SPT clusters with DES and HST weak lensing. II. Cosmological constraints from the abundance of massive halos

Journal Article · 02 October 2024 · Phys.Rev.D

DOI: https://doi.org/10.1103/PhysRevD.110.083510 · OSTI ID:2376962

Bocquet, S.  ^[1]; Grandis, S.  ^[2]; Bleem, L. E.  ^[3]; Klein, M.  ^[1]; Mohr, J. J.  ^[4]; Schrabback, T.  ^[5]; Abbott, T. M.C.  ^[6]; Ade, P. A.R. ^[7]; Aguena, M. ^[8]; Alarcon, A. ^[9]; Allam, S.  ^[10]; Allen, S. W. ^[11]; Alves, O. ^[12]; Amon, A. ^[13]; Anderson, A. J.  ^[10]; Annis, J. ^[10]; Ansarinejad, B.  ^[14]; Austermann, J. E. ^[15]; Avila, S.  ^[16]; Bacon, D. ^[17] ; Bayliss, M. ^[18]; Beall, J. A. ^[19]; Bechtol, K. ^[20]; Becker, M. R. ^[9]; Bender, A. N. ^[21]; Benson, B. A. ^[22]; Bernstein, G. M. ^[23]; Bhargava, S. ^[24]; Bianchini, F.  ^[11]; Brodwin, M. ^[25]; Brooks, D. ^[26]; Bryant, L. ^[27]; Campos, A.  ^[28]; Canning, R. E.A. ^[29]; Carlstrom, J. E. ^[30]; Carnero Rosell, A. ^[31]; Carrasco Kind, M. ^[32]; Carretero, J. ^[16]; Castander, F. J. ^[33]; Cawthon, R. ^[34]; Chang, C. L. ^[35]; Chang, C. ^[36]; Chaubal, P. ^[14]; Chen, R. ^[37]; Chiang, H. C. ^[38]; Choi, A. ^[39]; Chou, T-L. ^[40]; Citron, R. ^[27]; Moran, C. Corbett ^[41]; Cordero, J. ^[42]; Costanzi, M. ^[43]; Crawford, T. M. ^[44]; Crites, A. T. ^[45]; da Costa, L. N. ^[8]; Pereira, M. E.S. ^[46]; Davis, C. ^[47]; Davis, T. M.  ^[48]; DeRose, J. ^[49]; Desai, S. ^[50]; de Haan, T. ^[51]; Diehl, H. T.  ^[10]; Dobbs, M. A. ^[52]; Dodelson, S.  ^[28]; Doux, C. ^[53]; Drlica-Wagner, A.  ^[54]; Eckert, K. ^[23]; Elvin-Poole, J. ^[55]; Everett, S. ^[41]; Everett, W. ^[56]; Ferrero, I. ^[57]; Ferté, A. ^[58]; Flores, A. M. ^[59]; Frieman, J.  ^[60]; Gallicchio, J. ^[61]; García-Bellido, J. ^[62]; Gatti, M. ^[23]; George, E. M. ^[63]; Giannini, G.  ^[64]; Gladders, M. D. ^[36]; Gruen, D. ^[1]; Gruendl, R. A. ^[32]; Gupta, N. ^[65]; Gutierrez, G.  ^[10]; Halverson, N. W. ^[56]; Harrison, I. ^[7]; Hartley, W. G. ^[66]; Herner, K. ^[10]; Hinton, S. R. ^[48]; Holder, G. P. ^[67]; Hollowood, D. L. ^[68]; Holzapfel, W. L. ^[69]; Honscheid, K. ^[70]; Hrubes, J. D. ^[27]; Huang, N. ^[69]; Hubmayr, J.  ^[19]; Huff, E. M. ^[41]; Huterer, D. ^[12]; Irwin, K. D. ^[71]; James, D. J. ^[72]; Jarvis, M. ^[23]; Khullar, G. ^[44]; Kim, K. ^[18]; Knox, L. ^[73]; Kraft, R. ^[72]; Krause, E. ^[74]; Kuehn, K. ^[75]; Kuropatkin, N. ^[10]; Kéruzoré, F. ^[9]; Lahav, O. ^[26]; Lee, A. T. ^[76]; Leget, P.-F. ^[77]; Li, D. ^[78]; Lin, H. ^[10]; Lowitz, A. ^[79]; MacCrann, N. ^[80]; Mahler, G. ^[81]; Mantz, A. ^[82]; Marshall, J. L. ^[83]; McCullough, J.  ^[77]; McDonald, M. ^[84]; McMahon, J. J. ^[85]; Mena-Fernández, J. ^[86]; Menanteau, F. ^[32]; Meyer, S. S. ^[85]; Miquel, R. ^[87]; Montgomery, J.  ^[88]; Myles, J. ^[89]; Natoli, T. ^[36]; Navarro-Alsina, A.  ^[90]; Nibarger, J. P. ^[19]; Noble, G. I. ^[91]; Novosad, V. ^[9]; Ogando, R. L.C. ^[92]; Omori, Y. ^[93]; Padin, S. ^[94]; Pandey, S. ^[23]; Paschos, P. ^[27]; Patil, S. ^[14]; Pieres, A. ^[95]; Plazas Malagón, A. A. ^[96]; Porredon, A. ^[97]; Prat, J. ^[36]; Pryke, C. ^[98]; Raveri, M. ^[99]; Reichardt, C. L. ^[14]; Roberson, J. ^[18]; Rollins, R. P. ^[42]; Romero, C. ^[72]; Roodman, A. ^[96]; Ruhl, J. E. ^[100]; Rykoff, E. S. ^[96]; Saliwanchik, B. R. ^[101]; Salvati, L. ^[102]; Sánchez, C. ^[23]; Sanchez, E.  ^[103]; Sanchez Cid, D. ^[103]; Saro, A. ^[104]; Schaffer, K. K. ^[105]; Secco, L. F. ^[93]; Sevilla-Noarbe, I. ^[103]; Sharon, K. ^[106]; Sheldon, E. ^[101]; Shin, T. ^[107]; Sievers, C. ^[27]; Smecher, G. ^[108]; Smith, M. ^[109]; Somboonpanyakul, T. ^[110]; Sommer, M. ^[111]; Stalder, B. ^[72]; Stark, A. A. ^[72]; Stephen, J. ^[27]; Strazzullo, V. ^[43]; Suchyta, E. ^[112]; Tarle, G. ^[12]; To, C. ^[113]; Troxel, M. A. ^[37]; Tucker, C. ^[7]; Tutusaus, I. ^[114]; Varga, T. N. ^[115]; Veach, T. ^[116]; Vieira, J. D. ^[117]; Vikhlinin, A. ^[72]; von der Linden, A. ^[107]; Wang, G. ^[9]; Weaverdyck, N. ^[118]; Weller, J. ^[119]; Whitehorn, N. ^[120]; Wu, W. L.K. ^[58]; Yanny, B.  ^[10]; Yefremenko, V. ^[9]; Yin, B. ^[28]; Young, M. ^[91]; Zebrowski, J. A. ^[121]; Zhang, Y. ^[6]; Zohren, H. ^[111]; Zuntz, J. ^[122]

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1. Munich U.
