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47 results on '"T. Sadibekova"'

1. GRANDMA observations of advanced LIGO’s and advanced Virgo’s third observational campaign

Author

S Antier, S Agayeva, M Almualla, S Awiphan, A Baransky, K Barynova, S Beradze, M Blažek, M Boër, O Burkhonov, N Christensen, A Coleiro, D Corre, M W Coughlin, H Crisp, T Dietrich, J-G Ducoin, P-A Duverne, G Marchal-Duval, B Gendre, P Gokuldass, H B Eggenstein, L Eymar, P Hello, E J Howell, N Ismailov, D A Kann, S Karpov, A Klotz, N Kochiashvili, C Lachaud, N Leroy, W L Lin, W X Li, M Mašek, J Mo, R Menard, D Morris, K Noysena, N B Orange, M Prouza, R Rattanamala, T Sadibekova, D Saint-Gelais, M Serrau, A Simon, C Stachie, C C Thöne, Y Tillayev, D Turpin, A de Ugarte Postigo, V Vasylenko, Z Vidadi, M Was, X F Wang, J J Zhang, T M Zhang, and X H Zhang

Published
2020
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2. Multiwavelength classification of X-ray selected galaxy cluster candidates using convolutional neural networks

Author

Lukas Burget, C. Garrel, Marguerite Pierre, Nicolas Clerc, Norbert Werner, Matej Kosiba, Alina Khalikova, Sarah Kendrew, Miriam E. Ramos-Ceja, Filip Hroch, Mona Molham, M. Lieu, Bruno Altieri, Elias Koulouridis, T. Sadibekova, L. Faccioli, I. Valtchanov, Evelina R. Gaynullina, Faculty of Science [Brno] (SCI / MUNI), Masaryk University [Brno] (MUNI), European Space Astronomy Centre (ESAC), European Space Agency (ESA), Centre for Astronomy and Particle Theory, University of Nottingham, Institut de recherche en astrophysique et planétologie (IRAP), 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), 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), Space Telescope Science Institute (STSci), Telespazio, Services par satellites, Ulugh Beg Astronomical Institute, Uzbekistan Academy of Sciences, Eötvös Loránd University (ELTE), Hiroshima University, Faculty of Information Technology [Brno] (FIT / BUT), Brno University of Technology [Brno] (BUT), National Observatory of Athens (NOA), National Research Institute of Astronomy and Geophysics [Helwan] (NRIAG), Max Planck Institute for Extraterrestrial Physics (MPE), Max-Planck-Gesellschaft, 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), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), and 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)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Convolutional neural network, 010305 fluids & plasmas, 0103 physical sciences, Cluster (physics), Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Galaxy cluster, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Contextual image classification, business.industry, Astronomy and Astrophysics, Pattern recognition, Digitized Sky Survey, Sample (graphics), Data set, Binary classification, Space and Planetary Science, Artificial intelligence, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, business, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Galaxy clusters appear as extended sources in XMM-Newton images, but not all extended sources are clusters. So, their proper classification requires visual inspection with optical images, which is a slow process with biases that are almost impossible to model. We tackle this problem with a novel approach, using convolutional neural networks (CNNs), a state-of-the-art image classification tool, for automatic classification of galaxy cluster candidates. We train the networks on combined XMM-Newton X-ray observations with their optical counterparts from the all-sky Digitized Sky Survey. Our data set originates from the X-CLASS survey sample of galaxy cluster candidates, selected by a specially developed pipeline, the XAmin, tailored for extended source detection and characterisation. Our data set contains 1 707 galaxy cluster candidates classified by experts. Additionally, we create an official Zooniverse citizen science project, The Hunt for Galaxy Clusters, to probe whether citizen volunteers could help in a challenging task of galaxy cluster visual confirmation. The project contained 1 600 galaxy cluster candidates in total of which 404 overlap with the expert's sample. The networks were trained on expert and Zooniverse data separately. The CNN test sample contains 85 spectroscopically confirmed clusters and 85 non-clusters that appear in both data sets. Our custom network achieved the best performance in the binary classification of clusters and non-clusters, acquiring accuracy of 90 %, averaged after 10 runs. The results of using CNNs on combined X-ray and optical data for galaxy cluster candidate classification are encouraging and there is a lot of potential for future usage and improvements., 14 pages, 10 tables, 16 figures, accepted for publication in MNRAS

Published
2020

3. X-ray properties of the X-CLASS-redMaPPer galaxy cluster sample: the luminosity–temperature relation

Author

T. Sadibekova, Mona Molham, Shahinaz Yousef, Nicolas Clerc, Ali Takey, A. B. Morcos, Z. M. Hayman, Evelina R. Gaynullina, Somak Raychaudhury, M. Lieu, National Research Institute of Astronomy and Geophysics [Helwan] (NRIAG), Institut de recherche en astrophysique et planétologie (IRAP), 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), Hiroshima Astrophysical Science Center, Hiroshima University, 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, Department of Astronomy and Meteorology [Giza], Cairo University, European Space Astronomy Centre (ESAC), European Space Agency (ESA), Inter-University Centre for Astronomy and Astrophysics [Pune] (IUCAA), Ulugh Beg Astronomical Institute, Uzbekistan Academy of Sciences, Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), and Agence Spatiale Européenne = European Space Agency (ESA)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), galaxies: clusters: intracluster medium, Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Luminosity, 0103 physical sciences, Cluster (physics), Range (statistics), 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, Galaxy cluster, media_common, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astronomy and Astrophysics, Radius, Redshift, galaxies: clusters: general, Space and Planetary Science, Sky, X-rays: galaxies: clusters, Cluster sampling, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

This paper presents results of a spectroscopic analysis of the X-CLASS-redMaPPer (XC1-RM) galaxy cluster sample. X-CLASS is a serendipitous search for clusters in the X-ray wavebands based on the XMM-Newton archive, whereas redMaPPer is an optical cluster catalogue derived from the Sloan Digital Sky Survey (SDSS). The present sample comprises 92 X-ray extended sources identified in optical images within 1\arcmin~separation. The area covered by the cluster sample is $\sim$ 27 deg$^{2}$. The clusters span a wide redshift range (0.05 < z < 0.6) and 88 clusters benefit from spectrosopically confirmed redshifts using data from SDSS Data Release 14. We present an automated pipeline to derive the X-ray properties of the clusters in three distinct apertures: R\textsubscript{500} (at fixed mass overdensity), R\textsubscript{fit} (at fixed signal-to-noise ratio), R\textsubscript{300kpc} (fixed physical radius). The sample extends over wide temperature and luminosity ranges: from 1 to 10 keV and from 6$\times$10$^{42}$ to 11$\times$10$^{44}$ erg\,s$^{-1}$, respectively. We investigate the luminosity-temperature (L-T) relation of the XC1-RM sample and find a slope equals to 3.03 $\pm$ 0.26. It is steeper than predicted by self-similar assumptions, in agreement with independent studies. A simplified approach is developed to estimate the amount and impact of selection biases which might be affecting our recovered L-T parameters. The result of this simulation process suggests that the measured L-T relation is biased to a steeper slope and higher normalization., Accepted for publication in MNRAS

Published
2020

4. GRANDMA Observations of ZTF/Fink Transients during Summer 2021

Author

V Aivazyan, M Almualla, S Antier, A Baransky, K Barynova, S Basa, F Bayard, S Beradze, D Berezin, M Blazek, D Boutigny, D Boust, E Broens, O Burkhonov, A Cailleau, N Christensen, D Cejudo, A Coleiro, M W Coughlin, D Datashvili, T Dietrich, F Dolon, J-G Ducoin, P-A Duverne, G Marchal-Duval, C Galdies, L Granier, V Godunova, P Gokuldass, H B Eggenstein, M Freeberg, P Hello, R Inasaridze, E E O Ishida, P Jaquiery, D A Kann, G Kapanadze, S Karpov, R W Kiendrebeogo, A Klotz, R Kneip, N Kochiashvili, W Kou, F Kugel, C Lachaud, S Leonini, A Leroy, N Leroy, A Le Van Su, D Marchais, M Mašek, T Midavaine, A Möller, D Morris, R Natsvlishvili, F Navarete, K Noysena, S Nissanke, K Noonan, N B Orange, J Peloton, A Popowicz, T Pradier, M Prouza, G Raaijmakers, Y Rajabov, M Richmond, Ya Romanyuk, L Rousselot, T Sadibekova, M Serrau, O Sokoliuk, X Song, A Simon, C Stachie, A Taylor, Y Tillayev, D Turpin, M Vardosanidze, J Vlieghe, I Tosta e Melo, X F Wang, J Zhu, Ministerio de Ciencia e Innovación (España), European Commission, Centre National D'Etudes Spatiales (France), Netherlands Organization for Scientific Research, Dutch Research Council, National Natural Science Foundation of China, Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), 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), 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, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), 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), 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 d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS), Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Météo-France, Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique de Clermont (LPC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne (UCA), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Fédérale Toulouse Midi-Pyrénées, Observatoire de Paris - Site de Paris (OP), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Institut Pluridisciplinaire Hubert Curien (IPHC), Université de Strasbourg (UNISTRA)-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), and GRANDMA

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Neutron stars -- Mathematical models, FOS: Physical sciences, Astronomy and Astrophysics, Space telescopes, Neutron stars, Gravitational waves, Space and Planetary Science, Methods: data analysis, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Neutron star mergers
Abstract

Full list of authors: Aivazyan, V; Almualla, M.; Antier, S.; Baransky, A.; Barynova, K.; Basa, S.; Bayard, F.; Beradze, S.; Berezin, D.; Blazek, M.; Boutigny, D.; Boust, D.; Broens, E.; Burkhonov, O.; Cailleau, A.; Christensen, N.; Cejudo, D.; Coleiro, A.; Coughlin, M. W.; Datashvili, D.; Dietrich, T.; Dolon, F.; Ducoin, J-G; Duverne, P-A; Marchal-Duval, G.; Galdies, C.; Granier, L.; Godunova, V; Gokuldass, P.; Eggenstein, H. B.; Freeberg, M.; Hello, P.; Inasaridze, R.; Ishida, E. E. O.; Jaquiery, P.; Kann, D. A.; Kapanadze, G.; Karpov, S.; Kiendrebeogo, R. W.; Klotz, A.; Kneip, R.; Kochiashvili, N.; Kou, W.; Kugel, F.; Lachaud, C.; Leonini, S.; Leroy, A.; Leroy, N.; Su, A. Le Van; Marchais, D.; Midavaine, T.; Moeller, A.; Morris, D.; Natsvlishvili, R.; Navarete, F.; Noysena, K.; Nissanke, S.; Noonan, K.; Orange, N. B.; Peloton, J.; Popowicz, A.; Pradier, T.; Prouza, M.; Raaijmakers, G.; Rajabov, Y.; Richmond, M.; Romanyuk, Ya; Rousselot, L.; Sadibekova, T.; Serrau, M.; Sokoliuk, O.; Song, X.; Simon, A.; Stachie, C.; Taylor, A.; Tillayev, Y.; Turpin, D.; Vardosanidze, M.; Vlieghe, J.; Tosta e Melo, I; Wang, X. F.; Zhu, J., We present our follow-up observations with GRANDMA of transient sources revealed by the Zwicky Transient Facility (ZTF). Over a period of six months, all ZTF alerts were examined in real time by a dedicated science module implemented in the Fink broker, which will be used in filtering of transients discovered by the Vera C. Rubin Observatory. In this article, we present three selection methods to identify kilonova candidates. Out of more than 35 million alerts, a hundred sources have passed our selection criteria. Six were then followed-up by GRANDMA (by both professional and amateur astronomers). The majority were finally classified either as asteroids or as supernovae events. We mobilized 37 telescopes, bringing together a large sample of images, taken under various conditions and quality. To complement the orphan kilonova candidates, we included three additional supernovae alerts to conduct further observations during summer 2021. We demonstrate the importance of the amateur astronomer community that contributed images for scientific analyses of new sources discovered in a magnitude range r′ = 17 − 19 mag. We based our rapid kilonova classification on the decay rate of the optical source that should exceed 0.3 mag d−1. GRANDMA’s follow-up determined the fading rate within 1.5 ± 1.2 d post-discovery, without waiting for further observations from ZTF. No confirmed kilonovae were discovered during our observing campaign. This work will be continued in the coming months in the view of preparing for kilonova searches in the next gravitational-wave observing run O4. © 2022 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society., SA and CL acknowledge the financial support of the Programme National Hautes Energies (PNHE). SA acknowledges the financial support of CNES. SA is grateful for financial support from the Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO) through the VIDI (PI: Nissanke). SA dedicates her contribution to Rayan Ouram, who is a source of inspiration for bravity and humanity for GRANDMA. DT acknowledges the financial support of CNES post-doctoral program. UBAI acknowledges support from the Ministry of Innovative Development through projects FA-Atech-2018-392 and VA-FA-F-2-010. RI acknowledges Shota Rustaveli National Science Foundation (SRNSF) grant No - RF/18-1193. TAROT. has been built with the support of the Institut National des Sciences de l’Univers, CNRS, France. MP, SK, and MM are supported by European Structural and Investment Fund and the Czech Ministry of Education, Youth and Sports (Projects CZ.02.1.01/0.0/0.0/16_013/0001403, CZ.02.1.01/0.0/0.0/18_046/0016007 and CZ.02.1.01/0.0/0.0/15_003/0000437). The FRAM telescope is also supported by the Czech Ministry of Education, Youth and Sports (projects LM2015046, LM2018105, LTT17006). NBO and DM acknowledge financial support from NASA MUREP MIRO award 80NSSC21M0001, NASA EPSCoR award 80NSSC19M0060, and NSF EiR award 1901296. PG acknowledges financial support from NSF EiR award 1901296. DAK acknowledges support from Spanish National Research Project RTI2018-098104-J-I00 (GRBPhot) XW is supported by the National Science Foundation of China (NSFC grants 12033003 and 11633002), the Scholar Program of Beijing Academy of Science and Technology (DZ:BS202002), and the Tencent Xplorer Prize. The work of FN is supported by NOIRLab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The GRANDMA consortium thank the amateur participants to the kilonova-catcher program. The kilonova-catcher program is supported by the IdEx Université de Paris, ANR-18-IDEX-0001. This research made use of the cross-match service provided by CDS, Strasbourg. MC acknowledges support from the National Science Foundation with grant numbers PHY-2010970 and OAC-2117997. GR acknowledges financial support from the Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO) through the Projectruimte and VIDI grants (PI: Nissanke). Thanks to the National Astronomical Research Institute of Thailand (Public Organization), based on observations made with the Thai Robotic Telescope under program ID TRTC08D_005 and TRTC09A_002. S., With funding from the Spanish government through the Severo Ochoa Centre of Excellence accreditation SEV-2017-0709.

