Stellar population synthesis models with a physically varying IMF

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F25%3A10509457" target="_blank" >RIV/00216208:11320/25:10509457 - isvavai.cz</a>

Výsledek na webu

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

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1093/mnras/staf091" target="_blank" >10.1093/mnras/staf091</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Stellar population synthesis models with a physically varying IMF

Popis výsledku v původním jazyce

Interpreting galactic luminosity requires assumptions about the galaxy-wide initial mass function (gwIMF), often assumed invariant in most stellar population synthesis (SPS) models. If stars form in clusters with metallicity- and density-dependent stellar IMFs, the integrated galaxy-wide IMF (IGIMF) can be calculated, with its shape depending on the star formation rate (SFR) and metallicity. The shape of the IGIMF thus depends on the SFR and metallicity. We develop the SPS-VarIMF code which enables us for the first time to compute the spectra, luminosities, and remnant populations of galaxies in the context of the varying gwIMF with time, SFR, and an assumed metallicity. Using the SPS-VarIMF code one can calculate how the interpretation from the integrated galactic light may change if the underlying galaxy-wide IMF is assumed to be environmentally dependent instead of being invariant. In particular, we compare the time evolution of the galaxy colour and the stellar mass-to-light ratio in different bands for the IGIMF and invariant canonical gwIMF assuming constant and delayed-tau star formation histories. We show that the underlying gwIMF can be determined by examining the colours and luminosities of late-type galaxies in ultraviolet and optical bands. On the other hand, for early-type galaxies, it is difficult to distinguish which gwIMF is valid since adopting the different gwIMFs yields almost identical colours. However, their gwIMF-dependent mass-to-light (M/L) ratios differ by up to an order of magnitude. Massive present-day elliptical galaxies would have been 10(4 )times as bright as at present when they were forming.

Název v anglickém jazyce

Stellar population synthesis models with a physically varying IMF

Popis výsledku anglicky

Interpreting galactic luminosity requires assumptions about the galaxy-wide initial mass function (gwIMF), often assumed invariant in most stellar population synthesis (SPS) models. If stars form in clusters with metallicity- and density-dependent stellar IMFs, the integrated galaxy-wide IMF (IGIMF) can be calculated, with its shape depending on the star formation rate (SFR) and metallicity. The shape of the IGIMF thus depends on the SFR and metallicity. We develop the SPS-VarIMF code which enables us for the first time to compute the spectra, luminosities, and remnant populations of galaxies in the context of the varying gwIMF with time, SFR, and an assumed metallicity. Using the SPS-VarIMF code one can calculate how the interpretation from the integrated galactic light may change if the underlying galaxy-wide IMF is assumed to be environmentally dependent instead of being invariant. In particular, we compare the time evolution of the galaxy colour and the stellar mass-to-light ratio in different bands for the IGIMF and invariant canonical gwIMF assuming constant and delayed-tau star formation histories. We show that the underlying gwIMF can be determined by examining the colours and luminosities of late-type galaxies in ultraviolet and optical bands. On the other hand, for early-type galaxies, it is difficult to distinguish which gwIMF is valid since adopting the different gwIMFs yields almost identical colours. However, their gwIMF-dependent mass-to-light (M/L) ratios differ by up to an order of magnitude. Massive present-day elliptical galaxies would have been 10(4 )times as bright as at present when they were forming.

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

Monthly Notices of the Royal Astronomical Society

ISSN

0035-8711

e-ISSN

1365-2966

Svazek periodika

537

Číslo periodika v rámci svazku

3

Stát vydavatele periodika

GB - Spojené království Velké Británie a Severního Irska

Počet stran výsledku

16

Strana od-do

2782-2797

Kód UT WoS článku

001421952200001

EID výsledku v databázi Scopus

2-s2.0-86000620082