Author: "Hurley, K. C." - Searchworks@Jio Institute Digital Library Search Results

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142 results on '"Hurley, K. C."'

1. GrailQuest: hunting for atoms of space and time hidden in the wrinkle of Space-Time: A swarm of nano/micro/small-satellites to probe the ultimate structure of Space-Time and to provide an all-sky monitor to study high-energy astrophysics phenomena

Author: Burderi, L., Sanna, A., Di Salvo, T., Amati, L., Amelino-Camelia, G., Branchesi, M., Capozziello, S., Coccia, E., Colpi, M., Costa, E., D’Amico, N., De Bernardis, P., De Laurentis, M., Valle, M. Della, Falcke, H., Feroci, M., Fiore, F., Frontera, F., Gambino, A. F., Ghisellini, G., Hurley, K. C., Iaria, R., Kataria, D., Labanti, C., Lodato, G., Negri, B., Papitto, A., Piran, T., Riggio, A., Rovelli, C., Santangelo, A., Vidotto, F., and Zane, S.
Published: 2021
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2. Search for gravitational waves associated with gamma-ray bursts during LIGO science run 6 and Virgo science runs 2 and 3

Author: The LIGO Scientific Collaboration, Virgo Collaboration, Abadie, J., Abbott, B. P., Abbott, R., Abbott, T. D., Abernathy, M., Accadia, T., Acernese, F., Adams, C., Adhikari, R., Affeldt, C., Agathos, M., Agatsuma, K., Ajith, P., Allen, B., Ceron, E. Amador, Amariutei, D., Anderson, S. B., Anderson, W. G., Arai, K., Arain, M. A., Araya, M. C., Aston, S. M., Astone, P., Atkinson, D., Aufmuth, P., Aulbert, C., Aylott, B. E., Babak, S., Baker, P., Ballardin, G., Ballmer, S., Barayoga, J. C. B., Barker, D., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barton, M. A., Bartos, I., Bassiri, R., Bastarrika, M., Basti, A., Batch, J., Bauchrowitz, J., Bauer, Th. S., Bebronne, M., Beck, D., Behnke, B., Bejger, M., Beker, M. G., Bell, A. S., Belopolski, I., Benacquista, M., Berliner, J. M., Bertolini, A., Betzwieser, J., Beveridge, N., Beyersdorf, P. T., Bilenko, I. A., Billingsley, G., Birch, J., Biswas, R., Bitossi, M., Bizouard, M. A., Black, E., Blackburn, J. K., Blackburn, L., Blair, D., Bland, B., Blom, M., Bock, O., Bodiya, T. P., Bogan, C., Bondarescu, R., Bondu, F., Bonelli, L., Bonnand, R., Bork, R., Born, M., Boschi, V., Bose, S., Bosi, L., Bouhou, B., Braccini, S., Bradaschia, C., Brady, P. R., Braginsky, V. B., Branchesi, M., Brau, J. E., Breyer, J., Briant, T., Bridges, D. O., Brillet, A., Brinkmann, M., Brisson, V., Britzger, M., Brooks, A. F., Brown, D. A., Bulik, T., Bulten, H. J., Buonanno, A., Burguet--Castell, J., Buskulic, D., Buy, C., Byer, R. L., Cadonati, L., Calloni, E., Camp, J. B., Campsie, P., Cannizzo, J., Cannon, K., Canuel, B., Cao, J., Capano, C. D., Carbognani, F., Carbone, L., Caride, S., Caudill, S., Cavaglià, M., Cavalier, F., Cavalieri, R., Cella, G., Cepeda, C., Cesarini, E., Chaibi, O., Chalermsongsak, T., Charlton, P., Chassande-Mottin, E., Chelkowski, S., Chen, W., Chen, X., Chen, Y., Chincarini, A., Chiummo, A., Cho, H. S., Chow, J., Christensen, N., Chua, S. S. Y., Chung, C. T. Y., Chung, S., Ciani, G., Clara, F., Clark, D. E., Clark, J., Clayton, J. H., Cleva, F., Coccia, E., Cohadon, P. -F., Colacino, C. N., Colas, J., Colla, A., Colombini, M., Conte, A., Conte, R., Cook, D., Corbitt, T. R., Cordier, M., Cornish, N., Corsi, A., Costa, C. A., Coughlin, M., Coulon, J. -P., Couvares, P., Coward, D. M., Cowart, M., Coyne, D. C., Creighton, J. D. E., Creighton, T. D., Cruise, A. M., Cumming, A., Cunningham, L., Cuoco, E., Cutler, R. M., Dahl, K., Danilishin, S. L., Dannenberg, R., D'Antonio, S., Danzmann, K., Dattilo, V., Daudert, B., Daveloza, H., Davier, M., Daw, E. J., Day, R., Dayanga, T., De Rosa, R., DeBra, D., Debreczeni, G., Degallaix, J., Del Pozzo, W., del Prete, M., Dent, T., Dergachev, V., DeRosa, R., DeSalvo, R., Dhurandhar, S., Di Fiore, L., Di Lieto, A., Di Palma, I., Emilio, M. Di Paolo, Di Virgilio, A., Díaz, M., Dietz, A., Donovan, F., Dooley, K. L., Drago, M., Drever, R. W. P., Driggers, J. C., Du, Z., Dumas, J. -C., Dwyer, S., Eberle, T., Edgar, M., Edwards, M., Effler, A., Ehrens, P., Endröczi, G., Engel, R., Etzel, T., Evans, K., Evans, M., Evans, T., Factourovich, M., Fafone, V., Fairhurst, S., Fan, Y., Farr, B. F., Fazi, D., Fehrmann, H., Feldbaum, D., Feroz, F., Ferrante, I., Fidecaro, F., Finn, L. S., Fiori, I., Fisher, R. P., Flaminio, R., Flanigan, M., Foley, S., Forsi, E., Forte, L. A., Fotopoulos, N., Fournier, J. -D., Franc, J., Franco, S., Frasca, S., Frasconi, F., Frede, M., Frei, M., Frei, Z., Freise, A., Frey, R., Fricke, T. T., Friedrich, D., Fritschel, P., Frolov, V. V., Fujimoto, M. -K., Fulda, P. J., Fyffe, M., Gair, J., Galimberti, M., Gammaitoni, L., Garcia, J., Garufi, F., Gáspár, M. E., Gehrels, N., Gemme, G., Geng, R., Genin, E., Gennai, A., Gergely, L. Á., Ghosh, S., Giaime, J. A., Giampanis, S., Giardina, K. D., Giazotto, A., Gil-Casanova, S., Gill, C., Gleason, J., Goetz, E., Goggin, L. M., González, G., Gorodetsky, M. L., Goßler, S., Gouaty, R., Graef, C., Graff, P. B., Granata, M., Grant, A., Gras, S., Gray, C., Gray, N., Greenhalgh, R. J. S., Gretarsson, A. M., Greverie, C., Grosso, R., Grote, H., Grunewald, S., Guidi, G. M., Guido, C., Gupta, R., Gustafson, E. K., Gustafson, R., Ha, T., Hallam, J. M., Hammer, D., Hammond, G., Hanks, J., Hanna, C., Hanson, J., Hardt, A., Harms, J., Harry, G. M., Harry, I. W., Harstad, E. D., Hartman, M. T., Haughian, K., Hayama, K., Hayau, J. -F., Heefner, J., Heidmann, A., Heintze, M. C., Heitmann, H., Hello, P., Hendry, M. A., Heng, I. S., Heptonstall, A. W., Herrera, V., Hewitson, M., Hild, S., Hoak, D., Hodge, K. A., Holt, K., Holtrop, M., Hong, T., Hooper, S., Hosken, D. J., Hough, J., Howell, E. J., Hughey, B., Husa, S., Huttner, S. H., Huynh-Dinh, T., Ingram, D. R., Inta, R., Isogai, T., Ivanov, A., Izumi, K., Jacobson, M., James, E., Jang, Y. J., Jaranowski, P., Jesse, E., Johnson, W. W., Jones, D. I., Jones, G., Jones, R., Jonker, R. J. G., Ju, L., Kalmus, P., Kalogera, V., Kandhasamy, S., Kang, G., Kanner, J. B., Kasturi, R., Katsavounidis, E., Katzman, W., Kaufer, H., Kawabe, K., Kawamura, S., Kawazoe, F., Kelley, D., Kells, W., Keppel, D. G., Keresztes, Z., Khalaidovski, A., Khalili, F. Y., Khazanov, E. A., Kim, B. K., Kim, C., Kim, H., Kim, K., Kim, N., Kim, Y. M., King, P. J., Kinzel, D. L., Kissel, J. S., Klimenko, S., Kokeyama, K., Kondrashov, V., Koranda, S., Korth, W. Z., Kowalska, I., Kozak, D., Kranz, O., Kringel, V., Krishnamurthy, S., Krishnan, B., Królak, A., Kuehn, G., Kumar, P., Kumar, R., Kwee, P., Lam, P. K., Landry, M., Lantz, B., Lastzka, N., Lawrie, C., Lazzarini, A., Leaci, P., Lee, C. H., Lee, H. K., Lee, H. M., Leong, J. R., Leonor, I., Leroy, N., Letendre, N., Li, J., Li, T. G. F., Liguori, N., Lindquist, P. E., Liu, Y., Liu, Z., Lockerbie, N. A., Lodhia, D., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lough, J., Luan, J., Lubinski, M., Lück, H., Lundgren, A. P., Macdonald, E., Machenschalk, B., MacInnis, M., Macleod, D. M., Mageswaran, M., Mailand, K., Majorana, E., Maksimovic, I., Malvezzi, V., Man, N., Mandel, I., Mandic, V., Mantovani, M., Marandi, A., Marchesoni, F., Marion, F., Márka, S., Márka, Z., Markosyan, A., Maros, E., Marque, J., Martelli, F., Martin, I. W., Martin, R. M., Marx, J. N., Mason, K., Masserot, A., Matichard, F., Matone, L., Matzner, R. A., Mavalvala, N., Mazzolo, G., McCarthy, R., McClelland, D. E., McGuire, S. C., McIntyre, G., McIver, J., McKechan, D. J. A., McWilliams, S., Meadors, G. D., Mehmet, M., Meier, T., Melatos, A., Melissinos, A. C., Mendell, G., Mercer, R. A., Meshkov, S., Messenger, C., Meyer, M. S., Miao, H., Michel, C., Milano, L., Miller, J., Minenkov, Y., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Miyakawa, O., Moe, B., Mohan, M., Mohanty, S. D., Mohapatra, S. R. P., Moraru, D., Moreno, G., Morgado, N., Morgia, A., Mori, T., Morriss, S. R., Mosca, S., Mossavi, K., Mours, B., Mow--Lowry, C. M., Mueller, C. L., Mueller, G., Mukherjee, S., Mullavey, A., Müller-Ebhardt, H., Munch, J., Murphy, D., Murray, P. G., Mytidis, A., Nash, T., Naticchioni, L., Necula, V., Nelson, J., Neri, I., Newton, G., Nguyen, T., Nishizawa, A., Nitz, A., Nocera, F., Nolting, D., Normandin, M. E., Nuttall, L., Ochsner, E., O'Dell, J., Oelker, E., Ogin, G. H., Oh, J. J., Oh, S. H., O'Reilly, B., O'Shaughnessy, R., Osthelder, C., Ott, C. D., Ottaway, D. J., Ottens, R. S., Overmier, H., Owen, B. J., Page, A., Palladino, L., Palomba, C., Pan, Y., Pankow, C., Paoletti, F., Paoletti, R., Papa, M. A., Parisi, M., Pasqualetti, A., Passaquieti, R., Passuello, D., Patel, P., Pedraza, M., Peiris, P., Pekowsky, L., Penn, S., Perreca, A., Persichetti, G., Phelps, M., Pichot, M., Pickenpack, M., Piergiovanni, F., Pietka, M., Pinard, L., Pinto, I. M., Pitkin, M., Pletsch, H. J., Plissi, M. V., Poggiani, R., Pöld, J., Postiglione, F., Prato, M., Predoi, V., Prestegard, T., Price, L. R., Prijatelj, M., Principe, M., Privitera, S., Prix, R., Prodi, G. A., Prokhorov, L. G., Puncken, O., Punturo, M., Puppo, P., Quetschke, V., Quitzow-James, R., Raab, F. J., Rabeling, D. S., Rácz, I., Radkins, H., Raffai, P., Rakhmanov, M., Rankins, B., Rapagnani, P., Raymond, V., Re, V., Redwine, K., Reed, C. M., Reed, T., Regimbau, T., Reid, S., Reitze, D. H., Ricci, F., Riesen, R., Riles, K., Robertson, N. A., Robinet, F., Robinson, C., Robinson, E. L., Rocchi, A., Roddy, S., Rodriguez, C., Rodruck, M., Rolland, L., Rollins, J. G., Romano, J. D., Romano, R., Romie, J. H., Rosińska, D., Röver, C., Rowan, S., Rüdiger, A., Ruggi, P., Ryan, K., Sainathan, P., Salemi, F., Sammut, L., Sandberg, V., Sannibale, V., Santamaría, L., Santiago-Prieto, I., Santostasi, G., Sassolas, B., Sathyaprakash, B. S., Sato, S., Saulson, P. R., Savage, R. L., Schilling, R., Schnabel, R., Schofield, R. M. S., Schreiber, E., Schulz, B., Schutz, B. F., Schwinberg, P., Scott, J., Scott, S. M., Seifert, F., Sellers, D., Sentenac, D., Sergeev, A., Shaddock, D. A., Shaltev, M., Shapiro, B., Shawhan, P., Shoemaker, D. H., Sibley, A., Siemens, X., Sigg, D., Singer, A., Singer, L., Sintes, A. M., Skelton, G. R., Slagmolen, B. J. J., Slutsky, J., Smith, J. R., Smith, M. R., Smith, R. J. E., Smith-Lefebvre, N. D., Somiya, K., Sorazu, B., Soto, J., Speirits, F. C., Sperandio, L., Stefszky, M., Stein, A. J., Stein, L. C., Steinert, E., Steinlechner, J., Steinlechner, S., Steplewski, S., Stochino, A., Stone, R., Strain, K. A., Strigin, S. E., Stroeer, A. S., Sturani, R., Stuver, A. L., Summerscales, T. Z., Sung, M., Susmithan, S., Sutton, P. J., Swinkels, B., Tacca, M., Taffarello, L., Talukder, D., Tanner, D. B., Tarabrin, S. P., Taylor, J. R., Taylor, R., ter Braack, A. P. M., Thomas, P., Thorne, K. A., Thorne, K. S., Thrane, E., Thüring, A., Tokmakov, K. V., Tomlinson, C., Toncelli, A., Tonelli, M., Torre, O., Torres, C., Torrie, C. I., Tournefier, E., Tucker, E., Travasso, F., Traylor, G., Tseng, K., Ugolini, D., Vahlbruch, H., Vajente, G., Brand, J. F. J. van den, Broeck, C. Van Den, van der Putten, S., van Veggel, A. A., Vass, S., Vasuth, M., Vaulin, R., Vavoulidis, M., Vecchio, A., Vedovato, G., Veitch, J., Veitch, P. J., Veltkamp, C., Verkindt, D., Vetrano, F., Viceré, A., Villar, A. E., Vinet, J. -Y., Vitale, S., Vocca, H., Vorvick, C., Vyatchanin, S. P., Wade, A., Wade, L., Wade, M., Waldman, S. J., Wallace, L., Wan, Y., Wang, M., Wang, X., Wang, Z., Wanner, A., Ward, R. L., Was, M., Weinert, M., Weinstein, A. J., Weiss, R., Wen, L., Wessels, P., West, M., Westphal, T., Wette, K., Whelan, J. T., Whitcomb, S. E., White, D. J., Whiting, B. F., Wilkinson, C., Willems, P. A., Williams, L., Williams, R., Willke, B., Winkelmann, L., Winkler, W., Wipf, C. C., Wiseman, A. G., Wittel, H., Woan, G., Wooley, R., Worden, J., Yakushin, I., Yamamoto, H., Yamamoto, K., Yancey, C. C., Yang, H., Yeaton-Massey, D., Yoshida, S., Yu, P., Yvert, M., Zadrożny, A., Zanolin, M., Zendri, J. -P., Zhang, F., Zhang, L., Zhang, W., Zhao, C., Zotov, N., Zucker, M. E., Zweizig, J., Briggs, M. S., Connaughton, V., Hurley, K. C., Jenke, P. A., von Kienlin, A., Rau, A., and Zhang, X. -L.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology
Abstract: We present the results of a search for gravitational waves associated with 154 gamma-ray bursts (GRBs) that were detected by satellite-based gamma-ray experiments in 2009-2010, during the sixth LIGO science run and the second and third Virgo science runs. We perform two distinct searches: a modeled search for coalescences of either two neutron stars or a neutron star and black hole; and a search for generic, unmodeled gravitational-wave bursts. We find no evidence for gravitational-wave counterparts, either with any individual GRB in this sample or with the population as a whole. For all GRBs we place lower bounds on the distance to the progenitor, under the optimistic assumption of a gravitational-wave emission energy of 10^-2 M c^2 at 150 Hz, with a median limit of 17 Mpc. For short hard GRBs we place exclusion distances on binary neutron star and neutron star-black hole progenitors, using astrophysically motivated priors on the source parameters, with median values of 16 Mpc and 28 Mpc respectively. These distance limits, while significantly larger than for a search that is not aided by GRB satellite observations, are not large enough to expect a coincidence with a GRB. However, projecting these exclusions to the sensitivities of Advanced LIGO and Virgo, which should begin operation in 2015, we find that the detection of gravitational waves associated with GRBs will become quite possible., Comment: Accepted by ApJ. 19 pages, 8 figures, 2 tables, science summary page at http://www.ligo.org/science/Publication-S6GRB/index.php . Public access area to figures, tables at https://dcc.ligo.org/cgi-bin/DocDB/ShowDocument?docid=p1000121
Published: 2012
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3. Search for Gravitational Wave Bursts from Six Magnetars

