The SRG/eROSITA All-Sky Survey: Dark Energy Survey Year 3 Weak Gravitational Lensing by eRASS1 selected Galaxy Clusters

Journal Article · Tue Feb 13 00:00:00 EST 2024 · TBD

OSTI ID:2305630

Grandis, S. ^[1]; Ghirardini, V. ^[2]; Bocquet, S. ^[3]; Garrel, C. ^[2]; Mohr, J. J. ^[4]; Liu, A. ^[2]; Kluge, M. ^[2]; Kimmig, L. ^[3]; Reiprich, T. H. ^[5]; Alarcon, A. ^[6]; Amon, A. ^[7]; Artis, E. ^[2]; Bahar, Y. E. ^[2]; Balzer, F. ^[8]; Bechtol, K. ^[9]; Becker, M. R. ^[6]; Bernstein, G. ^[10]; Bulbul, E. ^[2]; Campos, A. ^[11]; Carnero Rosell, A. ^[12] ; Carrasco Kind, M. ^[13]; Cawthon, R. ^[14]; Chang, C. ^[15]; Chen, R. ^[16]; Chiu, I. ^[17]; Choi, A. ^[18]; Clerc, N. ^[19]; Comparat, J. ^[2]; Cordero, J. ^[20]; Davis, C. ^[21]; Derose, J. ^[22]; Diehl, H. T. ^[23]; Dodelson, S. ^[11]; Doux, C. ^[24]; Drlica-Wagner, A. ^[25]; Eckert, K. ^[10]; Elvin-Poole, J. ^[26]; Everett, S. ^[27]; Ferte, A. ^[28]; Gatti, M. ^[10]; Giannini, G. ^[29]; Giles, P. ^[30]; Gruen, D. ^[3]; Gruendl, R. A. ^[13]; Harrison, I. ^[31]; Hartley, W. G. ^[32]; Herner, K. ^[23]; Huff, E. M. ^[27]; Kleinebreil, F. ^[1]; Kuropatkin, N. ^[23]; Leget, P. F. ^[33]; Maccrann, N. ^[34]; Mccullough, J. ^[33]; Merloni, A. ^[2]; Myles, J. ^[35]; Nandra, K. ^[2]; Navarro-Alsina, A. ^[36]; Okabe, N. ^[37]; Pacaud, F. ^[5]; Pandey, S. ^[10]; Prat, J. ^[15]; Predehl, P. ^[2]; Ramos, M. ^[2]; Raveri, M. ^[38]; Rollins, R. P. ^[20]; Roodman, A. ^[39]; Ross, A. J. ^[40]; Rykoff, E. S. ^[39]; Sanchez, C. ^[41]; Sanders, J. ^[2]; Schrabback, T. ^[1]; Secco, L. F. ^[15]; Seppi, R. ^[2]; Sevilla-Noarbe, I. ^[41]; Sheldon, E. ^[42]; Shin, T. ^[43]; Troxel, M. ^[16]; Tutusaus, I. ^[44]; Varga, T. N. ^[8]; Wu, H. ^[45]; Yanny, B. ^[27]; Yin, B. ^[11]; Zhang, X. ^[2]; Zhang, Y. ^[46]; Alves, O. ^[46]; Bhargava, S. ^[30]; Brooks, D. ^[47]; Burke, D. L. ^[39]; Carretero, J. ^[29]; Costanzi, M. ^[48]; da Costa, L. N. ^[49]; Pereira, M. E.S. ^[50]; De Vicente, J. ^[41]; Desai, S. ^[51]; Doel, P. ^[52]; Ferrero, I. ^[53]; Flaugher, B. ^[23]; Friedel, D. ^[54]; Frieman, J. ^[55]; García-Bellido, J. ^[37]; Gutierrez, G. ^[23]; Hinton, S. R. ^[21]; Hollowood, D. L. ^[50]; Honscheid, K. ^[56]; James, D. J. ^[57]; Jeffrey, N. ^[53]; Lahav, O. ^[53]; Lee, S. ^[27]; Marshall, J. L. ^[58]; Menanteau, F. ^[13]; Ogando, R. L.C. ^[59]; Pieres, A. ^[60]; Plazas Malagón, A. A. ^[39]; Romer, A. K. ^[30]; Sanchez, E. ^[41]; Schubnell, M. ^[46]; Smith, M. ^[61]; Suchyta, E. ^[50]; Swanson, M. E.C. ^[54]; Tarle, G. ^[46]; Weaverdyck, N. ^[62]; Weller, J. ^[8]

