GRB 171010A/SN 2017htp: A Grb-Sn at z = 0.33

A. Melandri; D. B. Malesani; L. Izzo; J. Japelj; S. D. Vergani; P. Schady; A. Sagués Carracedo; A. de Ugarte Postigo; J. P. Anderson; C. Barbarino; J. Bolmer; A. Breeveld; P. Calissendorff; S. Campana; Z. Cano; R. Carini; S. Covino; P. D'Avanzo; V. D'Elia; M. della Valle; M. de Pasquale; J. P.U. Fynbo; M. Gromadzki; F. Hammer; D. H. Hartmann; K. E. Heintz; C. Inserra; P. Jakobsson; D. A. Kann; J. Kotilainen; K. Maguire; N. Masetti; M. Nicholl; F. E. Olivares; G. Pugliese; A. Rossi; R. Salvaterra; J. Sollerman; M. B. Stone; G. Tagliaferri; L. Tomasella; C. C. Thöne; D. Xu; D. R. Young

doi:10.1093/mnras/stz2900

GRB 171010A/SN 2017htp: A Grb-Sn at z = 0.33

A. Melandri
, D. B. Malesani
, L. Izzo
, J. Japelj
, S. D. Vergani
, P. Schady
, A. Sagués Carracedo
, A. de Ugarte Postigo
, J. P. Anderson
, C. Barbarino
, J. Bolmer
, A. Breeveld
, P. Calissendorff
, S. Campana
, Z. Cano
, R. Carini
, S. Covino
, P. D'Avanzo
, V. D'Elia
, M. della Valle

M. de Pasquale, J. P.U. Fynbo, M. Gromadzki, F. Hammer, D. H. Hartmann, K. E. Heintz, C. Inserra, P. Jakobsson, D. A. Kann, J. Kotilainen, K. Maguire, N. Masetti, M. Nicholl, F. E. Olivares, G. Pugliese, A. Rossi, R. Salvaterra, J. Sollerman, M. B. Stone, G. Tagliaferri, L. Tomasella, C. C. Thöne, D. Xu, D. R. Young

University of Iceland

Research output: Contribution to journal › Article › peer-review

Abstract

The number of supernovae known to be connected with long-duration gamma-ray bursts (GRBs) is increasing and the link between these events is no longer exclusively found at low redshift (z ≾ 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_Ni = 0.33 ± 0.02 M☉) with slightly lower ejected mass (M_ej = 4.1 ± 0.7 M☉) and kinetic energy (E_K = 8.1 ± 2.5 × 10⁵¹ 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 H II region of its face-on host galaxy, at a projected distance of ∼ 10 kpc from its galactic centre. The star-formation rate (SFR_GRB ∼ 0.2 M☉ yr⁻¹) and metallicity (12 + log(O/H) ∼8.15 ± 0.10) of the GRB star-forming region are consistent with those of the host galaxies of previously studied GRB-SN systems.

Original language	English
Pages (from-to)	5366-5374
Number of pages	9
Journal	Monthly Notices of the Royal Astronomical Society
Volume	490
Issue number	4
DOIs	https://doi.org/10.1093/mnras/stz2900
Publication status	Published - 1 Dec 2019

