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1. Search for Gravitational Waves Associated with Fast Radio Bursts Detected by CHIME/FRB during the LIGO–Virgo Observing Run O3a

Author: R. Abbott, T. D. Abbott, F. Acernese, K. Ackley, C. Adams, N. Adhikari, R. X. Adhikari, V. B. Adya, C. Affeldt, D. Agarwal, M. Agathos, K. Agatsuma, N. Aggarwal, O. D. Aguiar, L. Aiello, A. Ain, P. Ajith, T. Akutsu, S. Albanesi, A. Allocca, P. A. Altin, A. Amato, C. Anand, S. Anand, A. Ananyeva, S. B. Anderson, W. G. Anderson, M. Ando, T. Andrade, N. Andres, T. Andrić, S. V. Angelova, S. Ansoldi, J. M. Antelis, S. Antier, S. Appert, Koji Arai, Koya Arai, Y. Arai, S. Araki, A. Araya, M. C. Araya, J. S. Areeda, M. Arène, N. Aritomi, N. Arnaud, S. M. Aronson, K. G. Arun, H. Asada, Y. Asali, G. Ashton, Y. Aso, M. Assiduo, S. M. Aston, P. Astone, F. Aubin, C. Austin, S. Babak, F. Badaracco, M. K. M. Bader, C. Badger, S. Bae, Y. Bae, A. M. Baer, S. Bagnasco, Y. Bai, L. Baiotti, J. Baird, R. Bajpai, M. Ball, G. Ballardin, S. W. Ballmer, A. Balsamo, G. Baltus, S. Banagiri, D. Bankar, J. C. Barayoga, C. Barbieri, B. C. Barish, D. Barker, P. Barneo, F. Barone, B. Barr, L. Barsotti, M. Barsuglia, D. Barta, J. Bartlett, M. A. Barton, I. Bartos, R. Bassiri, A. Basti, M. Bawaj, J. C. Bayley, A. C. Baylor, M. Bazzan, B. Bécsy, V. M. Bedakihale, M. Bejger, I. Belahcene, V. Benedetto, D. Beniwal, T. F. Bennett, J. D. Bentley, M. BenYaala, F. Bergamin, B. K. Berger, S. Bernuzzi, C. P. L. Berry, D. Bersanetti, A. Bertolini, J. Betzwieser, D. Beveridge, R. Bhandare, U. Bhardwaj, D. Bhattacharjee, S. Bhaumik, I. A. Bilenko, G. Billingsley, S. Bini, I. A. Birney, O. Birnholtz, S. Biscans, M. Bischi, S. Biscoveanu, A. Bisht, B. Biswas, M. Bitossi, M.-A. Bizouard, J. K. Blackburn, C. D. Blair, D. G. Blair, R. M. Blair, F. Bobba, N. Bode, M. Boer, G. Bogaert, M. Boldrini, L. D. Bonavena, F. Bondu, E. Bonilla, R. Bonnand, P. Booker, B. A. Boom, R. Bork, V. Boschi, N. Bose, S. Bose, V. Bossilkov, V. Boudart, Y. Bouffanais, A. Boumerdassi, A. Bozzi, C. Bradaschia, P. R. Brady, A. Bramley, A. Branch, M. Branchesi, J. E. Brau, M. Breschi, T. Briant, J. H. Briggs, A. Brillet, M. Brinkmann, P. Brockill, A. F. Brooks, J. Brooks, D. D. Brown, S. Brunett, G. Bruno, R. Bruntz, J. Bryant, J. Buchanan, T. Bulik, H. J. Bulten, A. Buonanno, R. Buscicchio, D. Buskulic, C. Buy, R. L. Byer, L. Cadonati, G. Cagnoli, C. Cahillane, J. Calderón Bustillo, J. D. Callaghan, T. A. Callister, E. Calloni, J. Cameron, J. B. Camp, M. Canepa, S. Canevarolo, M. Cannavacciuolo, K. C. Cannon, H. Cao, Z. Cao, E. Capocasa, E. Capote, G. Carapella, F. Carbognani, J. B. Carlin, M. F. Carney, M. Carpinelli, G. Carrillo, G. Carullo, T. L. Carver, J. Casanueva Diaz, C. Casentini, G. Castaldi, S. Caudill, M. Cavaglià, F. Cavalier, R. Cavalieri, M. Ceasar, G. Cella, P. Cerdá-Durán, E. Cesarini, W. Chaibi, K. Chakravarti, S. Chalathadka Subrahmanya, E. Champion, C.-H. Chan, C. Chan, C. L. Chan, K. Chan, M. Chan, K. Chandra, P. Chanial, S. Chao, P. Charlton, E. A. Chase, E. Chassande-Mottin, C. Chatterjee, Debarati Chatterjee, Deep Chatterjee, M. Chaturvedi, S. Chaty, C. Chen, H. Y. Chen, J. Chen, K. Chen, X. Chen, Y.-B. Chen, Y.-R. Chen, Z. Chen, H. Cheng, C. K. Cheong, H. Y. Cheung, H. Y. Chia, F. Chiadini, C-Y. Chiang, G. Chiarini, R. Chierici, A. Chincarini, M. L. Chiofalo, A. Chiummo, G. Cho, H. S. Cho, R. K. Choudhary, S. Choudhary, N. Christensen, H. Chu, Q. Chu, Y-K. Chu, S. Chua, K. W. Chung, G. Ciani, P. Ciecielag, M. Cieślar, M. Cifaldi, A. A. Ciobanu, R. Ciolfi, F. Cipriano, A. Cirone, F. Clara, E. N. Clark, J. A. Clark, L. Clarke, P. Clearwater, S. Clesse, F. Cleva, E. Coccia, E. Codazzo, P.-F. Cohadon, D. E. Cohen, L. Cohen, M. Colleoni, C. G. Collette, A. Colombo, M. Colpi, C. M. Compton, M. Constancio Jr., L. Conti, S. J. Cooper, P. Corban, T. R. Corbitt, I. Cordero-Carrión, S. Corezzi, K. R. Corley, N. Cornish, D. Corre, A. Corsi, S. Cortese, C. A. Costa, R. Cotesta, M. W. Coughlin, J.-P. Coulon, S. T. Countryman, B. Cousins, P. Couvares, D. M. Coward, M. J. Cowart, D. C. Coyne, R. Coyne, J. D. E. Creighton, T. D. Creighton, A. W. Criswell, M. Croquette, S. G. Crowder, J. R. Cudell, T. J. Cullen, A. Cumming, R. Cummings, L. Cunningham, E. Cuoco, M. Curyło, P. Dabadie, T. Dal Canton, S. Dall’Osso, G. Dálya, A. Dana, L. M. DaneshgaranBajastani, B. D’Angelo, S. Danilishin, S. D’Antonio, K. Danzmann, C. Darsow-Fromm, A. Dasgupta, L. E. H. Datrier, S. Datta, V. Dattilo, I. Dave, M. Davier, G. S. Davies, D. Davis, M. C. Davis, E. J. Daw, R. Dean, D. DeBra, M. Deenadayalan, J. Degallaix, M. De Laurentis, S. Deléglise, V. Del Favero, F. De Lillo, N. De Lillo, W. Del Pozzo, L. M. DeMarchi, F. De Matteis, V. D’Emilio, N. Demos, T. Dent, A. Depasse, R. De Pietri, R. De Rosa, C. De Rossi, R. DeSalvo, R. De Simone, S. Dhurandhar, M. C. Díaz, M. Diaz-Ortiz Jr., N. A. Didio, T. Dietrich, L. Di Fiore, C. Di Fronzo, C. Di Giorgio, F. Di Giovanni, M. Di Giovanni, T. Di Girolamo, A. Di Lieto, B. Ding, S. Di Pace, I. Di Palma, F. Di Renzo, A. K. Divakarla, A. Dmitriev, Z. Doctor, L. D’Onofrio, F. Donovan, K. L. Dooley, S. Doravari, I. Dorrington, M. Drago, J. C. Driggers, Y. Drori, J.-G. Ducoin, P. Dupej, O. Durante, D. D’Urso, P.-A. Duverne, S. E. Dwyer, C. Eassa, P. J. Easter, M. Ebersold, T. Eckhardt, G. Eddolls, B. Edelman, T. B. Edo, O. Edy, A. Effler, S. Eguchi, J. Eichholz, S. S. Eikenberry, M. Eisenmann, R. A. Eisenstein, A. Ejlli, E. Engelby, Y. Enomoto, L. Errico, R. C. Essick, H. Estellés, D. Estevez, Z. Etienne, T. Etzel, M. Evans, T. M. Evans, B. E. Ewing, V. Fafone, H. Fair, S. Fairhurst, A. M. Farah, S. Farinon, B. Farr, W. M. Farr, N. W. Farrow, E. J. Fauchon-Jones, G. Favaro, M. Favata, M. Fays, M. Fazio, J. Feicht, M. M. Fejer, E. Fenyvesi, D. L. Ferguson, A. Fernandez-Galiana, I. Ferrante, T. A. Ferreira, F. Fidecaro, P. Figura, I. Fiori, M. Fishbach, R. P. Fisher, R. Fittipaldi, V. Fiumara, R. Flaminio, E. Floden, H. Fong, J. A. Font, B. Fornal, P. W. F. Forsyth, A. Franke, S. Frasca, F. Frasconi, C. Frederick, J. P. Freed, Z. Frei, A. Freise, R. Frey, P. Fritschel, V. V. Frolov, G. G. Fronzé, Y. Fujii, Y. Fujikawa, M. Fukunaga, M. Fukushima, P. Fulda, M. Fyffe, H. A. Gabbard, B. U. Gadre, J. R. Gair, J. Gais, S. Galaudage, R. Gamba, D. Ganapathy, A. Ganguly, D. Gao, S. G. Gaonkar, B. Garaventa, C. García-Núñez, C. García-Quirós, F. Garufi, B. Gateley, S. Gaudio, V. Gayathri, G.-G. Ge, G. Gemme, A. Gennai, J. George, O. Gerberding, L. Gergely, P. Gewecke, S. Ghonge, Abhirup Ghosh, Archisman Ghosh, Shaon Ghosh, Shrobana Ghosh, B. Giacomazzo, L. Giacoppo, J. A. Giaime, K. D. Giardina, D. R. Gibson, C. Gier, M. Giesler, P. Giri, F. Gissi, J. Glanzer, A. E. Gleckl, P. Godwin, E. Goetz, R. Goetz, N. Gohlke, B. Goncharov, G. González, A. Gopakumar, M. Gosselin, R. Gouaty, D. W. Gould, B. Grace, A. Grado, M. Granata, V. Granata, A. Grant, S. Gras, P. Grassia, C. Gray, R. Gray, G. Greco, A. C. Green, R. Green, A. M. Gretarsson, E. M. Gretarsson, D. Griffith, W. Griffiths, H. L. Griggs, G. Grignani, A. Grimaldi, S. J. Grimm, H. Grote, S. Grunewald, P. Gruning, D. Guerra, G. M. Guidi, A. R. Guimaraes, G. Guixé, H. K. Gulati, H.-K. Guo, Y. Guo, Anchal Gupta, Anuradha Gupta, P. Gupta, E. K. Gustafson, R. Gustafson, F. Guzman, S. Ha, L. Haegel, A. Hagiwara, S. Haino, O. Halim, E. D. Hall, E. Z. Hamilton, G. Hammond, W.-B. Han, M. Haney, J. Hanks, C. Hanna, M. D. Hannam, O. Hannuksela, H. Hansen, T. J. Hansen, J. Hanson, T. Harder, T. Hardwick, K. Haris, J. Harms, G. M. Harry, I. W. Harry, D. Hartwig, K. Hasegawa, B. Haskell, R. K. Hasskew, C.-J. Haster, K. Hattori, K. Haughian, H. Hayakawa, K. Hayama, F. J. Hayes, J. Healy, A. Heidmann, A. Heidt, M. C. Heintze, J. Heinze, J. Heinzel, H. Heitmann, F. Hellman, P. Hello, A. F. Helmling-Cornell, G. Hemming, M. Hendry, I. S. Heng, E. Hennes, J. Hennig, M. H. Hennig, A. G. Hernandez, F. Hernandez Vivanco, M. Heurs, S. Hild, P. Hill, Y. Himemoto, A. S. Hines, Y. Hiranuma, N. Hirata, E. Hirose, S. Hochheim, D. Hofman, J. N. Hohmann, D. G. Holcomb, N. A. Holland, I. J. Hollows, Z. J. Holmes, K. Holt, D. E. Holz, Z. Hong, P. Hopkins, J. Hough, S. Hourihane, E. J. Howell, C. G. Hoy, D. Hoyland, A. Hreibi, B-H. Hsieh, Y. Hsu, G-Z. Huang, H-Y. Huang, P. Huang, Y-C. Huang, Y.-J. Huang, Y. Huang, M. T. Hübner, A. D. Huddart, B. Hughey, D. C. Y. Hui, V. Hui, S. Husa, S. H. Huttner, R. Huxford, T. Huynh-Dinh, S. Ide, B. Idzkowski, A. Iess, B. Ikenoue, S. Imam, K. Inayoshi, C. Ingram, Y. Inoue, K. Ioka, M. Isi, K. Isleif, K. Ito, Y. Itoh, B. R. Iyer, K. Izumi, V. JaberianHamedan, T. Jacqmin, S. J. Jadhav, S. P. Jadhav, A. L. James, A. Z. Jan, K. Jani, J. Janquart, K. Janssens, N. N. Janthalur, P. Jaranowski, D. Jariwala, R. Jaume, A. C. Jenkins, K. Jenner, C. Jeon, M. Jeunon, W. Jia, H.-B. Jin, G. R. Johns, A. W. Jones, D. I. Jones, J. D. Jones, P. Jones, R. Jones, R. J. G. Jonker, L. Ju, P. Jung, K. Jung, J. Junker, V. Juste, K. Kaihotsu, T. Kajita, M. Kakizaki, C. V. Kalaghatgi, V. Kalogera, B. Kamai, M. Kamiizumi, N. Kanda, S. Kandhasamy, G. Kang, J. B. Kanner, Y. Kao, S. J. Kapadia, D. P. Kapasi, S. Karat, C. Karathanasis, S. Karki, R. Kashyap, M. Kasprzack, W. Kastaun, S. Katsanevas, E. Katsavounidis, W. Katzman, T. Kaur, K. Kawabe, K. Kawaguchi, N. Kawai, T. Kawasaki, F. Kéfélian, D. Keitel, J. S. Key, S. Khadka, F. Y. Khalili, S. Khan, E. A. Khazanov, N. Khetan, M. Khursheed, N. Kijbunchoo, C. Kim, J. C. Kim, J. Kim, K. Kim, W. S. Kim, Y.-M. Kim, C. Kimball, N. Kimura, M. Kinley-Hanlon, R. Kirchhoff, J. S. Kissel, N. Kita, H. Kitazawa, L. Kleybolte, S. Klimenko, A. M. Knee, T. D. Knowles, E. Knyazev, P. Koch, G. Koekoek, Y. Kojima, K. Kokeyama, S. Koley, P. Kolitsidou, M. Kolstein, K. Komori, V. Kondrashov, A. K. H. Kong, A. Kontos, N. Koper, M. Korobko, K. Kotake, M. Kovalam, D. B. Kozak, C. Kozakai, R. Kozu, V. Kringel, N. V. Krishnendu, A. Królak, G. Kuehn, F. Kuei, P. Kuijer, A. Kumar, P. Kumar, Rahul Kumar, Rakesh Kumar, J. Kume, K. Kuns, C. Kuo, H-S. Kuo, Y. Kuromiya, S. Kuroyanagi, K. Kusayanagi, S. Kuwahara, K. Kwak, P. Lagabbe, D. Laghi, E. Lalande, T. L. Lam, A. Lamberts, M. Landry, B. B. Lane, R. N. Lang, J. Lange, B. Lantz, I. La Rosa, A. Lartaux-Vollard, P. D. Lasky, M. Laxen, A. Lazzarini, C. Lazzaro, P. Leaci, S. Leavey, Y. K. Lecoeuche, H. K. Lee, H. M. Lee, H. W. Lee, J. Lee, K. Lee, R. Lee, J. Lehmann, A. Lemaître, M. Leonardi, N. Leroy, N. Letendre, C. Levesque, Y. Levin, J. N. Leviton, K. Leyde, A. K. Y. Li, B. Li, J. Li, K. L. Li, T. G. F. Li, X. Li, C-Y. Lin, F-K. Lin, F-L. Lin, H. L. Lin, L. C.-C. Lin, F. Linde, S. D. Linker, J. N. Linley, T. B. Littenberg, G. C. Liu, J. Liu, K. Liu, X. Liu, F. Llamas, M. Llorens-Monteagudo, R. K. L. Lo, A. Lockwood, L. T. London, A. Longo, D. Lopez, M. Lopez Portilla, M. Lorenzini, V. Loriette, M. Lormand, G. Losurdo, T. P. Lott, J. D. Lough, C. O. Lousto, G. Lovelace, J. F. Lucaccioni, H. Lück, D. Lumaca, A. P. Lundgren, L.