An H alpha/X-ray orphan cloud as a signpost of intracluster medium clumping
The result's identifiers
Result code in IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F21%3A00547946" target="_blank" >RIV/67985815:_____/21:00547946 - isvavai.cz</a>
Result on the web
<a href="https://doi.org/10.1093/mnras/stab1569" target="_blank" >https://doi.org/10.1093/mnras/stab1569</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.1093/mnras/stab1569" target="_blank" >10.1093/mnras/stab1569</a>
Alternative languages
Result language
angličtina
Original language name
An H alpha/X-ray orphan cloud as a signpost of intracluster medium clumping
Original language description
Recent studies have highlighted the potential significance of intracluster medium (ICM) clumping and its important implications for cluster cosmology and baryon physics. Many of the ICM clumps can originate from infalling galaxies, as stripped interstellar medium (ISM) mixing into the hot ICM. However, a direct connection between ICM clumping and stripped ISM has not been unambiguously established before. Here, we present the discovery of the first and still the only known isolated cloud (or orphan cloud [OC]) detected in both X-rays and H alpha in the nearby cluster A1367. With an effective radius of 30 kpc, this cloud has an average X-ray temperature of 1.6 keV, a bolometric X-ray luminosity of similar to 3.1 x 10(41) erg s(-1), and a hot gas mass of similar to 10(10) M-circle dot. From the Multi-Unit Spectroscopic Explorer (MUSE) data, the OC shows an interesting velocity gradient nearly along the east-west direction with a low level of velocity dispersion of similar to 80 km s(-1), which may suggest a low level of the ICM turbulence. The emission line diagnostics suggest little star formation in the main Ha cloud and a low-ionization (nuclear) emission-line regions like spectrum, but the excitation mechanisms remain unclear. This example shows that stripped ISM, even long after the initial removal from the galaxy, can still induce ICM inhomogeneities. We suggest that the magnetic field can stabilize the OC by suppressing hydrodynamic instabilities and thermal conduction. This example also suggests that at least some ICM clumps are multiphase in nature and implies that the ICM clumps can also be traced in H alpha. Thus, future deep and wide-field H alpha surveys can be used to probe the ICM clumping and turbulence.
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
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Continuities
I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace
Others
Publication year
2021
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
505
Issue of the periodical within the volume
4
Country of publishing house
GB - UNITED KINGDOM
Number of pages
15
Pages from-to
4702-4716
UT code for WoS article
000698549400001
EID of the result in the Scopus database
2-s2.0-85109488819