Bibliographical note

Funding Information: localization, and physics of transient sources’. MN is supported by a Royal Astronomical Society Research Fellowship. MG is supported by the Polish NCN MAESTRO grant 2014/14/A/ST9/00121. KM acknowledges support from H2020 ERC grant no. 58638. The Cosmic Dawn Center is funded by the DNRF. Support for FOE is provided by the Ministry of Economy, Development, and Tourism’s Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics. FOE acknowledges support from the FONDECYT grant no. 1170953. DX acknowledges the supports by the One-Hundred-Talent Program of the Chinese Academy of Sciences (CAS) and by the Strategic Priority Research Program ‘Multi-wavelength Gravitational Wave Universe of the CAS (no. XDB23000000). Funding Information: We thank the anonymous referee for the valuable comments that contributed to improving the quality of the publication. AM, PDA, SCa, and GT acknowledge support from ASI grant INAFI/004/11/3. DBM is supported by research grant 19054 from Villum Fonden. This study is partly based on data acquired under the extended Public ESO Spectroscopic Survey for Transient Objects (ePESSTO; http://www.pessto.org, under programme 199.D-0143) and within the Stargate collaboration (under programme 0100.D-0649). The study is based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programme 199.D-0143. LI and DAK acknowledge the support from the Spanish research project AYA2014-58381-P. LI and DAK acknowledge support from Juan de la Cierva Incorporaci?n fellowship IJCI-2016-30940 and IJCI-2015-26153, respectively. The study is based on observations collected at the Centro Astron?mico Hispano Alem?n (CAHA) at Calar Alto, operated jointly by the Max-Planck Institut f?r Astronomie and the Instituto de Astrof?sica de Andaluc?a (CSIC). AR acknowledges support from Premiale LBT 2013. The study is based on data collected with Large Binocular Cameras at the LBT. The LBT is an international collaboration among institutions in the United States, Italy, and Germany. The study is based on observations made with the Nordic Optical Telescope (thanks to the valuable support of D. Bettoni) under programme 51-504, operated by the Nordic Optical Telescope Scientific Association at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias. The study is partially based on observations collected at Copernico Telescope (Asiago, Mt. Ekar, Italy) of the INAF Osservatorio Astronomico di Padova. LT is partially supported by the PRIN-INAF 2017 'Towards the SKA and CTA era: discovery, localization, and physics of transient sources'. MN is supported by a Royal Astronomical Society Research Fellowship. MG is supported by the Polish NCN MAESTRO grant 2014/14/A/ST9/00121. KM acknowledges support from H2020 ERC grant no. 58638. The Cosmic Dawn Center is funded by the DNRF. Support for FOE is provided by the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics. FOE acknowledges support from the FONDECYT grant no. 1170953. DX acknowledges the supports by the One-Hundred-Talent Program of the Chinese Academy of Sciences (CAS) and by the Strategic Priority Research Program 'Multi-wavelength Gravitational Wave Universe of the CAS (no. XDB23000000). Funding Information: We thank the anonymous referee for the valuable comments that contributed to improving the quality of the publication. AM, PDA, SCa, and GT acknowledge support from ASI grant INAFI/004/11/3. DBM is supported by research grant 19054 from Villum Fonden. This study is partly based on data acquired under the extended Public ESO Spectroscopic Survey for Transient Objects (ePESSTO; http://www.pessto.org, under programme 199.D-0143) and within the Stargate collaboration (under programme 0100.D-0649). The study is based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programme 199.D-0143. LI and DAK acknowledge the support from the Spanish research project AYA2014-58381-P. LI and DAK acknowledge support from Juan de la Cierva Incorporación fellowship IJCI-2016-30940 and IJCI-2015-26153, respectively. The study is based on observations collected at the Centro Astronómico Hispano Alemán (CAHA) at Calar Alto, operated jointly by the Max-Planck Institut für Astronomie and the Instituto de Astrofísica de Andalucía (CSIC). AR acknowledges support from Premiale LBT 2013. The study is based on data collected with Large Binocular Cameras at the LBT. The LBT is an international collaboration among institutions in the United States, Italy, and Germany. The study is based on observations made with the Nordic Optical Telescope (thanks to the valuable support of D. Bettoni) under programme 51-504, operated by the Nordic Optical Telescope Scientific Association at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias. The study is partially based on observations collected at Copernico Telescope (Asiago, Mt. Ekar, Italy) of the INAF Osservatorio Astronomico di Padova. LT is partially supported by the PRIN-INAF 2017 ‘Towards the SKA and CTA era: discovery, Publisher Copyright: © 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society

Other keywords

Gamma-ray burst: individual: GRB 171010A - supernovae: individual: SN 2017htp

Access to Document

10.1093/mnras/stz2900

Cite this

Melandri, A., Malesani, D. B., Izzo, L., Japelj, J., Vergani, S. D., Schady, P., Sagués Carracedo, A., de Ugarte Postigo, A., Anderson, J. P., Barbarino, C., Bolmer, J., Breeveld, A., Calissendorff, P., Campana, S., Cano, Z., Carini, R., Covino, S., D'Avanzo, P., D'Elia, V., ... Young, D. R. (2019). GRB 171010A/SN 2017htp: A Grb-Sn at z = 0.33. Monthly Notices of the Royal Astronomical Society, 490(4), 5366-5374. https://doi.org/10.1093/mnras/stz2900

