Galaxies in X-ray selected clusters and groups in dark energy survey data – II. Hierarchical Bayesian modelling of the red-sequence galaxy luminosity function

Y. Zhang; C. J. Miller; P. Rooney; A. Bermeo; A. K. Romer; C. Vergara Cervantes; E. S. Rykoff; C. Hennig; R. Das; T. McKay; J. Song; H. Wilcox; D. Bacon; S. L. Bridle; C. Collins; C. Conselice; M. Hilton; B. Hoyle; S. Kay; A. R. Liddle; R. G. Mann; N. Mehrtens; J. Mayers; R. C. Nichol; M. Sahlén; J. Stott; P. T.P. Viana; R. H. Wechsler; T. Abbott; F. B. Abdalla; S. Allam; A. Benoit-Lévy; D. Brooks; E. Buckley-Geer; D. L. Burke; A. Carnero Rosell; M. Carrasco Kind; J. Carretero; F. J. Castander; M. Crocce; C. E. Cunha; C. B. D’Andrea; L. N. Da Costa; H. T. Diehl; J. P. Dietrich; T. F. Eifler; B. Flaugher; P. Fosalba; J. García-Bellido; E. Gaztanaga; D. W. Gerdes; D. Gruen; R. A. Gruendl; J. Gschwend; G. Gutierrez; K. Honscheid; D. J. James; T. Jeltema; K. Kuehn; N. Kuropatkin; M. Lima; H. Lin; M. A.G. Maia; M. March; J. L. Marshall; P. Melchior; F. Menanteau; R. Miquel; R. L.C. Ogando; A. A. Plazas; E. Sanchez; M. Schubnell; I. Sevilla-Noarbe; M. Smith; M. Soares-Santos; F. Sobreira; E. Suchyta; M. E.C. Swanson; G. Tarle; A. R. Walker

doi:10.1093/mnras/stz1612

Galaxies in X-ray selected clusters and groups in dark energy survey data – II. Hierarchical Bayesian modelling of the red-sequence galaxy luminosity function

Y. Zhang, C. J. Miller, P. Rooney, A. Bermeo, A. K. Romer, C. Vergara Cervantes, E. S. Rykoff, C. Hennig, R. Das, T. McKay, J. Song, H. Wilcox, D. Bacon, S. L. Bridle, C. Collins, C. Conselice, M. Hilton, B. Hoyle, S. Kay, A. R. LiddleR. G. Mann, N. Mehrtens, J. Mayers, R. C. Nichol, M. Sahlén, J. Stott, P. T.P. Viana, R. H. Wechsler, T. Abbott, F. B. Abdalla, S. Allam, A. Benoit-Lévy, D. Brooks, E. Buckley-Geer, D. L. Burke, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, F. J. Castander, M. Crocce, C. E. Cunha, C. B. D’Andrea, L. N. Da Costa, H. T. Diehl, J. P. Dietrich, T. F. Eifler, B. Flaugher, P. Fosalba, J. García-Bellido, E. Gaztanaga, D. W. Gerdes, D. Gruen, R. A. Gruendl, J. Gschwend, G. Gutierrez, K. Honscheid, D. J. James, T. Jeltema, K. Kuehn, N. Kuropatkin, M. Lima, H. Lin, M. A.G. Maia, M. March, J. L. Marshall, P. Melchior, F. Menanteau, R. Miquel, R. L.C. Ogando, A. A. Plazas, E. Sanchez, M. Schubnell, I. Sevilla-Noarbe, M. Smith, M. Soares-Santos, F. Sobreira, E. Suchyta, M. E.C. Swanson, G. Tarle, A. R. Walker

