The BIG X-ray tail

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F21%3A00552296" target="_blank" >RIV/67985815:_____/21:00552296 - isvavai.cz</a>

Výsledek na webu

<a href="https://doi.org/10.1093/mnrasl/slab108" target="_blank" >https://doi.org/10.1093/mnrasl/slab108</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1093/mnrasl/slab108" target="_blank" >10.1093/mnrasl/slab108</a>

Jazyk výsledku

angličtina

Název v původním jazyce

The BIG X-ray tail

Popis výsledku v původním jazyce

Galaxy clusters grow primarily through the continuous accretion of group-scale haloes. Group galaxies experience preprocessing during their journey into clusters. A star-bursting compact group, the Blue Infalling Group (BIG), is plunging into the nearby cluster A1367. Previous optical observations reveal rich tidal features in the BIG members, and a long H alpha trail behind. Here, we report the discovery of a projected similar to 250 kpc X-ray tail behind the BIG using Chandra and XMM-Newton observations. The total hot gas mass in the tail is similar to 7 x 10(10) M-circle dot with an X-ray bolometric luminosity of similar to 3.8 x 10(41) erg s(-1). The temperature along the tail is similar to 1 keV, but the apparent metallicity is very low, an indication of the multi-T nature of the gas. The X-ray and H alpha surface brightnesses in the front part of the BIG tail follow the tight correlation established from a sample of stripped tails in nearby clusters, which suggests the multiphase gas originates from the mixing of the stripped interstellar medium (ISM) with the hot intracluster medium (ICM). Because thermal conduction and hydrodynamic instabilities are significantly suppressed, the stripped ISM can be long lived and produce ICM clumps. The BIG provides us a rare laboratory to study galaxy transformation and preprocessing.

Název v anglickém jazyce

The BIG X-ray tail

Popis výsledku anglicky

Galaxy clusters grow primarily through the continuous accretion of group-scale haloes. Group galaxies experience preprocessing during their journey into clusters. A star-bursting compact group, the Blue Infalling Group (BIG), is plunging into the nearby cluster A1367. Previous optical observations reveal rich tidal features in the BIG members, and a long H alpha trail behind. Here, we report the discovery of a projected similar to 250 kpc X-ray tail behind the BIG using Chandra and XMM-Newton observations. The total hot gas mass in the tail is similar to 7 x 10(10) M-circle dot with an X-ray bolometric luminosity of similar to 3.8 x 10(41) erg s(-1). The temperature along the tail is similar to 1 keV, but the apparent metallicity is very low, an indication of the multi-T nature of the gas. The X-ray and H alpha surface brightnesses in the front part of the BIG tail follow the tight correlation established from a sample of stripped tails in nearby clusters, which suggests the multiphase gas originates from the mixing of the stripped interstellar medium (ISM) with the hot intracluster medium (ICM). Because thermal conduction and hydrodynamic instabilities are significantly suppressed, the stripped ISM can be long lived and produce ICM clumps. The BIG provides us a rare laboratory to study galaxy transformation and preprocessing.

Druh

J_ost - Ostatní články v recenzovaných periodicích

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

508

Číslo periodika v rámci svazku

1

Stát vydavatele periodika

GB - Spojené království Velké Británie a Severního Irska

Počet stran výsledku

5

Strana od-do

"L69"-"L73"

Kód UT WoS článku

000716727400002

EID výsledku v databázi Scopus

2-s2.0-85119529914