In pursuit of giants I. The evolution of the dust-to-stellar mass ratio in distant dusty galaxies

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F20%3A00553332" target="_blank" >RIV/67985815:_____/20:00553332 - isvavai.cz</a>

Výsledek na webu

<a href="https://doi.org/10.1051/0004-6361/202038405" target="_blank" >https://doi.org/10.1051/0004-6361/202038405</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/202038405" target="_blank" >10.1051/0004-6361/202038405</a>

Jazyk výsledku

angličtina

Název v původním jazyce

In pursuit of giants I. The evolution of the dust-to-stellar mass ratio in distant dusty galaxies

Popis výsledku v původním jazyce

In this work, we explore trends of M-dust/M-star with different physical parameters and using observations of 300 massive dusty star-forming galaxies detected with ALMA up to z approximate to 5. Additionally, we interpret our findings with different models of dusty galaxy formation. We find that M-dust/M-star evolves with redshift, stellar mass, specific star formation rates, and integrated dust size, but that evolution is different for main-sequence galaxies than it is for starburst galaxies. In both galaxy populations, M-dust/M-star increases until z similar to 2, followed by a roughly flat trend towards higher redshifts, suggesting efficient dust growth in the distant universe. We confirm that the inverse relation between M-dust/M-star and M-star holds up to z approximate to 5 and can be interpreted as an evolutionary transition from early to late starburst phases. We demonstrate that the M-dust/M-star in starbursts reflects the increase in molecular gas fraction with redshift and attains the highest values for sources with the most compact dusty star formation. State-of-the-art cosmological simulations that include self-consistent dust growth have the capacity to broadly reproduce the evolution of M-dust/M-star in main-sequence galaxies, but underestimating it in starbursts. The latter is found to be linked to lower gas-phase metallicities and longer dust-growth timescales relative to observations. The results of phenomenological models based on the main-sequence and starburst dichotomy as well as analytical models that include recipes for rapid metal enrichment are consistent with our observations. Therefore, our results strongly suggest that high M-dust/M-star is due to rapid dust grain growth in the metal-enriched interstellar medium. This work highlights the multi-fold benefits of using M-dust/M-star as a diagnostic tool for: (1) disentangling main-sequence and starburst galaxies up to z similar to 5, (2) probing the evolutionary phase of massive objects and (3) refining the treatment of the dust life cycle in simulations.

Název v anglickém jazyce

In pursuit of giants I. The evolution of the dust-to-stellar mass ratio in distant dusty galaxies

Popis výsledku anglicky

In this work, we explore trends of M-dust/M-star with different physical parameters and using observations of 300 massive dusty star-forming galaxies detected with ALMA up to z approximate to 5. Additionally, we interpret our findings with different models of dusty galaxy formation. We find that M-dust/M-star evolves with redshift, stellar mass, specific star formation rates, and integrated dust size, but that evolution is different for main-sequence galaxies than it is for starburst galaxies. In both galaxy populations, M-dust/M-star increases until z similar to 2, followed by a roughly flat trend towards higher redshifts, suggesting efficient dust growth in the distant universe. We confirm that the inverse relation between M-dust/M-star and M-star holds up to z approximate to 5 and can be interpreted as an evolutionary transition from early to late starburst phases. We demonstrate that the M-dust/M-star in starbursts reflects the increase in molecular gas fraction with redshift and attains the highest values for sources with the most compact dusty star formation. State-of-the-art cosmological simulations that include self-consistent dust growth have the capacity to broadly reproduce the evolution of M-dust/M-star in main-sequence galaxies, but underestimating it in starbursts. The latter is found to be linked to lower gas-phase metallicities and longer dust-growth timescales relative to observations. The results of phenomenological models based on the main-sequence and starburst dichotomy as well as analytical models that include recipes for rapid metal enrichment are consistent with our observations. Therefore, our results strongly suggest that high M-dust/M-star is due to rapid dust grain growth in the metal-enriched interstellar medium. This work highlights the multi-fold benefits of using M-dust/M-star as a diagnostic tool for: (1) disentangling main-sequence and starburst galaxies up to z similar to 5, (2) probing the evolutionary phase of massive objects and (3) refining the treatment of the dust life cycle in simulations.

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

2020

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

644

Číslo periodika v rámci svazku

December

Stát vydavatele periodika

FR - Francouzská republika

Počet stran výsledku

25

Strana od-do

A144

Kód UT WoS článku

000599931300001

EID výsledku v databázi Scopus

2-s2.0-85097912059