Author: Abadie, J., Abbott, B. P., Abbott, R., Abernathy, M., Accadia, T., Acerneseac, F., Adams, C., Adhikari, R., Affeldt, C., Allen, B., Allen, G. S., Ceron, E. Amador, Amariutei, D., Amin, R. S., Anderson, S. B., Anderson, W. G., Antonuccia, F., Arai, K., Arain, M. A., Araya, M. C., Aston, S. M., Astonea, P., Atkinson, D., Aufmuth, P., Aulbert, C., Aylott, B. E., Babak, S., Baker, P., Ballardin, G., Ballmer, S., Barker, D., Barnum, S., Baroneac, F., Barr, B., Barriga, P., Barsotti, L., Barsuglia, M., Barton, M. A., Bartos, I., Bassiri, R., Bastarrika, M., Bastiab, A., Bauchrowitz, J., Bauera, Th. S., Behnke, B., Bekera, M. G., Bell, A. S., Belletoile, A., Belopolski, I., Benacquista, M., Bertolini, A., Betzwieser, J., Beveridge, N., Beyersdorf, P. T., Bilenko, I. A., Billingsley, G., Birch, J., Birindellia, S., Biswas, R., Bitossia, M., Bizouarda, M. A., Black, E., Blackburn, J. K., Blackburn, L., Blair, D., Bland, B., Bloma, M., Bock, O., Bodiya, T. P., Bogan, C., Bondarescu, R., Bondub, F., Bonelliab, L., Bonnand, R., Bork, R., Born, M., Boschia, V., Bose, S., Bosia, L., Bouhou, B., Boyle, M., Braccinia, S., Bradaschiaa, C., Brady, P. R., Braginsky, V. B., Brau, J. E., Breyer, J., Bridges, D. O., Brilleta, A., Brinkmann, M., Brissona, V., Britzger, M., Brooks, A. F., Brown, D. A., Brummit, A., Budzyńskib, R., Bulikbc, T., Bultenab, H. J., Buonanno, A., Burguet--Castell, J., Burmeister, O., Buskulic, D., Buy, C., Byer, R. L., Cadonati, L., Cagnolia, G., Cain, J., Calloniab, E., Camp, J. B., Campagnaab, E., Campsie, P., Cannizzo, J., Cannon, K., Canuel, B., Cao, J., Capano, C., Carbognani, F., Caride, S., Caudill, S., Cavaglià, M., Cavaliera, F., Cavalieri, R., Cellaa, G., Cepeda, C., Cesarinib, E., Chaibia, O., Chalermsongsak, T., Chalkley, E., Charlton, P., Chassande-Mottin, E., Chelkowski, S., Chen, Y., Chincarini, A., Christensen, N., Chua, S. S. Y., Chung, C. T. Y., Chung, S., Clara, F., Clark, D., Clark, J., Clayton, J. H., Clevaa, F., Cocciaab, E., Colacinoab, C. N., Colas, J., Collaab, A., Colombinib, M., Conte, R., Cook, D., Corbitt, T. R., Cornish, N., Corsia, A., Costa, C. A., Coughlin, M., Coulona, J. -P., Coward, D. M., Coyne, D. C., Creighton, J. D. E., Creighton, T. D., Cruise, A. M., Culter, R. M., Cumming, A., Cunningham, L., Cuoco, E., Dahl, K., Danilishin, S. L., Dannenberg, R., D'Antonioa, S., Danzmann, K., Das, K., Dattilo, V., Daudert, B., Daveloza, H., Daviera, M., Davies, G., Daw, E. J., Day, R., Dayanga, T., De Rosaab, R., DeBra, D., Debreczeni, G., Degallaix, J., del Preteac, M., Dent, T., Dergachev, V., DeRosa, R., DeSalvo, R., Dhurandhar, S., Di Fiorea, L., Di Lietoab, A., Di Palma, I., Emilioac, M. Di Paolo, Di Virgilioa, A., Díaz, M., Dietz, A., Donovan, F., Dooley, K. L., Dorsher, S., Douglas, E. S. D., Dragocd, M., Drever, R. W. P., Driggers, J. C., Dumas, J. -C., Dwyer, S., Eberle, T., Edgar, M., Edwards, M., Effler, A., Ehrens, P., Engel, R., Etzel, T., Evans, M., Evans, T., Factourovich, M., Fafoneab, V., Fairhurst, S., Fan, Y., Farr, B. F., Fazi, D., Fehrmann, H., Feldbaum, D., Ferranteab, I., Fidecaroab, F., Finn, L. S., Fiori, I., Flaminio, R., Flanigan, M., Foley, S., Forsi, E., Fortea, L. A., Fotopoulos, N., Fourniera, J. -D., Franc, J., Frascaab, S., Frasconia, F., Frede, M., Frei, M., Frei, Z., Freise, A., Frey, R., Fricke, T. T., Friedrich, D., Fritschel, P., Frolov, V. V., Fulda, P., Fyffe, M., Galimberti, M., Gammaitoniab, L., Garcia, J., Garofoli, J. A., Garufiab, F., Gáspár, M. E., Gemme, G., Genin, E., Gennaia, A., Ghosh, S., Giaime, J. A., Giampanis, S., Giardina, K. D., Giazottoa, A., Gill, C., Goetz, E., Goggin, L. M., González, G., Gorodetsky, M. L., Goßler, S., Gouaty, R., Graef, C., Granata, M., Grant, A., Gras, S., Gray, C., Greenhalgh, R. J. S., Gretarsson, A. M., Greveriea, C., Grosso, R., Grote, H., Grunewald, S., Guidiab, G. M., Guido, C., Gupta, R., Gustafson, E. K., Gustafson, R., Hage, B., Hallam, J. M., Hammer, D., Hammond, G., Hanks, J., Hanna, C., Hanson, J., Harms, J., Harry, G. M., Harry, I. W., Harstad, E. D., Hartman, M. T., Haughian, K., Hayama, K., Hayaub, J. -F., Hayler, T., Heefner, J., Heitmann, H., Helloa, P., Hendry, M. A., Heng, I. S., Heptonstall, A. W., Herrera, V., Hewitson, M., Hild, S., Hoak, D., Hodge, K. A., Holt, K., Hong, T., Hooper, S., Hosken, D. J., Hough, J., Howell, E. J., Huet, D., Hughey, B., Husa, S., Huttner, S. H., Ingram, D. R., Inta, R., Isogai, T., Ivanov, A., Jaranowskid, P., Johnson, W. W., Jones, D. I., Jones, G., Jones, R., Ju, L., Kalmus, P., Kalogera, V., Kandhasamy, S., Kanner, J. B., Katsavounidis, E., Katzman, W., Kawabe, K., Kawamura, S., Kawazoe, F., Kells, W., Kelner, M., Keppel, D. G., Khalaidovski, A., Khalili, F. Y., Khazanov, E. A., Kim, H., Kim, N., King, P. J., Kinzel, D. L., Kissel, J. S., Klimenko, S., Kondrashov, V., Kopparapu, R., Koranda, S., Korth, W. Z., Kowalskab, I., Kozak, D., Kringel, V., Krishnamurthy, S., Krishnan, B., Królakae, A., Kuehn, G., Kumar, R., Kwee, P., Landry, M., Lantz, B., Lastzka, N., Lazzarini, A., Leaci, P., Leong, J., Leonor, I., Leroya, N., Letendre, N., Li, J., Lia, T. G. F., Liguoriab, N., Lindquist, P. E., Lockerbie, N. A., Lodhia, D., Lorenzinia, M., Lorietteb, V., Lormand, M., Losurdoa, G., Lu, P., Luan, J., Lubinski, M., Lück, H., Lundgren, A. P., Macdonald, E., Machenschalk, B., MacInnis, M., Mageswaran, M., Mailand, K., Majoranaa, E., Maksimovicb, I., Mana, N., Mandel, I., Mandic, V., Mantovaniac, M., Marandi, A., Marchesonia, F., Marion, F., Márka, S., Márka, Z., Maros, E., Marque, J., Martelliab, F., Martin, I. W., Martin, R. M., Marx, J. N., Mason, K., Masserot, A., Matichard, F., Matone, L., Matzner, R. A., Mavalvala, N., McCarthy, R., McClelland, D. E., McGuire, S. C., McIntyre, G., McKechan, D. J. 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A., Parameswaran, A., Pardiab, S., Parisiab, M., Pasqualetti, A., Passaquietiab, R., Passuelloa, D., Patel, P., Pathak, D., Pedraza, M., Pekowsky, L., Penn, S., Peralta, C., Perreca, A., Persichettiab, G., Phelps, M., Pichota, M., Pickenpack, M., Piergiovanniab, F., Pietkad, M., Pinard, L., Pinto, I. M., Pitkin, M., Pletsch, H. J., Plissi, M. V., Podkaminer, J., Poggianiab, R., Pöld, J., Postiglione, F., Prato, M., Predoi, V., Price, L. R., Prijatelj, M., Principe, M., Privitera, S., Prix, R., Prodiab, G. A., Prokhorov, L., Puncken, O., Punturoa, M., Puppoa, P., Quetschke, V., Raab, F. J., Rabelingab, D. S., Rácz, I., Radkins, H., Raffai, P., Rakhmanov, M., Ramet, C. R., Rankins, B., Rapagnaniab, P., Raymond, V., Reab, V., Redwine, K., Reed, C. M., Reed, T., Regimbaua, T., Reid, S., Reitze, D. H., Ricciab, F., Riesen, R., Riles, K., Roberts, P., Robertson, N. A., Robineta, F., Robinson, C., Robinson, E. L., Rocchia, A., Roddy, S., Rolland, L., Rollins, J., Romano, J. 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E., Vineta, J. -Y., Voccaa, H., Vorvick, C., Vyachanin, S. P., Waldman, S. J., Wallace, L., Wanner, A., Ward, R. L., Wasa, M., Wei, P., Weinert, M., Weinstein, A. J., Weiss, R., Wen, L., Wen, S., Wessels, P., West, M., Westphal, T., Wette, K., Whelan, J. T., Whitcomb, S. E., White, D., Whiting, B. F., Wilkinson, C., Willems, P. A., Williams, H. R., Williams, L., Willke, B., Winkelmann, L., Winkler, W., Wipf, C. C., Wiseman, A. G., Woan, G., Wooley, R., Worden, J., Yablon, J., Yakushin, I., Yamamoto, H., Yamamoto, K., Yang, H., Yeaton-Massey, D., Yoshida, S., Yu, P., Yvert, M., Zanolin, M., Zhang, L., Zhang, Z., Zhao, C., Zotov, N., Zucker, M. E., Zweizig, J., Aptekar, R. L., Boynton, W. V., Briggs, M. S., Cline, T. L., Connaughton, V., Frederiks, D. D., Gehrels, N., Goldsten, J. O, Golovin, D., van der Horst, A. J., Hurley, K. C., Kaneko, Y., von Kienlin, A., Kouveliotou, C., Krimm, H. A., Lin, L., Mitrofanov, I., Ohno, M., Palshin, V. D., Rau, A., Sanin, A., Tashiro, M. S., Terada, Y., and Yamaoka, K.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology
Abstract: Soft gamma repeaters (SGRs) and anomalous X-ray pulsars (AXPs) are thought to be magnetars: neutron stars powered by extreme magnetic fields. These rare objects are characterized by repeated and sometimes spectacular gamma-ray bursts. The burst mechanism might involve crustal fractures and excitation of non-radial modes which would emit gravitational waves (GWs). We present the results of a search for GW bursts from six galactic magnetars that is sensitive to neutron star f-modes, thought to be the most efficient GW emitting oscillatory modes in compact stars. One of them, SGR 0501+4516, is likely ~1 kpc from Earth, an order of magnitude closer than magnetars targeted in previous GW searches. A second, AXP 1E 1547.0-5408, gave a burst with an estimated isotropic energy >10^{44} erg which is comparable to the giant flares. We find no evidence of GWs associated with a sample of 1279 electromagnetic triggers from six magnetars occurring between November 2006 and June 2009, in GW data from the LIGO, Virgo, and GEO600 detectors. Our lowest model-dependent GW emission energy upper limits for band- and time-limited white noise bursts in the detector sensitive band, and for f-mode ringdowns (at 1090 Hz), are 3.0x10^{44} d_1^2 erg and 1.4x10^{47} d_1^2 erg respectively, where d_1 = d_{0501} / 1 kpc and d_{0501} is the distance to SGR 0501+4516. These limits on GW emission from f-modes are an order of magnitude lower than any previous, and approach the range of electromagnetic energies seen in SGR giant flares for the first time., Comment: 9 pages, 3 figures; v2 minor clarifications and new references
Published: 2010
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4. GRB 080503: Implications of a Naked Short Gamma-Ray Burst Dominated by Extended Emission