@article{8fd278b958bc4b4aa53a99a1d8dbcb4e,

title = "GRB 171010A/SN 2017htp: A Grb-Sn at z = 0.33",

abstract = "The number of supernovae known to be connected with long-duration gamma-ray bursts (GRBs) is increasing and the link between these events is no longer exclusively found at low redshift (z ≾ 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 (MNi = 0.33 ± 0.02 M☉) with slightly lower ejected mass (Mej = 4.1 ± 0.7 M☉) and kinetic energy (EK = 8.1 ± 2.5 × 1051 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 H II region of its face-on host galaxy, at a projected distance of ∼ 10 kpc from its galactic centre. The star-formation rate (SFRGRB ∼ 0.2 M☉ yr−1) and metallicity (12 + log(O/H) ∼8.15 ± 0.10) of the GRB star-forming region are consistent with those of the host galaxies of previously studied GRB-SN systems.",

keywords = "Gamma-ray burst: individual: GRB 171010A - supernovae: individual: SN 2017htp",

author = "A. Melandri and Malesani, \{D. B.\} and L. Izzo and J. Japelj and Vergani, \{S. D.\} and P. Schady and \{Sagu{\'e}s Carracedo\}, A. and \{de Ugarte Postigo\}, A. and Anderson, \{J. P.\} and C. Barbarino and J. Bolmer and A. Breeveld and P. Calissendorff and S. Campana and Z. Cano and R. Carini and S. Covino and P. D'Avanzo and V. D'Elia and \{della Valle\}, M. and \{de Pasquale\}, M. and Fynbo, \{J. P.U.\} and M. Gromadzki and F. Hammer and Hartmann, \{D. H.\} and Heintz, \{K. E.\} and C. Inserra and P. Jakobsson and Kann, \{D. A.\} and J. Kotilainen and K. Maguire and N. Masetti and M. Nicholl and Olivares, \{F. E.\} and G. Pugliese and A. Rossi and R. Salvaterra and J. Sollerman and Stone, \{M. B.\} and G. Tagliaferri and L. Tomasella and Th{\"o}ne, \{C. C.\} and D. Xu and Young, \{D. R.\}",

