TY - JOUR
T1 - The host of GRB 171205A in 3D
T2 - A resolved multiwavelength study of a rare grand-design spiral GRB host
AU - Thöne, C. C.
AU - de Ugarte Postigo, A.
AU - Izzo, L.
AU - Michalowski, M. J.
AU - Levan, A. J.
AU - Leung, J. K.
AU - Agüí Fernández, J. F.
AU - Géron, T.
AU - Friesen, R.
AU - Christensen, L.
AU - Covino, S.
AU - Da'Elia, V.
AU - Hartmann, D. H.
AU - Jakobsson, P.
AU - De Pasquale, M.
AU - Pugliese, G.
AU - Rossi, A.
AU - Schady, P.
AU - Wiersema, K.
AU - Zafar, T.
N1 - © The Authors 2024. Version archived for private and non-commercial use with the permission of the author/s and according to publisher conditions. For further rights please contact the publisher.
PY - 2024/10/1
Y1 - 2024/10/1
N2 - 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 21 cm data. The GRB is located in a small star-forming region in a spiral arm of the galaxy at a deprojected distance of ∼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% 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.
AB - 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 21 cm data. The GRB is located in a small star-forming region in a spiral arm of the galaxy at a deprojected distance of ∼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% 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.
KW - Galaxies: ISM
KW - Galaxies: kinematics and dynamics
KW - Galaxies: spiral
KW - Gamma-ray burst: individual: GRB 171205A
UR - http://www.scopus.com/inward/record.url?scp=85206493586&partnerID=8YFLogxK
U2 - 10.1051/0004-6361/202348141
DO - 10.1051/0004-6361/202348141
M3 - Article
AN - SCOPUS:85206493586
SN - 0004-6361
VL - 690
SP - 1
EP - 28
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
M1 - A66
ER -