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23 results on '"Department of Physics and Astronomy [Riverside]"'

1. Relationships between RNA Topology and Nucleocapsid Structure in a Model Icosahedral Virus

Author

Kalouna Kra, Yinan Dong, Stéphane Bressanelli, Roya Zandi, Guillaume Tresset, Laurent Marichal, Sanaz Panahandeh, Laetitia Gargowitsch, Christina Sizun, Rafael Leite Rubim, Laboratoire de Physique des Solides (LPS), Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Institut de Chimie des Substances Naturelles (ICSN), Institut de Chimie du CNRS (INC)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Institut de Biologie Intégrative de la Cellule (I2BC), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Department of Physics and Astronomy [Riverside], University of California [Riverside] (UC Riverside), University of California (UC)-University of California (UC), ANR-16-CE30-0017,GENPACK-VIRUS,Résoudre le paradoxe de Levinthal pour l'encapsidation du génome dans les virus icosaédriques à ARN simple brin(2016), University of California (UC), University of California [Riverside] (UCR), and University of California-University of California

Subjects
Icosahedral symmetry, viruses, [PHYS.PHYS.PHYS-BIO-PH]Physics [physics]/Physics [physics]/Biological Physics [physics.bio-ph], Biophysics, Genome, Viral, Topology, 01 natural sciences, Genome, Virus, Nucleic acid secondary structure, 03 medical and health sciences, 0103 physical sciences, 010306 general physics, Nucleocapsid, Topology (chemistry), ComputingMilieux_MISCELLANEOUS, 030304 developmental biology, 0303 health sciences, Chemistry, Virus Assembly, Virion, RNA, Articles, Capsid, Viruses, [SDV.MP.VIR]Life Sciences [q-bio]/Microbiology and Parasitology/Virology, RNA, Viral, Linear topology
Abstract

International audience; The process of genome packaging in most of viruses is poorly understood, notably the role of the genome itself in the nucleocapsid structure. For simple icosahedral single-stranded RNA viruses, the branched topology due to the RNA secondary structure is thought to lower the free energy required to complete a virion. We investigate the structure of nucleocapsids packaging RNA segments with various degrees of compactness by small-angle X-ray scattering and cryotransmission electron microscopy. The structural differences are mild even though compact RNA segments lead on average to better ordered and more uniform particles across the sample. Numerical calculations confirm that the free energy is lowered for the RNA segments displaying the larger number of branch points. The effect is however opposite with synthetic polyelectrolytes, where a star topology gives rise to more disorder in the capsids than a linear topology. If RNA compactness and size account in part for the proper assembly of the nucleocapsid and the genome selectivity, other factors most likely related to the host cell environment during viral assembly, must come into play as well.

Published
2021

5. Quantum error correction with the toric Gottesman-Kitaev-Preskill code

Author

Hamed Asasi, Christophe Vuillot, Barbara M. Terhal, Yang Wang, Leonid P. Pryadko, Faculty of Electrical Engineering, Mathematics and Computer Science [Delft], Delft University of Technology (TU Delft), Department of Physics and Astronomy [Riverside], University of California [Riverside] (UCR), University of California-University of California, JARA-Institute for Quantum Information (JARA-IQI), and JARA-IQI

Subjects
Physics, Toric code, Gaussian, Concatenation, 01 natural sciences, 010305 fluids & plasmas, symbols.namesake, [PHYS.QPHY]Physics [physics]/Quantum Physics [quant-ph], Quantum error correction, 0103 physical sciences, symbols, Code (cryptography), Quantum information, 010306 general physics, Error detection and correction, Algorithm, Decoding methods
Abstract

We examine the performance of the single-mode Gottesman-Kitaev-Preskill (GKP) code and its concatenation with the toric code for a noise model of Gaussian shifts, or displacement errors. We show how one can optimize the tracking of errors in repeated noisy error correction for the GKP code. We do this by examining the maximum-likelihood problem for this setting and its mapping onto a 1D Euclidean path-integral modeling a particle in a random cosine potential. We demonstrate the efficiency of a minimum-energy decoding strategy as a proxy for the path integral evaluation. In the second part of this paper, we analyze and numerically assess the concatenation of the GKP code with the toric code. When toric code measurements and GKP error correction measurements are perfect, we find that by using GKP error information the toric code threshold improves from $10%$ to $14%$. When only the GKP error correction measurements are perfect we observe a threshold at $6%$. In the more realistic setting when all error information is noisy, we show how to represent the maximum likelihood decoding problem for the toric-GKP code as a 3D compact QED model in the presence of a quenched random gauge field, an extension of the random-plaquette gauge model for the toric code. We present a decoder for this problem which shows the existence of a noise threshold at shift-error standard deviation ${\ensuremath{\sigma}}_{0}\ensuremath{\approx}0.243$ for toric code measurements, data errors and GKP ancilla errors. If the errors only come from having imperfect GKP states, then this corresponds to states with just four photons or more. Our last result is a no-go result for linear oscillator codes, encoding oscillators into oscillators. For the Gaussian displacement error model, we prove that encoding corresponds to squeezing the shift errors. This shows that linear oscillator codes are useless for quantum information protection against Gaussian shift errors.

Published
2019

6. Self Consistent Field Theory of Virus Assembly

Author

Roya Zandi, Siyu Li, Henri Orland, Department of Physics and Astronomy [Riverside], University of California [Riverside] (UCR), University of California-University of California, Institut de Physique Théorique - UMR CNRS 3681 (IPHT), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Beijing Computational Science Research Center [Beijing] (CSRC), National Science Foundation through Grant, DMR -1719550, University of California [Riverside] (UC Riverside), University of California (UC)-University of California (UC), and the National Science Foundation through Grant No. DMR -1719550

Subjects
Models, Molecular, Paper, 0301 basic medicine, Work (thermodynamics), Fluids & Plasmas, persistence length, Shell (structure), virus assembly, FOS: Physical sciences, Inverse, Special Issue on Viral Capsids, Condensed Matter - Soft Condensed Matter, field theory, 01 natural sciences, 03 medical and health sciences, Capsid, Models, 0103 physical sciences, Nanotechnology, General Materials Science, Field theory (psychology), Physics - Biological Physics, Statistical physics, 010306 general physics, Physics, Persistence length, [PHYS]Physics [physics], Quantitative Biology::Biomolecules, Virus Assembly, Molecular, Radius, Materials Engineering, Condensed Matter Physics, Quantitative Biology::Genomics, 030104 developmental biology, Biological Physics (physics.bio-ph), Excited state, Soft Condensed Matter (cond-mat.soft), Ground state
Abstract

International audience; The Ground State Dominance Approximation(GSDA) has been extensively used to study the assembly of viral shells. In this work we employ the self-consistent field theory (SCFT) to investigate the adsorption of RNA onto positively charged spherical viral shells and examine the conditions when GSDA does not apply and SCFT has to be used to obtain a reliable solution. We find that there are two regimes in which GSDA does work. First, when the genomic RNA length is long enough compared to the capsid radius, and second, when the interaction between the genome and capsid is so strong that the genome is basically localized next to the wall. We find that for the case in which RNA is more or less distributed uniformly in the shell, regardless of the length of RNA, GSDA is not a good approximation. We observe that as the polymer-shell interaction becomes stronger, the energy gap between the ground state and first excited state increases and thus GSDA becomes a better approximation. We also present our results corresponding to the genome persistence length obtained through the tangent-tangent correlation length and show that it is zero in case of GSDA but is equal to the inverse of the energy gap when using SCFT.

Published
2018

7. RNA Base Pairing Determines the Conformations of RNA Inside Spherical Viruses

Author

Henri Orland, Roya Zandi, Gonca Erdemci-Tandogan, Department of Physics and Astronomy [Riverside], University of California [Riverside] (UC Riverside), University of California (UC)-University of California (UC), Institut de Physique Théorique - UMR CNRS 3681 (IPHT), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Beijing Computational Science Research Center [Beijing] (CSRC), University of California [Riverside] (UCR), University of California-University of California, and Centre National de la Recherche Scientifique (CNRS)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)

Subjects
0301 basic medicine, Base pair, viruses, Shell (structure), General Physics and Astronomy, FOS: Physical sciences, 01 natural sciences, 03 medical and health sciences, Capsid, 0103 physical sciences, Physics - Biological Physics, 010306 general physics, [PHYS]Physics [physics], Continuous transition, Chemistry, RNA, Biomolecules (q-bio.BM), First order, Stem-loop, 030104 developmental biology, Quantitative Biology - Biomolecules, Biological Physics (physics.bio-ph), Pairing, FOS: Biological sciences, Biophysics, Nucleic Acid Conformation, RNA, Viral
Abstract

International audience; Many simple RNA viruses enclose their genetic material by a protein shell called the capsid. While the capsid structures are well characterized for most viruses, the structure of RNA inside the shells and the factors contributing to it remain poorly understood. We study the impact of base pairing on the conformations of RNA and find that it undergoes a swollen coil to globule continuous transition as a function of the strength of the pairing interaction. We also observe a first order transition and kink profile as a function of RNA length. All these transitions could explain the different RNA profiles observed inside viral shells.

