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1. The Fourth Fermi-GBM Gamma-Ray Burst Catalog: A Decade of Data

Author: von Kienlin, A., Meegan, C. A., Paciesas, W. S., Bhat, P. N., Bissaldi, E., Briggs, M. S., Burns, E., Cleveland, W. H., Gibby, M. H., Giles, M. M., Goldstein, A., Hamburg, R., Hui, C. M., Kocevski, D., Mailyan, B., Malacaria, C., Poolakkil, S., Preece, R. D., Roberts, O. J., Veres, P., and Wilson-Hodge, C. A.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present the fourth in a series of catalogs of gamma-ray bursts (GRBs) observed with Fermi's Gamma-Ray Burst Monitor (Fermi-GBM). It extends the six year catalog by four more years, now covering the ten year time period from trigger enabling on 2008 July 12 to 2018 July 11. During this time period GBM triggered almost twice a day on transient events of which we identifyied 2356 as cosmic GRBs. Additional trigger events were due to solar are events, magnetar burst activities, and terrestrial gamma-ray flashes. The intention of the GBM GRB catalog series is to provide updated information to the community on the most important observables of the GBM-detected GRBs. For each GRB the location and main characteristics of the prompt emission, the duration, peak flux, and fluence are derived. The latter two quantities are calculated for the 50-300 keV energy band, where the maximum energy release of GRBs in the instrument reference system is observed and also for a broader energy band from 10-1000 keV, exploiting the full energy range of GBM's low-energy detectors. Furthermore, information is given on the settings of the triggering criteria and exceptional operational conditions during years 7 to 10 in the mission. This fourth catalog is an official product of the Fermi-GBM science team, and the data files containing the complete results are available from the High-Energy Astrophysics Science Archive Research Center (HEASARC)., Comment: 273 pages, 10 figures, 8 tables. This is a 10 year catalog update of arXiv:1603.07612
Published: 2020
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2. A Fermi Gamma-ray Burst Monitor Search for Electromagnetic Signals Coincident with Gravitational-Wave Candidates in Advanced LIGO's First Observing Run

