Weak Lensing Mass Calibration of the ACT DR5 Galaxy Clusters with the DES Year 3 Weak Lensing Data

Journal Article · Mon Dec 22 00:00:00 EST 2025 · No journal information

OSTI ID:3012611

Shin, T. ^[1]; Baxter, E. J. ^[2]; Lee, E. ^[3]; Battaglia, N. ^[4]; Alarcon, A. ^[5]; Amon, A. ^[6]; Becker, M. ^[7]; Bernstein, G. ^[8]; Bond, J. R. ^[9]; Campos, A. ^[1]; Chang, C. ^[10]; Chen, R. ^[11]; Choi, A. ^[12]; DeRose, J. ^[13]; Dodelson, S. ^[14]; Doux, C. ^[15]; Dunkley, J. ^[16]; Elvin-Poole, J. ^[17]; Esteves, J. H. ^[18]; Everett, S. ^[19] ; Ferté, A. ^[20]; Gatti, M. ^[10]; Grandis, S. ^[21]; Gruen, D. ^[22]; Harrison, I. ^[23]; Hill, J. C. ^[24]; Hilton, M. ^[25]; Jarvis, M. ^[8]; MacCrann, N. ^[26]; McCullough, J. ^[27]; Moodley, K. ^[28]; Mroczkowski, T. ^[5]; Myles, J. ^[6]; Navarro Alsina, A. ^[29]; Nicola, A. ^[30]; Page, L. ^[31]; Pandey, S. ^[32]; Prat, J. ^[33]; Raveri, M. ^[34]; Ried Guachalla, B. ^[35]; Rollins, R. P. ^[30]; Sanchez, C. ^[36]; Secco, L. F. ^[10]; Sheldon, E. ^[13]; Sifón, C. ^[37]; Troxel, M. ^[38]; Tutusaus, I. ^[39]; von der Linden, A. ^[40]; Wollack, E. ^[12]; Yin, B. ^[38]; Aguena, M. ^[41]; Allam, S. S. ^[42]; Alves, O. ^[43]; Andrade-Oliveira, F. ^[44]; Bacon, D. ^[45]; Bocquet, S. ^[22]; Brooks, D. ^[46]; Camilleri, R. ^[47]; Carnero Rosell, A. ^[48]; Carretero, J. ^[49]; Castander, F. J. ^[50]; Costanzi, M. ^[51]; da Costa, L. ^[52]; da Silva Pereira, M. E. ^[53]; Davis, T. ^[47]; De Vicente, J. ^[54]; Desai, S. ^[55]; Flaugher, B. ^[42]; Frieman, J. ^[56]; Garcia-Bellido, J. ^[57]; Gutierrez, G. ^[42]; Hinton, S. ^[47]; Hollowood, D. L. ^[58]; Huterer, D. ^[43]; James, D. ^[59]; Lee, S. ^[60]; Marshall, J. ^[61]; Mena-Fernández, J. ^[15]; Menanteau, F. ^[62]; Miquel, R. ^[63]; Mohr, J. ^[22]; Muir, J. ^[64]; Ogando, R. ^[65]; Plazas Malagón, A. ^[66]; Porredon, A. ^[67]; Romer, K. ^[68]; Sanchez, E. ^[54]; Sanchez Cid, D. ^[69]; Sevilla, I. ^[54]; Smith, M. ^[70]; Soares-Santos, M. ^[44]; Suchyta, E. ^[71]; Swanson, M. ^[72]; To, C. ^[73]; Weaverdyck, N. ^[74]; Weller, J. ^[75]

