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1. J-PLUS: Morphological star/galaxy classification by PDF analysis

Author

Paula Coelho, Alberto Molino, Jesús A. Varela, D. Spinoso, David Cristóbal-Hornillos, Ana L. Chies-Santos, C. Hernández-Monteagudo, Devin D. Whitten, R. Logroño-García, C. Mendes de Oliveira, I. San Roman, Lluís Galbany, A. J. Cenarro, M. V. Costa-Duarte, B. Ascaso, Arianna Cortesi, C. López-Sanjuan, Laerte Sodré, L. Sampedro, S. Bonoli, D. Muniesa, G. Vilella-Rojo, Mariano Moles, L. A. Díaz-García, Kerttu Viironen, Vinicius M. Placco, Antonio Marín-Franch, Alessandro Ederoclite, Raul E. Angulo, Alvaro Orsi, R. A. Dupke, H. Vázquez Ramió, 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 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), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Observatoire de Paris, and 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)

Subjects
Be star, media_common.quotation_subject, Milky Way, Magnitude (mathematics), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Star (graph theory), 01 natural sciences, Naive Bayes classifier, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, galaxies: statistics, media_common, Physics, [PHYS]Physics [physics], Galaxy: stellar content, 010308 nuclear & particles physics, OBSERVATÓRIOS, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, methods: data analysis, Galaxy, Stars, Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA)
Abstract

Our goal is to morphologically classify the sources identified in the images of the J-PLUS early data release (EDR) into compact (stars) or extended (galaxies) using a suited Bayesian classifier. J-PLUS sources exhibit two distinct populations in the r-band magnitude vs. concentration plane, corresponding to compact and extended sources. We modelled the two-population distribution with a skewed Gaussian for compact objects and a log-normal function for the extended ones. The derived model and the number density prior based on J-PLUS EDR data were used to estimate the Bayesian probability of a source to be star or galaxy. This procedure was applied pointing-by-pointing to account for varying observing conditions and sky position. Finally, we combined the morphological information from g, r, and i broad bands in order to improve the classification of low signal-to-noise sources. The derived probabilities are used to compute the pointing-by-pointing number counts of stars and galaxies. The former increases as we approach to the Milky Way disk, and the latter are similar across the probed area. The comparison with SDSS in the common regions is satisfactory up to r ~ 21, with consistent numbers of stars and galaxies, and consistent distributions in concentration and (g - i) colour spaces. We implement a morphological star/galaxy classifier based on PDF analysis, providing meaningful probabilities for J-PLUS sources to one magnitude deeper (r ~ 21) than a classical boolean classification. These probabilities are suited for the statistical study of 150k stars and 101k galaxies with 15 < r < 21 present in the 31.7 deg2 of the J-PLUS EDR. In a future version of the classifier, we will include J-PLUS colour information from twelve photometric bands., Submitted to Astronomy and Astrophysics. 14 pages, 16 figures, 1 tables. Comments are welcome. All extra figures and the number counts files will be available with the paper in press

Published
2019

2. The ALHAMBRA survey: tight dependence of the optical mass-to-light ratio on galaxy colour up to z = 1.5

Author

A. del Olmo, Alberto Fernández-Soto, C. Husillos, J. Perea, I. Márquez, C. López-Sanjuan, Pablo Arnalte-Mur, Alberto Molino, Mirjana Pović, David Cristóbal-Hornillos, Francisco J. Castander, Kerttu Viironen, Jesús A. Varela, A. J. Cenarro, Mariano Moles, Miguel Cerviño, L. A. Díaz-García, R. M. González Delgado, Narciso Benítez, B. Ascaso, J. Masegosa, AstroParticule et Cosmologie (APC (UMR_7164)), 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), Ministry of Science and Technology (Ethiopia), Governo Brasil, Generalitat de Catalunya, Junta de Andalucía, Generalitat Valenciana, European Commission, Fundación Agencia Aragonesa para la Investigación y el Desarrollo, Ministerio de Ciencia e Innovación (España), Fondo de Inversiones de Teruel, 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), 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), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)

