Author: "Granot, J" - Searchworks@Jio Institute Digital Library Search Results

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698 results on '"Granot, J"'

201. Radio limits on off-axis GRB afterglows and VLBI observations of SN 2003gk

Author: Bietenholz, M. F., De Colle, F., Granot, J., Bartel, N., Soderberg, A. M., Bietenholz, M. F., De Colle, F., Granot, J., Bartel, N., and Soderberg, A. M.
Abstract: We report on a VLA survey for late-time radio emission from 59 supernovae (SNe) of Type I b/c, which have been associated with long-duration gamma-ray bursts (GRBs). An "off-axis" GRB burst (i.e. whose relativistic jet points away from us) is expected to have late-time radio emission even in the absence of significant prompt gamma-ray emission. From our sample, we detected only SN 2003gk with an 8.4-GHz flux density of $2260 \pm 130 \,\mu$Jy. Our subsequent VLBI observations of SN 2003gk, at an age of $\sim$8 yr, allowed us to determine its radius to be $(2.4 \pm 0.4) \times 10^{17}$ cm, or $94 \pm 15$ light days. This radius rules out relativistic expansion as expected for an off-axis GRB jet, and instead suggests an expansion speed of $\sim 10\:000$ km s$^{-1}$ typical for non-relativistic core-collapse supernovae. We attribute the late-onset radio emission to interaction of the ejecta with a dense shell caused by episodic mass-loss from the progenitor. In addition, we present new calculations for the expected radio lightcurves from GRB jets at various angles to the line of sight, and compare these to our observed limits on the flux densities of the remainder of our SN sample. From this comparison we can say that only a fraction of broadlined Type I b/c SNe have a radio-bright jet similar to those seen for GRB afterglows at cosmological distances. However, we also find that for a reasonable range of parameters, as might be representative of the actual population of GRB events rather than the detected bright ones, the radio emission from the GRB jets can be quite faint, and that at present, radio observations do not place strong constraints on off-axis GRB jets., Comment: 12 Pages, 6 figures; accepted for publication in MNRAS
Published: 2013
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202. Broadband monitoring tracing the evolution of the jet and disk in the black hole candidate X-ray binary MAXI J1659-152

Author: van der Horst, A. J., Curran, P. A., Miller-Jones, J. C. A., Linford, J. D., Gorosabel, J., Russell, D. M., Postigo, A. de Ugarte, Lundgren, A. A., Taylor, G. B., Maitra, D., Guziy, S., Belloni, T. M., Kouveliotou, C., Jonker, P. G., Kamble, A., Paragi, Z., Homan, J., Kuulkers, E., Granot, J., Altamirano, D., Buxton, M. M., Castro-Tirado, A., Fender, R. P., Garrett, M. A., Gehrels, N., Hartmann, D. H., Kennea, J. A., Krimm, H. A., Mangano, V., Ramirez-Ruiz, E., Romano, P., Wijers, R. A. M. J., Wijnands, R., Yang, Y. J., van der Horst, A. J., Curran, P. A., Miller-Jones, J. C. A., Linford, J. D., Gorosabel, J., Russell, D. M., Postigo, A. de Ugarte, Lundgren, A. A., Taylor, G. B., Maitra, D., Guziy, S., Belloni, T. M., Kouveliotou, C., Jonker, P. G., Kamble, A., Paragi, Z., Homan, J., Kuulkers, E., Granot, J., Altamirano, D., Buxton, M. M., Castro-Tirado, A., Fender, R. P., Garrett, M. A., Gehrels, N., Hartmann, D. H., Kennea, J. A., Krimm, H. A., Mangano, V., Ramirez-Ruiz, E., Romano, P., Wijers, R. A. M. J., Wijnands, R., and Yang, Y. J.
Abstract: MAXI J1659-152 was discovered on 2010 September 25 as a new X-ray transient, initially identified as a gamma-ray burst, but was later shown to be a new X-ray binary with a black hole as the most likely compact object. Dips in the X-ray light curves have revealed that MAXI J1659-152 is the shortest period black hole candidate identified to date. Here we present the results of a large observing campaign at radio, sub-millimeter, near-infrared (nIR), optical and ultraviolet (UV) wavelengths. We have combined this very rich data set with the available X-ray observations to compile a broadband picture of the evolution of this outburst. We have performed broadband spectral modeling, demonstrating the presence of a spectral break at radio frequencies and a relationship between the radio spectrum and X-ray states. Also, we have determined physical parameters of the accretion disk and put them into context with respect to the other parameters of the binary system. Finally, we have investigated the radio-X-ray and nIR/optical/UV-X-ray correlations up to ~3 years after the outburst onset to examine the link between the jet and the accretion disk, and found that there is no significant jet contribution to the nIR emission when the source is in the soft or intermediate X-ray spectral state, consistent with our detection of the jet break at radio frequencies during these states., Comment: 18 pages, 8 figures, 2 tables; accepted for publication in MNRAS after minor revisions
Published: 2013
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203. New Fermi-LAT event reconstruction reveals more high-energy gamma rays from Gamma-ray bursts

Author: Atwood, W. B., Baldini, L., Bregeon, J., Bruel, P., Chekhtman, A., Cohen-Tanugi, J., Drlica-Wagner, A., Granot, J., Longo, F., Omodei, N., Pesce-Rollins, M., Razzaque, S., Rochester, L. S., Sgro, C., Tinivella, M., Usher, T. L., Zimmer, S., Atwood, W. B., Baldini, L., Bregeon, J., Bruel, P., Chekhtman, A., Cohen-Tanugi, J., Drlica-Wagner, A., Granot, J., Longo, F., Omodei, N., Pesce-Rollins, M., Razzaque, S., Rochester, L. S., Sgro, C., Tinivella, M., Usher, T. L., and Zimmer, S.
Abstract: Based on the experience gained during the four and a half years of the mission, the Fermi -LAT collaboration has undertaken a comprehensive revision of the event-level analysis going under the name of Pass 8. Although it is not yet finalized, we can test the improvements in the new event reconstruction with the special case of the prompt phase of bright Gamma-Ray Bursts (GRBs), where the signal to noise ratio is large enough that loose selection cuts are sufficient to identify gamma- rays associated with the source. Using the new event reconstruction, we have re-analyzed ten GRBs previously detected by the LAT for which an x-ray/optical follow-up was possible and found four new gamma rays with energies greater than 10 GeV in addition to the seven previously known. Among these four is a 27.4 GeV gamma-ray from GRB 080916C, which has a redshift of 4.35, thus making it the gamma ray with the highest intrinsic energy (147 GeV) detected from a GRB. We present here the salient aspects of the new event reconstruction and discuss the scientific implications of these new high-energy gamma rays, such as constraining extragalactic background light models, Lorentz invariance violation (LIV) tests, the prompt emission mechanism and the bulk Lorentz factor of the emitting region., Comment: 6 pages, 2 figures, accepted by ApJ
Published: 2013
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204. VLBI observations of the shortest orbital period black hole binary, MAXI J1659-152

Author: Paragi, Z., van der Horst, A. J., Belloni, T., Miller-Jones, J. C. A., Linford, J., Taylor, G., Yang, J., Garrett, M. A., Granot, J., Kouveliotou, C., Kuulkers, E., Wijers, R. A. M. J., Paragi, Z., van der Horst, A. J., Belloni, T., Miller-Jones, J. C. A., Linford, J., Taylor, G., Yang, J., Garrett, M. A., Granot, J., Kouveliotou, C., Kuulkers, E., and Wijers, R. A. M. J.
Abstract: The X-ray transient MAXI J1659-152 was discovered by Swift/BAT and it was initially identified as a GRB. Soon its Galactic origin and binary nature were established. There exists a wealth of multi-wavelength monitoring data for this source, providing a great coverage of the full X-ray transition in this candidate black hole binary system. We obtained two epochs of European VLBI Network (EVN) electronic-VLBI (e-VLBI) and four epochs of Very Long Baseline Array (VLBA) data of MAXI J1659-152 which show evidence for outflow in the early phases. The overall source properties (polarization, milliarcsecond-scale radio structure, flat radio spectrum) are described well with the presence of a compact jet in the system through the transition from the hard-intermediate to the soft X-ray spectral state. The apparent dependence of source size and the radio core position on the observed flux density (luminosity dependent core shift) support this interpretation as well. We see no evidence for major discrete ejecta during the outburst. For the source proper motion we derive 2 sigma upper limits of 115 microas/day in right ascension, and 37 microas/day in declination, over a time baseline of 12 days. These correspond to velocities of 1400 km/s and 440 km/s, respectively, assuming a source distance of 7 kpc., Comment: 12 pages, 6 figures, 1 table. Accepted for publication in MNRAS
Published: 2013
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205. Introducing the CTA concept

