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1. Gravitational Waves and Gamma-Rays from a Binary Neutron Star Merger: GW170817 and GRB 170817A

Author: B. P. Abbott, R. Abbott, T. D. Abbott, F. Acernese, K. Ackley, C. Adams, T. Adams, P. Addesso, R. X. Adhikari, V. B. Adya, C. Affeldt, M. Afrough, B. Agarwal, M. Agathos, K. Agatsuma, N. Aggarwal, O. D. Aguiar, L. Aiello, A. Ain, P. Ajith, B. Allen, G. Allen, A. Allocca, M. A. Aloy, P. A. Altin, A. Amato, A. Ananyeva, S. B. Anderson, W. G. Anderson, S. V. Angelova, S. Antier, S. Appert, K. Arai, M. C. Araya, J. S. Areeda, N. Arnaud, K. G. Arun, S. Ascenzi, G. Ashton, M. Ast, S. M. Aston, P. Astone, D. V. Atallah, P. Aufmuth, C. Aulbert, K. AultONeal, C. Austin, A. Avila-Alvarez, S. Babak, P. Bacon, M. K. M. Bader, S. Bae, P. T. Baker, F. Baldaccini, G. Ballardin, S. W. Ballmer, S. Banagiri, J. C. Barayoga, S. E. Barclay, B. C. Barish, D. Barker, K. Barkett, F. Barone, B. Barr, L. Barsotti, M. Barsuglia, D. Barta, J. Bartlett, I. Bartos, R. Bassiri, A. Basti, J. C. Batch, M. Bawaj, J. C. Bayley, M. Bazzan, B. Bécsy, C. Beer, M. Bejger, I. Belahcene, A. S. Bell, B. K. Berger, G. Bergmann, J. J. Bero, C. P. L. Berry, D. Bersanetti, A. Bertolini, J. Betzwieser, S. Bhagwat, R. Bhandare, I. A. Bilenko, G. Billingsley, C. R. Billman, J. Birch, I. A. Birney, O. Birnholtz, S. Biscans, S. Biscoveanu, A. Bisht, M. Bitossi, C. Biwer, M. A. Bizouard, J. K. Blackburn, J. Blackman, C. D. Blair, D. G. Blair, R. M. Blair, S. Bloemen, O. Bock, N. Bode, M. Boer, G. Bogaert, A. Bohe, F. Bondu, E. Bonilla, R. Bonnand, B. A. Boom, R. Bork, V. Boschi, S. Bose, K. Bossie, Y. Bouffanais, A. Bozzi, C. Bradaschia, P. R. Brady, M. Branchesi, J. E. Brau, T. Briant, A. Brillet, M. Brinkmann, V. Brisson, P. Brockill, J. E. Broida, A. F. Brooks, D. A. Brown, D. D. Brown, S. Brunett, C. C. Buchanan, A. Buikema, T. Bulik, H. J. Bulten, A. Buonanno, D. Buskulic, C. Buy, R. L. Byer, M. Cabero, L. Cadonati, G. Cagnoli, C. Cahillane, J. Calderón Bustillo, T. A. Callister, E. Calloni, J. B. Camp, M. Canepa, P. Canizares, K. C. Cannon, H. Cao, J. Cao, C. D. Capano, E. Capocasa, F. Carbognani, S. Caride, M. F. Carney, J. Casanueva Diaz, C. Casentini, S. Caudill, M. Cavaglià, F. Cavalier, R. Cavalieri, G. Cella, C. B. Cepeda, P. Cerdá-Durán, G. Cerretani, E. Cesarini, S. J. Chamberlin, M. Chan, S. Chao, P. Charlton, E. Chase, E. Chassande-Mottin, D. Chatterjee, K. Chatziioannou, B. D. Cheeseboro, H. Y. Chen, X. Chen, Y. Chen, H.-P. Cheng, H. Chia, A. Chincarini, A. Chiummo, T. Chmiel, H. S. Cho, M. Cho, J. H. Chow, N. Christensen, Q. Chu, A. J. K. Chua, S. Chua, A. K. W. Chung, S. Chung, G. Ciani, R. Ciolfi, C. E. Cirelli, A. Cirone, F. Clara, J. A. Clark, P. Clearwater, F. Cleva, C. Cocchieri, E. Coccia, P.-F. Cohadon, D. Cohen, A. Colla, C. G. Collette, L. R. Cominsky, M. Constancio Jr., L. Conti, S. J. Cooper, P. Corban, T. R. Corbitt, I. Cordero-Carrión, K. R. Corley, N. Cornish, A. Corsi, S. Cortese, C. A. Costa, M. W. Coughlin, S. B. Coughlin, J.-P. Coulon, S. T. Countryman, P. Couvares, P. B. Covas, E. E. Cowan, D. M. Coward, M. J. Cowart, D. C. Coyne, R. Coyne, J. D. E. Creighton, T. D. Creighton, J. Cripe, S. G. Crowder, T. J. Cullen, A. Cumming, L. Cunningham, E. Cuoco, T. Dal Canton, G. Dálya, S. L. Danilishin, S. D’Antonio, K. Danzmann, A. Dasgupta, C. F. Da Silva Costa, V. Dattilo, I. Dave, M. Davier, D. Davis, E. J. Daw, B. Day, S. De, D. DeBra, J. Degallaix, M. De Laurentis, S. Deléglise, W. Del Pozzo, N. Demos, T. Denker, T. Dent, R. De Pietri, V. Dergachev, R. De Rosa, R. T. DeRosa, C. De Rossi, R. DeSalvo, O. de Varona, J. Devenson, S. Dhurandhar, M. C. Díaz, L. Di Fiore, M. Di Giovanni, T. Di Girolamo, A. Di Lieto, S. Di Pace, I. Di Palma, F. Di Renzo, Z. Doctor, V. Dolique, F. Donovan, K. L. Dooley, S. Doravari, I. Dorrington, R. Douglas, M. Dovale Álvarez, T. P. Downes, M. Drago, C. Dreissigacker, J. C. Driggers, Z. Du, M. Ducrot, P. Dupej, S. E. Dwyer, T. B. Edo, M. C. Edwards, A. Effler, H.-B. Eggenstein, P. Ehrens, J. Eichholz, S. S. Eikenberry, R. A. Eisenstein, R. C. Essick, D. Estevez, Z. B. Etienne, T. Etzel, M. Evans, T. M. Evans, M. Factourovich, V. Fafone, H. Fair, S. Fairhurst, X. Fan, S. Farinon, B. Farr, W. M. Farr, E. J. Fauchon-Jones, M. Favata, M. Fays, C. Fee, H. Fehrmann, J. Feicht, M. M. Fejer, A. Fernandez-Galiana, I. Ferrante, E. C. Ferreira, F. Ferrini, F. Fidecaro, D. Finstad, I. Fiori, D. Fiorucci, M. Fishbach, R. P. Fisher, M. Fitz-Axen, R. Flaminio, M. Fletcher, H. Fong, J. A. Font, P. W. F. Forsyth, S. S. Forsyth, J.-D. Fournier, S. Frasca, F. Frasconi, Z. Frei, A. Freise, R. Frey, V. Frey, E. M. Fries, P. Fritschel, V. V. Frolov, P. Fulda, M. Fyffe, H. Gabbard, B. U. Gadre, S. M. Gaebel, J. R. Gair, L. Gammaitoni, M. R. Ganija, S. G. Gaonkar, C. Garcia-Quiros, F. Garufi, B. Gateley, S. Gaudio, G. Gaur, V. Gayathri, N. Gehrels, G. Gemme, E. Genin, A. Gennai, D. George, J. George, L. Gergely, V. Germain, S. Ghonge, Abhirup Ghosh, Archisman Ghosh, S. Ghosh, J. A. Giaime, K. D. Giardina, A. Giazotto, K. Gill, L. Glover, E. Goetz, R. Goetz, S. Gomes, B. Goncharov, G. González, J. M. Gonzalez Castro, A. Gopakumar, M. L. Gorodetsky, S. E. Gossan, M. Gosselin, R. Gouaty, A. Grado, C. Graef, M. Granata, A. Grant, S. Gras, C. Gray, G. Greco, A. C. Green, E. M. Gretarsson, P. Groot, H. Grote, S. Grunewald, P. Gruning, G. M. Guidi, X. Guo, A. Gupta, M. K. Gupta, K. E. Gushwa, E. K. Gustafson, R. Gustafson, O. Halim, B. R. Hall, E. D. Hall, E. Z. Hamilton, G. Hammond, M. Haney, M. M. Hanke, J. Hanks, C. Hanna, M. D. Hannam, O. A. Hannuksela, J. Hanson, T. Hardwick, J. Harms, G. M. Harry, I. W. Harry, M. J. Hart, C.-J. Haster, K. Haughian, J. Healy, A. Heidmann, M. C. Heintze, H. Heitmann, P. Hello, G. Hemming, M. Hendry, I. S. Heng, J. Hennig, A. W. Heptonstall, M. Heurs, S. Hild, T. Hinderer, D. Hoak, D. Hofman, K. Holt, D. E. Holz, P. Hopkins, C. Horst, J. Hough, E. A. Houston, E. J. Howell, A. Hreibi, Y. M. Hu, E. A. Huerta, D. Huet, B. Hughey, S. Husa, S. H. Huttner, T. Huynh-Dinh, N. Indik, R. Inta, G. Intini, H. N. Isa, J.-M. Isac, M. Isi, B. R. Iyer, K. Izumi, T. Jacqmin, K. Jani, P. Jaranowski, S. Jawahar, F. Jiménez-Forteza, W. W. Johnson, N. K. Johnson-McDaniel, D. I. Jones, R. Jones, R. J. G. Jonker, L. Ju, J. Junker, C. V. Kalaghatgi, V. Kalogera, B. Kamai, S. Kandhasamy, G. Kang, J. B. Kanner, S. J. Kapadia, S. Karki, K. S. Karvinen, M. Kasprzack, W. Kastaun, M. Katolik, E. Katsavounidis, W. Katzman, S. Kaufer, K. Kawabe, F. Kéfélian, D. Keitel, A. J. Kemball, R. Kennedy, C. Kent, J. S. Key, F. Y. Khalili, I. Khan, S. Khan, Z. Khan, E. A. Khazanov, N. Kijbunchoo, Chunglee Kim, J. C. Kim, K. Kim, W. Kim, W. S. Kim, Y.-M. Kim, S. J. Kimbrell, E. J. King, P. J. King, M. Kinley-Hanlon, R. Kirchhoff, J. S. Kissel, L. Kleybolte, S. Klimenko, T. D. Knowles, P. Koch, S. M. Koehlenbeck, S. Koley, V. Kondrashov, A. Kontos, M. Korobko, W. Z. Korth, I. Kowalska, D. B. Kozak, C. Krämer, V. Kringel, B. Krishnan, A. Królak, G. Kuehn, P. Kumar, R. Kumar, S. Kumar, L. Kuo, A. Kutynia, S. Kwang, B. D. Lackey, K. H. Lai, M. Landry, R. N. Lang, J. Lange, B. Lantz, R. K. Lanza, A. Lartaux-Vollard, P. D. Lasky, M. Laxen, A. Lazzarini, C. Lazzaro, P. Leaci, S. Leavey, C. H. Lee, H. K. Lee, H. M. Lee, H. W. Lee, K. Lee, J. Lehmann, A. Lenon, M. Leonardi, N. Leroy, N. Letendre, Y. Levin, T. G. F. Li, S. D. Linker, T. B. Littenberg, J. Liu, R. K. L. Lo, N. A. Lockerbie, L. T. London, J. E. Lord, M. Lorenzini, V. Loriette, M. Lormand, G. Losurdo, J. D. Lough, C. O. Lousto, G. Lovelace, H. Lück, D. Lumaca, A. P. Lundgren, R. Lynch, Y. Ma, R. Macas, S. Macfoy, B. Machenschalk, M. MacInnis, D. M. Macleod, I. Magaña Hernandez, F. Magaña-Sandoval, L. Magaña Zertuche, R. M. Magee, E. Majorana, I. Maksimovic, N. Man, V. Mandic, V. Mangano, G. L. Mansell, M. Manske, M. Mantovani, F. Marchesoni, F. Marion, S. Márka, Z. Márka, C. Markakis, A. S. Markosyan, A. Markowitz, E. Maros, A. Marquina, F. Martelli, L. Martellini, I. W. Martin, R. M. Martin, D. V. Martynov, K. Mason, E. Massera, A. Masserot, T. J. Massinger, M. Masso-Reid, S. Mastrogiovanni, A. Matas, F. Matichard, L. Matone, N. Mavalvala, N. Mazumder, R. McCarthy, D. E. McClelland, S. McCormick, L. McCuller, S. C. McGuire, G. McIntyre, J. McIver, D. J. McManus, L. McNeill, T. McRae, S. T. McWilliams, D. Meacher, G. D. Meadors, M. Mehmet, J. Meidam, E. Mejuto-Villa, A. Melatos, G. Mendell, R. A. Mercer, E. L. Merilh, M. Merzougui, S. Meshkov, C. Messenger, C. Messick, R. Metzdorff, P. M. Meyers, H. Miao, C. Michel, H. Middleton, E. E. Mikhailov, L. Milano, A. L. Miller, B. B. Miller, J. Miller, M. Millhouse, M. C. Milovich-Goff, O. Minazzoli, Y. Minenkov, J. Ming, C. Mishra, S. Mitra, V. P. Mitrofanov, G. Mitselmakher, R. Mittleman, D. Moffa, A. Moggi, K. Mogushi, M. Mohan, S. R. P. Mohapatra, M. Montani, C. J. Moore, D. Moraru, G. Moreno, S. R. Morriss, B. Mours, C. M. Mow-Lowry, G. Mueller, A. W. Muir, Arunava Mukherjee, D. Mukherjee, S. Mukherjee, N. Mukund, A. Mullavey, J. Munch, E. A. Muñiz, M. Muratore, P. G. Murray, K. Napier, I. Nardecchia, L. Naticchioni, R. K. Nayak, J. Neilson, G. Nelemans, T. J. N. Nelson, M. Nery, A. Neunzert, L. Nevin, J. M. Newport, G. Newton, K. K. Y. Ng, T. T. Nguyen, D. Nichols, A. B. Nielsen, S. Nissanke, A. Nitz, A. Noack, F. Nocera, D. Nolting, C. North, L. K. Nuttall, J. Oberling, G. D. O’Dea, G. H. Ogin, J. J. Oh, S. H. Oh, F. Ohme, M. A. Okada, M. Oliver, P. Oppermann, Richard J. Oram, B. O’Reilly, R. Ormiston, L. F. Ortega, R. O’Shaughnessy, S. Ossokine, D. J. Ottaway, H. Overmier, B. J. Owen, A. E. Pace, J. Page, M. A. Page, A. Pai, S. A. Pai, J. R. Palamos, O. Palashov, C. Palomba, A. Pal-Singh, Howard Pan, Huang-Wei Pan, B. Pang, P. T. H. Pang, C. Pankow, F. Pannarale, B. C. Pant, F. Paoletti, A. Paoli, M. A. Papa, A. Parida, W. Parker, D. Pascucci, A. Pasqualetti, R. Passaquieti, D. Passuello, M. Patil, B. Patricelli, B. L. Pearlstone, M. Pedraza, R. Pedurand, L. Pekowsky, A. Pele, S. Penn, C. J. Perez, A. Perreca, L. M. Perri, H. P. Pfeiffer, M. Phelps, O. J. Piccinni, M. Pichot, F. Piergiovanni, V. Pierro, G. Pillant, L. Pinard, I. M. Pinto, M. Pirello, M. Pitkin, M. Poe, R. Poggiani, P. Popolizio, E. K. Porter, A. Post, J. Powell, J. Prasad, J. W. W. Pratt, G. Pratten, V. Predoi, T. Prestegard, M. Prijatelj, M. Principe, S. Privitera, G. A. Prodi, L. G. Prokhorov, O. Puncken, M. Punturo, P. Puppo, M. Pürrer, H. Qi, V. Quetschke, E. A. Quintero, R. Quitzow-James, F. J. Raab, D. S. Rabeling, H. Radkins, P. Raffai, S. Raja, C. Rajan, B. Rajbhandari, M. Rakhmanov, K. E. Ramirez, A. Ramos-Buades, P. Rapagnani, V. Raymond, M. Razzano, J. Read, T. Regimbau, L. Rei, S. Reid, D. H. Reitze, W. Ren, S. D. Reyes, F. Ricci, P. M. Ricker, S. Rieger, K. Riles, M. Rizzo, N. A. Robertson, R. Robie, F. Robinet, A. Rocchi, L. Rolland, J. G. Rollins, V. J. Roma, R. Romano, C. L. Romel, J. H. Romie, D. Rosińska, M. P. Ross, S. Rowan, A. Rüdiger, P. Ruggi, G. Rutins, K. Ryan, S. Sachdev, T. Sadecki, L. Sadeghian, M. Sakellariadou, L. Salconi, M. Saleem, F. Salemi, A. Samajdar, L. Sammut, L. M. Sampson, E. J. Sanchez, L. E. Sanchez, N. Sanchis-Gual, V. Sandberg, J. R. Sanders, B. Sassolas, B. S. Sathyaprakash, P. R. Saulson, O. Sauter, R. L. Savage, A. Sawadsky, P. Schale, M. Scheel, J. Scheuer, J. Schmidt, P. Schmidt, R. Schnabel, R. M. S. Schofield, A. Schönbeck, E. Schreiber, D. Schuette, B. W. Schulte, B. F. Schutz, S. G. Schwalbe, J. Scott, S. M. Scott, E. Seidel, D. Sellers, A. S. Sengupta, D. Sentenac, V. Sequino, A. Sergeev, D. A. Shaddock, T. J. Shaffer, A. A. Shah, M. S. Shahriar, M. B. Shaner, L. Shao, B. Shapiro, P. Shawhan, A. Sheperd, D. H. Shoemaker, D. M. Shoemaker, K. Siellez, X. Siemens, M. Sieniawska, D. Sigg, A. D. Silva, L. P. Singer, A. Singh, A. Singhal, A. M. Sintes, B. J. J. Slagmolen, B. Smith, J. R. Smith, R. J. E. Smith, S. Somala, E. J. Son, J. A. Sonnenberg, B. Sorazu, F. Sorrentino, T. Souradeep, A. P. Spencer, A. K. Srivastava, K. Staats, A. Staley, M. Steinke, J. Steinlechner, S. Steinlechner, D. Steinmeyer, S. P. Stevenson, R. Stone, D. J. Stops, K. A. Strain, G. Stratta, S. E. Strigin, A. Strunk, R. Sturani, A. L. Stuver, T. Z. Summerscales, L. Sun, S. Sunil, J. Suresh, P. J. Sutton, B. L. Swinkels, M. J. Szczepańczyk, M. Tacca, S. C. Tait, C. Talbot, D. Talukder, D. B. Tanner, M. Tápai, A. Taracchini, J. D. Tasson, J. A. Taylor, R. Taylor, S. V. Tewari, T. Theeg, F. Thies, E. G. Thomas, M. Thomas, P. Thomas, K. A. Thorne, K. S. Thorne, E. Thrane, S. Tiwari, V. Tiwari, K. V. Tokmakov, K. Toland, M. Tonelli, Z. Tornasi, A. Torres-Forné, C. I. Torrie, D. Töyrä, F. Travasso, G. Traylor, J. Trinastic, M. C. Tringali, L. Trozzo, K. W. Tsang, M. Tse, R. Tso, L. Tsukada, D. Tsuna, D. Tuyenbayev, K. Ueno, D. Ugolini, C. S. Unnikrishnan, A. L. Urban, S. A. Usman, H. Vahlbruch, G. Vajente, G. Valdes, N. van Bakel, M. van Beuzekom, J. F. J. van den Brand, C. Van Den Broeck, D. C. Vander-Hyde, L. van der Schaaf, J. V. van Heijningen, A. A. van Veggel, M. Vardaro, V. Varma, S. Vass, M. Vasúth, A. Vecchio, G. Vedovato, J. Veitch, P. J. Veitch, K. Venkateswara, G. Venugopalan, D. Verkindt, F. Vetrano, A. Viceré, A. D. Viets, S. Vinciguerra, D. J. Vine, J.-Y. Vinet, S. Vitale, T. Vo, H. Vocca, C. Vorvick, S. P. Vyatchanin, A. R. Wade, L. E. Wade, M. Wade, R. Walet, M. Walker, L. Wallace, S. Walsh, G. Wang, H. Wang, J. Z. Wang, W. H. Wang, Y. F. Wang, R. L. Ward, J. Warner, M. Was, J. Watchi, B. Weaver, L.-W. Wei, M. Weinert, A. J. Weinstein, R. Weiss, L. Wen, E. K. Wessel, P. Weßels, J. Westerweck, T. Westphal, K. Wette, J. T. Whelan, S. E. Whitcomb, B. F. Whiting, C. Whittle, D. Wilken, D. Williams, R. D. Williams, A. R. Williamson, J. L. Willis, B. Willke, M. H. Wimmer, W. Winkler, C. C. Wipf, H. Wittel, G. Woan, J. Woehler, J. Wofford, K. W. K. Wong, J. Worden, J. L. Wright, D. S. Wu, D. M. Wysocki, S. Xiao, H. Yamamoto, C. C. Yancey, L. Yang, M. J. Yap, M. Yazback, Hang Yu, Haocun Yu, M. Yvert, A. Zadrożny, M. Zanolin, T. Zelenova, J.-P. Zendri, M. Zevin, L. Zhang, M. Zhang, T. Zhang, Y.-H. Zhang, C. Zhao, M. Zhou, Z. Zhou, S. J. Zhu, X. J. Zhu, A. B. Zimmerman, M. E. Zucker, J. Zweizig, (LIGO Scientific Collaboration and Virgo Collaboration), E. Burns, P. Veres, D. Kocevski, J. Racusin, A. Goldstein, V. Connaughton, M. S. Briggs, L. Blackburn, R. Hamburg, C. M. Hui, A. von Kienlin, J. McEnery, R. D. Preece, C. A. Wilson-Hodge, E. Bissaldi, W. H. Cleveland, M. H. Gibby, M. M. Giles, R. M. Kippen, S. McBreen, C. A. Meegan, W. S. Paciesas, S. Poolakkil, O. J. Roberts, M. Stanbro, (Fermi Gamma-ray Burst Monitor), V. Savchenko, C. Ferrigno, E. Kuulkers, A. Bazzano, E. Bozzo, S. Brandt, J. Chenevez, T. J.-L. Courvoisier, R. Diehl, A. Domingo, L. Hanlon, E. Jourdain, P. Laurent, F. Lebrun, A. Lutovinov, S. Mereghetti, L. Natalucci, J. Rodi, J.-P. Roques, R. Sunyaev, P. Ubertini, and (INTEGRAL)
Subjects: binaries: close, gamma-ray burst: general, gravitational waves, Astrophysics, QB460-466
Abstract: On 2017 August 17, the gravitational-wave event GW170817 was observed by the Advanced LIGO and Virgo detectors, and the gamma-ray burst (GRB) GRB 170817A was observed independently by the Fermi Gamma-ray Burst Monitor, and the Anti-Coincidence Shield for the Spectrometer for the International Gamma-Ray Astrophysics Laboratory . The probability of the near-simultaneous temporal and spatial observation of GRB 170817A and GW170817 occurring by chance is $5.0\times {10}^{-8}$ . We therefore confirm binary neutron star mergers as a progenitor of short GRBs. The association of GW170817 and GRB 170817A provides new insight into fundamental physics and the origin of short GRBs. We use the observed time delay of $(+1.74\pm 0.05)\,{\rm{s}}$ between GRB 170817A and GW170817 to: (i) constrain the difference between the speed of gravity and the speed of light to be between $-3\times {10}^{-15}$ and $+7\times {10}^{-16}$ times the speed of light, (ii) place new bounds on the violation of Lorentz invariance, (iii) present a new test of the equivalence principle by constraining the Shapiro delay between gravitational and electromagnetic radiation. We also use the time delay to constrain the size and bulk Lorentz factor of the region emitting the gamma-rays. GRB 170817A is the closest short GRB with a known distance, but is between 2 and 6 orders of magnitude less energetic than other bursts with measured redshift. A new generation of gamma-ray detectors, and subthreshold searches in existing detectors, will be essential to detect similar short bursts at greater distances. Finally, we predict a joint detection rate for the Fermi Gamma-ray Burst Monitor and the Advanced LIGO and Virgo detectors of 0.1–1.4 per year during the 2018–2019 observing run and 0.3–1.7 per year at design sensitivity.
Published: 2017
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2. INTEGRAL search for GW counterparts and the GRB170817A/GW170817 detection

