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3 results on '"Héraudeau, P."'

1. The VLT LBG Redshift Survey - I. Clustering and dynamics of ≈1000 galaxies at z≈ 3.

Author

Bielby, R. M., Shanks, T., Weilbacher, P. M., Infante, L., Crighton, N. H. M., Bornancini, C., Bouché, N., Héraudeau, P., Lambas, D. G., Lowenthal, J., Minniti, D., Padilla, N., Petitjean, P., and Theuns, T.

Subjects
GALAXY clusters, GALACTIC dynamics, REDSHIFT, VERY Large Telescope (Chile), SPECTRUM analysis, IMAGING systems in astronomy, METAPHYSICAL cosmology
Abstract

We present the initial imaging and spectroscopic data acquired as part of the Very Large Telescope (VLT) VIMOS Lyman-break galaxy Survey. UBR (or UBVI) imaging covers five arcmin fields centred on bright quasi-stellar objects (QSOs), allowing galaxy candidates to be selected using the Lyman-break technique. We performed spectroscopic follow-up using VLT VIMOS, measuring redshifts for Lyman-break galaxies and QSOs from a total of 19 VIMOS pointings. From the galaxy spectra, we observe a velocity offset between the interstellar absorption and Lyman α emission-line redshifts, consistent with previous results. Using the photometric and spectroscopic catalogues, we have analysed the galaxy clustering at . The angular correlation function, , is well fitted by a double power law with clustering scalelength, and slope for and with at larger scales. Using the redshift sample we estimate the semiprojected correlation function, and, for a power law, find for the VLT sample and for a combined VLT+Keck sample. From and , and assuming the above models, we find that the combined VLT and Keck surveys require a galaxy pairwise velocity dispersion of , higher than assumed by previous authors. We also measure a value for the gravitational growth rate parameter of , again higher than that previously found and implying a low value for the bias of . This value is consistent with the galaxy clustering amplitude which gives , assuming the standard cosmology, implying that the evolution of the gravitational growth rate is also consistent with Einstein gravity. Finally, we have compared our Lyman-break galaxy clustering amplitudes with lower redshift measurements and find that the clustering strength is not inconsistent with that of low-redshift spirals for simple 'long-lived' galaxy models. [ABSTRACT FROM AUTHOR]

Published
2011
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2. The European Large-Area ISO Survey (ELAIS): the final band-merged catalogue.

Author

Rowan-Robinson, M., Lari, C., Perez-Fournon, I., Gonzalez-Solares, E.A., La Franca, F., Vaccari, M., Oliver, S., Gruppioni, C., Ciliegi, P., Héraudeau, P., Serjeant, S., Efstathiou, A., Babbedge, T., Matute, I., Pozzi, F., Franceschini, A., Vaisanen, P., Afonso-Luis, A., Alexander, D.M., and Almaini, O.

Subjects
ASTRONOMICAL observations, STAR formation, GALAXIES, METAPHYSICAL cosmology, REDSHIFT, ASTRONOMICAL spectroscopy
Abstract

We present the final band-merged European Large-Area ISO Survey (ELAIS) Catalogue at 6.7, 15, 90 and 175 μm, and the associated data at U, g′, r′, i′, Z, J, H, K and 20 cm. The origin of the survey, infrared and radio observations, data-reduction and optical identifications are briefly reviewed, and a summary of the area covered and the completeness limit for each infrared band is given. A detailed discussion of the band-merging and optical association strategy is given. The total Catalogue consists of 3762 sources. 23 per cent of the 15-μm sources and 75 per cent of the 6.7-μm sources are stars. For extragalactic sources observed in three or more infrared bands, colour–colour diagrams are presented and discussed in terms of the contributing infrared populations. Spectral energy distributions (SEDs) are shown for selected sources and compared with cirrus, M82 and Arp220 starburst, and active galactic nuclei (AGN) dust torus models. Spectroscopic redshifts are tabulated, where available. For the N1 and N2 areas, the Isaac Newton Telescope ugriz Wide Field Survey permits photometric redshifts to be estimated for galaxies and quasars. These agree well with the spectroscopic redshifts, within the uncertainty of the photometric method [∼10 per cent in for galaxies]. The redshift distribution is given for selected ELAIS bands and colour–redshift diagrams are discussed. There is a high proportion of ultraluminous infrared galaxies (log10 of 1–1000 μm luminosity ) in the ELAIS Catalogue (14 per cent of 15-μm galaxies with known z), many with Arp220-like SEDs. 10 per cent of the 15-μm sources are genuine optically blank fields to : these must have very high infrared-to-optical ratios and probably have , so are high-luminosity dusty starbursts or Type 2 AGN. Nine hyperluminous infrared galaxies and nine extremely red objects (EROs) are found in the survey. The latter are interpreted as ultraluminous dusty infrared galaxies at . The large numbers of ultraluminous galaxies imply very strong evolution in the star formation rate between z= 0 and 1. There is also a surprisingly large population of luminous , cool (cirrus-type SEDs) galaxies, with , implying . [ABSTRACT FROM AUTHOR]