Author: Acharya, B. S., Actis, M., Aghajani, T., Agnetta, G., Aguilar, J., Aharonian, F., Ajello, M., Akhperjanian, A., Alcubierre, M., Aleksic, J., Alfaro, R., Aliu, E., Allafort, A. J., Allan, D., Allekotte, I., Amato, E., Anderson, J., Anguener, E. O., Antonelli, L. A., Antoranz, P., Aravantinos, A., Arlen, T., Armstrong, T., Arnaldi, H., Arrabito, L., Asano, K., Ashton, T., Asorey, H. G., Awane, Y., Baba, H., Babic, A., Baby, N., Baehr, J., Bais, A., Baixeras, C., Bajtlik, S., Balbo, M., Balis, D., Balkowski, C., Bamba, A., Bandiera, R., Barber, A., Barbier, C., Barcelo, M., Barnacka, A., Barnstedt, J., Barres de Almeida, U., Barrio, J. A., Basili, A., Basso, S., Bastieri, D., Bauer, C., Baushev, A., Becerra, J., Becherini, Yvonne, Bechtol, K. C., Tjus, J. Becker, Beckmann, V., Bednarek, W., Behera, B., Belluso, M., Benbow, W., Berdugo, J., Berger, K., Bernard, F., Bernardino, T., Bernloehr, K., Bhat, N., Bhattacharyya, S., Bigongiari, C., Biland, A., Billotta, S., Bird, T., Birsin, E., Bissaldi, E., Biteau, J., Bitossi, M., Blake, S., Blanch Bigas, O., Blasi, P., Bobkov, A., Boccone, V., Boettcher, M., Bogacz, L., Bogart, J., Bogdan, M., Boisson, C., Boix Gargallo, J., Bolmont, J., Bonanno, G., Bonardi, A., Bonev, T., Bonifacio, P., Bonnoli, G., Bordas, P., Borgland, A., Borkowski, J., Bose, R., Botner, O., Bottani, A., Bouchet, L., Bourgeat, M., Boutonnet, C., Bouvier, A., Brau-Nogue, S., Braun, I., Bretz, T., Briggs, M., Bringmann, T., Brook, P., Brun, P., Brunetti, L., Buanes, T., Buckley, J., Buehler, R., Bugaev, V., Bulgarelli, A., Bulik, T., Busetto, G., Buson, S., Byrum, K., Cailles, M., Cameron, R., Camprecios, J., Canestrari, R., Cantu, S., Capalbi, M., Caraveo, P., Carmona, E., Carosi, A., Carr, J., Carton, P. -H, Casanova, S., Casiraghi, M., Catalano, O., Cavazzani, S., Cazaux, S., Cerruti, M., Chabanne, E., Chadwick, P., Champion, C., Chen, A., Chiang, J., Chiappetti, L., Chikawa, M., Chitnis, V. R., Chollet, F., Chudoba, J., Cieslar, M., Cillis, A., Cohen-Tanugi, J., Colafrancesco, S., Colin, P., Calome, J., Colonges, S., Compin, M., Conconi, P., Conforti, V., Connaughton, V., Conrad, J., Contreras, J. L., Coppi, P., Corona, P., Corti, D., Cortina, J., Cossio, L., Costantini, H., Cotter, G., Courty, B., Couturier, S., Covino, S., Crimi, G., Criswell, S. J., Croston, J., Cusumano, G., Dafonseca, M., Dale, O., Daniel, M., Darling, J., Davids, I., Dazzi, F., De Angelis, A., De Caprio, V., De Frondat, F., de Gouveia Dal Pino, E. M., de la Calle, I., De La Vega, G. A., Lopez, R. de los Reyes, De Lotto, B., De Luca, A., de Mello Neto, J. R. T., de Naurois, M., de Oliveira, Y., de Ona Wilhelmi, E., de Souza, V., Decerprit, G., Decock, G., Deil, C., Delagnes, E., Deleglise, G., Delgado, C., Della Volpe, D., Demange, P., Depaola, G., Dettlaff, A., Di Paola, A., Di Pierro, F., Diaz, C., Dick, J., Dickherber, R., Dickinson, H., Diez-Blanco, V., Digel, S., Dimitrov, D., Disset, G., Djannati-Atai, A., Doert, M., Dohmke, M., Domainko, W., Prester, D. Dominis, Donat, A., Dorner, D., Doro, M., Dournaux, J-L, Drake, G., Dravins, D., Drury, L., Dubois, F., Dubois, R., Dubus, G., Dufour, C., Dumas, D., Dumm, J., Durand, D., Dyks, J., Dyrda, M., Ebr, J., Edy, E., Egberts, K., Eger, P., Einecke, S., Eleftheriadis, C., Elles, S., Emmanoulopoulos, D., Engelhaupt, D., Enomoto, R., Ernenwein, J-P, Errando, M., Etchegoyen, A., Evans, P., Falcone, A., Fantinel, D., Farakos, K., Farnier, C., Fasola, G., Favill, B., Fede, E., Federici, S., Fegan, S., Feinstein, F., Ferenc, D., Ferrando, P., Fesquet, M., Fiasson, A., Fillin-Martino, E., Fink, D., Finley, C., Finley, J. P., Fiorini, M., Firpo Curcoll, R., Flores, H., Florin, D., Focke, W., Foehr, C., Fokitis, E., Font, L., Fontaine, G., Fornasa, M., Foerster, A., Fortson, L., Fouque, N., Franckowiak, A., Fransson, C., Fraser, G., Frei, R., Albuquerque, I. F. M., Fresnillo, L., Fruck, C., Fujita, Y., Fukazawa, Y., Fukui, Y., Funk, S., Gaebele, W., Gabici, S., Gabriele, R., Gadola, A., Galante, N., Gall, D., Gallant, Y., Gamez-Garcia, J., Garcia, B., Garcia Lopez, R., Gardiol, D., Garrido, D., Garrido, L., Gascon, D., Gaug, M., Gaweda, J., Gebremedhin, L., Geffroy, N., Gerard, L., Ghedina, A., Ghigo, M., Giannakaki, E., Gianotti, F., Giarrusso, S., Giavitto, G., Giebels, B., Gika, V., Giommi, P., Girard, N., Giro, E., Giuliani, A., Glanzman, T., Glicenstein, J. -F, Godinovic, N., Golev, V., Gomez Berisso, M., Gomez-Ortega, J., Gonzalez, M. M., Gonzalez, A., Gonzalez, F., Gonzalez Munoz, A., Gothe, K. S., Gougerot, M., Graciani, R., Grandi, P., Granena, F., Granot, J., Grasseau, G., Gredig, R., Green, A., Greenshaw, T., Gregoire, T., Grimm, O., Grube, J., Grudzinska, M., Gruev, V., Gruenewald, S., Grygorczuk, J., Guarino, V., Gunji, S., Gyuk, G., Hadasch, D., Hagiwara, R., Hahn, J., Hakansson, N., Hallgren, A., Hamer Heras, N., Hara, S., Hardcastle, M. J., Harris, J., Hassan, T., Hatanaka, K., Haubold, T., Haupt, A., Hayakawa, T., Hayashida, M., Heller, R., Henault, F., Henri, G., Hermann, G., Hermel, R., Herrero, A., Hidaka, N., Hinton, J., Hoffmann, D., Hofmann, W., Hofverberg, P., Holder, J., Horns, D., Horville, D., Houles, J., Hrabovsky, M., Hrupec, D., Huan, H., Huber, B., Huet, J. -M, Hughes, G., Humensky, T. B., Huovelin, J., Ibarra, A., Illa, J. M., Impiombato, D., Incorvaia, S., Inoue, S., Inoue, Y., Ioka, K., Ismailova, E., Jablonski, C., Jacholkowska, A., Jamrozy, M., Janiak, M., Jean, P., Jeanney, C., Jimenez, J. J., Jogler, T., Johnson, T., Journet, L., Juffroy, C., Jung, I., Kaaret, P., Kabuki, S., Kagaya, M., Kakuwa, J., Kalkuhl, C., Kankanyan, R., Karastergiou, A., Kaercher, K., Karczewski, M., Karkar, S., Kasperek, Aci., Kastana, D., Katagiri, H., Kataoka, J., Katarzynski, K., Katz, U., Kawanaka, N., Kellner-Leidel, B., Kelly, H., Kendziorra, E., Khelifi, B., Kieda, D. B., Kifune, T., Kihm, T., Kishimoto, T., Kitamoto, K., Kluzniak, W., Knapic, C., Knapp, J. w, Knoedlseder, J., Koeck, F., Kocot, J., Kodani, K., Koehne, J. -H, Kohri, K., Kokkotas, K., Kolitzus, D., Komin, N., Kominis, I., Konno, Y., Koeppel, H., Korohoda, P., Kosack, K., Koss, G., Kossakowski, R., Kostka, P., Koul, R., Kowal, G., Koyama, S., Koziol, J., Kraehenbuehl, T., Krause, J., Krawzcynski, H., Krennrich, F., Krepps, A., Kretzschmann, A., Krobot, R., Krueger, P., Kubo, H., Kudryavtsev, V. A., Kushida, J., Kuznetsov, A., La Barbera, A., La Palombara, N., La Parola, V., La Rosa, G., Lacombe, K., Lamanna, G., Lande, J., Languignon, D., Lapington, J., Laporte, P., Lavalley, C., Le Flour, T., Le Padellec, A., Lee, S. -H, Lee, W. H., Leigui de Oliveira, M. A., Lelas, D., Lenain, J. -P, Leopold, D. J., Lerch, T., Lessio, L., Lieunard, B., Lindfors, E., Liolios, A., Lipniacka, A., Lockart, H., Lohse, T., Lombardi, S., Lopatin, A., Lopez, M., Lopez-Coto, R., Lopez-Oramas, A., Lorca, A., Lorenz, E., Lubinski, P., Lucarelli, F., Luedecke, H., Ludwin, J., Luque-Escamilla, P. L., Lustermann, W., Luz, O., Lyard, E., Maccarone, M. C., Maccarone, T. J., Madejski, G. M., Madhavan, A., Mahabir, M., Maier, G., Majumdar, P., Malaguti, G., Maltezos, S., Manalaysay, A., Mancilla, A., Mandat, D., Maneva, G., Mangano, A., Manigot, P., Mannheim, K., Manthos, I., Maragos, N., Marcowith, A., Mariotti, M., Marisaldi, M., Markoff, S., Marszalek, A., Martens, C., Marti, J., Martin, J-M, Martin, P., Martinez, G., Martinez, F., Martinez, M., Masserot, A., Mastichiadis, A., Mathieu, A., Matsumoto, H., Mattana, F., Mattiazzo, S., Maurin, G., Maxfield, S., Maya, J., Mazin, D., Mc Comb, L., McCubbin, N., McHardy, I., McKay, R., Medina, C., Melioli, C., Melkumyan, D., Mereghetti, S., Mertsch, P., Meucci, M., Michalowski, J., Micolon, P., Mihailidis, A., Mineo, T., Minuti, M., Mirabal, N., Mirabel, F., Miranda, J. M., Mirzoyan, R., Mizuno, T., Moal, B., Moderski, R., Mognet, I., Molinari, E., Molinaro, M., Montaruli, T., Monteiro, I., Moore, P., Moralejo Olaizola, A., Mordalska, M., Morello, C., Mori, K., Mottez, F., Moudden, Y., Moulin, E., Mrusek, I., Mukherjee, R., Munar-Adrover, P., Muraishi, H., Murase, K., Murphy, A., Nagataki, S., Naito, T., Nakajima, D., Nakamori, T., Nakayama, K., Naumann, C., Naumann, D., Naumann-Godo, M., Nayman, P., Nedbal, D., Neise, D., Nellen, L., Neustroev, V., Neyroud, N., Nicastro, L., Nicolau-Kuklinski, J., Niedzwiecki, A., Niemiec, J., Nieto, D., Nikolaidis, A., Nishijima, K., Nolan, S., Northrop, R., Nosek, D., Nowak, N., Nozato, A., O'Brien, P., Ohira, Y., Ohishi, M., Ohm, S., Ohoka, H., Okuda, T., Okumura, A., Olive, J. -F, Ong, R. A., Orito, R., Orr, M., Osborne, J., Ostrowski, M., Otero, L. A., Otte, N., Ovcharov, E., Oya, I., Ozieblo, A., Padilla, L., Paiano, S., Paillot, D., Paizis, A., Palanque, S., Palatka, M., Pallota, J., Panagiotidis, K., Panazol, J. -L, Paneque, D., Panter, M., Paoletti, R., Papayannis, A., Papyan, G., Paredes, J. M., Pareschi, G., Parks, G., Parraud, J. -M, Parsons, D., Arribas, M. Paz, Pech, M., Pedaletti, G., Pelassa, V., Pelat, D., Perez, M. D. C., Persic, M., Petrucci, P-O, Peyaud, B., Pichel, A., Pita, S., Pizzolato, F., Platos, L., Platzer, R., Pogosyan, L., Pohl, M., Pojmanski, G., Ponz, J. D., Potter, W., Poutanen, J., Prandini, E., Prast, J., Preece, R., Profeti, F., Prokoph, Heike, Prouza, M., Proyetti, M., Puerto-Gimenez, I., Puehlhofer, G., Puljak, I., Punch, Michael, Pyziol, R., Quel, E. J., Quinn, J., Quirrenbach, A., Racero, E., Rajda, P. J., Ramon, P., Rando, R., Rannot, R. C., Rataj, M., Raue, M., Reardon, P., Reimann, O., Reimer, A., Reimer, O., Reitberger, K., Renaud, M., Renner, S., Reville, B., Rhode, W., Ribo, M., Ribordy, M., Richer, M. G., Rico, J., Ridky, J., Rieger, F., Ringegni, P., Ripken, J., Ristori, P. R., Riviere, A., Rivoire, S., Rob, L., Roeser, U., Rohlfs, R., Rojas, G., Romano, P., Romaszkan, W., Romero, G. E., Rosen, S., Lees, S. Rosier, Ross, D., Rouaix, G., Rousselle, J., Rousselle, S., Rovero, A. C., Roy, F., Royer, S., Rudak, B., Rulten, C., Rupinski, M., Russo, F., Ryde, F., Sacco, B., Saemann, E. O., Saggion, A., Safiakian, V., Saito, K., Saito, T., Saito, Y., Sakaki, N., Sakonaka, R., Salini, A., Sanchez, F., Sanchez-Conde, M., Sandoval, A., Sandaker, H., Sant'Ambrogio, E., Santangelo, A., Santos, E. M., Sanuy, A., Sapozhnikov, L., Sarkar, S., Sartore, N., Sasaki, H., Satalecka, K., Sawada, M., Scalzotto, V., Scapin, V., Scarcioffolo, M., Schafer, J., Schanz, T., Schlenstedt, S., Schlickeiser, R., Schmidt, T., Schmoll, J., Schovanek, P., Schroedter, M., Schultz, C., Schultze, J., Schulz, A., Schure, K., Schwab, T., Schwanke, U., Schwarz, J., Schwarzburg, S., Schweizer, T., Schwemmer, S., Segreto, A., Seiradakis, J. -H, Sembroski, G. H., Seweryn, K., Sharma, M., Shayduk, M., Shellard, R. C., Shi, J., Shibata, T., Shibuya, A., Shum, E., Sidoli, L., Sidz, M., Sieiro, J., Sikora, M., Silk, J., Sillanpaa, A., Singh, B. B., Sitarek, J., Skole, C., Smareglia, R., Smith, A., Smith, D., Smith, J., Smith, N., Sobczynska, D., Sol, H., Sottile, G., Sowinski, M., Spanier, F., Spiga, D., Spyrou, S., Stamatescu, V., Stamerra, A., Starling, R., Stawarz, L., Steenkamp, R., Stegmann, C., Steiner, S., Stergioulas, N., Sternberger, R., Sterzel, M., Stinzing, F., Stodulski, M., Straumann, U., Strazzeri, E., Stringhetti, L., Suarez, A., Suchenek, M., Sugawara, R., Sulanke, K. -H, Sun, S., Supanitsky, A. D., Suric, T., Sutcliffe, P., Sykes, J., Szanecki, M., Szepieniec, T., Szostek, A., Tagliaferri, G., Tajima, H., Takahashi, H., Takahashi, K., Takalo, L., Takami, H., Talbot, C., Tammi, J., Tanaka, M., Tanaka, S., Tasan, J., Tavani, M., Tavernet, J. -P, Tejedor, L. A., Telezhinsky, I., Temnikov, P., Tenzer, C., Terada, Y., Terrier, R., Teshima, M., Testa, V., Tezier, D., Thuermann, D., Tibaldo, L., Tibolla, O., Tiengo, A., Tluczykont, M., Todero Peixoto, C. J., Tokanai, F., Tokarz, M., Toma, K., Torii, K., Tornikoski, M., Torres, D. F., Torres, M., Tosti, G., Totani, T., Toussenel, C., Tovmassian, G., Travnicek, P., Trifoglio, M., Troyano, I., Tsinganos, K., Ueno, H., Umehara, K., Upadhya, S. S., Usher, T., Uslenghi, M., Valdes-Galicia, J. F., Vallania, P., Vallejo, G., van Driel, W., van Eldik, C., Vandenbrouke, J., Vanderwalt, J., Vankov, H., Vasileiadis, G., Vassiliev, V., Veberic, D., Vegas, I., Vercellone, S., Vergani, S., Veyssiere, C., Vialle, J. P., Viana, A., Videla, M., Vincent, P., Vincent, S., Vink, J., Vlahakis, N., Vlahos, L., Vogler, P., Vollhardt, A., von Gunten, H. -P, Vorobiov, S., Vuerli, C., Waegebaert, V., Wagner, R., Wagner, R. G., Wagner, S., Wakely, S. P., Walter, R., Walther, T., Warda, K., Warwick, R., Wawer, P., Wawrzaszek, R., Webb, N., Wegner, P., Weinstein, A., Weitzel, Q., Welsing, R., Werner, M., Wetteskind, H., White, R., Wierzcholska, A., Wiesand, S., Wilkinson, M., Williams, D. 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A., Willingale, R., Winiarski, K., Wischnewski, R., Wisniewski, L., Wood, M., Woernlein, A., Xiong, Q., Yadav, K. K., Yamamoto, H., Yamamoto, T., Yamazaki, R., Yanagita, S., Yebras, J. M., Yelos, D., Yoshida, A., Yoshida, T., Yoshikoshi, T., Zabalza, V., Zacharias, M., Zajczyk, A., Zanin, R., Zdziarski, A., Zech, A., Zhao, A., Zhou, X., Zietara, K., Ziolkowski, J., Ziolkowski, P., Zitelli, V., Zurbach, C., and Zychowski, P.
Abstract: The Cherenkov Telescope Array (CTA) is a new observatory for very high-energy (VHE) gamma rays. CTA has ambitions science goals, for which it is necessary to achieve full-sky coverage, to improve the sensitivity by about an order of magnitude, to span about four decades of energy, from a few tens of GeV to above 100 TeV with enhanced angular and energy resolutions over existing VHE gamma-ray observatories. An international collaboration has formed with more than 1000 members from 27 countries in Europe, Asia, Africa and North and South America. In 2010 the CTA Consortium completed a Design Study and started a three-year Preparatory Phase which leads to production readiness of CTA in 2014. In this paper we introduce the science goals and the concept of CTA, and provide an overview of the project. (C) 2013 Elsevier B.V. All rights reserved.
Published: 2013
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206. Broad-band monitoring tracing the evolution of the jet and disc in the black hole candidate X-ray binary MAXI J1659-152

Author: van der Horst, A. J., Curran, P. A., Miller-Jones, J. C. A., Linford, J. D., Gorosabel, J., Russell, D. M., Ugarte Postigo, Antonio de, Lundgren, Anne, Taylor, G. B., Maitra, D., Guziy, S., Belloni, T. M., Kouveliotou, C., Jonker, P. G., Kamble, A., Paragi, Z., Homan, J., Kuulkers, E., Granot, J., Altamirano, D., Buxton, M. M., Castro-Tirado, A., Fender, R. P., Garrett, M. A., Gehrels, N., Hartmann, D. H., Kennea, J. A., Krimm, H. A., Mangano, V., Ramirez-Ruiz, E., Romano, P., Wijers, R. A. M. J., Wijnands, R., Yang, Y. J., van der Horst, A. J., Curran, P. A., Miller-Jones, J. C. A., Linford, J. D., Gorosabel, J., Russell, D. M., Ugarte Postigo, Antonio de, Lundgren, Anne, Taylor, G. B., Maitra, D., Guziy, S., Belloni, T. M., Kouveliotou, C., Jonker, P. G., Kamble, A., Paragi, Z., Homan, J., Kuulkers, E., Granot, J., Altamirano, D., Buxton, M. M., Castro-Tirado, A., Fender, R. P., Garrett, M. A., Gehrels, N., Hartmann, D. H., Kennea, J. A., Krimm, H. A., Mangano, V., Ramirez-Ruiz, E., Romano, P., Wijers, R. A. M. J., Wijnands, R., and Yang, Y. J.
Published: 2013

207. Broad-band monitoring tracing the evolution of the jet and disc in the black hole candidate X-ray binary MAXI J1659-152

Author: van der Horst, A., Curran, Peter, Miller-Jones, James, Linford, J., Gorosabel, J., Russell, D., de Ugarte Postigo, A., Lundgren, A., Taylor, G., Maitra, D., Guziy, S., Belloni, T., Kouveliotou, C., Jonker, P., Kamble, A., Paragi, Z., Homan, J., Kuulkers, E., Granot, J., Altamirano, D., Buxton, M., Castro-Tirado, A., Fender, R., Garrett, M., Gehrels, N., Hartmann, D., Kennea, J., Krimm, H., Mangano, V., Ramirez-Ruiz, E., Romano, P., Wijers, R., Wijnands, R., Yang, Y., van der Horst, A., Curran, Peter, Miller-Jones, James, Linford, J., Gorosabel, J., Russell, D., de Ugarte Postigo, A., Lundgren, A., Taylor, G., Maitra, D., Guziy, S., Belloni, T., Kouveliotou, C., Jonker, P., Kamble, A., Paragi, Z., Homan, J., Kuulkers, E., Granot, J., Altamirano, D., Buxton, M., Castro-Tirado, A., Fender, R., Garrett, M., Gehrels, N., Hartmann, D., Kennea, J., Krimm, H., Mangano, V., Ramirez-Ruiz, E., Romano, P., Wijers, R., Wijnands, R., and Yang, Y.
Abstract: MAXI J1659-152 was discovered on 2010 September 25 as a new X-ray transient, initially identified as a gamma-ray burst, but was later shown to be a new X-ray binary with a black hole as the most likely compact object. Dips in the X-ray light curves have revealed that MAXI J1659-152 is the shortest period black hole candidate identified to date. Here we present the results of a large observing campaign at radio, submillimetre, near-infrared (nIR), optical and ultraviolet (UV) wavelengths. We have combined this very rich data set with the available X-ray observations to compile a broad-band picture of the evolution of this outburst. We have performed broad-band spectral modelling, demonstrating the presence of a spectral break at radio frequencies and a relationship between the radio spectrum and X-ray states. Also, we have determined physical parameters of the accretion disc and put them into context with respect to the other parameters of the binary system. Finally, we have investigated the radio–X-ray and nIR/optical/UV–X-ray correlations up to ~3?yr after the outburst onset to examine the link between the jet and the accretion disc, and found that there is no significant jet contribution to the nIR emission when the source is in the soft or intermediate X-ray spectral state, consistent with our detection of the jet break at radio frequencies during these states.
Published: 2013