note = "Funding Information: localization, and physics of transient sources{\textquoteright}. MN is supported by a Royal Astronomical Society Research Fellowship. MG is supported by the Polish NCN MAESTRO grant 2014/14/A/ST9/00121. KM acknowledges support from H2020 ERC grant no. 58638. The Cosmic Dawn Center is funded by the DNRF. Support for FOE is provided by the Ministry of Economy, Development, and Tourism{\textquoteright}s Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics. FOE acknowledges support from the FONDECYT grant no. 1170953. DX acknowledges the supports by the One-Hundred-Talent Program of the Chinese Academy of Sciences (CAS) and by the Strategic Priority Research Program {\textquoteleft}Multi-wavelength Gravitational Wave Universe of the CAS (no. XDB23000000). Funding Information: We thank the anonymous referee for the valuable comments that contributed to improving the quality of the publication. AM, PDA, SCa, and GT acknowledge support from ASI grant INAFI/004/11/3. DBM is supported by research grant 19054 from Villum Fonden. This study is partly based on data acquired under the extended Public ESO Spectroscopic Survey for Transient Objects (ePESSTO; http://www.pessto.org, under programme 199.D-0143) and within the Stargate collaboration (under programme 0100.D-0649). The study is based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programme 199.D-0143. LI and DAK acknowledge the support from the Spanish research project AYA2014-58381-P. LI and DAK acknowledge support from Juan de la Cierva Incorporaci?n fellowship IJCI-2016-30940 and IJCI-2015-26153, respectively. The study is based on observations collected at the Centro Astron?mico Hispano Alem?n (CAHA) at Calar Alto, operated jointly by the Max-Planck Institut f?r Astronomie and the Instituto de Astrof?sica de Andaluc?a (CSIC). AR acknowledges support from Premiale LBT 2013. The study is based on data collected with Large Binocular Cameras at the LBT. The LBT is an international collaboration among institutions in the United States, Italy, and Germany. The study is based on observations made with the Nordic Optical Telescope (thanks to the valuable support of D. Bettoni) under programme 51-504, operated by the Nordic Optical Telescope Scientific Association at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias. The study is partially based on observations collected at Copernico Telescope (Asiago, Mt. Ekar, Italy) of the INAF Osservatorio Astronomico di Padova. LT is partially supported by the PRIN-INAF 2017 'Towards the SKA and CTA era: discovery, localization, and physics of transient sources'. MN is supported by a Royal Astronomical Society Research Fellowship. MG is supported by the Polish NCN MAESTRO grant 2014/14/A/ST9/00121. KM acknowledges support from H2020 ERC grant no. 58638. The Cosmic Dawn Center is funded by the DNRF. Support for FOE is provided by the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics. FOE acknowledges support from the FONDECYT grant no. 1170953. DX acknowledges the supports by the One-Hundred-Talent Program of the Chinese Academy of Sciences (CAS) and by the Strategic Priority Research Program 'Multi-wavelength Gravitational Wave Universe of the CAS (no. XDB23000000). Funding Information: We thank the anonymous referee for the valuable comments that contributed to improving the quality of the publication. AM, PDA, SCa, and GT acknowledge support from ASI grant INAFI/004/11/3. DBM is supported by research grant 19054 from Villum Fonden. This study is partly based on data acquired under the extended Public ESO Spectroscopic Survey for Transient Objects (ePESSTO; http://www.pessto.org, under programme 199.D-0143) and within the Stargate collaboration (under programme 0100.D-0649). The study is based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programme 199.D-0143. LI and DAK acknowledge the support from the Spanish research project AYA2014-58381-P. LI and DAK acknowledge support from Juan de la Cierva Incorporaci{\'o}n fellowship IJCI-2016-30940 and IJCI-2015-26153, respectively. The study is based on observations collected at the Centro Astron{\'o}mico Hispano Alem{\'a}n (CAHA) at Calar Alto, operated jointly by the Max-Planck Institut f{\"u}r Astronomie and the Instituto de Astrof{\'i}sica de Andaluc{\'i}a (CSIC). AR acknowledges support from Premiale LBT 2013. The study is based on data collected with Large Binocular Cameras at the LBT. The LBT is an international collaboration among institutions in the United States, Italy, and Germany. The study is based on observations made with the Nordic Optical Telescope (thanks to the valuable support of D. Bettoni) under programme 51-504, operated by the Nordic Optical Telescope Scientific Association at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias. The study is partially based on observations collected at Copernico Telescope (Asiago, Mt. Ekar, Italy) of the INAF Osservatorio Astronomico di Padova. LT is partially supported by the PRIN-INAF 2017 {\textquoteleft}Towards the SKA and CTA era: discovery, Publisher Copyright: {\textcopyright} 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society",

year = "2019",

month = dec,

day = "1",

doi = "10.1093/mnras/stz2900",

language = "English",

volume = "490",

pages = "5366--5374",

journal = "Monthly Notices of the Royal Astronomical Society",

issn = "0035-8711",

publisher = "Oxford University Press",

number = "4",

}

Melandri, A, Malesani, DB, Izzo, L, Japelj, J, Vergani, SD, Schady, P, Sagués Carracedo, A, de Ugarte Postigo, A, Anderson, JP, Barbarino, C, Bolmer, J, Breeveld, A, Calissendorff, P, Campana, S, Cano, Z, Carini, R, Covino, S, D'Avanzo, P, D'Elia, V, della Valle, M, de Pasquale, M, Fynbo, JPU, Gromadzki, M, Hammer, F, Hartmann, DH, Heintz, KE, Inserra, C, Jakobsson, P, Kann, DA, Kotilainen, J, Maguire, K, Masetti, N, Nicholl, M, Olivares, FE, Pugliese, G, Rossi, A, Salvaterra, R, Sollerman, J, Stone, MB, Tagliaferri, G, Tomasella, L, Thöne, CC, Xu, D & Young, DR 2019, 'GRB 171010A/SN 2017htp: A Grb-Sn at z = 0.33', Monthly Notices of the Royal Astronomical Society, vol. 490, no. 4, pp. 5366-5374. https://doi.org/10.1093/mnras/stz2900

TY - JOUR

T1 - GRB 171010A/SN 2017htp

T2 - A Grb-Sn at z = 0.33

AU - Melandri, A.