Published
2017

8. RAPID COEVAL BLACK HOLE AND HOST GALAXY GROWTH IN MRC 1138-262: THE HUNGRY SPIDER

Author

Jaron Kurk, C. De Breuck, Bruno Altieri, Nina A. Hatch, Helmut Dannerbauer, Thomas R. Greve, Matt J. Jarvis, I. Valtchanov, D. Coia, George K. Miley, J. I. Rawlings, Daniel Stern, H. J. A. Röttgering, Alessandro Rettura, Pieter Barthel, Arjun Dey, Attila Kovács, Brigitte Rocca-Volmerange, L. Conversi, Martin Haas, J. S. Santos, Jason R. Stevens, Edo Ibar, Dominika Wylezalek, Audrey Galametz, Joel Vernet, Rob Ivison, Guillaume Drouart, Matt Lehnert, Mark Dickinson, Miguel Sánchez-Portal, Nick Seymour, Nicole P. H. Nesvadba, Kapteyn Astronomical Institute, Space Science & Technology Department, Rutheford Appleton Laboratory, XMM-Newton Science Operations Centre, Agence Spatiale Européenne = European Space Agency (ESA), 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), Herschel Science Centre, European Space Astronomy Centre (ESAC), 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), National Optical Astronomy Observatory (NOAO), INAF - Osservatorio Astronomico di Roma (OAR), Istituto Nazionale di Astrofisica (INAF), Royal Veterinary and Agricultural University = Kongelige Veterinær- og Landbohøjskole (KVL ), Laboratoire des technologies de la microélectronique (LTM), Université Joseph Fourier - Grenoble 1 (UJF)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS), UK Astronomy Technology Centre (UK ATC), Science and Technology Facilities Council (STFC), Royal Observatory Edinburgh (ROE), University of Edinburgh, Centre for Energy Research [Budapest] (MTAE), Hungarian Academy of Sciences (MTA), Max-Planck-Institut für Extraterrestrische Physik (MPE), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Department of Physics and Astronomy [Riverside], University of California [Riverside] (UC Riverside), University of California (UC)-University of California (UC), Leiden Observatory [Leiden], Universiteit Leiden, AUTRES, European Space Agency (ESA), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), 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), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), University of California [Riverside] (UCR), University of California-University of California, and Universiteit Leiden [Leiden]

Subjects
ACTIVE GALACTIC NUCLEI, Cosmology and Nongalactic Astrophysics (astro-ph.CO), SIMILAR-TO 2, Active galactic nucleus, H-ALPHA, Radio galaxy, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, K-Z RELATION, FOS: Physical sciences, SPECTRAL ENERGY-DISTRIBUTIONS, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, BULGE MASS RELATION, 01 natural sciences, Luminosity, galaxies: high-redshift, ELLIPTIC GALAXIES, 0103 physical sciences, STAR-FORMING GALAXIES, Galaxy formation and evolution, galaxies: formation, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, galaxies: individual (MRC 1138-262), Astrophysics::Galaxy Astrophysics, [PHYS]Physics [physics], Physics, 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, REDSHIFT RADIO GALAXIES, FAR-INFRARED PROPERTIES, Galaxy, Redshift, Space and Planetary Science, Spectral energy distribution, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present a detailed study of the infrared spectral energy distribution of the high-redshift radio galaxy MRC 1138-26 at z = 2.156, also known as the Spiderweb Galaxy. By combining photometry from Spitzer, Herschel and LABOCA we fit the rest-frame 5-300 um emission using a two component, starburst and active galactic nucleus (AGN), model. The total infrared (8 - 1000 um) luminosity of this galaxy is (1.97+/-0.28)x10^13 Lsun with (1.17+/-0.27) and (0.79+/-0.09)x10^13 Lsun due to the AGN and starburst components respectively. The high derived AGN accretion rate of \sim20% Eddington, and the measured star formation rate (SFR) of 1390pm150 Msun/yr, suggest that this massive system is in a special phase of rapid central black hole and host galaxy growth, likely caused by a gas rich merger in a dense environment. The accretion rate is sufficient to power both the jets and the previously observed large outflow. The high SFR and strong outflow suggest this galaxy could potentially exhaust its fuel for stellar growth in a few tens of Myr, although the likely merger of the radio galaxy with nearby satellites suggest bursts of star formation may recur again on time scales of several hundreds of Myr. The age of the radio lobes implies the jet started after the current burst of star formation, and therefore we are possibly witnessing the transition from a merger-induced starburst phase to a radio-loud AGN phase. We also note tentative evidence for [CII]158um emission. This paper marks the first results from the Herschel Galaxy Evolution Project (Project HeRGE), a systematic study of the evolutionary state of 71 high redshift, 1 < z < 5.2, radio galaxies., 11 pages, 2 figures, accepted for publication in ApJ

Published
2016

9. Fractal superconductivity near localization threshold

Author

Lev Ioffe, Vladimir E. Kravtsov, Emilio Cuevas, Mikhail Feigel'man, L.D. Landau Institute for Theoretical Physics of RAS, Russian Academy of Sciences [Moscow] (RAS), Moscow Institute of Physics and Technology [Moscow] (MIPT), Laboratoire de Physique Théorique et Modèles Statistiques (LPTMS), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), Department of Physics and Astronomy [Riverside], University of California [Riverside] (UCR), University of California-University of California, Abdus Salam International Centre for Theoretical Physics [Trieste] (ICTP), Izaña Atmospheric Research Center (IARC), and Agencia Estatal de Meteorología (AEMet)

Subjects
Superconductivity, Physics, Local density of states, Condensed matter physics, Condensed Matter - Superconductivity, Scanning tunneling spectroscopy, Fermi level, FOS: Physical sciences, General Physics and Astronomy, Fermi surface, Fermi energy, 01 natural sciences, 010305 fluids & plasmas, [PHYS.COND.CM-S]Physics [physics]/Condensed Matter [cond-mat]/Superconductivity [cond-mat.supr-con], Superconductivity (cond-mat.supr-con), symbols.namesake, Condensed Matter::Superconductivity, Pairing, 0103 physical sciences, symbols, 010306 general physics, Anderson impurity model
Abstract

We develop a semi-quantitative theory of electron pairing and resulting superconductivity in bulk "poor conductors" in which Fermi energy $E_F$ is located in the region of localized states not so far from the Anderson mobility edge $E_c$. We review the existing theories and experimental data and argue that a large class of disordered films is described by this model. Our theoretical analysis is based on the analytical treatment of pairing correlations, described in the basis of the exact single-particle eigenstates of the 3D Anderson model, which we combine with numerical data on eigenfunction correlations. Fractal nature of critical wavefunction's correlations is shown to be crucial for the physics of these systems. We identify three distinct phases: 'critical' superconductive state formed at $E_F=E_c$, superconducting state with a strong pseudogap, realized due to pairing of weakly localized electrons and insulating state realized at $E_F$ still deeper inside localized band. The 'critical' superconducting phase is characterized by the enhancement of the transition temperature with respect to BCS result, by the inhomogeneous spatial distribution of superconductive order parameter and local density of states. The major new feature of the pseudo-gaped state is the presence of two independent energy scales: superconducting gap $\Delta$, that is due to many-body correlations and a new "pseudogap" energy scale $\Delta_P$ which characterizes typical binding energy of localized electron pairs and leads to the insulating behavior of the resistivity as a function of temperature above superconductive $T_c$. Two gap nature of the "pseudo-gaped superconductor" is shown to lead to a number of unusual physical properties., Comment: 110 pages, 39 figures. The revised version corrects a number of typos, adds references and discussion of recent results