208. NuSTARobservations of grb 130427a establish a single component synchrotron afterglow origin for the late optical to multi-gev emission

Author: Kouveliotou, C., Granot, J., Racusin, J. L., Bellm, E., Vianello, G., Oates, S., Fryer, C. L., Boggs, S. E., Christensen, Finn Erland, Craig, W. W., Dermer, C. D., Gehrels, N., Hailey, C. J., Harrison, F. A., Melandri, A., McEnery, J. E., Mundell, C. G., Stern, D. K., Tagliaferri, G., Zhang, W. W., Kouveliotou, C., Granot, J., Racusin, J. L., Bellm, E., Vianello, G., Oates, S., Fryer, C. L., Boggs, S. E., Christensen, Finn Erland, Craig, W. W., Dermer, C. D., Gehrels, N., Hailey, C. J., Harrison, F. A., Melandri, A., McEnery, J. E., Mundell, C. G., Stern, D. K., Tagliaferri, G., and Zhang, W. W.
Abstract: GRB 130427A occurred in a relatively nearby galaxy; its prompt emission had the largest GRB fluence ever recorded. The afterglow of GRB 130427A was bright enough for the Nuclear Spectroscopic Telescope ARray (NuSTAR) to observe it in the 3-79 keV energy range long after its prompt emission (similar to 1.5 and 5 days). This range, where afterglow observations were previously not possible, bridges an important spectral gap. Combined with Swift, Fermi, and ground-based optical data, NuSTAR observations unambiguously establish a single afterglow spectral component from optical to multi-GeV energies a day after the event, which is almost certainly synchrotron radiation. Such an origin of the late-time Fermi/Large Area Telescope >10 GeV photons requires revisions in our understanding of collisionless relativistic shock physics.
Published: 2013

209. Constraining The High-Energy Emission From Gamma-Ray Bursts With Fermi

Author: Ackermann, M., Ajello, M., Baldini, L., Barbiellini, G., Baring, M. G., Bechtol, K., Bellazzini, R., Blandford, R. D., Bloom, E. D., Bonamente, E., Borgland, A. W., Bottacini, E., Bouvier, A., Brigida, M., Buehler, R., Buson, S., Caliandro, G. A., Cameron, R. A., Cecchi, C., Charles, E., Chekhtman, A., Chiang, J., Ciprini, S., Claus, R., Cohen-Tanugi, J., Cutini, S., D'Ammando, F., de Palma, F., Dermer, C. D., do Couto e Silva, E., Drell, P. S., Drlica-Wagner, A., Favuzzi, C., Fukazawa, Y., Fusco, P., Gargano, F., Gasparrini, D., Gehrels, N., Germani, S., Giglietto, N., Giordano, F., Giroletti, M., Glanzman, T., Granot, J., Grenier, I. A., Grove, J. E., Hadasch, D., Hanabata, Y., Harding, A. K., Hays, E., Horan, D., Johannesson, G., Kataoka, J., Knoedlseder, J., Kocevski, D., Kuss, M., Lande, J., Longo, F., Loparco, F., Lovellette, M. N., Lubrano, P., Mazziotta, M. N., McEnery, J., McGlynn, S., Michelson, P. F., Mitthumsiri, W., Monzani, M. E., Moretti, Elena, Morselli, A., Moskalenko, I. V., Murgia, S., Naumann-Godo, M., Norris, J. P., Nuss, E., Nymark, Tanja, Ohsugi, T., Okumura, A., Omodei, N., Orlando, E., Panetta, J. H., Parent, D., Pelassa, V., Pesce-Rollins, M., Piron, F., Pivato, G., Racusin, J. L., Raino, S., Rando, R., Razzaque, S., Reimer, A., Reimer, O., Ritz, S., Ryde, Felix, Sgro, C., Siskind, E. J., Sonbas, E., Spandre, G., Spinelli, P., Stamatikos, M., Stawarz, Eukasz, Suson, D. J., Takahashi, H., Tanaka, T., Thayer, J. G., Thayer, J. B., Tibaldo, L., Tinivella, M., Tosti, G., Uehara, T., Vandenbroucke, J., Vasileiou, V., Vianello, G., Vitale, V., Waite, A. P., Connaughton, V., Briggs, M. S., Guirec, S., Goldstein, A., Burgess, J. M., Bhat, P. N., Bissaldi, E., Camero-Arranz, A., Fishman, J., Fitzpatrick, G., Foley, S., Gruber, D., Jenke, P., Kippen, R. M., Kouveliotou, C., McBreen, S., Meegan, C., Paciesas, W. S., Preece, R., Rau, A., Tierney, D., van der Horst, A. J., von Kienlin, A., Wilson-Hodge, C., Xiong, S., Ackermann, M., Ajello, M., Baldini, L., Barbiellini, G., Baring, M. G., Bechtol, K., Bellazzini, R., Blandford, R. D., Bloom, E. D., Bonamente, E., Borgland, A. W., Bottacini, E., Bouvier, A., Brigida, M., Buehler, R., Buson, S., Caliandro, G. A., Cameron, R. A., Cecchi, C., Charles, E., Chekhtman, A., Chiang, J., Ciprini, S., Claus, R., Cohen-Tanugi, J., Cutini, S., D'Ammando, F., de Palma, F., Dermer, C. D., do Couto e Silva, E., Drell, P. S., Drlica-Wagner, A., Favuzzi, C., Fukazawa, Y., Fusco, P., Gargano, F., Gasparrini, D., Gehrels, N., Germani, S., Giglietto, N., Giordano, F., Giroletti, M., Glanzman, T., Granot, J., Grenier, I. A., Grove, J. E., Hadasch, D., Hanabata, Y., Harding, A. K., Hays, E., Horan, D., Johannesson, G., Kataoka, J., Knoedlseder, J., Kocevski, D., Kuss, M., Lande, J., Longo, F., Loparco, F., Lovellette, M. N., Lubrano, P., Mazziotta, M. N., McEnery, J., McGlynn, S., Michelson, P. F., Mitthumsiri, W., Monzani, M. E., Moretti, Elena, Morselli, A., Moskalenko, I. V., Murgia, S., Naumann-Godo, M., Norris, J. P., Nuss, E., Nymark, Tanja, Ohsugi, T., Okumura, A., Omodei, N., Orlando, E., Panetta, J. H., Parent, D., Pelassa, V., Pesce-Rollins, M., Piron, F., Pivato, G., Racusin, J. L., Raino, S., Rando, R., Razzaque, S., Reimer, A., Reimer, O., Ritz, S., Ryde, Felix, Sgro, C., Siskind, E. J., Sonbas, E., Spandre, G., Spinelli, P., Stamatikos, M., Stawarz, Eukasz, Suson, D. J., Takahashi, H., Tanaka, T., Thayer, J. G., Thayer, J. B., Tibaldo, L., Tinivella, M., Tosti, G., Uehara, T., Vandenbroucke, J., Vasileiou, V., Vianello, G., Vitale, V., Waite, A. P., Connaughton, V., Briggs, M. S., Guirec, S., Goldstein, A., Burgess, J. M., Bhat, P. N., Bissaldi, E., Camero-Arranz, A., Fishman, J., Fitzpatrick, G., Foley, S., Gruber, D., Jenke, P., Kippen, R. M., Kouveliotou, C., McBreen, S., Meegan, C., Paciesas, W. S., Preece, R., Rau, A., Tierney, D., van der Horst, A. J., von Kienlin, A., Wilson-Hodge, C., and Xiong, S.
Abstract: We examine 288 gamma-ray bursts (GRBs) detected by the Fermi Gamma-ray Space Telescope's Gamma-ray Burst Monitor (GBM) that fell within the field of view of Fermi's Large Area Telescope (LAT) during the first 2.5 years of observations, which showed no evidence for emission above 100 MeV. We report the photon flux upper limits in the 0.1-10 GeV range during the prompt emission phase as well as for fixed 30 s and 100 s integrations starting from the trigger time for each burst. We compare these limits with the fluxes that would be expected from extrapolations of spectral fits presented in the first GBM spectral catalog and infer that roughly half of the GBM-detected bursts either require spectral breaks between the GBM and LAT energy bands or have intrinsically steeper spectra above the peak of the nu F-nu spectra (E-pk). In order to distinguish between these two scenarios, we perform joint GBM and LAT spectral fits to the 30 brightest GBM-detected bursts and find that a majority of these bursts are indeed softer above E-pk than would be inferred from fitting the GBM data alone. Approximately 20% of this spectroscopic subsample show statistically significant evidence for a cutoff in their high-energy spectra, which if assumed to be due to gamma gamma attenuation, places limits on the maximum Lorentz factor associated with the relativistic outflow producing this emission. All of these latter bursts have maximum Lorentz factor estimates that are well below the minimum Lorentz factors calculated for LAT-detected GRBs, revealing a wide distribution in the bulk Lorentz factor of GRB outflows and indicating that LAT-detected bursts may represent the high end of this distribution., QC 20120907
Published: 2012
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210. SGR J1550-5418 bursts detected with the Fermi Gamma-ray Burst Monitor during its most prolific activity

Author: van der Horst, A. J., Kouveliotou, C., Gorgone, N. M., Kaneko, Y., Baring, M. G., Guiriec, S., Gogus, E., Granot, J., Watts, A. L., Lin, L., Bhat, P. N., Bissaldi, E., Chaplin, V. L., Finger, M. H., Gehrels, N., Gibby, M. H., Giles, M. M., Goldstein, A., Gruber, D., Harding, A. K., Kaper, L., von Kienlin, A., van der Klis, M., McBreen, S., Mcenery, J., Meegan, C. A., Paciesas, W. S., Pe'er, A., Preece, R. D., Ramirez-Ruiz, E., Rau, A., Wachter, S., Wilson-Hodge, C., Woods, P. M., Wijers, R. A. M. J., van der Horst, A. J., Kouveliotou, C., Gorgone, N. M., Kaneko, Y., Baring, M. G., Guiriec, S., Gogus, E., Granot, J., Watts, A. L., Lin, L., Bhat, P. N., Bissaldi, E., Chaplin, V. L., Finger, M. H., Gehrels, N., Gibby, M. H., Giles, M. M., Goldstein, A., Gruber, D., Harding, A. K., Kaper, L., von Kienlin, A., van der Klis, M., McBreen, S., Mcenery, J., Meegan, C. A., Paciesas, W. S., Pe'er, A., Preece, R. D., Ramirez-Ruiz, E., Rau, A., Wachter, S., Wilson-Hodge, C., Woods, P. M., and Wijers, R. A. M. J.
Abstract: We have performed detailed temporal and time-integrated spectral analysis of 286 bursts from SGR J1550-5418 detected with the Fermi Gamma-ray Burst Monitor (GBM) in January 2009, resulting in the largest uniform sample of temporal and spectral properties of SGR J1550-5418 bursts. We have used the combination of broadband and high time-resolution data provided with GBM to perform statistical studies for the source properties. We determine the durations, emission times, duty cycles and rise times for all bursts, and find that they are typical of SGR bursts. We explore various models in our spectral analysis, and conclude that the spectra of SGR J1550-5418 bursts in the 8-200 keV band are equally well described by optically thin thermal bremsstrahlung (OTTB), a power law with an exponential cutoff (Comptonized model), and two black-body functions (BB+BB). In the spectral fits with the Comptonized model we find a mean power-law index of -0.92, close to the OTTB index of -1. We show that there is an anti-correlation between the Comptonized Epeak and the burst fluence and average flux. For the BB+BB fits we find that the fluences and emission areas of the two blackbody functions are correlated. The low-temperature BB has an emission area comparable to the neutron star surface area, independent of the temperature, while the high-temperature blackbody has a much smaller area and shows an anti-correlation between emission area and temperature. We compare the properties of these bursts with bursts observed from other SGR sources during extreme activations, and discuss the implications of our results in the context of magnetar burst models., Comment: 13 pages, 10 figures, 2 tables; minor changes, ApJ in press
Published: 2012
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211. DETECTION OF HIGH-ENERGY GAMMA-RAY EMISSION DURING THE X-RAY FLARING ACTIVITY IN GRB 100728A

Author: Abdo, A. A., Ackermann, M., Ajello, M., Baldini, L., Ballet, J., Barbiellini, G., Baring, M. G., Bastieri, D., Bechtol, K., Bellazzini, R., Berenji, B., Bhat, P. N., Bissaldi, E., Blandford, R. D., Bonamente, E., Bonnell, J., Borgland, A. W., Bouvier, A., Bregeon, J., Brigida, M., Bruel, P., Buehler, R., Buson, S., Caliandro, G. A., Cameron, R. A., Caraveo, P. A., Casandjian, J. M., Cecchi, C., Charles, E., Chekhtman, A., Chiang, J., Ciprini, S., Claus, R., Connaughton, V., Conrad, Jan, Cutini, S., de Angelis, A., de Palma, F., Dermer, C. D., do Couto e Silva, E., Drell, P. S., Dubois, R., Favuzzi, C., Fukazawa, Y., Fusco, P., Gargano, F., Gehrels, N., Germani, S., Giglietto, N., Giommi, P., Giordano, F., Giroletti, M., Glanzman, T., Godfrey, G., Granot, J., Grenier, I. A., Guiriec, S., Hadasch, D., Hanabata, Y., Hughes, R. E., Johannesson, G., Johnson, A. S., Kamae, T., Katagiri, H., Kataoka, J., Kerr, M., Knoedlseder, J., Kuss, M., Lande, J., Latronico, L., Lee, S. -H, Longo, F., Loparco, F., Lott, B., Lubrano, P., Mazziotta, M. N., McEnery, J. E., Meszaros, P., Michelson, P. F., Mizuno, T., Moiseev, A. A., Monzani, M. E., Morselli, A., Moskalenko, I. V., Murgia, S., Nakamori, T., Naumann-Godo, M., Nolan, P. L., Norris, J. P., Nuss, E., Ohsugi, T., Okumura, A., Omodei, N., Orlando, E., Paciesas, W. S., Pelassa, V., Pesce-Rollins, M., Pierbattista, M., Piron, F., Porter, T. A., Racusin, J. L., Raino, S., Razzano, M., Razzaque, S., Reimer, A., Reimer, O., Reyes, L. C., Roth, M., Sadrozinski, H. F. -W, Sgro, C., Siskind, E. J., Smith, P. D., Sonbas, E., Spandre, G., Spinelli, P., Stamatikos, M., Strickman, M. S., Takahashi, H., Tanaka, T., Tanaka, Y., Thayer, J. G., Thayer, J. B., Torres, D. F., Tosti, G., Troja, E., Uehara, T., Usher, T. L., Vandenbroucke, J., Vasileiou, V., Vianello, G., Vilchez, N., Vitale, V., von Kienlin, A., Waite, A. P., Wang, P., Winer, B. L., Wood, K. S., Yamazaki, R., Yang, Zhaoyu, Ziegler, M., Piro, L., Abdo, A. A., Ackermann, M., Ajello, M., Baldini, L., Ballet, J., Barbiellini, G., Baring, M. G., Bastieri, D., Bechtol, K., Bellazzini, R., Berenji, B., Bhat, P. N., Bissaldi, E., Blandford, R. D., Bonamente, E., Bonnell, J., Borgland, A. W., Bouvier, A., Bregeon, J., Brigida, M., Bruel, P., Buehler, R., Buson, S., Caliandro, G. A., Cameron, R. A., Caraveo, P. A., Casandjian, J. M., Cecchi, C., Charles, E., Chekhtman, A., Chiang, J., Ciprini, S., Claus, R., Connaughton, V., Conrad, Jan, Cutini, S., de Angelis, A., de Palma, F., Dermer, C. D., do Couto e Silva, E., Drell, P. S., Dubois, R., Favuzzi, C., Fukazawa, Y., Fusco, P., Gargano, F., Gehrels, N., Germani, S., Giglietto, N., Giommi, P., Giordano, F., Giroletti, M., Glanzman, T., Godfrey, G., Granot, J., Grenier, I. A., Guiriec, S., Hadasch, D., Hanabata, Y., Hughes, R. E., Johannesson, G., Johnson, A. S., Kamae, T., Katagiri, H., Kataoka, J., Kerr, M., Knoedlseder, J., Kuss, M., Lande, J., Latronico, L., Lee, S. -H, Longo, F., Loparco, F., Lott, B., Lubrano, P., Mazziotta, M. N., McEnery, J. E., Meszaros, P., Michelson, P. F., Mizuno, T., Moiseev, A. A., Monzani, M. E., Morselli, A., Moskalenko, I. V., Murgia, S., Nakamori, T., Naumann-Godo, M., Nolan, P. L., Norris, J. P., Nuss, E., Ohsugi, T., Okumura, A., Omodei, N., Orlando, E., Paciesas, W. S., Pelassa, V., Pesce-Rollins, M., Pierbattista, M., Piron, F., Porter, T. A., Racusin, J. L., Raino, S., Razzano, M., Razzaque, S., Reimer, A., Reimer, O., Reyes, L. C., Roth, M., Sadrozinski, H. F. -W, Sgro, C., Siskind, E. J., Smith, P. D., Sonbas, E., Spandre, G., Spinelli, P., Stamatikos, M., Strickman, M. S., Takahashi, H., Tanaka, T., Tanaka, Y., Thayer, J. G., Thayer, J. B., Torres, D. F., Tosti, G., Troja, E., Uehara, T., Usher, T. L., Vandenbroucke, J., Vasileiou, V., Vianello, G., Vilchez, N., Vitale, V., von Kienlin, A., Waite, A. P., Wang, P., Winer, B. L., Wood, K. S., Yamazaki, R., Yang, Zhaoyu, Ziegler, M., and Piro, L.
Abstract: We present the simultaneous Swift and Fermi observations of the bright GRB 100728A and its afterglow. The early X-ray emission is dominated by a vigorous flaring activity continuing until 1 ks after the burst. In the same time interval, high-energy emission is significantly detected by the Fermi/Large Area Telescope. Marginal evidence of GeV emission is observed up to later times. We discuss the broadband properties of this burst within both the internal and external shock scenarios, with a particular emphasis on the relation between X-ray flares, the GeV emission, and a continued long-duration central engine activity as their power source., authorCount :141
Published: 2011
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212. X-ray flare candidates in short gamma-ray bursts

