[FeII] as a tracer supernova rate

TL;DR

This paper establishes a quantitative, linear relationship between [FeII] 1.26 micron luminosity and supernova rate in starburst galaxies, demonstrating [FeII] as an effective tracer for supernova activity.

Contribution

It introduces a new method to estimate supernova rates using [FeII] luminosity, validated through pixel-by-pixel analysis and comparison with radio data.

Findings

Strong linear correlation between [FeII] luminosity and supernova rate.

Agreement between [FeII]-based and radio-based supernova rates.

[FeII] can be used to estimate supernova activity on galactic scales.

Abstract

Supernovae play an integral role in the feedback of processed material into the ISMof galaxies and are responsible for most of the chemical enrichment of the universe. The rate of supernovae can also reveal the star formation histories. Supernova rate is usually measured through the non-thermal radio continuum luminosity, but in this paper we establish a quantitative relationship between the [FeII]1.26 luminosity and supernova rate in a sample of 11 near-by starburst galaxies. SINFONI data cubes are used to perform a pixel pixel analysis of this correlation. Using Br equivalent width and luminosity as the only observational inputs into Starburst 99, the supernova rate is derived at each pixel and a map of supernova rate is created. This is then compared morphologically and quantitatively to [FeII]1.26 luminosity map. We find a strong linear and morphological correlation between supernova rate and [FeII]1.26 on a pixel-pixel basis: log SNrate yr-1 pc-2 = (1.01 \pm 0.2) \ast log[FeII]1.26 ergs-1 pc-2 - 41.17 \pm 0.9 The Starburst 99 derived supernova rates are also in good agreement with the radio derived supernova rates, which further demonstrates the strength of [FeII] as a tracer of supernova rate. With the strong correlation found in this sample of galaxies, we now qualitatively use [FeII]1.26 to derive supernova rate on either a pixel-pixel or integrated galactic basis.