-W. Luo, J. E. Lynam, R. Macas, M. MacInnis, D. M. Macleod, I. A. O. MacMillan, A. Macquet, I. Magaña Hernandez, C. Magazzù, R. M. Magee, R. Maggiore, M. Magnozzi, S. Mahesh, E. Majorana, C. Makarem, I. Maksimovic, S. Maliakal, A. Malik, N. Man, V. Mandic, V. Mangano, J. L. Mango, G. L. Mansell, M. Manske, M. Mantovani, M. Mapelli, F. Marchesoni, M. Marchio, F. Marion, Z. Mark, S. Márka, Z. Márka, C. Markakis, A. S. Markosyan, A. Markowitz, E. Maros, A. Marquina, S. Marsat, F. Martelli, I. W. Martin, R. M. Martin, M. Martinez, V. A. Martinez, V. Martinez, K. Martinovic, D. V. Martynov, E. J. Marx, H. Masalehdan, K. Mason, E. Massera, A. Masserot, T. J. Massinger, M. Masso-Reid, S. Mastrogiovanni, A. Matas, M. Mateu-Lucena, F. Matichard, M. Matiushechkina, N. Mavalvala, J. J. McCann, R. McCarthy, D. E. McClelland, P. K. McClincy, S. McCormick, L. McCuller, G. I. McGhee, S. C. McGuire, C. McIsaac, J. McIver, T. McRae, S. T. McWilliams, D. Meacher, M. Mehmet, A. K. Mehta, Q. Meijer, A. Melatos, D. A. Melchor, G. Mendell, A. Menendez-Vazquez, C. S. Menoni, R. A. Mercer, L. Mereni, K. Merfeld, E. L. Merilh, J. D. Merritt, M. Merzougui, S. Meshkov, C. Messenger, C. Messick, P. M. Meyers, F. Meylahn, A. Mhaske, A. Miani, H. Miao, I. Michaloliakos, C. Michel, Y. Michimura, H. Middleton, L. Milano, A. L. Miller, A. Miller, B. Miller, M. Millhouse, J. C. Mills, E. Milotti, O. Minazzoli, Y. Minenkov, N. Mio, Ll. M. Mir, M. Miravet-Tenés, C. Mishra, T. Mishra, T. Mistry, S. Mitra, V. P. Mitrofanov, G. Mitselmakher, R. Mittleman, O. Miyakawa, A. Miyamoto, Y. Miyazaki, K. Miyo, S. Miyoki, Geoffrey Mo, E. Moguel, K. Mogushi, S. R. P. Mohapatra, S. R. Mohite, I. Molina, M. Molina-Ruiz, M. Mondin, M. Montani, C. J. Moore, D. Moraru, F. Morawski, A. More, C. Moreno, G. Moreno, Y. Mori, S. Morisaki, Y. Moriwaki, B. Mours, C. M. Mow-Lowry, S. Mozzon, F. Muciaccia, Arunava Mukherjee, D. Mukherjee, Soma Mukherjee, Subroto Mukherjee, Suvodip Mukherjee, N. Mukund, A. Mullavey, J. Munch, E. A. Muñiz, P. G. Murray, R. Musenich, S. Muusse, S. L. Nadji, K. Nagano, S. Nagano, A. Nagar, K. Nakamura, H. Nakano, M. Nakano, R. Nakashima, Y. Nakayama, V. Napolano, I. Nardecchia, T. Narikawa, L. Naticchioni, B. Nayak, R. K. Nayak, R. Negishi, B. F. Neil, J. Neilson, G. Nelemans, T. J. N. Nelson, M. Nery, P. Neubauer, A. Neunzert, K. Y. Ng, S. W. S. Ng, C. Nguyen, P. Nguyen, T. Nguyen, L. Nguyen Quynh, W.-T. Ni, S. A. Nichols, A. Nishizawa, S. Nissanke, E. Nitoglia, F. Nocera, M. Norman, C. North, S. Nozaki, L. K. Nuttall, J. Oberling, B. D. O’Brien, Y. Obuchi, J. O’Dell, E. Oelker, W. Ogaki, G. Oganesyan, J. J. Oh, K. Oh, S. H. Oh, M. Ohashi, N. Ohishi, M. Ohkawa, F. Ohme, H. Ohta, M. A. Okada, Y. Okutani, K. Okutomi, C. Olivetto, K. Oohara, C. Ooi, R. Oram, B. O’Reilly, R. G. Ormiston, N. D. Ormsby, L. F. Ortega, R. O’Shaughnessy, E. O’Shea, S. Oshino, S. Ossokine, C. Osthelder, S. Otabe, D. J. Ottaway, H. Overmier, A. E. Pace, G. Pagano, M. A. Page, G. Pagliaroli, A. Pai, S. A. Pai, J. R. Palamos, O. Palashov, C. Palomba, H. Pan, K. Pan, P. K. Panda, H. Pang, P. T. H. Pang, C. Pankow, F. Pannarale, B. C. Pant, F. H. Panther, F. Paoletti, A. Paoli, A. Paolone, A. Parisi, H. Park, J. Park, W. Parker, D. Pascucci, A. Pasqualetti, R. Passaquieti, D. Passuello, M. Patel, M. Pathak, B. Patricelli, A. S. Patron, S. Patrone, S. Paul, E. Payne, M. Pedraza, M. Pegoraro, A. Pele, F. E. Peña Arellano, S. Penn, A. Perego, A. Pereira, T. Pereira, C. J. Perez, C. Périgois, C. C. Perkins, A. Perreca, S. Perriès, J. Petermann, D. Petterson, H. P. Pfeiffer, K. A. Pham, K. S. Phukon, O. J. Piccinni, M. Pichot, M. Piendibene, F. Piergiovanni, L. Pierini, V. Pierro, G. Pillant, M. Pillas, F. Pilo, L. Pinard, I. M. Pinto, M. Pinto, B. J. Piotrzkowski, K. Piotrzkowski, M. Pirello, M. D. Pitkin, E. Placidi, L. Planas, W. Plastino, C. Pluchar, R. Poggiani, E. Polini, D. Y. T. Pong, S. Ponrathnam, P. Popolizio, E. K. Porter, R. Poulton, J. Powell, M. Pracchia, T. Pradier, A. K. Prajapati, K. Prasai, R. Prasanna, G. Pratten, M. Principe, G. A. Prodi, L. Prokhorov, P. Prosposito, L. Prudenzi, A. Puecher, M. Punturo, F. Puosi, P. Puppo, M. Pürrer, H. Qi, V. Quetschke, R. Quitzow-James, F. J. Raab, G. Raaijmakers, H. Radkins, N. Radulesco, P. Raffai, S. X. Rail, S. Raja, C. Rajan, K. E. Ramirez, T. D. Ramirez, A. Ramos-Buades, J. Rana, P. Rapagnani, U. D. Rapol, A. Ray, V. Raymond, N. Raza, M. Razzano, J. Read, L. A. Rees, T. Regimbau, L. Rei, S. Reid, S. W. Reid, D. H. Reitze, P. Relton, A. Renzini, P. Rettegno, M. Rezac, F. Ricci, D. Richards, J. W. Richardson, L. Richardson, G. Riemenschneider, K. Riles, S. Rinaldi, K. Rink, M. Rizzo, N. A. Robertson, R. Robie, F. Robinet, A. Rocchi, S. Rodriguez, L. Rolland, J. G. Rollins, M. Romanelli, R. Romano, C. L. Romel, A. Romero-Rodríguez, I. M. Romero-Shaw, J. H. Romie, S. Ronchini, L. Rosa, C. A. Rose, D. Rosińska, M. P. Ross, S. Rowan, S. J. Rowlinson, S. Roy, Santosh Roy, Soumen Roy, D. Rozza, P. Ruggi, K. Ryan, S. Sachdev, T. Sadecki, J. Sadiq, N. Sago, S. Saito, Y. Saito, K. Sakai, Y. Sakai, M. Sakellariadou, Y. Sakuno, O. S. Salafia, L. Salconi, M. Saleem, F. Salemi, A. Samajdar, E. J. Sanchez, J. H. Sanchez, L. E. Sanchez, N. Sanchis-Gual, J. R. Sanders, A. Sanuy, T. R. Saravanan, N. Sarin, B. Sassolas, H. Satari, S. Sato, T. Sato, O. Sauter, R. L. Savage, T. Sawada, D. Sawant, H. L. Sawant, S. Sayah, D. Schaetzl, M. Scheel, J. Scheuer, M. Schiworski, P. Schmidt, S. Schmidt, R. Schnabel, M. Schneewind, R. M. S. Schofield, A. Schönbeck, B. W. Schulte, B. F. Schutz, E. Schwartz, J. Scott, S. M. Scott, M. Seglar-Arroyo, T. Sekiguchi, Y. Sekiguchi, D. Sellers, A. S. Sengupta, D. Sentenac, E. G. Seo, V. Sequino, A. Sergeev, Y. Setyawati, T. Shaffer, M. S. Shahriar, B. Shams, L. Shao, A. Sharma, P. Sharma, P. Shawhan, N. S. Shcheblanov, S. Shibagaki, M. Shikauchi, R. Shimizu, T. Shimoda, K. Shimode, H. Shinkai, T. Shishido, A. Shoda, D. H. Shoemaker, D. M. Shoemaker, S. ShyamSundar, M. Sieniawska, D. Sigg, L. P. Singer, D. Singh, N. Singh, A. Singha, A. M. Sintes, V. Sipala, V. Skliris, B. J. J. Slagmolen, T. J. Slaven-Blair, J. Smetana, J. R. Smith, R. J. E. Smith, J. Soldateschi, S. N. Somala, K. Somiya, E. J. Son, K. Soni, S. Soni, V. Sordini, F. Sorrentino, N. Sorrentino, H. Sotani, R. Soulard, T. Souradeep, E. Sowell, V. Spagnuolo, A. P. Spencer, M. Spera, R. Srinivasan, A. K. Srivastava, V. Srivastava, K. Staats, C. Stachie, D. A. Steer, J. Steinlechner, S. Steinlechner, D. J. Stops, M. Stover, K. A. Strain, L. C. Strang, G. Stratta, A. Strunk, R. Sturani, A. L. Stuver, S. Sudhagar, V. Sudhir, R. Sugimoto, H. G. Suh, T. Z. Summerscales, H. Sun, L. Sun, S. Sunil, A. Sur, J. Suresh, P. J. Sutton, Takamasa Suzuki, Toshikazu Suzuki, B. L. Swinkels, M. J. Szczepańczyk, P. Szewczyk, M. Tacca, H. Tagoshi, S. C. Tait, H. Takahashi, R. Takahashi, A. Takamori, S. Takano, H. Takeda, M. Takeda, C. J. Talbot, C. Talbot, H. Tanaka, Kazuyuki Tanaka, Kenta Tanaka, Taiki Tanaka, Takahiro Tanaka, A. J. Tanasijczuk, S. Tanioka, D. B. Tanner, D. Tao, L. Tao, E. N. Tapia San Martin, E. N. Tapia San Martín, C. Taranto, J. D. Tasson, S. Telada, R. Tenorio, J. E. Terhune, L. Terkowski, M. P. Thirugnanasambandam, M. Thomas, P. Thomas, J. E. Thompson, S. R. Thondapu, K. A. Thorne, E. Thrane, Shubhanshu Tiwari, Srishti Tiwari, V. Tiwari, A. M. Toivonen, K. Toland, A. E. Tolley, T. Tomaru, Y. Tomigami, T. Tomura, M. Tonelli, A. Torres-Forné, C. I. Torrie, I. Tosta e Melo, D. Töyrä, A. Trapananti, F. Travasso, G. Traylor, M. Trevor, M. C. Tringali, A. Tripathee, L. Troiano, A. Trovato, L. Trozzo, R. J. Trudeau, D. S. Tsai, D. Tsai, K. W. Tsang, T. Tsang, J-S. Tsao, M. Tse, R. Tso, K. Tsubono, S. Tsuchida, L. Tsukada, D. Tsuna, T. Tsutsui, T. Tsuzuki, K. Turbang, M. Turconi, D. Tuyenbayev, A. S. Ubhi, N. Uchikata, T. Uchiyama, R. P. Udall, A. Ueda, T. Uehara, K. Ueno, G. Ueshima, C. S. Unnikrishnan, F. Uraguchi, A. L. Urban, T. Ushiba, A. Utina, H. Vahlbruch, G. Vajente, A. Vajpeyi, G. Valdes, M. Valentini, V. Valsan, 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, J. Vanosky, M. H. P. M. van Putten, N. van Remortel, M. Vardaro, A. F. Vargas, V. Varma, M. Vasúth, A. Vecchio, G. Vedovato, J. Veitch, P. J. Veitch, J. Venneberg, G. Venugopalan, D. Verkindt, P. Verma, Y. Verma, D. Veske, F. Vetrano, A. Viceré, S. Vidyant, A. D. Viets, A. Vijaykumar, V. Villa-Ortega, J.-Y. Vinet, A. Virtuoso, S. Vitale, T. Vo, H. Vocca, E. R. G. von Reis, J. S. A. von Wrangel, C. Vorvick, S. P. Vyatchanin, L. E. Wade, M. Wade, K. J. Wagner, R. C. Walet, M. Walker, G. S. Wallace, L. Wallace, S. Walsh, J. Wang, J. Z. Wang, W. H. Wang, R. L. Ward, J. Warner, M. Was, T. Washimi, N. Y. Washington, K. Watada, J. Watchi, B. Weaver, S. A. Webster, M. Weinert, A. J. Weinstein, R. Weiss, C. M. Weller, F. Wellmann, L. Wen, P. Weßels, K. Wette, J. T. Whelan, D. D. White, B. F. Whiting, C. Whittle, D. Wilken, D. Williams, M. J. Williams, A. R. Williamson, J. L. Willis, B. Willke, D. J. Wilson, W. Winkler, C. C. Wipf, T. Wlodarczyk, G. Woan, J. Woehler, J. K. Wofford, I. C. F. Wong, C. Wu, D. S. Wu, H. Wu, S. Wu, D. M. Wysocki, L. Xiao, W-R. Xu, T. Yamada, H. Yamamoto, Kazuhiro Yamamoto, Kohei Yamamoto, T. Yamamoto, K. Yamashita, R. Yamazaki, F. W. Yang, L. Yang, Y. Yang, Yang Yang, Z. Yang, M. J. Yap, D. W. Yeeles, A. B. Yelikar, M. Ying, K. Yokogawa, J. Yokoyama, T. Yokozawa, J. Yoo, T. Yoshioka, Hang Yu, Haocun Yu, H. Yuzurihara, A. Zadrożny, M. Zanolin, S. Zeidler, T. Zelenova, J.-P. Zendri, M. Zevin, M. Zhan, H. Zhang, J. Zhang, L. Zhang, T. Zhang, Y. Zhang, C. Zhao, G. Zhao, Y. Zhao, Yue Zhao, R. Zhou, Z. Zhou, X. J. Zhu, Z.-H. Zhu, A. B. Zimmerman, M. E. Zucker, J. Zweizig, M. Bhardwaj, P. J. Boyle, T. Cassanelli, F. Dong, E. Fonseca, V. Kaspi, C. Leung, K. W. Masui, B. W. Meyers, D. Michilli, C. Ng, A. B. Pearlman, E. Petroff, Z. Pleunis, M. Rafiei-Ravandi, M. Rahman, S. Ransom, P. Scholz, K. Shin, K. Smith, I. Stairs, S. P. Tendulkar, A. V. Zwaniga, The LIGO Scientific Collaboration, The Virgo Collaboration, The KAGRA Collaboration, and The CHIME/FRB Collaboration
Subjects: Gravitational wave astronomy, Radio transient sources, Astrophysics, QB460-466
Abstract: We search for gravitational-wave (GW) transients associated with fast radio bursts (FRBs) detected by the Canadian Hydrogen Intensity Mapping Experiment Fast Radio Burst Project, during the first part of the third observing run of Advanced LIGO and Advanced Virgo (2019 April 1 15:00 UTC–2019 October 1 15:00 UTC). Triggers from 22 FRBs were analyzed with a search that targets both binary neutron star (BNS) and neutron star–black hole (NSBH) mergers. A targeted search for generic GW transients was conducted on 40 FRBs. We find no significant evidence for a GW association in either search. Given the large uncertainties in the distances of our FRB sample, we are unable to exclude the possibility of a GW association. Assessing the volumetric event rates of both FRB and binary mergers, an association is limited to 15% of the FRB population for BNS mergers or 1% for NSBH mergers. We report 90% confidence lower bounds on the distance to each FRB for a range of GW progenitor models and set upper limits on the energy emitted through GWs for a range of emission scenarios. We find values of order 10 ^51 –10 ^57 erg for models with central GW frequencies in the range 70–3560 Hz. At the sensitivity of this search, we find these limits to be above the predicted GW emissions for the models considered. We also find no significant coincident detection of GWs with the repeater, FRB 20200120E, which is the closest known extragalactic FRB.
Published: 2023
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2. Revealing the Dynamic Magnetoionic Environments of Repeating Fast Radio Burst Sources through Multiyear Polarimetric Monitoring with CHIME/FRB

