Author: "Morokuma, T." / Language: english - Searchworks@Jio Institute Digital Library Search Results

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42 results on '"Morokuma, T."'

1. The host galaxy of a fast radio burst

Author: Keane, E.F., Johnston, S., Bhandari, S., Barr, E., Bhat, N.D.R., Burgay, M., Caleb, M., Flynn, C., Jameson, A., Kramer, M., Petroff, E., Possenti, A., van Straten, W., Bailes, M., Burke-Spolaor, S., Eatough, R.P., Stappers, B.W., Totani, T., Honma, M., Furusawa, H., Hattori, T., Morokuma, T., Niino, Y., Sugai, H., Terai, T., Tominaga, N., Yamasaki, S., Yasuda, N., Allen, R., Cooke, J., Jencson, J., Kasliwal, M.M., Kaplan, D.L., Tingay, S.J., Williams, A., Wayth, R., Chandra, P., Perrodin, D., Berezina, M., Mickaliger, M., and Bassa, C.
Subjects: Telescope -- Usage -- Research, Pulsars -- Observations -- Research, Environmental issues, Science and technology, Zoology and wildlife conservation
Abstract: In recent years, millisecond-duration radio signals originating in distant galaxies appear to have been discovered in the so-called fast radio bursts (1-9). These signals are dispersed according to a precise physical law and this dispersion is a key observable quantity, which, in tandem with a redshift measurement, can be used for fundamental physical investigations (10,11). Every fast radio burst has a dispersion measurement, but none before now have had a redshift measurement, because of the difficulty in pinpointing their celestial coordinates. Here we report the discovery of a fast radio burst and the identification of a fading radio transient lasting ~6 days after the event, which we use to identify the host galaxy; we measure the galaxy's redshift to be z = 0.492 ± 0.008. The dispersion measure and redshift, in combination, provide a direct measurement of the cosmic density of ionized baryons in the intergalactic medium of [Ω.sub.IGM] = 4.9 ± 1.3 per cent, in agreement with the expectation from the Wilkinson Microwave Anisotropy Probe (12), and including all of the so-called 'missing baryons'. The ~6-day radio transient is largely consistent with the radio afterglow of a short γ-ray burst (13), and its existence and timescale do not support progenitor models such as giant pulses from pulsars, and supernovae. This contrasts with the interpretation (8) of another recently discovered fast radio burst, suggesting that there are at least two classes of bursts., As part of the SUrvey for Pulsars and Extragalactic Radio Bursts (SUPERB) project at the Parkes radio telescope, we perform real-time searches of the sky at high time resolution (see [...]
Published: 2016

2. Large Polarization Degree of Comet 2P/Encke Continuum Based on Spectropolarimetric Signals During Its 2017 Apparition

Author: Kwon, Y. G., Ishiguro, M., Shinnaka, Y., Nakaoka, T., Kuroda, D., Hanayama, H., Takahashi, J., Baar, S., Saito, T., Kawabata, M., Uemura, M., Morokuma, T., Murata, K. L., Takagi, Seiko, Morihana, Kumiko, Nagayama, Takahiro, Sekiguchi, K., Kawabata, K. S., and Akitaya, H.
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), FOS: Physical sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract: Spectropolarimetry is a powerful technique for investigating the physical properties of gas and solid materials in cometary comae without mutual contamination, but there have been few spectropolarimetric studies to extract each component. We attempt to derive the continuum polarization degree of comet 2P/Encke, free from influence of molecular emissions. The target is unique in that it has an orbit dynamically decoupled from Jupiter like main-belt asteroids, while ejecting gas and dust like ordinary comets. We observed the comet using the Higashi-Hiroshima Optical and Near-Infrared Camera attached to the Cassegrain focus of the 150-cm Kanata telescope on UT 2017 February 21 when the comet was at the solar phase angle of 75.7 deg. We find that the continuum polarization degree with respect to the scattering plane is 33.8+/-2.7 % at the effective wavelength of 0.815 um, which is significantly higher than those of cometary dust in a high-Pmax group at similar phase angles. Assuming that an ensemble polarimetric response of 2P/Encke's dust as a function of phase angle is morphologically similar with those of other comets, its maximum polarization degree is estimated to > 40 % at the phase angle of ~100 deg. In addition, we obtain the polarization degrees of the C2 swan bands (0.51-0.56 um), the NH2 alpha bands (0.62-0.69 um) and the CN-red system (0.78-0.94 um) in a range of 3-19 %, which depend on the molecular species and rotational quantum numbers of each branch. The polarization vector aligns nearly perpendicularly to the scattering plane with the average of 0.4 deg over a wavelength range of 0.50-0.97 um. From the observational evidence, we conjecture that the large polarization degree of 2P/Encke would be attributable to a dominance of large dust particles around the nucleus, which have remained after frequent perihelion passages near the Sun., 9 pages, 4 figures, accepted for publication in Astronomy & Astrophysics
Published: 2018

3. Variability of Late-time Radio Emission in the Superluminous Supernova PTF10hgi.

Author: Hatsukade, B., Tominaga, N., Morokuma, T., Morokuma-Matsui, K., Tamura, Y., Niinuma, K., Hayashi, M., Matsuda, Y., and Motogi, K.
Published: 2021
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4. Multimessenger observations of a flaring blazar coincident with high-energy neutrino IceCube-170922A

