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1. Dark Energy Survey Year 1 Results: Wide Field Mass Maps via Forward Fitting in Harmonic Space

Author

B. Flaugher, Peter Doel, Michael Troxel, Ben Hoyle, H. T. Diehl, T. M. C. Abbott, David Bacon, E. J. Sanchez, Erin Sheldon, G. Gutierrez, I. Sevilla-Noarbe, N. Kuropatkin, L. N. da Costa, M. E. C. Swanson, Joshua A. Frieman, Peter Melchior, Douglas L. Tucker, Kyler Kuehn, K. Honscheid, Shantanu Desai, Matt J. Jarvis, J. Carretero, V. Scarpine, Jennifer L. Marshall, Sarah Bridle, Chihway Chang, G. Tarle, Stella Seitz, D. L. Hollowood, M. Smith, David J. James, Tesla E. Jeltema, Daniel Gruen, M. A. G. Maia, Alistair R. Walker, W. G. Hartley, Joe Zuntz, S. Serrano, B. Mawdsley, David J. Brooks, Pablo Fosalba, A. Roodman, Vinu Vikram, D. W. Gerdes, J. Annis, Marcos Lima, J. Gschwend, D. L. Burke, A. Carnero Rosell, E. Buckley-Geer, Robert A. Gruendl, A. A. Plazas, E. Suchyta, August E. Evrard, M. Gatti, Ramon Miquel, S. Samuroff, R. C. Smith, Niall Jeffrey, Juan Garcia-Bellido, E. Bertin, Eduardo Rozo, Flavia Sobreira, M. Carrasco Kind, Enrique Gaztanaga, J. De Vicente, 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), DES, Ministerio de Economía y Competitividad (España), European Commission, Generalitat de Catalunya, and UAM. Departamento de Física Teórica

Subjects
ST/S000550/1, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Large-scale structure of Universe, Library science, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, dark matter, gravitational lensing: weak, 0103 physical sciences, Dark matter, media_common.cataloged_instance, Weak, European union, 010303 astronomy & astrophysics, License, Publication, STFC, media_common, Physics, Matter, Harmonic space, 010308 nuclear & particles physics, business.industry, Non-Gaussianity, European research, Física, RCUK, Astronomy and Astrophysics, Galaxies, Des, Wide field, Cosmology, Alliance, Space and Planetary Science, Constraints, astro-ph.CO, large-scale structure of Universe, Resolution, business, weak [Gravitational lensing], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics, Minkowski Functionals
Abstract

We present new wide-field weak lensing mass maps for the Year 1 Dark Energy Survey (DES) data, generated via a forward fitting approach. This method of producing maps does not impose any prior constraints on the mass distribution to be reconstructed. The technique is found to improve the map reconstruction on the edges of the field compared to the conventional Kaiser–Squires method, which applies a direct inversion on the data; our approach is in good agreement with the previous direct approach in the central regions of the footprint. The mapping technique is assessed and verified with tests on simulations; together with the Kaiser–Squires method, the technique is then applied to data from the DES Year 1 data and the differences between the two methods are compared. We also produce the first DES measurements of the convergence Minkowski functionals and compare them to those measured in simulations., The DES data management system is supported by the National Science Foundation under Grant Numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015- 71825, ESP2015-66861, FPA2015-68048, SEV-2016-0588, SEV 2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciencia e Tecnologia (INCT) e-Universe (CNPq grant ˆ 465376/2014-2). This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics. The United States Government retains and the publisher, by accepting the article for publication, acknowledges that the United States Government retains a non-exclusive, paid-up, irrevocable, world-wide license to publish or reproduce the published form of this manuscript, or allow others to do so, for United States Government purposes.