Author: R. Mckinven, B. M. Gaensler, D. Michilli, K. Masui, V. M. Kaspi, J. Su, M. Bhardwaj, T. Cassanelli, P. Chawla, F. (Adam) Dong, E. Fonseca, C. Leung, D. Z. Li, C. Ng, C. Patel, A. B. Pearlman, E. Petroff, Z. Pleunis, M. Rafiei-Ravandi, M. Rahman, K. R. Sand, K. Shin, I. H. Stairs, and S. Tendulkar
Subjects: Radio transient sources, Polarimetry, Radio bursts, Astrophysics, QB460-466
Abstract: Fast radio bursts (FRBs) display a confounding variety of burst properties and host-galaxy associations. Repeating FRBs offer insight into the FRB population by enabling spectral, temporal, and polarimetric properties to be tracked over time. Here, we report on the polarized observations of 12 repeating sources using multiyear monitoring with the Canadian Hydrogen Intensity Mapping Experiment (CHIME) over 400–800 MHz. We observe significant rotation measure (RM) variations from many sources in our sample, including RM changes of several hundred radians per square meter over month timescales from FRBs 20181119A, 20190303A, and 20190417A, and more modest RM variability (ΔRM ≲ few tens of radians per square meter) from FRBs 20181030A, 20190208A, 20190213B, and 20190117A over equivalent timescales. Several repeaters display a frequency-dependent degree of linear polarization that is consistent with depolarization via scattering. Combining our measurements of RM variations with equivalent constraints on DM variability, we estimate the average line-of-sight magnetic field strength in the local environment of each repeater. In general, repeating FRBs display RM variations that are more prevalent and/or extreme than those seen from radio pulsars in the Milky Way and the Magellanic Clouds, suggesting repeating FRBs and pulsars occupy distinct magnetoionic environments.
Published: 2023
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3. A Large-scale Magneto-ionic Fluctuation in the Local Environment of Periodic Fast Radio Burst Source FRB 20180916B

