Time-scales for the effects of interactions on galaxy properties and SMBH growth

Result code in IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216224%3A14310%2F25%3A00144413" target="_blank" >RIV/00216224:14310/25:00144413 - isvavai.cz</a>

Result on the web

<a href="https://academic.oup.com/mnras/article/539/4/2967/8105726" target="_blank" >https://academic.oup.com/mnras/article/539/4/2967/8105726</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1093/mnras/staf541" target="_blank" >10.1093/mnras/staf541</a>

Result language

angličtina

Original language name

Time-scales for the effects of interactions on galaxy properties and SMBH growth

Original language description

Galaxy interaction and merging have clear effects on the systems involved. We find an increase in the star formation rate (SFR), potential ignition of active galactic nuclei (AGNs), and significant morphology changes. However, at what stage during interactions or mergers these changes begin to occur remains an open question. With a combination of machine learning and visual classification, we select a sample of 3162 interacting and merging galaxies in the Cosmic Evolutionary Survey (COSMOS) field across a redshift range of 0.0-1.2. We divide this sample into four distinct stages of interaction based on their morphology, each stage representing a different phase of the dynamical time-scale. We use the rich ancillary data available in COSMOS to probe the relation between interaction stage, stellar mass, SFR, and AGN fraction. We find that the distribution of SFRs rapidly changes with stage for mass distributions consistent with being drawn from the same parent sample. This is driven by a decrease in the fraction of red sequence galaxies (from 17 per cent as close pairs to 1.4 per cent during merging) and an increase in the fraction of starburst galaxies (from 7 per cent to 32 per cent). We find that the AGN fraction increases by a factor of 1.2 only at coalescence. We find that the effects of interaction peak at the point of closest approach and coalescence of the two systems. We show that the point in time of the underlying dynamical time-scale - and its related morphology - is as important to consider as its projected separation.

Czech name

—

Czech description

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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

<a href="/en/project/GM24-10599M" target="_blank" >GM24-10599M: Stars in galactic nuclei: interrelation with massive black holes</a><br>

Continuities

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

Publication year

2025

Confidentiality

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

Name of the periodical

Monthly Notices of the Royal Astronomical Society

ISSN

0035-8711

e-ISSN

1365-2966

Volume of the periodical

539

Issue of the periodical within the volume

4

Country of publishing house

GB - UNITED KINGDOM

Number of pages

20

Pages from-to

2967-2986

UT code for WoS article

001482817100001

EID of the result in the Scopus database

2-s2.0-105004675346