Abstract
The long gamma-ray burst (GRB) 100621A, at the time the brightest X-ray transient ever detected by Swift-XRT in the 0.3-10 keV range, has been observed with the H.E.S.S. imaging air Cherenkov telescope array, sensitive to gamma radiation in the very-high-energy (VHE, >100 GeV) regime. Due to its relatively small redshift of z ~ 0.5, the favourable position in the southern sky and the relatively short follow-up time (<700 s after the satellite trigger) of the H.E.S.S. observations, this GRB could be within the sensitivity reach of the H.E.S.S. instrument. The analysis of the H.E.S.S. data shows no indication of emission and yields an integral flux upper limit above ~380 GeV of 4.2 × 10-12 cm-2 s-1 (95% confidence level), assuming a simple Band function extension model. A comparison to a spectral-temporal model, normalised to the prompt flux at sub-MeV energies, constraints the existence of a temporally extended and strong additional hard power law, as has been observed in the other bright X-ray GRB 130427A. A comparison between the H.E.S.S. upper limit and the contemporaneous energy output in X-rays constrains the ratio between the X-ray and VHE gamma-ray fluxes to be greater than 0.4. This value is an important quantity for modelling the afterglow and can constrain leptonic emission scenarios, where leptons are responsible for the X-ray emission and might produce VHE gamma rays.
| Original language | English (US) |
|---|---|
| Article number | A16 |
| Journal | Astronomy and Astrophysics |
| Volume | 565 |
| DOIs | |
| State | Published - May 2014 |
Keywords
- Gamma rays: general
- Gamma rays: stars
- Gamma-ray burst: individual: GRB 100621A
- X-rays: stars
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Search for TeV gamma-ray emission from GRB 100621A, an extremely bright GRB in X-rays, with H.E.S.S. / Abramowski, A.; Aharonian, F.; Ait Benkhali, F.; Akhperjanian, A. G.; Angüner, E.; Anton, G.; Balenderan, S.; Balzer, A.; Barnacka, A.; Becherini, Y.; Becker Tjus, J.; Bernlöhr, K.; Birsin, E.; Bissaldi, E.; Biteau, J.; Böttcher, M.; Boisson, C.; Bolmont, J.; Bordas, P.; Brucker, J.; Brun, F.; Brun, P.; Bulik, T.; Carrigan, S.; Casanova, S.; Cerruti, M.; Chadwick, P. M.; Chalme-Calvet, R.; Chaves, R. C G; Cheesebrough, A.; Chrétien, M.; Colafrancesco, S.; Cologna, G.; Conrad, J.; Couturier, C.; Dalton, M.; Daniel, M. K.; Davids, I. D.; Degrange, B.; Deil, C.; Dewilt, P.; Dickinson, H. J.; Djannati-Ataï, A.; Domainko, W.; Drury, L. O