Author: Margutti, R., Chincarini, G., Granot, J., Guidorzi, C., Berger, E., Bernardini, M. G., Gehrels, N., Soderberg, A. M., Stamatikos, M., Zaninoni, E., Margutti, R., Chincarini, G., Granot, J., Guidorzi, C., Berger, E., Bernardini, M. G., Gehrels, N., Soderberg, A. M., Stamatikos, M., and Zaninoni, E.
Abstract: We present the first systematic study of X-ray flare candidates in short gamma-ray bursts (SGRBs) exploiting the large 6-year Swift database with the aim to constrain the physical nature of such fluctuations. We find that flare candidates appear in different types of SGRB host galaxy environments and show no clear correlation with the X-ray afterglow lifetime; flare candidates are detected both in SGRBs with a bright extended emission in the soft gamma-rays and in SGRBs which do not show such component. We furthermore show that SGRB X-ray flare candidates only partially share the set of observational properties of long GRB (LGRB) flares. In particular,the main parameter driving the duration evolution of X-ray variability episodes in both classes is found to be the elapsed time from the explosion, with very limited dependence on the different progenitors, environments, central engine life-times, prompt variability time-scales and energy budgets. On the contrary, SGRB flare candidates significantly differ from LGRB flares in terms of peak luminosity, isotropic energy, flare-to-prompt luminosity ratio and relative variability flux. However, these differences disappear when the central engine time-scales and energy budget are accounted for, suggesting that (i) flare candidates and prompt pulses in SGRBs likely have a common origin; (ii) similar dissipation and/or emission mechanisms are responsible for the prompt and flare emission in long and short GRBs, with SGRBs being less energetic albeit faster evolving versions of the long class. Finally, we show that in strict analogy to the SGRB prompt emission, flares candidates fall off the lag-luminosity relation defined by LGRBs, thus strengthening the SGRB flare-prompt pulse connection., Comment: 19 pages, 16 figures, MNRAS accepted
Published: 2011
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213. Magnetic field decay in neutron stars: from Soft Gamma Repeaters to 'weak field magnetars'

Author: Dall'Osso, S., Granot, J., Piran, T., Dall'Osso, S., Granot, J., and Piran, T.
Abstract: The recent discovery of the "weak field, old magnetar", the soft gamma repeater SGR 0418+5729, whose dipole magnetic field is less than 7.5 \times 10^{12} G, has raised perplexing questions: How can the neutron star produce SGR-like bursts with such a low magnetic field? What powers the observed X-ray emission when neither the rotational energy nor the magnetic dipole energy are sufficient? These observations, that suggest either a much larger energy reservoir or a much younger true age (or both), have renewed the interest in the evolutionary sequence of magnetars. We examine, here, a phenomenological model for the magnetic field decay: B_dip} \propto (B_dip)^{1+a} and compare its predictions with the observed period, P,the period derivative, \dot{P}, and the X-ray luminosity, L_X, of magnetar candidates. We find a strong evidence for a dipole field decay on a timescale of \sim 10^3 yr for the strongest (\sim 10^{15} G) field objects, with a decay index within the range 1 \leq a < 2 and more likely within 1.5\lesssim a \lesssim 1.8. The decaying field implies a younger age than what is implied by the spinown age. Surprisingly, even with the younger age, the energy released in the dipole field decay is insufficient to power the X-ray emission, suggesting the existence of a stronger internal field, B_int. Examining several models for the internal magnetic field decay we find that it must have a very large (> 10^{16} G) initial value. Our findings suggest two clear distinct evolutionary tracks -- the SGR/AXP branch and the transient branch, with a possible third branch involving high-field radio pulsars that age into low luminosity X-ray dim isolated neutron stars., Comment: 47 pages, 11 figures, accepted for publication on MNRAS, in press
Published: 2011
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214. The missing link: Merging neutron stars naturally produce jet-like structures and can power short gamma-ray bursts

Author: Rezzolla, L, Giacomazzo, B, Baiotti, L, Granot, J, Kouveliotou, C, Aloy, M, Aloy, MA, Rezzolla, L, Giacomazzo, B, Baiotti, L, Granot, J, Kouveliotou, C, Aloy, M, and Aloy, MA
Abstract: Short gamma-ray bursts (SGRBs) are among the most luminous explosions in the universe, releasing in less than one second the energy emitted by our Galaxy over one year. Despite decades of observations, the nature of their "central engine" remains unknown. Considering a binary of magnetized neutron stars and solving the Einstein equations, we show that their merger results in a rapidly spinning black hole surrounded by a hot and highly magnetized torus. Lasting over 35ms and much longer than previous simulations, our study reveals that magnetohydrodynamical instabilities amplify an initially turbulent magnetic field of ∼1012G to produce an ordered poloidal field of ∼1015G along the black hole spin axis, within a half-opening angle of ∼30°, which may naturally launch a relativistic jet. The broad consistency of our ab initio calculations with SGRB observations shows that the merger of magnetized neutron stars can provide the basic physical conditions for the central engine of SGRBs
Published: 2011

215. Detailed Radio View on Two Stellar Explosions and Their Host Galaxy: XRF 080109/SN 2008D and SN 2007uy in NGC 2770

Author: van der Horst, A., Kamble, A., Paragi, Z., Sage, L., Pal, S., Taylor, G., Kouveliotou, C., Granot, J., Ramirez-Ruiz, E., Ishwara-Chandra, C., Oosterloo, T., Wijers, R., Wiersema, K., Strom, R., Bhattacharya, D., Rol, E., Starling, R., Curran, Peter, Garrett, M., van der Horst, A., Kamble, A., Paragi, Z., Sage, L., Pal, S., Taylor, G., Kouveliotou, C., Granot, J., Ramirez-Ruiz, E., Ishwara-Chandra, C., Oosterloo, T., Wijers, R., Wiersema, K., Strom, R., Bhattacharya, D., Rol, E., Starling, R., Curran, Peter, and Garrett, M.
Abstract: The galaxy NGC 2770 hosted two core-collapse supernova (SN) explosions, SN 2008D and SN 2007uy, within10 days of each other and 9 years after the first SN of the same type, SN 1999eh, was found in that galaxy.In particular, SN 2008D attracted a lot of attention due to the detection of an X-ray outburst, which has beenhypothesized to be caused by either a (mildly) relativistic jet or the SN shock breakout. We present an extensivestudy of the radio emission from SN 2008D and SN 2007uy: flux measurements with the Westerbork SynthesisRadio Telescope and theGiant MetrewaveRadio Telescope, covering~600 days with observing frequencies rangingfrom 325 MHz to 8.4 GHz. The results of two epochs of global Very Long Baseline Interferometry observationsare also discussed. We have examined the molecular gas in the host galaxy NGC 2770 with the Arizona RadioObservatory 12 m telescope, and present the implications of our observations for the star formation and seeminglyhigh SN rate in this galaxy. Furthermore, we discuss the near-future observing possibilities of the two SNe andtheir host galaxy at low radio frequencies with the Low Frequency Array.
Published: 2011

216. Detailed Radio View on Two Stellar Explosions and Their Host Galaxy: XRF080109/SN2008D and SN2007uy in NGC2770

Author: van der Horst, A. J., Kamble, A. P., Paragi, Z., Sage, L. J., Pal, S., Taylor, G. B., Kouveliotou, C., Granot, J., Ramirez-Ruiz, E., Ishwara-Chandra, C. H., Oosterloo, T. A., Wijers, R. A. M. J., Wiersema, K., Strom, R. G., Bhattacharya, D., Rol, E., Starling, R. L. C., Curran, P. A., Garrett, M. A., van der Horst, A. J., Kamble, A. P., Paragi, Z., Sage, L. J., Pal, S., Taylor, G. B., Kouveliotou, C., Granot, J., Ramirez-Ruiz, E., Ishwara-Chandra, C. H., Oosterloo, T. A., Wijers, R. A. M. J., Wiersema, K., Strom, R. G., Bhattacharya, D., Rol, E., Starling, R. L. C., Curran, P. A., and Garrett, M. A.
Abstract: The galaxy NGC2770 hosted two core-collapse supernova explosions, SN2008D and SN2007uy, within 10 days of each other and 9 years after the first supernova of the same type, SN1999eh, was found in that galaxy. In particular SN2008D attracted a lot of attention due to the detection of an X-ray outburst, which has been hypothesized to be caused by either a (mildly) relativistic jet or the supernova shock breakout. We present an extensive study of the radio emission from SN2008D and SN2007uy: flux measurements with the Westerbork Synthesis Radio Telescope and the Giant Metrewave Radio Telescope, covering ~600 days with observing frequencies ranging from 325 MHz to 8.4 GHz. The results of two epochs of global Very Long Baseline Interferometry observations are also discussed. We have examined the molecular gas in the host galaxy NGC2770 with the Arizona Radio Observatory 12-m telescope, and present the implications of our observations for the star formation and seemingly high SN rate in this galaxy. Furthermore, we discuss the near-future observing possibilities of the two SNe and their host galaxy at low radio frequencies with the Low Frequency Array., Comment: 13 pages, 6 figures, 3 tables; accepted for publication in ApJ
Published: 2010
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217. A mildly relativistic radio jet from the otherwise normal Type Ic Supernova 2007gr

Author: Paragi, Z., Taylor, G. B., Kouveliotou, C., Granot, J., Ramirez-Ruiz, E., Bietenholz, M., van der Horst, A. J., Pidopryhora, Y., van Langevelde, H. J., Garrett, M. A., Szomoru, A., Argo, M., Bourke, S., Paczynski, B., Paragi, Z., Taylor, G. B., Kouveliotou, C., Granot, J., Ramirez-Ruiz, E., Bietenholz, M., van der Horst, A. J., Pidopryhora, Y., van Langevelde, H. J., Garrett, M. A., Szomoru, A., Argo, M., Bourke, S., and Paczynski, B.
Abstract: The class of type Ic supernovae have drawn increasing attention since 1998 owing to their sparse association (only four so far) with long duration gamma-ray bursts. Although both phenomena originate from the core collapse of a massive star, supernovae emit mostly at optical wavelengths, whereas GRBs emit mostly in soft gamma-rays or hard X-rays. Though the GRB central engine generates ultra-relativistic jets, which beam the early emission into a narrow cone, no relativistic outflows have hitherto been found in type Ib/c supernovae explosions, despite theoretical expectations and searches. Here we report radio (interferometric) observations that reveal a mildly relativistic expansion in a nearby type Ic supernova, SN 2007gr. Using two observational epochs 60 days apart, we detect expansion of the source and establish a conservative lower limit for the average apparent expansion velocity of 0.6c. Independently, a second mildly relativistic supernova has been reported. Contrary to the radio data, optical observations of SN 2007gr indicate a typical type Ic supernova with ejecta velocities ~6000 km/s, much lower than in GRB-associated supernovae. We conclude that in SN 2007gr a small fraction of the ejecta produced a low-energy mildly relativistic bipolar radio jet, while the bulk of the ejecta were slower and, as shown by optical spectro-polarimetry, mildly aspherical., Comment: Nature, 10 pages (including supplementary material), 2 figures
Published: 2010
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218. Fermi/Gamma-ray Burst Monitor detection of SGR J1550-5418

Author: Kaneko, Y., Gogus, E., Kouveliotou, C., Granot, J., Ramirez-Ruiz, E., Team, the GBM Magnetar, Kaneko, Y., Gogus, E., Kouveliotou, C., Granot, J., Ramirez-Ruiz, E., and Team, the GBM Magnetar
Abstract: SGR J1550-5418 exhibited three active bursting episodes in 2008 October and in 2009 January and March, emitting hundreds of typical Soft Gamma Repeater (SGR) bursts in soft gamma-rays. The second episode was especially intense, and our untriggered burst search on Fermi/GBM data (8-1000 keV) revealed ~450 bursts emitted over 24 hours during the peak of this activity. Using the GBM data, we identified a ~150-s-long enhanced persistent emission during 2009 January 22 that exhibited intriguing timing and spectral properties: (i) clear pulsations up to ~110 keV at the spin period of the neutron star, (ii) an additional (to a power-law) blackbody component required for the enhanced emission spectra with kT ~ 17 keV, (iii) pulsed fraction that is strongly energy dependent and highest in the 50-74 keV energy band. A total isotropic-equivalent energy emitted during this enhanced emission is estimated to be 2.9 x 10^{40}(D/5 kpc)^2 erg. The estimated area of the blackbody emitting region of ~0.046(D/5 kpc)^2 km^2 is the smallest "hot spot" ever measured for a magnetar and most likely corresponds to the size of magnetically-confined plasma near the neutron star surface., Comment: 6 pages, 2009 Fermi Symposium, eConf Proceedings C091122
Published: 2010

219. GRB 081028 and its late-time afterglow re-brightening

Author: Margutti....[et al.], R., Genet, F., Granot, J., Duran, R. B., Fynbo, Johan Peter Uldall, Malesani, Daniele, Margutti....[et al.], R., Genet, F., Granot, J., Duran, R. B., Fynbo, Johan Peter Uldall, and Malesani, Daniele
Published: 2010

