Constraints on the richness-mass relation and the optical-SZE positional offset distribution for SZE-selected clusters

A. Saro; S. Bocquet; E. Rozo; B. A. Benson; J. Mohr; E. S. Rykoff; M. Soares-Santos; L. Bleem; S. Dodelson; P. Melchior; F. Sobreira; V. Upadhyay; J. Weller; T. Abbott; F. B. Abdalla; S. Allam; R. Armstrong; M. Banerji; A. H. Bauer; M. Bayliss; A. Benoit-Lévy; G. M. Bernstein; E. Bertin; M. Brodwin; D. Brooks; E. Buckley-Geer; D. L. Burke; J. E. Carlstrom; R. Capasso; D. Capozzi; A. Carnero Rosell; M. Carrasco Kind; I. Chiu; R. Covarrubias; T. M. Crawford; M. Crocce; C. B. D'Andrea; L. N. da Costa; D. L. DePoy; S. Desai; T. de Haan; H. T. Diehl; J. P. Dietrich; P. Doel; C. E. Cunha; T. F. Eifler; A. E. Evrard; A. Fausti Neto; E. Fernandez; B. Flaugher; P. Fosalba; J. Frieman; C. Gangkofner; E. Gaztanaga; D. Gerdes; D. Gruen; R. A. Gruendl; N. Gupta; C. Hennig; W. L. Holzapfel; K. Honscheid; B. Jain; D. James; K. Kuehn; N. Kuropatkin; O. Lahav; T. S. Li; H. Lin; M. A.G. Maia; M. March; J. L. Marshall; Paul Martini; M. McDonald; C. J. Miller; R. Miquel; B. Nord; R. Ogando; A. A. Plazas; C. L. Reichardt; A. K. Romer; A. Roodman; M. Sako; E. Sanchez; M. Schubnell; I. Sevilla; R. C. Smith; B. Stalder; A. A. Stark; V. Strazzullo; E. Suchyta; M. E.C. Swanson; G. Tarle; J. Thaler; D. Thomas; D. Tucker; V. Vikram; A. von der Linden; A. R. Walker; R. H. Wechsler; W. Wester; A. Zenteno; K. E. Ziegler

doi:10.1093/mnras/stv2141

Constraints on the richness-mass relation and the optical-SZE positional offset distribution for SZE-selected clusters

A. Saro, S. Bocquet, E. Rozo, B. A. Benson, J. Mohr, E. S. Rykoff, M. Soares-Santos, L. Bleem, S. Dodelson, P. Melchior, F. Sobreira, V. Upadhyay, J. Weller, T. Abbott, F. B. Abdalla, S. Allam, R. Armstrong, M. Banerji, A. H. Bauer, M. BaylissA. Benoit-Lévy, G. M. Bernstein, E. Bertin, M. Brodwin, D. Brooks, E. Buckley-Geer, D. L. Burke, J. E. Carlstrom, R. Capasso, D. Capozzi, A. Carnero Rosell, M. Carrasco Kind, I. Chiu, R. Covarrubias, T. M. Crawford, M. Crocce, C. B. D'Andrea, L. N. da Costa, D. L. DePoy, S. Desai, T. de Haan, H. T. Diehl, J. P. Dietrich, P. Doel, C. E. Cunha, T. F. Eifler, A. E. Evrard, A. Fausti Neto, E. Fernandez, B. Flaugher, P. Fosalba, J. Frieman, C. Gangkofner, E. Gaztanaga, D. Gerdes, D. Gruen, R. A. Gruendl, N. Gupta, C. Hennig, W. L. Holzapfel, K. Honscheid, B. Jain, D. James, K. Kuehn, N. Kuropatkin, O. Lahav, T. S. Li, H. Lin, M. A.G. Maia, M. March, J. L. Marshall, Paul Martini, M. McDonald, C. J. Miller, R. Miquel, B. Nord, R. Ogando, A. A. Plazas, C. L. Reichardt, A. K. Romer, A. Roodman, M. Sako, E. Sanchez, M. Schubnell, I. Sevilla, R. C. Smith, B. Stalder, A. A. Stark, V. Strazzullo, E. Suchyta, M. E.C. Swanson, G. Tarle, J. Thaler, D. Thomas, D. Tucker, V. Vikram, A. von der Linden, A. R. Walker, R. H. Wechsler, W. Wester, A. Zenteno, K. E. Ziegler

