7 results on '"S Peirani"'
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2. Galaxies flowing in the oriented saddle frame of the cosmic web
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Stéphane Arnouts, M. Musso, Julien Devriendt, Charlotte Welker, Marie Treyer, Ho Seong Hwang, Christophe Pichon, D. Vibert, Yohan Dubois, Clotilde Laigle, K. Kraljic, S. Peirani, Sandrine Codis, C. Cadiou, Adrianne Slyz, 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), Centre de Recherche Astrophysique de Lyon (CRAL), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Laboratoire d'Astrophysique de Marseille (LAM), 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), 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), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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 Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Université 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, 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)
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Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Active galactic nucleus ,FOS: Physical sciences ,Kinematics ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,methods: numerical ,methods: analytical ,Saddle point ,0103 physical sciences ,galaxies: interactions ,galaxies: formation ,010303 astronomy & astrophysics ,Saddle ,Astrophysics::Galaxy Astrophysics ,galaxies: kinematics and dynamics ,Physics ,010308 nuclear & particles physics ,Star formation ,Astronomy and Astrophysics ,Astrophysics - Astrophysics of Galaxies ,Galaxy ,Redshift ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,Halo ,galaxies: evolution ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
The strikingly anisotropic large-scale distribution of matter made of an extended network of voids delimited by sheets, themselves segmented by filaments, within which matter flows towards compact nodes where they intersect, imprints its geometry on the dynamics of cosmic flows, ultimately shaping the distribution of galaxies and the redshift evolution of their properties. The (filament-type) saddle points of this cosmic web provide a local frame in which to quantify the induced physical and morphological evolution of galaxies on large scales. The properties of virtual galaxies within the Horizon-AGN simulation are stacked in such a frame. The iso-contours of the galactic number density, mass, specific star formation rate (sSFR), kinematics and age are clearly aligned with the filament axis with steep gradients perpendicular to the filaments. A comparison to a simulation without feedback from active galactic nuclei (AGN) illustrates its impact on quenching star formation of centrals away from the saddles. The redshift evolution of the properties of galaxies and their age distribution are consistent with the geometry of the bulk flow within that frame. They compare well with expectations from constrained Gaussian random fields and the scaling with the mass of non-linearity, modulo the redshift dependent impact of feedback processes. Physical properties such as sSFR and kinematics seem not to depend only on mean halo mass and density: the residuals trace the geometry of the saddle, which could point to other environment-sensitive physical processes, such as spin advection, and AGN feedback at high mass., Comment: 28 pages, 27 figures, submitted to MNRAS
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- 2019
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3. Mass determination of groups of galaxies: Effects of the cosmological constant
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S. Peirani, J. A. de Freitas Pacheco, Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides (CASSIOPEE), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, and Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)
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FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Cosmological constant ,Astrophysics ,98.62.Ck ,98.65.Bv ,98.65.Cw ,01 natural sciences ,[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO] ,Thermodynamics of the universe ,symbols.namesake ,0103 physical sciences ,Peculiar velocity ,010303 astronomy & astrophysics ,Instrumentation ,Astrophysics::Galaxy Astrophysics ,Physics ,Hubble constant ,[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph] ,010308 nuclear & particles physics ,Equation of state (cosmology) ,Astrophysics (astro-ph) ,Velocity dispersion ,Astronomy and Astrophysics ,Virgo Cluster ,Space and Planetary Science ,Local Group ,symbols ,Dark energy ,Hubble's law - Abstract
The spherical infall model first developed by Lema\^{i}tre and Tolman was modified in order to include the effects of a dark energy term. The resulting velocity-distance relation was evaluated numerically. This equation, when fitted to actual data, permits the simultaneous evaluation of the central mass and of the Hubble parameter. Application of this relation to the Local Group, when the dark energy is modeled by a cosmological constant, yields a total mass for the M31-Milky Way pair of (2.5 +/- 0.7) x 10^12 M\_sun, a Hubble parameter H\_0 = 74 +/- 4 km s^-1 Mpc^-1 and a 1-D velocity dispersion for the flow of about 39 km s^-1. The zero-velocity and the marginally bound surfaces of the Local Group are at about 1.0 and 2.3 Mpc respectively from the center of mass. A similar analysis for the Virgo cluster yields a mass of (1.10 +/- 0.12) x 10^15 M\_sun and H\_0 = 65 +/- 9 km s^-1 Mpc^-1. The zero-velocity is located at a distance of 8.6 +/- 0.8 Mpc from the center of the cluster. The predicted peculiar velocity of the Local Group towards Virgo is about 190 kms^-1, in agreement with other estimates. Slightly lower masses are derived if the dark energy is represented by a fluid with an equation of state P = w\epsilon with w = -2/3., Comment: 13 pages, 3 figures. Version to appear in New Astronomy. Typing errors corrected in relation (1) and in percentage value in page 5
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- 2006
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4. Simulations of BAO reconstruction with a quasar Ly-α survey
