2025/11/11 by Guy Worthey, Worthey, Guy, Tathagata Pal +1
Engineering · Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics of Galaxies (astro-ph.GA) #FOS: Physical sciences #Galaxies: Formation, Evolution, Phenomena #Solar and Stellar Astrophysics (astro-ph.SR) #Space Technology and Applications
paper · pdf · doi:10.48550/arxiv.2511.08827
openalex publication_date 2025/11/11 · openalex created_date 2025/11/14 · openalex updated_date 2026/07/28
Recent analysis of 2968 MaNGA early type galaxies has yielded two notable trends with velocity dispersion (σ) not previously discussed in the literature. First, Fe abundance rises with σ, but only until σ≈100 km s-1, after which it falls. This kink is reproduced by TNG100 simulations, implying that hierarchical merger processes might explain it. Second, astrophysical scatter in N is high for galaxies with σ< 100 km s-1. Due to the restricted list of nucleosynthetic sources for N, it is likely that asymptotic giant branch stars provide most of this N. A varied star formation history (compared to that of massive galaxies) along with variable retention and recycling of N-enriched gas might explain the fuzz of N abundance in low-σ galaxies. Because a timescale argument seems necessary to explain the nitrogen fuzz, and an initial mass function argument is ruled out, similar timescale arguments for the [Mg/Fe] trend as a function of velocity dispersion are supported.