Author: Angela Bazzano, Roland Diehl, Sl Brandt, Lorenzo Natalucci, T. J. L. Courvoisier, P. Laurent, Jean-Pierre Roques, R. A. Sunyaev, Francois Lebrun, J. Rodi, Jérôme Chenevez, Elisabeth Jourdain, Lorraine Hanlon, Pietro Ubertini, E. Kuulkers, A. von Kienlin, Antonio Martin-Carrillo, Carlo Ferrigno, V. G. Savchenko, Sandro Mereghetti, Enrico Bozzo, A. A. Lutovinov, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), 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), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, and 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)
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Gamma ray counterpart, Astrophysics, Kilonova, Magnetar, 01 natural sciences, Gravitational waves, GW170817, 03 medical and health sciences, 0103 physical sciences, 010303 astronomy & astrophysics, General Environmental Science, Physics, 0303 health sciences, GRB170817A, Gravitational wave, Neutron star inspiral, LIGO, Afterglow, Neutron star, 030301 anatomy & morphology, [SDU]Sciences of the Universe [physics], General Earth and Planetary Sciences, General Agricultural and Biological Sciences, Gamma-ray burst, Fermi Gamma-ray Space Telescope
Abstract: International audience; The INTernational Gamma-ray Astrophysics Laboratory (INTEGRAL) has detected the Short Gamma-Ray Burst (SGRB), GRB170817A with a signal-to-noise ratio of 4.6 and demonstrated its association with the binary neutron star merging event GW170817 detected by the LIGO and Virgo gravitational wave observatories. The association was immediately evident due to the timing and positional coincidence of this event with the initial error box, derived from gravitational wave (GW) measurements and the contemporaneous detection of a similar gamma-ray signal by Fermi/GBM. This SGRB was detected by the INTEGRAL SPI ACS about 1.7 s after the end of the GW emission, with a fluence of (1.4 ±0.4 ) ×10-7ergcm-2 in the 75-2000 keV energy range. After the serendipitous detection of the short prompt GRB, INTEGRAL continued the planned observation for about 20 h, and then performed a targeted follow-up ToO observation lasting several days. This ToO observation provided a stringent upper limit on any electromagnetic signal in a very broad energy range, from 3 keV to 8 MeV, in particular constraining the soft gamma-ray afterglow flux to 1ergcm-2s-1 in the range 80-300 keV. Exploiting the unique capabilities of INTEGRAL, we constrained the gamma-ray line emission intensity from radioactive decays expected to be the principal source of the energy behind a kilonova event following a NS-NS coalescence. Finally, we put a stringent upper limit on any delayed bursting activity, for example, from a newly formed magnetar. The INTEGRAL prompt detection and the subsequent continuous observations at all wavelengths have provided important constraints on the high energy emission of the resulting kilonova and the post inspiral object: NS, BH, or a new exotic object.
Published: 2019
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3. INTEGRAL follow-up of the gravitational wave events

Author: Alexander A. Lutovinov, Enrico Bozzo, V. G. Savchenko, T. J. L. Courvoisier, A. Domingo, Roland Diehl, E. Jourdain, Søren Brandt, A. Martin-Carillo, J. P. Roques, James Rodi, Sandro Mereghetti, Francois Lebrun, Jérôme Chenevez, A. von Kienlin, Carlo Ferrigno, Lorraine Hanlon, E. Kuulkers, Angela Bazzano, P. Laurent, Lorenzo Natalucci, P. Ubertini, R. A. Sunyaev, 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), 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), Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), 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, 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), 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), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Université de 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), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)
Subjects: 0209 industrial biotechnology, satellite: Planck, Astrophysics::High Energy Astrophysical Phenomena, Measure (physics), Orbital eccentricity, 02 engineering and technology, Astrophysics, gamma ray: burst, gravitational radiation: direct detection, 7. Clean energy, localization, electromagnetic field: production, 020901 industrial engineering & automation, Binary black hole, 0202 electrical engineering, electronic engineering, information engineering, Physics, Spectrometer, Gravitational wave, Astrophysics::Instrumentation and Methods for Astrophysics, gravitational radiation, LIGO, Neutron star, gravitational radiation: emission, 020201 artificial intelligence & image processing, Gamma-ray burst, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: International audience; We use observations of the INTErnational Gamma-Ray Astrophysics Laboratory (INTEGRAL) to search for gamma-ray and hard X-ray emission associated with the gravitational wave events discovered during the first and the second scientific runs of Advanced LIGO and Advanced Virgo. The highly eccentric orbit of INTEGRAL ensures high duty cycle, long-term stable background, and unobstructed view of nearly the entire sky. This enables us to use a combination of INTEGRAL instruments (SPectrometer onboard INTEGRAL - Anti-Coincidence Shield (SPI-ACS), Imager on Board the INTEGRAL Satellite (IBIS), and IBIS/Veto) to search for a hard X-ray electromagnetic signal in the full high-probability sky region for almost every single LIGO trigger. INTEGRAL observations of the binary black hole (BBH) mergers GW150914, LVT151012, GW170104, and GW170814 allowes to constrain the fraction of the energy promptly released in gamma-rays in 75 keV - 2 MeV energy range in the direction of the observer down to as little as one millionth of the gravitational wave energy, in the majority of the localization region. Moreover, in the case of LVT151012 INTEGRAL high-energy imaging instruments, IBIS, SPectrometer onboard INTEGRAL (SPI), and Joint European X-Ray Monitor (JEM-X), provided the unique opportunity to search also for long-lasting electromagnetic counterparts of this event over 3 decades in energy, from 5 keV to 8 MeV. Finally, we discuss the INTEGRAL detection of the short gamma-ray burst GRB 170817A (discovered by Fermi-Gamma-ray Burst Monitor (GBM)) with a signal-to-noise ratio of 4.6, and, for the first time, its association with the gravitational waves (GWs) from binary neutron star (BNS) merging event GW170817 detected by the LIGO and Virgo observatories. The significance of association between the gamma-ray burst observed by INTEGRAL and GW170817 is 3.2 σ, while the association between the Fermi-GBM and INTEGRAL detections is 4.2 σ. GRB 170817A was detected by the SPI-ACS instrument about 2 s after the end of the gravitational wave event. We measure a fluence of 1.4±0.4±0.6×10−7 erg cm−2 (75–2000 keV), where, respectively, the statistical error is given at the 1 σ confidence level, and the systematic error corresponds to the uncertainty in the spectral model and instrument response.
Published: 2017
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4. X-ray variability time scales in active galactic nuclei

Author: W. Ishibashi and T. J. L. Courvoisier
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Active galactic nucleus, Astrophysics::High Energy Astrophysical Phenomena, X-ray, FOS: Physical sciences, Spectral density, Astronomy and Astrophysics, Astrophysics, Accretion (astrophysics), Accretion rate, Wavelength, Space and Planetary Science, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: X-ray variability in Active Galactic Nuclei (AGN) is commonly analysed in terms of the Power Spectral Density (PSD). The break observed in the power spectrum can be interpreted as a characteristic X-ray variability time scale. Here we study variability properties within the framework of clumpy accretion flows, in which shocks between accreting elements account for the UV and X-ray emissions. We derive a characteristic X-ray time scale, $\tau_{X}$, and compare it with the measured PSD break time scale, $T_{B}$. A quite good agreement is found in both magnitude and trend. In particular, the model dependence on black hole mass and accretion rate precisely reproduces the empirical relation obtained by McHardy et al. (2006). We suggest a possible physical interpretation of the break time scale and briefly discuss the related aspects of optical/UV variability and correlations between different wavelengths., Comment: 6 pages, 1 figure, accepted for publication in Astronomy and Astrophysics
Published: 2009
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5. Hard X-ray variability of active galactic nuclei

Author: T. J. L. Courvoisier, George A. Wendt, Volker Beckmann, Simona Soldi, J. Tueller, Scott Barthelmy, and N. Gehrels
Subjects: Physics, Active galactic nucleus, Electromagnetic spectrum, Astrophysics::High Energy Astrophysical Phenomena, X-ray, Flux, Sigma, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy, Luminosity, Space and Planetary Science, Blazar, Astrophysics::Galaxy Astrophysics
Abstract: Aims: Active Galactic Nuclei are known to be variable throughout the electromagnetic spectrum. An energy domain poorly studied in this respect is the hard X-ray range above 20 keV. Methods: The first 9 months of the Swift/BAT all-sky survey are used to study the 14 - 195 keV variability of the 44 brightest AGN. The sources have been selected due to their detection significance of >10 sigma. We tested the variability using a maximum likelihood estimator and by analysing the structure function. Results: Probing different time scales, it appears that the absorbed AGN are more variable than the unabsorbed ones. The same applies for the comparison of Seyfert 2 and Seyfert 1 objects. As expected the blazars show stronger variability. 15% of the non-blazar AGN show variability of >20% compared to the average flux on time scales of 20 days, and 30% show at least 10% flux variation. All the non-blazar AGN which show strong variability are low-luminosity objects with L(14-195 keV) < 1E44 erg/sec. Conclusions: Concerning the variability pattern, there is a tendency of unabsorbed or type 1 galaxies being less variable than the absorbed or type 2 objects at hardest X-rays. A more solid anti-correlation is found between variability and luminosity, which has been previously observed in soft X-rays, in the UV, and in the optical domain.
Published: 2007
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6. Unveiling the Nature of IGR J17497-2821 Using X-Ray and Near-Infrared Observations

