Author: "Nousek, J" / Topic: fos: physical sciences - Searchworks@Jio Institute Digital Library Search Results

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29 results on '"Nousek, J"'

1. Swift/UVOT discovery of Swift J221951-484240: a UV luminous ambiguous nuclear transient

Author: Oates, S. R., Kuin, N. P. M., Nicholl, M., Marshall, F., Ridley, E., Boutsia, K., Breeveld, A. A., Buckley, D. A. H., Cenko, S. B., De Pasquale, M., Edwards, P. G., Gromadzki, M., Gupta, R., Laha, S., Morrell, N., Orio, M., Pandey, S. B., Page, M. J., Page, K. L., Parsotan, T., Rau, A., Schady, P., Stevens, J., Brown, P. J., Evans, P. A., Gronwall, C., Kennea, J. A., Klingler, N. J., Siegel, M. H., Tohuvavohu, A., Ambrosi, E., Barthelmy, S. D., Beardmore, A. P., Bernardini, M. G., Bonnerot, C., Campana, S., Caputo, R., Ciroi, S., Cusumano, G., D'Ai, A., D'Avanzo, P., D'Elia, V., Giommi, P., Hartmann, D. H., Krimm, H. A., Malesani, D. B., Melandri, A., Nousek, J. A., O'Brien, P. T., Osborne, J. P., Pagani, C., Palmer, D. M., Perri, M., Racusin, J. L., Sakamoto, T., Sbarufatti, B., Schlieder, J. E., Tagliaferri, G., Troja, E., and Xu, D.
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), FOS: Physical sciences, Astrophysics - High Energy Astrophysical Phenomena
Abstract: We report the discovery of Swift J221951-484240 (hereafter: J221951), a luminous slow-evolving blue transient that was detected by the Neil Gehrels Swift Observatory Ultra-violet/Optical Telescope (Swift/UVOT) during the follow-up of Gravitational Wave alert S190930t, to which it is unrelated. Swift/UVOT photometry shows the UV spectral energy distribution of the transient to be well modelled by a slowly shrinking black body with an approximately constant temperature of T~2.5x10^4 K. At a redshift z=0.5205, J221951 had a peak absolute magnitude of M_u,AB = -23 mag, peak bolometric luminosity L_max=1.1x10^45 erg s^-1 and a total radiated energy of E>2.6x10^52 erg. The archival WISE IR photometry shows a slow rise prior to a peak near the discovery date. Spectroscopic UV observations display broad absorption lines in N V and O VI, pointing toward an outflow at coronal temperatures. The lack of emission in the higher H~Lyman lines, N I and other neutral lines is consistent with a viewing angle close to the plane of the accretion or debris disc. The origin of J221951 can not be determined with certainty but has properties consistent with a tidal disruption event and the turn-on of an active galactic nucleus., 37 pages (25 main + 12 supplementary), submitted to MNRAS
Published: 2023

2. Supplement: Localization and broadband follow-up of the gravitational-wave transient GW150914

Author: Abbott, B. P., Abbott, R., Abbott, T. D., Abernathy, M. R., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R. X., Adya, V. B., Affeldt, C., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, B., Allocca, A., Altin, P. A., Anderson, S. B., Anderson, W. G., Arai, K., Araya, M. C., Arceneaux, C. C., Areeda, J. S., Arnaud, N., Arun, K. G., Ascenzi, S., Ashton, G., Ast, M., Aston, S. M., Astone, P., Aufmuth, P., Aulbert, C., Babak, S., Bacon, P., Bader, M. K. M., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Barthelmy, S., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Batch, J. C., Baune, C., Bavigadda, V., Bazzan, M., Behnke, B., Bejger, M., Bell, A. S., Bell, C. J., Berger, B. K., Bergman, J., Bergmann, G., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhagwat, S., Bhandare, R., Bilenko, I. A., Billingsley, G., Birch, J., Birney, R., Biscans, S., Bisht, A., Bitossi, M., Biwer, C., Bizouard, M. A., Blackburn, J. K., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bock, O., Bodiya, T. P., Boer, M., Bogaert, G., Bogan, C., Bohe, A., Bojtos, P., Bond, C., Bondu, F., Bonnand, R., Boom, B. A., Bork, R., Boschi, V., Bose, S., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Braginsky, V. B., Branchesi, M., Brau, J. E., Briant, T., Brillet, A., Brinkmann, M., Brisson, V., Brockill, P., Brooks, A. F., Brown, D. A., Brown, D. D., Brown, N. M., Buchanan, C. C., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. L., Cadonati, L., Cagnoli, G., Cahillane, C., Bustillo, J. C., Callister, T., Calloni, E., Camp, J. B., Cannon, K. C., Cao, J., Capano, C. D., Capocasa, E., Carbognani, F., Caride, S., Diaz, J. C., Casentini, C., Caudill, S., Cavaglià, M., Cavalier, F., Cavalieri, R., Cella, G., Cepeda, C. B., Baiardi, L. C., Cerretani, G., Cesarini, E., Chakraborty, R., Chalermsongsak, T., Chamberlin, S. J., Chan, M., Chao, S., Charlton, P., Chassande-Mottin, E., Chen, H. Y., Chen, Y., Cheng, C., Chincarini, A., Chiummo, A., Cho, H. S., Cho, M., Chow, J. H., Christensen, N., Chu, Q., Chua, S., Chung, S., Ciani, G., Clara, F., Clark, J. A., Cleva, F., Coccia, E., Cohadon, P. -F, Colla, A., Collette, C. G., Cominsky, L., Constancio, M., Conte, A., Conti, L., Cook, D., Corbitt, T. R., Cornish, N., Corsi, A., Cortese, S., Costa, C. A., Coughlin, M. W., Coughlin, S. B., Coulon, J. -P, Countryman, S. T., Couvares, P., Cowan, E. E., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Craig, K., Creighton, J. D. E., Cripe, J., Crowder, S. G., Cumming, A., Cunningham, L., Cuoco, E., Dal Canton, T., Danilishin, S. L., Antonio de Ugarte Postigo, Danzmann, K., Darman, N. S., Dattilo, V., Dave, I., Daveloza, H. P., Davier, M., Davies, G. S., Daw, E. J., Day, R., Debra, D., Debreczeni, G., Degallaix, J., Laurentis, M., Deléglise, S., Del Pozzo, W., Denker, T., Dent, T., Dereli, H., Dergachev, V., Derosa, R. T., Rosa, R., Desalvo, R., Dhurandhar, S., Díaz, M. C., Di Fiore, L., Di Giovanni, M., Di Lieto, A., Di Pace, S., Di Palma, I., Di Virgilio, A., Dojcinoski, G., Dolique, V., Donovan, F., Dooley, K. L., Doravari, S., Douglas, R., Downes, T. P., Drago, M., Drever, R. W. P., Driggers, J. C., Du, Z., Ducrot, M., Dwyer, S. E., Edo, T. B., Edwards, M. C., Effler, A., Eggenstein, H. -B, Ehrens, P., Eichholz, J., Eikenberry, S. S., Engels, W., Essick, R. C., Etzel, T., Evans, M., Evans, T. M., Everett, R., Factourovich, M., Fafone, V., Fair, H., Fairhurst, S., Fan, X., Fang, Q., Farinon, S., Farr, B., Farr, W. M., Favata, M., Fays, M., Fehrmann, H., Fejer, M. M., Ferrante, I., Ferreira, E. C., Ferrini, F., Fidecaro, F., Fiori, I., Fiorucci, D., Fisher, R. P., Flaminio, R., Fletcher, M., Fournier, J. -D, Franco, S., Frasca, S., Frasconi, F., Frei, Z., Freise, A., Frey, R., Frey, V., Fricke, T. T., Fritschel, P., Frolov, V. V., Fulda, P., Fyffe, M., Gabbard, H. A. G., Gair, J. R., Gammaitoni, L., Gaonkar, S. G., Garufi, F., Gatto, A., Gaur, G., Gehrels, N., Gemme, G., Gendre, B., Genin, E., Gennai, A., George, J., Gergely, L., Germain, V., Ghosh, A., Ghosh, S., Giaime, J. A., Giardina, K. D., Giazotto, A., Gill, K., Glaefke, A., Goetz, E., Goetz, R., Gondan, L., González, G., Castro, J. M. G., Gopakumar, A., Gordon, N. A., Gorodetsky, M. L., Gossan, S. E., Gosselin, M., Gouaty, R., Graef, C., Graff, P. B., Granata, M., Grant, A., Gras, S., Gray, C., Greco, G., Green, A. C., Groot, P., Grote, H., Grunewald, S., Guidi, G. M., Guo, X., Gupta, A., Gupta, M. K., Gushwa, K. E., Gustafson, E. K., Gustafson, R., Hacker, J. J., Hall, B. R., Hall, E. D., Hammond, G., Haney, M., Hanke, M. M., Hanks, J., Hanna, C., Hannam, M. D., Hanson, J., Hardwick, T., Harms, J., Harry, G. M., Harry, I. W., Hart, M. J., Hartman, M. T., Haster, C. -J, Haughian, K., Heidmann, A., Heintze, M. C., Heitmann, H., Hello, P., Hemming, G., Hendry, M., Heng, I. S., Hennig, J., Heptonstall, A. W., Heurs, M., Hild, S., Hoak, D., Hodge, K. A., Hofman, D., Hollitt, S. E., Holt, K., Holz, D. E., Hopkins, P., Hosken, D. J., Hough, J., Houston, E. A., Howell, E. J., Hu, Y. M., Huang, S., Huerta, E. A., Huet, D., Hughey, B., Husa, S., Huttner, S. H., Huynh-Dinh, T., Idrisy, A., Indik, N., Ingram, D. R., Inta, R., Isa, H. N., Isac, J. -M, Isi, M., Islas, G., Isogai, T., Iyer, B. R., Izumi, K., Jacqmin, T., Jang, H., Jani, K., Jaranowski, P., Jawahar, S., Jiménez-Forteza, F., Johnson, W. W., Jones, D. I., Jones, R., Jonker, R. J. G., Ju, L., K, H., Kalaghatgi, C. V., Kalogera, V., Kandhasamy, S., Kang, G., Kanner, J. 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L., Lord, J. E., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lough, J. D., Lück, H., Lundgren, A. P., Luo, J., Lynch, R., Ma, Y., Macdonald, T., Machenschalk, B., Macinnis, M., Macleod, D. M., Magaña-Sandoval, F., Magee, R. M., Mageswaran, M., Majorana, E., Maksimovic, I., Malvezzi, V., Man, N., Mandel, I., Mandic, V., Mangano, V., Mansell, G. L., Manske, M., Mantovani, M., Marchesoni, F., Marion, F., Márka, S., Márka, Z., Markosyan, A. S., Maros, E., Martelli, F., Martellini, L., Martin, I. W., Martin, R. M., Martynov, D. V., Marx, J. N., Mason, K., Masserot, A., Massinger, T. J., Masso-Reid, M., Matichard, F., Matone, L., Mavalvala, N., Mazumder, N., Mazzolo, G., Mccarthy, R., Mcclelland, D. E., Mccormick, S., Mcguire, S. C., Mcintyre, G., Mciver, J., Mcmanus, D. J., Mcwilliams, S. T., Meacher, D., Meadors, G. D., Meidam, J., Melatos, A., Mendell, G., Mendoza-Gandara, D., Mercer, R. A., Merilh, E., Merzougui, M., Meshkov, S., Messenger, C., Messick, C., Meyers, P. 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S., Shaltev, M., Shao, Z., Shapiro, B., Shawhan, P., Sheperd, A., Shoemaker, D. H., Shoemaker, D. M., Siellez, K., Siemens, X., Sigg, D., Silva, A. D., Simakov, D., Singer, A., Singh, A., Singh, R., Singhal, A., Sintes, A. M., Slagmolen, B. J. J., Smith, J. R., Smith, N. D., Smith, R. J. E., Son, E. J., Sorazu, B., Sorrentino, F., Souradeep, T., Srivastava, A. K., Staley, A., Steinke, M., Steinlechner, J., Steinlechner, S., Steinmeyer, D., Stephens, B. C., Stone, R., Strain, K. A., Straniero, N., Stratta, G., Strauss, N. A., Strigin, S., Sturani, R., Stuver, A. L., Summerscales, T. Z., Sun, L., Sutton, P. J., Swinkels, B. L., Szczepańczyk, M. J., Tacca, M., Talukder, D., Tanner, D. B., Tápai, M., Tarabrin, S. P., Taracchini, A., Taylor, R., Theeg, T., Thirugnanasambandam, M. P., Thomas, E. G., Thomas, M., Thomas, P., Thorne, K. A., Thorne, K. S., Thrane, E., Tiwari, S., Tiwari, V., Tokmakov, K. V., Tomlinson, C., Tonelli, M., Torres, C. V., Torrie, C. I., Töyrä, D., Travasso, F., Traylor, G., Trifirò, D., Tringali, M. C., Trozzo, L., Tse, M., Turconi, M., Tuyenbayev, D., Ugolini, D., Unnikrishnan, C. S., Urban, A. L., Usman, S. A., Vahlbruch, H., Vajente, G., Valdes, G., Bakel, N., Beuzekom, M., Den Brand, J. F. J., Den Broeck, C., Vander-Hyde, D. C., Schaaf, L., Heijningen, J. V., Veggel, A. A., Vardaro, M., Vass, S., Vasúth, M., Vaulin, R., Vecchio, A., Vedovato, G., Veitch, J., Veitch, P. J., Venkateswara, K., Verkindt, D., Vetrano, F., Viceré, A., Vinciguerra, S., Vine, D. J., Vinet, J. -Y, Vitale, S., Vo, T., Vocca, H., Vorvick, C., Voss, D., Vousden, W. D., Vyatchanin, S. P., Wade, A. R., Wade, L. E., Wade, M., Walker, M., Wallace, L., Walsh, S., Wang, G., Wang, H., Wang, M., Wang, X., Wang, Y., Ward, R. L., Warner, J., Was, M., Weaver, B., Wei, L. -W, Weinert, M., Weinstein, A. J., Weiss, R., Welborn, T., Wen, L., Weßels, P., Westphal, T., Wette, K., Whelan, J. T., White, D. J., Whiting, B. F., Williams, R. D., Williamson, A. R., Willis, J. L., Willke, B., Wimmer, M. H., Winkler, W., Wipf, C. C., Wittel, H., Woan, G., Worden, J., Wright, J. L., Wu, G., Yablon, J., Yam, W., Yamamoto, H., Yancey, C. C., Yap, M. J., Yu, H., Yvert, M., Zadrożny, A., Zangrando, L., Zanolin, M., Zendri, J. -P, Zevin, M., Zhang, F., Zhang, L., Zhang, M., Zhang, Y., Zhao, C., Zhou, M., Zhou, Z., Zhu, X. J., Zucker, M. E., Zuraw, S. E., Zweizig, J., Ligo, For The Scientific Collaboration, the Virgo Collaboration, Allison, J., Bannister, K., Bell, M. E., Chatterjee, S., Chippendale, A. P., Edwards, P. G., Harvey-Smith, L., Heywood, Ian, Hotan, A., Indermuehle, B., Marvil, J., Mcconnell, D., Murphy, T., Popping, A., Reynolds, J., Sault, R. J., Voronkov, M. A., Whiting, M. T., Australian Square Kilometer Array Pathfinder, For The, Collaboration, Castro-Tirado, A. J., Cunniffe, R., Jelínek, M., Tello, J. C., Oates, S. 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F., Estrada, J., Evrard, A. E., Fernandez, E., Finley, D. A., Flaugher, B., Foley, R. J., Fong, W. -F, Fosalba, P., Fox, D. B., Frieman, J., Fryer, C. L., Gaztanaga, E., Gerdes, D. W., Goldstein, D. A., Gruen, D., Gruendl, R. A., Gutierrez, G., Herner, K., Honscheid, K., James, D. J., Johnson, M. D., Johnson, M. W. G., Karliner, I., Kasen, D., Kent, S., Kessler, R., Kim, A. G., Kind, M. C., Kuehn, K., Kuropatkin, N., Lahav, O., Li, T. S., Lima, M., Lin, H., Maia, M. A. G., Margutti, R., Marriner, J., Martini, P., Matheson, T., Melchior, P., Metzger, B. D., Miller, C. J., Miquel, R., Neilsen, E., Nichol, R. C., Nord, B., Nugent, P., Ogando, R., Petravick, D., Plazas, A. A., Quataert, E., Roe, N., Romer, A. K., Roodman, A., Rosell, A. C., Rykoff, E. S., Sako, M., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Scolnic, D., Sevilla-Noarbe, I., Sheldon, E., Smith, N., Smith, R. C., Soares-Santos, M., Sobreira, F., Stebbins, A., Suchyta, E., Swanson, M. E. C., Tarle, G., Thaler, J., Thomas, D., Thomas, R. C., Tucker, D. L., Vikram, V., Walker, A. R., Wechsler, R. H., Wester, W., Yanny, B., Zuntz, J., Dark Energy Survey, For The, Gw-Em, The Dark Energy Camera Collaborations, Connaughton, V., Burns, E., Goldstein, A., Briggs, M. S., Hui, C. M., Jenke, P., Wilson-Hodge, C. A., Bhat, P. N., Bissaldi, E., Cleveland, W., Fitzpatrick, G., Giles, M. M., Gibby, M. H., Greiner, J., Kienlin, A., Kippen, R. M., Mcbreen, S., Mailyan, B., Meegan, C. A., Paciesas, W. S., Preece, R. D., Roberts, O., Sparke, L., Stanbro, M., Toelge, K., Veres, P., Yu, H. -F, Blackburn, L., Gbm, For The Fermi Collaboration, Ackermann, M., Ajello, M., Albert, A., Anderson, B., Atwood, W. B., Axelsson, M., Baldini, L., Barbiellini, G., Bastieri, D., Bellazzini, R., Blandford, R. D., Bloom, E. D., Bonino, R., Bottacini, E., Brandt, T. J., Bruel, P., Buson, S., Caliandro, G. A., Cameron, R. A., Caragiulo, M., Caraveo, P. A., Cavazzuti, E., Charles, E., Chekhtman, A., Chiang, J., Chiaro, G., Ciprini, S., Cohen-Tanugi, J., Cominsky, L. R., Costanza, F., Cuoco, A., D Ammando, F., Palma, F., Desiante, R., Digel, S. W., Di Lalla, N., Di Mauro, M., Di Venere, L., Domínguez, A., Drell, P. S., Dubois, R., Favuzzi, C., Ferrara, E. C., Franckowiak, A., Fukazawa, Y., Funk, S., Fusco, P., Gargano, F., Gasparrini, D., Giglietto, N., Giommi, P., Giordano, F., Giroletti, M., Glanzman, T., Godfrey, G., Gomez-Vargas, G. A., Green, D., Grenier, I. A., Grove, J. E., Guiriec, S., Hadasch, D., Harding, A. K., Hays, E., Hewitt, J. W., Hill, A. B., Horan, D., Jogler, T., Jóhannesson, G., Johnson, A. S., Kensei, S., Kocevski, D., Kuss, M., La Mura, G., Larsson, S., Latronico, L., Li, J., Li, L., Longo, F., Loparco, F., Lovellette, M. N., Lubrano, P., Magill, J., Maldera, S., Manfreda, A., Marelli, M., Mayer, M., Mazziotta, M. N., Mcenery, J. E., Meyer, M., Michelson, P. F., Mirabal, N., Mizuno, T., Moiseev, A. A., Monzani, M. E., Moretti, E., Morselli, A., Moskalenko, I. V., Negro, M., Nuss, E., Ohsugi, T., Omodei, N., Orienti, M., Orlando, E., Ormes, J. F., Paneque, D., Perkins, J. S., Pesce-Rollins, M., Piron, F., Pivato, G., Porter, T. A., Racusin, J. L., Rainò, S., Rando, R., Razzaque, S., Reimer, A., Reimer, O., Salvetti, D., Saz Parkinson, P. M., Sgrò, C., Simone, D., Siskind, E. J., Spada, F., Spandre, G., Spinelli, P., Suson, D. J., Tajima, H., Thayer, J. B., Thompson, D. J., Tibaldo, L., Torres, D. F., Troja, E., Uchiyama, Y., Venters, T. M., Vianello, G., Wood, K. S., Wood, M., Zhu, S., Zimmer, S., Lat, For The Fermi Collaboration, Brocato, E., Cappellaro, E., Covino, S., Grado, A., Nicastro, L., Palazzi, E., Pian, E., Amati, L., Antonelli, L. A., Capaccioli, M., D Avanzo, P., D Elia, V., Getman, F., Giuffrida, G., Iannicola, G., Limatola, L., Lisi, M., Marinoni, S., Marrese, P., Melandri, A., Piranomonte, S., Possenti, A., Pulone, L., Rossi, A., Stamerra, A., Stella, L., Testa, V., Tomasella, L., Yang, S., for the GRAvitational Wave Inaf TeAm, Bazzano, A., Bozzo, E., Brandt, S., Courvoisier, T. J. -L, Ferrigno, C., Hanlon, L., Kuulkers, E., Laurent, P., Mereghetti, S., Roques, J. P., Savchenko, V., Ubertini, P., Integral, For The Collaboration, Kasliwal, M. M., Singer, L. P., Cao, Y., Duggan, G., Kulkarni, S. R., Bhalerao, V., Miller, A. A., Barlow, T., Bellm, E., Manulis, I., Rana, J., Laher, R., Masci, F., Surace, J., Rebbapragada, U., Sistine, A., Sesar, B., Perley, D., Ferreti, R., Prince, T., Kendrick, R., Horesh, A., Intermediate Palomar Transient Factory, For The, Hurley, K., Golenetskii, S. V., Aptekar, R. L., Frederiks, D. D., Svinkin, D. S., Rau, A., Zhang, X., Smith, D. M., Cline, T., Krimm, H., Interplanetary Network, For The, Abe, F., Doi, M., Fujisawa, K., Kawabata, K. S., Morokuma, T., Motohara, K., Tanaka, M., Ohta, K., Yanagisawa, K., Yoshida, M., J-Gem, For The Collaboration, Baltay, C., Rabinowitz, D., Ellman, N., Rostami, S., La Silla--Quest Survey, For The, Bersier, D. F., Bode, M. F., Collins, C. A., Copperwheat, C. M., Darnley, M. J., Galloway, D. K., Gomboc, A., Kobayashi, S., Mazzali, P., Mundell, C. G., Piascik, A. S., Pollacco, Don, Steele, I. A., Ulaczyk, K., for the Liverpool Telescope Collaboration, Broderick, J. W., Fender, R. P., Jonker, P. G., Rowlinson, A., Stappers, B. W., Wijers, R. A. M. J., Low Frequency Array, For The, Lipunov, V., Gorbovskoy, E., Tyurina, N., Kornilov, V., Balanutsa, P., Kuznetsov, A., Buckley, D., Rebolo, R., Serra-Ricart, M., Israelian, G., Budnev, N. M., Gress, O., Ivanov, K., Poleshuk, V., Tlatov, A., Yurkov, V., Master, For The Collaboration, Kawai, N., Serino, M., Negoro, H., Nakahira, S., Mihara, T., Tomida, H., Ueno, S., Tsunemi, H., Matsuoka, M., Maxi, For The Collaboration, Croft, S., Feng, L., Franzen, T. M. O., Gaensler, B. M., Johnston-Hollitt, M., Kaplan, D. L., Morales, M. F., Tingay, S. J., Wayth, R. B., Williams, A., Murchison Wide-Field Array, For The, Smartt, S. J., Chambers, K. C., Smith, K. W., Huber, M. E., Young, D. R., Wright, D. E., Schultz, A., Denneau, L., Flewelling, H., Magnier, E. A., Primak, N., Rest, A., Sherstyuk, A., Stalder, B., Stubbs, C. W., Tonry, J., Waters, C., Willman, M., for the Pan-STARRS Collaboration, Olivares E, F., Campbell, H., Kotak, R., Sollerman, J., Smith, M., Dennefeld, M., Anderson, J. P., Botticella, M. T., Chen, T. -W, Valle, M. D., Elias-Rosa, N., Fraser, M., Inserra, C., Kankare, E., Kupfer, T., Harmanen, J., Galbany, L., Le Guillou, L., Lyman, J. D., Maguire, K., Mitra, A., Nicholl, M., Razza, A., Terreran, G., Valenti, S., Gal-Yam, A., Pessto, For The Collaboration, Ćwiek, A., Ćwiok, M., Mankiewicz, L., Opiela, R., Zaremba, M., Żarnecki, A. F., for the Pi of the Sky Collaboration, Onken, C. A., Scalzo, R. A., Schmidt, B. P., Wolf, C., Yuan, F., for the SkyMapper Collaboration, Evans, P. A., Kennea, J. A., Burrows, D. N., Campana, S., Cenko, S. B., Marshall, F. E., Nousek, J., O Brien, P., Osborne, J. P., Palmer, D., Perri, M., Racusin, J., Siegel, M., Tagliaferri, G., for the Swift Collaboration, Klotz, A., Turpin, D., Laugier, R., Tarot, For The, Zadko, National Observatory, Algerian, Pu Collaboration, C., Beroiz, M., Peñuela, T., Macri, L. M., Oelkers, R. J., Lambas, D. G., Vrech, R., Cabral, J., Colazo, C., Dominguez, M., Sanchez, B., Gurovich, S., Lares, M., Marshall, J. L., Depoy, D. L., Padilla, N., Pereyra, N. A., Benacquista, M., Toros, For The Collaboration, Tanvir, N. R., Wiersema, K., Levan, A. J., Steeghs, D., Hjorth, J., Fynbo, J. P. U., Malesani, D., Milvang-Jensen, B., Watson, D., Irwin, M., Fernandez, C. G., Mcmahon, R. G., Banerji, M., Gonzalez-Solares, E., Schulze, S., Postigo, A. U., Thoene, C. C., Cano, Z., Rosswog, S., Vista, For The Collaboration, LIGO, California Institute of Technology (CALTECH), Laboratoire de l'Accélérateur Linéaire (LAL), 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), Laboratoire des matériaux avancés (LMA), 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, Institut Lumière Matière [Villeurbanne] (ILM), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), 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), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA), AstroParticule et Cosmologie (APC (UMR_7164)), 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), 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 de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Particules de Montpellier (LUPM), Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Montpellier 2 - Sciences et Techniques (UM2), Laboratoire Leprince-Ringuet (LLR), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), VIRGO, 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), 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), Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-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)-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), Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-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)-École polytechnique (X)-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), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-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), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), and Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS)
Subjects: astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), Cosmology and Gravitation, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], gr-qc, ST/I001123/1, gravitational radiation, RCUK, FOS: Physical sciences, electromagnetic [current], General Relativity and Quantum Cosmology (gr-qc), gravitational radiation detector, localization, General Relativity and Quantum Cosmology, electromagnetic, emission [gravitational radiation], ST/L000709/1, Computer Science::Multimedia, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], ddc:520, Astrophysics - High Energy Astrophysical Phenomena, STFC, QB
Abstract: This Supplement provides supporting material for arXiv:1602.08492 . We briefly summarize past electromagnetic (EM) follow-up efforts as well as the organization and policy of the current EM follow-up program. We compare the four probability sky maps produced for the gravitational-wave transient GW150914, and provide additional details of the EM follow-up observations that were performed in the different bands., Comment: For the main Letter, see arXiv:1602.08492
Published: 2016
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3. Space Telescope and Optical Reverberation Mapping Project. IV. Anomalous Behavior of the Broad Ultraviolet Emission Lines in NGC 5548

