Constraints on the Richness-Mass Relation and the Optical-SZE Positional Offset Distribution for SZE-Selected Clusters

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

doi:10.1093/mnras/stv2141

Article
Report number	arXiv:1506.07814 ; FERMILAB-PUB-15-295-AE
Title	Constraints on the Richness-Mass Relation and the Optical-SZE Positional Offset Distribution for SZE-Selected Clusters
Author(s)	Saro, A. (Munich U. ; Munich, Tech. U., Universe) ; Bocquet, S. (Munich U. ; Munich, Tech. U., Universe) ; Rozo, E. (Arizona U.) ; Benson, B.A. (Fermilab ; Chicago U., KICP ; Chicago U., Astron. Astrophys. Ctr.) ; Mohr, J. (Munich U. ; Munich, Tech. U., Universe ; Garching, Max Planck Inst., MPE) ; Rykoff, E.S. (KIPAC, Menlo Park ; SLAC) ; Soares-Santos, M. (Fermilab) ; Bleem, L. (Chicago U., KICP ; Argonne) ; Dodelson, S. (Fermilab ; Chicago U., KICP ; Chicago U., Astron. Astrophys. Ctr.) ; Melchior, P. (Ohio State U., CCAPP ; Ohio State U.) ; Sobreira, F. (Fermilab ; LIneA, Rio de Janeiro) ; Upadhyay, V. (CERN) ; Weller, J. (Munich, Tech. U., Universe ; Garching, Max Planck Inst., MPE ; Munich U.) ; Abbott, T. (Cerro-Tololo InterAmerican Obs.) ; Abdalla, F.B. (University Coll. London) ; Allam, S. (Fermilab) ; Armstrong, R. (Pennsylvania U.) ; Banerji, M. (Cambridge U., Inst. of Astron.) ; Bauer, A.H. (Barcelona, IEEC) ; Bayliss, M. (Harvard U. ; Harvard-Smithsonian Ctr. Astrophys.) ; Benoit-Lévy, A. (University Coll. London) ; Bernstein, G.M. (Pennsylvania U.) ; Bertin, E. (Paris, Inst. Astrophys.) ; Brodwin, M. (Missouri U.) ; Brooks, D. (University Coll. London) ; Buckley-Geer, E. (Fermilab) ; Burke, D.L. (KIPAC, Menlo Park ; SLAC) ; Carlstrom, J.E. (Chicago U., KICP ; Chicago U., Astron. Astrophys. Ctr. ; Chicago U., EFI) ; Capasso, R. (Munich U. ; Munich, Tech. U., Universe) ; Capozzi, D. (Portsmouth U., ICG) ; Carnero Rosell, A. (LIneA, Rio de Janeiro ; Rio de Janeiro Observ.) ; Carrasco Kind, M. (Illinois U., Urbana, Astron. Dept. ; Illinois U., Urbana) ; Chiu, I. (Munich U. ; Munich, Tech. U., Universe) ; Covarrubias, R. (Illinois U., Urbana) ; Crawford, T.M. (Chicago U., KICP ; Chicago U., Astron. Astrophys. Ctr.) ; Crocce, M. (Barcelona, IEEC) ; D'Andrea, C.B. (Portsmouth U., ICG) ; da Costa, L.N. (LIneA, Rio de Janeiro ; Rio de Janeiro Observ.) ; DePoy, D.L. (Texas A-M) ; Desai, S. (Munich U.) ; de Haan, T. (McGill U. ; UC, Berkeley) ; Diehl, H.T. (Fermilab) ; Dietrich, J.P. (Munich U. ; Munich, Tech. U., Universe) ; Doel, P. (University Coll. London) ; Cunha, C.E. (KIPAC, Menlo Park) ; Eifler, T.F. (Pennsylvania U. ; Caltech) ; Evrard, A.E. (Michigan U.) ; Fausti Neto, A. (LIneA, Rio de Janeiro) ; Fernandez, E. (Barcelona, IFAE) ; Flaugher, B. (Fermilab) ; Fosalba, P. (Barcelona, IEEC) ; Frieman, J. (Fermilab ; Chicago U., KICP) ; Gangkofner, C. (Munich U. ; Munich, Tech. U., Universe) ; Gaztanaga, E. (Barcelona, IEEC) ; Gerdes, D. (Michigan U.) ; Gruen, D. (Garching, Max Planck Inst., MPE ; Munich U.) ; Gruendl, R.A. (Illinois U., Urbana, Astron. Dept. ; Illinois U., Urbana) ; Gupta, N. (Munich U. ; Munich, Tech. U., Universe) ; Hennig, C. (Munich U. ; Munich, Tech. U., Universe) ; Holzapfel, W.L. (UC, Berkeley) ; Honscheid, K. (Ohio State U., CCAPP ; Ohio State U.) ; Jain, B. (Pennsylvania U.) ; James, D. (Cerro-Tololo InterAmerican Obs.) ; Kuehn, K. (Australia, CSIRO, North Ryde) ; Kuropatkin, N. (Fermilab) ; Lahav, O. (University Coll. London) ; Li, T.S. (Texas A-M) ; Lin, H. (Fermilab) ; Maia, M.A.G. (LIneA, Rio de Janeiro ; Rio de Janeiro Observ.) ; March, M. (Pennsylvania U.) ; Marshall, J.L. (Texas A-M) ; Martini, Paul (Ohio State U., CCAPP ; Ohio State U., Dept. Astron.) ; McDonald, M. (MIT) ; Miller, C.J. (Michigan U.) ; Miquel, R. (Barcelona, IFAE) ; Nord, B. (Fermilab) ; Ogando, R. (LIneA, Rio de Janeiro ; Rio de Janeiro Observ.) ; Plazas, A.A. (Caltech ; Brookhaven) ; Reichardt, C.L. (UC, Berkeley ; Melbourne U.) ; Romer, A.K. (Sussex U.) ; Roodman, A. (KIPAC, Menlo Park ; SLAC) ; Sako, M. (Pennsylvania U.) ; Sanchez, E. (Madrid, CIEMAT) ; Schubnell, M. (Michigan U.) ; Sevilla, I. (Illinois U., Urbana, Astron. Dept. ; Madrid, CIEMAT) ; Smith, R.C. (Cerro-Tololo InterAmerican Obs.) ; Stalder, B. (Harvard-Smithsonian Ctr. Astrophys. ; Hawaii U.) ; Stark, A.A. (Harvard-Smithsonian Ctr. Astrophys.) ; Strazzullo, V. (Munich U. ; Munich, Tech. U., Universe) ; Suchyta, E. (Ohio State U., CCAPP ; Ohio State U.) ; Swanson, M.E.C. (Illinois U., Urbana) ; Tarle, G. (Michigan U.) ; Thaler, J. (Illinois U., Urbana) ; Thomas, D. (Portsmouth U., ICG) ; Tucker, D. (Fermilab) ; Vikram, V. (Argonne) ; von der Linden, A. (Stanford U., Phys. Dept.) ; Walker, A.R. (Cerro-Tololo InterAmerican Obs.) ; Wechsler, R.H. (KIPAC, Menlo Park ; SLAC ; Stanford U., Phys. Dept.) ; Wester, W. (Fermilab) ; Zenteno, A. (Cerro-Tololo InterAmerican Obs.) ; Ziegler, K.E. (Chicago U., KICP)
Publication	2015-12-11
Imprint	25 Jun 2015
Number of pages	15
Note	15 pages, 8 Figures, submitted to MNRAS
In:	Mon. Not. R. Astron. Soc. 454 (2015) 2305-2319
DOI	10.1093/mnras/stv2141
Subject category	Astrophysics and Astronomy
Abstract	We cross-match galaxy cluster candidates selected via their Sunyaev-Zel'dovich effect (SZE) signatures in 129.1 deg$^2$ of the South Pole Telescope 2500d SPT-SZ survey with optically identified clusters selected from the Dark Energy Survey (DES) science verification data. We identify 25 clusters between $0.1\lesssim z\lesssim 0.8$ 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 $\lambda$-mass relation with the following function $\langle\ln\lambda\|M_{500}\rangle\propto B_\lambda\ln M_{500}+C_\lambda\ln E(z)$ and use SPT-SZ cluster masses and RM richnesses $\lambda$ to constrain the parameters. We find $B_\lambda= 1.14^{+0.21}_{-0.18}$ and $C_\lambda=0.73^{+0.77}_{-0.75}$. The associated scatter in mass at fixed richness is $\sigma_{\ln M\|\lambda} = 0.18^{+0.08}_{-0.05}$ at a characteristic richness $\lambda=70$. 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 RM selected 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 sub-dominant population characterized by larger offsets. We also cross-match the RM catalog with SPT-SZ candidates below the official catalog threshold significance $\xi=4.5$, using the RM catalog to provide optical confirmation and redshifts for additional low-$\xi$ SPT-SZ candidates.In this way, we identify 15 additional clusters with $\xi\in [4,4.5]$ over the redshift regime explored by RM in the overlapping region between DES science verification data and the SPT-SZ survey.
Copyright/License	arXiv nonexclusive-distrib. 1.0 Publication: © 2015-2025 The Author(s)