Author: Sylvain Chaty, Ruben Farinelli, Jörn Wilms, A. Paizis, Michael A. Nowak, Pietro Ubertini, Jerome Rodriguez, K. Ebisawa, T. J. L. Courvoisier, and M. Del Santo
Subjects: Physics, Black hole, X-Rays: Binaries, Space and Planetary Science, Red giant, stars: individual (IGR J17497-2821), Near-infrared spectroscopy, X-ray, X-ray binary, Stars: Binaries: Close, Astronomy and Astrophysics, Astrophysics
Abstract: Accepted: 2007-01-30, 資料番号: SA1000584000
Published: 2007
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7. The application of slim disk models to ULX: The case of M33 X-8

Author: Paola Grandi, T. Kawaguchi, N. Cappelluti, T. J. L. Courvoisier, Giuseppe Malaguti, G. Di Cocco, J. Rodriguez, Luis C. Ho, Luigi Foschini, Ken Ebisawa, Giorgio G. C. Palumbo, Foschini L., Ebisawa K., Kawaguchi T., Cappelluti N., Grandi P., Malaguti G., Rodriguez J., Courvoisier T. J.-L., di Cocco G., Ho L. C., and Palumbo G. G. C.
Subjects: Physics, Atmospheric Science, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Aerospace Engineering, Binary number, Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Black hole, Geophysics, Space and Planetary Science, General Earth and Planetary Sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: 著者人数：11名, Accepted: 2005-06-13, 資料番号: SA1000579000
Published: 2006

8. INTEGRAL detection of hard X-rays from NGC 6334: nonthermal emission from colliding winds or an AGN?

Author: A. M. Bykov, A. M. Krassilchtchikov, Yu. A. Uvarov, F. Lebrun, M. Renaud, R. Terrier, H. Bloemen, B. McBreen, T. J.-L. Courvoisier, M. Yu. Gustov, W. Hermsen, J.-C. Leyder, T. A. Lozinskaya, G. Rauw, J.-P. Swings, 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), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), INTEGRAL, 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), 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), and High Energy Astrophys. & Astropart. Phys (API, FNWI)
Subjects: Photon, 010504 meteorology & atmospheric sciences, Field (physics), Infrared, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Gamma rays: observations, Star Forming Regions, 01 natural sciences, Spectral line, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Supernova remnant, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, individual: NGC 6334, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], biology, Astrophysics (astro-ph), Astronomy and Astrophysics, biology.organism_classification, Acis, Stars, Space and Planetary Science, Hard X-rays, X rays: ISM
Abstract: We report the detection of hard X-ray emission from the field of the star-forming region NGC 6334 with the the International Gamma-Ray Astrophysics Laboratory INTEGRAL. The JEM-X monitor and ISGRI imager aboard INTEGRAL and Chandra ACIS imager were used to construct 3-80 keV images and spectra of NGC 6334. The 3-10 keV and 10-35 keV images made with JEM-X show a complex structure of extended emission from NGC 6334. The ISGRI source detected in the energy ranges 20-40 keV and 40-80 keV coincides with the NGC 6334 ridge. The 20-60 keV flux from the source is (1.8+-0.37)*10(-11) erg cm(-2) s(-1). Spectral analysis of the source revealed a hard power-law component with a photon index about 1. The observed X-ray fluxes are in agreement with extrapolations of X-ray imaging observations of NGC 6334 by Chandra ACIS and ASCA GIS. The X-ray data are consistent with two very different physical models. A probable scenario is emission from a heavily absorbed, compact and hard Chandra source that is associated with the AGN candidate radio source NGC 6334B. Another possible model is the extended Chandra source of nonthermal emission from NGC 6334 that can also account for the hard X-ray emission observed by INTEGRAL. The origin of the emission in this scenario is due to electron acceleration in energetic outflows from massive early type stars. The possibility of emission from a young supernova remnant, as suggested by earlier infrared observations of NGC 6334, is constrained by the non-detection of 44Ti lines., 8 pages, 8 figures, Astronomy and Astrophysics (in press)
Published: 2006
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9. Cascades of shocks in active galactic nuclei and their radiation

Author: T. J. L. Courvoisier and Marc Türler
Subjects: Physics, Active galactic nucleus, Astrophysics::High Energy Astrophysical Phenomena, Central object, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Spectral domain, Quasar, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Radiation, Accretion (astrophysics), Galaxy, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We discuss accretion flows on massive black holes in which different elements of the flow (clumps) have velocities that may differ substantially. We estimate the consequence of collisions between these clumps as they come close to the central object and calculate the resulting radiation. We show that this radiation is similar to that observed in the optical to X-ray spectral domain in Seyfert galaxies and quasars. We also show that the large scale accretion is likely to be clumpy when arriving in the active region and that the clumps keep their identity between collisions., Accepted in A+A, 8 pages, 2 figures
Published: 2005
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10. Chandra observations of the peculiar X-ray transient IGR J16358-4726

Author: Andrew J. King, P. M. Woods, Chryssa Kouveliotou, Allyn F. Tennant, S. K. Patel, M. H. Finger, P. Ubertini, T. J. L. Courvoisier, C. Winkler, M. van der Klis, and Stefanie Wachter
Subjects: Physics, Nuclear and High Energy Physics, X-ray transient, Astrophysics::High Energy Astrophysical Phenomena, Astronomy, Flux, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Orbital period, Atomic and Molecular Physics, and Optics, Spectral line, Luminosity, Neutron star, Pulsar, Low Mass
Abstract: The new transient IGR J16358-4726 was discovered on 2003 March 19 with INTEGRAL. We detected the source serendipitously during our 2003 March 24 observation of SGR 1627 – 41 with the CHANDRA X-ray Observatory at the 1.7 × 10−10 ergs s−1 cm−2 flux level (2–10 keV) with a very high absorption column (NH=3.3×1023 cm−2) and a hard power law spectrum of photon index 0.5(1). We discovered a very strong flux modulation with a period of 5880(50) s and peak-to-peak pulse fraction of 70(6) % (2–10 keV), clearly visible in the x-ray data. The nature, however, of IGR 16357-4726 remains unresolved. Most likely, we are looking at a galactic binary neutron star system as evidenced by the detection of rest frame fluorescence line emission from neutral Fe K (6.4 keV) in the Chandra spectrum. If the detected modulation is a spin period, this transient is a new kind of object, belonging to a class of very hard transients recently revealed with the unique INTEGRAL capabilities. The only neutron star systems known with similar spin periods are low luminosity persistent wind-fed pulsars, which exhibit very soft X-ray spectra. If this is an orbital period, then the system could be a compact Low Mass X-ray Binary.
Published: 2004
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11. A possible feature of thermal matter in relativistic jets of radio-loud quasars

Author: Ruediger Staubert, Jian-Min Wang, and T. J.-L. Courvoisier
Subjects: Physics, Jet (fluid), Photon, Astrophysics::High Energy Astrophysical Phenomena, Metallicity, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Quasar, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Luminosity, Astrophysical jet, Space and Planetary Science, Equivalent width, Astrophysics::Galaxy Astrophysics, Line (formation)
Abstract: It has been suggested that relativistic jets in quasars may contain a considerable amount of thermal matter. In this paper, we explore the possibility that the K-alpha line from the thermal matter may appear at tens of keV due to a high Doppler blue-shift. In the jet comoving frame, the energy density of photons originally emitted by the accretion disk and reflected off the broad line region clouds dominates over that of photons of other origin. We discuss the photoionization states of the thermal matter and find that the irons elements are neutral. The high metallicity in quasars enhances the possibility to detect the thermal matter in the relativistic jet in some radio-loud quasars. A highly Doppler blue-shifted K-alpha line may be detected. We make a rediction for 3C 273, in which the K-alpha line luminosity might be of the order $3.0\times 10^{44}$ erg/s with an equivalent width of 2.4 keV. Such a line could be detected in a future mission., Comment: 4 pages, 1 Figure
Published: 2004
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12. Studying the evolution of the hot universe with the X-ray evolving universe spectroscopy mission - XEUS

Author: Keith O. Mason, G. Trinchieri, I. Georgantopoulos, J. H. M. M. Schmitt, Paola Grandi, N. Kawai, Allan Hornstrup, M. Cappi, Katsuji Koyama, Andrea Comastri, A. C. Fabian, Trevor J. Ponman, Arvind Parmar, T. J. L. Courvoisier, M. Arnaud, Didier Barret, Takaya Ohashi, Martin Ward, M. van der Klis, Mariano Mendez, Kazuo Makishima, Salvatore Sciortino, Hans Böhringer, Richard E. Griffiths, Xavier Barcons, Alain Blanchard, L. Piro, Günther Hasinger, C. Motch, F. B. S. Paerels, Giuseppe Malaguti, Fabrizio Fiore, and High Energy Astrophys. & Astropart. Phys (API, FNWI)
Subjects: Physics, Atmospheric Science, Spacecraft, business.industry, media_common.quotation_subject, Detector, European Robotic Arm, Dark matter, Aerospace Engineering, Astronomy, Astronomy and Astrophysics, Universe, Redshift, Geophysics, Space and Planetary Science, Observatory, International Space Station, General Earth and Planetary Sciences, business, media_common
Abstract: Europe is one of the major partners building the International Space Station (ISS) and European industry, together with ESA, is responsible for many station components including the Columbus Orbital Facility, the Automated Transport Vehicle, two connecting modules and the European Robotic Arm. Together with this impressive list of contributions there is a strong desire within the ESA Member States to benefit from this investment by utilizing the unique capabilities of the ISS to perform world-class science. XEUS is one of the astronomical applications being studied by ESA to utilize the capabilities of the ISS. XEUS will be a long-term X-ray observatory with an initial mirror area of 6 m 2 at 1 keV that will be expanded to 30 m 2 following a visit to the ISS. The 1 keV spatial resolution is expected to be 2–5″ half-energy-width. XEUS will consist of separate detector and mirror spacecraft (MSC) aligned by active control to provide a focal length of 50 m. A new detector spacecraft, complete with the next generation of instruments, will also be added after visiting the ISS. The limiting 0.1–2.5 keV sensitivity will then be 4 × 10 −18 erg cm −2 s −1 , around 200 times better than XMM-Newton, allowing XEUS to study the properties of the hot baryons and dark matter at high redshift.
Published: 2004

13. Active Galactic Nuclei

Author: Professor R. D. Blandford, Professor H. Netzer, Professor L. Woltjer, Dr. T. J.-L. Courvoisier, Professor M. Mayor, Professor R. D. Blandford, Professor H. Netzer, Professor L. Woltjer, Dr. T. J.-L. Courvoisier, and Professor M. Mayor
Subjects: Astronomy
Published: 2013

14. Time resolved spectroscopy of GRB 030501 using INTEGRAL

Author: J. Borkowski, Sandro Mereghetti, T. J. L. Courvoisier, D. Gotz, René Hudec, F. Hroch, Volker Beckmann, Niels Lund, A. von Kienlin, S. E. Shaw, and C. Wigger
Subjects: Physics, Spectral index, Astrophysics::High Energy Astrophysical Phenomena, Resolution (electron density), Flux, Astronomy, Astronomy and Astrophysics, Field of view, Astrophysics, Space and Planetary Science, Emission spectrum, Time-resolved spectroscopy, Spectroscopy, Gamma-ray burst
Abstract: The gamma-ray instruments on-board INTEGRAL offer an unique opportunity to perform time resolved analysis on GRBs. The imager IBIS allows accurate positioning of GRBs and broad band spectral analysis, while SPI provides high resolution spectroscopy. GRB 030501 was discovered by the INTEGRAL Burst Alert System in the ISGRI field of view. Although the burst was fairly weak (fluence F 2 0 - 2 0 0 k e V ≃ 3.5 x 10 - 6 erg cm - 2 ) it was possible to perform time resolved spectroscopy with a resolution of a few seconds. The GRB shows a spectrum in the 20-400 keV range which is consistent with a spectral index r = -1.8. No emission line or spectral break was detectable in the spectrum. Although the flux seems to be correlated with the hardness of the GRB spectrum, there is no clear soft to hard evolution seen over the duration of the burst. The INTEGRAL data have been compared with results from the Ulysses and RHESSI experiments.
Published: 2003
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15. INTEGRAL and XMM-Newton Observations of the Weak Gamma-Ray Burst GRB 030227

Author: D. Gotz, P. R. den Hartog, A. von Kienlin, J. Borkowski, Niels Lund, Volker Schoenfelder, Volker Beckmann, L. Bouchet, Sandro Mereghetti, W. Hermsen, A. J. Castro-Tirado, Francois Lebrun, C. Winkler, Andrea Tiengo, J. P. Roques, M. Mas Hesse, P. Ubertini, T. J. L. Courvoisier, and J. A. Paul
Subjects: Physics, Photon, Astrophysics::High Energy Astrophysical Phenomena, Flux, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Power law, Redshift, Afterglow, Space and Planetary Science, Emission spectrum, Gamma-ray burst, Absorption (electromagnetic radiation)
Abstract: We present INTEGRAL and XMM-Newton observations of the prompt gamma-ray emission and the X-ray afterglow of GRB030227, the first GRB for which the quick localization obtained with the INTEGRAL Burst Alert System (IBAS) has led to the discovery of X-ray and optical afterglows. GRB030227 had a duration of about 20 s and a peak flux of 1.1 photons cm^-2 s^-1 in the 20-200 keV energy range. The time averaged spectrum can be fit by a single power law with photon index about 2 and we find some evidence for a hard to soft spectral evolution. The X-ray afterglow has been detected starting only 8 hours after the prompt emission, with a 0.2-10 keV flux decreasing as t^-1 from 1.3x10e-12 to 5x10e-13 erg cm^-2 s^-1. The afterglow spectrum is well described by a power law with photon index 1.94+/-0.05 modified by a redshifted neutral absorber with column density of several 10e22 cm^-2. A possible emission line at 1.67 keV could be due to Fe for a redshift z=3, consistent with the value inferred from the absorption.
Published: 2003
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16. The Large Observatory For x-ray Timing