Author: Goad, M. R., Korista, K. T., De Rosa, G., Kriss, G. A., Edelson, R., Barth, A. J., Ferland, G. J., Kochanek, C. S., Netzer, H., Peterson, B. M., Bentz, M. C., Bisogni, S., Crenshaw, D. M., Denney, K. D., Ely, J., Fausnaugh, M. M., Grier, C. J., Gupta, A., Horne, K. D., Kaastra, J., Pancoast, A., Pei, L., Pogge, R. W., Skielboe, A., Starkey, D., Vestergaard, M., Zu, Y., Anderson, M. D., Arevalo, P., Bazhaw, C., Borman, G. A., Boroson, T. A., Bottorff, M. C., Brandt, W. N., Breeveld, A. A., Brewer, B. J., Cackett, E. M., Carini, M. T., Croxall, K. V., Bonta, E. Dalla, de Lorenzo-Caceres, A., Dietrich, M., Efimova, N. V., Evans, P. A., Filippenko, A. V., Flatland, K., Gehrels, N., Geier, S., Gelbord, G. M., Gonzalez, L., Gorjian, V., Grupe, D., Hall, P. B., Hicks, S., Horenstein, D., Hutchison, T., Im, M., Jensen, J. J., Joner, M. D., Jones, J., Kaspi, S., Kelly, B. C., Kennea, J. A., Kim, M., Kim, S. C., Klimanov, S. A., Larionov, V. M., Lee, J. C., Leonard, D. C., Lira, P., MacInnis, F., Manne-Nicholas, E. R., Mathur, S., McHardy, I. M., Montouri, C., Musso, R., Nazarov, S. V., Norris, R. P., Nousek, J. A., Okhmat, D. N., Papadakis, I., Parks, J. R., Pott, J. -U., Rafter, S. E., Rix, H. -W., Saylor, D. A., Schimoia, J. S., Schnulle, K., Sergeev, S. G., Siegel, M., Spencer, M., Sung, H. -I., Teems, K. G., Treu, T., Turner, C. S., Uttley, P., Villforth, C., Weiss, Y., Woo, J. -H., Yan, H., Young, S., Zheng, W. -K., High Energy Astrophys. & Astropart. Phys (API, FNWI), Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, ITA, USA, and GBR
Subjects: Active galactic nucleus, 010504 meteorology & atmospheric sciences, Cosmic Origins Spectrograph, active [Galaxies], Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, galaxies: individual (NGC-5548), galaxies: nuclei, galaxies: Seyfert Supporting material: animation, Continuum (design consultancy), Doubly ionized oxygen, NDAS, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, QB Astronomy, Emission spectrum, Seyfert Supporting material: animation [Galaxies], 010303 astronomy & astrophysics, QC, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, QB, Galáxia NGC 5548, Physics, individual (NGC – 5548) [Galaxies], active, galaxies: individual (NGC, 5548), galaxies: nuclei, galaxies: Seyfert [galaxies], Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxias seyfert, Galaxy, Galáxias ativas, QC Physics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), nuclei [Galaxies], individual (NGC-5548) [Galaxies], Reverberation mapping, Equivalent width, Nucleo galatico
Abstract: During an intensive Hubble Space Telescope (HST) Cosmic Origins Spectrograph (COS) UV monitoring campaign of the Seyfert~1 galaxy NGC 5548 performed from 2014 February to July, the normally highly correlated far-UV continuum and broad emission-line variations decorrelated for ~60 to 70 days, starting ~75 days after the first HST/COS observation. Following this anomalous state, the flux and variability of the broad emission lines returned to a more normal state. This transient behavior, characterised by significant deficits in flux and equivalent width of the strong broad UV emission lines, is the first of its kind to be unambiguously identified in an active galactic nucleus reverberation mapping campaign. The largest corresponding emission-line flux deficits occurred for the high-ionization collisionally excited lines, C IV and Si IV(+O IV]), and also He II(+O III]), while the anomaly in Ly-alpha was substantially smaller. This pattern of behavior indicates a depletion in the flux of photons with E_{\rm ph} > 54 eV, relative to those near 13.6 eV. We suggest two plausible mechanisms for the observed behavior: (i) temporary obscuration of the ionizing continuum incident upon BLR clouds by a moving veil of material lying between the inner accretion disk and inner BLR, perhaps resulting from an episodic ejection of material from the disk, or (ii) a temporary change in the intrinsic ionizing continuum spectral energy distribution resulting in a deficit of ionizing photons with energies > 54 eV, possibly due to a transient restructuring of the Comptonizing atmosphere above the disk. Current evidence appears to favor the latter explanation., 12 pages, 2 figures, accepted for publication in ApJ, Friday 25th March 2016. A movie of the anomalous emission-line behavior can be found in the ancilliary documents
Published: 2016

4. Space Telescope and Optical Reverberation Mapping Project. VII. Understanding the Ultraviolet Anomaly in NGC 5548 with X-Ray Spectroscopy

Author: Mathur, S., Gupta, A., Page, K., Pogge, R. W., Krongold, Y., Goad, M. R., Adams, S. M., Anderson, M. D., Arã©valo, P., Barth, A. J., Bazhaw, C., Beatty, T. G., Bentz, M. C., Bigley, A., Bisogni, S., Borman, G. A., Boroson, T. A., Bottorff, M. C., Brandt, W. N., Breeveld, A. A., Brown, J. E., Brown, J. S., Cackett, E. M., Canalizo, G., Carini, M. T., Clubb, K. I., Comerford, J. M., Coker, C. T., Corsini, E. M., Crenshaw, D. M., Croft, S., Croxall, K. V., Dalla Bontã , E., Deason, A. J., Denney, K. D., De Lorenzo-cã¡ceres, A., De Rosa, G., Dietrich, M., Edelson, R., Ely, J., Eracleous, M., Evans, P. A., Fausnaugh, M. M., Ferland, G. J., Filippenko, A. V., Flatland, K., Fox, O. D., Gates, E. L., Gehrels, N., Geier, S., Gelbord, J. M., Gorjian, V., Greene, J. E., Grier, C. J., Grupe, D., Hall, P. B., Henderson, C. B., Hicks, S., Holmbeck, E., Holoien, T. W. -. S., Horenstein, D., Horne, Keith, Hutchison, T., Im, M., Jensen, J. J., Johnson, C. A., Joner, M. D., Jones, J., Kaastra, J., Kaspi, S., Kelly, B. C., Kelly, P. L., Kennea, J. A., Kim, M., Kim, S., Kim, S. C., King, A., Klimanov, S. A., Kochanek, C. S., Korista, K. T., Kriss, G. A., Lau, M. W., Lee, J. C., Leonard, D. C., Li, M., Lira, P., Ma, Z., Macinnis, F., Manne-nicholas, E. R., Malkan, M. A., Mauerhan, J. C., Mcgurk, R., Mchardy, I. M., Montouri, C., Morelli, L., Mosquera, A., Mudd, D., Muller-sanchez, F., Musso, R., Nazarov, S. V., Netzer, H., Nguyen, M. L., Norris, R. P., Nousek, J. A., Ochner, P., Okhmat, D. N., Ou-yang, B., Pancoast, A., Papadakis, I., Parks, J. R., Pei, L., Peterson, B. M., Pizzella, A., Poleski, R., Pott, J. -. U., Rafter, S. E., Rix, H. -. W., Runnoe, J., Saylor, D. A., Schimoia, J. S., Schnã¼lle, K., Sergeev, S. G., Shappee, B. J., Shivvers, I., Siegel, M., Simonian, G. V., Siviero, A., Skielboe, A., Somers, G., Spencer, M., Starkey, D., Stevens, D. J., Sung, H. -. I., Tayar, J., Tejos, N., Turner, C. S., Uttley, P., Van Saders, J., Vestergaard, M., Vican, L., Villanueva, S., Villforth, C., Weiss, Y., Woo, J. -. H., Yan, H., Young, S., Yuk, H., Zheng, W., Zhu, W., Zu, Y., Corsini, ENRICO MARIA, USA, High Energy Astrophys. & Astropart. Phys (API, FNWI), Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, and University of St Andrews. St Andrews Centre for Exoplanet Science
Subjects: active [Galaxies], individual (NGC 5548) [Galaxies], Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, Continuum (design consultancy), FOS: Physical sciences, Flux, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Spectral line, individual (NGC 5548) [X-rays], galaxies: individual (NGC 5548), X-rays: galaxies, X-rays: individual (NGC 5548), Astronomy and Astrophysics, Space and Planetary Science, Spitzer Space Telescope, 0103 physical sciences, QB Astronomy, Emission spectrum, 010303 astronomy & astrophysics, QC, Optical depth, QB, Physics, 010308 nuclear & particles physics, 3rd-DAS, Astrophysics - Astrophysics of Galaxies, galaxies [X-rays], QC Physics, 13. Climate action, Astrophysics of Galaxies (astro-ph.GA), Reverberation mapping, Anomaly (physics)
Abstract: During the Space Telescope and Optical Reverberation Mapping Project (STORM) observations of NGC 5548, the continuum and emission-line variability became de-correlated during the second half of the 6-month long observing campaign. Here we present Swift and Chandra X-ray spectra of NGC 5548 obtained as a part of the campaign. The Swift spectra show that excess flux (relative to a power-law continuum) in the soft X-ray band appears before the start of the anomalous emission-line behavior, peaks during the period of the anomaly, and then declines. This is a model-independent result suggesting that the soft excess is related to the anomaly. We divide the Swift data into on- and off-anomaly spectra to characterize the soft excess via spectral fitting. The cause of the spectral differences is likely due to a change in the intrinsic spectrum rather than being due to variable obscuration or partial covering. The Chandra spectra have lower signal-to-noise ratios, but are consistent with Swift data. Our preferred model of the soft excess is emission from an optically thick, warm Comptonizing corona, the effective optical depth of which increases during the anomaly. This model simultaneously explains all the three observations: the UV emission line flux decrease, the soft-excess increase, and the emission line anomaly., ApJ in press. Replaced with the accepted version
Published: 2017

5. UVES/VLT high resolution spectroscopy of GRB 050730 afterglow: probing the features of the GRB environment

Author: d'Elia, V., Fiore, F., Meurs, E., Chincarini, G., Melandri, A., Norci, L., Pellizza, L., Perna, R., Piranomonte, S., Sbordone, L., Stella, L., Tagliaferri, G., Vergani, S., Ward, P., Angelini, L., Antonelli, L.A., Burrows, D.N., Campana, S., Capalbi, M., Caraveo, P. A., Cimatti, Alessandro, Costa, E., Cusumano, G., d'Avanzo, P., Della Valle, M., Filliatre, P., Fontana, A., Frontera, F., Fugazza, D., Gehrels, N., Giannini, T., Giommi, P., Goldoni, P., Guetta, D., Israel, G., Lazzati, D., Malesani, D., Marconi, G., Mason, K., Mereghetti, S., Molinari, E., Moretti, A., Nousek, J., Perri, M., Piro, L., Stratta, G., Testa, V., Vietri, M., Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), APC - Astrophysique des Hautes Energies (APC - AHE), 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)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Dipartimento di Astronomia, Universita degli Studi di Bologna, Università di Bologna [Bologna] (UNIBO)-Università di Bologna [Bologna] (UNIBO)-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)-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), D'Elia V., Fiore F., Meurs E. J. A., Chincarini G., Melandri A., Norci L., Pellizza L., Perna R., Piranomonte S., Sbordone L., Stella L., Tagliaferri G., Vergani S. D., Ward P., Angelini, L., Antonelli L. A., Burrows D. N., Campana S., Capalbi M., Cimatti A., Costa E., Cusumano G., Della Valle M., Filliatre P., Fontana A., Frontera F., Fugazza D., Gehrels, N., Giannini T., Giommi P., Goldoni P., Guetta D., Israel G., Lazzati D., Malesani D., Marconi G., Mason K., Mereghetti S., Mirabel F., Molinari E., Moretti A., Nousek J., Perri M., Piro L., Stratta G., Testa V., Vietri M., 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)-Dipartimento di Astronomia, Universita degli Studi di Bologna, and Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO)
Subjects: Absorption spectroscopy, gamma rays: bursts, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Metallicity, Ciencias Físicas, FOS: Physical sciences, ISM [GALAXIES], Astrophysics, 01 natural sciences, BURSTS [GAMMA RAYS], purl.org/becyt/ford/1 [https], [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Ionization, 0103 physical sciences, ABUNDANCES [GALAXY], IDENTIFICATION [LINE], Spectroscopy, PROFILES [LINE], 010303 astronomy & astrophysics, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics (astro-ph), Astronomy and Astrophysics, line: profiles, purl.org/becyt/ford/1.3 [https], Galaxy, Redshift, Afterglow, Astronomía, cosmology: observations, Galaxy: abundances, galaxies: ISM, line: identification, Space and Planetary Science, OBSERVATIONS [COSMOLOGY], Gamma-ray burst, CIENCIAS NATURALES Y EXACTAS
Abstract: We analyze high resolution spectroscopic observations of the optical afterglow of GRB050730, obtained with UVES@VLT about hours after the GRB trigger. The spectrum shows that the ISM of the GRB host galaxy at z = 3.967 is complex, with at least five components contributing to the main absorption system. We detect strong CII*, SiII*, OI* and FeII* fine structure absorption lines associated to the second and third component. For the first three components we derive information on the relative distance from the site of the GRB explosion. Component 1, which has the highest redshift, does not present any fine structure nor low ionization lines; it only shows very high ionization features, such as CIV and OVI, suggesting that this component is very close to the GRB site. From the analysis of low and high ionization lines and fine structure lines, we find evidences that the distance of component 2 from the site of the GRB explosion is 10-100 times smaller than that of component 3. We evaluated the mean metallicity of the z=3.967 system obtaining values about 0.01 of the solar metallicity or less. However, this should not be taken as representative of the circumburst medium, since the main contribution to the hydrogen column density comes from the outer regions of the galaxy while that of the other elements presumably comes from the ISM closer to the GRB site. Furthermore, difficulties in evaluating dust depletion correction can modify significantly these values. The mean [C/Fe] ratio agrees well with that expected by single star-formation event models. Interestingly the [C/Fe] of component 2 is smaller than that of component 3, in agreement with GRB dust destruction scenarios, if component 2 is closer than component 3 to the GRB site., 11 pages, 15 postscript figures, accepted for pubblication in A&A
Published: 2007

