The ultra-long GRB 220627A at z = 3.08

S. De Wet; L. Izzo; P. J. Groot; S. Bisero; V. D' Elia; M. De Pasquale; D. H. Hartmann; K. E. Heintz; P. Jakobsson; T. Laskar; A. Levan; A. Martin-Carrillo; A. Melandri; A. Nicuesa Guelbenzu; G. Pugliese; A. Rossi; A. Saccardi; S. Savaglio; P. Schady; N. R. Tanvir; H. Van Eerten; S. D. Vergani

doi:10.1051/0004-6361/202347017

The ultra-long GRB 220627A at z = 3.08

S. De Wet, L. Izzo, P. J. Groot, S. Bisero, V. D' Elia, M. De Pasquale, D. H. Hartmann, K. E. Heintz, P. Jakobsson, T. Laskar, A. Levan, A. Martin-Carrillo, A. Melandri, A. Nicuesa Guelbenzu, G. Pugliese, A. Rossi, A. Saccardi, S. Savaglio, P. Schady, N. R. TanvirH. Van Eerten, S. D. Vergani

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

7 Citations (SciVal)

Abstract

Context. GRB 220627A is a rare burst with two distinct γ-ray emission episodes separated by almost 1000 s that triggered the Fermi Gamma-ray Burst Monitor twice. High-energy GeV emission was detected by the Fermi Large Area Telescope coincident with the first emission episode but not the second. The discovery of the optical afterglow with MeerLICHT led to MUSE observations which secured the burst redshift to z'., ='., 3.08, making this the most distant ultra-long gamma-ray burst (GRB) detected to date. Aims. The progenitors of some ultra-long GRBs have been suggested in the literature to be different to those of normal long GRBs. Our aim is to determine whether the afterglow and host properties of GRB 220627A agree with this interpretation. Methods. We performed empirical and theoretical modelling of the afterglow data within the external forward shock framework, and determined the metallicity of the GRB environment through modelling the absorption lines in the MUSE spectrum. Results. Our optical data show evidence for a jet break in the light curve at 1.2 days, while our theoretical modelling shows a preference for a homogeneous circumburst medium. Our forward shock parameters are typical for the wider GRB population, and we find that the environment of the burst is characterised by a sub-solar metallicity. Conclusions. Our observations and modelling of GRB 220627A do not suggest that a different progenitor compared to the progenitor of normal long GRBs is required. We find that more observations of ultra-long GRBs are needed to determine if they form a separate population with distinct prompt and afterglow features, and possibly distinct progenitors.

Original language	English
Article number	A32
Journal	Astronomy and Astrophysics
Volume	677
Early online date	29 Aug 2023
DOIs	https://doi.org/10.1051/0004-6361/202347017
Publication status	Published - 1 Sept 2023

Bibliographical note

Funding Information:
The MeerLICHT consortium is a partnership between Radboud University, the University of Cape Town, the South African Astronomical Observatory (SAAO), the University of Oxford, the University of Manchester and the University of Amsterdam, in association with and, partly supported by, the South African Radio Astronomy Observatory (SARAO), the European Research Council and The Netherlands Research School for Astronomy (NOVA). We acknowledge the use of the Inter-University Institute for Data Intensive Astronomy (IDIA) data intensive research cloud for data processing. IDIA is a South African university partnership involving the University of Cape Town, the University of Pretoria and the University of the Western Cape. S.dW. and P.J.G. are supported by NRF SARChI Grant 111692. The research leading to these results has received funding from the European Union’s Horizon 2020 Programme under the AHEAD2020 project (grant agreement number 871158). Part of the funding for GROND (both hardware and personnel) was generously granted from the Leibniz-Prize to G. Hasinger (DFG grant HA 1850/28-1) and by the Thüringer Landessternwarte Tautenburg. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. A.S. and S.D.V. acknowledge support from DIM-ACAV+.

Funding

The MeerLICHT consortium is a partnership between Radboud University, the University of Cape Town, the South African Astronomical Observatory (SAAO), the University of Oxford, the University of Manchester and the University of Amsterdam, in association with and, partly supported by, the South African Radio Astronomy Observatory (SARAO), the European Research Council and The Netherlands Research School for Astronomy (NOVA). We acknowledge the use of the Inter-University Institute for Data Intensive Astronomy (IDIA) data intensive research cloud for data processing. IDIA is a South African university partnership involving the University of Cape Town, the University of Pretoria and the University of the Western Cape. S.dW. and P.J.G. are supported by NRF SARChI Grant 111692. The research leading to these results has received funding from the European Union’s Horizon 2020 Programme under the AHEAD2020 project (grant agreement number 871158). Part of the funding for GROND (both hardware and personnel) was generously granted from the Leibniz-Prize to G. Hasinger (DFG grant HA 1850/28-1) and by the Thüringer Landessternwarte Tautenburg. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. A.S. and S.D.V. acknowledge support from DIM-ACAV+.

