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

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 cluster...

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Detalles Bibliográficos
Autores principales: 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., Bayliss, M., Benoit-Lévy, A., Bernstein, G.M., Bertin, E., Brodwin, M., Brooks, D., Buckley-Geer, E., Burke, D.L., Carlstrom, J.E., Capasso, R., Capozzi, D., Carnero Rosell, A., Carrasco Kind, M., Chiu, I., Covarrubias, R., Crawford, T.M., Crocce, M., D'Andrea, C.B., da Costa, L.N., DePoy, D.L., Desai, S., de Haan, T., Diehl, H.T., Dietrich, J.P., Doel, P., Cunha, C.E., Eifler, T.F., Evrard, A.E., Fausti Neto, A., Fernandez, E., Flaugher, B., Fosalba, P., Frieman, J., Gangkofner, C., Gaztanaga, E., Gerdes, D., Gruen, D., Gruendl, R.A., Gupta, N., Hennig, C., Holzapfel, W.L., Honscheid, K., Jain, B., James, D., Kuehn, K., Kuropatkin, N., Lahav, O., Li, T.S., Lin, H., Maia, M.A.G., March, M., Marshall, J.L., Martini, Paul, McDonald, M., Miller, C.J., Miquel, R., Nord, B., Ogando, R., Plazas, A.A., Reichardt, C.L., Romer, A.K., Roodman, A., Sako, M., Sanchez, E., Schubnell, M., Sevilla, I., Smith, R.C., Stalder, B., Stark, A.A., Strazzullo, V., Suchyta, E., Swanson, M.E.C., Tarle, G., Thaler, J., Thomas, D., Tucker, D., Vikram, V., von der Linden, A., Walker, A.R., Wechsler, R.H., Wester, W., Zenteno, A., Ziegler, K.E.
Lenguaje:eng
Publicado: 2015
Materias:
Acceso en línea:https://dx.doi.org/10.1093/mnras/stv2141
http://cds.cern.ch/record/2028348
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author 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.
Bayliss, M.
Benoit-Lévy, A.
Bernstein, G.M.
Bertin, E.
Brodwin, M.
Brooks, D.
Buckley-Geer, E.
Burke, D.L.
Carlstrom, J.E.
Capasso, R.
Capozzi, D.
Carnero Rosell, A.
Carrasco Kind, M.
Chiu, I.
Covarrubias, R.
Crawford, T.M.
Crocce, M.
D'Andrea, C.B.
da Costa, L.N.
DePoy, D.L.
Desai, S.
de Haan, T.
Diehl, H.T.
Dietrich, J.P.
Doel, P.
Cunha, C.E.
Eifler, T.F.
Evrard, A.E.
Fausti Neto, A.
Fernandez, E.
Flaugher, B.
Fosalba, P.
Frieman, J.
Gangkofner, C.
Gaztanaga, E.
Gerdes, D.
Gruen, D.
Gruendl, R.A.
Gupta, N.
Hennig, C.
Holzapfel, W.L.
Honscheid, K.
Jain, B.
James, D.
Kuehn, K.
Kuropatkin, N.
Lahav, O.
Li, T.S.
Lin, H.
Maia, M.A.G.
March, M.
Marshall, J.L.
Martini, Paul
McDonald, M.
Miller, C.J.
Miquel, R.
Nord, B.
Ogando, R.
Plazas, A.A.
Reichardt, C.L.
Romer, A.K.
Roodman, A.
Sako, M.
Sanchez, E.
Schubnell, M.
Sevilla, I.
Smith, R.C.
Stalder, B.
Stark, A.A.
Strazzullo, V.
Suchyta, E.
Swanson, M.E.C.
Tarle, G.
Thaler, J.
Thomas, D.
Tucker, D.
Vikram, V.
von der Linden, A.
Walker, A.R.
Wechsler, R.H.
Wester, W.
Zenteno, A.
Ziegler, K.E.
author_facet 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.
Bayliss, M.
Benoit-Lévy, A.