Author: Team, The Fermi Gamma-ray Burst Monitor, Collaboration, The LIGO Scientific, Collaboration, the Virgo, Burns, E., Goldstein, A., Hui, C. M., Blackburn, L., Briggs, M. S., Connaughton, V., Hamburg, R., Kocevski, D., Veres, P., Wilson-Hodge, C. A., Bissaldi, E., Cleveland, W. H., Giles, M. M., Mailyan, B., Meegan, C. A., Paciesas, W. A., Poolakkil, S., Preece, R. D., Racusin, J. L., Roberts, O. J., von Kienlin, A., Abbott, B. P., Abbott, R., Abbott, T. D., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R. X., Adya, V. B., Affeldt, C., Agarwal, B., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, B., Allen, G., Allocca, A., Aloy, M. A., Altin, P. A., Amato, A., Ananyeva, A., Anderson, S. B., Anderson, W. G., Angelova, S. V., Antier, S., Appert, S., Arai, K., Araya, M. C., Areeda, J. S., Ar`ene, M., Arnaud, N., Arun, K. G., Ascenzi, S., Ashton, G., Ast, M., Aston, S. M., Astone, P., Atallah, D. V., Aubin, F., Aufmuth, P., Aulbert, C., AultONeal, K., Austin, C., Avila-Alvarez, A., Babak, S., Bacon, P., Badaracco, F., Bader, M. K. M., Bae, S., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Banagiri, S., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barkett, K., Barnum, S., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Batch, J. C., Bawaj, M., Bayley, J. C., Bazzan, M., B'ecsy, B., Beer, C., Bejger, M., Belahcene, I., Bell, A. S., Beniwal, D., Bensch, M., Berger, B. K., Bergmann, G., Bernuzzi, S., Bero, J. J., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhandare, R., Bilenko, I. A., Bilgili, S. A., Billingsley, G., Billman, C. R., Birch, J., Birney, R., Birnholtz, O., Biscans, S., Biscoveanu, S., Bisht, A., Bitossi, M., Bizouard, M. A., Blackburn, J. K., Blackman, J., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bock, O., Bode, N., Boer, M., Boetzel, Y., Bogaert, G., Bohe, A., Bondu, F., Bonilla, E., Bonnand, R., Booker, P., Boom, B. A., Booth, C. D., Bork, R., Boschi, V., Bose, S., Bossie, K., Bossilkov, V., Bosveld, J., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Bramley, A., Branchesi, M., Brau, J. E., Briant, T., Brighenti, F., Brillet, A., Brinkmann, M., Brisson, V., Brockill, P., Brooks, A. F., Brown, D. D., Brunett, S., Buchanan, C. C., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. L., Cabero, M., Cadonati, L., Cagnoli, G., Cahillane, C., Bustillo, J. Calder'on, Callister, T. A., Calloni, E., Camp, J. B., Canepa, M., Canizares, P., Cannon, K. C., Cao, H., Cao, J., Capano, C. D., Capocasa, E., Carbognani, F., Caride, S., Carney, M. F., Diaz, J. Casanueva, Casentini, C., Caudill, S., a, M. Cavagli`, Cavalier, F., Cavalieri, R., Cella, G., Cepeda, C. B., Cerd'a-Dur'an, P., Cerretani, G., Cesarini, E., Chaibi, O., Chamberlin, S. J., Chan, M., Chao, S., Charlton, P., Chase, E., Chassande-Mottin, E., Chatterjee, D., Cheeseboro, B. D., Chen, H. Y., Chen, X., Chen, Y., Cheng, H. -P., Chia, H. Y., Chincarini, A., Chiummo, A., Chmiel, T., Cho, H. S., Cho, M., Chow, J. H., Christensen, N., Chu, Q., Chua, A. J. K., Chua, S., Chung, K. W., Chung, S., Ciani, G., Ciobanu, A. A., Ciolfi, R., Cipriano, F., Cirelli, C. E., Cirone, A., Clara, F., Clark, J. A., Clearwater, P., Cleva, F., Cocchieri, C., Coccia, E., Cohadon, P. -F., Cohen, D., Colla, A., Collette, C. G., Collins, C., Cominsky, L. R., Constancio Jr., M., Conti, L., Cooper, S. J., Corban, P., Corbitt, T. R., Cordero-Carri'on, I., Corley, K. R., Cornish, N., Corsi, A., Cortese, S., Costa, C. A., Cotesta, R., Coughlin, M. W., Coughlin, S. B., Coulon, J. -P., Countryman, S. T., Couvares, P., Covas, P. B., Cowan, E. E., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Creighton, J. D. E., Creighton, T. D., Cripe, J., Crowder, S. G., Cullen, T. J., Cumming, A., Cunningham, L., Cuoco, E., Canton, T. Dal, D'alya, G., Danilishin, S. L., D'Antonio, S., Danzmann, K., Dasgupta, A., Costa, C. F. Da Silva, Dattilo, V., Dave, I., Davier, M., Davis, D., Daw, E. J., Day, B., DeBra, D., Deenadayalan, M., Degallaix, J., De Laurentis, M., Del'eglise, S., Del Pozzo, W., Demos, N., Denker, T., Dent, T., De Pietri, R., Derby, J., Dergachev, V., De Rosa, R., De Rossi, C., DeSalvo, R., de Varona, O., Dhurandhar, S., D'ıaz, M. C., Di Fiore, L., Di Giovanni, M., Di Girolamo, T., Di Lieto, A., Ding, B., Di Pace, S., Di Palma, I., Di Renzo, F., Dmitriev, A., Doctor, Z., Dolique, V., Donovan, F., Dooley, K. L., Doravari, S., Dorrington, I., 'Alvarez, M. Dovale, Downes, T. P., Drago, M., Dreissigacker, C., Driggers, J. C., Du, Z., Dupej, P., Dwyer, S. E., Easter, P. J., Edo, T. B., Edwards, M. C., Effler, A., Eggenstein, H. -B., Ehrens, P., Eichholz, J., Eikenberry, S. S., Eisenmann, M., Eisenstein, R. A., Essick, R. C., Estelles, H., Estevez, D., Etienne, Z. B., Etzel, T., Evans, M., Evans, T. M., Fafone, V., Fair, H., Fairhurst, S., Fan, X., Farinon, S., Farr, B., Farr, W. M., Fauchon-Jones, E. J., Favata, M., Fays, M., Fee, C., Fehrmann, H., Feicht, J., Fejer, M. M., Feng, F., Fernandez-Galiana, A., Ferrante, I., Ferreira, E. C., Ferrini, F., Fidecaro, F., Fiori, I., Fiorucci, D., Fishbach, M., Fisher, R. P., Fishner, J. M., Fitz-Axen, M., Flaminio, R., Fletcher, M., Fong, H., Font, J. A., Forsyth, P. W. F., Forsyth, S. S., Fournier, J. -D., Frasca, S., Frasconi, F., Frei, Z., Freise, A., Frey, R., Frey, V., Fritschel, P., Frolov, V. V., Fulda, P., Fyffe, M., Gabbard, H. A., Gadre, B. U., Gaebel, S. M., Gair, J. R., Gammaitoni, L., Ganija, M. R., Gaonkar, S. G., Garcia, A., Garc'ıa-Quir'os, C., Garufi, F., Gateley, B., Gaudio, S., Gaur, G., Gayathri, V., Gemme, G., Genin, E., Gennai, A., George, D., George, J., Gergely, L., Germain, V., Ghonge, S., Ghosh, Abhirup, Ghosh, Archisman, Ghosh, S., Giacomazzo, B., Giaime, J. A., Giardina, K. D., Giazotto, A., Gill, K., Giordano, G., Glover, L., Goetz, E., Goetz, R., Goncharov, B., Gonz'alez, G., Castro, J. M. Gonzalez, Gopakumar, A., Gorodetsky, M. L., Gossan, S. E., Gosselin, M., Gouaty, R., Grado, A., Graef, C., Granata, M., Grant, A., Gras, S., Gray, C., Greco, G., Green, A. C., Green, R., Gretarsson, E. M., Groot, P., Grote, H., Grunewald, S., Gruning, P., Guidi, G. M., Gulati, H. K., Guo, X., Gupta, A., Gupta, M. K., Gushwa, K. E., Gustafson, E. K., Gustafson, R., Halim, O., Hall, B. R., Hall, E. D., Hamilton, E. Z., Hamilton, H. F., Hammond, G., Haney, M., Hanke, M. M., Hanks, J., Hanna, C., Hannam, M. D., Hannuksela, O. A., Hanson, J., Hardwick, T., Harms, J., Harry, G. M., Harry, I. W., Hart, M. J., Haster, C. -J., Haughian, K., Healy, J., Heidmann, A., Heintze, M. C., Heitmann, H., Hello, P., Hemming, G., Hendry, M., Heng, I. S., Hennig, J., Heptonstall, A. W., Hernandez, F. J., Heurs, M., Hild, S., Hinderer, T., Hoak, D., Hochheim, S., Hofman, D., Holland, N. A., Holt, K., Holz, D. E., Hopkins, P., Horst, C., Hough, J., Houston, E. A., Howell, E. J., Hreibi, A., Huerta, E. A., Huet, D., Hughey, B., Hulko, M., Husa, S., Huttner, S. H., Huynh-Dinh, T., Iess, A., Indik, N., Ingram, C., Inta, R., Intini, G., Isa, H. N., Isac, J. -M., Isi, M., Iyer, B. R., Izumi, K., Jacqmin, T., Jani, K., Jaranowski, P., Johnson, D. S., Johnson, W. W., Jones, D. I., Jones, R., Jonker, R. J. G., Ju, L., Junker, J., Kalaghatgi, C. V., Kalogera, V., Kamai, B., Kandhasamy, S., Kang, G., Kanner, J. B., Kapadia, S. J., Karki, S., Karvinen, K. S., Kasprzack, M., Katolik, M., Katsanevas, S., Katsavounidis, E., Katzman, W., Kaufer, S., Kawabe, K., Keerthana, N. V., ef'elian, F. K', Keitel, D., Kemball, A. J., Kennedy, R., Key, J. S., Khalili, F. Y., Khamesra, B., Khan, H., Khan, I., Khan, S., Khan, Z., Khazanov, E. A., Kijbunchoo, N., Kim, Chunglee, Kim, J. C., Kim, K., Kim, W., Kim, W. S., Kim, Y. -M., King, E. J., King, P. J., Kinley-Hanlon, M., Kirchhoff, R., Kissel, J. S., Kleybolte, L., Klimenko, S., Knowles, T. D., Koch, P., Koehlenbeck, S. M., Koley, S., Kondrashov, V., Kontos, A., Korobko, M., Korth, W. Z., Kowalska, I., Kozak, D. B., Krämer, C., Kringel, V., Krishnan, B., Kr'olak, A., Kuehn, G., Kumar, P., Kumar, R., Kumar, S., Kuo, L., Kutynia, A., Kwang, S., Lackey, B. D., Lai, K. H., Landry, M., Lang, R. N., Lange, J., Lantz, B., Lanza, R. K., Lartaux-Vollard, A., Lasky, P. D., Laxen, M., Lazzarini, A., Lazzaro, C., Leaci, P., Leavey, S., Lee, C. H., Lee, H. K., Lee, H. M., Lee, H. W., Lee, K., Lehmann, J., Lenon, A., Leonardi, M., Leroy, N., Letendre, N., Levin, Y., Li, J., Li, T. G. F., Li, X., Linker, S. D., Littenberg, T. B., Liu, J., Liu, X., Lo, R. K. L., Lockerbie, N. A., London, L. T., Longo, A., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lough, J. D., Lousto, C. O., Lovelace, G., Lück, H., Lumaca, D., Lundgren, A. P., Lynch, R., Ma, Y., Macas, R., Macfoy, S., Machenschalk, B., MacInnis, M., Macleod, D. M., Hernandez, I. Magaña, Magaña-Sandoval, F., Zertuche, L. Magaña, Magee, R. M., Majorana, E., Maksimovic, I., Man, N., Mandic, V., Mangano, V., Mansell, G. L., Manske, M., Mantovani, M., Marchesoni, F., Marion, F., M'arka, S., M'arka, Z., Markakis, C., Markosyan, A. S., Markowitz, A., Maros, E., Marquina, A., Martelli, F., Martellini, L., Martin, I. W., Martin, R. M., Martynov, D. V., Mason, K., Massera, E., Masserot, A., Massinger, T. J., Masso-Reid, M., Mastrogiovanni, S., Matas, A., Matichard, F., Matone, L., Mavalvala, N., Mazumder, N., McCann, J. J., McCarthy, R., McClelland, D. E., McCormick, S., McCuller, L., McGuire, S. C., McIver, J., McManus, D. J., McRae, T., McWilliams, S. T., Meacher, D., Meadors, G. D., Mehmet, M., Meidam, J., Mejuto-Villa, E., Melatos, A., Mendell, G., Mendoza-Gandara, D., Mercer, R. A., Mereni, L., Merilh, E. L., Merzougui, M., Meshkov, S., Messenger, C., Messick, C., Metzdorff, R., Meyers, P. M., Miao, H., Michel, C., Middleton, H., Mikhailov, E. E., Milano, L., Miller, A. L., Miller, A., Miller, B. B., Miller, J., Millhouse, M., Mills, J., Milovich-Goff, M. C., Minazzoli, O., Minenkov, Y., Ming, J., Mishra, C., Mitra, S., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Moffa, D., Mogushi, K., Mohan, M., Mohapatra, S. R. P., Montani, M., Moore, C. J., Moraru, D., Moreno, G., Morisaki, S., Mours, B., Mow-Lowry, C. M., Mueller, G., Muir, A. W., Mukherjee, Arunava, Mukherjee, D., Mukherjee, S., Mukund, N., Mullavey, A., Munch, J., Muñiz, E. A., Muratore, M., Murray, P. G., Nagar, A., Napier, K., Nardecchia, I., Naticchioni, L., Nayak, R. K., Neilson, J., Nelemans, G., Nelson, T. J. N., Nery, M., Neunzert, A., Nevin, L., Newport, J. M., Ng, K. Y., Ng, S., Nguyen, P., Nguyen, T. T., Nichols, D., Nielsen, A. B., Nissanke, S., Nitz, A., Nocera, F., Nolting, D., North, C., Nuttall, L. K., Obergaulinger, M., Oberling, J., O'Brien, B. D., O'Dea, G. D., Ogin, G. H., Oh, J. J., Oh, S. H., Ohme, F., Ohta, H., Okada, M. A., Oliver, M., Oppermann, P., Oram, Richard J., O'Reilly, B., Ormiston, R., Ortega, L. F., O'Shaughnessy, R., Ossokine, S., Ottaway, D. J., Overmier, H., Owen, B. J., Pace, A. E., Pagano, G., Page, J., Page, M. A., Pai, A., Pai, S. A., Palamos, J. R., Palashov, O., Palomba, C., Pal-Singh, A., Pan, Howard, Pan, Huang-Wei, Pang, B., Pang, P. T. H., Pankow, C., Pannarale, F., Pant, B. C., Paoletti, F., Paoli, A., Papa, M. A., Parida, A., Parker, W., Pascucci, D., Pasqualetti, A., Passaquieti, R., Passuello, D., Patil, M., Patricelli, B., Pearlstone, B. L., Pedersen, C., Pedraza, M., Pedurand, R., Pekowsky, L., Pele, A., Penn, S., Perez, C. J., Perreca, A., Perri, L. M., Pfeiffer, H. P., Phelps, M., Phukon, K. S., Piccinni, O. J., Pichot, M., Piergiovanni, F., Pierro, V., Pillant, G., Pinard, L., Pinto, I. M., Pirello, M., Pitkin, M., Poggiani, R., Popolizio, P., Porter, E. K., Possenti, L., Post, A., Powell, J., Prasad, J., Pratt, J. W. W., Pratten, G., Predoi, V., Prestegard, T., Principe, M., Privitera, S., Prodi, G. A., Prokhorov, L. G., Puncken, O., Punturo, M., Puppo, P., Pürrer, M., Qi, H., Quetschke, V., Quintero, E. A., Quitzow-James, R., Raab, F. J., Rabeling, D. S., Radkins, H., Raffai, P., Raja, S., Rajan, C., Rajbhandari, B., Rakhmanov, M., Ramirez, K. E., Ramos-Buades, A., Rana, Javed, Rapagnani, P., Raymond, V., Razzano, M., Read, J., Regimbau, T., Rei, L., Reid, S., Reitze, D. H., Ren, W., Ricci, F., Ricker, P. M., Riles, K., Rizzo, M., Robertson, N. A., Robie, R., Robinet, F., Robson, T., Rocchi, A., Rolland, L., Rollins, J. G., Roma, V. J., Romano, R., Romel, C. L., Romie, J. H., Rosi'nska, D., Ross, M. P., Rowan, S., Rüdiger, A., Ruggi, P., Rutins, G., Ryan, K., Sachdev, S., Sadecki, T., Sakellariadou, M., Salconi, L., Saleem, M., Salemi, F., Samajdar, A., Sammut, L., Sampson, L. M., Sanchez, E. J., Sanchez, L. E., Sanchis-Gual, N., Sandberg, V., Sanders, J. R., Sarin, N., Sassolas, B., Sathyaprakash, B. S., Saulson, P. R., Sauter, O., Savage, R. L., Sawadsky, A., Schale, P., Scheel, M., Scheuer, J., Schmidt, P., Schnabel, R., Schofield, R. M. S., Schönbeck, A., Schreiber, E., Schuette, D., Schulte, B. W., Schutz, B. F., Schwalbe, S. G., Scott, J., Scott, S. M., Seidel, E., Sellers, D., Sengupta, A. S., Sentenac, D., Sequino, V., Sergeev, A., Setyawati, Y., Shaddock, D. A., Shaffer, T. J., Shah, A. A., Shahriar, M. S., Shaner, M. B., Shao, L., Shapiro, B., Shawhan, P., Shen, H., Shoemaker, D. H., Shoemaker, D. M., Siellez, K., Siemens, X., Sieniawska, M., Sigg, D., Silva, A. D., Singer, L. P., Singh, A., Singhal, A., Sintes, A. M., Slagmolen, B. J. J., Slaven-Blair, T. J., Smith, B., Smith, J. R., Smith, R. J. E., Somala, S., Son, E. J., Sorazu, B., Sorrentino, F., Souradeep, T., Spencer, A. P., Srivastava, A. K., Staats, K., Steinke, M., Steinlechner, J., Steinlechner, S., Steinmeyer, D., Steltner, B., Stevenson, S. P., Stocks, D., Stone, R., Stops, D. J., Strain, K. A., Stratta, G., Strigin, S. E., Strunk, A., Sturani, R., Stuver, A. L., Summerscales, T. Z., Sun, L., Sunil, S., Suresh, J., Sutton, P. J., Swinkels, B. L., Szczepa'nczyk, M. J., Tacca, M., Tait, S. C., Talbot, C., Talukder, D., Tanner, D. B., T'apai, M., Taracchini, A., Tasson, J. D., Taylor, J. A., Taylor, R., Tewari, S. V., Theeg, T., Thies, F., Thomas, E. G., Thomas, M., Thomas, P., Thorne, K. A., Thrane, E., Tiwari, S., Tiwari, V., Tokmakov, K. V., Toland, K., Tonelli, M., Tornasi, Z., e, A. Torres-Forn', Torrie, C. I., a, D. Töyr\", Travasso, F., Traylor, G., Trinastic, J., Tringali, M. C., Trozzo, L., Tsang, K. W., Tse, M., Tso, R., Tsuna, D., Tsukada, L., Tuyenbayev, D., Ueno, K., Ugolini, D., Urban, A. L., Usman, S. A., Vahlbruch, H., Vajente, G., Valdes, G., van Bakel, N., van Beuzekom, M., Brand, J. F. J. van den, Broeck, C. Van Den, Vander-Hyde, D. C., van der Schaaf, L., van Heijningen, J. V., van Veggel, A. A., Vardaro, M., Varma, V., Vass, S., Vas'uth, M., Vecchio, A., Vedovato, G., Veitch, J., Veitch, P. J., Venkateswara, K., Venugopalan, G., Verkindt, D., Vetrano, F., e, A. Vicer', Viets, A. D., Vinciguerra, S., Vine, D. J., Vinet, J. -Y., Vitale, S., Vo, T., Vocca, H., Vorvick, C., Vyatchanin, S. P., Wade, A. R., Wade, L. E., Wade, M., Walet, R., Walker, M., Wallace, L., Walsh, S., Wang, G., Wang, H., Wang, J. Z., Wang, W. H., Wang, Y. F., Ward, R. L., Warner, J., Was, M., Watchi, J., Weaver, B., Wei, L. -W., Weinert, M., Weinstein, A. J., Weiss, R., Wellmann, F., Wen, L., Wessel, E. K., Weßels, P., Westerweck, J., Wette, K., Whelan, J. T., Whiting, B. F., Whittle, C., Wilken, D., Williams, D., Williams, R. D., Williamson, A. R., Willis, J. L., Willke, B., Wimmer, M. H., Winkler, W., Wipf, C. C., Wittel, H., Woan, G., Woehler, J., Wofford, J. K., Wong, W. K., Worden, J., Wright, J. L., Wu, D. S., Wysocki, D. M., Xiao, S., Yam, W., Yamamoto, H., Yancey, C. C., Yang, L., Yap, M. J., Yazback, M., Yu, Hang, Yu, Haocun, Yvert, M., zny, A. Zadro., Zanolin, M., Zelenova, T., Zendri, J. -P., Zevin, M., Zhang, J., Zhang, L., Zhang, M., Zhang, T., Zhang, Y. -H., Zhao, C., Zhou, M., Zhou, Z., Zhu, S. J., Zhu, X. J., Zucker, M. E., and Zweizig, J.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present a search for prompt gamma-ray counterparts to compact binary coalescence gravitational wave (GW) candidates from Advanced LIGO's first observing run (O1). As demonstrated by the multimessenger observations of GW170817/GRB 170817A, electromagnetic and GW observations provide complementary information about the astrophysical source and, in the case of weaker candidates, may strengthen the case for an astrophysical origin. Here we investigate low-significance GW candidates from the O1 compact-binary coalescence searches using the Fermi Gamma-ray Burst Monitor (GBM), leveraging its all-sky and broad energy coverage. Candidates are ranked and compared to background to measure significance. Those with false alarm rates of less than 10^-5 Hz (about one per day) are used as the search sample for gamma-ray follow-up. No GW candidates were found to be coincident with gamma-ray transients independently identified by blind searches of the GBM data. In addition, GW candidate event times were followed up by a separate targeted search of GBM data. Among the resulting GBM events, the two with lowest false alarm rates were the gamma-ray transient GW150914-GBM presented in Connaughton et al. (2016) and a solar flare in chance coincidence with a GW candidate., Comment: Published in ApJ
Published: 2018
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3. On the interpretation of the Fermi GBM transient observed in coincidence with LIGO Gravitational Wave Event GW150914

Author: Connaughton, V., Burns, E., Goldstein, A., Blackburn, L., Briggs, M. S., Christensen, N., Hui, C. M., Kocevski, D., Littenberg, T., McEnery, J. E., Racusin, J., Shawhan, P., Veitch, J., Wilson-Hodge, C. A., Bhat, P. N., Bissaldi, E., Cleveland, W., Giles, M. M., Gibby, M. H., von Kienlin, A., Kippen, R. M., McBreen, S., Meegan, C. A., Paciesas, W. S., Preece, R. D., Roberts, O. J., Stanbro, M., and Veres, P.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: The weak transient detected by the Fermi Gamma-ray Burst Monitor (GBM) 0.4 s after GW150914 has generated much speculation regarding its possible association with the black-hole binary merger. Investigation of the GBM data by Connaughton et al. (2016) revealed a source location consistent with GW150914 and a spectrum consistent with a weak, short Gamma-Ray Burst. Greiner et al. (2016) present an alternative technique for fitting background-limited data in the low-count regime, and call into question the spectral analysis and the significance of the detection of GW150914-GBM presented in Connaughton et al. (2016). The spectral analysis of Connaughton et al. (2016) is not subject to the limitations of the low-count regime noted by Greiner et al. (2016). We find Greiner et al. (2016) used an inconsistent source position and did not follow the steps taken in Connaughton et al. (2016) to mitigate the statistical shortcomings of their software when analyzing this weak event. We use the approach of Greiner et al. (2016) to verify that our original spectral analysis is not biased. The detection significance of GW150914-GBM is established empirically, with a False Alarm Rate (FAR) of $\sim 10^{-4}$~Hz. A post-trials False Alarm Probability (FAP) of $2.2 \times 10^{-3}$ ($2.9 \sigma$) of this transient being associated with GW150914 is based on the proximity in time to the GW event of a transient with that FAR. The FAR and the FAP are unaffected by the spectral analysis that is the focus of Greiner et al. (2016)., Comment: Accepted for publication in ApJL
Published: 2018
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4. An Ordinary Short Gamma-Ray Burst with Extraordinary Implications: Fermi-GBM Detection of GRB 170817A