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

Author: LIGO Scientific Collaboration, Barthelmy, S., Gehrels, N., Hurley, K. C., and Palmer, D.
Subjects: Astrophysics
Abstract: We present the results of a LIGO search for short-duration gravitational waves (GWs) associated with Soft Gamma Repeater (SGR) bursts. This is the first search sensitive to neutron star f-modes, usually considered the most efficient GW emitting modes. We find no evidence of GWs associated with any SGR burst in a sample consisting of the 27 Dec. 2004 giant flare from SGR 1806-20 and 190 lesser events from SGR 1806-20 and SGR 1900+14 which occurred during the first year of LIGO's fifth science run. GW strain upper limits and model-dependent GW emission energy upper limits are estimated for individual bursts using a variety of simulated waveforms. The unprecedented sensitivity of the detectors allows us to set the most stringent limits on transient GW amplitudes published to date. We find upper limit estimates on the model-dependent isotropic GW emission energies (at a nominal distance of 10 kpc) between 3x10^45 and 9x10^52 erg depending on waveform type, detector antenna factors and noise characteristics at the time of the burst. These upper limits are within the theoretically predicted range of some SGR models., Comment: 6 pages, 1 Postscript figure
Published: 2008
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6. The afterglow of GRB050709 and the nature of the short-hard gamma-ray bursts

Author: Fox, D. B., Frail, D. A., Price, P. A., Kulkarni, S. R., Berger, E., Piran, T., Soderberg, A. M., Cenko, S. B., Cameron, P. B., Gal-Yam, A., Kasliwal, M. M., Moon, D. -S., Harrison, F. A., Nakar, E., Schmidt, B. P., Penprase, B., Chevalier, R. A., Kumar, P., Roth, K., Watson, D., Lee, B. L., Shectman, S., Phillips, M. M., Roth, M., McCarthy, P. J., Rauch, M., Cowie, L., Peterson, B. A., Rich, J., Kawai, N., Aoki, K., Kosugi, G., Totani, T., Park, H. -S., MacFadyen, A., and Hurley, K. C.
Subjects: Astrophysics
Abstract: The final chapter in the long-standing mystery of the gamma-ray bursts (GRBs) centres on the origin of the short-hard class, suspected on theoretical grounds to result from the coalescence of neutron star or black hole binary systems. Numerous searches for the afterglows of short-hard bursts have been made, galvanized by the revolution in our understanding of long-duration GRBs that followed the discovery in 1997 of their broadband (X-ray, optical, and radio) afterglow emission. Here we present the discovery of the X-ray afterglow of a short-hard burst whose accurate position allows us to unambiguously associate it with a star-forming galaxy at redshift z=0.160, and whose optical lightcurve definitively excludes a supernova association. Together with results from three other recent short-hard bursts, this suggests that short-hard bursts release much less energy than the long-duration GRBs. Models requiring young stellar populations, such as magnetars and collapsars, are ruled out, while coalescing degenerate binaries remain the most promising progenitor candidates., Comment: Nature in press (Oct 6 issue). 23 pages, 4 figures
Published: 2005
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7. An HST Search for Supernovae Accompanying X-ray Flashes

Author: Soderberg, A. M., Kulkarni, S. R., Fox, D. B., Berger, E., Price, P. A., Cenko, S. B., Howell, D. A., Gal-Yam, A., Leonard, D. C., Frail, D. A., Moon, D., Chevalier, R. A., Hamuy, M., Hurley, K. C., Kelson, D., Koviak, K., Krzeminski, W., Kumar, P., MacFadyen, A., McCarthy, P. J., Park, H. S., Peterson, B. A., Phillips, M. M., Rauch, M., Roth, M., Schmidt, B. P., and Shectman, S.
Subjects: Astrophysics
Abstract: We present the results from an Hubble Space Telescope/ACS search for supernovae associated with X-ray flashes 020903, 040701, 040812 and 040916. We find strong evidence that XRF 020903 (z=0.25) was associated with a SN 1998bw-like supernova and confirm this using optical spectroscopy at t ~ 25 days. We find no evidence, however, for SN 1998bw-like supernovae associated with the other three events. In the case of XRF 040701 (z=0.21), we rule out even a faint supernova similar to SN 2002ap, using template light-curves for several local Type Ic supernovae. For the two cases in which the redshift is not known, XRFs 040812 and 040916, we derive robust redshift limits assuming they were accompanied by supernovae similar to SN 1998bw and compare these limits with photometric redshift constraints provided by their host galaxies. We supplement this analysis with results for three additional events (XRFs 011030, 020427 and 030723) and discuss the observed diversity of supernovae associated with X-ray flashes and gamma-ray bursts. We conclude that XRF-SNe exist, but can be significantly fainter than SN 1998bw, possibly consistent with the observed spread in local Type Ibc supernovae., Comment: Submitted to ApJ, 22 pages, 11 figures. High resolution figures available at http://www.astro.caltech.edu/~ams/XRF-SNe.html
Published: 2005
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8. The Swift Gamma-Ray Burst Mission

Author: Gehrels, N., Chincarini, G, Giommi, P., Mason, K. O., Nousek, J. A., Wells, A. A., White, N. E., Barthelmy, S. D., Burrows, D. N., Cominsky, L. R., Hurley, K. C., Marshall, F. E., Meszaros, P., Roming, P. W. A., and Team, Swift Science
Subjects: Astrophysics
Abstract: The Swift mission, scheduled for launch in early 2004, is a multiwavelength observatory for gamma-ray burst (GRB) astronomy. It is the first-of-its-kind autonomous rapid-slewing satellite for transient astronomy and pioneers the way for future rapid-reaction and multiwavelength missions. It will be far more powerful than any previous GRB mission, observing more than 100 bursts per year and performing detailed X-ray and UV/optical afterglow observations spanning timescales from 1 minute to several days after the burst. The objectives are to determine the origin of GRBs; classify GRBs and search for new types; study the interaction of the ultra-relativistic outflows of GRBs with their surrounding medium; and use GRBs to study the early universe out to z>10. The mission is being developed by a NASA-led international collaboration. It will carry three instruments: a new-generation wide-field gamma-ray (15-150 keV) detector; a narrow-field X-ray telescope; and a narrow-field UV/optical telescope. Redshift determinations will be made for most bursts. In addition to the primary GRB science, the mission will perform a hard X-ray survey to a sensitivity of ~1 mCrab (~2x10^{-11} erg cm^{-2} s^{-1} in the 15-150 keV band), more than an order of magnitude better than HEAO A-4. A flexible data and operations system will allow rapid follow-up observations of all types of high-energy transients, with rapid data downlink and uplink available through the NASA TDRSS system. The mission is currently funded for 2 years of operations and the spacecraft will have a lifetime to orbital decay of ~8 years. [ABRIDGED], Comment: 38 pages, including 10 figures; accepted for publication in ApJ v611
Published: 2004
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9. Localizations of Thirteen Gamma-ray Bursts by the All-Sky Monitor on RXTE

Author: Smith, D. A., Levine, A. M., Bradt, H. V., Remillard, R., Jernigan, J. G., Hurley, K. C., Wen, L., Briggs, M., Cline, T., Mazets, E., Golenetskii, S., and Frederics, D.
Subjects: Astrophysics
Abstract: The All-Sky Monitor (ASM) on the Rossi X-ray Timing Explorer (RXTE) has been used to localize thirteen confirmed X-ray counterparts to Gamma-Ray Bursts (GRBs) detected over three years of operation. We quantify the errors in ASM localizations of brief transient sources by using observations of persistent sources with well-known locations. We apply the results of this analysis to obtain accurate error boxes with reliable confidence levels for the thirteen GRBs. In six of these thirteen cases, multiple detections by the ASM allow the positions to be localized to a diamond of order ~15' x 3'. In five further cases, the Interplanetary Network (IPN) constrains the usually ~3 deg. x 3' (full-width) ASM error box to an area of a few tens of square arcminutes. This work adds eleven burst localizations to the list of ~60 well-localized GRBs., Comment: 14 pages, two-column,"emulateapj" style, accepted by ApJ for publication
Published: 1999

10. 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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11. The IPN I: From the Past to the Future

Author: Cline, T. L., Hurley, K. C., Barthelmy, S., Butterworth, P., Feroci, M., Frontera, F., Golenetskii, S., Mazets, E., Trombka, J., Costa, Enrico, editor, Frontera, Filippo, editor, and Hjorth, Jens, editor
Published: 2001
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12. ROSAT Observations of X-Ray Emissions from Jupiter During the Impact of Comet Shoemaker-Levy 9

Author: Waite, J. H., Gladstone, G. R., Franke, K., Lewis, W. S., Fabian, A. C., Brandt, W. N., Na, C., Haberl, F., Clarke, J. T., Hurley, K. C., Sommer, M., and Bolton, S.
Published: 1995

13. A short γ-ray burst apparently associated with an elliptical galaxy at redshift z = 0.225

Author: Gehrels, N., Sarazin, C. L., O'Brien, P. T., Zhang, B., Barbier, L., Barthelmy, S. D., Blustin, A., Burrows, D. N., Cannizzo, J., Cummings, J. R., Goad, M., Holland, S. T., Hurkett, C. P., Kennea, J. A., Levan, A., Markwardt, C. B., Mason, K. O., Meszaros, P., Page, M., Palmer, D. M., Rol, E., Sakamoto, T., Willingale, R., Angelini, L., Beardmore, A., Boyd, P. T., Breeveld, A., Campana, S., Chester, M. M., Chincarini, G., Cominsky, L. R., Cusumano, G., de Pasquale, M., Fenimore, E. E., Giommi, P., Gronwall, C., Grupe, D., Hill, J. E., Hinshaw, D., Hjorth, J., Hullinger, D., Hurley, K. C., Klose, S., Kobayashi, S., Kouveliotou, C., Krimm, H. A., Mangano, V., Marshall, F. E., McGowan, K., Moretti, A., Mushotzky, R. F., Nakazawa, K., Norris, J. P., Nousek, J. A., Osborne, J. P., Page, K., Parsons, A. M., Patel, S., Perri, M., Poole, T., Romano, P., Roming, P. W. A., Rosen, S., Sato, G., Schady, P., Smale, A. P., Sollerman, J., Starling, R., Still, M., Suzuki, M., Tagliaferri, G., Takahashi, T., Tashiro, M., Tueller, J., Wells, A. A., White, N. E., and Wijers, R. A. M. J.
Subjects: Environmental issues, Science and technology, Zoology and wildlife conservation
Abstract: Author(s): N. Gehrels (corresponding author) [1]; C. L. Sarazin [2]; P. T. O'Brien [3]; B. Zhang [4]; L. Barbier [1]; S. D. Barthelmy [1]; A. Blustin [5]; D. N. Burrows [...]
Published: 2005
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14. The IPN I: From the Past to the Future

Author: Cline, T. L., primary, Hurley, K. C., additional, Barthelmy, S., additional, Butterworth, P., additional, Feroci, M., additional, Frontera, F., additional, Golenetskii, S., additional, Mazets, E., additional, and Trombka, J., additional
Published: 2003
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15. The afterglow of GRB 050709 and the nature of the short-hard γ-ray bursts

Author: Fox, D. B., Frail, D. A., Price, P. A., Kulkarni, S. R., Berger, E., Piran, T., Soderberg, A. M., Cenko, S. B., Cameron, P. B., Gal-Yam, A., Kasliwal, M. M., Moon, D.-S., Harrison, F. A., Nakar, E., Schmidt, B. P., Penprase, B., Chevalier, R. A., Kumar, P., Roth, K., Watson, D., Lee, B. L., Shectman, S., Phillips, M. M., Roth, M., McCarthy, P. J., Rauch, M., Cowie, L., Peterson, B. A., Rich, J., Kawai, N., Aoki, K., Kosugi, G., Totani, T., Park, H.-S., MacFadyen, A., and Hurley, K. C.
Published: 2005

16. A search for hard X-ray microflares near solar minimum

Author: Lin, R. P., Hurley, K. C., Smith, D. M., and Pelling, R. M.
Published: 1991
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17. The most dilute lake in the world?

