GROND coverage of the main peak of gamma-ray burst 130925A

J. Greiner; H. -F. Yu; T. Krühler; D.~D. Frederiks; A. Beloborodov; P.~N. Bhat; J. Bolmer; H. van Eerten; R.~L. Aptekar; J. Elliott; S.~V. Golenetskii; J.~F. Graham; K. Hurley; D.~A. Kann; S. Klose; A. Nicuesa Guelbenzu; A. Rau; P. Schady; S. Schmidl; V. Sudilovsky; D.~S. Svinkin; M. Tanga; M.~V. Ulanov; K. Varela; A. von Kienlin; X. -L. Zhang

doi:10.1051/0004-6361/201424250

GROND coverage of the main peak of gamma-ray burst 130925A

J. Greiner
, H. -F. Yu
, T. Krühler
, D.~D. Frederiks
, A. Beloborodov
, P.~N. Bhat
, J. Bolmer
, H. van Eerten
, R.~L. Aptekar
, J. Elliott
, S.~V. Golenetskii
, J.~F. Graham
, K. Hurley
, D.~A. Kann
, S. Klose
, A. Nicuesa Guelbenzu
, A. Rau
, P. Schady
, S. Schmidl
, V. Sudilovsky

D.~S. Svinkin, M. Tanga, M.~V. Ulanov, K. Varela, A. von Kienlin, X. -L. Zhang

Max Planck Institut für Extraterrestrische Physik
Technical University of Munich
European Southern Observatory Santiago
Ioffe Institute
Columbia University
University of Alabama
University of California
Thüringer Landessternwarte Tautenburg

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

Abstract

Aims.Prompt or early optical emission in gamma-ray bursts (GRBs) is notoriously difficult to measure, and observations of the dozen cases show a large variety of properties. Yet, such early emission promises to help us achieve a better understanding of the GRB emission process(es).
Methods. We performed dedicated observations of the ultra-long duration (T90 about 7000 s) Swift GRB 130925A in the optical/near-infrared with the 7-channel Gamma-Ray burst Optical and Near-infrared Detector (GROND) at the 2.2 m MPG/ESO telescope.
Results. We detect an optical/near-infrared flare with an amplitude of nearly 2 mag which is delayed with respect to the keV−MeV prompt emission by about 300−400 s. The decay time of this flare is shorter than the duration of the flare (500 s) or its delay.
Conclusions. While we cannot offer a straightforward explanation, we discuss the implications of the flare properties and suggest ways toward understanding it.

Original language	English
Article number	A75
Pages (from-to)	1-9
Number of pages	9
Journal	Astronomy & Astrophysics
Volume	568
DOIs	https://doi.org/10.1051/0004-6361/201424250
Publication status	Published - 20 Aug 2014

Keywords

gamma rays
stars
radiation mechanisms
non-thermal

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10.1051/0004-6361/201424250

https://arxiv.org/abs/1407.4210

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Greiner, J., Yu, H. .-F., Krühler, T., Frederiks, D. D., Beloborodov, A., Bhat, P. N., Bolmer, J., van Eerten, H., Aptekar, R. L., Elliott, J., Golenetskii, S. V., Graham, J. F., Hurley, K., Kann, D. A., Klose, S., Nicuesa Guelbenzu, A., Rau, A., Schady, P., Schmidl, S., ... Zhang, X. .-L. (2014). GROND coverage of the main peak of gamma-ray burst 130925A. Astronomy & Astrophysics, 568, 1-9. Article A75. https://doi.org/10.1051/0004-6361/201424250

Greiner, J, Yu, H-F, Krühler, T, Frederiks, DD, Beloborodov, A, Bhat, PN, Bolmer, J, van Eerten, H, Aptekar, RL, Elliott, J, Golenetskii, SV, Graham, JF, Hurley, K, Kann, DA, Klose, S, Nicuesa Guelbenzu, A, Rau, A, Schady, P, Schmidl, S, Sudilovsky, V, Svinkin, DS, Tanga, M, Ulanov, MV, Varela, K, von Kienlin, A & Zhang, X-L 2014, 'GROND coverage of the main peak of gamma-ray burst 130925A', Astronomy & Astrophysics, vol. 568, A75, pp. 1-9. https://doi.org/10.1051/0004-6361/201424250