Published
2022

5. The first six months of the Advanced LIGO’s and Advanced Virgo’s third observing run with GRANDMA

Author

Jicheng Zhang, M. Boer, C. Delattre, Wenxiong Li, V. Aivazyan, Jérôme Berthier, N. Ismailov, Stéphane Basa, A. de Ugarte Postigo, N. Kochiashvili, M. Blažek, J. C. Chen, A. Cailleau, A. Simon, E. Arbouch, A. Baransky, Christina C. Thöne, Michael W. Coughlin, Bruce Gendre, Frédéric Vachier, Alain Klotz, O. A. Burkhonov, P. Thierry, Jun Mo, Xuhui Han, S. Perrigault, A. Burrell, S. Beradze, S. Antier, P. Fock-Hang, J. Moore, Jun-Jie Wei, Eric Howell, G. Marchal-Duval, D. Corre, Jie Zhang, K. Noysena, M. Vardosanidze, Shengyu Yan, D. Turpin, J. G. Ducoin, R. Inasaridze, J. P. Teng, T. Sadibekova, Patrice Hello, C. Wang, C. Lachaud, R. Marron, Z. Vidadi, S. Alishov, A. Le Van Su, G. Kapanadze, P.-A. Duverne, Xinghan Zhang, H. Crisp, V. Vasylenko, J. M. Bai, B. Chabert, A. Peyrot, R. Natsvlishvili, S. Agayeva, David Coward, P. Lognone, X. F. Wang, N. Leroy, David Alexander Kann, Tim Dietrich, K. Barynova, Alexis Coleiro, L. Eymar, Weili Lin, E. Bertin, B. Cordier, D. Samadov, Yusufjon Tillayev, Nelson Christensen, C. Stachie, 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, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'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 Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, 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), Institut de recherche en astrophysique et planétologie (IRAP), 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), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, 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), Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), GRANDMA, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-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 Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Université Nice Sophia Antipolis (1965 - 2019) (UNS), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université de Toulouse (UT), 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), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Australian Research Council, Ministerio de Economía y Competitividad (España), European Commission, California Institute of Technology, Centre National D'Etudes Spatiales (France), Sorbonne Université, Chinese Academy of Sciences, Agence Nationale de la Recherche (France), and Shota Rustaveli National Science Foundation

Subjects
neutron star: binary, Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, gamma ray: burst, Kilonova, 01 natural sciences, localization, Gravitational waves, stars: neutron, 0103 physical sciences, optical, observational [Methods], Spatial localization, structure, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], LIGO, 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Gravitational wave, gravitational radiation, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, neutron [Stars], Astronomy and Astrophysics, Methods observational, messenger, Neutron star, electromagnetic, VIRGO, gravitational waves, efficiency, Space and Planetary Science, Sky, network, methods: observational, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Gamma-ray burst
Abstract

We present the Global Rapid Advanced Network Devoted to the Multi-messenger Addicts (GRANDMA). The network consists of 21 telescopes with both photometric and spectroscopic facilities. They are connected together thanks to a dedicated infrastructure. The network aims at coordinating the observations of large sky position estimates of transient events to enhance their follow-up and reduce the delay between the initial detection and optical confirmation. The GRANDMA programme mainly focuses on follow-up of gravitational-wave alerts to find and characterize the electromagnetic counterpart during the third observational campaign of the Advanced LIGO and Advanced Virgo detectors. But it allows for follow-up of any transient alerts involving neutrinos or gamma-ray bursts, even those with poor spatial localization. We present the different facilities, tools, and methods we developed for this network and show its efficiency using observations of LIGO/Virgo S190425z, a binary neutron star merger candidate.We furthermore report on allGRANDMAfollow-up observations performed during the first six months of the LIGO-Virgo observational campaign, and we derive constraints on the kilonova properties assuming that the events' locations were imaged by our telescopes. © 2019 The Author(s)., Parts of this research were conducted by the Australian Research Council Centre of Excellence for Gravitational Wave Discovery (OzGrav), through project number CE170100004. EJH acknowledges support from a Australian Research Council DECRA Fellowship (DE170100891). AdUP and CCT acknowledge support from Ramon y Cajal fellowships RyC-2012-09975 and RyC-201209984 and the Spanish Ministry of Economy and Competitiveness through project AYA2017-89384-P. DAK acknowledges support from the Spanish research projectAYA2017-89384-P. MBacknowledges funding as `personal tecnico de apoyo' under fellowship number PTA2016-13192-I. MC is supported by the David and Ellen Lee Postdoctoral Fellowship at the California Institute of Technology. SA is supported by the CNES Postdoctoral Fellowship at Laboratoire AstroParticule et Cosmologie. SA, AC, CL, and RM acknowledge the financial support of the UnivEarthS Labex program at Sorbonne Paris Cite (ANR-10-LABX-0023 and ANR-11-IDEX-0005-02). SA and NL acknowledge the financial support of the Programme National Hautes Energies (PNHE). DT acknowledges the financial support of the Chinese Academy of Sciences (CAS) PIFI post-doctoral fellowship program (program C). UBAI acknowledges support from the Ministry of Innovative Development through projects FA-Atech-2018-392 and VA-FAF-2-010. IRiS has been carried out thanks to the support of the OCEVU Labex (ANR-11-LABX-0060) and the A*MIDEX project (ANR-11-IDEX-0001-02) funded by the 'Investissements d'Avenir' French government program. IRiS and T120 thank all the Observatoire de Haute-Provence staff for the permanent support. SB, NK, RN, and MV acknowledge the Shota Rustaveli National Science Foundation (SRNSF grant No 218070). TAROT has been built with the support of the Institut National des Sciences de l'Univers, CNRS,France. TAROT is funded by theCNESand thanks the help of the technical staff of the Observatoire de Haute Provence, OSU-Pytheas.

Published
2019

6. Understanding X-ray and optical selection of galaxy clusters: A comparison of the XXL and CAMIRA cluster catalogues obtained in the common XXL-HSC SSP area

Author

Keiichi Umetsu, Atsushi J. Nishizawa, L. Chiappetti, Akinari Hamabata, Emanuela Pompei, Bruno Altieri, Elias Koulouridis, P. S. Corasaniti, Paul Giles, Sotiria Fotopoulou, Taizo Okabe, Sinan Aliş, Florian Pacaud, S. Paltani, M. Lieu, C. Garrel, Patrick Valageas, Marguerite Pierre, J. P. Willis, Ben J Maughan, T. Sadibekova, J. Lefevre, Miriam E. Ramos-Ceja, F. Gastaldello, Masamune Oguri, Mauro Sereno, Manolis Plionis, C. Adami, Stefano Ettori, Dominique Eckert, L. Faccioli, Bianca M. Poggianti, Nobuhiro Okabe, Yen-Ting Lin, 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), Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), 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), 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 de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut de Physique Théorique - UMR CNRS 3681 (IPHT), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), 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
[PHYS]Physics [physics], Physics, Brightness, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, media_common.quotation_subject, FOS: Physical sciences, Astronomy and Astrophysics, Cosmological model, Astrophysics, 01 natural sciences, Universe, Space and Planetary Science, Sky, galaxies: clusters: general, 0103 physical sciences, Cluster (physics), clusters: general [galaxies], Cluster sampling, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Galaxy cluster, Selection (genetic algorithm), media_common, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Large samples of galaxy clusters provide knowledge of both astrophysics in the most massive virialised environments and the properties of the cosmological model that defines our Universe. However, an important issue that affects the interpretation of galaxy cluster samples is the role played by the selection waveband and the potential for this to introduce a bias in the physical properties of clusters thus selected. We aim to investigate waveband-dependent selection effects in the identification of galaxy clusters by comparing the X-ray Multi-Mirror (XMM) Ultimate Extra-galactic Survey (XXL) and Subaru Hyper Suprime-Cam (HSC) CAMIRA cluster samples identified from a common 22.6 deg2 sky area. We compare 150 XXL and 270 CAMIRA clusters in a common parameter space defined by X-ray aperture brightness and optical richness. We find that 71/150 XXL clusters are matched to the location of a CAMIRA cluster, the majority of which (67/71) display richness values N>15 that exceed the CAMIRA catalogue richness threshold. We find that 67/270 CAMIRA clusters are matched to the location of an XXL cluster (defined within XXL as an extended X-ray source). Of the unmatched CAMIRA clusters, the majority display low X-ray fluxes consistent with the lack of an XXL counterpart. However, a significant fraction (64/107) CAMIRA clusters that display high X-ray fluxes are not asociated with an extended source in the XXL catalogue. We demonstrate that this disparity arises from a variety of effects including the morphological criteria employed to identify X-ray clusters and the properties of the XMM PSF., 15 pages, 14 figures, MNRAS accepted

Published
2021

7. GRANDMA observations of advanced LIGO's and advanced Virgo's third observational campaign

Author

David Alexander Kann, Bruce Gendre, Tim Dietrich, A. Baransky, N. Ismailov, Christina C. Thöne, Z. Vidadi, Yusufjon Tillayev, Nelson Christensen, V. Vasylenko, P. Gokuldass, Weili Lin, C. Stachie, R. Menard, D. Turpin, Jun Mo, D. Corre, D. Morris, J.-G. Ducoin, A. de Ugarte Postigo, C. Lachaud, H. Crisp, Supachai Awiphan, M. Was, K. Barynova, S. Antier, L. Eymar, G. Marchal-Duval, N. Leroy, N. B. Orange, O. A. Burkhonov, Jie Zhang, R. Rattanamala, M. Serrau, Wenxiong Li, S. Beradze, Sergey Karpov, K. Noysena, M. Boer, X. F. Wang, T. Zhang, Patrice Hello, Mouza Almualla, D. Saint-Gelais, Xinghan Zhang, Heinz-Bernd Eggenstein, Alain Klotz, S. Agayeva, M. Prouza, T. Sadibekova, N. Kochiashvili, Eric Howell, M. Blažek, Martin Mašek, P. A. Duverne, A. Simon, Michael W. Coughlin, Alexis Coleiro, Australian Research Council, Ministerio de Economía y Competitividad (España), European Commission, Centre National de la Recherche Scientifique (France), Centre National D'Etudes Spatiales (France), Ministry of Education, Youth and Sports (Czech Republic), Shota Rustaveli National Science Foundation, National Aeronautics and Space Administration (US), 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, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), 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), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-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), Université de Toulouse (UT), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), ANR-18-IDEX-0001,Université de Paris,Université de Paris(2018), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Université Nice Sophia Antipolis (... - 2019) (UNS), 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), Université Fédérale Toulouse Midi-Pyrénées, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), and 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)

Subjects
observational [methods], Binary number, FOS: Physical sciences, Kilonova, 01 natural sciences, Gravitational waves, stars: neutron, neutron [stars], 0103 physical sciences, 010306 general physics, Large distance, 010303 astronomy & astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Gravitational wave, Astronomy, Astronomy and Astrophysics, Methods observational, LIGO, Neutron star, gravitational waves, Space and Planetary Science, Observational study, methods: observational, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

