Author: "Van Der Horst, AJ" / Language: english - Searchworks@Jio Institute Digital Library Search Results

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24 results on '"Van Der Horst, AJ"'

1. The first pulse of the extremely bright GRB 130427a: A test lab for synchrotron shocks

Author: Preece, R, Burgess, JM, Von Kienlin, A, Bhat, PN, Briggs, MS, Byrne, D, Chaplin, V, Cleveland, W, Collazzi, AC, Connaughton, V, Diekmann, A, Fitzpatrick, G, Foley, S, Gibby, M, Giles, M, Goldstein, A, Greiner, J, Gruber, D, Jenke, P, Kippen, RM, Kouveliotou, C, McBreen, S, Meegan, C, Paciesas, WS, Pelassa, V, Tierney, D, Van Der Horst, AJ, Wilson-Hodge, C, Xiong, S, Younes, G, Yu, HF, Ackermann, M, Ajello, M, Axelsson, M, Baldini, L, Barbiellini, G, Baring, MG, Bastieri, D, Bellazzini, R, Bissaldi, E, Bonamente, E, Bregeon, J, Brigida, M, Bruel, P, Buehler, R, Buson, S, Caliandro, GA, Cameron, RA, Caraveo, PA, Cecchi, C, Charles, E, Chekhtman, A, Chiang, J, Chiaro, G, Ciprini, S, Claus, R, Cohen-Tanugi, J, Cominsky, LR, Conrad, J, D'Ammando, F, De Angelis, A, De Palma, F, Dermer, CD, Desiante, R, Digel, SW, Di Venere, L, Drell, PS, Drlica-Wagner, A, Favuzzi, C, Franckowiak, A, Fukazawa, Y, Fusco, P, Gargano, F, Gehrels, N, Germani, S, Giglietto, N, and Giordano, F
Subjects: Astrophysics::High Energy Astrophysical Phenomena
Abstract: Gamma-ray burst (GRB) 130427A is one of the most energetic GRBs ever observed. The initial pulse up to 2.5 seconds is possibly the brightest well-isolated pulse observed to date. A fine time resolution spectral analysis shows power-law decays of the peak energy from the onset of the pulse, consistent with models of internal synchrotron shock pulses. However, a strongly correlated power-law behavior is observed between the luminosity and the spectral peak energy that is inconsistent with curvature effects arising in the relativistic outflow. It is difficult for any of the existing models to account for all of the observed spectral and temporal behaviors simultaneously.
Published: 2014
Full Text: View/download PDF