C; Dubus, G.; Dutson, K.; Dyks, J.; Dyrda, M.; Edwards, T.; Egberts, K.; Eger, P.; Espigat, P.; Farnier, C.; Fegan, S.; Feinstein, F.; Fernandes, M. V.; Fernandez, D.; Fiasson, A.; Fontaine, G.; Förster, A.; Füßling, M.; Gajdus, M.; Gallant, Y. A.; Garrigoux, T.; Giebels, B.; Glicenstein, J. F.; Grondin, M. H.; Grudzińska, M.; Häffner, S.; Hahn, J.; Harris, J.; Heinzelmann, G.; Henri, G.; Hermann, G.; Hervet, O.; Hillert, A.; Hinton, J. A.; Hofmann, W.; Hofverberg, P.; Holler, M.; Horns, D.; Jacholkowska, A.; Jahn, C.; Jamrozy, M.; Janiak, M.; Jankowsky, F.; Jung, I.; Kastendieck, M. A.; Katarzyński, K.; Katz, U.; Kaufmann, S.; Khélifi, B.; Kieffer, M.; Klepser, S.; Klochkov, D.; KluÅniak, W.; Kneiske, T.; Kolitzus, D.; Komin, Nu; Kosack, K.; Krakau, S.; Krayzel, F.; Krüger, P. P.; Laffon, H.; Lamanna, G.; Lefaucheur, J.; Lemière, A.; Lemoine-Goumard, M.; Lenain, J. P.; Lennarz, D.; Lohse, T.; Lopatin, A.; Lu, C. C.; Marandon, V.; Marcowith, A.; Marx, R.; Maurin, G.; Maxted, N.; Mayer, M.; McComb, T. J L; Méhault, J.; Menzler, U.; Meyer, M.; Moderski, R.; Mohamed, M.; Moulin, E.; Murach, T.; Naumann, C. L.; De Naurois, M.; Niemiec, J.; Nolan, S. J.; Oakes, L.; O'Brien, P. T.; Ohm, S.; De Oña Wilhelmi, E.; Opitz, B.; Ostrowski, M.; Oya, I.; Panter, M.; Parsons, R. D.; Paz Arribas, M.; Pekeur, N. W.; Pelletier, G.; Perez, J.; Petrucci, P. O.; Peyaud, B.; Pita, S.; Poon, H.; Pühlhofer, G.; Punch, M.; Quirrenbach, A.; Raab, S.; Raue, M.; Reimer, A.; Reimer, O.; Renaud, M.; De Los Reyes, R.; Rieger, F.; Rob, L.; Romoli, C.; Rosier-Lees, S.; Rowell, G.; Rudak, B.; Rulten, C. B.; Sahakian, V.; Sanchez, D. A.; Santangelo, A.; Schlickeiser, R.; Schüssler, F.; Schulz, A.; Schwanke, U.; Schwarzburg, S.; Schwemmer, S.; Sol, H.; Spengler, G.; Spies, F.; Stawarz, Å; Steenkamp, R.; Stegmann, C.; Stinzing, F.; Stycz, K.; Sushch, I.; Szostek, A.; Tam, P. H T; Tavernet, J. P.; Tavernier, T.; Taylor, A. M.; Terrier, R.; Tluczykont, M.; Trichard, C.; Valerius, K.; Van Eldik, C.; Vasileiadis, G.; Venter, C.; Viana, A.; Vincent, P.; Völk, H. J.; Volpe, F.; Vorster, M.; Wagner, S. J.; Wagner, P.; Ward, M.; Weidinger, M.; Weitzel, Q.; White, R.; Wierzcholska, A.; Willmann, P.; Wörnlein, A.; Wouters, D.; Zacharias, M.; Zajczyk, A.; Zdziarski, A. A.; Zech, A.; Zechlin, H. S.
In: Astronomy and Astrophysics, Vol. 565, A16, 05.2014.Research output: Contribution to journal › Article › peer-review
}
TY - JOUR
T1 - Search for TeV gamma-ray emission from GRB 100621A, an extremely bright GRB in X-rays, with H.E.S.S.
AU - Abramowski, A.
AU - Aharonian, F.
AU - Ait Benkhali, F.
AU - Akhperjanian, A. G.
AU - Angüner, E.
AU - Anton, G.
AU - Balenderan, S.
AU - Balzer, A.
AU - Barnacka, A.
AU - Becherini, Y.
AU - Becker Tjus, J.
AU - Bernlöhr, K.
AU - Birsin, E.
AU - Bissaldi, E.
AU - Biteau, J.
AU - Böttcher, M.
AU - Boisson, C.
AU - Bolmont, J.
AU - Bordas, P.
AU - Brucker, J.
AU - Brun, F.
AU - Brun, P.
AU - Bulik, T.
AU - Carrigan, S.
AU - Casanova, S.
AU - Cerruti, M.
AU - Chadwick, P. M.
AU - Chalme-Calvet, R.
AU - Chaves, R. C G
AU - Cheesebrough, A.
AU - Chrétien, M.
AU - Colafrancesco, S.
AU - Cologna, G.
AU - Conrad, J.
AU - Couturier, C.
AU - Dalton, M.
AU - Daniel, M. K.
AU - Davids, I. D.
AU - Degrange, B.
AU - Deil, C.
AU - Dewilt, P.
AU - Dickinson, H. J.
AU - Djannati-Ataï, A.
AU - Domainko, W.
AU - Drury, L. O C
AU - Dubus, G.
