Metallicity estimation of core-collapse Supernova H iiregions in galaxies within 30 Mpc

Abstract

This work presents measurements of the local H ii environment metallicities of core-collapse supernovae (SNe) within a luminosity distance of 30 Mpc. 76 targets were observed at the Isaac Newton Telescope and environment metallicities could be measured for 65 targets using the N2 and O3N2 strong emission line method. The cumulative distribution functions (CDFs) of the environment metallicities of Type Ib and Ic SNe tend to higher metallicity than Type IIP, however Type Ic are also present at lower metallicities whereas Type Ib are not. The Type Ib frequency distribution is narrower (standard deviation ∼0.06 dex) than the Ic and IIP distributions (∼0.15 dex) giving some evidence for a significant fraction of single massive progenitor stars; the low metallicity of Type Ic suggests a significant fraction of compact binary progenitors. However, both the Kolmogorov-Smirnov test and the Anderson-Darling test indicate no statistical significance for a difference in the local metallicities of the three SN types. Monte Carlo simulations reveal a strong sensitivity of these tests to the uncertainties of the derived metallicities. Given the uncertainties of the strong emission methods, the applicability of the tests seems limited. We extended our analysis with the data of the Type Ib/Ic/IIP SN sample from Galbany et al. (2018). The CDFs created with their sample confirm our CDFs very well. The statistical tests, combining our sample and the Galbany et al. (2018) sample, indicate a significant difference between Type Ib and Type IIP with <5 per cent probability that they are drawn from the same parent population.

Detection of Metal Enrichment by SN 2011jm in NGC 4809

“…This method, however, is applicable mainly in H II regions with high temperatures and minimal cooling in metal-poor galaxies, a condition not uniformly met. As the MUSE spectral wavelength does not cover the [O II]λ3727 and [O III]λ4363 lines, we employed the strong-line calibrator, O3N2, to ascertain the oxygen abundance following the calculation in Xiao et al (2019) and Ganss et al (2022).…”

“…These explosive events eject heavy elements created during core nuclear burning (e.g., Hoyle & Fowler 1960;Nomoto et al 2006;Johnson 2019), leading to the chemical enrichment of the interstellar medium (ISM; e.g., Timmes et al 1995;Roy et al 2022) and potentially influencing the formation of new stars (e.g., Thornton et al 1998). CCSNe play a crucial role in the formation and distribution of chemical elements during the evolution of galaxies (e.g., Scannapieco et al 2008;Kuncarayakti et al 2013;Niino et al 2015;Kuncarayakti et al 2018;Xiao et al 2019;Ganss et al 2022;Sarbadhicary et al 2022;Kourniotis et al 2023;Molero et al 2023).…”