2. Measurement of ZZ Production in Leptonic Final States at root s of 1.96 TeV at CDF

Author: Aaltonen, T., Alvarez Gonzalez, B., Amerio, S., Amidei, D., Anastassov, A., Annovi, A., Antos, J., Apollinari, G., Appel, J. A., Arisawa, T., Artikov, A., Asaadi, J., Ashmanskas, W., Auerbach, B., Aurisano, A., Azfar, F., Badgett, W., Bae, T., Barbaro Galtieri, A., Barnes, V. E., Barnett, B. A., Barria, P., Bartos, P., Bauce, M., Bedeschi, F., Behari, S., Bellettini, G., Bellinger, J., Benjamin, D., Beretvas, A., Bhatti, A., Bisello, D., Bizjak, I., Bland, K. R., Blumenfeld, B., Bocci, A., Bodek, A., Bortoletto, D., Boudreau, J., Boveia, A., Brigliadori, L., Bromberg, C., Brucken, E., Budagov, J., Budd, H. S., Burkett, K., Busetto, G., Bussey, P., Buzatu, A., Calamba, A., Calancha, C., Camarda, S., Campanelli, M., Campbell, M., Canelli, F., Carls, B., Carlsmith, D., Carosi, R., Carrillo, S., Carron, S., Casal, B., Casarsa, M., Castro, A., Catastini, P., Cauz, D., Cavaliere, V., Cavalli Sforza, M., Cerri, A., Cerrito, L., Chen, Y. C., Chertok, M., Chiarelli, G., Chlachidze, G., Chlebana, F., Cho, K., Chokheli, D., Chung, W. H., Chung, Y. S., Ciocci, MARIA AGNESE, Clark, A., Clarke, C., Compostella, G., Convery, M. E., Conway, J., Corbo, M., Cordelli, M., Cox, C. A., Cox, D. J., Crescioli, F., Cuevas, J., Culbertson, R., Dagenhart, D., D'Ascenzo, N., Datta, M., de Barbaro, P., Dell'Orso, Mauro, Demortier, L., Deninno, M., Devoto, F., D'Errico, M., Di Canto, A., Di Ruzza, B., Dittmann, J. R., D'Onofrio, M., Donati, Simone, Dong, P., Dorigo, M., Dorigo, T., Ebina, K., Elagin, A., Eppig, A., Erbacher, R., Errede, S., Ershaidat, N., Eusebi, R., Farrington, S., Feindt, M., Fernandez, J. P., Field, R., Flanagan, G., Forrest, R., Frank, M. J., Franklin, M., Freeman, J. C., Funakoshi, Y., Furic, I., Gallinaro, M., Garcia, J. E., Garfinkel, A. F., Garosi, P., Gerberich, H., Gerchtein, E., Giagu, S., Giakoumopoulou, V., Giannetti, P., Gibson, K., Ginsburg, C. M., Giokaris, N., Giromini, P., Giurgiu, G., Glagolev, V., Glenzinski, D., Gold, M., Goldin, D., Goldschmidt, N., Golossanov, A., Gomez, G., Gomez Ceballos, G., Goncharov, M., Gonzalez, O., Gorelov, I., Goshaw, A. T., Goulianos, K., Grinstein, S., Grosso Pilcher, C., Group, R. C., Guimaraes, da Costa J., Hahn, S. R., Halkiadakis, E., Hamaguchi, A., Han, J. Y., Happacher, F., Hara, K., Hare, D., Hare, M., Harr, R. F., Hatakeyama, K., Hays, C., Heck, M., Heinrich, J., Herndon, M., Hewamanage, S., Hocker, A., Hopkins, W., Horn, D., Hou, S., Hughes, R. E., Hurwitz, M., Husemann, U., Hussain, N., Hussein, M., Huston, J., Introzzi, G., Iori, M., Ivanov, A., James, E., Jang, D., Jayatilaka, B., Jeon, E. J., Jindariani, S., Jones, M., Joo, K. K., Jun, S. Y., Junk, T. R., Kamon, T., Karchin, P. E., Kasmi, A., Kato, Y., Ketchum, W., Keung, J., Khotilovich, V., Kilminster, B., Kim, D. H., Kim, H. S., Kim, J. E., Kim, M. J., Kim, S. B., Kim, S. H., Kim, Y. K., Kim, Y. J., Kimura, N., Kirby, M., Klimenko, S., Knoepfel, K., Kondo, K., Kong, D. J., Konigsberg, J., Kotwal, A. V., Kreps, M., Kroll, J., Krop, D., Kruse, M., Krutelyov, V., Kuhr, T., Kurata, M., Kwang, S., Laasanen, A. T., Lami, S., Lammel, S., Lancaster, M., Lander, R. L., Lannon, K., Lath, A., Latino, G., Lecompte, T., Lee, E., Lee, H. S., Lee, J. S., Lee, S. W., Leo, S., Leone, S., Lewis, J. D., Limosani, A., Lin, C. J., Lindgren, M., Lipeles, E., Lister, A., Litvintsev, D. O., Liu, C., Liu, H., Liu, Q., Liu, T., Lockwitz, S., Loginov, A., Lucchesi, D., Lueck, J., Lujan, P., Lukens, P., Lungu, G., Lys, J., Lysak, R., Madrak, R., Maeshima, K., Maestro, P., Malik, S., Manca, G., Manousakis Katsikakis, A., Margaroli, F., Marino, C., Martinez, M., Mastrandrea, P., Matera, K., Mattson, M. E., Mazzacane, A., Mazzanti, P., Mcfarland, K. S., Mcintyre, P., Mcnulty, R., Mehta, A., Mehtala, P., Mesropian, C., Miao, T., Mietlicki, D., Mitra, A., Miyake, H., Moed, S., Moggi, N., Mondragon, M. N., Moon, C. S., Moore, R., Morello, M. J., Morlock, J., Movilla, Fernandez P., Mukherjee, A., Muller, Th, Murat, P., Mussini, M., Nachtman, J., Nagai, Y., Naganoma, J., Nakano, I., Napier, A., Nett, J., Neu, C., Neubauer, M. S., Nielsen, J., Nodulman, L., Noh, S. Y., Norniella, O., Oakes, L., S. H., Oh, Y. D., Oh, Oksuzian, I., Okusawa, T., Orava, R., Ortolan, L., Pagan, Griso S., Pagliarone, C., Palencia, E., Papadimitriou, V., Paramonov, A. A., Patrick, J., Pauletta, G., Paulini, M., Paus, C., Pellett, D. E., Penzo, A., Phillips, T. J., Piacentino, G., Pianori, E., Pilot, J., Pitts, K., Plager, C., Pondrom, L., Poprocki, S., Potamianos, K., Prokoshin, F., Pranko, A., Ptohos, F., Punzi, Giovanni, Rahaman, A., Ramakrishnan, V., Ranjan, N., Redondo, I., Renton, P., Rescigno, M., Riddick, T., Rimondi, F., Ristori, L., Robson, A., Rodrigo, T., Rodriguez, T., Rogers, E., Rolli, S., Roser, R., Ruffini, F., Ruiz, A., Russ, J., Rusu, V., Safonov, A., Sakumoto, W. K., Sakurai, Y., Santi, L., Sato, K., Saveliev, V., Savoy Navarro, A., Schlabach, P., Schmidt, A., Schmidt, E. E., Schwarz, T., Scodellaro, L., Scribano, A., Scuri, F., Seidel, S., Seiya, Y., Semenov, A., Sforza, F., Shalhout, S. Z., Shears, T., Shepard, P. F., Shimojima, M., Shochet, M., Shreyber Tecker, I., Simonenko, A., Sinervo, P., Sliwa, K., Smith, J. R., Snider, F. D., Soha, A., Sorin, V., Song, H., Squillacioti, P., Stancari, M., St Denis, R., Stelzer, B., Stelzer Chilton, O., Stentz, D., Strologas, J., Strycker, G. L., Sudo, Y., Sukhanov, A., Suslov, I., Takemasa, K., Takeuchi, Y., Tang, J., Tecchio, M., Teng, P. K., Thom, J., Thome, J., Thompson, G. A., Thomson, E., Toback, D., Tokar, S., Tollefson, K., Tomura, T., Tonelli, D., Torre, S., Torretta, D., Totaro, P., Trovato, M., Ukegawa, F., Uozumi, S., Varganov, A., Vazquez, F., Velev, G., Vellidis, C., Vidal, M., Vila, I., Vilar, R., Vizan, J., Vogel, M., Volpi, G., Wagner, P., Wagner, R. L., Wakisaka, T., Wallny, R., Wang, S. M., Warburton, A., Waters, D., Iii, Wester W. C., Whiteson, D., Wicklund, A. B., Wicklund, E., Wilbur, S., Wick, F., Williams, H. H., Wilson, J. S., Wilson, P., Winer, B. L., Wittich, P., Wolbers, S., Wolfe, H., Wright, T., Wu, X., Wu, Z., Yamamoto, K., Yamato, D., Yang, T., Yang, U. K., Yang, Y. C., Yao, W. M., Yeh, G. P., Yi, K., Yoh, J., Yorita, K., Yoshida, T., G. B., Yu, Yu, I., S. S., Yu, Yun, J. C., Zanetti, A. C., Weinberger, M., Wenzel, H., Whitehouse, B., Yamaoka, J., Zanetti, A., Zeng, Y., Zucchelli, S. chelli S., Sannibale, V, Santamaria, L, Santiago Prieto, I, Santostasi, G, Saraf, S, Sassolas, B, Sathyaprakash, Bs, Sato, S, Satterthwaite, M, Saulson, Pr, Savage, R, Schilling, R, Schlamminger, S, Schnabel, R, Schofield, Rms, Schulz, B, Schutz, Bf, Schwinberg, P, Scott, J, Scott, Sm, Searle, Ac, Seifert, F, Sellers, D, Sengupta, As, Sentenac, D, Sergeev, A, Shaddock, Da, Shaltev, M, Shapiro, B, Shawhan, P, Weerathunga, Ts, Shoemaker, Dh, Sibley, A, Siemens, X, Sigg, D, Singer, A, Singer, L, Sintes, Am, Skelton, G, Slagmolen, Bjj, Slutsky, J, Smith, Jr, Smith, Mr, Smith, Nd, Smith, R, Somiya, K, Sorazu, B, Soto, J, Speirits, Fc, Sperandio, L, Stefszky, M, Stein, Aj, Steinlechner, J, Steinlechner, S, Steplewski, S, Stochino, A, Stone, R, Strain, Ka, Strigin, S, Stroeer, As, Sturani, R, Stuver, Al, Summerscales, Tz, Sung, M, Susmithan, S, Sutton, Pj, Swinkels, B, Szokoly, Gp, Tacca, M, Talukder, D, Tanner, Db, Tarabrin, Sp, Taylor, Jr, Taylor, R, Thomas, P, Thorne, Ka, Thorne, Ks, Thrane, E, Thuring, A, Titsler, C, Tokmakov, Kv, Toncelli, A, Tonelli, M, Torre, O, Torres, C, Torrie, Ci, Tournefier, E, Travasso, F, Traylor, G, Trias, M, Tseng, K, Turner, L, Ugolini, D, Urbanek, K, Vahlbruch, H, Vaishnav, B, Vajente, G, Vallisneri, M, van den Brand JFJ, Van Den Broeck, C, van der Putten, S, van der Sluys MV, van Veggel AA, Vass, S, Vasuth, M, Vaulin, R, Vavoulidis, M, Vecchio, A, Vedovato, G, Veitch, J, Veitch, Pj, Veltkamp, C, Verkindt, D, Vetrano, F, Vicere, A, Villar, Ae, Vinet, Jy, Vocca, H, Vorvick, C, Vyachanin, Sp, Waldman, Sj, Wallace, L, Wanner, A, Ward, Rl, Was, M, Wei, P, Weinert, M, Weinstein, Aj, Weiss, R, Wen, L, Wen, S, Wessels, P, West, M, Westphal, T, Wette, K, Whelan, Jt, Whitcomb, Se, White, D, Whiting, Bf, Wilkinson, C, Willems, Pa, Williams, Hr, Williams, L, Willke, B, Winkelmann, L, Winkler, W, Wipf, Cc, Wiseman, Ag, Woan, G, Wooley, R, Worden, J, Yablon, J, Yakushin, I, Yamamoto, H, Yamamoto, K, Yang, H, Yeaton Massey, D, Yoshida, S, Yu, P, Yvert, M, Zanolin, M, Zhang, L, Zhang, Z, Zhao, C, Zotov, N, Zucker, Me, Zweizig, J, Aptekar, Rl, Boynton, Wv, Briggs, Ms, Cline, Tl, Connaughton, V, Frederiks, Dd, Gehrels, N, Goldsten, Jo, Golovin, D, van der Horst AJ, Hurley, Kc, Kaneko, Y, von Kienlin, A, Kouveliotou, C, Krimm, Ha, Lin, L, Mitrofanov, I, Ohno, M, Pal'Shin, Vd, Rau, A, Sanin, A, Tashiro, Ms, Terada, Y, Yamaoka, K, Mastroberardino, A, Masubuchi, T, Mathes, M, Matsumoto, H, Matsunaga, H, Matsushita, T, Mattravers, C, Vlaugai, T., Aaltonen, B. A., Gonzalez, S., Amerio, D., Amidei, A., Anastassov, A., Annovi, J., Anto, G., Apollinari, J. A., Appel, T., Arisawa, A., Artikov, J., Asaadi, W., Ashmanska, B., Auerbach, A., Aurisano, F., Azfar, W., Badgett, T., Bae, A., Barbaro Galtieri, V. E., Barne, B. A., Barnett, P., Barria, P., Barto, M., Bauce, F., Bedeschi, S., Behari, G., Bellettini, J., Bellinger, D., Benjamin, A., Beretva, A., Bhatti, D., Bisello, I., Bizjak, K. R., Bland, B., Blumenfeld, A., Bocci, A., Bodek, D., Bortoletto, J., Boudreau, A., Boveia, L., Brigliadori, C., Bromberg, E., Brucken, J., Budagov, H. S., Budd, K., Burkett, G., Busetto, P., Bussey, A., Buzatu, A., Calamba, C., Calancha, S., Camarda, M., Campanelli, M., Campbell, F., Canelli, B., Carl, D., Carlsmith, R., Carosi, S., Carrillo, S., Carron, B., Casal, M., Casarsa, A., Castro, P., Catastini, D., Cauz, V., Cavaliere, M., Cavalli Sforza, A., Cerri, L., Cerrito, Y. C., Chen, M., Chertok, G., Chiarelli, G., Chlachidze, F., Chlebana, K., Cho, D., Chokheli, W. H., Chung, Y. S., Chung, M. A., Ciocci, A., Clark, C., Clarke, G., Compostella, M. E., Convery, J., Conway, M., Corbo, M., Cordelli, C. A., Cox, D. J., Cox, F., Crescioli, J., Cueva, R., Culbertson, D., Dagenhart, N., D'Ascenzo, M., Datta, P. d., Barbaro, M., Dell'Orso, L., Demortier, M., Deninno, F., Devoto, M., D'Errico, A. D., Canto, B. D., Ruzza, J. R., Dittmann, M., D'Onofrio, S., Donati, P., Dong, M., Dorigo, T., Dorigo, K., Ebina, A., Elagin, A., Eppig, R., Erbacher, S., Errede, N., Ershaidat, R., Eusebi, S., Farrington, M., Feindt, J. P., Fernandez, R., Field, G., Flanagan, R., Forrest, M. J., Frank, M., Franklin, J. C., Freeman, Y., Funakoshi, I., Furic, M., Gallinaro, J. E., Garcia, A. F., Garfinkel, P., Garosi, H., Gerberich, E., Gerchtein, S., Giagu, V., Giakoumopoulou, P., Giannetti, K., Gibson, C. M., Ginsburg, N., Giokari, P., Giromini, G., Giurgiu, V., Glagolev, D., Glenzinski, M., Gold, D., Goldin, N., Goldschmidt, A., Golossanov, G., Gomez, G., Gomez Ceballo, M., Goncharov, O., Gonzalez, I., Gorelov, A. T., Goshaw, K., Gouliano, S., Grinstein, C., Grosso Pilcher, R. C., Group, J. G., Da, S. R., Hahn, E., Halkiadaki, A., Hamaguchi, J. Y., Han, F., Happacher, K., Hara, D., Hare, M., Hare, R. F., Harr, K., Hatakeyama, C., Hay, M., Heck, J., Heinrich, M., Herndon, S., Hewamanage, A., Hocker, W., Hopkin, D., Horn, S., Hou, R. E., Hughe, M., Hurwitz, U., Husemann, N., Hussain, M., Hussein, J., Huston, G., Introzzi, M., Iori, A., Ivanov, E., Jame, D., Jang, B., Jayatilaka, E. J., Jeon, S., Jindariani, M., Jone, K. K., Joo, S. Y., Jun, T. R., Junk, T., Kamon, P. E., Karchin, A., Kasmi, Y., Kato, W., Ketchum, J., Keung, V., Khotilovich, B., Kilminster, D. H., Kim, H. S., Kim, J. E., Kim, M. J., Kim, S. B., Kim, S. H., Kim, Y. K., Kim, Y. J., Kim, N., Kimura, M., Kirby, S., Klimenko, K., Knoepfel, K., Kondo, D. J., Kong, J., Konigsberg, A. V., Kotwal, M., Krep, J., Kroll, D., Krop, M., Kruse, V., Krutelyov, T., Kuhr, M., Kurata, S., Kwang, A. T., Laasanen, S., Lami, S., Lammel, M., Lancaster, R. L., Lander, K., Lannon, A., Lath, G., Latino, T., Lecompte, E., Lee, H. S., Lee, J. S., Lee, S. W., Lee, S., Leo, S., Leone, J. D., Lewi, A., Limosani, C. J., Lin, M., Lindgren, E., Lipele, A., Lister, D. O., Litvintsev, C., Liu, H., Liu, Q., Liu, T., Liu, S., Lockwitz, A., Loginov, D., Lucchesi, J., Lueck, P., Lujan, P., Luken, G., Lungu, J., Ly, R., Lysak, R., Madrak, K., Maeshima, P., Maestro, S., Malik, G., Manca, A., Manousakis Katsikaki, F., Margaroli, C., Marino, M., Martinez, P., Mastrandrea, K., Matera, M. E., Mattson, A., Mazzacane, P., Mazzanti, K. S., Mcfarland, P., Mcintyre, R., Mcnulty, A., Mehta, P., Mehtala, C., Mesropian, T., Miao, D., Mietlicki, A., Mitra, H., Miyake, S., Moed, N., Moggi, M. N., Mondragon, C. S., Moon, R., Moore, Morello, MICHAEL JOSEPH, J., Morlock, P. M., Fernandez, A., Mukherjee, T., Muller, P., Murat, M., Mussini, J., Nachtman, Y., Nagai, J., Naganoma, I., Nakano, A., Napier, J., Nett, C., Neu, M. S., Neubauer, J., Nielsen, L., Nodulman, S. Y., Noh, O., Norniella, L., Oake, S. H., Oh, Y. D., Oh, I., Oksuzian, T., Okusawa, R., Orava, L., Ortolan, S. P., Griso, C., Pagliarone, E., Palencia, V., Papadimitriou, A. A., Paramonov, J., Patrick, G., Pauletta, M., Paulini, C., Pau, D. E., Pellett, A., Penzo, T. J., Phillip, G., Piacentino, E., Pianori, J., Pilot, K., Pitt, C., Plager, L., Pondrom, S., Poprocki, K., Potamiano, F., Prokoshin, A., Pranko, F., Ptoho, G., Punzi, A., Rahaman, V., Ramakrishnan, N., Ranjan, I., Redondo, P., Renton, M., Rescigno, T., Riddick, F., Rimondi, L., Ristori, A., Robson, T., Rodrigo, T., Rodriguez, E., Roger, S., Rolli, R., Roser, F., Ruffini, A., Ruiz, J., Ru, V., Rusu, A., Safonov, W. K., Sakumoto, Y., Sakurai, L., Santi, K., Sato, V., Saveliev, A., Savoy Navarro, P., Schlabach, A., Schmidt, E. E., Schmidt, T., Schwarz, L., Scodellaro, A., Scribano, F., Scuri, S., Seidel, Y., Seiya, A., Semenov, F., Sforza, S. Z., Shalhout, T., Shear, P. F., Shepard, M., Shimojima, M., Shochet, I., Shreyber Tecker, A., Simonenko, P., Sinervo, K., Sliwa, J. R., Smith, F. D., Snider, A., Soha, V., Sorin, H., Song, P., Squillacioti, M., Stancari, R. S., Deni, B., Stelzer, O., Stelzer Chilton, D., Stentz, J., Strologa, G. L., Strycker, Y., Sudo, A., Sukhanov, I., Suslov, K., Takemasa, Y., Takeuchi, J., Tang, M., Tecchio, P. K., Teng, J., Thom, J., Thome, G. A., Thompson, E., Thomson, D., Toback, S., Tokar, K., Tollefson, T., Tomura, D., Tonelli, S., Torre, D., Torretta, P., Totaro, M., Trovato, F., Ukegawa, S., Uozumi, A., Varganov, F., Vazquez, G., Velev, C., Vellidi, M., Vidal, I., Vila, R., Vilar, J., Vizan, M., Vogel, G., Volpi, P., Wagner, R. L., Wagner, T., Wakisaka, R., Wallny, S. M., Wang, A., Warburton, D., Water, W. C., Wester, D., Whiteson, A. B., Wicklund, E., Wicklund, S., Wilbur, F., Wick, H. H., William, J. S., Wilson, P., Wilson, B. L., Winer, P., Wittich, S., Wolber, H., Wolfe, T., Wright, X., Wu, Z., Wu, K., Yamamoto, D., Yamato, T., Yang, U. K., Yang, Y. C., Yang, W. M., Yao, G. P., Yeh, K., Yi, J., Yoh, K., Yorita, T., Yoshida, G. B., Yu, I., Yu, S. S., Yu, J. C., Yun, and A., Zanetti
Subjects: FERMILAB TEVATRON COLLIDER, High Energy Physics::Phenomenology, STANDARD MODEL, WEAK-BOSON SECTOR, High Energy Physics::Experiment
Abstract: In this Letter, we present a precise measurement of the total ZZ production cross section in p (p) over bar collisions at root s 1: 96 TeV, using data collected with the CDF II detector corresponding to an integrated luminosity of approximately 6 fb(-1). The result is obtained by combining separate measurements in the four-charged (lll'l') and two-charged-lepton and two-neutral-lepton (llvv) decay modes of the Z boson pair. The combined measured cross section for p (p) over bar -> ZZ is 1.64(-0.38)(+0.11) pb. This is the most precise measurement of the ZZ production cross section in 1.96 TeV p (p) over bar collisions to date.
Published: 2012