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C. Yeche, S. Peirani, C. Pichon, R. Charlassier, J. C. Hamilton, Jeffrey A. Rich, Éric Aubourg, P. Petitjean, Emmanuel Rollinde, M. Vargas, N. Palanque Delabrouille, Christophe Magneville, I. Paris, J. M. Le Goff, Nicolás G. Busca, T. Delubac, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)
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Scale (ratio) ,[SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO] ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,Gaussian random field ,[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO] ,0103 physical sciences ,method: numerical ,dark energy ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,Physics ,010308 nuclear & particles physics ,Matter power spectrum ,Astrophysics::Instrumentation and Methods for Astrophysics ,Spectral density ,Astronomy and Astrophysics ,Quasar ,Redshift ,Baryon ,quasars: absorption lines ,Space and Planetary Science ,Baryon acoustic oscillations ,large-scale structure of Universe ,intergalactic medium - Abstract
Context. The imprint of baryonic acoustic oscillations (BAO) on the matter power spectrum can be constrained using the neutral hydrogen density in the intergalactic medium (IGM) as a tracer of the matter density. One of the goals of the baryon oscillation spectroscopic survey (BOSS) of the Sloan Digital Sky Survey (SDSS-III) is to derive the Hubble expansion rate and the angular scale from the BAO signal in the IGM. To this aim, the Lyman-α forest about 150 000 quasars will be observed in the redshift range 2.2 < z < 3.5 and over ~10 000 deg2. Aims: We simulated the BOSS QSO survey to estimate the statistical accuracy on the BAO scale determination provided by such a large-scale survey. In particular, we discuss the effect of the poorly constrained estimate of the quasar's unabsorbed intrinsic spectrum. Methods: The volume of current N-body simulations being too small for such studies, we resorted to Gaussian random field (GRF) simulations. We validated the use of GRFs by comparing the output of GRF simulations with that of the Horizon-4Π N-body dark-matter-only simulation with the same initial conditions. Realistic mock samples of QSO Lyman-α forest were generated and their power spectrum computed and fitted to obtain the BAO scale. The rms of the results for 100 different simulations provides an estimate of the statistical error expected from the BOSS survey. Results: We confirm the results from the Fisher matrix estimate. In the absence of error on the quasar's unabsorbed spectrum, our simulations give an expected uncertainty of 2.3% for the BOSS quasar survey measurement of the BAO scale. The expected uncertainties for the transverse and radial BAO scales are 6.8% and 3.9%, respectively. The significance of the BAO detection is assessed by an average Δχ2 = 17 but Δχ2 ranges from 2 to 35 for individual realizations. The error on the quasar's unabsorbed spectrum increases the error on the BAO scale by 10 to 20% and results in a subpercent bias.
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- 2011
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5. Artificial neural networks for quasar selection and photometric redshift determination
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Ch Yèche, C. Pichon, I. Paris, Mariana Vargas-Magaña, Nicolás G. Busca, J. M. Le Goff, S. Peirani, Éric Aubourg, Jeffrey A. Rich, J.-Ch. Hamilton, Emmanuel Rollinde, Patrick Petitjean, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), SDSS-III, Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)
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[SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO] ,media_common.quotation_subject ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,Photometry (optics) ,[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO] ,0103 physical sciences ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,Photometric redshift ,media_common ,Physics ,010308 nuclear & particles physics ,Matter power spectrum ,Astrophysics::Instrumentation and Methods for Astrophysics ,Astronomy ,Astronomy and Astrophysics ,Quasar ,Cosmology and Extragalactic Astrophysics ,Redshift survey ,Redshift ,Space and Planetary Science ,Sky ,Baryon acoustic oscillations - Abstract
7 pages, 7 figures; Context. Baryonic acoustic oscillations (BAO) and their effects on the matter power spectrum can be studied using the Lyman-α absorption signature of the matter density field along quasar (QSO) lines of sight. A measurement sufficiently accurate to provide useful cosmological constraints requires the observation of ~105 quasars in the redshift range 2.2 < z < 3.5 over ~8000 deg2. Such a survey is planned by the Baryon Oscillation Spectroscopic Survey (BOSS) project of the Sloan Digital Sky Survey (SDSS-III). Aims: We assess one of the challenges for this project, that of building from five-band imaging data a list of targets that contains the largest number of quasars in the required redshift range. In practice, we perform a stellar rejection of more than two orders of magnitude with a selection efficiency for quasars better than 50% to magnitudes as bright as g ~ 22. Methods: To obtain an appropriate target list and estimate quasar redshifts, we develop artificial neural networks (ANNs) with a multilayer perceptron architecture. The input variables are photometric measurements, i.e., the object magnitudes and their errors in the five bands (ugriz) of the SDSS photometry. The ANN developed for target selection provides a continuous output variable between 0 for non-quasar point-like objects to 1 for quasars. A second ANN estimates the QSO redshift z using the photometric information. Results: For target selection, we achieve a non-quasar point-like object rejection of 99.6% and 98.5% for a quasar efficiency of, respectively, 50% and 85%, comparable to the performances of traditional methods. The photometric redshift precision is on the order of 0.1 over the region relevant to BAO studies. These statistical methods, developed in the context of the BOSS project, can easily be extended to any quasar selection and/or determination of their photometric redshift.
