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Selection Function of Clusters in Dark Energy Survey Year 3 Data from Cross-Matching with South Pole Telescope Detections

Fuente: arXiv

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Main Authors:	Grandis, S., Costanzi, M., Mohr, J. J., Bleem, L. E., Wu, H. -Y., Aguena, M., Allam, S., Andrade-Oliveira, F., Bocquet, S., Brooks, D., Rosell, A. Carnero, Carretero, J., da Costa, L. N., Pereira, M. E. S., Davis, T. M., Desai, S., Diehl, H. T., Doel, P., Everett, S., Flaugher, B., Frieman, J., García-Bellido, J., Gaztanaga, E., Gruen, D., Gruendl, R. A., Gutierrez, G., Hinton, S. R., Hlacacek-Larrondo, J., Hollowood, D. L., Honscheid, K., James, D. J., Klein, M., Marshall, J. L., Mena-Fernández, J., Miquel, R., Palmese, A., Malagón, A. A. Plazas, Reichardt, C. L., Romer, A. K., Samuroff, S., Cid, D. Sanchez, Sanchez, E., Santiago, B., Saro, A., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Sommer, M. W., Suchyta, E., Tarle, G., To, C., Tucker, D. L., Weaverdyck, N., Weller, J., Wiseman, P.
Format:	Preprint
Published:	2025
Subjects:	Cosmology and Nongalactic Astrophysics
Online Access:	Acceder al recurso
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_version_	1866916867656908800
author	Grandis, S. Costanzi, M. Mohr, J. J. Bleem, L. E. Wu, H. -Y. Aguena, M. Allam, S. Andrade-Oliveira, F. Bocquet, S. Brooks, D. Rosell, A. Carnero Carretero, J. da Costa, L. N. Pereira, M. E. S. Davis, T. M. Desai, S. Diehl, H. T. Doel, P. Everett, S. Flaugher, B. Frieman, J. García-Bellido, J. Gaztanaga, E. Gruen, D. Gruendl, R. A. Gutierrez, G. Hinton, S. R. Hlacacek-Larrondo, J. Hollowood, D. L. Honscheid, K. James, D. J. Klein, M. Marshall, J. L. Mena-Fernández, J. Miquel, R. Palmese, A. Malagón, A. A. Plazas Reichardt, C. L. Romer, A. K. Samuroff, S. Cid, D. Sanchez Sanchez, E. Santiago, B. Saro, A. Sevilla-Noarbe, I. Smith, M. Soares-Santos, M. Sommer, M. W. Suchyta, E. Tarle, G. To, C. Tucker, D. L. Weaverdyck, N. Weller, J. Wiseman, P.
author_facet	Grandis, S. Costanzi, M. Mohr, J. J. Bleem, L. E. Wu, H. -Y. Aguena, M. Allam, S. Andrade-Oliveira, F. Bocquet, S. Brooks, D. Rosell, A. Carnero Carretero, J. da Costa, L. N. Pereira, M. E. S. Davis, T. M. Desai, S. Diehl, H. T. Doel, P. Everett, S. Flaugher, B. Frieman, J. García-Bellido, J. Gaztanaga, E. Gruen, D. Gruendl, R. A. Gutierrez, G. Hinton, S. R. Hlacacek-Larrondo, J. Hollowood, D. L. Honscheid, K. James, D. J. Klein, M. Marshall, J. L. Mena-Fernández, J. Miquel, R. Palmese, A. Malagón, A. A. Plazas Reichardt, C. L. Romer, A. K. Samuroff, S. Cid, D. Sanchez Sanchez, E. Santiago, B. Saro, A. Sevilla-Noarbe, I. Smith, M. Soares-Santos, M. Sommer, M. W. Suchyta, E. Tarle, G. To, C. Tucker, D. L. Weaverdyck, N. Weller, J. Wiseman, P.
