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547 results on '"Max Planck Institut für Extraterrestrische Physik (MPE)"'

151. The XXL Survey:XIII. Baryon content of the bright cluster sample

Author: S. Lavoie, Jean-Baptiste Melin, Marguerite Pierre, Ian G. McCarthy, L. Faccioli, Jean Coupon, M. Lieu, Dominique Eckert, L. Chiappetti, Stefano Ettori, Adam Mantz, Florian Pacaud, Stéphane Paltani, J. P. Lefevre, Sean L. McGee, C. Adami, Fabio Gastaldello, F. Ziparo, B. J. Maughan, A. M. C. Le Brun, Paul Giles, T. Sadibekova, Graham P. Smith, University of Geneva [Switzerland], INAF-IASF Milano, Istituto Nazionale di Astrofisica (INAF), INAF - Osservatorio Astronomico di Bologna (OABO), 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), Ecosystèmes aquatiques et changements globaux (UR EABX), Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA), Département de Physique des Particules (ex SPP) (DPP), 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), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), INAF- Milano, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Université Quebec, Université du Québec à Chicoutimi (UQAC), B. Maughan, CEA/DCC/DRRV/SCD, Commissariat à l'Energie Atomique, Marcoule, Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), ISDC Data Centre for Astrophysics, 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), University of Reading (UOR), Max-Planck-Institut für Extraterrestrische Physik (MPE), Université de Genève = University of Geneva (UNIGE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Département de Physique des Particules (ex SPP) (DPhP), 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), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), and 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)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Population, Cosmic microwave background, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, Cluster (physics), clusters: general [galaxies], education, 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, QB, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), education.field_of_study, 010308 nuclear & particles physics, groups: general [galaxies], Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Baryon, Stars, Space and Planetary Science, [SDU]Sciences of the Universe [physics], clusters: intracluster medium [galaxies], Astrophysics of Galaxies (astro-ph.GA), Content (measure theory), Halo, galaxies: clusters [X-rays], large-scale structure of Universe, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Traditionally, galaxy clusters have been expected to retain all the material accreted since their formation epoch. For this reason, their matter content should be representative of the Universe as a whole, and thus their baryon fraction should be close to the Universal baryon fraction. We make use of the sample of the 100 brightest galaxy clusters discovered in the XXL Survey to investigate the fraction of baryons in the form of hot gas and stars in the cluster population. We measure the gas masses of the detected halos and use a mass--temperature relation directly calibrated using weak-lensing measurements for a subset of XXL clusters to estimate the halo mass. We find that the weak-lensing calibrated gas fraction of XXL-100-GC clusters is substantially lower than was found in previous studies using hydrostatic masses. Our best-fit relation between gas fraction and mass reads $f_{\rm gas,500}=0.055_{-0.006}^{+0.007}\left(M_{\rm 500}/10^{14}M_\odot\right)^{0.21_{-0.10}^{+0.11}}$. The baryon budget of galaxy clusters therefore falls short of the Universal baryon fraction by about a factor of two at $r_{\rm 500}$. Our measurements require a hydrostatic bias $1-b=M_X/M_{\rm WL}=0.72_{-0.07}^{+0.08}$ to match the gas fraction obtained using lensing and hydrostatic equilibrium. Comparing our gas fraction measurements with the expectations from numerical simulations, our results favour an extreme feedback scheme in which a significant fraction of the baryons are expelled from the cores of halos. This model is, however, in contrast with the thermodynamical properties of observed halos, which might suggest that weak-lensing masses are overestimated. We note that a mass bias $1-b=0.58$ as required to reconcile Planck CMB and cluster counts should translate into an even lower baryon fraction, which poses a major challenge to our current understanding of galaxy clusters. [Abridged], Comment: 13th paper in the XXL series, A&A in press
Published: 2016

152. The XXL Survey VIII. MUSE characterisation of intracluster light in a z similar to 0.53 cluster of galaxies

Author: Adami, C., Pompei, E., Sadibekova, T., Clerc, N., Iovino, A., McGee, S. L., Guennou, L., Birkinshaw, M., Horellou, C., Maurogordato, S., Pacaud, F., Pierre, M., Poggianti, B., Willis, J., 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), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / 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), Max-Planck-Institut für Extraterrestrische Physik (MPE), AUTRES, Department of Earth and Space Sciences [Göteborg], Chalmers University of Technology [Göteborg], 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), CEA/DCC/DRRV/SCD, Commissariat à l'Energie Atomique, Marcoule, Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Ecosystèmes aquatiques et changements globaux (UR EABX), Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), 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), 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)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), California Institute of Technology (CALTECH)-NASA, 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)
Subjects: [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics
Abstract: International audience; Aims. Within a cluster, gravitational effects can lead to the removal of stars from their parent galaxies and their subsequent dispersal into the intracluster medium. Gas hydrodynamical effects can additionally strip gas and dust from galaxies; both gas and stars contribute to intracluster light (ICL). The properties of the ICL can therefore help constrain the physical processes at work in clusters by serving as a fossil record of the interaction history. Methods. The present study is designed to characterise this ICL for the first time in a similar to 10(14) M-circle dot and z similar to 0.53 cluster of galaxies from imaging and spectroscopic points of view. By applying a wavelet-based method to CFHT Megacam and WIRCAM images, we detect significant quantities of diffuse light and are able to constrain their spectral energy distributions. These sources were then spectroscopically characterised with ESO Multi Unit Spectroscopic Explorer (MUSE) spectroscopic data. MUSE data were also used to compute redshifts of 24 cluster galaxies and search for cluster substructures. Results. An atypically large amount of ICL, equivalent in i' to the emission from two brightest cluster galaxies, has been detected in this cluster. Part of the detected diffuse light has a very weak optical stellar component and apparently consists mainly of gas emission, while other diffuse light sources are clearly dominated by old stars. Furthermore, emission lines were detected in several places of diffuse light. Our spectral analysis shows that this emission likely originates from low-excitation parameter gas. Globally, the stellar contribution to the ICL is about 2.3 x 10(9) yr old even though the ICL is not currently forming a large number of stars. On the other hand, the contribution of the gas emission to the ICL in the optical is much greater than the stellar contribution in some regions, but the gas density is likely too low to form stars. These observations favour ram pressure stripping, turbulent viscous stripping, or supernovae winds as the origin of the large amount of intracluster light. Since the cluster appears not to be in a major merging phase, we conclude that ram pressure stripping is the most plausible process that generates the observed ICL sources. Conclusions. This is one of the first times that we are able to spectroscopically study diffuse light in such a distant and massive cluster, and it demonstrates the potential of MUSE observations for such studies.
Published: 2016

153. The XXL Survey I. Scientific motivations - XMM-Newton observing plan - Follow-up observations and simulation programme

Author: David Rapetti, Bruno Altieri, Nicolas Clerc, N. Fourmanoit, R. Gastaud, Felipe Menanteau, Bianca M. Poggianti, Angela Bongiorno, M. E. Ramos-Ceja, Marcella Brusa, Andrii Elyiv, Stefano Ettori, Y. Dubois, S. Paltani, O. V. Melnyk, L. Guennou, Sean L. McGee, Emanuela Pompei, A. Butler, Dominique Eckert, C. Adami, F. Finet, C. De Breuck, V. Guglielmo, J. Delhaize, C. Schimd, A. Iovino, Cristian Vignali, K. Husband, Mauro Sereno, S. Desai, Arya Farahi, Steven L. Snowden, Cathy Horellou, Jean-Baptiste Melin, H. J. A. Röttgering, Vernesa Smolčić, Piero Ranalli, J. P. Le Fevre, Elias Koulouridis, J. L. Willis, A. Valotti, David N. Spergel, Minh Huynh, S. A. Stanford, I. Valtchanov, C. Lidman, Manolis Plionis, L. Chiappetti, Jean Surdej, M. Lieu, Thomas H. Reiprich, E. S. Rykoff, Daniel Pomarède, Florian Pacaud, Paolo Ciliegi, T. Sadibekova, I. Georgantopoulos, Sotiria Fotopoulou, C. Benoist, Julien Devriendt, F. Ziparo, S. Lavoie, Ian G. McCarthy, Jean Coupon, J. Démoclès, Mladen Novak, L. Faccioli, José Paulo Santos, Paul Giles, Adam Mantz, Malcolm N. Bremer, Graham P. Smith, Poshak Gandhi, Mark Birkinshaw, S. Maurogordato, Trevor J. Ponman, Ben J Maughan, Pier Stefano Corasaniti, August E. Evrard, Fabio Gastaldello, S. Raychaudury, A. M. C. Le Brun, Martin Kilbinger, J. L. Sauvageot, Sinan Aliş, Chieh-An Lin, E. Rozo, Patrick Valageas, Marguerite Pierre, Chiara Ferrari, B. Baran, Ecosystèmes aquatiques et changements globaux (UR EABX), Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA), CEA/DCC/DRRV/SCD, Commissariat à l'Energie Atomique, Marcoule, Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), 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), Herschel Science Centre, Agence Spatiale Européenne = European Space Agency (ESA), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), College of Computing (GATECH), Georgia Institute of Technology [Atlanta], Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), INAF- Milano, Max-Planck-Institut für Extraterrestrische Physik (MPE), 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), European Southern Observatory (ESO), 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), Sub-department of Astrophysics [Oxford], Department of Physics [Oxford], University of Oxford-University of Oxford, Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université de Genève = University of Geneva (UNIGE), INAF-IASF Milano, Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Département de Géologie, Université de Montréal (UdeM), Aristotle University of Thessaloniki, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Sr. PLM Consultant, Département d'Electronique, des Détecteurs et d'Informatique pour la Physique (ex SEDI) (DEDIP), 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, Institute for Space Applications and Remote Sensing (ISARS/NOA), National Observatory of Athens (NOA), Department of Earth and Space Sciences [Göteborg], Chalmers University of Technology [Göteborg], Université Quebec, Université du Québec à Chicoutimi (UQAC), AUTRES, Astronomical Observatory of Kiev, Taras Shevchenko National University of Kyiv, Laboratoire SUBATECH Nantes (SUBATECH), Mines Nantes (Mines Nantes)-Université de Nantes (UN)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), ISDC Data Centre for Astrophysics, INAF - Osservatorio Astronomico di Padova (OAPD), Lund Observatory, Lund University [Lund], Argelander Institute for Astronomy (AlfA), Rheinische Friedrich-Wilhelms-Universität Bonn, Leiden Observatory [Leiden], Universiteit Leiden, KIPAC, Stanford (KIPAC), Stanford University-SLAC National Accelerator Laboratory (SLAC), Stanford University, Institut des Sciences Moléculaires d'Orsay (ISMO), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), University of Reading (UOR), NASA Goddard Space Flight Center (GSFC), Service de Physique Théorique (SPhT), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), European Space Agency (ESA), 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), Università di Bologna, Dipartimento di Astronomia, Università di Bologna [Bologna] (UNIBO), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), University of Oxford [Oxford]-University of Oxford [Oxford], École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), University of Geneva [Switzerland], Université de Montréal [Montréal], Département d'Electronique, des Détecteurs et d'Informatique (ex SEDI) (DEDI), National Observatory of Athens, Institute for Space Applications and Remote Sensing, Universiteit Leiden [Leiden], Stanford University [Stanford]-SLAC, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Nantes (UN)-Mines Nantes (Mines Nantes), 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), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), California Institute of Technology (CALTECH)-NASA, 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), Pierre, M., Pacaud, F., Adami, C., Alis, S., Altieri, B., Baran, N., Benoist, C., Birkinshaw, M., Bongiorno, A., Bremer, M.N., Brusa, M., Butler, A., Ciliegi, P., Chiappetti, L., Clerc, N., Corasaniti, P.S., Coupon, J., De Breuck, C., Democles, J., Desai, S., Delhaize, J., Devriendt, J., Dubois, Y., Eckert, D., Elyiv, A., Ettori, S., Evrard, A., Faccioli, L., Farahi, A., Ferrari, C., Finet, F., Fotopoulou, S., Fourmanoit, N., Gandhi, P., Gastaldello, F., Gastaud, R., Georgantopoulos, I., Giles, P., Guennou, L., Guglielmo, V., Horellou, C., Husband, K., Huynh, M., Iovino, A., Kilbinger, M., Koulouridis, E., Lavoie, S., Le Brun, A.M.C., Le Fevre, J.P., Lidman, C., Lieu, M., Lin, C.A., Mantz, A., Maughan, B.J., Maurogordato, S., Mccarthy, I.G., Mcgee, S., Melin, J.B., Melnyk, O., Menanteau, F., Novak, M., Paltani, S., Plionis, M., Poggianti, B.M., Pomarede, D., Pompei, E., Ponman, T.J., Ramos-Ceja, M.E., Ranalli, P., Rapetti, D., Raychaudury, S., Reiprich, T.H., Rottgering, H., Rozo, E., Rykoff, E., Sadibekova, T., Santos, J., Sauvageot, J.L., Schimd, C., Sereno, M., Smith, G.P., Smolčić, V., Snowden, S., Spergel, D., Stanford, S., Surdej, J., Valageas, P., Valotti, A., Valtchanov, I., Vignali, C., Willis, J., Ziparo, F., ITA, FRA, DEU, ESP, BEL, CAN, and TUR
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Large-scale structure of Universe, PRIRODNE ZNANOSTI. Fizika. Astronomija i astrofizika, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Table (information), X-rays: general, 01 natural sciences, X-rays, general, large-scale structure of Universe, galaxies, clusters, surveys, general [X-rays], 0103 physical sciences, Electronic form, NATURAL SCIENCES. Physics. Astronomy and Astrophysics, Survey, 010303 astronomy & astrophysics, media_common, QB, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Photon statistics, 010308 nuclear & particles physics, Plan (archaeology), Astronomy and Astrophysics, Astronomy and Astrophysic, X-rays: galaxies: cluster, Galaxy, Pathfinder, Sky, Space and Planetary Science, X-rays: galaxies: clusters, Dark energy, galaxies: clusters [X-rays], Astrophysics - High Energy Astrophysical Phenomena, X-rays: diffuse background, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present the XXL Survey, the largest XMM programme totaling some 6.9 Ms to date and involving an international consortium of roughly 100 members. The XXL Survey covers two extragalactic areas of 25 deg2 each at a point-source sensitivity of ~ 5E-15 erg/sec/cm2 in the [0.5-2] keV band (completeness limit). The survey's main goals are to provide constraints on the dark energy equation of state from the space-time distribution of clusters of galaxies and to serve as a pathfinder for future, wide-area X-ray missions. We review science objectives, including cluster studies, AGN evolution, and large-scale structure, that are being conducted with the support of approximately 30 follow-up programmes. We describe the 542 XMM observations along with the associated multi-lambda and numerical simulation programmes. We give a detailed account of the X-ray processing steps and describe innovative tools being developed for the cosmological analysis. The paper provides a thorough evaluation of the X-ray data, including quality controls, photon statistics, exposure and background maps, and sky coverage. Source catalogue construction and multi-lambda associations are briefly described. This material will be the basis for the calculation of the cluster and AGN selection functions, critical elements of the cosmological and science analyses. The XXL multi-lambda data set will have a unique lasting legacy value for cosmological and extragalactic studies and will serve as a calibration resource for future dark energy studies with clusters and other X-ray selected sources. With the present article, we release the XMM XXL photon and smoothed images along with the corresponding exposure maps. The XMM XXL observation list (Table B.1) is available in electronic form at the CDS. The present paper is the first in a series reporting results of the XXL-XMM survey., Comment: 17 pages, accepted in A&A
Published: 2016

154. A high definition view of the COSMOS Wall at z similar to 0.73

Author: Iovino, A., Petropoulou, V., Scodeggio, M., Bolzonella, M., Zamorani, G., Bardelli, S., Cucciati, O., Pozzetti, L., Tasca, L., Vergani, D., Zucca, E., Finoguenov, A., Ilbert, O., Tanaka, M., Salvato, M., Kovac, K., Cassata, P., AUTRES, INAF- Milano, Istituto Nazionale di Astrofisica (INAF), Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), INAF - Osservatorio Astronomico di Bologna (OABO), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astrofisico di Arcetri (OAA), Oncology Institute of Southern Switzerland, Max-Planck-Institut für Extraterrestrische Physik (MPE), Excellence Cluster Universe, and excellence cluster centre
Subjects: [SDU]Sciences of the Universe [physics], Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics
Abstract: International audience; Aims. We present a study of a large filamentary structure at z similar to 0.73 in the field of the COSMOS survey, the so-called COSMOS Wall. This structure encompasses a comprehensive range of environments from a dense cluster and a number of galaxy groups to filaments, less dense regions, and adjacent voids. It thus provides a valuable laboratory for the accurate mapping of environmental effects on galaxy evolution at a look-back time of similar to 6.5 Gyr, when the Universe was roughly half its present age. Methods. We performed deep spectroscopic observations with VIMOS at VLT of a K-band selected sample of galaxies in this complex structure, building a sample of galaxies complete in galaxy stellar mass down to a lower limit of log(M-*/M-circle dot)similar to 9.8, which is significantly deeper than previously available data. Thanks to its location within the COSMOS survey, each galaxy benefits from a wealth of ancillary information: HST-ACS data with I-band exposures down to I-AB similar to 28 complemented by extensive multiwavelength ground-and space-based observations spanning the entire electromagnetic spectrum. Results. In this paper we detail the survey strategy and weighting scheme adopted to account for the biases introduced by the photometric preselection of our targets. We present our galaxy stellar mass and rest-frame magnitudes estimates together with a group catalog obtained with our new data and their member galaxies color / mass distribution. Conclusions. Owing to our new sample we can perform a detailed, high definition mapping of the complex COSMOS Wall structure. The sharp environmental information, coupled with high quality spectroscopic information and rich ancillary data available in the COSMOS field, enables a detailed study of galaxy properties as a function of local environment in a redshift slice where environmental effects are important, and in a stellar mass range where mass and environment driven effects are both at work.
Published: 2016

155. The XXL Survey: X. K-band luminosity - weak-lensing mass relation for groups and clusters of galaxies

Author: Ziparo, F., Smith, G. P., Mulroy, S. L., Lieu, M., Willis, J. P., Hudelot, P., Mcgee, S. L., Fotopoulou, S., Lidman, C., Lavoie, S., Pierre, M., Adami, C., Chiappetti, L., Clerc, N., Giles, P., Maughan, B., Pacaud, F., Sadibekova, T., School of Physics and Astronomy [Birmingham], University of Birmingham [Birmingham], University of Victoria [Canada] (UVIC), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Department of Astronomy [Geneva], University of Geneva [Switzerland], Australian Astronomical Observatory, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / 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-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), 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 Milano (OAM), Istituto Nazionale di Astrofisica (INAF), Max-Planck-Institut für Extraterrestrische Physik (MPE), H. H. Wills Physics Laboratory [Bristol], University of Bristol [Bristol], Argelander-Institut für Astronomie (AlfA), Rheinische Friedrich-Wilhelms-Universität Bonn, Université de Genève = University of Geneva (UNIGE), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES)
Subjects: galaxies: photometry, gravitational lensing: weak, galaxies: clusters: general, galaxies: groups: general, [SDU]Sciences of the Universe [physics], X-rays: galaxies: clusters, galaxies: stellar content, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: International audience; Galaxy clusters and groups are important cosmological probes and giant cosmic laboratories for studying galaxy evolution. Much effort has been devoted to understanding how and when baryonic matter cools at the centre of potential wells. However, a clear picture of the efficiency with which baryons are converted into stars is still missing. We present the K-band luminosity-halo mass relation, $L_{K,500} - M_{500,WL}$, for a subsample of 20 of the 100 brightest clusters in the XXL Survey observed with WIRCam at the Canada-France-Hawaii Telescope (CFHT). For the first time, we have measured this relation via weak-lensing analysis down to $M_{500,WL}$ = 3.5 x 10$^{13}$ $M_\odot$. This allows us to investigate whether the slope of the $L_K - M$ relation is different for groups and clusters, as seen in other works. The clusters in our sample span a wide range in mass, $M_{500,WL}$ = 0.35-12.10 x 10$^{14}$ $M\odot$, at 0 \ $z$ \ 0.6. The K-band luminosity scales as log$_{10}$($L_{K,500}$/10$^{12}$ $L_\odot$ $\propto \beta$ log$_{10}$($M_{500,WL}$/10$^{14}$ $M_\odot$) with $\beta$ = 0.85$_{-0.27}^{+0.35}$ and an intrinsic scatter of $\sigma_{lnLK lM}$ = 0.37$_{-0.17}^{+0.19}$. Combining our sample with some clusters in the Local Cluster Substructure Survey (LoCuSS) present in the literature, we obtain a slope of 1.05$_{-0.14}^{+0.16}$ and an intrinsic scatter of 0.14$_{-0.07}^{+0.09}$ . The flattening in the $L_K - M$ seen in previous works is not seen here and might be a result of a bias in the mass measurement due to assumptions on the dynamical state of the systems. We also study the richness-mass relation and find that group-sized halos have more galaxies per unit halo mass than massive clusters. However, the brightest cluster galaxy (BCG) in low-mass systems contributes a greater fraction to the total cluster light than BCGs do in massive clusters; the luminosity gap between the two brightest galaxies is more prominent for group-sized halos. This result is a natural outcome of the hierarchical growth of structures, where massive galaxies form and gain mass within low-mass groups and are ultimately accreted into more massive clusters to become either part of the BCG or one of the brighter galaxies.
Published: 2016