220. Late-time Observations of GRB 080319B: Jet Break, Host Galaxy, and Accompanying Supernova

Author: Tanvir, N., Rol, E., Levan, A., Svensson, K., Fruchter, A., Granot, J., O’Brien, P., Wiersema, K., Starling, R., Jakobsson, P., Fynbo, J., Hjorth, J., Curran, Peter, van der Horst, A., Kouveliotou, C., Racusin, J., Burrows, D., Genet, F., Tanvir, N., Rol, E., Levan, A., Svensson, K., Fruchter, A., Granot, J., O’Brien, P., Wiersema, K., Starling, R., Jakobsson, P., Fynbo, J., Hjorth, J., Curran, Peter, van der Horst, A., Kouveliotou, C., Racusin, J., Burrows, D., and Genet, F.
Abstract: The Swift-discovered GRB 080319B was by far the most distant source ever observed at naked-eye brightness,reaching a peak apparent magnitude of 5.3 at a redshift of z = 0.937. We present our late-time optical (HubbleSpace Telescope, Gemini, and Very Large Telescope) and X-ray (Chandra) observations, which confirm that anachromatic break occurred in the power-law afterglow light curve at~ 11 days post-burst. This most likely indicatesthat the gamma-ray burst (GRB) outflow was collimated, which for a uniform jet would imply a total energy inthe jet Ejet 1052 erg. Our observations also show a late-time excess of red light, which is well explained ifthe GRB was accompanied by a supernova (SN), similar to those seen in some other long-duration GRBs. Thelatest observations are dominated by light from the host and show that the GRB took place in a faint dwarf galaxy(r(AB) ˜ 27.0, rest frame MB ˜ -17.2). This galaxy is small even by the standards of other GRB hosts, whichis suggestive of a low-metallicity environment. Intriguingly, the properties of this extreme event—a small hostand bright SN—are entirely typical of the very low luminosity bursts such as GRB 980425 and GRB 060218.
Published: 2010

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

Author: Abdo, A. A., Ackermann, M., Ajello, M., Asano, K., Atwood, W. B., Axelsson, M., Baldini, L., Ballet, J., Barbiellini, G., Baring, M. 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, P., Burgess, J. M., Burrows, D. N., Buson, S., Caliandro, G. A., Cameron, R. A., Caraveo, P. A., Casandjian, J. M., Cecchi, C., Celik, O., Chekhtman, A., Cheung, C. C., Chiang, J., Ciprini, S., Claus, R., Cohen-Tanugi, J., Cominsky, L. R., Connaughton, V., Conrad, J., Cutini, S., d'Elia, V., Dermer, C. D., de Angelis, A., de Palma, F., Digel, S. W., Dingus, B. L., Silva, E. D. E., Drell, P. S., Dubois, R., Dumora, D., Farnier, C., Favuzzi, C., Fegan, S. J., Finke, J., Fishman, G., Focke, W. B., Fortin, P., Frailis, M., Fukazawa, Y., 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, J., 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., Johannesson, G., Johnson, A. S., Johnson, R. P., Johnson, W. N., Kamae, T., Katagiri, H., Kataoka, J., Kawai, N., Kerr, M., Kippen, R. M., Knodlseder, J., Kocevski, D., Komin, N., Kouveliotou, C., Kuss, M., Lande, J., Latronico, L., Lemoine-Goumard, M., Longo, F., Loparco, F., Lott, B., Lovellette, M. N., Lubrano, P., Madejski, G. M., Makeev, A., Mazziotta, M. N., McBreen, S., McEnery, J. E., McGlynn, Sinéad, Meegan, C., Meszaros, P., Meurer, C., Michelson, P. F., Mitthumsiri, W., Mizuno, T., Moiseev, A. A., Monte, C., Monzani, M. E., Moretti, E., Morselli, A., Moskalenko, I. V., Murgia, S., Nakamori, T., Nolan, P. L., Norris, J. P., Nuss, E., Ohno, M., Ohsugi, T., Omodei, N., Orlando, E., Ormes, J. F., Paciesas, W. S., Paneque, D., Panetta, J. H., Pelassa, V., Pepe, M., Pesce-Rollins, M., Petrosian, V., Piron, F., Porter, T. A., Preece, R., Raino, S., Rando, R., Rau, A., Razzano, M., Razzaque, S., Reimer, A., Reimer, O., Reposeur, T., Ritz, S., Rochester, L. S., Rodriguez, A. Y., Roming, P. W. A., Roth, M., Ryde, Felix, Sadrozinski, H. F. W., Sanchez, D., Sander, A., Parkinson, P. M. S., Scargle, J. D., Schalk, T. L., Sgro, 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, T., Thayer, J. B., Thayer, J. G., Thompson, D. J., Tibaldo, L., Torres, D. F., Tosti, G., Tramacere, A., Uchiyama, Y., Uehara, T., Usher, T. L., van der Horst, A. J., Vasileiou, V., Vilchez, N., Vitale, V., von Kienlin, A., Waite, A. P., Wang, P., Wilson-Hodge, C., Winer, B. L., Wood, K. S., Yamazaki, R., Ylinen, Tomi, Ziegler, M., Abdo, A. A., Ackermann, M., Ajello, M., Asano, K., Atwood, W. B., Axelsson, M., Baldini, L., Ballet, J., Barbiellini, G., Baring, M. 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, P., Burgess, J. M., Burrows, D. N., Buson, S., Caliandro, G. A., Cameron, R. A., Caraveo, P. A., Casandjian, J. M., Cecchi, C., Celik, O., Chekhtman, A., Cheung, C. C., Chiang, J., Ciprini, S., Claus, R., Cohen-Tanugi, J., Cominsky, L. R., Connaughton, V., Conrad, J., Cutini, S., d'Elia, V., Dermer, C. D., de Angelis, A., de Palma, F., Digel, S. W., Dingus, B. L., Silva, E. D. E., Drell, P. S., Dubois, R., Dumora, D., Farnier, C., Favuzzi, C., Fegan, S. J., Finke, J., Fishman, G., Focke, W. B., Fortin, P., Frailis, M., Fukazawa, Y., 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, J., 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., Johannesson, G., Johnson, A. S., Johnson, R. P., Johnson, W. N., Kamae, T., Katagiri, H., Kataoka, J., Kawai, N., Kerr, M., Kippen, R. M., Knodlseder, J., Kocevski, D., Komin, N., Kouveliotou, C., Kuss, M., Lande, J., Latronico, L., Lemoine-Goumard, M., Longo, F., Loparco, F., Lott, B., Lovellette, M. N., Lubrano, P., Madejski, G. M., Makeev, A., Mazziotta, M. N., McBreen, S., McEnery, J. E., McGlynn, Sinéad, Meegan, C., Meszaros, P., Meurer, C., Michelson, P. F., Mitthumsiri, W., Mizuno, T., Moiseev, A. A., Monte, C., Monzani, M. E., Moretti, E., Morselli, A., Moskalenko, I. V., Murgia, S., Nakamori, T., Nolan, P. L., Norris, J. P., Nuss, E., Ohno, M., Ohsugi, T., Omodei, N., Orlando, E., Ormes, J. F., Paciesas, W. S., Paneque, D., Panetta, J. H., Pelassa, V., Pepe, M., Pesce-Rollins, M., Petrosian, V., Piron, F., Porter, T. A., Preece, R., Raino, S., Rando, R., Rau, A., Razzano, M., Razzaque, S., Reimer, A., Reimer, O., Reposeur, T., Ritz, S., Rochester, L. S., Rodriguez, A. Y., Roming, P. W. A., Roth, M., Ryde, Felix, Sadrozinski, H. F. W., Sanchez, D., Sander, A., Parkinson, P. M. S., Scargle, J. D., Schalk, T. L., Sgro, 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, T., Thayer, J. B., Thayer, J. G., Thompson, D. J., Tibaldo, L., Torres, D. F., Tosti, G., Tramacere, A., Uchiyama, Y., Uehara, T., Usher, T. L., van der Horst, A. J., Vasileiou, V., Vilchez, N., Vitale, V., von Kienlin, A., Waite, A. P., Wang, P., Wilson-Hodge, C., Winer, B. L., Wood, K. S., Yamazaki, R., Ylinen, Tomi, and Ziegler, M.
Abstract: We report on the observation of the bright, long gamma-ray burst (GRB), GRB 090902B, by the Gamma-ray Burst Monitor (GBM) and Large Area Telescope (LAT) instruments on-board the Fermi observatory. This was one of the brightest GRBs to have been observed by the LAT, which detected several hundred photons during the prompt phase. With a redshift of z = 1.822, this burst is among the most luminous detected by Fermi. Time-resolved spectral analysis reveals a significant power-law component in the LAT data that is distinct from the usual Band model emission that is seen in the sub-MeV energy range. This power-law component appears to extrapolate from the GeV range to the lowest energies and is more intense than the Band component, both below similar to 50 keV and above 100 MeV. The Band component undergoes substantial spectral evolution over the entire course of the burst, while the photon index of the power-law component remains constant for most of the prompt phase, then hardens significantly toward the end. After the prompt phase, power-law emission persists in the LAT data as late as 1 ks post-trigger, with its flux declining as t(-1.5). The LAT detected a photon with the highest energy so far measured from a GRB, 33.4(-3.5)(+ 2.7) GeV. This event arrived 82 s after the GBM trigger and similar to 50 s after the prompt phase emission had ended in the GBM band. We discuss the implications of these results for models of GRB emission and for constraints on models of the extragalactic background light., QC 20120221
Published: 2009
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222. Prospects for GRB Science with the Fermi Large Area Telescope

Author: Band, D. L., Axelsson, M., Baldini, L., Barbiellini, G., Baring, M. G., Bastieri, D., Battelino, M., Bellazzini, R., Bissaldi, E., Bogaert, G., Bonnell, J., Chiang, J., Cohen-Tanugi, J., Connaughton, V., Cutini, S., de Palma, F., Dingus, B. L., do Couto e Silva, E., Fishman, G., Galli, A., Gehrels, N., Giglietto, N., Granot, J., Guiriec, S., Hughes, R. E., Kamae, T., Komin, N., Kuehn, F., Kuss, M., Longo, F., Lubrano, P., Kippen, R. M., Mazziotta, M. N., McEnery, J. E., McGlynn, S., Moretti, E., Nakamori, T., Norris, J. P., Ohno, M., Olivo, M., Omodei, N., Pelassa, V., Piron, F., Preece, R., Razzano, M., Russell, J. J., Ryde, F., Saz Parkinson, P. M., Scargle, J. D., Sgrò, C., Shimokawabe, T., Smith, P. D., Spandre, G., Spinelli, P., Stamatikos, M., Winer, B. L., Yamazaki, R., Band, D. L., Axelsson, M., Baldini, L., Barbiellini, G., Baring, M. G., Bastieri, D., Battelino, M., Bellazzini, R., Bissaldi, E., Bogaert, G., Bonnell, J., Chiang, J., Cohen-Tanugi, J., Connaughton, V., Cutini, S., de Palma, F., Dingus, B. L., do Couto e Silva, E., Fishman, G., Galli, A., Gehrels, N., Giglietto, N., Granot, J., Guiriec, S., Hughes, R. E., Kamae, T., Komin, N., Kuehn, F., Kuss, M., Longo, F., Lubrano, P., Kippen, R. M., Mazziotta, M. N., McEnery, J. E., McGlynn, S., Moretti, E., Nakamori, T., Norris, J. P., Ohno, M., Olivo, M., Omodei, N., Pelassa, V., Piron, F., Preece, R., Razzano, M., Russell, J. J., Ryde, F., Saz Parkinson, P. M., Scargle, J. D., Sgrò, C., Shimokawabe, T., Smith, P. D., Spandre, G., Spinelli, P., Stamatikos, M., Winer, B. L., and Yamazaki, R.
Abstract: The Large Area Telescope (LAT) instrument on the Fermi mission will reveal the rich spectral and temporal gamma-ray burst (GRB) phenomena in the >100 MeV band. The synergy with Fermi's Gamma-ray Burst Monitor detectors will link these observations to those in the well explored 10-1000 keV range; the addition of the >100 MeV band observations will resolve theoretical uncertainties about burst emission in both the prompt and afterglow phases. Trigger algorithms will be applied to the LAT data both onboard the spacecraft and on the ground. The sensitivity of these triggers will differ because of the available computing resources onboard and on the ground. Here we present the LAT's burst detection methodologies and the instrument's GRB capabilities.
Published: 2009
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223. Discovery of a new Soft Gamma Repeater: SGR J0418+5729

Author: van der Horst, A. J., Connaughton, V., Kouveliotou, C., Gogus, E., Kaneko, Y., Wachter, S., Briggs, M. S., Granot, J., Ramirez-Ruiz, E., Woods, P. M., Aptekar, R. L., Barthelmy, S. D., Cummings, J. R., Finger, M. H., Frederiks, D. D., Gehrels, N., Gelino, C. R., Gelino, D. M., Golenetskii, S., Hurley, K., Krimm, H. A., Mazets, E. P., McEnery, J. E., Meegan, C. A., Oleynik, P. P., Palmer, D. M., Pal'shin, V. D., Pe'er, A., Svinkin, D., Ulanov, M. V., van der Klis, M., von Kienlin, A., Watts, A. L., Wilson-Hodge, C. A., van der Horst, A. J., Connaughton, V., Kouveliotou, C., Gogus, E., Kaneko, Y., Wachter, S., Briggs, M. S., Granot, J., Ramirez-Ruiz, E., Woods, P. M., Aptekar, R. L., Barthelmy, S. D., Cummings, J. R., Finger, M. H., Frederiks, D. D., Gehrels, N., Gelino, C. R., Gelino, D. M., Golenetskii, S., Hurley, K., Krimm, H. A., Mazets, E. P., McEnery, J. E., Meegan, C. A., Oleynik, P. P., Palmer, D. M., Pal'shin, V. D., Pe'er, A., Svinkin, D., Ulanov, M. V., van der Klis, M., von Kienlin, A., Watts, A. L., and Wilson-Hodge, C. A.
Abstract: On 2009 June 5, the Gamma-ray Burst Monitor (GBM) onboard the Fermi Gamma-ray Space Telescope triggered on two short, and relatively dim bursts with spectral properties similar to Soft Gamma Repeater (SGR) bursts. Independent localizations of the bursts by triangulation with the Konus-RF and with the Swift satellite, confirmed their origin from the same, previously unknown, source. The subsequent discovery of X-ray pulsations with the Rossi X-ray Timing Explorer (RXTE), confirmed the magnetar nature of the new source, SGR J0418+5729. We describe here the Fermi/GBM observations, the discovery and the localization of this new SGR, and our infrared and Chandra X-ray observations. We also present a detailed temporal and spectral study of the two GBM bursts. SGR J0418+5729 is the second source discovered in the same region of the sky in the last year, the other one being SGR J0501+4516. Both sources lie in the direction of the galactic anti-center and presumably at the nearby distance of ~2 kpc (assuming they reside in the Perseus arm of our galaxy). The near-threshold GBM detection of bursts from SGR J0418+5729 suggests that there may be more such dim SGRs throughout our galaxy, possibly exceeding the population of bright SGRs. Finally, using sample statistics, we conclude that the implications of the new SGR discovery on the number of observable active magnetars in our galaxy at any given time is <10, in agreement with our earlier estimates., Comment: 6 pages, 3 figures, 2 tables; accepted for publication in ApJL on 2010 January 8
Published: 2009
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224. The spectral-temporal properties of the prompt pulses and rapid decay phase of GRBs

Author: Willingale, R., Genet, F., Granot, J., O'Brien, P. T., Willingale, R., Genet, F., Granot, J., and O'Brien, P. T.
Abstract: The prompt emission from GRBs is the brightest electromagnetic emission known yet it's origin is not understood. The flux density of individual prompt pulses of a GRB can be represented by an analytical expression derived assuming the emission is from a thin, ultra-relativistically expanding, uniform, spherical shell over a finite range of radii. We present the results of fitting this analytical expression to the lightcurves from the four standard Swift BAT energy bands and two standard Swift XRT energy bands of 12 bursts. The expression includes the High Latitude Emission (HLE) component and the fits provide a rigourous demonstration that the HLE can explain the Rapid Decay Phase (RDP) of the prompt emission. The model also accommodates some aspects of energy-dependent lag and energy-dependent pulse width, but there are features in the data which are not well represented. Some pulses have a hard, narrow peak which is not well fitted or a rise and decay which is faster than expected using the standard indices derived assuming synchrotron emission from internal shocks, although it might be possible to accommodate these features using a different emission mechanism within the same overall framework. The luminosity of pulses is correlated with the peak energy of the pulse spectrum, Lf ~ (Epeak(1+z))^1.8, and anti-correlated with the time since ejection of the pulse, Lf ~ (Tf/(1 + z))^-2.0., Comment: Accepted for publication in MNRAS
Published: 2009
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225. Magnetar Twists: Fermi/Gamma ray Burst Monitor (GBM) detection of SGR J1550-5418