Published
2020

2. Dark Energy Survey Year 1 results: Validation of weak lensing cluster member contamination estimates from P(z) decomposition

Author

M. Carrasco Kind, Marcos Lima, Enrique Gaztanaga, Joshua A. Frieman, Douglas L. Tucker, J. DeRose, Kyler Kuehn, D. L. Burke, Peter Doel, A. Carnero Rosell, I. Sevilla-Noarbe, H. T. Diehl, N. Kuropatkin, Daniel Thomas, E. Buckley-Geer, Robert A. Gruendl, Michael Schubnell, Melanie Simet, T. N. Varga, L. N. da Costa, A. K. Romer, David Brooks, M. E. C. Swanson, A. A. Plazas, K. Honscheid, J. Carretero, E. J. Sanchez, J. P. Dietrich, Juan Garcia-Bellido, David J. James, B. Flaugher, Pablo Fosalba, G. Gutierrez, Eli S. Rykoff, Eduardo Rozo, J. Annis, Thomas McClintock, Stella Seitz, Daniel Gruen, A. von der Linden, Tesla E. Jeltema, W. G. Hartley, J. De Vicente, V. Scarpine, Devon L. Hollowood, S. Serrano, E. Suchyta, August E. Evrard, Jennifer L. Marshall, C. B. D'Andrea, Shantanu Desai, D. W. Gerdes, Mathew Smith, Felipe Menanteau, Gregory Tarle, Christopher J. Miller, Yanxi Zhang, M. Costanzi, Ramon Miquel, Santiago Avila, Carlos E. Cunha, M. A. G. Maia, Risa H. Wechsler, Niall MacCrann, E. Bertin, J. Gschwend, Flavia Sobreira, M. March, R. L. C. Ogando, Peter Melchior, Ben Hoyle, 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), DES, Varga, T. N., Derose, J., Gruen, D., Mcclintock, T., Seitz, S., Rozo, E., Costanzi, M., Hoyle, B., Maccrann, N., Plazas, A. A., Rykoff, E. S., Simet, M., Von Der Linden, A., Wechsler, R. H., Annis, J., Avila, S., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Cunha, C. E., D'Andrea, C. B., Da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Evrard, A. E., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hollowood, D. L., Honscheid, K., James, D. J., Jeltema, T., Kuehn, K., Kuropatkin, N., Lima, M., Maia, M. A. G., March, M., Marshall, J. L., Melchior, P., Menanteau, F., Miller, C. J., Miquel, R., Ogando, R. L. C., Romer, A. K., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, D. L., and Zhang, Y.

Subjects
High energy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Higher education, FOS: Physical sciences, Library science, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, gravitational lensing: weak, Clusters: General [Galaxies], 0103 physical sciences, media_common.cataloged_instance, European union, Observation [Cosmology], 010303 astronomy & astrophysics, STFC, QC, media_common, Physics, 010308 nuclear & particles physics, business.industry, European research, RCUK, Astronomy and Astrophysics, observations [cosmology], Cosmology: Observations, Galaxies: Clusters: General, Gravitational lensing: weak, 13. Climate action, Space and Planetary Science, Research council, galaxies: clusters: general, cosmology: observations, Fundamental physics, Christian ministry, CLUSTERS, weak [Gravitational lensing], business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Weak lensing source galaxy catalogs used in estimating the masses of galaxy clusters can be heavily contaminated by cluster members, prohibiting accurate mass calibration. In this study we test the performance of an estimator for the extent of cluster member contamination based on decomposing the photometric redshift $P(z)$ of source galaxies into contaminating and background components. We perform a full scale mock analysis on a simulated sky survey approximately mirroring the observational properties of the Dark Energy Survey Year One observations (DES Y1), and find excellent agreement between the true number profile of contaminating cluster member galaxies in the simulation and the estimated one. We further apply the method to estimate the cluster member contamination for the DES Y1 redMaPPer cluster mass calibration analysis, and compare the results to an alternative approach based on the angular correlation of weak lensing source galaxies. We find indications that the correlation based estimates are biased by the selection of the weak lensing sources in the cluster vicinity, which does not strongly impact the $P(z)$ decomposition method. Collectively, these benchmarks demonstrate the strength of the $P(z)$ decomposition method in alleviating membership contamination and enabling highly accurate cluster weak lensing studies without broad exclusion of source galaxies, thereby improving the total constraining power of cluster mass calibration via weak lensing., Comment: 14 pages, 8 figures; submitted to MNNRAS

