# Outflows from GRB hosts are ubiquitous: Kinematics of z<0.3 GRB-SN hosts resolved with FLAMES

## TL;DR

This study uses high-resolution 3D spectroscopy to analyze the gas kinematics and outflows in six low-redshift GRB host galaxies, revealing diverse dynamics and metal-rich outflows linked to star formation.

## Contribution

It provides the first detailed resolved gas kinematic analysis of a sample of low-redshift GRB hosts, highlighting the prevalence of outflows and complex dynamics.

## Key findings

- Most galaxies show non-regular kinematics, including rotation, dispersion, or merger signatures.
- All galaxies exhibit broad, metal-rich outflow components associated with star-forming regions.
- GRBs are located in star-forming regions with wind signatures, not necessarily the brightest areas.

## Abstract

The hosts of long duration gamma-ray bursts are predominantly starburst galaxies at subsolar metallicity. At redshifts z<1, this implies that most of them are low-mass galaxies similar to the populations of blue compact dwarfs and dwarf irregulars. What triggers the massive star-formation (SF) needed for producing a GRB progenitor is still largely unknown, as are the resolved gas properties and kinematics of these galaxies and their formation history. Here we present a sample of six spatially resolved GRB hosts at z<0.3 observed with 3D spectroscopy at high spectral resolution (R=8,000-13,000) using FLAMES/VLT. We analyzed the resolved gas kinematics of the full sample and the abundances in a subsample. Only two galaxies show a regular disk-like rotation field, another two are dispersion-dominated, the remaining two have a double emission component associated with different parts of the galaxy, which might indicate a recent merger. All galaxies show evidence for broad components underlying the main emission peak (sigma = 50-110 km/s). This broad component is more metal-rich than the narrow components, it is blueshifted in most cases, and it follows a different velocity structure. We find a weak correlation between the SF rate and the width of the broad component, its flux compared to the narrow component, and the maximum outflow velocity of the gas, but we do not find any correlation with the SF density, metallicity or stellar mass. We associate this broad component with a metal-rich outflow from star-forming regions. The GRB is not located in the brightest region of the host, but is always associated with some star-forming region showing a clear wind component. Our study shows the potential of 3D spectroscopy to study the SF processes in galaxies hosting extreme transients, the need for high S/N, and the perils using unresolved or only partially resolved data for these kinds of studies.