Author: Goldstein, A., Veres, P., Burns, E., Briggs, M. S., Hamburg, R., Kocevski, D., Wilson-Hodge, C. A., Preece, R. D., Poolakkil, S., Roberts, O. J., Hui, C. M., Connaughton, V., Racusin, J., von Kienlin, A., Canton, T. Dal, Christensen, N., Littenberg, T. B., Siellez, K., Blackburn, L., Broida, J., Bissaldi, E., Cleveland, W. H., Gibby, M. H., Giles, M. M., Kippen, R. M., McBreen, S., McEnery, J., Meegan, C. A., Paciesas, W. S., and Stanbro, M.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: On August 17, 2017 at 12:41:06 UTC the Fermi Gamma-ray Burst Monitor (GBM) detected and triggered on the short gamma-ray burst GRB 170817A. Approximately 1.7 s prior to this GRB, the Laser Interferometer Gravitational-Wave Observatory (LIGO) triggered on a binary compact merger candidate associated with the GRB. This is the first unambiguous coincident observation of gravitational waves and electromagnetic radiation from a single astrophysical source and marks the start of gravitational-wave multi-messenger astronomy. We report the GBM observations and analysis of this ordinary short GRB, which extraordinarily confirms that at least some short GRBs are produced by binary compact mergers., Comment: Published in Astrophysical Journal Letters
Published: 2017
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5. Searching the Gamma-ray Sky for Counterparts to Gravitational Wave Sources: Fermi GBM and LAT Observations of LVT151012 and GW151226

Author: Racusin, J. L., Burns, E., Goldstein, A., Connaughton, V., Wilson-Hodge, C. A., Jenke, P., Blackburn, L., Briggs, M. S., Broida, J., Camp, J., Christensen, N., Hui, C. M., Littenberg, T., Shawhan, P., Singer, L., Veitch, J., Bhat, P. N., Cleveland, W., Fitzpatrick, G., Gibby, M. H., von Kienlin, A., McBreen, S., Mailyan, B., Meegan, C. A., Paciesas, W. S., Preece, R. D., Roberts, O. J., Stanbro, M., Veres, P., Zhang, B. -B., Ackermann, M., Albert, A., Atwood, W. B., Axelsson, M., Baldini, L., Ballet, J., Barbiellini, G., Baring, M. G., Bastieri, D., Bellazzini, R., Bissaldi, E., Blandford, R. D., Bloom, E. D., Bonino, R., Bregeon, J., Bruel, P., Buson, S., Caliandro, G. A., Cameron, R. A., Caputo, R., Caragiulo, M., Caraveo, P. A., Cavazzuti, E., Charles, E., Chiang, J., Ciprini, S., Costanza, F., Cuoco, A., Cutini, S., D'Ammando, F., de Palma, F., Desiante, R., Digel, S. W., Di Lalla, N., Di Mauro, M., Di Venere, L., Drell, P. S., Favuzzi, C., Ferrara, E. C., Focke, W. B., Fukazawa, Y., Funk, S., Fusco, P., Gargano, F., Gasparrini, D., Giglietto, N., Gill, R., Giroletti, M., Glanzman, T., Granot, J., Green, D., Grove, J. E., Guillemot, L., Guiriec, S., Harding, A. K., Jogler, T., Johannesson, G., Kamae, T., Kensei, S., Kocevski, D., Kuss, M., Larsson, S., Latronico, L., Li, J., Longo, F., Loparco, F., Lubrano, P., Magill, J. D., Maldera, S., Malyshev, D., McEnery, J. E., Michelson, P. F., Mizuno, T., Morselli, A., Moskalenko, I. V., Negro, M., Nuss, E., Omodei, N., Orienti, M., Orlando, E., Ormes, J. F., Paneque, D., Perkins, J. S., Pesce-Rollins, M., Piron, F., Pivato, G., Porter, T. A., Principe, G., Raino, S., Rando, R., Razzano, M., Razzaque, S., Reimer, A., Reimer, O., Parkinson, P. M. Saz, Scargle, J. D., Sgro, C., Simone, D., Siskind, E. J., Smith, D. A., Spada, F., Spinelli, P., Suson, D. J., Tajima, H., Thayer, J. B., Torres, D. F., Troja, E., Uchiyama, Y., Vianello, G., Wood, K. S., and Wood, M.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present the Fermi Gamma-ray Burst Monitor (GBM) and Large Area Telescope (LAT) observations of the LIGO binary black hole merger event GW151226 and candi- date LVT151012. No candidate electromagnetic counterparts were detected by either the GBM or LAT. We present a detailed analysis of the GBM and LAT data over a range of timescales from seconds to years, using automated pipelines and new techniques for char- acterizing the upper limits across a large area of the sky. Due to the partial GBM and LAT coverage of the large LIGO localization regions at the trigger times for both events, dif- ferences in source distances and masses, as well as the uncertain degree to which emission from these sources could be beamed, these non-detections cannot be used to constrain the variety of theoretical models recently applied to explain the candidate GBM counterpart to GW150914., Comment: 27 pages, 1 table, 11 figures, Submitted to ApJ
Published: 2016
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6. Supplement: Localization and broadband follow-up of the gravitational-wave transient GW150914

Author: Abbott, B. P., Abbott, R., Abbott, T. D., Abernathy, M. R., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R. X., Adya, V. B., Affeldt, C., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, B., Allocca, A., Altin, P. A., Anderson, S. B., Anderson, W. G., Arai, K., Araya, M. C., Arceneaux, C. C., Areeda, J. S., Arnaud, N., Arun, K. G., Ascenzi, S., Ashton, G., Ast, M., Aston, S. M., Astone, P., Aufmuth, P., Aulbert, C., Babak, S., Bacon, P., Bader, M. K. M., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Barthelmy, S., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Batch, J. C., Baune, C., Bavigadda, V., Bazzan, M., Behnke, B., Bejger, M., Bell, A. S., Bell, C. J., Berger, B. K., Bergman, J., Bergmann, G., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhagwat, S., Bhandare, R., Bilenko, I. A., Billingsley, G., Birch, J., Birney, R., Biscans, S., Bisht, A., Bitossi, M., Biwer, C., Bizouard, M. A., Blackburn, J. K., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bock, O., Bodiya, T. P., Boer, M., Bogaert, G., Bogan, C., Bohe, A., Bojtos, P., Bond, C., Bondu, F., Bonnand, R., Boom, B. A., Bork, R., Boschi, V., Bose, S., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Braginsky, V. B., Branchesi, M., Brau, J. E., Briant, T., Brillet, A., Brinkmann, M., Brisson, V., Brockill, P., Brooks, A. F., Brown, D. A., Brown, D. D., Brown, N. M., Buchanan, C. C., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. L., Cadonati, L., Cagnoli, G., Cahillane, C., Bustillo, J. C., Callister, T., Calloni, E., Camp, J. B., Cannon, K. C., Cao, J., Capano, C. D., Capocasa, E., Carbognani, F., Caride, S., Diaz, J. C., Casentini, C., Caudill, S., Cavaglià, M., Cavalier, F., Cavalieri, R., Cella, G., Cepeda, C. B., Baiardi, L. C., Cerretani, G., Cesarini, E., Chakraborty, R., Chalermsongsak, T., Chamberlin, S. J., Chan, M., Chao, S., Charlton, P., Chassande-Mottin, E., Chen, H. Y., Chen, Y., Cheng, C., Chincarini, A., Chiummo, A., Cho, H. S., Cho, M., Chow, J. H., Christensen, N., Chu, Q., Chua, S., Chung, S., Ciani, G., Clara, F., Clark, J. A., Cleva, F., Coccia, E., Cohadon, P. -F., Colla, A., Collette, C. G., Cominsky, L., Constancio Jr., M., Conte, A., Conti, L., Cook, D., Corbitt, T. R., Cornish, N., Corsi, A., Cortese, S., Costa, C. A., Coughlin, M. W., Coughlin, S. B., Coulon, J. -P., Countryman, S. T., Couvares, P., Cowan, E. E., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Craig, K., Creighton, J. D. E., Cripe, J., Crowder, S. G., Cumming, A., Cunningham, L., Cuoco, E., Canton, T. Dal, Danilishin, S. L., D'Antonio, S., Danzmann, K., Darman, N. S., Dattilo, V., Dave, I., Daveloza, H. P., Davier, M., Davies, G. S., Daw, E. J., Day, R., DeBra, D., Debreczeni, G., Degallaix, J., De Laurentis, M., Deléglise, S., Del Pozzo, W., Denker, T., Dent, T., Dereli, H., Dergachev, V., DeRosa, R. T., De Rosa, R., DeSalvo, R., Dhurandhar, S., Díaz, M. C., Di Fiore, L., Di Giovanni, M., Di Lieto, A., Di Pace, S., Di Palma, I., Di Virgilio, A., Dojcinoski, G., Dolique, V., Donovan, F., Dooley, K. L., Doravari, S., Douglas, R., Downes, T. P., Drago, M., Drever, R. W. P., Driggers, J. C., Du, Z., Ducrot, M., Dwyer, S. E., Edo, T. B., Edwards, M. C., Effler, A., Eggenstein, H. -B., Ehrens, P., Eichholz, J., Eikenberry, S. S., Engels, W., Essick, R. C., Etzel, T., Evans, M., Evans, T. M., Everett, R., Factourovich, M., Fafone, V., Fair, H., Fairhurst, S., Fan, X., Fang, Q., Farinon, S., Farr, B., Farr, W. M., Favata, M., Fays, M., Fehrmann, H., Fejer, M. M., Ferrante, I., Ferreira, E. C., Ferrini, F., Fidecaro, F., Fiori, I., Fiorucci, D., Fisher, R. P., Flaminio, R., Fletcher, M., Fournier, J. -D., Franco, S., Frasca, S., Frasconi, F., Frei, Z., Freise, A., Frey, R., Frey, V., Fricke, T. T., Fritschel, P., Frolov, V. V., Fulda, P., Fyffe, M., Gabbard, H. A. G., Gair, J. R., Gammaitoni, L., Gaonkar, S. G., Garufi, F., Gatto, A., Gaur, G., Gehrels, N., Gemme, G., Gendre, B., Genin, E., Gennai, A., George, J., Gergely, L., Germain, V., Ghosh, A., Ghosh, S., Giaime, J. A., Giardina, K. D., Giazotto, A., Gill, K., Glaefke, A., Goetz, E., Goetz, R., Gondan, L., González, G., Castro, J. M. G., Gopakumar, A., Gordon, N. A., Gorodetsky, M. L., Gossan, S. E., Gosselin, M., Gouaty, R., Graef, C., Graff, P. B., Granata, M., Grant, A., Gras, S., Gray, C., Greco, G., Green, A. C., Groot, P., Grote, H., Grunewald, S., Guidi, G. M., Guo, X., Gupta, A., Gupta, M. K., Gushwa, K. E., Gustafson, E. K., Gustafson, R., Hacker, J. J., Hall, B. R., Hall, E. D., Hammond, G., Haney, M., Hanke, M. M., Hanks, J., Hanna, C., Hannam, M. D., Hanson, J., Hardwick, T., Haris, K., Harms, J., Harry, G. M., Harry, I. W., Hart, M. J., Hartman, M. T., Haster, C. -J., Haughian, K., Heidmann, A., Heintze, M. C., Heitmann, H., Hello, P., Hemming, G., Hendry, M., Heng, I. S., Hennig, J., Heptonstall, A. W., Heurs, M., Hild, S., Hoak, D., Hodge, K. A., Hofman, D., Hollitt, S. E., Holt, K., Holz, D. E., Hopkins, P., Hosken, D. J., Hough, J., Houston, E. A., Howell, E. J., Hu, Y. M., Huang, S., Huerta, E. A., Huet, D., Hughey, B., Husa, S., Huttner, S. H., Huynh-Dinh, T., Idrisy, A., Indik, N., Ingram, D. R., Inta, R., Isa, H. N., Isac, J. -M., Isi, M., Islas, G., Isogai, T., Iyer, B. R., Izumi, K., Jacqmin, T., Jang, H., Jani, K., Jaranowski, P., Jawahar, S., Jiménez-Forteza, F., Johnson, W. W., Jones, D. I., Jones, R., Jonker, R. J. G., Ju, L., Kalaghatgi, C. V., Kalogera, V., Kandhasamy, S., Kang, G., Kanner, J. 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S., Radkins, H., Raffai, P., Raja, S., Rakhmanov, M., Rapagnani, P., Raymond, V., Razzano, M., Re, V., Read, J., Reed, C. M., Regimbau, T., Rei, L., Reid, S., Reitze, D. H., Rew, H., Reyes, S. D., Ricci, F., Riles, K., Robertson, N. A., Robie, R., Robinet, F., Rocchi, A., Rolland, L., Rollins, J. G., Roma, V. J., Romano, R., Romanov, G., Romie, J. H., Rosińska, D., Rowan, S., Rüdiger, A., Ruggi, P., Ryan, K., Sachdev, S., Sadecki, T., Sadeghian, L., Salconi, L., Saleem, M., Salemi, F., Samajdar, A., Sammut, L., Sanchez, E. J., Sandberg, V., Sandeen, B., Sanders, J. R., Sassolas, B., Sathyaprakash, B. S., Saulson, P. R., Sauter, O., Savage, R. L., Sawadsky, A., Schale, P., Schilling, R., Schmidt, J., Schmidt, P., Schnabel, R., Schofield, R. M. S., Schönbeck, A., Schreiber, E., Schuette, D., Schutz, B. F., Scott, J., Scott, S. M., Sellers, D., Sentenac, D., Sequino, V., Sergeev, A., Serna, G., Setyawati, Y., Sevigny, A., Shaddock, D. A., Shah, S., Shahriar, M. 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Subjects: Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology
Abstract: This Supplement provides supporting material for arXiv:1602.08492 . We briefly summarize past electromagnetic (EM) follow-up efforts as well as the organization and policy of the current EM follow-up program. We compare the four probability sky maps produced for the gravitational-wave transient GW150914, and provide additional details of the EM follow-up observations that were performed in the different bands., Comment: For the main Letter, see arXiv:1602.08492
Published: 2016
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7. Localization and broadband follow-up of the gravitational-wave transient GW150914