Author: R. Mckinven, B. M. Gaensler, D. Michilli, K. Masui, V. M. Kaspi, M. Bhardwaj, T. Cassanelli, P. Chawla, F. (Adam) Dong, E. Fonseca, C. Leung, D. Z. Li, C. Ng, C. Patel, E. Petroff, A. B. Pearlman, Z. Pleunis, M. Rafiei-Ravandi, M. Rahman, K. R. Sand, K. Shin, P. Scholz, I. H. Stairs, K. Smith, J. Su, and S. Tendulkar
Subjects: Radio transient sources, Magnetic fields, Spectropolarimetry, Interstellar medium, Astrophysics, QB460-466
Abstract: Fast radio burst (FRB) source FRB 20180916B exhibits a 16.33-day periodicity in its burst activity. It is as of yet unclear what proposed mechanism produces the activity, but polarization information is a key diagnostic. Here we report on the polarization properties of 44 bursts from FRB 20180916B detected between 2018 December and 2021 December by CHIME/FRB, the FRB project on the Canadian Hydrogen Intensity Mapping Experiment. In contrast to previous observations, we find significant variations in the Faraday rotation measure (RM) of FRB 20180916B. Over the 9-month period 2021 April and 2021 December we observe an apparent secular increase in RM of ∼50 rad m ^−2 (a fractional change of over 40%) that is accompanied by a possible drift of the emitting band to lower frequencies. This interval displays very little variation in the dispersion measure (ΔDM ≲ 0.8 pc cm ^−3 ), which indicates that the observed RM evolution is likely produced from coherent changes in the Faraday-active medium’s magnetic field. Burst-to-burst RM variations appear unrelated to the activity cycle phase. The degree of linear polarization of our burst sample (≳80%) is consistent with the negligible depolarization expected for this source in the 400–800 MHz bandpass of CHIME. FRB 20180916B joins other repeating FRBs in displaying substantial RM evolution. This is consistent with the notion that repeater progenitors may be associated with young stellar populations by their preferential occupation of dynamic magnetized environments commonly found in supernova remnants, in pulsar wind nebulae, or near high-mass stellar companions.
Published: 2023
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4. A bright, high rotation-measure FRB that skewers the M33 halo

Author: L Connor, J van Leeuwen, L C Oostrum, E Petroff, Y Maan, E A K Adams, J J Attema, J E Bast, O M Boersma, H Dénes, D W Gardenier, J E Hargreaves, E Kooistra, I Pastor-Marazuela, R Schulz, A Sclocco, R Smits, S M Straal, D van der Schuur, D Vohl, B Adebahr, W J G de Blok, W A van Cappellen, A H W M Coolen, S Damstra, G N J van Diepen, B S Frank, K M Hess, B Hut, A Kutkin, G Marcel Loose, D M Lucero, Á Mika, V A Moss, H Mulder, T A Oosterloo, M Ruiter, H Vedantham, N J Vermaas, S J Wijnholds, and J Ziemke
Published: 2020
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5. Polarization studies of rotating radio transients

Author: M Caleb, W van Straten, E F Keane, A Jameson, M Bailes, E D Barr, C Flynn, C D Ilie, E Petroff, A Rogers, B W Stappers, V Venkatraman Krishnan, and P Weltevrede
Published: 2019
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6. A fast radio burst with frequency-dependent polarization detected during Breakthrough Listen observations

Author: D C Price, G Foster, M Geyer, W van Straten, V Gajjar, G Hellbourg, A Karastergiou, E F Keane, A P V Siemion, I Arcavi, R Bhat, M Caleb, S-W Chang, S Croft, D DeBoer, I de Pater, J Drew, J E Enriquez, W Farah, N Gizani, J A Green, H Isaacson, J Hickish, A Jameson, M Lebofsky, D H E MacMahon, A Möller, C A Onken, E Petroff, D Werthimer, C Wolf, S P Worden, and Y G Zhang
Published: 2019
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7. Burst timescales and luminosities as links between young pulsars and fast radio bursts

Author: K. Nimmo, J. W. T. Hessels, F. Kirsten, A. Keimpema, J. M. Cordes, M. P. Snelders, D. M. Hewitt, R. Karuppusamy, A. M. Archibald, V. Bezrukovs, M. Bhardwaj, R. Blaauw, S. T. Buttaccio, T. Cassanelli, J. E. Conway, A. Corongiu, R. Feiler, E. Fonseca, O. Forssén, M. Gawroński, M. Giroletti, M. A. Kharinov, C. Leung, M. Lindqvist, G. Maccaferri, B. Marcote, K. W. Masui, R. Mckinven, A. Melnikov, D. Michilli, A. G. Mikhailov, C. Ng, A. Orbidans, O. S. Ould-Boukattine, Z. Paragi, A. B. Pearlman, E. Petroff, M. Rahman, P. Scholz, K. Shin, K. M. Smith, I. H. Stairs, G. Surcis, S. P. Tendulkar, W. Vlemmings, N. Wang, J. Yang, J. P. Yuan, and High Energy Astrophys. & Astropart. Phys (API, FNWI)
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: Fast radio bursts (FRBs) are extragalactic radio flashes of unknown physical origin. Their high luminosities and short durations require extreme energy densities, such as those found in the vicinity of neutron stars and black holes. Studying the burst intensities and polarimetric properties on a wide range of timescales, from milliseconds down to nanoseconds, is key to understanding the emission mechanism. However, high-time-resolution studies of FRBs are limited by their unpredictable activity levels, available instrumentation and temporal broadening in the intervening ionized medium. Here we show that the repeating FRB 20200120E can produce isolated shots of emission as short as about 60 nanoseconds in duration, with brightness temperatures as high as 3 × 10⁴¹ K (excluding relativistic effects), comparable with ‘nano-shots’ from the Crab pulsar. Comparing both the range of timescales and luminosities, we find that FRB 20200120E observationally bridges the gap between known Galactic young pulsars and magnetars and the much more distant extragalactic FRBs. This suggests a common magnetically powered emission mechanism spanning many orders of magnitude in timescale and luminosity. In this Article, we probe a relatively unexplored region of the short-duration transient phase space; we highlight that there probably exists a population of ultrafast radio transients at nanosecond to microsecond timescales, which current FRB searches are insensitive to.
Published: 2022

8. A repeating fast radio burst source in a globular cluster

Author: F. Kirsten, B. Marcote, K. Nimmo, J. W. T. Hessels, M. Bhardwaj, S. P. Tendulkar, A. Keimpema, J. Yang, M. P. Snelders, P. Scholz, A. B. Pearlman, C. J. Law, W. M. Peters, M. Giroletti, Z. Paragi, C. Bassa, D. M. Hewitt, U. Bach, V. Bezrukovs, M. Burgay, S. T. Buttaccio, J. E. Conway, A. Corongiu, R. Feiler, O. Forssén, M. P. Gawroński, R. Karuppusamy, M. A. Kharinov, M. Lindqvist, G. Maccaferri, A. Melnikov, O. S. Ould-Boukattine, A. Possenti, G. Surcis, N. Wang, J. Yuan, K. Aggarwal, R. Anna-Thomas, G. C. Bower, R. Blaauw, S. Burke-Spolaor, T. Cassanelli, T. E. Clarke, E. Fonseca, B. M. Gaensler, A. Gopinath, V. M. Kaspi, N. Kassim, T. J. W. Lazio, C. Leung, D. Z. Li, H. H. Lin, K. W. Masui, R. Mckinven, D. Michilli, A. G. Mikhailov, C. Ng, A. Orbidans, U. L. Pen, E. Petroff, M. Rahman, S. M. Ransom, K. Shin, K. M. Smith, I. H. Stairs, W. Vlemmings, and High Energy Astrophys. & Astropart. Phys (API, FNWI)
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Multidisciplinary, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Fast radio bursts (FRBs) are exceptionally luminous flashes of unknown physical origin, reaching us from other galaxies (Petroff et al. 2019). Most FRBs have only ever been seen once, while others flash repeatedly, though sporadically (Spitler et al. 2016, CHIME/FRB Collaboration et al. 2021). Many models invoke magnetically powered neutron stars (magnetars) as the engines producing FRB emission (Margalit & Metzger 2018, CHIME/FRB Collaboration et al. 2020). Recently, CHIME/FRB announced the discovery (Bhardwaj et al. 2021) of the repeating FRB 20200120E, coming from the direction of the nearby grand design spiral galaxy M81. Four potential counterparts at other observing wavelengths were identified (Bhardwaj et al. 2021) but no definitive association with these sources, or M81, could be made. Here we report an extremely precise localisation of FRB 20200120E, which allows us to associate it with a globular cluster (GC) in the M81 galactic system and to place it ~2pc offset from the optical center of light of the GC. This confirms (Bhardwaj et al. 2021) that FRB 20200120E is 40 times closer than any other known extragalactic FRB. Because such GCs host old stellar populations, this association strongly challenges FRB models that invoke young magnetars formed in a core-collapse supernova as powering FRB emission. We propose, instead, that FRB 20200120E is a highly magnetised neutron star formed via either accretion-induced collapse of a white dwarf or via merger of compact stars in a binary system (Margalit et al. 2019). Alternative scenarios involving compact binary systems, efficiently formed inside globular clusters, could also be responsible for the observed bursts., Submitted. Comments welcome
Published: 2022