Subjects
Research groups, Library science, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, statistics [Galaxies], 0103 physical sciences, media_common.cataloged_instance, Astrophysics::Solar and Stellar Astrophysics, European union, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, galaxies: statistics, media_common, Funding Agency, Physics, [PHYS]Physics [physics], 010308 nuclear & particles physics, Astronomy and Astrophysics, galaxies: fundamental parameters, Astrophysics - Astrophysics of Galaxies, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), fundamental parameters [Galaxies], galaxies: stellar content, stellar content [Galaxies], Christian ministry
Abstract

[Aims] Our goal is to characterise the dependence of the optical mass-to-light ratio on galaxy colour up to z = 1.5, expanding the redshift range explored in previous work. [Methods] From the redshifts, stellar masses, and rest-frame luminosities of the ALHAMBRA multi-filter survey, we derive the mass-to-light ratio versus colour relation for quiescent and for star-forming galaxies. The intrinsic relation and its physical dispersion are derived with a Bayesian inference model. [Results] The rest-frame i-band mass-to-light ratio of quiescent and star-forming galaxies presents a tight correlation with the rest-frame (g - i) colour up to z = 1.5. The mass-to-light ratio versus colour relation is linear for quiescent galaxies and quadratic for star-forming galaxies. The intrinsic dispersion in these relations is 0.02 dex for quiescent galaxies and 0.06 dex for star-forming ones. The derived relations do not present a significant redshift evolution and are compatible with previous local results in the literature. Finally, these tight relations also hold for g- and r-band luminosities. [Conclusions] The derived mass-to-light ratio versus colour relations in ALHAMBRA can be used to predict the mass-to-light ratio from a rest-frame optical colour up to z = 1.5. These tight correlations do not change with redshift, suggesting that galaxies have evolved along the derived relations during the last 9 Gyr., This work has been mainly funded by the FITE (Fondos de Inversiones de Teruel) and the Spanish MINECO/FEDER projects AYA2015-66211-C2-1-P, AYA2012-30789, AYA2006-14056, and CSD2007-00060. We also acknowledge the financial support from the Aragón Government Research Groups E96, E103, and E16_17R. We acknowledge support from the Spanish Ministry for Economy and Competitiveness and FEDER funds through grants AYA2010-15081, AYA2010-22111-C03-01, AYA2010-22111-C03-02, AYA2012-39620, AYA2013-40609-P, AYA2013-42227-P, AYA2013-48623-C2-1, AYA2013-48623-C2-2, AYA2016-76682-C3-1-P, AYA2016-76682-C3-3-P, ESP2013-48274, Generalitat Valen-ciana project Prometeo PROMETEOII/2014/060, Junta de Andalucía grants TIC114, JA2828, P10-FQM-6444, and Generalitat de Catalunya project SGR-1398. K.V. acknowledges the Juan de la Cierva incorporación fellowship, IJCI-2014-21960, of the Spanish government. A.M. acknowledges the financial support of the Brazilian funding agency FAPESP (Post-doc fellowship - process number 2014/11806-9). B.A. has received funding from the European Union’s Horizon 2020 research and innovation programme under the Marie Sklodowska-Curie grant agreement No. 656354. M.P. acknowledges financial support from the Ethiopian Space Science and Technology Institute (ESSTI) under the Ethiopian Ministry of Science Science and Technology (MoST).

Published
2019

3. High redshift galaxies in the ALHAMBRA survey. II. Strengthening the evidence of bright-end excess in UV luminosity functions at 2.5 <= z<= 4.5 by PDF analysis