Research output: Contribution to journal › Article › peer-review

102 Scopus citations

Abstract

We cross-match galaxy cluster candidates selected via their Sunyaev-Zel'dovich effect (SZE) signatures in 129.1 deg² of the South Pole Telescope 2500d SPT-SZ survey with optically identified clusters selected from the Dark Energy Survey science verification data. We identify 25 clusters between 0.1 ≲ z ≲ 0.8 in the union of the SPT-SZ and redMaPPer (RM) samples. RM is an optical cluster finding algorithm that also returns a richness estimate for each cluster. We model the richness λ-mass relation with the following function 〈lnλ|M₅₀₀〉 ∝ BλlnM₅₀₀ + Cλln E(z) and use SPT-SZ cluster masses and RM richnesses λ to constrain the parameters. We find Bλ = 1.14_-0.18^+0.21 and Cλ = 0.73_-0.75^+0.77. The associated scatter in mass at fixed richness is σlnM|λ = 0.18_-0.05^+0.08 at a characteristic richness λ=70.We demonstrate that our model provides an adequate description of the matched sample, showing that the fraction of SPT-SZ-selected clusters with RM counterparts is consistent with expectations and that the fraction of RMselected clusters with SPT-SZ counterparts is in mild tension with expectation. We model the optical-SZE cluster positional offset distribution with the sum of two Gaussians, showing that it is consistent with a dominant, centrally peaked population and a subdominant population characterized by larger offsets. We also cross-match the RMcatalogue with SPT-SZ candidates below the official catalogue threshold significance ξ = 4.5, using the RM catalogue to provide optical confirmation and redshifts for 15 additional clusters with ξ ∈ [4, 4.5].

Original language	English
Pages (from-to)	2305-2319
Number of pages	15
Journal	Monthly Notices of the Royal Astronomical Society
Volume	454
Issue number	3
DOIs	https://doi.org/10.1093/mnras/stv2141
State	Published - Dec 11 2015
Externally published	Yes

Funding

We acknowledge the support by the DFG Cluster of Excellence ‘Origin and Structure of the Universe’, the Transregio program TR33 ‘The Dark Universe’ and the Ludwig-Maximilians University. The South Pole Telescope is supported by the National Science Foundation through grant PLR-1248097. Partial support is also provided by the NSF Physics Frontier Center grant PHY-1125897 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation and the Gordon and Betty Moore Foundation grant GBMF 947. AAS acknowledges a Pell grant from the Smithsonian Institution. TDH is supported by a Miller Research Fellowship. This work was partially completed at Fermilab, operated by Fermi Research Alliance, LLC under contract no. De-AC02-07CH11359 with the United States Department of Energy. The Dark Cosmology Centre is funded by the Danish National Research Foundation. CR acknowledges support from the Australian Research Council’s Discovery Projects scheme (DP150103208). Funding for the DES Projects has been provided by the US Department of Energy, the US 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, Con-selho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência e Tecnologia, the Deutsche Forschungs-gemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2012-39559, ESP2013-48274, FPA2013-47986 and Centro de Excelencia Severo Ochoa SEV-2012-0234, some of which include ERDF funds from the European Union. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energet-icas, Medioambientales y Tecnologicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Edinburgh, the University of Illinois at Urbana-Champaign, the Institut de Cien-cies de l’Espai (IEEC/CSIC), the Institut de Fisica d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität and the associated Excellence Cluster Universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex and Texas A&M University. We acknowledge the support by the DFG Cluster of Excellence 'Origin and Structure of the Universe', the Transregio program TR33 'The Dark Universe' and the Ludwig-Maximilians University. The South Pole Telescope is supported by the National Science Foundation through grant PLR-1248097. Partial support is also provided by the NSF Physics Frontier Center grant PHY- 1125897 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation and the Gordon and Betty Moore Foundation grant GBMF 947. AAS acknowledges a Pell grant from the Smithsonian Institution. TDH is supported by a Miller Research Fellowship. This work was partially completed at Fermilab, operated by Fermi Research Alliance, LLC under contract no. De-AC02-07CH11359 with the United States Department of Energy. The Dark Cosmology Centre is funded by the Danish National Research Foundation. CR acknowledges support from the Australian Research Council's Discovery Projects scheme (DP150103208). Funding for the DES Projects has been provided by the US Department of Energy, the US 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, Fundação 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 e Tecnologia, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2012-39559, ESP2013-48274, FPA2013-47986 and Centro de Excelencia Severo Ochoa SEV-2012-0234, some of which include ERDF funds from the European Union. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Edinburgh, the University of Illinois at Urbana-Champaign, the Institut de Ciencies de l'Espai (IEEC/CSIC), the Institut de Fisica d'Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität and the associated Excellence Cluster Universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex and Texas A&M University.