6. A Statistical Comparison of the Optical/UV and X-ray Afterglows of Gamma-Ray Bursts using the Swift Ultra-violet Optical and X-ray Telescopes

Author: Oates, S. R., Page, M. J., Schady, P., De Pasquale, M., Evans, P. A., Page, K. L., Chester, M. M., Curran, P. A., Koch, T. S., Kuin, N. P. M., Roming, P. W. A., Siegel, M. H., Zane, S., and Nousek, J. A.
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, gamma-ray burst: general, FOS: Physical sciences, Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present the systematic analysis of the UVOT and XRT light curves for a sample of 26 Swift Gamma-Ray Bursts (GRBs). By comparing the optical/UV and X-ray light curves, we found that they are remarkably different during the first 500s after the BAT trigger, while they become more similar during the middle phase of the afterglow, i.e. between 2000s and 20000s. If we take literally the average properties of the sample, we find that the mean temporal indices observed in the optical/UV and X-rays after 500s are consistent with a forward-shock scenario, under the assumptions that electrons are in the slow cooling regime, the external medium is of constant density and the synchrotron cooling frequency is situated between the optical/UV and X-ray observing bands. While this scenario describes well the averaged observed properties, some individual GRB afterglows require different or additional assumptions, such as the presence of late energy injection. We show that a chromatic break (a break in the X-ray light curve that is not seen in the optical) is present in the afterglows of 3 GRBs and demonstrate evidence for chromatic breaks in a further 4 GRBs. The average properties of these breaks cannot be explained in terms of the passage of the synchrotron cooling frequency through the observed bands, nor a simple change in the external density. It is difficult to reconcile chromatic breaks in terms of a single component outflow and instead, more complex jet structure or additional emission components are required., Comment: 20 pages, 5 figures and 4 tables. Accepted for publication by MNRAS
Published: 2010
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7. Swift detects a remarkable gamma-ray burst, GRB 060614, that introduces a new classification scheme

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

8. The gamma-ray burst GRB060614 requires a novel explosive process

Author: Gal-Yam, A., Fox, D., Price, P., Davis, M., Leonard, D., Soderberg, A., Nakar, E., Ofek, E., Schmidt, B., Lewis, K., Peterson, B., Kulkarni, S., Berger, E., Cenko, B., Sari, R., Sharon, K., Frail, D., Gehrels, N., Nousek, J., Burrows, D., Mangano, V., Holland, S., Brown, P., Moon, D. -S., Harrison, F., Piran, T., McCarthy, P., Penprase, B., and Chevalier, R.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: Over the past decade our physical understanding of gamma-ray bursts (GRBs) has progressed rapidly thanks to the discovery and observation of their long-lived afterglow emission. Long-duration (T < 2 s) GRBs are associated with the explosive deaths of massive stars (``collapsars''), which produce accompanying supernovae, while the short-duration (T > 2 s) GRBs arise from a different origin, which has been argued to be the merger of two compact objects, either neutron stars or black holes. Here we present observations of GRB060614, a 100-s long burst discovered by the Swift satellite, which require the invocation of a new explosive process: either a massive ``collapsar'' that powers a GRB without any associated supernova, or a new type of engine, as long-lived as the collapsar but without any such massive stellar host. We also discuss the properties of this burst's redshift z=0.125 host galaxy, which distinguish it from other long-duration GRBs and suggest that an entirely new type of GRB progenitor may be required.
Published: 2006

9. Swift observations of GRB050712

Author: De Pasquale, M., Grupe, D., Poole, T. S., Breeveld, A. A., Zane, S., Rosen, S. R., Page, M. J., Mason, K. O., Burrows, D. N., Krimm., H. A., Gehrels, N., Nousek, J. A., Roming, P. W. A., Kobayashi, S., and Zhang, B.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics
Abstract: We present the results of X-ray and optical observations of GRB050712 performed by Swift. The X-ray lightcurve of this burst exhibits episodes of flares in the first 1000s, the same epoch at which the UVOT detected an optical counterpart. A shallow X-ray decay, with a decay slope of -0.73, followed and lasted ~70ks. This behaviour can be explained in terms of activity of GRB 'inner engine', with the possibility of that the last flare is caused by the interaction of the ejecta with the surrounding medium. We also find interesting spectral parameters for the X-ray emission. In particular, data suggest the presence of an intrinsic absorption in the first 1000s, which can be explained if circumbust medium clouds lie along the line of sight., 13 pages, 5 figures. Accepted for publication by MNRAS
Published: 2006

10. Relativistic ejecta from XRF 060218 and the rate of cosmic explosions

Author: Soderberg, A. M., Kulkarni, S. R., Nakar, E., Berger, E., Fox, D. B., Frail, D. A., Gal-Yam, A., Sari, R., Cenko, S. B., Kasliwal, M., Cameron, P. B., Chevalier, R. A., Piran, T., Price, P. A., Schmidt, B. P., Pooley, G., Moon, D. -S., Penprase, B. E., Rau, A., Ofek, E., Gehrels, N., Nousek, J. A., Burrows, D. N., Perrson, S. E., and McCarthy, P. J.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics
Abstract: Over the last decade, long-duration gamma-ray bursts (GRBs) including the subclass of X-ray flashes (XRFs) have been revealed to be a rare variety of Type Ibc supernova (SN). While all these events result from the death of massive stars, the electromagnetic luminosities of GRBs and XRFs exceed those of ordinary Type Ibc SNe by many orders of magnitude. The essential physical process that causes a dying star to produce a GRB or XRF, and not just an SN, remains the crucial open question. Here we present radio and X-ray observations of XRF 060218 (associated with SN 2006aj), the second nearest GRB identified to-date, which allow us to measure its total energy and place it in the larger context of cosmic explosions. We show that this event is 100 times less energetic but ten times more common than cosmological GRBs. Moreover, it is distinguished from ordinary Type Ibc SNe by the presence of 10^48 erg coupled to mildly-relativistic ejecta, along with a central engine (an accretion-fed, rapidly rotating compact source) which produces X-rays for weeks after the explosion. This suggests that the production of relativistic ejecta is the key physical distinction between GRBs/XRFs and ordinary SNe, while the nature of the central engine (black hole or magnetar) may distinguish typical bursts from low-luminosity, spherical events like XRF 060218., To appear in Nature on August 31 2006 (15 pages, 3 figures, 1 table, including Supplementary Information)
Published: 2006

11. Evidence for chromatic X-ray light-curve breaks in Swift GRB afterglows and their theoretical implications

Author: Panaitescu, A., Meszaros, P., Burrows, D., Nousek, J., Gehrels, N., O'Brien, P., and Willingale, R.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: The power-law decay of the X-ray emission of GRB afterglows 050319, 050401, 050607, 050713A, 050802 and 050922C exhibits a steepening at about 1--4 hours after the burst which, surprisingly, is not accompanied by a break in the optical emission. If it is assumed that both the optical and X-ray afterglows arise from the same outflow then, in the framework of the standard forward shock model, the chromaticity of the X-ray light-curve breaks indicates that they do not arise solely from a mechanism related to the outflow dynamics (e.g. energy injection) or the angular distribution of the blast-wave kinetic energy (structured outflows or jets). The lack of a spectral evolution accompanying the X-ray light-curve breaks shows that these breaks do not arise from the passage of a spectral break (e.g. the cooling frequency) either. Under these circumstances, the decoupling of the X-ray and optical decays requires that the microphysical parameters for the electron and magnetic energies in the forward shock evolve in time, whether the X-ray afterglow is synchrotron or inverse-Compton emission. For a steady evolution of these parameters with the Lorentz factor of the forward shock and an X-ray light-curve break arising from cessation of energy injection into the blast-wave, the optical and X-ray properties of the above six Swift afterglows require a circumburst medium with a r^{-2} radial stratification, as expected for a massive star origin for long GRBs. Alternatively, the chromatic X-ray light-curve breaks may indicate that the optical and X-ray emissions arise from different outflows. Neither feature (evolution of microphysical parameters or the different origin of the optical and X-ray emissions) were clearly required by pre-Swift afterglows., 6 pages, sumbitted to MNRAS
Published: 2006

12. The shock break-out of GRB 060218/SN 2006aj

Author: Campana, S., Mangano, V., Blustin, A. J., Brown, P., Burrows, D. N., Chincarini, G., Cummings, J. R., Cusumano, G., Della Valle, M., Malesani, D., Meszaros, P., Nousek, J. A., Page, M., Sakamoto, T., Waxman, E., Zhang, B., Dai, Z. G., Gehrels, N., Immler, S., Marshall, F. E., Mason, K. O., Moretti, A., O'Brien, P. T., Osborne, J. P., Page, K. L., Romano, P., Roming, P. W. A., Tagliaferri, G., Cominsky, L. R., Giommi, P., Godet, O., Kennea, J. A., Krimm, H., Angelini, L., Barthelmy, S. D., Boyd, P. T., Palmer, D. M., Wells, A. A., and White, N. E.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: Although the link between long Gamma Ray Bursts (GRBs) and supernovae (SNe) has been established, hitherto there have been no observations of the beginning of a supernova explosion and its intimate link to a GRB. In particular, we do not know however how a GRB jet emerges from the star surface nor how a GRB progenitor explodes. Here we report on observations of the close GRB060218 and its connection to SN2006aj. In addition to the classical non-thermal emission, GRB060218 shows a thermal component in its X-ray spectrum, which cools and shifts into the optical/UV band as time passes. We interpret these features as arising from the break out of a shock driven by a mildly relativistic shell into the dense wind surrounding the progenitor. Our observations allow us for the first time to catch a SN in the act of exploding, to directly observe the shock break-out and to provide strong evidence that the GRB progenitor was a Wolf-Rayet star., Comment: 12 pages, 3 color figures (final version). Accepted for publication in Nature
Published: 2006
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13. Swift-UVOT Observations of the X-Ray Flash 050406

Author: Schady, P., Mason, K. O., Osborne, J. P., Page, M. J., Roming, P. W. A., Still, M., Zhang, B., Blustin, A. J., Boyd, P., Cucchiara, A., Gehrels, N., Gronwall, C., De Pasquale, M., Holland, S. T., Marshall, F. E., McGowan, K. E., and Nousek, J. A.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics
Abstract: We present Swift-UVOT data on the optical afterglow of the X-ray flash of 2005 April 6 (XRF 050406) from 88s to \sim 10^5s after the initial prompt gamma-ray emission. Our observations in the V, B and U bands are the earliest that have been taken of an XRF optical counterpart. Combining the early -time optical temporal and spectral properties with \gamma- and simultaneous X-ray data taken with the BAT and XRT telescopes on-board Swift, we are able to constrain possible origins of the XRF. The prompt emission had a FRED profile (fast-rise, exponential decay) with a duration of T_90 = 5.7\pm 0.2s, putting it at the short end of the long-burst duration distribution. The absence of photoelectric absorption red-ward of 4000 \AA in the UV/optical spectrum provides a firm upper limit of z\leq 3.1 on the redshift, thus excluding a high redshift as the sole reason for the soft spectrum. The optical light curve is consistent with a power-law decay with slope alpha = -0.75\pm 0.26 (F_{\nu}\propto t^{\alpha}), and a maximum occurring in the first 200s after the initial gamma-ray emission. The softness of the prompt emission is well described by an off-axis structured jet model, which is able to account for the early peak flux and shallow decay observed in the optical and X-ray bands., Comment: 14 pages, 4 figures, accepted for publication in ApJ; typos corrected and upper limits in table 1 changed from background subtracted count rate in extraction region to the error associated with this
Published: 2006
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14. The X-ray Telescope on board Swift: status and main results

Author: Tagliaferri, G., Campana, S., Chincarini, G., Giommi, P., Cusumano, G., Burrows, D. N., Hill, J. E., Kennea, J. A., Nousek, J. A., Osborne, J. P., O'Brien, P. T., Wells, A., Angelini, L., and team, the XRT
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics
Abstract: The X-ray Telescope (XRT), on board the {\it Swift} satellite, provides: automated source detection and position with few arcsecond accuracy within few seconds from target acquisition; CCD spectroscopy and imaging capability (0.2-10 keV), with the capability of detecting a milliCrab source in about 10 seconds; automatic adjusting of the CCD readout mode to optimize the science return as the source fades. Swift main scientific goal is the study of gamma-ray burst (GRBs). XRT can observe GRB afterglows over several orders of magnitude in flux. The first results obtained during the first ten months of operation confirm that XRT is fully compliant with the requirements and is providing excellent results. In particular it is detecting a very steep decay in the early X-ray light curve of many afterglows. Often there are also strong flares superimposed to the X-ray light curve, probably related to the continued internal engine activity. XRT is also localising for the first time the X-ray counterparts to short bursts., 6 pages, 7 figures. Proceedings of the Conferenxe "The X-ray Universe", San Lorenzo de El Escorial (madrid, Spain), 26-30 September 2005
Published: 2005

15. Evidence for a Canonical GRB Afterglow Light Curve in the Swift/XRT Data

Author: Nousek, J. A., Kouveliotou, C., Grupe, D., Page, K., Granot, J., Ramirez-Ruiz, E., Patel, S. K., Burrows, D. N., Mangano, V., Barthelmy, S., Beardmore, A. P., Campana, S., Capalbi, M., Chincarini, G., Cusumano, G., Falcone, A. D., Gehrels, N., Giommi, P., Goad, M., Godet, O., Hurkett, C., Kennea, J. A., Moretti, A., O'Brien, P., Osborne, J., Romano, P., Tagliaferri, G., and Wells, A.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics
Abstract: We present new observations of the early X-ray afterglows of the first 27 gamma-ray bursts (GRBs) detected with the Swift X-ray Telescope (XRT). The early X-ray afterglows show a canonical behavior, where the light curve broadly consists of three distinct power law segments: (i) an initial very steep decay (t^{-alpha} with 34, and augments the already severe requirements for the efficiency of the prompt gamma-ray emission., Comment: 35 pages, 8 figures, accepted for publication in ApJ
Published: 2005

16. Gamma-Ray Observations of a Giant Flare from The Magnetar SGR 1806-20

Author: Palmer, D. M., Barthelmy, S., Gehrels, N., Kippen, R. M., Cayton, T., Kouveliotou, C., Eichler, D., Wijers, R. A. M. J., Woods, P. M., Granot, J., Lyubarsky, Y. E., Ramirez-Ruiz, E., Barbier, L., Chester, M., Cummings, J., Fenimore, E. E., Finger, M. H., Gaensler, B. M., Hullinger, D., Krimm, H., Markwardt, C. B., Nousek, J. A., Parsons, A., Patel, S., Sakamoto, T., Sato, G., Suzuki, M., and Tueller, J.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics
Abstract: Magnetars comprise two classes of rotating neutron stars (Soft Gamma Repeaters (SGRs) and Anomalous X-ray Pulsars), whose X-ray emission is powered by an ultrastrong magnetic field, B ~ 10^15 G. Occasionally SGRs enter into active episodes producing many short X-ray bursts; extremely rarely (about once per 50 years per source), SGRs emit a giant flare, an event with total energy at least 1000 times higher than their typical bursts. Here we report that, on 2004 December 27, SGR 1806-20 emitted the brightest extra-solar transient event ever recorded, even surpassing the full moon brightness for 0.2 seconds. The total (isotropic) flare energy is 2x10^46 erg, 100 times higher than the only two previous events, making this flare a once in a century event. This colossal energy release likely occurred during a catastrophic reconfiguration of the magnetar's magnetic field. Such an event would have resembled a short, hard Gamma Ray Burst (GRB) if it had occurred within 40 Mpc, suggesting that extragalactic SGR flares may indeed form a subclass of GRBs., Submitted to Nature 2005-02-02, revised 2005-03-01. 21 pp, incl. 6 figures
Published: 2005

17. Swift XRT Observations of X-ray Flares in GRB Afterglows

Author: Burrows, David N., Romano, P., Godet, O., Falcone, A., Pagani, C., Cusumano, G., Campana, S., Chincarini, G., Hill, J. E., Giommi, P., Goad, M. R., Kennea, J. A., Kobayashi, S., Meszaros, P., Nousek, J. A., Osborne, J. P., O'Brien, P. T., Page, K. L., Tagliaferri, G., Zhang, B., and team, the Swift XRT
Subjects: Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract: The Swift XRT has been observing GRB afterglows since December 23, 2004. Three-quarters of these observations begin within 300 s of the burst onset, providing an unprecendented look at the behavior of X-ray emission from GRB afterglows in the first few hours after the burst. While most of the early afterglows have smoothly declining lightcurves, a substantial fraction has large X-ray flares on short time-scales. We suggest that these flares provide support for models with extended central engine activity producing late-time internal shocks., Comment: 7 pages, 12 figures, X-Ray Universe 2005 conference proceedings
Published: 2005
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18. 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: Physics, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics, Orbital decay, Redshift, Optical telescope, law.invention, Afterglow, Telescope, law, Observatory, Satellite, Gamma-ray burst
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], 38 pages, including 10 figures; accepted for publication in ApJ v611
Published: 2004