Author: Eilers, J. M., Sullivan, T. J., and Hurley, K. C.
Published: 1990
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18. Strategies for Studying the Sources of Gamma Ray Bursts

Author: Cline, T. L, Norris, J. P, and Hurley, K. C
Subjects: Astronomy
Abstract: The study of gamma ray bursts (GRBs) has rapidly evolved in recent years with the discovery of their cosmological nature and with BATSE, BeppoSAX, HETE and the IPN enabling a wide variety of associated . afterglow measurements. Multiwavelength observations ranging through the radio, optical, soft and hard x-ray, and gamma-ray regimes have exploded the field of GRB interpretation. Also, the Amanda, Milagro and LIGO experiments can search for related neutrino, cosmic-ray photon, and gravitational radiation events, even with the delayed alerts, such as from the IPN. The infrared region, where the optical emissions from sources at the extreme distances may be shifted, will become important but is undersubscribed. The soon-to-be launched Swift mission will greatly broaden the GRB discipline, and a strategy for associated ground-based measurements is outlined. The need for the improved global distribution of all instruments, in particular, robotic infrared detectors, is cited.
Published: 2003

19. The Swift Mission and the REM Telescope

Author: Gehrels, N, Chincarini, G, Giommi, P, Mason, K. O, Nousek, J. A, Wells, A. A, White, N. E, Barthelemy, S. D, Burrow, D. N, and Hurley, K. C
Subjects: Spacecraft Design, Testing And Performance
Abstract: Following a description of the science drive which originated the Swift Mission, this is US NASA MIDEX Mission with the collaboration of Italy and the UK, we will describe the status of the hardware and the observing strategy. The telemetry is carried out via the TDRSS satellite for those communications that need immediate response. The data transfer and the scheduled uploading of routine commands will be done through the ASI Malindi station in Kenia. Both in the US and in Europe a large effort will be done to follow the bursts with the maximum of efficiency and as soon as possible after the alert. We will describe how the ESO VLT telescopes are able to respond to the alert. To address the problematic of the dark bursts and to immediately follow up all of the bursts also in the Near Infrared we designed and built a 60 cm NIR Robotic telescope, REM, to be located on the ESO ground at Cerro La Silla. The instrumentation includes also a low dispersion spectrograph with the capability of multi wavelength optical photometry.
Published: 2003

20. Discovery of Soft X-Ray Emission From Io, Europa and the Io Plasma Torus

Author: Elsner, R. F, Gladstone, G. R, Waite, J. H, Crary, F. J, Howell, R. R, Johnson, R. E, Ford, P. G, Metzger, A. E, Hurley, K. C, Feigelson, E. D, and Six, N. Frank
Subjects: Space Radiation
Abstract: We report the discovery of soft (0.25 - 2 keV) x-ray emission from the moons Io and Europa, probably Ganymede, and from the Io Plasma Torus (IPT). Bombardment by energetic (greater than 10 keV) H, O, and S ions from the region of the IPT seems the likely source of the x-ray emission from the Galilean moons. According to our estimates, fluorescent x-ray emission excited by solar x-rays, even during flares from the active Sun, charge-exchange processes, previously invoked to explain Jupiter's x-ray aurora and cometary x-ray emission, and ion stripping by dust grains fall to account for the observed emission. On the other hand, bremsstrahlung emission of soft X-rays from non-thermal electrons in the few hundred to few thousand eV range may account for a substantial fraction of the observed x-ray flux from the IPT.
Published: 2001

21. Chandra Observations of Io and the Io Plasma Torus

Author: Elsner, Ronald F, Gladstone, G. R, Waite, J. H., Jr, Grodent, D. C, Crary, F. J, Metzger, A. E, Hurley, K. C, Ford, P, Feigelson, E, Garmire, G, and Whitaker, Ann
Subjects: Lunar And Planetary Science And Exploration
Abstract: Chandra observed the Jovian system for approximately 1 day with ACIS-S in Nov, 1999, and approximately 10 hours with HRC-I in Dec, 2000. Among the many results of great interest to planetary scientists are the detection of x-ray emission from the Io Plasma Torus (IPT) and, very faintly, associated with the Jovian moon Io itself. The IPT is an almost self-generating donut of S and O ions in Io's orbit that ultimately derive from volcanoes on the surface. While EUV and visible emissions from the IPT are relatively well understood to result from low charge state transitions of S and O and from electron impact, the x-ray emissions are too energetic to be explained this way and seem to require the presence of higher charge states of S and O. We present current ideas as to origins of these x-ray emissions.
Published: 2001

22. Gamma-Ray Burst Arrival-Time Localizations: Simultaneous Observations by Mars Observer, Compton Observatory, and Ulysses

Author: Laros, J. G, Boynton, W. V, Hurley, K. C, McCollough, M. L, Fishman, G. J, Meegan, C. A, Cline, T. L, Palmer, D. M, Starr, R. D, Trombka, J. I, Boer, M, Niel, M, and Metzger, A. E
Published: 1996

23. A search for the radio counterpart to the 1994 March 1 gamma-ray burst

Author: Frail, D. A, Kulkarni, S. R, Hurley, K. C, Fishman, G. J, Kouveliotou, C, Meegan, C. A, Sommer, M, Boer, M, Niel, M, and Cline, T
Subjects: Astrophysics
Abstract: We report on the results of a search for the radio counterpart to the bright gamma-ray burst of 1994 March 1. Using the Dominion Radio Astrophysical Observatory Synthesis Telescope sensitive, wide-field radio images at 1.4 GHz and 0.4 GHz were made of a region around GRB 940301. A total of 15 separate radio images were obtained at each frequency, sampling a near-continuous range of post-burst timescales between 3 and 15 days, as well as 26, 47, and 99 days. We place an upper limit of 3.5 mJy on a fading/flaring radio counterpart at 1.4 GHz and 55 mJy at 0.4 GHz. Unlike past efforts our counterpart search maintains high sensitivity over two decades of post-burst time durations. Time-variable radio emission after the initial gamma-ray burst is a prediction of all fireball models, currently the most popular model for gamma-ray bursts. Our observations allow us to put significant constraints on the fireball parameters for cosmological models of gamma-ray bursts.
Published: 1994
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24. ROSAT observations of the Jupiter aurora

Author: Waite, J. H., Jr, Bagenal, F, Seward, F, Na, C, Gladstone, G. R, Cravens, T. E, Hurley, K. C, Clarke, J. T, Elsner, R, and Stern, S. A
Subjects: Lunar And Planetary Exploration
Abstract: Roentgen satellite (ROSAT) high-resolution imager (HRI) and position sensitive proportional counter (PSPC) observations of Jupiter obtained in April 1991 and May 1992 reveal soft X-ray emissions apparently associated with Jupiter's aurora and similar to X-ray emssions observed earlier by the Einstein Observatory. The HRI images show emission mainly from Jupiter's northern hemisphere at all Jovian longitudes observed, and there is some indication of a longitudinal modulation of the emission in phase with well-known ultraviolet modulation of the northern aurora. The PSPC data reveal a very soft spectrum. Comparison of the observed spectrum with models for both electron bremsstrahlung radiation and line emission from S and O ions indicates that the line spectrum gives a much better statistical fit to the observed spectrum. The X ray observations presented here therefore support the hypothesis that ion precipitation is the most likely cause of the Jovian X ray emissions, a result first suggested by the Einstein results (Metzger et al., 1983).
Published: 1994
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25. Observational evidence linking a quasar with an optical transient

Author: Vrba, F. J, Luginbuhl, C. B, Hartmann, D. H, Hudec, R, Chaffee, F. H, Foltz, C. B, and Hurley, K. C
Subjects: Astronomy
Abstract: We present evidence for the association of a quasi stellar object (QSO) with a bright optical transient (OT). A V = 20.6 mag QSO with redshift z = 1.78 has been found within the 38 seconds x 62 seconds error ellipse of a bright OT discovered on a Harvard Patrol Camera plate taken in 1905. The chance of finding a random QSO at V less than or equal to 20.6 mag within this area is estimated as approximately 0.5%. Although the OT is within the error circle of the gamma-ray burst (GRB) GB 910219 position determined from the WATCH experiment, the localization for this same event determined from the Third Interplanetary Network does not include the OT or the QSO. Whether the GRB is related to the OT/QSO or not, the probable association of a bright OT with a QSO is a discovery that warrants further investigation.
Published: 1994
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26. Jovian bremsstrahlung X-rays - A Ulysses prediction

Author: Waite, J. H., Jr, Boice, D. C, Hurley, K. C, Stern, S. A, and Sommer, M
Subjects: Lunar And Planetary Exploration
Abstract: Modeling results reported here show that precipitating auroral electrons with sufficient energy to be consistent with the Voyager UVS observations produce bremsstrahlung X-rays with sufficient energy and intensity to be detected by the Solar Flare X-ray and Cosmic-Ray-Burst Instrument on board the Ulysses spacecraft. The detection of such bremsstrahlung X-rays at Jupiter would provide strong evidence for the electron-precipitation mechanism, although it does not rule out the possibility of some heavy ion involvement, and thus makes a significant contribution toward solving the mystery of the Jovian aurora.
Published: 1992

27. Gamma ray burst source locations with the Ulysses/Compton/PVO network

Author: Cline, T. L, Hurley, K. C, Boer, M, Sommer, M, Niel, M, Fishman, G. J, Kouveliotou, C, Meegan, C. A, Paciesas, W. S, and Wilson, R. B
Subjects: Space Radiation
Abstract: The new interplanetary gamma-ray burst network will determine source fields with unprecedented accuracy. The baseline of the Ulysses mission and the locations of Pioneer-Venus Orbiter and of Mars Observer will ensure precision to a few tens of arc seconds. Combined with the event phenomenologies of the Burst and Transient Source Experiment on Compton Observatory, the source locations to be achieved with this network may provide a basic new understanding of the puzzle of gamma ray bursts.
Published: 1992