Published
2019

3. CLASH: Accurate Photometric Redshifts with 14 HST bands in Massive Galaxy Cluster Cores

Author

Marc Postman, William Schoenell, Italo Balestra, Adi Zitrin, Ofer Lahav, Y. Jimenez-Teja, D. D. Kelson, Tom Broadhurst, Genevieve J. Graves, Holland C. Ford, Massimo Meneghetti, Jack Sayers, Larry Bradley, Keiichi Umetsu, Stella Seitz, Elinor Medezinski, Saurabh Jha, Leopoldo Infante, Nicole G. Czakon, R. Lazkoz, D. Lemze, Claudio Grillo, Steven A. Rodney, W. Zheng, Megan Donahue, Mario Nonino, Adam G. Riess, Ole Host, Matthias Bartelmann, Dan Coe, Or Graur, Begoña Ascaso, Anton M. Koekemoer, Alberto Molino, D. Maoz, Leonidas A. Moustakas, Narciso Benítez, Piero Rosati, Amata Mercurio, Julian Merten, Rychard Bouwens, Stephanie Jouvel, S. Orgaz, Peter Melchior, 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 d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Ministerio de Ciencia e Innovación (España), European Commission, European Southern Observatory, Ministerio de Educación y Ciencia (España), Sao Paulo Research Foundation, 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, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, distances and redshifts galaxies [Galaxies], [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], intracluster medium [Clusters], FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, clusters: general [Galaxies], 01 natural sciences, NO, Photometry (optics), Galaxies: distances and redshifts, Clusters: intracluster medium, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Brightest cluster galaxy, 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, Photometric redshift, Physics, 010308 nuclear & particles physics, photometry [Galaxies], James Webb Space Telescope, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Ultraviolet: galaxies, Galaxies: photometry, Catalogues, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Galaxies: distances and redshifts galaxies, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies. [Ultraviolet], Galaxies: clusters: general, Galaxies: clusters: intracluster medium, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present accurate photometric redshifts for galaxies observed by the Cluster Lensing And Supernova survey with Hubble (CLASH). CLASH observed 25 massive galaxy cluster cores with the Hubble Space Telescope in 16 filters spanning 0.2-1.7 μm. Photometry in such crowded fields is challenging. Compared to our previously released catalogues, we make several improvements to the photometry, including smaller apertures, intracluster light subtraction, point spread function matching and empirically measured uncertainties. We further improve the Bayesian photometric redshift estimates by adding a redder elliptical template and by inflating the photometric uncertainties of the brightest galaxies. The resulting photometric redshift accuracies are dz/(1+z) ~ 0.8, 1.0 and 2.0 per cent for galaxies with I-band F814W AB magnitudes < 18, 20 and 23, respectively. These results are consistent with our expectations. They improve on our previously reported accuracies by a factor of 4 at the bright end and a factor of 2 at the faint end. Our new catalogue includes 1257 spectroscopic redshifts, including 382 confirmed cluster members. We also provide stellar mass estimates. Finally, we include lensing magnification estimates of background galaxies based on our public lens models. Our new catalogue of all 25 CLASH clusters is available via Mikulski Archive for Space Telescopes. The analysis techniques developed here will be useful in other surveys of crowded fields, including the Frontier Fields and surveys carried out with Javalambre-Physics of the Accelerated Universe Astrophysical Survey and James Webb Space Telescope.© 2017 The Authors., We acknowledge the financial support of the Brazilian funding agency FAPESP (Post-doc fellowship - process number 2014/11806-9). Likewise, we also acknowledge the Spanish Ministerio de Educacion y Ciencia through grant AYA2006-14056 BES-2007-16280. We acknowledge the financial support from the Spanish MICINN under the Consolider-Ingenio 2010 Program grant CSD2006-00070: First Science with the GTC. AM acknowledges the CEFCA (Centro de Estudios de Fisica del Cosmos de Aragon) and the IAA-CSIC (Instituto de Astrofisica de Andalucia) institutes for hosting him during the period 2015/2016. PR, MM, AMe and MN acknowledge the financial support from PRIN-INAF 2014 1.05.01.94.02. Likewise, AMacknowledges the STScI (Space Telescope Science Institute) for hosting him during 2010 AugustSeptember, 2011 June-August and 2016 July. We acknowledge the financial support of ESO since most of the spectroscopic redshifts used in the work were based on ESO VLT programme ID 186.A-0798. BA has received funding from the European Union's Horizon 2020 research and innovation programme under the Marie Sklodowska-Curie grant agreement no. 656354.