Author: Aartsen, M. G., Ackermann, M., Adams, J., Aguilar, J. A., Ahlers, M., Ahrens, M., Al Samarai, I., Altmann, D., Andeen, K., Anderson, T., Ansseau, I., Anton, G., Argüelles, C., Auffenberg, J., Axani, S., Bagherpour, H., Bai, X., Barron, J. P., Barwick, S. W. Baum V., Bay, R., Beatty, J. J., Becker Tjus, J., Becker, K. -H., Benzvi, S., Berley, D., Bernardini, E., Besson, D. Z., Binder, G., Bindig, D., Blaufuss, E., Blot, S., Bohm, C., Börner, M., Bos, F., Böser, S., Botner, O., Bourbeau, E., Bourbeau, J., Bradascio, F., Braun, J., Brenzke, M., Bretz, H. -P., Bron, S., Brostean-Kaiser, J., Burgman, A., Busse, R. S., Carver, T., Cheung, E., Chirkin, D., Christov, A., Clark, K., Classen, L., Coenders, S., Collin, G. H., Conrad, J. M., Coppin, P., Correa, P., Cowen, D. F., Cross, R., Dave, P., Day, M., de André, J. P. A. M., De Clercq, C., Delaunay, J. J., Dembinski, H., De Ridder, S., Desiati, P., de Vries, K. D., de Wasseige, G., de With, M., Deyoung, T., Díaz-Vélez, J. C., di Lorenzo, V., Dujmovic, H., Dumm, J. P., Dunkman, M., Dvorak, E., Eberhardt, B., Ehrhardt, T., Eichmann, B., Eller, P., Evenson, P. A., Fahey, S., Fazely, A. R., Felde, J., Filimonov, K., Finley, C., Flis, S., Franckowiak, A., Friedman, E., Fritz, A., Gaisser, T. K., Gallagher, J., Gerhardt, L., Ghorbani, K., Glauch, T., Glüsenkamp, T., Goldschmidt, A., Gonzalez, J. G., Grant, D., Griffith, Z., Haack, C., Hallgren, A., Halzen, F., Hanson, K., Hebecker, D., Heereman, D., Helbing, K., Hellauer, R., Hickford, S., Hignight, J., Hill, G. C., Hoffman, K. D., Hoffmann, R., Hoinka, T., Hokanson-Fasig, B., Hoshina, K., Huang, F., Huber, M., Hultqvist, K., Hünnefeld, M., Hussain, R., In, S., Iovine, N., Ishihara, A., Jacobi, E., Japaridze, G. S., Jeong, M., Jero, K., Jones, B. J. P., Kalaczynski, P., Kang, W., Kappes, A., Kappesser, D., Karg, T., Karle, A., Katz, U., Kauer, M., Keivani, A., Kelley, J. L., Kheirandish, A., Kim, J., Kim, M., Kintscher, T., Kiryluk, J., Kittler, T., Klein, S. R., Koirala, R., Kolanoski, H., Köpke, L., Kopper, C., Kopper, S., Koschinsky, J. P., Koskinen, D. J., Kowalski, M., Krings, K., Kroll, M., Krückl, G., Kunwar, S., Kurahashi, N., Kuwabara, T., Kyriacou, A., Labare, M., Lanfranchi, J. L., Larson, M. J., Lauber, F., Leonard, K., Lesiak-Bzdak, M., Leuermann, M., Liu, Q. R., Lozano Mariscal, C. J., Lu, L., Lünemann, J., Luszczak, W., Madsen, J., Maggi, G., Mahn, K. B. M., Mancina, S., Maruyama, R., Mase, K., Maunu, R., Meagher, K., Medici, M., Meier, M., Menne, T., Merino, G., Meures, T., Miarecki, S., Micallef, J., Momenté, G., Montaruli, T., Moore, R. W., S, Morse, R., Moulai, M., Nahnhauer, R., Nakarmi, P., Naumann, U., Neer, G., Niederhausen, H., Nowicki, S. C., Nygren, D. R., Obertacke Pollmann, A., Olivas, A., O'Murchadha, A., O'Sullivan, E., Palczewski, T., Pandya, H., Pankova, D. V., Peiffer, P., Pepper, J. A., Pérez de los Heros, C., Pieloth, D., Pinat, E., Plum, M., Price, P. B., Przybylski, G. T., Raab, C., Rädel, L., Rameez, M., Rauch, L., Rawlins, K., Rea, I. C., Reimann, R., Relethford, B., Relich, M., Resconi, E., Rhode, W., Richman, M., Robertson, S., Rongen, M., Rott, C., Ruhe, T., Ryckbosch, D., Rysewyk, D., Safa, I., Sälzer, T., Sanchez Herrera, S. E., Sandrock, A., Sandroos, J., Santander, M., Sarkar, S., Satalecka, K., Schlunder, P., Schmidt, T., Schneider, A., Schoenen, S., Schöneberg, S., Schumacher, L., Sclafani, S., Seckel, D., Seunarine, S., Soedingrekso, J., Soldin, D., Song, M., Spiczak, G. M., Spiering, C., Stachurska, J., Stamatikos, M., Stanev, T., Stasik, A., Stein, R., Stettner, J., Steuer, A., Stezelberger, T., Stokstad, R. G., Stößl, A., Strotjohann, N. L., Stuttard, T., Sullivan, G. W., Sutherland, M., Taboada, I., Tatar, J., Tenholt, F., Ter-Antonyan, S., Terliuk, A., Tilav, S., Toale, P. A., Tobin, M. N., Toennis, C., Toscano, S., Tosi, D., Tselengidou, M., Tung, C. F., Turcati, A., Turley, C. F., Ty, B., Unger, E., Usner, M., Vandenbroucke, J., Van Driessche, W., van Eijk, D., van Eijndhoven, N., Vanheule, S., van Santen, J., Vogel, E., Vraeghe, M., Walck, C., Wallace, A., Wallraff, M., Wandler, F. D., Wandkowsky, N., Waza, A., Weaver, C., Weiss, M. J., Wendt, C., Werthebach, J., Westerhoff, S., Whelan, B. J., Whitehorn, N., Wiebe, K., Wiebusch, C. H., Wille, L., Williams, D. R., Wills, L., Wolf, M., Wood, J., Wood, T. R., Woschnagg, K., D. L., Xu, X. W., Xu, Xu, Y., Yanez, J. P., Yodh, G., Yoshida, S., Yuan, T., Fermi-LAT, Collaboration, Abdollahi, S., Ajello, M., Angioni, R., Baldini, L., Ballet, J., Barbiellini, G., Bastieri, D., Bechtol, K., Bellazzini, R., Berenji, B., Bissaldi, E., Blandford, R. D., Bonino, R., Bottacini, E., Bregeon, J., Bruel, P., Buehler, R., Burnett, T. H., Burns, E., Buson, S., Cameron, R. A., Caputo, R., Caraveo, P. A., Cavazzuti, E., Charles, E., Chen, S., Cheung, C. C., Chiang, J., Chiaro, G., Ciprini, S., Cohen-Tanugi, J., Conrad, J., Costantin, D., Cutini, S., D'Ammando, F., de Palma, F., Digel, S. W., Di Lalla, N., Di Mauro, M., Di Venere, L., Domínguez, A., Favuzzi, C., Fukazawa, Y., Funk, S., Fusco, P., Gargano, F., Gasparrini, D., Giglietto, N., Giomi, M., Giommi, P., Giordano, F., Giroletti, M., Glanzman, T., Green, D., Grenier, I. A., Grondin, M. -H., Guiriec, S., Harding, A. K., Hayashida, M., Hays, E., Hewitt, J. W., Horan, D., Jóhannesson, G., Kadler, M., Kensei, S., Kocevski, D., Krauss, F., Kreter, M., Kuss, M., La Mura, G., Larsson, S., Latronico, L., Lemoine-Goumard, M., Li, J., Longo, F., Loparco, F., Lovellette, M. N., Lubrano, P., Magill, J. D., Maldera, S., Malyshev, D., Manfreda, A., Mazziotta, M. N., Mcenery, J. E., Meyer, M., Michelson, P. F., Mizuno, T., Monzani, M. E., Morselli, A., Moskalenko, I. V., Negro, M., Nuss, E., Ojha, R., Omodei, N., Orienti, M., Orlando, E., Palatiello, M., Paliya, V. S., Perkins, J. S., Persic, M., Pesce-Rollins, M., Piron, F., Porter, T. A., Principe, G., Rainò, S., Rando, R., Rani, B., Razzano, M., Razzaque, S., Reimer, A., Reimer, O., Renault-Tinacci, N., Ritz, S., Rochester, L. S., Saz Parkinson, P. M., Sgrò, C., Siskind, E. J., Spandre, G., Spinelli, P., Suson, D. J., Tajima, H., Takahashi, M., Tanaka, Y., Thayer, J. B., Thompson, D. J., Tibaldo, L., Torres, D. F., Torresi, E., Tosti, G., Troja, E., Valverde, J., Vianello, G., Vogel, M., Wood, K., Wood, M., Zaharijas, G., Magic, Collaboration, Ahnen, M. L., Ansoldi, S., Antonelli, L. A., Arcaro, C., Baack, D., Babić, A., Banerjee, B., Bangale, P., Barres de Almeida, U., Barrio, J. A., Becerra González, J., Bednarek, W., Berti, A., Bhattacharyya, W., Biland, A., Blanch, O., Bonnoli, G., Carosi, A., Carosi, R., Ceribella, G., Chatterjee, A., Colak, S. M., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., Cumani, P., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., Delfino, M., Delgado, J., Di Pierro, F., Dominis Prester, D., Dorner, D., Doro, M., Einecke, S., Elsaesser, D., Fallah Ramazani, V., Fernández-Barral, A., Fidalgo, D., Foffano, L., Pfrang, K., Fonseca, M. V., Font, L., Franceschini, A., Fruck, C., Galindo, D., Gallozzi, S., García López, R. J., Garczarczyk, M., Gaug, M., Giammaria, P., Godinović, N., Gora, D., Guberman, D., Hadasch, D., Hahn, A., Hassan, T., Herrera, J., Hose, J., Hrupec, D., Inoue, S., Ishio, K., Konno, Y., Kubo, H., Kushida, J., Lelas, D., Lindfors, E., Lombardi, S., López, M., Maggio, C., Majumdar, P., Makariev, M., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Mariotti, M., Martínez, M., Masuda, S., Mazin, D., Minev, M., J. M., M, Mirzoyan, R., Moralejo, A., Moreno, V., Moretti, E., Nagayoshi, T., Neustroev, V., Niedzwiecki, A., Nievas Rosillo, M., Nigro, C., Nilsson, K., Ninci, D., Nishijima, K., Noda, K., Nogués, L., Paiano, S., Palacio, J., Paneque, D., Paoletti, R., Paredes, J. M., Pedaletti, G., Peresano, M., Prada Moroni, P. G., Prandini, E., Puljak, I., Rodriguez Garcia, J., Reichardt, I., Ribó, M., Rico, J., Righi, C., Rugliancich, A., Saito, T., Schweizer, T., Sitarek, J., Šnidaric ́, I., Sobczynska, D., Stamerra, A., Strzys, M., Surić, T., Tavecchio, F., Temnikov, P., Terzić, T., Teshima, M., Torres-Albà, N., Treves, A., Tsujimoto, S., Vanzo, G., Vazquez Acosta, M., Vovk, I., Ward, J. E., Will, M., Zaric ́, D., Agile, Team, Lucarelli, F., Tavani, M., Piano, G., Donnarumma, I., Pittori, C., Verrecchia, F., Bulgarelli, A., Caraveo, P., Cattaneo, P. W., Colafrancesco, S., Costa, E., Di Cocco, G., Ferrari, A., Gianotti, F., Giuliani, A., Lipari, P., Mereghetti, S., Pacciani, L., Paoletti, F., Parmiggiani, N., Pellizzoni, A., Picozza, P., Pilia, M., Rappoldi, A., Trois, A., Vercellone, S., Vittorini, V., ASAS-SN, Team, Stanek, A. Franckowiak K. Z., Kochanek, C. S., Beacom, J. F., Thompson, T. A., Holoien, T. W. -S., Dong, S., Prieto, J. L., Shappee, B. J., Holmbo, S., Hawc, Collaboration, Abeysekara, A. U., Albert, A., Alfaro, R., Alvarez, C., Arceo, R., Arteaga-Velázquez, J. C., Avila Rojas, D., Ayala Solares, H. A., Becerril, A., Belmont-Moreno, E., Bernal, A., Caballero-Mora, K. S., Capistrán, T., Carramiñana, A., Casanova, S., Castillo, M., Cotti, U., Cotzomi, J., Coutiño de León, S., De León, C., De la Fuente, E., Diaz Hernandez, R., Dichiara, S., Dingus, B. L., Duvernois, M. A., Ellsworth, R. W., Engel, K., Fiorino, D. W., Fleischhack, H., Fraija, N., García-González, J. A., Garfias, F., González Muñoz, A., González, M. M., Goodman, J. A., Hampel-Arias, Z., Harding, J. P., Hernandez, S., Hona, B., Hueyotl-Zahuantitla, F., Hui, C. M., Hüntemeyer, P., Iriarte, A., Jardin-Blicq, A., Joshi, V., Kaufmann, S., Kunde, G. J., Lara, A., Lauer, R. J., Lee, W. H., Lennarz, D., León Vargas, H., Linnemann, J. T., Longinotti, A. L., Luis-Raya, G., Luna-García, R., Malone, K., Marinelli, S. S., Martinez, O., Martinez-Castellanos, I., Martínez-Castro, J., Martínez-Huerta, H., Matthews, J. A., Miranda-Romagnoli, P., Moreno, E., Mostafá, M., Nayerhoda, A., Nellen, L., Newbold, M., Nisa, M. U., Noriega-Papaqui, R., Pelayo, R., Pretz, J., Pérez-Pérez, E. G., Ren, Z., Rho, C. D., Rivière, C., Rosa-González, D., Rosenberg, M., Ruiz-Velasco, E., Salesa Greus, F., Sandoval, A., Schneider, M., Schoorlemmer, H., Sinnis, G., Smith, A. J., Springer, R. W., Surajbali, P., Tibolla, O., Tollefson, K., Torres, I., Villaseñor, L., Weisgarber, T., Werner, F., Yapici, T., Gaurang, Y., Zepeda, A., Zhou, H., Álvarez, J. D., Collaboration, H. E. S. S., Abdalla, H., Angüner, E. O., Armand, C., Backes, M., Becherini, Y., Berge, D., Böttcher, M., Boisson, C., Bolmont, J., Bonnefoy, S., Bordas, P., Brun, F., Büchele, M., Bulik, T., Caroff, S., Cerruti, M., Chakraborty, N., Chandra, S., Chen, A., Davids, I. D., Deil, C., Devin, J., Djannati-Ataï, A., Egberts, K., Emery, G., Eschbach, S., Fiasson, A., Fontaine, G., Füßling, M., Gallant, Y. A., Gaté, F., Giavitto, G., Glawion, D., Glicenstein, J. F., Gottschall, D., Haupt, M., Henri, G., Hinton, J. A., Hoischen, C., Holch, T. L., Huber, D., Jamrozy, M., Jankowsky, D., Jankowsky, F., Jouvin, L., Jung-Richardt, I., Kerszberg, D., Khélifi, B., King, J., Klepser, S., Kluz ́niak, W., Komin, Nu., Kraus, M., Lefaucheur, J., Lemière, A., Lenain, J. -P., Leser, E., Lohse, T., López-Coto, R., Lorentz, M., Lypova, I., Marandon, V., Guillem Martí-Devesa, G., Maurin, G., Mitchell, A. M. W., Moderski, R., Mohamed, M., Mohrmann, L., Moulin, E., Murach, T., de Naurois, M., Niederwanger, F., Niemiec, J., Oakes, L., O'Brien, P., Ohm, S., Ostrowski, M., Oya, I., Panter, M., Parsons, R. D., Perennes, C., Piel, Q., Pita, S., Poireau, V., Priyana Noel, A., Prokoph, H., Pühlhofer, G., Quirrenbach, A., Raab, S., Rauth, R., Renaud, M., Rieger, F., Rinchiuso, L., Romoli, C., Rowell, G., Rudak, B., Sasaki, D. A., Sanchez, M., Schlickeiser, R., Schüssler, F., Schulz, A., Schwanke, U., Seglar-Arroyo, M., Shafi, N., Simoni, R., Sol, H., Stegmann, C., Steppa, C., Tavernier, T., Taylor, A. M., Tiziani, D., Trichard, C., Tsirou, M., van Eldik, C., van Rensburg, C., van Soelen, B., Veh, J., Vincent, P., Voisin, F., Wagner, S. J., Wagner, R. M., Wierzcholska, A., Zanin, R., Zdziarski, A. A., Zech, A., Ziegler, A., Zorn, J., Żywucka, N., Integral, Team, Savchenko, V., Ferrigno, C., Bazzano, A., Diehl, R., Kuulkers, E., Laurent, P., Natalucci, L., Panessa, F., Rodi, J., Ubertini, P., Kanata Kiso and Subaru Observing Teams, Morokuma, T., Ohta, K., Tanaka, Y. T., Mori, H., Yamanaka, M., Kawabata, K. S., Utsumi, Y., Nakaoka, T., Kawabata, M., Nagashima, H., Yoshida, M., Matsuoka, Y., Itoh, R., Kapteyn, Team, Keel, W., Liverpool Telescope Team, Copperwheat, C., Steele, I., Swift/nustar, Team, Cenko, S. B., Evans, P. A., Fox, D. B., Kennea, J. A., Marshall, F. E., Osborne, J. P., Tohuvavohu, A., Veritas, Collaboration, Archer, A., Benbow, W., Bird, R., Brill, A., Brose, R., Buchovecky, M., Buckley, J. H., Bugaev, V., Christiansen, J. L., Connolly, M. P., Cui, W., Daniel, M. K., Errando, M., Falcone, A., Feng, Q., Finley, J. P., Fortson, L., Furniss, A., Gueta, O., Hütten, M., Hervet, O., Hughes, G., Humensky, T. B., Johnson, C. A., Kaaret, P., Kar, P., Kelley-Hoskins, N., Kertzman, M., Kieda, D., Krause, M., Krennrich, F., Kumar, S., Lang, M. J., Lin, T. T. Y., Maier, G., Mcarthur, S., Moriarty, P., Mukherjee, R., Nieto, D., O'Brien, S., Ong, R. A., Otte, A. N., Park, N., Petrashyk, A., Pohl, M., Popkow, A., Pueschel, S. E., Quinn, J., Ragan, K., Reynolds, P. T., Richards, G. T., Roache, E., Rulten, C., Sadeh, I., Scott, S. S., Sembroski, G. H., Shahinyan, K., Sushch, I., Trépanier, S., Tyler, J., Vassiliev, V. V., Wakely, S. P., Weinstein, A., Wells, R. M., Wilcox, P., Wilhelm, A., Williams, D. A., Zitzer, B., Vla/b, Team, Tetarenko, A. J., Kimball, A. E., Miller-Jones, J. C. A., Sivakoff, G. R., Massachusetts Institute of Technology. Laboratory for Nuclear Science, Massachusetts Institute of Technology. Department of Nuclear Science and Engineering, Massachusetts Institute of Technology. Department of Physics, ITA, High Energy Astrophys. & Astropart. Phys (API, FNWI), Faculty of Science, API Other Research (FNWI), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Particules de Montpellier (LUPM), 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), 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), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Centre de Physique des Particules de Marseille (CPPM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), 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), Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-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), Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Département d'Astrophysique (ex SAP) (DAP), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, IceCube, Fermi-LAT, Kapteyn, Liverpool Telescope, Subaru, Swift NuSTAR, VERITAS, VLA/17B-403, MAGIC, AGILE, ASAS-SN, HAWC, H.E.S.S., INTEGRAL, Kanata, Kiso, Aartsen, M. G., Ackermann, M., Adams, J., Aguilar, J. A., Ahlers, M., Ahrens, M., Al Samarai, I., Altmann, D., Andeen, K., Anderson, T., Ansseau, I., Anton, G., Argüelles, C., Auffenberg, J., Axani, S., Bagherpour, H., Bai, X., Barron, J. P., Barwick, S. W., Baum, V., Bay, R., Beatty, J. J., Becker Tjus, J., Becker, K. -H., Benzvi, S., Berley, D., Bernardini, E., Besson, D. Z., Binder, G., Bindig, D., Blaufuss, E., Blot, S., Bohm, C., Börner, M., Bos, F., Böser, S., Botner, O., Bourbeau, E., Bourbeau, J., Bradascio, F., Braun, J., Brenzke, M., Bretz, H. -P., Bron, S., Brostean-Kaiser, J., Burgman, A., Busse, R. S., Carver, T., Cheung, E., Chirkin, D., Christov, A., Clark, K., Classen, L., Coenders, S., Collin, G. H., Conrad, J. M., Coppin, P., Correa, P., Cowen, D. F., Cross, R., Dave, P., Day, M., de André, J. P. A. M., De Clercq, C., Delaunay, J. J., Dembinski, H., De Ridder, S., Desiati, P., de Vries, K. D., de Wasseige, G., de With, M., Deyoung, T., Díaz-Vélez, J. C., Di Lorenzo, V., Dujmovic, H., Dumm, J. P., Dunkman, M., Dvorak, E., Eberhardt, B., Ehrhardt, T., Eichmann, B., Eller, P., Evenson, P. A., Fahey, S., Fazely, A. R., Felde, J., Filimonov, K., Finley, C., Flis, S., Franckowiak, A., Friedman, E., Fritz, A., Gaisser, T. K., Gallagher, J., Gerhardt, L., Ghorbani, K., Glauch, T., Glüsenkamp, T., Goldschmidt, A., Gonzalez, J. G., Grant, D., Griffith, Z., Haack, C., Hallgren, A., Halzen, F., Hanson, K., Hebecker, D., Heereman, D., Helbing, K., Hellauer, R., Hickford, S., Hignight, J., Hill, G. C., Hoffman, K. D., Hoffmann, R., Hoinka, T., Hokanson-Fasig, B., Hoshina, K., Huang, F., Huber, M., Hultqvist, K., Hünnefeld, M., Hussain, R., In, S., Iovine, N., Ishihara, A., Jacobi, E., Japaridze, G. S., Jeong, M., Jero, K., Jones, B. J. P., Kalaczynski, P., Kang, W., Kappes, A., Kappesser, D., Karg, T., Karle, A., Katz, U., Kauer, M., Keivani, A., Kelley, J. L., Kheirandish, A., Kim, J., Kim, M., Kintscher, T., Kiryluk, J., Kittler, T., Klein, S. R., Koirala, R., Kolanoski, H., Köpke, L., Kopper, C., Kopper, S., Koschinsky, J. P., Koskinen, D. J., Kowalski, M., Krings, K., Kroll, M., Krückl, G., Kunwar, S., Kurahashi, N., Kuwabara, T., Kyriacou, A., Labare, M., Lanfranchi, J. L., Larson, M. J., Lauber, F., Leonard, K., Lesiak-Bzdak, M., Leuermann, M., Liu, Q. R., Lozano