19. The Chandra Deep Field North Survey. V. 1 Ms Source Catalogs

Author: Brandt, W. N., Alexander, D. M., Hornschemeier, A. E., Garmire, G. P., Schneider, D. P., Barger, A. J., Bauer, F. E., Broos, P. S., Cowie, L. L., Townsley, L. K., Burrows, D. N., Chartas, G., Feigelson, E. D., Griffiths, R. E., Nousek, J. A., and Sargent, W. L. W.
Subjects: Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract: An extremely deep X-ray survey (about 1 Ms) of the Hubble Deep Field North and its environs (about 450 arcmin^2) has been performed with the Advanced CCD Imaging Spectrometer on board the Chandra X-ray Observatory. This is one of the two deepest X-ray surveys ever performed; for point sources near the aim point it reaches 0.5-2.0 keV and 2-8 keV flux limits of 3 x 10^{-17} erg/cm^2/s and 2 x 10^{-16} erg/cm^2/s, respectively. Here we provide source catalogs along with details of the observations, data reduction, and technical analysis. Observing conditions, such as background, were excellent for almost all of the exposure. We have detected 370 distinct point sources: 360 in the 0.5-8.0 keV band, 325 in the 0.5-2.0 keV band, 265 in the 2-8 keV band, and 145 in the 4-8 keV band. Two new Chandra sources in the HDF-N itself are reported and discussed. Source positions are accurate to within 0.6-1.7 arcsec (at 90% confidence) depending mainly on the off-axis angle. We also detect two highly significant extended X-ray sources and several other likely extended X-ray sources. We present basic number count results for sources located near the center of the field. Source densities of 7100^{+1100}_{-940} deg^{-2} (at 4.2 x 10^{-17} erg/cm^2/s) and 4200^{+670}_{-580} deg^{-2} (at 3.8 x 10^{-16} erg/cm^2/s) are observed in the soft and hard bands, respectively., 41 pages, AJ, in press; tables 3 and 6, images, and version with full-resolution figures at http://www.astro.psu.edu/users/niel/hdf/hdf-chandra.html
Published: 2001

20. X-ray imaging of the Seyfert 2 galaxy Circinus with Chandra

Author: Sambruna, R. M., Brandt, W. N., Chartas, G., Netzer, H., Kaspi, S., Garmire, G. P., Nousek, J. A., and Weaver, K. A.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We present results from the zeroth-order imaging of a Chandra HETGS observation of the nearby Seyfert 2 galaxy Circinus. Twelve X-ray sources were detected in the ACIS-S image of the galaxy, embedded in diffuse X-ray emission. The latter shows a prominent (~18arcsec) soft ``plume'' in the N-W direction, coincident with the [OIII] ionization cone. The radial profiles of the brightest X-ray source at various energies are consistent with an unresolved (FWHM ~0.8arcsec) component, which we identify as the active nucleus, plus two extended components with FWHMs ~ 2.3arcsec and 18arcsec, respectively. In a radius of 3arcsec, the nucleus contributes roughly the same flux as the extended components at the softest energies (< 2 keV). However, at harder energies (> 2 keV), the contribution of the nucleus is dominant. The zeroth-order ACIS spectrum of the nucleus exhibits emission lines at both soft and hard X-rays, including a prominent Fe Kalpha line at 6.4 keV, showing that most of the X-ray lines previously detected with ASCA originate in a compact region (, Figure 1 in color. ApJ Letters, in press
Published: 2000

21. High-resolution X-ray spectroscopy of the Seyfert 2 galaxy Circinus with Chandra

Author: Sambruna, R. M., Netzer, H., Kaspi, S., Brandt, W. N., Chartas, G., Garmire, G. P., Nousek, J. A., and Weaver, K. A.
Subjects: Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract: Results from a 60 ks Chandra HETGS observation of the nearby Seyfert 2 Circinus are presented. The spectrum shows a wealth of emission lines at both soft and hard X-rays, including lines of Ne, Mg, Si, S, Ar, Ca, and Fe, and a prominent Fe Kalpha line at 6.4 keV. We identify several of the He-like components and measure several of the Lyman lines of the H-like ions. The lines' profiles are unresolved at the limited signal-to-noise ratio of the data. Our analysis of the zeroth-order image in a companion paper constrains the size of the emission region to be 20-60 pc, suggesting that emission within this volume is almost entirely due to the reprocessing of the obscured central source. Here we show that a model containing two distinct components can reproduce almost all the observed properties of this gas. The ionized component can explain the observed intensities of the ionized species, assuming twice-solar composition and an N \propto r^{-1.5} density distribution. The neutral component is highly concentrated, well within the 0.8arcsec point source, and is responsible for almost all of the observed Kalpha (6.4 keV) emission. Circinus seems to be different than Mkn~3 in terms of its gas distribution., Figure 1 in color. ApJ Letters, in press
Published: 2000

22. Chandra uncovers a hidden Low-Luminosity AGN in the radio galaxy Hydra~A (3C~218)

Author: Sambruna, R. M., Chartas, G., Eracleous, M., Mushotzky, R., and Nousek, J.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We report the detection with Chandra of a Low-Luminosity AGN (LLAGN) in the Low Ionization Emission Line Region (LINER) hosted by Hydra A, a nearby (z=0.0537) powerful FRI radio galaxy with complex radio and optical morphology. In a 20 ks ACIS-S exposure during the calibration phase of the instrument, a point source is detected at energies $\grtsim$ 2 keV at the position of the compact radio core, embedded in diffuse thermal X-ray emission ($kT \sim 1$ keV) at softer energies. The spectrum of the point source is well fitted by a heavily absorbed power law with intrinsic column density N$_H^{int} \sim 3 \times 10^{22}$ \nh and photon index $\Gamma \sim 1.7$. The intrinsic (absorption-corrected) luminosity is $L_{2-10 keV} \sim 1.3 \times 10^{42}$ \lum. These results provide strong evidence that an obscured AGN is present in the nuclear region of Hydra~A. We infer that the optical/UV emission of the AGN is mostly hidden by the heavy intrinsic reddening. In order to balance the photon budget of the nebula, we must either postulate that the ionizing spectrum includes a UV bump or invoke and additional power source (shocks in the cooling flow or interaction with the radio jets). Using an indirect estimate of the black hole mass and the X-ray luminosity, we infer that the accretion rate is low, suggesting that the accretion flow is advection dominated. Finally, our results support current unification schemes for radio-loud sources, in particular the presence of the putative molecular torus in FR~Is. These observations underscore the power of the X-rays and of \chandra in the quest for black holes., Comment: figure 1 in color. accepted for publication in ApJ Letters
Published: 2000

23. Observations of Faint, Hard-Band X-ray Sources in the Field of CRSS J0030.5+2618 with the Chandra X-ray Observatory and the Hobby-Eberly Telescope

Author: Brandt, W. N., Hornschemeier, A. E., Schneider, D. P., Garmire, G. P., Chartas, G., Hill, Gary J., MacQueen, P. J., Townsley, L. K., Burrows, D. N., Koch, T. S., Nousek, J. A., and Ramsey, L. W.
Subjects: Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract: We present results from a study of 2-8 keV X-ray sources detected by the Advanced CCD Imaging Spectrometer (ACIS) instrument on the Chandra X-ray Observatory in the field of the z=0.516 cluster CRSS J0030.5+2618. In our 63.5 arcmin^2 search area, we detect 10 sources with 2-8 keV fluxes down to approximately 4x10^{-15} erg cm^{-2} s$^{-1}; our lowest flux sources are approximately 10 times fainter than those previously available for study in this band. Our derived source density is about an order of magnitude larger than previous source counts above 2 keV, although this density may be enhanced somewhat due to the presence of the cluster. We detail our methods for source detection and characterization, and we show that the resulting source list and parameters are robust. We have used the Marcario Low Resolution Spectrograph on the Hobby-Eberly Telescope to obtain optical spectra for several of our sources; combining these spectra with archival data we find that the sources appear to be active galaxies, often with narrow permitted lines, red optical continua or hard X-ray spectra. Four of the X-ray sources are undetected to R=21.7; if they reside in L* galaxies they must have z > 0.55-0.75 and hard X-ray luminosities of L_{2-8} > 4x10^{42} erg s^{-1}. We detect all but one of our 2-8 keV sources in the 0.2-2 keV band as well. This result extends to significantly lower fluxes the constraints on any large, completely new population of X-ray sources that appears above 2-3 keV., 22 pages, AJ, in press
Published: 2000

24. Mitigating Charge Transfer Inefficiency in the Chandra X-ray Observatory's ACIS Instrument

Author: Townsley, L. K., Broos, P. S., Garmire, G. P., and Nousek, J. A.
Subjects: Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics
Abstract: The ACIS front-illuminated CCDs onboard the Chandra X-ray Observatory were damaged in the extreme environment of the Earth's radiation belts, resulting in enhanced charge transfer inefficiency (CTI). This produces a row dependence in gain, event grade, and energy resolution. We model the CTI as a function of input photon energy, including the effects of de-trapping (charge trailing), shielding within an event (charge in the leading pixels of the 3X3 event island protect the rest of the island by filling traps), and non-uniform spatial distribution of traps. This technique cannot fully recover the degraded energy resolution, but it reduces the position dependence of gain and grade distributions. By correcting the grade distributions as well as the event amplitudes, we can improve the instrument's quantum efficiency. We outline our model for CTI correction and discuss how the corrector can improve astrophysical results derived from ACIS data., Comment: Accepted by ApJ Letters; see http://www.astro.psu.edu/users/townsley/cti/
Published: 2000
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25. Prompt and afterglow early X-ray phases in the comoving frame. Evidence for Universal properties?

Author: Chincarini, G., alberto moretti, Romano, P., Covino, S., Tagliaferri, G., Campana, S., Goad, M., Kobayashi, S., Zhang, B., Angelini, L., Banat, P., Barthelmy, S., Beardmore, A. P., Boyd, P. T., Breeveld, A., Burrows, D. N., Capalbi, M., Chester, M. M., Cusumano, G., Fenimore, E. E., Gehrels, N., Giommi, P., Hill, J. E., Hinshaw, D., Holland, S. T., Kennea, J. A., Krimm, H. A., La Parola, V., Mangano, V., Marshall, F. E., Mason, K. O., Nousek, J. A., O Brien, P. T., Osborne, J. P., Perri, M., Meszaros, P., Roming, P. W. A., Sakamoto, T., Schady, P., Still, M., and Wells, A. A.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics
Abstract: We analyze the Swift XRT light curves and spectra of the gamma-ray bursts (GRBs) for which the redshift has been measured. The sample consists of seven GRBs. The soft X-ray light curves of all these GRBs are separated into at least two morphological classes: 1) those starting off with a very steep light curve decay and 2) those showing a rather mild initial decay. This initial decay is followed by a flattening and by a further steepening. During these transitions the soft X-ray spectrum of these GRBs remains constant within the observational errors (except for one case, GRB050319). For the first time we are able to exploit the early light curve of GRB afterglows in the comoving frame. Besides the temporal and spectral behavior we find that the energy of the afterglow emitted in the (rest frame) time interval 20-200 s and 1300-12600 s after the trigger correlates with the mean energy of the prompt emission, hinting at a close link between the two. Averaging over the bursts that have a rather well sampled light curve and starting immediately after the prompt phase, the energy emitted in the soft X-rays is about 3% of the energy emitted during the prompt phase, except for GRB050315, where the soft X-ray emission is as high as 14% of the prompt emission., Submitted to ApJ

26. Space Telescope and Optical Reverberation Mapping Project. VIII. Time Variability of Emission and Absorption in NGC 5548 Based on Modeling the Ultraviolet Spectrum

Author: Andrew J. King, K. G. Teems, Gabriele Ponti, J. S. Schimoia, Calen B. Henderson, Michael S. Brotherton, S. Paltani, Nahum Arav, Alessandro Siviero, Radosław Poleski, P. Lira, Sang Chul Kim, Thomas W.-S. Holoien, Wei Zhu, A. de Lorenzo-Cáceres, M. C. Bottorff, Dirk Grupe, Gabriela Canalizo, M. Eracleous, S. G. Sergeev, F. MacInnis, Massimo Cappi, M. Dietrich, Alis J. Deason, Haojing Yan, Giorgio Matt, Ciro Pinto, Michael T. Carini, Minjin Kim, Brandon C. Kelly, I. M. McHardy, Scott M. Adams, L. Gonzalez, J. J. Jensen, Julia M. Comerford, Yair Krongold, Tim Waters, B. Scott, C. S. Turner, G. A. Borman, R. McGurk, Nicolas Tejos, J. R. Parks, K. Flatland, Michael D. Joner, Kirk T. Korista, L. Di Gesu, Emma Gardner, Jon C. Mauerhan, Jessie C. Runnoe, Douglas C. Leonard, Kelsey I. Clubb, M. H. Siegel, C. A. Johnson, D. A. Starkey, H. Yuk, M. A. Malkan, Justin Ely, Ying Zu, Aaron J. Barth, Cassandra Lochhaas, Patrick L. Kelly, E. Holmbeck, Hyun-Il Sung, Patrick B. Hall, C. Montuori, Christopher S. Kochanek, Bradley M. Peterson, Tommaso Treu, Missagh Mehdipour, Marie Wingyee Lau, A. Skielboe, Catherine J. Grier, J. A. Kennea, Thomas G. Beatty, R. W. Pogge, J. van Saders, A. Bigley, S. Hicks, Catia Silva, H. W. Rix, Vardha N. Bennert, D. M. Crenshaw, E. Dalla Bontà, Miao Li, A. A. Breeveld, Dom Walton, D. N. Okhmat, Elisa Costantini, P. Ochner, Y. Weiss, M. L. Nguyen, Ryan Norris, Susanna Bisogni, Ehud Behar, Jacobo Ebrero, Garrett Somers, Phil Uttley, S. Rafter, Kelly D. Denney, K. Schnülle, Carolin Villforth, Keith Horne, Smita Mathur, G. V. Simonian, R. Boissay-Malaquin, Gary J. Ferland, J. S. Brown, Jelle Kaastra, Ana M. Mosquera, Stefano Bianchi, Misty C. Bentz, A. Pancoast, Alessandro Pizzella, WeiKang Zheng, N. Gehrels, Daniel J. Stevens, M. Dehghanian, Kevin V. Croxall, Isaac Shivvers, A. Gupta, Chris Done, J. E. Brown, B. De Marco, Gerard A. Kriss, Steve Croft, S. V. Nazarov, J. A. Nousek, Jae-Ok Lee, P. Arévalo, G. De Rosa, Michael Fausnaugh, Rick Edelson, Phil Evans, Lorenzo Morelli, S. Geier, Enrico Maria Corsini, M. R. Goad, V. Gorjian, W. N. Brandt, Elinor L. Gates, Shai Kaspi, D. A. Saylor, Jong-Hak Woo, Edward M. Cackett, Liuyi Pei, T. Hutchison, Jamie Tayar, E. R. Manne-Nicholas, Laura Vican, Daniel Proga, Steven Villanueva, D. Mudd, J.-U. Pott, F. Müller-Sánchez, Alexei V. Filippenko, Hagai Netzer, S. A. Klimanov, B. J. Shappee, J. M. Gelbord, Marianne Vestergaard, M. Spencer, Zhiyuan Ma, Carl T. Coker, S. Y. Kim, Myungshin Im, Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, University of St Andrews. St Andrews Centre for Exoplanet Science, High Energy Astrophys. & Astropart. Phys (API, FNWI), Kriss, G. A., De Rosa, G., Ely, J., Peterson, B. M., Kaastra, J., Mehdipour, M., Ferland, G. J., Dehghanian, M., Mathur, S., Edelson, R., Korista, K. T., Arav, N., Barth, A. J., Bentz, M. C., Brandt, W. N., Crenshaw, D. M., Bontà, E. Dalla, Denney, K. D., Done, C., Eracleous, M., Fausnaugh, M. M., Gardner, E., Goad, M. R., Grier, C. J., Horne, Keith, Kochanek, C. S., Mchardy, I. M., Netzer, H., Pancoast, A., Pei, L., Pogge, R. W., Proga, D., Silva, C., Tejos, N., Vestergaard, M., Adams, S. M., Anderson, M. D., Arévalo, P., Beatty, T G., Behar, E., Bennert, V. N., Bianchi, S., Bigley, A., Bisogni, S., Boissay-Malaquin, R., Borman, G. A., Bottorff, M. C., Breeveld, A. A., Brotherton, M., Brown, J. E., Brown, J. S., Cackett, E. M., Canalizo, G., Cappi, M., Carini, M. T., Clubb, K. I., Comerford, J. M., Coker, C. T., Corsini, E. M., Costantini, E., Croft, S., Croxall, K. V., Deason, A. J., De Lorenzo-Cáceres, A., De Marco, B., Dietrich, M., Di Gesu, L., Ebrero, J., Evans, P. A., Filippenko, A. V., Flatland, K., Gates, E. L., Gehrels, N., Geier, S., Gelbord, J. M., Gonzalez, L., Gorjian, V., Grupe, D., Gupta, A., Hall, P. B., Henderson, C. B., Hicks, S., Holmbeck, E., Holoien, T. W. -S., Hutchison, T. A., Im, M., Jensen, J. J., Johnson, C. A., Joner, M. D., Kaspi, S., Kelly, B. C., Kelly, P. L., Kennea, J. A., Kim, M., Kim, S. C., Kim, S. Y., King, A., Klimanov, S. A., Krongold, Y., Lau, M. W., Lee, J. C., Leonard, D. C., Li, Miao, Lira, P., Lochhaas, C., Ma, Zhiyuan, Macinnis, F., Malkan, M. A., Manne-Nicholas, E. R., Matt, G., Mauerhan, J. C., Mcgurk, R., Montuori, C., Morelli, L., Mosquera, A., Mudd, D., Müller-Sánchez, F., Nazarov, S. V., Norris, R. P., Nousek, J. A., Nguyen, M. L., Ochner, P., Okhmat, D. N., Paltani, S., Parks, J. R., Pinto, C., Pizzella, A., Poleski, R., Ponti, G., Pott, J. -U., Rafter, S. E., Rix, H. -W., Runnoe, J., Saylor, D. A., Schimoia, J. S., Schnülle, K., Scott, B., Sergeev, S. G., Shappee, B. J., Shivvers, I., Siegel, M., Simonian, G. V., Siviero, A., Skielboe, A., Somers, G., Spencer, M., Starkey, D., Stevens, D. J., Sung, H. -I., Tayar, J., Teems, K. G., Treu, T., Turner, C. S., Uttley, P., Van Saders, J ., Vican, L., Villforth, C., Villanueva Jr., S., Walton, D. J., Waters, T., Weiss, Y., Woo, J. -H., Yan, H., Yuk, H., Zheng, W., Zhu, W., Zu, Y., and USA
Subjects: Seyfert [Galaxies], galaxies: active, galaxies: individual (NGC 5548), galaxies: nuclei, galaxies: Seyfert, 010504 meteorology & atmospheric sciences, Absorption spectroscopy, active [Galaxies], individual (NGC 5548) [Galaxies], Astrophysics::High Energy Astrophysical Phenomena, Continuum (design consultancy), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Spectral line, Luminosity, 0103 physical sciences, QB Astronomy, Emission spectrum, Absorption (electromagnetic radiation), 010303 astronomy & astrophysics, QC, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, QB, Physics, Astronomy and Astrophysics, DAS, Astrophysics - Astrophysics of Galaxies, Galaxy, QC Physics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), nuclei [Galaxies], Reverberation mapping
Abstract: We model the ultraviolet spectra of the Seyfert 1 galaxy NGC~5548 obtained with the Hubble Space Telescope during the 6-month reverberation-mapping campaign in 2014. Our model of the emission from NGC 5548 corrects for overlying absorption and deblends the individual emission lines. Using the modeled spectra, we measure the response to continuum variations for the deblended and absorption-corrected individual broad emission lines, the velocity-dependent profiles of Ly$\alpha$ and C IV, and the narrow and broad intrinsic absorption features. We find that the time lags for the corrected emission lines are comparable to those for the original data. The velocity-binned lag profiles of Ly$\alpha$ and C IV have a double-peaked structure indicative of a truncated Keplerian disk. The narrow absorption lines show delayed response to continuum variations corresponding to recombination in gas with a density of $\sim 10^5~\rm cm^{-3}$. The high-ionization narrow absorption lines decorrelate from continuum variations during the same period as the broad emission lines. Analyzing the response of these absorption lines during this period shows that the ionizing flux is diminished in strength relative to the far-ultraviolet continuum. The broad absorption lines associated with the X-ray obscurer decrease in strength during this same time interval. The appearance of X-ray obscuration in $\sim\,2012$ corresponds with an increase in the luminosity of NGC 5548 following an extended low state. We suggest that the obscurer is a disk wind triggered by the brightening of NGC 5548 following the decrease in size of the broad-line region during the preceding low-luminosity state., Comment: 50 pages, 30 figures, uses aastex62.cls. Accepted for publication in ApJ, 07/06/2019. High-level products page in MAST will go live after 7/15/2019. Replaced Figure 4 on 7/12/2019 to be more red/green color-blind friendly
Published: 2019

