The role of stellar mass in the cosmic history of star formation as seen by Herschel and ALMA

Result code in IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A90106%2F24%3A00617606" target="_blank" >RIV/67985815:90106/24:00617606 - isvavai.cz</a>

Result on the web

<a href="https://doi.org/10.1051/0004-6361/202348341" target="_blank" >https://doi.org/10.1051/0004-6361/202348341</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/202348341" target="_blank" >10.1051/0004-6361/202348341</a>

Result language

angličtina

Original language name

The role of stellar mass in the cosmic history of star formation as seen by Herschel and ALMA

Original language description

Aims. We explore the contribution of galaxies, as a function of their stellar mass, to the cosmic star formation history (CSFH). In order to avoid uncertain extrapolations of the infrared luminosity function, which is often polluted by the contribution of starbursts, we base our analysis on stellar mass. Attenuation by dust is accounted for thanks to the combination of deep surveys by Herschel and the Atacama Large Millimeter/submillimeter array (ALMA). Methods. We combined for the first time the deepest Herschel (GOODS-South, GOODS-North, COSMOS and UDS) and ALMA (GOODS-South) surveys. We constrained the star formation rate (SFR), dust mass (M-dust), dust temperature (T-dust) and gas mass (M-gas) of galaxies as a function of their stellar mass (M-star) from z similar to 5 to z similar to 0 by performing a stacking analysis of over 128 000 Hubble Space Telescope (HST) H-band selected galaxies. We studied the evolution of the star formation efficiency of galaxies as a function of redshift and M-star. Results. We show that the addition of ALMA to Herschel allows us to reach lower M-star and higher redshifts. We confirm that the SFR-M-star star formation main sequence (MS) follows a linear evolution with a slope close to unity with a bending at the high-mass end at z < 2. The mean T-dust of MS galaxies evolves linearly with redshift, with no apparent correlation with M-star. We show that, up to z similar to 5, massive galaxies (i.e. M-star >= 10(10) M-circle dot) account for most of the total SFR density (rho(SFR)), while the contribution of lower-mass galaxies (i.e. M-star <= 10(10) M-circle dot) is rather constant. We compare the evolution of star-forming galaxy (SFGs) to the cosmological simulation TNG100. We find that TNG100 exhibits a noticeable difference in the evolution of the CSFH, that is, the marked evolution of massive galaxies found in the observations appears to be smoothed in the simulation, possibly due to feedback that is too efficient. In this mass complete analysis, H-dropout (also called HST-dark) galaxies account for similar to 23% of the CSFH in massive galaxies at z > 3. Finally, we find hints that the star formation efficiency of distant galaxies (z = 3-5) is stronger (shorter depletion time) as compared to low-redshift galaxies.

Czech name

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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

—

Continuities

—

Publication year

2024

Confidentiality

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

Name of the periodical

Astronomy & Astrophysics

ISSN

0004-6361

e-ISSN

1432-0746

Volume of the periodical

691

Issue of the periodical within the volume

Nov.

Country of publishing house

FR - FRANCE

Number of pages

25

Pages from-to

A248

UT code for WoS article

001358034000007

EID of the result in the Scopus database

2-s2.0-85210520854