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Abstract

Using ∼100 X-ray selected clusters in the Dark Energy Survey Science Verification data, we constrain the luminosity function (LF) of cluster red-sequence galaxies as a function of redshift. This is the first homogeneous optical/X-ray sample large enough to constrain the evolution of the LF simultaneously in redshift (0.1 < z < 1.05) and cluster mass (13.5 ≤ log₁₀(M_200crit) ∼< 15.0). We pay particular attention to completeness issues and the detection limit of the galaxy sample. We then apply a hierarchical Bayesian model to fit the cluster galaxy LFs via a Schechter function, including its characteristic break (m^∗) to a faint end power-law slope (α). Our method enables us to avoid known issues in similar analyses based on stacking or binning the clusters. We find weak and statistically insignificant (∼1.9σ) evolution in the faint end slope α versus redshift. We also find no dependence in α or m^∗ with the X-ray inferred cluster masses. However, the amplitude of the LF as a function of cluster mass is constrained to ∼20 per cent precision. As a by-product of our algorithm, we utilize the correlation between the LF and cluster mass to provide an improved estimate of the individual cluster masses as well as the scatter in true mass given the X-ray inferred masses. This technique can be applied to a larger sample of X-ray or optically selected clusters from the Dark Energy Survey, significantly improving the sensitivity of the analysis.

Original language	English
Pages (from-to)	1-17
Number of pages	17
Journal	Monthly Notices of the Royal Astronomical Society
Issue number	1
DOIs	https://doi.org/10.1093/mnras/stz1612
State	Published - Sep 1 2019

Funding

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, ESP2015-88861, FPA2015-68048, SEV-2012-0234, 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 Australian Research Council Centre of Excellence for All-sky Astrophysics (CAAS-TRO), through project number CE110001020. C. Miller as well as Y. Zhang acknowledges support from Department of Energy grant DE-SC0013520. Y. Zhang thanks Alex Drlica-Wagner, Gary Bernstein, and Chris Davis for careful reading of the draft. We use DES Science Verification in this paper. We are grateful for the extraordinary contributions of our CTIO colleagues and the DECam Construction, Commissioning and Science Verification teams in achieving the excellent instrument and telescope conditions that have made this work possible. The success of this project also relies critically on the expertise and dedication of the DES Data Management group. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundac¸ão Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovac¸ão, the Deutsche C. Miller as well as Y. Zhang acknowledges support from Department of Energy grant DE-SC0013520. Y. Zhang thanks Alex Drlica-Wagner, Gary Bernstein, and Chris Davis for careful reading of the draft. We use DES Science Verification in this paper. We are grateful for the extraordinary contributions of our CTIO colleagues and the DECam Construction, Commissioning and Science Verification teams in achieving the excellent instrument and telescope conditions that have made this work possible. The success of this project also relies critically on the expertise and dedication of the DES Data Management group. 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, ESP2015-88861, FPA2015-68048, SEV-2012-0234, 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 Australian Research Council Centre of Excellence for All-sky Astrophysics (CAAS-TRO), through project number CE110001020. 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. 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.

Funders	Funder number
Not added	ST/P00038X/1
Australian Research Council Centre of Excellence for All-sky Astrophysics
CAAS-TRO	CE110001020
European Union?s Seventh Framework Program
FP7/2007
Fermi Research Alliance, LLC	DE-AC02-07CH11359
Ministério da Ciência
Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University
Science and Technology Facilities Council of the United Kingdom
United States Government
National Science Foundation	1138766, AST-1138766, AST-1536171
National Science Foundation
U.S. Department of Energy	DE-SC0013520
U.S. Department of Energy
Office of Science
High Energy Physics
Ohio State University
University of Chicago
National Centre for Supercomputing Applications
Seventh Framework Programme	240672, 306478, 291329
Seventh Framework Programme
Higher Education Funding Council for England
Engineering Research Centers
Science and Technology Facilities Council	ST/P000649/1
Science and Technology Facilities Council
European Commission
European Research Council
Australian Research Council
Generalitat de Catalunya
Ministerio de Economía y Competitividad	ESP2015-88861, SEV-2016-0597, MDM-2015-0509, FPA2015-68048, SEV-2012-0234, AYA2015-71825
Ministerio de Economía y Competitividad
Conselho Nacional de Desenvolvimento Científico e Tecnológico
Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro
Financiadora de Estudos e Projetos
Ministry of Education and Science of Ukraine
European Regional Development Fund