AU - Malesani, D. B.

AU - Izzo, L.

AU - Japelj, J.

AU - Vergani, S. D.

AU - Schady, P.

AU - Sagués Carracedo, A.

AU - de Ugarte Postigo, A.

AU - Anderson, J. P.

AU - Barbarino, C.

AU - Bolmer, J.

AU - Breeveld, A.

AU - Calissendorff, P.

AU - Campana, S.

AU - Cano, Z.

AU - Carini, R.

AU - Covino, S.

AU - D'Avanzo, P.

AU - D'Elia, V.

AU - della Valle, M.

AU - de Pasquale, M.

AU - Fynbo, J. P.U.

AU - Gromadzki, M.

AU - Hammer, F.

AU - Hartmann, D. H.

AU - Heintz, K. E.

AU - Inserra, C.

AU - Jakobsson, P.

AU - Kann, D. A.

AU - Kotilainen, J.

AU - Maguire, K.

AU - Masetti, N.

AU - Nicholl, M.

AU - Olivares, F. E.

AU - Pugliese, G.

AU - Rossi, A.

AU - Salvaterra, R.

AU - Sollerman, J.

AU - Stone, M. B.

AU - Tagliaferri, G.

AU - Tomasella, L.

AU - Thöne, C. C.

AU - Xu, D.

AU - Young, D. R.

N1 - Funding Information: localization, and physics of transient sources’. MN is supported by a Royal Astronomical Society Research Fellowship. MG is supported by the Polish NCN MAESTRO grant 2014/14/A/ST9/00121. KM acknowledges support from H2020 ERC grant no. 58638. The Cosmic Dawn Center is funded by the DNRF. Support for FOE is provided by the Ministry of Economy, Development, and Tourism’s Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics. FOE acknowledges support from the FONDECYT grant no. 1170953. DX acknowledges the supports by the One-Hundred-Talent Program of the Chinese Academy of Sciences (CAS) and by the Strategic Priority Research Program ‘Multi-wavelength Gravitational Wave Universe of the CAS (no. XDB23000000). Funding Information: We thank the anonymous referee for the valuable comments that contributed to improving the quality of the publication. AM, PDA, SCa, and GT acknowledge support from ASI grant INAFI/004/11/3. DBM is supported by research grant 19054 from Villum Fonden. This study is partly based on data acquired under the extended Public ESO Spectroscopic Survey for Transient Objects (ePESSTO; http://www.pessto.org, under programme 199.D-0143) and within the Stargate collaboration (under programme 0100.D-0649). The study is based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programme 199.D-0143. LI and DAK acknowledge the support from the Spanish research project AYA2014-58381-P. LI and DAK acknowledge support from Juan de la Cierva Incorporaci?n fellowship IJCI-2016-30940 and IJCI-2015-26153, respectively. The study is based on observations collected at the Centro Astron?mico Hispano Alem?n (CAHA) at Calar Alto, operated jointly by the Max-Planck Institut f?r Astronomie and the Instituto de Astrof?sica de Andaluc?a (CSIC). AR acknowledges support from Premiale LBT 2013. The study is based on data collected with Large Binocular Cameras at the LBT. The LBT is an international collaboration among institutions in the United States, Italy, and Germany. The study is based on observations made with the Nordic Optical Telescope (thanks to the valuable support of D. Bettoni) under programme 51-504, operated by the Nordic Optical Telescope Scientific Association at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias. The study is partially based on observations collected at Copernico Telescope (Asiago, Mt. Ekar, Italy) of the INAF Osservatorio Astronomico di Padova. LT is partially supported by the PRIN-INAF 2017 'Towards the SKA and CTA era: discovery, localization, and physics of transient sources'. MN is supported by a Royal Astronomical Society Research Fellowship. MG is supported by the Polish NCN MAESTRO grant 2014/14/A/ST9/00121. KM acknowledges support from H2020 ERC grant no. 58638. The Cosmic Dawn Center is funded by the DNRF. Support for FOE is provided by the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics. FOE acknowledges support from the FONDECYT grant no. 1170953. DX acknowledges the supports by the One-Hundred-Talent Program of the Chinese Academy of Sciences (CAS) and by the Strategic Priority Research Program 'Multi-wavelength Gravitational Wave Universe of the CAS (no. XDB23000000). Funding Information: We thank the anonymous referee for the valuable comments that contributed to improving the quality of the publication. AM, PDA, SCa, and GT acknowledge support from ASI grant INAFI/004/11/3. DBM is supported by research grant 19054 from Villum Fonden. This study is partly based on data acquired under the extended Public ESO Spectroscopic Survey for Transient Objects (ePESSTO; http://www.pessto.org, under programme 199.D-0143) and within the Stargate collaboration (under programme 0100.D-0649). The study is based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programme 199.D-0143. LI and DAK acknowledge the support from the Spanish research project AYA2014-58381-P. LI and DAK acknowledge support from Juan de la Cierva Incorporación fellowship IJCI-2016-30940 and IJCI-2015-26153, respectively. The study is based on observations collected at the Centro Astronómico Hispano Alemán (CAHA) at Calar Alto, operated jointly by the Max-Planck Institut für Astronomie and the Instituto de Astrofísica de Andalucía (CSIC). AR acknowledges support from Premiale LBT 2013. The study is based on data collected with Large Binocular Cameras at the LBT. The LBT is an international collaboration among institutions in the United States, Italy, and Germany. The study is based on observations made with the Nordic Optical Telescope (thanks to the valuable support of D. Bettoni) under programme 51-504, operated by the Nordic Optical Telescope Scientific Association at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias. The study is partially based on observations collected at Copernico Telescope (Asiago, Mt. Ekar, Italy) of the INAF Osservatorio Astronomico di Padova. LT is partially supported by the PRIN-INAF 2017 ‘Towards the SKA and CTA era: discovery, Publisher Copyright: © 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society