Mariscal, C. J., Lu, L., Lünemann, J., Luszczak, W., Madsen, J., Maggi, G., Mahn, K. B. M., Mancina, S., Maruyama, R., Mase, K., Maunu, R., Meagher, K., Medici, M., Meier, M., Menne, T., Merino, G., Meures, T., Miarecki, S., Micallef, J., Momenté, G., Montaruli, T., Moore, R. W., Morse, R., Moulai, M., Nahnhauer, R., Nakarmi, P., Naumann, U., Neer, G., Niederhausen, H., Nowicki, S. C., Nygren, D. R., Obertacke Pollmann, A., Olivas, A., O’Murchadha, A., O’Sullivan, E., Palczewski, T., Pandya, H., Pankova, D. V., Peiffer, P., Pepper, J. A., Pérez de los Heros, C., Pieloth, D., Pinat, E., Plum, M., Price, P. B., Przybylski, G. T., Raab, C., Rädel, L., Rameez, M., Rauch, L., Rawlins, K., Rea, I. C., Reimann, R., Relethford, B., Relich, M., Resconi, E., Rhode, W., Richman, M., Robertson, S., Rongen, M., Rott, C., Ruhe, T., Ryckbosch, D., Rysewyk, D., Safa, I., Sälzer, T., Sanchez Herrera, S. E., Sandrock, A., Sandroos, J., Santander, M., Sarkar, S., Satalecka, K., Schlunder, P., Schmidt, T., Schneider, A., Schoenen, S., Schöneberg, S., Schumacher, L., Sclafani, S., Seckel, D., Seunarine, S., Soedingrekso, J., Soldin, D., Song, M., Spiczak, G. M., Spiering, C., Stachurska, J., Stamatikos, M., Stanev, T., Stasik, A., Stein, R., Stettner, J., Steuer, A., Stezelberger, T., Stokstad, R. G., Stößl, A., Strotjohann, N. L., Stuttard, T., Sullivan, G. W., Sutherland, M., Taboada, I., Tatar, J., Tenholt, F., Ter-Antonyan, S., Terliuk, A., Tilav, S., Toale, P. A., Tobin, M. N., Toennis, C., Toscano, S., Tosi, D., Tselengidou, M., Tung, C. F., Turcati, A., Turley, C. F., Ty, B., Unger, E., Usner, M., Vandenbroucke, J., Van Driessche, W., van Eijk, D., van Eijndhoven, N., Vanheule, S., van Santen, J., Vogel, E., Vraeghe, M., Walck, C., Wallace, A., Wallraff, M., Wandler, F. D., Wandkowsky, N., Waza, A., Weaver, C., Weiss, M. J., Wendt, C., Werthebach, J., Westerhoff, S., Whelan, B. J., Whitehorn, N., Wiebe, K., Wiebusch, C. H., Wille, L., Williams, D. R., Wills, L., Wolf, M., Wood, J., Wood, T. R., Woschnagg, K., Xu, D. L., Xu, X. W., Xu, Y., Yanez, J. P., Yodh, G., Yoshida, S., Yuan, T., Abdollahi, S., Ajello, M., Angioni, R., Baldini, L., Ballet, J., Barbiellini, G., Bastieri, D., Bechtol, K., Bellazzini, R., Berenji, B., Bissaldi, E., Blandford, R. D., Bonino, R., Bottacini, E., Bregeon, J., Bruel, P., Buehler, R., Burnett, T. H., Burns, E., Buson, S., Cameron, R. A., Caputo, R., Caraveo, P. A., Cavazzuti, E., Charles, E., Chen, S., Cheung, C. C., Chiang, J., Chiaro, G., Ciprini, S., Cohen-Tanugi, J., Conrad, J., Costantin, D., Cutini, S., D’Ammando, F., de Palma, F., Digel, S. W., Di Lalla, N., Di Mauro, M., Di Venere, L., Domínguez, A., Favuzzi, C., Fukazawa, Y., Funk, S., Fusco, P., Gargano, F., Gasparrini, D., Giglietto, N., Giomi, M., Giommi, P., Giordano, F., Giroletti, M., Glanzman, T., Green, D., Grenier, I. A., Grondin, M. -H., Guiriec, S., Harding, A. K., Hayashida, M., Hays, E., Hewitt, J. W., Horan, D., Jóhannesson, G., Kadler, M., Kensei, S., Kocevski, D., Krauss, F., Kreter, M., Kuss, M., La Mura, G., Larsson, S., Latronico, L., Lemoine-Goumard, M., Li, J., Longo, F., Loparco, F., Lovellette, M. N., Lubrano, P., Magill, J. D., Maldera, S., Malyshev, D., Manfreda, A., Mazziotta, M. N., Mcenery, J. E., Meyer, M., Michelson, P. F., Mizuno, T., Monzani, M. E., Morselli, A., Moskalenko, I. V., Negro, M., Nuss, E., Ojha, R., Omodei, N., Orienti, M., Orlando, E., Palatiello, M., Paliya, V. S., Perkins, J. S., Persic, M., Pesce-Rollins, M., Piron, F., Porter, T. A., Principe, G., Rainò, S., Rando, R., Rani, B., Razzano, M., Razzaque, S., Reimer, A., Reimer, O., Renault-Tinacci, N., Ritz, S., Rochester, L. S., Saz Parkinson, P. M., Sgrò, C., Siskind, E. J., Spandre, G., Spinelli, P., Suson, D. J., Tajima, H., Takahashi, M., Tanaka, Y., Thayer, J. B., Thompson, D. J., Tibaldo, L., Torres, D. F., Torresi, E., Tosti, G., Troja, E., Valverde, J., Vianello, G., Vogel, M., Wood, K., Wood, M., Zaharijas, G., Ahnen, M. L., Ansoldi, S., Antonelli, L. A., Arcaro, C., Baack, D., Babić, A., Banerjee, B., Bangale, P., Barres de Almeida, U., Barrio, J. A., Becerra González, J., Bednarek, W., Berti, A., Bhattacharyya, W., Biland, A., Blanch, O., Bonnoli, G., Carosi, A., Carosi, R., Ceribella, G., Chatterjee, A., Colak, S. M., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., Cumani, P., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., Delfino, M., Delgado, J., Di Pierro, F., Dominis Prester, D., Dorner, D., Doro, M., Einecke, S., Elsaesser, D., Fallah Ramazani, V., Fernández-Barral, A., Fidalgo, D., Foffano, L., Pfrang, K., Fonseca, M. V., Font, L., Franceschini, A., Fruck, C., Galindo, D., Gallozzi, S., García López, R. J., Garczarczyk, M., Gaug, M., Giammaria, P., Godinović, N., Gora, D., Guberman, D., Hadasch, D., Hahn, A., Hassan, T., Herrera, J., Hose, J., Hrupec, D., Inoue, S., Ishio, K., Konno, Y., Kubo, H., Kushida, J., Lelas, D., Lindfors, E., Lombardi, S., López, M., Maggio, C., Majumdar, P., Makariev, M., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Mariotti, M., Martínez, M., Masuda, S., Mazin, D., Minev, M., M, J. M., Mirzoyan, R., Moralejo, A., Moreno, V., Moretti, E., Nagayoshi, T., Neustroev, V., Niedzwiecki, A., Nievas, Rosillo, M., Nigro, Nilsson, K., Ninci, D., Nishijima, K., Noda, K., Nogués, L., Paiano, S., Palacio, J., Paneque, D., Paoletti, R., Paredes, J. M., Pedaletti, G., Peresano, M., Prada Moroni, P. G., Prandini, E., Puljak, I., Rodriguez Garcia, J., Reichardt, I., Ribó, M., Rico, J., Righi, C., Rugliancich, A., Saito, T., Schweizer, T., Sitarek, J., Šnidarić, I., Sobczynska, D., Stamerra, A., Strzys, M., Surić, T., Tavecchio, F., Temnikov, P., Terzić, T., Teshima, M., Torres-Albà, N., Treves, A., Tsujimoto, S., Vanzo, G., Vazquez Acosta, M., Vovk, I., Ward, J. E., Will, M., Zarić, D., Lucarelli, F., Tavani, M., Piano, G., Donnarumma, I., Pittori, C., Verrecchia, F., Bulgarelli, A., Caraveo, P., Cattaneo, P. W., Colafrancesco, S., Costa, E., Di Cocco, G., Ferrari, A., Gianotti, F., Giuliani, A., Lipari, P., Mereghetti, S., Pacciani, L., Paoletti, F., Parmiggiani, N., Pellizzoni, A., Picozza, P., Pilia, M., Rappoldi, A., Trois, A., Vercellone, S., Vittorini, V., Stanek, K. Z., Kochanek, C. S., Beacom, J. F., Thompson, T. A., Holoien, T. W. -S., Dong, S., Prieto, J. L., Shappee, B. J., Holmbo, S., Abeysekara, A. U., Albert, A., Alfaro, R., Alvarez, C., Arceo, R., Arteaga-Velázquez, J. C., Avila Rojas, D., Ayala Solares, H. A., Becerril, A., Belmont-Moreno, E., Bernal, A., Caballero-Mora, K. S., Capistrán, T., Carramiñana, A., Casanova, S., Castillo, M., Cotti, U., Cotzomi, J., Coutiño de León, S., De León, C., De la Fuente, E., Diaz Hernandez, R., Dichiara, S., Dingus, B. L., Duvernois, M. A., Ellsworth, R. W., Engel, K., Fiorino, D. W., Fleischhack, H., Fraija, N., García-González, J. A., Garfias, F., González Muñoz, A., González, M. M., Goodman, J. A., Hampel-Arias, Z., Harding, J. P., Hernandez, S., Hona, B., Hueyotl-Zahuantitla, F., Hui, C. M., Hüntemeyer, P., Iriarte, A., Jardin-Blicq, A., Joshi, V., Kaufmann, S., Kunde, G. J., Lara, A., Lauer, R. J., Lee, W. H., Lennarz, D., León Vargas, H., Linnemann, J. T., Longinotti, A. L., Luis-Raya, G., Luna-García, R., Malone, K., Marinelli, S. S., Martinez, O., Martinez-Castellanos, I., Martínez-Castro, J., Martínez-Huerta, H., Matthews, J. A., Miranda-Romagnoli, P., Moreno, E., Mostafá, M., Nayerhoda, A., Nellen, L., Newbold, M., Nisa, M. U., Noriega-Papaqui, R., Pelayo, R., Pretz, J., Pérez-Pérez, E. G., Ren, Z., Rho, C. D., Rivière, C., Rosa-González, D., Rosenberg, M., Ruiz-Velasco, E., Salesa Greus, F., Sandoval, A., Schneider, M., Schoorlemmer, H., Sinnis, G., Smith, A. J., Springer, R. W., Surajbali, P., Tibolla, O., Tollefson, K., Torres, I., Villaseñor, L., Weisgarber, T., Werner, F., Yapici, T., Gaurang, Y., Zepeda, A., Zhou, H., Álvarez, J. D., Abdalla, H., Angüner, E. O., Armand, C., Backes, M., Becherini, Y., Berge, D., Böttcher, M., Boisson, C., Bolmont, J., Bonnefoy, S., Bordas, P., Brun, F., Büchele, M., Bulik, T., Caroff, S., Cerruti, M., Chakraborty, N., Chandra, S., Chen, A., Davids, I. D., Deil, C., Devin, J., Djannati-Ataï, A., Egberts, K., Emery, G., Eschbach, S., Fiasson, A., Fontaine, G., Füßling, M., Gallant, Y. A., Gaté, F., Giavitto, G., Glawion, D., Glicenstein, J. F., Gottschall, D., Haupt, M., Henri, G., Hinton, J. A., Hoischen, C., Holch, T. L., Huber, D., Jamrozy, M., Jankowsky, D., Jankowsky, F., Jouvin, L., Jung-Richardt, I., Kerszberg, D., Khélifi, B., King, J., Klepser, S., Kluźniak, W., Komin, Nu., Kraus, M., Lefaucheur, J., Lemière, A., Lenain, J. -P., Leser, E., Lohse, T., López-Coto, R., Lorentz, M., Lypova, I., Marandon, V., Guillem Martí-Devesa, G., Maurin, G., Mitchell, A. M. W., Moderski, R., Mohamed, M., Mohrmann, L., Moulin, E., Murach, T., de Naurois, M., Niederwanger, F., Niemiec, J., Oakes, L., O’Brien, P., Ohm, S., Ostrowski, M., Oya, I., Panter, M., Parsons, R. D., Perennes, C., Piel, Q., Pita, S., Poireau, V., Priyana Noel, A., Prokoph, H., Pühlhofer, G., Quirrenbach, A., Raab, S., Rauth, R., Renaud, M., Rieger, F., Rinchiuso, L., Romoli, C., Rowell, G., Rudak, B., Sanchez, D. A., Sasaki, M., Schlickeiser, R., Schüssler, F., Schulz, A., Schwanke, U., Seglar-Arroyo, M., Shafi, N., Simoni, R., Sol, H., Stegmann, C., Steppa, C., Tavernier, T., Taylor, A. M., Tiziani, D., Trichard, C., Tsirou, M., van Eldik, C., van Rensburg, C., van Soelen, B., Veh, J., Vincent, P., Voisin, F., Wagner, S. J., Wagner, R. M., Wierzcholska, A., Zanin, R., Zdziarski, A. A., Zech, A., Ziegler, A., Zorn, J., Żywucka, N., Savchenko, V., Ferrigno, C., Bazzano, A., Diehl, R., Kuulkers, E., Laurent, P., Natalucci, L., Panessa, F., Rodi, J., Ubertini, P., Morokuma, T., Ohta, K., Tanaka, Y. T., Mori, H., Yamanaka, M., Kawabata, K. S., Utsumi, Y., Nakaoka, T., Kawabata, M., Nagashima, H., Yoshida, M., Matsuoka, Y., Itoh, R., Keel, W., Copperwheat, C., Steele, I., Cenko, S. B., Evans, P. A., Fox, D. B., Kennea, J. A., Marshall, F. E., Osborne, J. P., Tohuvavohu, A., Archer, A., Benbow, W., Bird, R., Brill, A., Brose, R., Buchovecky, M., Buckley, J. H., Bugaev, V., Christiansen, J. L., Connolly, M. P., Cui, W., Daniel, M. K., Errando, M., Falcone, A., Feng, Q., Finley, J. P., Fortson, L., Furniss, A., Gueta, O., Hütten, M., Hervet, O., Hughes, G., Humensky, T. B., Johnson, C. A., Kaaret, P., Kar, P., Kelley-Hoskins, N., Kertzman, M., Kieda, D., Krause, M., Krennrich, F., Kumar, S., Lang, M. J., Lin, T. T. Y., Maier, G., Mcarthur, S., Moriarty, P., Mukherjee, R., Nieto, D., O’Brien, S., Ong, R. A., Otte, A. N., Park, N., Petrashyk, A., Pohl, M., Popkow, A., Pueschel, E., Quinn, J., Ragan, K., Reynolds, P. T., Richards, G. T., Roache, E., Rulten, C., Sadeh, I., Scott, S. S., Sembroski, G. H., Shahinyan, K., Sushch, I., Trépanier, S., Tyler, J., Vassiliev, V. V., Wakely, S. P., Weinstein, A., Wells, R. M., Wilcox, P., Wilhelm, A., Williams, D. A., Zitzer, B., Tetarenko, A. J., Kimball, A. E., Miller-Jones, J. C. A., Sivakoff, G. R., Physics, Elementary Particle Physics, Vriendenkring VUB, Faculty of Sciences and Bioengineering Sciences, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), 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), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Aix Marseille Université (AMU)-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), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), 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)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Współautorami artykułu są członkowie różnych grup badawczych w liczbie 875, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), 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), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), 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, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)
Subjects: High energy, Kanata, Swift/NuSTAR, Astrophysics, Blazar, blazar: emission, 01 natural sciences, 7. Clean energy, Coincidence, Multidisciplinary, Blazar, Neutrino, High Energy Physics - Experiment, neutrino, High Energy Physics - Experiment (hep-ex), ASAS-SN, 010303 astronomy & astrophysics, HESS - Abteilung Hofmann, Computer Science::Databases, Physics, HAWC - Abteilung Hinton, High Energy Astrophysical Phenomena (astro-ph.HE), COSMIC cancer database, Multidisciplinary, Supernova, gamma ray: emission, VERITAS, Neutrino, Kapteyn, Astrophysics - High Energy Astrophysical Phenomena, General Science & Technology, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, IceCube Collaboration, jet: relativistic, AGILE, Coincident, Subaru, 0103 physical sciences, Kiso, supernova, neutrino event IceCube-170922A, gamma-ray blazar TXS 0506+056, quasar, Astrophysics::Galaxy Astrophysics, ta115, 010308 nuclear & particles physics, INTEGRAL, background, Liverpool Telescope, VLA/17B-403 teams, MAGIC, messenger, flux, gamma ray: VHE, 13. Climate action, general, Diffuse flux, High Energy Physics::Experiment, Fermi-LAT, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], HAWC, H.E.S.S
Abstract: INTRODUCTION Neutrinos are tracers of cosmic-ray acceleration: electrically neutral and traveling at nearly the speed of light, they can escape the densest environments and may be traced back to their source of origin. High-energy neutrinos are expected to be produced in blazars: intense extragalactic radio, optical, x-ray, and, in some cases, γ-ray sources characterized by relativistic jets of plasma pointing close to our line of sight. Blazars are among the most powerful objects in the Universe and are widely speculated to be sources of high-energy cosmic rays. These cosmic rays generate high-energy neutrinos and γ-rays, which are produced when the cosmic rays accelerated in the jet interact with nearby gas or photons. On 22 September 2017, the cubic-kilometer IceCube Neutrino Observatory detected a ~290-TeV neutrino from a direction consistent with the flaring γ-ray blazar TXS 0506+056. We report the details of this observation and the results of a multiwavelength follow-up campaign. RATIONALE Multimessenger astronomy aims for globally coordinated observations of cosmic rays, neutrinos, gravitational waves, and electromagnetic radiation across a broad range of wavelengths. The combination is expected to yield crucial information on the mechanisms energizing the most powerful astrophysical sources. That the production of neutrinos is accompanied by electromagnetic radiation from the source favors the chances of a multiwavelength identification. In particular, a measured association of high-energy neutrinos with a flaring source of γ-rays would elucidate the mechanisms and conditions for acceleration of the highest-energy cosmic rays. The discovery of an extraterrestrial diffuse flux of high-energy neutrinos, announced by IceCube in 2013, has characteristic properties that hint at contributions from extragalactic sources, although the individual sources remain as yet unidentified. Continuously monitoring the entire sky for astrophysical neutrinos, IceCube provides real-time triggers for observatories around the world measuring γ-rays, x-rays, optical, radio, and gravitational waves, allowing for the potential identification of even rapidly fading sources. RESULTS A high-energy neutrino-induced muon track was detected on 22 September 2017, automatically generating an alert that was distributed worldwide within 1 min of detection and prompted follow-up searches by telescopes over a broad range of wavelengths. On 28 September 2017, the Fermi Large Area Telescope Collaboration reported that the direction of the neutrino was coincident with a cataloged γ-ray source, 0.1° from the neutrino direction. The source, a blazar known as TXS 0506+056 at a measured redshift of 0.34, was in a flaring state at the time with enhanced γ-ray activity in the GeV range. Follow-up observations by imaging atmospheric Cherenkov telescopes, notably the Major Atmospheric Gamma Imaging Cherenkov (MAGIC) telescopes, revealed periods where the detected γ-ray flux from the blazar reached energies up to 400 GeV. Measurements of the source have also been completed at x-ray, optical, and radio wavelengths. We have investigated models associating neutrino and γ-ray production and find that correlation of the neutrino with the flare of TXS 0506+056 is statistically significant at the level of 3 standard deviations (sigma). On the basis of the redshift of TXS 0506+056, we derive constraints for the muon-neutrino luminosity for this source and find them to be similar to the luminosity observed in γ-rays. CONCLUSION The energies of the γ-rays and the neutrino indicate that blazar jets may accelerate cosmic rays to at least several PeV. The observed association of a high-energy neutrino with a blazar during a period of enhanced γ-ray emission suggests that blazars may indeed be one of the long-sought sources of very-high-energy cosmic rays, and hence responsible for a sizable fraction of the cosmic neutrino flux observed by IceCube.
Published: 2018
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5. Multi-messenger Observations of a Binary Neutron Star Merger