Full list of authors: Antier, S.; Agayeva, S.; Almualla, M.; Awiphan, S.; Baransky, A.; Barynova, K.; Beradze, S.; Blažek, M.; Boër, M.; Burkhonov, O.; Christensen, N.; Coleiro, A.; Corre, D.; Coughlin, M. W.; Crisp, H.; Dietrich, T.; Ducoin, J. -G.; Duverne, P. -A.; Marchal-Duval, G.; Gendre, B.; Gokuldass, P.; Eggenstein, H. B.; Eymar, L.; Hello, P.; Howell, E. J.; Ismailov, N.; Kann, D. A.; Karpov, S.; Klotz, A.; Kochiashvili, N.; Lachaud, C.; Leroy, N.; Lin, W. L.; Li, W. X.; Mašek, M.; Mo, J.; Menard, R.; Morris, D.; Noysena, K.; Orange, N. B.; Prouza, M.; Rattanamala, R.; Sadibekova, T.; Saint-Gelais, D.; Serrau, M.; Simon, A.; Stachie, C.; Thöne, C. C.; Tillayev, Y.; Turpin, D.; de Ugarte Postigo, A.; Vasylenko, V.; Vidadi, Z.; Was, M.; Wang, X. F.; Zhang, J. J.; Zhang, T. M.; Zhang, X. H., GRANDMA (Global Rapid Advanced Network Devoted to the Multi-messenger Addicts) is a network of 25 telescopes of different sizes, including both photometric and spectroscopic facilities. The network aims to coordinate follow-up observations of gravitational-wave (GW) candidate alerts, especially those with large localization uncertainties, to reduce the delay between the initial detection and the optical confirmation. In this paper, we detail GRANDMA's observational performance during Advanced LIGO/Advanced Virgo Observing Run 3 (O3), focusing on the second part of O3; this includes summary statistics pertaining to coverage and possible astrophysical origin of the candidates. To do so, we quantify our observation efficiency in terms of delay between GW candidate trigger time, observations, and the total coverage. Using an optimized and robust coordination system, GRANDMA followed-up about 90 per cent of the GW candidate alerts, that is 49 out of 56 candidates. This led to coverage of over 9000 deg2 during O3. The delay between the GW candidate trigger and the first observation was below 1.5 h for 50 per cent of the alerts. We did not detect any electromagnetic counterparts to the GW candidates during O3, likely due to the very large localization areas (on average thousands of degrees squares) and relatively large distance of the candidates (above 200 Mpc for 60 per cent of binary neutron star, BNS candidates). We derive constraints on potential kilonova properties for two potential BNS coalescences (GW190425 and S200213t), assuming that the events' locations were imaged. © 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society., Parts of this research were conducted by the Australian Research Council Centre of Excellence for Gravitational Wave Discovery (OzGrav), through project number CE170100004. EJH acknowledges support from an Australian Research Council DECRA Fellowship (DE170100891). AdUP and CCT acknowledge support from Ramon y Cajal fellowships RyC-2012-09975 and RyC-2012-09984 and the Spanish Ministry of Economy and Competitiveness through project AYA2017-89384-P. DAK acknowledges Spanish research project RTI2018-098104-J-I00 (GRBPhot). MB acknowledges funding as 'personal tecnico de apoyo' under fellowship number PTA2016-13192-I. SA is supported by the CNES Postdoctoral Fellowship at Laboratoire AstroParticule et Cosmologie. SA and CL acknowledge the financial support of the Programme National Hautes Energies (PNHE). DT acknowledges the financial support of CNES postdoctoral program. UBAI acknowledges support from the Ministry of Innovative Development through projects FA-Atech-2018-392 and VA-FA-F-2-010. SB acknowledges Shota Rustaveli National Science Foundation (SRNSF) grant no. -PHDF/18-1327. TAROT has been built with the support of the Institut National des Sciences de l'Univers, CNRS, France. TAROT is funded by the CNES and thanks the help of the technical staff of the Observatoire de Haute Provence, OSUPytheas. MP, SK, and MM are supported by European Structural and Investment Fund and the Czech Ministry of Education, Youth and Sports (Projects CZ.02.1.01/0.0/0.0/16 013/0001402, CZ.02.1.01/0.0/0.0/16 013/0001403, and CZ.02.1.01/0.0/0.0/15 003/0000437). NBO, DM, and PG acknowledge financial support from NASA-MUREP-MIRO grant NNX15AP95A, NASA-EPSCoR grant NNX13AD28A, and NSF EiR AST Award 1901296. The GRANDMA collaboration thank the amateur participants to the kilonova-catcher program. The kilonova-catcher program is supported by the IdEx Universite de Paris, ANR-18-IDEX-0001. This research made use of the crossmatch service provided by CDS, Strasbourg. We thank Ulrich Hopp to provide the precise date of observations for AT2019wxt Wendelstein optical observations.

Published
2020

8. The XXL survey: First results and future

Author

M. Pierre, C. Adami, M. Birkinshaw, L. Chiappetti, S. Ettori, A. Evrard, L. Faccioli, F. Gastaldello, P. Giles, C. Horellou, A. Iovino, E. Koulouridis, C. Lidman, A. Le Brun, B. Maughan, S. Maurogordato, I. McCarthy, S. Miyazaki, F. Pacaud, S. Paltani, M. Plionis, T. Reiprich, T. Sadibekova, V. Smolcic, S. Snowden, J. Surdej, M. Tsirou, C. Vignali, J. Willis, S. Alis, B. Altieri, N. Baran, C. Benoist, A. Bongiorno, M. Bremer, A. Butler, A. Cappi, C. Caretta, P. Ciliegi, N. Clerc, P. S. Corasaniti, J. Coupon, J. Delhaize, I. Delvecchio, J. Democles, Sh. Desai, J. Devriendt, Y. Dubois, D. Eckert, A. Elyiv, A. Farahi, C. Ferraril, S. Fotopoulou, W. Forman, I. Georgantopoulos, V. Guglielmo, M. Huynh, N. Jerlin, Ch. Jones, S. Lavoie, J.-P. Le Fevre, M. Lieu, M. Kilbinger, F. MaruIli, A. Mantz, S. McGee, J.-B. Melin, O. Melnyk, L. Moscardini, M. Novak, E. Piconcelli, B. Poggianti, D. Pomarede, E. Pompei, T. Ponman, M. E. Ramos Ceja, P. Rana, D. Rapetti, S. Raychaudhury, M. Ricci, H. Rottgering, M. Sahlen, J.-L. Sauvageot, C. Schimd, M. Sereno, G.P. Smith, K. Umetsu, P. Valageas, A. Valotti, I. Valtchanov, A. Veropalumbo, B. Ascaso, D. Barnes, M. De Petris, F. Durret, M. Donahue, M. Ithana, M. Jarvis, M. Johnston-Hollitt, E. Kalfountzou, S. Kay, F. La Franca, N. Okabe, A. Muzzin, A. Rettura, F. Ricci, J. Ridl, G. Risaliti, M. Takizawa, P. Thomas, and N. Truong

Subjects
Physics, 010308 nuclear & particles physics, Space and Planetary Science, 0103 physical sciences, Astronomy and Astrophysics, Astrophysics, 010303 astronomy & astrophysics, 01 natural sciences
Abstract

The XXL survey currently covers two 25 sq. deg. patches with XMM observations of ~10ks. We summarise the scientific results associated with the first release of the XXL data set, that occurred mid 2016. We review several arguments for increasing the survey depth to 40 ks during the next decade of XMM operations. X-ray (z 1 cluster density. It will eventually constitute a reference study and an ideal calibration field for the upcoming eROSITA and Euclid missions.

Published
2017

9. The XXL Survey : XXVII. The 3XLSS point source catalogue

Author

Ivan Valtchanov, Michael J. I. Brown, P. Franzetti, E. Elmer, Bruno Altieri, Sinan Aliş, Matt S. Owers, Maria del Carmen Polletta, Bianca M. Poggianti, Ivan K. Baldry, Trevor J. Ponman, Meiert W. Grootes, C. Adami, T. Sadibekova, Angela Bongiorno, Elias Koulouridis, Stéphane Paltani, Florian Pacaud, Christopher Lidman, Manolis Plionis, Jochen Liske, Cristian Vignali, Sotiria Fotopoulou, Glenn Wagner, V. Guglielmo, Simon P. Driver, O. Melnyk, Richard J. Tuffs, Marguerite Pierre, L. Chiappetti, Sophie Maurogordato, A. Iovino, M. Bolzonella, Andrii Elyiv, J. P. Lefevre, L. Faccioli, Aaron S. G. Robotham, E. Pompei, University of St Andrews. School of Physics and Astronomy, 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)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), 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), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), 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), 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, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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), Chiappetti, L., Fotopoulou, S., Lidman, C., Faccioli, L., Pacaud, F., Elyiv, A., Paltani, S., Pierre, M., Plionis, M., Adami, C., Alis, S., Altieri, B., Baldry, I., Bolzonella, M., Bongiorno, A., Brown, M., Driver, S., Elmer, E., Franzetti, P., Grootes, M., Guglielmo, V., Iovino, A., Koulouridis, E., Lefèvre, J.P., Liske, J., Maurogordato, S., Melnyk, O., Owers, M., Poggianti, B., Polletta, M., Pompei, E., Ponman, T., Robotham, A., Sadibekova, T., Tuffs, R., Valtchanov, I., Vignali, C., and Wagner, G.

Subjects
Point source, FOS: Physical sciences, Astrophysics, Surveys, X-rays: general, 01 natural sciences, surveys, general [X-rays], 0103 physical sciences, QB Astronomy, Survey, 010303 astronomy & astrophysics, QC, QB, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Astronomy and Astrophysics, DAS, Astronomy and Astrophysic, Astrophysics - Astrophysics of Galaxies, Redshift, NATURAL SCIENCES. Physics, PRIRODNE ZNANOSTI. Fizika, catalogs, QC Physics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Catalog, Catalogs, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

We present the version of the point source catalogue of the XXL Survey that was used, in part, in the first series of XXL papers. In this paper we release, in our database in Milan and at CDS: (i) the X-ray source catalogue with 26056 objects in two areas of 25 deg2; (ii) the associated multiwavelength catalogues with candidate counterparts of the X-ray sources in the infrared, near-infrared, optical, and ultraviolet (plus spectroscopic redshift when available); and (iii) a catalogue of spectroscopic redshifts recently obtained in the southern XXL area. We also present the basic properties of the X-ray point sources and their counterparts. Other catalogues described in the second series of XXL papers will be released contextually, and will constitute the second XXL data release., Comment: 19 pages, 11 figures, part of A&A Special Issue "The XXL Survey: second series" https://www.aanda.org/component/toc/?task=topic&id=927

Published
2018

10. The XXL Survey

Author

F. Gastaldello, Matt J. Jarvis, J. P. Le Fevre, C. Adami, B. Häußler, Keiichi Umetsu, Bianca M. Poggianti, Florian Pacaud, Elias Koulouridis, L. Faccioli, J. L. Willis, Stefano Ettori, T. Sadibekova, A. Trudeau, N. J. Adams, C. Garrel, Marguerite Pierre, Rebecca A. A. Bowler, L. Chiappetti, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire 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 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)), and 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)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, Population, 85A99, FOS: Physical sciences, Context (language use), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Luminosity, galaxies: high-redshift, 0103 physical sciences, Cluster (physics), Galaxy formation and evolution, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Galaxy cluster, media_common, Physics, education.field_of_study, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, galaxies: photometry, galaxies: clusters: general, Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA), X-rays: galaxies: clusters, galaxies: distances and redshifts, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Context. Distant galaxy clusters provide an effective laboratory in which to study galaxy evolution in dense environments and at early cosmic times. Aims. We aim to identify distant galaxy clusters as extended X-ray sources coincident with overdensities of characteristically bright galaxies. Methods. We use optical and near-infrared (NIR) data from the Hyper Suprime-Cam (HSC) and VISTA Deep Extragalactic Observations (VIDEO) surveys to identify distant galaxy clusters as overdensities of bright, $z_{phot}\geq 0.8$ galaxies associated with extended X-ray sources detected in the ultimate XMM extragalactic survey (XXL). Results. We identify a sample of 35 candidate clusters at $0.80\leq z\leq 1.93$ from an approximately 4.5 deg$^2$ sky area. This sample includes 15 newly discovered candidate clusters, ten previously detected but unconfirmed clusters, and ten spectroscopically confirmed clusters. Although these clusters host galaxy populations that display a wide variety of quenching levels, they exhibit well-defined relations between quenching, cluster-centric distance, and galaxy luminosity. The brightest cluster galaxies (BCGs) within our sample display colours consistent with a bimodal population composed of an old and red subsample together with a bluer, more diverse subsample. Conclusions. The relation between galaxy masses and quenching seem to be already in place at $z\sim 1$, although there is no significant variation of the quenching fraction with the cluster-centric radius. The BCG bimodality might be explained by the presence of a younger stellar component in some BCGs but additional data are needed to confirm this scenario., Comment: 27 pages, 15 figures, accepted in A&A

Published
2020

11. The XXL Survey: XVI. The clustering of X-ray selected galaxy clusters at z~0.3

Author

Fabio Gastaldello, Sinan Aliş, Bruno Altieri, Alfonso Veropalumbo, Mark Birkinshaw, J. P. Le Fevre, Lauro Moscardini, Bianca M. Poggianti, Elias Koulouridis, L. Faccioli, Stefano Ettori, E. Pompei, Federico Marulli, Mauro Sereno, Sophie Maurogordato, C. Adami, T. Sadibekova, M. Pierre, Ivan Valtchanov, Florian Pacaud, A. Cappi, Christopher Lidman, Manolis Plionis, 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 (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), 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), 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), CEA/DSM, 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 Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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), 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), Marulli, F., Veropalumbo, A., Sereno, M., Moscardini, L., Pacaud, F., Pierre, M., Plionis, M., Cappi, A., Adami, C., Alis, S., Altieri, B., Birkinshaw, M., Ettori, S., Faccioli, L., Gastaldello, F., Koulouridis, E., Lidman, C., Le Fèvre, J.-P., Maurogordato, S., Poggianti, B., Pompei, E., Sadibekova, T., and Valtchanov, I.