27. LOCALIZATION AND BROADBAND FOLLOW-UP OF THE GRAVITATIONAL-WAVE TRANSIENT GW 150914

Author: Abbott1, B. P., Abbott1, R., Abbott2, T. D., Abernathy1, M. R., Acernese3, F., 4, Ackley5, K., Adams6, C., Adams7, T., Addesso3, P., Adhikari1, R. X., Adya8, V. B., Affeldt8, C., Agathos9, M., Agatsuma9, K., Aggarwal10, N., Aguiar11, O. D., Aiello12, L., Ain14, A., Ajith15, P., Allen8, B., 17, 16, Allocca18, A., Altin20, P. A., Anderson1, S. B., Anderson16, W. G., Arai1, K., Araya1, M. C., Arceneaux21, C. C., Areeda22, J. S., Arnaud23, N., Arun24, K. G., Ascenzi13, S., Ashton26, G., Ast27, M., Aston6, S. M., Astone28, P., Aufmuth8, P., Aulbert8, C., Babak29, S., Bacon30, P., Bader9, M. K. M., Baker31, P. T., Baldaccini32, F., Ballardin34, G., Ballmer35, S. W., Barayoga1, J. C., Barclay36, S. E., Barish1, B. C., Barker37, D., Barone3, F., Barr36, B., Barsotti10, L., Barsuglia30, M., Barta38, D., Barthelmy39, S., Bartlett37, J., Bartos40, I., Bassiri41, R., Basti18, A., Batch37, J. C., Baune8, C., Bavigadda34, V., Bazzan42, M., Behnke29, B., Bejger44, M., Bell36, A. S., Bell36, C. J., Berger1, B. K., Bergman37, J., Bergmann8, G., Berry45, C. P. L., Bersanetti46, D., Bertolini9, A., Betzwieser6, J., Bhagwat35, S., Bhandare48, R., Bilenko49, I. A., Billingsley1, G., Birch6, J., Birney50, R., Biscans10, S., Bisht8, A., Bitossi34, M., Biwer35, C., Bizouard23, M. A., Blackburn1, J. K., Blair51, C. D., Blair51, D. G., Blair37, R. M., Bloemen52, S., Bock8, O., Bodiya10, T. P., Boer53, M., Bogaert53, G., Bogan8, C., Bohe29, A., Bojtos54, P., Bond45, C., Bondu55, F., Bonnand7, R., Boom9, B. A., Bork1, R., Boschi18, V., Bose14, S., Bouffanais30, Y., Bozzi34, A., Bradaschia19, C., Brady16, P. R., Braginsky49, V. B., Branchesi57, M., Brau59, J. E., Briant60, T., Brillet53, A., Brinkmann8, M., Brisson23, V., Brockill16, P., Brooks1, A. F., Brown35, D. A., Brown45, D. D., Brown10, N. M., Buchanan2, C. C., Buikema10, A., Bulik61, T., Bulten9, H. J., Buonanno29, A., Buskulic7, D., Buy30, C., Byer41, R. L., Cadonati64, L., Cagnoli65, G., Cahillane1, C., Bustillo64, J. C., Callister1, T., Calloni4, E., Camp39, J. B., Cannon69, K. C., Cao70, J., Capano8, C. D., Capocasa30, E., Carbognani34, F., Caride71, S., Diaz23, J. C., Casentini13, C., Caudill16, S., Cavagliá21, M., Cavalier23, F., Cavalieri34, R., Cella19, G., Cepeda1, C. B., Baiardi57, L. C., Cerretani18, G., Cesarini13, E., Chakraborty1, R., Chalermsongsak1, T., Chamberlin72, S. J., Chan36, M., Chao73, S., Charlton74, P., Chassande Mottin30, E., Chen75, H. Y., Chen76, Y., Cheng73, C., Chincarini47, A., Chiummo34, A., Cho77, H. S., Cho63, M., Chow20, J. H., Christensen78, N., Chu51, Q., Chua60, S., Chung51, S., Ciani5, G., Clara37, F., Clark64, J. A., Cleva53, F., Coccia12, E., 25, 13, Cohadon60, P. F., Colla28, A., Collette80, C. G., Cominsky81, L., M. Constancio J. r., 11, Conte28, A., Conti43, L., Cook37, D., Corbitt2, T. R., Cornish31, N., Corsi71, A., Cortese34, S., Costa11, C. A., Coughlin78, M. W., Coughlin82, S. B., Coulon53, J. P., Countryman40, S. T., Couvares1, P., Cowan64, E. E., Coward51, D. M., Cowart6, M. J., Coyne1, D. C., Coyne71, R., Craig36, K., Creighton16, J. D. E., Cripe2, J., Crowder83, S. G., Cumming36, A., Cunningham36, L., Cuoco34, E., Dal Canton8, T., Danilishin36, S. L., D'Antonio13, S., Danzmann8, K., Darman84, N. S., Dattilo34, V., Dave48, I., Daveloza85, H. P., Davier23, M., Davies36, G. S., Daw86, E. J., Day34, R., Debra41, D., Debreczeni38, G., Degallaix66, J., De Laurentis4, M., Deléglise60, S., Del Pozzo45, W., Denker8, T., Dent8, T., Dereli53, H., Dergachev1, V., Derosa6, R. T., De Rosa4, R., Desalvo87, R., Dhurandhar14, S., Díaz85, M. C., Di Fiore4, L., Di Giovanni28, M., Di Lieto18, A., Di Pace28, S., Di Palma8, I., Di Virgilio19, A., Dojcinoski88, G., Dolique66, V., Donovan10, F., Dooley21, K. L., Doravari6, S., 8, Douglas36, R., Downes16, T. P., Drago8, M., 90, 89, Drever1, R. W. P., Driggers37, J. C., Du70, Z., Ducrot7, M., Dwyer37, S. E., Edo86, T. B., Edwards78, M. C., Effler6, A., Eggenstein8, H. B., Ehrens1, P., Eichholz5, J., Eikenberry5, S. S., Engels76, W., Essick10, R. C., Etzel1, T., Evans10, M., Evans6, T. M., Everett72, R., Factourovich40, M., Fafone12, V., Fair35, H., Fairhurst91, S., Fan70, X., Fang51, Q., Farinon47, S., Farr75, B., Farr45, W. M., Favata88, M., Fays91, M., Fehrmann8, H., Fejer41, M. M., Ferrante18, I., Ferreira11, E. C., Ferrini34, F., Fidecaro18, F., Fiori34, I., Fiorucci30, D., Fisher35, R. P., Flaminio66, R., Fletcher36, M., Fournier53, J. D., Franco23, S., Frasca28, S., Frasconi19, F., Frei54, Z., Freise45, A., Frey59, R., Frey23, V., Fricke8, T. T., Fritschel10, P., Frolov6, V. V., Fulda5, P., Fyffe6, M., Gabbard21, H. A. G., Gair93, J. R., Gammaitoni32, L., Gaonkar14, S. G., Garufi4, F., Gatto30, A., Gaur94, G., Gehrels39, N., Gemme47, G., Gendre53, B., Genin34, E., Gennai19, A., George48, J., Gergely96, L., Germain7, V., Ghosh15, A., Ghosh9, S., Giaime2, J. A., 6, Giardina6, K. D., Giazotto19, A., Gill97, K., Glaefke36, A., Goetz98, E., Goetz5, R., Gondan54, L., González2, G., Castro18, J. M. G., Gopakumar99, A., Gordon36, N. A., Gorodetsky49, M. L., Gossan1, S. E., Gosselin34, M., Gouaty7, R., Graef36, C., Graff63, P. B., Granata66, M., Grant36, A., Gras10, S., Gray37, C., Greco57, G., Green45, A. C., Groot52, P., Grote8, H., Grunewald29, S., Guidi57, G. M., Guo70, X., Gupta14, A., Gupta95, M. K., Gushwa1, K. E., Gustafson1, E. K., Gustafson98, R., Hacker22, J. J., Hall56, B. R., Hall1, E. D., Hammond36, G., Haney99, M., Hanke8, M. M., Hanks37, J., Hanna72, C., Hannam91, M. D., Hanson6, J., Hardwick2, T., Haris106, K., Harms57, J., Harry100, G. M., Harry29, I. W., Hart36, M. J., Hartman5, M. T., Haster45, C. J., Haughian36, K., Heidmann60, A., Heintze5, M. C., Heitmann53, H., Hello23, P., Hemming34, G., Hendry36, M., Heng36, I. S., Hennig36, J., Heptonstall1, A. W., Heurs8, M., Hild36, S., Hoak101, D., Hodge1, K. A., Hofman66, D., Hollitt102, S. E., Holt6, K., Holz75, D. E., Hopkins91, P., Hosken102, D. J., Hough36, J., Houston36, E. A., Howell51, E. J., Hu36, Y. M., Huang73, S., Huerta82, E. A., 103, Huet23, D., Hughey97, B., Husa67, S., Huttner36, S. H., Huynh Dinh6, T., Idrisy72, A., Indik8, N., Ingram37, D. R., Inta71, R., Isa36, H. N., Isac60, J. M., Isi1, M., Islas22, G., Isogai10, T., Iyer15, B. R., Izumi37, K., Jacqmin60, T., Jang77, H., Jani64, K., Jaranowski104, P., Jawahar105, S., Jiménez Forteza67, F., Johnson2, W. W., Jones26, D. I., Jones36, R., Jonker9, R. J. G., Ju51, L., Kalaghatgi24, C. V., Kalogera82, V., Kandhasamy21, S., Kang77, G., Kanner1, J. B., Karki59, S., Kasprzack2, M., 34, 23, Katsavounidis10, E., Katzman6, W., Kaufer17, S., Kaur51, T., Kawabe37, K., Kawazoe8, F., Kéfélian53, F., Kehl69, M. S., Keitel8, D., Kelley35, D. B., Kells1, W., Kennedy86, R., Key85, J. S., Khalaidovski8, A., Khalili49, F. Y., Khan12, I., Khan91, S., Khan95, Z., Khazanov107, E. A., Kijbunchoo37, N., Kim77, C., Kim108, J., Kim109, K., Kim77, N., Kim41, N., Kim108, Y. M., King102, E. J., King37, P. J., Kinzel6, D. L., Kissel37, J. S., Kleybolte27, L., Klimenko5, S., Koehlenbeck8, S. M., Kokeyama2, K., Koley9, S., Kondrashov1, V., Kontos10, A., Korobko27, M., Korth1, W. Z., Kowalska61, I., Kozak1, D. B., Kringel8, V., Królak110, A., 111, Krueger17, C., Kuehn8, G., Kumar69, P., Kuo73, L., Kutynia110, A., Lackey35, B. D., Landry37, M., Lange112, J., Lantz41, B., Lasky113, P. D., Lazzarini1, A., Lazzaro43, C., Leaci28, P., 79, 29, Leavey36, S., Lebigot30, E. O., Lee108, C. H., Lee109, H. K., Lee114, H. M., Lee36, K., Lenon35, A., Leonardi89, M., Leong8, J. R., Leroy23, N., Letendre7, N., Levin113, Y., Levine37, B. M., Li1, T. G. F., Libson10, A., Littenberg115, T. B., Lockerbie105, N. A., Logue36, J., Lombardi101, A. L., Lord35, J. E., Lorenzini12, M., Loriette116, V., Lormand6, M., Losurdo58, G., Lough8, J. D., Lück8, H., Lundgren8, A. P., Luo78, J., Lynch10, R., Ma51, Y., Macdonald41, T., Machenschalk8, B., Macinnis10, M., Macleod2, D. M., Magaña Sandoval35, F., Magee56, R. M., Mageswaran1, M., Majorana28, E., Maksimovic116, I., Malvezzi13, V., Man53, N., Mandel45, I., Mandic83, V., Mangano36, V., Mansell20, G. L., Manske16, M., Mantovani34, M., Marchesoni33, F., 117, Marion7, F., Márka40, S., Márka40, Z., Markosyan41, A. S., Maros1, E., Martelli57, F., Martellini53, L., Martin36, I. W., Martin5, R. M., Martynov1, D. V., Marx1, J. N., Mason10, K., Masserot7, A., Massinger35, T. J., Masso Reid36, M., Matichard10, F., Matone40, L., Mavalvala10, N., Mazumder56, N., Mazzolo8, G., Mccarthy37, R., Mcclelland20, D. E., Mccormick6, S., Mcguire118, S. C., Mcintyre1, G., Mciver1, J., Mcmanus20, D. J., Mcwilliams103, S. T., Meacher72, D., Meadors8, G. D., Meidam9, J., Melatos84, A., Mendell37, G., Mendoza Gandara8, D., Mercer16, R. A., Merilh37, E., Merzougui53, M., Meshkov1, S., Messenger36, C., Messick72, C., Meyers83, P. M., Mezzani28, F., Miao45, H., Michel66, C., Middleton45, H., Mikhailov119, E. E., Milano4, L., Miller10, J., Millhouse31, M., Minenkov13, Y., Ming8, J., Mirshekari120, S., Mishra15, C., Mitra14, S., Mitrofanov49, V. P., Mitselmakher5, G., Mittleman10, R., Moggi19, A., Mohan34, M., Mohapatra10, S. R. P., Montani57, M., Moore88, B. C., Moore121, C. J., Moraru37, D., Moreno37, G., Morriss85, S. R., Mossavi8, K., Mours7, B., Mow Lowry45, C. M., Mueller5, C. L., Mueller5, G., Muir91, A. W., Mukherjee15, A., Mukherjee16, D., Mukherjee85, S., Mukund14, N., Mullavey6, A., Munch102, J., Murphy40, D. J., Murray36, P. G., Mytidis5, A., Nardecchia13, I., Naticchioni28, L., Nayak122, R. K., Necula5, V., Nedkova101, K., Nelemans9, G., Neri46, M., Neunzert98, A., Newton36, G., Nguyen20, T. T., Nielsen8, A. B., Nissanke9, S., Nitz8, A., Nocera34, F., Nolting6, D., Normandin85, M. E. N., Nuttall35, L. K., Oberling37, J., Ochsner16, E., O'Dell123, J., Oelker10, E., Ogin124, G. H., Oh125, J. 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A., Prokhorov49, L., Puncken8, O., Punturo33, M., Puppo28, P., Pürrer29, M., Qi16, H., Qin51, J., Quetschke85, V., Quintero1, E. A., Quitzow James59, R., Raab37, F. J., Rabeling20, D. S., Radkins37, H., Raffai54, P., Raja48, S., Rakhmanov85, M., Rapagnani28, P., Raymond29, V., Razzano18, M., Re25, V., Read22, J., Reed37, C. M., Regimbau53, T., Rei47, L., Reid50, S., Reitze1, D. H., 5, Rew119, H., Reyes35, S. D., Ricci28, F., Riles98, K., Robertson1, N. A., Robie36, R., Robinet23, F., Rocchi13, A., Rolland7, L., Rollins1, J. G., Roma59, V. J., Romano3, R., Romanov119, G., Romie6, J. H., Rosińska44, D., 127, Rowan36, S., Rüdiger8, A., Ruggi34, P., Ryan37, K., Sachdev1, S., Sadecki37, T., Sadeghian16, L., Salconi34, L., Saleem106, M., Salemi8, F., Samajdar122, A., Sammut84, L., 113, Sanchez1, E. J., Sandberg37, V., Sandeen82, B., Sanders35, J. R., Sassolas66, B., Sathyaprakash91, B. S., Saulson35, P. R., Sauter98, O., Savage37, R. L., Sawadsky17, A., Schale59, P., Schilling8, R., Schmidt8, J., Schmidt1, P., Schnabel27, R., Schofield59, R. M. S., Schönbeck27, A., Schreiber8, E., Schuette8, D., Schutz29, B. F., Scott36, J., Scott20, S. M., Sellers6, D., Sentenac34, D., Sequino13, V., Sergeev107, A., Serna22, G., Setyawati9, Y., Sevigny37, A., Shaddock20, D. A., Shah9, S., Shahriar82, M. S., Shaltev8, M., Shao1, Z., Shapiro41, B., Shawhan63, P., Sheperd16, A., Shoemaker10, D. H., Shoemaker64, D. M., Siellez53, K., Siemens16, X., Sigg37, D., Silva11, A. D., Simakov8, D., Singer1, A., Singh8, A., Singh2, R., Singhal12, A., Sintes67, A. M., Slagmolen20, B. J. J., Smith22, J. R., Smith1, N. D., Smith1, R. J. E., Son125, E. J., Sorazu36, B., Sorrentino47, F., Souradeep14, T., Srivastava95, A. K., Staley40, A., Steinke8, M., Steinlechner36, J., Steinlechner36, S., Steinmeyer8, D., Stephens16, B. C., Stone85, R., Strain36, K. A., Straniero66, N., Stratta57, G., Strauss78, N. A., Strigin49, S., Sturani120, R., Stuver6, A. L., Summerscales128, T. Z., Sun84, L., Sutton91, P. J., Swinkels34, B. L., Szczepańczyk97, M. J., Tacca30, M., Talukder59, D., Tanner5, D. B., Tápai96, M., Tarabrin8, S. P., Taracchini29, A., Taylor1, R., Theeg8, T., Thirugnanasambandam1, M. P., Thomas45, E. G., Thomas6, M., Thomas37, P., Thorne6, K. A., Thorne76, K. S., Thrane113, E., Tiwari12, S., Tiwari91, V., Tokmakov105, K. V., Tomlinson86, C., Tonelli18, M., Torres85, C. V., Torrie1, C. I., Töyrä45, D., Travasso32, F., Traylor6, G., Trifirò21, D., Tringali89, M. C., Trozzo19, L., 129, Tse10, M., Turconi53, M., Tuyenbayev85, D., Ugolini130, D., Unnikrishnan99, C. S., Urban16, A. L., Usman35, S. A., Vahlbruch17, H., Vajente1, G., Valdes85, G., van Bakel9, N., van Beuzekom9, M., van den Brand9, J. F. J., Van Den Broeck9, C., Vander Hyde22, D. C., van der Schaaf9, L., van Heijningen9, J. V., van Veggel36, A. A., Vardaro42, M., Vass1, S., Vasúth38, M., Vaulin10, R., Vecchio45, A., Vedovato43, G., Veitch45, J., Veitch102, P. J., Venkateswara131, K., Verkindt7, D., Vetrano57, F., Viceré57, A., Vinciguerra45, S., Vine50, D. J., Vinet53, J. Y., Vitale10, S., Vo35, T., Vocca32, H., Vorvick37, C., Voss5, D., Vousden45, W. D., Vyatchanin49, S. P., Wade20, A. R., Wade132, L. E., Wade132, M., Walker2, M., Wallace1, L., Walsh8, S., Wang12, G., Wang45, H., Wang45, M., Wang70, X., Wang51, Y., Ward20, R. L., Warner37, J., Was7, M., Weaver37, B., Wei53, L. W., Weinert8, M., Weinstein1, A. J., Weiss10, R., Welborn6, T., Wen51, L., Weßels8, P., Westphal8, T., Wette8, K., Whelan8, J. T., 112, White86, D. J., Whiting5, B. F., Williams1, R. D., Williamson91, A. R., Willis133, J. L., Willke8, B., Wimmer8, M. H., Winkler8, W., Wipf1, C. C., Wittel8, H., Woan36, G., Worden37, J., Wright36, J. L., Wu6, G., Yablon82, J., Yam10, W., Yamamoto1, H., Yancey63, C. C., Yap20, M. J., Yu10, H., Yvert7, M., Zadrożny110, A., Zangrando43, L., Zanolin97, M., Zendri43, J. P., Zevin82, M., Zhang10, F., Zhang1, L., Zhang119, M., Zhang112, Y., Zhao51, C., Zhou82, M., Zhou82, Z., Zhu51, X. J., Zucker1, M. E., Zuraw101, S. E., Zweizig1, J., Allison134, J., 135, Bannister134, K., Bell134, M. E., Chatterjee136, S., Chippendale134, A. P., Edwards134, P. G., Harvey Smith134, L., Ian, Heywood134, 137, Hotan138, A., Indermuehle134, B., Marvil134, J., Mcconnell134, D., Murphy135, T., 139, Popping135, A., 140, Reynolds134, J., Sault84, R. J., 134, Voronkov134, M. A., Whiting134 (The Australian Square Kilometer Array Pathfinder, M. T., Castro Tirado141, A. J., 142, Cunniffe141, R., Jelínek143, M., Tello141, J. C., Oates141, S. R., Hu141, Y. D., Kubánek144, P., Guziy145, S., Castellón146, A., García Cerezo142, A., Muñoz142, V. F., Pérez del Pulgar142, C., Castillo Carrión147, S., Castro Cerón148, J. M., Hudec143, R., 149, Caballero García150, M. D., Páta149, P., Vitek149, S., Adame151, J. A., Konig151, S., Rendón141, F., 151, Mateo Sanguino152, T. de J., Fernández Muñoz153, R., Yock154, P. C., Rattenbury154, N., Allen155, W. H., Querel156, R., Jeong141, S., 157, Park157, I. H., Bai158, J., Cui159, C. h., Fan158, Y., Wang158, C. h., Hiriart160, D., Lee161, W. H., Claret141, A., Sánchez Ramírez141, R., Pandey162, S. B., Mediavilla163, T., Sabau Graziati164, L., Abbott165, T. M. C., Abdalla137, F. B., 166, Allam167, S., Annis167, J., Armstrong168, R., Benoit Lévy166, A., 169, 170, Berger171, E., Bernstein172, R. A., Bertin169, E., 170, Brout173, D., Buckley Geer167, E., Burke174, D. L., 175, Capozzi176, D., Carretero177, J., 178, Castander177, F. J., Chornock179, R., Cowperthwaite171, P. S., Crocce177, M., Cunha174, C. E., D'Andrea26, C. B., 176, da Costa180, L. N., Desai181, S., 182, Diehl167, H. T., Dietrich181, J. P., Doctor183, Z., Drlica Wagner167, A., Drout171, M. R., Eifler173, T. F., 184, Estrada167, J., Evrard98, A. E., Fernandez178, E., Finley167, D. A., Flaugher167, B., Foley185, R. J., 186, Fong187, W. F., Fosalba177, P., Fox188, D. B., Frieman167, J., 183, Fryer189, C. L., Gaztanaga177, E., Gerdes190, D. W., Goldstein191, D. A., 192, Gruen174, D., Gruendl185, R. A., 193, Gutierrez167, G., Herner167, K., Honscheid194, K., 195, James165, D. J., Johnson193, M. D., Johnson193, M. W. G., Karliner186, I., Kasen192, D., 196, Kent167, S., Kessler183, R., Kim192, A. G., Kind185, M. C., Kuehn197, K., Kuropatkin167, N., Lahav166, O., Li198, T. S., Lima180, M., 199, Lin167, H., Maia180, M. A. G., Margutti200, R., Marriner167, J., Martini194, P., 201, Matheson202, T., Melchior168, P., Metzger203, B. D., Miller190, C. J., 204, Miquel178, R., 205, Neilsen167, E., Nichol176, R. C., Nord167, B., Nugent192, P., Ogando180, R., Petravick193, D., Plazas184, A. A., Quataert206, E., Roe192, N., Romer207, A. K., Roodman174, A., Rosell180, A. C., Rykoff174, E. S., Sako173, M., Sanchez208, E., Scarpine167, V., Schindler175, R., Schubnell190, M., Scolnic183, D., Sevilla Noarbe185, I., 208, Sheldon209, E., Smith187, N., Smith165, R. C., Soares Santos167, M., Sobreira180, F., Stebbins167, A., Suchyta173, E., Swanson193, M. E. C., Tarle190, G., Thaler186, J., Thomas176, D., Thomas192, R. C., Tucker167, D. L., Vikram210, V., Walker165, A. R., Wechsler41, R. H., 174, 175, Wester167, W., Yanny167, B., Zhang98, Y., Zuntz211, J., Connaughton212, V., Burns213, E., Goldstein214, A., 378, Briggs215, M. S., Zhang216, B. B., 217, Hui214, C. M., Jenke216, P., Wilson Hodge214, C. A., Bhat216, P. N., Bissaldi218, E., Cleveland212, W., Fitzpatrick216, G., Giles219, M. M., Gibby219, M. H., Greiner220, J., von Kienlin220, A., Kippen221, R. M., Mcbreen222, S., Mailyan216, B., Meegan216, C. A., Paciesas212, W. S., Preece215, R. D., Roberts222, O., Sparke223, L., Stanbro213, M., Toelge220, K., Veres216, P., Yu220, H. F., 224, Blackburn171, L., Ackermann225, M., Ajello226, M., Albert227, A., Anderson228, B., 229, Atwood230, W. B., Axelsson231, M., 232, Baldini227, L., 