Funders	Funder number
Centro de Excelencia Severo Ochoa	SEV-2012-0234
Collaborating Institutions in the Dark Energy Survey
DFG Cluster of Excellence ‘Origin and Structure of the Universe
Deutsche Forschungs-gemeinschaft
Fermi Research Alliance, LLC	De-AC02-07CH11359
Kavli Institute of Cosmological Physics at the University of Chicago
Ludwig-Maximilians University
Ministry of Science and Education of Spain
Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University
NSF Physics Frontier Center	PHY-1125897
National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign
US Department of Energy
US National Science Foundation
United States Department of Energy
National Science Foundation	1009012, PLR-1248097, 1248097, 1125897, 1311924
Smithsonian Institution
Gordon and Betty Moore Foundation	GBMF 947
Kavli Foundation
Stanford University
Texas A and M University
Higher Education Funding Council for England
Center for Cosmology and Astroparticle Physics, Ohio State University
Science and Technology Facilities Council	ST/K000985/1, ST/K00090X/1, ST/M003574/1, ST/M001334/1, ST/N001087/1, ST/M007030/1, ST/H001581/1, ST/L006529/1, ST/M004708/1, ST/I000976/1, ST/L000652/1
European Commission
University of Nottingham
University of Sussex
Australian Research Council	DP150103208
Danmarks Grundforskningsfond
Ministerio de Economía y Competitividad	FPA2013-47986, AYA2012-39559, ESP2013-48274
Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro
Financiadora de Estudos e Projetos
Ministério da Ciência e Tecnologia
European Regional Development Fund
National Science Foundation

Keywords

Catalogues
Cosmology: miscellaneous
Galaxies: abundances
Galaxies: clusters: general
Galaxies: haloes
Galaxies: statistics
Large-scale structure of Universe
Methods: data analysis

Access to Document

10.1093/mnras/stv2141

Cite this

Saro, A., Bocquet, S., Rozo, E., Benson, B. A., Mohr, J., Rykoff, E. S., Soares-Santos, M., Bleem, L., Dodelson, S., Melchior, P., Sobreira, F., Upadhyay, V., Weller, J., Abbott, T., Abdalla, F. B., Allam, S., Armstrong, R., Banerji, M., Bauer, A. H., ... Ziegler, K. E. (2015). Constraints on the richness-mass relation and the optical-SZE positional offset distribution for SZE-selected clusters. Monthly Notices of the Royal Astronomical Society, 454(3), 2305-2319. https://doi.org/10.1093/mnras/stv2141

@article{6900799f30244f1899475ce4c52b0619,

title = "Constraints on the richness-mass relation and the optical-SZE positional offset distribution for SZE-selected clusters",

abstract = "We cross-match galaxy cluster candidates selected via their Sunyaev-Zel'dovich effect (SZE) signatures in 129.1 deg2 of the South Pole Telescope 2500d SPT-SZ survey with optically identified clusters selected from the Dark Energy Survey science verification data. We identify 25 clusters between 0.1 ≲ z ≲ 0.8 in the union of the SPT-SZ and redMaPPer (RM) samples. RM is an optical cluster finding algorithm that also returns a richness estimate for each cluster. We model the richness λ-mass relation with the following function 〈lnλ|M500〉 ∝ BλlnM500 + Cλln E(z) and use SPT-SZ cluster masses and RM richnesses λ to constrain the parameters. We find Bλ = 1.14-0.18+0.21 and Cλ = 0.73-0.75+0.77. The associated scatter in mass at fixed richness is σlnM|λ = 0.18-0.05+0.08 at a characteristic richness λ=70.We demonstrate that our model provides an adequate description of the matched sample, showing that the fraction of SPT-SZ-selected clusters with RM counterparts is consistent with expectations and that the fraction of RMselected clusters with SPT-SZ counterparts is in mild tension with expectation. We model the optical-SZE cluster positional offset distribution with the sum of two Gaussians, showing that it is consistent with a dominant, centrally peaked population and a subdominant population characterized by larger offsets. We also cross-match the RMcatalogue with SPT-SZ candidates below the official catalogue threshold significance ξ = 4.5, using the RM catalogue to provide optical confirmation and redshifts for 15 additional clusters with ξ ∈ [4, 4.5].",