Keywords

Clusters
Evolution
Galaxies
General – galaxies

Access to Document

10.1093/mnras/stz1612

Cite this

Zhang, Y., Miller, C. J., Rooney, P., Bermeo, A., Romer, A. K., Vergara Cervantes, C., Rykoff, E. S., Hennig, C., Das, R., McKay, T., Song, J., Wilcox, H., Bacon, D., Bridle, S. L., Collins, C., Conselice, C., Hilton, M., Hoyle, B., Kay, S., ... Walker, A. R. (2019). Galaxies in X-ray selected clusters and groups in dark energy survey data – II. Hierarchical Bayesian modelling of the red-sequence galaxy luminosity function. Monthly Notices of the Royal Astronomical Society, (1), 1-17. https://doi.org/10.1093/mnras/stz1612

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title = "Galaxies in X-ray selected clusters and groups in dark energy survey data – II. Hierarchical Bayesian modelling of the red-sequence galaxy luminosity function",

abstract = "Using ∼100 X-ray selected clusters in the Dark Energy Survey Science Verification data, we constrain the luminosity function (LF) of cluster red-sequence galaxies as a function of redshift. This is the first homogeneous optical/X-ray sample large enough to constrain the evolution of the LF simultaneously in redshift (0.1 < z < 1.05) and cluster mass (13.5 ≤ log10(M200crit) ∼< 15.0). We pay particular attention to completeness issues and the detection limit of the galaxy sample. We then apply a hierarchical Bayesian model to fit the cluster galaxy LFs via a Schechter function, including its characteristic break (m∗) to a faint end power-law slope (α). Our method enables us to avoid known issues in similar analyses based on stacking or binning the clusters. We find weak and statistically insignificant (∼1.9σ) evolution in the faint end slope α versus redshift. We also find no dependence in α or m∗ with the X-ray inferred cluster masses. However, the amplitude of the LF as a function of cluster mass is constrained to ∼20 per cent precision. As a by-product of our algorithm, we utilize the correlation between the LF and cluster mass to provide an improved estimate of the individual cluster masses as well as the scatter in true mass given the X-ray inferred masses. This technique can be applied to a larger sample of X-ray or optically selected clusters from the Dark Energy Survey, significantly improving the sensitivity of the analysis.",

keywords = "Clusters, Evolution, Galaxies, General – galaxies",

author = "Y. Zhang and Miller, {C. J.} and P. Rooney and A. Bermeo and Romer, {A. K.} and {Vergara Cervantes}, C. and Rykoff, {E. S.} and C. Hennig and R. Das and T. McKay and J. Song and H. Wilcox and D. Bacon and Bridle, {S. L.} and C. Collins and C. Conselice and M. Hilton and B. Hoyle and S. Kay and Liddle, {A. R.} and Mann, {R. G.} and N. Mehrtens and J. Mayers and Nichol, {R. C.} and M. Sahl{\'e}n and J. Stott and Viana, {P. T.P.} and Wechsler, {R. H.} and T. Abbott and Abdalla, {F. B.} and S. Allam and A. Benoit-L{\'e}vy and D. Brooks and E. Buckley-Geer and Burke, {D. L.} and {Carnero Rosell}, A. and {Carrasco Kind}, M. and J. Carretero and Castander, {F. J.} and M. Crocce and Cunha, {C. E.} and D{\textquoteright}Andrea, {C. B.} and {Da Costa}, {L. N.} and Diehl, {H. T.} and Dietrich, {J. P.} and Eifler, {T. F.} and B. Flaugher and P. Fosalba and J. Garc{\'i}a-Bellido and E. Gaztanaga and Gerdes, {D. W.} and D. Gruen and Gruendl, {R. A.} and J. Gschwend and G. Gutierrez and K. Honscheid and James, {D. J.} and T. Jeltema and K. Kuehn and N. Kuropatkin and M. Lima and H. Lin and Maia, {M. A.G.} and M. March and Marshall, {J. L.} and P. Melchior and F. Menanteau and R. Miquel and Ogando, {R. L.C.} and Plazas, {A. A.} and E. Sanchez and M. Schubnell and I. Sevilla-Noarbe and M. Smith and M. Soares-Santos and F. Sobreira and E. Suchyta and Swanson, {M. E.C.} and G. Tarle and Walker, {A. R.}",

