The spatially resolved relation between dust, gas, and metal abundance with the TYPHOON survey

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A90106%2F24%3A00617503" target="_blank" >RIV/67985815:90106/24:00617503 - isvavai.cz</a>

Výsledek na webu

<a href="https://doi.org/10.1093/mnras/stae2298" target="_blank" >https://doi.org/10.1093/mnras/stae2298</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1093/mnras/stae2298" target="_blank" >10.1093/mnras/stae2298</a>

Jazyk výsledku

angličtina

Název v původním jazyce

The spatially resolved relation between dust, gas, and metal abundance with the TYPHOON survey

Popis výsledku v původním jazyce

We present the spatially resolved relationship between the dust-to-gas mass ratio (DGR) and gas-phase metallicity (Z(gas) or 12 + log(O/H)) (i.e. DGR-Z(gas) relation) of 11 nearby galaxies with a large-metallicity range (1.5 dex of 12 + log(O/H)) at (sub-)kpc scales. We used the large field-of-view (greater than or similar to 3 arcmin) optical pseudo-Integral Field Spectroscopy data taken by the TYPHOON/Progressive Integral Step Method survey, covering the optical size of galaxies, combining them with multiwavelength data [far-ultrviolet (UV) to far-infrared (IR), CO, and H i 21 cm radio]. A large scatter of DGR in the intermediate-metallicity galaxies (8.0 < 12 + log(O/H)< 8.3) is found, which is in line with dust evolution models, where grain growth begins to dominate the mechanism of dust mass accumulation. In the lowest metallicity galaxy of our sample, Sextans A (12 + log(O/H)< 7.6), the star-forming regions have significantly higher DGR values (by 0.5-2 dex) than the global estimates from literature at the same metallicity, but aligns with the DGR values from metal depletion method from damped Lyman alpha systems and high hydrogen gas density regions of Sextans A. Using dust evolution models with a Bayesian Monte Carlo Markov Chain approach suggests: (1) a high supernova dust yield and (2) a negligible amount of photofragmentation by UV radiation, although we note that our sample in the low-metallicity regime is limited to Sextans A. On the other hand, it is also possible that while metallicity influences DGR, gas density also plays a role, indicating an early onset of dust grain growth in the dust mass build-up process despite its low metallicity.

Název v anglickém jazyce

The spatially resolved relation between dust, gas, and metal abundance with the TYPHOON survey

Popis výsledku anglicky

We present the spatially resolved relationship between the dust-to-gas mass ratio (DGR) and gas-phase metallicity (Z(gas) or 12 + log(O/H)) (i.e. DGR-Z(gas) relation) of 11 nearby galaxies with a large-metallicity range (1.5 dex of 12 + log(O/H)) at (sub-)kpc scales. We used the large field-of-view (greater than or similar to 3 arcmin) optical pseudo-Integral Field Spectroscopy data taken by the TYPHOON/Progressive Integral Step Method survey, covering the optical size of galaxies, combining them with multiwavelength data [far-ultrviolet (UV) to far-infrared (IR), CO, and H i 21 cm radio]. A large scatter of DGR in the intermediate-metallicity galaxies (8.0 < 12 + log(O/H)< 8.3) is found, which is in line with dust evolution models, where grain growth begins to dominate the mechanism of dust mass accumulation. In the lowest metallicity galaxy of our sample, Sextans A (12 + log(O/H)< 7.6), the star-forming regions have significantly higher DGR values (by 0.5-2 dex) than the global estimates from literature at the same metallicity, but aligns with the DGR values from metal depletion method from damped Lyman alpha systems and high hydrogen gas density regions of Sextans A. Using dust evolution models with a Bayesian Monte Carlo Markov Chain approach suggests: (1) a high supernova dust yield and (2) a negligible amount of photofragmentation by UV radiation, although we note that our sample in the low-metallicity regime is limited to Sextans A. On the other hand, it is also possible that while metallicity influences DGR, gas density also plays a role, indicating an early onset of dust grain growth in the dust mass build-up process despite its low metallicity.

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

2024

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

535

Číslo periodika v rámci svazku

1

Stát vydavatele periodika

US - Spojené státy americké

Počet stran výsledku

24

Strana od-do

729-752

Kód UT WoS článku

001348151100001

EID výsledku v databázi Scopus

2-s2.0-85209379147