3. Fermi/GBM observations of the ultra-long GRB 091024

Author: Gruber, D, Krühler, T, Foley, S, NARDINI, MARCO, Burlon, D, Rau, A, Bissaldi, E, von Kienlin, A, McBreen, S, Greiner, J, Bhat, PN, Briggs, MS, Burgess, JM, Chaplin, VL, Connaughton, V, Diehl, R, Fishman, GJ, Gibby, MH, Giles, MM, Goldstein, A, Guiriec, S, van der Horst, AJ, Kippen, RM, Kouveliotou, C, Lin, L, Meegan, CA, Paciesas, WS, Preece, RD, Tierney, D, Wilson Hodge, C., Gruber, D, Krühler, T, Foley, S, Nardini, M, Burlon, D, Rau, A, Bissaldi, E, von Kienlin, A, Mcbreen, S, Greiner, J, Bhat, P, Briggs, M, Burgess, J, Chaplin, V, Connaughton, V, Diehl, R, Fishman, G, Gibby, M, Giles, M, Goldstein, A, Guiriec, S, van der Horst, A, Kippen, R, Kouveliotou, C, Lin, L, Meegan, C, Paciesas, W, Preece, R, Tierney, D, and Wilson Hodge, C
Subjects: FIS/05 - ASTRONOMIA E ASTROFISICA, amma-ray burst: general, gamma-ray burst: individual: GRB 091024
Abstract: Aims: In this paper we examine gamma-ray and optical data of GRB 091024, a gamma-ray burst (GRB) with an extremely long duration of T90 ≈ 1020 s, as observed with the Fermi Gamma-ray Burst Monitor (GBM). Methods. We present spectral analysis of all three distinct emission episodes using data from Fermi/GBM. Because of the long nature of this event, many ground-based optical telescopes slewed to its location within a few minutes and thus were able to observe the GRB during its active period. We compare the optical and gamma-ray light curves. Furthermore, we estimate a lower limit on the bulk Lorentz factor from the variability and spectrum of the GBM light curve and compare it with that obtained from the peak time of the forward shock of the optical afterglow. Results. From the spectral analysis we note that, despite its unusually long duration, this burst is similar to other long GRBs, i.e. there is spectral evolution (both the peak energy and the spectral index vary with time) and spectral lags are measured. We find that the optical light curve is highly anti-correlated to the prompt gamma-ray emission, with the optical emission reaching the maximum during an epoch of quiescence in the prompt emission. We interpret this behavior as the reverse shock (optical flash), expected in the internal-external shock model of GRB emission but observed only in a handful of GRBs so far. The lower limit on the initial Lorentz factor deduced from the variability time scale (Γmin = 195 -110+90) is consistent within the error to the one obtained using the peak time of the forward shock (Γ0 = 120) and is also consistent with Lorentz factors of other long GRBs. © ESO, 2011.
Published: 2011

4. The First Pulse of the Extremely Bright GRB 130427A: A Test Lab for Synchrotron Shocks

Author: Preece, R., Burgess, J. Michael, von, Kienlin A., Bhat, P. N., Briggs, M. S., Byrne, D., Chaplin, V., Cleveland, W., Collazzi, A. C., Connaughton, V., Diekmann, A., Fitzpatrick, G., Foley, S., Gibby, M., Giles, M., Goldstein, A., Greiner, J., Gruber, D., Jenke, P., Kippen, R. M., Kouveliotou, C., McBreen, S., Meegan, C., Paciesas, W. S., Pelassa, V., Tierney, D., van, der Horst A. J., Wilson-Hodge, C., Xiong, S., Younes, G., Yu, H.-F., Ackermann, M., Ajello, M., Axelsson, M., Baldini, L., Barbiellini, G., Baring, M. G., Bastieri, D., Bellazzini, R., Bissaldi, E., Bonamente, E., Bregeon, J., Brigida, M., Bruel, P., Buehler, R., Buson, S., Caliandro, G. A., Cameron, R. A., Caraveo, P. A., Cecchi, C., Charles, E., Chekhtman, A., Chiang, J., Chiaro, G., Ciprini, S., Claus, R., Cohen-Tanugi, J., Cominsky, L. R., Conrad, J., D'Ammando, F., de, Angelis A., de, Palma F., Dermer, C. D., Desiante, R., Digel, S. W., Di, Venere L., Drell, P. S., Drlica-Wagner, A., Favuzzi, C., Franckowiak, A., Fusco, P., Gargano, F., Gehrels, N., Germani, S., Giglietto, N., Giordano, F., Giroletti, M., Godfrey, G., Granot, J., Grenier, I. A., Guiriec, S., Hadasch, D., Harding, A. K., Iyyani, S., Jogler, T., Joannesson, G., Kawano, T., Knodlseder, J., Kocevski, D., Kuss, M., Lande, J., Larsson, J., Larsson, S., Latronico, L., Longo, F., Loparco, F., Lovellette, M. N., Lubrano, P., Mayer, M., Mazziotta, M. N., Michelson, P. F., Monzani, M. E., Moretti, E., Morselli, A., Murgia, S., Nemmen, R., Nuss, E., Nymark, T., Fukazawa, Yasushi, Hanabata, Yoshitaka, Hayashida, Masaaki, Mizuno, Tsunefumi, Ohno, Masanori, R., Preece, J. M., Burge, A. v., Kienlin, P. N., Bhat, M. S., Brigg, D., Byrne, V., Chaplin, W., Cleveland, A. C., Collazzi, V., Connaughton, A., Diekmann, G., Fitzpatrick, S., Foley, M., Gibby, M., Gile, A., Goldstein, J., Greiner, D., Gruber, P., Jenke, R. M., Kippen, C., Kouveliotou, S., Mcbreen, C., Meegan, W. S., Paciesa, V., Pelassa, D., Tierney, A. J., Van, C., Wilson Hodge, S., Xiong, G., Youne, H. . ., F., M., Ackermann, M., Ajello, M., Axelsson, L., Baldini, BARBIELLINI AMIDEI, Guido, M. G., Baring, D., Bastieri, R., Bellazzini, Bissaldi, Elisabetta, E., Bonamente, J., Bregeon, M., Brigida, P., Bruel, R., Buehler, S., Buson, G. A., Caliandro, R. A., Cameron, P. A., Caraveo, C., Cecchi, E., Charle, A., Chekhtman, J., Chiang, G., Chiaro, S., Ciprini, R., Clau, J., Cohen Tanugi, L. R., Cominsky, J., Conrad, F., D'Ammando, A. d., Angeli, F. d., Palma, C. D., Dermer, R., Desiante, S. W., Digel, L. D., Venere, P. S., Drell, A., Drlica Wagner, C., Favuzzi, A., Franckowiak, Y., Fukazawa, P., Fusco, F., Gargano, N., Gehrel, S., Germani, N., Giglietto, F., Giordano, M., Giroletti, G., Godfrey, J., Granot, I. A., Grenier, S., Guiriec, D., Hadasch, Y., Hanabata, A. K., Harding, M., Hayashida, S., Iyyani, T., Jogler, G., Joannesson, T., Kawano, J., Knoedlseder, D., Kocevski, M., Ku, J., Lande, J., Larsson, S., Larsson, L., Latronico, Longo, Francesco, F., Loparco, M. N., Lovellette, P., Lubrano, M., Mayer, M. N., Mazziotta, P. F., Michelson, T., Mizuno, M. E., Monzani, E., Moretti, A., Morselli, S., Murgia, R., Nemmen, E., Nu, T., Nymark, M., Ohno, T., Ohsugi, A., Okumura, N., Omodei, M., Orienti, D., Paneque, J. S., Perkin, M., Pesce Rollin, F., Piron, G., Pivato, T. A., Porter, J. L., Racusin, S., Raino, R., Rando, M., Razzano, S., Razzaque, A., Reimer, O., Reimer, S., Ritz, M., Roth, F., Ryde, A., Sartori, J. D., Scargle, A., Schulz, C., Sgro, E. J., Siskind, G., Spandre, P., Spinelli, D. J., Suson, H., Tajima, H., Takahashi, J. G., Thayer, J. B., Thayer, L., Tibaldo, M., Tinivella, D. F., Torre, G., Tosti, E., Troja, T. L., Usher, J., Vandenbroucke, V., Vasileiou, G., Vianello, V., Vitale, M., Werner, B. L., Winer, K. S., Wood, S., Zhu, Laboratoire Univers et Particules de Montpellier (LUPM), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Leprince-Ringuet (LLR), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Preece R, Burgess JM, von Kienlin A, Bhat PN, Briggs MS, Byrne D, Chaplin V, Cleveland W, Collazzi AC, Connaughton V, Diekmann A, Fitzpatrick G, Foley S, Gibby M, Giles M, Goldstein A, Greiner J, Gruber D, Jenke P, Kippen RM, Kouveliotou C, McBreen S, Meegan C, Paciesas WS, Pelassa V, Tierney D, van der Horst AJ, Wilson-Hodge C, Xiong S, Younes G, Yu HF, Ackermann M, Ajello M, Axelsson M, Baldini L, Barbiellini G, Baring MG, Bastieri D, Bellazzini R, Bissaldi E, Bonamente E, Bregeon J, Brigida M, Bruel P, Buehler R, Buson S, Caliandro GA, Cameron RA, Caraveo PA, Cecchi C, Charles E, Chekhtman A, Chiang J, Chiaro G, Ciprini S, Claus R, Cohen-Tanugi J, Cominsky LR, Conrad J, DAmmando F, de Angelis A, de Palma F, Dermer CD, Desiante R, Digel SW, Di Venere L, Drell PS, Drlica-Wagner A, Favuzzi C, Franckowiak A, Fukazawa Y, Fusco P, Gargano F, Gehrels N, Germani S, Giglietto N, Giordano F, Giroletti M, Godfrey G, Granot J, Grenier IA, Guiriec S, Hadasch D, Hanabata Y, Harding AK, Hayashida M, Iyyani S, Jogler T, Joannesson G, Kawano T, Knodlseder J, Kocevski D, Kuss M, Lande J, Larsson J, Larsson S, Latronico L, Longo F, Loparco F, Lovellette MN, Lubrano P, Mayer M, Mazziotta MN, Michelson PF, Mizuno T, Monzani ME, Moretti E, Morselli A, Murgia S, Nemmen R, Nuss E, Nymark T, Ohno M, Ohsugi T, Okumura A, Omodei N, Orienti M, Paneque D, Perkins JS, Pesce-Rollins M, Piron F, Pivato G, Porter TA, Racusin JL, Raino S, Rando R, Razzano M, Razzaque S, Reimer A, Reimer O, Ritz S, Roth M, Ryde F, Sartori A, Scargle JD, Schulz A, Sgro C, Siskind EJ, Spandre G, Spinelli P, Suson DJ, Tajima H, Takahashi H, Thayer JG, Thayer JB, Tibaldo L, Tinivella M, Torres DF, Tosti G, Troja E, Usher TL, Vandenbroucke J, Vasileiou V, Vianello G, Vitale V, Werner M, Winer BL, Wood KS, Zhu S, and High Energy Astrophys. & Astropart. Phys (API, FNWI)
Subjects: Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], 01 natural sciences, Spectral line, High Energy Gamma-ray Astronomy, law.invention, Luminosity, law, 0103 physical sciences, 010306 general physics, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Photosphere, Multidisciplinary, GRB 130427A, GRB 130427A, Synchrotron Shocks, Light curve, Synchrotron, Pulse (physics), ddc:500, Gamma-ray burst, Astrophysics - High Energy Astrophysical Phenomena
Abstract: Science 343(6166), 51 - 54(2014). doi:10.1126/science.1242302, Gamma-ray burst (GRB) 130427A is one of the most energetic GRBs ever observed. The initial pulse up to 2.5 seconds is possibly the brightest well-isolated pulse observed to date. A fine time resolution spectral analysis shows power-law decays of the peak energy from the onset of the pulse, consistent with models of internal synchrotron shock pulses. However, a strongly correlated power-law behavior is observed between the luminosity and the spectral peak energy that is inconsistent with curvature effects arising in the relativistic outflow. It is difficult for any of the existing models to account for all of the observed spectral and temporal behaviors simultaneously., Published by American Association for the Advancement of Science, Washington, DC [u.a.]
Published: 2014
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5. Fermi-LAT Observations of the Gamma-Ray Burst GRB 130427A

