X-Ray Emission from Star-cluster Winds in Starburst Galaxies

Result code in IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F22%3A00556102" target="_blank" >RIV/67985815:_____/22:00556102 - isvavai.cz</a>

Result on the web

<a href="http://hdl.handle.net/11104/0330921" target="_blank" >http://hdl.handle.net/11104/0330921</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.3847/1538-4357/ac4fc2" target="_blank" >10.3847/1538-4357/ac4fc2</a>

Result language

angličtina

Original language name

X-Ray Emission from Star-cluster Winds in Starburst Galaxies

Original language description

Inspired by the excess soft X-ray emission recently detected in Green Pea galaxies, we model the soft X-ray emission (0.5-2.0 keV) of hot gas from star-cluster winds. By combining individual star clusters, we estimate the soft X-ray emission expected from the typically unresolved diffuse hot gas in starburst galaxies, devoid of competing emission from, e.g., active galactic nuclei (AGNs) or other unresolved point sources. We use stellar models of subsolar metallicities (0.02 Z (circle dot) and 0.4 Z (circle dot)) and take into account supernova explosions for massive stars. For lower metallicities, we find that stellar winds do not contribute significantly (less than or similar to 3% of the mechanical energy) to the observed soft X-ray emission of normal star-forming galaxies. For higher metallicities and possibly also for larger proportions of massive star clusters in the simulated starburst galaxies, we reproduce well the observed correlation between star formation rate and X-ray luminosity previously reported in the literature. However, we find that no combination of model assumptions is capable of reproducing the substantial soft X-ray emission observed from Green Pea galaxies, indicating that other emission mechanisms (i.e., unusually large quantities of high-/low-mass X-ray binaries, ultraluminous X-ray sources, a modified initial mass function, intermediate-mass black holes, or AGNs) are more likely to be responsible for the X-ray excess.

Czech name

—

Czech description

—

Type

J_imp - Article in a specialist periodical, which is included in the Web of Science database

CEP classification

—

OECD FORD branch

10308 - Astronomy (including astrophysics,space science)

Project

Result was created during the realization of more than one project. More information in the Projects tab.

Continuities

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Publication year

2022

Confidentiality

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

Name of the periodical

Astrophysical Journal

ISSN

0004-637X

e-ISSN

1538-4357

Volume of the periodical

927

Issue of the periodical within the volume

2

Country of publishing house

GB - UNITED KINGDOM

Number of pages

14

Pages from-to

212

UT code for WoS article

000770133700001

EID of the result in the Scopus database

2-s2.0-85127308513