TY - JOUR
T1 - CLASH-VLT
T2 - Abell S1063: Cluster assembly history and spectroscopic catalogue
AU - Mercurio, A.
AU - Rosati, P.
AU - Biviano, A.
AU - Annunziatella, M.
AU - Girardi, M.
AU - Sartoris, B.
AU - Nonino, M.
AU - Brescia, M.
AU - Riccio, G.
AU - Grillo, C.
AU - Balestra, I.
AU - Caminha, G. B.
AU - De Lucia, G.
AU - Gobat, R.
AU - Seitz, S.
AU - Tozzi, P.
AU - Scodeggio, M.
AU - Vanzella, E.
AU - Angora, G.
AU - Bergamini, P.
AU - Borgani, S.
AU - Demarco, R.
AU - Meneghetti, M.
AU - Strazzullo, V.
AU - Tortorelli, L.
AU - Umetsu, K.
AU - Fritz, A.
AU - Gruen, D.
AU - Kelson, D.
AU - Lombardi, M.
AU - Maier, C.
AU - Postman, M.
AU - Rodighiero, G.
AU - Ziegler, B.
N1 - Funding Information:
The authors thank the anonymous referee for the very useful comments, that improved the manuscript. We acknowledge financial contributions by PRIN-MIUR 2017WSCC32 "Zooming into dark matter and protogalaxies with massive lensing clusters" (P.I.: P.Rosati), INAF "main-stream" 1.05.01.86.20: "Deep and wide view of galaxy clusters (P.I.: M. Nonino)" and INAF "main-stream" 1.05.01.86.31 "The deepest view of high-redshift galaxies and globular cluster precursors in the early Universe" (P.I.: E. Vanzella). M.B. acknowledges financial contributions from the agreement ASI/INAF 2018-23- HH.0, Euclid ESA mission - Phase D and with AM the INAF PRIN-SKA 2017 program 1.05.01.88.04. C.G. acknowledges support through grant no. 10123 of the VILLUM FONDEN Young Investigator Programme. G.B.C. acknowledges the Max Planck Society for financial support through the Max Planck Research Group for S. H. Suyu and the academic support from the German Centre for Cosmological Lensing. P.B. acknowledges financial support from ASI through the agreement ASI-INAF n. 2018-29-HH.0. R.D. gratefully acknowledges support from the Chilean Centro de Excelencia en Astrof?sica y Tecnolog?as Afines (CATA) BASAL grant AFB-170002".
Publisher Copyright:
© ESO 2018.
PY - 2021/12/1
Y1 - 2021/12/1
N2 - Context. The processes responsible for galaxy evolution in different environments as a function of galaxy mass remain heavily debated. Rich galaxy clusters are ideal laboratories in which to distinguish the role of environmental versus mass quenching because they consist of a full range of galaxies and environments. Aims. Using the CLASH-VLT survey, we assembled an unprecedentedly large sample of 1234 spectroscopically confirmed members in Abell S1063. We found a dynamically complex structure at «zcl»= 0.3457 with a velocity dispersion σv = 1380-32+26 km s-1. We investigated cluster environmental and dynamical effects by analysing the projected phase-space diagram and the orbits as a function of galaxy spectral properties. Methods. We classified cluster galaxies according to the presence and strength of the [OII] emission line, the strength of the Hδ absorption line, and colours. We investigated the relation between the spectral classes of galaxies and their position in the projected phase-space diagram. We separately analysed red and blue galaxy orbits. By correlating the observed positions and velocities with the projected phase-space constructed from simulations, we constrained the accretion redshift of galaxies with different spectral types. Results. Passive galaxies are mainly located in the virialised region, while emission-line galaxies lie beyond r200 and are accreted into the cluster at a later time. Emission-line and post-starburst galaxies show an asymmetric distribution in projected phase-space within r200; emission-line galaxies are prominent at Δv/σ ≲ -1.5 and post-starburst galaxies at Δv/σ ≲ 1.5, suggesting that backsplash galaxies lie at high positive velocities. We find that low-mass passive galaxies are accreted into the cluster before high-mass galaxies. This suggests that we observe as passives only the low-mass galaxies that are accreted early into the cluster as blue galaxies. They had the time to quench their star formation. We also find that red galaxies move on more radial orbits than blue galaxies. This can be explained if infalling galaxies can remain blue by moving on tangential orbits.
AB - Context. The processes responsible for galaxy evolution in different environments as a function of galaxy mass remain heavily debated. Rich galaxy clusters are ideal laboratories in which to distinguish the role of environmental versus mass quenching because they consist of a full range of galaxies and environments. Aims. Using the CLASH-VLT survey, we assembled an unprecedentedly large sample of 1234 spectroscopically confirmed members in Abell S1063. We found a dynamically complex structure at «zcl»= 0.3457 with a velocity dispersion σv = 1380-32+26 km s-1. We investigated cluster environmental and dynamical effects by analysing the projected phase-space diagram and the orbits as a function of galaxy spectral properties. Methods. We classified cluster galaxies according to the presence and strength of the [OII] emission line, the strength of the Hδ absorption line, and colours. We investigated the relation between the spectral classes of galaxies and their position in the projected phase-space diagram. We separately analysed red and blue galaxy orbits. By correlating the observed positions and velocities with the projected phase-space constructed from simulations, we constrained the accretion redshift of galaxies with different spectral types. Results. Passive galaxies are mainly located in the virialised region, while emission-line galaxies lie beyond r200 and are accreted into the cluster at a later time. Emission-line and post-starburst galaxies show an asymmetric distribution in projected phase-space within r200; emission-line galaxies are prominent at Δv/σ ≲ -1.5 and post-starburst galaxies at Δv/σ ≲ 1.5, suggesting that backsplash galaxies lie at high positive velocities. We find that low-mass passive galaxies are accreted into the cluster before high-mass galaxies. This suggests that we observe as passives only the low-mass galaxies that are accreted early into the cluster as blue galaxies. They had the time to quench their star formation. We also find that red galaxies move on more radial orbits than blue galaxies. This can be explained if infalling galaxies can remain blue by moving on tangential orbits.
KW - Galaxies: clusters: general
KW - Galaxies: clusters: individual: A S1063
KW - Galaxies: evolution
KW - Galaxies: kinematics and dynamics
KW - Galaxies: stellar content
UR - http://www.scopus.com/inward/record.url?scp=85122025717&partnerID=8YFLogxK
U2 - 10.1051/0004-6361/202142168
DO - 10.1051/0004-6361/202142168
M3 - Article
AN - SCOPUS:85122025717
VL - 656
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
SN - 0004-6361
M1 - A147
ER -