Subjects
Cosmological parameter, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Large-scale structure of Universe, Cosmological parameters, Dark matter, FOS: Physical sciences, Context (language use), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Cosmology: observation, 01 natural sciences, 0103 physical sciences, Cluster (physics), cosmological parameters, observations [Cosmology], Cluster analysis, 010303 astronomy & astrophysics, Galaxy cluster, Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astronomy and Astrophysic, X-rays: galaxies: cluster, Redshift, Determining the number of clusters in a data set, Space and Planetary Science, X-rays: galaxies: clusters, cosmology: observations, Cluster sampling, galaxies: clusters [X-rays], large-scale structure of Universe, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Galaxy clusters trace the highest density peaks in the large-scale structure of the Universe. Their clustering provides a powerful probe that can be exploited in combination with cluster mass measurements to strengthen the cosmological constraints provided by cluster number counts. We investigate the spatial properties of a homogeneous sample of X-ray selected galaxy clusters from the XXL survey, the largest programme carried out by the XMM-Newton satellite. The measurements are compared to $\Lambda$-cold dark matter predictions, and used in combination with self-calibrated mass scaling relations to constrain the effective bias of the sample, $b_{eff}$, and the matter density contrast, $\Omega_{\rm M}$. We measured the angle-averaged two-point correlation function of the XXL cluster sample. The analysed catalogue consists of $182$ X-ray selected clusters from the XXL second data release, with median redshift $\langle z \rangle=0.317$ and median mass $\langle M_{500} \rangle\simeq1.3\cdot10^{14} M_\odot$. A Markov chain Monte Carlo analysis is performed to extract cosmological constraints using a likelihood function constructed to be independent of the cluster selection function. Modelling the redshift-space clustering in the scale range $10, Comment: 10 pages, 10 figures. Accepted for publication in Astronomy & Astrophysics

Published
2018

12. The XXL Survey. XXX. Characterisation of the XLSSsC N01 supercluster and analysis of the galaxy stellar populations

Author

August E. Evrard, Angela Bongiorno, Cathy Horellou, Mark Birkinshaw, Elias Koulouridis, Andrii Elyiv, R. J. Tuffs, Sophie Maurogordato, A. Iovino, Fabio Gastaldello, L. Guennou, Aaron S. G. Robotham, Florian Pacaud, Paul Giles, M. E. Ramos Ceja, Jacopo Fritz, Stéphane Paltani, Vernesa Smolčić, T. Sadibekova, Matt S. Owers, Cristian Vignali, Marguerite Pierre, J. Willis, V. Guglielmo, Bianca M. Poggianti, César A. Caretta, Ivan K. Baldry, Andrew M. Hopkins, Trevor J. Ponman, Meiert W. Grootes, Michael J. I. Brown, Manolis Plionis, C. Adami, L. Chiappetti, Alberto Moretti, Benedetta Vulcani, Simon P. Driver, University of St Andrews. School of Physics and Astronomy, Guglielmo, V., Poggianti, B.M., Vulcani, B., Moretti, A., Fritz, J., Gastaldello, F., Adami, C., Caretta, C.A., Willis, J., Koulouridis, E., Ramos Ceja, M.E., Giles, P., Baldry, I., Birkinshaw, M., Bongiorno, A., Brown, M., Chiappetti, L., Driver, S., Elyiv, A., Evrard, A., Grootes, M., Guennou, L., Hopkins, A., Horellou, C., Iovino, A., Maurogordato, S., Owers, M., Pacaud, F., Paltani, S., Pierre, M., Plionis, M., Ponman, T., Robotham, A., Sadibekova, T., Smolčić, V., Tuffs, R., and Vignali, C.

Subjects
PRIRODNE ZNANOSTI. Fizika. Astronomija i astrofizika, Stellar population, FOS: Physical sciences, Perturbation (astronomy), large-scale structure of Universe, X-rays: galaxies: clusters, galaxies: groups: general, galaxies: evolution, galaxies: star formation, galaxies: stellar content, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, star formation [Galaxies], Virial theorem, Supercluster, Large-scale structure of the universe, 0103 physical sciences, Cluster (physics), NATURAL SCIENCES. Physics. Astronomy and Astrophysics, QB Astronomy, 010303 astronomy & astrophysics, QC, Astrophysics::Galaxy Astrophysics, QB, Physics, 85A04, 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, 3rd-DAS, evolution [Galaxies], Astrophysics - Astrophysics of Galaxies, Galaxy, groups: general [Galaxies], QC Physics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Spectral energy distribution, stellar content [Galaxies], galaxies: clusters [X-rays]
Abstract

Superclusters form from the largest enhancements in the primordial density perturbation field and extend for tens of Mpc, tracing the large-scale structure of the Universe. We characterise XLSSsCN01, a rich supercluster at z~0.3 detected in the XXL Survey, composed of X-ray clusters of different virial masses and luminosities. As one of the first studies on this topic, we investigate the stellar populations of galaxies in different environments in the supercluster region. We study a magnitude-limited (r10.8) of galaxies in the virialised region and in the outskirts of 11 XLSSsCN01 clusters, in high- and low-density field. We compute the stellar population properties of galaxies using spectral energy distribution and spectral fitting techniques, and study the dependence of star formation rates (SFR), colours, and stellar ages on environment. For r-12 and with (g-r)_rf10.8, no trends with environment emerge, as massive galaxies are mostly already passive in all environments. No differences among low- and high-density field members and cluster members emerge in the sSFR-mass relation. The luminosity-weighted age-mass relation of the passive populations within cluster virial radii show signatures of recent environmental quenching. The study of luminous and massive galaxies in this supercluster shows that while environment has a prominent role in determining the fractions of SFing/blue galaxies, its effects on the star formation activity in SFing galaxies are negligible., 16 pages, 10 figures, 2 tables, accepted for publication in A&A

Published
2018

13. The XXL Survey: XXV. Cosmological analysis of the C1 cluster number counts

Author

C. Adami, T. Sadibekova, Florian Pacaud, C. Lidman, Sinan Aliş, Jon Willis, Bruno Altieri, Mark Birkinshaw, J. P. Le Fevre, Mauro Sereno, Lauro Moscardini, Bianca M. Poggianti, Sophie Maurogordato, F. Gastaldello, Manolis Plionis, A. Iovino, I. Valtchanov, Paul Giles, S. Galli, Jean-Baptiste Melin, M. Lieu, Marguerite Pierre, L. Faccioli, Ben J Maughan, August E. Evrard, L. Chiappetti, Emanuela Pompei, Cathy Horellou, Elias Koulouridis, 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), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Observatoire de la Côte d'Azur (OCA), Centre National de la Recherche Scientifique (CNRS), XXL, 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 national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), 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), Pacaud, F., Pierre, M., Melin, J.-B., Adami, C., Evrard, A.E., Galli, S., Gastaldello, F., Maughan, B.J., Sereno, M., Alis, S., Altieri, B., Birkinshaw, M., Chiappetti, L., Faccioli, L., Giles, P.A., Horellou, C., Iovino, A., Koulouridis, E., Le Fèvre, J.-P., Lidman, C., Lieu, M., Maurogordato, S., Moscardini, L., Plionis, M., Poggianti, B.M., Pompei, E., Sadibekova, T., Valtchanov, I., Willis, J.P., 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
Cosmological parameter, Cold dark matter, Cosmology and Nongalactic Astrophysics (astro-ph.CO), galaxies: clusters: intracluster medium, Large-scale structure of Universe, Cosmic microwave background, Cosmological parameters, FOS: Physical sciences, Context (language use), Astrophysics, clusters: intracluster medium [Galaxies], Astrophysics::Cosmology and Extragalactic Astrophysics, Surveys, 01 natural sciences, Cosmology, symbols.namesake, surveys, 0103 physical sciences, Planck, cosmological parameters, Survey, 010303 astronomy & astrophysics, Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astronomy and Astrophysic, X-rays: galaxies: cluster, Redshift, Galaxy, Space and Planetary Science, X-rays: galaxies: clusters, symbols, 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. We present an estimation of cosmological parameters with clusters of galaxies. Aims. We constrain the $\Omega_m$, $\sigma_8$, and $w$ parameters from a stand-alone sample of X-ray clusters detected in the 50 deg$^2$ XMM-XXL survey with a well-defined selection function. Methods. We analyse the redshift distribution of a sample comprising 178 high S/N clusters out to a redshift of unity. The cluster sample scaling relations are determined in a self-consistent manner. Results. In a lambda cold dark matter ($\Lambda$CDM) model, the cosmology favoured by the XXL clusters compares well with results derived from the Planck S-Z clusters for a totally different sample (mass/redshift range, selection biases, and scaling relations). However, with this preliminary sample and current mass calibration uncertainty, we find no inconsistency with the Planck CMB cosmology. If we relax the $w$ parameter, the Planck CMB uncertainties increase by a factor of $\sim$10 and become comparable with those from XXL clusters. Combining the two probes allows us to put constraints on $\Omega_m$=0.316$\pm$0.060, $\sigma_8$=0.814$\pm$0.054, and $w$=-1.02$\pm$0.20. Conclusions. This first self-consistent cosmological analysis of a sample of serendipitous XMM clusters already provides interesting insights into the constraining power of the XXL survey. Subsequent analysis will use a larger sample extending to lower confidence detections and include additional observable information, potentially improving posterior uncertainties by roughly a factor of 3., Comment: 11 pages, 5 figures, 5 tables, accepted as a letter by Astronomy & Astrophysics

Published
2018

14. Cosmology with XMM galaxy clusters: the X-CLASS/GROND catalogue and photometric redshifts

Author

Florian Pacaud, H. Steinle, Nicolas Clerc, Thomas Krühler, T. Sadibekova, Mara Salvato, Jochen Greiner, L. Faccioli, M. L. Menzel, Kirpal Nandra, Arne Rau, Jeremy S. Sanders, P. Wiseman, J. Ridl, 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)-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 (UMR7158 / UMR_E_9005 / UM_112)), Laboratoire AIM, and Université Paris Diderot - Paris 7 ( UPD7 ) -Centre d'Etudes de Saclay

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmology, Luminosity, law.invention, Telescope, techniques: photometric, Observatory, law, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 10. No inequality, 010303 astronomy & astrophysics, Galaxy cluster, catalogues, Astrophysics::Galaxy Astrophysics, Photometric redshift, media_common, Physics, 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Redshift, Space and Planetary Science, Sky, galaxies: clusters: general, cosmology: observations, X-rays: galaxies: clusters, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics, large-scale structure of Universe, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The XMM Cluster Archive Super Survey (X-CLASS) is a serendipitously-detected X-ray-selected sample of 845 galaxy clusters based on 2774 XMM archival observations and covering approximately 90 deg$^2$ spread across the high-Galactic latitude ($|b|>20$ deg) sky. The primary goal of this survey is to produce a well-selected sample of galaxy clusters on which cosmological analyses can be performed. This article presents the photometric redshift followup of a high signal-to-noise subset of 266 of these clusters with declination $\delta, Comment: Accepted for publication in MNRAS. 26 pages, 14 figures. Catalogue information available on request to the authors pending a digital version (see in paper)

Published
2017
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15. The XXL Survey

Author

Paul Giles, Cathy Horellou, Stefano Ettori, Elias Koulouridis, C. Lidman, V. Smolvcic, Mark Birkinshaw, C. Adami, M. Bolzonella, S. Paltani, T. Sadibekova, Matt S. Owers, R. J. Tuffs, Florian Pacaud, L. Chiappetti, B. Garilli, L. Guennou, S. Maurogordato, Jochen Liske, Andrii Elyiv, Trevor J. Ponman, Meiert W. Grootes, A. Iovino, M. E. Ramos Ceja, Mauro Sereno, Michael J. I. Brown, Sean L. McGee, J. L. Willis, Bruno Altieri, I. Valtchanov, Andrew M. Hopkins, Ivan K. Baldry, Angela Bongiorno, S. Fotoupoulou, Aaron S. G. Robotham, Bianca M. Poggianti, V. Guglielmo, Cristian Vignali, Simon P. Driver, August E. Evrard, Fabio Gastaldello, Benedetta Vulcani, M. Plionis, Marco Scodeggio, Marguerite Pierre, University of St Andrews. School of Physics and Astronomy, Guglielmo, V., Poggianti, B.M., Vulcani, B., Adami, C., Gastaldello, F., Ettori, S., Fotoupoulou, S., Koulouridis, E., Ramos Ceja, M.E., Giles, P., McGee, S., Altieri, B., Baldry, I., Birkinshaw, M., Bolzonella, M., Bongiorno, A., Brown, M., Chiappetti, L., Driver, S., Elyiv, A., Evrard, A., Garilli, B., Grootes, M., Guennou, L., Hopkins, A., Horellou, C., Iovino, A., Lidman, C., Liske, J., Maurogordato, S., Owers, M., Pacaud, F., Paltani, S., Pierre, M., Plionis, M., Ponman, T., Robotham, A., Sadibekova, T., Scodeggio, M., Sereno, M., Smolčić, V., Tuffs, R., Valtchanov, I., Vignali, C., Willis, J., Laboratoire d'Astrophysique de Marseille (LAM), and 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)

