BEDE: Bayesian estimates of dust evolution for nearby galaxies. Issue 3 (7th June 2021)

• Record Type: Journal Article
• Authors: De Vis, P; Maddox, S J; Gomez, H L; Jones, A P; Dunne, L
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 505:Issue 3(2021)
• Page Start: 3228
• Page End: 3246
• Publication Date: 2021-06-07
• Subjects: ISM: abundances -- ISM: dust, extinction -- IZM: evolution -- galaxies: evolution -- galaxies: fundamental parameters -- galaxies: ISM; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stab1604
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: We build a rigorous statistical framework to provide constraints on the chemical and dust evolution parameters for nearby late-type galaxies with a wide range of gas fractions ($3{{\ \rm per\ cent}}\lt f_g\lt 94{{\ \rm per\ cent}}$ ). A Bayesian Monte Carlo Markov Chain framework provides statistical constraints on the parameters used in chemical evolution models. Nearly a million one-zone chemical and dust evolution models were compared to 340 galaxies. Relative probabilities were calculated from the χ 2 between data and models, marginalized over the different time-steps, galaxy masses, and star formation histories. We applied this method to find 'best-fitting' model parameters related to metallicity, and subsequently fix these metal parameters to study the dust parameters. For the metal parameters, a degeneracy was found between the choice of initial mass function, supernova metal yield tables, and outflow prescription. For the dust parameters, the uncertainties on the best-fitting values are often large except for the fraction of metals available for grain growth, which is well constrained. We find a number of degeneracies between the dust parameters, limiting our ability to discriminate between chemical models using observations only. For example, we show that the low dust content of low-metallicity galaxies can be resolved by either reducing the supernova dust yields and/or including photofragmentation. We also show that supernova dust dominates the dust mass for low-metallicity galaxies and grain growth dominates for high-metallicity galaxies. The transition occurs around 12 + log (O/H) = 7.75, which is lower than found in most studies in the literature.