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Published March 11, 2016 | Submitted + Published
Journal Article Open

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


The impending Javalambre Physics of the accelerating Universe Astrophysical Survey (J-PAS) will be the first wide-field survey of ≳ 8500 deg^2 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 z<1. The photometric redshift dispersion is estimated to be only ∼0.003 with few outliers ≲4 per cent for galaxies brighter than i ∼ 23 AB, because of the sensitivity of narrow band imaging to absorption and emission lines. Here, we evaluate the cluster selection function for J-PAS using N-body+semi-analytical realistic mock catalogues. We optimally detect clusters from this simulation with the Bayesian Cluster Finder, and we assess the completeness and purity of cluster detection against the mock data. The minimum halo mass threshold we find for detections of galaxy clusters and groups with both >80 per cent completeness and purity is M_h ∼ 5 × 10^(13) M_⊙ up to z ∼ 0.7. We also model the optical observable, M^∗_(CL)–halo mass relation, finding a non-evolution with redshift and main scatter of σM^∗_(CL)|M_h∼0.14dex down to a factor 2 lower in mass than other planned broad-band stage IV surveys, at least. For the M_h ∼ 1 × 10^(14) M_⊙ Planck mass limit, J-PAS will arrive up to z ∼ 0.85 with a σM^∗_(CL)|M_h∼0.12dex. 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.

Additional Information

© 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2015 December 22. Received 2015 November 24; in original form 2015 July 31. First published online January 14, 2016. We thank the referee of this paper for his/her useful and insightful suggestions and comments that helped improving the original manuscript. BA acknowledges financial support for a post-doctoral fellowship from the Observatory of Paris. 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. BA also thanks the hospitality of the University of Sao Paulo and Observatόrio Nacional for hosting her for a visit. BA dedicates this paper to the memory of the J-PAS member Javier Gorosabel.

Attached Files

Published - MNRAS-2016-Ascaso-4291-304.pdf

Submitted - 1601.00656v1.pdf


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