Author

A. J. Cenarro, Mirjana Pović, Francisco Prada, A. del Olmo, Mariano Moles, Alberto Fernández-Soto, Alberto Molino, J. Varela, J. M. Quintana, C. Hernández-Monteagudo, Miguel Cerviño, Vivian Martínez, Narciso Benítez, Emilio J. Alfaro, I. Márquez, J. Masegosa, C. Husillos, Tom Broadhurst, Kerttu Viironen, L. A. Díaz-García, T. Aparicio-Villegas, Jonás Chaves-Montero, Jesús Cabrera-Caño, R. M. González Delgado, Jaime Perea, C. López-Sanjuan, J. A. L. Aguerri, B. Ascaso, Leopoldo Infante, S. Bonoli, Francisco J. Castander, David Cristóbal-Hornillos, J. Cepa, 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), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Spanish National Research Council (CSIC), Laboratoire Leprince-Ringuet (LLR), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Services communs OMP (UMS 831), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), 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), AUTRES, Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), 'Federico II' University of Naples Medical School, INTA - Instituto Nacional de Tecnología Agropecuaria, Instituto de Física Teórica UAM/CSIC (IFT), Universidad Autonoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Services communs OMP - UMS 831 (UMS 831), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Universidad Autonoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), 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), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), 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), Universidad Autónoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Generalitat Valenciana, Junta de Andalucía, Generalitat de Catalunya, Fundación Agencia Aragonesa para la Investigación y el Desarrollo, Fondo de Inversiones de Teruel, European Commission, Ministry of Science and Technology (Ethiopia), and Ministerio de Economía y Competitividad (España)

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Context (language use), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, high-redshift [Galaxies], galaxies: high-redshift, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Luminosity function (astronomy), Physics, [PHYS]Physics [physics], 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, Cosmic variance, evolution [Galaxies], Astrophysics - Astrophysics of Galaxies, luminosity function [Galaxies], Redshift, Galaxy, Dark matter halo, galaxies: luminosity function, Space and Planetary Science, mass function, Mass function, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

Context. Knowing the exact shape of the ultraviolet (UV) luminosity function (LF) of high-redshift galaxies is important to understand the star formation history of the early Universe. However, the uncertainties, especially at the faint and bright ends of the LFs, remain significant. Aims. In this paper, we study the UV LF of redshift z = 2:5 4.5 galaxies in 2.38 deg of ALHAMBRA data with I ≤ 24. Thanks to the large area covered by ALHAMBRA, we particularly constrain the bright end of the LF. We also calculate the cosmic variance and the corresponding bias values for our sample and derive their host dark matter halo masses. Methods.We have used a novel methodology based on redshift and magnitude probability distribution functions (PDFs). This methodology robustly takes into account the uncertainties due to redshift and magnitude errors, shot noise, and cosmic variance, and models the LF in two dimensions (z; M). Results. We find an excess of bright ∼M∗ galaxies as compared to the studies based on broad-band photometric data. However, our results agree well with the LF of the magnitude-selected spectroscopic VVDS data. We measure high bias values, b ∼ 8 10, that are compatible with the previous measurements considering the redshifts and magnitudes of our galaxies and further reinforce the real high-redshift nature of our bright galaxies. Conclusions. We call into question the shape of the LF at its bright end; is it a double power-law as suggested by the recent broadband photometric studies or rather a brighter Schechter function, as suggested by our multi-filter analysis and the spectroscopic VVDS data.© ESO 2018., K. Viironen acknowledges the >Juan de la Cierva incorporacion> fellowship, IJCI-2014-21960, of the Spanish government. This work has mainly been funded by the FITE (Fondos de Inversiones de Teruel) and the projects AYA2015-66211-C2-1 and AYA2012-30789. We also acknowledge support from the Aragon Government Research Group E103 and support from the Spanish Ministry for Economy and Competitiveness and FEDER funds through grants AYA2010-15081, AYA2010-15169, AYA2010-22111-C03-01, AYA2010-22111-C03-02, AYA2011-29517-C03-01, AYA2012-39620, AYA2013-40611-P, AYA2013-42227-P, AYA2013-43188-P, AYA2013-48623-C2-1, AYA2013-48623-C2-2, ESP2013-48274, AYA2014-58861-C3-1, AYA2016-76682-C3-1-P, Generalitat Valenciana projects Prometeo 2009/064 and PROMETEOII/2014/060, Junta de Andalucia grants TIC114, JA2828, P10-FQM-6444, and Generalitat de Catalunya project SGR-1398. BA has received funding from the European Union's Horizon 2020 research and innovation programme under the Marie Sklodowska-Curie grant agreement No 656354. MP acknowledges financial supports from the Ethiopian Space Science and Technology Institute (ESSTI) under the Ethiopian Ministry of Science Science and Technology (MoST)