Author: P. A. Jenke, Brian L Winer, Soebur Razzaque, A. A. Moiseev, L. R. Cominsky, Igor V. Moskalenko, Melissa Gibby, Yoshiyuki Inoue, Justin D. Finke, Olaf Reimer, Katsuaki Asano, Robert D. Preece, F. Loparco, E. Moretti, André Schulz, Akira Okumura, George Younes, Matthew G. Baring, D. Byrne, William S. Paciesas, Chryssa Kouveliotou, C. Favuzzi, Judith Racusin, Melissa Pesce-Rollins, Charles A. Meegan, Robert R. Rando, T. Jogler, S. J. Fegan, Luca Baldini, J. G. Thayer, W. B. Focke, P. Spinelli, Sylvain Guiriec, Ryo Yamazaki, P. N. Bhat, Alex Drlica-Wagner, Shuze Zhu, A. von Kienlin, Vandiver Chaplin, Francesco Giordano, Anne M. Diekmann, M. E. Monzani, Jean Ballet, T. A. Porter, Hoi-Fung Yu, A. Franckowiak, J. Michael Burgess, G. Godfrey, W. N. Johnson, W. B. Atwood, Nicola Omodei, S. Rainò, Jeffrey D. Scargle, J. R. Cummings, J. S. Perkins, R. A. Cameron, Tsunefumi Mizuno, R. E. Hughes, Denis Bastieri, Misty Giles, Nicola Giglietto, Rodrigo Nemmen, Shaolin Xiong, Stefano Ciprini, D. Hadasch, S. Germani, K. S. Wood, T. Ohsugi, Eleonora Troja, Stefan Funk, Colleen A. Wilson-Hodge, P. Bruel, G. Chiaro, D. Horan, F. de Palma, A. C. Collazzi, Julie McEnery, V. Pelassa, A. J. van der Horst, Neil Gehrels, L. Di Venere, David Gruber, J. E. Grove, Yasushi Fukazawa, E. J. Siskind, Hiromitsu Takahashi, Valerie Connaughton, A. De Angelis, Adam Goldstein, M. Mayer, V. La Parola, D. J. Thompson, Carmelo Sgrò, G. Tosti, M. N. Lovellette, P. A. Caraveo, Persis S. Drell, M. Roth, Gudlaugur Johannesson, D. Kocevski, V. Vasileiou, Marco Ajello, J. B. Thayer, J. Lande, Jonathan Granot, S. Murgia, P. Fusco, E. Nuss, David Paneque, Sheila McBreen, M. Kuss, T. L. Usher, Francesco Longo, S. Buson, F. Piron, Giacomo Vianello, Masanori Ohno, Felix Ryde, W. H. Cleveland, Emanuele Bonamente, Charles D. Dermer, Magnus Axelsson, Alice K. Harding, I. A. Grenier, Markus Ackermann, Justin Vandenbroucke, Michael S. Briggs, Vahé Petrosian, Luca Latronico, Jürgen Knödlseder, Gloria Spandre, P. M. Saz Parkinson, Ronaldo Bellazzini, Johann Cohen-Tanugi, R. Desiante, T. Kawano, M. Tinivella, Elizabeth C. Ferrara, Guido Barbiellini, Stephen F. Foley, G. A. Caliandro, C. C. Cheung, M. Deklotz, Elisabetta Bissaldi, E. Hays, A. Morselli, F. Gargano, M. Orienti, V. Vitale, J. Bregeon, R. Claus, Alberto Sartori, Y. Hanabata, L. Tibaldo, G. Pivato, A. Reimer, M. Brigida, D. Tierney, M. N. Mazziotta, Eda Sonbas, Arne Rau, Giancarlo Cusumano, Claudia Cecchi, S. Larsson, Diego F. Torres, Gerard Fitzpatrick, S. Cutini, R. M. Kippen, James Chiang, M. Hayashida, Hiroyasu Tajima, Jan Conrad, R. Buehler, Peter F. Michelson, Marcello Giroletti, Eric Charles, Steven Ritz, A. Chekhtman, P. Lubrano, Keith Bechtol, M. Razzano, Filippo D'Ammando, Ackermann M, Ajello M, Asano K, Atwood WB, Axelsson M, Baldini L, Ballet J, Barbiellini G, Baring MG, Bastieri D, Bechtol K, Bellazzini R, Bissaldi E, Bonamente E, Bregeon J, Brigida M, Bruel P, Buehler R, Burgess JM, Buson S, Caliandro GA, Cameron RA, Caraveo PA, Cecchi C, Chaplin V, Charles E, Chekhtman A, Cheung CC, Chiang J, Chiaro G, Ciprini S, Claus R, Cleveland W, Cohen-Tanugi J, Collazzi A, Cominsky LR, Connaughton V, Conrad J, Cutini S, DAmmando F, de Angelis A, DeKlotz M, de Palma F, Dermer CD, Desiante R, Diekmann A, Di Venere L, Drell PS, Drlica-Wagner A, Favuzzi C, Fegan SJ, Ferrara EC, Finke J, Fitzpatrick G, Focke WB, Franckowiak A, Fukazawa Y, Funk S, Fusco P, Gargano F, Gehrels N, Germani S, Gibby M, Giglietto N, Giles M, Giordano F, Giroletti M, Godfrey G, Granot J, Grenier IA, Grove JE, Gruber D, Guiriec S, Hadasch D, Hanabata Y, Harding AK, Hayashida M, Hays E, Horan D, Hughes RE, Inoue Y, Jogler T, Johannesson G, Johnson WN, Kawano T, Knodlseder J, Kocevski D, Kuss M, Lande J, Larsson S, Latronico L, Longo F, Loparco F, Lovellette MN, Lubrano P, Mayer M, Mazziotta MN, McEnery JE, Michelson PF, Mizuno T, Moiseev AA, Monzani ME, Moretti E, Morselli A, Moskalenko IV, Murgia S, Nemmen R, Nuss E, Ohno M, Ohsugi T, Okumura A, Omodei N, Orienti M, Paneque D, Pelassa V, Perkins JS, Pesce-Rollins M, Petrosian V, Piron F, Pivato G, Porter TA, Racusin JL, Raino S, Rando R, Razzano M, Razzaque S, Reimer A, Reimer O, Ritz S, Roth M, Ryde F, Sartori A, Parkinson PMS, Scargle JD, Schulz A, Sgro C, Siskind EJ, Sonbas E, Spandre G, Spinelli P, Tajima H, Takahashi H, Thayer JG, Thayer JB, Thompson DJ, Tibaldo L, Tinivella M, Torres DF, Tosti G, Troja E, Usher TL, Vandenbroucke J, Vasileiou V, Vianello G, Vitale V, Winer BL, Wood KS, Yamazaki R, Younes G, Yu HF, Zhu SJ, Bhat PN, Briggs MS, Byrne D, Foley S, Goldstein A, Jenke P, Kippen RM, Kouveliotou C, McBreen S, Meegan C, Paciesas WS, Preece R, Rau A, Tierney D, van der Horst AJ, von Kienlin A, Wilson-Hodge C, Xiong S, Cusumano G, La Parola V, Cummings JR, M., Ackermann, M., Ajello, K., Asano, W. B., Atwood, M., Axelsson, L., Baldini, J., Ballet, BARBIELLINI AMIDEI, Guido, M. G., Baring, D., Bastieri, K., Bechtol, R., Bellazzini, Bissaldi, Elisabetta, E., Bonamente, J., Bregeon, M., Brigida, P., Bruel, R., Buehler, J. M., Burge, S., Buson, G. A., Caliandro, R. A., Cameron, P. A., Caraveo, C., Cecchi, V., Chaplin, E., Charle, A., Chekhtman, C. C., Cheung, J., Chiang, G., Chiaro, S., Ciprini, R., Clau, W., Cleveland, J., Cohen Tanugi, A., Collazzi, L. R., Cominsky, V., Connaughton, J., Conrad, S., Cutini, F., D'Ammando, A. d., Angeli, M., Deklotz, F. d., Palma, C. D., Dermer, R., Desiante, A., Diekmann, L. D., Venere, P. S., Drell, A., Drlica Wagner, C., Favuzzi, S. J., Fegan, E. C., Ferrara, J., Finke, G., Fitzpatrick, W. B., Focke, A., Franckowiak, Y., Fukazawa, S., Funk, P., Fusco, F., Gargano, N., Gehrel, S., Germani, M., Gibby, N., Giglietto, M., Gile, F., Giordano, M., Giroletti, G., Godfrey, J., Granot, I. A., Grenier, J. E., Grove, D., Gruber, S., Guiriec, D., Hadasch, Y., Hanabata, A. K., Harding, M., Hayashida, E., Hay, D., Horan, R. E., Hughe, Y., Inoue, T., Jogler, G., Johannesson, W. N., Johnson, T., Kawano, J., Knoedlseder, D., Kocevski, M., Ku, J., Lande, S., Larsson, L., Latronico, Longo, Francesco, F., Loparco, M. N., Lovellette, P., Lubrano, M., Mayer, M. N., Mazziotta, J. E., Mcenery, P. F., Michelson, T., Mizuno, A. A., Moiseev, M. E., Monzani, E., Moretti, A., Morselli, I. V., Moskalenko, S., Murgia, R., Nemmen, E., Nu, M., Ohno, T., Ohsugi, A., Okumura, N., Omodei, M., Orienti, D., Paneque, V., Pelassa, J. S., Perkin, M., Pesce Rollin, V., Petrosian, F., Piron, G., Pivato, T. A., Porter, J. L., Racusin, S., Raino, R., Rando, M., Razzano, S., Razzaque, A., Reimer, O., Reimer, S., Ritz, M., Roth, F., Ryde, A., Sartori, P. M., Saz, J. D., Scargle, A., Schulz, C., Sgro, E. J., Siskind, E., Sonba, G., Spandre, P., Spinelli, H., Tajima, H., Takahashi, J. G., Thayer, J. B., Thayer, D. J., Thompson, L., Tibaldo, M., Tinivella, D. F., Torre, G., Tosti, E., Troja, T. L., Usher, J., Vandenbroucke, V., Vasileiou, G., Vianello, V., Vitale, B. L., Winer, K. S., Wood, R., Yamazaki, G., Youne, H. . ., F., S. J., Zhu, P. N., Bhat, M. S., Brigg, D., Byrne, S., Foley, A., Goldstein, P., Jenke, R. M., Kippen, C., Kouveliotou, S., Mcbreen, C., Meegan, W. S., Paciesa, R., Preece, A., Rau, D., Tierney, A. J., Van, A. v., Kienlin, C., Wilson Hodge, S., Xiong, G., Cusumano, V. L., Parola, J. R., Cummings, and High Energy Astrophys. & Astropart. Phys (API, FNWI)
Subjects: Astrophysics::High Energy Astrophysical Phenomena, SPECTRAL COMPONENT, Synchrotron radiation, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, LARGE-AREA TELESCOPE, HIGH-ENERGY EMISSION, AFTERGLOWS, PROMPT, law.invention, Telescope, Spitzer Space Telescope, law, Astrophysics::Galaxy Astrophysics, Physics, Multidisciplinary, Gamma ray, GRB 130427A, Astronomy, Afterglow, GRB, Fermi-LAT, ddc:500, Astrophysics - High Energy Astrophysical Phenomena, Gamma-ray burst, Fermi Gamma-ray Space Telescope
Abstract: The observations of the exceptionally bright gamma-ray burst (GRB) 130427A by the Large Area Telescope aboard the Fermi Gamma-ray Space Telescope provide constraints on the nature of such unique astrophysical sources. GRB 130427A had the largest fluence, highest-energy photon (95 GeV), longest $\gamma$-ray duration (20 hours), and one of the largest isotropic energy releases ever observed from a GRB. Temporal and spectral analyses of GRB 130427A challenge the widely accepted model that the non-thermal high-energy emission in the afterglow phase of GRBs is synchrotron emission radiated by electrons accelerated at an external shock., Comment: 30 pages, 6 figures. Accepted for publication in Science. Corresponding authors: S. Zhu (sjzhu@umd.edu); J. Chiang (jchiang@slac.stanford.edu); C. Dermer (charles.dermer@nrl.navy.mil); N. Omodei (nicola.omodei@stanford.edu); G. Vianello (giacomov@slac.stanford.edu); S. Xiong (Shaolin.Xiong@uah.edu)
Published: 2014
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6. MULTIWAVELENGTH OBSERVATIONS OF GRB 110731A: GeV EMISSION FROM ONSET TO AFTERGLOW