Author: Abbott, B. P., Abbott, R., Abbott, T. D., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R. X., Adya, V. B., Affeldt, C., Afrough, M., Agarwal, B., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, B., Allen, G., Allocca, A., Altin, P. A., Amato, A., Ananyeva, A., Anderson, S. B., Anderson, W. G., Angelova, S. V., Antier, S., Appert, S., Arai, K., Araya, M. C., Areeda, J. S., Arnaud, N., Arun, K. G., Ascenzi, S., Ashton, G., Ast, M., Aston, S. M., Astone, P., Atallah, D. V., Aufmuth, P., Aulbert, C., AultONeal, K., Austin, C., Avila-Alvarez, A., Babak, S., Bacon, P., Bader, M. K. M., Bae, S., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Banagiri, S., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barkett, K., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Barthelmy, S. D., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Batch, J. C., Bawaj, M., Bayley, J. C., Bazzan, M., Bécsy, B., Beer, C., Bejger, M., Belahcene, I., Bell, A. S., Berger, B. K., Bergmann, G., Bero, J. J., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhagwat, S., Bhandare, R., Bilenko, I. A., Billingsley, G., Billman, C. R., Birch, J., Birney, R., Birnholtz, O., Biscans, S., Biscoveanu, S., Bisht, A., Bitossi, M., Biwer, C., Bizouard, M. A., Blackburn, J. K., Blackman, J., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bock, O., Bode, N., Boer, M., Bogaert, G., Bohe, A., Bondu, F., Bonilla, E., Bonnand, R., Boom, B. A., Bork, R., Boschi, V., Bose, S., Bossie, K., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Branchesi, M., Brau, J. E., Briant, T., Brillet, A., Brinkmann, Markus, Brisson, V., Brockill, P., Broida, J. E., Brooks, A. F., Brown, D. A., Brown, D. D., Brunett, S., Buchanan, C. C., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. 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Abstract: 59 Seiten : Illustrationen, Tabellen, Diagramme (2017).
Published: 2017
Full Text: View/download PDF

