A3 COSMOS: The dust content of massive quiescent galaxies and its evolution with cosmic time

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A90106%2F25%3A00646369" target="_blank" >RIV/67985815:90106/25:00646369 - isvavai.cz</a>

Výsledek na webu

<a href="https://doi.org/10.1051/0004-6361/202554400" target="_blank" >https://doi.org/10.1051/0004-6361/202554400</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/202554400" target="_blank" >10.1051/0004-6361/202554400</a>

Jazyk výsledku

angličtina

Název v původním jazyce

A3 COSMOS: The dust content of massive quiescent galaxies and its evolution with cosmic time

Popis výsledku v původním jazyce

Aims. We study the dust content of massive (log(M-*/M-circle dot)>= 10.8) quiescent galaxies (QGs) at redshifts z = 0.5 3 to place constraints on the evolution of their cold interstellar medium (ISM) and thereby obtain insights into the processes of galaxy quenching throughout cosmic time. Methods. We used a robust sample of 458 colour-selected QGs covered by the A(3)COSMOS+A(3)GOODSS database to perform a stacking analysis in the uv domain and measured their mean dust masses from their stacked sub-millimetre luminosities. We used the CIGALE spectral energy distribution fitting code to obtain star formation histories and infer the time since quenching for all the QGs in our sample. We used this information to gain insight into the time evolution of the dust content after quenching. Results. Most QGs in our sample quenched around a redshift of z similar to 1.3, following the peak of cosmic star formation. The majority of QGs observed at z > 1 are recently quenched (i.e. quenched for no longer than 500 Myr), whereas the majority of QGs observed at z < 1 have already been quenched for a significant amount of time (greater than or similar to 1 Gyr). This implies that high-redshift galaxies (z greater than or similar to 2) are ideal for studying the mechanisms of quenching and its effects on the ISM, while lower-redshift galaxies are more suitable for studying the long-term effects of the QG environment on their ISM. We obtain upper limits on the dust mass fraction of the QG population that indicate a lower dust content in high-redshift massive QGs than what was found by earlier stacking studies, and significantly lower (by a factor of similar to 2-6) than that of normal star-forming galaxies. We also place constraints on the initial gas fraction right after quenching. We find that within the first similar to 600 Myr after quenching, QGs already lose on average greater than or similar to 70% of their cold ISM. Our findings support a gas consumption or removal scenario acting on short timescales.

Název v anglickém jazyce

A3 COSMOS: The dust content of massive quiescent galaxies and its evolution with cosmic time

Popis výsledku anglicky

Aims. We study the dust content of massive (log(M-*/M-circle dot)>= 10.8) quiescent galaxies (QGs) at redshifts z = 0.5 3 to place constraints on the evolution of their cold interstellar medium (ISM) and thereby obtain insights into the processes of galaxy quenching throughout cosmic time. Methods. We used a robust sample of 458 colour-selected QGs covered by the A(3)COSMOS+A(3)GOODSS database to perform a stacking analysis in the uv domain and measured their mean dust masses from their stacked sub-millimetre luminosities. We used the CIGALE spectral energy distribution fitting code to obtain star formation histories and infer the time since quenching for all the QGs in our sample. We used this information to gain insight into the time evolution of the dust content after quenching. Results. Most QGs in our sample quenched around a redshift of z similar to 1.3, following the peak of cosmic star formation. The majority of QGs observed at z > 1 are recently quenched (i.e. quenched for no longer than 500 Myr), whereas the majority of QGs observed at z < 1 have already been quenched for a significant amount of time (greater than or similar to 1 Gyr). This implies that high-redshift galaxies (z greater than or similar to 2) are ideal for studying the mechanisms of quenching and its effects on the ISM, while lower-redshift galaxies are more suitable for studying the long-term effects of the QG environment on their ISM. We obtain upper limits on the dust mass fraction of the QG population that indicate a lower dust content in high-redshift massive QGs than what was found by earlier stacking studies, and significantly lower (by a factor of similar to 2-6) than that of normal star-forming galaxies. We also place constraints on the initial gas fraction right after quenching. We find that within the first similar to 600 Myr after quenching, QGs already lose on average greater than or similar to 70% of their cold ISM. Our findings support a gas consumption or removal scenario acting on short timescales.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

—

Návaznosti

—

Rok uplatnění

2025

Kód důvěrnosti údajů

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

Název periodika

Astronomy & Astrophysics

ISSN

0004-6361

e-ISSN

1432-0746

Svazek periodika

702

Číslo periodika v rámci svazku

Oct.

Stát vydavatele periodika

FR - Francouzská republika

Počet stran výsledku

15

Strana od-do

A186

Kód UT WoS článku

001597841900011

EID výsledku v databázi Scopus

2-s2.0-105020012422