Bernstein, G.M.
Bertin, E.
Brodwin, M.
Brooks, D.
Buckley-Geer, E.
Burke, D.L.
Carlstrom, J.E.
Capasso, R.
Capozzi, D.
Carnero Rosell, A.
Carrasco Kind, M.
Chiu, I.
Covarrubias, R.
Crawford, T.M.
Crocce, M.
D'Andrea, C.B.
da Costa, L.N.
DePoy, D.L.
Desai, S.
de Haan, T.
Diehl, H.T.
Dietrich, J.P.
Doel, P.
Cunha, C.E.
Eifler, T.F.
Evrard, A.E.
Fausti Neto, A.
Fernandez, E.
Flaugher, B.
Fosalba, P.
Frieman, J.
Gangkofner, C.
Gaztanaga, E.
Gerdes, D.
Gruen, D.
Gruendl, R.A.
Gupta, N.
Hennig, C.
Holzapfel, W.L.
Honscheid, K.
Jain, B.
James, D.
Kuehn, K.
Kuropatkin, N.
Lahav, O.
Li, T.S.
Lin, H.
Maia, M.A.G.
March, M.
Marshall, J.L.
Martini, Paul
McDonald, M.
Miller, C.J.
Miquel, R.
Nord, B.
Ogando, R.
Plazas, A.A.
Reichardt, C.L.
Romer, A.K.
Roodman, A.
Sako, M.
Sanchez, E.
Schubnell, M.
Sevilla, I.
Smith, R.C.
Stalder, B.
Stark, A.A.
Strazzullo, V.
Suchyta, E.
Swanson, M.E.C.
Tarle, G.
Thaler, J.
Thomas, D.
Tucker, D.
Vikram, V.
von der Linden, A.
Walker, A.R.
Wechsler, R.H.
Wester, W.
Zenteno, A.
Ziegler, K.E.
author_sort Saro, A.
collection CERN
description 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.
id cern-2028348
institution Organización Europea para la Investigación Nuclear
language eng
publishDate 2015
record_format invenio
spelling cern-20283482023-08-19T02:34:44Zdoi:10.1093/mnras/stv2141http://cds.cern.ch/record/2028348engSaro, 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.Bayliss, M.Benoit-Lévy, A.Bernstein, G.M.Bertin, E.Brodwin, M.Brooks, D.Buckley-Geer, E.Burke, D.L.Carlstrom, J.E.Capasso, R.Capozzi, D.Carnero Rosell, A.Carrasco Kind, M.Chiu, I.Covarrubias, R.Crawford, T.M.Crocce, M.D'Andrea, C.B.da Costa, L.N.DePoy, D.L.Desai, S.de Haan, T.Diehl, H.T.Dietrich, J.P.Doel, P.Cunha, C.E.Eifler, T.F.Evrard, A.E.Fausti Neto, A.Fernandez, E.Flaugher, B.Fosalba, P.Frieman, J.Gangkofner, C.Gaztanaga, E.Gerdes, D.Gruen, D.Gruendl, R.A.Gupta, N.Hennig, C.Holzapfel, W.L.Honscheid, K.Jain, B.James, D.Kuehn, K.Kuropatkin, N.Lahav, O.Li, T.S.Lin, H.Maia, M.A.G.March, M.Marshall, J.L.Martini, PaulMcDonald, M.Miller, C.J.Miquel, R.Nord, B.Ogando, R.Plazas, A.A.Reichardt, C.L.Romer, A.K.Roodman, A.Sako, M.Sanchez, E.Schubnell, M.Sevilla, I.Smith, R.C.Stalder, B.Stark, A.A.Strazzullo, V.Suchyta, E.Swanson, M.E.C.Tarle, G.Thaler, J.Thomas, D.Tucker, D.Vikram, V.von der Linden, A.Walker, A.R.Wechsler, R.H.Wester, W.Zenteno, A.Ziegler, K.E.Constraints on the Richness-Mass Relation and the Optical-SZE Positional Offset Distribution for SZE-Selected ClustersAstrophysics and AstronomyWe 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.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 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 〈ln λ|M_500〉 ∝ B_λln M_500 + C_λln E(z) and use SPT-SZ cluster masses and RM richnesses λ 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 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 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 subdominant population characterized by larger offsets. We also cross-match the RM catalogue 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].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.arXiv:1506.07814FERMILAB-PUB-15-295-AEoai:cds.cern.ch:20283482015-06-25
spellingShingle Astrophysics and Astronomy
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.
