Cosmic evolution of grain size distribution in galaxies using the ν2GC semi-analytical model

Abstract

We investigate the cosmological evolution of interstellar dust with a semi-analytical galaxy formation model (ν2GC), focusing on the evolution of grain size distribution. The model predicts the statistical properties of dust mass and grain size distribution in galaxies across cosmic history. We confirm that the model reproduces the relation between dust-to-gas ratio and metallicity in the local Universe, and that the grain size distributions of the Milky Way (MW)-like sample become similar to the so-called MRN distribution that reproduces the observed MW extinction curve. Our model, however, tends to overpredict the dust mass function at the massive end at redshift z ≲ 0.8 while it reproduces the abundance of dusty galaxies at higher redshifts. We also examine the correlation between grain size distribution and galaxy properties (metallicity, specific star formation rate, gas fraction, and stellar mass), and observe a clear trend of large-grain-dominated, small-grain-dominated, and MRN-like grain size distributions from unevolved to evolved stages. As a consequence, the extinction curve shapes are flat, steep, and intermediate (MW-like) from the unevolved to evolved phases. At a fixed metallicity, the grain size distribution tends to have larger fractions of small grains at lower redshift; accordingly, the extinction curve tends to be steeper at lower redshift. We also predict that supersolar-metallicity objects at high redshift have flat extinction curves with weak 2175 Å bump strength.

Dust attenuation evolution in z ∼ 2 − 12 JWST galaxies

“…Scenario (3) invokes changes in the grain properties. First, we note that our results are consistent with predictions from theoretical studies [60][61][62] that have investigated the cosmological evolution of interstellar dust. A recent study 62 finds that, at a fixed metallicity, extinction curves flatten and the UV bump becomes less prominent with redshift.…”

“…First, we note that our results are consistent with predictions from theoretical studies [60][61][62] that have investigated the cosmological evolution of interstellar dust. A recent study 62 finds that, at a fixed metallicity, extinction curves flatten and the UV bump becomes less prominent with redshift. The study concluded that such trends are driven by a shift in the grain size distribution, favouring larger grains at early epochs.…”

“…These dust sources are predicted to predominantly form large (≈ 0.1µm) grains 8,60,63 . Grains are then released into the ISM where they undergo shattering processes [60][61][62]64 breaking them into smaller units. However, shattering is a rather slow process, with typical timescales of ≳ 0.5 − 1 Gyr 8,60 .…”

“…At z ≲ 5 − 5.5, a larger variety of attenuation curves is observed. This is likely due to a combination of several effects, including the transition from SNII to asymptotic giant branch (AGB) stars 67,68 as the dominant dust sources, dust growth in the ISM 8,69 , more efficient shattering and sputtering [60][61][62]64 . Concurrently, the UV bump emerges at z ≲ 5 (around ∼ 1.2 Gyr), marking the epoch when dust formation in AGB stars becomes dominant, leading to enhanced production of carbonaceous grains.…”

Cosmic Sands: The Origin of Dusty, Star-forming Galaxies in the Epoch of Reionization

“…Constraints on the optical properties of dust at high redshift are not widely available; thus, we elect to use a fixed dust extinction curve that matches the average Milky Way curve. However, recent numerical studies including an evolving dust grain size distribution in Li et al (2020; see also Makiya & Hirashita 2022) have shown that galaxies can initially exhibit steep dust extinction curves that then evolve toward shallower UV-optical slopes as the grain size distribution evolves to match the Mathis, Rumpl & Nordsieck (MRN) distribution (Mathis et al 1977).…”