Published
2004
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3. The European Large-Area ISO Survey (ELAIS): the final band-merged catalogue

Author

M. Rowan-Robinson, C. Lari, I. Perez-Fournon, E. A. Gonzalez-Solares, F. La Franca, M. Vaccari, S. Oliver, C. Gruppioni, P. Ciliegi, P. Héraudeau, S. Serjeant, A. Efstathiou, T. Babbedge, I. Matute, F. Pozzi, A. Franceschini, P. Vaisanen, A. Afonso-Luis, D. M. Alexander, O. Almaini, A. C. Baker, S. Basilakos, M. Barden, C. del Burgo, I. Bellas-Velidis, F. Cabrera-Guerra, R. Carballo, C. J. Cesarsky, D. L. Clements, H. Crockett, L. Danese, A. Dapergolas, B. Drolias, N. Eaton, E. Egami, D. Elbaz, D. Fadda, M. Fox, R. Genzel, P. Goldschmidt, J. I. Gonzalez-Serrano, M. Graham, G. L. Granato, E. Hatziminaoglou, U. Herbstmeier, M. Joshi, E. Kontizas, M. Kontizas, J. K. Kotilainen, D. Kunze, A. Lawrence, D. Lemke, M. J. D. Linden-Vørnle, R. G. Mann, I. Márquez, J. Masegosa, R. G. McMahon, G. Miley, V. Missoulis, B. Mobasher, T. Morel, H. Nørgaard-Nielsen, A. Omont, P. Papadopoulos, J.-L. Puget, D. Rigopoulou, B. Rocca-Volmerange, N. Sedgwick, L. Silva, T. Sumner, C. Surace, B. Vila-Vilaro, P. van der Werf, A. Verma, L. Vigroux, M. Villar-Martin, C. J. Willott, A. Carramiñana, R. Mujica, Universidad de Cantabria, Steward Observatory, University of Arizona, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), 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), Max Planck Institute for Extraterrestrial Physics (MPE), Max-Planck-Gesellschaft, AUTRES, Space Telescope Science Institute (STSci), Science et Ingénierie des Matériaux et Procédés (SIMaP), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National Polytechnique de Grenoble (INPG)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Physics [Oxford], University of Oxford [Oxford], Centro de Fisica de Plasmas (GoLP), Instituto Superior Técnico, Universidade Técnica de Lisboa (IST), Imperial College London, 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), Oxford Astrophysics, Instituto de Astrofisica de Canarias (IAC), Dipartimento di Astronomia [Padova], Universita degli Studi di Padova, INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), Department of Physics and Astronomy [Milton Keynes], The Open University [Milton Keynes] (OU), Laboratoire de Physico-Chimie des Polymères et des Milieux Dispersés (PPMD), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de thermodynamique et physico-chimie métallurgiques (LTPCM), Institut National Polytechnique de Grenoble (INPG)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), University of Oxford, Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Padova = University of Padua (Unipd), Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National Polytechnique de Grenoble (INPG)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Department of Physics, Dipartimento di Astronomia, Université Pierre et Marie Curie - Paris 6 (UPMC)-ESPCI ParisTech-Centre National de la Recherche Scientifique (CNRS), Kapteyn Astronomical Institute, Rowan-Robinson M., Lari C., Perez-Fournon I., Gonzalez-Solares E. A., La Franca F., Vaccari M., Oliver S., Gruppioni C., Ciliegi P., Héraudeau P., Serjeant S., Efstathiou A., Babbedge T., Matute I., Pozzi F., Franceschini A., Vaisanen P., Afonso-Luis A., Alexander D. M., Almaini O., Baker A. C., Basilakos S., Barden M., del Burgo C., Bellas-Velidis I., Cabrera-Guerra F., Carballo R., Cesarsky C. J., Clements D. L., Crockett H., Danese L., Dapergolas A., Drolias B., Eaton N., Egami E., Elbaz D., Fadda D., Fox M., Genzel R., Goldschmidt P., Gonzalez-Serrano J. I., Graham M., Granato G. L., Hatziminaoglou E., Herbstmeier U., Joshi M., Kontizas E., Kontizas M., Kotilainen J. K., Kunze D., Lawrence A., Lemke D., Linden-Vørnle M. J. D., Mann R. G., Márquez I., Masegosa J., McMahon R. G., Miley G., Missoulis V., Mobasher B., Morel T., Nørgaard-Nielsen H., Omont A., Papadopoulos P., Puget J.-L., Rigopoulou D., Rocca-Volmerange B., Sedgwick N., Silva L., Sumner T., Surace C., Vila-Vilaro B., van der Werf P., Verma A., Vigroux L., Villar-Martin M., Willott C. J., Carramiñana A., and Mujica R.