Bayliss, M.
Benoit-Lévy, A.
Bernstein, G.M.
Bertin, E.
Brodwin, M.
Brooks, D.
Buckley-Geer, E.
Burke, D.L.
Carlstrom, J.E.
Capasso, R.
Capozzi, D.
Carnero Rosell, A.
Carrasco Kind, M.
Chiu, I.
Covarrubias, R.
Crawford, T.M.
Crocce, M.
D'Andrea, C.B.
da Costa, L.N.
DePoy, D.L.
Desai, S.
de Haan, T.
Diehl, H.T.
Dietrich, J.P.
Doel, P.
Cunha, C.E.
Eifler, T.F.
Evrard, A.E.
Fausti Neto, A.
Fernandez, E.
Flaugher, B.
Fosalba, P.
Frieman, J.
Gangkofner, C.
Gaztanaga, E.
Gerdes, D.
Gruen, D.
Gruendl, R.A.
Gupta, N.
Hennig, C.
Holzapfel, W.L.
Honscheid, K.
Jain, B.
James, D.
Kuehn, K.
Kuropatkin, N.
Lahav, O.
Li, T.S.
Lin, H.
Maia, M.A.G.
March, M.
Marshall, J.L.
Martini, Paul
McDonald, M.
Miller, C.J.
Miquel, R.
Nord, B.
Ogando, R.
Plazas, A.A.
Reichardt, C.L.
Romer, A.K.
Roodman, A.
Sako, M.
Sanchez, E.
Schubnell, M.
Sevilla, I.
Smith, R.C.
Stalder, B.
Stark, A.A.
Strazzullo, V.
Suchyta, E.
Swanson, M.E.C.
Tarle, G.
Thaler, J.
Thomas, D.
Tucker, D.
Vikram, V.
von der Linden, A.
Walker, A.R.
Wechsler, R.H.
Wester, W.
Zenteno, A.
Ziegler, K.E.
Constraints on the Richness-Mass Relation and the Optical-SZE Positional Offset Distribution for SZE-Selected Clusters
title Constraints on the Richness-Mass Relation and the Optical-SZE Positional Offset Distribution for SZE-Selected Clusters
title_full Constraints on the Richness-Mass Relation and the Optical-SZE Positional Offset Distribution for SZE-Selected Clusters
title_fullStr Constraints on the Richness-Mass Relation and the Optical-SZE Positional Offset Distribution for SZE-Selected Clusters
title_full_unstemmed Constraints on the Richness-Mass Relation and the Optical-SZE Positional Offset Distribution for SZE-Selected Clusters
title_short Constraints on the Richness-Mass Relation and the Optical-SZE Positional Offset Distribution for SZE-Selected Clusters
title_sort constraints on the richness-mass relation and the optical-sze positional offset distribution for sze-selected clusters
topic Astrophysics and Astronomy
url https://dx.doi.org/10.1093/mnras/stv2141
http://cds.cern.ch/record/2028348
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AT lits constraintsontherichnessmassrelationandtheopticalszepositionaloffsetdistributionforszeselectedclusters
AT linh constraintsontherichnessmassrelationandtheopticalszepositionaloffsetdistributionforszeselectedclusters
AT maiamag constraintsontherichnessmassrelationandtheopticalszepositionaloffsetdistributionforszeselectedclusters
AT marchm constraintsontherichnessmassrelationandtheopticalszepositionaloffsetdistributionforszeselectedclusters
AT marshalljl constraintsontherichnessmassrelationandtheopticalszepositionaloffsetdistributionforszeselectedclusters
AT martinipaul constraintsontherichnessmassrelationandtheopticalszepositionaloffsetdistributionforszeselectedclusters
AT mcdonaldm constraintsontherichnessmassrelationandtheopticalszepositionaloffsetdistributionforszeselectedclusters
AT millercj constraintsontherichnessmassrelationandtheopticalszepositionaloffsetdistributionforszeselectedclusters
AT miquelr constraintsontherichnessmassrelationandtheopticalszepositionaloffsetdistributionforszeselectedclusters