6. Supplement: 'Localization and Broadband Follow-up of the Gravitational-wave Transient GW150914' (2016, ApJS, 225, 8)

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., Bodiya, T. P., Goetz, R., Mihara, T., Gondan, L., González, G., Castro, J. M. G., Gopakumar, A., Gordon, N. A., Gorodetsky, M. L., Miao, H., Gossan, S. E., Walsh, S., Johnson, M. D., Aston, S. M., Tomida, H., Gosselin, M., Gouaty, R., Graef, C., Graff, P. B., Granata, M., Grant, A., Gras, S., Wang, G., Michel, C., Gray, C., Greco, G., Ueno, S., Johnson, M. W. G., Green, A. C., Astone, P., Groot, P., Grote, H., Grunewald, S., Vikram, V., Guidi, G. M., Guo, X., Nichol, R. C., Gupta, A., Tsunemi, H., Gupta, M. K., Gushwa, K. E., Karliner, I., Gustafson, E. K., Gustafson, R., Wang, H., Aufmuth, P., Hacker, J. J., Hall, B. R., Hall, E. D., Middleton, H., Cavalier, F., Hammond, G., Haney, M., Hanke, M. M., Hanks, J., Wang, M., Braginsky, V. B., Hanna, C., Hannam, M. D., Hanson, J., Aulbert, C., Hardwick, T., Cowperthwaite, P. S., Mikhailov, E. E., Haris, K., Harms, J., Wang, X., Harry, G. M., Harry, I. W., Hart, M. J., Kasen, D., Hartman, M. T., Haster, C. -J., Haughian, K., Matsuoka, M., Heidmann, A., Milano, L., Wang, Y., Babak, S., Heintze, M. C., Heitmann, H., Hello, P., Hemming, G., Hendry, M., Kent, S., Heng, I. S., MAXI Collaboration, Hennig, J., Ward, R. L., Heptonstall, A. W., Miller, J., Heurs, M., Hild, S., Bacon, P., Hoak, D., Hodge, K. A., Hofman, D., Hollitt, S. E., Mason, K., Warner, J., Kessler, R., Holt, K., Holz, D. E., Millhouse, M., Hopkins, P., Hosken, D. J., Hough, J., Houston, E. A., Bader, M. K. M., Howell, E. J., Smith, M., Fraser, M., Croft, S., Hu, Y. M., Huang, S., Kim, A. G., Huerta, E. A., Królak, A., Batch, J. C., Huet, D., Hughey, B., Husa, S., Martini, P., Huttner, S. H., Feng, L., Huynh-Dinh, T., Idrisy, A., Baker, P. T., Indik, N., Ingram, D. R., Carrasco Kind, M., Minenkov, Y., Inta, R., Was, M., Isa, H. N., Isac, J. -M., Franzen, T. M. O., Isi, M., Islas, G., Isogai, T., Iyer, B. R., Izumi, K., Baldaccini, F., Jacqmin, T., Weaver, B., Ming, J., Kuehn, K., Jang, H., Gaensler, B. M., Jani, K., Jaranowski, P., Jawahar, S., Jiménez-Forteza, F., Johnson, W. W., Jones, D. I., Boer, M., Jones, R., Jonker, R. J. G., Mirshekari, S., Ballardin, G., Johnston-Hollitt, M., Kuropatkin, N., Ju, L., Kalaghatgi, C. V., Kalogera, V., Kandhasamy, S., Wei, L. -W., Kang, G., Kanner, J. B., Karki, S., Kasprzack, M., Mishra, C., Kaplan, D. L., Katsavounidis, E., Katzman, W., Lahav, O., Ballmer, S. W., Walker, A. R., Kaufer, S., Kaur, T., Kawabe, K., Kawazoe, F., Kéfélian, F., Kehl, M. S., Morales, M. F., Nord, B., Keitel, D., Kelley, D. B., Weinert, M., Kells, W., Li, T. S., Kennedy, R., Barayoga, J. C., Key, J. S., Khalaidovski, A., Khalili, F. Y., Tingay, S. J., Khan, I., Mitra, S., Weinstein, A. J., Khan, S., Khan, Z., Khazanov, E. A., Kijbunchoo, N., Lima, M., Kim, C., Kim, J., Barclay, S. E., Crocce, M., Kim, K., Weiss, R., Kim, N., Mitrofanov, V. P., Kim, Y. -M., King, E. J., King, P. J., Kinzel, D. L., Kissel, J. S., Branchesi, M., Kleybolte, L., Cavalieri, R., Blackburn, J. K., Welborn, T., Klimenko, S., Koehlenbeck, S. M., Barish, B. C., Mitselmakher, G., Kokeyama, K., Koley, S., Kondrashov, V., Kontos, A., Korobko, M., Korth, W. Z., Martin, R. M., Masserot, A., Mittleman, R., Barker, D., Moggi, A., Mohan, M., Baune, C., Mohapatra, S. R. P., Montani, M., Moore, B. C., Nugent, P., Matone, L., Moore, C. J., Wayth, R. B., Moraru, D., Moreno, G., Krueger, C., Morriss, S. R., Mossavi, K., Mours, B., Mow-Lowry, C. M., Bavigadda, V., Wen, L., Mueller, C. L., Mueller, G., Williams, A., Ogando, R., Muir, A. W., Mukherjee, A., Kuehn, G., Mukherjee, D., Mukherjee, S., Mukund, N., Lord, J. E., Mullavey, A., Munch, J., Murphy, D. J., Murchison Wide-field Array (MWA Collaboration), Bazzan, M., Murray, P. 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H., Pan, H., Pankow, C., Pannarale, F., Pant, B. C., Affeldt, C., Paoletti, F., Paoli, A., Papa, M. A., Berger, B. K., Paris, H. R., White, D. J., Cunha, C. E., Lange, J., Parker, W., Pascucci, D., Pasqualetti, A., Passaquieti, R., Passuello, D., Briant, T., Patricelli, B., Patrick, Z., Inserra, C., Pearlstone, B. L., Massinger, T. J., Pedraza, M., Lantz, B., Bergman, J., Pedurand, R., Pekowsky, L., Pele, A., Penn, S., Perreca, A., Whiting, B. F., Roodman, A., Phelps, M., Schultz, A., Piccinni, O., Pichot, M., Lasky, P. D., Piergiovanni, F., Pierro, V., Bergmann, G., Pillant, G., Williams, R. D., Pinard, L., Pinto, I. M., Pitkin, M., Cella, G., Rosell, A. C., Poggiani, R., Popolizio, P., Barone, F., Post, A., Powell, J., Lorenzini, M., Prasad, J., Predoi, V., Berry, C. P. L., Premachandra, S. S., Denneau, L., Prestegard, T., Price, L. R., Rykoff, E. S., Prijatelj, M., Lazzarini, A., Williamson, A. R., Principe, M., Privitera, S., Prodi, G. 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C., Schubnell, M., Rüdiger, A., Bhandare, R., Ruggi, P., Ryan, K., Kankare, E., Sachdev, S., Stubbs, C. W., Lee, C. H., Sadecki, T., Sadeghian, L., Salconi, L., Saleem, M., Salemi, F., Scolnic, D., Samajdar, A., Wester, W., Sammut, L., Bilenko, I. A., Masso-Reid, M., Sanchez, E. J., Lee, H. K., Sandberg, V., Sandeen, B., Sanders, J. R., Sassolas, B., Sathyaprakash, B. S., Bogan, C., Saulson, P. R., Sevilla-Noarbe, I., Sauter, O., D'Andrea, C. B., Savage, R. L., Sawadsky, A., Lee, H. M., Billingsley, G., Schale, P., Schilling, R., Woan, G., Schmidt, J., Schmidt, P., Schnabel, R., Schofield, R. M. S., Tonry, J., Brillet, A., Schönbeck, A., Schreiber, E., Lee, K., Schuette, D., Loriette, V., Schutz, B. F., Birch, J., Scott, J., Scott, S. M., Sellers, D., Waters, C., Sentenac, D., Sequino, V., Sheldon, E., Sergeev, A., Worden, J., Lenon, A., Serna, G., Setyawati, Y., Sevigny, A., Shaddock, D. A., Birney, R., Cepeda, C. B., Shah, S., Shahriar, M. S., Shaltev, M., Thrane, E., Wright, J. 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G., Messick, C., Garufi, F., Gatto, A., Gaur, G., Gehrels, N., Gemme, G., Gendre, B., Genin, E., Negoro, H., Lombardi, A. L., Ashton, G., Gennai, A., Honscheid, K., Kringel, V., Meyers, P. M., George, J., Gergely, L., Germain, V., Ghosh, A., Ghosh, S., ELIAS DE LA ROSA, NANCY DEL CARMEN, Nakahira, S., Giaime, J. A., Giardina, K. D., Giazotto, A., Gill, K., Ast, M., Mezzani, F., James, D. J., Glaefke, A., and Goetz, E.
Abstract: This Supplement provides supporting material for Abbott et al. (2016a). 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.
Published: 2016

7. Dust from Comet 209P/LINEAR during its 2014 Return: Parent Body of a New Meteor Shower, the May Camelopardalids

Author: Ishiguro, M, Kuroda, D, Hanayama, H, Takahashi, J, Hasegawa, S, Sarugaku, Y, Watanabe, M, Imai, M, Goda, S, Akitaya, H, Takagi, Y, Morihana, K, Honda, S, Arai, A, Sekiguchi, K, Oasa, Y, Saito, Yoshihiko, Morokuma, T, Murata, K, Nogami, D, Nagayama, T, Yanagisawa, K, Yoshida, M, Ohta, K, Kawai, Nobuyuki, Miyaji, T, Fukushima, H, Watanabe, J.-i., Opitom, C, Jehin, E, Gillon, M, Vaubaillon, J.~J., Department of Physics and Astronomy and Center for Theoretical Physics, Seoul National University, Seoul National University [Seoul], Okayama Astrophysical Observatory ( OAO ), National Astronomical Observatory of Japan ( NAOJ ), Ishigakijima Astronomical Observatory, Nishi-Harima Astronomical Observatory, Center for Astronomy, Institute of Space and Astronautical Science ( ISAS ), Department of Cosmosciences, Hokkaido University, Hiroshima Astrophysical Science Center, Hiroshima University, Japan, Faculty of Education, Saitama University, Department of Physics [Tokyo], Tokyo Institure of Technology, Institute of Astronomy, Graduate School of Science, The University of Tokyo, Department of Astrophysics, Nagoya University, Department of astronomy, Kyoto University, Graduate School of Science and Engineering, Kagoshima University, Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, Institut de Mécanique Céleste et de Calcul des Ephémérides ( IMCCE ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université de Lille-Centre National de la Recherche Scientifique ( CNRS ), Department of Physics and Astronomy [Seoul], Seoul National University [Seoul] (SNU), Center for Theoretical Physics [Seoul], Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Okayama Astrophysical Observatory (OAO), National Astronomical Observatory of Japan (NAOJ), Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency [Sagamihara] (JAXA), Hokkaido University [Sapporo, Japan], Hiroshima University, The University of Tokyo (UTokyo), Department of Astrophysics [Nagoya], Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics, 010504 meteorology & atmospheric sciences, Terminal velocity, Meteoroid, Comet, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Escape velocity, comets: individual: 209P/LINEAR, 01 natural sciences, comets: individual (209P/LINEAR), Jupiter, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Comet nucleus, 0103 physical sciences, interplanetary medium, Meteor shower, 010303 astronomy & astrophysics, [ SDU ] Sciences of the Universe [physics], Astrophysics - Earth and Planetary Astrophysics, 0105 earth and related environmental sciences, Cosmic dust
Abstract: 著者人数: 32名, Accepted: 2014-12-11, 資料番号: SA1005017000
Published: 2015
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8. Spectroscopic characterization of galaxy clusters in RCS-1: spectroscopic confirmation, redshift accuracy, and dynamical mass-richness relation.

Author: Gilbank, David G., Barrientos, L. Felipe, Ellingson, Erica, Blindert, Kris, Yee, H. K. C., Anguita, T., Gladders, M. D., Hall, P. B., Hertling, G., Infante, L., Yan, R., Carrasco, M., Garcia-Vergara, Cristina, Dawson, K. S., Lidman, C., and Morokuma, T.
Subjects: GALAXY clusters, GALACTIC redshift, ASTRONOMICAL spectroscopy, STELLAR mass, ASTRONOMICAL photometry
Abstract: We present follow-up spectroscopic observations of galaxy clusters from the first Red-sequence Cluster Survey (RCS-1). This work focuses on two samples, a lower redshift sample of ~30 clusters ranging in redshift from z~0.2-0.6 observed with multiobject spectroscopy (MOS) on 4-6.5-m class telescopes and a z ~ 1 sample of ~10 clusters 8-m class telescope observations. We examine the detection efficiency and redshift accuracy of the now widely used red-sequence technique for selecting clusters via over densities of red-sequence galaxies. Using both these data and extended samples including previously published RCS-1 spectroscopy and spectroscopic redshifts from SDSS, we find that the red-sequence redshift using simple two- filter cluster photometric redshifts is accurate to σz ≈ 0.035(1 + z) in RCS-1. This accuracy can potentially be improved with better survey photometric calibration. For the lower redshift sample, ~5 per cent of clusters show some (minor) contamination from secondary systems with the same red-sequence intruding into the measurement aperture of the original cluster. At z ~ 1, the rate rises to ~20 per cent. Approximately ten per cent of projections are expected to be serious, where the two components contribute significant numbers of their red-sequence galaxies to another cluster. Finally, we present a preliminary study of the mass-richness calibration using velocity dispersions to probe the dynamical masses of the clusters. We find a relation broadly consistent with that seen in the local universe from the WINGS sample at z ~ 0.05. [ABSTRACT FROM AUTHOR]
Published: 2018
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9. Constraints on core-collapse supernova progenitors from explosion site integral field spectroscopy.

Author: Kuncarayakti, H., Anderson, J. P., Galbany, L., Maeda, K., Hamuy, M., Aldering, G., Arimoto, N., Doi, M., Morokuma, T., and Usuda, T.
Subjects: SUPERNOVAE, INTEGRAL field spectroscopy, STAR observations, STELLAR mass, STELLAR evolution
Abstract: Context. Observationally, supernovae (SNe) are divided into subclasses according to their distinct characteristics. This diversity naturally reflects the diversity in the progenitor stars. It is not entirely clear, however, how different evolutionary paths leading massive stars to become an SN are governed by fundamental parameters such as progenitor initial mass and metallicity. Aims. This paper places constraints on progenitor initial mass and metallicity in distinct core-collapse SN subclasses through a study of the parent stellar populations at the explosion sites. Methods. Integral field spectroscopy (IFS) of 83 nearby SN explosion sites with a median distance of 18 Mpc has been collected and analysed, enabling detection and spectral extraction of the parent stellar population of SN progenitors. From the parent stellar population spectrum, the initial mass and metallicity of the coeval progenitor are derived by means of comparison to simple stellar population models and strong-line methods. Additionally, near-infrared IFS was employed to characterise the star formation history at the explosion sites. Results. No significant metallicity differences are observed among distinct SN types. The typical progenitor mass is found to be highest for SN type Ic, followed by type Ib, then types IIb and II. Type IIn is the least associated with young stellar populations and thus massive progenitors. However, statistically significant differences in progenitor initial mass are observed only when comparing SNe IIn with other subclasses. Stripped-envelope SN progenitors with initial mass estimates lower than 25 M☉ are found; they are thought to be the result of binary progenitors. Confirming previous studies, these results support the notion that core-collapse SN progenitors cannot arise from single-star channels only, and both single and binary channels are at play in the production of core-collapse SNe. Near-infrared IFS suggests that multiple stellar populations with different ages may be present in some of the SN sites. As a consequence, there could be a non-negligible amount of contamination from old populations, and therefore the individual age estimates are effectively lower limits. [ABSTRACT FROM AUTHOR]
Published: 2018
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10. The radio structure of the peculiar narrow-line Seyfert 1 galaxy candidate J1100+4421.