28. Search For Gravitational Wave Bursts From Six Magnetars

Author: Abadie, J., Abbott, B. P., Abbott, R., Abernathy, M., Accadia, T., Acernese, F., Adams, C., Adhikari, R., Affeldt, C., Allen, B., Allen, G. S., Ceron, E. A., Amariutei, D., Amin, R. S., Anderson, S. B., Anderson, W. G., Antonucci, F., Arai, K., Arain, M. A., Araya, M. C., Aston, S. M., Astone, P., Atkinson, D., Aufmuth, P., Aulbert, C., Aylott, B. E., Babak, S., Baker, P., Ballardin, G., Ballmer, S., Barker, D., Barnum, S., Barone, F., Barr, B., Barriga, P., Barsotti, L., Barsuglia, M., Barton, M. A., Bartos, I., Bassiri, R., Bastarrika, M., Basti, A., Bauchrowitz, J., Bauer, T. S., Behnke, B., Beker, M. G., Bell, A. S., Belletoile, A., Belopolski, I., Benacquista, M., Bertolini, A., Betzwieser, J., Beveridge, N., Beyersdorf, P. T., Bilenko, I. A., Billingsley, G., Birch, J., Birindelli, S., Biswas, R., Bitossi, M., Bizouard, M. A., Black, E., Blackburn, J. K., Blackburn, L., Blair, D., Bland, B., Blom, M., Bock, O., Bodiya, T. P., Bogan, C., Bondarescu, R., Bondu, F., Bonelli, L., Bonnand, R., Bork, R., Born, M., Boschi, V., Bose, S., Bosi, L., Bouhou, B., Boyle, M., Braccini, S., Bradaschia, C., Brady, P. R., Braginsky, V. B., Brau, J. E., Breyer, J., Bridges, D. O., Brillet, A., Brinkmann, M., Brisson, V., Britzger, M., Brooks, A. F., Brown, D. A., Brummit, A., Budzynski, R., Bulik, T., Bulten, H. J., Buonanno, A., Burguet-Castell, J., Burmeister, O., Buskulic, D., Buy, C., Byer, R. L., Cadonati, L., Cagnoli, G., Cain, J., Calloni, E., Camp, J. B., Campagna, E., Campsie, P., Cannizzo, J., Cannon, K., Canuel, B., Cao, J., Capano, C., Carbognani, F., Caride, S., Caudill, S., Cavaglia, M., Cavalier, F., Cavalieri, R., Cella, G., Cepeda, C., Cesarini, E., Chaibi, O., Chalermsongsak, T., Chalkley, E., Charlton, P., Chassande-Mottin, E., Chelkowski, S., Chen, Y., Chincarini, A., Christensen, N., S. S. Y., C. T. Y., Chung, S., Clara, F., Clark, D., Clark, J., Clayton, J. H., Cleva, F., Coccia, E., Colacino, C. N., Colas, J., Colla, A., Colombini, M., Conte, R., Cook, D., Corbitt, T. R., Cornish, N., Corsi, A., Costa, C. A., Coughlin, M., Coulon, J. P., Coward, D. M., Coyne, D. C., J. D. E., Creighton, T. D., Cruise, A. M., Culter, R. M., Cumming, A., Cunningham, L., Cuoco, E., Dahl, K., Danilishin, S. L., Dannenberg, R., Antonio, S. D., Danzmann, K., Das, K., Dattilo, V., Daudert, B., Daveloza, H., Davier, M., Davies, G., Daw, E. J., Day, R., Dayanga, T., Rosa, R. D., Debra, D., Debreczeni, G., Degallaix, J., Prete, M. D., Dent, T., Dergachev, V., Derosa, R., Desalvo, R., Dhurandhar, S., Fiore, L. D., Lieto, A. D., Palma, I. D., Paolo, M. D., Virgilio, A. D., Diaz, M., Dietz, A., Donovan, F., Dooley, K. L., Dorsher, S., E. S. D., Drago, M., R. W. P., Driggers, J. C., Dumas, J. C., Dwyer, S., Eberle, T., Edgar, M., Edwards, M., Effler, A., Ehrens, P., Engel, R., Etzel, T., Evans, M., Evans, T., Factourovich, M., Fafone, V., Fairhurst, S., Fan, Y., Farr, B. F., Fazi, D., Fehrmann, H., Feldbaum, D., Ferrante, I., Fidecaro, F., Finn, L. S., Fiori, I., Flaminio, R., Flanigan, M., Foley, S., Forsi, E., Forte, L. A., Fotopoulos, N., Fournier, J. D., Franc, J., Frasca, S., Frasconi, F., Frede, M., Frei, M., Frei, Z., Freise, A., Frey, R., Fricke, T. T., Friedrich, D., Fritschel, P., Frolov, V. V., Fulda, P., Fyffe, M., Galimberti, M., Gammaitoni, L., Garcia, J., Garofoli, J. A., Garufi, F., Gaspar, M. E., Gemme, G., Genin, E., Gennai, A., Ghosh, S., Giaime, J. A., Giampanis, S., Giardina, K. D., Giazotto, A., Gill, C., Goetz, E., Goggin, L. M., Gonzalez, G., Gorodetsky, M. L., Gossler, S., Gouaty, R., Graef, C., Granata, M., Grant, A., Gras, S., Gray, C., R. J. S., Gretarsson, A. M., Greverie, C., Grosso, R., Grote, H., Grunewald, S., Guidi, G. M., Guido, C., Gupta, R., Gustafson, E. K., Gustafson, R., Hage, B., Hallam, J. M., Hammer, D., Hammond, G., Hanks, J., Hanna, C., Hanson, J., Harms, J., Harry, G. M., Harry, I. W., Harstad, E. D., Hartman, M. T., Haughian, K., Hayama, K., Hayau, J. F., Hayler, T., Heefner, J., Heitmann, H., Hello, P., Hendry, M. A., Heng, I. S., Heptonstall, A. W., Herrera, V., Hewitson, M., Hild, S., Hoak, D., Hodge, K. A., Holt, K., Hong, T., Hooper, S., Hosken, D. J., Hough, J., Howell, E. J., Huet, D., Hughey, B., Husa, S., Huttner, S. H., Ingram, D. R., Inta, R., Isogai, T., Ivanov, A., Jaranowski, P., Johnson, W. W., Jones, D. I., Jones, G., Jones, R., Ju, L., Kalmus, P., Kalogera, V., Kandhasamy, S., Kanner, J. B., Katsavounidis, E., Katzman, W., Kawabe, K., Kawamura, S., Kawazoe, F., Kells, W., Kelner, M., Keppel, D. G., Khalaidovski, A., Khalili, F. Y., Khazanov, E. A., Kim, H., Kim, N., King, P. J., Kinzel, D. L., Kissel, J. S., Klimenko, S., Kondrashov, V., Kopparapu, R., Koranda, S., Korth, W. Z., Kowalska, I., Kozak, D., Kringel, V., Krishnamurthy, S., Krishnan, B., Krolak, A., Kuehn, G., Kumar, R., Kwee, P., Landry, M., Lantz, B., Lastzka, N., Lazzarini, A., Leaci, P., Leong, J., Leonor, I., Leroy, N., Letendre, N., Li, J., T. G. F., Liguori, N., Lindquist, P. E., Lockerbie, N. A., Lodhia, D., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lu, P., Luan, J., Lubinski, M., Lueck, H., Lundgren, A. P., Macdonald, E., Machenschalk, B., Macinnis, M., Mageswaran, M., Mailand, K., Majorana, E., Maksimovic, I., Man, N., Mandel, I., Mandic, V., Mantovani, M., Marandi, A., Marchesoni, F., Marion, F., Marka, S., Marka, Z., Maros, E., Marque, J., Martelli, F., Martin, I. W., Martin, R. M., Marx, J. N., Mason, K., Masserot, A., Matichard, F., Matone, L., Matzner, R. A., Mavalvala, N., Mccarthy, R., Mcclelland, D. E., Mcguire, S. C., Mcintyre, G., D. J. A., Meadors, G., Mehmet, M., Meier, T., Melatos, A., Melissinos, A. C., Mendell, G., Mercer, R. A., Merill, L., Meshkov, S., Messenger, C., Meyer, M. S., Miao, H., Michel, C., Milano, L., Miller, J., Minenkov, Y., Mino, Y., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Miyakawa, O., Moe, B., Moesta, P., Mohan, M., Mohanty, S. D., S. R. P., Moraru, D., Moreno, G., Morgado, N., Morgia, A., Mosca, S., Moscatelli, V., Mossavi, K., Mours, B., Mow-Lowry, C. M., Mueller, G., Mukherjee, S., Mullavey, A., Mueller-Ebhardt, H., Munch, J., Murray, P. G., Nash, T., Nawrodt, R., Nelson, J., Neri, I., Newton, G., Nishida, E., Nishizawa, A., Nocera, F., Nolting, D., Ochsner, E., J. O'Dell, Ogin, G. H., Oldenburg, R. G., Reilly, B. O., Shaughnessy, R. O., Osthelder, C., Ott, C. D., Ottaway, D. J., Ottens, R. S., Overmier, H., Owen, B. J., Page, A., Pagliaroli, G., Palladino, L., Palomba, C., Pan, Y., Pankow, C., Paoletti, F., Papa, M. A., Parameswaran, A., Pardi, S., Parisi, M., Pasqualetti, A., Passaquieti, R., Passuello, D., Patel, P., Pathak, D., Pedraza, M., Pekowsky, L., Penn, S., Peralta, C., Perreca, A., Persichetti, G., Phelps, M., Pichot, M., Pickenpack, M., Piergiovanni, F., Pietka, M., Pinard, L., Pinto, I. M., Pitkin, M., Pletsch, H. J., Plissi, M. V., Podkaminer, J., Poggiani, R., Poeld, J., Postiglione, F., Prato, M., Predoi, V., Price, L. R., Prijatelj, M., Principe, M., Privitera, S., Prix, R., Prodi, G. A., Prokhorov, L., Puncken, O., Punturo, M., Puppo, P., Quetschke, V., Raab, F. J., Rabeling, D. S., Racz, I., Radkins, H., Raffai, P., Rakhmanov, M., Ramet, C. R., Rankins, B., Rapagnani, P., Raymond, V., Re, V., Redwine, K., Reed, C. M., Reed, T., Regimbau, T., Reid, S., Reitze, D. H., Ricci, F., Riesen, R., Riles, K., Roberts, P., Robertson, N. A., Robinet, F., Robinson, C., Robinson, E. L., Rocchi, A., Roddy, S., Rolland, L., Rollins, J., Romano, J. D., Romano, R., Romie, J. H., Rosinska, D., Roever, C., Rowan, S., Udiger, A. R., Ruggi, P., Ryan, K., Sakata, S., Sakosky, M., Salemi, F., Salit, M., Sammut, L., L. S. de, Sandberg, V., Sannibale, V., Santamaria, L., Santiago-Prieto, I., Santostasi, G., Saraf, S., Sassolas, B., Sathyaprakash, B. S., Sato, S., Satterthwaite, M., Saulson, P. R., Savage, R., Schilling, R., Schlamminger, S., Schnabel, R., R. M. S., Schulz, B., Schutz, B. F., Schwinberg, P., Scott, J., Scott, S. M., Searle, A. C., Seifert, F., Sellers, D., Sengupta, A. S., Sentenac, D., Sergeev, A., Shaddock, D. A., Shaltev, M., Shapiro, B., Shawhan, P., Weerathunga, T. S., Shoemaker, D. H., Sibley, A., Siemens, X., Sigg, D., Singer, A., Singer, L., Sintes, A. M., Skelton, G., B. J. J., Slutsky, J., Smith, J. R., Smith, M. R., Smith, N. D., Smith, R., Somiya, K., Sorazu, B., Soto, J., Speirits, F. C., Sperandio, L., Stefszky, M., Stein, A. J., Steinlechner, J., Steinlechner, S., Steplewski, S., Stochino, A., Stone, R., Strain, K. A., Strigin, S., Stroeer, A. S., Sturani, R., Stuver, A. L., Summerscales, T. Z., Sung, M., Susmithan, S., Sutton, P. J., Swinkels, B., Szokoly, G. P., Tacca, M., Talukder, D., Tanner, D. B., Tarabrin, S. P., Taylor, J. R., Taylor, R., Thomas, P., Thorne, K. A., Thorne, K. S., Thrane, E., Thuering, A., Titsler, C., Tokmakov, K. V., Toncelli, A., Tonelli, M., Torre, O., Torres, C., Torrie, C. I., Tournefier, E., Travasso, F., Traylor, G., Trias, M., Tseng, K., Turner, L., Ugolini, D., Urbanek, K., Vahlbruch, H., Vaishnav, B., Vajente, G., Vallisneri, M., J. F. J., Den, C. V., S. v. der, M. V. van, A. A. van, Vass, S., Vasuth, M., Vaulin, R., Vavoulidis, M., Vecchio, A., Vedovato, G., Veitch, J., Veitch, P. J., Veltkamp, C., Verkindt, D., Vetrano, F., Vicere, A., Villar, A. E., Vinet, J. Y., Vocca, H., Vorvick, C., Vyachanin, S. P., Waldman, S. J., Wallace, L., Wanner, A., Ward, R. L., Was, M., Wei, P., Weinert, M., Weinstein, A. J., Weiss, R., Wen, L., Wen, S., Wessels, P., West, M., Westphal, T., Wette, K., Whelan, J. T., Whitcomb, S. E., White, D., Whiting, B. F., Wilkinson, C., Willems, P. A., Williams, H. R., Williams, L., Willke, B., Winkelmann, L., Winkler, W., Wipf, C. C., Wiseman, A. G., Woan, G., Wooley, R., Worden, J., Yablon, J., Yakushin, I., Yamamoto, H., Yamamoto, K., Yang, H., Yeaton-Massey, D., Yoshida, S., Yu, P., Yvert, M., Zanolin, M., Zhang, L., Zhang, Z., Zhao, C., Zotov, N., Zucker, M. E., Zweizig, J., Aptekar, R. L., Boynton, W. V., Briggs, M. S., Cline, T. L., Connaughton, V., Frederiks, D. D., Gehrels, N., Goldsten, J. O., Golovin, D., A. J. van, Hurley, K. C., Kaneko, Y., Kienlin, A. V., Kouveliotou, C., Krimm, H. A., Lin, L., Mitrofanov, I., Ohno, M., Pal Shin, V. D., Rau, A., Sanin, A., Tashiro, M. S., Terada, Y., Yamaoka, K., Collaboration, L. S., Collaboration, V., Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique de Rennes (IPR), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), Laboratoire des matériaux avancés (LMA), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), APC - Gravitation (APC-Gravitation), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), (Astro)-Particles Physics, Student Lab and Education, Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Ecole Supérieure de Physique et de Chimie Industrielles (ESPCI), Mairie de Paris, Laboratoire d'Annecy de Physique des Particules ( LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules ), Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Savoie Mont Blanc ( USMB [Université de Savoie] [Université de Chambéry] ) -Centre National de la Recherche Scientifique ( CNRS ), Physique Corpusculaire et Cosmologie - Collège de France ( PCC ), Collège de France ( CdF ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ) -Collège de France ( CdF ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ) -AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Centre National de la Recherche Scientifique ( CNRS ) -Observatoire de Paris-Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Observatoire de la Côte d'Azur ( OCA ), Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de l'Accélérateur Linéaire ( LAL ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ), Institut de Physique de Rennes ( IPR ), Université de Rennes 1 ( UR1 ), Université de Rennes ( UNIV-RENNES ) -Université de Rennes ( UNIV-RENNES ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire des matériaux avancés ( LMA ), Université Claude Bernard Lyon 1 ( UCBL ), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), APC - Gravitation ( APC-Gravitation ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Max-Planck-Institut für Gravitationsphysik (Albert-Einstein-Institut), Max-Planck-Institut-Max-Planck-Institut, Ecole Supérieure de Physique et de Chimie Industrielles ( ESPCI ), The LIGO Scientific Collaboration, The Virgo Collaboration, F., Acernese, F., Barone, Calloni, Enrico, DE ROSA, Rosario, L., Di Fiore, Garufi, Fabio, Milano, Leopoldo, S., Mosca, M., Parisi, G., Persichetti, R., Romano, and Pinto, Innocenzo
Subjects: Astrophysics::High Energy Astrophysical Phenomena, SGR 1900+14, FOS: Physical sciences, Astrophysics, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, Magnetar, 01 natural sciences, General Relativity and Quantum Cosmology, [ PHYS.GRQC ] Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], stars: magnetars, Settore FIS/05 - Astronomia e Astrofisica, Pulsar, X-RAY PULSAR, gravitational waves, 0103 physical sciences, QC176, Gravitational waves, Stars, Magnetars, OSCILLATIONS, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Gravitational wave, ORIGIN, MAGNETIZED NEUTRON-STARS, Settore FIS/01 - Fisica Sperimentale, SOFT-GAMMA-REPEATER, Astronomy and Astrophysics, LOCALIZATION, GEO600, LIGO, Magnetic field, Neutron star, 13. Climate action, Space and Planetary Science, DISCOVERY, DISTANCE, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Astrophysics - High Energy Astrophysical Phenomena, GIANT FLARE
Abstract: Soft gamma repeaters (SGRs) and anomalous X-ray pulsars (AXPs) are thought to be magnetars: neutron stars powered by extreme magnetic fields. These rare objects are characterized by repeated and sometimes spectacular gamma-ray bursts. The burst mechanism might involve crustal fractures and excitation of non-radial modes which would emit gravitational waves (GWs). We present the results of a search for GW bursts from six galactic magnetars that is sensitive to neutron star f-modes, thought to be the most efficient GW emitting oscillatory modes in compact stars. One of them, SGR 0501+4516, is likely ~1 kpc from Earth, an order of magnitude closer than magnetars targeted in previous GW searches. A second, AXP 1E 1547.0-5408, gave a burst with an estimated isotropic energy >10^{44} erg which is comparable to the giant flares. We find no evidence of GWs associated with a sample of 1279 electromagnetic triggers from six magnetars occurring between November 2006 and June 2009, in GW data from the LIGO, Virgo, and GEO600 detectors. Our lowest model-dependent GW emission energy upper limits for band- and time-limited white noise bursts in the detector sensitive band, and for f-mode ringdowns (at 1090 Hz), are 3.0x10^{44} d_1^2 erg and 1.4x10^{47} d_1^2 erg respectively, where d_1 = d_{0501} / 1 kpc and d_{0501} is the distance to SGR 0501+4516. These limits on GW emission from f-modes are an order of magnitude lower than any previous, and approach the range of electromagnetic energies seen in SGR giant flares for the first time., 9 pages, 3 figures; v2 minor clarifications and new references
Published: 2011

