2015/06/25 by Lin Xiao, J. J. Eldridge · 25 citations
Physics and Astronomy · #Astronomy #Astrophysics #Astrophysics and Cosmic Phenomena #Galaxies: Formation, Evolution, Phenomena #Galaxy #Gamma-ray bursts and supernovae #Physics #Population #Star formation #Stars #Stellar population #Supernova #Type II supernova #astro-ph.GA
paper · pdf · doi:10.1093/mnras/stv1425
published in Monthly Notices of the Royal Astronomical Society 452(3), 2597-2605 (Oxford University Press) · 11 pages, 5 figures, 6 tables. Accepted by MNRAS
arxiv created 2015/06/25 · openalex publication_date 2015/07/30 · arxiv updated 2015/08/06 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
The 11 Mpc Hα and Ultraviolet Galaxy Survey (11HUGS) traces the star formation activity of nearby galaxies. In addition, within this volume the detection completeness of core-collapse supernovae (CCSNe) is high therefore by comparing these observed stellar births and deaths we can make a sensitive test of our understanding of how stars live and die. In this paper, we use the results of the Binary Population and Spectral Synthesis (bpass) code to simulate the 11HUGS galaxies’ Hα and far-ultraviolet (FUV) star formation rate indicators (SFRIs) and simultaneously match the CCSN rate. We find that stellar population including interacting binary stars makes little difference to the total CCSN rate but increases the Hα and FUV fluxes for a constant number of stars being formed. In addition, they significantly increase the predicted rate of Type Ibc SNe relative to Type II SNe to the level observed in the 11HUGS galaxies. We also find that instead of assuming a constant star formation history for the galaxies our best-fitting models have an SFR that peaked more than 3 Myr ago.