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Validation of selection function, sample contamination and mass calibration in galaxy cluster samples

Research output: Contribution to journalArticlepeer-review

  • S. Grandis
  • M. Klein
  • J. J. Mohr
  • S. Bocquet
  • M. Paulus
  • T. M. C. Abbott
  • M. Aguena
  • S. Allam
  • J. Annis
  • B. A. Benson
  • E. Bertin
  • S. Bhargava
  • D. Brooks
  • D. L. Burke
  • A. Carnero Rosell
  • M. Carrasco Kind
  • J. Carretero
  • R. Capasso
  • M. Costanzi
  • L. N. Da Costa
  • J. De Vicente
  • S. Desai
  • J. P. Dietrich
  • P. Doel
  • T. F. Eifler
  • A. E. Evrard
  • B. Flaugher
  • P. Fosalba
  • J. Frieman
  • J. Garcia-Bellido
  • E. Gaztanaga
  • D. W. Gerdes
  • D. Gruen
  • R. A. Gruendl
  • J. Gschwend
  • G. Gutierrez
  • W. G. Hartley
  • S. R. Hinton
  • D. L. Hollowood
  • K. Honscheid
  • D. J. James
  • T. Jeltema
  • K. Kuehn
  • N. Kuropatkin
  • M. Lima
  • M. A. G. Maia
  • J. L. Marshall
  • P. Melchior
  • F. Menanteau
  • R. Miquel
  • R. L. C. Ogando
  • A. Palmese
  • F. Paz-Chinchon
  • A. A. Plazas
  • A. K. Romer
  • A. Roodman
  • E. Sanchez
  • A. Saro
  • V. Scarpine
  • M. Schubnell
  • S. Serrano
  • E. Sheldon
  • M. Smith
  • A. A. Stark
  • E. Suchyta
  • M. E. C. Swanson
  • G. Tarle
  • D. L. Tucker
  • T. N. Varga
  • J. Weller
  • R. Wilkinson

We construct and validate the selection function of the MARD-Y3 galaxy cluster sample. This sample was selected through optical follow-up of the 2nd ROSAT faint source catalogue with Dark Energy Survey year 3 data. The selection function is modelled by combining an empirically constructed X-ray selection function with an incompleteness model for the optical follow-up. We validate the joint selection function by testing the consistency of the constraints on the X-ray flux-mass and richness-mass scaling relation parameters derived from different sources of mass information: (1) cross-calibration using South Pole Telescope Sunyaev-Zel'dovich (SPT-SZ) clusters, (2) calibration using number counts in X-ray, in optical and in both X-ray and optical while marginalizing over cosmological parameters, and (3) other published analyses. We find that the constraints on the scaling relation from the number counts and SPT-SZ cross-calibration agree, indicating that our modelling of the selection function is adequate. Furthermore, we apply a largely cosmology independent method to validate selection functions via the computation of the probability of finding each cluster in the SPT-SZ sample in the MARD-Y3 sample and vice versa. This test reveals no clear evidence for MARD-Y3 contamination, SPT-SZ incompleteness or outlier fraction. Finally, we discuss the prospects of the techniques presented here to limit systematic selection effects in future cluster cosmological studies.

Original languageEnglish
Pages (from-to)771-798
Number of pages28
JournalMonthly Notices of the Royal Astronomical Society
Issue number1
Early online date11 Aug 2020
Publication statusPublished - 1 Oct 2020


  • staa2333

    Rights statement: This article has been accepted for publication in MNRAS © 2020 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.

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