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1. Carnegie Mellon U.
2. Gemini Observ., Hilo
3. Pennsylvania U.; Cornell U.
4. Cornell U.
5. ICE, Bellaterra
6. Princeton U., Astrophys. Sci. Dept.
7. Argonne (main)
8. Pennsylvania U.
9. Canadian Inst. Theor. Astrophys.
10. Chicago U., Astron. Astrophys. Ctr.; Chicago U., EFI; Chicago U., KICP
11. Stanford U., ITP
12. NASA, Goddard
13. Brookhaven
14. Chicago U., Astron. Astrophys. Ctr.; Chicago U., EFI; Chicago U., KICP; Fermilab
15. LPSC, Grenoble
16. Princeton U.; Princeton U., Astrophys. Sci. Dept.
17. Waterloo U.
18. Harvard U.
19. Caltech
20. SLAC
21. Innsbruck U., Inst. Astrophys.
22. Munich U. Observ.
23. Cardiff U.
24. Columbia U.; Columbia U., Astron. Astrophys.
25. U. Witwatersrand, Johannesburg, Sch. Phys.; KwaZulu Natal U.
26. Cambridge U., DAMTP
27. Princeton U., Astrophys. Sci. Dept.; Stanford U., ITP; SLAC
28. KwaZulu Natal U.
29. Campinas State U.
30. Jodrell Bank; U. Manchester (main)
31. Princeton U.
32. Johns Hopkins U.
33. Nordita; Royal Inst. Tech., Stockholm
34. INFN, Genoa
35. Stanford U.; Stanford U., ITP
36. Barcelona, IFAE; Barcelona, Autonoma U.
37. Valparaiso U., Catolica
38. Duke U.
39. IRAP, Toulouse
40. Stony Brook U.
41. Trieste Observ.; LIneA, Rio de Janeiro
42. Fermilab
43. U. Michigan, Ann Arbor
44. Zurich U.
45. Portsmouth U., ICG
46. University Coll. London
47. Queensland U.
48. IAC, La Laguna; LIneA, Rio de Janeiro; Laguna U., Tenerife
49. Barcelona, IFAE
50. Barcelona, IEEC; ICE, Bellaterra
51. Trieste Observ.; SISSA, Trieste; INFN, Trieste; IFPU, Trieste
52. LIneA, Rio de Janeiro
53. Hamburg Observ.
54. Madrid, CIEMAT; Madrid, Escuela Tec. Sup. Ing. Ind.
55. Indian Inst. Tech., Hyderabad
56. Chicago U., Astron. Astrophys. Ctr.; Fermilab; Chicago U., EFI; Chicago U., KICP
57. Madrid, IFT
58. UC, Santa Cruz
59. Harvard-Smithsonian Ctr. Astrophys.
60. Caltech, JPL
61. Texas A-M
62. Illinois U., Urbana (main); Illinois U., Urbana, Astron. Dept.
63. ICREA, Barcelona; Barcelona, IFAE
64. Cincinnati U.; Perimeter Inst. Theor. Phys.
65. Campinas State U.; Rio de Janeiro Observ.
66. Stanford U., ITP; SLAC
67. Madrid, CIEMAT; Madrid, Escuela Tec. Sup. Ing. Ind.; Ruhr U., Bochum
68. Sussex U.
69. Madrid, CIEMAT; Madrid, Escuela Tec. Sup. Ing. Ind.; Zurich U.
70. Lancaster U.
71. ORNL, Oak Ridge (main)
72. Illinois U., Urbana (main)
73. Chicago U., Astron. Astrophys. Ctr.
74. BCCP, Berkeley; UC, Berkeley; LBL, Berkeley
75. Garching, Max Planck Inst., MPE; Munich U. Observ.