156. The XXL Survey II. The bright cluster sample: catalogue and luminosity function

Author: Dominique Eckert, Sophie Maurogordato, A. Iovino, L. Guennou, Sinan Aliş, C. Benoist, J. Démoclès, Daniel Pomarède, Jochen Liske, L. Faccioli, Ivan K. Baldry, J. P. Le Fevre, L. Chiappetti, Matt S. Owers, David Rapetti, N. Clerc, Florian Pacaud, Christopher Lidman, Trevor J. Ponman, Thomas H. Reiprich, Ivan Valtchanov, C. Adami, Patrick Valageas, Graham P. Smith, Marguerite Pierre, T. Sadibekova, Felipe Menanteau, Bianca M. Poggianti, F. Ardila, Cathy Horellou, Elias Koulouridis, F. Ziparo, Ben J Maughan, Mark Birkinshaw, M. Lieu, Bruno Altieri, V. Le Brun, Paul Giles, August E. Evrard, Fabio Gastaldello, Jon Willis, Richard J. Tuffs, E. Pompei, CEA/DCC/DRRV/SCD, Commissariat à l'Energie Atomique, Marcoule, Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Max-Planck-Institut für Extraterrestrische Physik (MPE), 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), 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), Ecosystèmes aquatiques et changements globaux (UR EABX), Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA), Herschel Science Centre, European Space Agency (ESA), Joseph Louis LAGRANGE (LAGRANGE), 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), INAF- Milano, Istituto Nazionale di Astrofisica (INAF), University of Geneva [Switzerland], INAF-IASF Milano, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), 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], AUTRES, Institute for Space Applications and Remote Sensing (ISARS/NOA), National Observatory of Athens (NOA), Argelander Institute for Astronomy (AlfA), Rheinische Friedrich-Wilhelms-Universität Bonn, University of Reading (UOR), Service de Physique Théorique (SPhT), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS), 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)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), National Observatory of Athens, Institute for Space Applications and Remote Sensing, 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), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Agence Spatiale Européenne = European Space Agency (ESA), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université de Genève = University of Geneva (UNIGE), 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 Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Active galactic nucleus, Infrarot-Astrophysik - Abteilung Hofmann, FOS: Physical sciences, Context (language use), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmology, surveys, 0103 physical sciences, Cluster (physics), cosmological parameters, 010303 astronomy & astrophysics, Galaxy cluster, QB, Luminosity function (astronomy), Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Redshift, Space and Planetary Science, clusters: intracluster medium [galaxies], [SDU]Sciences of the Universe [physics], Cluster sampling, galaxies: clusters [X-rays], large-scale structure of Universe, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Context. The XXL Survey is the largest survey carried out by the XMM-Newton satellite and covers a total area of 50 square degrees distributed over two fields. It primarily aims at investigating the large-scale structures of the Universe using the distribution of galaxy clusters and active galactic nuclei as tracers of the matter distribution. Aims. This article presents the XXL bright cluster sample, a subsample of 100 galaxy clusters selected from the full XXL catalogue by setting a lower limit of $3\times 10^{-14}\,\mathrm{erg \,s^{-1}cm^{-2}}$ on the source flux within a 1$^{\prime}$ aperture. Methods. The selection function was estimated using a mixture of Monte Carlo simulations and analytical recipes that closely reproduce the source selection process. An extensive spectroscopic follow-up provided redshifts for 97 of the 100 clusters. We derived accurate X-ray parameters for all the sources. Scaling relations were self-consistently derived from the same sample in other publications of the series. On this basis, we study the number density, luminosity function, and spatial distribution of the sample. Results. The bright cluster sample consists of systems with masses between $M_{500}=7\times 10^{13}$ and $3\times 10^{14} M_\odot$, mostly located between $z=0.1$ and 0.5. The observed sky density of clusters is slightly below the predictions from the WMAP9 model, and significantly below the predictions from the Planck 2015 cosmology. In general, within the current uncertainties of the cluster mass calibration, models with higher values of $\sigma_8$ and/or $\Omega_m$ appear more difficult to accommodate. We provide tight constraints on the cluster differential luminosity function and find no hint of evolution out to $z\sim1$. We also find strong evidence for the presence of large-scale structures in the XXL bright cluster sample and identify five new superclusters., Comment: Accepted by A&A, 25 pages, 17 figures, 7 tables. The XXL-100-GC Master catalogue is available from the XXL Milan database (http://cosmosdb.iasf-milano.inaf.it/XXL/) and through the CDS (cdsarc.u-strasbg.fr)
Published: 2016

157. The XXL Survey III. Luminosity-temperature relation of the bright cluster sample

Author: T. Sadibekova, C. Adami, Marguerite Pierre, J. P. Le Fevre, Trevor J. Ponman, L. Chiappetti, Paul Giles, J. Démoclès, F. Ziparo, Graham P. Smith, M. Lieu, B. J. Maughan, Florian Pacaud, N. Clerc, Jon Willis, Stefano Ettori, CEA/DCC/DRRV/SCD, Commissariat à l'Energie Atomique, Marcoule, Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Max-Planck-Institut für Extraterrestrische Physik (MPE), Ecosystèmes aquatiques et changements globaux (UR EABX), Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), INAF- Milano, Istituto Nazionale di Astrofisica (INAF), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / 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), INAF - Osservatorio Astronomico di Bologna (OABO), University of Reading (UOR), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), and Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112))
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, Flux, FOS: Physical sciences, Scale (descriptive set theory), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Measure (mathematics), Luminosity, 0103 physical sciences, clusters: general [galaxies], Sensitivity (control systems), 010303 astronomy & astrophysics, Galaxy cluster, 0105 earth and related environmental sciences, Physics, Astronomy and Astrophysics, Redshift, clusters: intracluster medium [galaxies], Space and Planetary Science, Cluster sampling, galaxies: clusters [X-rays], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The XXL Survey is the largest homogeneous survey carried out with XMM-Newton. Covering an area of 50 deg$^{2}$, the survey contains several hundred galaxy clusters out to a redshift of $\approx$2 above an X-ray flux limit of $\sim$5$\times10^{-15}$ erg cm$^{-2}$ s$^{-1}$. This paper belongs to the first series of XXL papers focusing on the bright cluster sample. We investigate the luminosity-temperature (LT) relation for the brightest clusters detected in the XXL Survey, taking fully into account the selection biases. We investigate the form of the LT relation, placing constraints on its evolution. We have classified the 100 brightest clusters in the XXL Survey based on their measured X-ray flux. These 100 clusters have been analysed to determine their luminosity and temperature to evaluate the LT relation. We used three methods to fit the LT relation, with two of these methods providing a prescription to fully take into account the selection effects of the survey. We measure the evolution of the LT relation internally using the broad redshift range of the sample. Taking into account selection effects, we find a slope of the bolometric LT relation of B$_{\rm LT}=3.08\pm$0.15, steeper than the self-similar expectation (B$_{\rm LT}$=2). Our best-fit result for the evolution factor is $E(z)^{1.64\pm0.77}$, consistent with "strong self-similar" evolution where clusters scale self-similarly with both mass and redshift. However, this result is marginally stronger than "weak self-similar" evolution, where clusters scale with redshift alone. We investigate the sensitivity of our results to the assumptions made in our model, finding that using an external LT relation as a low-z baseline can have a profound effect on the measured evolution. However, more clusters are needed to break the degeneracy between the choice of likelihood model and mass-temperature relation on the derived evolution., Comment: 16 pages, 9 figures. Accepted for publication in A&A
Published: 2016

158. The ATLAS(3D) project - XVI. Physical parameters and spectral line energy distributions of the molecular gas in gas-rich early-type galaxies

Author: Harald Kuntschner, E. Bayet, P. T. de Zeeuw, Timothy A. Davis, Roger L. Davies, Pierre-Alain Duc, M. Bois, Leo Blitz, Richard M. McDermid, Thorsten Naab, Anne-Marie Weijmans, Sadegh Khochfar, Martin Bureau, Marc Sarzi, Tom Oosterloo, Paolo Serra, Frédéric Bournaud, Raffaella Morganti, Eric Emsellem, Alison F. Crocker, Katherine Alatalo, Lisa M. Young, Michele Cappellari, Davor Krajnović, Nicholas Scott, Dept of physics and astrophysics, University College of London [London] (UCL), Sub-department of Astrophysics [Oxford], Department of Physics [Oxford], University of Oxford [Oxford]-University of Oxford [Oxford], Department of Computer and Information Science and Engineering [Gainesville] (UF|CISE), University of Florida [Gainesville] (UF), Department of Astronomy [Berkeley], University of California [Berkeley], University of California-University of California, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), 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, European Southern Observatory (ESO), Max-Planck-Institut für Extraterrestrische Physik (MPE), Netherlands Institute for Radio Astronomy (ASTRON), Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Centre for Astrophysics Research [Hatfield], University of Hertfordshire [Hatfield] (UH), Centre for Astrophysics & Supercomputing, Swinburne University of Technology [Melbourne], NASA Ames Research Center (ARC), Dunlap Institute for Astronomy and Astrophysics [Toronto], University of Toronto, University of Oxford-University of Oxford, University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), École normale supérieure - Paris (ENS-PSL), Astronomy, and Kapteyn Astronomical Institute
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Mean kinetic temperature, Milky Way, FOS: Physical sciences, Astrophysics, Disc galaxy, 01 natural sciences, Spectral line, COLOGNE DATABASE, cD, STAR-FORMATION, INTEGRAL-FIELD SPECTROSCOPY, ELLIPTIC GALAXIES, 0103 physical sciences, NEARBY GALAXIES, CENTAURUS-A, galaxies: elliptical and lenticular, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Line (formation), Physics, [PHYS]Physics [physics], stars: formation, INTERSTELLAR-MEDIUM, NEUTRAL-HYDROGEN, 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, methods: data analysis, SAURON PROJECT, Galaxy, ISM: molecules, Volume (thermodynamics), Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], SPIRAL GALAXIES, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: [Abridged] We present a detailed study of the physical properties of the molecular gas in a sample of 18 molecular gas-rich early-type galaxies (ETGs) from the ATLAS$ 3D sample. Our goal is to better understand the star formation processes occurring in those galaxies, starting here with the dense star-forming gas. We use existing integrated $^{12}$CO(1-0, 2-1), $^{13}$CO(1-0, 2-1), HCN(1-0) and HCO$^{+}$(1-0) observations and present new $^{12}$CO(3-2) single-dish data. From these, we derive for the first time the average kinetic temperature, H$_{2}$ volume density and column density of the emitting gas, this using a non-LTE theoretical model. Since the CO lines trace different physical conditions than of those the HCN and HCO$^{+}$ lines, the two sets of lines are treated separately. We also compare for the first time the predicted CO spectral line energy distributions (SLEDs) and gas properties of our molecular gas-rich ETGs with those of a sample of nearby well-studied disc galaxies. The gas excitation conditions in 13 of our 18 ETGs appear analogous to those in the centre of the Milky Way. Such results have never been obtained before for ETGs and open a new window to explore further star-formation processes in the Universe. The conclusions drawn should nevertheless be considered carefully, as they are based on a limited number of observations and on a simple model. In the near future, with higher CO transition observations, it should be possible to better identify the various gas components present in ETGs, as well as more precisely determine their associated physical conditions. To achieve these goals, we show here from our theoretical study, that mid-J CO lines (such as the $^{12}$CO(6-5) line) are particularly useful., 28 pages, Accepted in MNRAS, 7 figures, 6 tables
Published: 2016

159. Herschel deep far-infrared counts through Abell 2218 cluster-lens

Author: G. Rodighiero, Ángel Bongiovanni, Roberto Maiolino, Raanan Nordon, Albrecht Poglitsch, I. Valtchanov, Ekkehard Wieprecht, P. Popesso, Bruno Altieri, Dieter Lutz, J. Cepa, Johan Richard, Eckhard Sturm, Antonio Cava, E. Daddi, P. Andreani, H. Dominguez, A. Cimatti, A. M. Pérez García, J. P. Kneib, Reinhard Genzel, Lijing Shao, Laure Ciesla, D. Elbaz, S. Berta, M. Wetzstein, M. Sánchez-Portal, Carlotta Gruppioni, L. Riguccini, Georgios E. Magdis, Linda J. Tacconi, Francesca Pozzi, H. Aussel, L. Metcalfe, P. Santini, Amelie Saintonge, N. M. Förster Schreiber, Benjamin Magnelli, XMM-Newton Science Operations Centre, European Space Agency (ESA), AUTRES, Max-Planck-Institut für Extraterrestrische Physik (MPE), 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), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / 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), Station de Pathologie Végétale [Angers], Institut National de la Recherche Agronomique (INRA), Max Planck Institute for Extraterrestrial Physics (MPE), Max-Planck-Gesellschaft, Department of Physics [Berkeley], University of California [Berkeley], University of California-University of California, 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 de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Mecanique des Fluides et d'Acoustique (LMFA), École Centrale de Lyon (ECL), Université de Lyon-Université de Lyon-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), B. Altieri, S. Berta, D. Lutz, J.-P. Kneib, L. Metcalfe, P. Andreani, H. Aussel, A. Bongiovanni, A. Cava, J. Cepa, L. Ciesla, A. Cimatti, E. Daddi, H. Dominguez, D. Elbaz, N.M. Forster Schreiber, R. Genzel, C. Gruppioni, B. Magnelli, G. Magdi, R. Maiolino, R. Nordon, A.M. Perez Garcia, A. Poglitsch, P. Popesso, F. Pozzi, J. Richard, L. Riguccini, G. Rodighiero, A. Saintonge, P. Santini, M. Sanchez-Portal, L. Shao, E. Sturm, L.J. Tacconi, I. Valtchanov, M. Wetzstein, E. Wieprecht, Agence Spatiale Européenne = European Space Agency (ESA), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), 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), and École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL)
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], Strong gravitational lensing, Population, FOS: Physical sciences, Astrophysics, 01 natural sciences, infrared: galaxies, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], surveys, galaxies: high-redshift, Cosmic infrared background, 0103 physical sciences, Source counts, Surface brightness, education, 010303 astronomy & astrophysics, Galaxy cluster, Physics, Luminous infrared galaxy, Galaxy: evolution, education.field_of_study, 010308 nuclear & particles physics, gravitational lensing: strong, Astronomy and Astrophysics, Gravitational lens, Space and Planetary Science, galaxies: clusters: general, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Gravitational lensing by massive galaxy clusters allows study of the population of intrinsically faint infrared galaxies that lie below the sensitivity and confusion limits of current infrared and submillimeter telescopes. We present ultra-deep PACS 100 and 160 microns observations toward the cluster lens Abell 2218, to penetrate the Herschel confusion limit. We derive source counts down to a flux density of 1 mJy at 100 microns and 2 mJy at 160 microns, aided by strong gravitational lensing. At these levels, source densities are 20 and 10 beams/source in the two bands, approaching source density confusion at 160 microns. The slope of the counts below the turnover of the Euclidean-normalized differential curve is constrained in both bands and is consistent with most of the recent backwards evolutionary models. By integrating number counts over the flux range accessed by Abell 2218 lensing (0.94-35 mJy at 100 microns and 1.47-35 mJy at 160 microns, we retrieve a cosmic infrared background (CIB) surface brightness of ~8.0 and ~9.9 nW m^-2 sr^-1, in the respective bands. These values correspond to 55% (+/- 24%) and 77% (+/- 31%) of DIRBE direct measurements. Combining Abell 2218 results with wider/shallower fields, these figures increase to 62% (+/- 25%) and 88% (+/- 32%) CIB total fractions, resolved at 100 and 160 microns, disregarding the high uncertainties of DIRBE absolute values., Accepted for publication on the A&A Herschel Special Issue, final version
Published: 2016

160. Modeling effects of common molecular contaminants on the Euclid infrared detectors

Author: Gennadiy N. Lotkin, Remi Barbier, Anne Ealet, Roger Foltz, Analia N. Cillis, Murzy D. Jhabvala, Laddawan Miko, N. Ferraro, Jason Williams, T. Powers, Hyung Cho, Olivia R. Dawson, Em. Kan, Duncan M. Kahle, Augustyn Waczynski, L. Nguyen, J.-C. Clemens, Michael Hickey, F. Wang, S. McClure, P. Strada, Michael Seiffert, Thierry Maciaszek, Ulf E. Israelsson, Gregory Delo, Emily Kan, T. Hwang, K. Turck, Eric Prieto, Warren Holmes, A. Feizi, C. Weber, Carole Tucker, Chris McKenney, T. Goodsall, S. Pravdo, 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), National Space Institute [Lyngby] (DTU Space), Technical University of Denmark [Lyngby] (DTU), University of Copenhagen = Københavns Universitet (KU), Max-Planck-Institut für Extraterrestrische Physik (MPE), Centre National d’Études Spatiales [Paris] (CNES), 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), EUClID, 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), Danmarks Tekniske Universitet = Technical University of Denmark (DTU), and University of Copenhagen = Københavns Universitet (UCPH)
Subjects: 010302 applied physics, Materials science, Spacecraft, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Physics::Instrumentation and Detectors, business.industry, Detector, 02 engineering and technology, Cryopump, engineering.material, 021001 nanoscience & nanotechnology, 01 natural sciences, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Optics, Coating, 13. Climate action, 0103 physical sciences, engineering, Quantum efficiency, Area density, Infrared detector, 0210 nano-technology, business, Absorption (electromagnetic radiation)
Abstract: International audience; Cleanliness specifications for infrared detector arrays are usually so stringent that effects are neglibile. However, the specifications determine only the level of particulates and areal density of molecular layer on the surface, but the chemical composition of these contaminants are not specified. Here, we use a model to assess the impact on system quantum efficiency from possible contaminants that could accidentally transfer or cryopump to the detector during instrument or spacecraft testing and on orbit operation. Contaminant layers thin enough to meet typical specifications, < 0.5μgram/cm2, have a negligible effect on the net quantum efficiency of the detector, provided that the contaminant does not react with the detector surface, Performance impacts from these contaminant plating onto the surface become important for thicknesses 5 - 50μgram/cm2. Importantly, detectable change in the "ripple" of the anti reflection coating occurs at these coverages and can enhance the system quantum efficiency. This is a factor 10 less coverage for which loss from molecular absorption lines is important. Thus, should contamination be suspected during instrument test or flight, detailed modelling of the layer on the detector and response to very well known calibrations sources would be useful to determine the impact on detector performance
Published: 2016

161. 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

162. Self-similarity in the chemical evolution of galaxies and the delay time distribution of SNe Ia

Author: Robert M. Yates, Marie Martig, Cristina Chiappini, Maria Bergemann, C. J. Walcher, Gustavo Bruzual, Ivan Minchev, Stephane Charlot, Paula Coelho, Anna Gallazzi, Leibniz-Institut für Astrophysik Potsdam (AIP), Max-Planck-Institut für Extraterrestrische Physik (MPE), Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Instituto de Astronomia, Geofisica et Ciencias Atmosfericas, Universidade de São Paulo (USP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and Universidade de São Paulo = University of São Paulo (USP)
Subjects: Self-similarity, stars: abundances, Milky Way, FOS: Physical sciences, galaxies: elliptical and lenticular cD, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, supernovae: general, 0103 physical sciences, Galaxy formation and evolution, Astrophysics::Solar and Stellar Astrophysics, QD, 010303 astronomy & astrophysics, QC, Astrophysics::Galaxy Astrophysics, QB, Physics, Galaxy: evolution, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Universality (dynamical systems), Chemical evolution, Stars, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies: abundances, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Delay time
Abstract: Recent improvements in the age dating of stellar populations and single stars allow us to study the ages and abundance of stars and galaxies with unprecedented accuracy. We here compare the relation between age and \alpha-element abundances for stars in the solar neighborhood to that of local, early-type galaxies. We find both relations to be very similar. Both fall into two regimes with a flat slope for ages younger than ~9 Gyr and a steeper slope for ages older than that value. This quantitative similarity seems surprising, given the different types of galaxies and scales involved. For the sample of early-type galaxies we also show that the data are inconsistent with literature delay time distributions of either single or double Gaussian shape. The data are consistent with a power law delay time distribution. We thus confirm that the delay time distribution inferred for the Milky Way from chemical evolution arguments also must apply to massive early-type galaxies. We also offer a tentative explanation for the seeming universality of the age-[\alpha/Fe] relation as the manifestation of averaging of different stellar populations with varying chemical evolution histories., Comment: 8 pages, 3 figures, submitted to A&A, version in reply to first referee report
Published: 2016