Published
2018

4. 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

5. THE ALHAMBRA SURVEY: EVOLUTION OF GALAXY SPECTRAL SEGREGATION

Author

Mirjana Pović, Francisco J. Castander, Tom Broadhurst, Narciso Benítez, Emilio J. Alfaro, T. Aparicio-Villegas, A. del Olmo, Leopoldo Infante, David Cristóbal-Hornillos, J. Cepa, Pablo Arnalte-Mur, J. A. L. Aguerri, Ll. Hurtado-Gil, Silvestre Paredes, C. Husillos, Francisco Prada, Jesús Cabrera-Caño, Jaime Perea, Vicent J. Martínez, R. M. González Delgado, C. López-Sanjuan, Alberto Molino, Kerttu Viironen, Miguel Cerviño, Mariano Moles, I. Márquez, J. Masegosa, B. Ascaso, Mauro Stefanon, Alberto Fernández-Soto, J. M. Quintana, Department of Chemistry and Institute for Nanoscale Physics and chemistry (INPAC), Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), Spanish National Research Council (CSIC), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), 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), 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), AUTRES, Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), 'Federico II' University of Naples Medical School, Instituto de Física Teórica UAM/CSIC (IFT), Universidad Autonoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Universidad de Sevilla. Departamento de Física Atómica, Molecular y Nuclear, Ministerio de Economía y Competitividad (MINECO). España, Junta de Andalucía, 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, 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), Universidad Autónoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), European Commission, Ministerio de Economía y Competitividad (España), Generalitat Valenciana, Generalitat de Catalunya, 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), PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Universidad Autonoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), and UAM. Departamento de Física Teórica

Subjects
statistical [Methods], Cosmology and Nongalactic Astrophysics (astro-ph.CO), Large-scale structure of universe, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Methods statistical, Galaxies: distances and redshifts, Methods: data analysis, 0103 physical sciences, distances and redshifts [Galaxies], observations [Cosmology], data analysis [Methods], 010303 astronomy & astrophysics, Methods: statistical, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, Physics, [PHYS]Physics [physics], 010308 nuclear & particles physics, Cosmology: observations, Física, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

arXiv:1601.03668v1, We study the clustering of galaxies as a function of spectral type and redshift in the range 0.35, This work was mainly supported by the Spanish Ministry for Economy and Competitiveness and FEDER funds through grants AYA2010-22111-C03-02 and AYA2013-48623-C2-2, and by the Generalitat Valenciana through project PrometeoII 2014/060. We also acknowledge support from the Spanish Ministry for Economy and Competitiveness and FEDER funds through grants AYA2012-39620, AYA2013-40611-P, AYA2013-42227-P, AYA2013-43188-P, AYA2013-48623-C2-1, ESP2013-48274, AYA2014-58861-C3-1, Junta de Andalucia grants TIC114, JA2828, P10-FQM-6444, and Generalitat de Catalunya project SGR-1398. Begona Ascaso acknowledge funding from the European Union's Horizon 2020 research and innovation program under the Marie Sklodowska-Curie grant agreement No. 656354.