Author: Antonios Manousakis, S. Boutloukos, F. Zwart, Jose M. Torrejon, C. Pittori, Alessandro Drago, Dieter H. Hartmann, Feryal Özel, T. J. L. Courvoisier, Tim Johannsen, Jordi José, M. Michalska, Christian Schmid, I. Rashevskaya, Gottfried Kanbach, V. Petracek, L. Bradley, Allan Hornstrup, M. H. Erkut, Sergio Campana, Rudy Wijnands, Andrew Cumming, Nils Andersson, Tomaso Belloni, M. C. Miller, Roman Wawrzaszek, Stefano Bianchi, Enrique García-Berro, Sandro Mereghetti, C. Guidorzi, C. Corral Van Damme, Søren Brandt, Francesco Tombesi, Felix Ryde, Didier Barret, Simon Vaughan, Marco Feroci, T. Di Salvo, C. van Baren, Angelo Antonelli, Marc Ribó, J. L. Atteia, P. Soleri, Alessio Trois, Silvia Zane, G. Mouret, Ersin Gogus, Emanuele Perinati, J. Coker, Piero Malcovati, V. Mangano, F. Jetter, P. Uter, P. Romano, M. Nowak, Roberto Turolla, Laura Tolos, Antonino D'Ai, Laura Alvarez, C. Amoros, Simone Scaringi, A. Possenti, David M. Smith, M. Falanga, A. Goldwurm, René Hudec, Ignacio Negueruela, M. van der Klis, Francesco Longo, José A. Pons, I. M. McHardy, R. Rohlfs, P. Cais, Luigi Stella, S. Di Cosimo, Antoine Rousseau, M. Ayre, M. Gschwender, D. Klochkov, Niels Lund, Chryssa Kouveliotou, P. Azzarello, F. Château, Michael Gabler, S. Vercellone, Martin Durant, I. Donnarumma, Giorgio Matt, Mauro Orlandini, P. Kaaret, Patrick Smith, P. T. O'Brien, A. Argan, M. Orienti, Marco Grassi, Claudio Labanti, Edward F. Brown, Christopher S. Reynolds, Gloria Sala, Y. Evangelista, Gabriel Török, José Braga, Riccardo Campana, Alan Smith, C. Gouiffes, Nevin N. Weinberg, Leonardo Gualtieri, Yannick Favre, P.G. Jonker, Gabriele Giovannini, D. de Martino, Irfan Kuvvetli, S. Motta, Teresa Mineo, Paul J. Groot, Pablo Reig, Martino Marisaldi, Andrea Sanna, Lorenzo Amati, G. L. Israel, D. Macera, K. S. Wood, Pablo Cerdá-Durán, F. Fuschino, Suvi Gezari, Mariano Mendez, Slawomir Suchy, Damien Rambaud, Nanda Rea, R. Artigue, J.-Y. Seyler, S. N. Shore, Frederick K. Lamb, Jörn Wilms, Mark G. Alford, Margarita Hernanz, Thomas M. Tauris, Luca Izzo, Tobias Boenke, J. J. M. in 't Zand, J. Mulačová, P. Binko, Daniel Maier, Jan Schee, Bruce Gendre, Enrico Bozzo, Paul S. Ray, Giuseppe Bertuccio, Simone Migliari, Ignazio Bombaci, Vladimir Karas, Nikolaos Stergioulas, P. P. Laubert, D. Karelin, A. C. Fabian, Giovanni Miniutti, Dacheng Lin, L. Guy, Martine Mouchet, Colleen A. Wilson-Hodge, Valeria Ferrari, Kai Hebeler, Mark H. Finger, Shigeto Watanabe, Pawel Haensel, H. Jacobs, Adrian Martindale, A. A. Zdziarski, Andrea Santangelo, Giuseppe Baldazzi, Piergiorgio Casella, Fabio Muleri, M. Hailey, Antonio Bianchini, Giuseppe Lodato, E. Del Monte, M. Rapisarda, Zdeněk Stuchlík, Alain Cros, V. Sochora, Laurens Keek, Jorge Casares, Andrew Melatos, Pere Blay, E. Rossi, A. P. Spencer, G. Stratta, Conrado Albertus, J. M. Paredes, M. Ahangarianabhari, Anna L. Watts, M. Del Santo, I. Kreykenbohm, Alessandro Patruno, G. A. Caliandro, C. Feldman, M. Pohl, Fabrizio Tamburini, G. Zampa, Marina Orio, Flemming Hansen, P. Ramon, Ruben Salvaterra, David H. Lumb, Edward M. Cackett, Andrew Shearer, Sharon M. Morsink, L. Pacciani, J.-M. Bonnet Bidaud, A. De Luca, Jérôme Chenevez, Sebastian Diebold, N. Zampa, Carole A. Haswell, Luciano Burderi, E. Cavazzuti, Adam Ingram, Dhiren Kataria, Berend Winter, A. Vacchi, W. Hermsen, P. Giommi, Dong Lai, N. A. Webb, P. Bodin, Dom Walton, Solen Balman, Benjamin Stappers, M. Burgay, Luca Zampieri, Carl Budtz-Jørgensen, Ralph A. M. J. Wijers, Giancarlo Cusumano, J. L. Galvez Sanchez, Raffaella Schneider, Luciano Rezzolla, Alexander Heger, S. Korpela, Dimitrios Emmanoulopoulos, Biswajit Paul, Diego Götz, B. Artigues, Paolo Soffitta, M. H. Finger, J. W. den Herder, Paolo Esposito, Kazushi Iwasawa, Poul Erik Holmdahl Olsen, J. Neilsen, Marco Barbera, Deepto Chakrabarty, R. A. Osten, M. Reina Aranda, A. J. Castro-Tirado, Andrea Tramacere, D. Haas, Johannes Dercksen, John A. Tomsick, A. V. Penacchioni, V. D'Elia, Alfonso Collura, Altan Baykal, P. Le Provost, S. Turriziani, Kostas D. Kokkotas, Duncan K. Galloway, Ron Remillard, Juhani Huovelin, Somak Bhattacharyya, Pavel Bakala, Phil Uttley, Richard E. Cole, Mahesh Prakash, L. Kuiper, T. Munoz-Darias, Diego F. Torres, S. Mahmoodifar, G. Ramsay, Andrew Norton, T. Kennedy, Achim Schwenk, L. Zdunik, A. B. Giles, Jerome Rodriguez, C. Motch, Ilya Mandel, Marcello Giroletti, Dimitrios Psaltis, J. Sandberg, Fiamma Capitanio, Remon Cornelisse, M. R. Gilfanov, Peggy Varniere, Franck Cadoux, Peter J. Wheatley, M. de Pasquale, Juri Poutanen, S. Maestre, A. Pellizzoni, Axel Schwope, Diego Altamirano, Piotr Orleanski, V. Vrba, Agata Różańska, Kateřina Goluchová, P. Rodríguez Gil, Niccolò Bucciantini, Stéphane Schanne, Carlo Ferrigno, Thomas J. Maccarone, H. Wende, Tod E. Strohmayer, Tadayuki Takahashi, Francois Lebrun, E. Kuulkers, Jeroen Homan, Maurizio Paolillo, M. A. Perez, J. P. Osborne, A. Alpar, Sanjay Reddy, G.W. Fraser, V. Sulemainov, D. Linder, L. Sabau-Graziati, A. Rachevski, Bing Zhang, Alessandro Papitto, C. Tenzer, Alex Markowitz, J. Portell, Roberto Mignani, Fabrizio Bocchino, Arnau Rios, R. de la Rie, M. Wille, A. de Rosa, Alessandro Riggio, M. Frericks, Andrew W. Steiner, Michal Bursa, Federico Bernardini, Jon M. Miller, W. Kluzniak, INAF - Osservatorio Astronomico di Roma ( OAR ), Istituto Nazionale di Astrofisica ( INAF ), Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées ( LATT ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Variable Energy Cyclotron Centre, Institut Pasteur de Montevideo, Réseau International des Instituts Pasteur ( RIIP ) -Institut Pasteur de Montevideo, Mullard Space Science Laboratory ( MSSL ), University College of London [London] ( UCL ), FORMATION STELLAIRE 2014, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux ( L3AB ), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Observatoire aquitain des sciences de l'univers ( OASU ), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Laboratoire d'Astrophysique de Bordeaux [Pessac] ( LAB ), Université de Bordeaux ( UB ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Bordeaux ( UB ), Instituto de Astrofísica de Andalucía ( IAA ), Consejo Superior de Investigaciones Científicas [Spain] ( CSIC ), Institut de Recherches sur les lois Fondamentales de l'Univers ( IRFU ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay, Interactions et dynamique des environnements de surface ( IDES ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Licryl Laboratory ( CNR-IPCF UOS Cosenza ), University of Calabria, Laboratori Nazionali di Frascati ( LNF ), National Institute for Nuclear Physics ( INFN ), PCAS, Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano ( IASF-MI ), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Astrophysique Interactions Multi-échelles ( AIM - UMR 7158 - UMR E 9005 ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Paris Diderot - Paris 7 ( UPD7 ), Canada's National Laboratory for Particle and Nuclear Physics ( TRIUMF ), NRC, Dipartimento di Astronomia, Universita degli Studi di Bologna, Università di Bologna [Bologna] ( UNIBO ), Institut de recherches sur la catalyse et l'environnement de Lyon ( IRCELYON ), Université Claude Bernard Lyon 1 ( UCBL ), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique ( CNRS ), Laboratoire Univers et Théories ( LUTH ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de Spectrochimie Infrarouge et Raman - UMR 8516 ( LASIR ), Université de Lille-Centre National de la Recherche Scientifique ( CNRS ), Dipartimento di Scienze Fisiche [Naples], Università degli studi di Napoli Federico II, Energétique, propulsion, espace, environnement ( EPEE ), Université d'Orléans ( UO ) -Centre National de la Recherche Scientifique ( CNRS ), Department of Physics and Astronomy [Hanover], Dartmouth College [Hanover], Institut de recherche en astrophysique et planétologie ( IRAP ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire d’Optique Atmosphérique - UMR 8518 ( LOA ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Université de Lille-Centre National de la Recherche Scientifique ( CNRS ), Institut de Biologie du Développement de Marseille ( IBDM ), Aix Marseille Université ( AMU ) -Institut National de la Santé et de la Recherche Médicale ( INSERM ) -Centre National de la Recherche Scientifique ( CNRS ), Universitat Politècnica de Catalunya [Barcelona] ( UPC ), INAF-IASF Milano, Climate and Environmental Physics [Bern], University of Bern, Centre National d'Etudes Spatiales ( CNES ), Institute of Geology, Eidgenössische Technische Hochschule [Zürich] ( ETH Zürich ), IEEC-CSIC, Universitat Autònoma de Barcelona [Barcelona] ( UAB ), MedisysResearch Lab ( Medisys ), Philips Research, European Space Astronomy Center ( ESAC ), European Space Agency ( ESA ), High Energy Astrophys. & Astropart. Phys (API, FNWI), INAF - Osservatorio Astronomico di Roma (OAR), Istituto Nazionale di Astrofisica (INAF), Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées (LATT), Université Toulouse III - Paul Sabatier (UT3), 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), Réseau International des Instituts Pasteur (RIIP), Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Interactions et dynamique des environnements de surface (IDES), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Licryl Laboratory (CNR-IPCF UOS Cosenza), Università della Calabria [Arcavacata di Rende] (Unical), Laboratori Nazionali di Frascati (LNF), Istituto Nazionale di Fisica Nucleare (INFN), Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano (IASF-MI), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / 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), Canada's particle accelerator centre (TRIUMF), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Institut de recherches sur la catalyse et l'environnement de Lyon (IRCELYON), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut de Chimie du CNRS (INC)-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, Laboratoire Avancé de Spectroscopie pour les Intéractions la Réactivité et l'Environnement - UMR 8516 (LASIRE), Institut de Chimie du CNRS (INC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), University of Naples Federico II = Università degli studi di Napoli Federico II, Energétique, propulsion, espace, environnement (EPEE), Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Laboratoire d’Optique Atmosphérique - UMR 8518 (LOA), Institut national des sciences de l'Univers (INSU - CNRS)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Institut de Biologie du Développement de Marseille (IBDM), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS), Universitat Politècnica de Catalunya [Barcelona] (UPC), Climate and Environmental Physics [Bern] (CEP), Physikalisches Institut [Bern], Universität Bern [Bern] (UNIBE)-Universität Bern [Bern] (UNIBE), Centre National d'Études Spatiales [Toulouse] (CNES), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Universitat Autònoma de Barcelona (UAB), MedisysResearch Lab (Medisys), European Space Astronomy Centre (ESAC), Agence Spatiale Européenne = European Space Agency (ESA), SPIE, Takahashi, Tadayuki, Feroci M., Den Herder J.W., Bozzo E., Barret D., Brandt S., Hernanz M., Van Der Klis M., Pohl M., Santangelo A., Stella L., Watts A., Wilms J., Zane S., Ahangarianabhari M., Albertus C., Alford M., Alpar A., Altamirano D., Alvarez L., Amati L., Amoros C., Andersson N., Antonelli A., Argan A., Artigue R., Artigues B., Atteia J.-L., Azzarello P., Bakala P., Baldazzi G., Balman S., Barbera M., Van Baren C., Bhattacharyya S., Baykal A., Belloni T., Bernardini F., Bertuccio G., Bianchi S., Bianchini A., Binko P., Blay P., Bocchino F., Bodin P., Bombaci I., Bonnet Bidaud J.-M., Boutloukos S., Bradley L., Braga J., Brown E., Bucciantini N., Burderi L., Burgay M., Bursa M., Budtz-Jorgensen C., Cackett E., Cadoux F.R., Cais P., Caliandro G.A., Campana R., Campana S., Capitanio F., Casares J., Casella P., Castro-Tirado A.J., Cavazzuti E., Cerda-Duran P., Chakrabarty D., Chateau F., Chenevez J., Coker J., Cole R., Collura A., Cornelisse R., Courvoisier T., Cros A., Cumming A., Cusumano G., D'ai A., D'elia V., Del Monte E., De Luca A., De Martino D., Dercksen J.P.C., De Pasquale M., De Rosa A., Del Santo M., Di Cosimo S., Diebold S., Di Salvo T., Donnarumma I., Drago A., Durant M., Emmanoulopoulos D., Erkut M.H., Esposito P., Evangelista Y., Fabian A., Falanga M., Favre Y., Feldman C., Ferrari V., Ferrigno C., Finger M., Finger M.H., Fraser G.W., Frericks M., Fuschino F., Gabler M., Galloway D.K., Galvez Sanchez J.L., Garcia-Berro E., Gendre B., Gezari S., Giles A.B., Gilfanov M., Giommi P., Giovannini G., Giroletti M., Gogus E., Goldwurm A., Goluchova K., Gotz D., Gouiffes C., Grassi M., Groot P., Gschwender M., Gualtieri L., Guidorzi C., Guy L., Haas D., Haensel P., Hailey M., Hansen F., Hartmann D.H., Haswell C.A., Hebeler K., Heger A., Hermsen W., Homan J., Hornstrup A., Hudec R., Huovelin J., Ingram A., In't Zand J.J.M., Israel G., Iwasawa K., Izzo L., Jacobs H.M., Jetter F., Johannsen T., Jonker P., Jose J., Kaaret P., Kanbach G., Karas V., Karelin D., Kataria D., Keek L., Kennedy T., Klochkov D., Kluzniak W., Kokkotas K., Korpela S., Kouveliotou C., Kreykenbohm I., Kuiper L.M., Kuvvetli I., Labanti C., Lai D., Lamb F.K., Laubert P.P., Lebrun F., Lin D., Linder D., Lodato G., Longo F., Lund N., Maccarone T.J., Macera D., Maestre S., Mahmoodifar S., Maier D., Malcovati P., Mandel I., Mangano V., Manousakis A., Marisaldi M., Markowitz A., Martindale A., Matt G., Mchardy I.M., Melatos A., Mendez M., Mereghetti S., Michalska M., Migliari S., Mignani R., Miller M.C., Miller J.M., Mineo T., Miniutti G., Morsink S., Motch C., Motta S., Mouchet M., Mouret G., Mulaova J., Muleri F., Munoz-Darias T., Negueruela I., Neilsen J., Norton A.J., Nowak M., O'brien P., Olsen P.E.H., Orienti M., Orio M., Orlandini M., Orleaaski P., Osborne J.P., Osten R., Ozel F., Pacciani L., Paolillo M., Papitto A., Paredes J.M., Patruno A., Paul B., Perinati E., Pellizzoni A., Penacchioni A.V., Perez M.A., Petracek V., Pittori C., Pons J., Portell J., Possenti A., Poutanen J., Prakash M., Le Provost P., Psaltis D., Rambaud D., Ramon P., Ramsay G., Rapisarda M., Rachevski A., Rashevskaya I., Ray P.S., Rea N., Reddy S., Reig P., Reina Aranda M., Remillard R., Reynolds C., Rezzolla L., Ribo M., De La Rie R., Riggio A., Rios A., Rodriguez-Gil P., Rodriguez J., Rohlfs R., Romano P., Rossi E.M.R., Rozanska A., Rousseau A., Ryde F., Sabau-Graziati L., Sala G., Salvaterra R., Sanna A., Sandberg J., Scaringi S., Schanne S., Schee J., Schmid C., Shore S., Schneider R., Schwenk A., Schwope A.D., Seyler J.-Y., Shearer A., Smith A., Smith D.M., Smith P.J., Sochora V., Soffitta P., Soleri P., Spencer A., Stappers B., Steiner A.W., Stergioulas N., Stratta G., Strohmayer T.E., Stuchlik Z., Suchy S., Sulemainov V., Takahashi T., Tamburini F., Tauris T., Tenzer C., Tolos L., Tombesi F., Tomsick J., Torok G., Torrejon J.M., Torres D.F., Tramacere A., Trois A., Turolla R., Turriziani S., Uter P., Uttley P., Vacchi A., Varniere P., Vaughan S., Vercellone S., Vrba V., Walton D., Watanabe S., Wawrzaszek R., Webb N., Weinberg N., Wende H., Wheatley P., Wijers R., Wijnands R., Wille M., Wilson-Hodge C.A., Winter B., Wood K., Zampa G., Zampa N., Zampieri L., Zdunik L., Zdziarski A., Zhang B., Zwart F., Ayre M., Boenke T., Corral Van Damme C., Kuulkers E., Lumb D., Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), 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), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), 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), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), 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), 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 de Chimie du CNRS (INC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Centrale Lille Institut (CLIL), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Universität Bern [Bern]-Universität Bern [Bern], European Space Agency (ESA), Feroci, M., den Herder, J., Bozzo, E., Barret, D., Brandt, S., Hernanz, M., van der Klis, M., Pohl, M., Santangelo, A., Stella, L., Watts, A., Wilms, J., Zane, S., Ahangarianabhari, M., Albertus, C., Alford, M., Alpar, A., Altamirano, D., Alvarez, L., Amati, L., Amoros, C., Andersson, N., Antonelli, A., Argan, A., Artigue, R., Artigues, B., Atteia, J., Azzarello, P., Bakala, P., Baldazzi, G., Balman, S., Barbera, M., van Baren, C., Bhattacharyya, S., Baykal, A., Belloni, T., Bernardini, F., Bertuccio, G., Bianchi, S., Bianchini, A., Binko, P., Blay, P., Bocchino, F., Bodin, P., Bombaci, I., Bonnet Bidaud, J., Boutloukos, S., Bradley, L., Braga, J., Brown, E., Bucciantini, N., Burderi, L., Burgay, M., Bursa, M., Budtz Jørgensen, C., Cackett, E., Cadoux, F., Caïs, P., Caliandro, G., Campana, R., Campana, S., Capitanio, F., Casares, J., Casella, P., Castro Tirado, A., Cavazzuti, E., Cerda Duran, P., Chakrabarty, D., Château, F., Chenevez, J., Coker, J., Cole, R., Collura, A., Cornelisse, R., Courvoisier, T., Cros, A., Cumming, A., Cusumano, G., D'Ai', A., D'Elia, V., Del Monte, E., de Luca, A., de Martino, D., Dercksen, J., de Pasquale, M., De Rosa, A., Del Santo, M., Di Cosimo, S., Diebold, S., DI SALVO, T., Donnarumma, I., Drago, A., Durant, M., Emmanoulopoulos, D., Erkut, M., Esposito, P., Evangelista, Y., Fabian, A., Falanga, M., Favre, Y., Feldman, C., Ferrari, V., Ferrigno, C., Finger, M., Fraser, G., Frericks, M., Fuschino, F., Gabler, M., Galloway, D., Galvez Sanchez, J., Garcia Berro, E., Gendre, B., Gezari, S., Giles, A., Gilfanov, M., Giommi, P., Giovannini, G., Giroletti, M., Gogus, E., Goldwurm, A., Goluchová, K., Götz, D., Gouiffes, C., Grassi, M., Groot, P., Gschwender, M., Gualtieri, L., Guidorzi, C., Guy, L., Haas, D., Haensel, P., Hailey, M., Hansen, F., Hartmann, D., Haswell, C., Hebeler, K., Heger, A., Hermsen, W., Homan, J., Hornstrup, A., Hudec, R., Huovelin, J., Ingram, A., In't Zand, J., Israel, G., Iwasawa, K., Izzo, L., Jacobs, H., Jetter, F., Johannsen, T., Jonker, P., Josè, J., Kaaret, P., Kanbach, G., Karas, V., Karelin, D., Kataria, D., Keek, L., Kennedy, T., Klochkov, D., Kluzniak, W., Kokkotas, K., Korpela, S., Kouveliotou, C., Kreykenbohm, I., Kuiper, L., Kuvvetli, I., Labanti, C., Lai, D., Lamb, F., Laubert, P., Lebrun, F., Lin, D., Linder, D., Lodato, G., Longo, F., Lund, N., Maccarone, T., Macera, D., Maestre, S., Mahmoodifar, S., Maier, D., Malcovati, P., Mandel, I., Mangano, V., Manousakis, A., Marisaldi, M., Markowitz, A., Martindale, A., Matt, G., Mchardy, I., Melatos, A., Mendez, M., Mereghetti, S., Michalska, M., Migliari, S., Mignani, R., Miller, M., Miller, J., Mineo, T., Miniutti, G., Morsink, S., Motch, C., Motta, S., Mouchet, M., Mouret, G., Mulačová, J., Muleri, F., Muñoz Darias, T., Negueruela, I., Neilsen, J., Norton, A., Nowak, M., O'Brien, P., Olsen, P., Orienti, M., Orio, M., Orlandini, M., Orleański, P., Osborne, J., Osten, R., Ozel, F., Pacciani, L., Paolillo, M., Papitto, A., Paredes, J., Patruno, A., Paul, B., Perinati, E., Pellizzoni, A., Penacchioni, A., Perez, M., Petracek, V., Pittori, C., Pons, J., Portell, J., Possenti, A., Poutanen, J., Prakash, M., Le Provost, P., Psaltis, D., Rambaud, D., Ramon, P., Ramsay, G., Rapisarda, M., Rachevski, A., Rashevskaya, I., Ray, P., Rea, N., Reddy, S., Reig, P., Reina Aranda, M., Remillard, R., Reynolds, C., Rezzolla, L., Ribo, M., de la Rie, R., Riggio, A., Rios, A., Rodríguez Gil, P., Rodriguez, J., Rohlfs, R., Romano, P., Rossi, E., Rozanska, A., Rousseau, A., Ryde, F., Sabau Graziati, L., Sala, G., Salvaterra, R., Sanna, A., Sandberg, J., Scaringi, S., Schanne, S., Schee, J., Schmid, C., Shore, S., Schneider, R., Schwenk, A., Schwope, A., Seyler, J., Shearer, A., Smith, A., Smith, D., Smith, P., Sochora, V., Soffitta, P., Soleri, P., Spencer, A., Stappers, B., Steiner, A., Stergioulas, N., Stratta, G., Strohmayer, T., Stuchlik, Z., Suchy, S., Sulemainov, V., Takahashi, T., Tamburini, F., Tauris, T., Tenzer, C., Tolos, L., Tombesi, F., Tomsick, J., Torok, G., Torrejon, J., Torres, D., Tramacere, A., Trois, A., Turolla, R., Turriziani, S., Uter, P., Uttley, P., Vacchi, A., Varniere, P., Vaughan, S., Vercellone, S., Vrba, V., Walton, D., Watanabe, S., Wawrzaszek, R., Webb, N., Weinberg, N., Wende, H., Wheatley, P., Wijers, R., Wijnands, R., Wille, M., Wilson Hodge, C., Winter, B., Wood, K., Zampa, G., Zampa, N., Zampieri, L., Zdunik, L., Zdziarski, A., Zhang, B., Zwart, F., Ayre, M., Boenke, T., Corral van Damme, C., Kuulkers, E., Lumb, D., Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), National Institute for Nuclear Physics (INFN), 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), Canada's National Laboratory for Particle and Nuclear Physics (TRIUMF), Università di Bologna [Bologna] (UNIBO), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Spectrochimie Infrarouge et Raman - UMR 8516 (LASIR), Centre National de la Recherche Scientifique (CNRS)-Université de Lille, Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Lille, Aix Marseille Université (AMU)-Collège de France (CdF)-Centre National de la Recherche Scientifique (CNRS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), Universitat Autònoma de Barcelona [Barcelona] (UAB), Astronomy, den Herder, J. W., Atteia, J. L., Bonnet Bidaud, J. M., Cadoux, F. R., Cais, P., Caliandro, G. A., Castro Tirado, A. J., D'Aì, A., De Luca, A., De Martino, D., Dercksen, J. P. C., De Pasquale, M., Di Salvo, T., Erkut, M. H., Finger, M. H., Fraser, G. W., Galloway, D. K., Galvez Sanchez, J. L., Giles, A. B., Hartmann, D. H., Haswell, C. A., in't Zand, J. J. M., Jacobs, H. M., Kuiper, L. M., Lamb, F. K., Laubert, P. P., Maccarone, T. J., Mchardy, I. M., Miller, M. C., Miller, J. M., Norton, A. J., Olsen, P. E. H., Orleanski, P., Osborne, J. P., Paolillo, Maurizio, Paredes, J. M., Penacchioni, A. V., Perez, M. A., Ray, P. S., Rossi, E. M. R., Schwope, A. D., Seyler, J. Y., Smith, D. M., Smith, P. J., Steiner, A. W., Strohmayer, T. E., Torrejon, J. M., Torres, D. F., and Wilson Hodge, C. A.
Subjects: x-ray and γ-ray instrumentation, compact objects, microchannel plates, X-ray detectors, X-ray imaging, X-ray spectroscopy, X-ray timing, Electronic, Optical and Magnetic Materials, Condensed Matter Physics, Computer Science Applications1707 Computer Vision and Pattern Recognition, Applied Mathematics, Electrical and Electronic Engineering, Vision, Observatories, Field of view, 01 natural sciences, 7. Clean energy, neutron stars, Observatory, 010303 astronomy & astrophysics, Physics, Equipment and services, Astrophysics::Instrumentation and Methods for Astrophysics, Steradian, [ SDU.ASTR.IM ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Astrophysics - Instrumentation and Methods for Astrophysics, X-ray detector, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Cosmic Vision, Spectral resolution, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, NO, microchannel plate, Settore FIS/05 - Astronomia e Astrofisica, X-rays, compact object, 0103 physical sciences, Electronic, Optical and Magnetic Materials, Instrumentation and Methods for Astrophysics (astro-ph.IM), dense hadronic matter, Sensors, 010308 nuclear & particles physics, Astronomy, Accretion (astrophysics), [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Neutron star, 13. Climate action, [ PHYS.ASTR.IM ] Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Gamma-ray burst, astro-ph.IM
Abstract: The Large Observatory For x-ray Timing (LOFT) was studied within ESA M3 Cosmic Vision framework and participated in the final down-selection for a launch slot in 2022-2024. Thanks to the unprecedented combination of effective area and spectral resolution of its main instrument, LOFT will study the behaviour of matter under extreme conditions, such as the strong gravitational field in the innermost regions of accretion flows close to black holes and neutron stars, and the supra-nuclear densities in the interior of neutron stars. The science payload is based on a Large Area Detector (LAD, 10 m 2 effective area, 2-30 keV, 240 eV spectral resolution, 1 deg collimated field of view) and a WideField Monitor (WFM, 2-50 keV, 4 steradian field of view, 1 arcmin source location accuracy, 300 eV spectral resolution). The WFM is equipped with an on-board system for bright events (e.g. GRB) localization. The trigger time and position of these events are broadcast to the ground within 30 s from discovery. In this paper we present the status of the mission at the end of its Phase A study., Proc. SPIE 9144, Space Telescopes and Instrumentation 2014: Ultraviolet to Gamma Ray, 91442T
Published: 2014
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17. Simultaneous UV, optical and radio monitoring of the BL Lac object OJ 287 in March 1993