163. Control bandwidth improvements in GRAVITY fringe tracker by switching to a synchronous real time computer architecture

Author: Frank Eisenhauer, Julien Woillez, Pierre Fedou, Than Phan Duc, Roberto Abuter, Nicola Di Lieto, Roderick Dembet, Sylvestre Lacour, European Southern Observatory (Germany), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Haute résolution angulaire en astrophysique, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), and Max-Planck-Institut für Extraterrestrische Physik (MPE)
Subjects: Hardware architecture, Very Large Telescope, 010504 meteorology & atmospheric sciences, Computer science, business.industry, Bandwidth (signal processing), Detector, Real-time computing, Kalman filter, 01 natural sciences, Interferometry, Control system, 0103 physical sciences, Astronomical interferometer, business, Baseline (configuration management), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Computer hardware, Optical path length, 0105 earth and related environmental sciences, Group delay and phase delay, Data transmission
Abstract: International audience; The new VLTI (Very Large Telescope Interferometer) 1 instrument GRAVITY5, 22, 23 is equipped with a fringe tracker16 able to stabilize the K-band fringes on six baselines at the same time. It has been designed to achieve a performance for average seeing conditions of a residual OPD (Optical Path Difference) lower than 300 nm with objects brighter than K = 10. The control loop implementing the tracking is composed of a four stage real time computer system compromising: a sensor where the detector pixels are read in and the OPD and GD (Group Delay) are calculated; a controller receiving the computed sensor quantities and producing commands for the piezo actuators; a concentrator which combines both the OPD commands with the real time tip/tilt corrections offloading them to the piezo actuator; and finally a Kalman15 parameter estimator. This last stage is used to monitor current measurements over a window of few seconds and estimate new values for the main Kalman15 control loop parameters. The hardware and software implementation of this design runs asynchronously and communicates the four computers for data transfer via the Reflective Memory Network3. With the purpose of improving the performance of the GRAVITY5, 23 fringe tracking16, 22 control loop, a deviation from the standard asynchronous communication mechanism has been proposed and implemented. This new scheme operates the four independent real time computers involved in the tracking loop synchronously using the Reflective Memory Interrupts2 as the coordination signal. This synchronous mechanism had the effect of reducing the total pure delay of the loop from 3.5 [ms] to 2.0 [ms] which then translates on a better stabilization of the fringes as the bandwidth of the system is substantially improved. This paper will explain in detail the real time architecture of the fringe tracker in both is synchronous and synchronous implementation. The achieved improvements on reducing the delay via this mechanism will be quantified.
Published: 2016

164. How to test NISP instrument for EUCLID mission in laboratory

Author: Anne Ealet, Peter Viggo Jakobsen, Niels Christian Jessen, Anne Costille, W. Gillard, Michael I. Andersen, J. C. Clemens, Florent Beaumont, A. N. Sørensen, Christophe Fabron, Frank Grupp, M. Carle, Eric Prieto, Thierry Maciaszek, 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), National Space Institute [Lyngby] (DTU Space), Danmarks Tekniske Universitet = Technical University of Denmark (DTU), University of Copenhagen = Københavns Universitet (UCPH), Max-Planck-Institut für Extraterrestrische Physik (MPE), Centre National d'Études Spatiales [Toulouse] (CNES), 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), Euclid, 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), Technical University of Denmark [Lyngby] (DTU), University of Copenhagen = Københavns Universitet (KU), MacEwen, Howard A., Fazio, Giovanni G., and Lystrup, Makenzie
Subjects: Cryogenics, Vacuum, Computer science, 02 engineering and technology, 7. Clean energy, 01 natural sciences, law.invention, 010309 optics, Telescope, Set (abstract data type), Great Rift, GSE, law, Thermal environment, 0103 physical sciences, Calibration, Aerospace engineering, Simulation, Measure (data warehouse), Ground support equipment, business.industry, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Photometer, Test configuration, 021001 nanoscience & nanotechnology, Metrology, 0210 nano-technology, Focus (optics), business
Abstract: International audience; The ESA mission Euclid is designed to explore the dark side of the Universe. The NISP (Near Infrared Spectro- Photometer) is one of its two instruments operating in the near-IR spectral region (0.9-2μm), that will be fully integrated and tested at Laboratory d’Astrophysique de Marseille (LAM) under vacuum and thermal conditions. The test campaign will regroup functional tests, performance tests, calibration procedure validation and observations scenario test. One of the main objectives of the test campaign will be the measurement of the focus position of NISP with respect to the EUCLID object plane. To achieve these tests campaign, a global Ground Support Equipment (GSE) called the Verification Ground System (VGS) has to be developed. It will be a complex set of GSE integrated in ERIOS chamber made of: a telescope simulator to simulate the EUCLID telescope and to inject light into NISP, a thermal environment to be used for NISP thermal balance and verification, a sets of mechanical interfaces to align all the parts into ERIOS chamber, the NISP Electrical GSE (EGSE) to control the instrument during the test and a metrology system to measure the positions of the components during the test. We will present the preliminary design and concepts of the VGS and we will show the main difficulties we have to deal with: design of thermal environment at 80K with 4mK stability, the development of a metrology system in vacuum, knowledge of the focus position within 150μm in cold, etc. The main objectives of the NISP test will be explained and how the VGS responds to the test requirement.
Published: 2016

165. The COSMOS2015 Catalog: Exploring the 1 <z <6 Universe with Half a Million Galaxies

Author: M. Stockmann, Stefano Marchesi, Vernesa Smolčić, O. Le Fèvre, Mattia Vaccari, Anton M. Koekemoer, Francesca Civano, Johan P. U. Fynbo, Bo Milvang-Jensen, Lidia Tasca, David B. Sanders, Sune Toft, Bau-Ching Hsieh, James Dunlop, Paolo Cassata, Mara Salvato, Lihwai Lin, N. Z. Scoville, John D. Silverman, H. J. McCracken, Johannes Zabl, Simon J. Lilly, D. Le Borgne, Jeyhan S. Kartaltepe, Christophe Pichon, Alexie Leauthaud, Peter Capak, O. Ilbert, Guenther Hasinger, Yu-Yen Chang, Karina Caputi, I. Davidzon, E. Le Floc'h, Jean Coupon, Clotilde Laigle, Yoshiaki Taniguchi, Herve Aussel, Astronomy, Centre de résonance magnétique biologique et médicale (CRMBM), Aix Marseille Université (AMU)-Assistance Publique - Hôpitaux de Marseille (APHM)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), 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), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Institute for Astronomy [Honolulu], University of Hawai‘i [Mānoa] (UHM), Kavli Institute for the Physics and Mathematics of the Universe [Tokyo] (Kavli IPMU), The University of Tokyo Institutes for Advanced Study (UTIAS), The University of Tokyo (UTokyo)-The University of Tokyo (UTokyo), 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), Kapteyn Astronomical Institute [Groningen], University of Groningen [Groningen], SUPA, Institute for Astronomy, University of Edinburgh, Space Telescope Science Institute (STSci), 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), California Institute of Technology (CALTECH), Institute of Astronomy [ETH Zürich], Department of Physics [ETH Zürich] (D-PHYS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Dark Cosmology Centre (DARK), Niels Bohr Institute [Copenhagen] (NBI), Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU)-Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU), Max-Planck-Institut für Extraterrestrische Physik (MPE), Excellence Cluster Universe, excellence cluster centre, Faculty of Science and Engineering [Higashiosaka], Kindai University, ANR-11-IDEX-0004,SUPER,Sorbonne Universités à Paris pour l'Enseignement et la Recherche(2011), ANR-10-LABX-0063,ILP,Institute Lagrange of Paris(2010), ANR-13-BS05-0005,spin(e),L'origine cosmique de la séquence de Hubble(2013), European Project: 278202,EC:FP7:ERC,ERC-2011-StG_20101014,EGGS(2011), European Project: 648179,H2020,ERC-2014-CoG,ConTExt(2015), European Project: 0337595(2004), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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), 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 Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH)-Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH), Kavli Institute for the Physics and Mathematics of the Universe, The University of Tokyo, Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich)-Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), Faculty of Science and Engineering [Osaka], ANR-11-IDEX-0004-02/11-IDEX-0004,SUPER,SUPER(2011), ANR-10-LABX-63,ANR-10-LABX-63, ANR-13-BS05-0005,spin(e),L’origine cosmique de la séquence de Hubble(2013), ITA, USA, GBR, FRA, and DEU
Subjects: PRIRODNE ZNANOSTI. Fizika. Astronomija i astrofizika, media_common.quotation_subject, observational [methods], Field (mathematics), Astrophysics, 01 natural sciences, photometric [techniques], techniques: photometric, galaxies: high-redshift, 0103 physical sciences, Galaxy formation and evolution, NATURAL SCIENCES. Physics. Astronomy and Astrophysics, 010303 astronomy & astrophysics, evolution [galaxies], media_common, Photometric redshift, Physics, 010308 nuclear & particles physics, Sigma, Astronomy and Astrophysics, AB magnitude, Astrophysics - Astrophysics of Galaxies, Universe, Redshift, Galaxy, galaxies: photometry, Space and Planetary Science, photometry [galaxies], methods: observational, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], galaxies: evolution, catalogs, catalogs, galaxies: evolution, galaxies: high-redshift, galaxies: photometry, methods: observational, techniques: photometric, high-redshift [galaxies], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present the COSMOS2015 catalog which contains precise photometric redshifts and stellar masses for more than half a million objects over the 2deg$^{2}$ COSMOS field. Including new $YJHK_{\rm s}$ images from the UltraVISTA-DR2 survey, $Y$-band from Subaru/Hyper-Suprime-Cam and infrared data from the Spitzer Large Area Survey with the Hyper-Suprime-Cam Spitzer legacy program, this near-infrared-selected catalog is highly optimized for the study of galaxy evolution and environments in the early Universe. To maximise catalog completeness for bluer objects and at higher redshifts, objects have been detected on a $\chi^{2}$ sum of the $YJHK_{\rm s}$ and $z^{++}$ images. The catalog contains $\sim 6\times 10^5$ objects in the 1.5 deg$^{2}$ UltraVISTA-DR2 region, and $\sim 1.5\times 10^5$ objects are detected in the "ultra-deep stripes" (0.62 deg$^{2}$) at $K_{\rm s}\leq 24.7$ (3$\sigma$, 3", AB magnitude). Through a comparison with the zCOSMOS-bright spectroscopic redshifts, we measure a photometric redshift precision of $\sigma_{\Delta z/(1+z_s)}$ = 0.007 and a catastrophic failure fraction of $\eta=0.5$%. At $3, Comment: Accepted for publication in ApJ
Published: 2016

166. Water in star-forming regions with Herschel (WISH). VI. Constraints on UV and X-ray irradiation from a survey of hydrides in low- to high-mass young stellar objects

Author: E. F. van Dishoeck, Javier R. Goicoechea, Ruud Visser, Friedrich Wyrowski, M. Tafalla, Nick Indriolo, S. F. Wampfler, Edwin Bergin, Simon Bruderer, Paola Caselli, Michiel R. Hogerheijde, Fabrice Herpin, M. Melchior, Joseph C. Mottram, René Liseau, Brunella Nisini, Lars E. Kristensen, Darek Lis, Arnold O. Benz, Doug Johnstone, F. F. S. van der Tak, Institute of Astronomy [ETH Zürich], Department of Physics [ETH Zürich] (D-PHYS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Max-Planck-Institut für Extraterrestrische Physik (MPE), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Institut Pierre Louis d'Epidémiologie et de Santé Publique (iPLESP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de la Santé et de la Recherche Médicale (INSERM), SRON Netherlands Institute for Space Research (SRON), Instituto de Ciencia de Materiales de Madrid (ICMM), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Bergen University College, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Department of Astronomy University of Michigan, University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, FORMATION STELLAIRE 2016, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), foreign laboratories (FL), CERN [Genève], Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7 Canada, Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, INAF - Osservatorio Astronomico di Roma (OAR), Istituto Nazionale di Astrofisica (INAF), Plant Breeding, Wageningen University and Research [Wageningen] (WUR), Max-Planck-Institut für Radioastronomie (MPIFR), Swiss National Science Foundation, Royal Netherlands Academy of Arts and Sciences, Netherlands Research School for Astronomy, National Aeronautics and Space Administration (US), European Research Council, Astronomy, Universiteit Leiden, and École normale supérieure - Paris (ENS-PSL)
Subjects: 010504 meteorology & atmospheric sciences, Absorption spectroscopy, Astrophysics::High Energy Astrophysical Phenomena, Extinction (astronomy), Flux, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, ultraviolet: ISM, Luminosity, low-mass [Stars], stars: low-mass, 0103 physical sciences, massive [Stars], Physics::Atomic and Molecular Clusters, Protostar, Astrophysics::Solar and Stellar Astrophysics, 14. Life underwater, Emission spectrum, Physics::Chemical Physics, 010303 astronomy & astrophysics, molecules [ISM], formation [Stars], Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Astrochemistry, Physics, stars: formation, astrochemistry, Astronomy and Astrophysics, Circumstellar envelope, Radius, ISM: molecules, stars: massive, 13. Climate action, Space and Planetary Science, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], ISM [Ultraviolet]
Abstract: [Context] Hydrides are simple compounds containing one or a few hydrogen atoms bonded to a heavier atom. They are fundamental precursor molecules in cosmic chemistry and many hydride ions have become observable in high quality for the first time thanks to the Herschel Space Observatory. Ionized hydrides such as CH+ and OH+ (and also HCO+), which affect the chemistry of molecules such as water, provide complementary information on irradiation by far-UV (FUV) or X-rays and gas temperature., [Aims] We explore hydrides of the most abundant heavier elements in an observational survey covering young stellar objects (YSOs) with different mass and evolutionary state. The focus is on hydrides associated with the dense protostellar envelope and outflows, contrary to previous work that focused on hydrides in diffuse foreground clouds., [Methods] Twelve YSOs were observed with HIFI on Herschel in six spectral settings providing fully velocity-resolved line profiles as part of the Water in star-forming regions with Herschel (WISH) program. The YSOs include objects of low (Class 0 and I), intermediate, and high mass, with luminosities ranging from 4 L⊙ to 2 × 105 L⊙., [Results] The targeted lines of CH+, OH+, H2O+, C+, and CH are detected mostly in blue-shifted absorption. H3O+ and SH+ are detected in emission and only toward some high-mass objects. The observed line parameters and correlations suggest two different origins related to gas entrained by the outflows and to the circumstellar envelope. The derived column densities correlate with bolometric luminosity and envelope mass for all molecules, best for CH, CH+, and HCO+. The column density ratios of CH+/OH+ are estimated from chemical slab models, assuming that the H2 density is given by the specific density model of each object at the beam radius. For the low-mass YSOs the observed ratio can be reproduced for an FUV flux of 2–400 times the interstellar radiation field (ISRF) at the location of the molecules. In two high-mass objects, the UV flux is 20–200 times the ISRF derived from absorption lines, and 300–600 ISRF using emission lines. Upper limits for the X-ray luminosity can be derived from H3O+ observations for some low-mass objects., [Conclusions] If the FUV flux required for low-mass objects originates at the central protostar, a substantial FUV luminosity, up to 1.5 L⊙, is required. There is no molecular evidence for X-ray induced chemistry in the low-mass objects on the observed scales of a few 1000 AU. For high-mass regions, the FUV flux required to produce the observed molecular ratios is smaller than the unattenuated flux expected from the central object(s) at the Herschel beam radius. This is consistent with an FUV flux reduced by circumstellar extinction or by bloating of the protostar., The work on star formation at ETH Zurich was partially funded by the Swiss National Science Foundation (grant No. 200020-113556). Astrochemistry in Leiden is supported by the Netherlands Research School for Astronomy (NOVA), by a Royal Netherlands Academy of Arts and Sciences (KNAW) professor prize, and by the European Union A-ERC grant 291141 CHEMPLAN. Support for this work was also provided by NASA (Herschel OT funding) through an award issued by JPL/ Caltech.
Published: 2016

167. The type Iax supernova, SN 2015H: a white dwarf deflagration candidate

Author: Stephen J. Smartt, Mark Sullivan, T.-W. Chen, David Rabinowitz, David Young, Wolfgang Hillebrandt, Kate Maguire, S. Valenti, M. R. Magee, Lluís Galbany, L. Le Guillou, Stuart A. Sim, Heather Campbell, Ruediger Pakmor, Avishay Gal-Yam, Ashley J. Ruiter, J. D. Lyman, Markus Kromer, Cosimo Inserra, M. Fink, C. Baltay, Friedrich K. Röpke, Erkki Kankare, Ivo R. Seitenzahl, Rubina Kotak, Astrophysics Research Centre [Belfast] (ARC), Queen's University [Belfast] (QUB), The Oskar Klein Centre for Cosmoparticle Physics and Department of Physics, Stockholm University, department of physics, Yale University, Yale University [New Haven], Institute of Astronomy [Cambridge], University of Cambridge [UK] (CAM), Max-Planck-Institut für Extraterrestrische Physik (MPE), Institut für Theoretische Physik und Astrophysik [Würzburg], Julius-Maximilians-Universität Würzburg [Wurtzbourg, Allemagne] (JMU), Department of Particle Physics and Astrophysics, Weizmann Institute of Science [Rehovot, Israël], Departamento de Astronomía, Universidad de Chile = University of Chile [Santiago] (UCHILE), Millennium Institute of Astrophysics, Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Sorbonne Université (SU), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Department of Physics, University of Warwick, University of Warwick [Coventry], Heidelberger Institut für Theoretische Studien (H-ITS), Research School of Astronomy and Astrophysics [Canberra] (RSAA), Australian National University (ANU), Centre of Excellence for All-Sky Astrophysics (CAASTRO), School of Physics and Astronomy [Southampton], University of Southampton, Department of Physics, University of California, University of California [Los Angeles] (UCLA), and University of California-University of California
Subjects: [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], FOS: Physical sciences, Astrophysics, Type (model theory), 01 natural sciences, Spectral line, individual: SN 2015H [supernovae], 0103 physical sciences, 010306 general physics, Ejecta, 010303 astronomy & astrophysics, Chandrasekhar limit, Solar and Stellar Astrophysics (astro-ph.SR), Physics, High Energy Astrophysical Phenomena (astro-ph.HE), White dwarf, Astronomy and Astrophysics, Light curve, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Supernova, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Magnitude (astronomy), Astrophysics - High Energy Astrophysical Phenomena, general [supernovae]
Abstract: We present results based on observations of SN 2015H which belongs to the small group of objects similar to SN 2002cx, otherwise known as type Iax supernovae. The availability of deep pre-explosion imaging allowed us to place tight constraints on the explosion epoch. Our observational campaign began approximately one day post-explosion, and extended over a period of about 150 days post maximum light, making it one of the best observed objects of this class to date. We find a peak magnitude of M$_r$ = -17.27 $\pm$ 0.07, and a ($\Delta m_{15})_r$ = 0.69 $\pm$ 0.04. Comparing our observations to synthetic spectra generated from simulations of deflagrations of Chandrasekhar mass carbon-oxygen white dwarfs, we find reasonable agreement with models of weak deflagrations that result in the ejection of ~0.2 M$_{\odot}$ of material containing ~0.07 M$_{\odot}$ of 56Ni. The model light curve however, evolves more rapidly than observations, suggesting that a higher ejecta mass is to be favoured. Nevertheless, empirical modelling of the pseudo-bolometric light curve suggests that $\lesssim$0.6 M_sun of material was ejected, implying that the white dwarf is not completely disrupted, and that a bound remnant is a likely outcome., Comment: 19 pages, 12 figures, accepted for publication in Astronomy & Astrophysics
Published: 2016