Published
2016

6. An accurate cluster selection function for the J-PAS narrow-band wide-field survey

Author

Tom Broadhurst, G.B. Lima-Neto, Carlos López-Sanjuan, C. Mendes de Oliveira, C. Hernández-Monteagudo, B. Ascaso, Simona Mei, R. A. Dupke, Alberto Molino, Carlos A. Fernandes, Jesús A. Varela, L. A. Díaz-García, J. S. Alcaniz, Narciso Benítez, A. J. Cenarro, William Schoenell, Antonio Marin-Franch, Eduardo Serra Cypriano, Kerttu Viironen, Ivan Oteo, L. Sodré, N. Chandrachani Devi, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), 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), Centre for Environmental Biology, Lisbon University, Universidade de Lisboa (ULISBOA), 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), 'Federico II' University of Naples Medical School, Institute for Astronomy [Edinburgh] (IfA), University of Edinburgh, Ministerio de Economía y Competitividad (España), European Research Council, Conselho Nacional de Desenvolvimento Científico e Tecnológico (Brasil), 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), 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), Universidade de Lisboa = University of Lisbon (ULISBOA), and École normale supérieure - Paris (ENS-PSL)

Subjects
General - cosmology, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Dark matter, Planck mass, FOS: Physical sciences, Astrophysics, 01 natural sciences, Clusters, 0103 physical sciences, Cluster (physics), Observations - dark matter - large-scale structure of Universe, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Physics, [PHYS]Physics [physics], 010308 nuclear & particles physics, Astronomy and Astrophysics, Observable, Function (mathematics), Surveys - galaxies, Wide field, Redshift, Narrow band, Miscellaneous - cosmology, Space and Planetary Science, ESTRUTURA DO UNIVERSO, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The impending Javalambre Physics of the accelerating Universe Astrophysical Survey (J-PAS) will be the first wide-field survey of ≳ 8500 deg2 to reach the 'stage IV' category. Because of the redshift resolution afforded by 54 narrow-band filters, J-PAS is particularly suitable for cluster detection in the range z80 per cent completeness and purity is M ~ 5 × 10M⊙ up to z ~ 0.7. We also model the optical observable, M-halo mass relation, finding a non-evolution with redshift and main scatter of σM|M ~ 0.14 dex down to a factor 2 lower in mass than other planned broad-band stage IV surveys, at least. For the M ~ 1 × 10M⊙ Planck mass limit, J-PAS will arrive up to z ~ 0.85 with a σM|M ~ 0.12 dex. Therefore, J-PAS will provide the largest sample of clusters and groups up to z ~ 0.8 with a mass calibration accuracy comparable to X-ray data. © 2016 The Authors., EC, GLN, CMdO, AM and LS acknowledge funding from PAPESP and CNPq. IO acknowledges support from the European Research Council (ERC) in the form of Advanced Grant, COSMICISM. We acknowledge support from the Spanish Ministry for Economy and Competitiveness through grants ilink0862 and AYA2013-48623-C02-1-P.

Published
2016

7. The ALHAMBRA survey: Estimation of the clustering signal encoded in the cosmic variance

Author

Vicent J. Martínez, C. Hernández-Monteagudo, Kerttu Viironen, A. del Olmo, Mariano Moles, A. J. Cenarro, Alberto Fernández-Soto, Mirjana Pović, T. Aparicio-Villegas, J. M. Quintana, Leopoldo Infante, B. Ascaso, Emilio J. Alfaro, Alberto Molino, Miguel Cerviño, J. Varela, David Cristóbal-Hornillos, J. Cepa, Ll. Hurtado-Gil, Jaime Perea, L. A. Díaz-García, Narciso Benítez, Francisco Prada, I. Márquez, Tom Broadhurst, R. M. González Delgado, Francisco J. Castander, Pablo Arnalte-Mur, C. Husillos, J. A. L. Aguerri, J. Masegosa, Jesús Cabrera-Caño, C. López-Sanjuan, 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), Spanish National Research Council (CSIC), 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), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), 'Federico II' University of Naples Medical School, INTA - Instituto Nacional de Tecnología Agropecuaria, Instituto de Astrofisica de Canarias (IAC), Centro de Astrobiologia [Madrid] (CAB), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), Instituto de Física Teórica UAM/CSIC (IFT), Universidad Autonoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Gobierno de Aragón, Generalitat Valenciana, Junta de Andalucía, European Commission, Ministerio de Economía y Competitividad (España), Generalitat de Catalunya, Fondo de Inversiones de Teruel, Fundação de Amparo à Pesquisa do Estado de São Paulo, Consejo Superior de Investigaciones Científicas (España), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), and Universidad Autónoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Dark matter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Correlation function (astronomy), 01 natural sciences, Luminosity, Statistics [Galaxies], 0103 physical sciences, Statistical dispersion, Cluster analysis, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, Physics, [PHYS]Physics [physics], 010308 nuclear & particles physics, Astronomy and Astrophysics, Cosmic variance, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Galaxies: Statistics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