29. Implications for the Origin of GRB 070201 from LIGO Observations

Author: Abbott, B., Abbott, R., Adhikari, R., Agresti, J., Ajith, P., Allen, B., Amin, R., Anderson, S. B., Anderson, W. G., Arain, M., Araya, M., Armandula, H., Ashley, M., Aston, S., Aufmuth, P., Aulbert, C., Babak, S., Ballmer, S., Bantilan, H., Barish, B. C., Barker, C., Barker, D., Barr, B., Barriga, P., Barton, M. A., Bayer, K., Betzwieser, J., Beyersdorf, P. T., Bhawal, B., Bilenko, I. A., Billingsley, G., Biswas, R., Black, E., Blackburn, K., Blackburn, L., Blair, D., Bland, B., Bogenstahl, J., Bogue, L., Bork, R., Boschi, V., Bose, S., Brady, P. R., Braginsky, V. B., Brau, J. E., Brinkmann, M., Brooks, A., Brown, D. A., Bullington, A., Bunkowski, A., Buonanno, A., Burmeister, O., Busby, D., Byer, R. L., Cadonati, L., Cagnoli, G., Camp, J. B., Cannizzo, J., Cannon, K., Cantley, C. A., Cao, J., Cardenas, L., Castaldi, G., Cepeda, C., Chalkley, E., Charlton, P., Chatterji, S., Chelkowski, S., Chen, Y., Chiadini, Francesco, Christensen, N., Clark, J., Cochrane, P., Cokelaer, T., Coldwell, R., Conte, Roberto, Cook, D., Corbitt, T., Coyne, D., Creighton, J. D. E., Croce, R. P., Crooks, D. R. M., Cruise, A. M., Cumming, A., Dalrymple, J., D'Ambrosio, E., Danzmann, K., Davies, G., Debra, D., Degallaix, J., Degree, M., Demma, T., Dergachev, V., Desai, S., Desalvo, R., Dhurandhar, S., Díaz, M., Dickson, J., Di Credico, A., Diederichs, G., Dietz, A., Doomes, E. E., Drever, R. W. P., Dumas, J. C., Dupuis, R. J., Dwyer, J. G., Ehrens, P., Espinoza, E., Etzel, T., Evans, M., Evans, T., Fairhurst, S., Fan, Y., Fazi, D., Fejer, M. M., Finn, L. S., Fiumara, V., Fotopoulos, N., Franzen, A., Franzen, K. Y., Freise, A., Frey, R., Fricke, T., Fritschel, P., Frolov, V. V., Fyffe, M., Galdi, V., Garofoli, J., Gholami, I., Giaime, J. A., Giampanis, S., Giardina, K. D., Goda, K., Goetz, E., Goggin, L. M., González, G., Gossler, S., Grant, A., Gras, S., Gray, C., Gray, M., Greenhalgh, J., Gretarsson, A. M., Grosso, R., Grote, H., Grunewald, S., Guenther, M., Gustafson, R., Hage, B., Hammer, D., Hanna, C., Hanson, J., Harms, J., Harry, G., Harstad, E., Hayler, T., Heefner, J., Heng, I. S., Heptonstall, A., Heurs, M., Hewitson, M., Hild, S., Hirose, E., Hoak, D., Hosken, D., Hough, J., Hoyland, D., Huttner, S. H., Ingram, D., Innerhofer, E., Ito, M., Itoh, Y., Ivanov, A., Johnson, B., Johnson, W. W., Jones, D. I., Jones, G., Jones, R., Ju, L., Kalmus, P., Kalogera, V., Kasprzyk, D., Katsavounidis, E., Kawabe, K., Kawamura, S., Kawazoe, F., Kells, W., Keppel, D. G., Khalili, F. Y. a., Kim, C., King, P., Kissel, J. S., Klimenko, S., Kokeyama, K., Kondrashov, V., Kopparapu, R. K., Kozak, D., Krishnan, B., Kwee, P., Lam, P. K., Landry, M., Lantz, B., Lazzarini, A., Lei, M., Leiner, J., Leonhardt, V., Leonor, I., Libbrecht, K., Lindquist, P., Lockerbie, N. A., Longo, Maurizio, Lormand, M., Lubinski, M., Lück, H., Machenschalk, B., Macinnis, M., Mageswaran, M., Mailand, K., Malec, M., Mandic, V., Marano, Stefano, Márka, S., Markowitz, J., Maros, E., Martin, I., Marx, J. N., Mason, K., Matone, L., Matta, Vincenzo, Mavalvala, N., Mccarthy, R., Mcclelland, D. E., Mcguire, S. C., Mchugh, M., Mckenzie, K., Mcwilliams, S., Meier, T., Melissinos, A., Mendell, G., Mercer, R. A., Meshkov, S., Messenger, C. J., Meyers, D., Mikhailov, E., Mitra, S., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Miyakawa, O., Mohanty, S., Moreno, G., Mossavi, K., Mowlowry, C., Moylan, A., Mudge, D., Mueller, G., Mukherjee, S., Müller Ebhardt, H., Munch, J., Murray, P., Myers, E., Myers, J., Nash, T., Newton, G., Nishizawa, A., Numata, K., O'Reilly, B., O'Shaughnessy, R., Ottaway, D. J., Overmier, H., Owen, B. J., Pan, Y., Papa, M. A., Parameshwaraiah, V., Patel, P., Pedraza, M., Penn, S., Pierro, V., Pinto, I. M., Pitkin, M., Pletsch, H., Plissi, M. V., Postiglione, Fabio, Prix, R., Quetschke, V., Raab, F., Rabeling, D., Radkins, H., Rahkola, R., Rainer, N., Rakhmanov, M., Ramsunder, M., Ray Majumder, S., Re, V., Rehbein, H., Reid, S., Reitze, D. H., Ribichini, L., Riesen, R., Riles, K., Rivera, B., Robertson, N. A., Robinson, C., Robinson, E. L., Roddy, S., Rodriguez, A., Rogan, A. M., Rollins, J., Romano, J. D., Romie, J., Route, R., Rowan, S., Rüdiger, A., Ruet, L., Russell, P., Ryan, K., Sakata, S., Samidi, M., Sancho, de la Jordana L., Sandberg, V., Sannibale, V., Saraf, S., Sarin, P., Sathyaprakash, B. S., Sato, S., Saulson, P. R., Savage, R., Savov, P., Schediwy, S., Schilling, R., Schnabel, R., Schofield, R., Schutz, B. F., Schwinberg, P., Scott, S. M., Searle, A. C., Sears, B., Seifert, F., Sellers, D., Sengupta, A. S., Shawhan, P., Shoemaker, D. H., Sibley, A., Siemens, X., Sigg, D., Sinha, S., Sintes, A. M., Slagmolen, B. J. J., Slutsky, J., Smith, J. R., Smith, M. R., Somiya, K., Strain, K. A., Strom, D. M., Stuver, A., Summerscales, T. Z., Sun, K. X., Sung, M., Sutton, P. J., Takahashi, H., Tanner, D. B., Taylor, R., Thacker, J., Thorne, K. A., Thorne, K. S., Thüring, A., Tokmakov, K. V., Torres, C., Torrie, C., Traylor, G., Trias, M., Tyler, W., Ugolini, D., Urbanek, K., Vahlbruch, H., Vallisneri, M., Van Den Broeck, C., Varvella, M., Vass, S., Vecchio, A., Veitch, J., Veitch, P., Villar, A., Vorvick, C., Vyachanin, S. P., Waldman, S. J., Wallace, L., Ward, H., Ward, R., Watts, K., Weidner, A., Weinert, M., Weinstein, A., Weiss, R., Wen, S., Wette, K., Whelan, J. T., Whitcomb, S. E., Whiting, B. F., Wilkinson, C., Willems, P. A., Williams, L., Willke, B., Wilmut, I., Winkler, W., Wipf, C. C., Wise, S., Wiseman, A. G., Woan, G., Woods, D., Wooley, R., Worden, J., Wu, W., Yakushin, I., Yamamoto, H., Yan, Z., Yoshida, S., Yunes, N., Zanolin, M., Zhang, J., Zhang, L., Zhao, C., Zotov, N., Zucker, M., zur Mühlen, H., Zweizig, J., Hurley, K. C., LSC Collaboration, The, Castaldi, G., Galdi, V., Pierro, V., and Pinto, I. M.
Subjects: Physics, Spiral galaxy, Andromeda Galaxy, Gravitational wave, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, General Relativity and Quantum Cosmology (gr-qc), LIGO, General Relativity and Quantum Cosmology, Black hole, Neutron star, Space and Planetary Science, Sky, Astrophysics::Solar and Stellar Astrophysics, Gamma-ray burst, Astrophysics::Galaxy Astrophysics, media_common, QB
Abstract: We analyzed the available LIGO data coincident with GRB 070201, a short duration hard spectrum gamma-ray burst whose electromagnetically determined sky position is coincident with the spiral arms of the Andromeda galaxy (M31). Possible progenitors of such short hard GRBs include mergers of neutron stars or a neutron star and black hole, or soft gamma-ray repeater (SGR) flares. These events can be accompanied by gravitational-wave emission. No plausible gravitational wave candidates were found within a 180 s long window around the time of GRB 070201. This result implies that a compact binary progenitor of GRB 070201, with masses in the range 1 M_sun < m_1 < 3 M_sun and 1 M_sun < m_2 < 40 M_sun, located in M31 is excluded at >99% confidence. Indeed, if GRB 070201 were caused by a binary neutron star merger, we find that D < 3.5 Mpc is excluded, assuming random inclination, at 90% confidence. The result also implies that an unmodeled gravitational wave burst from GRB 070201 most probably emitted less than 4.4 x 10^(-4) M_sun c^2 (7.9 x 10^(50) ergs) in any 100 ms long period within the signal region if the source was in M31 and radiated isotropically at the same frequency as LIGO's peak sensitivity (f ~ 150 Hz). This upper limit does not exclude current models of SGRs at the M31 distance., 10 pages 5 figures 1 table to be submitted to ApJ Changes after GWIC review period: minor corrections, typographical tweaks
Published: 2007
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30. Search for gravitational waves associated with gamma-ray bursts during Ligo science run 6 and Virgo science runs 2 and 3

Author: Chow, Jong, Chua, Sheon, Inta, Ra, Lam, Ping Koy, McClelland, David, Miller, John, Mow-Lowry, C, Mullavey, Adam, Nguyen, Thanh, Scott, Susan M, Zhao, Chunnong, Wang, Xiaofeng, Hurley, K C, Shaddock, Daniel, Slagmolen, Bram, Stefszky, Michael, Wade, Andrew, Abadie, J, Abbott, B, Adhikari, A, Adhikari, Rana, Arai, Koji, Blackburn, James Kent, Patel, P, Wallace, L, Weinstein, A, Willems, P, Acernese, F, Adams, C, Allen, B, Anderson, WG, Arain, M, Aston, S, Barone, F, Bartos, I, Basti, A, Beker, M G, Beyersdorf, P T, Blair, David Gerald, Blom, M, Bose, S, Brau, J E, Bulten, H.J., Byer, Robert L, Cao, J, Charlton, Philip, Christensen, N, Chung, C. T.Y., Conte, R., Coward, D, Danilishin, S L, Dooley, Katherine L, Dumas, J-C, Factourovich, M, Fairhurst, S, Fan, Y, Finn, Lee, Fricke, Tobin T, Frolov, V, Gehrels, N, Genin, E, Giaime, J, Gras, S, Greenhalgh, R. J. S., Gustafson, R, Hammer, D, Jones, D I, Kawabe, Keita, Khazanov, E, Landry, M, Lockerbie, N.A., Mandic, V., Meadors, G.D., Melatos, Andrew, Melissinos, A, Mendell, G, Mitrofanov, V P, Mueller, Guido, Munch, Jesper, Owen, Benjamin, Penn, S, Reed, C M, Reitze, D, Riles, K, Sammut, L, Sathyaprakash, B, Saulson, P, Savage, R, Schofield, R, Schwinberg, P, Sigg, D, Sintes, A, Strigin, S, Summerscales, T.Z., Susmithan, S, Talukder, D, Tanner, D B, Veitch, Peter John, Vinet, J-Y, Vorvick, C, Waldman, S, Chow, Jong, Chua, Sheon, Inta, Ra, Lam, Ping Koy, McClelland, David, Miller, John, Mow-Lowry, C, Mullavey, Adam, Nguyen, Thanh, Scott, Susan M, Zhao, Chunnong, Wang, Xiaofeng, Hurley, K C, Shaddock, Daniel, Slagmolen, Bram, Stefszky, Michael, Wade, Andrew, Abadie, J, Abbott, B, Adhikari, A, Adhikari, Rana, Arai, Koji, Blackburn, James Kent, Patel, P, Wallace, L, Weinstein, A, Willems, P, Acernese, F, Adams, C, Allen, B, Anderson, WG, Arain, M, Aston, S, Barone, F, Bartos, I, Basti, A, Beker, M G, Beyersdorf, P T, Blair, David Gerald, Blom, M, Bose, S, Brau, J E, Bulten, H.J., Byer, Robert L, Cao, J, Charlton, Philip, Christensen, N, Chung, C. T.Y., Conte, R., Coward, D, Danilishin, S L, Dooley, Katherine L, Dumas, J-C, Factourovich, M, Fairhurst, S, Fan, Y, Finn, Lee, Fricke, Tobin T, Frolov, V, Gehrels, N, Genin, E, Giaime, J, Gras, S, Greenhalgh, R. J. S., Gustafson, R, Hammer, D, Jones, D I, Kawabe, Keita, Khazanov, E, Landry, M, Lockerbie, N.A., Mandic, V., Meadors, G.D., Melatos, Andrew, Melissinos, A, Mendell, G, Mitrofanov, V P, Mueller, Guido, Munch, Jesper, Owen, Benjamin, Penn, S, Reed, C M, Reitze, D, Riles, K, Sammut, L, Sathyaprakash, B, Saulson, P, Savage, R, Schofield, R, Schwinberg, P, Sigg, D, Sintes, A, Strigin, S, Summerscales, T.Z., Susmithan, S, Talukder, D, Tanner, D B, Veitch, Peter John, Vinet, J-Y, Vorvick, C, and Waldman, S
Abstract: We present the results of a search for gravitational waves associated with 154 gamma-ray bursts (GRBs) that were detected by satellite-based gamma-ray experiments in 2009-2010, during the sixth LIGO science run and the second and third Virgo science runs. We perform two distinct searches: a modeled search for coalescences of either two neutron stars or a neutron star and black hole, and a search for generic, unmodeled gravitational-wave bursts. We find no evidence for gravitational-wave counterparts, either with any individual GRB in this sample or with the population as a whole. For all GRBs we place lower bounds on the distance to the progenitor, under the optimistic assumption of a gravitational-wave emission energy of 10 -2 M ⊙ c 2 at 150 Hz, with a median limit of 17Mpc. For short-hard GRBs we place exclusion distances on binary neutron star and neutron-star-black-hole progenitors, using astrophysically motivated priors on the source parameters, with median values of 16Mpc and 28Mpc, respectively. These distance limits, while significantly larger than for a search that is not aided by GRB satellite observations, are not large enough to expect a coincidence with a GRB. However, projecting these exclusions to the sensitivities of Advanced LIGO and Virgo, which should begin operation in 2015, we find that the detection of gravitational waves associated with GRBs will become quite possible.
Published: 2012