Author: Martin Ward, Megan Donahue, Elena Pian, Rick Edelson, G. Pike, Andreas Quirrenbach, Ian M. George, Alexei V. Filippenko, R. S. Warwick, H. R. Miller, Michael L. Sitko, Willem Wamsteker, L. Maraschi, Andy Lawrence, H. Bock, N.H. Shakhovskoy, H. H. Fink, T. J. L. Courvoisier, M. T. Carini, Paul S. Smith, Esko Valtaoja, Aldo Treves, Yu. S. Efimov, Joel N. Bregman, A. Sillanpää, Stefan Wagner, L. O. Takalo, Harri Teräsranta, and Jochen Heidt
Subjects: Physics, Atmospheric Science, business.industry, Aerospace Engineering, Flux, Astronomy and Astrophysics, Astrophysics, Light curve, Wavelength, Geophysics, Optics, Space and Planetary Science, Ultraviolet astronomy, General Earth and Planetary Sciences, Light emission, Emission spectrum, business, BL Lac object, Radio astronomy
Abstract: The BL Lacertae object OJ 287 was intensively monitored with the IUE satellite from 1993 March 15 to 20 in the 2000-3000 A wavelength region. The very low emission state of the source hampered the detection during part of the 23 performed exposures. The light curve at 2650 A constructed with the 11 best images exhibits a variable trend with a factor is less than or approximately 2 enhancement of the flux in about 3 hours. Simultaneous ground based observations show an optical flux variability of smaller amplitude, but correlated with the UV light curve without any apparent lag. The radio light curve is nearly constant. The UV emission state is the weakest observed in 15 years for this flaring blazard, being a factor of less than orapproximately 20 lower than the maximum recorded one.
Published: 1995
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18. The physical origin of the X-ray power spectral density break timescale in accreting black holes

Author: W. Ishibashi and T. J.-L. Courvoisier
Subjects: Active galactic nucleus, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, Binary number, FOS: Physical sciences, Electron, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, General Relativity and Quantum Cosmology, 0103 physical sciences, 010303 astronomy & astrophysics, Scaling, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Supermassive black hole, 010308 nuclear & particles physics, Spectral density, Astronomy and Astrophysics, Accretion (astrophysics), Black hole, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: X-ray variability of active galactic nuclei (AGN) and black hole binaries can be analysed by means of the power spectral density (PSD). The break observed in the power spectrum defines a characteristic variability timescale of the accreting system. The empirical variability scaling that relates characteristic timescale, black hole mass, and accretion rate ($T_B \propto M_{BH}^{2.1}/\dot{M}^{0.98}$) extends from supermassive black holes in AGN down to stellar-mass black holes in binary systems. We suggest that the PSD break timescale is associated with the cooling timescale of electrons in the Comptonisation process at the origin of the observed hard X-ray emission. We obtain that the Compton cooling timescale directly leads to the observational scaling and naturally reproduces the functional dependence on black hole mass and accretion rate ($t_C \propto M_{BH}^{2}/\dot{M}$). This result simply arises from general properties of the emission mechanism and is independent of the details of any specific accretion model., Comment: 4 pages, accepted for publication in Astronomy and Astrophysics, Letters to the Editor
Published: 2012
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19. Timing properties of gamma-ray bursts detected by SPI-ACS detector on board of INTEGRAL

Author: V. Savchenko, Andrii Neronov, and T. J. L. Courvoisier
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, Population, FOS: Physical sciences, Cosmic ray, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Coincidence, 0103 physical sciences, 010306 general physics, education, 010303 astronomy & astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), education.field_of_study, Solar flare, Spectrometer, Detector, Astronomy and Astrophysics, Large sample, 13. Climate action, Space and Planetary Science, Gamma-ray burst, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We study timing properties of a large sample of gamma-ray bursts (GRB) detected by the Anti-Coincidence Shield (ACS) of the SPI spectrometer of INTEGRAL telescope. We identify GRB-like events in the SPI-ACS data. The data set under investigation is the history of count rate of the SPI-ACS detector recorded with a binning of 50 ms over the time span of ~10 yr. In spite of the fact that SPI-ACS does not have imaging capability, it provides high statistics signal for each GRB event, because of its large effective area. We classify all isolated excesses in the SPI-ACS count rate into three types: short spikes produced by cosmic rays, GRBs and Solar flare induced events. We find some ~1500 GRB-like events in the 10 yr exposure. A significant fraction of the GRB-like events identified in SPI-ACS occur in coincidence with triggers of other gamma-ray telescopes and could be considered as confirmed GRBs. We study the distribution of durations of the GRBs detected by SPI-ACS and find that the peak of the distribution of long GRBs is at ~ 20, i.e. somewhat shorter than for the long GRBs detected by BATSE. Contrary to the BATSE observation, the population of short GRBs does not have any characteristic time scale. Instead, the distribution of durations extends as a powerlaw to the shortest time scale accessible for SPI-ACS, < 50 ms. We also find that a large fraction of long GRBs has a characteristic variability time scale of the order of 1 s. We discuss the possible origin of this time scale., Accepted for publication in A&A
Published: 2012
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20. EUVITA - an extreme UV imaging telescope array with spectral capability

Author: G. Babalyan, M. N. Pavlinsky, J. Biakhowski, O. H. W. Siegmund, A. Zchnder, T. J. L. Courvoisier, F. Stauffacher, J. Platonov, N. Salaschenko, T. Carone, V. A. Aref'ev, P. Bühler, Reinhold Henneck, J. P. Delaboudinière, R. A. Sunyaev, A. Mchedlishvili, N. Schlumpf, Astrid Orr, D.A. Leahy, W. Schoeps, A. Yascovich, and John K. Warren
Subjects: Physics, Atmospheric Science, X-ray astronomy, business.industry, Astrophysics::High Energy Astrophysical Phenomena, Extreme ultraviolet lithography, Astrophysics::Instrumentation and Methods for Astrophysics, Aerospace Engineering, Astronomy, Astronomy and Astrophysics, Field of view, Spectral bands, law.invention, Telescope, Geophysics, Optics, Space and Planetary Science, law, Ultraviolet astronomy, Extreme ultraviolet, General Earth and Planetary Sciences, Satellite, Angular resolution, Detectors and Experimental Techniques, business
Abstract: EUVITA is a set of 8 extreme UV and soft X-ray normal incidence imaging telescopes, each of them sensitive in a narrow band (λ/Δλ=15 to 80), centered at wavelengths between 50 and 175 A. Each telescope has an effective area of a few cm2, a field of view of 1.2° and an angular resolution of 10 arcseconds. EUVITA will be Sown on the Russian mission SPECTRUM X-G. This satellite will be launched in a highly eccentric orbit with a period of 4 days, allowing long, uninterrupted observations (e.g. 105 seconds). The present paper includes an overview of EUVITA's scientific capabilities and a short description of the instrument. Simulations of various types of sources show EUVITA's capability to detect galactic and extragalactic EUV sources. EUVITA's narrow spectral bands allow the measurement of source parameters such as temperature or power law index as well as interstellar absorption, and will resolve groups of strong lines emitted by optically thin hot plasmas.
Published: 1993
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21. Multi-zone warm and cold clumpy absorbers in three Seyfert galaxies