Author: Abbott, B. P., Abbott, R., Abbott, T. D., Abernathy, M. R., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R. X., Adya, V. B., Affeldt, C., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, B., Allocca, A., Altin, P. A., Anderson, S. B., Anderson, W. G., Arai, K., Araya, M. C., Arceneaux, C. C., Areeda, J. S., Arnaud, N., Arun, K. G., Ascenzi, S., Ashton, G., Ast, M., Aston, S. M., Astone, P., Aufmuth, P., Aulbert, C., Babak, S., Bacon, P., Bader, M. K. M., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Barthelmy, S., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Batch, J. C., Baune, C., Bavigadda, V., Bazzan, M., Behnke, B., Bejger, M., Bell, A. S., Bell, C. J., Berger, B. K., Bergman, J., Bergmann, G., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhagwat, S., Bhandare, R., Bilenko, I. A., Billingsley, G., Birch, J., Birney, R., Biscans, S., Bisht, A., Bitossi, M., Biwer, C., Bizouard, M. A., Blackburn, J. K., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bock, O., Bodiya, T. P., Boer, M., Bogaert, G., Bogan, C., Bohe, A., Bojtos, P., Bond, C., Bondu, F., Bonnand, R., Boom, B. A., Bork, R., Boschi, V., Bose, S., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Braginsky, V. B., Branchesi, M., Brau, J. E., Briant, T., Brillet, A., Brinkmann, M., Brisson, V., Brockill, P., Brooks, A. F., Brown, D. A., Brown, D. D., Brown, N. M., Buchanan, C. C., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. L., Cadonati, L., Cagnoli, G., Cahillane, C., Bustillo, J. C., Callister, T., Calloni, E., Camp, J. B., Cannon, K. C., Cao, J., Capano, C. D., Capocasa, E., Carbognani, F., Caride, S., Diaz, J. C., Casentini, C., Caudill, S., Cavaglià, M., Cavalier, F., Cavalieri, R., Cella, G., Cepeda, C. B., Baiardi, L. C., Cerretani, G., Cesarini, E., Chakraborty, R., Chalermsongsak, T., Chamberlin, S. J., Chan, M., Chao, S., Charlton, P., Chassande-Mottin, E., Chen, H. Y., Chen, Y., Cheng, C., Chincarini, A., Chiummo, A., Cho, H. S., Cho, M., Chow, J. H., Christensen, N., Chu, Q., Chua, S., Chung, S., Ciani, G., Clara, F., Clark, J. A., Cleva, F., Coccia, E., Cohadon, P. -F., Colla, A., Collette, C. G., Cominsky, L., Constancio Jr., M., Conte, A., Conti, L., Cook, D., Corbitt, T. R., Cornish, N., Corsi, A., Cortese, S., Costa, C. A., Coughlin, M. W., Coughlin, S. B., Coulon, J. -P., Countryman, S. T., Couvares, P., Cowan, E. E., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Craig, K., Creighton, J. D. E., Cripe, J., Crowder, S. G., Cumming, A., Cunningham, L., Cuoco, E., Canton, T. Dal, Danilishin, S. L., D'Antonio, S., Danzmann, K., Darman, N. 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Subjects: Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology
Abstract: A gravitational-wave (GW) transient was identified in data recorded by the Advanced Laser Interferometer Gravitational-wave Observatory (LIGO) detectors on 2015 September 14. The event, initially designated G184098 and later given the name GW150914, is described in detail elsewhere. By prior arrangement, preliminary estimates of the time, significance, and sky location of the event were shared with 63 teams of observers covering radio, optical, near-infrared, X-ray, and gamma-ray wavelengths with ground- and space-based facilities. In this Letter we describe the low-latency analysis of the GW data and present the sky localization of the first observed compact binary merger. We summarize the follow-up observations reported by 25 teams via private Gamma-ray Coordinates Network circulars, giving an overview of the participating facilities, the GW sky localization coverage, the timeline and depth of the observations. As this event turned out to be a binary black hole merger, there is little expectation of a detectable electromagnetic (EM) signature. Nevertheless, this first broadband campaign to search for a counterpart of an Advanced LIGO source represents a milestone and highlights the broad capabilities of the transient astronomy community and the observing strategies that have been developed to pursue neutron star binary merger events. Detailed investigations of the EM data and results of the EM follow-up campaign are being disseminated in papers by the individual teams., Comment: For Supplement, see https://arxiv.org/abs/1604.07864
Published: 2016
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8. Fermi GBM Observations of LIGO Gravitational Wave event GW150914

Author: Connaughton, V., Burns, E., Goldstein, A., Blackburn, L., Briggs, M. S., Zhang, B. -B., Camp, J., Christensen, N., Hui, C. M., Jenke, P., Littenberg, T., McEnery, J. E., Racusin, J., Shawhan, P., Singer, L., Veitch, J., Wilson-Hodge, C. A., Bhat, P. N., Bissaldi, E., Cleveland, W., Fitzpatrick, G., Giles, M. M., Gibby, M. H., von Kienlin, A., Kippen, R. M., McBreen, S., Mailyan, B., Meegan, C. A., Paciesas, W. S., Preece, R. D., Roberts, O., Sparke, L., Stanbro, M., Toelge, K., and Veres, P.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: With an instantaneous view of 70% of the sky, the Fermi Gamma-ray Burst Monitor (GBM) is an excellent partner in the search for electromagnetic counterparts to gravitational wave (GW) events. GBM observations at the time of the Laser Interferometer Gravitational-wave Observatory (LIGO) event GW150914 reveal the presence of a weak transient above 50 keV, 0.4~s after the GW event, with a false alarm probability of 0.0022 (2.9$\sigma$). This weak transient lasting 1 s was not detected by any other instrument and does not appear connected with other previously known astrophysical, solar, terrestrial, or magnetospheric activity. Its localization is ill-constrained but consistent with the direction of GW150914. The duration and spectrum of the transient event are consistent with a weak short Gamma-Ray Burst arriving at a large angle to the direction in which Fermi was pointing, where the GBM detector response is not optimal. If the GBM transient is associated with GW150914, this electromagnetic signal from a stellar mass black hole binary merger is unexpected. We calculate a luminosity in hard X-ray emission between 1~keV and 10~MeV of $1.8^{+1.5}_{-1.0} \times 10^{49}$~erg~s$^{-1}$. Future joint observations of GW events by LIGO/Virgo and Fermi GBM could reveal whether the weak transient reported here is a plausible counterpart to GW150914 or a chance coincidence, and will further probe the connection between compact binary mergers and short Gamma-Ray Bursts., Comment: Accepted for publication in ApJL
Published: 2016
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9. Localization of Gamma-Ray Bursts using the Fermi Gamma-Ray Burst Monitor

Author: Connaughton, V., Briggs, M. S., Goldstein, A., Meegan, C. A., Paciesas, W. S., Preece, R. D., Wilson-Hodge, C. A., Gibby, M. H., Greiner, J., Gruber, D., Jenke, P., Kippen, R. M., Pelassa, V., Xiong, S., Yu, H. -F., Bhat, P. N., Burgess, J. M., Byrne, D., Fitzpatrick, G., Foley, S., Giles, M. M., Guiriec, S., van der Horst, A. J., von Kienlin, A., McBreen, S., McGlynn, S., Tierney, D., and Zhang, B. -B.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: The Fermi Gamma-ray Burst Monitor (GBM) has detected over 1400 Gamma-Ray Bursts (GRBs) since it began science operations in July, 2008. We use a subset of over 300 GRBs localized by instruments such as Swift, the Fermi Large Area Telescope, INTEGRAL, and MAXI, or through triangulations from the InterPlanetary Network (IPN), to analyze the accuracy of GBM GRB localizations. We find that the reported statistical uncertainties on GBM localizations, which can be as small as 1 degree, underestimate the distance of the GBM positions to the true GRB locations and we attribute this to systematic uncertainties. The distribution of systematic uncertainties is well represented (68% confidence level) by a 3.7 degree Gaussian with a non-Gaussian tail that contains about 10% of GBM-detected GRBs and extends to approximately 14 degrees. A more complex model suggests that there is a dependence of the systematic uncertainty on the position of the GRB in spacecraft coordinates, with GRBs in the quadrants on the Y-axis better localized than those on the X-axis., Comment: accepted for publication in the Astrophysical Journal Supplement Series
Published: 2014
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10. 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., Fukazawa, Y., 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., Hanabata, Y., Harding, A. K., Hayashida, M., Iyyani, S., Jogler, T., Jóannesson, G., Kawano, T., Knödlseder, 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., Mizuno, T., Monzani, M. E., 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, J. S., Pesce-Rollins, M., Piron, F., Pivato, G., Porter, T. A., Racusin, J. L., Rainò, S., Rando, R., Razzano, M., Razzaque, S., Reimer, A., Reimer, O., Ritz, S., Roth, M., Ryde, F., Sartori, A., Scargle, J. D., Schulz, A., Sgrò, C., Siskind, E. J., Spandre, G., Spinelli, P., Suson, D. J., Tajima, H., Takahashi, H., Thayer, J. G., Thayer, J. B., Tibaldo, L., Tinivella, M., Torres, D. F., Tosti, G., Troja, E., Usher, T. L., Vandenbroucke, J., Vasileiou, V., Vianello, G., Vitale, V., Werner, M., Winer, B. L., Wood, K. S., and Zhu, S.
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 s 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., Comment: This is the author's version of the work. It is posted here by permission of the AAAS for personal use, not for redistribution. The definitive version was published online in Science Express on 21 November 2013 [DOI:10.1126/science.1242302] 15 pages, 4 figures and 1 table; includes supplementary online materials
Published: 2013
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11. Time-resolved Analysis of Fermi GRBs with Fast and Slow-Cooled Synchrotron Photon Models

Author: Burgess, J. M., Preece, R. D., Connaughton, V., Briggs, M. S., Goldstein, A., Bhat, P. N., Greiner, J., Gruber, D., Kienlin, A., Kouveliotou, C., McGlynn, S., Meegan, C. A., Paciesas, W. S., Rau, A., Xiong, S., Axelsson, M., Baring, M. G., Dermer, C. D., Iyyani, S., Kocevski, D., Omodei, N., Ryde, F., and Vianello, G.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Time-resolved spectroscopy is performed on eight bright, long gamma-ray bursts (GRBs) dominated by single emission pulses that were observed with the {\it Fermi Gamma-ray Space Telescope}. Fitting the prompt radiation of GRBs by empirical spectral forms such as the Band function leads to ambiguous conclusions about the physical model for the prompt radiation. Moreover, the Band function is often inadequate to fit the data. The GRB spectrum is therefore modeled with two emission components consisting of optically thin nonthermal synchrotron radiation from relativistic electrons and, when significant, thermal emission from a jet photosphere, which is represented by a blackbody spectrum. To produce an acceptable fit, the addition of a blackbody component is required in 5 out of the 8 cases. We also find that the low-energy spectral index \alpha is consistent with a synchrotron component with \alpha = -0.81\pm 0.1. This value lies between the limiting values of \alpha = -2/3 and \alpha = -3/2 for electrons in the slow and fast-cooling regimes, respectively, suggesting ongoing acceleration at the emission site. The blackbody component can be more significant when using a physical synchrotron model instead of the Band function, illustrating that the Band function does not serve as a good proxy for a nonthermal synchrotron emission component. The temperature and characteristic emission-region size of the blackbody component are found to, respectively, decrease and increase as power laws with time during the prompt phase. In addition, we find that the blackbody and nonthermal components have separate temporal behaviors.
Published: 2013
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12. IPN localizations of Konus short gamma-ray bursts

