The host of GRB 171205A in 3D

Abstract

Long GRB hosts at $z<1$ are usually low-mass, low-metallicity star-forming galaxies. Here we present the most detailed, spatially resolved study of the host of GRB 171205A so far, a grand-design barred spiral galaxy at $z=0.036$. Our analysis includes MUSE integral field spectroscopy complemented with high-spatial-resolution UV/VIS HST imaging and CO(1--0) and H i 21cm data. The GRB is located in a small star-forming region in a spiral arm of the galaxy at a deprojected distance of sim 8\,kpc from the center. The galaxy shows a smooth negative metallicity gradient and the metallicity at the GRB site is half solar, slightly below the mean metallicity at the corresponding distance from the center. Star formation in this galaxy is concentrated in a few H ii regions between 5 and 7\,kpc from the center and at the end of the bar, inwards from the GRB region; however the H ii region hosting the GRB is in the top 10<!PCT!> of the regions with the highest specific star-formation rate. The stellar population at the GRB site has a very young component ($<$ 5\,Myr) that contributes a significant part of the light. Ionized and molecular gas show only minor deviations at the end of the bar. A parallel study found an asymmetric H i distribution and some additional gas near the position of the GRB, which might explain the star-forming region of the GRB site. Our study shows that long GRBs can occur in many types of star-forming galaxies; however the actual GRB sites have consistently low metallicity, high star formation rates, and a young population. Furthermore, gas inflow or interactions triggering the star formation producing the GRB progenitor might not be evident in ionized or even molecular gas but only in H i