Distribution of star formation rates during the rapid assembly of NGC 1399 as deduced from its globular cluster system

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F16%3A10336330" target="_blank" >RIV/00216208:11320/16:10336330 - isvavai.cz</a>

Výsledek na webu

<a href="http://dx.doi.org/10.1051/0004-6361/201628927" target="_blank" >http://dx.doi.org/10.1051/0004-6361/201628927</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/201628927" target="_blank" >10.1051/0004-6361/201628927</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Distribution of star formation rates during the rapid assembly of NGC 1399 as deduced from its globular cluster system

Popis výsledku v původním jazyce

Ultra-compact dwarf galaxies (UCDs) share many properties with globular clusters (GCs) and are found in similar environments. Here, a large sample of UCDs and GCs around NGC 1399, the central giant elliptical of the Fornax galaxy cluster, is used to infer their formation history and also to shed light on the formation of NGC 1399 itself. We assumed that all GCs and UCDs in our sample are the result of star cluster (SC) formation processes and used them as tracers of past star formation activities. After correcting our GC/UCD sample for mass loss, we interpreted their overall mass function to be a superposition of SC populations that formed coevally during different formation epochs. The SC masses of each population were distributed according to the embedded cluster mass function (ECMF), a pure power law with the slope -beta. Each ECMF was characterized by a stellar upper mass limit, M-max, which depended on the star formation rate (SFR). We decomposed the observed GC/UCD mass function into individual SC populations and converted M-max of each SC population to an SFR. The overall distribution of SFRs reveals under which conditions the GC /UCD sample around NGC 1399 formed. Considering the constraints set by the age of the GCs/UCDs and the present stellar mass of NGC 1399, we found that the formation of the GCs /UCDs can be well explained within our framework with values for beta below 2.3. This finding agrees very well with the observation of young SCs where beta approximate to 2 : 0 is usually found. Even though we took into account that some of the most massive objects might not be genuine SCs and applied different corrections for the mass loss, we found that these considerations do not influence much the outcome.

Název v anglickém jazyce

Distribution of star formation rates during the rapid assembly of NGC 1399 as deduced from its globular cluster system

Popis výsledku anglicky

Ultra-compact dwarf galaxies (UCDs) share many properties with globular clusters (GCs) and are found in similar environments. Here, a large sample of UCDs and GCs around NGC 1399, the central giant elliptical of the Fornax galaxy cluster, is used to infer their formation history and also to shed light on the formation of NGC 1399 itself. We assumed that all GCs and UCDs in our sample are the result of star cluster (SC) formation processes and used them as tracers of past star formation activities. After correcting our GC/UCD sample for mass loss, we interpreted their overall mass function to be a superposition of SC populations that formed coevally during different formation epochs. The SC masses of each population were distributed according to the embedded cluster mass function (ECMF), a pure power law with the slope -beta. Each ECMF was characterized by a stellar upper mass limit, M-max, which depended on the star formation rate (SFR). We decomposed the observed GC/UCD mass function into individual SC populations and converted M-max of each SC population to an SFR. The overall distribution of SFRs reveals under which conditions the GC /UCD sample around NGC 1399 formed. Considering the constraints set by the age of the GCs/UCDs and the present stellar mass of NGC 1399, we found that the formation of the GCs /UCDs can be well explained within our framework with values for beta below 2.3. This finding agrees very well with the observation of young SCs where beta approximate to 2 : 0 is usually found. Even though we took into account that some of the most massive objects might not be genuine SCs and applied different corrections for the mass loss, we found that these considerations do not influence much the outcome.

Druh

J_x - Nezařazeno - Článek v odborném periodiku (Jimp, Jsc a Jost)

CEP obor

BN - Astronomie a nebeská mechanika, astrofyzika

OECD FORD obor

—

Projekt

—

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2016

Kód důvěrnosti údajů

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

Název periodika

Astronomy and Astrophysics [online]

ISSN

1432-0746

e-ISSN

—

Svazek periodika

594

Číslo periodika v rámci svazku

říjen

Stát vydavatele periodika

PL - Polská republika

Počet stran výsledku

17

Strana od-do

—

Kód UT WoS článku

000385832200101

EID výsledku v databázi Scopus

2-s2.0-84992690587