168. The type Iax supernova, SN 2015H

Author: Magee, MR, Kotak, R, Sim, SA, Kromer, M, Rabinowitz, D, Smartt, SJ, Baltay, C, Campbell, HC, Chen, T-W, Fink, M, Gal-Yam, A, Galbany, L, Hillebrandt, W, Inserra, C, Kankare, E, Le Guillou, L, Lyman, JD, Maguire, K, Pakmor, R, Röpke, FK, Ruiter, AJ, Seitenzahl, IR, Sullivan, M, Valenti, S, Young, DR, Apollo - University of Cambridge Repository, Astrophysics Research Centre [Belfast] (ARC), Queen's University [Belfast] (QUB), The Oskar Klein Centre for Cosmoparticle Physics and Department of Physics, Stockholm University, department of physics, Yale University, Yale University [New Haven], Institute of Astronomy [Cambridge], University of Cambridge [UK] (CAM), Max-Planck-Institut für Extraterrestrische Physik (MPE), Institut für Theoretische Physik und Astrophysik [Wurzburg], Julius-Maximilians-Universität Würzburg [Wurtzbourg, Allemagne] (JMU), Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Departamento de Astronomía, Universidad de Chile, Millennium Institute of Astrophysics, Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Sorbonne Université (SU), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Department of Physics, University of Warwick, University of Warwick [Coventry], Heidelberger Institut für Theoretische Studien (H-ITS), Research School of Astronomy and Astrophysics [Canberra] (RSAA), Australian National University (ANU), Centre of Excellence for All-Sky Astrophysics (CAASTRO), School of Physics and Astronomy [Southampton], University of Southampton, Department of Physics, University of California, University of California [Los Angeles] (UCLA), and University of California-University of California
Subjects: [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], supernovae: individual: SN 2015H, supernovae: general, ComputingMilieux_MISCELLANEOUS
Abstract: This is the final version of the article. It first appeared from EDP Sciences via http://dx.doi.org/10.1051/0004-6361/201528036, We present results based on observations of SN 2015H which belongs to the small group of objects similar to SN 2002cx, otherwise known as type Iax supernovae. The availability of deep pre-explosion imaging allowed us to place tight constraints on the explosion epoch. Our observational campaign began approximately one day post-explosion, and extended over a period of about 150 days post maximum light, making it one of the best observed objects of this class to date. We find a peak magnitude of M$_{r}$ = −17.27± 0.07, and a (Δm$_{15}$)$_{r}$ = 0.69 ± 0.04. Comparing our observations to synthetic spectra generated from simulations of deflagrations of Chandrasekhar mass carbon-oxygen white dwarfs, we find reasonable agreement with models of weak deflagrations that result in the ejection of ~0.2 M$_{⊙}$ of material containing ~0.07 M$_{⊙}$ of $^{56}$Ni. The model light curve however, evolves more rapidly than observations, suggesting that a higher ejecta mass is to be favoured. Nevertheless, empirical modelling of the pseudo-bolometric light curve suggests that ≲0.6 M$_{⊙}$ of material was ejected, implying that the white dwarf is not completely disrupted, and that a bound remnant is a likely outcome.
Published: 2016

169. Discovery of a Metal-Poor Field Giant with a Globular Cluster Second-Generation Abundance Pattern

Author: S. Blanco-Cuaresma, Matthew Shetrone, D. A. García-Hernández, Sz. Meszaros, Diogo Souto, José G. Fernández-Trincado, K. Cunha, L. A. Martinez-Medina, Steven R. Majewski, Ricardo P. Schiavon, Jennifer Sobeck, Angeles Pérez-Villegas, Kaike Pan, Christopher Sneden, Olga Zamora, Ricardo Carrera, Baitian Tang, Friedrich Anders, Ronald E. Mennickent, Octavio Valenzuela, John Asher Johnson, E. Moreno, Alexandre Roman-Lopes, A. E. Garcia Perez, Douglas Geisler, Andres Meza, Céline Reylé, Katherine Vieira, Annie C. Robin, M. Schultheis, Barbara Pichardo, Gail Zasowski, F. Allard, Christian Nitschelm, Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Universidad Nacional Autónoma de México = National Autonomous University of Mexico (UNAM), Liverpool John Moores University (LJMU), Instituto de Astrofisica de Canarias (IAC), Universidad de La Laguna [Tenerife - SP] (ULL), Johns Hopkins University (JHU), University of Texas at Austin [Austin], Observatorio Nacional [Rio de Janeiro], Ohio State University [Columbus] (OSU), University of Virginia, Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève = University of Geneva (UNIGE), Max-Planck-Institut für Extraterrestrische Physik (MPE), Universidad Andrés Bello [Santiago] (UNAB), ELTE Gothard Astrophysical Observatory, Eötvös Loránd University (ELTE), Universidad de Concepción - University of Concepcion [Chile], Leibniz-Institut für Astrophysik Potsdam (AIP), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Universidad de La Serena (USERENA), New Mexico State University, Universidad Católica del Norte [Antofagasta], Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: 010504 meteorology & atmospheric sciences, Milky Way, Population II [Stars], Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, education, 010303 astronomy & astrophysics, QC, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, QB, 0105 earth and related environmental sciences, Physics, education.field_of_study, Galactic Center, Astronomy and Astrophysics, Galactic plane, Giant star, Astrophysics - Astrophysics of Galaxies, Stars, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), abundances [Stars], Globular cluster, general [Globular clusters], Halo, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: We report on detection, from observations obtained with the APOGEE spectroscopic survey, of a metal-poor ([Fe/H] $= -1.3$ dex) field giant star with an extreme Mg-Al abundance ratio ([Mg/Fe] $= -0.31$ dex; [Al/Fe] $= 1.49$ dex). Such low Mg/Al ratios are seen only among the second-generation population of globular clusters, and are not present among Galactic disk field stars. The light element abundances of this star, 2M16011638-1201525, suggest that it could have been born in a globular cluster. We explore several origin scenarios, in particular studying the orbit of the star to check the probability of it being kinematically related to known globular clusters. We performed simple orbital integrations assuming the estimated distance of 2M16011638-1201525 and the available six-dimensional phase-space coordinates of 63 globular clusters, looking for close encounters in the past with a minimum distance approach within the tidal radius of each cluster. We found a very low probability that 2M16011638-1201525 was ejected from most globular clusters; however, we note that the best progenitor candidate to host this star is globular cluster $��$ Centauri (NGC 5139). Our dynamical investigation demonstrates that 2M16011638-1201525 reaches a distance $|Z_{max}| < 3 $ kpc from the Galactic plane and a minimum and maximum approach to the Galactic center of $R_{min}, Accepted for publication in ApJ
Published: 2016

170. A COHERENT STUDY OF EMISSION LINES FROM BROADBAND PHOTOMETRY: SPECIFIC STAR FORMATION RATES AND [O III]/H beta RATIO AT 3 \textless z \textless 6

Author: Faisst, A. L., Capak, P., Hsieh, B. C., Laigle, C., Salvato, M., Tasca, L., Cassata, P., Davidzon, I., Ilbert, O., Le Fevre, O., Masters, D., McCracken, H. J., Steinhardt, C., Silverman, J. D., Barros, S., Hasinger, G., Scoville, N. Z., Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Centre de résonance magnétique biologique et médicale (CRMBM), Aix Marseille Université (AMU)-Assistance Publique - Hôpitaux de Marseille (APHM)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Extraterrestrische Physik (MPE), Excellence Cluster Universe, excellence cluster centre, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), AUTRES, Institute for Astronomy [Honolulu], University of Hawai‘i [Mānoa] (UHM), California Institute of Technology (CALTECH), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-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), and Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics
Abstract: International audience; We measure the H alpha and [O III] emission line properties as well as specific star formation rates (sSFRs) of spectroscopically confirmed 3 \textless z \textless 6 galaxies in COSMOS from their observed colors versus redshift evolution. Our model describes consistently the ensemble of galaxies including intrinsic properties (age, metallicity, star formation history), dust attenuation, and optical emission lines. We forward-model the measured Ha. equivalent widths (EW) to obtain the sSFR out to z similar to 6 without stellar mass fitting. We find a strongly increasing rest-frame Ha. EW that is flattening off above z similar to 2.5 with average EWs of 300-600 angstrom at z similar to 6. The sSFR is increasing proportionally to (1 + z)(2.4) at z \textless 2.2 and to (1 + z)(1.5) at higher redshifts, indicative of a fast build-up of mass in high-z galaxies within e-folding times of 100-200 Myr at z similar to 6. The redshift evolution at z \textgreater 3 cannot be fully explained in a picture of growth driven by cold accretion. We find a progressively increasing [O III]lambda 5007/H beta ratio out to z similar to 6, consistent with the ratios in local galaxies selected by increasing H alpha EW (i.e., sSFR). This demonstrates the potential of using “local high-z analogs” to investigate the spectroscopic properties and relations of galaxies in the re-ionization epoch.
Published: 2016

171. The XXL Survey: VI. The 1000 brightest X-ray point sources

Author: M. E. Ramos-Ceja, C. Adami, T. Sadibekova, Florian Pacaud, Dominique Eckert, Sophie Maurogordato, A. Iovino, L. Guennou, Matt S. Owers, Cathy Horellou, F. Ardila, Elias Koulouridis, Ivan K. Baldry, Christer Lidman, Andrii Elyiv, E. Pompei, Manolis Plionis, Stéphane Arnouts, Sinan Aliş, O. Melnyk, Marcella Brusa, Cristian Vignali, L. Faccioli, Sotiria Fotopoulou, Jon Willis, Seema Y Desai, Richard J. Tuffs, A. Stanford, Jochen Liske, Stéphane Paltani, Joseph J. Mohr, Malcolm N. Bremer, Angela Bongiorno, Marguerite Pierre, Enrico Piconcelli, Felipe Menanteau, Bianca M. Poggianti, L. Chiappetti, Piero Ranalli, Aristotle University of Thessaloniki, CEA/DCC/DRRV/SCD, Commissariat à l'Energie Atomique, Marcoule, Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), ISDC Data Centre for Astrophysics, University of Geneva [Switzerland], Lund Observatory, Lund University [Lund], National Observatory of Athens, Institute for Space Applications and Remote Sensing, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), 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), College of Computing (GATECH), Georgia Institute of Technology [Atlanta], Università di Bologna, Dipartimento di Astronomia, Università di Bologna [Bologna] (UNIBO), INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), INAF- Milano, Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, AUTRES, Astronomical Observatory of Kiev, Taras Shevchenko National University of Kyiv, Ecosystèmes aquatiques et changements globaux (UR EABX), Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA), INAF - Osservatorio Astronomico di Roma (OAR), Canada-France-Hawaii Telescope Corporation (CFHT), National Research Council of Canada (NRC)-Centre National de la Recherche Scientifique (CNRS)-University of Hawai'i [Honolulu] (UH), INAF-IASF Milano, Department of Earth and Space Sciences [Göteborg], Chalmers University of Technology [Göteborg], Astrophysique Interprétation Modélisation (AIM (UMR_7158 / 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), 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), Excellence Cluster Universe, excellence cluster centre, Max-Planck-Institut für Extraterrestrische Physik (MPE), Ludwig-Maximilians-Universität München (LMU), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Fotopoulou, S., Pacaud, F., Paltani, S., Ranalli, P., Ramos-Ceja, M.E., Faccioli, L., Plionis, M., Adami, C., Bongiorno, A., Brusa, M., Chiappetti, L., Desai, S., Elyiv, A., Lidman, C., Melnyk, O., Pierre, M., Piconcelli, E., Vignali, C., Alis, S., Ardila, F., Arnouts, S., Baldry, I., Bremer, M., Eckert, D., Guennou, L., Horellou, C., Iovino, A., Koulouridis, E., Liske, J., Maurogordato, S., Menanteau, F., Mohr, J.J., Owers, M., Poggianti, B., Pompei, E., Sadibekova, T., Stanford, A., Tuffs, R., Willis, J., Université de Genève = University of Geneva (UNIGE), Institute for Space Applications and Remote Sensing (ISARS/NOA), National Observatory of Athens (NOA), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), 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), 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)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), 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 Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Active galactic nucleus, Point source, Astrophysics::High Energy Astrophysical Phenomena, Infrarot-Astrophysik - Abteilung Hofmann, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Parameter space, catalogs, surveys, galaxies: active, X-rays: general, 01 natural sciences, Spectral line, Supercluster, general [X-rays], 0103 physical sciences, Survey, 010303 astronomy & astrophysics, Luminosity function, Astrophysics::Galaxy Astrophysics, QB, Photometric redshift, Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Galaxies: active, Astronomy and Astrophysic, Astrophysics - Astrophysics of Galaxies, Redshift, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), active [galaxies], Catalog, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: X-ray extragalactic surveys are ideal laboratories for the study of the evolution and clustering of active galactic nuclei (AGN). The XXL Survey spans two fields of a combined 50 $deg^2$ observed for more than 6Ms with XMM-Newton, occupying the parameter space between deep surveys and very wide area surveys; at the same time it benefits from a wealth of ancillary data. This paper marks the first release of the XXL point source catalogue selected in the 2-10 keV energy band with limiting flux $F_{2-10keV}=4.8\cdot10^{-14}\rm{erg\,s^{-1}\,cm^{-2}}$. We use both public and proprietary data sets to identify the counterparts of the X-ray point-like sources and improved upon the photometric redshift determination for AGN by applying a Random Forest classification trained to identify for each object the optimal photometric redshift model library. We also assign a probability to each source to be a star or an outlier. We model with Bayesian analysis the X-ray spectra assuming a power-law model with the presence of an absorbing medium. We find an average unabsorbed photon index of $\Gamma=1.85$ and average hydrogen column density $\log{N_{H}}=21.07 cm^{-2}$. We find no trend of $\Gamma$ or $N_H$ with redshift and a fraction of 26% absorbed sources ($\log N_{H}>22$). We show that the XXL-1000-AGN number counts extended the number counts of the COSMOS survey to higher fluxes and are fully consistent with the Euclidean expectation. We constrain the intrinsic luminosity function of AGN in the 2-10 keV energy band where the unabsorbed X-ray flux is estimated from the X-ray spectral fit up to z=3. Finally, we demonstrate the presence of a supercluster size structure at redshift 0.14, identified by means of percolation analysis of the XXL-1000-AGN sample. The XXL survey, reaching a medium flux limit and covering a wide area is a stepping stone between current deep fields and planned wide area surveys., Comment: 29 pages, 20 figures, 120 figures in the appendix, accepted for publication in A&A
Published: 2016

172. The long-wavelength thermal emission of the Pluto-Charon system from Herschel observations. Evidence for emissivity effects

Author: Raphael Moreno, P. Panuzzo, John Stansberry, Esa Vilenius, Silvia Protopapa, Tanya Lim, Tamás Müller, Pablo Santos-Sanz, Sonia Fornasier, Gábor Marton, Cs. Kiss, Emmanuel Lellouch, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Lunar and Planetary Laboratory [Tucson] (LPL), University of Arizona, Max-Planck-Institut für Extraterrestrische Physik (MPE), Konkoly Observatory, Research Centre for Astronomy and Earth Sciences [Budapest], Hungarian Academy of Sciences (MTA)-Hungarian Academy of Sciences (MTA), TKK Helsinki University of Technology (TKK), Southwest Research Institute [Boulder] (SwRI), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), and 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)
Subjects: Physics, [PHYS]Physics [physics], Earth and Planetary Astrophysics (astro-ph.EP), 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astronomy and Astrophysics, Context (language use), Astrophysics, Light curve, 01 natural sciences, Pluto, Wavelength, 13. Climate action, Space and Planetary Science, Asteroid, Brightness temperature, 0103 physical sciences, Emissivity, Penetration depth, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract: Thermal observations of the Pluto-Charon system acquired by the Herschel Space Observatory in February 2012 are presented. They consist of photometric measurements with the PACS and SPIRE instruments (nine visits to the Pluto system each), covering six wavelengths from 70 to 500 $\mu$m altogether. The thermal light curve of Pluto-Charon is observed in all filters, albeit more marginally at 160 and especially 500 $\mu$m. Putting these data into the context of older ISO, Spitzer and ground-based observations indicates that the brightness temperature (T$_B$) of the system (rescaled to a common heliocentric distance) drastically decreases with increasing wavelength, from $\sim$53 K at 20 $\mu$m to $\sim$35 K at 500 $\mu$m, and perhaps ever less at longer wavelengths. Considering a variety of diurnal and/or seasonal thermophysical models, we show that T$_B$ values of 35 K are lower than any expected temperature for the dayside surface or subsurface of Pluto and Charon, implying a low surface emissivity. Based on multiterrain modeling, we infer a spectral emissivity that decreases steadily from 1 at 20-25 $\mu$m to $\sim$0.7 at 500~$\mu$m. This kind of behavior is usually not observed in asteroids (when proper allowance is made for subsurface sounding), but is found in several icy surfaces of the solar system. We tentatively identify that a combination of a strong dielectric constant and a considerable surface material transparency (typical penetration depth $\sim$1 cm) is responsible for the effect. Our results have implications for the interpretation of the temperature measurements by REX/New Horizons at 4.2 cm wavelength., Comment: 15 pages, 9 figures, 2 tables
Published: 2016

173. A spectroscopic survey of X-ray-selected AGNs in the northern XMM-XXL field

Author: Johannes Buchner, Éric Aubourg, Tom Dwelly, M. L. Menzel, W. N. Brandt, Patrick Petitjean, Mara Salvato, Andrea Merloni, Isabelle Pâris, Kirpal Nandra, Antonis Georgakakis, Marcella Brusa, Axel Schwope, Max-Planck-Institut für Extraterrestrische Physik (MPE), 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), Dipartimento di Fisica e Astronomia [Bologna], Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Leibniz-Institut für Astrophysik Potsdam (AIP), 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), Università di Bologna [Bologna] (UNIBO), Menzel, M.-L., Merloni, A., Georgakakis, A., Salvato, M., Aubourg, E., Brandt, W.N., Brusa, M., Buchner, J., Dwelly, T., Nandra, K., Pâris, I., Petitjean, P., Schwope, A., 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)
Subjects: Infrared: galaxie, Active galactic nucleus, Infrared, Astrophysics::High Energy Astrophysical Phenomena, Techniques: spectroscopic, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Spectral line, 0103 physical sciences, Emission spectrum, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, Line (formation), Physics, Luminous infrared galaxy, [PHYS]Physics [physics], 010308 nuclear & particles physics, Quasars: emission line, Astronomy, Astronomy and Astrophysics, Galaxies: active, Astronomy and Astrophysic, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Galaxies: starburst, X-rays: galaxie
Abstract: This paper presents a survey of X-ray selected active galactic nuclei (AGN) with optical spectroscopic follow-up in a $\sim 18\, \rm{deg^2}$ area of the equatorial XMM-XXL north field. A sample of 8445 point-like X-ray sources detected by XMM-Newton above a limiting flux of $F_{\rm 0.5-10\, keV} > 10^{-15} \rm\,erg\, cm^{-2}\, s^{-1}$ was matched to optical (SDSS) and infrared (WISE) counterparts. We followed up 3042 sources brighter than $r=22.5$ mag with the SDSS BOSS spectrograph. The spectra yielded a reliable redshift measurement for 2578 AGN in the redshift range $z=0.02-5.0$, with $0.5-2\rm\, keV$ luminosities ranging from $10^{39}-10^{46}\rm\,erg\,s^{-1}$. This is currently the largest published spectroscopic sample of X-ray selected AGN in a contiguous area. The BOSS spectra of AGN candidates show a bimodal distribution of optical line widths allowing a separation between broad- and narrow-emission line AGN. The former dominate our sample (70 per cent) due to the relatively bright X-ray flux limit and the optical BOSS magnitude limit. We classify the narrow emission line objects (22 per cent of full sample) using standard BPT diagnostics: the majority have line ratios indicating the dominant source of ionization is the AGN. A small number (8 per cent of full sample) exhibit the typical narrow line ratios of star-forming galaxies, or only have absorption lines in their spectra. We term the latter two classes "elusive'' AGN. We also compare X-ray, optical and infrared color AGN selections in this field. X-ray observations reveal, the largest number of AGN. The overlap between the selections, which is a strong function of the imaging depth in a given band, is also remarkably small. We show using spectral stacking that a large fraction of the X-ray AGN would not be selectable via optical or IR colours due to host galaxy contamination., 26 pages, 21 figures. Accepted for publication in MNRAS. We publicly release the catalogue of X-ray selected AGN on the following webpage: http://www.mpe.mpg.de/XraySurveys/XMM-XXL/
Published: 2016