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year = "2019",

month = sep,

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doi = "10.1093/mnras/stz1612",

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Zhang, Y, Miller, CJ, Rooney, P, Bermeo, A, Romer, AK, Vergara Cervantes, C, Rykoff, ES, Hennig, C, Das, R, McKay, T, Song, J, Wilcox, H, Bacon, D, Bridle, SL, Collins, C, Conselice, C, Hilton, M, Hoyle, B, Kay, S, Liddle, AR, Mann, RG, Mehrtens, N, Mayers, J, Nichol, RC, Sahlén, M, Stott, J, Viana, PTP, Wechsler, RH, Abbott, T, Abdalla, FB, Allam, S, Benoit-Lévy, A, Brooks, D, Buckley-Geer, E, Burke, DL, Carnero Rosell, A, Carrasco Kind, M, Carretero, J, Castander, FJ, Crocce, M, Cunha, CE, D’Andrea, CB, Da Costa, LN, Diehl, HT, Dietrich, JP, Eifler, TF, Flaugher, B, Fosalba, P, García-Bellido, J, Gaztanaga, E, Gerdes, DW, Gruen, D, Gruendl, RA, Gschwend, J, Gutierrez, G, Honscheid, K, James, DJ, Jeltema, T, Kuehn, K, Kuropatkin, N, Lima, M, Lin, H, Maia, MAG, March, M, Marshall, JL, Melchior, P, Menanteau, F, Miquel, R, Ogando, RLC, Plazas, AA, Sanchez, E, Schubnell, M, Sevilla-Noarbe, I, Smith, M, Soares-Santos, M, Sobreira, F, Suchyta, E, Swanson, MEC, Tarle, G & Walker, AR 2019, 'Galaxies in X-ray selected clusters and groups in dark energy survey data – II. Hierarchical Bayesian modelling of the red-sequence galaxy luminosity function', Monthly Notices of the Royal Astronomical Society, no. 1, pp. 1-17. https://doi.org/10.1093/mnras/stz1612

TY - JOUR

T1 - Galaxies in X-ray selected clusters and groups in dark energy survey data – II. Hierarchical Bayesian modelling of the red-sequence galaxy luminosity function

AU - Zhang, Y.

AU - Miller, C. J.

AU - Rooney, P.

AU - Bermeo, A.

AU - Romer, A. K.

AU - Vergara Cervantes, C.

AU - Rykoff, E. S.

AU - Hennig, C.

AU - Das, R.

AU - McKay, T.

AU - Song, J.

AU - Wilcox, H.

AU - Bacon, D.

AU - Bridle, S. L.

AU - Collins, C.

AU - Conselice, C.

AU - Hilton, M.

AU - Hoyle, B.

AU - Kay, S.

AU - Liddle, A. R.

AU - Mann, R. G.

AU - Mehrtens, N.

AU - Mayers, J.

AU - Nichol, R. C.

AU - Sahlén, M.

AU - Stott, J.

AU - Viana, P. T.P.

AU - Wechsler, R. H.

AU - Abbott, T.

AU - Abdalla, F. B.

AU - Allam, S.

AU - Benoit-Lévy, A.

AU - Brooks, D.

AU - Buckley-Geer, E.

AU - Burke, D. L.

AU - Carnero Rosell, A.

AU - Carrasco Kind, M.

AU - Carretero, J.

AU - Castander, F. J.

AU - Crocce, M.

AU - Cunha, C. E.

AU - D’Andrea, C. B.

AU - Da Costa, L. N.

AU - Diehl, H. T.

AU - Dietrich, J. P.

AU - Eifler, T. F.

AU - Flaugher, B.

AU - Fosalba, P.

AU - García-Bellido, J.

AU - Gaztanaga, E.

AU - Gerdes, D. W.

AU - Gruen, D.

AU - Gruendl, R. A.

