TY - JOUR
T1 - Free-floating molecular clumps and gas mixing
T2 - Hydrodynamic aftermaths of the intracluster-interstellar medium interaction
AU - Ruggiero, Rafael
AU - Teyssier, Romain
AU - Neto, Gastao B.Lima
AU - Perret, Valentin
N1 - Funding Information:
This work is a part of the research project funded by the São Paulo R esearch Foundation, FAPESP (grants 15/13141-7 and 16/19586-3). GBLN thanks Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq) for partial financial support. The simulations presented here were run at the Swiss National Supercomputing Center (CSCS), specifically using the Piz Daint supercomputer. Our data analysis has been largely done using the Hydra cluster at the University of Zurich, and it has extensively used YT (Turk et al. 2011). We thank Daisuke Nagai and Tom Abel for the suggestions that helped shape this paper.
Publisher Copyright:
© 2018 The Author(s).
PY - 2018/10
Y1 - 2018/10
N2 - The interaction of gas-rich galaxies with the intracluster medium (ICM) of galaxy clusters has a remarkable impact on their evolution, mainly due to the gas loss associated with this process. In this work, we use an idealized, high-resolution simulation of a Virgo-like cluster, run with RAMSES and with dynamics reproducing that of a zoom cosmological simulation, to investigate the interaction of infalling galaxies with the ICM. We find that the tails of ram pressure stripped galaxies give rise to a population of up to more than a hundred clumps of molecular gas lurking in the cluster. The number count of those clumps varies a lot overtime - they are preferably generated when a large galaxy crosses the cluster (M200c > 1012 M⊙), and their lifetime (≲ 300 Myr) is small compared to the age of the cluster. We compute the intracluster luminosity associated with the star formation that takes place within those clumps, finding that the stars formed in all of the galaxy tails combined amount to an irrelevant contribution to the intracluster light. Surprisingly, we also find in our simulation that the ICM gas significantly changes the composition of the gaseous discs of the galaxies: after crossing the cluster once, typically 20 per cent of the cold gas still in those discs comes from the ICM.
AB - The interaction of gas-rich galaxies with the intracluster medium (ICM) of galaxy clusters has a remarkable impact on their evolution, mainly due to the gas loss associated with this process. In this work, we use an idealized, high-resolution simulation of a Virgo-like cluster, run with RAMSES and with dynamics reproducing that of a zoom cosmological simulation, to investigate the interaction of infalling galaxies with the ICM. We find that the tails of ram pressure stripped galaxies give rise to a population of up to more than a hundred clumps of molecular gas lurking in the cluster. The number count of those clumps varies a lot overtime - they are preferably generated when a large galaxy crosses the cluster (M200c > 1012 M⊙), and their lifetime (≲ 300 Myr) is small compared to the age of the cluster. We compute the intracluster luminosity associated with the star formation that takes place within those clumps, finding that the stars formed in all of the galaxy tails combined amount to an irrelevant contribution to the intracluster light. Surprisingly, we also find in our simulation that the ICM gas significantly changes the composition of the gaseous discs of the galaxies: after crossing the cluster once, typically 20 per cent of the cold gas still in those discs comes from the ICM.
KW - Galaxies: ISM- galaxies: clusters: intracluster medium
KW - Galaxies: clusters: general
KW - Galaxies: dwarf
KW - Galaxies: interactions
KW - Methods: numerical
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U2 - 10.1093/MNRAS/STY2010
DO - 10.1093/MNRAS/STY2010
M3 - Article
AN - SCOPUS:85055350226
SN - 0035-8711
VL - 480
SP - 2191
EP - 2199
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 2
ER -