Optical emission-line Luminosity Function models for populations of Supernova Remnants

TL;DR

This paper develops a theoretical model for the luminosity functions of supernova remnants, matching observed distributions in nearby galaxies by combining evolution and shock excitation models.

Contribution

It introduces a new combined modeling approach for supernova remnant luminosity functions, integrating evolution and shock physics with different environmental parameters.

Findings

Model luminosity functions agree well with observations

Different pre-shock densities and magnetic parameters influence luminosity distributions

The approach provides a framework for understanding SNR populations in galaxies

Abstract

We present a basic model for the calculation of the luminosity distribution of supernova remnant populations. We construct theoretical Ha and joint [S II] - Ha luminosity functions for supernova remnants by combining prescriptions from a basic evolution model that provides the shock velocity and radius for SNRs of different age and pre-shock density, with shock excitation models that give the gas emissivity for shocks of different physical parameters. We assume a flat age distribution, and we explore the effect of different pre-shock density distributions or different magnetic parameters. We find very good agreement between the shape of the model Ha and the joint [S II] - Ha luminosity functions and those measured from SNR surveys in nearby galaxies.