Published
2010

10. Candidate Clusters of Galaxies at z > 1.3 Identified in the Spitzer South Pole Telescope Deep Field Survey

Author

J. Martinez-Manso, Alessandro Rettura, S. A. Stanford, D. Stern, Simona Mei, Anthony H. Gonzalez, D. Gettings, James G. Bartlett, Mark Brodwin, M. L. N. Ashby, Jet Propulsion Laboratory, California Institute of Technology, MS 169-234, Pasadena, CA 91109, USA, Department of Astronomy, University of Florida, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Paris Cité (UPCité), Infrared Processing Analysis Center, California Institute of Technology (IPAC), Harvard-Smithsonian Center for Astrophysics, Department of Physics and Astronomy, University of Missouri, Kansas City, MO 64110, USA, Department of Physics, Le Conte Hall, University of California, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Department of Physics and Astronomy [Riverside], University of California [Riverside] (UCR), University of California-University of California, Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), DLO Winand Staring Centre, Services communs OMP - UMS 831 (UMS 831), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Météo France-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Météo France-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, and 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)

Subjects
Physics, Luminous infrared galaxy, [PHYS]Physics [physics], Hubble Deep Field, Dark matter, Astronomy and Astrophysics, BOOTES, Astrophysics, Galaxy, Redshift, South Pole Telescope, Space and Planetary Science, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Galaxy cluster, ComputingMilieux_MISCELLANEOUS
Abstract

We present 279 galaxy cluster candidates at z > 1.3 selected from the 94 deg^2 Spitzer South Pole Telescope Deep Field (SSDF) survey. We use a simple algorithm to select candidate high-redshift clusters of galaxies based on Spitzer/IRAC mid-infrared data combined with shallow all-sky optical data. We identify distant cluster candidates adopting an overdensity threshold that results in a high purity (80%) cluster sample based on tests in the Spitzer Deep, Wide-Field Survey of the Boötes field. Our simple algorithm detects all three 1.4 < z ≤ 1.75 X-ray detected clusters in the Boötes field. The uniqueness of the SSDF survey resides not just in its area, one of the largest contiguous extragalactic fields observed with Spitzer, but also in its deep, multi-wavelength coverage by the South Pole Telescope (SPT), Herschel/SPIRE, and XMM-Newton. This rich data set will allow direct or stacked measurements of Sunyaev-Zel'dovich effect decrements or X-ray masses for many of the SSDF clusters presented here, and enable a systematic study of the most distant clusters on an unprecedented scale. We measure the angular correlation function of our sample and find that these candidates show strong clustering. Employing the COSMOS/UltraVista photometric catalog in order to infer the redshift distribution of our cluster selection, we find that these clusters have a comoving number density N_c = (0.7^(+6.3)_(0.6)) x 10^(-7) h^3 Mpc^(-3) and a spatial clustering correlation scale length r_ 0 = (32 ± 7) h^(–1) Mpc. Assuming our sample is comprised of dark matter halos above a characteristic minimum mass, M _(min), we derive that at z = 1.5 these clusters reside in halos larger than M_(min) = 1.5^(+0.9)_(0.7) x 10^(14) h^(-1) M_⊙. We find that the mean mass of our cluster sample is equal to M_(mean) = 1.9^(+1.0)_(0.8) x 10^(14) h^(-1) M_⊙ ; thus, our sample contains the progenitors of present-day massive galaxy clusters.

Published
2014

11. VizieR Online Data Catalog: GOODS-Herschel North and South catalogs (Elbaz+, 2011)

Author

Elbaz, D., Dickinson, M., Hwang, H.~s., Diaz-Santos, T., Magdis, G., Magnelli, B., Le Borgne, Damien, Galliano, F., Pannella, M., Chanial, P., Armus, L., Charmandaris, V., Daddi, Emanuele, Aussel, H., Popesso, P., Kartaltepe, J., Altieri, B., Valtchanov, I., Coia, D., Dannerbauer, H., Dasyra, K., Leiton, R., Mazzarella, J., Alexander, D.~m., Buat, V., Burgarella, D., Chary, R.-R., Gilli, R., Ivison, R.~j., Juneau, S., Le Floc'H, E., Lutz, D., Morrison, G.~e., Mullaney, J.~r., Murphy, E., Pope, A., Scott, D., Brodwin, M., Calzetti, D., Cesarsky, C., Charlot, S., Dole, H., Eisenhardt, P., Ferguson, H.~c., Foerster Schreiber, N., Frayer, D., Giavalisco, M., Huynh, M., Koekemoer, A.~m., Papovich, C., Reddy, N., Surace, C., Teplitz, H., Yun, M.~s., Wilson, G., 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), National Optical Astronomy Observatory (NOAO), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Institut 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'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 Extraterrestrische Physik (MPE), AUTRES, Herschel Science Centre, Agence Spatiale Européenne = European Space Agency (ESA), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, 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 Nazionale di Astrofisica (INAF), Steward observatory, University of Arizona, Ecosystèmes lagunaires : organisation biologique et fonctionnement (ECOLAG), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut Français de Recherche pour l'Exploitation de la Mer (IFREMER)-Centre National de la Recherche Scientifique (CNRS), Department of Astronomy, University of Massachusetts System (UMASS), 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), 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), Histoire naturelle de l'Homme préhistorique (HNHP), Muséum national d'Histoire naturelle (MNHN)-Université de Perpignan Via Domitia (UPVD)-Centre National de la Recherche Scientifique (CNRS), Department of Astronomy [Amherst], University of Massachusetts [Amherst] (UMass Amherst), University of Massachusetts System (UMASS)-University of Massachusetts System (UMASS), Department of Physics and Astronomy [Riverside], University of California [Riverside] (UC Riverside), and University of California (UC)-University of California (UC)

Subjects
[INFO]Computer Science [cs], Surveys, Galaxies: IR, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Photometry: infrared, Galaxy catalogs
Abstract

International audience; The sample of high-redshift galaxies analyzed here consists of galaxies observed in the two Great Observatories Origins Deep Survey (GOODS) fields in the Northern and Southern hemispheres. Observations with the Herschel Space Observatory were obtained as part of the open time key program GOODS-Herschel (PI Elbaz), for a total time of 361.3h. PACS observations at 100 and 160um cover the whole GOODS-north field of 10'x16' and part of GOODS-south, i.e., 10'x10' (but reaching the largest depths over ~64arcmin^2). When considering the total observing times of 124h in GOODS-N and 206.3h in GOODS-S (including 2.6 and 5h of overheads), the PACS GOODS-Herschel observations reach a total integration time per sky position of 2.4h in GOODS-N and of 15.1h in GOODS-S, i.e., 6.3 times longer. Due to the larger beam size and observing configuration, the SPIRE observations of GOODS-N cover a field of 900 arcmin2, hence largely encompassing the central 10'x16', for a total observing time of 31.1h and an integration time per sky position of 16.8h. (2 data files).

Published
2013

12. The importance of major mergers in the build up of stellar mass in brightest cluster galaxies at z=1

Author

Strazzullo, V., Huertas-Company, M., Mei, S., Meyers, J., Muzzin, A., Noble, A., Nantais, J., Rettura, A., Rosati, P., Sánchez-Janssen, R., Webb, T., Wilson, G., Yan, R., Yee, H., Lidman, C., Iacobuta, G., Bauer, A., Barrientos, L., Cerulo, P., Couch, W., Gilbank, D., Faloon, A., Ellingson, E., Delaye, L., Demarco, R., Sanchez-Janssen, R., Lidman, C, Iacobuta, G, Bauer, Ae, Barrientos, Lf, Cerulo, P, Couch, Wj, Delaye, L, Demarco, R, Ellingson, E, Faloon, Aj, Gilbank, D, Huertas-Company, M, Mei, S, Meyers, J, Muzzin, A, Noble, A, Nantais, J, Rettura, A, Rosati, P, Sanchez-Janssen, R, Strazzullo, V, Webb, Tma, Wilson, G, Yan, R, Yee, Hkc, Centre for Astrophysics and Supercomputing [Swinburne] (CAS), Swinburne University of Technology [Melbourne], Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Universidad de Concepción [Chile], Center for Astrophysics and Space Astronomy [Boulder] (CASA), University of Colorado [Boulder], York University [Toronto], Department of Physics and Astronomy [Riverside], University of California [Riverside] (UCR), University of California-University of California, Università degli Studi di Ferrara (UniFE), European Southern Observatory [Santiago] (ESO), European Southern Observatory (ESO), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), and University of Ferrara [Ferrara]