Keywords

Gamma rays: stars

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

Access to Document

10.1051/0004-6361/202347017Licence: CC BY

Cite this

De Wet, S., Izzo, L., Groot, P. J., Bisero, S., D' Elia, V., De Pasquale, M., Hartmann, D. H., Heintz, K. E., Jakobsson, P., Laskar, T., Levan, A., Martin-Carrillo, A., Melandri, A., Nicuesa Guelbenzu, A., Pugliese, G., Rossi, A., Saccardi, A., Savaglio, S., Schady, P., ... Vergani, S. D. (2023). The ultra-long GRB 220627A at z = 3.08. Astronomy and Astrophysics, 677, Article A32. https://doi.org/10.1051/0004-6361/202347017

De Wet, S, Izzo, L, Groot, PJ, Bisero, S, D' Elia, V, De Pasquale, M, Hartmann, DH, Heintz, KE, Jakobsson, P, Laskar, T, Levan, A, Martin-Carrillo, A, Melandri, A, Nicuesa Guelbenzu, A, Pugliese, G, Rossi, A, Saccardi, A, Savaglio, S, Schady, P, Tanvir, NR, Van Eerten, H & Vergani, SD 2023, 'The ultra-long GRB 220627A at z = 3.08', Astronomy and Astrophysics, vol. 677, A32. https://doi.org/10.1051/0004-6361/202347017

@article{29197c7a2e84402ca32ec84d59acc57b,

title = "The ultra-long GRB 220627A at z = 3.08",

abstract = "Context. GRB 220627A is a rare burst with two distinct γ-ray emission episodes separated by almost 1000 s that triggered the Fermi Gamma-ray Burst Monitor twice. High-energy GeV emission was detected by the Fermi Large Area Telescope coincident with the first emission episode but not the second. The discovery of the optical afterglow with MeerLICHT led to MUSE observations which secured the burst redshift to z'., ='., 3.08, making this the most distant ultra-long gamma-ray burst (GRB) detected to date. Aims. The progenitors of some ultra-long GRBs have been suggested in the literature to be different to those of normal long GRBs. Our aim is to determine whether the afterglow and host properties of GRB 220627A agree with this interpretation. Methods. We performed empirical and theoretical modelling of the afterglow data within the external forward shock framework, and determined the metallicity of the GRB environment through modelling the absorption lines in the MUSE spectrum. Results. Our optical data show evidence for a jet break in the light curve at 1.2 days, while our theoretical modelling shows a preference for a homogeneous circumburst medium. Our forward shock parameters are typical for the wider GRB population, and we find that the environment of the burst is characterised by a sub-solar metallicity. Conclusions. Our observations and modelling of GRB 220627A do not suggest that a different progenitor compared to the progenitor of normal long GRBs is required. We find that more observations of ultra-long GRBs are needed to determine if they form a separate population with distinct prompt and afterglow features, and possibly distinct progenitors.",

keywords = "Gamma rays: stars",

author = "{De Wet}, S. and L. Izzo and Groot, {P. J.} and S. Bisero and {D' Elia}, V. and {De Pasquale}, M. and Hartmann, {D. H.} and Heintz, {K. E.} and P. Jakobsson and T. Laskar and A. Levan and A. Martin-Carrillo and A. Melandri and {Nicuesa Guelbenzu}, A. and G. Pugliese and A. Rossi and A. Saccardi and S. Savaglio and P. Schady and Tanvir, {N. R.} and {Van Eerten}, H. and Vergani, {S. D.}",

note = "Funding Information: The MeerLICHT consortium is a partnership between Radboud University, the University of Cape Town, the South African Astronomical Observatory (SAAO), the University of Oxford, the University of Manchester and the University of Amsterdam, in association with and, partly supported by, the South African Radio Astronomy Observatory (SARAO), the European Research Council and The Netherlands Research School for Astronomy (NOVA). We acknowledge the use of the Inter-University Institute for Data Intensive Astronomy (IDIA) data intensive research cloud for data processing. IDIA is a South African university partnership involving the University of Cape Town, the University of Pretoria and the University of the Western Cape. S.dW. and P.J.G. are supported by NRF SARChI Grant 111692. The research leading to these results has received funding from the European Union{\textquoteright}s Horizon 2020 Programme under the AHEAD2020 project (grant agreement number 871158). Part of the funding for GROND (both hardware and personnel) was generously granted from the Leibniz-Prize to G. Hasinger (DFG grant HA 1850/28-1) and by the Th{\"u}ringer Landessternwarte Tautenburg. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. A.S. and S.D.V. acknowledge support from DIM-ACAV+. ",

year = "2023",

month = sep,

day = "1",

doi = "10.1051/0004-6361/202347017",

language = "English",

volume = "677",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

}

TY - JOUR

T1 - The ultra-long GRB 220627A at z = 3.08

AU - De Wet, S.

AU - Izzo, L.

AU - Groot, P. J.

AU - Bisero, S.

AU - D' Elia, V.

AU - De Pasquale, M.

AU - Hartmann, D. H.

AU - Heintz, K. E.

AU - Jakobsson, P.

AU - Laskar, T.

AU - Levan, A.

AU - Martin-Carrillo, A.

AU - Melandri, A.

