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Selection function of clusters in Dark Energy Survey year 3 data from cross-matching with South Pole Telescope detections

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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. et al.
In: Astronomy and Astrophysics, Vol. 700, A15, 31.08.2025.

Research output: Contribution to Journal/Magazine › Journal article › peer-review

Harvard

Grandis, S, Costanzi, M, Mohr, JJ, Bleem, LE, Wu, H-Y, Aguena, M, Allam, S, Andrade-Oliveira, F, Bocquet, S, Brooks, D, Carnero Rosell, A, Carretero, J, Da Costa, LN, Pereira, MES, Davis, TM, Desai, S, Diehl, HT, Doel, P, Everett, S, Flaugher, B, Frieman, J, García-Bellido, J, Gaztanaga, E, Gruen, D, Gruendl, RA, Gutierrez, G, Hinton, SR, Hlacacek-Larrondo, J, Hollowood, DL, Honscheid, K, James, DJ, Klein, M, Marshall, JL, Mena-Fernández, J, Miquel, R, Palmese, A, Plazas Malagón, AA, Reichardt, CL, Romer, AK, Samuroff, S, Sanchez Cid, D, Sanchez, E, Santiago, B, Saro, A, Sevilla-Noarbe, I, Smith, M, Soares-Santos, M, Sommer, MW, Suchyta, E, Tarle, G, To, C, Tucker, DL, Weaverdyck, N, Weller, J & Wiseman, P 2025, 'Selection function of clusters in Dark Energy Survey year 3 data from cross-matching with South Pole Telescope detections', Astronomy and Astrophysics, vol. 700, A15. https://doi.org/10.1051/0004-6361/202554177

APA

Grandis, S., Costanzi, M., Mohr, J. J., Bleem, L. E., Wu, H.-Y., Aguena, M., Allam, S., Andrade-Oliveira, F., Bocquet, S., Brooks, D., Carnero Rosell, A., Carretero, J., Da Costa, L. N., Pereira, M. E. S., Davis, T. M., Desai, S., Diehl, H. T., Doel, P., Everett, S., ... Wiseman, P. (2025). Selection function of clusters in Dark Energy Survey year 3 data from cross-matching with South Pole Telescope detections. Astronomy and Astrophysics, 700, Article A15. Advance online publication. https://doi.org/10.1051/0004-6361/202554177

Vancouver

Grandis S, Costanzi M, Mohr JJ, Bleem LE, Wu HY, Aguena M et al. Selection function of clusters in Dark Energy Survey year 3 data from cross-matching with South Pole Telescope detections. Astronomy and Astrophysics. 2025 Aug 31;700:A15. Epub 2025 Jul 25. doi: 10.1051/0004-6361/202554177

Author

Grandis, S. ; Costanzi, M. ; Mohr, J.J. et al. / Selection function of clusters in Dark Energy Survey year 3 data from cross-matching with South Pole Telescope detections. In: Astronomy and Astrophysics. 2025 ; Vol. 700.

Bibtex

@article{66609b8db52a45f9b10902e44d49ebea,
title = "Selection function of clusters in Dark Energy Survey year 3 data from cross-matching with South Pole Telescope detections",
abstract = "Context. Galaxy clusters selected based on overdensities of galaxies in photometric surveys provide the largest cluster samples. However, modeling the selection function of such samples is complicated by noncluster members projected along the line of sight (projection effects) and the potential detection of unvirialized objects (contamination).Aims. We empirically constrained the magnitude of these effects by cross-matching galaxy clusters selected in the Dark Energy Survey data with the redMaPPer  algorithm with significant detections in three South Pole Telescope surveys (SZ, pol-ECS, pol-500d).Methods. For matched clusters, we augmented the redMaPPer catalog with the SPT detection significance. For unmatched objects we used the SPT detection threshold as an upper limit on the SZe signature. Using a Bayesian population model applied to the collected multiwavelength data, we explored various physically motivated models to describe the relationship between observed richness and halo mass.Results. Our analysis reveals a clear preference for models with an additional skewed scatter component associated with projection effects over a purely log-normal scatter model. 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 that requires a combination of simulation and data-driven approaches.",
author = "S. Grandis and M. Costanzi and J.J. Mohr and L.E. Bleem and H.-Y. Wu and M. Aguena and S. Allam and F. Andrade-Oliveira and S. Bocquet and D. Brooks and {Carnero Rosell}, A. and J. Carretero and {Da Costa}, L.N. and M.E.S. Pereira and T.M. Davis and S. Desai and H.T. Diehl and P. Doel and S. Everett and B. Flaugher and J. Frieman and J. Garc{\'i}a-Bellido and E. Gaztanaga and D. Gruen and R.A. Gruendl and G. Gutierrez and S.R. Hinton and J. Hlacacek-Larrondo and D.L. Hollowood and K. Honscheid and D.J. James and M. Klein and J.L. Marshall and J. Mena-Fern{\'a}ndez and R. Miquel and A. Palmese and {Plazas Malag{\'o}n}, A.A. and C.L. Reichardt and A.K. Romer and S. Samuroff and {Sanchez Cid}, D. and E. Sanchez and B. Santiago and A. Saro and I. Sevilla-Noarbe and M. Smith and M. Soares-Santos and M.W. Sommer and E. Suchyta and G. Tarle and C. To and D.L. Tucker and N. Weaverdyck and J. Weller and P. Wiseman",
year = "2025",
month = jul,
day = "25",
doi = "10.1051/0004-6361/202554177",
language = "English",
volume = "700",
journal = "Astronomy and Astrophysics",
issn = "1432-0746",
publisher = "EDP Sciences",