31. Search for gravitational wave bursts from six magnetars

Author: Chua, Sheon, Inta, Ra, McClelland, David, Mow-Lowry, C, Mullavey, Adam, Satterthwaite, Matthew, Scott, Susan M, Shaddock, Daniel, Slagmolen, Bram, Stefszky, Michael, Abadie, J, Abbott, B, Adhikari, R, Anderson, S B, Araya, M, Black, E, Blackburn, James Kent, Heefner, J, Hough, J, Lindquist, P, LIGO , Scientific Collaboration (700 Scientists), Hurley, K C, Ivanov, A, Chua, Sheon, Inta, Ra, McClelland, David, Mow-Lowry, C, Mullavey, Adam, Satterthwaite, Matthew, Scott, Susan M, Shaddock, Daniel, Slagmolen, Bram, Stefszky, Michael, Abadie, J, Abbott, B, Adhikari, R, Anderson, S B, Araya, M, Black, E, Blackburn, James Kent, Heefner, J, Hough, J, Lindquist, P, LIGO , Scientific Collaboration (700 Scientists), Hurley, K C, and Ivanov, A
Abstract: Soft gamma repeaters (SGRs) and anomalous X-ray pulsars (AXPs) are thought to be magnetars: neutron stars powered by extreme magnetic fields. These rare objects are characterized by repeated and sometimes spectacular gamma-ray bursts. The burst mechanism
Published: 2011

32. The broad-lined Type Ic supernova 2003jd

Author: Valenti, S, Benetti, Stefano, Cappellaro, Enrico, Patat, Ferdinando, Mazzali, Paolo A, Turatto, Massimo, Hurley, K C, Maeda, Keiichi, Gal-Yam, Avishay, Foley, Ryan, Filippenko, Alexei, Salvo, Maria, Schmidt, Brian, Valenti, S, Benetti, Stefano, Cappellaro, Enrico, Patat, Ferdinando, Mazzali, Paolo A, Turatto, Massimo, Hurley, K C, Maeda, Keiichi, Gal-Yam, Avishay, Foley, Ryan, Filippenko, Alexei, Salvo, Maria, and Schmidt, Brian
Abstract: The results of a worldwide coordinated observational campaign on the broad-lined Type Ic supernova (SN Ic) 2003jd are presented. In total, 74 photometric data points and 26 spectra were collected using 11 different telescopes. SN 2003jd is one of the most luminous SN Ic ever observed. A comparison with other Type Ic supernovae (SNe Ic) confirms that SN 2003jd represents an intermediate case between broad-line events (2002ap, 2006aj) and highly energetic SNe (1997ef, 1998bw, 2003dh, 2003lw), with an ejected mass of Mej = 3.0 ± 1 M⊙ and a kinetic energy of Ek(tot) = 7+3-2 × 1051 erg. SN 2003jd is similar to SN 1998bw in terms of overall luminosity, but it is closer to SNe 2006aj and 2002ap in terms of light-curve shape and spectral evolution. The comparison with other SNe Ic suggests that the V-band light curves of SNe Ic can be partially homogenized by introducing a time-stretch factor. Finally, because of the similarity of SN 2003jd to the SN 2006aj/XRF 060218 event, we discuss the possible connection of SN 2003jd with a gamma-ray burst (GRB). Journal compilation
Published: 2008

33. Search for Gravitational-Wave Bursts from Soft Gamma Repeaters

Author: Abbott, B, Abbott, Robert, Adhikari, Rana, Ajith, P, Allen, B, Allen, G, Amin, R, Anderson, S B, Anderson, W G, Anderson, WG, Dickson, James, Gray, Malcolm, Lam, Ping Koy, McClelland, David, McKenzie, Kirk, Mow-Lowry, C, Rabeling, David, Scott, Susan M, Searle, Antony, Slagmolen, Bram, Wette, Karl, Heefner, J, Hosken, Dave, Hough, J, Hurley, K C, Ivanov, A, Abbott, B, Abbott, Robert, Adhikari, Rana, Ajith, P, Allen, B, Allen, G, Amin, R, Anderson, S B, Anderson, W G, Anderson, WG, Dickson, James, Gray, Malcolm, Lam, Ping Koy, McClelland, David, McKenzie, Kirk, Mow-Lowry, C, Rabeling, David, Scott, Susan M, Searle, Antony, Slagmolen, Bram, Wette, Karl, Heefner, J, Hosken, Dave, Hough, J, Hurley, K C, and Ivanov, A
Abstract: We present a LIGO search for short-duration gravitational waves (GWs) associated with soft gamma ray repeater (SGR) bursts. This is the first search sensitive to neutron star f modes, usually considered the most efficient GW emitting modes. We find no evidence of GWs associated with any SGR burst in a sample consisting of the 27 Dec. 2004 giant flare from SGR 1806-20 and 190 lesser events from SGR 1806-20 and SGR 1900+14. The unprecedented sensitivity of the detectors allows us to set the most stringent limits on transient GW amplitudes published to date. We find upper limit estimates on the model-dependent isotropic GW emission energies (at a nominal distance of 10 kpc) between 3×1045 and 9×1052 erg depending on waveform type, detector antenna factors and noise characteristics at the time of the burst. These upper limits are within the theoretically predicted range of some SGR models.
Published: 2008

34. Infrared observations of soft gamma repeaters

Author: Paradijs, J., Waters, L. B. F. M., Paul Groot, Kouveliotou, C., Smith, I. A., Hurley, K. C., Schultz, A. S. B., Wallyn, P., Telesco, C., Hooft, F., Bontekoe, T. R., Kester, D. J. M., and High Energy Astrophys. & Astropart. Phys (API, FNWI)
Published: 1996

35. An HST Search for Supernovae Accompanying X-Ray Flashes

Author: Soderberg, A M, Kulkarni, Shrinivas R, Fox, Derek B, Berger, Edo, Price, Paul Antony, Cenko, Stephen B, Howell, D A, Gal-Yam, Avishay, Leonard, D C, Frail, Dale A, Moon, D-S, Chevalier, Roger A, Hamuy, M, Hurley, K C, Kelson, Daniel D, Koviak, K, Krzeminski, W, Kumar, P, MacFadyen, A, McCarthy, P J, Park, H-S, Peterson, Bruce, Phillips, Mark M, Rauch, M, Roth, M, Shectman, Stephen, Soderberg, A M, Kulkarni, Shrinivas R, Fox, Derek B, Berger, Edo, Price, Paul Antony, Cenko, Stephen B, Howell, D A, Gal-Yam, Avishay, Leonard, D C, Frail, Dale A, Moon, D-S, Chevalier, Roger A, Hamuy, M, Hurley, K C, Kelson, Daniel D, Koviak, K, Krzeminski, W, Kumar, P, MacFadyen, A, McCarthy, P J, Park, H-S, Peterson, Bruce, Phillips, Mark M, Rauch, M, Roth, M, and Shectman, Stephen
Abstract: We present the results from a Hubble Space Telescope ACS search for supernovae associated with X-ray flashes 020903, 040701, 040812, and 040916. We find strong evidence that XRF 020903 (z = 0.25) was associated with a SN 1998bw-like supernova and confirm
Published: 2005

36. GRB 010921: Strong Limits on an Underlying Supernova from the Hubble Space Telescope

Author: Price, Paul, Kulkarni, Shrinivas R, Schmidt, Brian, Galama, T J, Bloom, J S, Berger, Edo, Frail, Dale A, Djorgovski, S G, Fox, Derek B, Henden, A A, Klose, S, Harrison, F A, Reichart, D E, Sari, R, Yost, S A, Axelrod, Tim, McCarthy, P J, Holtzman, Jon A, Halpern, J., Kimble, Randy A, Wheeler, J Craig, Chevalier, Roger A, Hurley, K C, Ricker, G R, Costa, E, Frontera, F, Piro, L, Price, Paul, Kulkarni, Shrinivas R, Schmidt, Brian, Galama, T J, Bloom, J S, Berger, Edo, Frail, Dale A, Djorgovski, S G, Fox, Derek B, Henden, A A, Klose, S, Harrison, F A, Reichart, D E, Sari, R, Yost, S A, Axelrod, Tim, McCarthy, P J, Holtzman, Jon A, Halpern, J., Kimble, Randy A, Wheeler, J Craig, Chevalier, Roger A, Hurley, K C, Ricker, G R, Costa, E, Frontera, F, and Piro, L
Abstract: GRB 010921 was the first HETE-2 gamma-ray burst (GRB) to be localized via its afterglow emission. The low redshift of the host galaxy, z = 0.451, prompted us to undertake intensive multicolor observations with the Hubble Space Telescope with the goal of searching for an underlying supernova (SN) component. We do not detect any coincident SN to a limit 1.33 mag fainter than SN 1998bw at 99.7% confidence, making this one of the most sensitive searches for an underlying SN. Analysis of the afterglow data allows us to infer that the GRB was situated behind a net extinction (Milky Way and the host galaxy) of Av ∼ 1.8 mag in the observer frame. Thus, had it not been for such heavy extinction, our data would have allowed us to probe for an underlying SN with brightness approaching those of more typical Type Ib/c SNe.
Published: 2003

37. Detection of a Supernova Signature Associated with GRB 011121

Author: Bloom, J S, Kulkarni, Shrinivas R, Price, Paul, Reichart, D E, Galama, T J, Schmidt, Brian, Frail, Dale A, Berger, Edo, McCarthy, P J, Chevalier, Roger A, Wheeler, J Craig, Halpern, J., Fox, Derek B, Djorgovski, S G, Harrison, F A, Sari, R, Kimble, Randy A, Axelrod, Tim, Holtzman, Jon A, Hurley, K C, Frontera, F, Piro, L, Costa, E, Bloom, J S, Kulkarni, Shrinivas R, Price, Paul, Reichart, D E, Galama, T J, Schmidt, Brian, Frail, Dale A, Berger, Edo, McCarthy, P J, Chevalier, Roger A, Wheeler, J Craig, Halpern, J., Fox, Derek B, Djorgovski, S G, Harrison, F A, Sari, R, Kimble, Randy A, Axelrod, Tim, Holtzman, Jon A, Hurley, K C, Frontera, F, Piro, L, and Costa, E
Abstract: Using observations from an extensive monitoring campaign with the Hubble Space Telescope, we present the detection of an intermediate-time flux excess that is redder in color relative to the afterglow of GRB 011121, currently distinguished as the gamma-ray burst with the lowest known redshift. The red "bump," which exhibits a spectral rollover at ∼7200 A, is well described by a redshifted Type le supernova that occurred approximately at the same time as the gamma-ray burst event. The inferred luminosity is about half that of the bright supernova SN 1998bw. These results serve as compelling evidence for a massive star origin of long-duration gamma-ray bursts. Models that posit a supernova explosion weeks to months preceding the gamma-ray burst event are excluded by these observations. Finally, we discuss the relationship between spherical core-collapse supernovae and gamma-ray bursts.
Published: 2002

38. The Faint Optical Afterglow and Host Galaxy of GRB 020124: Implications for the Nature of Dark Gamma-ray Bursts

Author: Berger, Edo, Kulkarni, Shrinivas R, Bloom, J S, Price, Paul, Fox, Derek B, Frail, Dale A, Axelrod, Tim, Chevalier, Roger A, Colbert, E, Costa, E, Djorgovski, S G, Frontera, F, Galama, T J, Halpern, J., Harrison, F A, Holtzman, Jon A, Hurley, K C, Kimble, Randy A, McCarthy, P J, Piro, L, Reichart, D E, Ricker, G R, Sari, R, Schmidt, Brian, Wheeler, J Craig, Vanderppek, R, Yost, S A, Berger, Edo, Kulkarni, Shrinivas R, Bloom, J S, Price, Paul, Fox, Derek B, Frail, Dale A, Axelrod, Tim, Chevalier, Roger A, Colbert, E, Costa, E, Djorgovski, S G, Frontera, F, Galama, T J, Halpern, J., Harrison, F A, Holtzman, Jon A, Hurley, K C, Kimble, Randy A, McCarthy, P J, Piro, L, Reichart, D E, Ricker, G R, Sari, R, Schmidt, Brian, Wheeler, J Craig, Vanderppek, R, and Yost, S A
Abstract: We present ground-based optical observations of GRB 020124 starting 1.6 hr after the burst, as well as subsequent Very Large Array and Hubble Space Telescope (HST) observations. The optical afterglow of GRB 020124 is one of the faintest afterglows detected to date, and it exhibits a relatively rapid decay, Fv ∝ t-1.60±0.04, followed by further steepening. In addition, a weak radio source was found coincident with the optical afterglow. The HST observations reveal that a positionally coincident host galaxy must be the faintest host to date, R ≳ 29.5 mag. The afterglow observations can be explained by several models requiring little or no extinction within the host galaxy, AVhost ≈ 0-0.9 mag. These observations have significant implications for the interpretation of the so-called dark bursts (bursts for which no optical afterglow is detected), which are usually attributed to dust extinction within the host galaxy. The faintness and relatively rapid decay of the afterglow of GRB 020124, combined with the low inferred extinction, indicate that some dark bursts are intrinsically dim and not dust obscured. Thus, the diversity in the underlying properties of optical afterglows must be observationally determined before substantive inferences can be drawn from the statistics of dark bursts.
Published: 2002