Published
2017

4. The Music Of Clash: Predictions On The Concentration-Mass Relation

Author

Tom Broadhurst, Elena Rasia, Gustavo Yepes, Piero Rosati, Alberto Molino, Amata Mercurio, Stefan Gottloeber, WeiKang Zheng, Italo Balestra, Larry Bradley, Stella Seitz, Andrea Biviano, Holland C. Ford, Narciso Benítez, J. Sayers, Marc Postman, Rychard Bouwens, Leonidas A. Moustakas, Adi Zitrin, Jason Rhodes, N. Czakon, D. Lemze, Jesús Vega, Massimo Meneghetti, Peter Melchior, Claudio Grillo, L. Infante, Ofer Lahav, S. Jouvel, Matthias Bartelmann, Carlo Giocoli, Keiichi Umetsu, John Moustakas, Elinor Medezinski, Mario Nonino, A. Monna, M. De Petris, Federico Sembolini, Anton M. Koekemoer, Stefano Ettori, Lauro Moscardini, Megan Donahue, Dan Coe, D. D. Kelson, J. Merten, AUTRES, Laboratorio Nacional de Fusión [Madrid], Asociación Euratom-CIEMAT, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), University of Michigan [Ann Arbor], University of Michigan System, 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), Academia Sinica Institute of Astronomy and Astrophysics (ASIAA), Academia Sinica, INAF - Osservatorio Astronomico di Trieste (OAT), Istituto Nazionale di Astrofisica (INAF), UCO/Lick Observatory, University of California [Santa Cruz] (UC Santa Cruz), University of California (UC)-University of California (UC), Dept. of Physics, University Park, Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA), Space Telescope Science Institute (STSci), Laboratoire de l'intégration, du matériau au système (IMS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut Polytechnique de Bordeaux-Centre National de la Recherche Scientifique (CNRS), 'Federico II' University of Naples Medical School, University of Bologna/Università di Bologna, Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Università degli Studi di Ferrara = University of Ferrara (UniFE), Department of Computer Science and Technology (CST), Tsinghua University [Beijing] (THU), M. Meneghetti, E. Rasia, J. Vega, J. Merten, M. Postman, G. Yepe, F. Sembolini, M. Donahue, S. Ettori, K. Umetsu, I. Balestra, M. Bartelmann, N. Benítez, A. Biviano, R. Bouwen, L. Bradley, T. Broadhurst, D. Coe, N. Czakon, M. De Petri, H. Ford, C. Giocoli, S. Gottlöber, C. Grillo, L. Infante, S. Jouvel, D. Kelson, A. Koekemoer, O. Lahav, D. Lemze, E. Medezinski, P. Melchior, A. Mercurio, A. Molino, L. Moscardini, A. Monna, J. Moustaka, L. A. Moustaka, M. Nonino, J. Rhode, P. Rosati, J. Sayer, S. Seitz, W. Zheng, A. Zitrin, École normale supérieure - Paris (ENS Paris), 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 California [Santa Cruz] (UCSC), University of California-University of California, Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], Centre National de la Recherche Scientifique (CNRS)-Institut Polytechnique de Bordeaux-Université Sciences et Technologies - Bordeaux 1, University of Bologna, and Università degli Studi di Ferrara (UniFE)