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy merger, 01 natural sciences, Peculiar galaxy, 0103 physical sciences, Brightest cluster galaxy, 010303 astronomy & astrophysics, Galaxy cluster, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, Physics, Luminous infrared galaxy, [PHYS]Physics [physics], 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, Galaxy, Space and Planetary Science, Elliptical galaxy, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Recent independent results from numerical simulations and observations have shown that brightest cluster galaxies (BCGs) have increased their stellar mass by a factor of almost two between z~0.9 and z~0.2. The numerical simulations further suggest that more than half this mass is accreted through major mergers. Using a sample of 18 distant galaxy clusters with over 600 spectroscopically confirmed cluster members between them, we search for observational evidence that major mergers do play a significant role. We find a major merger rate of 0.38 +/- 0.14 mergers per Gyr at z~1. While the uncertainties, which stem from the small size of our sample, are relatively large, our rate is consistent with the results that are derived from numerical simulations. If we assume that this rate continues to the present day and that half of the mass of the companion is accreted onto the BCG during these mergers, then we find that this rate can explain the growth in the stellar mass of the BCGs that is observed and predicted by simulations. Major mergers therefore appear to be playing an important role, perhaps even the dominant one, in the build up of stellar mass in these extraordinary galaxies., Comment: 15 pages, 6 figures, accepted for publication in MNRAS. Reduced data will be made available through the ESO archive

Published
2013
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13. Material Dependence of the Wire-Particle Casimir Interaction

Author

Ehsan Noruzifar, Roya Zandi, Thorsten Emig, Pablo Rodriguez-Lopez, Department of Physics and Astronomy [Riverside], University of California [Riverside] (UCR), University of California-University of California, Departamento de Fisica Aplicada, Universidad Complutense de Madrid = Complutense University of Madrid [Madrid] (UCM), Laboratoire de Physique Théorique et Modèles Statistiques (LPTMS), and Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11)

Subjects
Physics, Casimir pressure, Statistical Mechanics (cond-mat.stat-mech), Condensed matter physics, Scattering, Isotropy, FOS: Physical sciences, 01 natural sciences, Atomic and Molecular Physics, and Optics, 010305 fluids & plasmas, Condensed Matter - Other Condensed Matter, Casimir effect, Formalism (philosophy of mathematics), Asymptotic form, 0103 physical sciences, [PHYS.COND.CM-SM]Physics [physics]/Condensed Matter [cond-mat]/Statistical Mechanics [cond-mat.stat-mech], 010306 general physics, Material properties, Condensed Matter - Statistical Mechanics, Other Condensed Matter (cond-mat.other)
Abstract

International audience; We study the Casimir interaction between a metallic cylindrical wire and a metallic spherical particle by employing the scattering formalism. At large separations, we derive the asymptotic form of the interaction. In addition, we find the interaction between a metallic wire and an isotropic atom, both in the non-retarded and retarded limits. We identify the conditions under which the asymptotic Casimir interaction does not depend on the material properties of the metallic wire and the particle. Moreover, we compute the exact Casimir interaction between the particle and the wire numerically. We show that there is a complete agreement between the numerics and the asymptotic energies at large separations. For short separations, our numerical results show good agreement with the proximity force approximation.

Published
2013

14. The Spitzer Extragalactic Representative Volume Survey (SERVS): Survey Definition and Goals

Author

E. A. Gonzalez-Solares, Roy R. Gal, Ray P. Norris, Luca Bizzocchi, Jamie Stevens, Huub Röttgering, S. A. Stanford, Marguerite Pierre, Giovanni Covone, Anna Sajina, Scott Chapman, A. M. J. Mortier, E. Dyke, D. Rigopoulou, Janine Pforr, Hugo Messias, S. Foucaud, A. Rettura, G. Parish, Steve Rawlings, S. J. Oliver, James Dunlop, H. C. Ferguson, Jose Afonso, N. Castro, Russell H. Taylor, Chris Simpson, Ian Smail, Bruno M. B. Henriques, Ross J. McLure, Nick Seymour, S. E. Ridgway, Lori M. Lubin, Tanya Urrutia, Jason Surace, Ismael Perez-Fournon, Antonio Cava, D. M. Nielsen, N. Dubois, M. Trichas, C. J. Lonsdale, Aprajita Verma, Gordon T. Richards, J. T. Falder, Minh Huynh, Philip Best, N. Christopher, James E. Geach, Jacqueline Hodge, R. H. Becker, David M. Alexander, E. van Kampen, Duncan Farrah, David L. Clements, Gordon K. Squires, Marco Grossi, A. Martinez-Sansigre, Alberto Franceschini, Alastair C. Edge, Mattia Vaccari, M. D. Lehnert, J. K. Grant, Peter A. Thomas, Masami Ouchi, Evanthia Hatziminaoglou, J.-S. Huang, Claudia Maraston, Gillian Wilson, Anthony C. S. Readhead, O. LeFevre, Mark Lacy, C. K. Xu, M. Kim, Gregory R. Zeimann, Samantha Hickey, A. K. Romer, Lucia Marchetti, Michael Rowan-Robinson, I. G. Rosebloom, Matt J. Jarvis, David Bonfield, Andreea Petric, J. C. Mauduit, Rob Ivison, Infrared Processing and Analysis Center (IPAC), California Institute of Technology (CALTECH), National Radio Astronomy Observatory [Charlottesville] (NRAO), National Radio Astronomy Observatory (NRAO), Department of Physics and Astronomy [Brighton] (DPA), University of Sussex, Centre for Astrophysics Research [Hatfield], University of Hertfordshire [Hatfield] (UH), Institute of Cosmology and Gravitation [Portsmouth] (ICG), University of Portsmouth, Dipartimento di Fisica e Astronomia 'Galileo Galilei', Università degli Studi di Padova = University of Padua (Unipd), University of the Western Cape (UWC), Visual servoing in robotics, computer vision, and augmented reality (Lagadic), Inria Sophia Antipolis - Méditerranée (CRISAM), Institut National de Recherche en Informatique et en Automatique (Inria)-Institut National de Recherche en Informatique et en Automatique (Inria)-Inria Rennes – Bretagne Atlantique, Institut National de Recherche en Informatique et en Automatique (Inria)-SIGNAUX ET IMAGES NUMÉRIQUES, ROBOTIQUE (IRISA-D5), Institut de Recherche en Informatique et Systèmes Aléatoires (IRISA), Université de Rennes (UR)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université de Bretagne Sud (UBS)-École normale supérieure - Rennes (ENS Rennes)-Institut National de Recherche en Informatique et en Automatique (Inria)-Télécom Bretagne-CentraleSupélec-Centre National de la Recherche Scientifique (CNRS)-Université de Rennes (UR)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université de Bretagne Sud (UBS)-École normale supérieure - Rennes (ENS Rennes)-Institut National de Recherche en Informatique et en Automatique (Inria)-Télécom Bretagne-CentraleSupélec-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche en Informatique et Systèmes Aléatoires (IRISA), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université de Bretagne Sud (UBS)-École normale supérieure - Rennes (ENS Rennes)-Télécom Bretagne-CentraleSupélec-Centre National de la Recherche Scientifique (CNRS), Department of Physics and Astronomy [Univ California Davis] (Physics - UC Davis), University of California [Davis] (UC Davis), University of California (UC)-University of California (UC), Institute of Astronomy [Cambridge], University of Cambridge [UK] (CAM), National Optical Astronomy Observatory (NOAO), Observatório Astronómico de Lisboa, Centro de Astronomia e Astrofísica da Universidade de Lisboa (CAAUL), Universidade de Lisboa = University of Lisbon (ULISBOA), Department of Physics and Astronomy [Riverside], University of California [Riverside] (UC Riverside), Department of Physics [Montréal], McGill University = Université McGill [Montréal, Canada], International Centre for Radio Astronomy Research (ICRAR), The University of Western Australia (UWA)-Government of Western Australia-Curtin University [Perth], Planning and Transport Research Centre (PATREC)-Planning and Transport Research Centre (PATREC), CSIRO Astronomy and Space Science, Commonwealth Scientific and Industrial Research Organisation [Canberra] (CSIRO), Department of Physics - Drexel University, Drexel University, Lawrence Livermore National Laboratory (LLNL), Department of Physics [Durham University], Durham University, Royal Observatory Edinburgh (ROE), University of Edinburgh, Instituto de Astrofisica de Canarias (IAC), Department of Physics [Oxford], University of Oxford, Astrophysics Group, Blackett Laboratory, Imperial College London-Imperial College London, Dipartimento di Scienze Fisiche [Naples], University of Naples Federico II = Università degli studi di Napoli Federico II, Institute for Computational Cosmology (ICC), Space Telescope Science Institute (STSci), National Taiwan Normal University (NTNU), University of Hawai'i [Honolulu] (UH), Department of Physics and Astronomy [Calgary], University of Calgary, European Southern Observatory (ESO), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Department of Astronomy [Madison], University of Wisconsin-Madison, Carnegie Institution for Science, Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Caltech Department of Astronomy [Pasadena], Cerro Tololo Inter-American Observatory, Leiden Observatory [Leiden], Universiteit Leiden, Haverford College, Astrophysics Research Institute [Liverpool] (ARI), Liverpool John Moores University (LJMU), Leibniz Institute for Astrophysics Potsdam (AIP), Mauduit, J. C., Lacy, M., Farrah, D., Surace, J. A., Jarvis, M., Oliver, S., Maraston, C., Vaccari, M., Marchetti, L., Zeimann, G., Gonzalez Solares, E. A., Pforr, J., Petric, A. O., Henriques, B., Thomas, P. A., Afonso, J., Rettura, A., Wilson, G., Falder, J. T., Geach, J. E., Huynh, M., Norris, R. P., Seymour, N., Richards, G. T., Stanford, S. A., Alexander, D. M., Becker, R. H., Best, P. N., Bizzocchi, L., Bonfield, D., Castro, N., Cava, A., Chapman, S., Christopher, N., Clements, D. L., Covone, Giovanni, Dubois, N., Dunlop, J. S., Dyke, E., Edge, A., Ferguson, H. C., Foucaud, S., Franceschini, A., Gal, R. R., Grant, J. K., Grossi, M., Hatziminaoglou, E., Hickey, S., Hodge, J. A., Huang, J. S., Ivison, R. J., Kim, M., Lefevre, O., Lehnert, M., Lonsdale, C. J., Lubin, L. M., Mclure, R. J., Messias, H., Martinez Sansigre, A., Mortier, A. M. J., Nielsen, D. M., Ouchi, M., Parish, G., Perez Fournon, I., Pierre, M., Rawlings, S., Readhead, A., Ridgway, S. E., Rigopoulou, D., Romer, A. K., Rosebloom, I. G., Rottgering, H. J. A., Rowan Robinson, M., Sajina, A., Simpson, C. J., Smail, I., Squires, G. K., Stevens, J. A., Taylor, R., Trichas, M., Urrutia, T., van Kampen, E., Verma, A., Xu, C. K., Universita degli Studi di Padova, University of the Western Cape, CentraleSupélec-Télécom Bretagne-Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Institut National de Recherche en Informatique et en Automatique (Inria)-École normale supérieure - Rennes (ENS Rennes)-Université de Bretagne Sud (UBS)-Centre National de la Recherche Scientifique (CNRS)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Université de Rennes (UNIV-RENNES)-Institut National des Sciences Appliquées (INSA)-CentraleSupélec-Télécom Bretagne-Université de Rennes 1 (UR1), Institut National des Sciences Appliquées (INSA)-Université de Rennes (UNIV-RENNES)-Institut National des Sciences Appliquées (INSA)-Institut de Recherche en Informatique et Systèmes Aléatoires (IRISA), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-École normale supérieure - Rennes (ENS Rennes)-Université de Bretagne Sud (UBS)-Centre National de la Recherche Scientifique (CNRS)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Université de Rennes (UNIV-RENNES)-Institut National des Sciences Appliquées (INSA), Department of Physics [Davis], University of California-University of California, Universidade de Lisboa (ULISBOA), University of California [Riverside] (UCR), University of Oxford [Oxford], Università degli studi di Napoli Federico II, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Carnegie Institution for Science [Washington], and Universiteit Leiden [Leiden]