Author: T. Ohsugi, Akihiko Fukui, W. S. Paciesas, P. Fusco, Eleonora Troja, G. Godfrey, Miranda Jackson, Dario Gasparrini, Marco Ajello, J. B. Thayer, S. Rainò, Tsunefumi Mizuno, S. Murgia, J. E. Grove, Yasushi Fukazawa, Luca Latronico, I. A. Grenier, O. Littlejohns, Matthew G. Baring, Daniel Sánchez, Peter Mészáros, L. Tibaldo, Jonathan Granot, A. De Angelis, R. M. Kippen, Judith Racusin, V. Vasileiou, Elisabetta Bissaldi, R. Filgas, S. Buson, M. Tinivella, F. de Palma, G. Tosti, F. Piron, Stefano Ciprini, Sheila McBreen, P. Bruel, Jan Conrad, C. Monte, T. Jogler, Nicola Omodei, Masanori Ohno, A. P. Waite, Hiromitsu Takahashi, Melissa Pesce-Rollins, Valerie Connaughton, Giacomo Vianello, T. L. Usher, J. G. Thayer, Takashi Sako, Luca Baldini, Eda Sonbas, Alex Drlica-Wagner, E. Orlando, A. Reimer, K. S. Wood, Jürgen Knödlseder, M. Roth, J. Mehault, D. Kocevski, S. McGlynn, A. S. Johnson, S. Cutini, V. Pelassa, E. J. Siskind, A. von Kienlin, David Gruber, Johan Bregeon, T. Glanzman, J. M. Burgess, P. N. Bhat, M. Naumann-Godo, Ronaldo Bellazzini, R. Buehler, C. Romoli, E. Hays, J. S. Perkins, S. J. Fegan, Igor V. Moskalenko, Julie McEnery, Brian L Winer, Nicola Giglietto, Katsuaki Asano, M. E. Monzani, Peter F. Michelson, Marcello Giroletti, Markus Ackermann, T. Nymark, Y. Hanabata, G. Pivato, Olaf Reimer, M. N. Lovellette, M. Hayashida, Robert D. Preece, P. A. Caraveo, A. Franckowiak, R. E. Hughes, Persis S. Drell, Charles D. Dermer, E. Do Couto E Silva, Eugenio Bottacini, Denis Bastieri, E. Moretti, F. D'Ammando, F. Loparco, C. Favuzzi, T. Krühler, W. Mitthumsiri, A. J. van der Horst, R. Claus, J. Lande, Sylvain Guiriec, F. Gargano, Johann Cohen-Tanugi, Zhenwei Yang, Daniela Hadasch, Michael S. Briggs, Carmelo Sgrò, Riccardo Rando, Francesco Longo, E. Nuss, David Paneque, M. Kuss, T. N. Ukwatta, Jay P. Norris, G. A. Caliandro, R. C. G. Chaves, James Chiang, Roger Blandford, M. Razzano, Soebur Razzaque, S. R. Oates, N. Gehrels, Suzanne Foley, Arne Rau, Gudlaugur Johannesson, Claudia Cecchi, Felix Ryde, M. Stamatikos, Justin Vandenbroucke, Guido Barbiellini, M. Orienti, A. Morselli, V. Vitale, A. Chekhtman, M. N. Mazziotta, M. Brigida, W. B. Focke, P. Spinelli, Chryssa Kouveliotou, S. Larsson, Francesco Giordano, R. A. Cameron, Jochen Greiner, S. Klose, Emanuele Bonamente, A. W. Borgland, Takaaki Tanaka, Paul J. Tristram, P. Lubrano, D. A. Kann, Eric Charles, Ackermann M, Ajello M, Asano K, Baldini L, Barbiellini G, Baring MG, Bastieri D, Bellazzini R, Blandford RD, Bonamente E, Borgland AW, Bottacini E, Bregeon J, Brigida M, Bruel P, Buehler R, Buson S, Caliandro GA, Cameron RA, Caraveo PA, Cecchi C, Charles E, Chaves RCG, Chekhtman A, Chiang J, Ciprini S, Claus R, Cohen-Tanugi J, Conrad J, Cutini S, DAmmando F, de Angelis A, de Palma F, Dermer CD, Silva EDE, Drell PS, Drlica-Wagner A, Favuzzi C, Fegan SJ, Focke WB, Franckowiak A, Fukazawa Y, Fusco P, Gargano F, Gasparrini D, Gehrels N, Giglietto N, Giordano F, Giroletti M, Glanzman T, Godfrey G, Granot J, Greiner J, Grenier IA, Grove JE, Guiriec S, Hadasch D, Hanabata Y, Hayashida M, Hays E, Hughes RE, Jackson MS, Jogler T, Johannesson G, Johnson AS, Knodlseder J, Kocevski D, Kuss M, Lande J, Larsson S, Latronico L, Longo F, Loparco F, Lovellette MN, Lubrano P, Mazziotta MN, McEnery JE, Mehault J, Meszaros P, Michelson PF, Mitthumsiri W, Mizuno T, Monte C, Monzani ME, Moretti E, Morselli A, Moskalenko IV, Murgia S, Naumann-Godo M, Norris JP, Nuss E, Nymark T, Ohno M, Ohsugi T, Omodei N, Orienti M, Orlando E, Paneque D, Perkins JS, Pesce-Rollins M, Piron F, Pivato G, Racusin JL, Raino S, Rando R, Razzano M, Razzaque S, Reimer A, Reimer O, Romoli C, Roth M, Ryde F, Sanchez DA, Sgro C, Siskind EJ, Sonbas E, Spinelli P, Stamatikos M, Takahashi H, Tanaka T, Thayer JG, Thayer JB, Tibaldo L, Tinivella M, Tosti G, Troja E, Usher TL, Vandenbroucke J, Vasileiou V, Vianello G, Vitale V, Waite AP, Winer BL, Wood KS, Yang Z, Gruber D, Bhat PN, Bissaldi E, Briggs MS, Burgess JM, Connaughton V, Foley S, Kippen RM, Kouveliotou C, McBreen S, McGlynn S, Paciesas WS, Pelassa V, Preece R, Rau A, van der Horst AJ, von Kienlin A, Kann DA, Filgas R, Klose S, Kruhler T, Fukui A, Sako T, Tristram PJ, Oates SR, Ukwatta TN, Littlejohns O, High Energy Astrophys. & Astropart. Phys (API, FNWI), Ackermann, M., Ajello, M., Asano, K., Baldini, L., BARBIELLINI AMIDEI, Guido, Baring, M. G., Bastieri, D., Bellazzini, R., Blandford, R. D., Bonamente, E., Borgland, A. W., Bottacini, E., Bregeon, J., Brigida, M., Bruel, P., Buehler, R., Buson, S., Caliandro, G. A., Cameron, R. A., Caraveo, P. A., Cecchi, C., Charles, E., Chaves, R. C. G., Chekhtman, A., Chiang, J., Ciprini, S., Claus, R., Cohen Tanugi, J., Conrad, J., Cutini, S., D'Ammando, F., de Angelis, A., de Palma, F., Dermer, C. D., Silva, E. do Couto e., Drell, P. S., Drlica Wagner, A., Favuzzi, C., Fegan, S. J., Focke, W. B., Franckowiak, A., Fukazawa, Y., Fusco, P., Gargano, F., Gasparrini, D., Gehrels, N., Giglietto, N., Giordano, F., Giroletti, M., Glanzman, T., Godfrey, G., Granot, J., Greiner, J., Grenier, I. A., Grove, J. E., Guiriec, S., Hadasch, D., Hanabata, Y., Hayashida, M., Hays, E., Hughes, R. E., Jackson, M. S., Jogler, T., Jóhannesson, G., Johnson, A. S., Knödlseder, J., Kocevski, D., Kuss, M., Lande, J., Larsson, S., Latronico, L., Longo, Francesco, Loparco, F., Lovellette, M. N., Lubrano, P., Mazziotta, M. N., Mcenery, J. E., Mehault, J., Mészáros, P., Michelson, P. F., Mitthumsiri, W., Mizuno, T., Monte, C., Monzani, M. E., Moretti, E., Morselli, A., Moskalenko, I. V., Murgia, S., Naumann Godo, M., Norris, J. P., Nuss, E., Nymark, T., Ohno, M., Ohsugi, T., Omodei, N., Orienti, M., Orlando, E., Paneque, D., Perkins, J. S., Pesce Rollins, M., Piron, F., Pivato, G., Racusin, J. L., Rainò, S., Rando, R., Razzano, M., Razzaque, S., Reimer, A., Reimer, O., Romoli, C., Roth, M., Ryde, F., Sanchez, D. A., Sgrò, C., Siskind, E. J., Sonbas, E., Spinelli, P., Stamatikos, M., Takahashi, H., Tanaka, T., Thayer, J. G., Thayer, J. B., Tibaldo, L., Tinivella, M., Tosti, G., Troja, E., Usher, T. L., Vandenbroucke, J., Vasileiou, V., Vianello, G., Vitale, V., Waite, A. P., Winer, B. L., Wood, K. S., Yang, Z., Gruber, D., Bhat, P. N., Bissaldi, Elisabetta, Briggs, M. S., Burgess, J. M., Connaughton, V., Foley, S., Kippen, R. M., Kouveliotou, C., Mcbreen, S., Mcglynn, S., Paciesas, W. S., Pelassa, V., Preece, R., Rau, A., van der Horst, A. J., von Kienlin, A., Kann, D. A., Filgas, R., Klose, S., Krühler, T., Fukui, A., Sako, T., Tristram, P. J., Oates, S. R., Ukwatta, T. N., and Littlejohns, O.
Subjects: Physics, Opacity, Astrophysics::High Energy Astrophysical Phenomena, Astronomy, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, individual (GRB110731A) [gamma-ray burst], Light curve, gamma-ray burst: individual (GRB110731A), Afterglow, law.invention, Telescope, Lorentz factor, symbols.namesake, Space and Planetary Science, law, Observatory, symbols, ddc:520, Astrophysics - High Energy Astrophysical Phenomena, Gamma-ray burst, Astrophysics::Galaxy Astrophysics, Fermi Gamma-ray Space Telescope
Abstract: The astrophysical journal 763(2), 71 (2013). doi:10.1088/0004-637X/763/2/71, We report on the multiwavelength observations of the bright, long gamma-ray burst GRB 110731A, by the Fermi and Swift observatories, and by the MOA and GROND optical telescopes. The analysis of the prompt phase reveals that GRB 110731A shares many features with bright Large Area Telescope bursts observed by Fermi during the first three years on-orbit: a light curve with short time variability across the whole energy range during the prompt phase, delayed onset of the emission above 100 MeV, extra power-law component and temporally extended high-energy emission. In addition, this is the first GRB for which simultaneous GeV, X-ray, and optical data are available over multiple epochs beginning just after the trigger time and extending for more than 800 s, allowing temporal and spectral analysis in different epochs that favor emission from the forward shock in a wind-type medium. The observed temporally extended GeV emission is most likely part of the high-energy end of the afterglow emission. Both the single-zone pair transparency constraint for the prompt signal and the spectral and temporal analysis of the forward-shock afterglow emission independently lead to an estimate of the bulk Lorentz factor of the jet Γ ~ 500-550., Published by Univ.11032, Chicago, Ill. [u.a.]
Published: 2013
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7. Constraining the High-energy Emission from Gamma-Ray Bursts with Fermi

Author: The, Fermi Large Area Telescope Team, 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., 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., Harding, A. K., Hays, E., Horan, D., Johannesson, G., Knodlseder, 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, E., Morselli, A., Moskalenko, I. V., Murgia, S., Naumann-Godo, M., Norris, J. P., Nuss, E., Nymark, T., 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, F., Sgro, C., Siskind, E. J., Sonbas, E., Spandre, G., Spinelli, P., Stamatikos, M., Stawarz, Lukasz, Fukazawa, Yasushi, Hanabata, Yoshitaka, Kataoka, Jun, Ohsugi, Takashi, Okumura, Akira, High Energy Astrophys. & Astropart. Phys (API, FNWI), Ackermann M, Ajello M, Baldini L, Barbiellini G, Baring MG, Bechtol K, Bellazzini R, Blandford RD, Bloom ED, Bonamente E, Borgland AW, Bottacini E, Bouvier A, Brigida M, Buehler R, Buson S, Caliandro GA, Cameron RA, Cecchi C, Charles E, Chekhtman A, Chiang J, Ciprini S, Claus R, Cohen-Tanugi J, Cutini S, DAmmando F, de Palma F, Dermer CD, Silva EDE, Drell PS, 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 IA, Grove JE, Hadasch D, Hanabata Y, Harding AK, Hays E, Horan D, Johannesson G, Kataoka J, Knodlseder J, Kocevski D, Kuss M, Lande J, Longo F, Loparco F, Lovellette MN, Lubrano P, Mazziotta MN, McEnery J, McGlynn S, Michelson PF, Mitthumsiri W, Monzani ME, Moretti E, Morselli A, Moskalenko IV, Murgia S, Naumann-Godo M, Norris JP, Nuss E, Nymark T, Ohsugi T, Okumura A, Omodei N, Orlando E, Panetta JH, Parent D, Pelassa V, Pesce-Rollins M, Piron F, Pivato G, Racusin JL, Raino S, Rando R, Razzaque S, Reimer A, Reimer O, Ritz S, Ryde F, Sgro C, Siskind EJ, Sonbas E, Spandre G, Spinelli P, Stamatikos M, Stawarz E, Suson DJ, Takahashi H, Tanaka T, Thayer JG, Thayer JB, Tibaldo L, Tinivella M, Tosti G, Uehara T, Vandenbroucke J, Vasileiou V, Vianello G, Vitale V, Waite AP, Connaughton V, Briggs MS, Guirec S, Goldstein A, Burgess JM, Bhat PN, Bissaldi E, Camero-Arranz A, Fishman J, Fitzpatrick G, Foley S, Gruber D, Jenke P, Kippen RM, Kouveliotou C, McBreen S, Meegan C, Paciesas WS, Preece R, Rau A, Tierney D, van der Horst AJ, von Kienlin A, Wilson-Hodge C, Xiong S, Ackermann, M., Ajello, M., Baldini, L., BARBIELLINI AMIDEI, Guido, 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., Palma, F., Dermer, C. D., E. d. C., 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., Kn\odlseder, J., Kocevski, D., Kuss, M., Lande, J., Longo, Francesco, Loparco, F., Lovellette, M. N., Lubrano, P., Mazziotta, M. N., Mcenery, J., Mcglynn, S., Michelson, P. F., Mitthumsiri, W., Monzani, M. E., Moretti, E., Morselli, A., Moskalenko, I. V., Murgia, S., Naumann Godo, M., Norris, J. P., Nuss, E., Nymark, T., 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., Rain\`o, S., Rando, R., Razzaque, S., Reimer, A., Reimer, O., Ritz, S., Ryde, F., Sgr\`o, C., Siskind, E. J., Sonbas, E., Spandre, G., Spinelli, P., Stamatikos, M., Stawarz, ., 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., Gamma ray, . F., Connaughton, V., Briggs, M. S., Guirec, S., Goldstein, A., Burgess, J. M., Bhat, P. N., Bissaldi, Elisabetta, 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, A. J., Kienlin, A., Wilson Hodge, C., and Xiong, S.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, gamma-ray burst: general, Astrophysics, general [gamma-ray burst], Astronomical spectroscopy, Spectral line, symbols.namesake, Gamma rays: general, Physics, Astronomy, Astronomy and Astrophysics, Spectral bands, Gamma-ray astronomy, gamma rays: general, Spectral component, Space and Planetary Science, Lorentz factor, gamma-ray burst: general – gamma rays: general, symbols, ddc:520, Astrophysics - High Energy Astrophysical Phenomena, Gamma-ray burst, general [gamma rays], Astrophysics - Cosmology and Nongalactic Astrophysics, Fermi Gamma-ray Space Telescope
Abstract: 著者人数: 139名, Accepted: 2012-05-22, 資料番号: SA1004166000
Published: 2012
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8. A structured jet explains the extreme GRB 221009A.