Subjects
Physics, [PHYS]Physics [physics], Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astronomy and Astrophysics, Function (mathematics), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, dark matter – galaxies: clusters: general – gravitation lensing: weak – gravitational lensing: strong, Collision, Measure (mathematics), Standard deviation, Redshift, dark matter, galaxies clusters, gravitation lensing weak and strong, Space and Planetary Science, Range (statistics), Cluster sampling, Halo, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present the results of a numerical study based on the analysis of the MUSIC-2 simulations, aimed at estimating the expected concentration-mass relation for the CLASH cluster sample. We study nearly 1400 halos simulated at high spatial and mass resolution, which were projected along many lines-of-sight each. We study the shape of both their density and surface-density profiles and fit them with a variety of radial functions, including the Navarro-Frenk-White, the generalised Navarro-Frenk-White, and the Einasto density profiles. We derive concentrations and masses from these fits and investigate their distributions as a function of redshift and halo relaxation. We use the X-ray image simulator X-MAS to produce simulated Chandra observations of the halos and we use them to identify objects resembling the X-ray morphologies and masses of the clusters in the CLASH X-ray selected sample. We also derive a concentration-mass relation for strong-lensing clusters. We find that the sample of simulated halos which resemble the X-ray morphology of the CLASH clusters is composed mainly by relaxed halos, but it also contains a significant fraction of un-relaxed systems. For such a sample we measure an average 2D concentration which is ~11% higher than found for the full sample of simulated halos. After accounting for projection and selection effects, the average NFW concentrations of CLASH clusters are expected to be intermediate between those predicted in 3D for relaxed and super-relaxed halos. Matching the simulations to the individual CLASH clusters on the basis of the X-ray morphology, we expect that the NFW concentrations recovered from the lensing analysis of the CLASH clusters are in the range [3-6], with an average value of 3.87 and a standard deviation of 0.61. Simulated halos with X-ray morphologies similar to those of the CLASH clusters are affected by a modest orientation bias., Comment: 21 pages, 16 figures, 3 tables, submitted to ApJ

Published
2014

5. Mining the gap: evolution of the magnitude gap in X-ray galaxy groups from the 3-square-degree XMM coverage of CFHTLS

Author

G. Erfanianfar, Eiichi Egami, M. Lerchster, H. J. McCracken, Yannick Mellier, Stella Seitz, M. J. Pereira, Paola Popesso, M. Mirkazemi, Masayuki Tanaka, T. Erben, Jean-Paul Kneib, Ghassem Gozaliasl, Habib G. Khosroshahi, Alexis Finoguenov, F. Brimioulle, Mara Salvato, D. M. Z. Jassur, 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
Physics, Active galactic nucleus, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Square degree, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Galaxy group, Magnitude (astronomy), Cluster (physics), Brightest cluster galaxy, Astrophysics::Galaxy Astrophysics
Abstract

International audience; We present a catalog of 129 X-ray galaxy groups, covering a redshift range 0.04 \textless z \textless 1.23, selected in the similar to 3 deg(2) part of the CFHTLS W1 field overlapping XMM observations performed under the XMM-LSS project. We carry out a statistical study of the redshift evolution out to redshift one of the magnitude gap between the first and the second brightest cluster galaxies of a well defined mass-selected group sample. We find that the slope of the relation between the fraction of groups and the magnitude gap steepens with redshift, indicating a larger fraction of fossil groups at lower redshifts. We find that 22.2 +/- 6% of our groups at z \textless= 0.6 are fossil groups. We compare our results with the predictions of three semi-analytic models based on the Millennium simulation. The intercept of the relation between the magnitude of the brightest galaxy and the value of magnitude gap becomes brighter with increasing redshift. This trend is steeper than the model predictions which we attribute to the younger stellar age of the observed brightest cluster galaxies. This trend argues in favor of stronger evolution of the feedback from active galactic nuclei at z \textless 1 compared to the models. The slope of the relation between the magnitude of the brightest cluster galaxy and the value of the gap does not evolve with redshift and is well reproduced by the models, indicating that the tidal galaxy stripping, put forward as an explanation of the occurrence of the magnitude gap, is both a dominant mechanism and sufficiently well modeled.

Published
2014

6. CLASH-VLT: The mass, velocity-anisotropy, and pseudo-phase-space density profiles of the z = 0.44 galaxy cluster MACS J1206.2-0847

