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

ABSTRACT We present the spatially resolved relationship between the dust-to-gas mass ratio (DGR) and gas-phase metallicity ($Z_{\rm gas}$ or 12 + log(O/H)) (i.e. DGR–$Z_{\rm gas}$ 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 ($\gtrsim$ 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 $\lt $ 12 + log(O/H)$\lt $ 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)$\lt $ 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.

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Journal
Monthly Notices of the Royal Astronomical Society
Published
2024-10-07
DOI
https://doi.org/10.1093/mnras/stae2298
Citations
3
Primary Topic
Geochemistry and Geologic Mapping
Type
article
Field-Weighted Citation Impact
1.04

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article

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

N. M. McClure‐Griffiths, Mark Seibert, Barry F. Madore, Qianhui Chen et al.
3 citations
Monthly Notices of the Royal Astronomical Society
Geochemistry and Geologic Mapping
1.04
article

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

N. M. McClure‐Griffiths, Mark Seibert, Barry F. Madore, Qianhui Chen, L. Cortese, Lisa J. Kewley, Marcie Mun, Kathryn Grasha, Brent A Groves, W. J. G. de Blok, Rachael L. Beaton, J. Rich, Andrew Battisti, Emily Wisnioski, Hye-Jin Park
article en
3 citations

Abstract

ABSTRACT We present the spatially resolved relationship between the dust-to-gas mass ratio (DGR) and gas-phase metallicity ($Z_{\rm gas}$ or 12 + log(O/H)) (i.e. DGR–$Z_{\rm gas}$ 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 ($\gtrsim$ 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 $\lt $ 12 + log(O/H)$\lt $ 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)$\lt $ 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.

Monthly Notices of the Royal Astronomical SocietyVol. 535(1)
Australian National University (AU), University of Cape Town (ZA), University of Groningen (NL), The University of Western Australia (AU), Carnegie Institution for Science (US), Princeton University (US), University of Chicago (US), ASTRO-3D (AU), AstroTec Holding (Netherlands) (NL), Center for Astrophysics Harvard & Smithsonian (US), Carnegie Observatories (US), Astronomical Institute of the Slovak Academy of Sciences (SK), ARC Centre of Excellence for All-sky Astrophysics (AU), International Centre for Radio Astronomy Research (AU), Netherlands Institute for Radio Astronomy (NL)
National Science Foundation, National Aeronautics and Space Administration, California Institute of Technology, Australian Government, European Space Agency, Australian Research Council
Openalex Percentile: Top 19%
Geochemistry and Geologic Mapping
1.04
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