Author: O'Connor B, Troja E, Ryan G, Beniamini P, van Eerten H, Granot J, Dichiara S, Ricci R, Lipunov V, Gillanders JH, Gill R, Moss M, Anand S, Andreoni I, Becerra RL, Buckley DAH, Butler NR, Cenko SB, Chasovnikov A, Durbak J, Francile C, Hammerstein E, van der Horst AJ, Kasliwal MM, Kouveliotou C, Kutyrev AS, Lee WH, Srinivasaragavan GP, Topolev V, Watson AM, Yang Y, and Zhirkov K
Abstract: Long-duration gamma-ray bursts (GRBs) are powerful cosmic explosions, signaling the death of massive stars. Among them, GRB 221009A is by far the brightest burst ever observed. Because of its enormous energy ( E iso ≈ 10 55 erg) and proximity ( z ≈ 0.15), GRB 221009A is an exceptionally rare event that pushes the limits of our theories. We present multiwavelength observations covering the first 3 months of its afterglow evolution. The x-ray brightness decays as a power law with slope ≈ t -1.66 , which is not consistent with standard predictions for jetted emission. We attribute this behavior to a shallow energy profile of the relativistic jet. A similar trend is observed in other energetic GRBs, suggesting that the most extreme explosions may be powered by structured jets launched by a common central engine.
Published: 2023
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9. Rapid spectral variability of a giant flare from a magnetar in NGC 253.

Author: Roberts OJ, Veres P, Baring MG, Briggs MS, Kouveliotou C, Bissaldi E, Younes G, Chastain SI, DeLaunay JJ, Huppenkothen D, Tohuvavohu A, Bhat PN, Göğüş E, van der Horst AJ, Kennea JA, Kocevski D, Linford JD, Guiriec S, Hamburg R, Wilson-Hodge CA, and Burns E
Abstract: Magnetars are neutron stars with extremely strong magnetic fields (10 13 to 10 15 gauss) 1,2 , which episodically emit X-ray bursts approximately 100 milliseconds long and with energies of 10 40 to 10 41 erg. Occasionally, they also produce extremely bright and energetic giant flares, which begin with a short (roughly 0.2 seconds), intense flash, followed by fainter, longer-lasting emission that is modulated by the spin period of the magnetar 3,4 (typically 2 to 12 seconds). Over the past 40 years, only three such flares have been observed in our local group of galaxies 3-6 , and in all cases the extreme intensity of the flares caused the detectors to saturate. It has been proposed that extragalactic giant flares are probably a subset 7-11 of short γ-ray bursts, given that the sensitivity of current instrumentation prevents us from detecting the pulsating tail, whereas the initial bright flash is readily observable out to distances of around 10 to 20 million parsecs. Here we report X-ray and γ-ray observations of the γ-ray burst GRB 200415A, which has a rapid onset, very fast time variability, flat spectra and substantial sub-millisecond spectral evolution. These attributes match well with those expected for a giant flare from an extragalactic magnetar 12 , given that GRB 200415A is directionally associated 13 with the galaxy NGC 253 (roughly 3.5 million parsecs away). The detection of three-megaelectronvolt photons provides evidence for the relativistic motion of the emitting plasma. Radiation from such rapidly moving gas around a rotating magnetar may have generated the rapid spectral evolution that we observe.
Published: 2021
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10. Observation of inverse Compton emission from a long γ-ray burst.

Author: Veres P, Bhat PN, Briggs MS, Cleveland WH, Hamburg R, Hui CM, Mailyan B, Preece RD, Roberts OJ, von Kienlin A, Wilson-Hodge CA, Kocevski D, Arimoto M, Tak D, Asano K, Axelsson M, Barbiellini G, Bissaldi E, Dirirsa FF, Gill R, Granot J, McEnery J, Omodei N, Razzaque S, Piron F, Racusin JL, Thompson DJ, Campana S, Bernardini MG, Kuin NPM, Siegel MH, Cenko SB, O'Brien P, Capalbi M, Daì A, De Pasquale M, Gropp J, Klingler N, Osborne JP, Perri M, Starling RLC, Tagliaferri G, Tohuvavohu A, Ursi A, Tavani M, Cardillo M, Casentini C, Piano G, Evangelista Y, Verrecchia F, Pittori C, Lucarelli F, Bulgarelli A, Parmiggiani N, Anderson GE, Anderson JP, Bernardi G, Bolmer J, Caballero-García MD, Carrasco IM, Castellón A, Segura NC, Castro-Tirado AJ, Cherukuri SV, Cockeram AM, D'Avanzo P, Di Dato A, Diretse R, Fender RP, Fernández-García E, Fynbo JPU, Fruchter AS, Greiner J, Gromadzki M, Heintz KE, Heywood I, van der Horst AJ, Hu YD, Inserra C, Izzo L, Jaiswal V, Jakobsson P, Japelj J, Kankare E, Kann DA, Kouveliotou C, Klose S, Levan AJ, Li XY, Lotti S, Maguire K, Malesani DB, Manulis I, Marongiu M, Martin S, Melandri A, Michałowski MJ, Miller-Jones JCA, Misra K, Moin A, Mooley KP, Nasri S, Nicholl M, Noschese A, Novara G, Pandey SB, Peretti E, Del Pulgar CJP, Pérez-Torres MA, Perley DA, Piro L, Ragosta F, Resmi L, Ricci R, Rossi A, Sánchez-Ramírez R, Selsing J, Schulze S, Smartt SJ, Smith IA, Sokolov VV, Stevens J, Tanvir NR, Thöne CC, Tiengo A, Tremou E, Troja E, de Ugarte Postigo A, Valeev AF, Vergani SD, Wieringa M, Woudt PA, Xu D, Yaron O, and Young DR
Abstract: Long-duration γ-ray bursts (GRBs) originate from ultra-relativistic jets launched from the collapsing cores of dying massive stars. They are characterized by an initial phase of bright and highly variable radiation in the kiloelectronvolt-to-megaelectronvolt band, which is probably produced within the jet and lasts from milliseconds to minutes, known as the prompt emission 1,2 . Subsequently, the interaction of the jet with the surrounding medium generates shock waves that are responsible for the afterglow emission, which lasts from days to months and occurs over a broad energy range from the radio to the gigaelectronvolt bands 1-6 . The afterglow emission is generally well explained as synchrotron radiation emitted by electrons accelerated by the external shock 7-9 . Recently, intense long-lasting emission between 0.2 and 1 teraelectronvolts was observed from GRB 190114C 10,11 . Here we report multi-frequency observations of GRB 190114C, and study the evolution in time of the GRB emission across 17 orders of magnitude in energy, from 5 × 10 -6 to 10 12 electronvolts. We find that the broadband spectral energy distribution is double-peaked, with the teraelectronvolt emission constituting a distinct spectral component with power comparable to the synchrotron component. This component is associated with the afterglow and is satisfactorily explained by inverse Compton up-scattering of synchrotron photons by high-energy electrons. We find that the conditions required to account for the observed teraelectronvolt component are typical for GRBs, supporting the possibility that inverse Compton emission is commonly produced in GRBs.
Published: 2019
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11. Needle-like structures discovered on positively charged lightning branches.

Author: Hare BM, Scholten O, Dwyer J, Trinh TNG, Buitink S, Ter Veen S, Bonardi A, Corstanje A, Falcke H, Hörandel JR, Huege T, Mitra P, Mulrey K, Nelles A, Rachen JP, Rossetto L, Schellart P, Winchen T, Anderson J, Avruch IM, Bentum MJ, Blaauw R, Broderick JW, Brouw WN, Brüggen M, Butcher HR, Ciardi B, Fallows RA, de Geus E, Duscha S, Eislöffel J, Garrett MA, Grießmeier JM, Gunst AW, van Haarlem MP, Hessels JWT, Hoeft M, van der Horst AJ, Iacobelli M, Koopmans LVE, Krankowski A, Maat P, Norden MJ, Paas H, Pandey-Pommier M, Pandey VN, Pekal R, Pizzo R, Reich W, Rothkaehl H, Röttgering HJA, Rowlinson A, Schwarz DJ, Shulevski A, Sluman J, Smirnov O, Soida M, Tagger M, Toribio MC, van Ardenne A, Wijers RAMJ, van Weeren RJ, Wucknitz O, Zarka P, and Zucca P
Abstract: Lightning is a dangerous yet poorly understood natural phenomenon. Lightning forms a network of plasma channels propagating away from the initiation point with both positively and negatively charged ends-called positive and negative leaders 1 . Negative leaders propagate in discrete steps, emitting copious radio pulses in the 30-300-megahertz frequency band 2-8 that can be remotely sensed and imaged with high spatial and temporal resolution 9-11 . Positive leaders propagate more continuously and thus emit very little high-frequency radiation 12 . Radio emission from positive leaders has nevertheless been mapped 13-15 , and exhibits a pattern that is different from that of negative leaders 11-13,16,17 . Furthermore, it has been inferred that positive leaders can become transiently disconnected from negative leaders 9,12,16,18-20 , which may lead to current pulses that both reconnect positive leaders to negative leaders 11,16,17,20-22 and cause multiple cloud-to-ground lightning events 1 . The disconnection process is thought to be due to negative differential resistance 18 , but this does not explain why the disconnections form primarily on positive leaders 22 , or why the current in cloud-to-ground lightning never goes to zero 23 . Indeed, it is still not understood how positive leaders emit radio-frequency radiation or why they behave differently from negative leaders. Here we report three-dimensional radio interferometric observations of lightning over the Netherlands with unprecedented spatiotemporal resolution. We find small plasma structures-which we call 'needles'-that are the dominant source of radio emission from the positive leaders. These structures appear to drain charge from the leader, and are probably the reason why positive leaders disconnect from negative ones, and why cloud-to-ground lightning connects to the ground multiple times.
Published: 2019
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12. Low-radio-frequency eclipses of the redback pulsar J2215+5135 observed in the image plane with LOFAR.

Author: Broderick JW, Fender RP, Breton RP, Stewart AJ, Rowlinson A, Swinbank JD, Hessels JW, Staley TD, van der Horst AJ, Bell ME, Carbone D, Cendes Y, Corbel S, Eislöffel J, Falcke H, Grießmeier JM, Hassall TE, Jonker P, Kramer M, Kuniyoshi M, Law CJ, Markoff S, Molenaar GJ, Pietka M, Scheers LH, Serylak M, Stappers BW, Ter Veen S, van Leeuwen J, Wijers RA, Wijnands R, Wise MW, and Zarka P
Abstract: The eclipses of certain types of binary millisecond pulsars (i.e. 'black widows' and 'redbacks') are often studied using high-time-resolution, 'beamformed' radio observations. However, they may also be detected in images generated from interferometric data. As part of a larger imaging project to characterize the variable and transient sky at radio frequencies <200 MHz, we have blindly detected the redback system PSR J2215+5135 as a variable source of interest with the Low-Frequency Array (LOFAR). Using observations with cadences of two weeks - six months, we find preliminary evidence that the eclipse duration is frequency dependent (∝ν -0.4 ), such that the pulsar is eclipsed for longer at lower frequencies, in broad agreement with beamformed studies of other similar sources. Furthermore, the detection of the eclipses in imaging data suggests an eclipsing medium that absorbs the pulsed emission, rather than scattering it. Our study is also a demonstration of the prospects of finding pulsars in wide-field imaging surveys with the current generation of low-frequency radio telescopes.
Published: 2016
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13. New methods to constrain the radio transient rate: results from a survey of four fields with LOFAR.