2. Innsbruck U.; Munich U.
3. Argonne; Chicago U., KICP
4. Munich U.; Garching, Max Planck Inst., MPE
5. Innsbruck U.; Argelander Inst. Astron.
6. Cerro-Tololo InterAmerican Obs.
7. Cardiff U.
8. LIneA, Rio de Janeiro
9. Argonne
10. Fermilab
11. KIPAC, Menlo Park; Stanford U., HEPL; Stanford U.; SLAC
12. U. Michigan, Ann Arbor
13. Cambridge U., Inst. of Astron.; Cambridge U., KICC
14. Melbourne U.
15. NIST, Boulder; Colorado U.
16. Barcelona, IFAE
17. Portsmouth U., ICG
18. Cincinnati U.
19. NIST, Boulder
20. Wisconsin U., Madison
21. Argonne; Chicago U., KICP; Chicago U., Astron. Astrophys. Ctr.
22. Chicago U., Astron. Astrophys. Ctr.; Chicago U., KICP; Fermilab
23. UPenn, Philadelphia
24. Sussex U.
25. Missouri U., Kansas City
26. University Coll. London
27. Chicago U., EFI
28. Carnegie Mellon U.
29. Portsmouth U.
30. Chicago U., Astron. Astrophys. Ctr.; Chicago U., KICP; Chicago U., EFI; Argonne
31. IAC, La Laguna; LIneA, Rio de Janeiro; Laguna U., Tenerife
32. NCSA, Urbana; Illinois U., Urbana, Astron. Dept.
33. Barcelona, IEEC
34. William-Mary Coll.
35. Chicago U., KICP; Argonne; Chicago U., Astron. Astrophys. Ctr.
36. Chicago U., Astron. Astrophys. Ctr.; Chicago U., KICP
37. Duke U.
38. McGill U.; KwaZulu Natal U.
39. NASA, Goddard
40. Chicago U., KICP; Chicago U., EFI
41. Caltech, JPL
42. Jodrell Bank
43. Trieste Observ.; SISSA, Trieste; IFPU, Trieste; INFN, Trieste
44. Chicago U., KICP; Chicago U., Astron. Astrophys. Ctr.
45. Cornell U.
46. Hamburg Observ.
47. KIPAC, Menlo Park; Stanford U., HEPL
48. Queensland U.
49. LBNL, Berkeley
50. Indian Inst. Tech., Hyderabad
51. KEK, Tsukuba
52. McGill U.; Canadian Inst. Advanced Res.
53. UPenn, Philadelphia; LPSC, Grenoble
54. Chicago U., Astron. Astrophys. Ctr.; Fermilab; Chicago U., KICP
55. Waterloo U.
56. Colorado U.
57. Inst. Theor. Astrophys., Oslo
58. SLAC
59. Stanford U.; KIPAC, Menlo Park; Stanford U., HEPL
60. Fermilab; Chicago U., KICP
61. Chicago U., KICP; Harvey Mudd Coll.
62. Madrid, IFT
63. European Southern Observ.
64. Barcelona, IFAE; Chicago U., KICP
65. Western Australia Inst. Tech.; NRAO, Socorro
66. Geneva Observ.
67. Illinois U., Urbana, Astron. Dept.; Illinois U., Urbana; Canadian Inst. Advanced Res.
68. UC, Santa Cruz
69. UC, Berkeley
70. Ohio State U., CCAPP; Ohio State U.
71. SLAC; Stanford U.
72. Harvard-Smithsonian Ctr. Astrophys.
73. UC, Davis
74. Arizona U.
75. Australia, CSIRO, North Ryde; Lowell Observ.
76. UC, Berkeley; LBNL, Berkeley; Sao Paulo, IFT
77. KIPAC, Menlo Park
78. NIST, Boulder; SLAC
79. Chicago U., Astron. Astrophys. Ctr.
80. Cambridge U., DAMTP
81. Durham U.; Durham U., ICC
82. KIPAC, Menlo Park; Stanford U., HEPL; Stanford U.
83. Texas A-M
84. MIT; MIT, MKI
85. Chicago U., KICP; Chicago U., EFI; Chicago U., Astron. Astrophys. Ctr.
86. LPSC, Grenoble
87. ICREA, Barcelona; Barcelona, Autonoma U.; Barcelona, IFAE
88. McGill U.
89. Princeton U., Astrophys. Sci. Dept.
90. Campinas State U.
91. U. Toronto, Dunlap Inst. Astron. Astrophys.
92. Rio de Janeiro Observ.
93. Chicago U., KICP
94. Caltech
95. LIneA, Rio de Janeiro; Rio de Janeiro Observ.
96. KIPAC, Menlo Park; SLAC
