SPT-SZ MCMF: an extension of the SPT-SZ catalogue over the DES region

Journal Article · 14 June 2024 · Mon.Not.Roy.Astron.Soc.

DOI: https://doi.org/10.1093/mnras/stae1359 · OSTI ID:2202833

Klein, M.  ^[1]; Mohr, J. J. ^[2]; Bocquet, S. ^[1]; Aguena, M. ^[3]; Allen, S. W. ^[4]; Alves, O. ^[5]; Ansarinejad, B.  ^[6]; Ashby, M. L.N. ^[7]; Bacon, D. ^[8]; Bayliss, M. ^[9]; Benson, B. A. ^[10]; Bleem, L. E. ^[11]; Brodwin, M. ^[12]; Brooks, D. ^[13]; Bulbul, E. ^[14]; Burke, D. L. ^[15]; Canning, R. E.A. ^[16]; Carlstrom, J. E. ^[17]; Carnero Rosell, A. ^[18]; Carretero, J. ^[19] ; Chang, C. L. ^[20]; Conselice, C. ^[21]; Costanzi, M. ^[22]; Crites, A. T. ^[23]; da Costa, L. N. ^[3]; Pereira, M. E.S. ^[24]; Davis, T. M.  ^[25]; De Vicente, J. ^[26]; Desai, S.  ^[27]; de Haan, T. ^[28]; Dobbs, M. A. ^[29]; Doel, P. ^[13]; Ferrero, I. ^[30]; Flores, A. M. ^[31]; Frieman, J.  ^[32]; George, E. M. ^[33]; Giannini, G.  ^[19]; Gladders, M. D. ^[34]; Gonzalez, A. H. ^[35]; Grandis, S. ^[36]; Gruen, D. ^[1]; Gruendl, R. A. ^[37]; Gutierrez, G.  ^[38]; Halverson, N. W. ^[39]; Hinton, S. R. ^[25]; Holder, G. P. ^[40]; Hollowood, D. L. ^[41]; Holzapfel, W. L. ^[42]; Honscheid, K. ^[43]; Hrubes, J. D. ^[44]; Huang, N. ^[42]; James, D. J. ^[45]; Khullar, G. ^[34]; Kim, K. ^[46]; Knox, L. ^[47]; Kraft, R. ^[7]; Kéruzoré, F. ^[48]; Lee, A. T. ^[49]; Luong-Van, D. ^[44]; Mahler, G. ^[50]; Mantz, A. ^[51]; Marrone, D. P. ^[52]; Marshall, J. L. ^[53]; McDonald, M. ^[54]; McMahon, J. J. ^[5]; Mena-Fernández, J. ^[26]; Menanteau, F. ^[37]; Meyer, S. S. ^[55]; Miquel, R. ^[56]; Myles, J. ^[57]; Padin, S. ^[23]; Pieres, A. ^[58]; Plazas Malagón, A. A. ^[15]; Pryke, C. ^[59]; Reichardt, C. L. ^[6]; Reil, K. ^[60]; Roberson, J. ^[46]; Romer, A. K. ^[61]; Romero, C. ^[45]; Ruhl, J. E. ^[62]; Saliwanchik, B. R. ^[63]; Salvati, L. ^[64]; Sanchez, E.  ^[26]; Saro, A. ^[65]; Schaffer, K. K. ^[66]; Schrabback, T. ^[36]; Schubnell, M. ^[5]; Sevilla-Noarbe, I. ^[26]; Sharon, K. ^[67]; Shirokoff, E. ^[34]; Smith, M. ^[68]; Somboonpanyakul, T. ^[69]; Stalder, B. ^[7]; Stanford, S. A. ^[70]; Stark, A. A. ^[7]; Strazzullo, V. ^[71]; Suchyta, E. ^[72]; Swanson, M. E.C. ^[73]; Tarle, G. ^[5]; To, C. ^[74]; Vanderlinde, K. ^[75]; Vieira, J. D. ^[76]; von der Linden, A. ^[77]; Weaverdyck, N. ^[78]; Williamson, R. ^[23]; Wiseman, P. ^[68]; Young, M. ^[75]