174. Dust attenuation in z ~ 1 galaxies from Herschel and 3D-HST Hα measurements

Author: Kevin Schawinski, A. Puglisi, S. Berta, Alberto Franceschini, Chiara Mancini, Giulia Rodighiero, Alvio Renzini, Margherita Talia, Andrea Cimatti, Dieter Lutz, Carlotta Gruppioni, S. J. Oliver, E. Daddi, Ivano Baronchelli, John D. Silverman, Dipartimento di Fisica e Astronomia 'Galileo Galilei', Universita degli Studi di Padova, INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), 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), INAF - Osservatorio Astronomico di Padova (OAPD), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), Kavli Institute for the Physics and Mathematics of the Universe, The University of Tokyo, Max-Planck-Institut für Extraterrestrische Physik (MPE), University of Sussex, Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Kavli Institute for the Physics and Mathematics of the Universe [Tokyo] (Kavli IPMU), The University of Tokyo Institutes for Advanced Study (UTIAS), The University of Tokyo (UTokyo)-The University of Tokyo (UTokyo), ITA, USA, GBR, FRA, DEU, JPN, Puglisi, A., Rodighiero, G., Franceschini, A., Talia, Margherita, Cimatti, Andrea, Baronchelli, I., Daddi, E., Renzini, A., Schawinski, K., Mancini, C., Silverman, J., Gruppioni, C., Lutz, D., Berta, S., Oliver, S. J., Università degli Studi di Padova = University of Padua (Unipd), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), and 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)
Subjects: Infrared, astro-ph.GA, Astrophysics, 01 natural sciences, Spectral line, galaxies: high-redshift, 0103 physical sciences, 010303 astronomy & astrophysics, Dust, extinction, Physics, infrared: ISM, 010308 nuclear & particles physics, extinction, Attenuation, Low resolution, Galaxies: high-redshift, Galaxies: star formation, Infrared: ISM, astro-ph.CO, Astronomy and Astrophysics, Space and Planetary Science, Astronomy, Spectral density, Astronomy and Astrophysic, Galaxy, Redshift, galaxies: star formation, dust, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: We combined the spectroscopic information from the 3D-HST survey with Herschel data to characterize the Hα dust attenuation properties of a sample of 79 main sequence star-forming galaxies at z ~ 1 in the GOODS-S field. The sample was selected in the far-IR at λ = 100 and/or 160 μm and only includes galaxies with a secure Hα detection (S/N > 3). From the low resolution 3D-HST spectra we measured the redshifts and the Hα fluxes for the whole sample. (A factor of 1/1.2 was applied to the observed fluxes to remove the [NII] contamination.) The stellar masses (M⋆), infrared (LIR), and UV luminosities (LUV) were derived from the spectral energy distributions by fitting multiband data from GALEX near-UV to SPIRE 500 μm. We estimated the continuum extinction Estar(B-V) from both the IRX = LIR/LUV ratio and the UV-slope, β, and found excellent agreement between the two. The nebular extinction was estimated from comparison of the observed SFRHα and SFRUV. We obtained f = Estar(B-V) /Eneb(B-V) = 0.93 ± 0.06, which is higher than the canonical value of f = 0.44 measured in the local Universe. Our derived dust correction produces good agreement between the Hα and IR+UV SFRs for galaxies with SFR ≳ 20M☉/yr and M⋆ ≳ 5 × 1010M☉, while objects with lower SFR and M⋆ seem to require a smaller f-factor (I.e. higher Hα extinction correction). Our results then imply that the nebular extinction for our sample is comparable to extinction in the optical-UV continuum and suggest that the f-factor is a function of both M⋆ and SFR, in agreement with previous studies.
Published: 2016

175. Two evolved supernova remnants with newly identified Fe-rich cores in the Large Magellanic Cloud

Author: Evan J Crawford, P. J. Kavanagh, P. Maggi, Miroslav Filipovic, Sean D Points, Luke M Bozzetto, Frank Haberl, Manami Sasaki, John R. Dickel, Emma Whelan, Institut für Astronomie und Astrophysik [Tübingen] (IAAT), Eberhard Karls Universität Tübingen = Eberhard Karls University of Tuebingen, Western Sydney University, Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory (NOAO), The University of New Mexico [Albuquerque], Max-Planck-Institut für Extraterrestrische Physik (MPE), 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), 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), Eberhard Karls Universität Tübingen, and Western Sydney University (UWS)
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Spectral index, 010308 nuclear & particles physics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, X-rays: ISM, law.invention, Interstellar medium, Telescope, Supernova, Space and Planetary Science, law, 0103 physical sciences, Magellanic Clouds, Emission spectrum, Astrophysics - High Energy Astrophysical Phenomena, Large Magellanic Cloud, Ejecta, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Blast wave, ISM: supernova remnants
Abstract: Aims. We present a multi-wavelength analysis of the evolved supernova remnants MCSNR J0506-7025 and MCSNR J0527-7104 in the Large Magellanic Cloud. Methods. We used data from XMM-Newton, the Australian Telescope Compact Array, and the Magellanic Cloud Emission Line Survey to study their broadband emission and used Spitzer and HI data to gain a picture of their environments. We performed a multi-wavelength morphological study and detailed radio and X-ray spectral analyses to determine their physical characteristics. Results. Both remnants were found to have bright X-ray cores, dominated by Fe L-shell emission, consistent with reverse shock heated ejecta with determined Fe masses in agreement with Type Ia explosion yields. A soft X-ray shell, consistent with swept-up interstellar medium, was observed in MCSNR J0506-7025, suggestive of a remnant in the Sedov phase. Using the spectral fit results and the Sedov self-similar solution, we estimated the age of MCSNR J0506-7025 to be ~16-28 kyr, with an initial explosion energy of (0.07-0.84)x10^51 erg. A soft shell was absent in MCSNR J0527-7104, with only ejecta emission visible in an extremely elongated morphology extending beyond the optical shell. We suggest that the blast wave has broken out into a low density cavity, allowing the shock heated ejecta to escape. We found that the radio spectral index of MCSNR J0506-7025 is consistent with the standard ~0.5 for SNRs. Radio polarisation at 6 cm indicates a higher degree of polarisation along the western front and at the eastern knot, with a mean fractional polarisation across the remnant of P~(20 \pm 6)%. Conclusions. The detection of Fe-rich ejecta in the remnants suggests that both resulted from Type Ia explosions. The newly identified Fe-rich cores in MCSNR J0506-7025 and MCSNR J0527-7104 makes them members of the expanding class of evolved Fe-rich remnants in the Magellanic Clouds., Comment: 16 pages, 13 figures, accepted for publication in A&A. arXiv admin note: text overlap with arXiv:1509.06475
Published: 2016

176. Inflow of atomic gas fuelling star formation

Author: Patricia Schady, Sandra Savaglio, E. Le Floc'h, A. Nicuesa Guelbenzu, Gianfranco Gentile, Andrea Rossi, Maarten Baes, J. Juul Rasmussen, S. D. Vergani, A. de Ugarte Postigo, D. Burlon, J. Elliott, P. van der Werf, J. M. Castro Cerón, L. K. Hunt, M. P. Koprowski, Michał J. Michałowski, Darach Watson, Peter Kamphuis, Jeppe Hjorth, D. Malesani, D. Crosby, S. Klose, S. Berta, Tara Murphy, Dong Xu, Mark R. Krumholz, V. D'Elia, Eliana Palazzi, Jochen Greiner, S. Basa, Nial R. Tanvir, Niels Bohr Institute [Copenhagen] (NBI), Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU), Department of Physics and Astronomy [Leicester], University of Leicester, Astronomisches Institut der Ruhr-Universität Bochum, Ruhr-Universität Bochum [Bochum], Universiteit Gent [Ghent], Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), Scottish Universities Physics Alliance, Institute for Astronomy (SUPA), University of Edinburgh, Max-Planck-Institut für Extraterrestrische Physik (MPE), 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), CNR Institute of Atmospheric Sciences and Climate (ISAC), Consiglio Nazionale delle Ricerche (CNR), Medcom [Odense], Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Universiteit Gent = Ghent University [Belgium] (UGENT), 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, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)
Subjects: [PHYS]Physics [physics], Physics, 13. Climate action, Space and Planetary Science, Star formation, Astronomy and Astrophysics, Astrophysics, Inflow, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], ComputingMilieux_MISCELLANEOUS
Abstract: Gamma-ray burst host galaxies are deficient in molecular gas, and show anomalous metal-poor regions close to GRB positions. Using recent Australia Telescope Compact Array (ATCA) Hi observations we show that they have substantial atomic gas reservoirs. This suggests that star formation in these galaxies may be fuelled by recent inflow of metal-poor atomic gas. While this process is debated, it can happen in low-metallicity gas near the onset of star formation because gas cooling (necessary for star formation) is faster than the Hi-to-H2 conversion.
Published: 2016

177. James Webb Space Telescope Observations of Stellar Occultations by Solar System Bodies and Rings

Author: Felipe Braga-Ribas, Stefanie N. Milam, Noemi Pinilla-Alonso, Zhong-Yi Lin, Leslie A. Young, Th. Müller, Esa Vilenius, Pablo Santos-Sanz, J. L. Ortiz, Gonzalo Tancredi, John Stansberry, Amanda S. Bosh, Z. W. Zhang, Rene Duffard, Emmanuel Lellouch, Richard G. French, Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Lunar and Planetary Laboratory [Tucson] (LPL), University of Arizona, Max-Planck-Institut für Extraterrestrische Physik (MPE), Observatório Nacional/MCT, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, 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)
Subjects: Physics, [PHYS]Physics [physics], Solar System, 010504 meteorology & atmospheric sciences, James Webb Space Telescope, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Lagrangian point, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Occultation, Space and Planetary Science, 0103 physical sciences, Orbit (dynamics), Astrophysics::Solar and Stellar Astrophysics, Stellar occultation, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences
Abstract: In this paper, we investigate the opportunities provided by the James Webb Space Telescope (JWST) for significant scientific advances in the study of Solar System bodies and rings using stellar occultations. The strengths and weaknesses of the stellar occultation technique are evaluated in light of JWST's unique capabilities. We identify several possible JWST occultation events by minor bodies and rings and evaluate their potential scientific value. These predictions depend critically on accurate a priori knowledge of the orbit of JWST near the Sun–Earth Lagrange point 2 (L2). We also explore the possibility of serendipitous stellar occultations by very small minor bodies as a byproduct of other JWST observing programs. Finally, to optimize the potential scientific return of stellar occultation observations, we identify several characteristics of JWST's orbit and instrumentation that should be taken into account during JWST's development.
Published: 2016

178. Diagnostic and model dependent uncertainty of simulated Tibetan permafrost area

Author: Charles D. Koven, Kazuyuki Saito, Chenghai Wang, Xuefeng Cui, Weiya Zhang, John C. Moore, Qinglin Li, Bertrand Decharme, Annette Rinke, S. Zhang, David M. Lawrence, Wenli Wang, Christine Delire, N. Zhang, Andrew H. MacDougall, A. D. McGuire, Duoying Ji, E. Burke, Max-Planck-Institut für Extraterrestrische Physik (MPE), College of Global Change and Earth System Science (GCESS), Beijing Normal University (BNU), State Key Laboratory of Earth Surface Processes and Resource Ecology (ESPRE), Zhejiang University, Centre de Nanosciences et de Nanotechnologies [Orsay] (C2N), Université Paris-Sud - Paris 11 (UP11)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Centre national de recherches météorologiques (CNRM), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Helmholtz Zentrum für Umweltforschung = Helmholtz Centre for Environmental Research (UFZ), and Météo France-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: 010504 meteorology & atmospheric sciences, Soil texture, Permafrost, Oceanography, 010502 geochemistry & geophysics, 01 natural sciences, Physical Geography and Environmental Geoscience, Meteorology & Atmospheric Sciences, [SDU.ENVI]Sciences of the Universe [physics]/Continental interfaces, environment, lcsh:Environmental sciences, ComputingMilieux_MISCELLANEOUS, Earth-Surface Processes, Water Science and Technology, 0105 earth and related environmental sciences, lcsh:GE1-350, geography, Plateau, geography.geographical_feature_category, lcsh:QE1-996.5, 15. Life on land, lcsh:Geology, Climate Action, 13. Climate action, Air temperature, Climatology, Ground temperature, Frost, Environmental science, Seasonal cycle, Snow cover
Abstract: We perform a land-surface model intercomparison to investigate how the simulation of permafrost area on the Tibetan Plateau (TP) varies among six modern stand-alone land-surface models (CLM4.5, CoLM, ISBA, JULES, LPJ-GUESS, UVic). We also examine the variability in simulated permafrost area and distribution introduced by five different methods of diagnosing permafrost (from modeled monthly ground temperature, mean annual ground and air temperatures, air and surface frost indexes). There is good agreement (99 to 135 × 104 km2) between the two diagnostic methods based on air temperature which are also consistent with the observation-based estimate of actual permafrost area (101 × 104 km2). However the uncertainty (1 to 128 × 104 km2) using the three methods that require simulation of ground temperature is much greater. Moreover simulated permafrost distribution on the TP is generally only fair to poor for these three methods (diagnosis of permafrost from monthly, and mean annual ground temperature, and surface frost index), while permafrost distribution using air-temperature-based methods is generally good. Model evaluation at field sites highlights specific problems in process simulations likely related to soil texture specification, vegetation types and snow cover. Models are particularly poor at simulating permafrost distribution using the definition that soil temperature remains at or below 0 °C for 24 consecutive months, which requires reliable simulation of both mean annual ground temperatures and seasonal cycle, and hence is relatively demanding. Although models can produce better permafrost maps using mean annual ground temperature and surface frost index, analysis of simulated soil temperature profiles reveals substantial biases. The current generation of land-surface models need to reduce biases in simulated soil temperature profiles before reliable contemporary permafrost maps and predictions of changes in future permafrost distribution can be made for the Tibetan Plateau.
Published: 2016

179. Non-linearity and environmental dependence of the star-forming galaxies main sequence

Author: Paola Popesso, F. Ziparo, Jeffrey A. Newman, G. Erfanianfar, N. Brandt, Andrea Biviano, S. Berta, H. Aussel, Albrecht Poglitsch, D. Wilman, M. Mirkazemi, Francesca Pozzi, Benjamin Magnelli, Mark Dickinson, Raanan Nordon, E. Le Floc'h, Kirpal Nandra, O. Ilbert, D. Fadda, D. Elbaz, Alexis Finoguenov, Andrea Cimatti, John S. Mulchaey, M. C. Cooper, R. M. Bielby, Nico Cappelluti, Masaomi Tanaka, L. Morselli, Dieter Lutz, Mara Salvato, Franz E. Bauer, M. B. Altieri, Stijn Wuyts, Max-Planck-Institut für Extraterrestrische Physik (MPE), Excellence Cluster Universe, excellence cluster centre, INAF - Osservatorio Astronomico di Trieste (OAT), Istituto Nazionale di Astrofisica (INAF), 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 de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Durham University, INAF - Osservatorio Astronomico di Bologna (OABO), AUTRES, 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 Bologna/Università di Bologna, Erfanianfar, G., Popesso, P., Finoguenov, A., Wilman, D., Wuyts, S., Biviano, A., Salvato, M., Mirkazemi, M., Morselli, L., Ziparo, F., Nandra, K., Lutz, D., Elbaz, D., Dickinson, M., Tanaka, M., Altieri, M.B., Aussel, H., Bauer, F., Berta, S., Bielby, R.M., Brandt, N., Cappelluti, N., Cimatti, A., Cooper, M.C., Fadda, D., Ilbert, O., Le Floch, E., Magnelli, B., Mulchaey, J.S., Nordon, R., Newman, J.A., Poglitsch, A., Pozzi, F., 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), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), University of Bologna, and NOAO
Subjects: Infrared: galaxie, haloes [Galaxies], FOS: Physical sciences, Astrophysics, Galaxies: groups: general, Astrophysics::Cosmology and Extragalactic Astrophysics, star formation [Galaxies], 01 natural sciences, evolution [Galaxy], Peculiar galaxy, galaxies [Infrared], Galaxy group, 0103 physical sciences, Disc, Galaxies: haloe, 010303 astronomy & astrophysics, Lenticular galaxy, Galaxy: structure, Galaxy cluster, Astrophysics::Galaxy Astrophysics, Luminous infrared galaxy, Physics, Galaxy: evolution, Galaxies: star formation, 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, Quasar, Astronomy and Astrophysic, Astrophysics - Astrophysics of Galaxies, groups: general [Galaxies], 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Elliptical galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], structure [Galaxy]
Abstract: Using data from four deep fields (COSMOS, AEGIS, ECDFS, and CDFN), we study the correlation between the position of galaxies in the star formation rate (SFR) versus stellar mass plane and local environment at $z10^{10.4-10.6}$ $M_{\odot}$), across all environments. At high redshift ( $0.5, Comment: 14 pages, 14 figures, accepted for publication in MNRAS
Published: 2016

180. Linking low- to high-mass YSOs with Herschel-HIFI observations of water

Author: Jose-Garcia, I. San, Mottram, J. C., van Dishoeck, E. F., Kristensen, L. E., van der Tak, F. F. S., Braine, J., Herpin, F., Johnstone, D., van Kempen, T. A., Wyrowski, F., Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Max-Planck-Institut für Extraterrestrische Physik (MPE), Danish Meat Research Institute (DMRI), SRON Netherlands Institute for Space Research (SRON), FORMATION STELLAIRE 2016, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7 Canada, Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, foreign laboratories (FL), and CERN [Genève]
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Astrophysics - Astrophysics of Galaxies, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: Water probes the dynamics in young stellar objects (YSOs) effectively, especially shocks in molecular outflows. It is a key molecule for exploring whether the physical properties of low-mass protostars can be extrapolated to massive YSOs. As part of the WISH key programme, we investigate the dynamics and the excitation conditions of shocks along the outflow cavity wall as function of source luminosity. Velocity-resolved Herschel-HIFI spectra of the H2O 988, 752, 1097 GHz and 12CO J=10-9, 16-15 lines were analysed for 52 YSOs with bolometric luminosities (L_bol) ranging from 10^5 L_sun. The profiles of the H2O lines are similar, indicating that they probe the same gas. We see two main Gaussian emission components in all YSOs: a broad component associated with non-dissociative shocks in the outflow cavity wall (cavity shocks) and a narrow component associated with quiescent envelope material. More than 60% of the total integrated intensity of the H2O lines (L_H2O) comes from the cavity shock component. The H2O line widths are similar for all YSOs, whereas those of 12CO 10-9 increase slightly with L_bol. The excitation analysis of the cavity shock component, performed with the non-LTE radiative transfer code RADEX, shows stronger 752 GHz emission for high-mass YSOs, likely due to pumping by an infrared radiation field. As previously found for CO, a strong correlation with slope unity is measured between log(L_H2O) and log(L_bol), which can be extrapolated to extragalactic sources. We conclude that the broad component of H2O and high-J CO lines originate in shocks in the outflow cavity walls for all YSOs, whereas lower-J CO transitions mostly trace entrained outflow gas. The higher UV field and turbulent motions in high-mass objects compared to their low-mass counterparts may explain the slightly different kinematical properties of 12CO 10-9 and H2O lines from low- to high-mass YSOs., Abridged abstract, 31 pages, 18 figures, 12 tables, accepted in Astronomy & Astrophysics
Published: 2016

181. CLASH-VLT: A highly precise strong lensing model of the galaxy cluster RXC J2248.7 - 4431 (Abell S1063) and prospects for cosmography