$Distribution of probability $p$ of chance associations for the $\xi>4.5$ (filled) and $\xi>4$ (empty) samples. Black lines show the sample used in this work, red lines show the sample rejected (Section \ref{sec:catalog_match}).$ $\textit{Left panel:} Richness as a function of the SZE significance $\xi$ for the matched cluster sample. SPT-SZ candidates with $\xi<4.5$ (vertical line) are shown in red. Clusters at $z<0.25$ (cyan) and clusters with miscentering due to a high masked fraction (magenta) are not used in the richness analysis. Large circles indicate the newly confirmed SPT-SZ candidates with $\xi>4.5$. Solid and dashed lines represent the upper 84 and 95 percentiles in richness of chance associations of SPT-SZ candidates and clusters from the randomly generated RM catalog. \textit{Right panel:} The estimated redshift for the RM sample as a function of SPT redshifts as presented in B15 from independent optical follow-up data. SPT-SZ candidates with spectroscopic redshift are shown in green. Magenta symbols are the same as in the left panel.$ $\textit{Left panel:} Richness as a function of the SZE significance $\xi$ for the matched cluster sample. SPT-SZ candidates with $\xi<4.5$ (vertical line) are shown in red. Clusters at $z<0.25$ (cyan) and clusters with miscentering due to a high masked fraction (magenta) are not used in the richness analysis. Large circles indicate the newly confirmed SPT-SZ candidates with $\xi>4.5$. Solid and dashed lines represent the upper 84 and 95 percentiles in richness of chance associations of SPT-SZ candidates and clusters from the randomly generated RM catalog. \textit{Right panel:} The estimated redshift for the RM sample as a function of SPT redshifts as presented in B15 from independent optical follow-up data. SPT-SZ candidates with spectroscopic redshift are shown in green. Magenta symbols are the same as in the left panel.$ Show more plots

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