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Title: Mass calibration of distant SPT galaxy clusters through expanded weak-lensing follow-up observations with HST, VLT, & Gemini-South

Journal Article · · Monthly Notices of the Royal Astronomical Society
ORCiD logo [1];  [2]; ORCiD logo [1]; ORCiD logo [1];  [3];  [1]; ORCiD logo [4]; ORCiD logo [1]; ORCiD logo [5];  [6];  [7];  [8];  [9];  [2]; ORCiD logo [10];  [2];  [11];  [12]; ORCiD logo [13];  [14] more »;  [1] « less
  1. Univ. of Bonn (Germany)
  2. Ludwig Maximilian Univ. of Munich, Munich (Germany)
  3. Univ. of Bonn (Germany); Ruhr Univ., Bochum (Germany)
  4. Leiden University (Netherlands)
  5. Max Planck Institut für Astronomie (Germany)
  6. Univ. of Bonn (Germany); Univ. of Chicago, IL (United States)
  7. Univ. of Cincinnati, OH (United States)
  8. Fermi National Accelerator Lab. (FNAL), Batavia, IL (United States); Univ. of Chicago, IL (United States)
  9. Univ. of Chicago, IL (United States); Argonne National Lab. (ANL), Argonne, IL (United States)
  10. Univ. of Missouri, Kansas City, MO (United States)
  11. Univ. of Montreal, QC (Canada)
  12. Massachusetts Inst. of Technology (MIT), Cambridge, MA (United States)
  13. Univ. of Trieste (Italy); Istituto Nazionale di Astrofisica (INAF), Trieste (Italy)
  14. Harvard-Smithsonian Center for Astrophysics, Cambridge, MA (United States)
+ Show Author Affiliations

Expanding from previous work, we present weak-lensing (WL) measurements for a total sample of 30 distant (zmedian = 0.93) massive galaxy clusters from the South Pole Telescope Sunyaev–Zel’dovich (SPT-SZ) Survey, measuring galaxy shapes in Hubble Space Telescope (HST) Advanced Camera for Surveys images. We remove cluster members and preferentially select z ≳ 1.4 background galaxies via V-I colour, employing deep photometry from VLT/FORS2 and Gemini-South/GMOS. We apply revised calibrations for the WL shape measurements and the source redshift distribution to estimate the cluster masses. In combination with earlier Magellan/Megacam results for lower-redshifts clusters, we infer refined constraints on the scaling relation between the SZ detection significance and the cluster mass, in particular regarding its redshift evolution. The mass scale inferred from the WL data is lower by a factor $$0.76^{+0.10}_{-0.14}$$ (at our pivot redshift z = 0.6) compared to what would be needed to reconcile a flat Planck νΛCDM cosmology (in which the sum of the neutrino masses is a free parameter) with the observed SPT-SZ cluster counts. In order to sensitively test the level of (dis-)agreement between SPT clusters and Planck, further expanded WL follow-up samples are needed.

Research Organization:
Argonne National Lab. (ANL), Argonne, IL (United States); Fermi National Accelerator Lab. (FNAL), Batavia, IL (United States)
Sponsoring Organization:
USDOE Office of Science (SC), High Energy Physics (HEP); German Research Foundation (DFG); Netherlands Organization for Scientific Research (NWO); European Research Council (ERC); National Science Foundation (NSF)
Grant/Contract Number:
AC02-07CH11359; AC02-06CH11357
OSTI ID:
1706157
Alternate ID(s):
OSTI ID: 1835055
Report Number(s):
FERMILAB-PUB-20-535-AE; arXiv:2009.07591; oai:inspirehep.net:1817522; TRN: US2204588
Journal Information:
Monthly Notices of the Royal Astronomical Society, Vol. 505, Issue 3; ISSN 0035-8711
Publisher:
Royal Astronomical SocietyCopyright Statement
Country of Publication:
United States
Language:
English

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79 ASTRONOMY AND ASTROPHYSICS
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