233, Barbiellini234, G., 235, Bastieri236, D., 237, Bellazzini238, R., Bissaldi239, E., Blandford227, R. D., Bloom227, E. D., Bonino, Raffaella, Bottacini227, E., Brandt242, T. J., Bruel243, P., Buson242, S., 244, 245, Caliandro227, G. A., 246, Cameron227, R. A., Caragiulo239, M., 247, Caraveo248, P. A., Cavazzuti249, E., Charles227, E., Chekhtman250, A., Chiang227, J., Chiaro237, G., Ciprini249, S., 251, Cohen Tanugi252, J., Cominsky253, L. R., Costanza239, F., Cuoco240, A., 241, D'Ammando254, F., 255, de Palma239, F., 256, Desiante240, R., 257, Digel227, S. W., Di Lalla238, N., Di Mauro227, M., Di Venere239, L., Domínguez226, A., Drell227, P. S., Dubois227, R., Favuzzi239, C., Ferrara242, E. C., Franckowiak227, A., Fukazawa258, Y., Funk259, S., Fusco239, P., Gargano239, F., Gasparrini249, D., Giglietto239, N., Giommi249, P., Giordano239, F., Giroletti254, M., Glanzman227, T., Godfrey227, G., Gomez Vargas260, G. A., 261, Green242, D., 262, Grenier263, I. A., Grove264, J. E., Guiriec242, S., Hadasch265, D., Harding242, A. K., Hays242, E., Hewitt266, J. W., Hill227, A. B., 267, Horan243, D., Jogler227, T., Jóhannesson268, G., Johnson227, A. S., Kensei258, S., Kocevski242, D., Kuss238, M., La Mura237, G., 265, Larsson229, S., 231, Latronico240, L., Li269, J., Li229, L., Longo234, F., Loparco239, F., Lovellette264, M. N., Lubrano251, P., Magill262, J., Maldera240, S., Manfreda238, A., Marelli248, M., Mayer225, M., Mazziotta239, M. N., Mcenery242, J. E., Meyer228, M., Michelson227, P. F., Mirabal242, N., Mizuno270, T., Moiseev245, A. A., Monzani227, M. E., Moretti271, E., Morselli261, A., Moskalenko227, I. V., Negro240, M., Nuss252, E., Ohsugi270, T., Omodei227, N., Orienti254, M., Orlando227, E., Ormes272, J. F., Paneque227, D., 271, Perkins242, J. S., Pesce Rollins227, M., 238, Piron252, F., Pivato238, G., Porter227, T. A., Racusin242, J. L., Rainò239, S., Rando236, R., Razzaque273, S., Reimer227, A., Reimer227, O., Salvetti248, D., Saz Parkinson230, P. M., 274, 275, Sgrò238, C., Simone239, D., Siskind276, E. J., Spada238, F., Spandre238, G., Spinelli239, P., Suson277, D. J., Tajima227, H., 278, Thayer227, J. B., Thompson242, D. J., Tibaldo279, L., Torres269, D. F., 280, Troja242, E., Uchiyama281, Y., Venters242, T. M., Vianello227, G., Wood264, K. S., Wood227, M., Zhu262, S., Zimmer228, S., Brocato282, E., Cappellaro283, E., Covino284, S., Grado285, A., Nicastro286, L., Palazzi286, E., Pian286, E., 287, Amati286, L., Antonelli282, L. A., 288, Capaccioli289, M., D'Avanzo284, P., D'Elia282, V., Getman285, F., Giuffrida282, G., Iannicola282, G., Limatola285, L., Lisi282, M., Marinoni282, S., Marrese282, P., 283, Melandri284, A., Piranomonte282, S., Possenti290, A., Pulone282, L., Rossi286, A., Stamerra287, A., 291, Stella282, L., Testa282, V., Tomasella283, L., Yang283 (The GRAvitational Wave Inaf TeAm, S., Bazzano292, A., Bozzo293, E., Brandt294, S., Courvoisier293, T. J. L., Ferrigno293, C., Hanlon295, L., Kuulkers296, E., Laurent297, P., Mereghetti298, S., Roques299, J. P., Savchenko300, V., Ubertini292, P., Kasliwal301, M. M., Singer39, L. P., Cao301, Y., Duggan301, G., Kulkarni301, S. R., Bhalerao14, V., Miller184, A. A., 301, 379, Barlow301, T., Bellm301, E., Manulis302, I., Rana14, J., Laher303, R., Masci303, F., Surace303, J., Rebbapragada184, U., Cook301, D., Van Sistine16, A., Sesar304, B., Perley305, D., Ferreti306, R., Prince301, T., Kendrick307, R., Horesh302 (The Intermediate Palomar Transient Factory, A., Hurley308, K., Golenetskii309, S. V., Aptekar309, R. L., Frederiks309, D. D., Svinkin309, D. S., Rau220, A., Zhang220, X., Smith230, D. M., Cline39, T., 380, Krimm245, H., 310, Abe311, F., Doi312, M., Fujisawa313, K., Kawabata314, K. S., Morokuma312, T., Motohara312, K., Tanaka315, M., Ohta316, K., Yanagisawa317, K., Yoshida314, M., Baltay318, C., Rabinowitz318, D., Ellman318, N., Rostami318, S., Bersier319, D. F., Bode319, M. F., Collins319, C. A., Copperwheat319, C. M., Darnley319, M. J., Galloway320, D. K., 321, Gomboc322, A., 323, Kobayashi319, S., Mazzali319, P., Mundell324, C. G., Piascik319, A. S., Don, Pollacco325, Steele319, I. A., Ulaczyk325, K., Broderick326, J. W., Fender327, R. P., Jonker52, P. G., 328, Rowlinson135, A., 326, 329, Stappers211, B. W., Wijers329 (The Low Frequency Array, R. A. M. J., Lipunov330, V., Gorbovskoy330, E., Tyurina330, N., Kornilov330, V., Balanutsa330, P., Kuznetsov330, A., Buckley331, D., Rebolo332, R., Serra Ricart332, M., Israelian332, G., Budnev333, N. M., Gress333, O., Ivanov333, K., Poleshuk333, V., Tlatov334, A., Yurkov335, V., Kawai336, N., Serino337, M., Negoro338, H., Nakahira339, S., Mihara337, T., Tomida340, H., Ueno340, S., Tsunemi341, H., Matsuoka337, M., Croft342, S., 343, Feng344, L., Franzen345, T. M. O., Gaensler135, B. M., 139, 346, Johnston Hollitt347, M., Kaplan16, D. L., Morales131, M. F., Tingay135, S. J., 345, 348, Wayth135, R. B., 345, Williams345 (The Murchison Wide field Array, A., Smartt349, S. J., Chambers350, K. C., Smith349, K. W., Huber350, M. E., Young349, D. R., Wright349, D. E., Schultz350, A., Denneau350, L., Flewelling350, H., Magnier350, E. A., Primak350, N., Rest351, A., Sherstyuk350, A., Stalder350, B., Stubbs352, C. W., Tonry350, J., Waters350, C., Willman350, M., 353, F. Olivares E., 354, Campbell355, H., Kotak349, R., Sollerman306, J., Smith26, M., Dennefeld356, M., Anderson357, J. P., Botticella285, M. T., Chen220, T. W., Valle285, M. D., Elias Rosa283, N., Fraser355, M., Inserra349, C., Kankare349, E., Kupfer301, T., Harmanen358, J., Galbany353, L., 359, Le Guillou360, L., 361, Lyman325, J. D., Maguire349, K., Mitra361, A., Nicholl171, M., Razza353, A., Terreran283, G., 349, Valenti362, S., 363, Gal Yam364, A., Ćwiek110, A., Ćwiok365, M., Mankiewicz366, L., Opiela366, R., Zaremba365, M., Żarnecki365, A. F., Onken20, C. A., Scalzo20, R. A., Schmidt20, B. P., Wolf20, C., Yuan20, F., Evans367, P. A., Kennea72, J. A., Burrows72, D. N., Campana284, S., Cenko39, S. B., 368, Giommi288, P., Marshall39, F. E., Nousek72, J., O'Brien367, P., Osborne367, J. P., Palmer369, D., Perri282, M., Siegel72, M., Tagliaferri284, G., Klotz370, A., Turpin370, D., Laugier53, R., Beroiz85, M., 371, Peñuela85, T., 372, Macri373, L. M., Oelkers373, R. J., Lambas374, D. G., Vrech374, R., Cabral374, J., Colazo374, C., Dominguez374, M., Sanchez374, B., Gurovich374, S., Lares374, M., Marshall373, J. L., Depoy373, D. L., Padilla375, N., Pereyra85, N. A., Benacquista85, M., Tanvir367, N. R., Wiersema367, K., Levan325, A. J., Steeghs325, D., Hjorth305, J., Fynbo305, J. P. U., Malesani305, D., Milvang Jensen305, B., Watson305, D., Irwin355, M., Fernandez355, C. G., Mcmahon355, R. G., Banerji355, M., Gonzalez Solares355, E., Schulze353, S., 375, de Ugarte Postigo305, A., 376, Thoene376, C. C., Cano377, Z., Rosswog306, S., (Astro)-Particles Physics, Abbott, B. P., Abbott, R., Abbott, T. D., Abernathy, M. R., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R. X., Adya, V. B., Affeldt, C., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, B., Allocca, A., Altin, P. A., Anderson, S. B., Anderson, W. G., Arai, K., Araya, M. C., Arceneaux, C. C., Areeda, J. S., Arnaud, N., Arun, K. G., Ascenzi, S., Ashton, G., Ast, M., Aston, S. M., Astone, P., Aufmuth, P., Aulbert, C., Babak, S., Bacon, P., Bader, M. K. M., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Barthelmy, S., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Batch, J. C., Baune, C., Bavigadda, V., Bazzan, M., Behnke, B., Bejger, M., Bell, A. S., Bell, C. J., Berger, B. K., Bergman, J., Bergmann, G., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhagwat, S., Bhandare, R., Bilenko, I. A., Billingsley, G., Birch, J., Birney, R., Biscans, S., Bisht, A., Bitossi, M., Biwer, C., Bizouard, M. A., Blackburn, J. K., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bock, O., Bodiya, T. P., Boer, M., Bogaert, G., Bogan, C., Bohe, A., Bojtos, P., Bond, C., Bondu, F., Bonnand, R., Boom, B. A., Bork, R., Boschi, V., Bose, S., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Braginsky, V. B., Branchesi, M., Brau, J. E., Briant, T., Brillet, A., Brinkmann, M., Brisson, V., Brockill, P., Brooks, A. F., Brown, D. A., Brown, D. D., Brown, N. M., Buchanan, C. C., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. L., Cadonati, L., Cagnoli, G., Cahillane, C., Bustillo, J. C., Callister, T., Calloni, Enrico, Camp, J. B., Cannon, K. C., Cao, J., Capano, C. D., Capocasa, E., Carbognani, F., Caride, S., Diaz, J. C., Casentini, C., Caudill, S., Cavagliá, M., Cavalier, F., Cavalieri, R., Cella, G., Cepeda, C. B., Baiardi, L. C., Cerretani, G., Cesarini, E., Chakraborty, R., Chalermsongsak, T., Chamberlin, S. J., Chan, M., Chao, S., Charlton, P., Chassande Mottin, E., Chen, H. Y., Chen, Y., Cheng, C., Chincarini, A., Chiummo, A., Cho, H. S., Cho, M., Chow, J. H., Christensen, N., Chu, Q., Chua, S., Chung, S., Ciani, G., Clara, F., Clark, J. A., Cleva, F., Coccia, E., Cohadon, P. F., Colla, A., Collette, C. G., Cominsky, L., Constancio, M., Conte, A., Conti, L., Cook, D., Corbitt, T. R., Cornish, N., Corsi, A., Cortese, S., Costa, C. A., Coughlin, M. W., Coughlin, S. B., Coulon, J. P., Countryman, S. T., Couvares, P., Cowan, E. E., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Craig, K., Creighton, J. D. E., Cripe, J., Crowder, S. G., Cumming, A., Cunningham, L., Cuoco, E., Dal Canton, T., Danilishin, S. L., D'Antonio, S., Danzmann, K., Darman, N. S., Dattilo, V., Dave, I., Daveloza, H. P., Davier, M., Davies, G. S., Daw, E. J., Day, R., Debra, D., Debreczeni, G., Degallaix, J., DE LAURENTIS, Martina, Deléglise, S., Del Pozzo, W., Denker, T., Dent, T., Dereli, H., Dergachev, V., Derosa, R. T., DE ROSA, Rosario, Desalvo, R., Dhurandhar, S., Díaz, M. C., Di Fiore, L., Di Giovanni, M., Di Lieto, A., Di Pace, S., Di Palma, I., Di Virgilio, A., Dojcinoski, G., Dolique, V., Donovan, F., Dooley, K. L., Doravari, S., Douglas, R., Downes, T. P., Drago, M., Drever, R. W. P., Driggers, J. C., Du, Z., Ducrot, M., Dwyer, S. E., Edo, T. B., Edwards, M. C., Effler, A., Eggenstein, H. B., Ehrens, P., Eichholz, J., Eikenberry, S. S., Engels, W., Essick, R. C., Etzel, T., Evans, M., Evans, T. M., Everett, R., Factourovich, M., Fafone, V., Fair, H., Fairhurst, S., Fan, X., Fang, Q., Farinon, S., Farr, B., Farr, W. M., Favata, M., Fays, M., Fehrmann, H., Fejer, M. M., Ferrante, I., Ferreira, E. C., Ferrini, F., Fidecaro, F., Fiori, I., Fiorucci, D., Fisher, R. P., Flaminio, R., Fletcher, M., Fournier, J. D., Franco, S., Frasca, S., Frasconi, F., Frei, Z., Freise, A., Frey, R., Frey, V., Fricke, T. T., Fritschel, P., Frolov, V. V., Fulda, P., Fyffe, M., Gabbard, H. A. G., Gair, J. R., Gammaitoni, L., Gaonkar, S. G., Garufi, Fabio, Gatto, A., Gaur, G., Gehrels, N., Gemme, G., Gendre, B., Genin, E., Gennai, A., George, J., Gergely, L., Germain, V., Ghosh, A., Ghosh, S., Giaime, J. A., Giardina, K. D., Giazotto, A., Gill, K., Glaefke, A., Goetz, E., Goetz, R., Gondan, L., González, G., Castro, J. M. G., Gopakumar, A., Gordon, N. A., Gorodetsky, M. L., Gossan, S. E., Gosselin, M., Gouaty, R., Graef, C., Graff, P. B., Granata, M., Grant, A., Gras, S., Gray, C., Greco, G., Green, A. C., Groot, P., Grote, H., Grunewald, S., Guidi, G. M., Guo, X., Gupta, A., Gupta, M. K., Gushwa, K. E., Gustafson, E. K., Gustafson, R., Hacker, J. J., Hall, B. R., Hall, E. D., Hammond, G., Haney, M., Hanke, M. M., Hanks, J., Hanna, C., Hannam, M. D., Hanson, J., Hardwick, T., Haris, K., Harms, J., Harry, G. M., Harry, I. W., Hart, M. J., Hartman, M. T., Haster, C. J., Haughian, K., Heidmann, A., Heintze, M. C., Heitmann, H., Hello, P., Hemming, G., Hendry, M., Heng, I. S., Hennig, J., Heptonstall, A. W., Heurs, M., Hild, S., Hoak, D., Hodge, K. A., Hofman, D., Hollitt, S. E., Holt, K., Holz, D. E., Hopkins, P., Hosken, D. J., Hough, J., Houston, E. A., Howell, E. J., Hu, Y. M., Huang, S., Huerta, E. A., Huet, D., Hughey, B., Husa, S., Huttner, S. H., Huynh Dinh, T., Idrisy, A., Indik, N., Ingram, D. R., Inta, R., Isa, H. N., Isac, J. M., Isi, M., Islas, G., Isogai, T., Iyer, B. R., Izumi, K., Jacqmin, T., Jang, H., Jani, K., Jaranowski, P., Jawahar, S., Jiménez Forteza, F., Johnson, W. W., Jones, D. I., Jones, R., Jonker, R. J. G., Ju, L., Kalaghatgi, C. V., Kalogera, V., Kandhasamy, S., Kang, G., Kanner, J. B., Karki, S., Kasprzack, M., Katsavounidis, E., Katzman, W., Kaufer, S., Kaur, T., Kawabe, K., Kawazoe, F., Kéfélian, F., Kehl, M. S., Keitel, D., Kelley, D. B., Kells, W., Kennedy, R., Key, J. S., Khalaidovski, A., Khalili, F. Y., Khan, I., Khan, S., Khan, Z., Khazanov, E. A., Kijbunchoo, N., Kim, C., Kim, J., Kim, K., Kim, N., Kim, Y. M., King, E. J., King, P. J., Kinzel, D. L., Kissel, J. S., Kleybolte, L., Klimenko, S., Koehlenbeck, S. M., Kokeyama, K., Koley, S., Kondrashov, V., Kontos, A., Korobko, M., Korth, W. Z., Kowalska, I., Kozak, D. B., Kringel, V., Królak, A., Krueger, C., Kuehn, G., Kumar, P., Kuo, L., Kutynia, A., Lackey, B. D., Landry, M., Lange, J., Lantz, B., Lasky, P. D., Lazzarini, A., Lazzaro, C., Leaci, P., Leavey, S., Lebigot, E. O., Lee, C. H., Lee, H. K., Lee, H. M., Lee, K., Lenon, A., Leonardi, M., Leong, J. R., Leroy, N., Letendre, N., Levin, Y., Levine, B. M., Li, T. G. F., Libson, A., Littenberg, T. B., Lockerbie, N. A., Logue, J., Lombardi, A. L., Lord, J. E., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lough, J. D., Lück, H., Lundgren, A. P., Luo, J., Lynch, R., Ma, Y., Macdonald, T., Machenschalk, B., Macinnis, M., Macleod, D. M., Magaña Sandoval, F., Magee, R. M., Mageswaran, M., Majorana, E., Maksimovic, I., Malvezzi, V., Man, N., Mandel, I., Mandic, V., Mangano, V., Mansell, G. L., Manske, M., Mantovani, M., Marchesoni, F., Marion, F., Márka, S., Márka, Z., Markosyan, A. S., Maros, E., Martelli, F., Martellini, L., Martin, I. W., Martin, R. M., Martynov, D. V., Marx, J. N., Mason, K., Masserot, A., Massinger, T. J., Masso Reid, M., Matichard, F., Matone, L., Mavalvala, N., Mazumder, N., Mazzolo, G., Mccarthy, R., Mcclelland, D. E., Mccormick, S., Mcguire, S. C., Mcintyre, G., Mciver, J., Mcmanus, D. J., Mcwilliams, S. T., Meacher, D., Meadors, G. D., Meidam, J., Melatos, A., Mendell, G., Mendoza Gandara, D., Mercer, R. A., Merilh, E., Merzougui, M., Meshkov, S., Messenger, C., Messick, C., Meyers, P. M., Mezzani, F., Miao, H., Michel, C., Middleton, H., Mikhailov, E. E., Milano, Leopoldo, Miller, J., Millhouse, M., Minenkov, Y., Ming, J., Mirshekari, S., Mishra, C., Mitra, S., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Moggi, A., Mohan, M., Mohapatra, S. R. P., Montani, M., Moore, B. C., Moore, C. J., Moraru, D., Moreno, G., Morriss, S. R., Mossavi, K., Mours, B., Mow Lowry, C. M., Mueller, C. L., Mueller, G., Muir, A. W., Mukherjee, A., Mukherjee, D., Mukherjee, S., Mukund, N., Mullavey, A., Munch, J., Murphy, D. J., Murray, P. G., Mytidis, A., Nardecchia, I., Naticchioni, L., Nayak, R. K., Necula, V., Nedkova, K., Nelemans, G., Neri, M., Neunzert, A., Newton, G., Nguyen, T. T., Nielsen, A. B., Nissanke, S., Nitz, A., Nocera, F., Nolting, D., Normandin, M. E. N., Nuttall, L. K., Oberling, J., Ochsner, E., O'Dell, J., Oelker, E., Ogin, G. H., Oh, J. J., Oh, S. H., Ohme, F., Oliver, M., Oppermann, P., Oram, R. J., O'Reilly, B., O'Shaughnessy, R., Ottaway, D. J., Ottens, R. S., Overmier, H., Owen, B. J., Pai, A., Pai, S. A., Palamos, J. R., Palashov, O., Palliyaguru, N., Palomba, C., Pal Singh, A., Pan, H., Pankow, C., Pannarale, F., Pant, B. C., Paoletti, F., Paoli, A., Papa, M. A., Paris, H. R., Parker, W., Pascucci, D., Pasqualetti, A., Passaquieti, R., Passuello, D., Patricelli, B., Patrick, Z., Pearlstone, B. L., Pedraza, M., Pedurand, R., Pekowsky, L., Pele, A., Penn, S., Perreca, A., Phelps, M., Piccinni, O., Pichot, M., Piergiovanni, F., Pierro, V., Pillant, G., Pinard, L., Pinto, I. M., Pitkin, M., Poggiani, R., Popolizio, P., Post, A., Powell, J., Prasad, J., Predoi, V., Premachandra, S. S., Prestegard, T., Price, L. R., Prijatelj, M., Principe, M., Privitera, S., Prodi, G. A., Prokhorov, L., Puncken, O., Punturo, M., Puppo, P., Pürrer, M., Qi, H., Qin, J., Quetschke, V., Quintero, E. A., Quitzow James, R., Raab, F. J., Rabeling, D. S., Radkins, H., Raffai, P., Raja, S., Rakhmanov, M., Rapagnani, P., Raymond, V., Razzano, M., Re, V., Read, J., Reed, C. M., Regimbau, T., Rei, L., Reid, S., Reitze, D. H., Rew, H., Reyes, S. D., Ricci, F., Riles, K., Robertson, N. A., Robie, R., Robinet, F., Rocchi, A., Rolland, L., Rollins, J. G., Roma, V. J., Romano, R., Romanov, G., Romie, J. H., Rosińska, D., Rowan, S., Rüdiger, A., Ruggi, P., Ryan, K., Sachdev, S., Sadecki, T., Sadeghian, L., Salconi, L., Saleem, M., Salemi, F., Samajdar, A., Sammut, L., Sanchez, E. J., Sandberg, V., Sandeen, B., Sanders, J. R., Sassolas, B., Sathyaprakash, B. S., Saulson, P. R., Sauter, O., Savage, R. L., Sawadsky, A., Schale, P., Schilling, R., Schmidt, J., Schmidt, P., Schnabel, R., Schofield, R. M. S., Schönbeck, A., Schreiber, E., Schuette, D., Schutz, B. F., Scott, J., Scott, S. M., Sellers, D., Sentenac, D., Sequino, V., Sergeev, A., Serna, G., Setyawati, Y., Sevigny, A., Shaddock, D. A., Shah, S., Shahriar, M. S., Shaltev, M., Shao, Z., Shapiro, B., Shawhan, P., Sheperd, A., Shoemaker, D. H., Shoemaker, D. M., Siellez, K., Siemens, X., Sigg, D., Silva, A. D., Simakov, D., Singer, A., Singh, A., Singh, R., Singhal, A., Sintes, A. M., Slagmolen, B. J. J., Smith, J. R., Smith, N. D., Smith, R. J. E., Son, E. J., Sorazu, B., Sorrentino, F., Souradeep, T., Srivastava, A. K., Staley, A., Steinke, M., Steinlechner, J., Steinlechner, S., Steinmeyer, D., Stephens, B. C., Stone, R., Strain, K. A., Straniero, N., Stratta, G., Strauss, N. A., Strigin, S., Sturani, R., Stuver, A. L., Summerscales, T. Z., Sun, L., Sutton, P. J., Swinkels, B. L., Szczepańczyk, M. J., Tacca, M., Talukder, D., Tanner, D. B., Tápai, M., Tarabrin, S. P., Taracchini, A., Taylor, R., Theeg, T., Thirugnanasambandam, M. P., Thomas, E. G., Thomas, M., Thomas, P., Thorne, K. A., Thorne, K. S., Thrane, E., Tiwari, S., Tiwari, V., Tokmakov, K. V., Tomlinson, C., Tonelli, M., Torres, C. V., Torrie, C. I., Töyrä, D., Travasso, F., Traylor, G., Trifirò, D., Tringali, M. C., Trozzo, L., Tse, M., Turconi, M., Tuyenbayev, D., Ugolini, D., Unnikrishnan, C. S., Urban, A. L., Usman, S. A., Vahlbruch, H., Vajente, G., Valdes, G., Van