Author: Kaneko, Y., Gogus, E., Kouveliotou, C., Granot, J., Ramirez-Ruiz, E., van der Horst, A. J., Watts, A. L., Finger, M. H., Gehrels, N., Pe'er, A., van der Klis, M., von Kienlin, A., Wachter, S., Wilson-Hodge, C. A., Woods, P. M., Kaneko, Y., Gogus, E., Kouveliotou, C., Granot, J., Ramirez-Ruiz, E., van der Horst, A. J., Watts, A. L., Finger, M. H., Gehrels, N., Pe'er, A., van der Klis, M., von Kienlin, A., Wachter, S., Wilson-Hodge, C. A., and Woods, P. M.
Abstract: SGR J1550-5418 (previously known as AXP 1E 1547.0-5408 or PSR J1550-5418) went into three active bursting episodes in 2008 October and in 2009 January and March, emitting hundreds of typical Soft Gamma Repeater (SGR) bursts in soft gamma-rays. The second episode was especially intense, and our untriggered burst search on Fermi/GBM data (8-1000 keV) revealed ~450 bursts emitted over 24 hours during the peak of this activity. Using the GBM data, we identified a ~150-s-long enhanced persistent emission during 2009 January 22 that exhibited intriguing timing and spectral properties: (i) clear pulsations up to ~110 keV at the spin period of the neutron star (P ~ 2.07 s, the fastest of all magnetars), (ii) an additional (to a power-law) blackbody component required for the enhanced emission spectra with kT ~ 17 keV, (iii) pulsed fraction that is strongly energy dependent and highest in the 50-74 keV energy band. A total isotropic-equivalent energy emitted during this enhanced emission is estimated to be 2.9 x 10^{40} (D/5 kpc)^2 erg. The estimated area of the blackbody emitting region of ~0.046(D/5 kpc)^2 km^2 (roughly a few x 10^{-5} of the neutron star area) is the smallest "hot spot" ever measured for a magnetar and most likely corresponds to the size of magnetically-confined plasma near the neutron star surface., Comment: 21 pages, 5 figures, 1 table, resubmitted to ApJ after addressing the referee's comments
Published: 2009
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226. GRB081028 and its late-time afterglow re-brightening

Author: Margutti, R., Genet, F., Granot, J., Duran, R. Barniol, Guidorzi, C., Chincarini, G., Mao, J., Schady, P., Sakamoto, T., Miller, A. A., Olofsson, G., Bloom, J. S., Evans, P. A., Fynbo, J. P. U., Malesani, D., Moretti, A., Pasotti, F., Starr, D., Burrows, D. N., Barthelmy, S. D., Roming, P. W. A., Gehrels, N., Margutti, R., Genet, F., Granot, J., Duran, R. Barniol, Guidorzi, C., Chincarini, G., Mao, J., Schady, P., Sakamoto, T., Miller, A. A., Olofsson, G., Bloom, J. S., Evans, P. A., Fynbo, J. P. U., Malesani, D., Moretti, A., Pasotti, F., Starr, D., Burrows, D. N., Barthelmy, S. D., Roming, P. W. A., and Gehrels, N.
Abstract: Swift captured for the first time a smoothly rising X-ray re-brightening of clear non-flaring origin after the steep decay in a long gamma-ray burst (GRB): GRB081028. A rising phase is likely present in all GRBs but is usually hidden by the prompt tail emission and constitutes the first manifestation of what is later to give rise to the shallow decay phase. Contemporaneous optical observations reveal a rapid evolution of the injection frequency of a fast cooling synchrotron spectrum through the optical band, which disfavours the afterglow onset (start of the forward shock emission along our line of sight when the outflow is decelerated) as the origin of the observed re-brightening. We investigate alternative scenarios and find that the observations are consistent with the predictions for a narrow jet viewed off-axis. The high on-axis energy budget implied by this interpretation suggests different physical origins of the prompt and (late) afterglow emission. Strong spectral softening takes place from the prompt to the steep decay phase: we track the evolution of the spectral peak energy from the gamma-rays to the X-rays and highlight the problems of the high latitude and adiabatic cooling interpretations. Notably, a softening of both the high and low spectral slopes with time is also observed. We discuss the low on-axis radiative efficiency of GRB081028 comparing its properties against a sample of Swift long GRBs with secure E_gamma,iso measurements., Comment: 22 pages, 11 figures; MNRAS accepted
Published: 2009
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227. Rise and fall of the X-ray flash 080330: an off-axis jet?

Author: Guidorzi, C., Clemens, C., Kobayashi, S., Granot, J., Melandri, A., D'Avanzo, P., Kuin, N. P. M., Klotz, A., Fynbo, J. P. U., Covino, S., Greiner, J., Malesani, D., Mao, J., Mundell, C. G., Steele, I. A., Jakobsson, P., Margutti, R., Bersier, D., Campana, S., Chincarini, G., D'Elia, V., Fugazza, D., Genet, F., Gomboc, A., Kruehler, T., Yoldacs, A. Kupcu, Moretti, A., Mottram, C. J., O'Brien, P. T., Smith, R. J., Szokoly, G., Tagliaferri, G., Tanvir, N. R., Gehrels, N., Guidorzi, C., Clemens, C., Kobayashi, S., Granot, J., Melandri, A., D'Avanzo, P., Kuin, N. P. M., Klotz, A., Fynbo, J. P. U., Covino, S., Greiner, J., Malesani, D., Mao, J., Mundell, C. G., Steele, I. A., Jakobsson, P., Margutti, R., Bersier, D., Campana, S., Chincarini, G., D'Elia, V., Fugazza, D., Genet, F., Gomboc, A., Kruehler, T., Yoldacs, A. Kupcu, Moretti, A., Mottram, C. J., O'Brien, P. T., Smith, R. J., Szokoly, G., Tagliaferri, G., Tanvir, N. R., and Gehrels, N.
Abstract: X-ray flashes (XRFs) are a class of gamma-ray bursts (GRBs) with the peak energy of the time-integrated spectrum, Ep, below 30 keV, whereas classical GRBs have Ep of a few hundreds keV. Apart from Ep and the lower luminosity, the properties of XRFs are typical of the classical GRBs. Yet, the nature of XRFs and the differences from that of GRBs are not understood. In addition, there is no consensus on the interpretation of the shallow decay phase observed in most X-ray afterglows of both XRFs and GRBs. We examine in detail the case of XRF 080330 discovered by Swift at the redshift of 1.51. This burst is representative of the XRF class and exhibits an X-ray shallow decay. The rich and broadband (from NIR to UV) photometric data set we collected across this phase makes it an ideal candidate to test the off-axis jet interpretation proposed to explain both the softness of XRFs and the shallow decay phase. We present prompt gamma-ray, early and late IR/visible/UV and X-ray observations of the XRF 080330. We derive a SED from NIR to X-ray bands across the plateau phase with a power-law index of 0.79 +- 0.01 and negligible rest-frame dust extinction. The multi-wavelength evolution of the afterglow is achromatic from ~10^2 s out to ~8x10^4 s. We describe the temporal evolution of the multi-wavelength afterglow within the context of the standard afterglow model and show that a single-component jet viewed off-axis explains the observations (abriged)., Comment: accepted to A&A, 19 pages, 11 figures
Published: 2009
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228. What Are Gamma-Ray Bursts -- The Unique Role of Very High Energy Gamma-Ray Observations

Author: Williams, D. A., Falcone, A. D., Baring, M. G., Buckley, J., Connaughton, V., Coppi, P., Dermer, C., Digel, S., Dingus, B., Fryer, C., Gehrels, N., Granot, J., Horan, D., Katz, J. I., Meszaros, P., Norris, J., Parkinson, P. Saz, Pe'er, A., Razzaque, S., Sinnis, G., Wang, X. Y., Weekes, T. C., Zhang, B., Williams, D. A., Falcone, A. D., Baring, M. G., Buckley, J., Connaughton, V., Coppi, P., Dermer, C., Digel, S., Dingus, B., Fryer, C., Gehrels, N., Granot, J., Horan, D., Katz, J. I., Meszaros, P., Norris, J., Parkinson, P. Saz, Pe'er, A., Razzaque, S., Sinnis, G., Wang, X. Y., Weekes, T. C., and Zhang, B.
Abstract: Gamma-ray bursts (GRBs) have been an enigma since their discovery forty years ago. However, considerable progress unraveling their mysteries has been made in recent years. Developments in observations, theory, and instrumentation have prepared the way so that the next decade can be the one in which we finally answer the question, "What are gamma-ray bursts?" This question encompasses not only what the progenitors are that produce the GRBs, but also how the enormous luminosity of the GRBs, concentrated in gamma rays, is achieved. Observations across the electromagnetic spectrum, from both the ground and space, will be required to fully tackle this important question. This white paper, mostly distilled from a recent study commissioned by the Division of Astrophysics of the American Physical Society, focuses on what very high energy (~100 GeV and above) gamma-ray observations can contribute. Very high energy gamma rays probe the most extreme high energy particle populations in the burst environment, testing models of lepton and proton acceleration in GRBs and constraining the bulk Lorentz factor and opacity of the outflow. Sensitivity improvements of more than an order of magnitude in the very high energy gamma-ray band can be achieved early in the next decade, in order to contribute to this science., Comment: White paper contributed to the Stars and Stellar Evolution Science Frontier Panel of the Astro2010 Decadal Survey
Published: 2009

229. Is the Rapid Decay Phase from High Latitude Emission?

Author: Genet, F., Granot, J., Genet, F., and Granot, J.
Abstract: There is good observationnal evidence that the Steep Decay Phase (SDP) that is observed in most Swift GRBs is the tail of the prompt emission. The most popular model to explain the SDP is Hight Latitude Emission (HLE). Many models for the prompt emission give rise to HLE, like the popular internal shocks (IS) model, but some models do not, such as sporadic magnetic reconnection events. Knowing if the SDP is consistent with HLE would thus help distinguish between different prompt emission models. In order to test this, we model the prompt emission (and its tail) as the sum of independent pulses (and their tails). A single pulse is modeled as emission arising from an ultra-relativistic thin spherical expanding shell. We obtain analytic expressions for the flux in the IS model with a Band function spectrum. We find that in this framework the observed spectrum is also a Band function, and naturally softens with time. The decay of the SDP is initially dominated by the tail of the last pulse, but other pulses can dominate later. Modeling several overlapping pulses as a single broader pulse would overestimates the SDP flux. One should thus be careful when testing the HLE., Comment: 3 pages, submitted to the proceedings of the Sixth Huntsville gamma-ray bursts symposium
Published: 2009
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230. Rise and fall of the X-ray flash 080330:an off-axis jet ?

Author: Guidorzi, C., Clemens, C., Kobayashi, S., Granot, J., Melandri, A., D'Avanzo, P., Kuin, N.~P.~M., Klotz, A., Fynbo, Johan Peter Uldall, Covino, S., Greiner, J., Malesani, D., Mao, J., Mundell, C.~G., Steele, I.~A., Jakobsson, P., Margutti, R., Bersier, D., Campana, S., Chincarini, G., D'Elia, V., Fugazza, D., Genet, F., Gomboc, A., Krühler, T., Küpcü Yoldas, A., Moretti, A., Mottram, C.~J., O'Brien, P.~T., Smith, R.~J., Szokoly, G., Tagliaferri, G., Tanvir, N.~R., Gehrels, N., Guidorzi, C., Clemens, C., Kobayashi, S., Granot, J., Melandri, A., D'Avanzo, P., Kuin, N.~P.~M., Klotz, A., Fynbo, Johan Peter Uldall, Covino, S., Greiner, J., Malesani, D., Mao, J., Mundell, C.~G., Steele, I.~A., Jakobsson, P., Margutti, R., Bersier, D., Campana, S., Chincarini, G., D'Elia, V., Fugazza, D., Genet, F., Gomboc, A., Krühler, T., Küpcü Yoldas, A., Moretti, A., Mottram, C.~J., O'Brien, P.~T., Smith, R.~J., Szokoly, G., Tagliaferri, G., Tanvir, N.~R., and Gehrels, N.
Abstract: Udgivelsesdato: May
Published: 2009

231. Realistic analytic model for the prompt and high latitude emission in GRBs

Author: Genet, F., Granot, J., Genet, F., and Granot, J.
Abstract: Most gamma-ray bursts (GRBs) observed by the Swift satellite show an early rapid decay phase (RDP) in their X-ray lightcurve, which is usually a smooth continuation of the prompt gamma-ray emission, strongly suggesting that it is its tail. However, the mechanism behind it is still not clear. The most popular model for this RDP is High Latitude Emission (HLE). While HLE is expected in many models for the prompt GRB emission, such as the popular internal shocks model, there are models in which it is not expected, such as sporadic magnetic reconnection events. Therefore, testing whether the RDP is consistent with HLE can help distinguish between different prompt emission models. We address this question by modeling the prompt emission as the sum of its individual pulses with their HLE tails. Analytic expressions for the observed flux density are obtained for power-law and Band function emission spectra. For internal shocks the observed instantaneous spectrum is very close to the emitted one, and should be well described by a Band function also during the RDP. Our model naturally produces, the observed spectral softening and steepening of the flux decay. The observed flux during the RDP is initially dominated by the tail of the last pulse, but the tails of one or more earlier pulses can become dominant later on. Moreover, modeling several overlapping pulses as a single wider pulse would over-predict the emission tail. Thus, one should be very careful when testing the predictions of HLE and do a combined temporal and spectral fit of the prompt GRB emission and the RDP., Comment: 24 pages, 9 figures. Text reorganized. Accepted by MNRAS
Published: 2008
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232. GRB 080503: Implications of a Naked Short Gamma-Ray Burst Dominated by Extended Emission

Author: Perley, D. A., Metzger, B. D., Granot, J., Butler, N. R., Sakamoto, T., Ramirez-Ruiz, E., Levan, A. J., Bloom, J. S., Miller, A. A., Bunker, A., Chen, H. -W., Filippenko, A. V., Gehrels, N., Glazebrook, K., Hall, P. B., Hurley, K. C., Kocevski, D., Li, W., Lopez, S., Norris, J., Piro, A. L., Poznanski, D., Prochaska, J. X., Quataert, E., Tanvir, N., Perley, D. A., Metzger, B. D., Granot, J., Butler, N. R., Sakamoto, T., Ramirez-Ruiz, E., Levan, A. J., Bloom, J. S., Miller, A. A., Bunker, A., Chen, H. -W., Filippenko, A. V., Gehrels, N., Glazebrook, K., Hall, P. B., Hurley, K. C., Kocevski, D., Li, W., Lopez, S., Norris, J., Piro, A. L., Poznanski, D., Prochaska, J. X., Quataert, E., and Tanvir, N.
Abstract: We report on observations of GRB 080503, a short gamma-ray burst with very bright extended emission (about 30 times the gamma-ray fluence of the initial spike) in conjunction with a thorough comparison to other short Swift events. In spite of the prompt-emission brightness, however, the optical counterpart is extraordinarily faint, never exceeding 25 mag in deep observations starting at ~1 hr after the BAT trigger. The optical brightness peaks at ~1 day and then falls sharply in a manner similar to the predictions of Li & Paczynski (1998) for supernova-like emission following compact-binary mergers. However, a shallow spectral index and similar evolution in X-rays inferred from Chandra observations are more consistent with an afterglow interpretation. The extreme faintness of this probable afterglow relative to the bright gamma-ray emission argues for a very low-density medium surrounding the burst (a "naked" GRB), consistent with the lack of a coincident host galaxy down to 28.5 mag in deep HST imaging. Our observations reinforce the notion that short GRBs generally occur outside regions of active star formation, but demonstrate that in some cases the luminosity of the extended prompt emission can greatly exceed that of the short spike, which may constrain theoretical interpretation of this class of events. Because most previous BAT short bursts without observed extended emission are too faint for this signature to have been detectable even if it were present at typical level, conclusions based solely on the observed presence or absence of extended emission in the existing Swift sample are premature. (abridged), Comment: 16 pages, 11 figures; accepted for publication in ApJ
Published: 2008
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233. Gamma Ray Burst Section of the White Paper on the Status and Future of Ground-based TeV Gamma-ray Astronomy

