Growth of black holes at the centre of early-type galaxies in MOND

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F25%3A10509578" target="_blank" >RIV/00216208:11320/25:10509578 - isvavai.cz</a>

Výsledek na webu

<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=DxgLLG95lv" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=DxgLLG95lv</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1017/pasa.2025.10034" target="_blank" >10.1017/pasa.2025.10034</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Growth of black holes at the centre of early-type galaxies in MOND

Popis výsledku v původním jazyce

The formation of supermassive black holes (SMBHs) in early-type galaxies (ETGs) is a key challenge for galaxy formation theories. Using the monolithic collapse models of ETGs formed in Milgromian Dynamics (MOND) from 2022MNRAS.516.1081E, we investigate the conditions necessary to form SMBHs in MOND and test whether these systems adhere to observed SMBH-galaxy scaling relations. We analyse the evolution of the gravitational potential and gas inflow rates in the model relics with a total stellar mass ranging from 0.1x10(11)M(circle dot) to 0.7x10(11)M(circle dot). The gravitational potential exhibits a rapid deepening during the initial galaxy formation phase, accompanied by high gas inflow rates. These conditions suggest efficient central gas accumulation capable of fuelling SMBH formation. We further examine the MBH-sigma relation by assuming that a fraction of the central stellar mass contributes to black hole formation. Black hole masses derived from 10%-100 % of the central mass are comparable with the observed relation, particularly at higher central velocity dispersions (sigma&gt;200km/s). This highlights the necessity of substantial inner mass collapse to produce SMBHs consistent with observations. Our results demonstrate that MOND dynamics, through the rapid evolution of the gravitational potential and sustained gas inflows, provide a favourable environment for SMBH formation in ETGs. These findings support the hypothesis that MOND can naturally account for the observed SMBH-galaxy scaling relations without invoking cold dark matter, emphasizing the importance of early gas dynamics in determining final SMBH properties.

Název v anglickém jazyce

Growth of black holes at the centre of early-type galaxies in MOND

Popis výsledku anglicky

The formation of supermassive black holes (SMBHs) in early-type galaxies (ETGs) is a key challenge for galaxy formation theories. Using the monolithic collapse models of ETGs formed in Milgromian Dynamics (MOND) from 2022MNRAS.516.1081E, we investigate the conditions necessary to form SMBHs in MOND and test whether these systems adhere to observed SMBH-galaxy scaling relations. We analyse the evolution of the gravitational potential and gas inflow rates in the model relics with a total stellar mass ranging from 0.1x10(11)M(circle dot) to 0.7x10(11)M(circle dot). The gravitational potential exhibits a rapid deepening during the initial galaxy formation phase, accompanied by high gas inflow rates. These conditions suggest efficient central gas accumulation capable of fuelling SMBH formation. We further examine the MBH-sigma relation by assuming that a fraction of the central stellar mass contributes to black hole formation. Black hole masses derived from 10%-100 % of the central mass are comparable with the observed relation, particularly at higher central velocity dispersions (sigma&gt;200km/s). This highlights the necessity of substantial inner mass collapse to produce SMBHs consistent with observations. Our results demonstrate that MOND dynamics, through the rapid evolution of the gravitational potential and sustained gas inflows, provide a favourable environment for SMBH formation in ETGs. These findings support the hypothesis that MOND can naturally account for the observed SMBH-galaxy scaling relations without invoking cold dark matter, emphasizing the importance of early gas dynamics in determining final SMBH properties.

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

2025

Kód důvěrnosti údajů

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

Název periodika

Publications of the Astronomical Society of Australia

ISSN

1323-3580

e-ISSN

1448-6083

Svazek periodika

42

Číslo periodika v rámci svazku

cerven

Stát vydavatele periodika

AU - Austrálie

Počet stran výsledku

7

Strana od-do

e065

Kód UT WoS článku

001515297700001

EID výsledku v databázi Scopus

2-s2.0-105005649776