Turbulence in the tail of a jellyfish galaxy
The result's identifiers
Result code in IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F23%3A00571484" target="_blank" >RIV/67985815:_____/23:00571484 - isvavai.cz</a>
Result on the web
<a href="https://doi.org/10.1093/mnras/stad874" target="_blank" >https://doi.org/10.1093/mnras/stad874</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.1093/mnras/stad874" target="_blank" >10.1093/mnras/stad874</a>
Alternative languages
Result language
angličtina
Original language name
Turbulence in the tail of a jellyfish galaxy
Original language description
When galaxies move through the intracluster medium (ICM) inside galaxy clusters, the ram pressure of the ICM can strip the gas from galaxies. The stripped gas forms tails on the trailing side. These galaxies are hence dubbed 'jellyfish galaxies'. ESO 137-001 is a quintessential jellyfish galaxy located in the nearest rich cluster, the Norma cluster. Its spectacular multiphase tail has complex morphology and kinematics both from the imprinted galaxy's interstellar medium (ISM) and as a result of the interactions between the stripped gas and the surrounding hot plasma, mediated by radiative cooling and magnetic fields. We study the kinematics of the multiphase tail using high-resolution observations of the ionized and the molecular gas in the entire structure. We calculate the velocity structure functions in moving frames along the tail and find that turbulence driven by Kelvin-Helmholtz (KH) instability quickly overwhelms the original ISM turbulence and saturates at similar to 30 kpc. There is also a hint that the far end of the tail has possibly started to inherit pre-existing large-scale ICM turbulence likely caused by structure formation. Turbulence measured by the molecular gas is generally consistent with that measured by the ionized gas in the tail but has a slightly lower amplitude. Most of the measured turbulence is below the mean free path of the hot ICM (similar to 11 kpc). Using warm/cool gas as a tracer of the hot ICM, we find that the isotropic viscosity of the hot plasma must be suppressed below 0.01 per cent Spitzer level.
Czech name
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Czech description
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Classification
Type
J<sub>imp</sub> - Article in a specialist periodical, which is included in the Web of Science database
CEP classification
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OECD FORD branch
10308 - Astronomy (including astrophysics,space science)
Result continuities
Project
<a href="/en/project/LM2023059" target="_blank" >LM2023059: Atacama Large Millimeter /submillimeter Array – participation of the Czech Republic</a><br>
Continuities
I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace
Others
Publication year
2023
Confidentiality
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů
Data specific for result type
Name of the periodical
Monthly Notices of the Royal Astronomical Society
ISSN
0035-8711
e-ISSN
1365-2966
Volume of the periodical
521
Issue of the periodical within the volume
3
Country of publishing house
US - UNITED STATES
Number of pages
7
Pages from-to
4785-4791
UT code for WoS article
000961536600016
EID of the result in the Scopus database
2-s2.0-85159595064