@article{097ce0bc391a47028bfd8fc5d13a027e,

title = "GROND coverage of the main peak of gamma-ray burst 130925A",

abstract = "Aims.Prompt or early optical emission in gamma-ray bursts (GRBs) is notoriously difficult to measure, and observations of the dozen cases show a large variety of properties. Yet, such early emission promises to help us achieve a better understanding of the GRB emission process(es). Methods. We performed dedicated observations of the ultra-long duration (T90 about 7000 s) Swift GRB 130925A in the optical/near-infrared with the 7-channel Gamma-Ray burst Optical and Near-infrared Detector (GROND) at the 2.2 m MPG/ESO telescope. Results. We detect an optical/near-infrared flare with an amplitude of nearly 2 mag which is delayed with respect to the keV−MeV prompt emission by about 300−400 s. The decay time of this flare is shorter than the duration of the flare (500 s) or its delay. Conclusions. While we cannot offer a straightforward explanation, we discuss the implications of the flare properties and suggest ways toward understanding it.",

keywords = "gamma rays, stars, radiation mechanisms, non-thermal",

author = "J. Greiner and Yu, \{H. -F.\} and T. Kr{\"u}hler and D.\textasciitilde{}D. Frederiks and A. Beloborodov and P.\textasciitilde{}N. Bhat and J. Bolmer and \{van Eerten\}, H. and R.\textasciitilde{}L. Aptekar and J. Elliott and S.\textasciitilde{}V. Golenetskii and J.\textasciitilde{}F. Graham and K. Hurley and D.\textasciitilde{}A. Kann and S. Klose and \{Nicuesa Guelbenzu\}, A. and A. Rau and P. Schady and S. Schmidl and V. Sudilovsky and D.\textasciitilde{}S. Svinkin and M. Tanga and M.\textasciitilde{}V. Ulanov and K. Varela and \{von Kienlin\}, A. and Zhang, \{X. -L.\}",

year = "2014",

month = aug,

day = "20",

doi = "10.1051/0004-6361/201424250",

language = "English",

volume = "568",

pages = "1--9",

journal = "Astronomy \& Astrophysics",

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TY - JOUR

T1 - GROND coverage of the main peak of gamma-ray burst 130925A

AU - Greiner, J.

AU - Yu, H. -F.

AU - Krühler, T.

AU - Frederiks, D.~D.

AU - Beloborodov, A.

AU - Bhat, P.~N.

AU - Bolmer, J.

AU - van Eerten, H.

AU - Aptekar, R.~L.

AU - Elliott, J.

AU - Golenetskii, S.~V.

AU - Graham, J.~F.

AU - Hurley, K.

AU - Kann, D.~A.

AU - Klose, S.

AU - Nicuesa Guelbenzu, A.

AU - Rau, A.

AU - Schady, P.

AU - Schmidl, S.

AU - Sudilovsky, V.

AU - Svinkin, D.~S.

AU - Tanga, M.

AU - Ulanov, M.~V.

AU - Varela, K.

AU - von Kienlin, A.

AU - Zhang, X. -L.

PY - 2014/8/20

Y1 - 2014/8/20

N2 - Aims.Prompt or early optical emission in gamma-ray bursts (GRBs) is notoriously difficult to measure, and observations of the dozen cases show a large variety of properties. Yet, such early emission promises to help us achieve a better understanding of the GRB emission process(es). Methods. We performed dedicated observations of the ultra-long duration (T90 about 7000 s) Swift GRB 130925A in the optical/near-infrared with the 7-channel Gamma-Ray burst Optical and Near-infrared Detector (GROND) at the 2.2 m MPG/ESO telescope. Results. We detect an optical/near-infrared flare with an amplitude of nearly 2 mag which is delayed with respect to the keV−MeV prompt emission by about 300−400 s. The decay time of this flare is shorter than the duration of the flare (500 s) or its delay. Conclusions. While we cannot offer a straightforward explanation, we discuss the implications of the flare properties and suggest ways toward understanding it.

AB - Aims.Prompt or early optical emission in gamma-ray bursts (GRBs) is notoriously difficult to measure, and observations of the dozen cases show a large variety of properties. Yet, such early emission promises to help us achieve a better understanding of the GRB emission process(es). Methods. We performed dedicated observations of the ultra-long duration (T90 about 7000 s) Swift GRB 130925A in the optical/near-infrared with the 7-channel Gamma-Ray burst Optical and Near-infrared Detector (GROND) at the 2.2 m MPG/ESO telescope. Results. We detect an optical/near-infrared flare with an amplitude of nearly 2 mag which is delayed with respect to the keV−MeV prompt emission by about 300−400 s. The decay time of this flare is shorter than the duration of the flare (500 s) or its delay. Conclusions. While we cannot offer a straightforward explanation, we discuss the implications of the flare properties and suggest ways toward understanding it.

KW - gamma rays

KW - stars

KW - radiation mechanisms

KW - non-thermal

U2 - 10.1051/0004-6361/201424250

DO - 10.1051/0004-6361/201424250

M3 - Article

SN - 0004-6361

VL - 568

SP - 1

EP - 9

JO - Astronomy & Astrophysics

JF - Astronomy & Astrophysics

M1 - A75

ER -

GROND coverage of the main peak of gamma-ray burst 130925A

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Keywords

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