We use weak gravitational lensing measurements from Year 3 Dark Energy Survey data to calibrate the masses of 443 galaxy clusters selected via the Sunyaev-Zel'dovich effect from Atacama Cosmology Telescope Data Release 5 maps of the cosmic microwave background. We incorporate redshift and SZ measurements for individual clusters into a hierarchical model for the stacked lensing signals and perform Bayesian analyses to constrain the hydrostatic mass bias of the clusters. Our treatment of systematic uncertainties includes a prescription for measuring and accounting for the weak lensing boost factor, consideration of a miscentering effect, as well as marginalization over uncertainties in the source galaxy photometric redshift distributions and shear calibration. The resultant constraints on the normalization of the mass-observable relation have a precision of approximately 7%, with the mean WL halo mass of $$M_{\rm 500c} = 5.4 \times 10^{14} M_{\odot}$$. We measure the bias between the true cluster mass and the mass estimated from the SZ signal based on an X-ray--calibrated scaling relation assuming hydrostatic equilibrium, to be $$1-b = 0.75^{+0.04}_{-0.06}$$ over the full sample. When splitting the clusters into high ($$z$$=0.43-0.70) and low ($$z$$=0.15-0.43) redshift bins, we measure $$1-b = 0.58^{+0.06}_{-0.05}$$ and $$0.82^{+0.07}_{-0.07}$$, respectively. When introducing additional freedom in redshift and mass to the hydrostatic bias model, we find that $1-b$ decreases with redshift (with the power law of $$-2.0^{+0.7}_{-0.4}$$, 99.95% confidence), consistent with findings from other recent studies, while we do not find any significant trend in mass. We also demonstrate that our result is robust against various systematics. The weak-lensing mass calibration presented in this study will be a useful tool for using the ACT clusters as probes of astrophysics and cosmology.

• Research Organization: Argonne National Laboratory (ANL), Argonne, IL (United States); Jodrell Bank; Hamburg Observ.; Canadian Inst. Theor. Astrophys.; Innsbruck U., Inst. Astrophys.; Lancaster U.; Oak Ridge National Laboratory (ORNL), Oak Ridge, TN (United States); Trieste Observ.; Madrid, IFT; Stanford U., ITP; Lawrence Berkeley National Laboratory (LBNL), Berkeley, CA (United States); Harvard-Smithsonian Ctr. Astrophys.; Gemini Observ., Hilo; U. Witwatersrand, Johannesburg, Sch. Phys.; Madrid, Escuela Tec. Sup. Ing. Ind.; Perimeter Inst. Theor. Phys.; Duke U.; Chicago U., EFI; IAC, La Laguna; Campinas State U.; Waterloo U.; Barcelona, Autonoma U.; ICE, Bellaterra; Stony Brook U.; IFPU, Trieste; Munich U. Observ.; Johns Hopkins U.; Pennsylvania U.; Princeton U., Astrophys. Sci. Dept.; Zurich U.; NASA, Goddard; U. Michigan, Ann Arbor; Harvard U.; UC, Berkeley; Laguna U., Tenerife; Portsmouth U., ICG; Princeton U.; Cambridge U., DAMTP; Carnegie Mellon U.; Columbia U., Astron. Astrophys.; INFN, Trieste; IRAP, Toulouse; Illinois U., Urbana (main); Barcelona, IEEC; INFN, Genoa; SLAC National Accelerator Laboratory (SLAC), Menlo Park, CA (United States); Caltech, JPL; LIneA, Rio de Janeiro; Brookhaven National Laboratory (BNL), Upton, NY (United States); Barcelona, IFAE; Cornell U.; KwaZulu Natal U.; Cardiff U.; Cincinnati U.; Chicago U., Astron. Astrophys. Ctr.; Stanford U.; Caltech; SISSA, Trieste; Texas A-M; University Coll. London; Fermi National Accelerator Laboratory (FNAL), Batavia, IL (United States); Madrid, CIEMAT; Illinois U., Urbana, Astron. Dept.; Ruhr U., Bochum; UC, Santa Cruz; Valparaiso U., Catolica; U. Manchester (main); Sussex U.; Rio de Janeiro Observ.; Royal Inst. Tech., Stockholm; Nordita; Queensland U.; Indian Inst. Tech., Hyderabad; Chicago U., KICP; Columbia U.; ICREA, Barcelona; Garching, Max Planck Inst., MPE; LPSC, Grenoble; BCCP, Berkeley
• Sponsoring Organization: US Department of Energy
• DOE Contract Number: 89243024CSC000002
• OSTI ID: 3012611
• Report Number(s): FERMILAB-PUB-25-0859-V; oai:inspirehep.net:3095012; arXiv:2512.18935
• Journal Information: No journal information, Journal Name: No journal information
• Country of Publication: United States
• Language: English