keywords = "Catalogues, Cosmology: miscellaneous, Galaxies: abundances, Galaxies: clusters: general, Galaxies: haloes, Galaxies: statistics, Large-scale structure of Universe, Methods: data analysis",

author = "A. Saro and S. Bocquet and E. Rozo and Benson, {B. A.} and J. Mohr and Rykoff, {E. S.} and M. Soares-Santos and L. Bleem and S. Dodelson and P. Melchior and F. Sobreira and V. Upadhyay and J. Weller and T. Abbott and Abdalla, {F. B.} and S. Allam and R. Armstrong and M. Banerji and Bauer, {A. H.} and M. Bayliss and A. Benoit-L{\'e}vy and Bernstein, {G. M.} and E. Bertin and M. Brodwin and D. Brooks and E. Buckley-Geer and Burke, {D. L.} and Carlstrom, {J. E.} and R. Capasso and D. Capozzi and {Carnero Rosell}, A. and {Carrasco Kind}, M. and I. Chiu and R. Covarrubias and Crawford, {T. M.} and M. Crocce and D'Andrea, {C. B.} and {da Costa}, {L. N.} and DePoy, {D. L.} and S. Desai and {de Haan}, T. and Diehl, {H. T.} and Dietrich, {J. P.} and P. Doel and Cunha, {C. E.} and Eifler, {T. F.} and Evrard, {A. E.} and {Fausti Neto}, A. and E. Fernandez and B. Flaugher and P. Fosalba and J. Frieman and C. Gangkofner and E. Gaztanaga and D. Gerdes and D. Gruen and Gruendl, {R. A.} and N. Gupta and C. Hennig and Holzapfel, {W. L.} and K. Honscheid and B. Jain and D. James and K. Kuehn and N. Kuropatkin and O. Lahav and Li, {T. S.} and H. Lin and Maia, {M. A.G.} and M. March and Marshall, {J. L.} and Paul Martini and M. McDonald and Miller, {C. J.} and R. Miquel and B. Nord and R. Ogando and Plazas, {A. A.} and Reichardt, {C. L.} and Romer, {A. K.} and A. Roodman and M. Sako and E. Sanchez and M. Schubnell and I. Sevilla and Smith, {R. C.} and B. Stalder and Stark, {A. A.} and V. Strazzullo and E. Suchyta and Swanson, {M. E.C.} and G. Tarle and J. Thaler and D. Thomas and D. Tucker and V. Vikram and {von der Linden}, A. and Walker, {A. R.} and Wechsler, {R. H.} and W. Wester and A. Zenteno and Ziegler, {K. E.}",