Author: Carbone D, van der Horst AJ, Wijers RA, Swinbank JD, Rowlinson A, Broderick JW, Cendes YN, Stewart AJ, Bell ME, Breton RP, Corbel S, Eislöffel J, Fender RP, Grießmeier JM, Hessels JW, Jonker P, Kramer M, Law CJ, Miller-Jones JC, Pietka M, Scheers LH, Stappers BW, van Leeuwen J, Wijnands R, Wise M, and Zarka P
Abstract: We report on the results of a search for radio transients between 115 and 190 MHz with the LOw-Frequency ARray (LOFAR). Four fields have been monitored with cadences between 15 min and several months. A total of 151 images were obtained, giving a total survey area of 2275 deg 2 . We analysed our data using standard LOFAR tools and searched for radio transients using the LOFAR Transients Pipeline. No credible radio transient candidate has been detected; however, we are able to set upper limits on the surface density of radio transient sources at low radio frequencies. We also show that low-frequency radio surveys are more sensitive to steep-spectrum coherent transient sources than GHz radio surveys. We used two new statistical methods to determine the upper limits on the transient surface density. One is free of assumptions on the flux distribution of the sources, while the other assumes a power-law distribution in flux and sets more stringent constraints on the transient surface density. Both of these methods provide better constraints than the approach used in previous works. The best value for the upper limit we can set for the transient surface density, using the method assuming a power-law flux distribution, is 1.3 × 10 -3 deg -2 for transients brighter than 0.3 Jy with a time-scale of 15 min, at a frequency of 150 MHz. We also calculated for the first time upper limits for the transient surface density for transients of different time-scales. We find that the results can differ by orders of magnitude from previously reported, simplified estimates.
Published: 2016
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14. A radio jet from the optical and x-ray bright stellar tidal disruption flare ASASSN-14li.

Author: van Velzen S, Anderson GE, Stone NC, Fraser M, Wevers T, Metzger BD, Jonker PG, van der Horst AJ, Staley TD, Mendez AJ, Miller-Jones JC, Hodgkin ST, Campbell HC, and Fender RP
Abstract: The tidal disruption of a star by a supermassive black hole leads to a short-lived thermal flare. Despite extensive searches, radio follow-up observations of known thermal stellar tidal disruption flares (TDFs) have not yet produced a conclusive detection. We present a detection of variable radio emission from a thermal TDF, which we interpret as originating from a newly launched jet. The multiwavelength properties of the source present a natural analogy with accretion-state changes of stellar mass black holes, which suggests that all TDFs could be accompanied by a jet. In the rest frame of the TDF, our radio observations are an order of magnitude more sensitive than nearly all previous upper limits, explaining how these jets, if common, could thus far have escaped detection., (Copyright © 2016, American Association for the Advancement of Science.)
Published: 2016
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15. Circular polarization in the optical afterglow of GRB 121024A.

Author: Wiersema K, Covino S, Toma K, van der Horst AJ, Varela K, Min M, Greiner J, Starling RL, Tanvir NR, Wijers RA, Campana S, Curran PA, Fan Y, Fynbo JP, Gorosabel J, Gomboc A, Götz D, Hjorth J, Jin ZP, Kobayashi S, Kouveliotou C, Mundell C, O'Brien PT, Pian E, Rowlinson A, Russell DM, Salvaterra R, di Serego Alighieri S, Tagliaferri G, Vergani SD, Elliott J, Fariña C, Hartoog OE, Karjalainen R, Klose S, Knust F, Levan AJ, Schady P, Sudilovsky V, and Willingale R
Abstract: Gamma-ray bursts (GRBs) are most probably powered by collimated relativistic outflows (jets) from accreting black holes at cosmological distances. Bright afterglows are produced when the outflow collides with the ambient medium. Afterglow polarization directly probes the magnetic properties of the jet when measured minutes after the burst, and it probes the geometric properties of the jet and the ambient medium when measured hours to days after the burst. High values of optical polarization detected minutes after the burst of GRB 120308A indicate the presence of large-scale ordered magnetic fields originating from the central engine (the power source of the GRB). Theoretical models predict low degrees of linear polarization and no circular polarization at late times, when the energy in the original ejecta is quickly transferred to the ambient medium and propagates farther into the medium as a blast wave. Here we report the detection of circularly polarized light in the afterglow of GRB 121024A, measured 0.15 days after the burst. We show that the circular polarization is intrinsic to the afterglow and unlikely to be produced by dust scattering or plasma propagation effects. A possible explanation is to invoke anisotropic (rather than the commonly assumed isotropic) electron pitch-angle distributions, and we suggest that new models are required to produce the complex microphysics of realistic shocks in relativistic jets.
Published: 2014
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16. The first pulse of the extremely bright GRB 130427A: a test lab for synchrotron shocks.

Author: Preece R, Burgess JM, von Kienlin A, Bhat PN, Briggs MS, Byrne D, Chaplin V, Cleveland W, Collazzi AC, Connaughton V, Diekmann A, Fitzpatrick G, Foley S, Gibby M, Giles M, Goldstein A, Greiner J, Gruber D, Jenke P, Kippen RM, Kouveliotou C, McBreen S, Meegan C, Paciesas WS, Pelassa V, Tierney D, van der Horst AJ, Wilson-Hodge C, Xiong S, Younes G, Yu HF, Ackermann M, Ajello M, Axelsson M, Baldini L, Barbiellini G, Baring MG, Bastieri D, Bellazzini R, Bissaldi E, Bonamente E, Bregeon J, Brigida M, Bruel P, Buehler R, Buson S, Caliandro GA, Cameron RA, Caraveo PA, Cecchi C, Charles E, Chekhtman A, Chiang J, Chiaro G, Ciprini S, Claus R, Cohen-Tanugi J, Cominsky LR, Conrad J, D'Ammando F, de Angelis A, de Palma F, Dermer CD, Desiante R, Digel SW, Di Venere L, Drell PS, Drlica-Wagner A, Favuzzi C, Franckowiak A, Fukazawa Y, Fusco P, Gargano F, Gehrels N, Germani S, Giglietto N, Giordano F, Giroletti M, Godfrey G, Granot J, Grenier IA, Guiriec S, Hadasch D, Hanabata Y, Harding AK, Hayashida M, Iyyani S, Jogler T, Jóhannesson G, Kawano T, Knödlseder J, Kocevski D, Kuss M, Lande J, Larsson J, Larsson S, Latronico L, Longo F, Loparco F, Lovellette MN, Lubrano P, Mayer M, Mazziotta MN, Michelson PF, Mizuno T, Monzani ME, Moretti E, Morselli A, Murgia S, Nemmen R, Nuss E, Nymark T, Ohno M, Ohsugi T, Okumura A, Omodei N, Orienti M, Paneque D, Perkins JS, Pesce-Rollins M, Piron F, Pivato G, Porter TA, Racusin JL, Rainò S, Rando R, Razzano M, Razzaque S, Reimer A, Reimer O, Ritz S, Roth M, Ryde F, Sartori A, Scargle JD, Schulz A, Sgrò C, Siskind EJ, Spandre G, Spinelli P, Suson DJ, Tajima H, Takahashi H, Thayer JG, Thayer JB, Tibaldo L, Tinivella M, Torres DF, Tosti G, Troja E, Usher TL, Vandenbroucke J, Vasileiou V, Vianello G, Vitale V, Werner M, Winer BL, Wood KS, and Zhu S
Abstract: Gamma-ray burst (GRB) 130427A is one of the most energetic GRBs ever observed. The initial pulse up to 2.5 seconds is possibly the brightest well-isolated pulse observed to date. A fine time resolution spectral analysis shows power-law decays of the peak energy from the onset of the pulse, consistent with models of internal synchrotron shock pulses. However, a strongly correlated power-law behavior is observed between the luminosity and the spectral peak energy that is inconsistent with curvature effects arising in the relativistic outflow. It is difficult for any of the existing models to account for all of the observed spectral and temporal behaviors simultaneously.
Published: 2014
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17. A possible relativistic jetted outburst from a massive black hole fed by a tidally disrupted star.

Author: Bloom JS, Giannios D, Metzger BD, Cenko SB, Perley DA, Butler NR, Tanvir NR, Levan AJ, O'Brien PT, Strubbe LE, De Colle F, Ramirez-Ruiz E, Lee WH, Nayakshin S, Quataert E, King AR, Cucchiara A, Guillochon J, Bower GC, Fruchter AS, Morgan AN, and van der Horst AJ
Abstract: Gas accretion onto some massive black holes (MBHs) at the centers of galaxies actively powers luminous emission, but most MBHs are considered dormant. Occasionally, a star passing too near an MBH is torn apart by gravitational forces, leading to a bright tidal disruption flare (TDF). Although the high-energy transient Sw 1644+57 initially displayed none of the theoretically anticipated (nor previously observed) TDF characteristics, we show that observations suggest a sudden accretion event onto a central MBH of mass about 10(6) to 10(7) solar masses. There is evidence for a mildly relativistic outflow, jet collimation, and a spectrum characterized by synchrotron and inverse Compton processes; this leads to a natural analogy of Sw 1644+57 to a temporary smaller-scale blazar.
Published: 2011
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18. An extremely luminous panchromatic outburst from the nucleus of a distant galaxy.

Author: Levan AJ, Tanvir NR, Cenko SB, Perley DA, Wiersema K, Bloom JS, Fruchter AS, Postigo Ade U, O'Brien PT, Butler N, van der Horst AJ, Leloudas G, Morgan AN, Misra K, Bower GC, Farihi J, Tunnicliffe RL, Modjaz M, Silverman JM, Hjorth J, Thöne C, Cucchiara A, Cerón JM, Castro-Tirado AJ, Arnold JA, Bremer M, Brodie JP, Carroll T, Cooper MC, Curran PA, Cutri RM, Ehle J, Forbes D, Fynbo J, Gorosabel J, Graham J, Hoffman DI, Guziy S, Jakobsson P, Kamble A, Kerr T, Kasliwal MM, Kouveliotou C, Kocevski D, Law NM, Nugent PE, Ofek EO, Poznanski D, Quimby RM, Rol E, Romanowsky AJ, Sánchez-Ramírez R, Schulze S, Singh N, van Spaandonk L, Starling RL, Strom RG, Tello JC, Vaduvescu O, Wheatley PJ, Wijers RA, Winters JM, and Xu D
Abstract: Variable x-ray and γ-ray emission is characteristic of the most extreme physical processes in the universe. We present multiwavelength observations of a unique γ-ray-selected transient detected by the Swift satellite, accompanied by bright emission across the electromagnetic spectrum, and whose properties are unlike any previously observed source. We pinpoint the event to the center of a small, star-forming galaxy at redshift z = 0.3534. Its high-energy emission has lasted much longer than any γ-ray burst, whereas its peak luminosity was ∼100 times higher than bright active galactic nuclei. The association of the outburst with the center of its host galaxy suggests that this phenomenon has its origin in a rare mechanism involving the massive black hole in the nucleus of that galaxy.
Published: 2011
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19. A mildly relativistic radio jet from the otherwise normal type Ic supernova 2007gr.

Author: Paragi Z, Taylor GB, Kouveliotou C, Granot J, Ramirez-Ruiz E, Bietenholz M, van der Horst AJ, Pidopryhora Y, van Langevelde HJ, Garrett MA, Szomoru A, Argo MK, Bourke S, and Paczyński 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 (GRBs). 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 approximately 6,000 km s(-1), 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 spectropolarimetry, mildly aspherical.
Published: 2010
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20. A limit on the variation of the speed of light arising from quantum gravity effects.