Author: Eros Vanzella, G. B. Caminha, Andrea Biviano, Brenda Frye, Bodo L. Ziegler, Keiichi Umetsu, Marc Postman, Christian Maier, Dan Coe, Italo Balestra, Marco Lombardi, M. Annunziatella, Anton M. Koekemoer, Stella Seitz, Piero Rosati, Amata Mercurio, Stefano Ettori, Sherry H. Suyu, Alexander Fritz, Tom Broadhurst, Stefano Borgani, Claudio Grillo, Peter Melchior, Paolo Tozzi, Karina Caputi, Mario Nonino, Marisa Girardi, A. Monna, Adi Zitrin, Raphael Gobat, C. Delgado-Correal, W. Karman, Massimo Meneghetti, Barbara Sartoris, E. Munari, Caminha, G. B, Grillo, C., Rosati, P., Balestra, I., Karman, W., Lombardi, M., Mercurio, A., Nonino, M., Tozzi, P., Zitrin, A., Biviano, A., Girardi, Marisa, Koekemoer, A. M., Melchior, P., Meneghetti, M., Munari, Emiliano, Suyu, S. H., Umetsu, K., Annunziatella, Marianna, Borgani, Stefano, Broadhurst, T., Caputi, K. I., Coe, D., Delgado Correal, C., Ettori, S., Fritz, A., Frye, B., Gobat, R., Maier, C., Monna, A., Postman, M., Sartoris, Barbara, Seitz, S., Vanzella, E., Ziegler, B., Università degli Studi di Ferrara (UniFE), Dark Cosmology Centre (DARK), Niels Bohr Institute [Copenhagen] (NBI), Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU)-Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU), INAF - Osservatorio Astronomico di Trieste (OAT), Istituto Nazionale di Astrofisica (INAF), 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 Extraterrestrische Physik (MPE), Università degli Studi di Ferrara = University of Ferrara (UniFE), University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH)-Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH), 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), Astronomy, and University of Ferrara [Ferrara]
Subjects: Observational cosmology, galaxy cluster, Cosmological parameters, Dark matter, Galaxies: clusters: individual: RXC J2248.7-4431, Gravitational lensing: strong, Astronomy and Astrophysics, Space and Planetary Science, COSMOLOGICAL CONSTRAINTS, Cosmology and Nongalactic Astrophysics (astro-ph.CO), MAGNIFICATION MAPS, media_common.quotation_subject, gravitational lensing, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Lambda, 01 natural sciences, Omega, Cosmology, dark matter, NO, SPACE-TELESCOPE OBSERVATIONS, galaxy clusters, 0103 physical sciences, DARK-MATTER, LY-ALPHA NEBULA, cosmological parameters, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, MASS-DISTRIBUTION, media_common, Physics, Line-of-sight, Mass distribution, 010308 nuclear & particles physics, FRONTIER FIELDS CLUSTERS, gravitational lensing: strong, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Universe, GRAVITATIONAL LENSES, LYMAN-BREAK GALAXIES, galaxies: clusters: individual: RXC J2248.7-4431, Astrophysics of Galaxies (astro-ph.GA), HIGH-REDSHIFT, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We perform a comprehensive study of the total mass distribution of the galaxy cluster RXCJ2248 ($z=0.348$) with a set of high-precision strong lensing models, which take advantage of extensive spectroscopic information on many multiply lensed systems. In the effort to understand and quantify inherent systematics in parametric strong lensing modelling, we explore a collection of 22 models where we use different samples of multiple image families, parametrizations of the mass distribution and cosmological parameters. As input information for the strong lensing models, we use the CLASH HST imaging data and spectroscopic follow-up observations, carried out with the VIMOS and MUSE spectrographs, to identify bona-fide multiple images. A total of 16 background sources, over the redshift range $1.0-6.1$, are multiply lensed into 47 images, 24 of which are spectroscopically confirmed and belong to 10 individual sources. The cluster total mass distribution and underlying cosmology in the models are optimized by matching the observed positions of the multiple images on the lens plane. We show that with a careful selection of a sample of spectroscopically confirmed multiple images, the best-fit model reproduces their observed positions with a rms of $0.3$ in a fixed flat $\Lambda$CDM cosmology, whereas the lack of spectroscopic information lead to biases in the values of the model parameters. Allowing cosmological parameters to vary together with the cluster parameters, we find (at $68\%$ confidence level) $\Omega_m=0.25^{+0.13}_{-0.16}$ and $w=-1.07^{+0.16}_{-0.42}$ for a flat $\Lambda$CDM model, and $\Omega_m=0.31^{+0.12}_{-0.13}$ and $\Omega_\Lambda=0.38^{+0.38}_{-0.27}$ for a universe with $w=-1$ and free curvature. Using toy models mimicking the overall configuration of RXCJ2248, we estimate the impact of the line of sight mass structure on the positional rms to be $0.3\pm 0.1$.(ABRIDGED), Comment: 23 pages, 13 figures, accepted for publication in A&A
Published: 2016

182. Forced mode-coupling instability in two-dimensional complex plasmas

Author: Couëdel, L, Röcker, T. B., Zhdanov, S. K., Nosenko, V., Morfill, G. E., Ivlev, A. V., Physique des interactions ioniques et moléculaires (PIIM), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Extraterrestrische Physik (MPE), DLR Forschungsgruppe Komplexe Plasmen, Deutsches Zentrum für Luft- und Raumfahrt [Oberpfaffenhofen-Wessling] (DLR), and Couëdel, Lénaïc
Subjects: [SPI.PLASMA]Engineering Sciences [physics]/Plasmas, [SPI.PLASMA] Engineering Sciences [physics]/Plasmas
Abstract: It is demonstrated experimentally that the wake-mediated resonant coupling of the in-plane and out-of-plane collective motion in two-dimensional plasma crystals can be induced by applying various types of external forcing. When the forcing is sufficiently strong, it can trigger the mode-coupling instability leading to the melting of the crystalline monolayer. The experimental observations are supported by numerical analysis of the forced collective dynamics of particles with the wake-mediated interactions. The reported results show the universal nature of the wake-mediated mode coupling (also occurring for the " forced " wave modes) and confirm characteristic features of the mode-coupling instability predicted theoretically by Ivlev et al. [Phys. Rev. Lett. 113, 135002 (2014)].
Published: 2015

183. IKT 16: the first X-ray confirmed composite SNR in the SMC

Author: Kevin Grieve, Quentin Roper, Miroslav Filipovic, Jean Ballet, Frank Haberl, Chandreyee Maitra, Andrea Tiengo, 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), Western Sydney University (UWS), Max-Planck-Institut für Extraterrestrische Physik (MPE), Western Sydney University, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), and 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)
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Spectral index, Nebula, 010308 nuclear & particles physics, Point source, Astrophysics::High Energy Astrophysical Phenomena, Resolution (electron density), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Pulsar wind nebula, Pulsar, Space and Planetary Science, 0103 physical sciences, Magellanic Clouds, Small Magellanic Cloud, Astrophysics - High Energy Astrophysical Phenomena, Supernova remnant, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ISM: supernova remnants
Abstract: Aims: IKT 16 is an X-ray and radio-faint supernova remnant (SNR) in the Small Magellanic Cloud (SMC). A detailed X-ray study of this SNR with XMM-Newton confirmed the presence of a hard X-ray source near its centre, indicating the detection of the first composite SNR in the SMC. With a dedicated Chandra observation we aim to resolve the point source and confirm its nature. We also acquire new ATCA observations of the source at 2.1 GHz with improved flux density estimates and resolution. Methods: We perform detailed spatial and spectral analysis of the source. With the highest resolution X-ray and radio image of the centre of the SNR available today, we resolve the source and confirm its pulsar wind nebula (PWN) nature. Further, we constrain the geometrical parameters of the PWN and perform spectral analysis for the point source and the PWN separately. We also test for the radial variations of the PWN spectrum and its possible east west asymmetry. Results: The X-ray source at the centre of IKT 16 can be resolved into a symmetrical elongated feature centering a point source, the putative pulsar. Spatial modeling indicates an extent of 5.2 arcsec of the feature with its axis inclined at 82 degree east from north, aligned with a larger radio feature consisting of two lobes almost symmetrical about the X-ray source. The picture is consistent with a PWN which has not yet collided with the reverse shock. The point source is about three times brighter than the PWN and has a hard spectrum of spectral index 1.1 compared to a value 2.2 for the PWN. This points to the presence of a pulsar dominated by non-thermal emission. The expected E_{dot} is ~ 10^37 erg s^-1 and spin period < 100 ms. However, the presence of a compact nebula unresolved by Chandra at the distance of the SMC cannot completely be ruled out., 9 pages, 6 figures, 2 tables, Accepted for publication in Astronomy & Astrophysics
Published: 2015

184. Concurrent Starbursts in Molecular Gas Disks within a Pair of Colliding Galaxies at z = 1.52

Author: H. J. McCracken, Alvio Renzini, A. Puglisi, Christopher C. Hayward, John D. Silverman, Georgios E. Magdis, Anton M. Koekemoer, Jeyhan S. Kartaltepe, Jeremy Fensch, Matthieu Béthermin, Tohru Nagao, Mark Sargent, C. Mancini, Daichi Kashino, Nobuo Arimoto, Giulia Rodighiero, Francesco Valentino, Vernesa Smolčić, Wiphu Rujopakarn, Emanuele Daddi, Kartik Sheth, Frederic Bournaud, Daizhong Liu, The University of Tokyo (UTokyo), 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), Chulalongkorn University [Bangkok], Max-Planck-Institut für Extraterrestrische Physik (MPE), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Dipartimento di Astronomia, Università degli Studi di Padova = University of Padua (Unipd), National Astronomical Observatory of Japan (NAOJ), 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), Center for Computational Astrophysics [New York], Flatiron Institute, National Optical Astronomy Observatory (NOAO), Nagoya University, Space Telescope Science Institute (STSci), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), RIKEN International Frontier Research Group on Earthquakes at Earthquake Prediction Research Center, Tokai University, Spitzer Science Center, California Institute of Technology, Pasadena, California Institute of Technology (CALTECH), University of Zagreb, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), Universita degli Studi di Padova, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), University of Tokyo (University of Tokyo), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), and NOAO
Subjects: Angular momentum, PRIRODNE ZNANOSTI. Fizika. Astronomija i astrofizika, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], FOS: Physical sciences, galaxies: high-redshift, galaxies: ISM, galaxies: starburst, galaxies: star formation, galaxies: starburst, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy merger, 01 natural sciences, galaxies: high-redshift, 0103 physical sciences, NATURAL SCIENCES. Physics. Astronomy and Astrophysics, Interacting galaxy, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, QB, Physics, Coalescence (physics), ISM [galaxies], starburst [galaxies], 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Stars, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies: star formation, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Astrophysics::Earth and Planetary Astrophysics, star formation [galaxies], high-redshift [galaxies], galaxies: ISM
Abstract: We report on the discovery of a merger-driven starburst at z = 1.52, PACS-787, based on high signal-to-noise ALMA observations. CO(5-4) and continuum emission (850um) at a spatial resolution of 0.3" reveal two compact (r_1/2 ~ 1 kpc) and interacting molecular gas disks at a separation of 8.6 kpc thus indicative of an early stage in a merger. With a SFR of 991 Msun/yr, this starburst event should occur closer to final coalescence, as usually seen in hydrodynamical simulations. From the CO size, inclination, and velocity profile for both disks, the dynamical mass is calculated through a novel method that incorporates a calibration using simulations of galaxy mergers. Based on the dynamical mass, we measure (1) the molecular gas mass, independent from the CO luminosity, (2) the ratio of the total gas mass and the CO(1 - 0) luminosity (alpha_CO = M_gas/L'_CO(1-0)), and (3) the gas-to-dust ratio, with the latter two being lower than typically assumed. We find that the high star formation, triggered in both galaxies, is caused by a set of optimal conditions: a high gas mass/fraction, a short depletion time (t_depl=85 and 67 Myrs) to convert gas into stars, and the interaction of likely counter-rotating molecular disks that may accelerate the loss of angular momentum. The state of interaction is further established by the detection of diffuse CO and continuum emission, tidal debris that bridges the two nuclei and is associated with stellar emission seen by HST/WFC3. This observation demonstrates the power of ALMA to study the dynamics of galaxy mergers at high redshift., Comment: 21 pages, 16 figures, accepted to ApJ
Published: 2018

185. The SINS/zC-SINF Survey of z ∼ 2 Galaxy Kinematics: SINFONI Adaptive Optics–assisted Data and Kiloparsec-scale Emission-line Properties

Author: Philipp Lang, Thorsten Naab, Jaron Kurk, Giovanni Cresci, Richard Davies, E. Daddi, C. Mancini, Alvio Renzini, H. J. McCracken, V. Mainieri, G. Zamorani, Stijn Wuyts, Andrea Cimatti, Pascal Oesch, Linda J. Tacconi, K. Shapiro Griffin, N. Bouché, Reinhard Genzel, S. J. Lilly, Lucia Pozzetti, Shy Genel, Sandro Tacchella, Alice E. Shapley, Amiel Sternberg, Y. Peng, C. M. Carollo, Marco Scodeggio, Erin K. S. Hicks, M. Mignoli, Andreas Burkert, Dieter Lutz, N. M. Förster Schreiber, Max Planck Institute for Extraterrestrial Physics (MPE), Max-Planck-Gesellschaft, Max-Planck-Institut für Extraterrestrische Physik (MPE), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), AUTRES, Hunan Normal University (HNU), Universitätssternwarte der Ludwig-Maximiliansuniversität, Ludwig-Maximiliansuniversität, 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 St Andrews [Scotland], European Southern Observatory (ESO), 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), Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), INAF - Osservatorio Astronomico di Capodimonte (OAC), University of Bologna/Università di Bologna, Department of Physics and Astronomy [Irvine], University of California [Irvine] (UC Irvine), University of California (UC)-University of California (UC), Institut of Physics - Riga, Latvian Academy of Sciences, ITA, USA, FRA, DEU, CYP, ISR, CHN, CHE, Schreiber, N. M. Förster, Renzini, A., Mancini, C., Genzel, R., Bouché, N., Cresci, G., Hicks, E.K.S., Lilly, S.J., Peng, Y., Burkert, A., Carollo, C.M., Cimatti, A., Daddi, E., Davies, R.I., Genel, S., Kurk, J.D., Lang, P., Lutz, D., Mainieri, V., McCracken, H.J., Mignoli, M., Naab, T., Oesch, P., Pozzetti, L., Scodeggio, M., Griffin, K. Shapiro, Shapley, A.E., Sternberg, A., Tacchella, S., Tacconi, L.J., Wuyts, S., Zamorani, G., Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Osservatorio Astronomico (INAF), Hunan Normal University, 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), University of St Andrews, University of Bologna, University of California [Irvine] (UCI), University of California-University of California, Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)
Subjects: [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Population, FOS: Physical sciences, Flux, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, galaxies: high-redshift, kinematics and dynamics [galaxies], 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Emission spectrum, education, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, Physics, education.field_of_study, Very Large Telescope, ISM [galaxies], 010308 nuclear & particles physics, Astronomy and Astrophysics, Astronomy and Astrophysic, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), structure [galaxies], galaxies: structure, galaxies: kinematics and dynamic, H-alpha, Astrophysics::Earth and Planetary Astrophysics, galaxies: ISM, high-redshift [galaxies], Data reduction
Abstract: We present the "SINS/zC-SINF AO survey" of 35 star-forming galaxies, the largest sample with deep adaptive optics-assisted (AO) near-infrared integral field spectroscopy at z~2. The observations, taken with SINFONI at the Very Large Telescope, resolve the Ha and [NII] line emission and kinematics on scales of ~1.5 kpc. In stellar mass, star formation rate, rest-optical colors and size, the AO sample is representative of its parent seeing-limited sample and probes the massive (M* ~ 2x10^9 - 3x10^11 Msun), actively star-forming (SFR ~ 10-600 Msun/yr) part of the z~2 galaxy population over a wide range in colors ((U-V)_rest ~ 0.15-1.5 mag) and half-light radii (R_e,H ~ 1-8.5 kpc). The sample overlaps largely with the "main sequence" of star-forming galaxies in the same redshift range to a similar K_AB = 23 magnitude limit; it has ~0.3 dex higher median specific SFR, ~0.1 mag bluer median (U-V)_rest color, and ~10% larger median rest-optical size. We describe the observations, data reduction, and extraction of basic flux and kinematic properties. With typically 3-4 times higher resolution and 4-5 times longer integrations (up to 23hr) than the seeing-limited datasets of the same objects, the AO data reveal much more detail in morphology and kinematics. The now complete AO observations confirm the majority of kinematically-classified disks and the typically elevated disk velocity dispersions previously reported based on subsets of the data. We derive typically flat or slightly negative radial [NII]/Ha gradients, with no significant trend with global galaxy properties, kinematic nature, or the presence of an AGN. Azimuthal variations in [NII]/Ha are seen in several sources and are associated with ionized gas outflows, and possible more metal-poor star-forming clumps or small companions. [Abridged], Comment: Submitted to the Astrophysical Journal Supplement Series. 64 pages, 36 figures. The reduced data sets will be made available once the paper is accepted for publication. A version with full resolution Figures is available at http://www.mpe.mpg.de/~forster/FS18_AOsurvey_ApJSsubm.html
Published: 2018

186. Nuclear versus integrated spectroscopy of galaxies in the Herschel Reference Survey

Author: A. Boselli, Matteo Fossati, S. Belladitta, G. Consolandi, Giuseppe Gavazzi, Università degli Studi di Milano-Bicocca = University of Milano-Bicocca (UNIMIB), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Extraterrestrische Physik (MPE), Università degli Studi di Milano-Bicocca [Milano] (UNIMIB), Gavazzi, G, Consolandi, G, Belladitta, S, Boselli, A, and Fossati, M
Subjects: Active galactic nucleus, Stellar mass, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Population, Galaxies: fundamental parameter, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Stellar classification, 01 natural sciences, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Supermassive black hole, education.field_of_study, Galaxies: star formation, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Star formation, Galaxies: evolution, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Virgo Cluster, Galaxy, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics
Abstract: Context. The determination of the relative frequency of active galactic nuclei (AGN) versus other spectral classes, for example, HII region-like (HII), transition objects (TRAN), passive (PAS), and retired (RET), in a complete set of galaxies in the local Universe is of primary importance to discriminate the source of ionization in the nuclear region of galaxies. Aims. Here we aim to provide a spectroscopic characterization of the nuclei of galaxies belonging to the Herschel Reference Survey (HRS), a volume and magnitude limited sample representative of the local Universe, which has become a benchmark for local and high-z studies, for semianalytical models and cosmological simulations. The comparison between the nuclear spectral classification and the one determined on the global galactic scale provides information about how galaxy properties change from the nuclear to the outer regions. Moreover, the extrapolation of the global star formation (SF) properties from the SDSS fiber spectroscopy compared to the one computed by Halpha photometry can be useful for testing the method based on aperture correction for determining the global star formation rate (SFR) for local galaxies. Methods. By collecting the existing nuclear spectroscopy available from the literature, complemented with new observations obtained using the Loiano 1.52m telescope, we analyze the 322 nuclear spectra of HRS galaxies. Results. Using two diagnostic diagrams (the BPT and the WHAN) we provide a nuclear and an integrated spectral classification for the HRS galaxies. Conclusions. We find that the fraction of AGNs increases with stellar mass, such that at logM > 10.0 M\odot or 66% of the LTGs are AGNs or TRAN., 21 pages
Published: 2018

187. High-frequency elastic moduli of two-dimensional Yukawa fluids and solids

Author: B. A. Klumov, Sergey A. Khrapak, Theory, Max-Planck-Institut für Extraterrestrische Physik (MPE), Physique des interactions ioniques et moléculaires (PIIM), and Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)
Subjects: HIGH FREQUENCY HF, Differential equation, FOS: Physical sciences, Yukawa systems, YUKAWA FLUIDS, complex (dusty) plasmas, Condensed Matter - Soft Condensed Matter, 01 natural sciences, 010305 fluids & plasmas, Moduli, Shear modulus, ANALYTICAL RESULTS, [PHYS.PHYS.PHYS-PLASM-PH]Physics [physics]/Physics [physics]/Plasma Physics [physics.plasm-ph], 0103 physical sciences, Gruppe Komplexe Plasmen, ACOUSTIC WAVE VELOCITY, 010306 general physics, Elastic modulus, Condensed Matter - Statistical Mechanics, ComputingMilieux_MISCELLANEOUS, TWO DIMENSIONAL (2 D), Physics, Statistical Mechanics (cond-mat.stat-mech), two-dimensional systems, Numerical analysis, Yukawa potential, Plasma, Mechanics, Condensed Matter Physics, Physics - Plasma Physics, Plasma Physics (physics.plasm-ph), Transverse plane, DIFFERENTIAL EQUATIONS, ELASTIC MODULI, Soft Condensed Matter (cond-mat.soft), high-frequency elastic moduli, sound velocity, elastic properties, NUMERICAL CALCULATION, two-dimensional plasma crystals
Abstract: An approach to calculate high-frequency bulk and shear modului of two-dimensional (2D) weakly screened Yukawa fluids and solids is presented. Elastic moduli are directly related to sound velocities and other important characteristics of the system. In this article we discuss these relations and present exemplary calculation of the longitudinal, transverse, and instantaneous sound velocities and derive a differential equation for the Einstein frequency. Simple analytical results presented demonstrate good accuracy when compared with numerical calculations. The obtained results can be particularly useful in the context of 2D colloidal and complex (dusty) plasma monolayers., Comment: To be published in Phys. Plasmas
Published: 2018