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- 2010
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6. Determining the morpho-kinematic properties of a face-on merger atz~ 0.7
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C. Balkowski, S. Peirani, Myriam Rodrigues, Hector Flores, I. Fuentes-Carrera, Y. B. Yang, and Francois Hammer
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Physics ,010308 nuclear & particles physics ,Star formation ,Perturbation (astronomy) ,Astronomy and Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Kinematics ,Astrophysics ,Mass ratio ,01 natural sciences ,Galaxy ,Redshift ,Integral field spectrograph ,Space and Planetary Science ,0103 physical sciences ,Galaxy formation and evolution ,10. No inequality ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics - Abstract
Context. At intermediate redshifts, many galaxies seem to have experienced an interaction. It is not always straightforward to determine what type of encounter or perturbation is observed, nor the outcome of this event. In some cases, only the use of both morphological and kinematical information can determine the true configuration of an encounter at intermediate redshift. Aims. We present the morphological and kinematical analysis of a system at z = 0.74 to understand its configuration, interacting stage, and evolution. Methods. Using the integral field spectrograph GIRAFFE, long-slit spectroscopy by FORS2, direct optical images from the HST-ACS, and ISAAC near-infrared images, we determine the morphology of this system, its star-formation history, and its extended kinematics to propose a possible configuration for the system. Numerical simulations are used to test different interacting scenarii. Results. We identify this system to be a face-on disk galaxy with a very bright bar that is interacting with a smaller companion such that the galaxy and the companion have a mass ratio of 3:1. The relevance of kinematical information and the constraints that it imposes on the interpretation of the observations of distant galaxies are particularly greater in this case. Conclusions. This object represents one of the clearest examples of how one can misinterpret morphology in the absence of kinematical information.
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- 2010
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7. Virgo status and commissioning results
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Acernese, F., Amico, P., Alshourbagy, M., Antonucci, F., Aoudia, S., Astone, P., Avino, S., Babusci, D., Ballardin, G., Barone, F., Barsotti, L., Barsuglia, M., Beauville, F., Bigotta, S., Birindelli, S., Bizouard, M. A., Boccara, C., Bondu, F., Bosi, L., Bradaschia, C., Braccini, S., Brillet, A., Brisson, V., Buskulic, D., Calloni, E., Campagna, E., Carbognani, F., Cavalier, F., Cavalieri, R., Cella, G., Cesarini, E., Chassande Mottin, E., Christensen, N., Corda, C., Corsi, A., Cottone, F., Clapson, A. C., Cleva, F., Coulon, J. P., Cuoco, E., Dari, A., Dattilo, V., Davier, M., Del Prete, M., De Rosa, R., Di Fiore, L., Di Virgilio, A., Dujardin, B., Eleuteri, A., Ferrante, I., Fidecaro, F., Fiori, I., Flaminio, R., Fournier, J. D., Frasca, Sergio, Frasconi, F., Gammaitoni, L., Garufi, F., Genin, E., Gennai, A., Giazotto, A., Giordano, G., Giordano, L., Gouaty, R., Grosjean, D., Guidi, G., Hebri, S., Heitmann, H., Hello, P., Karkar, S., Kreckelbergh, S., La Penna, P., Laval, M., Leroy, N., Letendre, N., Lopez, B., Lorenzini, M., Loriette, V., Losurdo, G., Mackowski, J. M., Majorana, E., Man, C. N., Mantovani, M., Marchesoni, F., Marion, F., Marque, J., Martelli, F., Masserot, A., Mazzoni, M., Milano, L., Menzinger, F., Moins, C., Moreau, J., Morgado, N., Mours, B., Nocera, F., Palomba, C., Paoletti, F., Pardi, S., Pasqualetti, A., Passaquieti, R., Passuello, D., Piergiovanni, F., Pinard, L., Poggiani, R., Punturo, M., Puppo, P., Qipiani, K., Rapagnani, Piero, Reita, V., Remillieux, A., Ricci, Fulvio, Ricciardi, I., Ruggi, P., Russo, G., Solimeno, S., Spallicci, A., Tarallo, M., Tonelli, M., Toncelli, A., Tournefier, E., Travasso, F., Tremola, C., Gabriele, Vajente, Verkindt, D., Vetrano, F., Vicere, A., Vinet, J. Y., Vocca, H., Yvert, M., Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux ( ARTEMIS ), Université Nice Sophia Antipolis ( UNS ), Université Côte d'Azur ( UCA ) -Université Côte d'Azur ( UCA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de la Côte d'Azur, Université Côte d'Azur ( UCA ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de l'Accélérateur Linéaire ( LAL ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire d'Annecy de Physique des Particules ( LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules ), Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Savoie Mont Blanc ( USMB [Université de Savoie] [Université de Chambéry] ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire des matériaux avancés ( LMA ), Université Claude Bernard Lyon 1 ( UCBL ), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), VIRGO, Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Laboratoire des matériaux avancés (LMA), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon, F., Acernese, P., Amico, S., Aoudia, N., Arnaud, S., Avino, D., Babusci, G., Ballardin, R., Barillé, F., Barone, L., Barsotti, M., Barsuglia, F., Beauville, M. A., Bizouard, C., Boccara, F., Bondu, L., Bosi, C., Bradaschia, S., Braccini, A., Brillet, V., Brisson, L., Brocco, D., Buskulic, Calloni, Enrico, E., Campagna, F., Cavalier, R., Cavalieri, G., Cella, E., Chassande Mottin, F., Cleva, J. P., Coulon, E., Cuoco, V., Dattilo, M., Davier, DE ROSA, Rosario, L., Di Fiore, A., Di Virgilio, B., Dujardin, A., Eleuteri, D., Enard, I., Ferrante, F., Fidecaro, I., Fiori, R., Flaminio, J. D., Fournier, S., Frasca, F., Frasconi, A., Freise, L., Gammaitoni, A., Gennai, A., Giazotto, G., Giordano, L., Giordano, R., Gouaty, D., Grosjean, G., Guidi, S., Hebri, H., Heitmann, P., Hello, P., Heusse, L., Holloway, S., Kreckelbergh, P., La Penna, V., Loriette, M., Loupia, G., Losurdo, J. M., Mackowski, E., Majorana, C. N., Man, F., Marchesoni, F., Marion, J., Marque, F., Martelli, A., Masserot, M., Mazzoni, Milano, Leopoldo, C., Moin, J., Moreau, N., Morgado, B., Mour, J., Pacheco, A., Pai, C., Palomba, F., Paoletti, Pardi, Silvio, A., Pasqualetti, R., Passaquieti, D., Passuello, S., Peirani, B., Perniola, F., Piergiovanni, L., Pinard, R., Poggiani, M., Punturo, P., Puppo, K., Qipiani, P., Rapagnani, V., Reita, A., Remillieux, F., Ricci, I., Ricciardi, P., Ruggi, Russo, Guido, Solimeno, Salvatore, A., Spallicci, R., Stanga, R., Taddei, D., Tombolato, E., Tournefier, F., Travasso, D., Verkindt, F., Vetrano, A., Viceré, J. Y., Vinet, H., Vocca, M., Yvert, and Z., Zhang
- Subjects
Physics ,Gravitational wave detectors and experiments ,[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph] ,Physics and Astronomy (miscellaneous) ,010308 nuclear & particles physics ,Project commissioning ,Gravitational wave ,Detector ,Astronomy ,Long wave radiation ,[ PHYS.ASTR.CO ] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO] ,01 natural sciences ,04.80.Nn ,[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO] ,Interferometry ,0103 physical sciences ,Sensitivity (control systems) ,Antenna (radio) ,010303 astronomy & astrophysics ,[ SDU.ASTR ] Sciences of the Universe [physics]/Astrophysics [astro-ph] - Abstract
International audience; Virgo is a French–Italian collaboration for the construction and operation of a 3 km long interferometric gravitational wave antenna. The construction of the detector is already completed and the commissioning is quite advanced, while the data taking is expected to start in 2005. In this paper, we report on the present status of Virgo and on the results of commissioning activity. In particular, we analyse the first four engineering runs (C1–C4) and discuss the sensitivity obtained in C4.
- Published
- 2004
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