Author: Pal'shin, V. D., Hurley, K., Svinkin, D. S., Aptekar, R. L., Golenetskii, S. V., Frederiks, D. D., Mazets, E. P., Oleynik, P. P., Ulanov, M. V., Cline, T., Mitrofanov, I. G., Golovin, D. V., Kozyrev, A. S., Litvak, M. L., Sanin, A. B., Boynton, W., Fellows, C., Harshman, K., Trombka, J., McClanahan, T., Starr, R., Goldsten, J., Gold, R., Rau, A., von Kienlin, A., Savchenko, V., Smith, D. M., Hajdas, W., Barthelmy, S. D., Cummings, J., Gehrels, N., Krimm, H., Palmer, D., Yamaoka, K., Ohno, M., Fukazawa, Y., Hanabata, Y., Takahashi, T., Tashiro, M., Terada, Y., Murakami, T., Makishima, K., Briggs, M. S., Kippen, R. M., Kouveliotou, C., Meegan, C., Fishman, G., Connaughton, V., Boer, M., Guidorzi, C., Frontera, F., Montanari, E., Rossi, F., Feroci, M., Amati, L., Nicastro, L., Orlandini, M., Del Monte, E., Costa, E., Donnarumma, I., Evangelista, Y., Lapshov, I., Lazzarotto, F., Pacciani, L., Rapisarda, M., Soffitta, P., Di Cocco, G., Fuschino, F., Galli, M., Labanti, C., Marisaldi, M., Atteia, J. -L., Vanderspek, R., and Ricker, G.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Between the launch of the \textit{GGS Wind} spacecraft in 1994 November and the end of 2010, the Konus-\textit{Wind} experiment detected 296 short-duration gamma-ray bursts (including 23 bursts which can be classified as short bursts with extended emission). During this period, the IPN consisted of up to eleven spacecraft, and using triangulation, the localizations of 271 bursts were obtained. We present the most comprehensive IPN localization data on these events. The short burst detection rate, $\sim$18 per year, exceeds that of many individual experiments., Comment: Published version
Published: 2013
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13. The Interplanetary Network Supplement to the Fermi GBM Catalog of Cosmic Gamma-Ray Bursts

Author: Hurley, K., Pal'shin, V. D., Aptekar, R. L., Golenetskii, S. V., Frederiks, D. D., Mazets, E. P., Svinkin, D. S., Briggs, M. S., Connaughton, V., Meegan, C., Goldsten, J., Boynton, W., Fellows, C., Harshman, K., Mitrofanov, I. G., Golovin, D. V., Kozyrev, A. S., Litvak, M. L., Sanin, A. B., Rau, A., von Kienlin, A., Zhang, X., Yamaoka, K., Fukazawa, Y., Hanabata, Y., Ohno, M., Takahashi, T., Tashiro, M., Terada, Y., Murakami, T., Makishima, K., Barthelmy, S., Cline, T., Gehrels, N., Cummings, J., Krimm, H. A., Smith, D. M., Del Monte, E., Feroci, M., and Marisaldi, M.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present Interplanetary Network (IPN) data for the gamma-ray bursts in the first Fermi Gamma-Ray Burst Monitor (GBM) catalog. Of the 491 bursts in that catalog, covering 2008 July 12 to 2010 July 11, 427 were observed by at least one other instrument in the 9-spacecraft IPN. Of the 427, the localizations of 149 could be improved by arrival time analysis (or triangulation). For any given burst observed by the GBM and one other distant spacecraft, triangulation gives an annulus of possible arrival directions whose half-width varies between about 0.4' and 32 degrees, depending on the intensity, time history, and arrival direction of the burst, as well as the distance between the spacecraft. We find that the IPN localizations intersect the 1 sigma GBM error circles in only 52% of the cases, if no systematic uncertainty is assumed for the latter. If a 6 degree systematic uncertainty is assumed and added in quadrature, the two localization samples agree about 87% of the time, as would be expected. If we then multiply the resulting error radii by a factor of 3, the two samples agree in slightly over 98% of the cases, providing a good estimate of the GBM 3 sigma error radius. The IPN 3 sigma error boxes have areas between about 1 square arcminute and 110 square degrees, and are, on the average, a factor of 180 smaller than the corresponding GBM localizations. We identify two bursts in the IPN/GBM sample that did not appear in the GBM catalog. In one case, the GBM triggered on a terrestrial gamma flash, and in the other, its origin was given as uncertain. We also discuss the sensitivity and calibration of the IPN., Comment: 52 pages, 12 figures, 4 tables. Revised version, resubmitted to the Astrophysical Journal Supplement Series following refereeing. Figures of the localizations in Table 3 may be found on the IPN website, at ssl.berkeley.edu/ipn3/YYMMDD, where YY, MM, and DD are the year, month, and day of the burst, sometimes with suffixes A or B
Published: 2013
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14. 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., and Wijers, R. A. M. J.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
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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15. THE INTERPLANETARY NETWORK

Author: Hurley, K., primary, Mitrofanov, I. G., additional, Golovin, D., additional, Litvak, M. L., additional, Sanin, A. B., additional, Boynton, W., additional, Fellows, C., additional, Harshman, K., additional, Starr, R., additional, Golenetskii, S., additional, Aptekar, R., additional, Mazets, E., additional, Palshin, V., additional, Frederiks, D., additional, Svinkin, D., additional, Smith, D. M., additional, Hajdas, W., additional, Kienlin, A. von, additional, Zhang, X., additional, Rau, A., additional, Yamaoka, K., additional, Takahashi, T., additional, Ohno, M., additional, Hanabata, Y., additional, Fukazawa, Y., additional, Tashiro, M., additional, Terada, Y., additional, Murakami, T., additional, Makishima, K., additional, Cline, T., additional, Barthelmy, S., additional, Cummings, J., additional, Gehrels, N., additional, Krimm, H., additional, Palmer, D., additional, Goldsten, J., additional, Del Monte, E., additional, Feroci, M., additional, Marisaldi, M., additional, Connaughton, V., additional, Briggs, M. S., additional, and Meegan, C., additional
Published: 2020
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16. The Interplanetary Network Supplement to the Fermi GBM Catalog - An AO-2 and AO-3 Guest Investigator Project

Author: Hurley, K., Briggs, M., Connaughton, V., Meegan, C., von Kienlin, A., Rau, A., Zhang, X., Golenetskii, S., Aptekar, R., Mazets, E., Pal'shin, V., Frederiks, D., Barthelmy, S., Cline, T., Cummings, J., Gehrels, N., Krimm, H. A., Mitrofanov, I. G., Golovin, D., Litvak, M. L., Sanin, A. B., Boynton, W., Fellows, C., Harshman, K., Starr, R., Smith, D. M., Hajdas, W., Yamaoka, K., Ohno, M., Fukazawa, Y., Takahashi, T., Tashiro, M., Terada, Y., Murakami, T., Makishima, K., Palmer, D. M., Goldsten, J., Del Monte, E., Feroci, M., and Marisaldi, M.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: In the first two years of operation of the Fermi GBM, the 9-spacecraft Interplanetary Network (IPN) detected 158 GBM bursts with one or two distant spacecraft, and triangulated them to annuli or error boxes. Combining the IPN and GBM localizations leads to error boxes which are up to 4 orders of magnitude smaller than those of the GBM alone. These localizations comprise the IPN supplement to the GBM catalog, and they support a wide range of scientific investigations., Comment: 2011 Fermi Symposium proceedings - eConf C110509
Published: 2011

17. Quasi-Periodic Pulsations in Solar Flares: new clues from the Fermi Gamma-Ray Burst Monitor

Author: Gruber, D., Lachowicz, P., Bissaldi, E., Briggs, M. S., Connaughton, V., Greiner, J., van der Horst, A. J., Kanbach, G., Rau, A., Bhat, P. N., Diehl, R., von Kienlin, A., Kippen, R. M., Meegan, C. A., Paciesas, W. S., Preece, R. D., and Wilson-Hodge, C.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: In the last four decades it has been observed that solar flares show quasi-periodic pulsations (QPPs) from the lowest, i.e. radio, to the highest, i.e. gamma-ray, part of the electromagnetic spectrum. To this day, it is still unclear which mechanism creates such QPPs. In this paper, we analyze four bright solar flares which show compelling signatures of quasi-periodic behavior and were observed with the Gamma-Ray Burst Monitor (\gbm) onboard the Fermi satellite. Because GBM covers over 3 decades in energy (8 keV to 40 MeV) it can be a key instrument to understand the physical processes which drive solar flares. We tested for periodicity in the time series of the solar flares observed by GBM by applying a classical periodogram analysis. However, contrary to previous authors, we did not detrend the raw light curve before creating the power spectral density spectrum (PSD). To assess the significance of the frequencies we made use of a method which is commonly applied for X-ray binaries and Seyfert galaxies. This technique takes into account the underlying continuum of the PSD which for all of these sources has a P(f) ~ f^{-\alpha} dependence and is typically labeled red-noise. We checked the reliability of this technique by applying it to a solar flare which was observed by the Reuven Ramaty High-Energy Solar Spectroscopic Imager (RHESSI) which contains, besides any potential periodicity from the Sun, a 4 s rotational period due to the rotation of the spacecraft around its axis. While we do not find an intrinsic solar quasi-periodic pulsation we do reproduce the instrumental periodicity. Moreover, with the method adopted here, we do not detect significant QPPs in the four bright solar flares observed by GBM. We stress that for the purpose of such kind of analyses it is of uttermost importance to appropriately account for the red-noise component in the PSD of these astrophysical sources., Comment: accepted by A&A
Published: 2011
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18. Panchromatic Observations of SN 2011dh Point to a Compact Progenitor Star

Author: Soderberg, Alicia M., Margutti, R., Zauderer, B. A., Krauss, M., Katz, B., Chomiuk, L., Dittmann, J. A., Nakar, E., Sakamoto, T., Kawai, N., Hurley, K., Barthelmy, S., Toizumi, T., Morii, M., Chevalier, R. A., Gurwell, M., Petitpas, G., Rupen, M., Alexander, K. D., Levesque, E. M., Fransson, C., Brunthaler, A., Bietenholz, M. F., Chugai, N., Grindlay, J., Copete, A., Connaughton, V., Briggs, M., Meegan, C., von Kienlin, A., Zhang, X., Rau, A., Golenetskii, S., Mazets, E., and Cline, T.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We report the discovery and detailed monitoring of X-ray emission associated with the Type IIb SN 2011dh using data from the Swift and Chandra satellites, placing it among the best studied X-ray supernovae to date. We further present millimeter and radio data obtained with the SMA, CARMA, and EVLA during the first three weeks after explosion. Combining these observations with early optical photometry, we show that the panchromatic dataset is well-described by non-thermal synchrotron emission (radio/mm) with inverse Compton scattering (X-ray) of a thermal population of optical photons. In this scenario, the shock partition fractions deviate from equipartition by a factor, (e_e/e_B) ~ 30. We derive the properties of the shockwave and the circumstellar environment and find a shock velocity, v~0.1c, and a progenitor mass loss rate of ~6e-5 M_sun/yr. These properties are consistent with the sub-class of Type IIb SNe characterized by compact progenitors (Type cIIb) and dissimilar from those with extended progenitors (Type eIIb). Furthermore, we consider the early optical emission in the context of a cooling envelope model to estimate a progenitor radius of ~1e+11 cm, in line with the expectations for a Type cIIb SN. Together, these diagnostics are difficult to reconcile with the extended radius of the putative yellow supergiant progenitor star identified in archival HST observations, unless the stellar density profile is unusual. Finally, we searched for the high energy shock breakout pulse using X-ray and gamma-ray observations obtained during the purported explosion date range. Based on the compact radius of the progenitor, we estimate that the breakout pulse was detectable with current instruments but likely missed due to their limited temporal/spatial coverage. [Abridged], Comment: (27 pages, 5 figures, 2 tables, final version to appear in ApJ)
Published: 2011
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19. Rest-frame properties of 32 gamma-ray bursts observed by the Fermi Gamma-Ray Burst Monitor

Author: Gruber, D., Greiner, J., von Kienlin, A., Rau, A., Briggs, M. S., Connaughton, V., Goldstein, A., van der Horst, A. J., Nardini, M., Bhat, P. N., Bissaldi, E., Burgess, J. M., Chaplin, V. L., Diehl, R., Fishman, G. J., Fitzpatrick, G., Foley, S., Gibby, M. H., Giles, M. M., Guiriec, S., Kippen, R. M., Kouveliotou, C., Lin, L., McBreen, S., Meegan, C. A., E., F. Olivares, Paciesas, W. S., Preece, R. D., Tierney, D., and Wilson-Hodge, C.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Aims: In this paper we study the main spectral and temporal properties of gamma-ray bursts (GRBs) observed by Fermi/GBM. We investigate these key properties of GRBs in the rest-frame of the progenitor and test for possible intra-parameter correlations to better understand the intrinsic nature of these events. Methods: Our sample comprises 32 GRBs with measured redshift that were observed by GBM until August 2010. 28 of them belong to the long-duration population and 4 events were classified as short/hard bursts. For all of these events we derive, where possible, the intrinsic peak energy in the $\nu F_{\nu}$ spectrum (\eprest), the duration in the rest-frame, defined as the time in which 90% of the burst fluence was observed (\tninetyrest) and the isotropic equivalent bolometric energy (\eiso). Results: The distribution of \eprest has mean and median values of 1.1 MeV and 750 keV, respectively. A log-normal fit to the sample of long bursts peaks at ~800 keV. No high-\ep population is found but the distribution is biased against low \ep values. We find the lowest possible \ep that GBM can recover to be ~ 15 keV. The \tninetyrest distribution of long GRBs peaks at ~10 s. The distribution of \eiso has mean and median values of $8.9\times 10^{52}$ erg and $8.2 \times 10^{52}$ erg, respectively. We confirm the tight correlation between \eprest and \eiso (Amati relation) and the one between \eprest and the 1-s peak luminosity ($L_p$) (Yonetoku relation). Additionally, we observe a parameter reconstruction effect, i.e. the low-energy power law index $\alpha$ gets softer when \ep is located at the lower end of the detector energy range. Moreover, we do not find any significant cosmic evolution of neither \eprest nor \tninetyrest., Comment: accepted by A&A
Published: 2011
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20. Fermi/GBM observations of the ultra-long GRB 091024: A burst with an optical flash