AU - Dutson, K.
AU - Dyks, J.
AU - Dyrda, M.
AU - Edwards, T.
AU - Egberts, K.
AU - Eger, P.
AU - Espigat, P.
AU - Farnier, C.
AU - Fegan, S.
AU - Feinstein, F.
AU - Fernandes, M. V.
AU - Fernandez, D.
AU - Fiasson, A.
AU - Fontaine, G.
AU - Förster, A.
AU - Füßling, M.
AU - Gajdus, M.
AU - Gallant, Y. A.
AU - Garrigoux, T.
AU - Giebels, B.
AU - Glicenstein, J. F.
AU - Grondin, M. H.
AU - Grudzińska, M.
AU - Häffner, S.
AU - Hahn, J.
AU - Harris, J.
AU - Heinzelmann, G.
AU - Henri, G.
AU - Hermann, G.
AU - Hervet, O.
AU - Hillert, A.
AU - Hinton, J. A.
AU - Hofmann, W.
AU - Hofverberg, P.
AU - Holler, M.
AU - Horns, D.
AU - Jacholkowska, A.
AU - Jahn, C.
AU - Jamrozy, M.
AU - Janiak, M.
AU - Jankowsky, F.
AU - Jung, I.
AU - Kastendieck, M. A.
AU - Katarzyński, K.
AU - Katz, U.
AU - Kaufmann, S.
AU - Khélifi, B.
AU - Kieffer, M.
AU - Klepser, S.
AU - Klochkov, D.
AU - KluÅniak, W.
AU - Kneiske, T.
AU - Kolitzus, D.
AU - Komin, Nu
AU - Kosack, K.
AU - Krakau, S.
AU - Krayzel, F.
AU - Krüger, P. P.
AU - Laffon, H.
AU - Lamanna, G.
AU - Lefaucheur, J.
AU - Lemière, A.
AU - Lemoine-Goumard, M.
AU - Lenain, J. P.
AU - Lennarz, D.
AU - Lohse, T.
AU - Lopatin, A.
AU - Lu, C. C.
AU - Marandon, V.
AU - Marcowith, A.
AU - Marx, R.
AU - Maurin, G.
AU - Maxted, N.
AU - Mayer, M.
AU - McComb, T. J L
AU - Méhault, J.
AU - Menzler, U.
AU - Meyer, M.
AU - Moderski, R.
AU - Mohamed, M.
AU - Moulin, E.
AU - Murach, T.
AU - Naumann, C. L.
AU - De Naurois, M.
AU - Niemiec, J.
AU - Nolan, S. J.
AU - Oakes, L.
AU - O'Brien, P. T.
AU - Ohm, S.
AU - De Oña Wilhelmi, E.
AU - Opitz, B.
AU - Ostrowski, M.
AU - Oya, I.
AU - Panter, M.
AU - Parsons, R. D.
AU - Paz Arribas, M.
AU - Pekeur, N. W.
AU - Pelletier, G.
AU - Perez, J.
AU - Petrucci, P. O.
AU - Peyaud, B.
AU - Pita, S.
AU - Poon, H.
AU - Pühlhofer, G.
AU - Punch, M.
AU - Quirrenbach, A.
AU - Raab, S.
AU - Raue, M.
AU - Reimer, A.
AU - Reimer, O.
AU - Renaud, M.
AU - De Los Reyes, R.
AU - Rieger, F.
AU - Rob, L.
AU - Romoli, C.
AU - Rosier-Lees, S.
AU - Rowell, G.
AU - Rudak, B.
AU - Rulten, C. B.
AU - Sahakian, V.
AU - Sanchez, D. A.
AU - Santangelo, A.
AU - Schlickeiser, R.
AU - Schüssler, F.
AU - Schulz, A.
AU - Schwanke, U.
AU - Schwarzburg, S.
AU - Schwemmer, S.
AU - Sol, H.
AU - Spengler, G.
AU - Spies, F.
AU - Stawarz, Å
AU - Steenkamp, R.
AU - Stegmann, C.
AU - Stinzing, F.
AU - Stycz, K.
AU - Sushch, I.
AU - Szostek, A.
AU - Tam, P. H T
AU - Tavernet, J. P.