9. Apertif: Phased array feeds for the Westerbork Synthesis Radio Telescope. System overview and performance characteristics

Author: W. A. van Cappellen, T. A. Oosterloo, M. A. W. Verheijen, E. A. K. Adams, B. Adebahr, R. Braun, K. M. Hess, H. Holties, J. M. van der Hulst, B. Hut, E. Kooistra, J. van Leeuwen, G. M. Loose, R. Morganti, V. A. Moss, E. Orrú, M. Ruiter, A. P. Schoenmakers, N. J. Vermaas, S. J. Wijnholds, A. S. van Amesfoort, M. J. Arts, J. J. Attema, L. Bakker, C. G. Bassa, J. E. Bast, P. Benthem, R. Beukema, R. Blaauw, W. J. G. de Blok, M. Bouwhuis, R. H. van den Brink, L. Connor, A. H. W. M. Coolen, S. Damstra, G. N. J. van Diepen, R. de Goei, H. Dénes, M. Drost, N. Ebbendorf, B. S. Frank, D. W. Gardenier, M. Gerbers, Y. G. Grange, T. Grit, A. W. Gunst, N. Gupta, M. V. Ivashina, G. I. G. Józsa, G. H. Janssen, A. Koster, G. H. Kruithof, S. J. Kuindersma, A. Kutkin, D. M. Lucero, Y. Maan, F. M. Maccagni, J. van der Marel, A. Mika, J. Morawietz, H. Mulder, E. Mulder, M. J. Norden, A. R. Offringa, L. C. Oostrum, R. E. Overeem, Z. Paragi, H. J. Pepping, E. Petroff, D. J. Pisano, A. G. Polatidis, P. Prasad, J. P. R. de Reijer, J. W. Romein, J. Schaap, G. W. Schoonderbeek, R. Schulz, D. van der Schuur, A. Sclocco, J. J. Sluman, R. Smits, B. W. Stappers, S. M. Straal, K. J. C. Stuurwold, J. Verstappen, D. Vohl, K. J. Wierenga, E. E. M. Woestenburg, A. W. Zanting, J. Ziemke, Astronomy, and Kapteyn Astronomical Institute
Subjects: Radio telescope, Physics, Space and Planetary Science, Phased array, Instrumentation: interferometers, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Surveys, Telescopes
Abstract: We describe the APERture Tile In Focus (Apertif) system, a phased array feed (PAF) upgrade of the Westerbork Synthesis Radio Telescope that transforms this telescope into a high-sensitivity, wide-field-of-view L-band imaging and transient survey instrument. Using novel PAF technology, up to 40 partially overlapping beams are formed on the sky simultaneously, significantly increasing the survey speed of the telescope. With this upgraded instrument, an imaging survey covering an area of 2300 deg2 is being performed that will deliver both continuum and spectral line datasets, of which the first data have been publicly released. In addition, a time domain transient and pulsar survey covering 15 000 deg2 is in progress. An overview of the Apertif science drivers, hardware, and software of the upgraded telescope is presented, along with its key performance characteristics.
Published: 2022

10. Dual-frequency single-pulse study of PSR B0950+08

Author: A. V. Bilous, J. M. Grießmeier, T. Pennucci, Z. Wu, L. Bondonneau, V. Kondratiev, J. van Leeuwen, Y. Maan, L. Connor, L. C. Oostrum, E. Petroff, J. P. W. Verbiest, D. Vohl, J. W. McKee, G. Shaifullah, G. Theureau, O. M. Ulyanov, B. Cecconi, A. H. Coolen, S. Corbel, S. Damstra, H. Dénes, J. N. Girard, B. Hut, M. Ivashina, O. O. Konovalenko, A. Kutkin, G. M. Loose, H. Mulder, M. Ruiter, R. Smits, P. L. Tokarsky, N. J. Vermaas, V. V. Zakharenko, P. Zarka, J. Ziemke, High Energy Astrophys. & Astropart. Phys (API, FNWI), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Unité Scientifique de la Station de Nançay (USN), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Théories (LUTH (UMR_8102)), 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), 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), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National d’Études Spatiales [Paris] (CNES), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), 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), Bilous, A, Griessmeier, J, Pennucci, T, Wu, Z, Bondonneau, L, Kondratiev, V, van Leeuwen, J, Maan, Y, Connor, L, Oostrum, L, Petroff, E, Verbiest, J, Vohl, D, Mckee, J, Shaifullah, G, Theureau, G, Ulyanov, O, Cecconi, B, Coolen, A, Corbel, S, Damstra, S, Denes, H, Girard, J, Hut, B, Ivashina, M, Konovalenko, O, Kutkin, A, Loose, G, Mulder, H, Ruiter, M, Smits, R, Tokarsky, P, Vermaas, N, Zakharenko, V, Zarka, P, and Ziemke, J
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Population, Frequency drift, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Spectral line, Radio telescope, stars: neutron, Pulsar, 0103 physical sciences, education, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, education.field_of_study, Scintillation, Line-of-sight, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astronomy and Astrophysics, Interstellar medium, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: PSR B0950+08 is a bright non-recycled pulsar whose single-pulse fluence variability is reportedly large. Based on observations at two widely separated frequencies, 55 MHz (NenuFAR) and 1.4 GHz (Westerbork Synthesis Radio Telescope), we review the properties of these single pulses. We conclude that they are more similar to ordinary pulses of radio emission than to a special kind of short and bright Giant Pulses, observed from only a handful of pulsars. We argue that temporal variation of properties of interstellar medium along the line of sight to this nearby pulsar, namely the fluctuating size of decorrelation bandwidth of diffractive scintillation makes important contribution to observed single-pulse fluence variability. We further present interesting structures in the low-frequency single-pulse spectra that resemble the "sad trombones" seen in Fast Radio Bursts (FRBs); although for PSR B0950+08 the upward frequency drift is also routinely present. We explain these spectral features with radius-to-frequency mapping, similar to the model developed by Wang et al. (2019) for FRBs. Finally, we speculate that microsecond-scale fluence variability of the general pulsar population remains poorly known, and that its further study may bring important clues about the nature of FRBs., Accepted by A&A. This version includes a number of minor corrections, including corrected FRB luminosities on the time-luminosity phase-space plot for radio pulses from neutron stars and repeating FRBs
Published: 2022

11. Modeling Fast Radio Burst Dispersion and Scattering Properties in the First CHIME/FRB Catalog

Author: P. Chawla, V. M. Kaspi, S. M. Ransom, M. Bhardwaj, P. J. Boyle, D. Breitman, T. Cassanelli, D. Cubranic, F. Q. Dong, E. Fonseca, B. M. Gaensler, U. Giri, A. Josephy, J. F. Kaczmarek, C. Leung, K. W. Masui, J. Mena-Parra, M. Merryfield, D. Michilli, M. Münchmeyer, C. Ng, C. Patel, A. B. Pearlman, E. Petroff, Z. Pleunis, M. Rahman, P. Sanghavi, K. Shin, K. M. Smith, I. Stairs, and S. P. Tendulkar
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
Abstract: We present a Monte Carlo-based population synthesis study of fast radio burst (FRB) dispersion and scattering focusing on the first catalog of sources detected with the Canadian Hydrogen Intensity Mapping Experiment Fast Radio Burst (CHIME/FRB) project. We simulate intrinsic properties and propagation effects for a variety of FRB population models and compare the simulated distributions of dispersion measures (DMs) and scattering timescales with the corresponding distributions from the CHIME/FRB catalog. Our simulations confirm the results of previous population studies, which suggested that the interstellar medium of the host galaxy alone (simulated based on the NE2001 model) cannot explain the observed scattering timescales of FRBs. We therefore consider additional sources of scattering, namely, the circumgalactic medium (CGM) of intervening galaxies and the circumburst medium whose properties are modeled based on typical Galactic plane environments. We find that a population of FRBs with scattering contributed by these media is marginally consistent with the CHIME/FRB catalog. In this scenario, our simulations favor a population of FRBs offset from their galaxy centers over a population which is distributed along the spiral arms. However, if the models proposing the CGM as a source of intense scattering are incorrect, then we conclude that FRBs may inhabit environments with more extreme properties than those inferred for pulsars in the Milky Way., Accepted for publication in ApJ
Published: 2021

12. Fast radio bursts at the dawn of the 2020s

Author: E. Petroff, J. W. T. Hessels, D. R. Lorimer, and High Energy Astrophys. & Astropart. Phys (API, FNWI)
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Cosmology and Nongalactic Astrophysics (astro-ph.CO), Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Since the discovery of the first fast radio burst (FRB) in 2007, and their confirmation as an abundant extragalactic population in 2013, the study of these sources has expanded at an incredible rate. In our 2019 review on the subject we presented a growing, but still mysterious, population of FRBs -- 60 unique sources, 2 repeating FRBs, and only 1 identified host galaxy. However, in only a few short years new observations and discoveries have given us a wealth of information about these sources. The total FRB population now stands at over 600 published sources, 24 repeaters, and 19 host galaxies. Higher time resolution data, sustained monitoring, and precision localisations have given us insight into repeaters, host galaxies, burst morphology, source activity, progenitor models, and the use of FRBs as cosmological probes. The recent detection of a bright FRB-like burst from the Galactic magnetar SGR~1935+2154 provides an important link between FRBs and magnetars. There also continue to be surprising discoveries, like periodic modulation of activity from repeaters and the localisation of one FRB source to a relatively nearby globular cluster associated with the M81 galaxy. In this review, we summarise the exciting observational results from the past few years. We also highlight their impact on our understanding of the FRB population and proposed progenitor models. We build on the introduction to FRBs in our earlier review, update our readers on recent results, and discuss interesting avenues for exploration as the field enters a new regime where hundreds to thousands of new FRBs will be discovered and reported each year., Invited review article for The Astronomy and Astrophysics Review. Resubmission with community feedback; thank you for your comments
Published: 2021