Author: Falcone, A. D., Williams, D. A., Baring, M. G., Blandford, R., Buckley, J., Connaughton, V., Coppi, P., Dermer, C., Dingus, B., Fryer, C., Gehrels, N., Granot, J., Horan, D., Katz, J. I., Kuehn, K., Meszaros, P., Norris, J., Parkinson, P. Saz, Pe'er, A., Ramirez-Ruiz, E., Razzaque, S., Wang, X. Y., Zhang, B., Falcone, A. D., Williams, D. A., Baring, M. G., Blandford, R., Buckley, J., Connaughton, V., Coppi, P., Dermer, C., Dingus, B., Fryer, C., Gehrels, N., Granot, J., Horan, D., Katz, J. I., Kuehn, K., Meszaros, P., Norris, J., Parkinson, P. Saz, Pe'er, A., Ramirez-Ruiz, E., Razzaque, S., Wang, X. Y., and Zhang, B.
Abstract: This is a report on the findings of the gamma ray burst working group for the white paper on the status and future of TeV gamma-ray astronomy. The white paper is an APS commissioned document, and the overall version has also been released and can be found on astro-ph. This detailed section of the white paper discusses the status of past and current attempts to observe gamma ray bursts at GeV-TeV energies. We concentrate on the potential of future ground-based gamma-ray experiments to observe the highest energy emission ever recorded for GRBs, particularly for those that are nearby and have high Lorentz factors in the GRB jet. It is clear that major advances are possible and that the detection of very high energy emission would have strong implications for GRB models, as well as cosmic ray origin., Comment: report from the Gamma Ray Burst Working group of the APS commissioned White paper on ground-based TeV gamma ray astronomy
Published: 2008

234. SN 2001em: Not so Fast

Author: Schinzel, F. K., Taylor, G. B., Stockdale, C. J., Granot, J., Ramirez-Ruiz, E., Schinzel, F. K., Taylor, G. B., Stockdale, C. J., Granot, J., and Ramirez-Ruiz, E.
Abstract: SN 2001em is a peculiar supernova, originally classified as Type Ib/c. About two years after the SN it was detected in the radio, showing a rising radio flux with an optically thin spectral slope, and it also displayed a large X-ray luminosity (~10^{41} erg/s). Thus it was suspected to harbor a decelerating (by then, mildly) relativistic jet pointing away from us. About 3 years after its discovery the optical spectrum of SN 2001em showed a broad H-alpha line, and it was therefore reclassified as Type IIn. Here we constrain its proper motion and expansion velocity by analyzing four epochs of VLBI observations, extending out to 5.4 years after the SN. The supernova is still unresolved 5.4 years after the explosion. For the proper motion we obtain (23,000 +/- 30,000) km/s while our 2-sigma upper limit on the expansion velocity is 6000 km/s. These limits are somewhat tighter than those derived by Bietenholz & Bartel, and confirm their conclusion that late time emission from SN 2001em, a few years after the explosion, is not driven by a relativistic jet. VLA observations of the radio flux density, at 8.46 GHz, show a decay as t^{-1.23 +/- 0.40} starting ~2.7 years after the SN. Collectively, the observations suggest interaction of the SN ejecta with a very dense circumstellar medium, though the implied opacity constraints still present a challenge., Comment: 21 pages, 8 figures, 4 tables, accepted for publication in ApJ (10/02/2008)
Published: 2008
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235. An infrared ring around the magnetar SGR 1900+14

Author: Wachter, S., Ramirez-Ruiz, E., Dwarkadas, V. V., Kouveliotou, C., Granot, J., Patel, S. K., Figer, D., Wachter, S., Ramirez-Ruiz, E., Dwarkadas, V. V., Kouveliotou, C., Granot, J., Patel, S. K., and Figer, D.
Abstract: Magnetars are a special class of slowly rotating neutron stars with extremely strong magnetic fields -- at least an order of magnitude larger than those of the "normal" radio pulsars. The potential evolutionary links and differences between these two types of objects are still unknown; recent studies, however, have provided circumstantial evidence connecting magnetars with very massive progenitor stars. Here we report the discovery of an infrared elliptical ring or shell surrounding the magnetar SGR 1900+14. The appearance and energetics of the ring are difficult to interpret within the framework of the progenitor's stellar mass loss or the subsequent evolution of the supernova remnant. We suggest instead that a dust-free cavity was produced in the magnetar environment by the giant flare emitted by the source in August 1998. Considering the total energy released in the flare, the theoretical dust--destruction radius matches well with the observed dimensions of the ring. We conclude that SGR 1900+14 is unambiguously associated with a cluster of massive stars, thereby solidifying the link between magnetars and massive stars., Comment: 19 pages, 1 figure
Published: 2008
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236. GRB 080319B: A Naked-Eye Stellar Blast from the Distant Universe

Author: Racusin, J. L., Karpov, S. V., Sokolowski, M., Granot, J., Wu, X. F., Pal'shin, V., Covino, S., van der Horst, A. J., Oates, S. R., Schady, P., Smith, R. J., Cummings, J., Starling, R. L. C., Piotrowski, L. W., Zhang, B., Evans, P. A., Holland, S. T., Malek, K., Page, M. T., Vetere, L., Margutti, R., Guidorzi, C., Kamble, A., Curran, P. A., Beardmore, A., Kouveliotou, C., Mankiewicz, L., Melandri, A., O'Brien, P. T., Page, K. L., Piran, T., Tanvir, N. R., Wrochna, G., Aptekar, R. L., Bartolini, C., Barthelmy, S., Beskin, G. M., Bondar, S., Campana, S., Cucchiara, A., Cwiok, M., D'Avanzo, P., D'Elia, V., Della Valle, M., Dominik, W., Falcone, A., Fiore, F., Fox, D. B., Frederiks, D. D., Fruchter, A. S., Fugazza, D., Garrett, M., Gehrels, N., Golenetskii, S., Gomboc, A., Greco, G., Guarnieri, A., Immler, S., Kasprowicz, G., Levan, A. J., Mazets, E. P., Molinari, E., Moretti, A., Nawrocki, K., Oleynik, P. P., Osborne, J. P., Pagani, C., Paragi, Z., Perri, M., Piccioni, A., Ramirez-Ruiz, E., Roming, P. W. A., Steele, I. A., Strom, R. G., Testa, V., Tosti, G., Ulanov, M. V., Wiersema, K., Wijers, R. A. M. J., Zarnecki, A. F., Zerbi, F., Meszaros, P., Chincarini, G., Burrows, D. N., Racusin, J. L., Karpov, S. V., Sokolowski, M., Granot, J., Wu, X. F., Pal'shin, V., Covino, S., van der Horst, A. J., Oates, S. R., Schady, P., Smith, R. J., Cummings, J., Starling, R. L. C., Piotrowski, L. W., Zhang, B., Evans, P. A., Holland, S. T., Malek, K., Page, M. T., Vetere, L., Margutti, R., Guidorzi, C., Kamble, A., Curran, P. A., Beardmore, A., Kouveliotou, C., Mankiewicz, L., Melandri, A., O'Brien, P. T., Page, K. L., Piran, T., Tanvir, N. R., Wrochna, G., Aptekar, R. L., Bartolini, C., Barthelmy, S., Beskin, G. M., Bondar, S., Campana, S., Cucchiara, A., Cwiok, M., D'Avanzo, P., D'Elia, V., Della Valle, M., Dominik, W., Falcone, A., Fiore, F., Fox, D. B., Frederiks, D. D., Fruchter, A. S., Fugazza, D., Garrett, M., Gehrels, N., Golenetskii, S., Gomboc, A., Greco, G., Guarnieri, A., Immler, S., Kasprowicz, G., Levan, A. J., Mazets, E. P., Molinari, E., Moretti, A., Nawrocki, K., Oleynik, P. P., Osborne, J. P., Pagani, C., Paragi, Z., Perri, M., Piccioni, A., Ramirez-Ruiz, E., Roming, P. W. A., Steele, I. A., Strom, R. G., Testa, V., Tosti, G., Ulanov, M. V., Wiersema, K., Wijers, R. A. M. J., Zarnecki, A. F., Zerbi, F., Meszaros, P., Chincarini, G., and Burrows, D. N.
Abstract: Long duration gamma-ray bursts (GRBs) release copious amounts of energy across the entire electromagnetic spectrum, and so provide a window into the process of black hole formation from the collapse of a massive star. Over the last forty years, our understanding of the GRB phenomenon has progressed dramatically; nevertheless, fortuitous circumstances occasionally arise that provide access to a regime not yet probed. GRB 080319B presented such an opportunity, with extraordinarily bright prompt optical emission that peaked at a visual magnitude of 5.3, making it briefly visible with the naked eye. It was captured in exquisite detail by wide-field telescopes, imaging the burst location from before the time of the explosion. The combination of these unique optical data with simultaneous gamma-ray observations provides powerful diagnostics of the detailed physics of this explosion within seconds of its formation. Here we show that the prompt optical and gamma-ray emissions from this event likely arise from different spectral components within the same physical region located at a large distance from the source, implying an extremely relativistic outflow. The chromatic behaviour of the broadband afterglow is consistent with viewing the GRB down the very narrow inner core of a two-component jet that is expanding into a wind-like environment consistent with the massive star origin of long GRBs. These circumstances can explain the extreme properties of this GRB., Comment: 43 pages, 18 figures, 3 tables, submitted to Nature May 11, 2008
Published: 2008
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237. The Gamma Ray Burst section of the White Paper on the Status and Future of Very High Energy Gamma Ray Astronomy: A Brief Preliminary Report

Author: Falcone, A. D., Williams, D. A., Baring, M. G., Blandford, R., Connaughton, V., Coppi, P., Dermer, C., Dingus, B., Fryer, C., Gehrels, N., Granot, J., Horan, D., Katz, J. I., Kuehn, K., Meszaros, P., Norris, J., Parkinson, P. Saz, Peer, A., Ramirez-Ruiz, E., Razzaque, S., Wang, X., Zhang, B., Falcone, A. D., Williams, D. A., Baring, M. G., Blandford, R., Connaughton, V., Coppi, P., Dermer, C., Dingus, B., Fryer, C., Gehrels, N., Granot, J., Horan, D., Katz, J. I., Kuehn, K., Meszaros, P., Norris, J., Parkinson, P. Saz, Peer, A., Ramirez-Ruiz, E., Razzaque, S., Wang, X., and Zhang, B.
Abstract: This is a short report on the preliminary findings of the gamma ray burst (GRB) working group for the white paper on the status and future of very high energy (VHE; >50 GeV) gamma-ray astronomy. The white paper discusses the status of past and current attempts to observe GRBs at GeV-TeV energies, including a handful of low-significance, possible detections. The white paper concentrates on the potential of future ground-based gamma-ray experiments to observe the highest energy emission ever recorded for GRBs, particularly for those that are nearby and have high Lorentz factors in the GRB jet. It is clear that the detection of VHE emission would have strong implications for GRB models, as well as cosmic ray origin. In particular, the extended emission phase (including both afterglow emission and possible flaring) of nearby long GRBs could provide the best possibility for detection. The difficult-to-obtain observations during the prompt phase of nearby long GRBs and short GRBs could also provide particularly strong constraints on the opacity and bulk Lorentz factors surrounding the acceleration site. The synergy with upcoming and existing observatories will, of course, be critical for both identification of GRBs and for multiwavelength/multimessenger studies., Comment: to appear in Proceedings of Gamma Ray Bursts 2007 Meeting, Santa Fe, New Mexico; 5 pages, 4 figures
Published: 2008
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238. Broadband observations of the naked-eye [gamma]-ray burst GRB 080319B

Author: Racusin, J., Karpov, S., Sokolowski, Marcin, Granot, J., Wu, X., Pal’shin, V., Covino, S., van der Horst, A., Oates, S., Schady, P., Smith, R., Cummings, J., Starling, R., Piotrowski, L., Zhang, B., Evans, P., Holland, S., Malek, K., Page, M., Vetere, L., Margutti, R., Guidorzi, C., Kamble, A., Curran, Peter, Beardmore, A., Kouveliotou, C., Mankiewicz, L., Melandri, A., O’Brien, P., Page, K., Piran, T., Tanvir, N., Wrochna, G., Aptekar, R., Barthelmy, S., Bartolini, C., Beskin, G., Bondar, S., Bremer, M., Campana, S., Castro-Tirado, A., Cucchiara, A., Cwiok, M., D’Avanzo, P., D’Elia, V., Della Valle, M., de Ugarte Postigo, A., Dominik, W., Falcone, A., Fiore, F., Fox, D., Frederiks, D., Fruchter, A., Fugazza, D., Garrett, M., Gehrels, N., Golenetskii, S., Gomboc, A., Gorosabel, J., Greco, G., Guarnieri, A., Immler, S., Jelinek, M., Kasprowicz, G., La Parola, V., Levan, A., Mangano, V., Mazets, E., Molinari, E., Moretti, A., Nawrocki, K., Oleynik, P., Osborne, J., Pagani, C., Pandey, S., Paragi, Z., Perri, M., Piccioni, A., Ramirez-Ruiz, E., Roming, P., Steele, I., Strom, R., Testa, V., Tosti, G., Ulanov, M., Wiersema, K., Wijers, R., Winters, J., Zarnecki, A., Zerbi, F., Meszaros, P., Chincarini, G., Burrows, D., Racusin, J., Karpov, S., Sokolowski, Marcin, Granot, J., Wu, X., Pal’shin, V., Covino, S., van der Horst, A., Oates, S., Schady, P., Smith, R., Cummings, J., Starling, R., Piotrowski, L., Zhang, B., Evans, P., Holland, S., Malek, K., Page, M., Vetere, L., Margutti, R., Guidorzi, C., Kamble, A., Curran, Peter, Beardmore, A., Kouveliotou, C., Mankiewicz, L., Melandri, A., O’Brien, P., Page, K., Piran, T., Tanvir, N., Wrochna, G., Aptekar, R., Barthelmy, S., Bartolini, C., Beskin, G., Bondar, S., Bremer, M., Campana, S., Castro-Tirado, A., Cucchiara, A., Cwiok, M., D’Avanzo, P., D’Elia, V., Della Valle, M., de Ugarte Postigo, A., Dominik, W., Falcone, A., Fiore, F., Fox, D., Frederiks, D., Fruchter, A., Fugazza, D., Garrett, M., Gehrels, N., Golenetskii, S., Gomboc, A., Gorosabel, J., Greco, G., Guarnieri, A., Immler, S., Jelinek, M., Kasprowicz, G., La Parola, V., Levan, A., Mangano, V., Mazets, E., Molinari, E., Moretti, A., Nawrocki, K., Oleynik, P., Osborne, J., Pagani, C., Pandey, S., Paragi, Z., Perri, M., Piccioni, A., Ramirez-Ruiz, E., Roming, P., Steele, I., Strom, R., Testa, V., Tosti, G., Ulanov, M., Wiersema, K., Wijers, R., Winters, J., Zarnecki, A., Zerbi, F., Meszaros, P., Chincarini, G., and Burrows, D.
Abstract: Long-duration c-ray bursts (GRBs) release copious amounts of energy across the entire electromagnetic spectrum, and soprovide a window into the process of black hole formation from the collapse of massive stars. Previous early opticalobservations of even the most exceptional GRBs (990123 and 030329) lacked both the temporal resolution to probe theoptical flash in detail and the accuracy needed to trace the transition from the prompt emission within the outflowto externalshocks caused by interaction with the progenitor environment. Here we report observations of the extraordinarily brightprompt optical and c-ray emission of GRB 080319B that provide diagnostics within seconds of its formation, followed bybroadband observations of the afterglow decay that continued for weeks. We show that the prompt emission stems from asingle physical region, implying an extremely relativistic outflow that propagates within the narrow inner core of atwo-component jet.
Published: 2008