PY - 2019/12/1

Y1 - 2019/12/1

N2 - The number of supernovae known to be connected with long-duration gamma-ray bursts (GRBs) is increasing and the link between these events is no longer exclusively found at low redshift (z ≾ 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 (MNi = 0.33 ± 0.02 M☉) with slightly lower ejected mass (Mej = 4.1 ± 0.7 M☉) and kinetic energy (EK = 8.1 ± 2.5 × 1051 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 H II region of its face-on host galaxy, at a projected distance of ∼ 10 kpc from its galactic centre. The star-formation rate (SFRGRB ∼ 0.2 M☉ yr−1) and metallicity (12 + log(O/H) ∼8.15 ± 0.10) of the GRB star-forming region are consistent with those of the host galaxies of previously studied GRB-SN systems.

AB - The number of supernovae known to be connected with long-duration gamma-ray bursts (GRBs) is increasing and the link between these events is no longer exclusively found at low redshift (z ≾ 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 (MNi = 0.33 ± 0.02 M☉) with slightly lower ejected mass (Mej = 4.1 ± 0.7 M☉) and kinetic energy (EK = 8.1 ± 2.5 × 1051 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 H II region of its face-on host galaxy, at a projected distance of ∼ 10 kpc from its galactic centre. The star-formation rate (SFRGRB ∼ 0.2 M☉ yr−1) and metallicity (12 + log(O/H) ∼8.15 ± 0.10) of the GRB star-forming region are consistent with those of the host galaxies of previously studied GRB-SN systems.

KW - Gamma-ray burst: individual: GRB 171010A - supernovae: individual: SN 2017htp

UR - https://www.scopus.com/pages/publications/85079594552

U2 - 10.1093/mnras/stz2900

DO - 10.1093/mnras/stz2900

M3 - Article

SN - 0035-8711

VL - 490

SP - 5366

EP - 5374

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 4

ER -

GRB 171010A/SN 2017htp: A Grb-Sn at z = 0.33

Abstract

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