}

RIS

TY - JOUR

T1 - Selection function of clusters in Dark Energy Survey year 3 data from cross-matching with South Pole Telescope detections

AU - Grandis, S.

AU - Costanzi, M.

AU - Mohr, J.J.

AU - Bleem, L.E.

AU - Wu, H.-Y.

AU - Aguena, M.

AU - Allam, S.

AU - Andrade-Oliveira, F.

AU - Bocquet, S.

AU - Brooks, D.

AU - Carnero Rosell, A.

AU - Carretero, J.

AU - Da Costa, L.N.

AU - Pereira, M.E.S.

AU - Davis, T.M.

AU - Desai, S.

AU - Diehl, H.T.

AU - Doel, P.

AU - Everett, S.

AU - Flaugher, B.

AU - Frieman, J.

AU - García-Bellido, J.

AU - Gaztanaga, E.

AU - Gruen, D.

AU - Gruendl, R.A.

AU - Gutierrez, G.

AU - Hinton, S.R.

AU - Hlacacek-Larrondo, J.

AU - Hollowood, D.L.

AU - Honscheid, K.

AU - James, D.J.

AU - Klein, M.

AU - Marshall, J.L.

AU - Mena-Fernández, J.

AU - Miquel, R.

AU - Palmese, A.

AU - Plazas Malagón, A.A.

AU - Reichardt, C.L.

AU - Romer, A.K.

AU - Samuroff, S.

AU - Sanchez Cid, D.

AU - Sanchez, E.

AU - Santiago, B.

AU - Saro, A.

AU - Sevilla-Noarbe, I.

AU - Smith, M.

AU - Soares-Santos, M.

AU - Sommer, M.W.

AU - Suchyta, E.

AU - Tarle, G.

AU - To, C.

AU - Tucker, D.L.

AU - Weaverdyck, N.

AU - Weller, J.

AU - Wiseman, P.

PY - 2025/7/25

Y1 - 2025/7/25

N2 - Context. Galaxy clusters selected based on overdensities of galaxies in photometric surveys provide the largest cluster samples. However, modeling the selection function of such samples is complicated by noncluster members projected along the line of sight (projection effects) and the potential detection of unvirialized objects (contamination).Aims. We empirically constrained the magnitude of these effects by cross-matching galaxy clusters selected in the Dark Energy Survey data with the redMaPPer  algorithm with significant detections in three South Pole Telescope surveys (SZ, pol-ECS, pol-500d).Methods. For matched clusters, we augmented the redMaPPer catalog with the SPT detection significance. For unmatched objects we used the SPT detection threshold as an upper limit on the SZe signature. Using a Bayesian population model applied to the collected multiwavelength data, we explored various physically motivated models to describe the relationship between observed richness and halo mass.Results. Our analysis reveals a clear preference for models with an additional skewed scatter component associated with projection effects over a purely log-normal scatter model. 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 that requires a combination of simulation and data-driven approaches.

AB - Context. Galaxy clusters selected based on overdensities of galaxies in photometric surveys provide the largest cluster samples. However, modeling the selection function of such samples is complicated by noncluster members projected along the line of sight (projection effects) and the potential detection of unvirialized objects (contamination).Aims. We empirically constrained the magnitude of these effects by cross-matching galaxy clusters selected in the Dark Energy Survey data with the redMaPPer  algorithm with significant detections in three South Pole Telescope surveys (SZ, pol-ECS, pol-500d).Methods. For matched clusters, we augmented the redMaPPer catalog with the SPT detection significance. For unmatched objects we used the SPT detection threshold as an upper limit on the SZe signature. Using a Bayesian population model applied to the collected multiwavelength data, we explored various physically motivated models to describe the relationship between observed richness and halo mass.Results. Our analysis reveals a clear preference for models with an additional skewed scatter component associated with projection effects over a purely log-normal scatter model. 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 that requires a combination of simulation and data-driven approaches.

U2 - 10.1051/0004-6361/202554177

DO - 10.1051/0004-6361/202554177

M3 - Journal article

VL - 700

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

SN - 1432-0746

M1 - A15

ER -