The Wolf-Rayet features and mass-metallicity relation of long-duration gamma-ray burst host galaxies

TL;DR

This study analyzes optical spectra of 8 long-duration GRB host galaxies to detect Wolf-Rayet stars, estimate their properties, and compare their metallicity-luminosity relations with other galaxies, supporting the core-collapsar model.

Contribution

It provides the first detection of Wolf-Rayet stars in several GRB hosts and links their low metallicity environments to the core-collapsar model of GRB progenitors.

Findings

Wolf-Rayet stars detected in 5 out of 8 GRB hosts.

GRB hosts exhibit lower metallicity than similar luminosity galaxies.

High WR/O star ratios support the core-collapsar model.

Abstract

Aims. We have gathered optical spectra of 8 long-duration GRB host galaxies selected from the archival data of VLT/FORS2. We investigated whether or not Wolf-Rayet (WR) stars can be detected in these GRB host galaxies. We also tried to estimate the physical properties of GRB host galaxies, such as metallicity. Methods. We identified the WR features in these spectra by fitting the WR bumps and WR emission lines in blue and red bumps. We also identified the subtypes of the WR stars, and estimated the numbers of stars in each subtype, then calculated the WR/O star ratios. The (O/H) abundances of GRB hosts were estimated from both the electron temperature (Te) and the metallicity-sensitive strong-line ratio (R23), for which we have broken the R23 degeneracy. We compared the environments of long-duration GRB host galaxies with those of other galaxies in terms of their luminosity (stellar mass)-metallicity relations (LZ, MZ). Results. We detected the presence of WR stars in 5 GRB host galaxies having spectra with relatively high signal-to-noise ratios (S/N). In the comparison of LZ, MZ relations, it shows that GRB hosts have lower metallicities than other samples with comparable luminosity and stellar mass. The presence of WR stars and the observed high WR/O star ratio, together with low metallicity, support the core-collapsar model and implie the first stage of star formation in the hosted regions of GRBs.