Author: Gruber, D., Krühler, T., Foley, S., Nardini, M., Burlon, D., Rau, A., Bissaldi, E., von Kienlin, A., McBreen, S., Greiner, J., Bhat, P. N., Briggs, M. S., Burgess, J. M., Chaplin, V. L., Connaughton, V., Diehl, R., Fishman, G. J., Gibby, M. H., Giles, M. M., Goldstein, A., Guiriec, S., van der Horst, A. J., Kippen, R. M., Kouveliotou, C., Lin, L., Meegan, C. A., Paciesas, W. S., Preece, R. D., Tierney, D., and Wilson-Hodge, C.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: 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). 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. 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 ($\Gamma_{min}=195_{-110}^+{90}$)is consistent within the error to the one obtained using the peak time of the forward shock ($\Gamma_0=120$) and is also consistent with Lorentz factors of other long GRBs., Comment: accepted for publication in A&A
Published: 2011
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21. Integrating the Fermi Gamma-Ray Burst Monitor into the 3rd Interplanetary Network

Author: Hurley, K., Briggs, M., Connaughton, V., Meegan, C., Cline, T., Mitrofanov, I., Golovin, D., Litvak, M. L., Sanin, A. B., Boynton, W., Fellows, C., Harshman, K., Starr, R., Golenetskii, S., Aptekar, R., Mazets, E., Pal'shin, V., Frederiks, D., Smith, D. M., Wigger, C., Rau, A., von Kienlin, A., Yamaoka, K., Ohno, M., Fukazawa, Y., Takahashi, T., Tashiro, M., Terada, Y., Murakami, T., Makishima, K., Barthelmy, S., Cummings, J., Gehrels, N., Krimm, H., Goldsten, J., Del Monte, E., Feroci, M., and Marisaldi, M.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We are integrating the Fermi Gamma-Ray Burst Monitor (GBM) into the Interplanetary Network (IPN) of Gamma-Ray Burst (GRB) detectors. With the GBM, the IPN will comprise 9 experiments. This will 1) assist the Fermi team in understanding and reducing their systematic localization uncertainties, 2) reduce the sizes of the GBM and Large Area Telescope (LAT) error circles by 1 to 4 orders of magnitude, 3) facilitate the identification of GRB sources with objects found by ground- and space-based observatories at other wavelengths, from the radio to very high energy gamma-rays, 4) reduce the uncertainties in associating some LAT detections of high energy photons with GBM bursts, and 5) facilitate searches for non-electromagnetic GRB counterparts, particularly neutrinos and gravitational radiation. We present examples and demonstrate the synergy between Fermi and the IPN. This is a Fermi Cycle 2 Guest Investigator project., Comment: 5 pages, 11 figures. 2009 Fermi Symposium. eConf Proceedings C091122
Published: 2009

22. 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., and Wilson-Hodge, C. A.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
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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23. 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, 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, H-F, 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, and Lovellette, MN
Subjects: astro-ph.HE, General Science & Technology
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

24. The Interplanetary Network Supplement to the BATSE 5B Catalog of Cosmic Gamma-Ray Bursts

Author: Hurley, K., Briggs, M. S., Kippen, R. M., Kouveliotou, C., Meegan, C., Fishman, G., Cline, T., Trombka, J., McClanahan, T., Boynton, W., Starr, R., McNutt, R., and Boer, M.
Subjects: Astrophysics
Abstract: We present Interplanetary Network (IPN) localization information for 343 gamma-ray bursts observed by the Burst and Transient Source Experiment (BATSE) between the end of the 4th BATSE catalog and the end of the Compton Gamma-Ray Observatory (CGRO) mission, obtained by analyzing the arrival times of these bursts at the Ulysses, Near Earth Asteroid Rendezvous (NEAR), and CGRO spacecraft. For any given burst observed by CGRO and one other spacecraft, arrival time analysis (or "triangulation") results in an annulus of possible arrival directions whose half-width varies between 11 arcseconds and 21 degrees, depending on the intensity, time history, and arrival direction of the burst,as well as the distance between the spacecraft. This annulus generally intersects the BATSE error circle, resulting in an average reduction of the area of a factor of 20. When all three spacecraft observe a burst, the result is an error box whose area varies between 1 and 48000 square arcminutes, resulting in an average reduction of the BATSE error circle area of a factor of 87., Comment: 60 pages, 8 figures. To be submitted to the Astrophysical Journal Supplement Series in conjunction with the BATSE 5B catalog. Revised version accepted for publication in ApJS 196, 1, 2011
Published: 2006
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25. The Interplanetary Network Supplement to the BATSE Catalogs of Untriggered Cosmic Gamma Ray Bursts

Author: Hurley, K., Stern, B., Kommers, J., Cline, T., Mazets, E., Golenetskii, S., Trombka, J., McClanahan, T., Goldsten, J., Feroci, M., Frontera, F., Guidorzi, C., Montanari, E., Lewin, W., Meegan, C., Fishman, G., Kouveliotou, C., Sinha, S., and Seetha, S.
Subjects: Astrophysics
Abstract: We present Interplanetary Network (IPN) detection and localization information for 211 gamma-ray bursts (GRBs) observed as untriggered events by the Burst and Transient Source Experiment (BATSE), and published in catalogs by Kommers et al. (2001) and Stern et al. (2001). IPN confirmations have been obtained by analyzing the data from 11 experiments. For any given burst observed by BATSE and one other distant spacecraft, arrival time analysis (or ``triangulation'') results in an annulus of possible arrival directions whose half-width varies between 14 arcseconds and 5.6 degrees, depending on the intensity, time history, and arrival direction of the burst, as well as the distance between the spacecraft. This annulus generally intersects the BATSE error circle, resulting in a reduction of the area of up to a factor of ~650. When three widely separated spacecraft observed a burst, the result is an error box whose area is as much as 30000 times smaller than that of the BATSE error circle. Because the IPN instruments are considerably less sensitive than BATSE, they generally did not detect the weakest untriggered bursts, but did detect the more intense ones which failed to trigger BATSE when the trigger was disabled. In a few cases, we have been able to identify the probable origin of bursts as soft gamma repeaters. The vast majority of the IPN-detected events, however, are GRBs, and the confirmation of them validates many of the procedures utilized to detect BATSE untriggered bursts., Comment: Minor revisions. Accepted for publication in the Astrophysical Journal Supplement Series, February 2005
Published: 2004
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26. Measurements of Gamma-Ray Bursts (GRBs) with Glast

Author: Lichti, G. G., Briggs, M., Diehl, R., Fishman, G., Greiner, J., Kippen, R. M., Kouveliotou, C., Meegan, C., Paciesas, W., Preece, R., Schoenfelder, V., and von Kienlin, A.
Subjects: Astrophysics
Abstract: One of the scientific goals of the main instrument of GLAST is the study of Gamma-Ray Bursts (GRBs) in the energy range from ~20 MeV to ~300 GeV. In order to extend the energy measurement towards lower energies a secondary instrument, the GLAST Burst Monitor (GBM), will measure GRBs from ~10 keV to ~25 MeV and will therefore allow the investigation of the relation between the keV and the MeV-GeV emission from GRBs over six energy decades. These unprecedented measurements will permit the exploration of the unknown aspects of the high-energy burst emission and the investigation of their connection with the well-studied low-energy emission. They will also provide ne insights into the physics of GRBs in general. In addition the excellent localization of GRBs by the LAT will stimulate follow-up observations at other wavelengths which may yield clues about the nature of the burst sources., Comment: 6 pages, 2 figures, to be published in Baltic Astronomy - Proceedings of the minisymposium "Physics of Gamma-Ray Bursts", JENAM Conference, August 29-30, 2003, Budapest
Published: 2004

27. The GLAST Burst Monitor (GBM)

Author: Lichti, G. G., Briggs, M. S., Diehl, R., Fishman, G., Georgii, R., Kippen, R. M., Kouveliotou, C., Meegan, C., Paciesas, W., Preece, R., Schoenfelder, V., and von Kienlin, A.
Subjects: Astrophysics
Abstract: The selection of the GLAST burst monitor (GBM) by NASA will allow the investigation of the relation between the keV and the MeV-GeV emission from gamma-ray bursts. The GBM consists of 12 NaI and 2 BGO crystals allowing a continuous measurement of the energy spectra of gamma-ray bursts from ~5 keV to \~30 MeV. One feature of the GBM is its high time resolution for time-resolved gamma-ray spectroscopy. Moreover the arrangement of the NaI crystals allows a rapid on-board location (<15 degrees) of a gamma-ray burst within a FoV of ~8.6 sr. This position will be communicated to the main instrument of GLAST making follow-up observations at high energies possible., Comment: 4 pages with 2 figures
Published: 2001

28. A Non-Triggered Burst Supplement to the BATSE Gamma-Ray Burst Catalogs

Author: Kommers, J. M., Lewin, W. H. G., Kouveliotou, C., van Paradijs, J., Pendleton, G. N., Meegan, C. A., and Fishman, G. J.
Subjects: Astrophysics
Abstract: The Burst and Transient Source Experiment (BATSE) on the Compton Gamma Ray Observatory detected gamma-ray bursts (GRBs) with a real-time burst detection (or "trigger") system running onboard the spacecraft. Under some circumstances, however, a GRB may not have activated the onboard burst trigger. For example, the burst may have been too faint to exceed the onboard detection threshold, or it may have occurred while the onboard burst trigger was disabled for technical reasons. This paper describes a catalog of 873 "non-triggered" GRBs that were detected in a search of the archival continuous data from BATSE, recorded between 1991 December 9.0 and 1997 December 17.0. For each burst, the catalog gives an estimated source direction, duration, peak flux, and fluence. Similar data are presented for 50 additional bursts of unknown origin that were detected in the 25--50 keV range; these events may represent the low-energy "tail" of the GRB spectral distribution. This catalog increases the number of GRBs detected with BATSE by 48% during the time period covered by the search., Comment: to appear in ApJ Supp Series; more information at http://space.mit.edu/BATSE
Published: 2000

29. Discovery of the Optical Transient of the Gamma Ray Burst 990308

Author: Schaefer, Bradley E., Snyder, J. A., Hernandez, J., Roscherr, B., Deng, M., Ellmann, N., Bailyn, C., Rengstorf, A., Smith, D., Levine, A., Barthelmy, S., Butterworth, P., Hurley, K., Cline, T., Meegan, C., Kouveliotou, C., Kippen, R., Park, H., Williams, G., Porrata, R., Bionta, R., Hartmann, D., Band, D., Frail, D., Kulkarni, S., Bloom, J., Djorgovski, S., Harris, F., Abad, C., Adams, B., Andrews, P., Baltay, C., Bongiovanni, A., Briceno, C., Bruzual, G., Coppi, P., Della Prugna, F., Dubuc, A., Emmet, W., Ferrin, I., Fuenmayor, F., Gebhard, M., Herrera, D., Honeycutt, K., Magris, G., Mateu, J., Muffson, S., Musser, J., Naranjo, O., Oemler, A., Pacheco, R., Paredes, G., Rengel, M., Romero, L., Rosenzweig, P., and al, C. Sabbey et
Subjects: Astrophysics
Abstract: The optical transient of the faint Gamma Ray Burst 990308 was detected by the QUEST camera on the Venezuelan 1-m Schmidt telescope starting 3.28 hours after the burst. Our photometry gives $V = 18.32 \pm 0.07$, $R = 18.14 \pm 0.06$, $B = 18.65 \pm 0.23$, and $R = 18.22 \pm 0.05$ for times ranging from 3.28 to 3.47 hours after the burst. The colors correspond to a spectral slope of close to $f_{\nu} \propto \nu^{1/3}$. Within the standard synchrotron fireball model, this requires that the external medium be less dense than $10^{4} cm^{-3}$, the electrons contain $> 20%$ of the shock energy, and the magnetic field energy must be less than 24% of the energy in the electrons for normal interstellar or circumstellar densities. We also report upper limits of $V > 12.0$ at 132 s (with LOTIS), $V > 13.4$ from 132-1029s (with LOTIS), $V > 15.3$ at 28.2 min (with Super-LOTIS), and a 8.5 GHz flux of $< 114 \mu Jy$ at 110 days (with the Very Large Array). WIYN 3.5-m and Keck 10-m telescopes reveal this location to be empty of any host galaxy to $R > 25.7$ and $K > 23.3$. The lack of a host galaxy likely implies that it is either substantially subluminous or more distant than a red shift of $\sim 1.2$., Comment: ApJ Lett submitted, 5 pages, 2 figures, no space for 12 coauthors
Published: 1999
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30. Average Emissivity Curve of BATSE Gamma-Ray Bursts with Different Intensities