Subjects
Physics, evoluzione delle galassie, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Volume (computing), FOS: Physical sciences, Astronomy and Astrophysics, Context (language use), Quasar, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Galaxy, Spitzer Space Telescope, Space and Planetary Science, 0103 physical sciences, Galaxy formation and evolution, Chandra Deep Field South, survey astronomica, 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present the Spitzer Extragalactic Representative Volume Survey (SERVS), an 18 square degrees medium-deep survey at 3.6 and 4.5 microns with the post-cryogenic Spitzer Space Telescope to ~2 microJy (AB=23.1) depth of five highly observed astronomical fields (ELAIS-N1, ELAIS-S1, Lockman Hole, Chandra Deep Field South and XMM-LSS). SERVS is designed to enable the study of galaxy evolution as a function of environment from z~5 to the present day, and is the first extragalactic survey both large enough and deep enough to put rare objects such as luminous quasars and galaxy clusters at z>1 into their cosmological context. SERVS is designed to overlap with several key surveys at optical, near- through far-infrared, submillimeter and radio wavelengths to provide an unprecedented view of the formation and evolution of massive galaxies. In this paper, we discuss the SERVS survey design, the data processing flow from image reduction and mosaicing to catalogs, as well as coverage of ancillary data from other surveys in the SERVS fields. We also highlight a variety of early science results from the survey., 21 pages, 23 figures, published in PASP. This version differs slightly from PASP, mainly due to formatting issues. Figure 2 was also corrected from the previous version

Published
2012

15. EARLY-TYPE GALAXIES AT z ∼ 1.3. IV. SCALING RELATIONS IN DIFFERENT ENVIRONMENTS

Author

S. A. Stanford, Myungkook J. Jee, R. L. White, A. Rettura, Francesco Shankar, Masayuki Tanaka, Marc Huertas-Company, Marc Postman, R. Demarco, T. Kodama, Fumiaki Nakata, Bradford P. Holden, G. D. Illingworth, Holland C. Ford, Anand Raichoor, Piero Rosati, John P. Blakeslee, Simona Mei, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Department of Physics and Astronomy [Riverside], University of California [Riverside] (UCR), University of California-University of California, and Departamento de Industrias, Universidad Técnica Federico Santa María, Av. España 1680, Valparaíso, Chile

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010504 meteorology & atmospheric sciences, Population, FOS: Physical sciences, Astrophysics, 01 natural sciences, NO, cD, Photometry (optics), galaxies: high-redshift, 0103 physical sciences, Cluster (physics), galaxies: formation, galaxies: elliptical and lenticular, education, 010303 astronomy & astrophysics, Scaling, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Physics, [PHYS]Physics [physics], education.field_of_study, Similar distribution, galaxies: fundamental parameters, Astronomy and Astrophysics, Galaxy, Early type, galaxies: elliptical and lenticular, cD, galaxies: evolution, Space and Planetary Science, Cluster sampling, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present the Kormendy and mass-size relations for early-type galaxies (ETGs) as a function of environment at z~1.3. Our sample includes 76 visually classified ETGs with masses 10^10 < M/Msun < 10^11.5, selected in the Lynx supercluster and in the GOODS/CDF-S field, 31 ETGs in clusters, 18 in groups and 27 in the field, all with multi-wavelength photometry and HST/ACS observations. The Kormendy relation, in place at z~1.3, does not depend on the environment. The mass-size relation reveals that ETGs overall appear to be more compact in denser environments: cluster ETGs have sizes on average around 30-50% smaller than those of the local universe, and a distribution with a smaller scatter, whereas field ETGs show a mass-size relation with a similar distribution than the local one. Our results imply that (1) the mass-size relation in the field did not evolve overall from z ~ 1.3 to present; this is interesting and in contrast to the trend found at higher masses from previous works; (2) in denser environments, either ETGs have increased their size by 30-50%, on average, and spread their distributions, or more ETGs have been formed within the dense environment from not ETG progenitors or larger galaxies have been accreted to a pristine compact population to reproduce the mass-size relation observed in the local Universe. Our results are driven by galaxies with masses M, 20 pages, ApJ in press

Published
2012

16. GOODS-HERSCHEL MEASUREMENTS OF THE DUST ATTENUATION OF TYPICAL STAR-FORMING GALAXIES AT HIGH REDSHIFT: OBSERVATIONS OF ULTRAVIOLET-SELECTED GALAXIES AT z similar to 2