note = "Publisher Copyright: {\textcopyright} 2015 The Author.",

year = "2015",

month = dec,

day = "11",

doi = "10.1093/mnras/stv2141",

language = "English",

volume = "454",

pages = "2305--2319",

journal = "Monthly Notices of the Royal Astronomical Society",

issn = "0035-8711",

publisher = "Oxford University Press",

number = "3",

}

Saro, A, Bocquet, S, Rozo, E, Benson, BA, Mohr, J, Rykoff, ES, Soares-Santos, M, Bleem, L, Dodelson, S, Melchior, P, Sobreira, F, Upadhyay, V, Weller, J, Abbott, T, Abdalla, FB, Allam, S, Armstrong, R, Banerji, M, Bauer, AH, Bayliss, M, Benoit-Lévy, A, Bernstein, GM, Bertin, E, Brodwin, M, Brooks, D, Buckley-Geer, E, Burke, DL, Carlstrom, JE, Capasso, R, Capozzi, D, Carnero Rosell, A, Carrasco Kind, M, Chiu, I, Covarrubias, R, Crawford, TM, Crocce, M, D'Andrea, CB, da Costa, LN, DePoy, DL, Desai, S, de Haan, T, Diehl, HT, Dietrich, JP, Doel, P, Cunha, CE, Eifler, TF, Evrard, AE, Fausti Neto, A, Fernandez, E, Flaugher, B, Fosalba, P, Frieman, J, Gangkofner, C, Gaztanaga, E, Gerdes, D, Gruen, D, Gruendl, RA, Gupta, N, Hennig, C, Holzapfel, WL, Honscheid, K, Jain, B, James, D, Kuehn, K, Kuropatkin, N, Lahav, O, Li, TS, Lin, H, Maia, MAG, March, M, Marshall, JL, Martini, P, McDonald, M, Miller, CJ, Miquel, R, Nord, B, Ogando, R, Plazas, AA, Reichardt, CL, Romer, AK, Roodman, A, Sako, M, Sanchez, E, Schubnell, M, Sevilla, I, Smith, RC, Stalder, B, Stark, AA, Strazzullo, V, Suchyta, E, Swanson, MEC, Tarle, G, Thaler, J, Thomas, D, Tucker, D, Vikram, V, von der Linden, A, Walker, AR, Wechsler, RH, Wester, W, Zenteno, A & Ziegler, KE 2015, 'Constraints on the richness-mass relation and the optical-SZE positional offset distribution for SZE-selected clusters', Monthly Notices of the Royal Astronomical Society, vol. 454, no. 3, pp. 2305-2319. https://doi.org/10.1093/mnras/stv2141

TY - JOUR

T1 - Constraints on the richness-mass relation and the optical-SZE positional offset distribution for SZE-selected clusters

AU - Saro, A.

AU - Bocquet, S.

AU - Rozo, E.

AU - Benson, B. A.

AU - Mohr, J.

AU - Rykoff, E. S.

AU - Soares-Santos, M.

AU - Bleem, L.

AU - Dodelson, S.

AU - Melchior, P.

AU - Sobreira, F.

AU - Upadhyay, V.

AU - Weller, J.

AU - Abbott, T.

AU - Abdalla, F. B.

AU - Allam, S.

AU - Armstrong, R.

AU - Banerji, M.

AU - Bauer, A. H.

AU - Bayliss, M.

AU - Benoit-Lévy, A.

AU - Bernstein, G. M.

AU - Bertin, E.

AU - Brodwin, M.

AU - Brooks, D.

AU - Buckley-Geer, E.

AU - Burke, D. L.

AU - Carlstrom, J. E.

AU - Capasso, R.

AU - Capozzi, D.

AU - Carnero Rosell, A.

AU - Carrasco Kind, M.

AU - Chiu, I.

AU - Covarrubias, R.

AU - Crawford, T. M.

AU - Crocce, M.

AU - D'Andrea, C. B.

AU - da Costa, L. N.

AU - DePoy, D. L.

AU - Desai, S.

AU - de Haan, T.

AU - Diehl, H. T.

AU - Dietrich, J. P.

AU - Doel, P.

AU - Cunha, C. E.

AU - Eifler, T. F.

AU - Evrard, A. E.

AU - Fausti Neto, A.

AU - Fernandez, E.

AU - Flaugher, B.

AU - Fosalba, P.

AU - Frieman, J.

AU - Gangkofner, C.

AU - Gaztanaga, E.

AU - Gerdes, D.

AU - Gruen, D.

AU - Gruendl, R. A.

AU - Gupta, N.

AU - Hennig, C.

AU - Holzapfel, W. L.

AU - Honscheid, K.

AU - Jain, B.

AU - James, D.

AU - Kuehn, K.

AU - Kuropatkin, N.

AU - Lahav, O.

AU - Li, T. S.

AU - Lin, H.

AU - Maia, M. A.G.

AU - March, M.

AU - Marshall, J. L.

AU - Martini, Paul

AU - McDonald, M.

AU - Miller, C. J.

AU - Miquel, R.

AU - Nord, B.

AU - Ogando, R.

AU - Plazas, A. A.

AU - Reichardt, C. L.

AU - Romer, A. K.

AU - Roodman, A.

AU - Sako, M.

AU - Sanchez, E.

AU - Schubnell, M.

AU - Sevilla, I.

AU - Smith, R. C.

AU - Stalder, B.

AU - Stark, A. A.

AU - Strazzullo, V.

