NIKA2 observations of 3 low-mass galaxy clusters at z ~ 1: Pressure profile and YSZ – M relation

/ Authors

R. A. H. Aussel, M. R. .. Beelen, 1. D.EckertBenoist, P. A. A. Benoît, S. B. H. Ajeddig 11, L. B. B. Altieri, M. P.André, 13 E.Artis, H. A. O. Bourrion, D. A. Beelen 9

and 57 more authors

M. C. Benoist 4, A. Benoît Bremer 13, S. Calvo, L. B. A. Cappi, 14 A. Catalano Birkinshaw M. Birkinshaw, O. B. M. D. Petris, D. B. F. Désert, M. Bremer S. Doyle 6, C. M.CalvoF., L. A. Cappi 12, C. F. A. Catalano 7, M. Gastaldello, A. F.-X. Désert P. Giles 18, S. Doyle Gomez 19, O. H. E. F. C. Driessen Goupy 11, L. Faccioli . Hanser 9, C. Horellou, 21 F.GastaldelloF.Kéruzoré, P. G. Koulouridis, 7. C. A. Gomez 22, B. J. Goupy 12, O. Hahn Ladjelate 23, C. H. .. Lagache, C. Leclercq, F. K. J. Lestrade, J. F. M. E. Koulouridis 24, S. C. Kramer Macías-Pérez 9, B. B. Ladjelate 7, S. G. Lagache Maughan 13, S. Maurogordato, J.-F. Lestrade A. Maury 7, 25 A. J.F. Macías-Pérez Mauskopf 6, S. Madden Monfardini 11, B. M. Muñoz-Echeverría, F. P. S. Maurogordato 9, A. Perotto, G. P. Mauskopf . Pierre 7, E. P. A. Monfardini 15, V. R. M. Muñoz-Echeverría N. Ponthieu 16, A. R. F. Pacaud, L. P. A. Ritacco, 29 C. M. Pierre, H. G. Pisano 30, F. E. Pompei Roussel 31, M. N. Ponthieu Ruppin 32, 33 K V. Revéret Sereno 14, A. Schuster, A. Sievers, C. R. Vidal, H. Roussel C. Tucker 6, F. R. R. Zylka, M. Sereno, K. Schuster, 1. A.Sievers, G. Vidal, C. Tucker, R. Zylka

/ Abstract

Three galaxy clusters selected from the XXL X-ray survey at high redshift and low mass (z ~ 1 and M500 ~ 1 – 2 × 1014 M⊙) were observed with NIKA2 to image their Sunyaev-Zel'dovich effect (SZ) signal. They all present an SZ morphology, together with the comparison with X-ray and optical data, that indicates dynamical activity related to merging events. Despite their disturbed intracluster medium, their high redshifts, and their low masses, the three clusters follow remarkably well the pressure profile and the SZ flux-mass relation expected from standard evolution. This suggests that the physics that drives cluster formation is already in place at z ~ 1 down to M500 ~ 1014 M⊙.

Journal: EPJ Web of Conferences

DOI: 10.1051/epjconf/202429300002