Author

Roger Leiton, J. Kartaltepe, Naveen A. Reddy, V. Charmandaris, Bruno Altieri, Georgios E. Magdis, P. Popesso, H. Aussel, Benjamin Magnelli, Kalliopi Dasyra, V. Buat, Rob Ivison, M. Giavalisco, Helmut Dannerbauer, Denis Burgarella, Eric J. Murphy, C. Papovich, Ho Seong Hwang, Mark Dickinson, Douglas Scott, G. E. Morrison, E. Daddi, D. Elbaz, Department of Physics and Astronomy [Riverside], University of California [Riverside] (UCR), University of California-University of California, NOAO, 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), Institute for Astronomy [Honolulu], University of Hawai‘i [Mānoa] (UHM), Department of Astronomy [Amherst], University of Massachusetts [Amherst] (UMass Amherst), University of Massachusetts System (UMASS)-University of Massachusetts System (UMASS), Royal Observatory Edinburgh (ROE), University of Edinburgh, AUTRES, Department of Physics and Astronomy [Vancouver], University of British Columbia (UBC), 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), IESL, Herschel Science Centre, European Space Agency (ESA), 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), Max-Planck-Institut für Extraterrestrische Physik (MPE), University of California [Riverside] (UC Riverside), University of California (UC)-University of California (UC), National Optical Astronomy Observatory (NOAO), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Texas A&M University [College Station], Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), University of Crete [Heraklion] (UOC), Spitzer Science Center, California Institute of Technology (CALTECH), and Agence Spatiale Européenne = European Space Agency (ESA)

Subjects
Physics, Luminous infrared galaxy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Infrared, Star formation, Attenuation, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Billion years, Galaxy, Redshift, Space and Planetary Science, 0103 physical sciences, Thermal, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We take advantage of the sensitivity and resolution of Herschel at 100 and 160 micron to directly image the thermal dust emission and investigate the infrared luminosities, L(IR), and dust obscuration of typical star-forming (L*) galaxies at high redshift. Our sample consists of 146 UV-selected galaxies with spectroscopic redshifts 1.51e10 Lsun at z~2 are luminous infrared galaxies (LIRGs) with a median L(IR)=(2.2+/-0.3)e11 Lsun. Typical galaxies at 1.5, Comment: 19 pages, 10 figures, 5 tables, submitted to the Astrophysical Journal

Published
2012

17. The Molecular Gas Content of Z = 3 Lyman Break Galaxies: Evidence of a Non-Evolving Gas Fraction in Main-Sequence Galaxies At Z > 2

Author

Chiara Feruglio, Georgios E. Magdis, Helmut Dannerbauer, Mark Dickinson, Raphael Gobat, Emanuele Daddi, Qinghua Tan, Vassilis Charmandaris, M. T. Sargent, D. Rigopoulou, N. Reddy, D. Elbaz, Herve Aussel, Department of Physics [Oxford], University of Oxford [Oxford], 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), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), Space Science and Technology Department [Didcot] (RAL Space), STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC)-Science and Technology Facilities Council (STFC), IESL, National Optical Astronomy Observatory (NOAO), Department of Physics and Astronomy [Riverside], University of California [Riverside] (UCR), University of California-University of California, UPGAL, ANR-08-JCJC-0008,UPGAL(2008), European Project: 240039,EC:FP7:ERC,ERC-2009-StG,UPGAL(2009), Department of Physics, NOAO, University of Oxford, 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), University of California [Riverside] (UC Riverside), and University of California (UC)-University of California (UC)

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Infrared, Star formation, FOS: Physical sciences, Plateau de Bure Interferometer, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Mass ratio, Plateau (mathematics), 01 natural sciences, Redshift, Flattening, Galaxy, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 13. Climate action, Space and Planetary Science, 0103 physical sciences, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present observations of the CO[3-2] emission towards two massive and infrared luminous Lyman Break Galaxies at z = 3.21 and z = 2.92, using the IRAM Plateau de Bure Interferometer, placing first constraints on the molecular gas masses (Mgas) of non-lensed LBGs. Their overall properties are consistent with those of typical (Main-Sequence) galaxies at their redshifts, with specific star formation rates ~1.6 and ~2.2 Gyr^(-1), despite their large infrared luminosities L_IR ~2-3 x 10^12 Lsun derived from Herschel. With one plausible CO detection (spurious detection probability of 10^(-3)) and one upper limit, we investigate the evolution of the molecular gas-to-stellar mass ratio (Mgas/M*) with redshift. Our data suggest that the steep evolution of Mgas/M* of normal galaxies up to z~2 is followed by a flattening at higher redshifts, providing supporting evidence for the existence of a plateau in the evolution of the specific star formation rate at z > 2.5., Accepted for publication in ApJL

Published
2012

18. Wrinkling Hierarchy in Constrained Thin Sheets from Suspended Graphene to Curtains

Author

Hugues Vandeparre, Miguel Piñeirua, Fabian Brau, Benoit Roman, José Bico, Cyprien Gay, Wenzhong Bao, Chun Ning Lau, Pedro M. Reis, Pascal Damman, Interfaces & Fluides Complexes (INFLUX), Université de Mons (UMons), Physique et mécanique des milieux hétérogenes (UMR 7636) (PMMH), Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Matière et Systèmes Complexes (MSC (UMR_7057)), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Department of Physics and Astronomy [Riverside], University of California [Riverside] (UCR), University of California-University of California, Department of Mechanical Engineering [Massachusetts Institute of Technology] (MIT-MECHE), Massachusetts Institute of Technology (MIT), Department of Civil and Environmental Engineering [Cambridge] (CEE), Physique et mécanique des milieux hétérogenes (PMMH), Centre National de la Recherche Scientifique (CNRS)-ESPCI ParisTech-Université Paris Diderot - Paris 7 (UPD7)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Department of Mechanical Engineering (MIT-MECHE), and Department of Civil and Environmental Engineering [Cambridge, USA] (CEE)

Subjects
Materials science, Nucleation, FOS: Physical sciences, General Physics and Astronomy, Nanotechnology, 02 engineering and technology, hierarchy, Condensed Matter - Soft Condensed Matter, 01 natural sciences, law.invention, law, 0103 physical sciences, Miniaturization, Electronics, 46.32.+x, Thin film, 010306 general physics, [NLIN.NLIN-AO]Nonlinear Sciences [physics]/Adaptation and Self-Organizing Systems [nlin.AO], Elasticité, Condensed Matter - Materials Science, Graphene, sheet elasticity, Materials Science (cond-mat.mtrl-sci), Mechanical failure, Thin sheet, bending, Physique des phénomènes non linéaires, 021001 nanoscience & nanotechnology, Engineering physics, Nonlinear Sciences - Adaptation and Self-Organizing Systems, Condensed Matter::Soft Condensed Matter, [PHYS.COND.CM-MS]Physics [physics]/Condensed Matter [cond-mat]/Materials Science [cond-mat.mtrl-sci], Mécanique des milieux continus, Soft Condensed Matter (cond-mat.soft), Fuel cells, elasticity, wrinkling, 0210 nano-technology, Adaptation and Self-Organizing Systems (nlin.AO), [PHYS.COND.CM-SCM]Physics [physics]/Condensed Matter [cond-mat]/Soft Condensed Matter [cond-mat.soft]
Abstract

We show that thin sheets under boundary confinement spontaneously generate a universal self-similar hierarchy of wrinkles. From simple geometry arguments and energy scalings, we develop a formalism based on wrinklons, the transition zone in the merging of two wrinkles, as building-blocks of the global pattern. Contrary to the case of crumple paper where elastic energy is focused, this transition is described as smooth in agreement with a recent numerical work. This formalism is validated from hundreds of nm for graphene sheets to meters for ordinary curtains, which shows the universality of our description. We finally describe the effect of an external tension to the distribution of the wrinkles., 7 pages, 4 figures, added references, submitted for publication

Published
2011

19. Universality versus material dependence of fluctuation forces between metallic wires

Author

Ehsan Noruzifar, Roya Zandi, Thorsten Emig, Department of Physics and Astronomy [Riverside], University of California [Riverside] (UCR), University of California-University of California, Laboratoire de Physique Théorique et Modèles Statistiques (LPTMS), and Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11)

Subjects
Physics, Condensed matter physics, Statistical Mechanics (cond-mat.stat-mech), 010308 nuclear & particles physics, Numerical analysis, Sigma, FOS: Physical sciences, Dielectric, Plasma, Condensed Matter::Mesoscopic Systems and Quantum Hall Effect, 01 natural sciences, Atomic and Molecular Physics, and Optics, Universality (dynamical systems), Casimir effect, Metal, visual_art, 0103 physical sciences, visual_art.visual_art_medium, Condensed Matter::Strongly Correlated Electrons, [PHYS.COND.CM-SM]Physics [physics]/Condensed Matter [cond-mat]/Statistical Mechanics [cond-mat.stat-mech], 010306 general physics, Material properties, Condensed Matter - Statistical Mechanics
Abstract

International audience; We calculate the Casimir interaction between two parallel wires and between a wire and a metall plate. The dielectric properties of the objects are described by the plasma, Drude and perfect metal models. We find that at asymptotically large separation interactions involving plasma wires and/or plates are independent of the material properties, but depend on the dc conductivity $\sigma$ for Drude wires. Counterintuitively, at intermediate separations the interaction involving Drude wires can become independent of $\sigma$. At smaller separations, we compute the interaction numerically and observe an approach to the proximity approximation.