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1. Munich U.
2. Munich U.; Garching, Max Planck Inst., MPE
3. LIneA, Rio de Janeiro
4. KIPAC, Menlo Park; Stanford U., HEPL; Stanford U.; SLAC
5. U. Michigan, Ann Arbor
6. Melbourne U.
7. Harvard U.
8. Portsmouth U., ICG
9. MIT, MKI; Cincinnati U.
10. Chicago U., Astron. Astrophys. Ctr.; Chicago U., EFI; Chicago U., KICP; Fermilab
11. Argonne; Chicago U., Astron. Astrophys. Ctr.; Chicago U., EFI; Chicago U., KICP
12. Missouri U., Kansas City
13. University Coll. London
14. Garching, Max Planck Inst., MPE
15. KIPAC, Menlo Park; SLAC
16. Portsmouth U.
17. Chicago U., Astron. Astrophys. Ctr.; Chicago U., EFI; Chicago U., KICP; Chicago U.; Argonne
18. IAC, La Laguna; LIneA, Rio de Janeiro; Laguna U., Tenerife
19. Barcelona, IFAE
20. Chicago U., Astron. Astrophys. Ctr.; Chicago U., EFI; Chicago U., KICP; Argonne
21. Jodrell Bank; Nottingham U.
22. Trieste U.; Arcetri Observ.; SISSA, Trieste; IFPU, Trieste; INFN, Trieste
23. Chicago U., Astron. Astrophys. Ctr.; Chicago U., EFI; Chicago U., KICP; Caltech
24. Hamburg Observ.
25. Queensland U.
26. Madrid, CIEMAT
27. Indian Inst. Tech., Hyderabad
28. KEK, Tsukuba
29. McGill U.; Canadian Inst. Advanced Res.
30. Inst. Theor. Astrophys., Oslo
31. Stanford U.; KIPAC, Menlo Park; Stanford U., HEPL
32. Fermilab; Chicago U., Astron. Astrophys. Ctr.; Chicago U., EFI; Chicago U., KICP
33. European Southern Observ.
34. Chicago U., Astron. Astrophys. Ctr.; Chicago U., EFI; Chicago U., KICP
35. Florida U.
36. Innsbruck U.
37. NCSA, Urbana; Illinois U., Urbana, Astron. Dept.
38. Fermilab
39. Colorado U.
40. McGill U.
41. UC, Santa Cruz
42. UC, Berkeley
43. Ohio State U., CCAPP; Ohio State U.
44. Chicago U.
45. Harvard-Smithsonian Ctr. Astrophys.
46. Cincinnati U.
47. UC, Davis
48. Argonne
49. UC, Berkeley; LBNL, Berkeley
50. Durham U.; Durham U., ICC
51. KIPAC, Menlo Park; Stanford U., HEPL; Stanford U.
52. Arizona U., Astron. Dept. - Steward Observ.
53. Texas A-M
54. MIT, MKI
55. Chicago U., Astron. Astrophys. Ctr.; Chicago U., EFI; Chicago U., KICP; Chicago U.
56. ICREA, Barcelona; Barcelona, Autonoma U.; Barcelona, IFAE
57. Stanford U.; KIPAC, Menlo Park; SLAC
58. LIneA, Rio de Janeiro; Rio de Janeiro Observ.
59. Minnesota U.
60. SLAC
61. Sussex U., Astron. Ctr.
62. Case Western Reserve U., CERCA
63. Case Western Reserve U.; Brookhaven
64. Orsay, IAS; Arcetri Observ.; SISSA, Trieste; IFPU, Trieste; INFN, Trieste
65. Trieste U.; SISSA, Trieste; IFPU, Trieste; INFN, Trieste; Arcetri Observ.; NCTS, Hsinchu
66. Chicago U., Astron. Astrophys. Ctr.; Chicago U., EFI; Chicago U., KICP; College de France; DSM, DAPNIA, Saclay; Chicago U.
67. U. Michigan, Dept. Astron.
68. Southampton U.
69. MIT, MKI; KIPAC, Menlo Park
70. UC, Davis; LLNL, Livermore
71. Arcetri Observ.; Brera Observ.; SISSA, Trieste; IFPU, Trieste; INFN, Trieste
72. ORNL, Oak Ridge (main)
73. Unlisted
74. Ohio State U., CCAPP
75. Toronto U., Astron. Dept.
76. Illinois U., Urbana, Astron. Dept.; Illinois U., Urbana
77. SUNY, Stony Brook
78. U. Michigan, Ann Arbor; LBNL, Berkeley