97. Ruhr U., Bochum
98. Minnesota U.
99. MIT, Cambridge, Dept. Phys.; INFN, Genoa
100. Case Western Reserve U.
101. Brookhaven
102. Orsay, IAS; Trieste Observ.; SISSA, Trieste; IFPU, Trieste; INFN, Trieste
103. Madrid, CIEMAT; Madrid, Escuela Tec. Sup. Ing. Ind.
104. Trieste U.; SISSA, Trieste; IFPU, Trieste; INFN, Trieste; Trieste Observ.; A-STAR, Singapore
105. Chicago U., KICP; Chicago U., EFI; Chicago U.
106. U. Michigan, Dept. Astron.
107. SUNY, Stony Brook
108. McGill U.; Unlisted, CA
109. Southampton U.
110. Chulalongkorn U.
111. Argelander Inst. Astron.
112. ORNL, Oak Ridge (main)
113. Ohio State U., CCAPP
114. IRAP, Toulouse
115. ORIGINS, Garching; Garching, Max Planck Inst., MPE; Munich U.
116. Texas U., San Antonio
117. Illinois U., Urbana, Astron. Dept.; Illinois U., Urbana
118. U. Michigan, Ann Arbor; LBNL, Berkeley
119. Garching, Max Planck Inst., MPE; Munich U.
120. Michigan State U.
121. Chicago U., KICP; Chicago U., Astron. Astrophys. Ctr.; Fermilab
122. Edinburgh U., Inst. Astron.

We present cosmological constraints from the abundance of galaxy clusters selected via the thermal Sunyaev-Zel’dovich (SZ) effect in South Pole Telescope (SPT) data with a simultaneous mass calibration using weak gravitational lensing data from the Dark Energy Survey (DES) and the Hubble Space Telescope (HST). The cluster sample is constructed from the combined SPT-SZ, SPTpol ECS, and SPTpol 500d surveys, and comprises 1,005 confirmed clusters in the redshift range 0.25–1.78 over a total sky area of $5200{\mathrm{deg}}^2$ . We use DES Year 3 weak-lensing data for 688 clusters with redshifts $z<0.95$ and HST weak-lensing data for 39 clusters with $0.6<z<1.7$ . The weak-lensing measurements enable robust mass measurements of sample clusters and allow us to empirically constrain the SZ observable-mass relation without having to make strong assumptions about, e.g., the hydrodynamical state of the clusters. For a flat $\mathrm{\Lambda }\mathrm{CDM}$ cosmology, and marginalizing over the sum of massive neutrinos, we measure ${\mathrm{\Omega }}_{\mathrm{m}}=0.286\pm 0.032$ , ${\sigma }_8=0.817\pm 0.026$ , and the parameter combination ${\sigma }_8({\mathrm{\Omega }}_{\mathrm{m}}/0.3{)}^{0.25}=0.805\pm 0.016$ . Our measurement of $S_8\equiv {\sigma }_8\sqrt{{\mathrm{\Omega }}_{\mathrm{m}}/0.3}=0.795\pm 0.029$ and the constraint from Planck CMB anisotropies (2018 TT, TE, $\mathrm{EE}+\mathrm{lowE}$ ) differ by $1.1\sigma$ . In combination with that Planck dataset, we place a 95% upper limit on the sum of neutrino masses $\sum m_{\nu }<0.18\mathrm{eV}$ . When additionally allowing the dark energy equation of state parameter $w$ to vary, we obtain $w=-1.45\pm 0.31$ from our cluster-based analysis. In combination with Planck data, we measure $w=-1.34_{-0.15}^{+0.22}$ , or a $2.2\sigma$ difference with a cosmological constant. We use the cluster abundance to measure ${\sigma }_8$ in five redshift bins between 0.25 and 1.8, and we find the results to be consistent with structure growth as predicted by the $\mathrm{\Lambda }\mathrm{CDM}$ model fit to Planck primary CMB data.