Author: Gabányi, K. É., Frey, S., Paragi, Z., Järvelä, E., Morokuma, T., An, T., Tanaka, M., and Tar, I.
Subjects: ACTIVE galaxies, BL Lacertae objects, BLACK holes, SPECTRAL energy distribution, RADIO sources (Astronomy), COMPACT objects (Astronomy)
Abstract: Narrow-line Seyfert 1 galaxies (NLS1) are an intriguing subclass of active galactic nuclei. Their observed properties indicate low central black hole mass and high accretion rate. The extremely radio-loud NLS1 sources often show relativistic beaming and are usually regarded as younger counterparts of blazars. Recently, the object SDSS J110006.07+442144.3 was reported as a candidate NLS1 source. The characteristics of its dramatic optical flare indicated its jet-related origin. The spectral energy distribution of the object was similar to that of the γ -ray detected radio-loud NLS1, PMNJ0948+0022. Our high-resolution European very long baseline interferometry network observations at 1.7 and 5 GHz revealed a compact core feature with a brightness temperature of ≳1010 K. Using the lowest brightness temperature value and assuming a moderate Lorentz factor of ∼9, the jet viewing angle is ≲26°. Archival Very Large Array data show a large-scale radio structure with a projected linear size of ∼150 kpc reminiscent of double-sided morphology. [ABSTRACT FROM AUTHOR]
Published: 2018
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11. SN 2016jhj at redshift 0.34: extending the Type II supernova Hubble diagram using the standard candle method.

Author: de Jaeger, T., Galbany, L., Filippenko, A. V., Gonzélez-Gaitén, S., Yasuda, N., Maeda, K., Tanaka, M., Morokuma, T., Moriya, T. J., Tominaga, N., Nomoto, K., Komiyama, Y., Anderson, J. P., Brink, T. G., Carlberg, R. G., Folatelli, G., Hamuy, M., Pignata, G., and Zheng, W.
Subjects: REDSHIFT, TYPE II supernovae, DARK energy, LARGE Synoptic Survey Telescope, EXTRAGALACTIC distances
Abstract: Although Type Ia supernova cosmology has now reached a mature state, it is important to develop as many independent methods as possible to understand the true nature of dark energy. Recent studies have shown that Type II supernovae (SNe II) offer such a path and could be used as alternative distance indicators. However, the majority of these studies were unable to extend the Hubble diagram above redshift z=0.3 because of observational limitations. Here, we show that we are now ready to move beyond low redshifts and attempt high-redshift (z ≳ 0.3) SN II cosmology as a result of new-generation deep surveys such as the Subaru/Hyper Suprime-Cam survey. Applying the 'standard candle method' toSN2016jhj (z=0.3398±0.0002; discovered by HSC) together with a low-redshift sample, we are able to construct the highest-redshift SN II Hubble diagram to date with an observed dispersion of 0.27 mag (i.e. 12--13 per cent in distance). This work demonstrates the bright future of SN II cosmology in the coming era of large, wide-field surveys like that of the Large Synoptic Survey Telescope. [ABSTRACT FROM AUTHOR]
Published: 2017
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12. SPECTRA AND HUBBLE SPACE TELESCOPE LIGHT CURVES OF SIX TYPE Ia SUPERNOVAE AT 0.511 < z < 1.12 AND THE UNION2 COMPILATION

Author: Amanullah, R, Lidman, C, Rubin, D, Aldering, G, Astier, P, Barbary, K, Burns, MS, Conley, A, Dawson, KS, Deustua, SE, Doi, M, Fabbro, S, Faccioli, L, Fakhouri, HK, Folatelli, G, Fruchter, AS, Furusawa, H, Garavini, G, Goldhaber, G, Goobar, A, Groom, DE, Hook, I, Howell, DA, Kashikawa, N, Kim, AG, Knop, RA, Kowalski, M, Linder, E, Meyers, J, Morokuma, T, Nobili, S, Nordin, J, Nugent, PE, Ostman, L, Pain, R, Panagia, N, Perlmutter, S, Raux, J, Ruiz-Lapuente, P, Spadafora, AL, Strovink, M, Suzuki, N, Wang, L, Wood-Vasey, WM, Yasuda, N, Project, SC, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), Department of Physics, Stockholm University, University of Oxford Astrophysics, Lawrence Berkeley National Laboratory [Berkeley] (LBNL), Supernova Cosmology Project, and 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)
Subjects: Physics, 010308 nuclear & particles physics, Equation of state (cosmology), [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Shape of the universe, Astronomy and Astrophysics, Astrophysics, Type (model theory), Light curve, 7. Clean energy, 01 natural sciences, Redshift, Photometry (optics), [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Supernova, supernovae: general, Space and Planetary Science, cosmology: observations, 0103 physical sciences, Dark energy, cosmological parameters, 010303 astronomy & astrophysics
Abstract: We report on work to increase the number of well-measured Type Ia supernovae (SNe Ia) at high redshifts. Light curves, including high signal-to-noise Hubble Space Telescope data, and spectra of six SNe Ia that were discovered during 2001, are presented. Additionally, for the two SNe with z > 1, we present ground-based J-band photometry from Gemini and the Very Large Telescope. These are among the most distant SNe Ia for which ground-based near-IR observations have been obtained. We add these six SNe Ia together with other data sets that have recently become available in the literature to the Union compilation. We have made a number of refinements to the Union analysis chain, the most important ones being the refitting of all light curves with the SALT2 fitter and an improved handling of systematic errors. We call this new compilation, consisting of 557 SNe, the Union2 compilation. The flat concordance ΛCDM model remains an excellent fit to the Union2 data with the best-fit constant equation-of-state parameter w = -0.997+0.050 -0.054(stat)+0.077 -0.082(stat + sys together) for a flat universe, or w = -1.038+0.056 -0.059(stat)+0.093 -0.097(stat + sys together) with curvature. We also present improved constraints on w(z). While no significant change in w with redshift is detected, there is still considerable room for evolution in w. The strength of the constraints depends strongly on redshift. In particular, at z >~ 1, the existence and nature of dark energy are only weakly constrained by the data. Based in part on observations made with the NASA/ESA Hubble Space Telescope, obtained from the data archive at the Space Telescope Science Institute (STScI). STScI is operated by the Association of Universities for Research in Astronomy (AURA), Inc. under the NASA contract NAS 5-26555. The observations are associated with programs HST-GO-08585 and HST-GO-09075. Based, in part, on observations obtained at the ESO La Silla Paranal Observatory (ESO programs 67.A-0361 and 169.A-0382). Based, in part, on observations obtained at the Cerro-Tololo Inter-American Observatory (CTIO), National Optical Astronomy Observatory (NOAO). Based on observations obtained at the Canada-France-Hawaii Telescope (CFHT). Based, in part, on observations obtained at the Gemini Observatory (Gemini programs GN-2001A-SV-19 and GN-2002A-Q-31). Based, in part on observations obtained at the Subaru Telescope. Based, in part, on data that were obtained at the W. M. Keck Observatory.
Published: 2010
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13. Spectra and Light Curves of Six Type Ia Supernovae at 0.511 < z < 1.12 and the Union2 Compilation

Author: Amanullah, R., Lidman, C., Rubin, D., Aldering, G., Astier, P., Barbary, K., Burns, M. S., Conley, A., Dawson, K. S., Deustua, S. E., Doi, M., Fabbro, S., Faccioli, L., Fakhouri, H. K., Folatelli, G., Fruchter, A. S., Furusawa, H., Garavini, G., Goldhaber, G., Goobar, A., Groom, D. E., Hook, I., Howell, D. A., Kashikawa, N., Kim, A. G., Knop, R. A., Kowalski, M., Linder, E., Meyers, J., Morokuma, T., Nobili, S., Nordin, J., Nugent, P. E., Ostman, L., Pain, R., Panagia, N., Perlmutter, S., Raux, J., Ruiz-Lapuente, P., Spadafora, A. L., Strovink, M., Suzuki, N., Wang, L., Wood-Vasey, W. M., and Yasuda, N.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We report on work to increase the number of well-measured Type Ia supernovae (SNe Ia) at high redshifts. Light curves, including high signal-to-noise HST data, and spectra of six SNe Ia that were discovered during 2001 are presented. Additionally, for the two SNe with z>1, we present ground-based J-band photometry from Gemini and the VLT. These are among the most distant SNe Ia for which ground based near-IR observations have been obtained. We add these six SNe Ia together with other data sets that have recently become available in the literature to the Union compilation (Kowalski et al. 2008). We have made a number of refinements to the Union analysis chain, the most important ones being the refitting of all light curves with the SALT2 fitter and an improved handling of systematic errors. We call this new compilation, consisting of 557 supernovae, the Union2 compilation. The flat concordance LambdaCDM model remains an excellent fit to the Union2 data with the best fit constant equation of state parameter w=-0.997^{+0.050}_{-0.054} (stat) ^{+0.077}_{-0.082} (stat+sys\ together) for a flat universe, or w=-1.035^{+0.055}_{-0.059} (stat)^{+0.093}_{-0.097} (stat+sys together) with curvature. We also present improved constraints on w(z). While no significant change in w with redshift is detected, there is still considerable room for evolution in w. The strength of the constraints depend strongly on redshift. In particular, at z > 1, the existence and nature of dark energy are only weakly constrained by the data., Comment: 33 pages, 18 figures; accepted for publication in Astrophysical Journal. For data tables, code for cosmological analysis and full-resolution figures, see http://supernova.lbl.gov/Union/
Published: 2010

14. An Intensive HST Survey for z>1 Supernovae by Targeting Galaxy Clusters

Author: Dawson, K. S., Aldering, G., Amanullah, R., Barbary, K., Barrientos, L. F., Brodwin, M., Connolly, N., Dey, A., Doi, M., Donahue, M., Eisenhardt, P., Ellingson, E., Faccioli, L., Fadeyev, V., Fakhouri, H. K., Fruchter, A. S., Gilbank, D. G., Gladders, M. D., Goldhaber, G., Gonzalez, A. H., Goobar, A., Gude, A., Hattori, T., Hoekstra, H., Huang, X., Ihara, Y., Jannuzi, B. T., Johnston, D., Kashikawa, K., Koester, B., Konishi, K., Kowalski, M., Lidman, C., Linder, E. V., Lubin, L., Meyers, J., Morokuma, T., Munshi, F., Mullis, C., Oda, T., Panagia, N., Perlmutter, S., Postman, M., Pritchard, T., Rhodes, J., Rosati, P., Rubin, D., Schlegel, D. J., Spadafora, A., Stanford, S. A., Stanishev, V., Stern, D., Strovink, M., Suzuki, N., Takanashi, N., Tokita, K., Wagner, M., Wang, L., Yasuda, N., and Yee, H. K. C.
Subjects: Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a new survey strategy to discover and study high redshift Type Ia supernovae (SNe Ia) using the Hubble Space Telescope (HST). By targeting massive galaxy clusters at 0.90.95, nine of which were in galaxy clusters. This strategy provides a SN sample that can be used to decouple the effects of host galaxy extinction and intrinsic color in high redshift SNe, thereby reducing one of the largest systematic uncertainties in SN cosmology., Comment: 15 pages, 8 figures, accepted by AJ, see http://www.supernova.lbl.gov for additional information pertaining to the HST Cluster SN Survey
Published: 2009

15. The Subaru/XMM-Newton Deep Survey (SXDS) - II. Optical Imaging and Photometric Catalogs

Author: Furusawa, H., Kosugi, G., Akiyama, M., Takata, T., Sekiguchi, K., Tanaka, I., Iwata, I., Kajisawa, M., Yasuda, N., Doi, M., Ouchi, M., Simpson, C., Shimasaku, K., Yamada, T., Furusawa, J., Morokuma, T., Ishida, C. M., Aoki, K., Fuse, T., Imanishi, M., Iye, M., Karoji, H., Kobayashi, N., Kodama, T., Komiyama, Y., Maeda, Y., Miyazaki, S., Mizumoto, Y., Nakata, F., Noumaru, J., Ogasawara, R., Okamura, S., Saito, T., Sasaki, T., Ueda, Y., and Yoshida, M.
Subjects: Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract: We present multi-waveband optical imaging data obtained from observations of the Subaru/XMM-Newton Deep Survey (SXDS). The survey field, centered at R.A.=02:18:00, decl.=-05:00:00, has been the focus of a wide range of multi-wavelength observing programs spanning from X-ray to radio wavelengths. A large part of the optical imaging observations are carried out with Suprime-Cam on Subaru Telescope at Mauna Kea in the course of Subaru Telescope Observatory Projects. This paper describes our optical observations, data reduction and analysis procedures employed, and the characteristics of the data products. A total area of 1.22 sqdeg is covered in five contiguous sub-fields, each of which corresponds to a single Suprime-Cam field of view (34'x27'), in five broad-band filters B, V, Rc, i', z' to the depths of B=28.4, V=27.8, Rc=27.7, i'=27.7 and z'=26.6 (AB, 3-sigma, 2-arcsec aperture). The data are reduced and compiled into five multi-waveband photometric catalogs, separately for each Suprime-Cam pointing. The i'-band catalogs contain about 900,000 objects, making the SXDS catalogs one of the largest multi-waveband catalogs in corresponding depth and area coverage. The SXDS catalogs can be used for an extensive range of astronomical applications such as the number density of the Galactic halo stars to the large scale structures at the distant universe. The number counts of galaxies are derived and compared with those of existing deep extragalactic surveys. The optical data, the source catalogs, and configuration files used to create the catalogs are publicly available via the SXDS web page (http://www.naoj.org/Science/SubaruProject/SXDS/index.html), 55 pages, 22 figures, 9 tables, accepted by ApJS, a higher-resolution version is available at http://step.mtk.nao.ac.jp/sxds/
Published: 2008