Subjects
luminosity function, mass function [Galaxies], Stellar mass, astro-ph.GA, FOS: Physical sciences, Astrophysics, clusters: general [Galaxies], 01 natural sciences, Virial theorem, galaxies: groups: general, 0103 physical sciences, QB Astronomy, Infrarot-Astrophysik - Abteilung Hinton, 010303 astronomy & astrophysics, QC, luminosity function [galaxies], QB, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 85A04, 010308 nuclear & particles physics, X-ray, DAS, Astronomy and Astrophysics, Virial mass, evolution [Galaxies], Astrophysics - Astrophysics of Galaxies, NATURAL SCIENCES. Physics, Redshift, Galaxy, PRIRODNE ZNANOSTI. Fizika, galaxies: luminosity function, groups: general [Galaxies], QC Physics, [SDU]Sciences of the Universe [physics], galaxies: clusters: general, mass function, Space and Planetary Science, Homogeneous, Astrophysics of Galaxies (astro-ph.GA), X-rays: galaxies: clusters, galaxies: luminosity function, mass function, galaxies: clusters [X-rays], Halo, galaxies: evolution
Abstract

The fraction of galaxies bound in groups in the nearby Universe is high (50% at z~0). Systematic studies of galaxy properties in groups are important in order to improve our understanding of the evolution of galaxies and of the physical phenomena occurring within this environment. We have built a complete spectrophotometric sample of galaxies within X-ray detected, optically spectroscopically confirmed groups and clusters (G&C), covering a wide range of halo masses at z, 20 pages, 18 figures, 6 tables, accepted for publication in A&A

Published
2018

16. Search for gravitational lens candidates in the XMM-LSS/CFHTLS common field

Author

T. Sadibekova, Anna Pospieszalska-Surdej, François Finet, Andrii Elyiv, Marguerite Pierre, L. Chiappetti, O. V. Melnyk, and Jean Surdej

Subjects
QSOS, Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Basis (linear algebra), Field (physics), Diagram, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Stars, Gravitational lens, Space and Planetary Science, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Our aim was to identify gravitational lens candidates among some 5500 optical counterparts of the X-ray point-like sources in the medium-deep ~11 sq. deg. XMM-LSS survey. We have visually inspected the optical counterparts of each QSOs/AGN using CFHTLS T006 images. We have selected compact pairs and groups of sources which could be multiply imaged QSO/AGN. We have measured the colors and characterized the morphological types of the selected sources using the multiple PSF fitting technique. We found three good gravitational lens candidates: J021511.4-034306, J022234.3-031616 and J022607.0-040301 which consist of pairs of point-like sources having similar colors. On the basis of a color-color diagram and X-ray properties we could verify that all these sources are good QSO/AGN candidates rather than stars. Additional secondary gravitational lens candidates are also reported., 6 pages, 3 figures, 1 table, Accepted for publication in MNRAS

Published
2013

17. 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

18. The XXL Survey:VIII. MUSE characterization of intra cluster light in a z ~ 0.53 cluster of galaxies

Author

T. Sadibekova, S. Maurogordato, L. Guennou, Bianca M. Poggianti, Sean L. McGee, C. Adami, Nicolas Clerc, J. L. Willis, Marguerite Pierre, Emanuela Pompei, Cathy Horellou, Florian Pacaud, Mark Birkinshaw, and A. Iovino

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, Cluster (physics), Astrophysics::Solar and Stellar Astrophysics, clusters: general [galaxies], Emission spectrum, 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Ram pressure, Stars, Supernova, Space and Planetary Science, clusters: intracluster medium [galaxies], Astrophysics of Galaxies (astro-ph.GA), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Within a cluster, gravitational effects can lead to the removal of stars from their parent galaxies. Gas hydrodynamical effects can additionally strip gas and dust from galaxies. 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. The present study is designed to characterise this ICL in a ~10^14 M_odot and z~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. These sources were then spectroscopically characterised with MUSE. MUSE data were also used to compute redshifts of 24 cluster galaxies and search for cluster substructures. An atypically large amount of ICL 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. The stellar contribution to the ICL is about 2.3x10^9 yrs 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., Accepted in A&A, english enhanced, figure location different than in the A&A version due to different style files, shortened abstract

Published
2016

19. The XXL Survey VII. A supercluster of galaxies at z=0.43

Author

Bruno Altieri, Sinan Aliş, N. Baran, C. Adami, T. Sadibekova, Ivan Valtchanov, Florian Pacaud, Elias Koulouridis, C. Benoist, Fabio Gastaldello, S. Lavoie, Marguerite Pierre, Dominique Eckert, Sophie Maurogordato, Vernesa Smolčić, Yara L. Jaffé, Bianca M. Poggianti, E. Pompei, 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), University of Geneva [Switzerland], INAF-IASF Milano, Istituto Nazionale di Astrofisica (INAF), Université Quebec, Université du Québec à Chicoutimi (UQAC), Herschel Science Centre, European Space Agency (ESA), Joseph Louis LAGRANGE (LAGRANGE), 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), Institute for Space Applications and Remote Sensing (ISARS/NOA), National Observatory of Athens (NOA), 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), 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), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Université de Genève = University of Geneva (UNIGE), Agence Spatiale Européenne = European Space Agency (ESA), 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), 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), 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), National Observatory of Athens, and Institute for Space Applications and Remote Sensing

Subjects
Active galactic nucleus, Cosmology and Nongalactic Astrophysics (astro-ph.CO), PRIRODNE ZNANOSTI. Fizika. Astronomija i astrofizika, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, Supercluster, 0103 physical sciences, William Herschel Telescope, NATURAL SCIENCES. Physics. Astronomy and Astrophysics, clusters: general [galaxies], 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, New Technology Telescope, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, galaxies: clusters: general, X-rays: galaxies: clusters, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies: clusters [X-rays], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The XXL Survey is the largest homogeneous and contiguous survey carried out with XMM-Newton. Covering an area of 50 square degrees distributed over two fields, it primarily investigates the large-scale structures of the Universe using the distribution of galaxy clusters and active galactic nuclei as tracers of the matter distribution. Given its depth and sky coverage, XXL is particularly suited to systematically unveiling the clustering of X-ray clusters and to identifying superstructures in a homogeneous X-ray sample down to the typical mass scale of a local massive cluster. A friends-of-friends algorithm in three-dimensional physical space was run to identify large-scale structures. In this paper we report the discovery of the highest redshift supercluster of galaxies found in the XXL Survey. We describe the X-ray properties of the clusters members of the structure and the optical follow-up. The newly discovered supercluster is composed of six clusters of galaxies at a median redshift z around 0.43 and distributed across approximately 30 by 15 arc minutes (10 by 5 Mpc on sky) on the sky. This structure is very compact with all the clusters residing in one XMM pointing; for this reason this is the first supercluster discovered with the XXL Survey. Spectroscopic follow-up with WHT (William Herschel Telescope) and NTT (New Technology Telescope) confirmed a median redshift of z = 0.43. An estimate of the X-ray mass and luminosity of this supercluster and of its total gas mass put XLSSC-e at the average mass range of superclusters; its appearance, with two members of equal size, is quite unusual with respect to other superclusters and provides a unique view of the formation process of a massive structure., A&A, accepted; special XXL issue

Published
2016

20. 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

21. 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

22. 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

23. 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

24. The XXL Survey XIV. AAOmega Redshifts for the Southern XXL Field

Author

C. Adami, François Finet, O. Melnyk, Andy D. Goulding, Jean Surdej, Matt S. Owers, L. Chiappetti, Christopher Lidman, Manolis Plionis, Sotiria Fotopoulou, Andrii Elyiv, F. Ardila, Francesca Civano, T. Sadibekova, Marguerite Pierre, Elias Koulouridis, Florian Pacaud, Felipe Menanteau, AUTRES, 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), Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, Aristotle University of Thessaloniki, National Observatory of Athens, Institute for Space Applications and Remote Sensing, 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), Astronomical Observatory of Kiev, Taras Shevchenko National University of Kyiv, 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), 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), 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), Institute for Space Applications and Remote Sensing (ISARS/NOA), National Observatory of Athens (NOA), and Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112))

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, law.invention, Telescope, catalogs, surveys, galaxies: clusters: general, galaxies: quasars: general, law, 0103 physical sciences, 010303 astronomy & astrophysics, Spectrograph, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Redshift, Stars, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present a catalogue containing the redshifts of 3,660 X-ray selected targets in the XXL southern field. The redshifts were obtained with the AAOmega spectrograph and 2dF fibre positioner on the Anglo-Australian Telescope. The catalogue contains 1,515 broad line AGN, 528 stars, and redshifts for 41 out of the 49 brightest X-ray selected clusters in the XXL southern field., Comment: 8 pages, 4 figures, PASA in press

Published
2016

25. The cosmological analysis of X-ray cluster surveys - II. Application of the CR-HR method to the XMM archive

Author

Bruno Altieri, Nicolas Clerc, Jean-Paul Le Fevre, Florian Pacaud, Marguerite Pierre, C. Adami, Ivan Valtchanov, and T. Sadibekova

Subjects
Physics, 010308 nuclear & particles physics, Equation of state (cosmology), media_common.quotation_subject, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Radius, 01 natural sciences, Galaxy, Universe, Redshift, Space and Planetary Science, 0103 physical sciences, Cluster (physics), Dark energy, 010303 astronomy & astrophysics, Scaling, media_common
Abstract

We have processed 2774 high-galactic observations from the XMM archive (as of May 2010) and extracted a serendipitous catalogue of some 850 clusters of galaxies based on purely X-ray criteria, following the methodology developed for the XMM-LSS survey. Restricting the sample to the highest signal-to-noise objects (347 clusters), we perform a cosmological analysis using the X-ray information only. The analysis consists in the modelling of the observed colour-magnitude (CR-HR) diagram constructed from cluster instrumental count-rates measured in the [0.5-2], [1-2] and [0.5-1] keV bands. A MCMC procedure simultaneously fits the cosmological parameters, the evolution of the cluster scaling laws and the selection effects. Our results are consistent with the sigma_8 and Omega_m values obtained by WMAP-5 and point toward a negative evolution of the cluster scaling relations with respect to the self-similar expectation. We are further able to constrain the cluster fractional radius xc0=r_c/r500c, to xc0=0.24 +/- 0.04. This study stresses again the critical role of selection effects in deriving cluster scaling relations, even in the local universe. Finally, we show that CR-HR method applied to the eRosita all-sky survey - provided that cluster photometric redshifts are available - will enable the determination of the equation of state of the dark energy at the level of the DETF stage IV predictions; simultaneously, the evolution of the cluster scaling-relations will be unambiguously determined. The XMM CLuster Archive Super Survey (XCLASS) serendipitous cluster catalogue is available online at: this http URL

Published
2012

26. The cosmological analysis of X-ray cluster surveys - I. A new method for interpreting number counts

Author

Marguerite Pierre, T. Sadibekova, Florian Pacaud, and N. Clerc

Subjects
Physics, Diagram, Astronomy and Astrophysics, Observable, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Function (mathematics), Redshift, Cosmology, Space and Planetary Science, Cluster (physics), Sensitivity (control systems), Statistical physics, Scaling
Abstract

We present a new method aiming to simplify the cosmological analysis of X-ray cluster surveys. It is based on purely instrumental observable quantities, considered in a two-dimensional X-ray colour-magnitude diagram (hardness ratio versus count-rate). The basic principle is that, even in rather shallow surveys, substantial information on cluster redshift and temperature is present in the raw X-ray data and can be statistically extracted; in parallel, such diagrams can be readily predicted from an ab initio cosmological modeling. We illustrate the methodology for the case of a 100 deg2 XMM survey having a sensitivity of ~10^{-14} ergs/s/cm^2 and fit at the same time, the survey selection function, the cluster evolutionary scaling-relations and the cosmology; our sole assumption -- driven by the limited size of the sample considered in the case-study -- is that the local cluster scaling relations are known. We devote special care to the realistic modeling of the count-rate measurement uncertainties and evaluate the potential of the method via a Fisher analysis. In the absence of individual cluster redshifts, the CR-HR method appears to be much more efficient than the traditional approach based on cluster counts (i.e. dn/dz, requiring redshifts). In the case where redshifts are available, our method performs similarly as the traditional mass function (dn/dM/dz) for the purely cosmological parameters, but better constrains parameters defining the cluster scaling relations and their evolution. A further practical advantage of the CR-HR method is its simplicity : this fully top-down approach totally bypasses the tedious steps consisting in deriving cluster masses from X-ray temperature measurements.

Published
2012

27. Choosing Dome C, Antarctic Plateau as Future Astronomical Observatory

Author

M. Azouit, H. Trinquet, Marc Sarazin, A. Agabi, T. Sadibekova, Eric Fossat, C. Genthon, Eric Aristidi, Gerhard Krinner, Merieme Chadid, Jean Vernin, Laboratoire Universitaire d'Astrophysique de Nice (LUAN), 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)-Centre National de la Recherche Scientifique (CNRS), Joseph Louis LAGRANGE (LAGRANGE), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Hippolyte Fizeau (FIZEAU), Laboratoire de glaciologie et géophysique de l'environnement (LGGE), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), European Southern Observatory (ESO), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-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), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Observatoire des Sciences de l'Univers de Grenoble (OSUG), and Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, Meteorology, 010308 nuclear & particles physics, General Engineering, Astronomy and Astrophysics, 01 natural sciences, Dome (geology), Space and Planetary Science, Observatory, Climatology, 0103 physical sciences, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Antarctic plateau
Abstract

International audience; In this paper we present year-round climatological analysis made from radio-sounding measurements and ECMWF Data. And we end up with a generalized conclusion (scientific aspect) from statistical results of site-testing at Concordia concerning the feasibility of the future astronomical exploitation of Dome C.