Subjects
010504 meteorology & atmospheric sciences, galaxies : evolution, Infrared, galaxies: starburst, Astrophysics, HUBBLE-DEEP-FIELD, 01 natural sciences, X-RAY SURVEY, SOUTHERN FIELD, galaxies [Infrared], EXTRAGALACTIC SOURCE COUNTS, Astrophysics::Solar and Stellar Astrophysics, observations [Cosmology], 010303 astronomy & astrophysics, formation [Stars], Physics, infrared : galaxies, stars : formation, Astrophysics (astro-ph), STAR-FORMATION HISTORY, FORMATION RATES, cosmology : observations, Cirrus, galaxies : starburst, Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution, ACTIVE GALACTIC NUCLEI, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, infrared: galaxies, 0103 physical sciences, 170 MU-M, DATA REDUCTION, [INFO]Computer Science [cs], Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Luminous infrared galaxy, stars: formation, Spectral density, Astronomy and Astrophysics, Torus, Quasar, evolution [Galaxies], Redshift, Galaxy, starburst [Galaxies], Space and Planetary Science, cosmology: observations, HIGH-REDSHIFT, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

We present the final band-merged ELAIS catalogue at 6.7, 15, 90, and 175 $��$m, and the associated data at u,g,r,i,z,J,H,K, and 20cm. The origin of the survey, infrared and radio observations, data-reduction and optical identifications are briefly reviewed, and a summary of the area covered, and completeness limit for each infrared band is given. A detailed discussion of the band-merging and optical association strategy is given. The total catalogues consists of 2860 sources. For extragalactic sources observed in 3 or more infrared bands, colour-colour diagrams are presented and discussed in terms of the contributing infrared populations. Spectral energy distributions are shown for selected sources and compared with cirrus, M82 and Arp220 starburst, and AGN dust torus models. Spectroscopic redshifts are tabulated, where available. For the N1 and N2 areas, the INT ugriz Wide Field Survey, permits photometric redshifts to be estimated for galaxies and quasars. These agree well with the spectroscopic redshifts, within the uncertainty of the photometric method. The redshift distribution is given for selected ELAIS bands and colour-redshift diagrams are discussed. There is a high proportion of ultraluminous infrared galaxies in the ELAIS Catalogue ($> 10 %$ of 15 $��$m sources), many with Arp220-like colours. 10 hyperluminous infrared galaxies and 10 EROs are found in the survey. The large numbers of ultraluminous galaxies imply very strong evolution in the star-formation rate between z = 0 and 1., 21 pages, 31 figures. Accepted for publication in MNRAS

Published
2004
Full Text
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