AU - Nicuesa Guelbenzu, A.

AU - Pugliese, G.

AU - Rossi, A.

AU - Saccardi, A.

AU - Savaglio, S.

AU - Schady, P.

AU - Tanvir, N. R.

AU - Van Eerten, H.

AU - Vergani, S. D.

N1 - Funding Information: The MeerLICHT consortium is a partnership between Radboud University, the University of Cape Town, the South African Astronomical Observatory (SAAO), the University of Oxford, the University of Manchester and the University of Amsterdam, in association with and, partly supported by, the South African Radio Astronomy Observatory (SARAO), the European Research Council and The Netherlands Research School for Astronomy (NOVA). We acknowledge the use of the Inter-University Institute for Data Intensive Astronomy (IDIA) data intensive research cloud for data processing. IDIA is a South African university partnership involving the University of Cape Town, the University of Pretoria and the University of the Western Cape. S.dW. and P.J.G. are supported by NRF SARChI Grant 111692. The research leading to these results has received funding from the European Union’s Horizon 2020 Programme under the AHEAD2020 project (grant agreement number 871158). Part of the funding for GROND (both hardware and personnel) was generously granted from the Leibniz-Prize to G. Hasinger (DFG grant HA 1850/28-1) and by the Thüringer Landessternwarte Tautenburg. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. A.S. and S.D.V. acknowledge support from DIM-ACAV+.

PY - 2023/9/1

Y1 - 2023/9/1

N2 - Context. GRB 220627A is a rare burst with two distinct γ-ray emission episodes separated by almost 1000 s that triggered the Fermi Gamma-ray Burst Monitor twice. High-energy GeV emission was detected by the Fermi Large Area Telescope coincident with the first emission episode but not the second. The discovery of the optical afterglow with MeerLICHT led to MUSE observations which secured the burst redshift to z'., ='., 3.08, making this the most distant ultra-long gamma-ray burst (GRB) detected to date. Aims. The progenitors of some ultra-long GRBs have been suggested in the literature to be different to those of normal long GRBs. Our aim is to determine whether the afterglow and host properties of GRB 220627A agree with this interpretation. Methods. We performed empirical and theoretical modelling of the afterglow data within the external forward shock framework, and determined the metallicity of the GRB environment through modelling the absorption lines in the MUSE spectrum. Results. Our optical data show evidence for a jet break in the light curve at 1.2 days, while our theoretical modelling shows a preference for a homogeneous circumburst medium. Our forward shock parameters are typical for the wider GRB population, and we find that the environment of the burst is characterised by a sub-solar metallicity. Conclusions. Our observations and modelling of GRB 220627A do not suggest that a different progenitor compared to the progenitor of normal long GRBs is required. We find that more observations of ultra-long GRBs are needed to determine if they form a separate population with distinct prompt and afterglow features, and possibly distinct progenitors.

AB - Context. GRB 220627A is a rare burst with two distinct γ-ray emission episodes separated by almost 1000 s that triggered the Fermi Gamma-ray Burst Monitor twice. High-energy GeV emission was detected by the Fermi Large Area Telescope coincident with the first emission episode but not the second. The discovery of the optical afterglow with MeerLICHT led to MUSE observations which secured the burst redshift to z'., ='., 3.08, making this the most distant ultra-long gamma-ray burst (GRB) detected to date. Aims. The progenitors of some ultra-long GRBs have been suggested in the literature to be different to those of normal long GRBs. Our aim is to determine whether the afterglow and host properties of GRB 220627A agree with this interpretation. Methods. We performed empirical and theoretical modelling of the afterglow data within the external forward shock framework, and determined the metallicity of the GRB environment through modelling the absorption lines in the MUSE spectrum. Results. Our optical data show evidence for a jet break in the light curve at 1.2 days, while our theoretical modelling shows a preference for a homogeneous circumburst medium. Our forward shock parameters are typical for the wider GRB population, and we find that the environment of the burst is characterised by a sub-solar metallicity. Conclusions. Our observations and modelling of GRB 220627A do not suggest that a different progenitor compared to the progenitor of normal long GRBs is required. We find that more observations of ultra-long GRBs are needed to determine if they form a separate population with distinct prompt and afterglow features, and possibly distinct progenitors.

KW - Gamma rays: stars

UR - http://www.scopus.com/inward/record.url?scp=85170820198&partnerID=8YFLogxK

U2 - 10.1051/0004-6361/202347017

DO - 10.1051/0004-6361/202347017

M3 - Article

AN - SCOPUS:85170820198

SN - 0004-6361

VL - 677

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A32

ER -

The ultra-long GRB 220627A at z = 3.08

Abstract

Bibliographical note

Funding

Keywords

ASJC Scopus subject areas

Access to Document

Other files and links

Fingerprint

Astrophysics at the University of Bath 2023-2026

Cite this

The ultra-long GRB 220627A at z = 3.08

Abstract

Bibliographical note

Funding

Keywords

ASJC Scopus subject areas

Access to Document

Other files and links

Fingerprint

Projects

Astrophysics at the University of Bath 2023-2026

Cite this