Velocity dispersion and dynamical mass for 270 galaxy clusters in the Planck PSZ1 catalogue^⋆

¹ Instituto de Astrofísica de Canarias (IAC), C/ Vía Láctea s/n, 38205 La Laguna, Tenerife, Spain
e-mail: ferragamoantonio@gmail.com
² Universidad de La Laguna, Departamento de Astrofísica, C/ Astrofísico Francisco Sánchez s/n, 38206 La Laguna, Tenerife, Spain
³ Dipartimento di Fisica, Sapienza Università di Roma, Piazzale Aldo Moro, 00185 Roma, Italy
⁴ Gran Telescopio Canarias, La Palma, Spain
⁵ Purple Mountain Observatory, No. 8 Yuanhua Road, Qixia District, Nanjing 210034, PR China
⁶ Universidad Andrés Bello, Departemento de Ciencias Físicas, 7591538 Santiago de Chile, Chile
⁷ Max-Planck Institute for Astronomy, Königstuhl 17, 69117 Heidelberg, Germany
⁸ Tartu Observatory, University of Tartu, 61602 Tõravere, Tartumaa, Estonia

Received: 20 January 2021
Accepted: 23 August 2021

Abstract

We present the velocity dispersion and dynamical mass estimates for 270 galaxy clusters included in the first Planck Sunyaev-Zeldovich (SZ) source catalogue, the PSZ1. Part of the results presented here were achieved during a two-year observational program, the ITP, developed at the Roque de los Muchachos Observatory (La Palma, Spain). In the ITP we carried out a systematic optical follow-up campaign of all the 212 unidentified PSZ1 sources in the northern sky that have a declination above −15° and are without known counterparts at the time of the publication of the catalogue. We present for the first time the velocity dispersion and dynamical mass of 58 of these ITP PSZ1 clusters, plus 35 newly discovered clusters that are not associated with the PSZ1 catalogue. Using Sloan Digital Sky Survey archival data, we extend this sample, including 212 already confirmed PSZ1 clusters in the northern sky. Using a subset of 207 of these galaxy clusters, we constrained the M_SZ–M_dyn scaling relation, finding a mass bias of (1 − B) = 0.83 ± 0.07(stat) ± 0.02(sys). We show that this value is consistent with other results in the literature that were obtained with different methods (X-ray, dynamical masses, or weak-lensing mass proxies). This result cannot dissolve the tension between primordial cosmic microwave background anisotropies and cluster number counts in the Ω_M–σ₈ plane.