Author

Stefano Ettori, Keiichi Umetsu, Italo Balestra, D. D. Kelson, Bodo L. Ziegler, Andrea Biviano, T. J. Broadhurst, Adi Zitrin, V. Strazzullo, Massimo Meneghetti, Claudio Grillo, M. Bartelmann, WeiKang Zheng, Marisa Girardi, U. Kuchner, P. Melchior, J. Merten, M. Annunziatella, Paolo Tozzi, Larry Bradley, E. Munari, E. Medezinski, R. Demarco, Mario Nonino, Massimo Brescia, Marco Scodeggio, V. Presotto, Piero Rosati, Raphael Gobat, G. Graves, Amata Mercurio, Holland C. Ford, Leonidas A. Moustakas, Marc Postman, D. Lemze, Barbara Sartoris, Marco Lombardi, Simona Mei, Megan Donahue, Christian Maier, Dan Coe, Anton M. Koekemoer, O. Czoske, Eniko Regos, A. Fritz, Stella Seitz, Narciso Benítez, INAF - Osservatorio Astronomico di Trieste (OAT), Istituto Nazionale di Astrofisica (INAF), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), 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, 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), Biviano, A., Rosati, P., Balestra, I., Mercurio, A., Girardi, Marisa, Nonino, M., Grillo, C., Scodeggio, M., Lemze, D., Kelson, D., Umetsu, K., Postman, M., Zitrin, A., Czoske, O., Ettori, S., Fritz, A., Lombardi, M., Maier, C., Medezinski, E., Mei, S., Presotto, Valentina, Strazzullo, V., Tozzi, P., Ziegler, B., Annunziatella, Marianna, Bartelmann, M., Benitez, N., Bradley, L., Brescia, M., Broadhurst, T., Coe, D., Demarco, R., Donahue, M., Ford, H., Gobat, R., Graves, G., Koekemoer, A., Kuchner, U., Melchior, P., Meneghetti, M., Merten, J., Moustakas, L., Munari, Emiliano, Regős, E., Sartoris, Barbara, Seitz, S., Zheng, W., 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), Girardi, M., Presotto, V., Annunziatella, M., Munari, E., Regos, E., and Sartoris, B.

Subjects
galaxy cluster, Astrophysics and Astronomy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Virial theorem, dark matter, 0103 physical sciences, galaxy clusters, Cluster (physics), galaxy kinematics and dynamics, Anisotropy, 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, galaxies: kinematics and dynamics, Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Radius, Galaxy, Redshift, galaxy kinematics and dynamic, galaxies: clusters: individual: MACS J1206-0847, Gravitational lens, Space and Planetary Science, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We use an unprecedented data-set of about 600 redshifts for cluster members, obtained as part of a VLT/VIMOS large programme, to constrain the mass profile of the z=0.44 cluster MACS J1206.2-0847 over the radial range 0-5 Mpc (0-2.5 virial radii) using the MAMPOSSt and Caustic methods. We then add external constraints from our previous gravitational lensing analysis. We invert the Jeans equation to obtain the velocity-anisotropy profiles of cluster members. With the mass-density and velocity-anisotropy profiles we then obtain the first determination of a cluster pseudo-phase-space density profile. The kinematics and lensing determinations of the cluster mass profile are in excellent agreement. This is very well fitted by a NFW model with mass M200=(1.4 +- 0.2) 10^15 Msun and concentration c200=6 +- 1, only slightly higher than theoretical expectations. Other mass profile models also provide acceptable fits to our data, of (slightly) lower (Burkert, Hernquist, and Softened Isothermal Sphere) or comparable (Einasto) quality than NFW. The velocity anisotropy profiles of the passive and star-forming cluster members are similar, close to isotropic near the center and increasingly radial outside. Passive cluster members follow extremely well the theoretical expectations for the pseudo-phase-space density profile and the relation between the slope of the mass-density profile and the velocity anisotropy. Star-forming cluster members show marginal deviations from theoretical expectations. This is the most accurate determination of a cluster mass profile out to a radius of 5 Mpc, and the only determination of the velocity-anisotropy and pseudo-phase-space density profiles of both passive and star-forming galaxies for an individual cluster [abridged], A&A in press; 22 pages, 19 figures