Published
2007

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

Author

N. Clerc, C. Adami, Florian Pacaud, Sotiria Fotopoulou, T. Sadibekova, F. Ziparo, Graham P. Smith, Jon Willis, Sean L. McGee, Christopher Lidman, L. Chiappetti, Marguerite Pierre, Paul Giles, Sarah L. Mulroy, B. J. Maughan, M. Lieu, S. Lavoie, P. Hudelot, Max-Planck-Institut für Extraterrestrische Physik (MPE), University of Reading (UOR), 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), Aristotle University of Thessaloniki, AUTRES, Université Quebec, Université du Québec à Chicoutimi (UQAC), 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), 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), 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), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, weak [gravitational lensing], 0103 physical sciences, Cluster (physics), clusters: general [galaxies], Brightest cluster galaxy, 010303 astronomy & astrophysics, Weak gravitational lensing, Astrophysics::Galaxy Astrophysics, Physics, groups: general [galaxies], 010308 nuclear & particles physics, Sigma, Astronomy and Astrophysics, State (functional analysis), stellar content [galaxies], Astrophysics - Astrophysics of Galaxies, Galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), photometry [galaxies], galaxies: clusters [X-rays], Halo, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

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 $M_{500,WL} =3.5 \times 10^{13}\,M_\odot$. 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, $M_{500,WL} =0.35-12.10 \times 10^{14}\,M_\odot$, at $0, Comment: A&A, in press

Published
2015
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29. First Whole Atmosphere Nighttime Seeing Measurements at Dome C, Antarctica

Author

Eric Aristidi, Jean Vernin, M. Azouit, T. Sadibekova, Abdelkrim Agabi, Eric Fossat, Aziz Ziad, François Martin, Laboratoire Universitaire d'Astrophysique de Nice (LUAN), 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)-Centre National de la Recherche Scientifique (CNRS), and IPEV

Subjects
Physics, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], 010308 nuclear & particles physics, Site testing, Astrophysics (astro-ph), Elevation, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Atmospheric sciences, 01 natural sciences, site testing, Atmosphere, High surface, Dome (geology), Space and Planetary Science, 0103 physical sciences, Polar, 010303 astronomy & astrophysics
Abstract

We report site testing results obtained in night-time during the polar autumn and winter at Dome C. These results were collected during the first Concordia winterover by A. Agabi. They are based upon seeing and isoplanatic angle monitoring, as well as in-situ balloon measurements 2 of the refractive index structure constant profiles Cn (h). Atmosphere is divided into two regions: (i) a 36 m high surface layer responsible of 87% of the turbulence and (ii) a very stable free atmosphere above with a median seeing of 0.36+-0.19 arcsec at an elevation of h = 30 m. The median seeing measured with a DIMM placed on top of a 8.5 m high tower is 1.3+-0.8 arcsec., accepted for publication in PASP (oct 2005)

Published
2006

30. The X-CLASS−redMaPPer galaxy cluster comparison

Author

Rene Gastaud, T. Sadibekova, Jean-Paul Le Fevre, Eli S. Rykoff, Nicolas Clerc, Marguerite Pierre, Eduardo Rozo, L. Faccioli, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Max-Planck-Institut für Extraterrestrische Physik (MPE), 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, KIPAC, Stanford (KIPAC), Stanford University-SLAC National Accelerator Laboratory (SLAC), Stanford University, This work was supported in part by the US Department of Energy contract to SLAC No. DE-AC02- 76SF0051, Département d'Electronique, des Détecteurs et d'Informatique (ex SEDI) (DEDI), and Stanford University [Stanford]-SLAC

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Weak signal, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Type (model theory), 01 natural sciences, Luminosity, Space and Planetary Science, galaxies: clusters: general, cosmology: observations, X-rays: galaxies: clusters, 0103 physical sciences, Cluster (physics), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Galaxy cluster, catalogs, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We performed a detailed and, for a large part interactive, analysis of the matching output between the X-CLASS and redMaPPer cluster catalogues. The overlap between the two catalogues has been accurately determined and possible cluster positional errors were manually recovered. The final samples comprise 270 and 355 redMaPPer and X-CLASS clusters respectively. X-ray cluster matching rates were analysed as a function of optical richness. In a second step, the redMaPPer clusters were correlated with the entire X-ray catalogue, containing point and uncharacterised sources (down to a few 10^{-15} erg s^{-1} cm^{-2} in the [0.5-2] keV band). A stacking analysis was performed for the remaining undetected optical clusters. Main results show that neither of the wavebands misses any massive cluster (as coded by X-ray luminosity or optical richness). After correcting for obvious pipeline short-comings (about 10% of the cases both in optical and X-ray), ~50% of the redMaPPer (down to a richness of 20) are found to coincide with an X-CLASS cluster; when considering X-ray sources of any type, this fraction increases to ~ 80%; for the remaining objects, the stacking analysis finds a weak signal within 0.5 Mpc around the cluster optical centers. The fraction of clusters totally dominated by AGN-type emission appears to be of the order of a few percent. Conversely ~ 40% of the X-CLASS clusters are identified with a redMaPPer (down to a richness of 20) - part of the non-matches being due to the fact that the X-CLASS sample extends further out than redMaPPer (z, 15 pages, 20 figures, 2 tables

Published
2014

31. The XMM-LSS survey: the Class 1 cluster sample over the extended 11 deg(2) and its spatial distribution

Author

S. Maurogordato, Ben J Maughan, C. Adami, Bruno Altieri, Florian Pacaud, Nicolas Clerc, Patrick Valageas, T. Sadibekova, Christophe Benoist, Jon Willis, Graham P. Smith, M. Lieu, Marguerite Pierre, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES)

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, Cosmic microwave background, Astronomy, Sigma, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Spatial distribution, Astrophysics - Astrophysics of Galaxies, Redshift, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Cluster (physics), Cluster sampling, Sample variance, Galaxy cluster, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

This paper presents 52 X-ray bright galaxy clusters selected within the 11 deg$^2$ XMM-LSS survey. 51 of them have spectroscopic redshifts ($0.053 \sigma$) constraints on the presence of a large void in the cluster distribution. We work out alternative hypotheses and demonstrate that a negative redshift evolution in the normalization of the $L_{X}-T_X$ relation (with respect to a self-similar evolution) is a plausible explanation for the observed deficit. We confirm this evolutionary trend by directly studying how C1 clusters populate the $L_{X}-T_X-z$ space, properly accounting for selection biases. We point out that a systematically evolving, unresolved, central component in clusters and groups (AGN contamination or cool core) can impact the classification as extended sources and be partly responsible for the observed redshift distribution.[abridged], Comment: 33 pages, 21 figures, 3 tables ; accepted for publication in MNRAS

Published
2014

32. Site testing study based on weather balloons measurements

Author

T. Sadibekova, W. L. Roth, Jean Vernin, Eric Aristidi, Eric Fossat, M. Azouit, Tony Travouillon, Von P. Walden, B. Halter, A. Agabi, Jon Lawrence, Laboratoire Hippolyte Fizeau (FIZEAU), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, and Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)

Subjects
020209 energy, General Engineering, FOS: Physical sciences, Astronomy and Astrophysics, 02 engineering and technology, Effects of high altitude on humans, Weather balloon, Atmospheric sciences, Snow, 01 natural sciences, Wind speed, Physics - Atmospheric and Oceanic Physics, 13. Climate action, Space and Planetary Science, Polar vortex, Atmospheric and Oceanic Physics (physics.ao-ph), 0103 physical sciences, 0202 electrical engineering, electronic engineering, information engineering, Polar, Surface layer, Tropopause, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Geology
Abstract

We present wind and temperature profiles at Dome C measured by balloon born sonds during the polar summer. Data from 197 flights have been processed for 4 campaigns between 2000 and 2004. We show the exceptionnal wind conditions at Dome C, Average ground wind speed is 3.6 m/s. We noticed in mid-november the presence of high altitude strong winds (40 m/s) probably due to the polar vortex which disappear in summer. These winds seem to have no effect on seeing measurements made with a DIMM at the same period. Temperature profiles exhibit a minimum at height 5500 m (over the snow surface) that defines the tropopause. Surface layer temperature profile has negative gradient in the first 50 m above ground in the afternoon and a strong inversion layer (5{\deg}C over 50 m) around midnight. Wind profiles are compared with other astronomical sites, and with a meteorological model from Meteo France.

Published
2005

33. VIMOS Ultra-Deep Survey (VUDS): Witnessing the Assembly of a Massive Cluster at z~3.3

Author

R. Thomas, Andrea Grazian, Jean-Gabriel Cuby, Daniel Schaerer, S. de la Torre, E. Zucca, Laurence Tresse, Letizia P. Cassarà, Dale D. Kocevski, Marco Castellano, Olivier Ilbert, D. Maccagni, N. Z. Scoville, Ricardo Amorín, Andrea Cimatti, T. Sadibekova, Stéphane Paltani, V. Sommariva, Sotiria Fotopoulou, Lidia Tasca, Stephane Charlot, Thierry Contini, C. López-Sanjuan, A. Durkalec, Margherita Talia, Yannick Mellier, Bianca Garilli, G. Zamorani, S. Bardelli, Olga Cucciati, L. M. Lubin, Daniela Vergani, Adriano Fontana, M. Scodeggio, B. Ribeiro, M. Giavalisco, P. W. Wang, Laura Pentericci, Peter Capak, Nimish P. Hathi, Brian C. Lemaux, V. Le Brun, Paolo Cassata, Yoshiaki Taniguchi, Eros Vanzella, C. Moreau, O. Le Fèvre, Roy R. Gal, Mara Salvato, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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), 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), European Project: 268107,EC:FP7:ERC,ERC-2010-AdG_20100224,EARLY(2011), 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), 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), 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 Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Lemaux, B.C., Cucciati, O., Tasca, L.A.M., Le Fèvre, O., Zamorani, G., Cassata, P., Garilli, B., Le Brun, V., Maccagni, D., Pentericci, L., Thomas, R., Vanzella, E., Zucca, E., Amorín, R., Bardelli, S., Capak, P., Cassarà, L.P., Castellano, M., Cimatti, A., Cuby, J.G., De La Torre, S., Durkalec, A., Fontana, A., Giavalisco, M., Grazian, A., Hathi, N.P., Ilbert, O., Moreau, C., Paltani, S., Ribeiro, B., Salvato, M., Schaerer, D., Scodeggio, M., Sommariva, V., Talia, M., Taniguchi, Y., Tresse, L., Vergani, D., Wang, P.W., Charlot, S., Contini, T., Fotopoulou, S., Gal, R.R., Kocevski, D.D., López-Sanjuan, C., Lubin, L.M., Mellier, Y., Sadibekova, T., and Scoville, N.

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, galaxies: active, FOS: Physical sciences, Astrophysics, Spectral line, techniques: photometric, galaxies: high-redshift, Coma Cluster, Galaxies: active, Galaxies: clusters: general, Galaxies: evolution, Galaxies: high-redshift, Techniques: photometric, Techniques: spectroscopic, Astronomy and Astrophysics, Space and Planetary Science, Photometric redshift, media_common, Physics, Star formation, Astronomy and Astrophysic, Redshift, Galaxy, Universe, galaxies: clusters: general, Halo, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], techniques: spectroscopic, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Using new spectroscopic observations obtained as part of the VIMOS Ultra-Deep Survey (VUDS), we perform a systematic search for overdense environments in the early universe ($z>2$) and report here on the discovery of Cl J0227-0421, a massive protocluster at $z=3.29$. This protocluster is characterized by both the large overdensity of spectroscopically confirmed members, $\delta_{gal}=10.5\pm2.8$, and a significant overdensity in photometric redshift members. The halo mass of this protocluster is estimated, by a variety of methods, to be roughly $3\times10^{14}$ $\mathcal{M}_{\odot}$ at $z\sim3.3$, which, evolved to $z=0$ results in a halo mass rivaling or exceeding that of the Coma cluster. The properties of 19 spectroscopically confirmed member galaxies are compared with a large sample of VUDS/VVDS galaxies in lower density field environments at similar redshifts. We find tentative evidence for an excess of redder, brighter, and more massive galaxies within the confines of the protocluster relative to the field population, which suggests that we may be observing the beginning of environmentally-induced quenching. The properties of these galaxies are investigated, including a discussion of the brightest protocluster galaxy which appears to be undergoing vigorous coeval nuclear and starburst activity. The remaining member galaxies appear to have characteristics which are largely similar to the field population. Though we find weaker evidence of the suppression of the median star formation rates amongst and differences in stacked spectra of member galaxies with respect to the field, we defer any conclusions of these trends to future work with the ensemble of protostructures that are found in the full VUDS sample., Comment: 23 pages, 15 figures, 3 tables, accepted for publication in A&A after minor changes, v3/v4 contains an additional online table and minor topical changes

Published
2014
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34. The XXL Survey