Published
2011

20. Quantum and thermal Casimir interaction between a sphere and a plate: Comparison of Drude and plasma models

Author

Roya Zandi, Thorsten Emig, Umar Mohideen, Department of Physics and Astronomy [Riverside], University of California [Riverside] (UCR), University of California-University of California, Institut für Theoretische Physik [Köln], Universität zu Köln, Laboratoire de Physique Théorique et Modèles Statistiques (LPTMS), and Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11)

Subjects
Superconductivity, Physics, Statistical Mechanics (cond-mat.stat-mech), Condensed matter physics, 010308 nuclear & particles physics, FOS: Physical sciences, Condensed Matter Physics, Magnetostatics, 01 natural sciences, Drude model, Electronic, Optical and Magnetic Materials, Magnetic field, Casimir effect, symbols.namesake, Entropy (classical thermodynamics), 0103 physical sciences, symbols, Drude particle, [PHYS.COND.CM-SM]Physics [physics]/Condensed Matter [cond-mat]/Statistical Mechanics [cond-mat.stat-mech], 010306 general physics, Quantum, Condensed Matter - Statistical Mechanics
Abstract

We calculate the Casimir interaction between a sphere and a plate, both described by the plasma model, the Drude model, or generalizations of the two models. We compare the results at both zero and finite temperatures. At asymptotically large separations we obtain analytical results for the interaction that reveal a non-universal, i.e., material dependent interaction for the plasma model. The latter result contains the asymptotic interaction for Drude metals and perfect reflectors as different but universal limiting cases. This observation is related to the screening of a static magnetic field by a London superconductor. For small separations we find corrections to the proximity force approximation (PFA) that support correlations between geometry and material properties that are not captured by the Lifshitz theory. Our results at finite temperatures reveal for Drude metals a non-monotonic temperature dependence of the Casimir free energy and a negative entropy over a sizeable range of separations., Comment: 11 pages, 5 figures

Published
2010

21. Superconductor-Insulator transition and energy localization

Author

Lev Ioffe, Mikhail Feigel'man, Marc Mézard, L.D. Landau Institute for Theoretical Physics of RAS, Russian Academy of Sciences [Moscow] (RAS), Moscow Institute of Physics and Technology [Moscow] (MIPT), Laboratoire de Physique Théorique et Modèles Statistiques (LPTMS), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), Department of Physics and Astronomy [Riverside], University of California [Riverside] (UCR), and University of California-University of California

Subjects
Physics, Quantum phase transition, Quantum Physics, Condensed matter physics, Bethe lattice, Condensed Matter - Superconductivity, FOS: Physical sciences, Disordered Systems and Neural Networks (cond-mat.dis-nn), Condensed Matter - Disordered Systems and Neural Networks, Condensed Matter Physics, 01 natural sciences, Omega, 010305 fluids & plasmas, Electronic, Optical and Magnetic Materials, [PHYS.COND.CM-S]Physics [physics]/Condensed Matter [cond-mat]/Superconductivity [cond-mat.supr-con], Superconductivity (cond-mat.supr-con), Superconductor Insulator Transition, [PHYS.QPHY]Physics [physics]/Quantum Physics [quant-ph], Critical point (thermodynamics), Quantum critical point, 0103 physical sciences, Spin model, 010306 general physics, Quantum Physics (quant-ph), Dimensionless quantity
Abstract

We develop an analytical theory for generic disorder-driven quantum phase transitions. We apply this formalism to the superconductor-insulator transition and we briefly discuss the applications to the order-disorder transition in quantum magnets. The effective spin-1/2 models for these transitions are solved in the cavity approximation which becomes exact on a Bethe lattice with large branching number K >> 1 and weak dimensionless coupling g << 1. The characteristic features of the low temperature phase is a large self-formed inhomogeneity of the order-parameter distribution near the critical point K_{c}(g) where the critical temperature T_{c} of the ordering transition vanishes. Near the quantum critical point, the typical value of the order parameter vanishes exponentially, B_{0}\propto e^{-C/(K-K_{c}(g))}. In the disordered regime, realized at K\omega_{d} the level acquire a non-zero width which is self-generated by the many-body interactions. In this phase the spin model provides by itself an intrinsic thermal bath. Another phase is obtained at smaller K, Comment: 59 pages, 11 figures

Published
2010
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22. Phase coherence, visibility, and the superfluid-mott-insulator transition on one-dimensional optical lattices

Author

G. George Batrouni, Pinaki Sengupta, P. J. H. Denteneer, Richard T. Scalettar, Marcos Rigol, Department of Physics and Astronomy [Riverside], University of California [Riverside] (UCR), University of California-University of California, Department of Physics [Davis], University of California [Davis] (UC Davis), Institut Non Linéaire de Nice Sophia-Antipolis (INLN), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Centre National de la Recherche Scientifique (CNRS), Lorentz Institute, and Universiteit Leiden [Leiden]

Subjects
localised states, PACS : 03.75Hh, O3.75Lm, 05.30Jp, Quantum Monte Carlo, Monte Carlo method, FOS: Physical sciences, General Physics and Astronomy, Bose-Einstein condensation, 01 natural sciences, 010305 fluids & plasmas, law.invention, laser cooling, Superfluidity, law, Lattice (order), Laser cooling, 0103 physical sciences, metal-insulator transition, Metal–insulator transition, 010306 general physics, Condensed Matter::Quantum Gases, Physics, Condensed matter physics, Mott insulator, Monte Carlo methods, 3. Good health, Condensed Matter - Other Condensed Matter, atom-photon collisions, superfluidity, Quantum Gases (cond-mat.quant-gas), [PHYS.COND.CM-GEN]Physics [physics]/Condensed Matter [cond-mat]/Other [cond-mat.other], Condensed Matter - Quantum Gases, Bose–Einstein condensate, Other Condensed Matter (cond-mat.other)
Abstract

We study the phase coherence and visibility of trapped atomic condensates on one-dimensional optical lattices, by means of quantum Monte-Carlo simulations. We obtain structures in the visibility similar to the kinks recently observed experimentally by Gerbier et.al.[Phy. Rev. Lett. 95, 050404 (2005); Phys. Rev. A 72, 053606 (2005)]. We examine these features in detail and offer a connection to the evolution of the density profiles as the depth of the lattice is increased. Our simulations reveal that as the interaction strength, U, is increased, the evolution of superfluid and Mott-insulating domains stall for finite intervals of U. The density profiles do not change with increasing U. We show here that in one dimension the visibility provides unequivocal signatures of the melting of Mott domains with densities larger than one., 4 pages, 5 figures