Author: Mitrofanov, I. G., Litvak, M. L., Briggs, M. S., Paciesas, W. S., Pendleton, G. N., Preece, R. D., and Meegan, C. A.
Subjects: Astrophysics
Abstract: Six intensity groups with ~150 BATSE gamma-ray bursts each are compared using average emissivity curves. Time-stretch factors for each of the dimmer groups are estimated with respect to the brightest group, which serves as the reference, taking into account the systematics of counts-produced noise effects and choice statistics. A stretching/intensity anti-correlation is found with good statistical significance during the average back slopes of bursts. A stretch factor ~2 is found between the 150 dimmest bursts, with peak flux <0.45ph cm^{-2} s^{-1}, and the 147 brightest bursts, with peak flux >4.1 ph cm^{-2} s^{-1}. On the other hand, while a trend of increasing stretching factor may exist for rise fronts for burst with decreasing peak flux from >4.1 ph cm^{-2} s^{-1} down to 0.7 ph cm^{-2} s^{-1}, the magnitude of the stretching factor is less than ~ 1.4 and is therefore inconsistent with stretching factor of back slope., Comment: 21 pages, 3 figures. Accepted to ApJ
Published: 1999
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31. Average Cosmological Invariant Parameters of Cosmic Gamma Ray Burst

Author: Mitrofanov, I. G., Anfimov, D. S., Litvak, M. L., Briggs, M. S., Paciesas, W. S., Pendleton, G. N., Preece, R. D., and Meegan, C. A.
Subjects: Astrophysics
Abstract: Average cosmological invariant parameters (ACIPs) are calculated for six groups of BATSE cosmic gamma-ray bursts selected by their peak fluxes on the 1.024 s time scale. The ACIPs represent the average temporal and spectral properties of these events equally in the observer frame of reference and in the co-moving frames of outbursting emitters. The parameters are determined separately for rise fronts and for back slopes of bursts, defined as the time profiles before and after the main peaks, respectively. The ACIPs for the rise fronts are found to be different for different intensity groups, while the ACIPs for the back slopes show no significant dependence on intensity. We conclude that emitters of bursts manifest standard average properties only during the back slopes of bursts., Comment: 18 pages, 3 figures. Accepted to ApJ (It is scheduled for the September 20, 1999 issue, Vol. 523)
Published: 1999
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32. A ROSAT Deep Survey of Four Small Gamma-Ray Burst Error Boxes

Author: Hurley, K., Li, P., Boer, M., Cline, T., Fishman, G. J., Meegan, C., Kouveliotou, C., Greiner, J., Laros, J., Luginbuhl, C., Vrba, F., Murakami, T., Pedersen, H., and van Paradijs, J.
Subjects: Astrophysics
Abstract: We have used the ROSAT High Resolution Imager to search for quiescent X-ray counterparts to four gamma-ray bursts which were localized to small (< 10 sq. arcmin.) error boxes with the Interplanetary Network. The observations took place years after the bursts, and the effective exposure times for each target varied from ~16 - 23 ks. We have not found any X-ray sources inside any of the error boxes. The 0.1 - 2.4 keV 3 sigma flux upper limits range from around 5 x 10^-14 erg cm^-2 s^-1 to 6 x 10^-13 erg cm^-2 s^-1 depending on the burst and the assumed shape of the quiescent spectrum. We consider four types of X-ray emitting galaxies (normal, AGN, faint, and star-forming) and use the flux upper limits to constrain their redshifts. We then use the GRB fluences to constrain the total energies of the bursts., Comment: 16 pages, 4 figures; submitted to the Astrophysical Journal
Published: 1999
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33. The Fourth BATSE Gamma-Ray Burst Catalog (Revised)

Author: Paciesas, W. S., Meegan, C. A., Pendleton, G. N., Briggs, M. S., Kouveliotou, C., Koshut, T. M., Lestrade, J. P., McCollough, M. L., Brainerd, J. J., Hakkila, J., Henze, W., Preece, R. D., Connaughton, V., Kippen, R. M., Mallozzi, R. S., Fishman, G. J., Richardson, G. A., and Sahi, M.
Subjects: Astrophysics
Abstract: The Burst and Transient Source Experiment (BATSE) on the Compton Gamma Ray Observatory (CGRO) has triggered on 1637 cosmic gamma-ray bursts between 1991 April 19 and 1996 August 29. These events constitute the Fourth BATSE burst catalog. The current version (4Br) has been revised from the version first circulated on CD-ROM in September 1997 (4B) to include improved locations for a subset of bursts that have been reprocssed using additional data. A significant difference from previous BATSE catalogs is the inclusion of bursts from periods when the trigger energy range differed from the nominal 50-300 keV. We present tables of the burst occurrence times, locations, peak fluxes, fluences, and durations. In general, results from previous BATSE catalogs are confirmed here with greater statistical significance., Comment: 45 pages, 12 Postscript figures, accepted for publication in Ap. J. Suppl
Published: 1999
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34. LOTIS Search for Early Time Optical Afterglows: GRB 971227

Author: Williams, G. G., Park, H. S., Ables, E., Band, D. L., Barthelmy, S. D., Bionta, R., Butterworth, P. S., Cline, T. L., Ferguson, D. H., Fishman, G. J., Gehrels, N., Hartmann, D. H., Hurley, K., Kouveliotou, C., Meegan, C. A., Ott, L., Parker, E., and Porrata, R.
Subjects: Astrophysics
Abstract: We report on the very early time search for an optical afterglow from GRB 971227 with the Livermore Optical Transient Imaging System (LOTIS). LOTIS began imaging the `Original' BATSE error box of GRB 971227 approximately 14 s after the onset of gamma-ray emission. Continuous monitoring of the position throughout the evening yielded a total of 499 images (10 s integration). Analysis of these images revealed no steady optical afterglow brighter than R=12.3 +- 0.2 in any single image. Coaddition of different combinations of the LOTIS images also failed to uncover transient optical emission. In particular, assuming a constant early time flux, no optical afterglow brighter than R=14.2 +- 0.2 was present within the first 1200 s and no optical afterglow brighter than R=15.0 +- 0.2 was present in the first 6.0 h. Follow up observations by other groups revealed a likely X-ray afterglow and a possible optical afterglow. Although subsequent deeper observations could not confirm a fading source, we show that these transients are not inconsistent with our present knowledge of the characteristics of GRB afterglows. We also demonstrate that with the upgraded thermoelectrically cooled CCDs, LOTIS is capable of either detecting very early time optical afterglow or placing stringent constraints on the relationship between the gamma-ray emission and the longer wavelength afterglow in relativistic blast wave models., Comment: 17 pages, 3 eps figures, revisions based on reviewers comments
Published: 1999
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35. The Ulysses Supplement to the BATSE 4Br Catalog of Cosmic Gamma-Ray Bursts

Author: Hurley, K., Briggs, M. S., Kippen, R. M., Kouveliotou, C., Meegan, C., Fishman, G., Cline, T., and Boer, M.
Subjects: Astrophysics
Abstract: We present Interplanetary Network localization information for 147 gamma-ray bursts observed by the Burst and Transient Source Experiment between the end of the 3rd BATSE catalog and the end of the 4th BATSE catalog, obtained by analyzing the arrival times of these bursts at the Ulysses and Compton Gamma-Ray Observatory (CGRO) spacecraft. For any given burst observed by these two spacecraft, arrival time analysis (or "triangulation") results in an annulus of possible arrival directions whose half-width varies between 7 arcseconds and 2.3 degrees, depending on the intensity and time history of the burst, and the distance of the Ulysses spacecraft from Earth. This annulus generally intersects the BATSE error circle, resulting in an average reduction of the error box area of a factor of 25., Comment: Accepted for publication in the Astrophysical Journal Supplement
Published: 1998
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36. The Ulysses Supplement to the BATSE 3B Catalog of Cosmic Gamma-Ray Bursts

Author: Hurley, K., Briggs, M. S., Kippen, R. M., Kouveliotou, C., Meegan, C., Fishman, G., Cline, T., and Boer, M.
Subjects: Astrophysics
Abstract: We present Interplanetary Network localization information for 218 gamma-ray bursts in the 3rd BATSE catalog, obtained by analyzing the arrival times of these bursts at the Ulysses and Compton Gamma-Ray Observatory (CGRO) spacecraft. For any given burst observed by these two spacecraft, arrival time analysis (or "triangulation") results in an annulus of possible arrival directions whose half-width varies between 7 arcseconds and 32 arcminutes, depending on the intensity and time history of the burst, and the distance of the Ulysses spacecraft from Earth. This annulus generally intersects the BATSE error circle, resulting in an average reduction of the error box area of a factor of 30., Comment: Accepted for publication in the Astrophysical Journal Supplement
Published: 1998
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37. The Intensity Distribution of Faint Gamma-ray Bursts Detected with BATSE

Author: Kommers, J. M., Lewin, W. H. G., Kouveliotou, C., van Paradijs, J., Pendleton, G. N., Meegan, C. A., and Fishman, G. J.
Subjects: Astrophysics
Abstract: We have recently completed a search of 6 years of archival BATSE data for gamma-ray bursts (GRBs) that were too faint to activate the real-time burst detection system running onboard the spacecraft. These "non-triggered" bursts can be combined with the "triggered" bursts detected onboard to produce a GRB intensity distribution that reaches peak fluxes a factor of 2 lower than could be studied previously. The value of the V/Vmax statistic (in Euclidean space) for the bursts we detect is 0.177 +/- 0.006. This surprisingly low value is obtained because we detected very few bursts on the 4.096 s and 8.192 s time scales (where most bursts have their highest signal-to-noise ratio) that were not already detected on the 1.024 s time scale. If allowance is made for a power-law distribution of intrinsic peak luminosities, the extended peak flux distribution is consistent with models in which the redshift distribution of the gamma-ray burst rate approximately traces the star formation history of the Universe. We argue that this class of models is preferred over those in which the burst rate is independent of redshift. We use the peak flux distribution to derive a limit of 10% (99% confidence) on the fraction of the total burst rate that could be contributed by a spatially homogeneous (in Euclidean space) subpopulation of burst sources, such as type Ib/c supernovae. These results lend support to the conclusions of previous studies predicting that relatively few faint "classical" GRBs will be found below the BATSE onboard detection threshold., Comment: 21 pp, figures included; LaTeX, uses aas2pp4.sty. Extended and updated discussion; to appear in ApJ. The burst catalog and further information are available at http://space.mit.edu/BATSE
Published: 1998

38. BATSE GRB Location Errors

Author: Briggs, M. S., Pendleton, G. N., Brainerd, J. J., Connaughton, V., Kippen, R. M., Meegan, C., and Hurley, K.
Subjects: Astrophysics
Abstract: We characterize the error distribution of BATSE GRB locations by modeling the distribution of separations between BATSE locations and IPN annuli. We determine error model parameters by maximizing likelihood and rank the models by their Bayesian odds ratios. The best models have several systematic error terms. The simplest good model has a 1.9 degree systematic error with probability 73% and 5.4 degrees with probability 27%. A more complex model adds a dependence on the datatype used to derive the location., Comment: to appear in Gamma-Ray Bursts: 4th Huntsville Symposium, ed. C. Meegan, R. Preece and T. Koshut
Published: 1997
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39. Super-LOTIS: A High-Sensitive Optical Counterpart Search Experiment

Author: Park, H. S., Ables, E., Band, D. L., Barthelmy, S. D., Bionta, R. M., Butterworth, P. S., Cline, T. L., Ferguson, D. H., Fishman, G. J., Gehrels, N., Hartmann, D., Hurley, K., Kouveliotou, C., Meegan, C. A., Ott, L., Parker, E., and Williams, G. G.
Subjects: Astrophysics
Abstract: We are constructing a 0.6 meter telescope system to search for early time gamma-ray burst(GRB) optical counterparts. Super-LOTIS (Super-Livermore Optical Transient Imaging System) is an automated telescope system that has a 0.8 x 0.8 deg field-of-view, is sensitive to Mv ~ 19 and responds to a burst trigger within 5 min. This telescope will record images of the gamma-ray burst coordinates that is given by the GCN (GRB Coordinate Network). A measurement of GRB light curves at early times will greatly enhance our understanding of GRB physics., Comment: LaTeX, 4 pages, 2 figures, requires aipproc.sty and epsfig.sty, To appear in the Proceedings of the 4th Huntsville Gamma-Ray Burst Symposium
Published: 1997

40. First Year Results From LOTIS

Author: Williams, G. G., Park, H. S., Ables, E., Band, D. L., Barthelmy, S. D., Bionta, R., Butterworth, P. S., Cline, T. L., Ferguson, D. H., Fishman, G. J., Gehrels, N., Hartmann, D. H., Hurley, K., Kouveliotou, C., Meegan, C. A., Ott, L., Parker, E., and Wurtz, R.
Subjects: Astrophysics
Abstract: LOTIS (Livermore Optical Transient Imaging System) is a gamma-ray burst optical counterpart search experiment located near Lawrence Livermore National Laboratory in California. The system is linked to the GCN (GRB Coordinates Network) real-time coordinate distribution network and can respond to a burst trigger in 6-15 seconds. LOTIS has a total field-of-view of 17.4 deg x 17.4 deg with a completeness sensitivity of m_V ~ 11 for a 10 second integration time. Since operations began in October 1996, LOTIS has responded to over 30 GCN/BATSE GRB triggers. Seven of these triggers are considered good events subject to the criteria of clear weather conditions, < 60 s response time, and > 50% coverage of the final BATSE 3sigma error circle. We discuss results from the first year of LOTIS operations with an emphasis on the observations and analysis of GRB 971006 (BATSE trigger 6414)., Comment: LaTeX, 5 pages, 2 figures, requires aipproc.sty and epsfig.sty, To appear in the Proceedings of the 4th Huntsville Gamma-Ray Burst Symposium
Published: 1997

