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

• Main Authors: Schrabback, T., Bocquet, S., Sommer, M., Zohren, H., Busch, J. L. van den, Hernández-Martín, B., Hoekstra, H., Raihan, S. F., Schirmer, M., Applegate, D., Bayliss, M., Benson, B. A., Bleem, L. E., Dietrich, J. P., Floyd, B., Hilbert, S., Hlavacek-Larrondo, J., McDonald, M., Saro, A., Stark, A. A., Weissgerber, N.
• Format: Article in Journal/Newspaper
• Language: unknown
• Published: arXiv 2020
• Subjects: Cosmology and Nongalactic Astrophysics astro-ph.CO; Astrophysics of Galaxies astro-ph.GA; General Relativity and Quantum Cosmology gr-qc; FOS Physical sciences; Gemini; Hubble; Pivot; South Pole; South pole
• Online Access: https://dx.doi.org/10.48550/arxiv.2009.07591; https://arxiv.org/abs/2009.07591

Expanding from previous work we present weak lensing measurements for a total sample of 30 distant ($z_\mathrm{median}=0.93$) 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 $z\gtrsim 1.4$ background galaxies via $V-I$ colour, employing deep photometry from VLT/FORS2 and Gemini-South/GMOS. We apply revised calibrations for the weak lensing 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 weak lensing 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 $νΛ$CDM 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 weak lensing follow-up samples are needed. : 32 pages, 20 figures, 12 tables, matches the version accepted for publication in MNRAS