GRB171010A / SN2017htp: a GRB-SN at z=0.33. (arXiv:1910.14160v1 [astro-ph.HE])

GRB171010A / SN2017htp: a GRB-SN at z=0.33. (arXiv:1910.14160v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Melandri_A/0/1/0/all/0/1">A. Melandri</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Malesani_D/0/1/0/all/0/1">D. B. Malesani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Izzo_L/0/1/0/all/0/1">L. Izzo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Japelj_J/0/1/0/all/0/1">J. Japelj</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vergani_S/0/1/0/all/0/1">S.D. Vergani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schady_P/0/1/0/all/0/1">P. Schady</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carracedo_A/0/1/0/all/0/1">A. Sagues Carracedo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Postigo_A/0/1/0/all/0/1">A. de Ugarte Postigo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Anderson_J/0/1/0/all/0/1">J.P. Anderson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barbarino_C/0/1/0/all/0/1">C. Barbarino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bolmer_J/0/1/0/all/0/1">J. Bolmer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Breeveld_A/0/1/0/all/0/1">A. Breeveld</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Calissendorff_P/0/1/0/all/0/1">P. Calissendorff</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Campana_S/0/1/0/all/0/1">S. Campana</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cano_Z/0/1/0/all/0/1">Z. Cano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carini_R/0/1/0/all/0/1">R. Carini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Covino_S/0/1/0/all/0/1">S. Covino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+DAvanzo_P/0/1/0/all/0/1">P. D'Avanzo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+DElia_V/0/1/0/all/0/1">V. D'Elia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Valle_M/0/1/0/all/0/1">M. della Valle</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pasquale_M/0/1/0/all/0/1">M. De Pasquale</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fynbo_J/0/1/0/all/0/1">J.P.U. Fynbo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gromadzki_M/0/1/0/all/0/1">M. Gromadzki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hammer_F/0/1/0/all/0/1">F. Hammer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hartmann_D/0/1/0/all/0/1">D.H. Hartmann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Heintz_K/0/1/0/all/0/1">K.E. Heintz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Inserra_C/0/1/0/all/0/1">C. Inserra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jakobsson_P/0/1/0/all/0/1">P. Jakobsson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kann_D/0/1/0/all/0/1">D.A. Kann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kotilainen_J/0/1/0/all/0/1">J. Kotilainen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Maguire_K/0/1/0/all/0/1">K. Maguire</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Masetti_N/0/1/0/all/0/1">N. Masetti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nicholl_M/0/1/0/all/0/1">M. Nicholl</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+E%2E_F/0/1/0/all/0/1">F. Olivares E.</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pugliese_G/0/1/0/all/0/1">G. Pugliese</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rossi_A/0/1/0/all/0/1">A. Rossi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Salvaterra_R/0/1/0/all/0/1">R. Salvaterra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sollerman_J/0/1/0/all/0/1">J. Sollerman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stone_M/0/1/0/all/0/1">M.B. Stone</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tagliaferri_G/0/1/0/all/0/1">G. Tagliaferri</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tomasella_L/0/1/0/all/0/1">L. Tomasella</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Thone_C/0/1/0/all/0/1">C.C. Thone</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Xu_D/0/1/0/all/0/1">D. Xu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Young_D/0/1/0/all/0/1">D.R. Young</a>

The number of supernovae known to be connected with long-duration gamma-ray
bursts is increasing and the link between these events is no longer exclusively
found at low redshift ($z lesssim 0.3$) but is well established also at larger
distances. We present a new case of such a liaison at $z = 0.33$ between
GRB,171010A and SN,2017htp. It is the second closest GRB with an associated
supernova of only three events detected by Fermi-LAT. The supernova is one of
the few higher redshift cases where spectroscopic observations were possible
and shows spectral similarities with the well-studied SN,1998bw, having
produced a similar Ni mass ($M_{rm Ni}=0.33pm0.02 ~rm{M_{odot}}$) with
slightly lower ejected mass ($M_{rm ej}=4.1pm0.7~rm{M_{odot}}$) and kinetic
energy ($E_{rm K} = 8.1pm2.5 times 10^{51} ~rm{erg}$). The host-galaxy is
bigger in size than typical GRB host galaxies, but the analysis of the region
hosting the GRB revealed spectral properties typically observed in GRB hosts
and showed that the progenitor of this event was located in a very bright HII
region of its face-on host galaxy, at a projected distance of $sim$ 10 kpc
from its galactic centre. The star-formation rate (SFR$_{GRB} sim$ 0.2
M$_{odot}$~yr$^{-1}$) and metallicity (12 + log(O/H) $sim 8.15 pm 0.10$) of
the GRB star-forming region are consistent with those of the host galaxies of
previously studied GRB-SN systems.

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