16. Quantitative comparison between type Ia supernova spectra at low and high redshifts: A case study

Author: Garavini, G, Folatelli, G, Nobili, S, Aldering, G, Amanullah, R, Antilogus, P, Astier, P, Blanc, G, Bronder, T, Burns, MS, Conley, A, Deustua, SE, Doi, M, Fabbro, S, Fadeyev, V, Gibbons, R, Goldhaber, G, Goobar, A, Groom, DE, Hook, I, Howell, DA, Kashikawa, N, Kim, AG, Kowalski, M, Kuznetsova, N, Lee, BC, Lidman, C, Mendez, J, Morokuma, T, Motohara, K, Nugent, PE, Pain, R, Perlmutter, S, Quimby, R, Raux, J, Regnault, N, Ruiz-Lapuente, P, Sainton, G, Schahmaneche, K, Smith, E, Spadafora, AL, Stanishev, V, Thomas, RC, Walton, NA, Wang, L, Wood-Vasey, WM, Yasuda, N, Project, SC, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), APC - Cosmologie, 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)-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), SUPERNOVAE, 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), 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), Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)
Subjects: [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, 01 natural sciences, Cosmology, Spectral line, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], astro-ph, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, supernovae : general [stars], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics (astro-ph), Astronomy and Astrophysics, Redshift, Blueshift, Supernova, 13. Climate action, Space and Planetary Science, Astronomical and Space Sciences, early Universe [cosmology]
Abstract: We develop a method to measure the strength of the absorption features in Type Ia supernova (SN Ia) spectra and use it to make a quantitative comparison between the spectra of Type Ia supernovae at low and high redshifts. In this case study, we apply the method to 12 high-redshift (0.212 < z < 0.912) SNe Ia observed by the Supernova Cosmology Project . Through measurements of the strengths of these features and of the blueshift of the absorption minimum in Ca II H&K, we show that the spectra of the high-redshift SNe Ia are quantitatively similar to spectra of nearby SNe Ia (z < 0.15). One supernova in our high redshift sample, SN 2002fd at z=0.279, is found to have spectral characteristics that are associated with peculiar SN 1991T/SN 1999aa-like supernovae., accepted for publication on A&A
Published: 2007
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17. Multi-wavelength Observations of the Black Widow Pulsar 2FGL J2339.6-0532 with OISTER and Suzaku

Author: Yatsu, Yoichi, KATAOKA, JUN, Takahashi, Y, Tachibana, Yutaro, Kawai, Nobuyuki, Shibata, S, Pike, S, Yoshii, Taketoshi, Arimoto, Makoto, Saito, Yoshihiko, Nakamori, T, Sekiguchi, K, Kuroda, D, Yanagisawa, K, Hanayama, H, Watanabe, M, Hamamoto, K, Nakao, H, Ozaki, A, Motohara, K, Konishi, M, Tateuchi, K, Matsunaga, N, Morokuma, T, Nagayama, T, Murata, K, Akitaya, H, Yoshida, M, Ali, G.~B., Essam Mohamed, A, Isogai, M, Arai, A, Takahashi, H, Hashimoto, O, Miyanoshita, R, Omodaka, T, Takahashi, J, Tokimasa, N, Matsuda, K, Okumura, S.-i., Nishiyama, K, Urakawa, S, Nogami, D, and Oasa, Y
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, J.2, Accretion (meteorology), Astrophysics::High Energy Astrophysical Phenomena, Extinction (astronomy), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Light curve, gamma rays: stars, Luminosity, Stars, X-rays: binaries, Pulsar, Space and Planetary Science, Millisecond pulsar, 85-02, pulsars: general, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, pulsars: individual: 2FGL J2339.6-0532, Fermi Gamma-ray Space Telescope
Abstract: Multi-wavelength observations of the black-widow binary system 2FGL J2339.6-0532 are reported. The Fermi gamma-ray source 2FGL J2339.6-0532 was recently categorized as a black widow in which a recycled millisecond pulsar (MSP) is evaporating up the companion star with its powerful pulsar wind. Our optical observations show clear sinusoidal light curves due to the asymmetric temperature distribution of the companion star. Assuming a simple geometry, we constrained the range of the inclination angle of the binary system to 52$^{\circ}$ < i < 59$^{\circ}$, which enables us to discuss the interaction between the pulsar wind and the companion in detail. The X-ray spectrum consists of two components: a soft, steady component that seems to originate from the surface of the MSP, and a hard variable component from the wind-termination shock near the companion star. The measured X-ray luminosity is comparable to the bolometric luminosity of the companion, meaning that the heating efficiency is less than 0.5. In the companion orbit, 10$^{11}$ cm from the pulsar, the pulsar wind is already in particle dominant-stage, with a magnetization parameter of $��$ < 0.1. In addition, we precisely investigated the time variations of the X-ray periodograms and detected a weakening of orbital modulation. The observed phenomenon may be related to an unstable pulsar-wind activity or a weak mass accretion, both of which can result in the temporal extinction of radio-pulse., 13pages, 11 figures, Accepted(ApJ)
Published: 2015

18. Instruments with Many Dichroic Mirrors and CCDs

Author: Doi, M., Hayano, J., Utsunomiya, H., Ihara, Y., Tokita, K., Takanashi, N., Sako, S., Okamura, S., Morokuma, T., Furusawa, H., Komiyama, Y., Yagi, M., Okada, N., Arai, A., Uemura, M., Kawabata, K., Yamashita, T., Osugi, T., Abe, M., and Hasegawa, S.
Abstract: 資料番号: PA0810003000
Published: 2008

19. Numerical and experimental investigation of TDOA-based positioning system by ultra-wideband impulse radio.

Author: Matsumoto, H., Kusano, H., Morokuma, T., and Sakamura, K.
Published: 2011
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20. A Dynamic Retargettable Multi-Protocol RFID Reader/Writer.

Author: Kobayashi, S., Sakamura, K., and Morokuma, T.
Published: 2007
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21. Supernovae in the Subaru Deep Field: an initial sample and Type Ia rate out to redshift 1.6.

Author: Poznanski, D., Maoz, D., Yasuda, N., Foley, R. J., Doi, M., Filippenko, A. V., Fukugita, M., Gal-Yam, A., Jannuzi, B. T., Morokuma, T., Oda, T., Schweiker, H., Sharon, K., Silverman, J. M., and Totani, T.
Subjects: TYPE I supernovae, STAR formation, REDSHIFT, GALAXIES, GALACTIC X-ray sources, CATACLYSMIC variable stars, ASTRONOMICAL observations, ASTRONOMICAL instruments
Abstract: Large samples of high-redshift supernovae (SNe) are potentially powerful probes of cosmic star formation, metal enrichment and SN physics. We present initial results from a new deep SN survey, based on re-imaging in the R, i′, z′ bands, of the 0.25 deg2 Subaru Deep Field (SDF), with the 8.2-m Subaru telescope and Suprime-Cam. In a single new epoch consisting of two nights of observations, we have discovered 33 candidate SNe, down to a z′-band magnitude of 26.3 (AB). We have measured the photometric redshifts of the SN host galaxies, obtained Keck spectroscopic redshifts for 17 of the host galaxies and classified the SNe using the Bayesian photometric algorithm of Poznanski et al. that relies on template matching. After correcting for biases in the classification, 55 per cent of our sample consists of Type Ia SNe and 45 per cent of core-collapse SNe. The redshift distribution of the SNe Ia reaches z≈ 1.6, with a median of z≈ 1.2. The core-collapse SNe reach z≈ 1.0, with a median of z≈ 0.5. Our SN sample is comparable to the Hubble Space Telescope/Great Observatories Origins Deep Survey (GOODS) sample in both size and redshift range. The redshift distributions of the SNe in the SDF and in GOODS are consistent, but there is a trend (which requires confirmation using a larger sample) for more high- z SNe Ia in the SDF. This trend is also apparent when comparing the SN Ia rates we derive to those based on GOODS data. Our results suggest a fairly constant rate at high redshift that could be tracking the star formation rate. Additional epochs on this field, already being obtained, will enlarge our SN sample to the hundreds, and determine whether or not there is a decline in the SN Ia rate at z≳ 1. [ABSTRACT FROM AUTHOR]
Published: 2007
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22. Conference Report.

Author: Murata, K., Minami, S., and Morokuma, T.
Published: 1975
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23. Absolute determination of the magnetic flux quantum using superconducting magnetic levitation.

Author: Shiota, F., Miki, Y., Namba, A., Nezu, Y., Sakamoto, Y., Morokuma, T., and Hara, K.
Published: 1995
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24. Meetings Calendar.

Author: Morokuma, T.
Published: 1975
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25. Improvements of measuring system on magnetic levitation system for the determination of magnetic flux quantum.

Author: Shiota, F. and Morokuma, T.
Published: 2002
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26. Toward absolute determination in NRLM proto-type superconducting magnetic levitation system for the future replacement of kilogram.

Author: Shiota, F., Miki, Y., Fujii, Y., Morokuma, T., and Nezu, Y.
Published: 2000
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27. Development of a new levitated-mass mechanism toward replacing the kilogram.

Author: Fujii, Y., Miki, Y., Shiota, F., Watanabe, R., Morokuma, T., and Nezu, Y.
Published: 2000
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28. Progress in absolute determination of /spl Phi//sub 0/ using superconducting magnetic levitation.

Author: Shiota, F., Miki, Y., Namba, A., Nezu, Y., Sakamoto, Y., Morokuma, T., and Hara, K.
Published: 1994
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29. Present status of the NRLM superconducting magnetic levitation system for absolute determination of the magnetic flux quantum.

Author: Shiota, F., Miki, Y., Fujii, Y., Namba, A., Morokuma, T., Nezu, Y., Kai, S., and Hara, K.
Published: 1996
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30. Improvements of NRLM superconducting magnetic levitation system for absolute determination of /spl Phi//sub 0/.

Author: Shiota, F., Miki, Y., Fujii, Y., Morokuma, T., and Nezu, Y.
Published: 1998
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31. Vertical displacement determination in the NRLM superconducting magnetic levitation system.

Author: Fujii, Y., Shiota, F., Miki, Y., and Morokuma, T.
Published: 1998
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32. THE SCHMIDT-KENNICUTT LAW OF MATCHED-AGE STAR-FORMING REGIONS; Paα OBSERVATIONS OF THE EARLY-PHASE INTERACTING GALAXY TAFFY I.

Author: Komugi, S., Tateuchi, K., Motohara, K., Takagi, T., Iono, D., Kaneko, H., Ueda, J., Saitoh, T. R., Kato, N., Konishi, M., Koshida, S., Morokuma, T., Takahashi, H., Tanabé, T., and Yoshii, Y.
Subjects: GALAXIES, STAR formation, MOLECULAR clouds, UNIVERSE, MOLECULAR gas lasers
Abstract: In order to test a recent hypothesis that the dispersion in the Schmidt-Kennicutt law arises from variations in the evolutionary stage of star-forming molecular clouds, we compared molecular gas and recent star formation in an early-phase merger galaxy pair, Taffy I (UGC 12915/UGC 12914, VV 254) which went through a direct collision 20 Myr ago and whose star-forming regions are expected to have similar ages. Narrowband Paα image is obtained using the ANIR near-infrared camera on the mini-TAO 1 m telescope. The image enables us to derive accurate star formation rates within the galaxy directly. The total star formation rate, 22.2 M☼ yr–1, was found to be much higher than previous estimates. Ages of individual star-forming blobs estimated from equivalent widths indicate that most star-forming regions are ∼7 Myr old, except for a giant H II region at the bridge which is much younger. Comparison between star formation rates and molecular gas masses for the regions with the same age exhibits a surprisingly tight correlation, a slope of unity, and star formation efficiencies comparable to those of starburst galaxies. These results suggest that Taffy I has just evolved into a starburst system after the collision, and the star-forming sites are at a similar stage in their evolution from natal molecular clouds except for the bridge region. The tight Schmidt-Kennicutt law supports the scenario that dispersion in the star formation law is in large part due to differences in evolutionary stage of star-forming regions. [ABSTRACT FROM AUTHOR]
Published: 2012
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33. CONSTRAINTS ON THE FAINT END OF THE QUASAR LUMINOSITY FUNCTION AT z ∼ 5 IN THE COSMOS FIELD.