188. Cluster survey of the mid-altitude cusp – Part 2: Large-scale morphology

Author: Iannis Dandouras, Berndt Klecker, F. Pitout, C. P. Escoubet, Laboratoire de Planétologie de Grenoble (LPG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), Max-Planck-Institut für Extraterrestrische Physik (MPE), Centre d'étude spatiale des rayonnements (CESR), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, MPE in Garching, Centre National d'Etudes Spatiales (CNES), Agence Spatiale Européenne = European Space Agency (ESA), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), and Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS)
Subjects: Atmospheric Science, 010504 meteorology & atmospheric sciences, Magnetosphere, Scale (descriptive set theory), Astrophysics, cusp and boundary layers, 01 natural sciences, and boundary layers, 0103 physical sciences, Earth and Planetary Sciences (miscellaneous), Cluster (physics), cusp, Proper time, Solar wind-magnetosphere interactions), Interplanetary magnetic field, lcsh:Science, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Cusp (singularity), lcsh:QC801-809, Geology, Astronomy and Astrophysics, Magnetospheric configuration and dy- namics, Geophysics, lcsh:QC1-999, Solar wind, lcsh:Geophysics. Cosmic physics, Magnetopause, Magnetospheric physics (Magnetopause, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Magnetospheric conﬁguration and dynamics, Magnetospheric physics, Physics::Space Physics, lcsh:Q, Solar wind-magnetosphere interactions, lcsh:Physics
Abstract: In this second part of our statistical study of the mid-altitude cusp, we compare the cusp morphology, as seen in the Cluster ion spectrometer (CIS), to the interplanetary magnetic field (IMF) orientation. We first recall the method we have used a) to define the cusp properties, b) to sort IMF conditions or behaviour in classes, c) to determine the proper time delay between the solar wind monitors and Cluster. Then, we define a few morphological features of the cusp and we relate these to the prevailing IMF. Our results reveal, among other things, that the occurrence of clearly dispersed ion structures in the cusp is 48%. From these dispersions, we infer the distance to reconnection site, which we relate to external conditions. In all other cases, the cusp exhibits a more disturbed behaviour in terms of ion structures and fall in our "discontinuous" or "irregular" categories. Among these, a few interesting cases of discontinuous cusps occurring under stable IMF conditions have been identified. They all occur when the IMF is dominated by its Y-component, which plays in principle in favour of anti-parallel reconnection but their wide MLT and latitudinal distributions is a priori incompatible with the anti-parallel reconnection hypothesis solely.
Published: 2009

189. ESSC-ESF Position Paper-Science-Driven Scenario for Space Exploration: Report from the European Space Sciences Committee (ESSC)

Author: Angioletta Coradini, Roberto Marco, Manuel Grande, Dave Rothery, Frances Westall, Jean-Pierre Bibring, Helmut Lammer, Antonella Barucci, Pascale Ehrenfreund, Peter Norsk, Gerhard Haerendel, Jean-Claude Worms, Bernhard Koch, J. E. Blamont, John Robert Brucato, Ian A. Crawford, Stephan Ulamec, Cam Tropea, Rupert Gerzer, Eric Chassefière, John C. Zarnecki, Monica M. Grady, Michel Blanc, Jean-Pierre Swings, Heno Falcke, Gerda Horneck, Reta Beebe, Andrei Lobanov, José Juan López-Moreno, Roger Bonnet, European Space Science Committee-European Science Foundation (ESSC-ESF), European Science Foundation (ESF), Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), New Mexico State University, 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 [Toulouse] (CNES), École polytechnique (X), International Space Science Institute [Bern] (ISSI), INAF - Osservatorio Astronomico di Capodimonte (OAC), Istituto Nazionale di Astrofisica (INAF), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Istituto di Fisica dello Spazio Interplanetario (IFSI), Consiglio Nazionale delle Ricerche (CNR), Birkbeck College [University of London], Universiteit Leiden [Leiden], Netherlands Institute for Radio Astronomy (ASTRON), Deutsches Zentrum für Luft- und Raumfahrt (DLR), Planetary and Space Sciences [Milton Keynes] (PSS), School of Physical Sciences [Milton Keynes], Faculty of Science, Technology, Engineering and Mathematics [Milton Keynes], The Open University [Milton Keynes] (OU)-The Open University [Milton Keynes] (OU)-Faculty of Science, Technology, Engineering and Mathematics [Milton Keynes], The Open University [Milton Keynes] (OU)-The Open University [Milton Keynes] (OU), University of Whales, Max-Planck-Institut für Extraterrestrische Physik (MPE), Max-Planck-Institut für Radioastronomie (MPIFR), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Universidad Autonoma de Madrid (UAM), University of Copenhagen = Københavns Universitet (KU), The Open University [Milton Keynes] (OU), Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, Technische Universität Darmstadt (TU Darmstadt), Centre de biophysique moléculaire (CBM), Université d'Orléans (UO)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC), 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), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Universiteit Leiden, Universidad Autónoma de Madrid (UAM), University of Copenhagen = Københavns Universitet (UCPH), Technische Universität Darmstadt - Technical University of Darmstadt (TU Darmstadt), and Université d'Orléans (UO)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Robotic exploration, Societies, Scientific, MARS-EXPRESS, European exploration programme, Robotic exploration, Human lunar missions, Human Mars missions, NEOs, Sample return missions, Planetary protection, International cooperation, NEAR-EARTH ASTEROIDS, MARS-EXPRESS, ASTRONOMY, MOON, Extraterrestrial Environment, 010504 meteorology & atmospheric sciences, Planetary protection, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Astronomy, International Cooperation, European exploration programme, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Human Mars missions, Mars, Library science, Context (language use), 01 natural sciences, Space exploration, Minor Planets, Astrobiology, 0103 physical sciences, Humans, Human lunar missions, Moon, GeneralLiterature_REFERENCE(e.g.,dictionaries,encyclopedias,glossaries), 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, NEAR-EARTH ASTEROIDS, 0105 earth and related environmental sciences, Human spaceflight, ASTRONOMY, International Agencies, Timeline, Robotics, Mars Exploration Program, Space Flight, Agricultural and Biological Sciences (miscellaneous), Europe, NEOs, 13. Climate action, Space and Planetary Science, Astronauts, Position paper, Sample return missions, Space Science, Goals, Geology
Abstract: International audience; In 2005 the then ESA Directorate for Human Spaceflight, Microgravity and Exploration (D-HME) commissioned a study from the European Science Foundation's (ESF) European Space Sciences Committee (ESSC) to examine the science aspects of the Aurora Programme in preparation for the December 2005 Ministerial Conference of ESA Member States, held in Berlin. A first interim report was presented to ESA at the second stakeholders meeting on 30 and 31 May 2005. A second draft report was made available at the time of the final science stakeholders meeting on 16 September 2005 in order for ESA to use its recommendations to prepare the Executive proposal to the Ministerial Conference. The final ESSC report on that activity came a few months after the Ministerial Conference (June 2006) and attempted to capture some elements of the new situation after Berlin, and in the context of the reduction in NASA's budget that was taking place at that time; e. g., the postponement sine die of the Mars Sample Return mission. At the time of this study, ESSC made it clear to ESA that the timeline imposed prior to the Berlin Conference had not allowed for a proper consultation of the relevant science community and that this should be corrected in the near future. In response to that recommendation, ESSC was asked again in the summer of 2006 to initiate a broad consultation to define a science-driven scenario for the Aurora Programme. This exercise ran between October 2006 and May 2007. ESA provided the funding for staff support, publication costs, and costs related to meetings of a Steering Group, two meetings of a larger ad hoc group ( 7 and 8 December 2006 and 8 February 2007), and a final scientific workshop on 15 and 16 May 2007 in Athens. As a result of these meetings a draft report was produced and examined by the Ad Hoc Group. Following their endorsement of the report and its approval by the plenary meeting of the ESSC, the draft report was externally refereed, as is now normal practice with all ESSC-ESF reports, and amended accordingly. The Ad Hoc Group defined overarching scientific goals for Europe's exploration programme, dubbed "Emergence and co-evolution of life with its planetary environments,"focusing on those targets that can ultimately be reached by humans, i.e., Mars, the Moon, and Near Earth Objects. Mars was further recognized as the focus of that programme, with Mars sample return as the recognized primary goal; furthermore the report clearly states that Europe should position itself as a major actor in defining and leading Mars sample return missions. The report is reproduced in this article. On 26 November 2008 the Ministers of ESA Member States decided to give a high strategic priority to the robotic exploration programme of Mars by funding the enhanced ExoMars mission component, in line therefore with the recommendations from this ESSC-ESF report.
Published: 2009

190. INTEGRALSPI All‐Sky View in Soft Gamma Rays: A Study of Point‐Source and Galactic Diffuse Emission

Author: Francois Lebrun, Regis Terrier, J. P. Roques, Roland Diehl, Andrew W. Strong, E. Jourdain, L. Bouchet, Centre d'étude spatiale des rayonnements (CESR), 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), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Extraterrestrische Physik (MPE), APC - Astrophysique des Hautes Energies (APC - AHE), Dipartimento di Astronomia, Universita degli Studi di Bologna, Università di Bologna [Bologna] (UNIBO)-Università di Bologna [Bologna] (UNIBO)-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)-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), AstroParticule et Cosmologie (APC (UMR_7164)), 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), INTEGRAL, Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, 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)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), 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 de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), 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)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), 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)
Subjects: Physics, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 010308 nuclear & particles physics, Point source, Astrophysics::High Energy Astrophysical Phenomena, Galactic ridge, Astrophysics (astro-ph), Gamma ray, FOS: Physical sciences, Flux, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Galaxy, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Space and Planetary Science, 0103 physical sciences, Halo, Emission spectrum, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Line (formation)
Abstract: We have processed the data accumulated with INTEGRAL SPI during 4 years (~ 51 Ms) to study the Galactic ``diffuse'' emission morphology in the 20 keV to 8 MeV energy range. To achieve this objective, we have derived simultaneously an all-sky census of emitting sources and images of the Galactic Ridge (GR) emission. In the central radian, the resolved point source emission amounts to 88%, 91% and 68% of the total emission in the 25-50, 50-100 and 100-300 keV domains respectively. We have compared the GR emission spatial distribution to those obtained from CO and NIR maps, and quantified our results through latitude and longitude profiles. Below 50 keV, the SPI data are better traced by the latter, supporting a stellar origin for this emission. Furthermore, we found that the GR emission spectrum follows a power law with a photon index ~ 1.55 above 50 keV while an additional component is required below this energy. This component shows a cutoff around 30 keV, reinforcing a stellar origin, as proposed by Krivonos et al. (2007). The annihilation diffuse emission component is extracted simultaneously, leading to the determination of the related parameters (positronium flux and fraction). A specific discussion is devoted to the annihilation line distribution since a significant emission is detected over a region as large as ~80 degrees by ~10 degrees potentially associated with the disk or halo surrounding the central regions of our Galaxy., 28 pages, 10 figures. Astrophysical journal (accepted for publication)
Published: 2008

191. Two sources of magnetosheath ions observed by Cluster in the mid-altitude polar cusp

Author: C. P. Escoubet, Andrew Fazakerley, Matthew Taylor, M. W. Dunlop, Arnaud Masson, Frederic Pitout, H. E. Laakso, C. Vallat, H. Rème, J. M. Bosqued, Jean Berchem, Karlheinz Trattner, Iannis Dandouras, European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), Institute of Geophysics and Planetary Physics [Los Angeles] (IGPP), University of California [Los Angeles] (UCLA), University of California-University of California, Centre d'étude spatiale des rayonnements (CESR), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Lockheed Martin Advanced Technology Center (ATC), Max-Planck-Institut für Extraterrestrische Physik (MPE), 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), Mullard Space Science Laboratory (MSSL), and University College of London [London] (UCL)
Subjects: Atmospheric Science, 010504 meteorology & atmospheric sciences, Mathematics::Number Theory, Population, Aerospace Engineering, Magnetosphere, Subsolar point, Astrophysics, Atmospheric sciences, 01 natural sciences, Magnetosheath, 0103 physical sciences, Interplanetary magnetic field, education, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, education.field_of_study, Astronomy and Astrophysics, Magnetic reconnection, Magnetopause, Geophysics, 13. Climate action, Space and Planetary Science, Magnetospheric physics, Physics::Space Physics, General Earth and Planetary Sciences, Cusp (anatomy), Cusp and boundary layers
Abstract: International audience; Double cusps have been observed on a few occasions by polar orbiting spacecraft and ground-based observatories. The four Cluster spacecraft observed two distinct regions, showing characteristics of a double cusp, during a mid-altitude cusp pass on 7 August 2004. The Wind spacecraft detected a southward turning of the Interplanetary Magnetic Field (IMF) at the beginning of the cusp crossings and IMF-Bz stayed negative throughout. Cluster 4 observed a high energy step in the ion precipitation around 1 keV on the equatorward side of the cusp and a dense ion population in the cusp centre. Cluster 1, entering the cusp around 1 min later, observed only a partial ion dispersion with a low energy cutoff reaching 100 eV, together with the dense ion population in the cusp centre. About 9 min later, Cluster 3 entered the cusp and observed full ion dispersion from a few keV down to around 50 eV, together with the dense ion population in the centre of the cusp. The ion flow was directed poleward and eastward in the step/dispersion, whereas in the centre of the cusp the flow was directed poleward and westward. In addition the altitude of the source region of ion injection in the step/dispersion was found 50% larger than in the cusp centre. This event could be explained by the onset of dayside reconnection when the IMF turned southward. The step would be the first signature of component reconnection near the subsolar point, and the injection in the centre of the cusp a result of anti-parallel reconnection in the northern dusk side of the cusp. A three-dimensional magnetohydrodynamic (MHD) simulation is used to display the topology of the magnetic field and locate the sources of the ions during the event.
Published: 2008

192. Signatures of the Primordial Universe from Its Emptiness: Measurement of Baryon Acoustic Oscillations from Minima of the Density Field

Author: Will J. Percival, Ashley J. Ross, Gong-Bo Zhao, Yu Liang, Héctor Gil-Marín, Mariana Vargas-Magaña, Chia-Hsun Chuang, Cheng Zhao, Cameron K. McBride, Charling Tao, Jean-Paul Kneib, Rita Tojeiro, Jeremy L. Tinker, Francisco-Shu Kitaura, Daniel J. Eisenstein, Ariel G. Sánchez, Sergio Rodríguez-Torres, Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, Leibniz-Institut für Astrophysik Potsdam (AIP), Tsinghua University [Beijing] (THU), 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), Instituto de Física Teórica UAM/CSIC (IFT), Universidad Autónoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Universidad Autónoma de Madrid (UAM), Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University-Smithsonian Institution, Institut Lagrange de Paris, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Ecole Polytechnique Fédérale de Lausanne (EPFL), University of Portsmouth, Center for Cosmology & AstroParticle Physics, Ohio State University [Columbus] (OSU), Max-Planck-Institut für Extraterrestrische Physik (MPE), New York University [New York] (NYU), NYU System (NYU), University of St Andrews [Scotland], Universidad Nacional Autónoma de México = National Autonomous University of Mexico (UNAM), Chinese Academy of Sciences [Beijing] (CAS), ANR-11-IDEX-0004,SUPER,Sorbonne Universités à Paris pour l'Enseignement et la Recherche(2011), Universidad Autonoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Universidad Autonoma de Madrid (UAM), Harvard University [Cambridge]-Smithsonian Institution, Sorbonne Université (SU), 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), Universidad Nacional Autónoma de México (UNAM), and UAM. Departamento de Física Teórica
Subjects: Void (astronomy), Cosmology and Gravitation, Density fields, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Observational data, Primordial fluctuations, media_common.quotation_subject, General Physics and Astronomy, FOS: Physical sciences, Disjoint sets, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Acoustic oscillation, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, 010303 astronomy & astrophysics, STFC, QC, Astrophysics::Galaxy Astrophysics, media_common, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Delaunay triangulation, Astronomy, RCUK, Física, Large scale structures, 3rd-DAS, Galaxy, Universe, QC Physics, astro-ph.CO, Halo, Baryon acoustic oscillations, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Sound waves from the primordial fluctuations of the Universe imprinted in the large-scale structure, called baryon acoustic oscillations (BAOs), can be used as standard rulers to measure the scale of the Universe. These oscillations have already been detected in the distribution of galaxies. Here we propose to measure BAOs from the troughs (minima) of the density field. Based on two sets of accurate mock halo catalogues with and without BAOs in the seed initial conditions, we demonstrate that the BAO signal cannot be obtained from the clustering of classical disjoint voids, but it is clearly detected from overlapping voids. The latter represent an estimate of all troughs of the density field. We compute them from the empty circumsphere centers constrained by tetrahedra of galaxies using Delaunay triangulation. Our theoretical models based on an unprecedented large set of detailed simulated void catalogues are remarkably well confirmed by observational data. We use the largest recently publicly available sample of luminous red galaxies from SDSS-III BOSS DR11 to unveil for the first time a > 3σ BAO detection from voids in observations. Since voids are nearly isotropically expanding regions, their centers represent the most quiet places in the Universe, keeping in mind the cosmos origin and providing a new promising window in the analysis of the cosmological large-scale structure from galaxy surveys, Y. L., C. T., and C. Z. acknowledge support from Tsinghua University through a 985 grant, 973 programme 2013CB834906, NSFC Grants No. 11033003 and No. 11173017, Sino French CNRS-CAS International Laboratories LIA Origins, and FCPPL. R. T. thanks the STFC for support. H. G. M. thanks the Labex ILP (Reference No. ANR-10-LABX-63), part of the Idex SUPER, for support, receiving financial state aid managed by the Agence Nationale de la Recherche, as part of the programme Investissements d’avenir under Reference No. ANR-11-IDEX-0004-02. G. Z. is supported by the Strategic Priority Research Program of the Chinese Academy of Sciences Grant No. XDB09000000. The authors are also thankful for the access to computing facilities at Barcelona (MareNostrum), LRZ (Supermuc), AIP (erebos), CCIN2P3 (Quentin Le Boulc’h), and Tsinghua University. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration, including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/ Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University
Published: 2015

193. Solar Wind Charge Exchange X-ray emission from Mercury’s exosphere: Detectability with Bepi Colombo’s MIXS spectrometer

Author: Koutroumpa, Dimitra, Dennerl, Konrad, Leblanc, François, Modolo, Ronan, HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Extraterrestrische Physik (MPE), and Cardon, Catherine
Subjects: Spectrometer MIXS, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], BepiColombo, Astrophysics::High Energy Astrophysical Phenomena, Mercury Planetary Orbiter, MPO, Mercury, Exopshere, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Solar wind interaction, [SDU.ASTR.IM] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Physics::Space Physics, [SDU.ASTR.SR] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astrophysics::Earth and Planetary Astrophysics
Abstract: International audience; We have conducted preliminary hybrid simulations to calculate the Solar Wind Charge Exchange (SWCX) X-ray emission in Mercury’s exosphere. Our results imply that the OVII triplet emission intensity for standard slow solar wind conditions is of the same order as the one predicted by simulations for Mars and measured by Chandra in past observations of Mars. Using an oversimplified detector and observation geometry we explore the detectability of Mercury's SWCX emission by the MIXS spectrometer on board Bepi Colombo’s planetary orbiter (MPO).
Published: 2015

194. The star formation rate cookbook at 1 < z < 3: Extinction-corrected relations for UV and [OII]λ3727 luminosities

Author: Jaron Kurk, G. Rodighiero, Margherita Talia, Alessandro Cimatti, Claudia Maraston, Francesca Pozzi, M. Mignoli, Emanuele Daddi, Lucia Pozzetti, Carlotta Gruppioni, University of Bologna/Università di Bologna, INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), Università degli Studi di Padova = University of Padua (Unipd), 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, Institute of Cosmology and Gravitation (Institute of Cosmology and Gravitation), University of Portsmouth, Max-Planck-Institut für Extraterrestrische Physik (MPE), University of Bologna, Universita degli Studi di Padova, Talia, M., Cimatti, A., Pozzetti, L., Rodighiero, G., Gruppioni, C., Pozzi, F., Daddi, E., Maraston, C., Mignoli, M., Kurk, J., and ITA
Subjects: Luminous infrared galaxy, Physics, galaxies: high-redshift, galaxies: star formation, ultraviolet: galaxies, infrared: galaxies, techniques: spectroscopic, Stellar mass, Star formation, Astronomy and Astrophysics, Astrophysics, Galaxy, Redshift, Spectral line, infrared: galaxies, Space and Planetary Science, galaxies: high-redshift, galaxies: star formation, Galaxies: high-redshift, Galaxies: star formation, Infrared: galaxies, Techniques: spectroscopic, Ultraviolet: galaxies, ultraviolet: galaxies, Emission spectrum, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Equivalent width, techniques: spectroscopic
Abstract: Aims: In this paper we use a well-controlled spectroscopic sample of galaxies at 1 IR) and continuum reddening. Using Spitzer-MIPS and Herschel-PACS data we derive LIR for two-thirds of our sample. The LIR/LUV ratio is used as a probe of effective attenuation (AIRX) to search for correlations with continuum and spectroscopic features in order to derive empirical calibrations to correct UV and [OII]λ3727 luminosities for dust extinction. Results: Through the analyses of the correlations between different dust attenuation probes, a set of relations is provided that allows the recovery of the total unattenuated SFR for star-forming galaxies at 1 IRX and UV continuum slope (β) was tested for our sample and found to be broadly consistent with the literature results at the same redshift, though with a larger dispersion with respect to UV-selected samples. We find a correlation between the rest-frame equivalent width of the [OII]λ3727 line and β, which is the main result of this work. We therefore propose the rest-frame equivalent width of the [OII]λ3727 line as a dust attenuation probe and calibrate it through AIRX, though the assumption of a reddening curve is still needed to derive the actual attenuation towards the [OII]λ3727 line (A[OII]). We tested the issue of differential attenuation towards stellar continuum and nebular emission: our results are in line with the traditional prescription of extra attenuation towards nebular lines. Finally, we use our set of cross-calibrated SFR estimates to look at the relation between SFR and stellar mass. The galaxies in our sample show a close linear relation (σ = 0.3 dex) at all redshifts with a slope ~0.7-0.8, which confirms several previous results. Appendix A is available in electronic form at "http://www.aanda.org/10.1051/0004-6361/201425430/olm"
Published: 2015