39. GRB 010921: Discovery of the First High Energy Transient Explorer Afterglow

Author: Price, Paul, Kulkarni, Shrinivas R, Berger, Edo, Djorgovski, S G, Frail, Dale A, Mahabal, A, Fox, Derek B, Harrison, F A, Bloom, J S, Yost, S A, Reichart, D E, Henden, A A, Ricker, G R, Van Der Spek, R, Hurley, K C, Atteia, J.-L., Kawai, N, Fenimore, F, Graziani, C, Price, Paul, Kulkarni, Shrinivas R, Berger, Edo, Djorgovski, S G, Frail, Dale A, Mahabal, A, Fox, Derek B, Harrison, F A, Bloom, J S, Yost, S A, Reichart, D E, Henden, A A, Ricker, G R, Van Der Spek, R, Hurley, K C, Atteia, J.-L., Kawai, N, Fenimore, F, and Graziani, C
Abstract: We report the discovery of the optical and radio afterglow of GRB 010921, the first gamma-ray burst afterglow to be found from a localization by the High Energy Transient Explorer satellite. We present optical spectroscopy of the host galaxy, which we find to be a dusty and apparently normal star-forming galaxy at z = 0.451. The unusually steep optical spectral slope of the afterglow can be explained by heavy extinction, Av > 0.5 mag, along the line of sight to the GRB. Dust with similar Av for the host galaxy as a whole appears to be required by the measurement of a Balmer decrement in the spectrum of the host galaxy.
Published: 2002

40. The Unusually Long Duration Gamma-ray Burst GRB 000911: Discovery of the afterglow and host galaxy

Author: Price, Paul, Berger, Edo, Kulkarni, Shrinivas R, Djorgovski, S G, Fox, Derek B, Mahabal, A, Hurley, K C, Bloom, J S, Frail, Dale A, Galama, T J, Harrison, F A, Morrison, Graham Lindsay, Reichart, D E, Yost, S A, Sari, R, Axelrod, Tim, Cline, T, Golenetskii, S, Mazets, E, Schmidt, Brian, Trombka, J, Price, Paul, Berger, Edo, Kulkarni, Shrinivas R, Djorgovski, S G, Fox, Derek B, Mahabal, A, Hurley, K C, Bloom, J S, Frail, Dale A, Galama, T J, Harrison, F A, Morrison, Graham Lindsay, Reichart, D E, Yost, S A, Sari, R, Axelrod, Tim, Cline, T, Golenetskii, S, Mazets, E, Schmidt, Brian, and Trombka, J
Abstract: Of all the well-localized gamma-ray bursts, GRB 000911 has the longest duration (T90 = 500 s) and ranks in the top 1% of BATSE bursts for fluence. Here we report the discovery of the afterglow of this unique burst. In order to simultaneously fit our radio and optical observations, we are required to invoke a model involving a hard electron distribution, p ∼ 1.5, and a jet-break time less than 1.5 days. A spectrum of the host galaxy taken 111 days after the burst reveals a single emission line, interpreted as [011] at a redshift z = 1.0585, and a continuum break that we interpret as the Balmer limit at this redshift. Despite the long 790, the afterglow of GRB 000911 is not unusual in any other way when compared to the set of afterglows studied to date. We conclude that the duration of the GRB plays little part in determining the physics of the afterglow.
Published: 2002

41. Afterglow Upper Limits for Four Short-duration, Hard Spectrum Gamma-ray Bursts

Author: Hurley, K C, Berger, Edo, Castro-Tirado, A J, Castro Ceron, J M, Cline, T, Feroci, M, Frail, Dale A, Frontera, F, Masetti, N, Guidorzi, C, Montanari, E, Hartmann, D H, Henden, A A, Levine, S E, Mazets, E, Golenetskii, S, Frederiks, D, Morrison, Graham Lindsay, Oksanen, A, Moilanen, M, Park, H-S, Price, Paul, Prochaska, J, Trombka, J, Williams, G G, Hurley, K C, Berger, Edo, Castro-Tirado, A J, Castro Ceron, J M, Cline, T, Feroci, M, Frail, Dale A, Frontera, F, Masetti, N, Guidorzi, C, Montanari, E, Hartmann, D H, Henden, A A, Levine, S E, Mazets, E, Golenetskii, S, Frederiks, D, Morrison, Graham Lindsay, Oksanen, A, Moilanen, M, Park, H-S, Price, Paul, Prochaska, J, Trombka, J, and Williams, G G
Abstract: We present interplanetary network localization, spectral, and time history information for four short-duration, hard spectrum gamma-ray bursts, GRB 000607, GRB 001025B, GRB 001204, and GRB 010119. All of these events were followed up with sensitive radio
Published: 2002

42. GRB 080503: IMPLICATIONS OF A NAKED SHORT GAMMA-RAY BURST DOMINATED BY EXTENDED EMISSION

Author: Perley, D. A., primary, Metzger, B. D., additional, Granot, J., additional, Butler, N. R., additional, Sakamoto, T., additional, Ramirez-Ruiz, E., additional, Levan, A. J., additional, Bloom, J. S., additional, Miller, A. A., additional, Bunker, A., additional, Chen, H.-W., additional, Filippenko, A. V., additional, Gehrels, N., additional, Glazebrook, K., additional, Hall, P. B., additional, Hurley, K. C., additional, Kocevski, D., additional, Li, W., additional, Lopez, S., additional, Norris, J., additional, Piro, A. L., additional, Poznanski, D., additional, Prochaska, J. X., additional, Quataert, E., additional, and Tanvir, N., additional
Published: 2009
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43. Broadband Observations of the Afterglow of GRB 000926: Observing the Effect of Inverse Compton Scattering

Author: Harrison, F A, Yost, S A, Sari, R, Berger, Edo, Galama, T J, Holtzman, Jon A, Axelrod, Tim, Bloom, J S, Chevalier, Roger A, Costa, E, Diercks, A, Djorgovski, S G, Frail, Dale A, Frontera, F, Hurley, K C, Kulkarni, Shrinivas R, McCarthy, P J, Piro, L, Pooley, G, Price, Paul, Reichart, D E, Ricker, G R, Shepherd, D, Walter, Fabian, Wheeler, C, Schmidt, Brian, Harrison, F A, Yost, S A, Sari, R, Berger, Edo, Galama, T J, Holtzman, Jon A, Axelrod, Tim, Bloom, J S, Chevalier, Roger A, Costa, E, Diercks, A, Djorgovski, S G, Frail, Dale A, Frontera, F, Hurley, K C, Kulkarni, Shrinivas R, McCarthy, P J, Piro, L, Pooley, G, Price, Paul, Reichart, D E, Ricker, G R, Shepherd, D, Walter, Fabian, Wheeler, C, and Schmidt, Brian
Abstract: GRB 000926 has one of the best-studied afterglows to date, with multiple X-ray observations, as well as extensive multifrequency optical and radio coverage. Broadband afterglow observations, spanning from X-ray to radio frequencies, provide a probe of the density structure of the circumburst medium, as well as of the ejecta energetics, geometry, and physical parameters of the relativistic blast wave resulting from the explosion. We present an analysis of Chandra X-Ray Observatory observations of this event, along with Hubble Space Telescope and radio monitoring data. We combine these data with ground-based optical and IR observations and fit the synthesized afterglow light curve using models where collimated ejecta expand into a surrounding medium. We find that we can explain the broadband light curve with reasonable physical parameters if the cooling is dominated by inverse Compton scattering. For this model, an excess due to inverse Compton scattering appears above the best-fit synchrotron spectrum in the X-ray band. No previous bursts have exhibited this component, and its observation would imply that the GRB exploded in a moderately dense (n ∼ 30 cm-3) medium, consistent with a diffuse interstellar cloud environment.
Published: 2001

44. Multicolor Observations of the GRB 000926 Afterglow

Author: Price, Paul, Harrison, F A, Galama, T J, Reichart, D E, Axelrod, Tim, Berger, Edo, Bloom, J S, Busche, J, Cline, T, Diercks, A, Djorgovski, S G, Frail, Dale A, Gal-Yam, Avishay, Halpern, J., Holtzman, Jon A, Hunt, M, Hurley, K C, Jacoby, B, Kimble, Randy A, Kulkarni, Shrinivas R, Mirabal, N, Morrison, Graham Lindsay, Ofek, Eran O, Pevunova, O, Sari, R, Schmidt, Brian, Turnshek, D, Yost, S A, Price, Paul, Harrison, F A, Galama, T J, Reichart, D E, Axelrod, Tim, Berger, Edo, Bloom, J S, Busche, J, Cline, T, Diercks, A, Djorgovski, S G, Frail, Dale A, Gal-Yam, Avishay, Halpern, J., Holtzman, Jon A, Hunt, M, Hurley, K C, Jacoby, B, Kimble, Randy A, Kulkarni, Shrinivas R, Mirabal, N, Morrison, Graham Lindsay, Ofek, Eran O, Pevunova, O, Sari, R, Schmidt, Brian, Turnshek, D, and Yost, S A
Abstract: We present multicolor light curves of the optical afterglow of gamma-ray burst (GRB) 000926. Beginning ∼1.5 days after the burst, the light curves of this GRB steepen measurably. The existence of such achromatic breaks is usually taken to be an importan
Published: 2001

45. An upper limit to X-ray emission from Saturn

Author: Gilman, D. A, Hurley, K. C, Seward, F. D, Schnopper, H. W, Sullivan, J. D, and Metzger, A. E
Subjects: Lunar And Planetary Exploration
Abstract: X-rays are produced in auroral discharges, and their measurement can serve to characterize the interaction processes responsible for the aurora itself. The existence of auroral activity on Saturn was suggested by the observation of a magnetosphere by Pioneer 11 and confirmed by UV measurements during the Voyager encounters. The detection of X-rays from Jupiter with the Einstein Observatory (HEAO 2) satellite provided the impetus for a subsequent observation of Saturn. No emission was detected. This article presents the upper limit established by the observation and derives an expected emission level assuming X-ray production to be the result of bremsstrahlung from keV electrons precipitating into Saturn's atmosphere. The difference is a factor of 100.
Published: 1986
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46. Advanced techniques for high resolution spectroscopic observations of cosmic gamma-ray sources

Author: Matteson, J. L, Pelling, M. R, Peterson, L. E, Lin, R. P, Anderson, K. A, Pehl, R. H, Hurley, K. C, Vedrenne, G, Sniel, M, and Durouchoux, P
Subjects: Space Radiation
Abstract: An advanced gamma-ray spectrometer that is currently in development is described. It will obtain a sensitivity of 0.0001 ph/sq cm./sec in a 6 hour balloon observation and uses innovative techniques for background reduction and source imaging.
Published: 1985

47. Solar hard X-ray microflares

Author: Lin, R. P, Schwartz, R. A, Kane, S. R, Pelling, R. M, and Hurley, K. C
Subjects: Solar Physics
Abstract: Using balloon-borne instrumentation of very high sensitivity, approximately 25 hard X-ray bursts with peak fluxes of above 7 x 10 to the -3rd/(sq cm s keV) at 20 keV have been detected, in 141 minutes of observation of the sun on June 27, 1980. These hard X-ray microflares last from a few seconds to several tens of seconds and have power-law energy spectra. They are generally accompanied by small soft X-ray bursts, but H-alpha flares and solar radio bursts are reported for only a few of these hard X-ray bursts. The integral number of events varies approximately as the inverse of the peak flux, down to the limits of the measurements. These observations suggest that even very small transient releases of energy by the sun may be primarily nonthermal in character. It is speculated that the energy released in accelerated electrons for these microflares, averaged over time, may contribute significantly to the heating of the active corona.
Published: 1984
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48. The detection of X rays from Jupiter

Author: Metzger, A. E, Luthey, J. L, Gilman, D. A, Hurley, K. C, Schnopper, H. W, Seward, F. D, and Sullivan, J. D
Subjects: Lunar And Planetary Exploration
Abstract: X rays in the energy band 0.2-3.0 keV have been detected coming from both polar regions of Jupiter. The observations were made in 1979 and 1981 by using the imaging proportional counter and high resolution imaging detectors on the Einstein X-ray astronomy satellite. The measured flux density of approximately 0.0006/sq cm-sec at earth corresponds to an X ray luminosity of approximately 4 x 10 to the 9th W in the 0.2- to 3.0-keV energy band. The energy spectrum of the X rays is extremely soft and can be characterized by a power law with an exponent of approximately 2.3. Detector energy resolution is insufficient to distinguish a soft line spectrum from a continuum. However, the shape of the response and the observed X ray power indicate that the source of this auroral emission is not electron bremsstrahlung as on the earth, but is most probably line emission from O and S ions with energies between 0.03 and 4.0 MeV/nucleon precipitating from the outer boundary of the Io plasma torus at L approximately 8.
Published: 1983

49. Persistent X-ray emission from a gamma-ray burst source

Author: Grindlay, J. E, Cline, T, Desai, U. D, Teegarden, B. J, Pizzichini, G, Evans, W. D, Laros, J. G, Hurley, K. C, Niel, M, and Klebesadel, R. W
Subjects: Astrophysics
Abstract: A quiescent X-ray source detected with the Einstein X-ray Observatory in a location consistent with that of an intense gamma ray burst is shown to be also consistent with the location of the 1928 optical transient, the likely optical counterpart of the gamma ray burst source GBS0117-29. The system appears to be underluminous in X-rays by a factor of 10; possible reasons for this are discussed. The observed X-ray flux would require an accretion rate of about 10 to the -14th (d/1 kpc/)-squared solar masses per year, which is probably too low to be consistent with published nuclear flash models for gamma bursts, unless the distance is substantially greater than about 1 kpc or the burst recurrence time is greater than about 50 yrs, or the accretion rate is highly variable. Such a long recurrence time appears to be inconsistent with the detection of the optical burst.
Published: 1982
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50. A new component of hard X-rays in solar flares

Author: Lin, R. P, Schwartz, R. A, Pelling, R. M, and Hurley, K. C
Subjects: Solar Physics
Abstract: High-resolution (approximately 1 keV FWHM) spectral measurements from 13 to 300 keV of a solar flare hard X-ray burst observed on 1980 June 27 by a balloon-borne array of cooled germanium planar detectors are presented. At energies below about 35 keV, a new component of solar flare hard X-rays is identified. This component is characterized by an extremely steep spectrum which fits closely to that from a Maxwellian electron distribution with a maximum temperature of about 34 x 10 to the 6th K and an emission measure of 2.9 x 10 to the 48th per cu cm. This hot isothermal component appears at the peak of the normal power-law-like impulsive X-ray burst component, and it remains isothermal and dominates the X-ray emission below about 30 keV through the decay of the flare event.
Published: 1981
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