• Research Organization: A-STAR, Singapore; Argelander Inst. Astron.; Argonne National Laboratory (ANL), Argonne, IL (United States); Arizona U.; Australia, CSIRO, North Ryde; Barcelona, Autonoma U.; Barcelona, IEEC; Barcelona, IFAE; Brookhaven National Laboratory (BNL), Upton, NY (United States); Caltech; Caltech, JPL; Cambridge U., DAMTP; Cambridge U., Inst. of Astron.; Cambridge U., KICC; Campinas State U.; Canadian Inst. Advanced Res.; Cardiff U.; Carnegie Mellon U.; Case Western Reserve U.; Cerro-Tololo InterAmerican Obs.; Chicago U.; Chicago U., Astron. Astrophys. Ctr.; Chicago U., EFI; Chicago U., KICP; Chulalongkorn U.; Cincinnati U.; Colorado U.; Cornell U.; Duke U.; Durham U.; Durham U., ICC; Edinburgh U., Inst. Astron.; European Southern Observ.; Fermi National Accelerator Laboratory (FNAL), Batavia, IL (United States); Garching, Max Planck Inst., MPE; Geneva Observ.; Hamburg Observ.; Harvard-Smithsonian Ctr. Astrophys.; Harvey Mudd Coll.; IAC, La Laguna; ICREA, Barcelona; IFPU, Trieste; INFN, Genoa; INFN, Trieste; IRAP, Toulouse; Illinois U., Urbana; Illinois U., Urbana, Astron. Dept.; Indian Inst. Tech., Hyderabad; Innsbruck U.; Inst. Theor. Astrophys., Oslo; Jodrell Bank; KEK, Tsukuba; KwaZulu Natal U.; LBNL, Berkeley; LIneA, Rio de Janeiro; LPSC, Grenoble; Laguna U., Tenerife; Lawrence Berkeley National Laboratory (LBNL), Berkeley, CA (United States); Lowell Observ.; MIT; MIT, Cambridge, Dept. Phys.; MIT, MKI; Madrid, CIEMAT; Madrid, Escuela Tec. Sup. Ing. Ind.; Madrid, IFT; McGill U.; Melbourne U.; Michigan State U.; Minnesota U.; Missouri U., Kansas City; Munich U.; NASA, Goddard; NCSA, Urbana; NIST, Boulder; NRAO, Socorro; ORIGINS, Garching; Oak Ridge National Laboratory (ORNL), Oak Ridge, TN (United States); Ohio State U.; Ohio State U., CCAPP; Orsay, IAS; Portsmouth U.; Portsmouth U., ICG; Princeton U., Astrophys. Sci. Dept.; Queensland U.; Rio de Janeiro Observ.; Ruhr U., Bochum; SISSA, Trieste; SLAC National Accelerator Laboratory (SLAC), Menlo Park, CA (United States); SUNY, Stony Brook; Sao Paulo, IFT; Southampton U.; Stanford U.; Stanford U., HEPL; Sussex U.; Texas A-M; Texas U., San Antonio; Trieste Observ.; Trieste U.; U. Michigan, Ann Arbor; U. Michigan, Dept. Astron.; U. Toronto, Dunlap Inst. Astron. Astrophys.; UC, Berkeley; UC, Davis; UC, Santa Cruz; UPenn, Philadelphia; University Coll. London; Unlisted, CA; Waterloo U.; Western Australia Inst. Tech.; William-Mary Coll.; Wisconsin U., Madison
• Sponsoring Organization: National Science Foundation (NSF); US Department of Energy; USDOE Office of Science (SC), High Energy Physics (HEP); USDOE Office of Science (SC), High Energy Physics (HEP) (SC-25)
• Grant/Contract Number: 89243024CSC000002; AC02-05CH11231; AC02-06CH11357; AC02-07CH11359; AC05-00OR22725
• OSTI ID: 2376962
• Report Number(s): DES--2023-787; DES-2023-787; FERMILAB-PUB--23-522-PPD; FERMILAB-PUB-23-522-PPD; arXiv:2401.02075; oai:inspirehep.net:2743345; arXiv:2401.02075
• Journal Information: Phys.Rev.D, Journal Name: Phys.Rev.D Journal Issue: 8 Vol. 110
• Country of Publication: United States
• Language: English