Author: Marc Audard, Volker Beckmann, T. J. L. Courvoisier, Claudio Ricci, APC - Astrophysique des Hautes Energies (APC - AHE), AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Università di Bologna [Bologna] (UNIBO)-Università di Bologna [Bologna] (UNIBO), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), and Beckmann, Volker
Subjects: [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Active galactic nucleus, [SDU.ASTR.HE] Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Radio galaxy, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, EPIC, Power law, 01 natural sciences, Spectral line, Ionization, 0103 physical sciences, Disc, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Luminous infrared galaxy, Physics, 010308 nuclear & particles physics, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astronomy, Torus, Astronomy and Astrophysics, Quasar, Light curve, Galaxy, Dust lane, Space and Planetary Science, Elliptical galaxy, [PHYS.ASTR.HE] Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE]
Abstract: International audience; Aims: We present the first detailed X-ray analysis of three active galactic nuclei, the Seyfert 1 galaxies UGC 3142 and ESO 140-43, and the Seyfert 2 galaxy ESO 383-18, to study the geometry and the physical characteristics of their absorbers. Methods: High-quality XMM-Newton EPIC and RGS data were analyzed as well as Swift/XRT and BAT and INTEGRAL IBIS/ISGRI data to cover the 0.3-110 keV energy range. For ESO 140-43 also XMM-Newton/OM and Swift/UVOT data were used. We studied the variability of the three AGN on a time-scale of seconds using the EPIC/PN light curves, and the long-term time-scale variability of ESO 140-43 using two observations performed six months apart by XMM-Newton. Results: The spectra of the three Seyfert galaxies present a "soft excess" at energies E < 2 keV above a power law continuum that can be modeled by complex absorption, without any additional emission component. The X-ray sources in UGC 3142 and ESO 383-18 are absorbed by two layers of neutral material, with covering fractions f1 ≃ 0.92 and f2 ≃ 0.57 for UGC 3142, and f1 ≃ 0.97 and f2 ≃ 0.86 for ESO 383-18. While the clumpy absorber could be part of a disk wind or of the broad line region for UGC 3142, for ESO 383-18 a clumpy torus plus Compton thin dust lanes are more likely. The spectra of ESO 140-43 can be well fitted with a power law absorbed by three clumpy ionized absorbers with different covering factors, column densities, and ionization parameters, likely part of a moving clumpy system, which could be a disk wind or the broad line region. The strong spectral and flux variability on a time-scale of six months seen in ESO 140-43 is likely due to changes in the moving absorbers. We were able to detect the variation of the covering factor of one of the three ionized absorbers on a kilo-seconds time-scale in the EPIC light-curve of ESO 140-43.
Published: 2010

22. X-ray power law spectra in active galactic nuclei

Author: W. Ishibashi and T. J. L. Courvoisier
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Active galactic nucleus, Photon, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Quasar, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Power law, Galaxy, Spectral line, Accretion (astrophysics), Space and Planetary Science, Spectral slope, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: X-ray spectra of active galactic nuclei (AGN) are usually described as power law spectra, characterized by the spectral slope $\alpha$ or photon index $\Gamma$. Here we discuss the X-ray spectral properties within the framework of clumpy accretion flows, and estimate the power law slope as a function of the source parameters. We expect harder spectra in massive objects than in less massive sources, and steeper spectra in higher accretion rate systems. The predicted values of the photon index cover the range of spectral slopes typically observed in Seyfert galaxies and quasars. The overall trends are consistent with observations, and may account for the positive correlation of the photon index with Eddington ratio (and the possible anticorrelation with black hole mass) observed in different AGN samples. Spectral properties are also closely related to variability properties. We obtain that shorter characteristic time scales are associated with steeper spectra. This agrees with the observed `spectral-timing' correlation., Comment: 6 pages, 1 figure, Astronomy and Astrophysics, accepted
Published: 2010

23. Clumpy accretion flows in active galactic nuclei: X-ray variability and spectral properties

Author: W. Ishibashi, T. J.-L. Courvoisier, A. Comastri, L. Angelini, and M. Cappi
Subjects: Physics, Active galactic nucleus, Photon, Astrophysics::High Energy Astrophysical Phenomena, Spectral density, Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Radiation, Power law, Accretion (astrophysics), Galaxy, Black hole, Astrophysics::Galaxy Astrophysics
Abstract: We discuss the fueling of the central black hole in active galactic nuclei (AGN) in the framework of a clumpy accretion flow. Shocks between elements (clumps) forming the accretion flow are at the origin of the observed radiation. We expect a cascade of shocks, with optically thick shocks giving rise to optical/UV emission and optically thin shocks accounting for the X‐ray emission. We associate the characteristic X‐ray variability time scale derived within our model with the break time scale observed in the X‐ray power spectral density (PSD). The predicted dependence of the variability time scale on black hole mass and accretion rate is in agreement with the observational relation obtained by McHardy et al. (2006). We further discuss X‐ray spectral properties, in particular we compare the predicted hard X‐ray power law slope with observations. Model results are able to reproduce the range of photon index typically measured in Seyfert galaxies and may account for the observed correlation between photon index and normalized accretion rate.
Published: 2010
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24. Synchrotron radio emission in radio-quiet AGNs

Author: W. Ishibashi and T. J.-L. Courvoisier
Subjects: Active galactic nucleus, Radio galaxy, Astrophysics::High Energy Astrophysical Phenomena, Synchrotron radiation, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmology, law.invention, law, 0103 physical sciences, Basso continuo, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Synchrotron, Black hole, Space and Planetary Science, Thermal radiation, Astrophysics of Galaxies (astro-ph.GA), Astrophysics - High Energy Astrophysical Phenomena
Abstract: The basic mechanism responsible for radio emission in radio-loud active galactic nuclei (AGNs) is assumed to be synchrotron radiation. We suggest here that radio emission in radio-quiet objects is also due to synchrotron radiation of particles accelerated in shocks. We consider generic shocks and study the resulting synchrotron properties. We estimate the synchrotron radio luminosity and compare it with the X-ray component produced by inverse Compton emission. We obtain that the radio to X-ray luminosity ratio is much smaller than unity, with values typical of radio-quiet sources. The predicted trends on source parameters, black hole mass and accretion rate, may account for the anticorrelation between radio-loudness and Eddington ratio observed in different AGN samples., Comment: 5 pages, accepted for publication in Astronomy and Astrophysics
Published: 2010
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25. Planck pre-launch status: The Planck-LFI programme

Author: P. B. Lilje, Amedeo Balbi, Fabio Finelli, S. Leach, Roger J. Hoyland, L. A. Wade, Krzysztof M. Gorski, F. Gasparo, E. Franceschi, Luigi Danese, Jose M. Diego, T. Riller, Christopher G. Paine, M. C. Falvella, Hannu Kurki-Suonio, A. Mennella, Francesca Perrotta, Joseph Silk, Matthias Bartelmann, U. Dörl, L. Mendes, A. Bonaldi, Jose Alberto Rubino-Martin, Carlo Burigana, Sabino Matarrese, Anne Lähteenmäki, G. de Zotti, Torsten A. Enßlin, G. Prézeau, M. Bremer, E. Keihänen, M. Prina, S. Galeotta, M. Sandri, G. De Troia, X. Dupac, L. Popa, L. Pérez-Cuevas, S. Donzelli, Althea Wilkinson, Adam Moss, M. Maris, Alessandro Melchiorri, F. Pasian, Kevin M. Huffenberger, R. Hell, J. Dick, Rafael Rebolo, R. J. Davis, Reijo Keskitalo, F. Gomez, M. López-Caniego, Michael Janssen, Ted Kisner, G. Giardino, Luca Terenzi, Davide Maino, Anna Gregorio, M. Tomasi, N. Mandolesi, F. K. Hansen, Pradeep Bhandari, Eduardo Artal, Fabrizio Villa, Enrique Martínez-González, Charles R. Lawrence, Todd Gaier, J. P. Leahy, O. D'Arcangelo, Andrea Zacchei, T. Passvogel, J. Sternberg, Alessandro Gruppuso, F. Matthai, Julian Borrill, Paolo Cabella, S. Ricciardi, Steven Levin, Jörg P. Rachen, Nicola Vittorio, Peter Meinhold, N. Morisset, Marc Türler, Jussi Varis, Marco Bersanelli, R. Rohlfs, A. Nash, Sergi R. Hildebrandt, B. Cappellini, Diego Herranz, J. Marti-Canales, J. González-Nuevo, Martin White, Douglas Scott, George F. Smoot, R. B. Barreiro, N. Roddis, Emanuele Salerno, Michael Seiffert, P. Vielva, S. N. White, Marcella Massardi, J. A. Tauber, F. Cuttaia, Renzo Nesti, T. Poutanen, A. J. Banday, R. C. Butler, R. D. Davies, Robert C. Bowman, S. R. Lowe, José Miguel Herreros, Luca Stringhetti, Paolo Natoli, J. Tuovinen, H. K. Eriksen, Rodrigo Leonardi, David Pearson, Bruce Partridge, T. Jaffe, G. Polenta, Clive Dickinson, G. de Gasperis, M. Frailis, L. De Angelis, Carlo Baccigalupi, Philip Lubin, C. Cantalupo, A. de Rosa, F. Stivoli, Gianluca Morgante, Andrea Zonca, G. Crone, Luca Valenziano, T. J. L. Courvoisier, M. Malaspina, Carlo Sozzi, Graca Rocha, M. Reinecke, A. Simonetto, G. Morigi, K. Bennett, W. Hovest, Department of Physics, Helsinki Institute of Physics, APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), PLANCK, 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), Mandolesi, N, Bersanelli, M, BUTLER R., C, Artal, E, Baccigalupi, C, Balbi, A, BANDAY A., J, BARREIRO R., B, Bartelmann, M, Bennett, K, Bhandari, P, Bonaldi, A, Borrill, J, Bremer, M, Burigana, C, BOWMAN R., C, Cabella, P, Cantalupo, C, Cappellini, B, Courvoisier, T, Crone, G, Cuttaia, F, Danese, L, Darcangelo, O, DAVIES R., D, DAVIS R., J, DE ANGELIS, L, DE GASPERIS, G, DE ROSA, A, DE TROIA, G, DE ZOTTI, G, Dick, J, Dickinson, C, DIEGO J., M, Donzelli, S, Dorl, U, Dupac, X, ENLIN T., A, ERIKSEN H., K, FALVELLA M., C, Finelli, F, Frailis, M, Franceschi, E, Gaier, T, Galeotta, S, Gasparo, F, Giardino, G, Gomez, F, GONZALEZ NUEVO, J, GORSKI K., M, Gregorio, Anna, Gruppuso, A, Hansen, F, Hell, R, Herranz, D, HERREROS J., M, Hildebrandt, S, Hovest, W, Hoyland, R, Huffenberger, K, Janssen, M, Jaffe, T, Keihanen, E, Keskitalo, R, Kisner, T, KURKI SUONIO, H, Lahteenmaki, A, LAWRENCE C., R, M., S, J., Leach, Leahy, P, Leonardi, R, Levin, S, LILJE P., B, LOPEZ CANIEGO, M, LOWE S., R, LUBIN P., M, Maino, D, Malaspina, M, Maris, M, MARTI CANALES, J, MARTINEZ GONZALEZ, E, Massardi, M, Matarrese, S, Matthai, F, Meinhold, P, Melchiorri, A, Mendes, L, Mennella, A, Morgante, G, Morigi, G, Morisset, N, Moss, A, Nash, A, Natoli, P, Nesti, R, Paine, C, Partridge, B, Pasian, F, Passvogel, T, Pearson, D, PEREZ CUEVAS, L, Perrotta, F, Polenta, G, POPA L., A, Poutanen, T, Prezeau, G, Prina, M, RACHEN J., P, Rebolo, R, Reinecke, M, Ricciardi, S, Riller, T, Rocha, G, Roddis, N, Rohlfs, R, RUBINO MARTIN J., A, Salerno, E, Sandri, M, Scott, D, Seiffert, M, Silk, J, Simonetto, A, SMOOT G., F, Sozzi, C, Sternberg, J, Stivoli, F, Stringhetti, L, Tauber, J, Terenzi, L, Tomasi, M, Tuovinen, J, Turler, M, Valenziano, L, Varis, J, Vielva, P, Villa, F, Vittorio, N, Wade, L, White, M, White, S, Wilkinson, A, Zacchei, A, Zonca, A., Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), and Universidad de Cantabria
Subjects: Electromagnetic spectrum, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], submillimeter: generaltelescopes, cosmic microwave background, space vehicles: instruments, submillimeter: general, instrumentation: polarimeters, telescopes, instrumentation: detectors, Cosmic microwave background, data analysis, Astrophysics, general [Submillimeter], 7. Clean energy, 01 natural sciences, LARGE-AREA TELESCOPE, CMB physics, cosmic microwave backgroundin, 010303 astronomy & astrophysics, detectors [Instrumentation], media_common, Physics, Data processing, Planck ESA mission, Galactic and extragalactic asrophysics, Astrophysics::Instrumentation and Methods for Astrophysics, STRAYLIGHT CONTAMINATION, LOW-FREQUENCY INSTRUMENT, DMR SKY MAPS, MICROWAVE BACKGROUND MAPS, galactic and extragalactic astrophysics, symbols, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, GALACTIC FOREGROUNDS, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], COMPONENT SEPARATION, Cosmic microwawe background, media_common.quotation_subject, ANGULAR POWER SPECTRA, education, strumentation: detectors, FOS: Physical sciences, Context (language use), Astrophysics::Cosmology and Extragalactic Astrophysics, 114 Physical sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], instruments [Space vehicles], symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Calibration, Ground segment, Planck, Instrumentation and Methods for Astrophysics (astro-ph.IM), DATA-PROCESSING CENTERS, Remote sensing, polarimeters [Instrumentation], 010308 nuclear & particles physics, Astronomy and Astrophysics, calibration, 115 Astronomy, Space science, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Space and Planetary Science, Sky, NON-GAUSSIANITY, space vehicles, Telescopes
Abstract: 24 páginas, 16 figuras, 5 tablas.-- et al., This paper provides an overview of the Low Frequency Instrument (LFI) programme within the ESA Planck mission. The LFI instrument has been developed to produce high precision maps of the microwave sky at frequencies in the range 27–77 GHz, below the peak of the cosmic microwave background (CMB) radiation spectrum. The scientific goals are described, ranging from fundamental cosmology to Galactic and extragalactic astrophysics. The instrument design and development are outlined, together with the model philosophy and testing strategy. The instrument is presented in the context of the Planck mission. The LFI approach to ground and inflight calibration is described. We also describe the LFI ground segment. We present the results of a number of tests demonstrating the capability of the LFI data processing centre (DPC) to properly reduce and analyse LFI flight data, from telemetry information to calibrated and cleaned time ordered data, sky maps at each frequency (in temperature and polarization), component emission maps (CMB and diffuse foregrounds), catalogs for various classes of sources (the Early Release Compact Source Catalogue and the Final Compact Source Catalogue). The organization of the LFI consortium is briefly presented as well as the role of the core team in data analysis and scientific exploitation. All tests carried out on the LFI flight model demonstrate the excellent performance of the instrument and its various subunits. The data analysis pipeline has been tested and its main steps verified. In the first three months after launch, the commissioning, calibration, performance, and verification phases will be completed, after which Planck will begin its operational life, in which LFI will have an integral part., The Planck-LFI project is developed by an International Consortium led by Italy and involving Canada, Finland, Germany, Norway, Spain, Switzerland, UK and USA. The Italian contribution to Planck is supported by the Agenzia Spaziale Italiana (ASI) and INAF. We also wish to thank the many people of the Herschel/Planck Project and RSSD of ESA, ASI, THALES Alenia Space Industries and the LFI Consortium that have contributed to the realization of LFI. We are grateful to our HFI colleagues for such a fruitful collaboration during so many years of common work. The German participation at the Max-Planck-Institut für Astrophysik is funded by the Bundesministerium für Wirtschaft und Technologie through the Raumfahrt- Agentur of the Deutsches Zentrum für Luft- und Raumfahrt (DLR) [FKZ: 50 OP 0901] and by the Max-Planck-Gesellschaft (MPG). The Finnish contribution is supported by the Finnish Funding Agency for Technology and Innovation (Tekes) and the Academy of Finland. The Spanish participation is funded by Ministerio de Ciencia e Innovacion through the project ESP2004-07067-C03 and AYA2007-68058-C03. The UK contribution is supported by the Science and Technology Facilities Council (STFC). C. Baccigalupi and F. Perrotta acknowledge partial support of the NASA LTSA Grant NNG04CG90G.
Published: 2010
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26. The unified scheme seen with INTEGRAL detected AGN