Author: Abdo AA, Ackermann M, Ajello M, Asano K, Atwood WB, Axelsson M, Baldini L, Ballet J, Barbiellini G, Baring MG, Bastieri D, Bechtol K, Bellazzini R, Berenji B, Bhat PN, Bissaldi E, Bloom ED, Bonamente E, Bonnell J, Borgland AW, Bouvier A, Bregeon J, Brez A, Briggs MS, Brigida M, Bruel P, Burgess JM, Burnett TH, Caliandro GA, Cameron RA, Caraveo PA, Casandjian JM, Cecchi C, Celik O, Chaplin V, Charles E, Cheung CC, Chiang J, Ciprini S, Claus R, Cohen-Tanugi J, Cominsky LR, Connaughton V, Conrad J, Cutini S, Dermer CD, de Angelis A, de Palma F, Digel SW, Dingus BL, do Couto E Silva E, Drell PS, Dubois R, Dumora D, Farnier C, Favuzzi C, Fegan SJ, Finke J, Fishman G, Focke WB, Foschini L, Fukazawa Y, Funk S, Fusco P, Gargano F, Gasparrini D, Gehrels N, Germani S, Gibby L, Giebels B, Giglietto N, Giordano F, Glanzman T, Godfrey G, Granot J, Greiner J, Grenier IA, Grondin MH, Grove JE, Grupe D, Guillemot L, Guiriec S, Hanabata Y, Harding AK, Hayashida M, Hays E, Hoversten EA, Hughes RE, Jóhannesson G, Johnson AS, Johnson RP, Johnson WN, Kamae T, Katagiri H, Kataoka J, Kawai N, Kerr M, Kippen RM, Knödlseder J, Kocevski D, Kouveliotou C, Kuehn F, Kuss M, Lande J, Latronico L, Lemoine-Goumard M, Longo F, Loparco F, Lott B, Lovellette MN, Lubrano P, Madejski GM, Makeev A, Mazziotta MN, McBreen S, McEnery JE, McGlynn S, Mészáros P, Meurer C, Michelson PF, Mitthumsiri W, Mizuno T, Moiseev AA, Monte C, Monzani ME, Moretti E, Morselli A, Moskalenko IV, Murgia S, Nakamori T, Nolan PL, Norris JP, Nuss E, Ohno M, Ohsugi T, Omodei N, Orlando E, Ormes JF, Ozaki M, Paciesas WS, Paneque D, Panetta JH, Parent D, Pelassa V, Pepe M, Pesce-Rollins M, Petrosian V, Piron F, Porter TA, Preece R, Rainò S, Ramirez-Ruiz E, Rando R, Razzano M, Razzaque S, Reimer A, Reimer O, Reposeur T, Ritz S, Rochester LS, Rodriguez AY, Roth M, Ryde F, Sadrozinski HF, Sanchez D, Sander A, Saz Parkinson PM, Scargle JD, Schalk TL, Sgrò C, Siskind EJ, Smith DA, Smith PD, Spandre G, Spinelli P, Stamatikos M, Stecker FW, Strickman MS, Suson DJ, Tajima H, Takahashi H, Takahashi T, Tanaka T, Thayer JB, Thayer JG, Thompson DJ, Tibaldo L, Toma K, Torres DF, Tosti G, Troja E, Uchiyama Y, Uehara T, Usher TL, van der Horst AJ, Vasileiou V, Vilchez N, Vitale V, von Kienlin A, Waite AP, Wang P, Wilson-Hodge C, Winer BL, Wood KS, Wu XF, Yamazaki R, Ylinen T, and Ziegler M
Abstract: A cornerstone of Einstein's special relativity is Lorentz invariance-the postulate that all observers measure exactly the same speed of light in vacuum, independent of photon-energy. While special relativity assumes that there is no fundamental length-scale associated with such invariance, there is a fundamental scale (the Planck scale, l(Planck) approximately 1.62 x 10(-33) cm or E(Planck) = M(Planck)c(2) approximately 1.22 x 10(19) GeV), at which quantum effects are expected to strongly affect the nature of space-time. There is great interest in the (not yet validated) idea that Lorentz invariance might break near the Planck scale. A key test of such violation of Lorentz invariance is a possible variation of photon speed with energy. Even a tiny variation in photon speed, when accumulated over cosmological light-travel times, may be revealed by observing sharp features in gamma-ray burst (GRB) light-curves. Here we report the detection of emission up to approximately 31 GeV from the distant and short GRB 090510. We find no evidence for the violation of Lorentz invariance, and place a lower limit of 1.2E(Planck) on the scale of a linear energy dependence (or an inverse wavelength dependence), subject to reasonable assumptions about the emission (equivalently we have an upper limit of l(Planck)/1.2 on the length scale of the effect). Our results disfavour quantum-gravity theories in which the quantum nature of space-time on a very small scale linearly alters the speed of light.
Published: 2009
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21. Fermi observations of high-energy gamma-ray emission from GRB 080916C.

Author: Abdo AA, Ackermann M, Arimoto M, Asano K, Atwood WB, Axelsson M, Baldini L, Ballet J, Band DL, Barbiellini G, Baring MG, Bastieri D, Battelino M, Baughman BM, Bechtol K, Bellardi F, Bellazzini R, Berenji B, Bhat PN, Bissaldi E, Blandford RD, Bloom ED, Bogaert G, Bogart JR, Bonamente E, Bonnell J, Borgland AW, Bouvier A, Bregeon J, Brez A, Briggs MS, Brigida M, Bruel P, Burnett TH, Burrows D, Busetto G, Caliandro GA, Cameron RA, Caraveo PA, Casandjian JM, Ceccanti M, Cecchi C, Celotti A, Charles E, Chekhtman A, Cheung CC, Chiang J, Ciprini S, Claus R, Cohen-Tanugi J, Cominsky LR, Connaughton V, Conrad J, Costamante L, Cutini S, Deklotz M, Dermer CD, de Angelis A, de Palma F, Digel SW, Dingus BL, do Couto E Silva E, Drell PS, Dubois R, Dumora D, Edmonds Y, Evans PA, Fabiani D, Farnier C, Favuzzi C, Finke J, Fishman G, Focke WB, Frailis M, Fukazawa Y, Funk S, Fusco P, Gargano F, Gasparrini D, Gehrels N, Germani S, Giebels B, Giglietto N, Giommi P, Giordano F, Glanzman T, Godfrey G, Goldstein A, Granot J, Greiner J, Grenier IA, Grondin MH, Grove JE, Guillemot L, Guiriec S, Haller G, Hanabata Y, Harding AK, Hayashida M, Hays E, Hernando Morat JA, Hoover A, Hughes RE, Jóhannesson G, Johnson AS, Johnson RP, Johnson TJ, Johnson WN, Kamae T, Katagiri H, Kataoka J, Kavelaars A, Kawai N, Kelly H, Kennea J, Kerr M, Kippen RM, Knödlseder J, Kocevski D, Kocian ML, Komin N, Kouveliotou C, Kuehn F, Kuss M, Lande J, Landriu D, Larsson S, Latronico L, Lavalley C, Lee B, Lee SH, Lemoine-Goumard M, Lichti GG, Longo F, Loparco F, Lott B, Lovellette MN, Lubrano P, Madejski GM, Makeev A, Marangelli B, Mazziotta MN, McBreen S, McEnery JE, McGlynn S, Meegan C, Mészáros P, Meurer C, Michelson PF, Minuti M, Mirizzi N, Mitthumsiri W, Mizuno T, Moiseev AA, Monte C, Monzani ME, Moretti E, Morselli A, Moskalenko IV, Murgia S, Nakamori T, Nelson D, Nolan PL, Norris JP, Nuss E, Ohno M, Ohsugi T, Okumura A, Omodei N, Orlando E, Ormes JF, Ozaki M, Paciesas WS, Paneque D, Panetta JH, Parent D, Pelassa V, Pepe M, Perri M, Pesce-Rollins M, Petrosian V, Pinchera M, Piron F, Porter TA, Preece R, Rainò S, Ramirez-Ruiz E, Rando R, Rapposelli E, Razzano M, Razzaque S, Rea N, Reimer A, Reimer O, Reposeur T, Reyes LC, Ritz S, Rochester LS, Rodriguez AY, Roth M, Ryde F, Sadrozinski HF, Sanchez D, Sander A, Saz Parkinson PM, Scargle JD, Schalk TL, Segal KN, Sgrò C, Shimokawabe T, Siskind EJ, Smith DA, Smith PD, Spandre G, Spinelli P, Stamatikos M, Starck JL, Stecker FW, Steinle H, Stephens TE, Strickman MS, Suson DJ, Tagliaferri G, Tajima H, Takahashi H, Takahashi T, Tanaka T, Tenze A, Thayer JB, Thayer JG, Thompson DJ, Tibaldo L, Torres DF, Tosti G, Tramacere A, Turri M, Tuvi S, Usher TL, van der Horst AJ, Vigiani L, Vilchez N, Vitale V, von Kienlin A, Waite AP, Williams DA, Wilson-Hodge C, Winer BL, Wood KS, Wu XF, Yamazaki R, Ylinen T, and Ziegler M
Abstract: Gamma-ray bursts (GRBs) are highly energetic explosions signaling the death of massive stars in distant galaxies. The Gamma-ray Burst Monitor and Large Area Telescope onboard the Fermi Observatory together record GRBs over a broad energy range spanning about 7 decades of gammaray energy. In September 2008, Fermi observed the exceptionally luminous GRB 080916C, with the largest apparent energy release yet measured. The high-energy gamma rays are observed to start later and persist longer than the lower energy photons. A simple spectral form fits the entire GRB spectrum, providing strong constraints on emission models. The known distance of the burst enables placing lower limits on the bulk Lorentz factor of the outflow and on the quantum gravity mass.
Published: 2009
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22. Broadband observations of the naked-eye gamma-ray burst GRB 080319B.

Author: Racusin JL, Karpov SV, Sokolowski M, Granot J, Wu XF, Pal'shin V, Covino S, van der Horst AJ, Oates SR, Schady P, Smith RJ, Cummings J, Starling RL, Piotrowski LW, Zhang B, Evans PA, Holland ST, Malek K, Page MT, Vetere L, Margutti R, Guidorzi C, Kamble AP, Curran PA, Beardmore A, Kouveliotou C, Mankiewicz L, Melandri A, O'Brien PT, Page KL, Piran T, Tanvir NR, Wrochna G, Aptekar RL, Barthelmy S, Bartolini C, Beskin GM, Bondar S, Bremer M, Campana S, Castro-Tirado A, Cucchiara A, Cwiok M, D'Avanzo P, D'Elia V, Valle MD, de Ugarte Postigo A, Dominik W, Falcone A, Fiore F, Fox DB, Frederiks DD, Fruchter AS, Fugazza D, Garrett MA, Gehrels N, Golenetskii S, Gomboc A, Gorosabel J, Greco G, Guarnieri A, Immler S, Jelinek M, Kasprowicz G, La Parola V, Levan AJ, Mangano V, Mazets EP, Molinari E, Moretti A, Nawrocki K, Oleynik PP, Osborne JP, Pagani C, Pandey SB, Paragi Z, Perri M, Piccioni A, Ramirez-Ruiz E, Roming PW, Steele IA, Strom RG, Testa V, Tosti G, Ulanov MV, Wiersema K, Wijers RA, Winters JM, Zarnecki AF, Zerbi F, Mészáros P, Chincarini G, and Burrows DN
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 massive stars. Previous early optical observations of even the most exceptional GRBs (990123 and 030329) lacked both the temporal resolution to probe the optical flash in detail and the accuracy needed to trace the transition from the prompt emission within the outflow to external shocks caused by interaction with the progenitor environment. Here we report observations of the extraordinarily bright prompt optical and gamma-ray emission of GRB 080319B that provide diagnostics within seconds of its formation, followed by broadband observations of the afterglow decay that continued for weeks. We show that the prompt emission stems from a single physical region, implying an extremely relativistic outflow that propagates within the narrow inner core of a two-component jet.
Published: 2008
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23. GRB 030329: 3 years of radio afterglow monitoring.

Author: van der Horst AJ, Kamble A, Wijers RA, Resmi L, Bhattacharya D, Rol E, Strom R, Kouveliotou C, Oosterloo T, and Ishwara-Chandra CH
Abstract: Radio observations of gamma-ray burst (GRB) afterglows are essential for our understanding of the physics of relativistic blast waves, as they enable us to follow the evolution of GRB explosions much longer than the afterglows in any other wave band. We have performed a 3-year monitoring campaign of GRB 030329 with the Westerbork Synthesis Radio Telescopes and the Giant Metrewave Radio Telescope. Our observations, combined with observations at other wavelengths, have allowed us to determine the GRB blast wave physical parameters, such as the total burst energy and the ambient medium density, as well as to investigate the jet nature of the relativistic outflow. Further, by modelling the late-time radio light curve of GRB 030329, we predict that the Low-Frequency Array (30-240 MHz) will be able to observe afterglows of similar GRBs, and constrain the physics of the blast wave during its non-relativistic phase.
Published: 2007
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24. An expanding radio nebula produced by a giant flare from the magnetar SGR 1806-20.

Author: Gaensler BM, Kouveliotou C, Gelfand JD, Taylor GB, Eichler D, Wijers RA, Granot J, Ramirez-Ruiz E, Lyubarsky YE, Hunstead RW, Campbell-Wilson D, van der Horst AJ, McLaughlin MA, Fender RP, Garrett MA, Newton-McGee KJ, Palmer DM, Gehrels N, and Woods PM
Abstract: Soft gamma-ray repeaters (SGRs) are 'magnetars', a small class of slowly spinning neutron stars with extreme surface magnetic fields, B approximately 10(15) gauss (refs 1 , 2 -3). On 27 December 2004, a giant flare was detected from the magnetar SGR 1806-20 (ref. 2), only the third such event recorded. This burst of energy was detected by a variety of instruments and even caused an ionospheric disturbance in the Earth's upper atmosphere that was recorded around the globe. Here we report the detection of a fading radio afterglow produced by this outburst, with a luminosity 500 times larger than the only other detection of a similar source. From day 6 to day 19 after the flare from SGR 1806-20, a resolved, linearly polarized, radio nebula was seen, expanding at approximately a quarter of the speed of light. To create this nebula, at least 4 x 10(43) ergs of energy must have been emitted by the giant flare in the form of magnetic fields and relativistic particles.
Published: 2005
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24 results on '"Van Der Horst, AJ"'

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24. An expanding radio nebula produced by a giant flare from the magnetar SGR 1806-20.

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