[Aims]: The relative cosmic variance (σv) is a fundamental source of uncertainty in pencil-beam surveys and, as a particular case of count-in-cell statistics, can be used to estimate the bias between galaxies and their underlying dark-matter distribution. Our goal is to test the significance of the clustering information encoded in the σv measured in the ALHAMBRA survey. [Methods]: We measure the cosmic variance of several galaxy populations selected with B-band luminosity at 0.35 ≤ z< 1.05 as the intrinsic dispersion in the number density distribution derived from the 48 ALHAMBRA subfields. We compare the observational σv with the cosmic variance of the dark matter expected from the theory, σv,dm. This provides an estimation of the galaxy bias b. [Results]: The galaxy bias from the cosmic variance is in excellent agreement with the bias estimated by two-point correlation function analysis in ALHAMBRA. This holds for different redshift bins, for red and blue subsamples, and for several B-band luminosity selections. We find that b increases with the B-band luminosity and the redshift, as expected from previous work. Moreover, red galaxies have a larger bias than blue galaxies, with a relative bias of brel = 1.4 ± 0.2. [Conclusions]: Our results demonstrate that the cosmic variance measured in ALHAMBRA is due to the clustering of galaxies and can be used to characterise the σv affecting pencil-beam surveys. In addition, it can also be used to estimate the galaxy bias b from a method independent of correlation functions., This work has been mainly funded by the FITE (Fondos de Inversiones de Teruel) and the projects AYA2012-30789, AYA2006-14056, and CSD2007-00060. We also acknowledge support from the Spanish Ministry for Economy and Competitiveness and FEDER funds through grants AYA2010-15081, AYA2010-15169, AYA2010-22111-C03-01, AYA2010-22111-C03-02, AYA2011-29517-C03-01, AYA2012-39620, AYA2013-40611-P, AYA2013-42227-P, AYA2013-43188-P, AYA2013-48623-C2-1, AYA2013-48623-C2-2, ESP2013-48274, AYA2014-58861-C3-1, Aragon Government Research Group E103, Generalitat Valenciana projects Prometeo 2009/064 and PROMETEOII/2014/060, Junta de Andalucia grants TIC114, JA2828, P10-FQM-6444, and Generalitat de Catalunya project SGR-1398. A.J.C. and C.H.-M. are Ramon y Cajal fellows of the Spanish government. A. M. acknowledges the financial support of the Brazilian funding agency FAPESP (Post-doc fellowship - process number 2014/11806-9). M.P. acknowledges financial support from JAE-Doc program of the Spanish National Research Council (CSIC), co-funded by the European Social Fund.

Published
2015

8. Galaxy clusters and groups in the ALHAMBRA survey

Author

J. M. Quintana, Narciso Benítez, A. J. Cenarro, David Cristóbal-Hornillos, Emilio J. Alfaro, Carlos López-Sanjuan, R. A. Dupke, Alberto Molino, Ll. Hurtado-Gil, Jesús A. Varela, Vicent J. Martínez, C. Husillos, Marc Huertas-Company, B. Ascaso, Francisco Prada, Jesús Cabrera-Caño, L. Nieves-Seoane, Tom Broadhurst, Kerttu Viironen, Yolanda Jiménez-Teja, A. del Olmo, Mirjana Pović, Jaime Perea, J. Masegosa, Leopoldo Infante, T. Aparício-Villegas, A. Fernández-Soto, Pablo Arnalte-Mur, J. A. L. Aguerri, L. A. Díaz-García, R. M. González Delgado, J. Cepa, Francisco J. Castander, Alex Merson, I. Márquez, Miguel Cerviño, William Schoenell, Mariano Moles, 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), Spanish National Research Council (CSIC), 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), 'Federico II' University of Naples Medical School, Department of Chemistry and Institute for Nanoscale Physics and chemistry (INPAC), Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), 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, Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), AUTRES, Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Instituto de Física Teórica UAM/CSIC (IFT), Universidad Autónoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Universidad Autonoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Universidad de Sevilla. Departamento de Física Atómica, Molecular y Nuclear, Gobierno de Aragón, Generalitat Valenciana, Consejo Superior de Investigaciones Científicas (España), European Commission, Ministerio de Economía y Competitividad (España), European Research Council, and Junta de Andalucía