Published
2005

23. The XXL survey: first results and future

Author

Pierre, M., Adami, C., Birkinshaw, M., Chiappetti, L., Ettori, S., Evrard, A., Faccioli, L., Gastaldello, F., Giles, P., Horellou, C., Iovino, A., Koulouridis, E., Lidman, C., Brun, A. Le, Maughan, B., Maurogordato, S., McCarthy, I., Miyazaki, S., Pacaud, F., Paltani, S., Plionis, M., Reiprich, T., Sadibekova, T., Smolcic, V., Snowden, S., Surdej, J., Tsirou, M., Vignali, C., Willis, J., Alis, S., Altieri, B., Baran, N., Benoist, C., Bongiorno, A., Bremer, M., Butler, A., Cappi, A., Caretta, C., Ciliegi, P., Clerc, N., Corasaniti, P. S., Coupon, J., Delhaize, J., Delvecchio, I., Democles, J., Desai, Sh., Devriendt, J., Dubois, Y., Eckert, D., Elyiv, A., Farahi, A., Ferrari, C., Fotopoulou, S., Forman, W., Georgantopoulos, I., Guglielmo, V., Huynh, M., Jerlin, N., Jones, Ch., Lavoie, S., Fevre, J. -P. Le, Lieu, M., Kilbinger, M., Marulli, F., Mantz, A., McGee, S., Melin, J. -B., Melnyk, O., Moscardini, L., Novak, M., Piconcelli, E., Poggianti, B., Pomarede, D., Pompei, E., Ponman, T., Ceja, M. E. Ramos, Ranalli, P., Rapetti, D., Raychaudhury, S., Ricci, M., Rottgering, H., Sahlén, M., Sauvageot, J. -L., Schimd, C., Sereno, M., Smith, G. P., Umetsu, K., Valageas, P., Valotti, A., Valtchanov, I., Veropalumbo, A., Ascaso, B., Barnes, D., De Petris, M., Durret, F., Donahue, M., Ithana, M., Jarvis, M., Johnston-Hollitt, M., Kalfountzou, E., Kay, S., La Franca, F., Okabe, N., Muzzin, A., Rettura, A., Ricci, F., Ridl, J., Risaliti, G., Takizawa, M., Thomas, P., Truong, N., Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), University of Bristol [Bristol], Istituto Nazionale di Astrofisica (INAF), Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano (IASF-MI), INAF - Osservatorio Astronomico di Bologna (OABO), University of Michigan [Ann Arbor], University of Michigan System, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Department of Earth and Space Sciences [Göteborg], Chalmers University of Technology [Göteborg], 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), Anglo-Australian Observatory (AAO), Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA), University of Liverpool, National Astronomical Observatory of Japan (NAOJ), Rheinische Friedrich-Wilhelms-Universität Bonn, Department of Physics [Thessaloniki], Aristotle University of Thessaloniki, Argelander-Institut für Astronomie (AlfA), University of Zagreb, NASA Goddard Space Flight Center (GSFC), Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, University of Victoria [Canada] (UVIC), Istanbul University, European Space Astronomy Centre (ESAC), European Space Agency (ESA), INAF - Osservatorio Astronomico di Roma (OAR), Department of Physics [Oxford], University of Oxford [Oxford], Max Planck Institute for Extraterrestrial Physics (MPE), Max-Planck-Gesellschaft, 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), 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), Indian Institute of Technology [Hyderabad] (IIT Hyderabad), University of Geneva [Switzerland], Uppsala University, INTEGRAL Science Data Center (ISDC), Geneva Observatory, University of Geneva [Switzerland]-University of Geneva [Switzerland], Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University [Cambridge]-Smithsonian Institution, Institute for Space Applications and Remote Sensing (ISARS/NOA), National Observatory of Athens (NOA), The University of Western Australia (UWA), University of Bologna, University of Chicago, University of Birmingham [Birmingham], CEA, DSM, SPP, Commissariat à l'énergie atomique et aux énergies alternatives (CEA), INAF - Osservatorio Astronomico di Padova (OAPD), European Southern Observatory (ESO), Lund University [Lund], University of Colorado [Boulder], Inter-University Centre for Astronomy and Astrophysics [Pune] (IUCAA), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Institut des Sciences Moléculaires d'Orsay (ISMO), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Academia Sinica Institute of Astronomy and Astrophysics (ASIAA), Academia Sinica, Service de Physique Théorique (SPhT), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS), 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), Jodrell Bank Centre for Astrophysics (JBCA), University of Manchester [Manchester], Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Yamagata University, Victoria University of Wellington, Roma Tre University, Hiroshima University, York University [Toronto], Department of Physics and Astronomy [Riverside], University of California [Riverside] (UCR), University of California-University of California, Caltech Department of Astronomy [Pasadena], California Institute of Technology (CALTECH), INAF - Osservatorio Astrofisico di Arcetri (OAA), University of Sussex, Università degli Studi di Roma Tor Vergata [Roma], 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)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), Smithsonian Institution-Harvard University [Cambridge], Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), 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), Université Côte d'Azur (UCA), PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), National Observatory of Athens, Institute for Space Applications and Remote Sensing, 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)-Centre National de la Recherche Scientifique (CNRS), Jodrell Bank Centre for Astrophysics, Università degli Studi di Roma 'La Sapienza' [Rome], Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Pierre, M, Adami, C., Birkinshaw, M., Chiappetti, L., Ettori, S., Evrard, A., Faccioli, L., Gastaldello, F., Giles, P., Horellou, C., Iovino, A., Koulouridis, E., Lidman, C., Le Brun, A., Maughan, B., Maurogordato, S., Mccarthy, I., Miyazaki, S., Pacaud, F., Paltani, S., Plionis, M., Reiprich, T., Sadibekova, T., Smolcic, V., Snowden, S., Surdej, J., Tsirou, M., Vignali, C., Willis, J., Alis, S., Altieri, B., Baran, N., Benoist, C., Bongiorno, A., Bremer, M., Butler, A., Cappi, A., Caretta, C., Ciliegi, P., Clerc, N., Corasaniti, P.S., Coupon, J., Delhaize, J., Delvecchio, I., Democles, J., Desai, Sh., Devriendt, J., Dubois, Y., Eckert, D., Elyiv, A., Farahi, A., Ferraril, C., Fotopoulou, S., Forman, W., Georgantopoulos, I., Guglielmo, V., Huynh, M., Jerlin, N., Jones, Ch., Lavoie, S., Le Fevre, J.-P., Lieu, M., Kilbinger, M., Marulli, F., Mantz, A., Mcgee, S., Melin, J.-B., Melnyk, O., Moscardini, L., Novak, M., Piconcelli, E., Poggianti, B., Pomarede, D., Pompei, E., Ponman, T., Ramos Ceja, M.E., Rana, P., Rapetti, D., Raychaudhury, S., Ricci, M., Rottgering, H., Sahlen, M., Sauvageot, J.-L., Schimd, C., Sereno, M., Smith, G.P., Umetsu, K., Valageas, P., Valotti, A., Valtchanov, I., Veropalumbo, A., Ascaso, B., Barnes, D., De Petris, M., Durret, F., Donahue, M., Ithana, M., Jarvis, M., Johnston-Hollitt, M., Kalfountzou, E., Kay, S., La Franca, F., Okabe, N., Muzzin, A., Rettura, A., Ricci, F., Ridl, J., Risaliti, G., Takizawa, M., Thomas, P., Truong, N., Corasaniti, P. S., Desai, S. h., Jones, C. h., Le Fevre, J. P., Maruili, F., Melin, J. B., Ramos Ceja, M. E., Sauvageot, J. L., Smith, G. P., Johnston Hollitt, M., LA FRANCA, Fabio, Ricci, Federica, 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), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA), Agence Spatiale Européenne = European Space Agency (ESA), University of Oxford, Université de Genève = University of Geneva (UNIGE), Université de Genève = University of Geneva (UNIGE)-Université de Genève = University of Geneva (UNIGE), Harvard University-Smithsonian Institution, University of Bologna/Università di Bologna, Universiteit Leiden, 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), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA), Università degli Studi Roma Tre = Roma Tre University (ROMA TRE), University of California [Riverside] (UC Riverside), and University of California (UC)-University of California (UC)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], galaxies: active, X-ray: general, FOS: Physical sciences, Astronomy and Astrophysic, Astrophysics - Astrophysics of Galaxies, XXL survey, Space and Planetary Science, galaxies: clusters: general, Astrophysics of Galaxies (astro-ph.GA), active [galaxies], clusters: general [galaxies], cosmological parameter, X-ray:general, cosmological parameters, general [X-ray], QC, Astrophysics - Cosmology and Nongalactic Astrophysics, QB
Abstract

The XXL survey currently covers two 25 sq. deg. patches with XMM observations of ~10ks. We summarise the scientific results associated with the first release of the XXL data set, that occurred mid 2016. We review several arguments for increasing the survey depth to 40 ks during the next decade of XMM operations. X-ray (z1 cluster density. It will eventually constitute a reference study and an ideal calibration field for the upcoming eROSITA and Euclid missions., Proceeding of the XMM Next Decade Workshop held at ESAC, 9-11 May 2016

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