<i>FERMI</i>
                    OBSERVATIONS OF GRB 090902B: A DISTINCT SPECTRAL COMPONENT IN THE PROMPT AND DELAYED EMISSION

Abdo, A. A.; Ackermann, M.; Ajello, M.; Asano, Katsuaki; Atwood, W. B.; Axelsson, M.; Baldini, Luca; Ballet, J.; Barbiellini, G.; Baring, Matthew G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Bhat, P. N.; Bissaldi, E.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Bregeon, J.; Brez, A.; Briggs, M. S.; Brigida, M.; Bruel, Pascal; Burgess, J. Michael; Burrows, D. N.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; Çelik, Ö.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Cominsky, L.; Connaughton, V.; Conrad, J.; Cutini, S.; D’Elia, V.; Dermer, C. D.; Angelis, A. De; Palma, F. de; Digel, S. W.; Dingus, B. L.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Finke, J.; Fishman, G. J.; Focke, W. B.; Fortin, P.; Frailis, M.; Fukazawa, Yasushi; Funk, S.; Fusco, P.; Gargano, F.; Gehrels, N.; Germani, S.; Giavitto, G.; Giebels, B.; Giglietto, N.; Giordano, F.; Glanzman, T.; Godfrey, G.; Goldstein, A.; Granot, Jonathan; Greiner, J.; Grenier, I. A.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hanabata, Y.; Harding, A. K.; Hayashida, M.; Hays, E.; Horan, D.; Hughes, R. E.; Jackson, M. S.; Jóhannesson, G.; Johnson, A. S.; Johnson, R. P.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kerr, M.; Kippen, R. M.; Knödlseder, J.; Kocevski, D.; Komin, Nu.; Kouveliotou, C.; Kuss, M.; Landé, J.; Latronico, L.; Lemoine‐Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G.; Makeev, A.; Mazziotta, M. N.; McBreen, S.; McEnery, J. E.; McGlynn, S.; Meegan, C.; Mészáros, P.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Моисеев, А. А.; Monte, C.; Monzani, M. E.; Moretti, E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, Takeshi; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohno, M.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Pačiesas, W. S.; Paneque, D.; Panetta, J.; Pelassa, V.; Pepé, M.; Pesce-Rollins, M.; Petrosian, V.; Piron, F.; Porter, T. A.; Preece, R.; Rainò, S.; Rando, R.; Rau, A.; Razzano, M.; Razzaque, S.; Reimer, A.; Reposeur, T.; Ritz, S.; Rochester, Lynn; Rodriguez, A. Y.; Roming, P. W. A.; Roth, M.; Ryde, F.; Sadrozinski, H. F-W.; Sánchez, David; Sander, A.; Parkinson, P. M. Saz; Scargle, Jeffrey D.; Schalk, T.; Sgrò, C.; Siskind, E. J.; Smith, P. D.; Spinelli, P.; Stamatikos, M.; Stecker, F. W.; Stratta, G.; Strickman, M. S.; Suson, D. J.; Swenson, C. A.; Tajima, H.; Takahashi, H.; Tanaka, Takaaki; Thayer, J. B.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Uehara, T.; Usher, T.; Horst, A. J. van der; Vasileiou, V.; Vilchez, N.; Vitale, V.; Kienlin, A. von; Waite, A. P.; Wang, P.; Wilson-Hodge, C.; Winer, B. L.; Wood, K. S.; Yamazaki, Ryo; Ylinen, T.; Ziegler, M.

doi:10.1088/0004-637x/706/1/l138

Cited by 406 publications

(330 citation statements)

References 25 publications

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“…Observations suggest that a GRB central engine should satisfy the following requirements: (1) It can drive an outflow with extremely high luminosity and energy. If the emission is isotropically distributed in all directions, the required jet luminosity ranges from Liso ∼ 10 47 − 10 54 erg s −1 , and the total gamma-ray energy ranges from Eiso ∼ 10 49 − 10 55 erg [80,81]; (2) The ejecta need to be "clean" with small baryon contamination, so that they can achieve a relativistic speed, with Lorentz factor Γ typically greater than 100 [82,83,84], some even close to 1000 [85,86,87]; (3) The outflow needs to be collimated, with a beaming factor f = ∆Ω/4π ∼ 1/500 for bright GRBs [88,89,90,91], so that the real luminosity and energy of a GRB is reduced by this factor; (4) The engine needs in general to be intermittent, with a range of variability time scales [80,92]. In some GRBs, the engine can generate smooth (but varying) lightcurves [93,14]; (5) The engine can last long, with renewed, progressively less powerful late activities to power X-ray flares and other activities (see §2.7 for full discussion).…”