13. The High Time Resolution Universe Pulsar Survey - XVI. Discovery and timing of 40 pulsars from the southern Galactic plane

Author: Cherry Ng, Samuel Bates, Caterina Tiburzi, N. D. R. Bhat, W. van Straten, Benjamin Stappers, Vishnu Balakrishnan, Chris Flynn, Jingwen Wu, Michael Kramer, Lina Levin, D. J. Champion, Michael Keith, Andrew Lyne, A. D. Cameron, C. G. Bassa, Andrew Jameson, Shivani Bhandari, Simon Johnston, David A. Smith, A. Possenti, Matthew Bailes, M. Burgay, Ewan Barr, E. Petroff, Sarah Burke-Spolaor, Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), and Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)
Subjects: media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, Population, FOS: Physical sciences, Astrophysics, 01 natural sciences, Binary pulsar, Luminosity, stars: neutron, Pulsar, surveys, Millisecond pulsar, pulsars: general, 0103 physical sciences, education, 010303 astronomy & astrophysics, media_common, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), education.field_of_study, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Galactic plane, Orbital period, Universe, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: We present the results of processing an additional 44% of the High Time Resolution Universe South Low Latitude (HTRU-S LowLat) pulsar survey, the most sensitive blind pulsar survey of the southern Galactic plane to date. Our partially-coherent segmented acceleration search pipeline is designed to enable the discovery of pulsars in short, highly-accelerated orbits, while our 72-min integration lengths will allow us to discover pulsars at the lower end of the pulsar luminosity distribution. We report the discovery of 40 pulsars, including three millisecond pulsar-white dwarf binary systems (PSRs J1537-5312, J1547-5709 and J1618-4624), a black-widow binary system (PSR J1745-23) and a candidate black-widow binary system (PSR J1727-2951), a glitching pulsar (PSR J1706-4434), an eclipsing binary pulsar with a 1.5-yr orbital period (PSR J1653-45), and a pair of long spin-period binary pulsars which display either nulling or intermittent behaviour (PSRs J1812-15 and J1831-04). We show that the total population of 100 pulsars discovered in the HTRU-S LowLat survey to date represents both an older and lower-luminosity population, and indicates that we have yet to reach the bottom of the luminosity distribution function. We present evaluations of the performance of our search technique and of the overall yield of the survey, considering the 94% of the survey which we have processed to date. We show that our pulsar yield falls below earlier predictions by approximately 25% (especially in the case of millisecond pulsars), and discuss explanations for this discrepancy as well as future adaptations in RFI mitigation and searching techniques which may address these shortfalls., Comment: 28 pages, 9 figures, 13 tables
Published: 2020

14. The High Time Resolution Universe Pulsar Survey – XV. Completion of the intermediate-latitude survey with the discovery and timing of 25 further pulsars

Author: Samuel Bates, Chris Flynn, Simon Johnston, D. J. Champion, Benjamin Stappers, Michael Kramer, M. Burgay, Matthew Bailes, Andrew Jameson, Michael Keith, Cherry Ng, Lina Levin, W. van Straten, L. Bondonneau, Ralph Eatough, Caterina Tiburzi, N. D. R. Bhat, Ewan Barr, Andrew Lyne, E. Petroff, A. D. Cameron, A. Possenti, Evan Keane, Sarah Burke-Spolaor, Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES)
Subjects: media_common.quotation_subject, J1757−1500, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, 01 natural sciences, J1826−2415, Latitude, Pulsar, J1837−0822, J1638−4233, 0103 physical sciences, Total count, 010303 astronomy & astrophysics, Line (formation), media_common, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Time resolution, Universe, Space and Planetary Science, Sky, [SDU]Sciences of the Universe [physics], Glitch (astronomy), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - High Energy Astrophysical Phenomena, pulsars: individual: J1635−2616
Abstract: We report on the latest six pulsars discovered through our standard pipeline in the intermediate-latitude region (|b| < 15 deg) of the Parkes High Time Resolution Universe Survey (HTRU). We also present timing solutions for the new discoveries and for 19 further pulsars for which only discovery parameters were previously published. Highlights of the presented sample include the isolated millisecond pulsar J1826-2415, the long-period binary pulsar J1837-0822 in a mildly eccentric 98-day orbit with a > 0.27 M_sun companion, and the nulling pulsar J1638-4233, detected only 10% of the time. Other interesting objects are PSR J1757-1500, exhibiting sporadic mode changes, and PSR J1635-2616 showing one glitch over 6 years. The new discoveries bring the total count of HTRU intermediate-latitude pulsars to 113, 25% of which are recycled pulsars. This is the higest ratio of recycled over ordinary pulsars discoveries of all recent pulsar surveys in this region of the sky. Among HTRU recycled pulsars, four are isolated objects. Comparing the characteristics of Galactic fully-recycled isolated MSPs with those of eclipsing binaries ('spiders'), from which the former are believed to have formed, we highlight a discrepancy in their spatial distribution. This may reflect a difference in the natal kick, hence, possibly, a different formation path. On the other hand, however, isolated fully-recycled MSPs spin periods are, on average, longer than those of spiders, in line with what one would expect, from simple magnetic-dipole spin-down, if the former were indeed evolved from the latter., Accepted for publication in MNRAS; 12 pages, 9 figures, 7 tables
Published: 2019

15. The host galaxy of a fast radio burst

Author: Mansi M. Kasliwal, Andrew Jameson, Tsuyoshi Terai, Naoki Yasuda, N. D. R. Bhat, Andrew Williams, Poonam Chandra, Ralph Eatough, W. van Straten, Delphine Perrodin, Yuu Niino, E. D. Barr, Matthew Bailes, Steven Tingay, M. Burgay, M. Caleb, Tomoki Morokuma, Hajime Sugai, Evan Keane, Jacob E. Jencson, Ben Stappers, Shotaro Yamasaki, Takashi Hattori, A. Possenti, Mitchell B. Mickaliger, Randall B. Wayth, Michael Kramer, Jeff Cooke, M. Berezina, Mareki Honma, Tomonori Totani, C. G. Bassa, R. Allen, David L. Kaplan, Shivani Bhandari, Nozomu Tominaga, Simon Johnston, Hisanori Furusawa, E. Petroff, Sarah Burke-Spolaor, and Chris Flynn
Subjects: Physics, Multidisciplinary, 010308 nuclear & particles physics, Radio galaxy, Fast radio burst, Astrophysics::High Energy Astrophysical Phenomena, Canadian Hydrogen Intensity Mapping Experiment, Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Redshift survey, 01 natural sciences, Redshift, Galaxy, Interstellar medium, X-shaped radio galaxy, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: In recent years, millisecond-duration radio signals originating in distant galaxies appear to have been discovered in the so-called fast radio bursts. These signals are dispersed according to a precise physical law and this dispersion is a key observable quantity, which, in tandem with a redshift measurement, can be used for fundamental physical investigations. Every fast radio burst has a dispersion measurement, but none before now have had a redshift measurement, because of the difficulty in pinpointing their celestial coordinates. Here we report the discovery of a fast radio burst and the identification of a fading radio transient lasting ~6 days after the event, which we use to identify the host galaxy; we measure the galaxy’s redshift to be z = 0.492 ± 0.008. The dispersion measure and redshift, in combination, provide a direct measurement of the cosmic density of ionized baryons in the intergalactic medium of ΩIGM = 4.9 ± 1.3 per cent, in agreement with the expectation from the Wilkinson Microwave Anisotropy Probe, and including all of the so-called ‘missing baryons’. The ~6-day radio transient is largely consistent with the radio afterglow of a short γ-ray burst, and its existence and timescale do not support progenitor models such as giant pulses from pulsars, and supernovae. This contrasts with the interpretation of another recently discovered fast radio burst, suggesting that there are at least two classes of bursts.
Published: 2016