contents	Galaxy clusters selected based on overdensities of galaxies in photometric surveys provide the largest cluster samples. Yet modeling the selection function of such samples is complicated by non-cluster members projected along the line of sight (projection effects) and the potential detection of unvirialized objects (contamination). We empirically constrain the magnitude of these effects by cross-matching galaxy clusters selected in the Dark Energy survey data with the \rdmpr$\,$ algorithm with significant detections in three South Pole Telescope surveys (SZ, pol-ECS, pol-500d). For matched clusters, we augment the \rdmpr$\,$catalog by the SPT detection significance. For unmatched objects we use the SPT detection threshold as an upper limit on the SZe signature. Using a Bayesian population model applied to the collected multi-wavelength data, we explore various physically motivated models to describe the relationship between observed richness and halo mass. Our analysis reveals the limitations of a simple lognormal scatter model in describing the data. We rule out significant contamination by unvirialized objects at the high-richness end of the sample. While dedicated simulations offer a well-fitting calibration of projection effects, our findings suggest the presence of redshift-dependent trends that these simulations may not have captured. Our findings highlight that modeling the selection function of optically detected clusters remains a complicated challenge, requiring a combination of simulation and data-driven approaches.
format	Preprint
id	arxiv_https___arxiv_org_abs_2502_12914
institution	arXiv
publishDate	2025
record_format	arxiv
spellingShingle	Selection Function of Clusters in Dark Energy Survey Year 3 Data from Cross-Matching with South Pole Telescope Detections Grandis, S. Costanzi, M. Mohr, J. J. Bleem, L. E. Wu, H. -Y. Aguena, M. Allam, S. Andrade-Oliveira, F. Bocquet, S. Brooks, D. Rosell, A. Carnero Carretero, J. da Costa, L. N. Pereira, M. E. S. Davis, T. M. Desai, S. Diehl, H. T. Doel, P. Everett, S. Flaugher, B. Frieman, J. García-Bellido, J. Gaztanaga, E. Gruen, D. Gruendl, R. A. Gutierrez, G. Hinton, S. R. Hlacacek-Larrondo, J. Hollowood, D. L. Honscheid, K. James, D. J. Klein, M. Marshall, J. L. Mena-Fernández, J. Miquel, R. Palmese, A. Malagón, A. A. Plazas Reichardt, C. L. Romer, A. K. Samuroff, S. Cid, D. Sanchez Sanchez, E. Santiago, B. Saro, A. Sevilla-Noarbe, I. Smith, M. Soares-Santos, M. Sommer, M. W. Suchyta, E. Tarle, G. To, C. Tucker, D. L. Weaverdyck, N. Weller, J. Wiseman, P. Cosmology and Nongalactic Astrophysics Galaxy clusters selected based on overdensities of galaxies in photometric surveys provide the largest cluster samples. Yet modeling the selection function of such samples is complicated by non-cluster members projected along the line of sight (projection effects) and the potential detection of unvirialized objects (contamination). We empirically constrain the magnitude of these effects by cross-matching galaxy clusters selected in the Dark Energy survey data with the \rdmpr$\,$ algorithm with significant detections in three South Pole Telescope surveys (SZ, pol-ECS, pol-500d). For matched clusters, we augment the \rdmpr$\,$catalog by the SPT detection significance. For unmatched objects we use the SPT detection threshold as an upper limit on the SZe signature. Using a Bayesian population model applied to the collected multi-wavelength data, we explore various physically motivated models to describe the relationship between observed richness and halo mass. Our analysis reveals the limitations of a simple lognormal scatter model in describing the data. We rule out significant contamination by unvirialized objects at the high-richness end of the sample. While dedicated simulations offer a well-fitting calibration of projection effects, our findings suggest the presence of redshift-dependent trends that these simulations may not have captured. Our findings highlight that modeling the selection function of optically detected clusters remains a complicated challenge, requiring a combination of simulation and data-driven approaches.
title	Selection Function of Clusters in Dark Energy Survey Year 3 Data from Cross-Matching with South Pole Telescope Detections
topic	Cosmology and Nongalactic Astrophysics
url	https://arxiv.org/abs/2502.12914