An H alpha/X-ray orphan cloud as a signpost of intracluster medium clumping

Kód výsledku v 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>

Výsledek na webu

<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>

Jazyk výsledku

angličtina

Název v původním jazyce

An H alpha/X-ray orphan cloud as a signpost of intracluster medium clumping

Popis výsledku v původním jazyce

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.

Název v anglickém jazyce

An H alpha/X-ray orphan cloud as a signpost of intracluster medium clumping

Popis výsledku anglicky

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.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

—

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2021

Kód důvěrnosti údajů

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Název periodika

Monthly Notices of the Royal Astronomical Society

ISSN

0035-8711

e-ISSN

1365-2966

Svazek periodika

505

Číslo periodika v rámci svazku

4

Stát vydavatele periodika

GB - Spojené království Velké Británie a Severního Irska

Počet stran výsledku

15

Strana od-do

4702-4716

Kód UT WoS článku

000698549400001

EID výsledku v databázi Scopus

2-s2.0-85109488819