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1. Innsbruck U.
2. Garching, Max Planck Inst., MPE
3. Munich U.
4. Munich U.; Garching, Max Planck Inst., MPE
5. Argelander Inst. Astron.
6. Argonne
7. Cambridge U., KICC; Cambridge U., Inst. of Astron.
8. Garching, Max Planck Inst., MPE; Munich U.
9. Wisconsin U., Madison
10. UPenn, Philadelphia
11. Carnegie Mellon U.
12. IAC, La Laguna; LIneA, Rio de Janeiro; Laguna U., Tenerife
13. Illinois U., Urbana (main); Illinois U., Urbana, Astron. Dept.
14. William-Mary Coll.
15. Chicago U., Astron. Astrophys. Ctr.; Chicago U., KICP
16. Duke U.
17. Taiwan, Natl. Cheng Kung U.
18. NASA, Goddard
19. IRAP, Toulouse
20. Jodrell Bank
21. Queensland U.
22. LBL, Berkeley
23. Fermilab
24. IAC, La Laguna; Laguna U., Tenerife; LPSC, Grenoble
25. Chicago U., Astron. Astrophys. Ctr.; Chicago U., KICP; Fermilab
26. Waterloo U.
27. Caltech, JPL
28. SLAC
29. Barcelona, IFAE
30. Sussex U.
31. Cardiff U.
32. U. Geneva (main)
33. KIPAC, Menlo Park
34. Cambridge U., DAMTP
35. Munich U.; KIPAC, Menlo Park; Stanford U.
36. Campinas State U.
37. Hiroshima U.; Hiroshima U. (main)
38. MIT, Cambridge, Dept. Phys.; INFN, Genoa
39. SLAC; KIPAC, Menlo Park
40. Ohio State U., CCAPP
41. Madrid, CIEMAT
42. Brookhaven
43. SUNY, Stony Brook
44. Geneva U., Dept. Theor. Phys.; Geneva U., CAP; IRAP, Toulouse
45. Boise State U.
46. U. Michigan, Ann Arbor
47. Trieste Observ.
48. IFPU, Trieste; UC, Santa Cruz; ORNL, Oak Ridge (main)
49. LIneA, Rio de Janeiro
50. Hamburg Observ.
51. Indian Inst. Tech., Hyderabad
52. University Coll. London
53. Inst. Theor. Astrophys., Oslo
54. Illinois U., Urbana (main)
55. Chicago U., KICP; Fermilab
56. Ohio State U., CCAPP; Harvard-Smithsonian Ctr. Astrophys.
57. Texas A-M
58. Rio de Janeiro Observ.
59. Southampton U.
60. LIneA, Rio de Janeiro; Southampton U.
61. Unlisted
62. LBL, Berkeley; U. Michigan, Ann Arbor

Number counts of galaxy clusters across redshift are a powerful cosmological probe, if a precise and accurate reconstruction of the underlying mass distribution is performed -- a challenge called mass calibration. With the advent of wide and deep photometric surveys, weak gravitational lensing by clusters has become the method of choice to perform this measurement. We measure and validate the weak gravitational lensing (WL) signature in the shape of galaxies observed in the first 3 years of the DES Y3 caused by galaxy clusters selected in the first all-sky survey performed by SRG/eROSITA. These data are then used to determine the scaling between X-ray photon count rate of the clusters and their halo mass and redshift. We empirically determine the degree of cluster member contamination in our background source sample. The individual cluster shear profiles are then analysed with a Bayesian population model that self-consistently accounts for the lens sample selection and contamination, and includes marginalization over a host of instrumental and astrophysical systematics. To quantify the accuracy of the mass extraction of that model, we perform mass measurements on mock cluster catalogs with realistic synthetic shear profiles. This allows us to establish that hydro-dynamical modelling uncertainties at low lens redshifts ($z<0.6$) are the dominant systematic limitation. At high lens redshift the uncertainties of the sources' photometric redshift calibration dominate. With regard to the X-ray count rate to halo mass relation, we constrain all its parameters. This work sets the stage for a joint analysis with the number counts of eRASS1 clusters to constrain a host of cosmological parameters. We demonstrate that WL mass calibration of galaxy clusters can be performed successfully with source galaxies whose calibration was performed primarily for cosmic shear experiments.

• Research Organization: Brookhaven National Laboratory (BNL), Upton, NY (United States); Argonne National Laboratory (ANL), Argonne, IL (United States); Fermi National Accelerator Laboratory (FNAL), Batavia, IL (United States); Lawrence Berkeley National Laboratory (LBNL), Berkeley, CA (United States); SLAC National Accelerator Laboratory (SLAC), Menlo Park, CA (United States)
• Sponsoring Organization: USDOE Office of Science (SC), High Energy Physics (HEP)
• Contributing Organization: DES; eROSITA-DE
• DOE Contract Number: AC02-07CH11359
• OSTI ID: 2305630
• Report Number(s): FERMILAB-PUB-24-0071-PPD; arXiv:2402.08455; oai:inspirehep.net:2758103
• Journal Information: TBD, Journal Name: TBD
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTRONOMY AND ASTROPHYSICS