Published
2013

7. CLASH: THE ENHANCED LENSING EFFICIENCY OF THE HIGHLY ELONGATED MERGING CLUSTER MACS J0416.1–2403

Author

Adi Zitrin, Stella Seitz, Piero Rosati, Mario Nonino, Mauricio Carrasco, Marc Postman, Tom Broadhurst, Larry Bradley, Xinwen Shu, Irene Sendra, Keiichi Umetsu, H. Ford, Wei Zheng, Elinor Medezinski, Jesús Vega, Massimo Meneghetti, Leonidas A. Moustakas, Anton M. Koekemoer, Daniel D. Kelson, Gregor Seidel, Dan Coe, Rychard Bouwens, Matthias Bartelmann, John Moustakas, Institut des Sciences Chimiques de Rennes (ISCR), Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC)-Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Ecole Nationale Supérieure de Chimie de Rennes (ENSCR)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Université de Rennes (UNIV-RENNES)-Institut National des Sciences Appliquées (INSA), Academia Sinica Institute of Astronomy and Astrophysics (ASIAA), Academia Sinica, UCO/Lick Observatory, University of California [Santa Cruz] (UCSC), University of California-University of California, Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), Space Telescope Science Institute (STSci), INAF - Osservatorio Astronomico di Trieste (OAT), Istituto Nazionale di Astrofisica (INAF), European Southern Observatory (ESO), 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), Laboratorio Nacional de Fusión [Madrid], Asociación Euratom-CIEMAT, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Institute of High Energy Physics (IHEP), Chinese Academy of Sciences [Changchun Branch] (CAS), Université de Rennes (UR)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Ecole Nationale Supérieure de Chimie de Rennes (ENSCR)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), University of California [Santa Cruz] (UC Santa Cruz), University of California (UC)-University of California (UC), 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), and École normale supérieure - Paris (ENS-PSL)

Subjects
Physics, [PHYS]Physics [physics], Range (particle radiation), Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Collision, 01 natural sciences, Space and Planetary Science, 0103 physical sciences, Cluster (physics), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Galaxy cluster, ComputingMilieux_MISCELLANEOUS, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We perform a strong-lensing analysis of the merging galaxy cluster MACS J0416.1-2403 (M0416; z=0.42) in recent CLASH/HST observations. We identify 70 new multiple images and candidates of 23 background sources in the range 0.76 x 10^{14} h^{-1}M_{\odot}) exhibit as elongated critical curves as M0416., Comment: 7 pages, 4 figures, 1 table. V2: accepted to ApJ Letters; minor changes and updates; in Fig.3 labeling error corrected. Mass models available online: ftp://wise-ftp.tau.ac.il/pub/adiz/M0416/

Published
2013

8. The Wendelstein Calar Alto Pixellensing Project (WeCAPP): the M 31 nova catalogue

Author

Ulrich Hopp, R. Bender, C. Ries, Otto Baernbantner, Chien-Hsiu Lee, C. Goessl, Stella Seitz, A. Riffeser, Juergen Fliri, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), and Ludwig-Maximilians-Universität München (LMU)

Subjects
Physics, [PHYS]Physics [physics], 010504 meteorology & atmospheric sciences, Dark matter, FOS: Physical sciences, Astronomy and Astrophysics, Nova (laser), Astrophysics, Light curve, Gravitational microlensing, Astrophysics - Astrophysics of Galaxies, 01 natural sciences, Highly sensitive, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Imaging technique, Halo, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences
Abstract

We present light curves from the novae detected in the long-term, M31 monitoring WeCAPP project. The goal of WeCAPP is to constrain the compact dark matter fraction of the M31 halo with microlensing observations. As a by product we have detected 91 novae benefiting from the high cadence and highly sensitive difference imaging technique required for pixellensing. We thus can now present the largest CCD and optical filters based nova light curve sample up-to-date towards M31. We also obtained thorough coverage of the light curve before and after the eruption thanks to the long-term monitoring. We apply the nova taxonomy proposed by Strope et al. (2010) to our nova candidates and found 29 S-class novae, 10 C-class novae, 2 O-class novae and 1 J-class nova. We have investigated the universal decline law advocated by Hachichu and Kato (2006) on the S-class novae. In addition, we correlated our catalogue with the literature and found 4 potential recurrent novae. Part of our catalogue has been used to search for optical counter-parts of the super soft X-ray sources detected in M31 (Pietsch et al. 2005). Optical surveys like WeCAPP, and coordinated with multi-wavelength observation, will continue to shed light on the underlying physical mechanism of novae in the future., Comment: 15 pages, 15 figures, 7 tables, A&A accepted for publication. The appendix is stored in the Data Conservancy

Published
2012

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