Author: Ikeda, H., Nagao, T., Matsuoka, K., Taniguchi, Y., Shioya, Y., Kajisawa, M., Enoki, M., Capak, P., Civano, F., Koekemoer, A. M., Masters, D., Morokuma, T., Salvato, M., Schinnerer, E., and Scoville, N. Z.
Subjects: STELLAR luminosity function, SPECTRA of quasars, REDSHIFT, METAPHYSICAL cosmology, PHOTOMETRY
Abstract: We present the result of our low-luminosity quasar survey in the redshift range of 4.5 ≲ z ≲ 5.5 in the COSMOS field. Using the COSMOS photometric catalog, we selected 15 quasar candidates with 22 < i′ < 24 at z ∼ 5 that are ∼3 mag fainter than the Sloan Digital Sky Survey quasars in the same redshift range. We obtained optical spectra for 14 of the 15 candidates using FOCAS on the Subaru Telescope and did not identify any low-luminosity type-1 quasars at z ∼ 5, while a low-luminosity type-2 quasar at z ∼ 5.07 was discovered. In order to constrain the faint end of the quasar luminosity function at z ∼ 5, we calculated the 1σ confidence upper limits of the space density of type-1 quasars. As a result, the 1σ confidence upper limits on the quasar space density are Φ < 1.33 × 10–7 Mpc–3 mag–1 for –24.52 < M1450 < –23.52 and Φ < 2.88 × 10–7 Mpc–3 mag–1 for –23.52 < M1450 < –22.52. The inferred 1σ confidence upper limits of the space density are then used to provide constraints on the faint-end slope and the break absolute magnitude of the quasar luminosity function at z ∼ 5. We find that the quasar space density decreases gradually as a function of redshift at low luminosity (M1450 ∼ –23), being similar to the trend found for quasars with high luminosity (M1450 < –26). This result is consistent with the so-called downsizing evolution of quasars seen at lower redshifts. [ABSTRACT FROM AUTHOR]
Published: 2012
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34. HUBBLE SPACE TELESCOPE DISCOVERY OF A z = 3.9 MULTIPLY IMAGED GALAXY BEHIND THE COMPLEX CLUSTER LENS WARPS J1415.1+36 AT z = 1.026.

Author: Huang, X., Morokuma, T., Fakhouri, H. K., Aldering, G., Amanullah, R., Barbary, K., Brodwin, M., Connolly, N. V., Dawson, K. S., Doi, M., Faccioli, L., Fadeyev, V., Fruchter, A. S., Goldhaber, G., Gladders, M. D., Hennawi, J. F., Ihara, Y., Jee, M. J., Kowalski, M., and Konishi, K.
Published: 2009
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35. PROPERTIES OF TYPE II PLATEAU SUPERNOVA SNLS-04D2dc: MULTICOLOR LIGHT CURVES OF SHOCK BREAKOUT AND PLATEAU.

Author: Tominaga, N., Blinnikov, S., Baklanov, P., Morokuma, T., Nomoto, K., and Suzuki, T.
Published: 2009
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36. A New Determination of the High-Redshift Type Ia Supernova Rates with the Hubble Space Telescope Advanced Camera for Surveys.

Author: Kuznetsova, N., Barbary, K., Connolly, B., Kim, A. G., Pain, R., Roe, N. A., Aldering, G., Amanullah, R., Dawson, K., Doi, M., Fadeyev, V., Fruchter, A. S., Gibbons, R., Goldhaber, G., Goobar, A., Gude, A., Knop, R. A., Kowalski, M., Lidman, C., and Morokuma, T.
Published: 2008
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37. 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. J., Oh125, S. H., Ohme91, F., Oliver67, M., Oppermann8, P., Oram6, R. J., O'Reilly6, B., O'Shaughnessy112, R., Ottaway102, D. J., Ottens5, R. S., Overmier6, H., Owen71, B. J., Pai106, A., Pai48, S. A., Palamos59, J. R., Palashov107, O., Palliyaguru71, N., Palomba28, C., Pal Singh27, A., Pan73, H., Pankow82, C., Pannarale91, F., Pant48, B. C., Paoletti19, F., Paoli34, A., Papa8, M. A., 29, 16, Paris41, H. R., Parker6, W., Pascucci36, D., Pasqualetti34, A., Passaquieti18, R., Passuello19, D., Patricelli18, B., Patrick41, Z., Pearlstone36, B. L., Pedraza1, M., Pedurand66, R., Pekowsky35, L., Pele6, A., Penn126, S., Perreca1, A., Phelps36, M., Piccinni28, O., Pichot53, M., Piergiovanni57, F., Pierro87, V., Pillant34, G., Pinard66, L., Pinto87, I. M., Pitkin36, M., Poggiani18, R., Popolizio34, P., Post8, A., Powell36, J., Prasad14, J., Predoi91, V., Premachandra113, S. S., Prestegard83, T., Price1, L. R., Prijatelj34, M., Principe87, M., Privitera29, S., Prodi89, G. 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. 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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. 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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. N., Drlica-Wagner, A., Fong, W. -. F., Sevilla-Noarbe, I., Soares-Santos, M., The Dark Energy Survey, the Dark Energy Camera GW-EM Collaborations, Zhang, B. -. B., Wilson-Hodge, C. A., von Kienlin, A., Yu, H. -. F., Cohen-Tanugi, J., D’Ammando, F., de Palma, F., Gomez-Vargas, G. A., Pesce-Rollins, M., Saz Parkinson, P. M., D’Avanzo, P., D’Elia, V., Courvoisier, T. J. -. L., The INTEGRAL Collaboration, Van Sistine, A., The La Silla–QUEST Survey, Galloway, D. K., Don, Pollacco, Serra-Ricart, M., Johnston-Hollitt, M., F. Olivares E., Chen, T. -. W., Elias-Rosa, N., Le Guillou, L., Gal-Yam, A., O’Brien, P., The, Tarot, Zadko, Algerian National Observatory, C2pu, Collaboration, Milvang-Jensen, B., Gonzalez-Solares, E., Postigo, A. de U., High Energy Astrophys. & Astropart. 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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
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38. Observing cosmic-ray extensive air showers with a silicon imaging detector.

Author: Kawanomoto S, Koike M, Bradfield F, Fujii T, Komiyama Y, Miyazaki S, Morokuma T, Murayama H, Oguri M, and Terai T
Abstract: Extensive air showers induced from high-energy cosmic rays provide a window into understanding the most energetic phenomena in the universe. We present a new method for observing these showers using the silicon imaging detector Subaru Hyper Suprime-Cam (HSC). This method has the advantage of being able to measure individual secondary particles. When paired with a surface detector array, silicon imaging detectors like Subaru HSC will be useful for studying the properties of extensive air showers in detail. The following report outlines the first results of observing extensive air showers with Subaru HSC. The potential for reconstructing the incident direction of primary cosmic rays is demonstrated and possible interdisciplinary applications are discussed., (© 2023. Springer Nature Limited.)
Published: 2023
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39. Possible Earlier Diagnosis of Ulcerative Colitis-Associated Neoplasia: A Retrospective Analysis of Interval Cases during Surveillance.

Author: Hisabe T, Matsui T, Yamasaki K, Morokuma T, Aomi K, Yoshizawa N, Takatsu N, Yao K, Ueki T, Futami K, Tanabe H, and Iwashita A
Abstract: Background: Early detection of ulcerative colitis-associated neoplasia (UCAN) is often difficult. The aim of this study was to clarify the morphology of initial UCAN., Methods: White-light colonoscopy images obtained within the 2 years before UCAN diagnosis were retrospectively reviewed. The primary endpoint was the frequency of visible or invisible neoplasia on the endoscopic images before UCAN diagnosis. The secondary endpoints were comparisons of (1) visible or invisible neoplasia on initial endoscopic images of early-stage and advanced cancers, (2) the clinical backgrounds of patients in whom neoplasia was visible or invisible on initial endoscopic images, and (3) the clinical backgrounds of patients with distinct and indistinct UCAN borders., Results: Of the 27 UCAN lesions (11 early-stage; 16 advanced-stage), 25.9% ( n = 7) were initially visible and 74.1% ( n = 20) were invisible. The mean interval between the last surveillance colonoscopy and UCAN diagnosis was 14.5 ± 6.7 months. Of early-stage cancers, 18.2% ( n = 2) were visible and 81.8% ( n = 9) were invisible. Of advanced-stage cancers, 31.3% ( n = 5) were visible and 68.8% ( n = 11) were invisible. Invisible lesions were significantly more common in the rectum ( p = 0.011) and tended to be more common in patients with inflammation and left-sided colitis ( p = 0.084, p = 0.068, respectively). Patients with indistinct UCAN borders were significantly more likely to present with inflammation than those with distinct UCAN borders ( p = 0.021)., Conclusion: More careful surveillance is needed because rectum lesions and inflammation are difficult to identify as neoplasia even within the 2 years before a UCAN diagnosis.
Published: 2021
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40. A hybrid type Ia supernova with an early flash triggered by helium-shell detonation.

Author: Jiang JA, Doi M, Maeda K, Shigeyama T, Nomoto K, Yasuda N, Jha SW, Tanaka M, Morokuma T, Tominaga N, Ivezić Ž, Ruiz-Lapuente P, Stritzinger MD, Mazzali PA, Ashall C, Mould J, Baade D, Suzuki N, Connolly AJ, Patat F, Wang L, Yoachim P, Jones D, Furusawa H, and Miyazaki S
Abstract: Type Ia supernovae arise from the thermonuclear explosion of white-dwarf stars that have cores of carbon and oxygen. The uniformity of their light curves makes these supernovae powerful cosmological distance indicators, but there have long been debates about exactly how their explosion is triggered and what kind of companion stars are involved. For example, the recent detection of the early ultraviolet pulse of a peculiar, subluminous type Ia supernova has been claimed as evidence for an interaction between a red-giant or a main-sequence companion and ejecta from a white-dwarf explosion. Here we report observations of a prominent but red optical flash that appears about half a day after the explosion of a type Ia supernova. This supernova shows hybrid features of different supernova subclasses, namely a light curve that is typical of normal-brightness supernovae, but with strong titanium absorption, which is commonly seen in the spectra of subluminous ones. We argue that this early flash does not occur through previously suggested mechanisms such as the companion-ejecta interaction. Instead, our simulations show that it could occur through detonation of a thin helium shell either on a near-Chandrasekhar-mass white dwarf, or on a sub-Chandrasekhar-mass white dwarf merging with a less-massive white dwarf. Our finding provides evidence that one branch of previously proposed explosion models-the helium-ignition branch-does exist in nature, and that such a model may account for the explosions of white dwarfs in a mass range wider than previously supposed.
Published: 2017
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41. Retrospective Analysis of Growth Speed of 54 Lesions of Colitis-associated Colorectal Neoplasia.

Author: Yamasaki K, Matsui T, Hisabe T, Yano Y, Hirai F, Morokuma T, Iwao Y, Matsumoto T, Ohi H, Andoh A, Esaki M, Aoyagi K, Sugita A, Nakase H, Fujiya M, Higashi D, and Futami K
Subjects: Adult, Aged, Disease Progression, Female, Humans, Male, Middle Aged, Retrospective Studies, Tumor Burden, Young Adult, Colitis, Ulcerative pathology, Colorectal Neoplasms pathology, Precancerous Conditions pathology
Abstract: Aim: This study used a multicenter questionnaire survey to evaluate the morphology and progression of the initial lesion in cases of colitis-associated colorectal neoplasia (CRN)., Patients and Methods: Endoscopic images of lesions that had been definitively diagnosed as CRN by pathological examination were retrospectively reviewed., Results: This resulted in the identification of 54 initial lesions in 49 patients. The 54 initial lesions fell into the following categories: 22 endoscopically visible localized lesions consisting of 18 elevated lesions and 4 depressed lesions, as well as 32 lesions that were not endoscopically visible as localized and consisted of 20 active-phase mucosal lesions and 12 remission-phase mucosal lesions. Nineteen of the lesions eventually became advanced cancers, while 35 lesions eventually became early-stage cancers. The final lesions were 40 elevated lesions, 5 flat or depressed lesions and 9 stenotic lesions. The form of growth of the advanced cancers was progressive stenosis or increased elevation. For approximately 69% of the early-stage cancers, the growth form was increasing elevation or development of elevation. For 73.6% of the advanced cancers, the initial lesion underwent rapid growth and became advanced cancer within 3 years; they accounted for 25.9% of the total cancers. Approximately 40% of the initial lesions of CRN were endoscopically visible as localized lesions, while approximately 60% were judged to be inflammatory mucosal lesions., Conclusion: It will be necessary to proactively take biopsy inflammatory mucosal lesions in order to discover tumors early and periodic surveillance should be performed with the knowledge that tumors may grow very quickly., (Copyright© 2016 International Institute of Anticancer Research (Dr. John G. Delinassios), All rights reserved.)
Published: 2016

42. A galaxy at a redshift z = 6.96.

Author: Iye M, Ota K, Kashikawa N, Furusawa H, Hashimoto T, Hattori T, Matsuda Y, Morokuma T, Ouchi M, and Shimasaku K
Abstract: When galaxy formation started in the history of the Universe remains unclear. Studies of the cosmic microwave background indicate that the Universe, after initial cooling (following the Big Bang), was reheated and reionized by hot stars in newborn galaxies at a redshift in the range 6 < z < 14 (ref. 1). Though several candidate galaxies at redshift z > 7 have been identified photometrically, galaxies with spectroscopically confirmed redshifts have been confined to z < 6.6 (refs 4-8). Here we report a spectroscopic redshift of z = 6.96 (corresponding to just 750 Myr after the Big Bang) for a galaxy whose spectrum clearly shows Lyman-alpha emission at 9,682 A, indicating active star formation at a rate of approximately 10M(o) yr(-1), where M(o) is the mass of the Sun. This demonstrates that galaxy formation was under way when the Universe was only approximately 6 per cent of its present age. The number density of galaxies at z approximately 7 seems to be only 18-36 per cent of the density at z = 6.6.
Published: 2006
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