Author: Volker Beckmann, S. Soldi, C. Ricci, T. J.-L. Courvoisier, J. Alfonso-Garzón, A. Domingo, J. M. Mas-Hesse, P. Lubiński, A. A. Zdziarski, N. Gehrels, A. Comastri, L. Angelini, M. Cappi, APC - Astrophysique des Hautes Energies (APC - AHE), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, NASA Goddard Space Flight Center (GSFC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Università di Bologna [Bologna] (UNIBO)-Università di Bologna [Bologna] (UNIBO), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Dipartimento di Astronomia, Universita degli Studi di Bologna, and Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO)
Subjects: Brightness, X-ray spectra, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], circumnuclear matter, Astrophysics::High Energy Astrophysical Phenomena, brightness, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, active or peculiar galaxies, and systems, Spectral line, objects, X-ray, Inclination angle, luminosities, Magnitudes and colors, Quasars, Astrophysics::Galaxy Astrophysics, Physics, Seyfert galaxies, Black holes, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astronomy, Quasar, Unified Model, Galaxy, Galactic nuclei, Reflection (physics), and bulges, X ray spectra
Abstract: International audience; The INTEGRAL mission provides a large data set for studying the hard X-ray properties of AGN and allows to test the unified scheme for AGN. We present results based on the analysis of 199 AGN. A difference between the Seyfert types is detected in slightly flatter spectra with higher cut-off energies and lower luminosities for the type 2 AGN. When applying a Compton reflection model, the underlying continua (Γ~=1.95) appear the same in Seyfert 1 and 2, and the reflection strength is R~=1 in both cases, with differences in the inclination angle only. More luminous objects appear to be more massive and there is also a general trend for the absorbed sources and type 2 AGN to have lower Eddington ratios. The number counts are consistent with no evolution of the observed AGN. The unified model for Seyfert galaxies seems to hold, showing in hard X-rays that the central engine is the same in Seyfert 1 and 2 galaxies, seen under different inclination angle and absorption.
Published: 2009
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27. Compton Reflection in AGN with Simbol-X

Author: V. Beckmann, T. J.-L. Courvoisier, N. Gehrels, P. Lubiński, J. Malzac, P. O. Petrucci, C. R. Shrader, S. Soldi, Jéro^me Rodriguez, Phillippe Ferrando, ISDC Data Centre for Astrophysics, University of Geneva [Switzerland], NASA Goddard Space Flight Center (GSFC), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), 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), Laboratoire d'Astrophysique de Grenoble (LAOG), and Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], circumnuclear matter, Astrophysics::High Energy Astrophysical Phenomena, Continuum (design consultancy), Cosmic background radiation, FOS: Physical sciences, Cosmic ray, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Spectral line, X-ray, cosmic rays, muon, Neutrino, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Line (formation), High Energy Astrophysical Phenomena (astro-ph.HE), Physics, COSMIC cancer database, 010308 nuclear & particles physics, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], pion, and other elementary particles, Astrophysics - Astrophysics of Galaxies, Astrophysics of Galaxies (astro-ph.GA), Galactic nuclei, Reflection (physics), Astrophysics - High Energy Astrophysical Phenomena, and bulges
Abstract: AGN exhibit complex hard X-ray spectra. Our current understanding is that the emission is dominated by inverse Compton processes which take place in the corona above the accretion disk, and that absorption and reflection in a distant absorber play a major role. These processes can be directly observed through the shape of the continuum, the Compton reflection hump around 30 keV, and the iron fluorescence line at 6.4 keV. We demonstrate the capabilities of Simbol-X to constrain complex models for cases like MCG-05-23-016, NGC 4151, NGC 2110, and NGC 4051 in short (10 ksec) observations. We compare the simulations with recent observations on these sources by INTEGRAL, Swift and Suzaku. Constraining reflection models for AGN with Simbol-X will help us to get a clear view of the processes and geometry near to the central engine in AGN, and will give insight to which sources are responsible for the Cosmic X-ray background at energies above 20 keV., 4 pages, 1 figure, to appear in the proceedings of the second Simbol-X Symposium "Simbol-X - Focusing on the Hard X-ray Universe", AIP Conf. Proc. Series, P. Ferrando and J. Rodriguez eds
Published: 2009
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28. Extragalactic Hard X-ray Surveys: From INTEGRAL to Simbol-X

Author: S. Paltani, T. Dwelly, R. Walter, I. M. McHardy, T. J.-L. Courvoisier, Jéro^me Rodriguez, and Phillippe Ferrando
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, education.field_of_study, COSMIC cancer database, Astrophysics::High Energy Astrophysical Phenomena, Population, X-ray, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics - Astrophysics of Galaxies, Redshift, Luminosity, Astrophysics of Galaxies (astro-ph.GA), Satellite, Astrophysics - High Energy Astrophysical Phenomena, education, Astrophysics::Galaxy Astrophysics, Galaxy cluster
Abstract: We present some results of the deepest extragalactic survey performed by the INTEGRAL satellite. The fraction of very absorbed AGN is quite large. The sharp decrease in the absorption fraction with X-ray luminosity observed at lower-energy X-rays is not observed. The current lack of truly Compton-thick objects, with an upper limit of 14% to the size of this population, is just compatible with recent modeling of the cosmic X-ray background. We also study the prospects for a future hard X-ray serendipitous survey with Simbol-X. We show that Simbol-X will easily detect a large number of serendipitous AGN, allowing us to study the evolution of AGN up to redshifts about 2, opening the door to the cosmological study of hard X-ray selected AGN, which is barely possible with existing satellites like Swift and INTEGRAL., Proceedings of the 2nd Simbol-X symposium: "Simbol-X - Focusing on the Hard X-ray Universe", AIP Conf. Proc. Series, 4 pages. Fixed affiliations
Published: 2009
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29. The Multi-component X-ray Emission of 3C 273

Author: S. Soldi, M. Türler, S. Paltani, T. J.-L. Courvoisier, Jéro^me Rodriguez, and Phillippe Ferrando
Subjects: Physics, Jet (fluid), Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, Gamma ray, Flux, Astronomy, Quasar, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy, Superposition principle, Sky, Astrophysics::Galaxy Astrophysics, Galaxy cluster, media_common
Abstract: 3C 273 is the brightest quasar in the sky and among the most extensively observed and studied AGN, therefore one of the most suitable targets for a long‐term, multi‐frequency study. The superposition of a thermal Comptonisation component, similar to that observed in Seyfert galaxies, and of a non‐thermal component, related to the jet emission, seems to explain some of the spectral and timing properties of the X‐ray emission of 3C 273. Yet, during some observations this dichotomy has not been observed and the variability properties could also be consistent with a single‐component scenario, characterised by two parameters varying independently. In order to understand the nature of the X‐ray emission in 3C 273, a series of observations up to 80–100 keV, possibly catching the source in different flux states, are essential. Simbol‐X will be able to study the emission of 3C 273 in the broad 0.5–80 keV band with high sensitivity, allowing us to disentangle the emission from different spectral components, with 20...
Published: 2009
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30. Hard X-ray Emission from Galaxy Clusters Observed with INTEGRAL and Prospects for Simbol-X

Author: D. Eckert, S. Paltani, T. J.-L. Courvoisier, Jéro^me Rodriguez, and Phillippe Ferrando
Subjects: Physics, Field (physics), Scattering, Astrophysics::High Energy Astrophysical Phenomena, Cosmic microwave background, Astronomy, Synchrotron radiation, Angular resolution, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Electron, Galaxy cluster, Magnetic field
Abstract: Some galaxy clusters are known to contain a large population of relativistic electrons, which produce radio emission through synchrotron radiation. Therefore, it is expected that inverse‐Compton scattering of the relativistic electrons with the CMB produce non‐thermal emission which should be observable in the hard X‐ray domain. Here we focus on the recent results by INTEGRAL, which shed a new light on the non‐thermal emission thanks to its angular resolution and sensitivity in the hard X‐ray range. We also present the exciting prospects in this field for Simbol‐X, which will allow us to detect the non‐thermal emission in a number of clusters and map the magnetic field throughout the intra‐cluster medium.
Published: 2009
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31. AGN's UV and X-ray luminosities in clumpy accretion flows

Author: T. J. L. Courvoisier and W. Ishibashi
Subjects: Physics, Active galactic nucleus, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), X-ray, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Accretion (astrophysics), Space and Planetary Science, Cascade, Astrophysics::Galaxy Astrophysics
Abstract: We consider the fuelling of the central massive black hole in Active Galactic Nuclei, through an inhomogeneous accretion flow. Performing simple analytical treatments, we show that shocks between elements (clumps) forming the accretion flow may account for the UV and X-ray emission in AGNs. In this picture, a cascade of shocks is expected, where optically thick shocks give rise to optical/UV emission, while optically thin shocks give rise to X-ray emission. The resulting blue bump temperature is found to be quite similar in different AGNs. We obtain that the ratio of X-ray luminosity to UV luminosity is smaller than unity, and that this ratio is smaller in massive objects compared to less massive sources. This is in agreement with the observed $L_{X}/L_{UV}$ ratio and suggests a possible interpretation of the $\alpha_{OX}-l_{UV}$ anticorrelation., Comment: 8 pages, 1 figure, accepted for publication in A&A
Published: 2008
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32. Average hard X‐ray emission from NS LMXBs

Author: Osmi Vilhu, Sandro Mereghetti, Volker Beckmann, J. Rodriguez, E. Kuulkers, A. Bazzano, P. Goldoni, Filippo Frontera, A. Paizis, Lev Titarchuk, R. Farinelli, and T. J. L. Courvoisier
Subjects: Physics, Neutron star, Accretion (meteorology), Bulge, Astrophysics::High Energy Astrophysical Phenomena, X-ray binary, Astronomy, Magnetosphere, Astrophysics, Electron, Spectral line, Luminosity
Abstract: We studied and compared the long term average hard X‐ray (>20 keV) spectra of a sample of twelve bright low‐mass X‐ray binaries hosting a neutron star (NS). Our sample comprises the six well studied Galactic Z sources and six Atoll sources, four of which are bright (“GX”) bulge sources while two are weaker ones in the 2–10 keV range (H 1750‐440 and H 1608‐55). For all the sources of our sample, we analysed available public data and extracted average spectra from the IBIS/ISGRI detector on board INTEGRAL. We extend the detection of H 1750‐440 up to 150 keV and discover a hard tail in the spectrum of the Atoll source GX 13+1. We can describe all the spectral states as well as the long known variability of the hard X‐ray tails detected in some of these objects in terms of the bulk motion Comptonisation scenario. We find evidence that bulk motion, at the origin of the hard X‐ray tail, is always present, its strength is related to the accretion rate and it is suppressed only in the presence of high local luminosity. Using radio data from the literature we find, in all Z sources and bright “GX” Atolls, a systematic positive correlation between the X‐ray hard tail (40–100 keV) and the radio luminosity. This suggests that hard tails and energetic electrons causing the radio emission may have the same origin, most likely the Compton cloud located inside the NS magnetosphere.
Published: 2007
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33. INTEGRAL observations of the blazar 3C454.3 in outburst

Author: René Hudec, G. Di Cocco, Laura Maraschi, C. M. Raiteri, Lars Fuhrmann, Gabriele Ghisellini, T. J. L. Courvoisier, Massimo Persic, Elena Pian, Simona Soldi, T. Pursimo, R. Walter, Luigi Foschini, P. Giommi, Giuseppe Malaguti, N. Gehrels, M. Villata, Volker Beckmann, G. Tagliaferri, Fabrizio Tavecchio, Aldo Treves, M. Turler, Merja Tornikoski, G. Tosti, and P. Barr
Subjects: Physics, Active galactic nucleus, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Compton scattering, Synchrotron radiation, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, law.invention, Wavelength, Space and Planetary Science, law, Spectral energy distribution, Blazar, Line (formation), Flare
Abstract: In Spring 2005, the blazar 3C454.3 underwent a dramatic outburst at all wavelengths from mm to X-rays. This prompted INTEGRAL observations, accomplished in 15-18 May 2005. The source was detected by the INTEGRAL instruments from 3 to 200 keV in a bright state (~5 x 10E-10 cgs), at least a factor of 2-3 higher than previously observed. This is one of the brightest blazar detections achieved by INTEGRAL. During the 2.5 days of INTEGRAL monitoring, we detected a ~20% decrease in the hard X-rays (20-40 keV), indicating that we have sampled the decaying part of the flare. The decrease is less apparent in the soft X-rays (5-15 keV). The simultaneous optical variations are weakly correlated with those at soft X-rays, and not clearly correlated with those at hard X-rays. The spectral energy distribution exhibits two components, as typically seen in blazars, which can be modeled with synchrotron radiation and inverse Compton scattering occurring in a region external to the broad line region., 5 pages, 3 eps figures, in press in A&A Letters
Published: 2006

34. A Possible Feature of the Thermal Matter in Relativistic Jets in Radio-Loud Quasars

Author: T. J. L. Courvoisier, J. M. Wang, and R. Staubert
Subjects: Physics, Astrophysical jet, Feature (computer vision), Thermal, Quasar, Astrophysics
Published: 2005
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35. The INTEGRAL mission an overview

Author: G. Di Cocco, T. J. L. Courvoisier, R. A. Sunyaev, N. Gehrels, J. A. Paul, Peter Kretschmar, Christoph Winkler, P. Ubertini, Roland Diehl, G. G. C. Palumbo, Niels Lund, Francois Lebrun, S. A. Grebenev, W. Hermsen, J. P. Roques, Bonnard J. Teegarden, J. M. Mas-Hesse, European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), 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, 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), National Space Institute [Lyngby] (DTU Space), Technical University of Denmark [Lyngby] (DTU), Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Istituto di Astrofisica Spaziale e Fisica cosmica - Roma (IASF-Roma), Istituto Nazionale di Astrofisica (INAF), E. J. A. Meurs & G. Fabbiano, INTEGRAL, Kretschmar P., Winkler C., Courvoisier T. J.-L., di Cocco G., Diehl R., Gehrels N., Grebenev S., Hermsen W., Mas-Hesse J. M., Lebrun F., Lund N., Palumbo G. G. C., Paul J., Roques J.-P., Sunyaev R., Teegarden B., Ubertini P., 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 Midi-Pyrénées (OMP), 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)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Agence Spatiale Européenne = European Space Agency (ESA), 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), Danmarks Tekniske Universitet = Technical University of Denmark (DTU), 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), and 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)
Subjects: Physics, High energy, 010504 meteorology & atmospheric sciences, Spectrometer, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], business.industry, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, High resolution, Astronomy and Astrophysics, X-rays: stars, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Optics, Space and Planetary Science, Observatory, 0103 physical sciences, High spatial resolution, business, Spectroscopy, 010303 astronomy & astrophysics, High resolution imaging, Energy (signal processing), gamma rays: observations, 0105 earth and related environmental sciences
Abstract: International audience; The ESA observatory INTEGRAL (International Gamma-Ray Astrophysics Laboratory) is dedicated to fine imaging and spectroscopy in the energy range 15 keV to 10 Mev with concurrent X-ray (3-35 keV) and optical monitoring. It was launched on October 17, 2002 and has been succesfully operating ever since. Its two main instruments the spectrometer SPI - optimized for high resolution spectroscopy - and the imager IBIS - optimized for for high resolution imaging - are complemented by the X-ray monitor JEM-X and the optical monitor OMC. All the high energy instruments use coded mask techniques, allowing imaging in the gamma-ray range and combining wide fields of view with high spatial resolution. The presentation gives an overview of the unique properties of INTEGRAL.
Published: 2005
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36. INTEGRAL observations of AGN in the Galactic Plane

Author: A. C. Fabian, A. J. Dean, A. de Rosa, Angela Malizia, Simona Soldi, Loredana Bassani, R. Walter, Raffaella Landi, T. J. L. Courvoisier, and Volker Beckmann
Subjects: Physics, Spectral index, Radio galaxy, Centaurus A, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Galactic plane, Power law, Galaxy, Spectral line, Space and Planetary Science, Circinus
Abstract: We present results on approximately one year of INTEGRAL observations of six AGN detected during the regular scans of the Galactic Plane. The sample is composed by five Seyfert 2 objects (MCG -05-23-16, NGC 4945, the Circinus galaxy, NGC 6300, ESO 103-G35) and the radio galaxy Centaurus A. The continuum emission of each of these sources is well represented by a highly absorbed (NH > 1e22 1/cm^2) power law, with average spectral index Gamma = 1.9 +/- 0.3. A high energy exponential cut-off at Ec ~ 50 keV is required to fit the spectrum of the Circinus galaxy, whereas a lower limit of 130 keV has been found for NGC 4945 and no cut-off has been detected for NGC 6300 in the energy range covered by these INTEGRAL data. The flux of Centaurus A was found to vary by a factor of ~ 2 in 10 months, showing a spectral change between the high and low state, which can be modelled equally well by a change in the absorption (NH from 17e22 to 33e22 1/cm^2) or by the presence of a cut-off at >~ 120 keV in the low state spectrum. A comparison with recently reprocessed BeppoSAX/PDS data shows a general agreement with INTEGRAL results. The high energy cut-off in the hard X-ray spectra appears to be a common but not universal characteristic of Seyfert 2 and to span a wide range of energies., 12 pages, 12 figures, accepted for publication in A&A
Published: 2005
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37. MAX, a Laue diffraction lens for nuclear astrophysics