Author

L. Chiappetti, Ian G. McCarthy, Stefano Ettori, C. Adami, Yannick M. Bahé, J. Démoclès, Jean-Paul Le Fevre, J. P. Willis, Martin Kilbinger, T. Sadibekova, Nicolas Clerc, Dominique Eckert, F. Ziparo, S. Lavoie, Marguerite Pierre, Trevor J. Ponman, Paul Giles, Florian Pacaud, Graham P. Smith, M. Lieu, Ben J Maughan, University of Reading (UOR), Max-Planck-Institut für Extraterrestrische Physik (MPE), 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), Argelander Institute for Astronomy (AlfA), Rheinische Friedrich-Wilhelms-Universität Bonn, 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), University of Geneva [Switzerland], INAF-IASF Milano, INAF - Osservatorio Astronomico di Bologna (OABO), Université Quebec, Université du Québec à Chicoutimi (UQAC), 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), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Université de Genève = University of Geneva (UNIGE), 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 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
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Flux, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, weak [gravitational lensing], 0103 physical sciences, Range (statistics), clusters: general [galaxies], 010303 astronomy & astrophysics, Scaling, Galaxy cluster, QB, Physics, groups: general [galaxies], 010308 nuclear & particles physics, Sigma, Astronomy and Astrophysics, Function (mathematics), Redshift, [SDU]Sciences of the Universe [physics], Space and Planetary Science, galaxies: clusters [X-rays], Halo, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The XXL survey is the largest survey carried out by XMM-Newton. Covering an area of 50deg$^2$, the survey contains $\sim450$ galaxy clusters out to a redshift $\sim$2 and to an X-ray flux limit of $\sim5\times10^{-15}erg\,s^{-1}cm^{-2}$. This paper is part of the first release of XXL results focussed on the bright cluster sample. We investigate the scaling relation between weak-lensing mass and X-ray temperature for the brightest clusters in XXL. The scaling relation is used to estimate the mass of all 100 clusters in XXL-100-GC. Based on a subsample of 38 objects that lie within the intersection of the northern XXL field and the publicly available CFHTLenS catalog, we derive the $M_{WL}$ of each system with careful considerations of the systematics. The clusters lie at $0.1, Comment: to be published in A&A

Published
2016

35. The XMM-LSS survey: optical assessment and properties of different X-ray selected cluster classes

Author

J. P. Lefevre, Jean Surdej, Jean-Baptiste Melin, C. Libbrecht, O. LeFevre, G. Hertling, Gaspar Galaz, Alain Detal, T. Sadibekova, C. Adami, D. Maccagni, L. Chiappetti, O. Ilbert, Trevor J. Ponman, B. Garilli, L. Tresse, L. Guennou, Marguerite Pierre, Hernan Quintana, Florian Pacaud, Pierre-Alain Duc, Bruno Altieri, Alain Mazure, A. Gueguen, I. Valtchanov, H. Aussel, J. P. Willis, V. LeBrun, Nicolas Clerc, P. G. Sprimont, Davide Ricci, Masayuki Akiyama, 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), and 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)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmic web, 0103 physical sciences, Cluster (physics), Spectroscopy, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, education.field_of_study, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Velocity dispersion, Astronomy and Astrophysics, Redshift, Galaxy, Space and Planetary Science, Low Mass, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

XMM and Chandra opened a new area for the study of clusters of galaxies. Not only for cluster physics but also, for the detection of faint and distant clusters that were inaccessible with previous missions. This article presents 66 spectroscopically confirmed clusters (0.05, Comment: Seven figures given in jpg format due to space limitation. The full sample of X-ray clusters with associated optical spectroscopic data is available via the L3SDB database (http://l3sdb.in2p3.fr:8080/l3sdb/)

Published
2011

36. The Optimal Gravitational Lens Telescope

Author

Christian Delacroix, Serge Habraken, Martin Dominik, Hernan Quintana, Jean Surdej, Charles Hanot, H. Le Coroller, T. Sadibekova, P. Coleman, Dominique Sluse, and Dimitri Mawet

Subjects
Physics, COSMIC cancer database, Cosmology and Nongalactic Astrophysics (astro-ph.CO), business.industry, Optical instrument, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Physics::Optics, Astronomy and Astrophysics, Quasar, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy, law.invention, Lens (optics), Telescope, Gravitational lens, Optics, Space and Planetary Science, law, Source image, Astrophysics - Instrumentation and Methods for Astrophysics, business, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Given an observed gravitational lens mirage produced by a foreground deflector (cf. galaxy, quasar, cluster, ...), it is possible via numerical lens inversion to retrieve the real source image, taking full advantage of the magnifying power of the cosmic lens. This has been achieved in the past for several remarkable gravitational lens systems. Instead, we propose here to invert an observed multiply imaged source directly at the telescope using an ad hoc optical instrument which is described in the present paper. Compared to the previous method, this should allow one to detect fainter source features as well as to use such an optimal gravitational lens telescope to explore even fainter objects located behind and near the lens. Laboratory and numerical experiments illustrate this new approach.

Published
2010

37. Single Star Scidar at Dome C

Author

M. Azouit, H. Trinquet, T. Sadibekova, Merieme Chadid, Jean Vernin, Eric Aristidi, Laboratoire Hippolyte Fizeau (FIZEAU), 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), Joseph Louis LAGRANGE (LAGRANGE), Laboratoire Universitaire d'Astrophysique de Nice (LUAN), and 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)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, 010308 nuclear & particles physics, General Engineering, Astronomy and Astrophysics, First light, Geodesy, 01 natural sciences, Single star, Atmosphere, Dome (geology), Space and Planetary Science, Long period, 0103 physical sciences, Optical turbulence, Surface layer, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics
Abstract

International audience; Here we present the first light of the Single Star Scidar (SSS) at Dome C, during January 2005 and the first results obtained during the winter 2006. We recall the SSS principle, how it is designed to resist to very low temperatures and to be adjusted in a very simple way. No exemple of long period of observation can be given since the huge amount of data cannot be sent back to our laboratory to be offline processed, due to low data transfer available from Dome C. But, a short file is shown, which demonstrates the major contribution of the surface layer to the whole atmosphere optical turbulence. Almost 300 hours of observations have been taken successfully during winter 2006.

Published
2007

38. History, Present Status & Future of Site Testing at Dome C

Author

Merieme Chadid, Jean Vernin, Eric Fossat, T. Sadibekova, A. Agabi, Eric Aristidi, M. Azouit, H. Trinquet, Aziz Ziad, 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), Laboratoire Universitaire d'Astrophysique de Nice (LUAN), 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)-Centre National de la Recherche Scientifique (CNRS), and Laboratoire Hippolyte Fizeau (FIZEAU)

Subjects
Physics, Katabatic wind, Polar night, 010308 nuclear & particles physics, Site testing, Launched, General Engineering, Astronomy and Astrophysics, Geodesy, 01 natural sciences, Space and Planetary Science, Image motion, 0103 physical sciences, Optical turbulence, Visible range, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics
Abstract

Hereafter we give a brief history of our contribution to astronomical site testing in Antarctica, at least for the high angular resolution in the visible range. The decision to undertake the first site testing at South Pole began one year after a congress organized by French Academie des Sciences, in year 1992. Indeed, in 1993 a meeting took place in Chicago with the participation of Peter Gillingham, Al Harper and Jean Vernin where each one took the respective responsibility of 1) giving a PhD student, 2) the South Pole infrastructure and 3) the relevant instruments. During winter 1995, thanks to a mast equipped with micro-thermal sensors, we demonstrated (Marks et al., 1996, A&AS, 118, 1) that the first 30 m of the surface layer was disrupted by strong optical turbulence. Then, the year after, 15 balloons equipped with micro-thermal probes were successfully launched from South Pole. Marks et al. (1999, A&AS, 134, 161) shown that most of the optical turbulence at South Pole was concentrated within a layer 200 m thick above the ice level. From this study, it becomes clear that the noticeable katabatic wind present at South Pole was generating this huge surface layer and that is why we oriented our astronomical site characterization toward Dome C. Our first summer seeing estimations began in 2000, which demonstrated (Aristidi et al., 2003, A&AS, 406, L19 & Aristidi et al., 2005, A&A, 444, 651) that, as expected, the surface wind was much less than at South Pole, and, as a matter of fact, the seeing was much better, and was even exceptional during the four hours of the afternoon where a seeing of less than 0.5 arcsec was measured. In 2005, the Concordia base was first open during the polar night, and one of us, A. Agabi was able to launch 41 balloons equipped with micro-thermal sensors. A differential image motion monitor (DIMM) was also setup with success. At mid winter, Agabi et al. (2006, PASP, 118, 344) showed that most of the optical turbulence came from the first 30 m surface layer and very little from the rest of the atmosphere (1.3 arcsec above 8.5 m and 0.37 arcsec above 30 m).

Published
2007

39. Generalized SCIDAR measurements at La Silla Observatory

Author

Jean Vernin, Marc Sarazin, T. Sadibekova, and M. Le Louarn

Subjects
Diffraction, Physics, Telescope, Tikhonov regularization, Altitude, Observatory, law, Binary star, Atmospheric turbulence, Image processing, Remote sensing, law.invention
Abstract

We present the results of vertical profiles of refractive index structure constant C n2 (h) measurements made at the 1-m telescope, La Silla Observatory (ESO,Chile) using the gene ralized SCIDAR technique. Obse rvations took place during July, August, November, 2002 an d February 2003. The instrume ntation, computer interface and a preliminary reduction software were provided by the Imperial College (London) scientific group. We describe the SCIDAR image processing technique and two inverting methods. The first, proposed by the Imperial College group, is based on the Tikhonov regularization and the second, on use at Nice University, is based on maximum entropy. Performances of both methods agree well. The profile integrals are compared to simultaneous DIMM seeing measurements made at La Silla Observatory. INTRODUCTION. Generalized SCIDAR (Scintilla tion Detection and Ranging) is one of the most effective methods to measure the altitude distribution of optical turbulence in the atmosphere above the site. With this instrument installed on the telescope a diameter of which is preferably not below 1m for the best altitude resolution (about 200-300 meters) we observe the diffraction patterns images from a binary star on the telescope pupil produced by an atmospheric turbulence. Then we recover a profile of the refractive index structure constant C

Published
2006

40. Site testing at Dome C: history and present status

Author

Eric Fossat, T. Sadibekova, M. Azouit, Merieme Chadid, H. Trinquet, Aziz Ziad, Jean Vernin, Eric Aristidi, A. Agabi, Laboratoire Universitaire d'Astrophysique de Nice (LUAN), 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)-Centre National de la Recherche Scientifique (CNRS), Joseph Louis LAGRANGE (LAGRANGE), 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), Département Fresnel (FRESNEL), 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)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Centre National de la Recherche Scientifique (CNRS), and Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS)

Subjects
010504 meteorology & atmospheric sciences, Site testing, Dome, Library science, Astronomy and Astrophysics, 01 natural sciences, Archaeology, Space and Planetary Science, Observatory, 0103 physical sciences, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Geology, 0105 earth and related environmental sciences
Abstract

International audience; The idea of starting an astronomical site testing in Antarctica began during a congress organized by French Académie des Sciences, in 1992, and entitled ‘Recherches polaires-Une Stratégie pour l'an 2000’. At this time, one of us (Vernin 1994) gave a proposal for an astronomical site testing in Antarctica. This proposal was rapidly followed by a meeting between Al Harper (from ‘Center for Astrophysical Research in Antarctica’, Chicago), Peter Gillingham (from the Anglo Australian Observatory, Australia) and Jean Vernin (from Nice University) at Lake Geneva, Wisconsin, in 1993. It was decided to investigate what was the astronomical quality of South Pole station, each institute bringing its own participation: CARA, the South Pole infrastructure, University of New South Wales, a PhD student and Nice University its expertise and instruments.

Published
2006

41. On the atmosphere for astronomers above Dome C, Antarctica

Author

M. Azouit, Christian Genthon, Eric Aristidi, Eric Fossat, Gerhard Krinner, Karim Agabi, T. Sadibekova, Laboratoire Universitaire d'Astrophysique de Nice (LUAN), 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)-Centre National de la Recherche Scientifique (CNRS), European Southern Observatory (ESO), Laboratoire de glaciologie et géophysique de l'environnement (LGGE), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Laboratoire Hippolyte Fizeau (FIZEAU), 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), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire des Sciences de l'Univers de Grenoble (OSUG), and Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)

Subjects
wind gradient, Wind gradient, 010504 meteorology & atmospheric sciences, Dome, Oceanography, Atmospheric sciences, 01 natural sciences, temperature gradient, Atmosphere, site testing, optical turbulence, ECMWF analyses, 0103 physical sciences, Atmospheric turbulence, [SDU.STU.GL]Sciences of the Universe [physics]/Earth Sciences/Glaciology, 010303 astronomy & astrophysics, Ecology, Evolution, Behavior and Systematics, 0105 earth and related environmental sciences, Site testing, radio-soundings, Geology, Antarctic plateau, 13. Climate action, Climatology, Optical turbulence, Environmental science
Abstract

This paper describes a comparison between balloon radio-soundings made in summer at the Concordia station, Dome C, Antarctica and coincident model-based meteorological analyses. The comparison allows the assessment of the reliability of the analyses in summer. This allows the use of the winter analyses within an estimated range of uncertainty, while the first in situ measurements are just becoming available. The astronomical interest is to produce an estimate of atmospheric turbulence during the Antarctic winter at this very promising site. For this work the 6-hourly ECMWF operational analyses were used, concurrently with the data obtained in situ by the radio-sounding made at Concordia with standard meteorological balloons and sondes during four summer seasons (November–January), from December 2000 to the end of January 2004.

