The radial supernova remnant distribution in the Galaxy

TL;DR

This paper reevaluates the spatial distribution of supernova remnants in the Milky Way, proposing an exponential model that better fits observed data and aligns with star formation and metallicity patterns.

Contribution

It challenges previous assumptions by analyzing the SNR distribution and advocates for an exponential model based on observational data and bias considerations.

Findings

Exponential distribution best fits the SNR radial distribution.

Previous models often assumed zero SNRs at the Galactic Centre.

The new model aligns with star formation and metallicity distributions.

Abstract

Supernovae are the dominant source of chemical enrichment of galaxies, and they are an important source of energy to heat the interstellar medium and accelerate cosmic rays. Our knowledge of supernovae in the Milky Way is based mostly on the study of Galactic supernova remnants (SNRs), providing an (incomplete) record to supernova activity over the last ~100,000 yr. Here we report on an investigation of the spatial distribution of Galactic SNRs. Given the limited number of SNRs it is common to assume a functional form for the Galactocentric distribution of SNRs. However, several functional forms have been used in the past, without much justification for the radial distribution. For example, one often used functional form implies that no supernova activity is present in the Galactic Centre region. However, the presence of a magnetar and a SNR near the Galactic Centre suggest that a spatial distribution with zero SNRs at the Galactic Centre is not realistic. In light of these concerns we reevaluate the Galactic SNR distribution. We provide a brief outline of the main detection biases in finding SNRs and we investigate whether or not the use of the most common functional form is justified and how it compares to other models for the SNR distribution. We do this by analysing the longitudinal distribution of SNRs. We find that a simple exponential distribution is the most consistent and simplest model for describing the radial SNR distribution in the Galaxy and draw comparisons with the massive star formation and metallicity distributions.