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Large-scale structure of Universe, FOS: Physical sciences, Astrophysics, X-rays galaxies clusters, clusters: general [Galaxies], Galaxies clusters general, observations [Cosmology], Galaxy cluster, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Cosmology: observations, Física, Astronomy, Galaxies: evolution, Astronomy and Astrophysics, evolution [Galaxies], Cosmology observations, Catalogues, Galaxies evolution, Space and Planetary Science, [SDU]Sciences of the Universe [physics], X-rays: galaxies: clusters, galaxies: clusters [X-rays], Galaxies: clusters: general, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Ascaso, Begoña et al., We present a catalogue of 348 galaxy clusters and groups with 0.2 < z < 1.2 selected in the 2.78 deg2 Advanced Large, Homogeneous Area Medium Band Redshift Astronomical (ALHAMBRA) survey. The high precision of our photometric redshifts, close to 1 per cent, and the wide spread of the seven ALHAMBRA pointings ensure that this catalogue has better mass sensitivity and is less affected by cosmic variance than comparable samples. The detection has been carried out with the Bayesian Cluster Finder, whose performance has been checked in ALHAMBRA-like light-cone mock catalogues. Great care has been taken to ensure that the observable properties of the mocks photometry accurately correspond to those of real catalogues. From our simulations, we expect to detect galaxy clusters and groups with both 70 per cent completeness and purity down to dark matter halo masses of Mh ∼ 3 × 1013 M⊙ for z < 0.85. Cluster redshifts are expected to be recovered with ∼0.6 per cent precision for z < 1. We also expect to measure cluster masses with σMh|M∗CL∼0.25-0.35dexσMh|MCL∗∼0.25-0.35dex precision down to ∼ 3 × 1013 M⊙, masses which are 50 per cent smaller than those reached by similar work. We have compared these detections with previous optical, spectroscopic and X-rays work, finding an excellent agreement with the rates reported from the simulations. We have also explored the overall properties of these detections such as the presence of a colour–magnitude relation, the evolution of the photometric blue fraction and the clustering of these sources in the different ALHAMBRA fields. Despite the small numbers, we observe tentative evidence that, for a fixed stellar mass, the environment is playing a crucial role at lower redshifts (z < 0.5)., We acknowledge support from the Spanish Ministry for Economy and Competitiveness and FEDER funds through grants AYA2010-22111-C03-02, AYA2010-15169, AYA2012-30789, AYA2013-48623-C2-2, AYA2013-42227-P, AYA2013-40611-P, AYA2011-29517-C03-01, AYA2014-58861-C3-1, AYA2010-15081, Generalitat Valenciana projects PROMETEOII/2014/060, Junta de Andalucia grant TIC114, JA2828, Aragon Gorvernment-Research Group E103. MP acknowledges financial support from JAE-Doc program of the Spanish National Research Council (CSIC), co-funded by the European Social Fund. PAM acknowledges support from ERC StG Grant DEGAS-259586 and from the Science and Technology Facilities Council grants ST/K003305/1 and ST/L00075X/1.