Published
2006

42. Single Star Scidar first light from Dôme C

Author

T. Sadibekova, Merieme Chadid, Eric Aristidi, Jean Vernin, M. Azouit, H. Trinquet, Laboratoire Hippolyte Fizeau (FIZEAU), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, and Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Dome (geology), Space and Planetary Science, 0103 physical sciences, Astronomy, Astronomy and Astrophysics, First light, 010306 general physics, 010303 astronomy & astrophysics, 01 natural sciences, Geology, Single star
Abstract

In the recent years, a lot of instruments have been put into operation during the polar summer at DômeC., Then, during the first polar night when the Astro-Concordia sation was open for the first time during winter, about 40 balloons (Azouit & Vernin) instrumented to measure optical turbulence profiles and 2 Differencial Image Motion Monitors (DIMM) were setup. The main results from this first important campaign are found in Agabi et al. (2006). It appears from this first night time observations that almost all the optical turbulence was concentrated in the first 30 m above the ice. At an elevation of 8.5 m above the ice the seeing is about 1″.4, while above an elevation of 30 m the seeing drops down to 0″.36. This last figure is coherent with the estimation from Lawrence et al. (2004) if one takes into account that they were not sensitive to the first 30 m., which corresponds to the turbulent surface layer.

Published
2006

43. Site testing in summer at Dome C, Antarctica

Author

Eric Aristidi, Aziz Ziad, Eric Fossat, Abdelkrim Agabi, M. Azouit, Jean Vernin, F. Martin, Tony Travouillon, T. Sadibekova, Laboratoire Universitaire d'Astrophysique de Nice (LUAN), 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)-Centre National de la Recherche Scientifique (CNRS), School of Physics [UNSW Sydney] (UNSW), University of New South Wales [Sydney] (UNSW), IPEV, Laboratoire Hippolyte Fizeau (FIZEAU), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, and Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, Bright star, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Site testing, Astrophysics (astro-ph), Canopus, Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, antarctica, 01 natural sciences, 010309 optics, site testing, Dome (geology), Space and Planetary Science, 0103 physical sciences, Almost Every Day, Late afternoon, 010303 astronomy & astrophysics
Abstract

International audience; We present summer site testing results based on DIMM data obtained at Dome C, Antarctica. These data have been collected on the bright star Canopus during two 3-months summer campaigns in 2003-2004 and 2004-2005. We performed continuous monitoring of the seeing a nd the isoplanatic angle in the visible. We found a median seeing of 0.54 \arcsec and a median isoplanatic angle of 6.8 \arcsec. The seeing appears to have a deep minimum around 0.4 \arcsec almost every day in late afternoon.

Published
2005

44. The XXL Survey: XXIII. The Mass Scale of XXL Clusters from Ensemble Spectroscopy

Author

Bruno Altieri, Marguerite Pierre, Richard J. Tuffs, C. Adami, T. Sadibekova, V. Guglielmo, Andrew M. Hopkins, Jochen Liske, M. Scodeggio, Aaron S. G. Robotham, Fabio Gastaldello, Arya Farahi, David Rapetti, August E. Evrard, Manolis Plionis, Andrii Elyiv, Mauro Sereno, Trevor J. Ponman, Ivan K. Baldry, Stefano Ettori, Elias Koulouridis, Sophie Maurogordato, A. Iovino, L. Guennou, Florian Pacaud, Michael J. I. Brown, Bianca M. Poggianti, L. Chiappetti, Ben J Maughan, Paul Giles, Simon P. Driver, Angela Bongiorno, Mark Birkinshaw, Micol Bolzonella, Bianca Garilli, Ivan Valtchanov, Matt S. Owers, 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), 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), 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), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), University of St Andrews. School of Physics and Astronomy, 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, and 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)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Dark matter, NDAS, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, clusters: general [Galaxies], Kinetic energy, 01 natural sciences, Virial theorem, Galaxy groups and clusters, galaxies: groups: general, 0103 physical sciences, QB Astronomy, 010303 astronomy & astrophysics, QC, Astrophysics::Galaxy Astrophysics, galaxies: kinematics and dynamics, QB, Physics, 010308 nuclear & particles physics, kinematics and dynamics [Galaxies], Velocity dispersion, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, groups: general [Galaxies], QC Physics, Space and Planetary Science, galaxies: clusters: general, Astrophysics of Galaxies (astro-ph.GA), X-rays: galaxies: clusters, Halo, galaxies: clusters [X-rays], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

An X-ray survey with the XMM-Newton telescope, XMM-XXL, has identified hundreds of galaxy groups and clusters in two 25 deg$^2$ fields. Combining spectroscopic and X-ray observations in one field, we determine how the kinetic energy of galaxies scales with hot gas temperature and also, by imposing prior constraints on the relative energies of galaxies and dark matter, infer a power-law scaling of total mass with temperature. Our goals are: i) to determine parameters of the scaling between galaxy velocity dispersion and X-ray temperature, $T_{\rm 300kpc}$, for the halos hosting XXL-selected clusters, and; ii) to infer the log-mean scaling of total halo mass with temperature, $\langle \ln M_{200} \, | \, T, z \rangle$. We apply an ensemble velocity likelihood to a sample of $> 1500$ spectroscopic redshifts within $132$ spectroscopically confirmed clusters with redshifts $z < 0.6$ to model, $\langle \ln \sigma_{\rm gal}\,|\,T,z\rangle$, where $\sigma_{\rm gal}$ is the velocity dispersion of XXL cluster member galaxies and $T$ is a 300 kpc aperture temperature. To infer total halo mass we use a precise virial relation for massive halos calibrated by N-body simulations along with a single degree of freedom summarizing galaxy velocity bias with respect to dark matter. For the XXL-N cluster sample, we find $\sigma_{\rm gal} \propto T^{0.63\pm0.05}$, a slope significantly steeper than the self-similar expectation of $0.5$. Assuming scale-independent galaxy velocity bias, we infer a mean logarithmic mass at a given X-ray temperature and redshift, $\langle\ln (E(z) M_{200}/10^{14}\,{\rm M}_{\odot})|T,z\rangle=\pi+\alpha \ln(T/T_p )+\beta\ln (E(z)/E(z_p) )$ using pivot values ${\rm k}T_{p}=2.2\,{\rm keV}$ and $z_p=0.25$, with normalization $\pi=0.45\pm0.24$ and slope $\alpha=1.89\pm0.15$. We obtain only weak constraints on redshift evolution, $\beta=-1.29\pm1.14$., Comment: 14 pages, 9 figures, 4 tables, accepted for publication in A&A

45. Grandma: a network to coordinate them all

Author

Yusufjon Tillayev, Christina C. Thöne, Martin Mašek, Patrice Hello, N. Ismailov, A. Le Van Su, Wenxiong Li, G. V. Kapanadze, D. Corre, M. Boer, V. R. Ayvazian, P. Lognone, A. Baransky, J. Zhang, S. Alishov, S. Antier, N. B. Orange, R. Ya. Inasaridze, A. de Ugarte Postigo, N. Kochiashvili, A. Cailleau, R. Marron, Alexis Coleiro, M. Blažek, S. Perrigault, Eric Howell, C. Delattre, T. Sadibekova, S. Basa, David Alexander Kann, J. P. Teng, Tim Dietrich, J.-G. Ducoin, Jérôme Berthier, Alain Klotz, J. Moore, D. Samadov, A. Simon, Michael W. Coughlin, Jun Mo, A. Burrell, P. A. Duverne, C. Lachaud, K. Noysena, K. Barynova, Sergey Karpov, L. Eymar, N. Leroy, J. C. Chen, M. Vardosanidze, S. Beradze, D. Turpin, Frédéric Vachier, Shengyu Yan, P. Thierry, Nelson Christensen, O. A. Burkhonov, D. Morris, H. Crisp, C. Stachie, A. Peyrot, G. Marchal-Duval, S. Agayeva, R. Natsvlishvili, P. Fock-Hang, David Coward, E. Bertin, J. M. Bai, V. Vasylenko, and Xinrong Zhang, B. Chabert, X.F. Wang, Bruce Gendre, Weili Lin, M. Prouza, J.J. Zhang, Z. Vidadi, C. Wang, 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, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), 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), 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), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Université de Toulouse (UT), 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), GRANDMA, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Université Nice Sophia Antipolis (... - 2019) (UNS), 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), Université Fédérale Toulouse Midi-Pyrénées, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), and 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)

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Gravitational wave, Astrophysics::High Energy Astrophysical Phenomena, Astronomy, FOS: Physical sciences, General Medicine, law.invention, Telescope, law, Transient (oscillation), [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Neutrino, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

GRANDMA is an international project that coordinates telescope observations of transient sources with large localization uncertainties. Such sources include gravitational wave events, gamma-ray bursts and neutrino events. GRANDMA currently coordinates 25 telescopes (70 scientists), with the aim of optimizing the imaging strategy to maximize the probability of identifying an optical counterpart of a transient source. This paper describes the motivation for the project, organizational structure, methodology and initial results., 8 pages, to appear in Revista Lexicana de Astronomia y Astrofisica Conference Series

46. SPIDERS: the spectroscopic follow-up of X-ray selected clusters of galaxies in SDSS-IV

Author

Mara Salvato, Kirpal Nandra, Chris A. Collins, J. Ridl, Nicolas Clerc, T. Sadibekova, Joel R. Brownstein, Yen-Ting Lin, Jean-Paul Kneib, Yu-Ying Zhang, Eli S. Rykoff, Kyle S. Dawson, Matthias Steinmetz, Jeremy L. Tinker, Alexis Finoguenov, Hee-Jong Seo, Eduardo Rozo, Axel Schwope, Andrea Merloni, Tom Dwelly, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), and Department of Physics

Subjects
VELOCITY DISPERSIONS, Temperature function, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Library science, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, SCALING RELATIONS, 01 natural sciences, Observatory, 0103 physical sciences, XMM-LSS SURVEY, 010303 astronomy & astrophysics, catalogues, Astrophysics::Galaxy Astrophysics, Mathematics, QB, MASS FUNCTION, TEMPERATURE FUNCTION, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, ROSAT SURVEY, RICH CLUSTERS, OUTER REGIONS, Astronomy, Astronomy and Astrophysics, 115 Astronomy, Space science, Red shift, LUMINOSITY FUNCTION, galaxies: clusters: general, [SDU]Sciences of the Universe [physics], Space and Planetary Science, cosmology: observations, X-rays: galaxies: clusters, DIGITAL SKY SURVEY, National laboratory, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

SPIDERS (The SPectroscopic IDentification of eROSITA Sources) is a program dedicated to the homogeneous and complete spectroscopic follow-up of X-ray AGN and galaxy clusters over a large area ($\sim$7500 deg$^2$) of the extragalactic sky. SPIDERS is part of the SDSS-IV project, together with the Extended Baryon Oscillation Spectroscopic Survey (eBOSS) and the Time-Domain Spectroscopic Survey (TDSS). This paper describes the largest project within SPIDERS before the launch of eROSITA: an optical spectroscopic survey of X-ray selected, massive ($\sim 10^{14}$ to $10^{15}~M_{\odot}$) galaxy clusters discovered in ROSAT and XMM-Newton imaging. The immediate aim is to determine precise ($\Delta_z \sim 0.001$) redshifts for 4,000-5,000 of these systems out to $z \sim 0.6$. The scientific goal of the program is precision cosmology, using clusters as probes of large-scale structure in the expanding Universe. We present the cluster samples, target selection algorithms and observation strategies. We demonstrate the efficiency of selecting targets using a combination of SDSS imaging data, a robust red-sequence finder and a dedicated prioritization scheme. We describe a set of algorithms and work-flow developed to collate spectra and assign cluster membership, and to deliver catalogues of spectroscopically confirmed clusters. We discuss the relevance of line-of-sight velocity dispersion estimators for the richer systems. We illustrate our techniques by constructing a catalogue of 230 spectroscopically validated clusters ($0.031 < z < 0.658$), found in pilot observations. We discuss two potential science applications of the SPIDERS sample: the study of the X-ray luminosity-velocity dispersion ($L_X-\sigma$) relation and the building of stacked phase-space diagrams., Comment: 27 pages, 31 figures, 9 tables. Tables in electronic format are available from http://www.sdss.org. Submitted to MNRAS

47. Method of estimating time scales of the atmospheric piston and its application at Dome C (Antarctica).

Author

Kellerer A, Sarazin M, du Foresto VC, Agabi K, Aristidi E, and Sadibekova T

Abstract

Analysis of the first interferometric fringes recorded at Dome C, Antarctica are presented. Measurements were taken 31 January and 1 February 2005 during daytime. Our purpose in performing the analysis was to measure temporal fluctuations of the atmospheric piston, which are critical for interferometers, and determine their sensitivity. These scales are derived through the motion of the image that is formed in the focal plane of a Fizeau interferometer. We could establish a lower limit to the coherence time by studying the decay rate of correlation between successive fringes. Coherence times are measured to be larger than 10 ms, i.e., at least three times higher than the median coherence time measured at the site of Paranal (3.3 ms).

Published
2006
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