Galaxy clusters and groups in the ALHAMBRA survey

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Show simple item record Ascaso, B. Benítez, N. Fernández-Soto, A. Arnalte-Mur, P. López-Sanjuan, C. Molino, A. Schoenell, W. Jiménez-Teja, Y. Merson, A. I. Huertas-Company, M. Díaz-García, L. A. Martínez, V. J. Cenarro, A. J. Dupke, R. Márquez, I. Masegosa, J. Nieves-Seoane, L. Pović, M. Varela, J. Viironen, K. Aguerri, J. A L Olmo, A.del Moles, M. Perea, J. Alfaro, E. Aparicio-Villegas, T. Broadhurst, Tom J. Cabrera-Caño, J. Castander, F. J. Cepa, J. Cerviño, M. González-Delgado, R. M Cristóbal-Hornillos, D. Hurtado-Gil, L. Husillos, C. Infante, L. Prada, F. Quintana, J. M. 2016-09-13T15:23:23Z 2016-09-13T15:23:23Z 2015-01-01
dc.identifier.citation Monthly Notices of Royal Astronomical Society 452.1 (2015): 549-565 es_ES
dc.identifier.issn 0035-8711 (print) es_ES
dc.identifier.issn 1365-2966 (online) es_ES
dc.description This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2015 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved es_ES
dc.description.abstract We present a catalogue of 348 galaxy clusters and groups with 0.2 < z < 1.2 selected in the 2.78 deg2 ALHAMBRA Survey. The high precision of our photometric redshifts, close to 1%, 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 (BCF), 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% completeness and purity down to dark matter halo masses of Mh 3 × 1013M⊙ for z < 0.85. Cluster redshifts are expected to be recovered with 0.6% precision for z < 1. We also expect to measure cluster masses with σMh|M CL 0.25 − 0.35 dex precision down to 3 × 1013M⊙, masses which are 50% 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) es_ES
dc.description.sponsorship 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 Andalucía grant TIC114, JA2828, Aragón 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 es_ES
dc.format.extent 19 pag. es_ES
dc.format.mimetype application/pdf es_ES
dc.language.iso spa es_ES
dc.publisher Oxford University Press es_ES
dc.relation.ispartof Monthly Notices of the Royal Astronomical Society es_ES
dc.rights © 2015 The Authors es_ES
dc.subject.other Catalogues es_ES
dc.subject.other Cosmology: observations es_ES
dc.subject.other Galaxies: clusters: general es_ES
dc.subject.other Galaxies: evolution es_ES
dc.subject.other Large-scale structure of Universe es_ES
dc.subject.other X-rays: galaxies: clusters es_ES
dc.title Galaxy clusters and groups in the ALHAMBRA survey es_ES
dc.type article es_ES
dc.subject.eciencia Física es_ES
dc.relation.publisherversion es_ES
dc.identifier.doi 10.1093/mnras/stv1317 es_ES
dc.identifier.publicationfirstpage 549 es_ES
dc.identifier.publicationissue 1 es_ES
dc.identifier.publicationlastpage 565 es_ES
dc.identifier.publicationvolume 452 es_ES
dc.relation.projectID Gobierno de España. AYA2010-22111-C03- 02 es_ES
dc.relation.projectID Gobierno de España. AYA2010-15169 es_ES
dc.relation.projectID Gobierno de España. AYA2012-30789 es_ES
dc.relation.projectID Gobierno de España. AYA2013-48623-C2- 2 es_ES
dc.relation.projectID Gobierno de España. AYA2013-42227-P es_ES
dc.relation.projectID Gobierno de España. AYA2013-40611-P es_ES
dc.relation.projectID Gobierno de España. AYA2011-29517- C03-01 es_ES
dc.relation.projectID Gobierno de España. AYA2010-15081 es_ES
dc.relation.projectID info:eu-repo/grantAgreement/EC/FP7/259586 es_ES
dc.type.version info:eu-repo/semantics/publishedVersion es_ES
dc.rights.accessRights openAccess es_ES

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