Author: G. Weidenspointner, Ken Haste Andersen, Cornelia B. Wunderer, B. Smither, P. Courtois, J. M. Alvarez, P. von Ballmoos, Hubert Halloin, P. Jean, G. K. Skinner, G. Vedrenne, Michael J. Harris, Nicolas M. Barrière, P. Ubertini, Steven E. Boggs, Nikolay V. Abrosimov, M. Hernanz, Jürgen Knödlseder, Jordi Isern, T. J. L. Courvoisier, Pierre Bastie, Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-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), Institut Laue-Langevin (ILL), ILL, Observatoire Midi-Pyrénées (OMP), 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)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, 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), 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), 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, and 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)
Subjects: Diffraction, Photon, Astrophysics::High Energy Astrophysical Phenomena, 7. Clean energy, 01 natural sciences, law.invention, Telescope, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Optics, law, 0103 physical sciences, Nuclear astrophysics, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], Focal length, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010303 astronomy & astrophysics, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, business.industry, Detector, Instrumentation: Gamma-ray Laue lens, Gamma-ray astrophysics, Astronomy and Astrophysics, Polarization (waves), Mosaic crystals, 95.55.Ka, 61.50.Ah, 61.10.-i, 41.50.+h, Space and Planetary Science, X-ray crystallography, business
Abstract: The next generation of instrumentation for nuclear astrophysics will have to achieve a factor of 10–100 improvement in sensitivity over present technologies. With the focusing gamma-ray telescope MAX we take up this challenge: combining unprecedented sensitivity with high spectral and angular resolution, and the capability of measuring the polarization of the incident photons. The feasibility of such a crystal diffraction gamma-ray lens has recently been demonstrated with the prototype lens CLAIRE. MAX is a proposed mission which will make use of satellite formation flight to achieve 86 m focal length, with the Laue lens being carried by one satellite and the detector by the other. In the current design, the Laue diffraction lens of MAX will consist of 13740 copper and germanium (Ge1−x Si x , x ∼ 0.02) crystal tiles arranged on 36 concentric rings. It simultaneously focuses in two energy bands, each centred on one of the main scientific objectives of the mission: the 800–900 keV band is dedicated to the study of nuclear gamma-ray lines from type Ia supernovae (e.g. 56 Co decay line at 847 keV) while the 450–530 keV band focuses on electron-positron annihilation (511 keV emission) from the Galactic centre region with the aim of resolving potential point sources. MAX promises a breakthrough in the study of point sources at gamma-ray energies by combining high narrow-line sensitivity (better than 10−6 cm−2 s−1) and high energy resolution (E/dE ∼ 500). The mission has successfully undergone a pre-phase A study with the French Space Agency CNES, and continues to evolve: new diffracting materials such as bent or composite crystals seem very promising.
Published: 2005
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38. INTEGRAL/RXTE Observations of Cygnus X-1

Author: Guy G. Pooley, Katja Pottschmidt, V. Schönfelder, Peter Kretschmar, Rüdiger Staubert, A. A. Zdziarski, Jörn Wilms, T. Gleissner, S. Martínez-Núñez, Michael A. Nowak, Jerome Rodriguez, T. J. L. Courvoisier, Maria Chernyakova, and Volker Beckmann
Subjects: Black hole physics, Individual stars, Cyg X-1, Gamma rays, X-rays observations, Binaries, Astrophysics::High Energy Astrophysical Phenomena, Phase (waves), FOS: Physical sciences, Flux, 02 engineering and technology, Astrophysics, UNESCO::ASTRONOMÍA Y ASTROFÍSICA, 01 natural sciences, Omega, Spectral line, Ionization, 0103 physical sciences, Optical depth (astrophysics), 0202 electrical engineering, electronic engineering, information engineering, Calibration, 010303 astronomy & astrophysics, Optical depth, Physics, 010308 nuclear & particles physics, Astrophysics (astro-ph), Gamma ray, Astronomy, Astronomy and Astrophysics, 020206 networking & telecommunications, ASTRONOMÍA Y ASTROFÍSICA::Cosmología y cosmogonia [UNESCO], Corona, Space and Planetary Science, Reflection (physics), 020201 artificial intelligence & image processing, UNESCO::ASTRONOMÍA Y ASTROFÍSICA::Cosmología y cosmogonia, ASTRONOMÍA Y ASTROFÍSICA [UNESCO]
Abstract: We present first results from contemporaneous observations of Cygnus X-1 with INTEGRAL and RXTE, made during INTEGRAL's performance verification phase in 2002 November and December. Consistent with earlier results, the 3-250 keV data are well described by Comptonization spectra from a Compton corona with a temperature of kT~50-90 keV and an optical depth of tau~1.0-1.3 plus reflection from a cold or mildly ionized slab with a covering factor of Omega/2pi~0.2-0.3. A soft excess below 10 keV, interpreted as emission from the accretion disk, is seen to decrease during the 1.5 months spanned by our observations. Our results indicate a remarkable consistency among the independently calibrated detectors, with the remaining issues being mainly related to the flux calibration of INTEGRAL., Comment: 6 pages, 3 figures. Figs. 2 and 3 are best viewed in color. Accepted for publication in the INTEGRAL special edition of A&AL
Published: 2004
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39. The Peculiar X-ray Transient IGR 16358-4726

Author: S. K. Patel, C. Kouveliotou, A. Tennant, P. M. Woods, A. King, M. H. Finger, P. Ubertini, C. Winkler, T. J.-L. Courvoisier, M. van der Klis, S. Wachter, B. M. Gaensler, C. J. Phillips, High Energy Astrophys. & Astropart. Phys (API, FNWI), and API (FNWI)
Subjects: Physics, X-ray transient, Astrophysics (astro-ph), Flux, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Orbital period, Luminosity, Neutron star, Pulsar, Space and Planetary Science, Observatory, Low Mass
Abstract: The new transient IGR 16358-4726 was discovered on 2003 March 19 with INTEGRAL. We detected the source serendipitously during our 2003 March 24 observation of SGR 1627-41 with the Chandra X-ray Observatory at the 1.7 x 10^{-10} ergs s^{-1} cm^{-2} flux level (2-10 keV) with a very high absorption column (N_H=3.3(1) x 10^{23} cm^{-2}) and a hard power law spectrum of index 0.5(1). We discovered a very strong flux modulation with a period of 5880(50) s and peak-to-peak pulse fraction of 70(6)% (2-10 keV), clearly visible in the x-ray data. The nature of IGR 16358-4726 remains unresolved. The only neutron star systems known with similar spin periods are low luminosity persistent wind-fed pulsars; if this is a spin period, this transient is a new kind of object. If this is an orbital period, then the system could be a compact Low Mass X-ray Binary (LMXB)., Comment: 4 pages, 3 figures, Submitted to The Astrophysical Journal Letters
Published: 2003
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40. The intrinsic emission of Seyfert galaxies observed with BeppoSAX/PDS I. Comparison of the average spectra of the three classes of Seyfert Galaxies

Author: T. J.-L. Courvoisier and S. Deluit
Subjects: Physics, Reflection (mathematics), Space and Planetary Science, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Galaxy, Spectral line
Abstract: We present a study of the hard X-ray spectrum (>15 keV) of different classes of Seyfert galaxies observed with BeppoSAX/PDS. Using hard X-ray data, we avoid absorption effects modifying the Seyfert emission and have direct access to the central engine of these sources. The aim of this study is first to characterize the general properties of the hard X-ray spectrum of Seyfert 1, 1.5 and 2 galaxies and secondly to compare their intrinsic emission to test unified models according to which all the classes have the same nucleus. We compute the average spectrum of 14 Sy 1, 9 Sy 1.5 and 22 Sy 2 galaxies observed by the PDS (15-136 keV). The average spectrum of Sy 1 differs from that of Sy 2, the first requiring the presence of a high energy cutoff which is absent in the second. We also show that the reflection component is possibly more important in the Sy 2 emission. The nature of Sy 1.5 galaxies is ambiguous as they have a negligible reflection component (like Sy 1) and do not require a cutoff (like Sy 2), 14 pages, 23 figures
Published: 2003
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41. Time resolved spectroscopy of GRB030501 using INTEGRAL

Author: Volker Beckmann, J. Borkowski, T. J. L. Courvoisier, Sandro Mereghetti, F. Hroch, Claudia Wigger, Niels Lund, D. Goetz, René Hudec, and S. E. Shaw
Subjects: Physics, Nuclear and High Energy Physics, Photon, Astrophysics::High Energy Astrophysical Phenomena, Resolution (electron density), Astrophysics (astro-ph), Flux, FOS: Physical sciences, Field of view, Astrophysics, Atomic and Molecular Physics, and Optics, Emission spectrum, Time-resolved spectroscopy, Gamma-ray burst, Spectroscopy
Abstract: The Gamma-ray instruments on-board INTEGRAL offer an unique opportunity to perform time resolved analysis on GRBs. The imager IBIS allows accurate positiioning of GRBs and broad band spectral analysis, while SPI provides high resolution spectroscopy. GRB 030501 was discovered by the INTEGRAL Burst Alert System in the ISGRI field of view. Although the burst was fairly weak (fluence F = 3.5 * 10^-6 erg cm^-2 in the 20-200 keV energy band) it was possible to perform time resolved spectroscopy with a resolution of a few seconds. The GRB shows a spectrum in the 20 - 400 keV range which is consistent with a spectral photon index of -1.7. No emission line or spectral break was detectable in the spectrum. Although the flux seems to be correlated with the hardness of the GRB spectrum, there is no clear soft to hard evolution seen over the duration of the burst. The INTEGRAL data have been compared with results from the Ulysses and RHESSI experiments., Comment: 4 pages, 5 figures, accepted for publication in Astronomy & Astrophysics
Published: 2003
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42. ISOPHOT Observations of Narrow-Line Seyfert 1 Galaxies

Author: T. J. L. Courvoisier and M. Polletta
Subjects: Physics, Line-of-sight, Opacity, Infrared, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Infrared spectroscopy, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy, Micrometre, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Absorption (electromagnetic radiation), Astrophysics::Galaxy Astrophysics, Line (formation)
Abstract: Broad infrared spectra (7-200 micrometer) of four NLS1 galaxies, obtained with the imaging photo-polarimeter (ISOPHOT) on board the Infrared Space Observatory (ISO), are presented. The infrared luminosities and temperatures, opacities and sizes of the emitting dust components are derived. A comparison between the observed infrared spectra and the optical emission line fluxes of a sample of 16 NLS1 galaxies suggests that these objects suffer different degrees of dust absorption according to the inclination of the line of sight with respect to the dust distribution., Comment: Contributed talk presented at the Joint MPE,AIP,ESO workshop on NLS1s, Bad Honnef, Dec. 1999, to appear in New Astronomy Reviews; also available at http://wave.xray.mpe.mpg.de/conferences/nls1-workshop
Published: 2000
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43. Multi-wavelength Observations of 3C 273 in 1993-1995

Author: C. von Montigny, H. Aller, M. Aller, F. Bruhweiler, W. Collmar, T. J.‐L. Courvoisier, P. G. Edwards, C. E. Fichtel, A. Fruscione, G. Ghisellini, R. C. Hartman, W. N. Johnson, M. Kafatos, T. Kii, D. A. Kniffen, G. G. Lichti, F. Makino, K. Mannheim, A. P. Marscher, B. McBreen, I. McHardy, J. E. Pesce, M. Pohl, E. Ramos, W. Reich, E. I. Robson, K. Sasaki, H. Terasranta, M. Tornikoski, C. M. Urry, E. Valtaoja, S. Wagner, and T. Weekes
Subjects: Physics, Spectral index, Photon, Active galactic nucleus, Proton, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Flux, Astronomy and Astrophysics, Quasar, Astrophysics, Radiation, 01 natural sciences, Synchrotron, law.invention, Space and Planetary Science, law, 0103 physical sciences, 010306 general physics, 010303 astronomy & astrophysics
Abstract: We present the results of the multi-wavelength campaigns on 3C 273 in 1993-1995. During the observations in late 1993 this quasar showed an increase of its flux for energies greater equal 100 MeV from about 2.1 x 10^-7 photons/cm^2/s to approximately 5.6 x 10^-7 photons/cm^2/s during a radio outburst at 14.5, 22 and 37 GHz. However, no one-to-one correlation of the gamma-ray radiation with any frequency could be found. The photon spectral index of the high energy spectrum changed from (3.20 +- 0.54) to (2.20 +- 0.22) in the sense that the spectrum flattened when the gamma-ray flux increased. Fits of the three most prominent models (synchrotron self-Comptonization, external inverse Comptonization and the proton initiated cascade model) for the explanation of the high gamma-ray emission of active galactic nuclei were performed to the multi-wavelength spectrum of 3C 273. All three models are able to represent the basic features of the multi-wavelength spectrum. Although there are some differences the data are still not decisive enough to discriminate between the models., 63 pages including 9 eps figures and 9 tables, LateX, uses aaspp4.sty and tighten.sty, accepted for publication in ApJ
Published: 1997

44. Principal Component Analysis of the CIV λ1549 Emission-Line in Active Galactic Nuclei

Author: M. Türler and T. J.-L. Courvoisier
Subjects: Physics, Active galactic nucleus, Astrophysics::High Energy Astrophysical Phenomena, Principal component analysis, Satellite, Astrophysics::Cosmology and Extragalactic Astrophysics, Emission spectrum, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We apply a principal component analysis (PCA) to the CIV λ1549 emission-line of 18 active galactic nuclei (AGN) observed more than 15 times with the IUE satellite from 1978 to 1991. The PCA method is described and some qualitative results are discussed. A more quantitative study is in preparation (Turler & Courvoisier 1997).
Published: 1997
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45. Relationship between X-ray and ultraviolet emission in 3C 273

Author: S. Paltani, M. Turler, R. Walter, and T. J. L. Courvoisier
Subjects: Physics, Nuclear and High Energy Physics, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), X-ray, Flux, FOS: Physical sciences, Astrophysics, medicine.disease_cause, Corona, Atomic and Molecular Physics, and Optics, medicine, Ultraviolet
Abstract: In 3C 273, ultraviolet flux and X-ray flux measured by BATSE are not well correlated, contrarily to predictions of several models, unless the X-ray flux lags the UV emission by 1.75 yr. The absence of observed correlation at small lag cannot be due to spectral variability. A Comptonizing corona model is however compatible with all UV and X-ray observations covering the BATSE period., Comment: LaTeX, 4 pages, 6 figures. espcrc2.sty style file included. Poster contribution to the symposium "The Active X-ray Sky: Results from BepppoSAX and Rossi-XTE", Rome, October 1997
Published: 1997
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46. A Deep Study of the 3C 273 Field in $\gamma$-rays

Author: P. H. Hauschildt, T. J. L. Courvoisier, I. Kreykenbohm, P. Lubinski, I. Brott, and Nicolas Produit
Subjects: Physics, Field (physics), Space and Planetary Science, Gamma ray, Astronomy, Astronomy and Astrophysics
Published: 2005
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47. Ground-Based Observations of PKS2155-304 in November 1991

Author: A. Blecha, T. J.-L. Courvoisier, H. D. Aller, M. F. Aller, P. Bouchet, P. Bratschi, M. T. Carini, M. Donahue, E. D. Feigelson, A. V. Filippenko, I. S. Glass, J. Heidt, P. A. Hughes, R. I. Kollgaard, T. Matheson, H. R. Miller, J. C. Noble, P. S. Smith, and S. Wagner
Published: 1994
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48. Simultaneous Observations of Seyfert 1 Galaxies with IUE, ROSAT and GINGA

Author: A. Orr, R. Walter, T. J.-L Courvoisier, H. H. Fink, F. Makino, C. Otani, and W. Wamsteker
Published: 1994
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49. ROSAT Spectra of Quasars

Author: P. Bühler, T. J.-L. Courvoisier, R. Staubert, H. Brunner, and G. Lamer
Published: 1994
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50. Spectral Variability of 3C 273 at soft X-rays

Author: R. Staubert, T. J.-L. Courvoisier, H. Fink, M.-H. Ulrich, H. Brunner, S. Friedrich, and K. Otterbein
Published: 1994
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