195. The population of X-ray supernova remnants in the Large Magellanic Cloud

Author: Matthias Ehle, P. J. Kavanagh, Frank Haberl, Wolfgang Pietsch, R. M. Williams, Sean D Points, Manami Sasaki, P. Maggi, Jochen Greiner, Luke M Bozzetto, Miroslav Filipovic, Georgios Vasilopoulos, You-Hua Chu, John R. Dickel, Max-Planck-Institut für Extraterrestrische Physik (MPE), 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), Eberhard Karls Universität Tübingen = Eberhard Karls University of Tuebingen, Western Sydney University, Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory (NOAO), Academia Sinica, The University of New Mexico [Albuquerque], XMM-Newton Science Operations Centre, European Space Agency (ESA), Ohio State University [Columbus] (OSU), 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), Agence Spatiale Européenne = European Space Agency (ESA), Eberhard Karls Universität Tübingen, and Western Sydney University (UWS)
Subjects: 010504 meteorology & atmospheric sciences, Milky Way, Population, FOS: Physical sciences, Astrophysics, 01 natural sciences, ISM: abundances, supernovae: general, 0103 physical sciences, Magellanic Clouds, education, Large Magellanic Cloud, 010303 astronomy & astrophysics, Galaxy cluster, 0105 earth and related environmental sciences, ISM: supernova remnants, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), education.field_of_study, stars: formation, Star formation, Local Group, Astronomy and Astrophysics, Galaxy, X-rays: ISM, Supernova, Space and Planetary Science, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present a comprehensive X-ray study of the population of supernova remnants (SNRs) in the LMC. Using primarily XMM-Newton, we conduct a systematic spectral analysis of LMC SNRs to gain new insights on their evolution and the interplay with their host galaxy. We combined all the archival XMM observations of the LMC with those of our Very Large Programme survey. We produced X-ray images and spectra of 51 SNRs, out of a list of 59. Using a careful modelling of the background, we consistently analysed all the X-ray spectra and measure temperatures, luminosities, and chemical compositions. We investigated the spatial distribution of SNRs in the LMC and the connection with their environment, characterised by various SFHs. We tentatively typed all LMC SNRs to constrain the ratio of core-collapse to type Ia SN rates in the LMC. We compared the X-ray-derived column densities to HI maps to probe the three-dimensional structure of the LMC. This work provides the first homogeneous catalogue of X-ray spectral properties of LMC SNRs. It offers a complete census of LMC SNRs exhibiting Fe K lines (13% of the sample), or revealing contribution from hot SN ejecta (39%). Abundances in the LMC ISM are found to be 0.2-0.5 solar, with a lower [$\alpha$/Fe] than in the Milky Way. The ratio of CC/type Ia SN in the LMC is $N_{\mathrm{CC}}/N_{\mathrm{Ia}} = 1.35(_{-0.24}^{+0.11})$, lower than in local SN surveys and galaxy clusters. Comparison of X-ray luminosity functions of SNRs in Local Group galaxies reveals an intriguing excess of bright objects in the LMC. We confirm that 30 Doradus and the LMC Bar are offset from the main disc of the LMC, to the far and near sides, respectively. (abridged), Comment: Accepted for publication in Astronomy and Astrophysics. 54 pages, 18 figures, 12 tables. The resolution of the figures has been reduced compared to the journal version; v2: New title, minor text edits; v3: Correct version 2
Published: 2015

196. The evolving star formation rate: M-star relation and sSFR since z similar or equal to 5 from the VUDS spectroscopic survey

Author: Tasca, L. A. M., Le Fevre, O., Hathi, N. P., Schaerer, D., Ilbert, O., Zamorani, G., Lemaux, B. C., Cassata, P., Garilli, B., Le Brun, V., Maccagni, D., Pentericci, L., Thomas, R., Vanzella, E., Zucca, E., Amorín, R., Bardelli, S., Cassara, L. P., Castellano, M., Cimatti, Alessandro, Cucciati, O., Durkalec, A., Fontana, A., Giavalisco, M., Grazian, A., Paltani, S., Ribeiro, B., Scodeggio, M., Sommariva, V., Talia, M., Tresse, L., Vergani, D., Capak, P., Charlot, S., Contini, T., Torre, S., Dunlop, J., Fotopoulou, S., Koekemoer, A., Lopez-Sanjuan, C., Mellier, Y., Pforr, J., Salvato, M., Scoville, N., Taniguchi, Y., Wang, P. W., Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Istituto Nazionale di Astrofisica (INAF), INAF - Osservatorio Astronomico di Roma (OAR), Oncology Institute of Southern Switzerland, INAF - Osservatorio Astronomico di Bologna (OABO), University of Bologna/Università di Bologna, Department of Astronomy [Amherst], University of Massachusetts [Amherst] (UMass Amherst), University of Massachusetts System (UMASS)-University of Massachusetts System (UMASS), ISDC Data Centre for Astrophysics, Université de Genève = University of Geneva (UNIGE), INAF- Milano, INAF - Osservatorio Astrofisico di Arcetri (OAA), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, 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), SUPA, Institute for Astronomy, University of Edinburgh, Aristotle University of Thessaloniki, Space Telescope Science Institute (STSci), Institute of cosmology and gravitation, University of Portsmouth, Max-Planck-Institut für Extraterrestrische Physik (MPE), Excellence Cluster Universe, excellence cluster centre, California Institute of Technology (CALTECH), European Project: 268107,EC:FP7:ERC,ERC-2010-AdG_20100224,EARLY(2011), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), University of Bologna, and University of Geneva [Switzerland]
Subjects: Galaxies: star formation, Galaxies: high-redshift, Galaxies: evolution, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxies: formation, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics
Abstract: International audience; We study the evolution of the star formation rate (SFR) - stellar mass (M-star) relation and specific star formation rate (sSFR) of star-forming galaxies (SFGs) since a redshift z similar or equal to 5.5 using 2435 (4531) galaxies with highly reliable spectroscopic redshifts in the VIMOS Ultra-Deep Survey (VUDS). It is the first time that these relations can be followed over such a large redshift range from a single homogeneously selected sample of galaxies with spectroscopic redshifts. The log(SFR) - log(M-star) relation for SFGs remains roughly linear all the way up to z = 5, but the SFR steadily increases at fixed mass with increasing redshift. We find that for stellar masses M-star \textgreater= 3.2 x 10(9) M-circle dot the SFR increases by a factor of similar to 13 between z = 0.4 and z = 2.3. We extend this relation up to z = 5, finding an additional increase in SFR by a factor of 1.7 from z = 2.3 to z = 4.8 for masses M-star = 1010 M-circle dot. We observe a turn-off in the SFR-M-star relation at the highest mass end up to a redshift z similar to 3.5. We interpret this turn-off as the signature of a strong on-going quenching mechanism and rapid mass growth. The sSFR increases strongly up to z similar to 2, but it grows much less rapidly in 2 \textless z \textless 5. We find that the shape of the sSFR evolution is not well reproduced by cold gas accretion-driven models or the latest hydrodynamical models. Below z similar to 2 these models have a flatter evolution (1+z)(Phi) with Phi = 2-2.25 compared to the data which evolves more rapidly with Phi = 2.8 +/- 0.2. Above z similar to 2, the reverse is happening with the data evolving more slowly with Phi = 1.2 +/- 0.1. The observed sSFR evolution over a large redshift range 0 \textless z \textless 5 and our finding of a non-linear main sequence at high mass both indicate that the evolution of SFR and M-star is not solely driven by gas accretion. The results presented in this paper emphasize the need to invoke a more complex mix of physical processes including major and minor merging to further understand the co-evolution of the SFR and stellar mass growth.
Published: 2015

197. The composite nature of Dust-Obscured Galaxies (DOGs) at z similar to 2-3 in the COSMOS field - I. A far-infrared view

Author: E. Le Floc'h, Dieter Lutz, Nick Scoville, James Mullaney, Benjamin Magnelli, J. A. Calanog, Asantha Cooray, H. J. McCracken, Mara Salvato, Anton M. Koekemoer, Peter Capak, D. B. Sanders, Ezequiel Treister, S. Berta, Karín Menéndez-Delmestre, Isaac Roseboom, Olivier Ilbert, Yoshiaki Taniguchi, L. Riguccini, Seb Oliver, Herve Aussel, J. S. Kartaltepe, Observatório do Valongo/UFRJ [Rio de Janeiro], Universidade Federal do Rio de Janeiro (UFRJ), 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), 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, Max-Planck-Institut für Extraterrestrische Physik (MPE), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, California Institute of Technology (CALTECH), 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), AUTRES, Space Telescope Science Institute (STSci), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Excellence Cluster Universe, excellence cluster centre, 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), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Universidade Federal do Rio de Janeiro [Rio de Janeiro] (UFRJ), Ecosystèmes lagunaires : organisation biologique et fonctionnement (ECOLAG), and 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)
Subjects: Luminous infrared galaxy, Physics, Active galactic nucleus, Opacity, Star formation, Astrophysics::High Energy Astrophysical Phenomena, Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, QB0460, Far infrared, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Spectral energy distribution, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics
Abstract: Dust-Obscured galaxies (DOGs) are bright 24 um-selected sources with extreme obscuration at optical wavelengths. They are typically characterized by a rising power-law continuum of hot dust (T_D ~ 200-1000K) in the near-IR indicating that their mid-IR luminosity is dominated by an an active galactic nucleus (AGN). DOGs with a fainter 24 um flux display a stellar bump in the near-IR and their mid-IR luminosity appears to be mainly powered by dusty star formation. Alternatively, it may be that the mid-IR emission arising from AGN activity is dominant but the torus is sufficiently opaque to make the near-IR emission from the AGN negligible with respect to the emission from the host component. In an effort to characterize the astrophysical nature of the processes responsible for the IR emission in DOGs, this paper exploits Herschel data (PACS + SPIRE) on a sample of 95 DOGs within the COSMOS field. We derive a wealth of far-IR properties (e.g., total IR luminosities; mid-to-far IR colors; dust temperatures and masses) based on SED fitting. Of particular interest are the 24 um-bright DOGs (F_24um > 1mJy). They present bluer far-IR/mid-IR colors than the rest of the sample, unveiling the potential presence of an AGN. The AGN contribution to the total 8-1000 um flux increases as a function of the rest-frame 8 um-luminosity irrespective of the redshift. This confirms that faint DOGs (L_8 um< 10^12 L_sun) are dominated by star-formation while brighter DOGs show a larger contribution from an AGN., Accepted for publication in MNRAS
Published: 2015

198. HIGH-RESOLUTION IMAGING OF PHIBSS z ∼ 2 MAIN-SEQUENCE GALAXIES IN CO J = 1 → 0

Author: Alberto D. Bolatto, N. M. Förster Schreiber, Linda J. Tacconi, Andreas Burkert, David Fisher, Steven R. Warren, Amélie Saintonge, Stijn Wuyts, Achim Weiss, Reinhard Genzel, F. Bournaud, Francoise Combes, Adam Leroy, Santiago García-Burillo, M. C. Cooper, Nicolas Bouché, Amiel Sternberg, Department of Astronomy [College Park], University of Maryland [College Park], University of Maryland System-University of Maryland System, Max Planck Institute for Extraterrestrial Physics (MPE), Max-Planck-Gesellschaft, Max-Planck-Institut für Extraterrestrische Physik (MPE), Departamento de Ciência do Solo, Universidade de São Paulo (USP), Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Chaire Galaxies et cosmologie, Collège de France (CdF (institution)), Observatorio Astronomico Nacional [Madrid] (OAN), Instituto Geografico Nacional (IGN), 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), Institut of Physics - Riga, Latvian Academy of Sciences, École normale supérieure - Paris (ENS Paris)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Universidade de São Paulo = University of São Paulo (USP), École normale supérieure - Paris (ENS-PSL), Collège de France - Chaire Galaxies et cosmologie, Observatorio Astronomico Nacional, Madrid, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), and 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)
Subjects: Physics, [PHYS]Physics [physics], Star formation, Sigma, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Projection (relational algebra), Space and Planetary Science, Brightness temperature, Astrophysics of Galaxies (astro-ph.GA), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Excitation, ComputingMilieux_MISCELLANEOUS, Line (formation)
Abstract: We present Karl G. Jansky Very Large Array observations of the CO J=1-0 transition in a sample of four $z\sim2$ main sequence galaxies. These galaxies are in the blue sequence of star-forming galaxies at their redshift, and are part of the IRAM Plateau de Bure HIgh-$z$ Blue Sequence Survey (PHIBSS) which imaged them in CO J=3-2. Two galaxies are imaged here at high signal-to-noise, allowing determinations of their disk sizes, line profiles, molecular surface densities, and excitation. Using these and published measurements, we show that the CO and optical disks have similar sizes in main-sequence galaxies, and in the galaxy where we can compare CO J=1-0 and J=3-2 sizes we find these are also very similar. Assuming a Galactic CO-to-H$_2$ conversion, we measure surface densities of $\Sigma_{mol}\sim1200$ M$_\odot$pc$^{-2}$ in projection and estimate $\Sigma_{mol}\sim500-900$ M$_\odot$pc$^{-2}$ deprojected. Finally, our data yields velocity-integrated Rayleigh-Jeans brightness temperature line ratios $r_{31}$ that are approximately unity. In addition to the similar disk sizes, the very similar line profiles in J=1-0 and J=3-2 indicate that both transitions sample the same kinematics, implying that their emission is coextensive. We conclude that in these two main sequence galaxies there is no evidence for significant excitation gradients or a large molecular reservoir that is diffuse or cold and not involved in active star-formation. We suggest that $r_{31}$ in very actively star-forming galaxies is likely an indicator of how well mixed the star formation activity and the molecular reservoir are., Comment: To appear in ApJ
Published: 2015

199. Missing baryons traced by the galaxy luminosity density in the large-scale WHIM filaments

Author: Carlo Giocoli, Antti Tamm, E. Branchini, Mauro Roncarelli, Jukka Nevalainen, L. J. Liivamägi, P. Nurmi, Elmo Tempel, Pekka Heinämäki, Enn Saar, A. Finoguenov, M. Bonamente, Tartu Observatory, Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Extraterrestrische Physik (MPE), Nevalainen, J., Tempel, E., Liivamägi, L. J., Branchini, ENZO FRANCO, Roncarelli, M., Giocoli, C., Heinämäki, P., Saar, E., Tamm, A., Finoguenov, A., Nurmi, P., Bonamente, M., Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, 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), Roncarelli, Mauro, and Giocoli, Carlo
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, Warm–hot intergalactic medium, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Cosmology: observation, 01 natural sciences, Luminosity, 0103 physical sciences, Blazar, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Line-of-sight, cosmology: observations, large-scale structure of Universe, intergalactic medium, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astronomy and Astrophysic, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, observations, large-scale structure of Universe, intergalactic medium [cosmology], Baryon, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Halo, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We propose a new approach to the missing baryons problem. Building on the common assumption that the missing baryons are in the form of the Warm Hot Intergalactic Medium (WHIM), we further assumed here that the galaxy luminosity density can be used as a tracer of the WHIM. The latter assumption is supported by our finding of a significant correlation between the WHIM density and the galaxy luminosity density in the hydrodynamical simulations of Cui et al. (2012). We further found that the fraction of the gas mass in the WHIM phase is substantially (by a factor of $\sim$1.6) higher within the large scale galactic filaments, i.e. $\sim$70\%, compared to the average in the full simulation volume of $\sim$0.1\,Gpc$^3$. The relation between the WHIM overdensity and the galaxy luminosity overdensity within the galactic filaments is consistent with linear: $\delta_{\rm whim}\,=\,0.7\,\pm\,0.1\,\times\,\delta_\mathrm{LD}^{0.9 \pm 0.2}$. We applied our procedure to the line of sight to the blazar H2356-309 and found evidence for the WHIM in correspondence of the Sculptor Wall (z $\sim$0.03 and $\log{N_H}$ = $19.9^{+0.1}_{-0.3}$) and Pisces-Cetus superclusters (z $\sim$0.06 and $\log{N_H}$ = $19.7^{+0.2}_{-0.3}$), in agreement with the redshifts and column densities of the X-ray absorbers identified and studied by Fang et al. (2010) and Zappacosta et al. (2010). This agreement indicates that the galaxy luminosity density and galactic filaments are reliable signposts for the WHIM and that our method is robust in estimating the WHIM density. The signal that we detected cannot originate from the halos of the nearby galaxies since they cannot account for the large WHIM column densities that our method and X-ray analysis consistently find in the Sculptor Wall and Pisces-Cetus superclusters., Comment: Accepted for Astronomy & Astrophysics
Published: 2015

200. GRB host galaxies with VLT/X-Shooter: properties at 0.8 < z < 1.3

Author: Valerio D'Elia, H. Flores, Fabrizio Fiore, Thomas Krühler, Francois Hammer, Andreja Gomboc, Silvia Piranomonte, Andrea Rossi, P. D'Avanzo, J. Japelj, Guido Cupani, Stefano Covino, Eliana Palazzi, Francesca Onori, Gianpiero Tagliaferri, Filippo Mannucci, Sofia Randich, Luigi Stella, Sandra Savaglio, S. D. Vergani, P. Goldoni, Elena Pian, INAF - Osservatorio Astronomico di Roma (OAR), Istituto Nazionale di Astrofisica (INAF), Faculty of Mathematics and Physics [Ljubljana] (FMF), University of Ljubljana, 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), Max-Planck-Institut für Extraterrestrische Physik (MPE), INAF - Osservatorio Astronomico di Brera (OAB), 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, Dark Cosmology Centre (DARK), Niels Bohr Institute [Copenhagen] (NBI), Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH)-Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH), INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano (IASF-MI), ETSF, European Theoretical Spectroscopy Facility, PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Osservatorio Astronomico di Brera (OAB), 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), University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU)-Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU), 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), ITA, DEU, and SVN
Subjects: 010504 meteorology & atmospheric sciences, Metallicity, Astrophysics::High Energy Astrophysical Phenomena, Extinction (astronomy), Population, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Physics, [PHYS]Physics [physics], education.field_of_study, Star formation, Astronomy, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Stars, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Gamma-ray burst, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: Long gamma-ray bursts (LGRBs) are associated with the death of massive stars. Their host galaxies therefore represent a unique class of objects tracing star formation across the observable Universe. Indeed, recently accumulated evidence shows that GRB hosts do not differ substantially from general population of galaxies at high (z > 2) redshifts. However, it has been long recognised that the properties of z < 1.5 hosts, compared to general star-forming population, are unusual. To better understand the reasons for the supposed difference in LGRB hosts properties at z < 1.5, we obtained VLT/X- Shooter spectra of six hosts lying in the redshift range of 0.8 < z < 1.3. Some of these hosts have been observed before, yet we still lack well constrained information on their characteristics such as metallicity, dust extinction and star formation rate. We search for emission lines in the VLT/X-Shooter spectra of the hosts and measure their fluxes. We perform a detailed analysis, estimating host average extinction, star-formation rates, metallicities and electron densities where possible. Measured quantities of our hosts are compared to a larger sample of previously observed GRB hosts at z < 2. Star-formation rates and metallicities are measured for all the hosts analyzed in this paper and metallicities are well determined for 4 hosts. The mass-metallicity relation, the fundamental metallicity relation and SFRs derived from our hosts occupy similar parameter space as other host galaxies investigated so-far at the same redshift. We therefore conclude that GRB hosts in our sample support the found discrepancy between the properties of low-redshift GRB hosts and the general population of star- forming galaxies., Comment: 13 pages, 6 figures, accepted for publication in MNRAS
Published: 2015

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