41. BATSE Observations of Gamma-Ray Burst Spectra. IV. Time-Resolved High-Energy Spectroscopy

Author: Preece, R. D., Pendleton, G. N., Briggs, M. S., Mallozzi, R. S., Paciesas, W. S., Band, D. L., Matteson, J. L., and Meegan, C. A.
Subjects: Astrophysics
Abstract: We report on the temporal behavior of the high-energy power law continuum component of gamma-ray burst spectra with data obtained by the Burst and Transient Source Experiment. We have selected 126 high fluence and high flux bursts from the beginning of the mission up until the present. Much of the data were obtained with the Large Area Detectors, which have nearly all-sky coverage, excellent sensitivity over two decades of energy and moderate energy resolution, ideal for continuum spectra studies of a large sample of bursts at high time resolution. At least 8 spectra from each burst were fitted with a spectral form that consisted of a low-energy power law, a spectral break at middle energies and a high-energy continuum. In most bursts (122), the high-energy continuum was consistent with a power law. The evolution of the fitted high-energy power-law index over the selected spectra for each burst is inconsistent with a constant for 34% of the total sample. The sample distribution of the average value for the index from each burst is fairly narrow, centered on -2.12. A linear trend in time is ruled out for only 20% of the bursts, with hard-to-soft evolution dominating the sample (100 events). The distribution for the total change in the power-law index over the duration of a burst peaks at the value -0.37, and is characterized by a median absolute deviation of 0.39, arguing that a single physical process is involved. We present analyses of the correlation of the power-law index with time, burst intensity and low-energy time evolution. In general, we confirm the general hard-to-soft spectral evolution observed in the low-energy component of the continuum, while presenting evidence that this evolution is different in nature from that of the rest of the continuum., Comment: 30 pages, with 2 tables and 9 figures To appear in The Astrophysical Journal, April 1, 1998
Published: 1997
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42. New Constraints on Simultaneous Optical Emission From GRBs Measured by the LOTIS Experiment

Author: Park, H. S., Williams, G. G., Ables, E., Band, D. L., Barthelmy, S. D., Bionta, R., Butterworth, P. S., Cline, T. L., Ferguson, D. H., Fishman, G. J., Gehrels, N., Hartmann, D., Hurley, K., Kouveliotou, C., Meegan, C. A., Ott, L., Parker, E., and Wurtz, R.
Subjects: Astrophysics
Abstract: LOTIS is a gamma-ray burst optical counterpart search experiment located near Lawrence Livermore National Laboratory in California. Since operations began in October 1996, LOTIS has responded to five triggers as of July 30, 1997, which occurred during good weather conditions. GRB970223 (BATSE Trigger #6100) was an exceptionally strong burst lasting $\sim30$ s with a peak at $\sim8$ s. LOTIS began imaging the error box $\sim 11$ s after the burst began, and achieved simultaneous optical coverage of 100% of the region enclosed by the BATSE $3\sigma$ error circle and the IPN annulus. No optical transients were observed brighter than the m$_V \sim 11$ completeness limit of the resulting images providing a new upper limit on the simultaneous optical to gamma-ray fluence ratio of $R_L < 1.1 \times 10^{-4}$ and on the simultaneous optical (at 700 nm) to gamma-ray (at 100 keV) flux density ratio of $R_F < 305$ for a B type spectrum and $R_F < 475$ for an M type spectrum., Comment: 15 pages, LaTeX, requires aasms4.sty, 3 EPS figures; submitted to Astrophysical Journal Letters
Published: 1997

43. Radio and Optical Follow-up Observations and Improved IPN Position of GRB 970111

Author: Galama, T. J., Groot, P. J., Strom, R. G., van Paradijs, J., Hurley, K., Kouveliotou, C., Fishman, G. J., Meegan, C. A., Heise, J., Zand, J. J. M. in 't, de Bruyn, A. G., Hanlon, L. O., Bennett, K., Telting, J. H., and Rutten, R. G. M.
Subjects: Astrophysics
Abstract: We report on Westerbork 840 MHz, 1.4 and 5 GHz radio observations of the improved IPN-WFC error box of the gamma-ray burst GRB 970111, between 26.4 hours and 120 days after the event onset. In the ~ 13 sq arcmin area defined by the IPN (BATSE and Ulysses) annulus and the published refined BeppoSAX Wide Field Camera error box we detected no steady sources brighter than 0.56 mJy (4 sigma), and no varying radio emission, down to 1.0 mJy (4 sigma). We also report on B, V, R and I band observations of the error box with the 4.2 m William Herschel Telescope at La Palma., Comment: 19 pages including 4 figures, Latex, accepted for APJL
Published: 1997
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44. A Search for Non-triggered Gamma Ray Bursts in the BATSE Data Base

Author: Kommers, J. M., Lewin, W. H. G., Kouveliotou, C., van Paradijs, J., Pendleton, G. N., Meegan, C. A., and Fishman, G. J.
Subjects: Astrophysics
Abstract: We describe a search of archival data from the Burst and Transient Source Experiment (BATSE). The purpose of the search is to find astronomically interesting transients that did not activate the burst detection (or ``trigger'') system onboard the spacecraft. Our search is sensitive to events with peak fluxes (on the 1.024 s time scale) that are lower by a factor of 2 than can be detected with the onboard burst trigger. In a search of 345 days of archival data, we detected 91 events in the 50--300 keV range that resemble classical gamma ray bursts but that did not activate the onboard burst trigger. We also detected 110 low-energy (25--50 keV) events of unknown origins which may include activity from SGR 1806-20 and bursts and flares from X-ray binaries. This paper gives the occurrence times, estimated source directions, durations, peak fluxes, and fluences for the 91 gamma ray burst candidates. The direction and intensity distributions of these bursts imply that the biases inherent in the onboard trigger mechanism have not significantly affected the completeness of the published BATSE gamma ray burst catalogs., Comment: Fixed incorrect values of and added erratum section
Published: 1997
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45. Real-Time Optical Flux Limits From Gamma-Ray Bursts Measured By The GROCSE Experiment

Author: Park, H. S., Ables, E., Band, D. L., Barthelmy, S. D., Bionta, R. M., Butterworth, P. S., Cline, T. L., Ferguson, D. H., Fishman, G. J., Gehrels, N., Hurley, K., Kouveliotou, C., Lee, B. C., Meegan, C. A., Ott, L. L., and Parker, E. L.
Subjects: Astrophysics
Abstract: The Gamma-Ray Optical Counterpart Search Experiment (GROCSE) presents new experimental upper limits on the optical flux from gamma-ray bursts (GRBs). Our experiment consisted of a fully-automated very wide-field opto-electronic detection system that imaged locations of GRBs within a few seconds of receiving trigger signals provided by BATSE's real-time burst coordinate distribution network (BACODINE). The experiment acquired ~3800 observing hours, recording 22 gamma-ray burst triggers within $\sim$30 s of the start of the burst event. Some of these bursts were imaged while gamma-ray radiation was being detected by BATSE. We identified no optical counterparts associated with gamma-ray bursts amongst these events at the m$_V$ $\sim$ 7.0 to 8.5 sensitivity level. We find the ratio of the upper limit to the V-band optical flux, F$_\nu$, to the gamma-ray fluence, $\Phi_\gamma$, from these data to be $2 \times 10^{-18} < F_\nu/\Phi_\gamma < 2 \times 10^{-16}$., Comment: 28 pages, LaTeX, requires aasms4.sty and apjpt4.sty, 5 EPS figures; submitted to Astrophysical Journal
Published: 1997
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46. Search for TeV Counterparts of Gamma-Ray Bursts with the HEGRA Experiment

Author: Krawczynski, H., Funk, B., collaboration, the HEGRA, Barthelmy, S., Butterworth, P., Cline, T., Gehrels, N., Kouveliotou, C., Fishman, J., and Meegan, C.
Subjects: Astrophysics
Abstract: The HEGRA experiment is an air shower detector system for the study of neutral and charged cosmic rays in the energy range between 500 GeV to 10 PeV. Here we give an overview of how the HEGRA detector is used to search for TeV gamma-radiation associated with Gamma-Ray Bursts (GRBs) registered with the Burst And Transient Source Experiment (BATSE) on board the Compton Gamma-Ray Observatory. Furthermore, results of an archival search for GRB radiation above 15 TeV carried out with the HEGRA air shower arrays are shown. We conclude with a summary of the search activities planned for the future., Comment: Latex file, 6 pages, 4 figures. Macros needed: epsf, sprocl. To appear in proceedings of the "International School Of Cosmic-ray Astrophysics", Erice, 16-23 June 1996, (World Scientific)
Published: 1996

47. A 23 GHz Survey of GRB Error Boxes

Author: Hewitt, J. N., Katz, C. A., Barthelmy, S. D., Baumgartner, W. H., Cline, T. L., Corey, B. E., Fishman, G. J., Gehrels, N., Hurley, K. C., Kouveliotou, C., Meegan, C. A., Moore, C. B., Rutledge, R. E., and Trotter, C. S.
Subjects: Astrophysics
Abstract: The Haystack 37-meter telescope was used in a pilot project in May 1995 to observe GRB error boxes at 23~GHz. Seven BATSE error boxes and two IPN arcs were scanned by driving the beam of the telescope rapidly across their area. For the BATSE error boxes, the radio observations took place two to eighteen days after the BATSE detection, and several boxes were observed more than once. Total power data were recorded continuously as the telescope was driven at a rate of 0.2~degrees/second, yielding Nyquist sampling of the beam with an integration time of 50~milliseconds, corresponding to a theoretical rms sensitivity of 0.5~Jy. Under conditions of good weather, this sensitivity was achieved. In a preliminary analysis of the data we detect only two sources, 3C273 and 0552+398, both catalogued sources that are known to be variable at 23~GHz. Neither had a flux density that was unusally high or low at the time of our observations., Comment: 5 pages, 1 postscript figure. To appear in Proceedings of the Third Huntsville Symposium on Gamma-Ray Bursts (eds. C. Kouveliotou, M. S. Briggs, and G. J. Fishman)
Published: 1996
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48. Time Dependent Clustering Analysis of the Second BATSE Gamma-Ray Burst Catalog

Author: Brainerd, J. J., Meegan, C. A., Briggs, Michael S., Pendleton, G. N., and Brock, M. N.
Subjects: Astrophysics
Abstract: A time dependent two-point correlation-function analysis of the BATSE 2B catalog finds no evidence of burst repetition. As part of this analysis, we discuss the effects of sky exposure on the observability of burst repetition and present the equation describing the signature of burst repetition in the data. For a model of all burst repetition from a source occurring in less than five days we derive upper limits on the number of bursts in the catalog from repeaters and model-dependent upper limits on the fraction of burst sources that produce multiple outbursts., Comment: To appear in the Astrophysical Journal Letters, uuencoded compressed PostScript, 11 pages with 4 embedded figures
Published: 1995
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49. Duration Distributions of Bright and Dim BATSE Gamma-Ray Bursts

Author: Norris, J. P., Bonnell, J. T., Nemiroff, R. J., Scargle, J. D., Kouveliotou, C., Paciesas, W. S., Meegan, C. A., and Fishman, G. J.
Subjects: Astrophysics
Abstract: We have measured the T90 and T50 durations of bright and dim gamma-ray bursts (GRBs) detected by the Compton Gamma Ray Observatory's Burst and Transient Source Experiment (BATSE). The T90 (T50) duration is defined as the interval over which 5\% (25\%) to 95\% (75\%) of the burst counts accumulate. Out of 775 bursts observed by BATSE, 159 bursts were analyzed; bursts with durations shorter than 1.5 s were excluded. A Kolmogorov-Smirnov test yields a probability of 6 x $10^{-5}$ that the T50 durations of the dim and bright samples are drawn from the same parent population. We find that the centroid and extent of the duration distribution for the dim sample are scaled by approximately a factor of two relative to those of the bright sample. The measured time dilation factor is not sensitive to choice of energy band. These results are quantitatively consistent with previous tests for time dilation in a smaller sample of BATSE bursts. The dimmer bursts, if cosmological, would lie at redshifts of order two., Comment: in press: The Astrophysical Journal, 15 pages of Plain TEX version 3.0. Postscript text, tables and figures available through RJN's Home Page URL of http://enemy.gsfc.nasa.gov/htmltest/rjn.html
Published: 1994
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50. Gross Spectral Differences between Bright and Dim Gamma-Ray Bursts

Author: Nemiroff, R. J., Norris, J. P., Bonnell, J. T., Wickramasinghe, W. A. D. T., Kouveliotou, C., Paciesas, W. S., Fishman, G. J., and Meegan, C. A.
Subjects: Astrophysics
Abstract: We find that dim gamma-ray bursts (GRBs) are softer than bright GRBs, as indicated on average by data from the Burst and Transient Source Experiment (BATSE) on board the Compton Gamma Ray Observatory. We show that this correlation is statistically significant with respect to variations due to random differences between GRBs. This effect is discernable using a variety of methods and data sets, including public domain data. We analyze several types of systematic errors and selection effects in the BATSE data and conclude that the observed effect is not dominated by any of them. We therefore assert that this dim/soft effect is a real property of GRBs. It is possible that this correlation is a consequence of the time dilation detected by Norris et al. (1994) and that this is additional evidence that burst sources are located at cosmological distances., Comment: in press: The Astrophysical Journal (Letters), 15 pages of Plain TEX version 3.0. Postscript text and figures available through RJN's Home Page URL of http://enemy.gsfc.nasa.gov/htmltest/rjn.html
Published: 1994
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