2020/11/30 by Robert M. Yates, Bruno M. B. Henriques, Bruno Henriques +8 · 59 citations
Physics and Astronomy · #Accretion (finance) #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Galaxies: Formation, Evolution, Phenomena #Galaxy #Galaxy formation and evolution #Gamma-ray bursts and supernovae #Metallicity #Physics #Star formation #Stars #Stellar mass #Supernova #astro-ph.CO #astro-ph.GA
paper · pdf · doi:10.1093/mnras/stab741
published in Monthly Notices of the Royal Astronomical Society 503(3), 4474-4495 (Oxford University Press) · 22 pages, 19 figures. Accepted by MNRAS. (Missing citation hyperlinks corrected)
openalex created_date 2020/11/23 · openalex publication_date 2021/03/10 · arxiv created 2021/06/03 · arxiv updated 2021/06/04 · openalex updated_date 2026/08/05
ABSTRACT We present a modified version of the L-galaxies2020 semi-analytic model of galaxy evolution, which includes significantly increased direct metal enrichment of the circumgalactic medium (CGM) by supernovae (SNe). These more metal-rich outflows do not require increased mass-loading factors, in contrast to some other galaxy evolution models. This modified L-galaxies2020 model is able to simultaneously reproduce the gas-phase metallicity (Z_\rm g) and stellar metallicity (Z*) radial profiles observed in nearby disc galaxies by MaNGA and MUSE, as well as the observed mass – metallicity relations for gas and stars at z = 0 and their evolution back to z ∼ 2−3. A direct CGM enrichment fraction of ∼90 per cent for SNe-II is preferred. We find that massive disc galaxies have slightly flatter Z_\rm g profiles than their lower-mass counterparts in L-galaxies2020, due to more efficient enrichment of their outskirts via inside-out growth and metal-rich accretion. Such a weak, positive correlation between stellar mass and Z_\rm g profile slope is also seen in our MaNGA-DR15 sample of 571 star-forming disc galaxies, although below log10(M*/M⊙) ∼ 10.0 this observational result is strongly dependent on the metallicity diagnostic and morphological selection chosen. In addition, a lowered maximum SN-II progenitor mass of 25 \rm M\odot , reflecting recent theoretical and observational estimates, can also provide a good match to observed Z_\rm g and Z* profiles at z = 0 in L-galaxies2020. However, this model version fails to reproduce an evolution in Z_\rm g at fixed mass over cosmic time, or the magnesium abundances observed in the intracluster medium (ICM).