Using dust, gas and stellar mass selected samples to probe dust sources and sinks in low metallicity galaxies

De Vis, P., Gomez, Haley Louise ORCID: https://orcid.org/0000-0003-3398-0052, Schofield, Simon, Maddox, Steve ORCID: https://orcid.org/0000-0001-5549-195X, Dunne, Loretta ORCID: https://orcid.org/0000-0001-9880-2543, Baes, M., Cigan, Phillip, Clark, Christopher J. R., Gomez, Edward Leocadio ORCID: https://orcid.org/0000-0001-5749-1507, Lara-Lopez, M. and Owers, M. 2017. Using dust, gas and stellar mass selected samples to probe dust sources and sinks in low metallicity galaxies. Monthly Notices of the Royal Astronomical Society 471 (2) , pp. 1743-1765. 10.1093/mnras/stx981

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Abstract

We combine samples of nearby galaxies with Herschel photometry selected on their dust, metal, H I and stellar mass content, and compare these to chemical evolution models in order to discriminate between different dust sources. In a companion paper, we used an H I-selected sample of nearby galaxies to reveal a subsample of very gas-rich (gas fraction >80 per cent) sources with dust masses significantly below predictions from simple chemical evolution models, and well below Md/M* and Md/Mgas scaling relations seen in dust and stellar-selected samples of local galaxies. We use a chemical evolution model to explain these dust-poor, but gas-rich, sources as well as the observed star formation rates (SFRs) and dust-to-gas ratios. We find that (i) a delayed star formation history is required to model the observed SFRs; (ii) inflows and outflows are required to model the observed metallicities at low gas fractions; (iii) a reduced contribution of dust from supernovae (SNe) is needed to explain the dust-poor sources with high gas fractions. These dust-poor, low stellar mass galaxies require a typical core-collapse SN to produce 0.01-0.16 M⊙ of dust. To match the observed dust masses at lower gas fractions, significant grain growth is required to counteract the reduced contribution from dust in SNe and dust destruction from SN shocks. These findings are statistically robust, though due to intrinsic scatter it is not always possible to find one single model that successfully describes all the data. We also show that the dust-to-metal ratio decreases towards lower metallicity.

Item Type:	Article
Date Type:	Publication
Status:	Published
Schools:	Physics and Astronomy
Subjects:	Q Science > QB Astronomy
Uncontrolled Keywords:	galaxies: evolution, galaxies: ISM, galaxies: dwarf, galaxies: fundamental parameters, galaxies: star formation, ISM: dust
Publisher:	Wiley-Blackwell
ISSN:	0035-8711
Funders:	ERC, STFC
Date of First Compliant Deposit:	7 June 2017
Date of Acceptance:	5 May 2017
Last Modified:	11 Oct 2023 19:46
URI:	https://orca.cardiff.ac.uk/id/eprint/101295

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