AU - Tavernier, T.
AU - Taylor, A. M.
AU - Terrier, R.
AU - Tluczykont, M.
AU - Trichard, C.
AU - Valerius, K.
AU - Van Eldik, C.
AU - Vasileiadis, G.
AU - Venter, C.
AU - Viana, A.
AU - Vincent, P.
AU - Völk, H. J.
AU - Volpe, F.
AU - Vorster, M.
AU - Wagner, S. J.
AU - Wagner, P.
AU - Ward, M.
AU - Weidinger, M.
AU - Weitzel, Q.
AU - White, R.
AU - Wierzcholska, A.
AU - Willmann, P.
AU - Wörnlein, A.
AU - Wouters, D.
AU - Zacharias, M.
AU - Zajczyk, A.
AU - Zdziarski, A. A.
AU - Zech, A.
AU - Zechlin, H. S.
N1 - Copyright: Copyright 2014 Elsevier B.V., All rights reserved.
PY - 2014/5
Y1 - 2014/5
N2 - The long gamma-ray burst (GRB) 100621A, at the time the brightest X-ray transient ever detected by Swift-XRT in the 0.3-10 keV range, has been observed with the H.E.S.S. imaging air Cherenkov telescope array, sensitive to gamma radiation in the very-high-energy (VHE, >100 GeV) regime. Due to its relatively small redshift of z ~ 0.5, the favourable position in the southern sky and the relatively short follow-up time (<700 s after the satellite trigger) of the H.E.S.S. observations, this GRB could be within the sensitivity reach of the H.E.S.S. instrument. The analysis of the H.E.S.S. data shows no indication of emission and yields an integral flux upper limit above ~380 GeV of 4.2 × 10-12 cm-2 s-1 (95% confidence level), assuming a simple Band function extension model. A comparison to a spectral-temporal model, normalised to the prompt flux at sub-MeV energies, constraints the existence of a temporally extended and strong additional hard power law, as has been observed in the other bright X-ray GRB 130427A. A comparison between the H.E.S.S. upper limit and the contemporaneous energy output in X-rays constrains the ratio between the X-ray and VHE gamma-ray fluxes to be greater than 0.4. This value is an important quantity for modelling the afterglow and can constrain leptonic emission scenarios, where leptons are responsible for the X-ray emission and might produce VHE gamma rays.
AB - The long gamma-ray burst (GRB) 100621A, at the time the brightest X-ray transient ever detected by Swift-XRT in the 0.3-10 keV range, has been observed with the H.E.S.S. imaging air Cherenkov telescope array, sensitive to gamma radiation in the very-high-energy (VHE, >100 GeV) regime. Due to its relatively small redshift of z ~ 0.5, the favourable position in the southern sky and the relatively short follow-up time (<700 s after the satellite trigger) of the H.E.S.S. observations, this GRB could be within the sensitivity reach of the H.E.S.S. instrument. The analysis of the H.E.S.S. data shows no indication of emission and yields an integral flux upper limit above ~380 GeV of 4.2 × 10-12 cm-2 s-1 (95% confidence level), assuming a simple Band function extension model. A comparison to a spectral-temporal model, normalised to the prompt flux at sub-MeV energies, constraints the existence of a temporally extended and strong additional hard power law, as has been observed in the other bright X-ray GRB 130427A. A comparison between the H.E.S.S. upper limit and the contemporaneous energy output in X-rays constrains the ratio between the X-ray and VHE gamma-ray fluxes to be greater than 0.4. This value is an important quantity for modelling the afterglow and can constrain leptonic emission scenarios, where leptons are responsible for the X-ray emission and might produce VHE gamma rays.
KW - Gamma rays: general
KW - Gamma rays: stars
KW - Gamma-ray burst: individual: GRB 100621A
KW - X-rays: stars
UR - http://www.scopus.com/inward/record.url?scp=84899126766&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=84899126766&partnerID=8YFLogxK
U2 - 10.1051/0004-6361/201322984
DO - 10.1051/0004-6361/201322984
M3 - Article
AN - SCOPUS:84899126766
VL - 565
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
SN - 0004-6361
M1 - A16
ER -