X-ray metal line emission from the hot circumgalactic medium: probing the effects of supermassive black hole feedback

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216224%3A14310%2F23%3A00134402" target="_blank" >RIV/00216224:14310/23:00134402 - isvavai.cz</a>

Výsledek na webu

<a href="https://arxiv.org/abs/2307.01277" target="_blank" >https://arxiv.org/abs/2307.01277</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1093/mnras/stad2216" target="_blank" >10.1093/mnras/stad2216</a>

Jazyk výsledku

angličtina

Název v původním jazyce

X-ray metal line emission from the hot circumgalactic medium: probing the effects of supermassive black hole feedback

Popis výsledku v původním jazyce

We derive predictions from state-of-the-art cosmological galaxy simulations for the spatial distribution of the hot circumgalactic medium (CGM, [0.1-1]R-200c) through its emission lines in the X-ray soft band ([0.3-1.3] keV). In particular, we compare IllustrisTNG, EAGLE, and SIMBA and focus on galaxies with stellar mass 10(10-11.6) M-circle dot at z = 0. The three simulation models return significantly different surface brightness radial profiles of prominent emission lines from ionized metals such as O VII(f), O VIII, and Fe XVII as a function of galaxy mass. Likewise, the three simulations predict varying azimuthal distributions of line emission with respect to the galactic stellar planes, with IllustrisTNG predicting the strongest angular modulation of CGM physical properties at radial range greater than or similar to 0.3-0.5 R-200c. This anisotropic signal is more prominent for higher energy lines, where it can manifest as X-ray eROSITA-like bubbles. Despite different models of stellar and supermassive black hole (SMBH) feedback, the three simulations consistently predict a dichotomy between star-forming and quiescent galaxies at the Milky Way and Andromeda mass range, where the former are X-ray brighter than the latter. This is a signature of SMBH-driven outflows, which are responsible for quenching star formation. Finally, we explore the prospect of testing these predictions with a microcalorimeter-based X-ray mission concept with a large field of view. Such a mission would probe the extended hot CGM via soft X-ray line emission, determine the physical properties of the CGM, including temperature, from the measurement of line ratios, and provide critical constraints on the efficiency and impact of SMBH feedback on the CGM.

Název v anglickém jazyce

X-ray metal line emission from the hot circumgalactic medium: probing the effects of supermassive black hole feedback

Popis výsledku anglicky

We derive predictions from state-of-the-art cosmological galaxy simulations for the spatial distribution of the hot circumgalactic medium (CGM, [0.1-1]R-200c) through its emission lines in the X-ray soft band ([0.3-1.3] keV). In particular, we compare IllustrisTNG, EAGLE, and SIMBA and focus on galaxies with stellar mass 10(10-11.6) M-circle dot at z = 0. The three simulation models return significantly different surface brightness radial profiles of prominent emission lines from ionized metals such as O VII(f), O VIII, and Fe XVII as a function of galaxy mass. Likewise, the three simulations predict varying azimuthal distributions of line emission with respect to the galactic stellar planes, with IllustrisTNG predicting the strongest angular modulation of CGM physical properties at radial range greater than or similar to 0.3-0.5 R-200c. This anisotropic signal is more prominent for higher energy lines, where it can manifest as X-ray eROSITA-like bubbles. Despite different models of stellar and supermassive black hole (SMBH) feedback, the three simulations consistently predict a dichotomy between star-forming and quiescent galaxies at the Milky Way and Andromeda mass range, where the former are X-ray brighter than the latter. This is a signature of SMBH-driven outflows, which are responsible for quenching star formation. Finally, we explore the prospect of testing these predictions with a microcalorimeter-based X-ray mission concept with a large field of view. Such a mission would probe the extended hot CGM via soft X-ray line emission, determine the physical properties of the CGM, including temperature, from the measurement of line ratios, and provide critical constraints on the efficiency and impact of SMBH feedback on the CGM.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

<a href="/cs/project/GX21-13491X" target="_blank" >GX21-13491X: Zkoumání žhavého vesmíru a porozumění kosmické zpětné vazbě</a><br>

Návaznosti

P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)

Rok uplatnění

2023

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

525

Číslo periodika v rámci svazku

2

Stát vydavatele periodika

GB - Spojené království Velké Británie a Severního Irska

Počet stran výsledku

22

Strana od-do

1976-1997

Kód UT WoS článku

001054211400002

EID výsledku v databázi Scopus

2-s2.0-85170412380