AT nordb constraintsontherichnessmassrelationandtheopticalszepositionaloffsetdistributionforszeselectedclusters
AT ogandor constraintsontherichnessmassrelationandtheopticalszepositionaloffsetdistributionforszeselectedclusters
AT plazasaa constraintsontherichnessmassrelationandtheopticalszepositionaloffsetdistributionforszeselectedclusters
AT reichardtcl constraintsontherichnessmassrelationandtheopticalszepositionaloffsetdistributionforszeselectedclusters
AT romerak constraintsontherichnessmassrelationandtheopticalszepositionaloffsetdistributionforszeselectedclusters
AT roodmana constraintsontherichnessmassrelationandtheopticalszepositionaloffsetdistributionforszeselectedclusters
AT sakom constraintsontherichnessmassrelationandtheopticalszepositionaloffsetdistributionforszeselectedclusters
AT sancheze constraintsontherichnessmassrelationandtheopticalszepositionaloffsetdistributionforszeselectedclusters
AT schubnellm constraintsontherichnessmassrelationandtheopticalszepositionaloffsetdistributionforszeselectedclusters
AT sevillai constraintsontherichnessmassrelationandtheopticalszepositionaloffsetdistributionforszeselectedclusters
AT smithrc constraintsontherichnessmassrelationandtheopticalszepositionaloffsetdistributionforszeselectedclusters
AT stalderb constraintsontherichnessmassrelationandtheopticalszepositionaloffsetdistributionforszeselectedclusters
AT starkaa constraintsontherichnessmassrelationandtheopticalszepositionaloffsetdistributionforszeselectedclusters
AT strazzullov constraintsontherichnessmassrelationandtheopticalszepositionaloffsetdistributionforszeselectedclusters
AT suchytae constraintsontherichnessmassrelationandtheopticalszepositionaloffsetdistributionforszeselectedclusters
AT swansonmec constraintsontherichnessmassrelationandtheopticalszepositionaloffsetdistributionforszeselectedclusters
AT tarleg constraintsontherichnessmassrelationandtheopticalszepositionaloffsetdistributionforszeselectedclusters
AT thalerj constraintsontherichnessmassrelationandtheopticalszepositionaloffsetdistributionforszeselectedclusters
AT thomasd constraintsontherichnessmassrelationandtheopticalszepositionaloffsetdistributionforszeselectedclusters
AT tuckerd constraintsontherichnessmassrelationandtheopticalszepositionaloffsetdistributionforszeselectedclusters
AT vikramv constraintsontherichnessmassrelationandtheopticalszepositionaloffsetdistributionforszeselectedclusters
AT vonderlindena constraintsontherichnessmassrelationandtheopticalszepositionaloffsetdistributionforszeselectedclusters
AT walkerar constraintsontherichnessmassrelationandtheopticalszepositionaloffsetdistributionforszeselectedclusters
AT wechslerrh constraintsontherichnessmassrelationandtheopticalszepositionaloffsetdistributionforszeselectedclusters
AT westerw constraintsontherichnessmassrelationandtheopticalszepositionaloffsetdistributionforszeselectedclusters
AT zentenoa constraintsontherichnessmassrelationandtheopticalszepositionaloffsetdistributionforszeselectedclusters
AT zieglerke constraintsontherichnessmassrelationandtheopticalszepositionaloffsetdistributionforszeselectedclusters