16. The SUrvey for Pulsars and Extragalactic Radio Bursts – II. New FRB discoveries and their follow-up

Author: Matthew Bailes, T. A. Pritchard, Mitchell B. Mickaliger, A. Trovato, C. Lachaud, Maurizio Spurio, A.J. Heijboer, M. Anghinolfi, N. El Khayati, Ivan Felis, Daniele Vivolo, S. Loucatos, Utane Sawangwit, M. Marcelin, R. Coniglione, Paolo Sapienza, A. Klotz, J. Zúñiga, S.F. Biagi, Dominique Lefèvre, Jörn Wilms, J. Hofestädt, Alba Domi, C. Racca, Silvia Celli, D. Dornic, S. Basa, M. de Jong, I. El Bojaddaini, A. Marinelli, V. Popa, Dominik Elsässer, Tomonori Totani, V. Bertin, M. Circella, Timothée Grégoire, A. Ettahiri, A. Sánchez-Losa, C. Pellegrino, Anne Deschamps, Yann Hello, Matteo Sanguineti, Eric Howell, Steffen Hallmann, J. Carr, Annarita Margiotta, Antoine Kouchner, M. Saldaña, M.C. Bouwhuis, J. A. Green, Michel André, F. Schüssler, I. Salvadori, D. Turpin, Paolo Piattelli, R. Bormuth, Thomas Eberl, Sarah Burke-Spolaor, Richard Wilson, R. Mele, C. Perrina, Alessandro Corongiu, Tommaso Chiarusi, G.E. Păvălaş, Hervé Glotin, V. Van Elewyck, J. Busto, Pablo Torne, P. Jaroenjittichai, E. Petroff, E. Nezri, V. Venkatraman Krishnan, M. Jongen, V. Morello, P. Migliozzi, A. Creusot, G. De Bonis, Joao Coelho, R. Bruijn, J. Hößl, T. Avgitas, Jürgen Brunner, D. Kießling, Federico Versari, M. Organokov, C. Distefano, Juan José Hernández-Rey, O. Kalekin, D. F. E. Samtleben, M. Taiuti, C. Tönnis, A. Enzenhöfer, Giulia Illuminati, I. Di Palma, J.A. Martínez-Mora, Alexis Coleiro, M. Caleb, C. Hugon, C. Sieger, Michael Kramer, H. Brânzaş, J-J. Aubert, Emanuele Leonora, Antonio F. Díaz, P. Coyle, Poonam Chandra, L. Caramete, Giorgio Riccobene, F. Jankowski, Richard Dodson, Th. Stolarczyk, J.D. Zornoza, B. Vallage, Alessio Trois, Vladimir Kulikovskiy, Miguel Ardid, B. Belhorma, Chris Flynn, M. Kreter, Gisela Anton, A. Jameson, A. Vizzocca, V. Giordano, A. Capone, H. van Haren, Timothy Butterley, T. Pradier, R. Cherkaoui El Moursli, Evan Keane, S. Bourret, Ralph Eatough, David Coward, W. van Straten, S. Navas, Delphine Perrodin, U. F. Katz, V. S. Dhillon, Farida Fassi, I. Andreoni, E. D. Barr, C. W. James, Kay Graf, Karel Melis, Jeff Cooke, S. P. Littlefair, Arnauld Albert, Caterina Tiburzi, T. R. Marsh, N. D. R. Bhat, L. K. Hardy, Abdelilah Moussa, Doriane Drouhin, Benjamin Stappers, I. Kreykenbohm, Yuu Niino, Bruny Baret, Simon Johnston, Robert Lahmann, A. Possenti, L. Quinn, Shivani Bhandari, Nozomu Tominaga, Yahya Tayalati, R. Gracia-Ruiz, Tsuyoshi Terai, H. Costantini, J. Barrios-Martí, Luigi Antonio Fusco, Matthias Kadler, T. Michael, T. W. B. Muxlow, M. Burgay, C. Donzaud, 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), Groupe de Recherche en Physique des Hautes Energies (GRPHE), Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut Universitaire de Technologie de Colmar, Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-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)), 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), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11), Laboratoire de Physique de Clermont (LPC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne (UCA), Laboratoire des Sciences de l'Information et des Systèmes (LSIS), Centre National de la Recherche Scientifique (CNRS)-Arts et Métiers Paristech ENSAM Aix-en-Provence-Université de Toulon (UTLN)-Aix Marseille Université (AMU), Institut Universitaire de France (IUF), Ministère de l'Education nationale, de l’Enseignement supérieur et de la Recherche (M.E.N.E.S.R.), Institut méditerranéen d'océanologie (MIO), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Département de Physique des Particules (ex SPP) (DPP), 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 Pluridisciplinaire Hubert Curien (IPHC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS), ANTARES, Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), 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)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Clermont Auvergne (UCA)-Centre National de la Recherche Scientifique (CNRS), Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Arts et Métiers Paristech ENSAM Aix-en-Provence-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université de Toulon (UTLN)-Aix Marseille Université (AMU)-Institut de Recherche pour le Développement (IRD), Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-IUT de Colmar, Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Département de Physique des Particules (ex SPP) (DPhP), Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), 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 ), Centre de Physique des Particules de Marseille ( CPPM ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Aix Marseille Université ( AMU ), 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 ), Laboratoire d'Astrophysique de Marseille ( LAM ), Aix Marseille Université ( AMU ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National d'Etudes Spatiales ( CNES ) -Centre National de la Recherche Scientifique ( CNRS ), Observatoire de la Côte d'Azur ( OCA ), Centre National de la Recherche Scientifique ( CNRS ), Université Paris-Sud - Paris 11 ( UP11 ), Laboratoire de Physique de Clermont ( LPC ), Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Clermont Auvergne ( UCA ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire des Sciences de l'Information et des Systèmes ( LSIS ), Aix Marseille Université ( AMU ) -Université de Toulon ( UTLN ) -Arts et Métiers Paristech ENSAM Aix-en-Provence-Centre National de la Recherche Scientifique ( CNRS ), Institut méditerranéen d'océanologie ( MIO ), Centre National de la Recherche Scientifique ( CNRS ) -Université de Toulon ( UTLN ) -Aix Marseille Université ( AMU ) -Institut de Recherche pour le Développement ( IRD ), Département de Physique des Particules (ex SPP) ( DPP ), 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 Pluridisciplinaire Hubert Curien ( IPHC ), Centre National de la Recherche Scientifique ( CNRS ) -Université de Strasbourg ( UNISTRA ), Centre Tecnològic de Vilanova i la Geltrú, Universitat Politècnica de Catalunya. LAB - Laboratori d'Aplicacions Bioacústiques, 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), Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS), KM3NeT (IHEF, IoP, FNWI), Bhandari, S, Keane, Ef, Barr, Ed, Jameson, A, Petroff, E, Johnston, S, Bailes, M, Bhat, Ndr, Burgay, M, Burke-Spolaor, S, Caleb, M, Eatough, Rp, Flynn, C, Green, Ja, Jankowski, F, Kramer, M, Krishnan, Vv, Morello, V, Possenti, A, Stappers, B, Tiburzi, C, van Straten, W, Andreoni, I, Butterley, T, Chandra, P, Cooke, J, Corongiu, A, Coward, Dm, Dhillon, V, Dodson, R, Hardy, Lk, Howell, Ej, Jaroenjittichai, P, Klotz, A, Littlefair, Sp, Marsh, Tr, Mickaliger, M, Muxlow, T, Perrodin, D, Pritchard, T, Sawangwit, U, Terai, T, Tominaga, N, Torne, P, Totani, T, Trois, A, Turpin, D, Niino, Y, Wilson, Rw, Albert, A, Andre, M, Anghinolfi, M, Anton, G, Ardid, M, Aubert, Jj, Avgitas, T, Baret, B, Barrios-Marti, J, Basa, S, Belhorma, B, Bertin, V, Biagi, S, Bormuth, R, Bourret, S, Bouwhuis, Mc, Branzas, H, Bruijn, R, Brunner, J, Busto, J, Capone, A, Caramete, L, Carr, J, Celli, S, El Moursli, Rc, Chiarusi, T, Circella, M, Coelho, Jab, Coleiro, A, Coniglione, R, Costantini, H, Coyle, P, Creusot, A, Diaz, Af, Deschamps, A, De Bonis, G, Distefano, C, Di Palma, I, Domi, A, Donzaud, C, Dornic, D, Drouhin, D, Eberl, T, El Bojaddaini, I, Khayati, N, Elasser, D, Enzenhoefer, A, Ettahiri, A, Fassi, F, Felis, I, Fusco, La, Gay, P, Giordano, V, Glotin, H, Gregoire, T, Gracia-Ruiz, R, Graf, K, Hallmann, S, van Haren, H, Heijboer, Aj, Hello, Y, Hernandez-Rey, Jj, Hossl, J, Hofestadt, J, Hugon, C, Illuminati, G, James, Cw, de Jong, M, Jongen, M, Kadler, M, Kalekin, O, Katz, U, Kiessling, D, Kouchner, A, Kreter, M, Kreykenbohm, I, Kulikovskiy, V, Lachaud, C, Lahmann, R, Lefevere, D, Leonora, E, Loucatos, S, Marcelin, M, Margiotta, A, Marinelli, A, Martinez-Mora, Ja, Mele, R, Melis, K, Michael, T, Migliozzi, P, Moussa, A, Navas, S, Nezri, E, Organokov, M, Pavalas, Ge, Pellegrino, C, Perrina, C, Piattelli, P, Popa, V, Pradier, T, Quinn, L, Racca, C, Riccobene, G, Sanchez-Losa, A, Saldana, M, Salvadori, I, Samtleben, Dfe, Sanguineti, M, Sapienza, P, Schussler, F, Sieger, C, Spurio, M, Stolarczyk, T, Taiuti, M, Tayalati, Y, Trovato, A, Tonnis, C, Vallage, B, Van Elewyck, V, Versari, F, Vivolo, D, Vizzocca, A, Wilms, J, Zornoza, Jd, Zuniga, J, Bhandari, S., Keane, E.F., Barr, E.D., Jameson, A., Petroff, E., Johnston, S., Bailes, M., Bhat, N.D.R., Burgay, M., Burke-Spolaor, S., Caleb, M., Eatough, R.P., Flynn, C., Green, J.A., Jankowski, F., Kramer, M., Venkatraman Krishnan, V., Morello, V., Possenti, A., Stappers, B., Tiburzi, C., van Straten, W., Andreoni, I., Butterley, T., Chandra, P., Cooke, J., Corongiu, A., Coward, D.M., Dhillon, V.S., Dodson, R., Hardy, L.K., Howell, E.J., Jaroenjittichai, P., Klotz, A., Littlefair, S.P., Marsh, T.R., Mickaliger, M., Muxlow, T., Perrodin, D., Pritchard, T., Sawangwit, U., Terai, T., Tominaga, N., Torne, P., Totani, T., Trois, A., Turpin, D., Niino, Y., Wilson, R.W., Albert, A., André, M., Anghinolfi, M., Anton, G., Ardid, M., Aubert, J.-J., Avgitas, T., Baret, B., Barrios-Martí, J., Basa, S., Belhorma, B., Bertin, V., Biagi, S., Bormuth, R., Bourret, S., Bouwhuis, M.C., Brănzas, H., Bruijn, R., Brunner, J., Busto, J., Capone, A., Caramete, L., Carr, J., Celli, S., El Moursli, R. Cherkaoui, Chiarusi, T., Circella, M., Coelho, J.A.B., Coleiro, A., Coniglione, R., Costantini, H., Coyle, P., Creusot, A., Díaz, A.F., Deschamps, A., De Bonis, G., Distefano, C., Di Palma, I., Domi, A., Donzaud, C., Dornic, D., Drouhin, D., Eberl, T., El Bojaddaini, I., El Khayati, N., Elsässer, D., Enzenhöfer, A., Ettahiri, A., Fassi, F., Felis, I., Fusco, L.A., Gay, P., Giordano, V., Glotin, H., Gregoire, T., Gracia-Ruiz, R., Graf, K., Hallmann, S., van Haren, H., Heijboer, A.J., Hello, Y., Hernández-Rey, J.J., Hößl, J., Hofestädt, J., Hugon, C., Illuminati, G., James, C.W., de Jong, M., Jongen, M., Kadler, M., Kalekin, O., Katz, U., Kießling, D., Kouchner, A., Kreter, M., Kreykenbohm, I., Kulikovskiy, V., Lachaud, C., Lahmann, R., Lefevre, D., Leonora, E., Loucatos, S., Marcelin, M., Margiotta, A., Marinelli, A., Martínez-Mora, J.A., Mele, R., Melis, K., Michael, T., Migliozzi, P., Moussa, A., Navas, S., Nezri, E., Organokov, M., Pavalas, G.E., Pellegrino, C., Perrina, C., Piattelli, P., Popa, V., Pradier, T., Quinn, L., Racca, C., Riccobene, G., Sánchez-Losa, A., Saldana, M., Salvadori, I., Samtleben, D.F.E., Sanguineti, M., Sapienza, P., Schüssler, F., Sieger, C., Spurio, M., Stolarczyk, Th., Taiuti, M., Tayalati, Y., Trovato, A., Tönnis, C., Vallage, B., Van Elewyck, V., Versari, F., Vivolo, D., Vizzocca, A., Wilms, J., Zornoza, J.D., Zúniga, J., Keane, E. F., Barr, E. D., Bhat, N. D. R., Eatough, R. P., Green, J. A., Coward, D. M., Dhillon, V. S., Hardy, L. K., Howell, E. J., Littlefair, S. P., Marsh, T. R., Wilson, R. W., Andre, M., Aubert, J. -J., Barrios-Marti, J., Bouwhuis, M. C., Branzas, H., El Moursli, R. C., Coelho, J. A. B., Diaz, A. F., Elsasser, D., Enzenhofer, A., Fusco, L. A., Heijboer, A. J., Hernandez-Rey, J. J., Hossl, J., Hofestadt, J., James, C. W., Kiessling, D., Martinez-Mora, J. A., Pavalas, G. E., Sanchez-Losa, A., Samtleben, D. F. E., Schussler, F., Stolarczyk, T., Tonnis, C., Zornoza, J. D., and Zuniga, J.
Subjects: surveys – intergalactic medium, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], data analysis, Astrophysics, Surveys, 7. Clean energy, 01 natural sciences, radiation mechanisms, observational surveys, intergalactic medium, radio continuum, Astronomical observatories, Methods: Data analysis, Survey, data analysis [Methods], 010303 astronomy & astrophysics, media_common, general [Radiation mechanisms], Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Fast radio burst, general [Radio continuum], Canadian Hydrogen Intensity Mapping Experiment, Intergalactic medium, Methods: Observational, Radiation mechanisms: General, Radio continuum: General, Neutrino, Observatoris astronòmics, Astrophysics - High Energy Astrophysical Phenomena, general [adio continuum], media_common.quotation_subject, FOS: Physical sciences, Methods: Data analysi, Radio telescope, Pulsar, 0103 physical sciences, Radiation mechanisms, observational [Methods], Source counts, Telescopis, Astronomy and Astrophysics, Space and Planetary Science, 010308 nuclear & particles physics, radiation mechanisms: general, methods: data analysis, methods: observational, radio continuum: general, Astronomy, Astronomy and Astrophysic, Afterglow, Radio continuum, 13. Climate action, Sky, FISICA APLICADA, Física::Astronomia i astrofísica [Àrees temàtiques de la UPC], data analysi [methods], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Telescopes
Abstract: SB would like to thank Tara Murphy, Martin Bell, Paul Hancock, Keith Bannister, Chris Blake and Bing Zhang for useful discussions., We report the discovery of four Fast Radio Bursts (FRBs) in the ongoing SUrvey for Pulsars and Extragalactic Radio Bursts at the Parkes Radio Telescope: FRBs 150610, 151206, 151230 and 160102. Our real-time discoveries have enabled us to conduct extensive, rapid multimessenger follow-up at 12 major facilities sensitive to radio, optical, X-ray, gamma-ray photons and neutrinos on time-scales ranging from an hour to a few months post-burst. No counterparts to the FRBs were found and we provide upper limits on afterglow luminosities. None of the FRBs were seen to repeat. Formal fits to all FRBs show hints of scattering while their intrinsic widths are unresolved in time. FRB 151206 is at low Galactic latitude, FRB 151230 shows a sharp spectral cut-off, and FRB 160102 has the highest dispersion measure (DM = 2596.1 ± 0.3 pc cm−3) detected to date. Three of the FRBs have high dispersion measures (DM > 1500 pc cm−3), favouring a scenario where the DM is dominated by contributions from the intergalactic medium. The slope of the Parkes FRB source counts distribution with fluences >2 Jy ms is α=−2.2+0.6−1.2 and still consistent with a Euclidean distribution (α = −3/2). We also find that the all-sky rate is 1.7+1.5−0.9×103 FRBs/(4π sr)/day above ∼2Jyms and there is currently no strong evidence for a latitude-dependent FRB sky rate., The Parkes radio telescope and the Australia Telescope Compact Array are part of the Australia Telescope National Facility which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. Parts of this research were conducted by the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020. The GMRT is run by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research. VLAis run by theNational Radio Astronomy Observatory (NRAO). NRAO is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This work was performed on the gSTAR national facility at Swinburne University of Technology. gSTAR is funded by Swinburne and the Australian Government’s Education Investment Fund. This work is also based on data collected at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. We thank the LSST Project for making their code available as free software at http://dm.lsstcorp.org. Funding from the European Research Council under the European Union’s Seventh Framework Programme (FP/2007-2013) / ERC Grant Agreement n. 617199 (EP). Access to the Lovell Telescope is supported through an STFC consolidated grant. The 100-m telescope in Effelsberg is operation by the Max- Planck-Institut für Radioastronomie with funds of the Max-Planck Society. The Sardinia Radio Telescope (SRT) is funded by the Department of University and Research (MIUR), the Italian Space Agency (ASI), and the Autonomous Region of Sardinia (RAS) and is operated as National Facility by the National Institute for Astrophysics (INAF). TB and RWW are grateful to the STFC for financial support (grant reference ST/P000541/1). Research support to IA is provided by the Australian Astronomical Observatory. The ANTARES authors acknowledge the financial support of the funding agencies: Centre National de la Recherche Scientifique (CNRS), Commissariat à l’énergie atomique et aux énergies alternatives (CEA), Commission Européenne (FEDER fund and Marie Curie Program), Institut Universitaire de France (IUF), IdEx program and UnivEarthS Labex program at Sorbonne Paris Cité (ANR-10- LABX-0023 and ANR-11-IDEX-0005-02), Labex OCEVU (ANR- 11-LABX-0060) and the A*MIDEX project (ANR-11-IDEX-0001- 02), Région Île-de-France (DIM-ACAV), Région Alsace (contrat CPER), Région Provence-Alpes-Côte d’Azur, Département du Var and Ville de La Seyne-sur-Mer, France; Bundesministerium für Bildung und Forschung (BMBF), Germany; IstitutoNazionale di Fisica Nucleare (INFN), Italy; Stichting voor Fundamenteel Onderzoek der Materie (FOM), Nederlandse organisatie voor Wetenschappelijk Onderzoek (NWO), the Netherlands; Council of the President of the Russian Federation for young scientists and leading scientific schools supporting grants, Russia; National Authority for Scientific Research (ANCS), Romania; Ministerio de Economía y Competitividad (MINECO): Plan Estatal de Investigación (refs. FPA2015- 65150-C3-1-P, -2-P and -3-P, (MINECO/FEDER)), Severo Ochoa Centre of Excellence and MultiDark Consolider (MINECO), and Prometeo and Grisolía programs (Generalitat Valenciana), Spain; Ministry of Higher Education, Scientific Research and Professional Training, Morocco. We also acknowledge the technical support of Ifremer, AIM and Foselev Marine for the sea operation and the CC-IN2P3 for the computing facilities. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. This research has made use of data, software and/or web tools obtained from the High Energy Astrophysics Science Archive Research Center (HEASARC), a service of the Astrophysics Science Division at NASA/GSFC and of the Smithsonian Astrophysical Observatory’s High Energy Astrophysics Division. This work is based in part on data collected at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. This paper makes use of software developed for the Large Synoptic Survey Telescope. We thank the LSST Project for making their code available as free software at http://dm.lsstcorp.org. RPE/MK gratefully acknowledges support from ERC Synergy Grant "BlackHoleCam" Grant Agreement Number 610058
Published: 2018