Bakel, N., Van Beuzekom, M., Van Den Brand, J. F. J., Van Den Broeck, C., Vander Hyde, D. C., Van Der Schaaf, L., Van Heijningen, J. V., Van Veggel, A. A., Vardaro, M., Vass, S., Vasúth, M., Vaulin, R., Vecchio, A., Vedovato, G., Veitch, J., Veitch, P. J., Venkateswara, K., Verkindt, D., Vetrano, F., Viceré, A., Vinciguerra, S., Vine, D. J., Vinet, J. Y., Vitale, S., Vo, T., Vocca, H., Vorvick, C., Voss, D., Vousden, W. D., Vyatchanin, S. P., Wade, A. R., Wade, L. E., Wade, M., Walker, M., Wallace, L., Walsh, S., Wang, G., Wang, H., Wang, M., Wang, X., Wang, Y., Ward, R. L., Warner, J., Was, M., Weaver, B., Wei, L. W., Weinert, M., Weinstein, A. J., Weiss, R., Welborn, T., Wen, L., Weßels, P., Westphal, T., Wette, K., Whelan, J. T., White, D. J., Whiting, B. F., Williams, R. D., Williamson, A. R., Willis, J. L., Willke, B., Wimmer, M. H., Winkler, W., Wipf, C. C., Wittel, H., Woan, G., Worden, J., Wright, J. L., Wu, G., Yablon, J., Yam, W., Yamamoto, H., Yancey, C. C., Yap, M. J., Yu, H., Yvert, M., Zadrożny, A., Zangrando, L., Zanolin, M., Zendri, J. P., Zevin, M., Zhang, F., Zhang, L., Zhang, M., Zhang, Y., Zhao, C., Zhou, M., Zhou, Z., Zhu, X. J., Zucker, M. E., Zuraw, S. E., Zweizig, J., Allison, J., Bannister, K., Bell, M. E., Chatterjee, S., Chippendale, A. P., Edwards, P. G., Harvey Smith, L., Heywood, Ian, Hotan, A., Indermuehle, B., Marvil, J., Mcconnell, D., Murphy, T., Popping, A., Reynolds, J., Sault, R. J., Voronkov, M. A., Whiting, M. T., Castro Tirado, A. J., Cunniffe, R., Jelínek, M., Tello, J. C., Oates, S. R., Hu, Y. D., Kubánek, P., Guziy, S., Castellón, A., García Cerezo, A., Muñoz, V. F., Pérez Del Pulgar, C., Castillo Carrión, S., Castro Cerón, J. M., Hudec, R., Caballero García, M. D., Páta, P., Vitek, S., Adame, J. A., Konig, S., Rendón, F., Mateo Sanguino, T. De J., Fernández Muñoz, R., Yock, P. C., Rattenbury, N., Allen, W. H., Querel, R., Jeong, S., Park, I. H., Bai, J., Cui, C. h., Fan, Y., Wang, C. h., Hiriart, D., Lee, W. H., Claret, A., Sánchez Ramírez, R., Pandey, S. B., Mediavilla, T., Sabau Graziati, L., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Armstrong, R., Benoit Lévy, A., Berger, E., Bernstein, R. A., Bertin, E., Brout, D., Buckley Geer, E., Burke, D. L., Capozzi, D., Carretero, J., Castander, F. J., Chornock, R., Cowperthwaite, P. S., Crocce, M., Cunha, C. E., D'Andrea, C. B., Da Costa, L. N., Desai, S., Diehl, H. T., Dietrich, J. P., Doctor, Z., Drlica Wagner, A., Drout, M. R., Eifler, T. F., Estrada, J., Evrard, A. E., Fernandez, E., Finley, D. A., Flaugher, B., Foley, R. J., Fong, W. F., Fosalba, P., Fox, D. B., Frieman, J., Fryer, C. L., Gaztanaga, E., Gerdes, D. W., Goldstein, D. A., Gruen, D., Gruendl, R. A., Gutierrez, G., Herner, K., Honscheid, K., James, D. J., Johnson, M. D., Johnson, M. W. G., Karliner, I., Kasen, D., Kent, S., Kessler, R., Kim, A. G., Kind, M. C., Kuehn, K., Kuropatkin, N., Lahav, O., Li, T. S., Lima, M., Lin, H., Maia, M. A. G., Margutti, R., Marriner, J., Martini, P., Matheson, T., Melchior, P., Metzger, B. D., Miller, C. J., Miquel, R., Neilsen, E., Nichol, R. C., Nord, B., Nugent, P., Ogando, R., Petravick, D., Plazas, A. A., Quataert, E., Roe, N., Romer, A. K., Roodman, A., Rosell, A. C., Rykoff, E. S., Sako, M., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Scolnic, D., Sevilla Noarbe, I., Sheldon, E., Smith, N., Smith, R. C., Soares Santos, M., Sobreira, F., Stebbins, A., Suchyta, E., Swanson, M. E. C., Tarle, G., Thaler, J., Thomas, D., Thomas, R. C., Tucker, D. L., Vikram, V., Walker, A. R., Wechsler, R. H., Wester, W., Yanny, B., Zuntz, J., Connaughton, V., Burns, E., Goldstein, A., Briggs, M. S., Zhang, B. B., Hui, C. M., Jenke, P., Wilson Hodge, C. A., Bhat, P. N., Bissaldi, E., Cleveland, W., Fitzpatrick, G., Giles, M. M., Gibby, M. H., Greiner, J., Von Kienlin, A., Kippen, R. M., Mcbreen, S., Mailyan, B., Meegan, C. A., Paciesas, W. S., Preece, R. D., Roberts, O., Sparke, L., Stanbro, M., Toelge, K., Veres, P., Yu, H. F., Blackburn, L., Ackermann, M., Ajello, M., Albert, A., Anderson, B., Atwood, W. B., Axelsson, M., Baldini, L., Barbiellini, G., Bastieri, D., Bellazzini, R., Blandford, R. D., Bloom, E. D., Bonino, R., Bottacini, E., Brandt, T. J., Bruel, P., Buson, S., Caliandro, G. A., Cameron, R. A., Caragiulo, M., Caraveo, P. A., Cavazzuti, E., Charles, E., Chekhtman, A., Chiang, J., Chiaro, G., Ciprini, S., Cohen Tanugi, J., Cominsky, L. R., Costanza, F., Cuoco, A., D'Ammando, F., De Palma, F., Desiante, R., Digel, S. W., Di Lalla, N., Di Mauro, M., Di Venere, L., Domínguez, A., Drell, P. S., Dubois, R., Favuzzi, C., Ferrara, E. C., Franckowiak, A., Fukazawa, Y., Funk, S., Fusco, P., Gargano, F., Gasparrini, D., Giglietto, N., Giommi, P., Giordano, F., Giroletti, M., Glanzman, T., Godfrey, G., Gomez Vargas, G. A., Green, D., Grenier, I. A., Grove, J. E., Guiriec, S., Hadasch, D., Harding, A. K., Hays, E., Hewitt, J. W., Hill, A. B., Horan, D., Jogler, T., Jóhannesson, G., Johnson, A. S., Kensei, S., Kocevski, D., Kuss, M., La Mura, G., Larsson, S., Latronico, L., Li, J., Li, L., Longo, F., Loparco, F., Lovellette, M. N., Lubrano, P., Magill, J., Maldera, S., Manfreda, A., Marelli, M., Mayer, M., Mazziotta, M. N., Mcenery, J. E., Meyer, M., Michelson, P. F., Mirabal, N., Mizuno, T., Moiseev, A. A., Monzani, M. E., Moretti, E., Morselli, A., Moskalenko, I. V., Negro, M., Nuss, E., Ohsugi, T., Omodei, N., Orienti, M., Orlando, E., Ormes, J. F., Paneque, D., Perkins, J. S., Pesce Rollins, M., Piron, F., Pivato, G., Porter, T. A., Racusin, J. L., Rainò, S., Rando, R., Razzaque, S., Reimer, A., Reimer, O., Salvetti, D., Parkinson, P. M. Saz, Sgrò, C., Simone, D., Siskind, E. J., Spada, F., Spandre, G., Spinelli, P., Suson, D. J., Tajima, H., Thayer, J. B., Thompson, D. J., Tibaldo, L., Torres, D. F., Troja, E., Uchiyama, Y., Venters, T. M., Vianello, G., Wood, K. S., Wood, M., Zhu, S., Zimmer, S., Brocato, E., Cappellaro, E., Covino, S., Grado, A., Nicastro, L., Palazzi, E., Pian, E., Amati, L., Antonelli, L. A., Capaccioli, M., D'Avanzo, P., D'Elia, V., Getman, F., Giuffrida, G., Iannicola, G., Limatola, L., Lisi, M., Marinoni, S., Marrese, P., Melandri, A., Piranomonte, S., Possenti, A., Pulone, L., Rossi, A., Stamerra, A., Stella, L., Testa, V., Tomasella, L., Yang, S., Bazzano, A., Bozzo, E., Brandt, S., Courvoisier, T. J. L., Ferrigno, C., Hanlon, L., Kuulkers, E., Laurent, P., Mereghetti, S., Roques, J. P., Savchenko, V., Ubertini, P., Kasliwal, M. M., Singer, L. P., Cao, Y., Duggan, G., Kulkarni, S. R., Bhalerao, V., Miller, A. A., Barlow, T., Bellm, E., Manulis, I., Rana, J., Laher, R., Masci, F., Surace, J., Rebbapragada, U., Sistine, A. Van, Sesar, B., Perley, D., Ferreti, R., Prince, T., Kendrick, R., Horesh, A., Hurley, K., Golenetskii, S. V., Aptekar, R. L., Frederiks, D. D., Svinkin, D. S., Rau, A., Zhang, X., Smith, D. M., Cline, T., Krimm, H., Abe, F., Doi, M., Fujisawa, K., Kawabata, K. S., Morokuma, T., Motohara, K., Tanaka, M., Ohta, K., Yanagisawa, K., Yoshida, M., Baltay, C., Rabinowitz, D., Ellman, N., Rostami, S., Bersier, D. F., Bode, M. F., Collins, C. A., Copperwheat, C. M., Darnley, M. J., Galloway, Duncan K., Gomboc, A., Kobayashi, S., Mazzali, P., Mundell, C. G., Piascik, A. S., Pollacco, Don, Steele, I. A., Ulaczyk, K., Broderick, J. W., Fender, R. P., Jonker, P. G., Rowlinson, A., Stappers, B. W., Wijers, R. A. M. J., Lipunov, V., Gorbovskoy, E., Tyurina, N., Kornilov, V., Balanutsa, P., Kuznetsov, A., Buckley, D., Rebolo, R., Serra Ricart, M., Israelian, G., Budnev, N. M., Gress, O., Ivanov, K., Poleshuk, V., Tlatov, A., Yurkov, V., Kawai, N., Serino, M., Negoro, H., Nakahira, S., Mihara, T., Tomida, H., Ueno, S., Tsunemi, H., Matsuoka, M., Croft, S., Feng, L., Franzen, T. M. O., Gaensler, B. M., Johnston Hollitt, M., Kaplan, D. L., Morales, M. F., Tingay, S. J., Wayth, R. B., Williams, A., Smartt, S. J., Chambers, K. C., Smith, K. W., Huber, M. E., Young, D. R., Wright, D. E., Schultz, A., Denneau, L., Flewelling, H., Magnier, E. A., Primak, N., Rest, A., Sherstyuk, A., Stalder, B., Stubbs, C. W., Tonry, J., Waters, C., Willman, M., Olivares, E. F., Campbell, H., Kotak, R., Sollerman, J., Smith, M., Dennefeld, M., Anderson, J. P., Botticella, M. T., Chen, T. W., Valle, M. D., Elias Rosa, N., Fraser, M., Inserra, C., Kankare, E., Kupfer, T., Harmanen, J., Galbany, L., Guillou, L. Le, Lyman, J. D., Maguire, K., Mitra, A., Nicholl, M., Razza, A., Terreran, G., Valenti, S., Gal Yam, A., Ćwiek, A., Ćwiok, M., Mankiewicz, L., Opiela, R., Zaremba, M., Żarnecki, A. F., Onken, C. A., Scalzo, R. A., Schmidt, B. P., Wolf, C., Yuan, F., Evans, P. A., Kennea, J. A., Burrows, D. N., Campana, S., Cenko, S. B., Marshall, F. E., Nousek, J., O'Brien, P., Osborne, J. P., Palmer, D., Perri, M., Siegel, M., Tagliaferri, G., Klotz, A., Turpin, D., Laugier, R., Beroiz, M., Peñuela, T., Macri, L. M., Oelkers, R. J., Lambas, D. G., Vrech, R., Cabral, J., Colazo, C., Dominguez, M., Sanchez, B., Gurovich, S., Lares, M., Marshall, J. L., Depoy, D. L., Padilla, N., Pereyra, N. A., Benacquista, M., Tanvir, N. R., Wiersema, K., Levan, A. J., Steeghs, D., Hjorth, J., Fynbo, J. P. U., Malesani, D., Milvang Jensen, B., Watson, D., Irwin, M., Fernandez, C. G., Mcmahon, R. G., Banerji, M., Gonzalez Solares, E., Schulze, S., De Ugarte Postigo, A., Thoene, C. C., Cano, Z., Rosswog, S., Institut Lumière Matière [Villeurbanne] ( ILM ), Université Claude Bernard Lyon 1 ( UCBL ), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique ( CNRS ), Laboratoire des matériaux avancés ( LMA ), 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 ), Laboratoire Leprince-Ringuet ( LLR ), Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -École polytechnique ( X ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire Univers et Particules de Montpellier ( LUPM ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Montpellier 2 - Sciences et Techniques ( UM2 ) -Université de Montpellier ( UM ), Laboratoire de Physique Nucléaire et de Hautes Énergies ( LPNHE ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -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 ), 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 ), 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 ), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux ( ARTEMIS ), Université Nice Sophia Antipolis ( UNS ), Université Côte d'Azur ( UCA ) -Université Côte d'Azur ( UCA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de la Côte d'Azur, Université Côte d'Azur ( UCA ) -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 ), LIGO, VIRGO, FERMI LAT, PESSTO, Institut Lumière Matière [Villeurbanne] (ILM), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), Laboratoire des matériaux avancés (LMA), 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), Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Particules de Montpellier (LUPM), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Université Pierre et Marie Curie - Paris 6 (UPMC)-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), 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), 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), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique de Rennes (IPR), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), The LIGO Scientific Collaboration, The Virgo Collaboration, The Australian Square Kilometer Array, Pathfinder (ASKAP) Collaboration, The BOOTES Collaboration, The Dark Energy Survey and the Dark Energy Camera GW-EM Collaborations, The Fermi GBM Collaboration, The Fermi LAT Collaboration, The GRAvitational Wave Inaf TeAm (GRAWITA), The Intermediate Palomar Transient Factory (iPTF) Collaboration, The InterPlanetary Network, The J-GEM Collaboration, The La Silla--QUEST Survey, The Liverpool Telescope Collaboration, The Low Frequency Array (LOFAR) Collaboration, The MASTER Collaboration, The MAXI Collaboration, The Murchison Wide-field Array (MWA) Collaboration, The Pan-STARRS Collaboration, The PESSTO Collaboration, The Pi of the Sky Collaboration, The SkyMapper Collaboration, The Swift Collaboration, The TAROT, Zadko, Algerian National Observatory, C2PU Collaboration, The TOROS Collaboration, The VISTA Collaboration, Calloni, E., De Laurentis, M., De Rosa, R., Garufi, F., Milano, L., Longo, Francesco, Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université Montpellier 2 - 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F., M. Constancio J. r., Coulon, J. -. P., D’Antonio, S., Eggenstein, H. -. B., Fournier, J. -. D., A., Gatto, Haster, C. -. J., Huynh-Dinh, T., Isac, J. -. M., Jiménez-Forteza, F., Kim, Y. -. M., Magaña-Sandoval, F., Masso-Reid, M., Mendoza-Gandara, D., C., Michel, Mow-Lowry, C. M., O’Dell, J., O’Reilly, B., O’Shaughnessy, R., Pal-Singh, A., Quitzow-James, R., A., Singh, van Bakel, N., van Beuzekom, M., van den Brand, J. F. J., Vander-Hyde, D. C., van der Schaaf, L., van Heijningen, J. V., van Veggel, A. A., Vinet, J. -. Y., M., Wade, Wei, L. -. W., Wessels, P., Zendri, J. -. P., the Virgo Collaboration, Harvey-Smith, L., Ian, Heywood, The Australian Square Kilometer Array Pathfinder (ASKAP) Collaboration, Castro-Tirado, A. J., Hu, Y. -. D., García-Cerezo, A., Pérez del Pulgar, C., Castillo-Carrión, S., Caballero-García, M. D., Mateo Sanguino, T. de J., Fernández-Muñoz, R., Sánchez-Ramírez, R., Sabau-Graziati, L., Benoit-Lévy, A., Buckley-Geer, E., D’Andrea, C. B., da Costa, L. 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Inst, Univ Tokyo, Yamaguchi Univ, Kyoto Univ, Yale Univ, Liverpool JMU, Univ Nova Gorica, Univ Ljubljana, Univ Bath, Univ Warwick, Netherlands Inst Radio Astron, Univ Oxford, SRON Netherlands Inst Space Res, Univ Amsterdam, South African Astron Observ, Inst Astrofis Canarias, Irkutsk State Univ, Main Pulkovo Observ RAS, Blagoveschensk State Pedag Univ, Tokyo Inst Technol, RIKEN, Nihon Univ, Japan Aerosp Explorat Agcy, Japan Aerosp Explorat Agcy JAXA, Osaka Univ, Eureka Sci Inc, Curtin Univ, Victoria Univ Wellington, and Ist Nazl Astrofis
Subjects: Astronomy, ADVANCED LIGO, 01 natural sciences, General Relativity and Quantum Cosmology, localization, GW150914, localization, EM follow-up, Observatory, Broadband, BURSTS, GeneralLiterature_REFERENCE(e.g.,dictionaries,encyclopedias,glossaries), 010303 astronomy & astrophysics, gravitational wave, QC, media_common, QB, Physics, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), gravitational waves, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], methods: observational, Astrophysics - High Energy Astrophysical Phenomena, Cosmology and Gravitation, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], gravitational waves – methods: observational, media_common.quotation_subject, gr-qc, Astrophysics::High Energy Astrophysical Phenomena, GW150914, FOS: Physical sciences, ENERGY CAMERA SEARCH, General Relativity and Quantum Cosmology (gr-qc), NEUTRON-STAR MERGERS, Gravitational waves, [ PHYS.GRQC ] Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Binary black hole, observational, Astronomy and Astrophysics, Space and Planetary Science [gravitational waves, methods], 0103 physical sciences, GW151226, observational [Methods], EM follow-up, STFC, RADIO, 010308 nuclear & particles physics, Gravitational wave, ST/I001123/1, RCUK, [ PHYS.ASTR.HE ] Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], COUNTERPARTS, Astronomy and Astrophysic, LIGO, Neutron star, Space and Planetary Science, Sky, ST/L000709/1, EMISSION
Abstract: A gravitational-wave (GW) transient was identified in data recorded by the Advanced Laser Interferometer Gravitational-wave Observatory (LIGO) detectors on 2015 September 14. The event, initially designated G184098 and later given the name GW150914, is described in detail elsewhere. By prior arrangement, preliminary estimates of the time, significance, and sky location of the event were shared with 63 teams of observers covering radio, optical, near-infrared, X-ray, and gamma-ray wavelengths with ground- and space-based facilities. In this Letter we describe the low-latency analysis of the GW data and present the sky localization of the first observed compact binary merger. We summarize the follow-up observations reported by 25 teams via private Gamma-ray Coordinates Network circulars, giving an overview of the participating facilities, the GW sky localization coverage, the timeline and depth of the observations. As this event turned out to be a binary black hole merger, there is little expectation of a detectable electromagnetic (EM) signature. Nevertheless, this first broadband campaign to search for a counterpart of an Advanced LIGO source represents a milestone and highlights the broad capabilities of the transient astronomy community and the observing strategies that have been developed to pursue neutron star binary merger events. Detailed investigations of the EM data and results of the EM follow-up campaign are being disseminated in papers by the individual teams., Comment: For Supplement, see https://arxiv.org/abs/1604.07864
Published: 2016