AU - Suchyta, E.

AU - Swanson, M. E.C.

AU - Tarle, G.

AU - Thaler, J.

AU - Thomas, D.

AU - Tucker, D.

AU - Vikram, V.

AU - von der Linden, A.

AU - Walker, A. R.

AU - Wechsler, R. H.

AU - Wester, W.

AU - Zenteno, A.

AU - Ziegler, K. E.

PY - 2015/12/11

Y1 - 2015/12/11

N2 - We cross-match galaxy cluster candidates selected via their Sunyaev-Zel'dovich effect (SZE) signatures in 129.1 deg2 of the South Pole Telescope 2500d SPT-SZ survey with optically identified clusters selected from the Dark Energy Survey science verification data. We identify 25 clusters between 0.1 ≲ z ≲ 0.8 in the union of the SPT-SZ and redMaPPer (RM) samples. RM is an optical cluster finding algorithm that also returns a richness estimate for each cluster. We model the richness λ-mass relation with the following function 〈lnλ|M500〉 ∝ BλlnM500 + Cλln E(z) and use SPT-SZ cluster masses and RM richnesses λ to constrain the parameters. We find Bλ = 1.14-0.18+0.21 and Cλ = 0.73-0.75+0.77. The associated scatter in mass at fixed richness is σlnM|λ = 0.18-0.05+0.08 at a characteristic richness λ=70.We demonstrate that our model provides an adequate description of the matched sample, showing that the fraction of SPT-SZ-selected clusters with RM counterparts is consistent with expectations and that the fraction of RMselected clusters with SPT-SZ counterparts is in mild tension with expectation. We model the optical-SZE cluster positional offset distribution with the sum of two Gaussians, showing that it is consistent with a dominant, centrally peaked population and a subdominant population characterized by larger offsets. We also cross-match the RMcatalogue with SPT-SZ candidates below the official catalogue threshold significance ξ = 4.5, using the RM catalogue to provide optical confirmation and redshifts for 15 additional clusters with ξ ∈ [4, 4.5].

AB - We cross-match galaxy cluster candidates selected via their Sunyaev-Zel'dovich effect (SZE) signatures in 129.1 deg2 of the South Pole Telescope 2500d SPT-SZ survey with optically identified clusters selected from the Dark Energy Survey science verification data. We identify 25 clusters between 0.1 ≲ z ≲ 0.8 in the union of the SPT-SZ and redMaPPer (RM) samples. RM is an optical cluster finding algorithm that also returns a richness estimate for each cluster. We model the richness λ-mass relation with the following function 〈lnλ|M500〉 ∝ BλlnM500 + Cλln E(z) and use SPT-SZ cluster masses and RM richnesses λ to constrain the parameters. We find Bλ = 1.14-0.18+0.21 and Cλ = 0.73-0.75+0.77. The associated scatter in mass at fixed richness is σlnM|λ = 0.18-0.05+0.08 at a characteristic richness λ=70.We demonstrate that our model provides an adequate description of the matched sample, showing that the fraction of SPT-SZ-selected clusters with RM counterparts is consistent with expectations and that the fraction of RMselected clusters with SPT-SZ counterparts is in mild tension with expectation. We model the optical-SZE cluster positional offset distribution with the sum of two Gaussians, showing that it is consistent with a dominant, centrally peaked population and a subdominant population characterized by larger offsets. We also cross-match the RMcatalogue with SPT-SZ candidates below the official catalogue threshold significance ξ = 4.5, using the RM catalogue to provide optical confirmation and redshifts for 15 additional clusters with ξ ∈ [4, 4.5].

KW - Catalogues

KW - Cosmology: miscellaneous

KW - Galaxies: abundances

KW - Galaxies: clusters: general

KW - Galaxies: haloes

KW - Galaxies: statistics

KW - Large-scale structure of Universe

KW - Methods: data analysis

UR - http://www.scopus.com/inward/record.url?scp=85040254034&partnerID=8YFLogxK

U2 - 10.1093/mnras/stv2141

DO - 10.1093/mnras/stv2141

M3 - Article

AN - SCOPUS:85040254034

SN - 0035-8711

VL - 454

SP - 2305

EP - 2319

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 3

ER -

Constraints on the richness-mass relation and the optical-SZE positional offset distribution for SZE-selected clusters

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Keywords

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