Jellyfish galaxies with the IllustrisTNG simulations: I. Gas-stripping phenomena in the full cosmological context
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1810.00005.pdf
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Accepted version
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Author(s)
Yun, Kiyun
Pillepich, Annalisa
Zinger, Elad
Nelson, Dylan
Donnari, Martina
Joshi, Gandhali
Rodriguez-Gomez, Vicente
Genel, Shy
Weinberger, Rainer
Vogelsberger, Mark
Date Issued
November 2018
Journal
Monthly Notices of the Royal Astronomical Society
Publisher
Oxford University Press (OUP)
Citation
Yun, Kiyun et al. "Jellyfish galaxies with the IllustrisTNG simulations: I. Gas-stripping phenomena in the full cosmological context." Monthly Notices of the Royal Astronomical Society 483, 1 (February 2019): 1042-1066 © 2018 The Author(s)
Version
Author's final manuscript
Abstract
We use the IllustrisTNG simulations to study the demographics and properties of jellyfish galaxies in the full cosmological context. By jellyfish galaxies, we mean satellites orbiting in massive groups and clusters that exhibit highly asymmetric distributions of gas and gas tails. In particular, we select TNG100 galaxies at low redshifts (z ≤ 0.6) with stellar mass exceeding 10[superscript 9.5] M[subscript ⊙] and with host halo masses in the range 10[superscript 13] ≤ M[subscript 200c]/M[subscript ⊙] ≤ 1014.6. Among more than about 6000 (2600) galaxies with stars (and some gas), we identify 800 jellyfish galaxies by visually inspecting their gas and stellar mass maps in random projections. Namely, about 31 per cent of cluster satellites are found with signatures of ram-pressure stripping and gaseous tails stemming from their main luminous bodies. This is a lower limit: the random orientation entails a loss of about 30 per cent of galaxies that in an optimal projection would otherwise be identified as jellyfish. Furthermore, jellyfish galaxies are more frequent at intermediate and large cluster-centric distances (r/R[subscript 200c] ≳ 0.25), in more massive hosts and at smaller satellite masses, and they typically orbit supersonically. The gaseous tails usually extend in opposite directions to the galaxy trajectory, with no relation between tail orientation and position of the host’s centre. Finally, jellyfish galaxies are late infallers (<2.5–3 Gyr ago, at z = 0) and the emergence of gaseous tails correlates well with the presence of bow shocks in the intracluster medium. Keywords: methods:numerical; galaxies:clusters:general; galaxies:clusters:intracluster medium; galaxies:evolution; galaxies:groups:general; cosmology:theory
MIT Department
MIT Kavli Institute for Astrophysics and Space Research
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DOI of Published Version
https://doi.org/10.1093/MNRAS/STY3156
