JINGLE – IV. Dust, H i gas, and metal scaling laws in the local Universe

Abstract

<jats:title>ABSTRACT</jats:title> <jats:p>Scaling laws of dust, H i gas, and metal mass with stellar mass, specific star formation rate, and metallicity are crucial to our understanding of the build-up of galaxies through their enrichment with metals and dust. In this work, we analyse how the dust and metal content varies with specific gas mass (MH i/M⋆) across a diverse sample of 423 nearby galaxies. The observed trends are interpreted with a set of Dust and Element evolUtion modelS (DEUS) – including stellar dust production, grain growth, and dust destruction – within a Bayesian framework to enable a rigorous search of the multidimensional parameter space. We find that these scaling laws for galaxies with −1.0 ≲ log MH i/M⋆ ≲ 0 can be reproduced using closed-box models with high fractions (37–89 ${{\ \rm per\ cent}}$) of supernova dust surviving a reverse shock, relatively low grain growth efficiencies (ϵ = 30–40), and long dust lifetimes (1–2 Gyr). The models have present-day dust masses with similar contributions from stellar sources (50–80 ${{\ \rm per\ cent}}$) and grain growth (20–50 ${{\ \rm per\ cent}}$). Over the entire lifetime of these galaxies, the contribution from stardust (&amp;gt;90 ${{\ \rm per\ cent}}$) outweighs the fraction of dust grown in the interstellar medium (&amp;lt;10 ${{\ \rm per\ cent}}$). Our results provide an alternative for the chemical evolution models that require extremely low supernova dust production efficiencies and short grain growth time-scales to reproduce local scaling laws, and could help solving the conundrum on whether or not grains can grow efficiently in the interstellar medium.</jats:p>

The impact of metallicity-dependent dust destruction on the dust-to-metals ratio in galaxies

“…which gives 1 M yr −1 for a gas mass of 5 × 10 9 M , in line with Milky Way values (Dame 1993;Robitaille & Whitney 2010), and produces an exponentially-declining SFR. The galaxy scaling relations we are interested in are typically more sensitive to the assumptions made regarding the dust physics, rather than the star formation history (De Vis et al 2017;De Looze et al 2020).…”

The mm-to-cm SED of spiral galaxies

“…Using a dust model and fitting tools such as, e.g., CIGALE [2] and HerBIE [3], a wealth of information can be extracted from the SED: star-formation rates (SFRs), stellar and dust masses, gas-to-dust ratios, etc. ( [4][5][6][7], just to mention a few recents works). Figure 1 shows an example of the current SED knowledge: it uses data from DustPedia [8], a database collecting photometry and imagery for all the large (D 25 > 1 0 ) and nearby (d < 30 Mpc) galaxies observed by Herschel; and mid radio continuum flux densities from [9].…”

The impact of metallicity-dependent dust destruction on the dust-to-metals ratio in galaxies

“…which gives 1 M yr −1 for a gas mass of 5 × 10 9 M , in line with Milky Way values (Dame 1993;Robitaille & Whitney 2010), and produces an exponentially-declining SFR. The galaxy scaling relations we are interested in are typically more sensitive to the assumptions made regarding the dust physics, rather than the star formation history (De Vis et al 2017;De Looze et al 2020).…”