239. NuSTAR OBSERVATIONS OF GRB 130427A ESTABLISH A SINGLE COMPONENT SYNCHROTRON AFTERGLOW ORIGIN FOR THE LATE OPTICAL TO MULTI-GEV EMISSION

Author: Kouveliotou, C., primary, Granot, J., additional, Racusin, J. L., additional, Bellm, E., additional, Vianello, G., additional, Oates, S., additional, Fryer, C. L., additional, Boggs, S. E., additional, Christensen, F. E., additional, Craig, W. W., additional, Dermer, C. D., additional, Gehrels, N., additional, Hailey, C. J., additional, Harrison, F. A., additional, Melandri, A., additional, McEnery, J. E., additional, Mundell, C. G., additional, Stern, D. K., additional, Tagliaferri, G., additional, and Zhang, W. W., additional
Published: 2013
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240. Broad-band monitoring tracing the evolution of the jet and disc in the black hole candidate X-ray binary MAXI J1659−152

Author: van der Horst, A. J., primary, Curran, P. A., additional, Miller-Jones, J. C. A., additional, Linford, J. D., additional, Gorosabel, J., additional, Russell, D. M., additional, de Ugarte Postigo, A., additional, Lundgren, A. A., additional, Taylor, G. B., additional, Maitra, D., additional, Guziy, S., additional, Belloni, T. M., additional, Kouveliotou, C., additional, Jonker, P. G., additional, Kamble, A., additional, Paragi, Z., additional, Homan, J., additional, Kuulkers, E., additional, Granot, J., additional, Altamirano, D., additional, Buxton, M. M., additional, Castro-Tirado, A., additional, Fender, R. P., additional, Garrett, M. A., additional, Gehrels, N., additional, Hartmann, D. H., additional, Kennea, J. A., additional, Krimm, H. A., additional, Mangano, V., additional, Ramirez-Ruiz, E., additional, Romano, P., additional, Wijers, R. A. M. J., additional, Wijnands, R., additional, and Yang, Y. J., additional
Published: 2013
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241. NEWFERMI-LAT EVENT RECONSTRUCTION REVEALS MORE HIGH-ENERGY GAMMA RAYS FROM GAMMA-RAY BURSTS

Author: Atwood, W. B., primary, Baldini, L., additional, Bregeon, J., additional, Bruel, P., additional, Chekhtman, A., additional, Cohen-Tanugi, J., additional, Drlica-Wagner, A., additional, Granot, J., additional, Longo, F., additional, Omodei, N., additional, Pesce-Rollins, M., additional, Razzaque, S., additional, Rochester, L. S., additional, Sgrò, C., additional, Tinivella, M., additional, Usher, T. L., additional, and Zimmer, S., additional
Published: 2013
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242. Constraints on Lorentz invariance violation fromFermi-Large Area Telescope observations of gamma-ray bursts

Author: Vasileiou, V., primary, Jacholkowska, A., additional, Piron, F., additional, Bolmont, J., additional, Couturier, C., additional, Granot, J., additional, Stecker, F. W., additional, Cohen-Tanugi, J., additional, and Longo, F., additional
Published: 2013
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243. VLBI observations of the shortest orbital period black hole binary, MAXI J1659−152

Author: Paragi, Z., primary, van der Horst, A. J., additional, Belloni, T., additional, Miller-Jones, J. C. A., additional, Linford, J., additional, Taylor, G., additional, Yang, J., additional, Garrett, M. A., additional, Granot, J., additional, Kouveliotou, C., additional, Kuulkers, E., additional, and Wijers, R. A. M. J., additional
Published: 2013
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244. MULTIWAVELENGTH OBSERVATIONS OF GRB 110731A: GeV EMISSION FROM ONSET TO AFTERGLOW

Author: Ackermann, M., primary, Ajello, M., additional, Asano, K., additional, Baldini, L., additional, Barbiellini, G., additional, Baring, M. G., additional, Bastieri, D., additional, Bellazzini, R., additional, Blandford, R. D., additional, Bonamente, E., additional, Borgland, A. W., additional, Bottacini, E., additional, Bregeon, J., additional, Brigida, M., additional, Bruel, P., additional, Buehler, R., additional, Buson, S., additional, Caliandro, G. A., additional, Cameron, R. A., additional, Caraveo, P. A., additional, Cecchi, C., additional, Charles, E., additional, Chaves, R. C. G., additional, Chekhtman, A., additional, Chiang, J., additional, Ciprini, S., additional, Claus, R., additional, Cohen-Tanugi, J., additional, Conrad, J., additional, Cutini, S., additional, D'Ammando, F., additional, de Angelis, A., additional, de Palma, F., additional, Dermer, C. D., additional, do Couto e Silva, E., additional, Drell, P. S., additional, Drlica-Wagner, A., additional, Favuzzi, C., additional, Fegan, S. J., additional, Focke, W. B., additional, Franckowiak, A., additional, Fukazawa, Y., additional, Fusco, P., additional, Gargano, F., additional, Gasparrini, D., additional, Gehrels, N., additional, Giglietto, N., additional, Giordano, F., additional, Giroletti, M., additional, Glanzman, T., additional, Godfrey, G., additional, Granot, J., additional, Greiner, J., additional, Grenier, I. A., additional, Grove, J. E., additional, Guiriec, S., additional, Hadasch, D., additional, Hanabata, Y., additional, Hayashida, M., additional, Hays, E., additional, Hughes, R. E., additional, Jackson, M. S., additional, Jogler, T., additional, Jóhannesson, G., additional, Johnson, A. S., additional, Knödlseder, J., additional, Kocevski, D., additional, Kuss, M., additional, Lande, J., additional, Larsson, S., additional, Latronico, L., additional, Longo, F., additional, Loparco, F., additional, Lovellette, M. N., additional, Lubrano, P., additional, Mazziotta, M. N., additional, McEnery, J. E., additional, Mehault, J., additional, Mészáros, P., additional, Michelson, P. F., additional, Mitthumsiri, W., additional, Mizuno, T., additional, Monte, C., additional, Monzani, M. E., additional, Moretti, E., additional, Morselli, A., additional, Moskalenko, I. V., additional, Murgia, S., additional, Naumann-Godo, M., additional, Norris, J. P., additional, Nuss, E., additional, Nymark, T., additional, Ohno, M., additional, Ohsugi, T., additional, Omodei, N., additional, Orienti, M., additional, Orlando, E., additional, Paneque, D., additional, Perkins, J. S., additional, Pesce-Rollins, M., additional, Piron, F., additional, Pivato, G., additional, Racusin, J. L., additional, Rainò, S., additional, Rando, R., additional, Razzano, M., additional, Razzaque, S., additional, Reimer, A., additional, Reimer, O., additional, Romoli, C., additional, Roth, M., additional, Ryde, F., additional, Sanchez, D. A., additional, Sgrò, C., additional, Siskind, E. J., additional, Sonbas, E., additional, Spinelli, P., additional, Stamatikos, M., additional, Takahashi, H., additional, Tanaka, T., additional, Thayer, J. G., additional, Thayer, J. B., additional, Tibaldo, L., additional, Tinivella, M., additional, Tosti, G., additional, Troja, E., additional, Usher, T. L., additional, Vandenbroucke, J., additional, Vasileiou, V., additional, Vianello, G., additional, Vitale, V., additional, Waite, A. P., additional, Winer, B. L., additional, Wood, K. S., additional, Yang, Z., additional, Gruber, D., additional, Bhat, P. N., additional, Bissaldi, E., additional, Briggs, M. S., additional, Burgess, J. M., additional, Connaughton, V., additional, Foley, S., additional, Kippen, R. M., additional, Kouveliotou, C., additional, McBreen, S., additional, McGlynn, S., additional, Paciesas, W. S., additional, Pelassa, V., additional, Preece, R., additional, Rau, A., additional, van der Horst, A. J., additional, von Kienlin, A., additional, Kann, D. A., additional, Filgas, R., additional, Klose, S., additional, Krühler, T., additional, Fukui, A., additional, Sako, T., additional, Tristram, P. J., additional, Oates, S. R., additional, Ukwatta, T. N., additional, and Littlejohns, O., additional
Published: 2013
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245. Gamma-Ray Burst Jet Dynamics

Author: Granot, J., primary
Published: 2013
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246. Stirring the Embers: High Sensitivity VLBI Observations of GRB030329

Author: Pihlström, Y. M., Taylor, G. B., Granot, J., Doeleman, S., Pihlström, Y. M., Taylor, G. B., Granot, J., and Doeleman, S.
Abstract: We present high sensitivity Very Long Baseline Interferometry (VLBI) observations 806 days after the gamma-ray burst of 2003 March 29 (GRB030329). The angular diameter of the radio afterglow is measured to be 0.347 +- 0.09 mas, corresponding to 0.99 +- 0.26 pc at the redshift of GRB030329 (z = 0.1685). The evolution of the image size favors a uniform external density over an R^-2 wind-like density profile (at distances of R >~10^18 cm from the source), although the latter cannot be ruled out yet. The current apparent expansion velocity of the image size is only mildly relativistic, suggesting a non-relativistic transition time of t_NR ~ 1 yr. A rebrightening, or at least a significant flattening in the flux decay, is expected within the next several years as the counter-jet becomes visible (this has not yet been observed). An upper limit of <1.9c is set on the proper motion of the flux centroid., Comment: 16 pages, 5 figures, accepted for publication in Astrophysical Journal
Published: 2007
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247. GRB 060714: No Clear Dividing Line Between Prompt Emission and X-ray Flares

Author: Krimm, H. A., Granot, J., Marshal, F., Perri, M., Barthelmy, S. D., Burrows, D. N., Gehrels, N., Mészáros, P., Morris, D., Krimm, H. A., Granot, J., Marshal, F., Perri, M., Barthelmy, S. D., Burrows, D. N., Gehrels, N., Mészáros, P., and Morris, D.
Abstract: The long gamma-ray burst GRB 060714 was observed to exhibit a series of five X-ray flares beginning ~70 s after the burst trigger T0 and continuing until T0 + ~200 s. The first two flares were detected by the Burst Alert Telescope (BAT) on the Swift satellite, before Swift had slewed to the burst location, while the last three flares were strongly detected by the X-Ray Telescope (XRT) but only weakly detected by the BAT. This burst provides an unusual opportunity to track a complete sequence of flares over a wide energy range. The flares were very similar in their light curve morphology, showing power-law rise and fall components, and in most cases significant sub-structure. The flares also showed strong evolution with time, both spectrally and temporally. The small time scale and large amplitude variability observed are incompatible with an external shock origin for the flares, and support instead late time sporadic activity either of the central source or of localized dissipation events within the outflow. We show that the flares in GRB 060714 cannot be the result of internal shocks in which the contrast in the Lorentz factor of the colliding shells is very small, and that this mechanism faces serious difficulties in most Swift GRBs. The morphological similarity of the flares and the prompt emission and the gradual and continual evolution of the flares with time makes it difficult and arbitrary to draw a dividing line between the prompt emission and the flares., Comment: Submitted to ApJ
Published: 2007
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248. Swift detects a remarkable gamma-ray burst, GRB 060614, that introduces a new classification scheme

Author: Gehrels, N., Norris, J. P., Mangano, V., Barthelmy, S. D., Burrows, D. N., Granot, J., Kaneko, Y., Kouveliotou, C., Markwardt, C. B., Meszaros, P., Nakar, E., Nousek, J. A., O'Brien, P. T., Page, M., Palmer, D. M., Parsons, A. M., Roming, P. W. A., Sakamoto, T., Sarazin, C. L., Schady, P., Stamatikos, M., Woosley, S. E., Gehrels, N., Norris, J. P., Mangano, V., Barthelmy, S. D., Burrows, D. N., Granot, J., Kaneko, Y., Kouveliotou, C., Markwardt, C. B., Meszaros, P., Nakar, E., Nousek, J. A., O'Brien, P. T., Page, M., Palmer, D. M., Parsons, A. M., Roming, P. W. A., Sakamoto, T., Sarazin, C. L., Schady, P., Stamatikos, M., and Woosley, S. E.
Abstract: Gamma ray bursts (GRBs) are known to come in two duration classes, separated at ~2 s. Long bursts originate from star forming regions in galaxies, have accompanying supernovae (SNe) when near enough to observe and are likely caused by massive-star collapsars. Recent observations show that short bursts originate in regions within their host galaxies with lower star formation rates consistent with binary neutron star (NS) or NS - black hole (BH) mergers. Moreover, although their hosts are predominantly nearby galaxies, no SNe have been so far associated with short GRBs. We report here on the bright, nearby GRB 060614 that does not fit in either class. Its ~102 s duration groups it with long GRBs, while its temporal lag and peak luminosity fall entirely within the short GRB subclass. Moreover, very deep optical observations exclude an accompanying supernova, similar to short GRBs. This combination of a long duration event without accompanying SN poses a challenge to both a collapsar and merging NS interpretation and opens the door on a new GRB classification scheme that straddles both long and short bursts., Comment: 13 pages, 2 figures, accepted in Nature
Published: 2006
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249. The Giant Flare from SGR 1806-20 and its Radio Afterglow

Author: Taylor, G. B., Granot, J., Taylor, G. B., and Granot, J.
Abstract: The multi-wavelength observations of the 2004 December~27 Giant Flare (GF) from SGR 1806-20 and its long-lived radio afterglow are briefly reviewed. The GF appears to have been produced by a dramatic reconfiguration of the magnetic field near the surface of the neutron star, possibly accompanied by fractures in the crust. The explosive release of over 10^46 ergs (isotropic equivalent) powered a one-sided mildly relativistic outflow. The outflow produced a new expanding radio nebula, that is still visible over a year after the GF. Also considered are the constraints on the total energy in the GF, the energy and mass in the outflow, and on the external density, as well as possible implications for short gamma-ray bursts and potential signatures in high energy neutrinos, photons, or cosmic rays. Some possible future observations of this and other GFs are briefly discussed., Comment: 25 pages, 7 figures, accepted for publication in Modern Physics Letters A
Published: 2006
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250. Prompt and Afterglow Emission Properties of Gamma-Ray Bursts with Spectroscopically Identified Supernovae

Author: Kaneko, Y., Ramirez-Ruiz, E., Granot, J., Kouveliotou, C., Woosley, S. E., Patel, S. K., Rol, E., Zand, J. J. M. in't, van der Horst, A. J., Wijers, R. A. M. J., Strom, R., Kaneko, Y., Ramirez-Ruiz, E., Granot, J., Kouveliotou, C., Woosley, S. E., Patel, S. K., Rol, E., Zand, J. J. M. in't, van der Horst, A. J., Wijers, R. A. M. J., and Strom, R.
Abstract: We present a detailed spectral analysis of the prompt and afterglow emission of four nearby long-soft gamma-ray bursts (GRBs 980425, 030329, 031203, and 060218) that were spectroscopically found to be associated with type Ic supernovae, and compare them to the general GRB population. For each event, we investigate the spectral and luminosity evolution, and estimate the total energy budget based upon broadband observations. The observational inventory for these events has become rich enough to allow estimates of their energy content in relativistic and sub-relativistic form. The result is a global portrait of the effects of the physical processes responsible for producing long-soft GRBs. In particular, we find that the values of the energy released in mildly relativistic outflows appears to have a significantly smaller scatter than those found in highly relativistic ejecta. This is consistent with a picture in which the energy released inside the progenitor star is roughly standard, while the fraction of that energy that ends up in highly relativistic ejecta outside the star can vary dramatically between different events., Comment: 55 pages including 23 figures and 8 tables. Accepted for publication in ApJ. Replaced with the accepted version
Published: 2006
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