28. The exceptionally extended flaring activity in the X-ray afterglow of GRB 050730 observed with Swift and XMM-Newton

Author: Paolo Giommi, P. Romano, G. Chincarini, James Reeves, Milvia Capalbi, J. A. Nousek, Gianpiero Tagliaferri, J. E. Hill, Teresa Mineo, L. A. Antonelli, Antonino Cucchiara, A. P. Beardmore, Neil Gehrels, Lorella Angelini, Sergio Campana, M. Perri, Eleonora Troja, David N. Burrows, C. Pagani, R. L. C. Starling, V. La Parola, Stephen T. Holland, L. Vetere, P. Boyd, Dafne Guetta, P. W. A. Roming, V. Mangano, Gaspare Cusumano, Alberto Moretti, J. P. Osborne, PERRI M, GUETTA D, ANTONELLI L A, CUCCHIARA A, MANGANO V, REEVES J, ANGELINI L, BEARDMORE A P, BOYD P, BURROWS D N, CAMPANA S, CAPALBI M, CHINCARINI G, CUSUMANO G, GIOMMI P, HILL J E, HOLLAND S T, LA PAROLA V, MINEO T, MORETTI A, NOUSEK J A, OSBORNE J P, PAGANI C, ROMANO P, ROMING P W A, STARLING R L C, TAGLIAFERRI G, TROJA E, VETERE L, and GEHRELS N
Subjects: Physics, Astrophysics (astro-ph), X-ray, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Redshift, Galaxy, law.invention, Afterglow, Spectral evolution, Space and Planetary Science, law, Gamma-ray burst, Order of magnitude, Flare
Abstract: We present the results of a detailed spectral and temporal analysis of Swift and XMM-Newton observations of the high redshift (z=3.969) GRB 050730. The X-ray afterglow of GRB 050730 was found to decline with time with superimposed intense flaring activity that extended over more than two orders of magnitude in time. Seven distinct re-brightening events starting from 236 s up to 41.2 ks after the burst were observed. The underlying decay of the afterglow was well described by a double broken power-law model with breaks at t_1= 237 +/- 20 s and t_2 = 10.1 (-2.2) (+4.6) ks. The temporal decay slopes before, between and after these breaks were alpha_1 = 2.1 +/- 0.3, alpha_2 = 0.44 (-0.08) (+0.14) and alpha_3 = 2.40 (+0.07) (-0.09), respectively. The spectrum of the X-ray afterglow was well described by a photoelectrically absorbed power-law with an absorbing column density N_H=(1.28 +/- 0.26) 10^22 cm^-2 in the host galaxy. Strong X-ray spectral evolution during the flaring activity was present. In the majority of the flares (6/7) the ratio Delta_t/t_p between the duration of the event and the time when the flare peaks was nearly constant and about 0.6-0.7. We showed that the observed spectral and temporal properties of the first three flares are consistent with being due both to high-latitude emission, as expected if the flares were produced by late internal shocks, or to refreshed shocks, i.e. late time energy injections into the main afterglow shock by slow moving shells ejected from the central engine during the prompt phase. The event fully satisfies the E_p-E_iso Amati relation while is not consistent with the E_p-E_jet Ghirlanda relation., Comment: 12 pages, 5 figures, accepted for publication in A&A
Published: 2007

29. Swift observations of GRB050904: the most distant cosmic explosion ever observed

Author: A. Panaitescu, C. Gronwall, Sergio Campana, G. Tagliaferri, Teresa Mineo, Stefan Immler, T. Sakamoto, J. A. Kennea, E. E. Fenimore, P. W. A. Roming, David N. Burrows, Lorella Angelini, M. R. Goad, Alan A. Wells, P. Giommi, A. P. Beardmore, D. M. Palmer, L. R. Cominsky, N. E. White, Bing Zhang, K. O. Mason, J. A. Nousek, V. La Parola, J. P. Osborne, K. Hurley, G. Chincarini, Peter Mészáros, S. D. Barthelemy, N. Gehrels, V. Mangano, P. T. Boyd, G. Cusumano, F. E. Marshall, Cusumano, G, Mangano, V, Chincarini, G, Panaitescu, A, Burrows, D, La Parola, V, Sakamoto, T, Campana, S, Mineo, T, Tagliaferri, G, Angelini, L, Barthelmy, S, Beardmore, A, Boyd, P, Cominsky, L, Gronwall, C, Fenimore, E, Gehrels, N, Giommi, P, Goad, M, Hurley, K, Immler, S, Kennea, J, Mason, K, Marshal, F, Meszaros, P, Nousek, J, Osborne, J, Palmer, D, Roming, P, Wells, A, White, N, and Zhang, B
Subjects: Physics, COSMIC cancer database, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, X-rays, bursts, gamma rays, observations, cosmology, early Universe, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Light curve, Redshift, Afterglow, law.invention, Telescope, FIS/05 - ASTRONOMIA E ASTROFISICA, Orders of magnitude (time), Space and Planetary Science, law, gamma rays, burst, Spectral energy distribution, Gamma-ray burst
Abstract: Swift discovered the high redshift (z=6.29) GRB050904 with the Burst Alert Telescope (BAT) and began observing with its narrow field instruments 161 s after the burst onset. This gamma-ray burst is the most distant cosmic explosion ever observed. Because of its high redshift, the X-ray Telescope (XRT) and BAT simultaneous observations provide 4 orders of magnitude of spectral coverage (0.2-150 keV; 1.4-1090 keV in the source rest frame) at a very early source-frame time (22 s). GRB050904 was a long, multi-peaked, bright GRB with strong variability during its entire evolution. The light curve observed by the XRT is characterized by the presence of a long flaring activity lasting up to 1-2 hours after the burst onset in the burst rest frame, with no evidence of a smooth power-law decay following the prompt emission as seen in other GRBs. However, the BAT tail extrapolated to the XRT band joins the XRT early light curve and the overall behavior resembles that of a very long GRB prompt. The spectral energy distribution softens with time, with the photon index decreasing from -1.2 during the BAT observation to -1.9 at the end of the XRT observation. The dips of the late X-ray flares may be consistent with an underlying X-ray emission arising from the forward shock and with the properties of the optical afterglow reported by Tagliaferri et al. (2005b). We interpret the BAT and XRT data as a single continuous observation of the prompt emission from a very long GRB. The peculiarities observed in GRB050904 could be due to its origin within one of the first star-forming regions in the Universe; very low metallicities of the progenitor at these epochs may provide an explanation., Comment: 9 pages, 2 table, 6 figures, accepted for publication on A&A
Published: 2006
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29 results on '"Nousek, J"'

1. Swift/UVOT discovery of Swift J221951-484240: a UV luminous ambiguous nuclear transient

2. Supplement: Localization and broadband follow-up of the gravitational-wave transient GW150914

3. Space Telescope and Optical Reverberation Mapping Project. IV. Anomalous Behavior of the Broad Ultraviolet Emission Lines in NGC 5548

4. Space Telescope and Optical Reverberation Mapping Project. VII. Understanding the Ultraviolet Anomaly in NGC 5548 with X-Ray Spectroscopy

5. UVES/VLT high resolution spectroscopy of GRB 050730 afterglow: probing the features of the GRB environment

6. A Statistical Comparison of the Optical/UV and X-ray Afterglows of Gamma-Ray Bursts using the Swift Ultra-violet Optical and X-ray Telescopes

7. Swift detects a remarkable gamma-ray burst, GRB 060614, that introduces a new classification scheme

8. The gamma-ray burst GRB060614 requires a novel explosive process

9. Swift observations of GRB050712

10. Relativistic ejecta from XRF 060218 and the rate of cosmic explosions

11. Evidence for chromatic X-ray light-curve breaks in Swift GRB afterglows and their theoretical implications

12. The shock break-out of GRB 060218/SN 2006aj

13. Swift-UVOT Observations of the X-Ray Flash 050406

14. The X-ray Telescope on board Swift: status and main results

15. Evidence for a Canonical GRB Afterglow Light Curve in the Swift/XRT Data

16. Gamma-Ray Observations of a Giant Flare from The Magnetar SGR 1806-20

17. Swift XRT Observations of X-ray Flares in GRB Afterglows

18. The Swift Gamma-Ray Burst Mission

19. The Chandra Deep Field North Survey. V. 1 Ms Source Catalogs

20. X-ray imaging of the Seyfert 2 galaxy Circinus with Chandra

21. High-resolution X-ray spectroscopy of the Seyfert 2 galaxy Circinus with Chandra

22. Chandra uncovers a hidden Low-Luminosity AGN in the radio galaxy Hydra~A (3C~218)

23. Observations of Faint, Hard-Band X-ray Sources in the Field of CRSS J0030.5+2618 with the Chandra X-ray Observatory and the Hobby-Eberly Telescope

24. Mitigating Charge Transfer Inefficiency in the Chandra X-ray Observatory's ACIS Instrument

25. Prompt and afterglow early X-ray phases in the comoving frame. Evidence for Universal properties?

26. Space Telescope and Optical Reverberation Mapping Project. VIII. Time Variability of Emission and Absorption in NGC 5548 Based on Modeling the Ultraviolet Spectrum

27. LOCALIZATION AND BROADBAND FOLLOW-UP OF THE GRAVITATIONAL-WAVE TRANSIENT GW 150914

28. The exceptionally extended flaring activity in the X-ray afterglow of GRB 050730 observed with Swift and XMM-Newton

29. Swift observations of GRB050904: the most distant cosmic explosion ever observed

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