Published
2015

9. The ALHAMBRA survey: accurate merger fractions derived by PDF analysis of photometrically close pairs

Author

Carlos López-Sanjuan, Kerttu Viironen, Jesús Cabrera-Caño, L. A. Díaz-García, C. Husillos, A. del Olmo, Mirjana Pović, R. M. González Delgado, Emilio J. Alfaro, Tom Broadhurst, L. Infante, David Cristóbal-Hornillos, T. Aparicio-Villegas, J. Cepa, Jaime Perea, Francisco J. Castander, Yolanda Jiménez-Teja, Francisco Prada, Isabel Márquez, Mariano Moles, Alberto Fernández-Soto, B. Ascaso, J. M. Quintana, Josefa Masegosa, Pablo Arnalte-Mur, J. A. L. Aguerri, A. J. Cenarro, Vicent J. Martínez, Alberto Molino, Jesús A. Varela, Miguel Cerviño, Narciso Benítez, 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), 'Federico II' University of Naples Medical School, 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), Spanish National Research Council (CSIC), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Instituto de Astrofisica de Canarias (IAC), Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), INTA - Instituto Nacional de Tecnología Agropecuaria, Instituto de Física Teórica UAM/CSIC (IFT), Universidad Autónoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Gobierno de Aragón, Generalitat Valenciana, Ministerio de Economía y Competitividad (España), Junta de Andalucía, European Commission, Fondo de Inversiones de Teruel, Ministerio de Ciencia e Innovación (España), Consejo Superior de Investigaciones Científicas (España), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), and Universidad Autonoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)

Subjects
Galaxies: statistics, media_common.quotation_subject, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, European Social Fund, interactions [Galaxies], Public administration, 01 natural sciences, statistics [Galaxies], Excellence, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, media_common, Physics, [PHYS]Physics [physics], Government, 010308 nuclear & particles physics, Galaxies: evolution, Astronomy and Astrophysics, evolution [Galaxies], Galaxies: interactions, Work (electrical), Space and Planetary Science, Research council, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

[Aims]: Our goal is to develop and test a novel methodology to compute accurate close-pair fractions with photometric redshifts. [Methods]: We improved the currently used methodologies to estimate the merger fraction fm from photometric redshifts by (i) using the full probability distribution functions (PDFs) of the sources in redshift space; (ii) including the variation in the luminosity of the sources with z in both the sample selection and the luminosity ratio constrain; and (iii) splitting individual PDFs into red and blue spectral templates to reliably work with colour selections.We tested the performance of our new methodology with the PDFs provided by the ALHAMBRA photometric survey. [Results]: The merger fractions and rates from the ALHAMBRA survey agree excellently well with those from spectroscopic work for both the general population and red and blue galaxies. With the merger rate of bright (MB ≤ -20 - 1:1z) galaxies evolving as (1 + z)n, the power-law index n is higher for blue galaxies (n = 2:7 0:5) than for red galaxies (n = 1:3 0:4), confirming previous results. Integrating the merger rate over cosmic time, we find that the average number of mergers per galaxy since z = 1 is Nm red = 0:57 0:05 for red galaxies and Nm blue = 0:26 0:02 for blue galaxies. [Conclusions]: Our new methodology statistically exploits all the available information provided by photometric redshift codes and yields accurate measurements of the merger fraction by close pairs from using photometric redshifts alone. Current and future photometric surveys will benefit from this new methodology., This work has been mainly funded by the FITE (Fondos de Inversiones de Teruel) and the projects AYA2012-30789, AYA2006-14056, and CSD2007-00060. We also acknowledge financial support from the Spanish Government grants AYA2010-15169, AYA2010-22111-C03-01, AYA2010-22111-C03-02, and AYA2013-48623-C2-2, from the Aragón Government through the Research Group E103, from the Junta de Andalucía through TIC-114 and the Excellence Project P08-TIC-03531, and from the Generalitat Valenciana through the projects Prometeo/2009/064 and PrometeoII/2014/060. A.J.C. is Ramón y Cajal fellow of the Spanish government. M.P. acknowledges the financial support from JAE-Doc program of the Spanish National Research Council (CSIC), co-funded by the European Social Fund.

Published
2015

10. 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

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