We present an extension to a Sunyaev–Zel’dovich Effect (SZE) selected cluster catalogue based on observations from the South Pole Telescope (SPT); this catalogue extends to lower signal to noise than the previous SPT–SZ catalogue and therefore includes lower mass clusters. Optically derived redshifts, centres, richnesses, and morphological parameters together with catalogue contamination and completeness statistics are extracted using the multicomponent matched filter (MCMF) algorithm applied to the S/N > 4 SPT–SZ candidate list and the Dark Energy Survey (DES) photometric galaxy catalogue. The main catalogue contains 811 sources above S/N = 4, has 91  per cent purity, and is 95 per cent complete with respect to the original SZE selection. It contains in total 50 per cent more clusters and twice as many clusters above z = 0.8 in comparison to the original SPT-SZ sample. The MCMF algorithm allows us to define subsamples of the desired purity with traceable impact on catalogue completeness. As an example, we provide two subsamples with S/N > 4.25 and S/N > 4.5 for which the sample contamination and cleaning-induced incompleteness are both as low as the expected Poisson noise for samples of their size. The subsample with S/N > 4.5 has 98 per cent purity and 96 per cent completeness and is part of our new combined SPT cluster and DES weak-lensing cosmological analysis. We measure the number of false detections in the SPT-SZ candidate list as function of S/N, finding that it follows that expected from assuming Gaussian noise, but with a lower amplitude compared to previous estimates from simulations.

• Research Organization: Laguna U., Tenerife; UC, Santa Cruz; Arizona U., Astron. Dept. - Steward Observ.; Caltech; Chicago U.; Ohio State U.; Illinois U., Urbana, Astron. Dept.; U. Michigan, Dept. Astron.; Rio de Janeiro Observ.; IFPU, Trieste; Illinois U., Urbana; Melbourne U.; Orsay, IAS; Barcelona, IFAE; Indian Inst. Tech., Hyderabad; U. Michigan, Ann Arbor; LBNL, Berkeley; Trieste U.; Case Western Reserve U., CERCA; Missouri U., Kansas City; MIT, MKI; Nottingham U.; Stanford U., HEPL; NCTS, Hsinchu; Hamburg Observ.; University Coll. London; SLAC National Accelerator Laboratory (SLAC), Menlo Park, CA (United States); Portsmouth U.; Portsmouth U., ICG; Inst. Theor. Astrophys., Oslo; Brookhaven National Laboratory (BNL), Upton, NY (United States); Lawrence Livermore National Laboratory (LLNL), Livermore, CA (United States); Colorado U.; European Southern Observ.; Texas A-M; Harvard U.; Chicago U., KICP; Madrid, CIEMAT; Chicago U., EFI; LIneA, Rio de Janeiro; Durham U., ICC; Southampton U.; Cincinnati U.; INFN, Trieste; McGill U.; KEK, Tsukuba; Chicago U., Astron. Astrophys. Ctr.; DSM, DAPNIA, Saclay; SISSA, Trieste; Argonne National Laboratory (ANL), Argonne, IL (United States); SUNY, Stony Brook; Brera Observ.; Minnesota U.; IAC, La Laguna; Stanford U.; Harvard-Smithsonian Ctr. Astrophys.; NCSA, Urbana; Sussex U., Astron. Ctr.; Toronto U., Astron. Dept.; Innsbruck U.; Fermi National Accelerator Laboratory (FNAL), Batavia, IL (United States); Queensland U.; Arcetri Observ.; Unlisted; Munich U.; Barcelona, Autonoma U.; Canadian Inst. Advanced Res.; College de France; UC, Berkeley; UC, Davis; Case Western Reserve U.; ICREA, Barcelona; Jodrell Bank; Durham U.; Garching, Max Planck Inst., MPE; Ohio State U., CCAPP; Florida U.; Oak Ridge National Laboratory (ORNL), Oak Ridge, TN (United States)
• Sponsoring Organization: US Department of Energy
• Grant/Contract Number: AC02-07CH11359; 89243024CSC000002
• OSTI ID: 2202833
• Report Number(s): FERMILAB-PUB-23-508-PPD; oai:inspirehep.net:2698983; arXiv:2309.09908
• Journal Information: Mon.Not.Roy.Astron.Soc., Journal Name: Mon.Not.Roy.Astron.Soc. Journal Issue: 4 Vol. 531
• Country of Publication: United States
• Language: English