non-IRA-dependent myocardium (from 27+/-15% to 38+/-16% and from 40+/-15% to 45+/-15%, respectively). Simultaneously, TIMI frame count decreased from 39+/-11 and 40+/-11 in the IRA and non-IRA, respectively, to 23+/-10 and 25+/-7 (P<0.05). Fifteen minutes after stenting, thickening worsened in both IRA- and non-IRA-dependent myocardium (to 19+/-14% and 28+/-14%, P<0.05), and TIMI frame count returned, in both the IRA and non-IRA, to the values obtained before stenting. Phentolamine and urapidil increased thickening to 36+/-17% and 41+/-14% in IRA and to 48+/-11% and 49+/-17% in non-IRA myocardium respectively, and TIMI frame count decreased to 16+/-6 and to 17+/-5, respectively. Changes were attenuated with beta-blocker pretreatment., Conclusions: Our finding that alpha-adrenergic blockade attenuates vasoconstriction and postischemic LV dysfunction supports the hypothesis of an important role of neural mechanisms in this phenomenon.
Published: 1999
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50. Acute profound thrombocytopenia after abciximab therapy during coronary angioplasty.

Author: Joseph T, Marco J, and Gregorini L
Subjects: Abciximab, Acute Disease, Aged, Aged, 80 and over, Coronary Disease therapy, Humans, Male, Angioplasty, Balloon, Coronary, Antibodies, Monoclonal adverse effects, Immunoglobulin Fab Fragments adverse effects, Platelet Aggregation Inhibitors adverse effects, Thrombocytopenia chemically induced
Abstract: Since the extensive use of abciximab, a potent antiplatelet agent directed against GP IIb/IIIa platelet receptors, to prevent ischemic complications of percutaneous transluminal coronary angioplasty, few cases of thrombocytopenia have been observed. This paper reports a case of acute profound thrombocytopenia (platelet count: 800/mm3) occurring 16 h after abciximab therapy during coronary angioplasty. As thrombocytopenia occurrence is not predictable, platelet count should be evaluated periodically after drug administration. Mechanisms of this adverse effect remain unknown. Platelet transfusion results in a rapid and sustained improvement of platelet count, avoiding the occurrence of major hemorrhagic complications.
Published: 1998
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