AU - Gschwend, J.

AU - Gutierrez, G.

AU - Honscheid, K.

AU - James, D. J.

AU - Jeltema, T.

AU - Kuehn, K.

AU - Kuropatkin, N.

AU - Lima, M.

AU - Lin, H.

AU - Maia, M. A.G.

AU - March, M.

AU - Marshall, J. L.

AU - Melchior, P.

AU - Menanteau, F.

AU - Miquel, R.

AU - Ogando, R. L.C.

AU - Plazas, A. A.

AU - Sanchez, E.

AU - Schubnell, M.

AU - Sevilla-Noarbe, I.

AU - Smith, M.

AU - Soares-Santos, M.

AU - Sobreira, F.

AU - Suchyta, E.

AU - Swanson, M. E.C.

AU - Tarle, G.

AU - Walker, A. R.

PY - 2019/9/1

Y1 - 2019/9/1

N2 - Using ∼100 X-ray selected clusters in the Dark Energy Survey Science Verification data, we constrain the luminosity function (LF) of cluster red-sequence galaxies as a function of redshift. This is the first homogeneous optical/X-ray sample large enough to constrain the evolution of the LF simultaneously in redshift (0.1 < z < 1.05) and cluster mass (13.5 ≤ log10(M200crit) ∼< 15.0). We pay particular attention to completeness issues and the detection limit of the galaxy sample. We then apply a hierarchical Bayesian model to fit the cluster galaxy LFs via a Schechter function, including its characteristic break (m∗) to a faint end power-law slope (α). Our method enables us to avoid known issues in similar analyses based on stacking or binning the clusters. We find weak and statistically insignificant (∼1.9σ) evolution in the faint end slope α versus redshift. We also find no dependence in α or m∗ with the X-ray inferred cluster masses. However, the amplitude of the LF as a function of cluster mass is constrained to ∼20 per cent precision. As a by-product of our algorithm, we utilize the correlation between the LF and cluster mass to provide an improved estimate of the individual cluster masses as well as the scatter in true mass given the X-ray inferred masses. This technique can be applied to a larger sample of X-ray or optically selected clusters from the Dark Energy Survey, significantly improving the sensitivity of the analysis.

AB - Using ∼100 X-ray selected clusters in the Dark Energy Survey Science Verification data, we constrain the luminosity function (LF) of cluster red-sequence galaxies as a function of redshift. This is the first homogeneous optical/X-ray sample large enough to constrain the evolution of the LF simultaneously in redshift (0.1 < z < 1.05) and cluster mass (13.5 ≤ log10(M200crit) ∼< 15.0). We pay particular attention to completeness issues and the detection limit of the galaxy sample. We then apply a hierarchical Bayesian model to fit the cluster galaxy LFs via a Schechter function, including its characteristic break (m∗) to a faint end power-law slope (α). Our method enables us to avoid known issues in similar analyses based on stacking or binning the clusters. We find weak and statistically insignificant (∼1.9σ) evolution in the faint end slope α versus redshift. We also find no dependence in α or m∗ with the X-ray inferred cluster masses. However, the amplitude of the LF as a function of cluster mass is constrained to ∼20 per cent precision. As a by-product of our algorithm, we utilize the correlation between the LF and cluster mass to provide an improved estimate of the individual cluster masses as well as the scatter in true mass given the X-ray inferred masses. This technique can be applied to a larger sample of X-ray or optically selected clusters from the Dark Energy Survey, significantly improving the sensitivity of the analysis.

KW - Clusters

KW - Evolution

KW - Galaxies

KW - General – galaxies

UR - http://www.scopus.com/inward/record.url?scp=85078439888&partnerID=8YFLogxK

U2 - 10.1093/mnras/stz1612

DO - 10.1093/mnras/stz1612

M3 - Article

AN - SCOPUS:85078439888

SN - 0035-8711

SP - 1

EP - 17

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 1

ER -

Galaxies in X-ray selected clusters and groups in dark energy survey data – II. Hierarchical Bayesian modelling of the red-sequence galaxy luminosity function

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