Section: Central Enginementioning

confidence: 99%

“…The Large Area Telescope (LAT) on board Fermi makes it possible to detect high energy emission from GRBs regularly. Although somewhat lower than the pre-launch predictions, the current detection rate of ∼ 9 per year allows collection of a moderate sample of GRBs with detected emission above 100 MeV [85,86,87,158,155]. A dedicated review on Fermi LAT GRB science can be also found in this volume [317].…”

Section: Origin Of High Energy Emissionmentioning

confidence: 99%

See 1 more Smart Citation

Open questions in GRB physics

Zhang

2011

Comptes Rendus. Physique

126

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Open questions in GRB physics are summarized as of 2011, including classification, progenitor, central engine, ejecta composition, energy dissipation and particle acceleration mechanism, radiation mechanism, long term engine activity, external shock afterglow physics, origin of high energy emission, and cosmological setting. Prospects of addressing some of these problems with the upcoming Chinese-French GRB mission, SVOM, are outlined.

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Section: Central Enginementioning

confidence: 99%

Section: Origin Of High Energy Emissionmentioning

confidence: 99%

Open questions in GRB physics

Zhang

2011

Comptes Rendus. Physique

126

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“…Four large photomultiplier tubes (PMTs) will be located near the bottom of each tank. 1 The PMTs capture Cherenkov light produced in water by the charged particles that compose an extensive air shower. Hit arrival times are used to reconstruct the incident direction of the shower.…”

Section: The Hawc Observatorymentioning

confidence: 99%

“…In particular, a hard power law component was detected in the spectra of the long GRB 090902B [1] and the short GRB 090510 [2]. The highest energy photon recorded from GRB 090902B was 33 GeV, or 94 GeV corrected for redshift.…”

Section: Introductionmentioning

confidence: 98%

The HAWC experiment and its sensitivity to gamma-ray bursts

Zaborov¹

2012

Proceedings of Gamma-Ray Bursts 2012 Conference — PoS(GRB 2012)

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The High Altitude Water Cherenkov Observatory (HAWC) is an air shower array currently under construction in Mexico at an altitude of 4100 m. HAWC will consist of 300 large water tanks covering an area of about 22000 square meters and instrumented with 4 photomultipliers each. The experimental design allows for highly efficient detection of photon-induced air showers in the TeV and sub-TeV range and gamma-hadron separation. We show that HAWC has a realistic opportunity to observe the high-energy power law components of GRBs that extend at least up to 30 GeV. In particular, HAWC will be capable of observing events similar to GRB 090510 and GRB 090902B. The observations (or non-observations) of GRBs by HAWC will provide information on the high-energy spectra of GRBs. An engineering array consisting of 6 water tanks was operated at the HAWC site since September 2011, collecting over 3 months of data. An upper limit on high energy emission from GRB 111016B is derived from these data.

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“…For this catalog, the LAT team has used the term "associations" for sources that have positional agreements with known objects, reserving the term "identifications" for sources with time variability, spectral, or spatial features that provide stron ger evidence about the nature of the source. Abdo et al, 2009e). …”

Section: Overview Of the Gamma-ray Skymentioning

confidence: 99%

Highlights of GeV gamma-ray astronomy

Thompson

2010

Astrophys. Space Sci. Trans.

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Abstract. Because high-energy gamma rays are primarily produced by high-energy particle interactions, the gammaray survey of the sky by the Fermi Gamma-ray Space Telescope offers a view of sites of cosmic ray production and interactions. Gamma-ray bursts, pulsars, pulsar wind nebulae, binary sources, and Active Galactic Nuclei are all phenomena that reveal particle acceleration through their gamma-ray emission. Diffuse Galactic gamma radiation, Solar System gamuna-ray sources, and energetic radiation from supernova remnants are likely tracers of high-energy particle interactions with matter and photon fields. This paper will present a broad overview of the constantly chan ging sky seen with the Large Area Telescope (LAT) on the Fem7i spacecraft.

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FERMI OBSERVATIONS OF GRB 090902B: A DISTINCT SPECTRAL COMPONENT IN THE PROMPT AND DELAYED EMISSION

Cited by 406 publications

References 25 publications

Open questions in GRB physics

Open questions in GRB physics

The HAWC experiment and its sensitivity to gamma-ray bursts

Highlights of GeV gamma-ray astronomy

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