17. Fast radio bursts: search sensitivities and completeness

Author: E. Petroff and Evan Keane
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, law.invention, Telescope, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, law, Sky, Intergalactic medium, Astrophysics - High Energy Astrophysical Phenomena, Completeness (statistics), Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Cosmology and Nongalactic Astrophysics, media_common
Abstract: In this paper we identify some sub-optimal performance in algorithms that search for Fast Radio Bursts (FRBs), which can reduce the cosmological volume probed by over 20%, and result in missed discoveries and incorrect flux density and sky rate determinations. Re-calculating parameters for all of the FRBs discovered with the Parkes telescope (i.e. all of the reported FRBs bar one), we find some inconsistencies with previously determined values, e.g. FRB 010125 was approximately twice as bright as previously reported. We describe some incompleteness factors not previously considered which are important in determining accurate population statistics, e.g. accounting for fluence incompleteness the Thornton et al. all-sky rate can be re-phrased as ~2500 FRBs per sky per day above a 1.4-GHz fluence of ~2 Jy ms. Finally we make data for the FRBs easily available, along with software to analyse these., Accepted for publication in MNRAS, 5 pages, 2 figures, 2 tables. FRB data to appear on Research Data Australia upon publication in MNRAS
Published: 2015

18. The High Time Resolution Universe Pulsar Survey - XIII. PSR J1757-1854, the most accelerated binary pulsar

Author: Thomas M. Tauris, Michael Kramer, Paulo C. C. Freire, Duncan R. Lorimer, Caterina Tiburzi, A. D. Cameron, Matthew Bailes, Andrew Jameson, Benjamin Stappers, N. D. R. Bhat, Michael Keith, Lina Levin, Cherry Ng, Ramesh Karuppusamy, Ralph Eatough, Ewan Barr, Norbert Wex, Shivani Bhandari, Simon Johnston, Chris Flynn, D. J. Champion, Maura McLaughlin, A. Possenti, W. van Straten, C. G. Bassa, E. Petroff, Alessandro Ridolfi, M. Burgay, Sarah Burke-Spolaor, and Andrew Lyne
Subjects: astro-ph.SR, Astrophysics::High Energy Astrophysical Phenomena, Pulsar planet, FOS: Physical sciences, Astrophysics, General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, Binary pulsar, General Relativity and Quantum Cosmology, Gravitation, Pulsar, surveys, Millisecond pulsar, Tests of general relativity, 0103 physical sciences, 010306 general physics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Physics, High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.HE, binaries: close, pulsars: individual: PSR, Astronomy, Astronomy and Astrophysics, J1757-1854, Neutron star, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, gravitation, Astrophysics::Earth and Planetary Astrophysics, Relativistic quantum chemistry, Astrophysics - High Energy Astrophysical Phenomena
Abstract: We report the discovery of PSR J1757$-$1854, a 21.5-ms pulsar in a highly-eccentric, 4.4-h orbit around a neutron star (NS) companion. PSR J1757$-$1854 exhibits some of the most extreme relativistic parameters of any known pulsar, including the strongest relativistic effects due to gravitational-wave (GW) damping, with a merger time of 76 Myr. Following a 1.6-yr timing campaign, we have measured five post-Keplerian (PK) parameters, yielding the two component masses ($m_\text{p}=1.3384(9)\,\text{M}_\odot$ and $m_\text{c}=1.3946(9)\,\text{M}_\odot$) plus three tests of general relativity (GR), which the theory passes. The larger mass of the NS companion provides important clues regarding the binary formation of PSR J1757$-$1854. With simulations suggesting 3-$\sigma$ measurements of both the contribution of Lense-Thirring precession to the rate of change of the semi-major axis and the relativistic deformation of the orbit within $\sim7-9$ years, PSR J1757$-$1854 stands out as a unique laboratory for new tests of gravitational theories., Comment: 6 pages, 2 figures, 2 tables
Published: 2017

19. Search for neutrinos from Fast Radio Bursts with ANTARES

Author: Damien Turpin, Damien Dornic, Shivani Bhandari, Evan Keane, Alexis Coleiro, Matteo Sanguineti, E. Petroff, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Centre de Physique des Particules de Marseille (CPPM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), 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), ANTARES, SUPERB, Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), 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), 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: Physics, ANTARES, radio wave: burst, Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, brightness, Astrophysics::Instrumentation and Methods for Astrophysics, model: hadronic, Astronomy, Context (language use), Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy, Universe, observatory, messenger, particle: acceleration, Particle acceleration, Observatory, galaxy, Neutrino, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics, Dwarf galaxy, media_common, Radio wave
Abstract: International audience; Fast Radio Bursts are one of the most mysterious transient sources. They are characterised by an intense radio-pulse lasting few milliseconds and mainly detected in the GHz energy band. Many unknowns remain concerning the nature of the transient progenitor, the nature of the radio emission and their distribution in the Universe. Recently, the first evidence on the association between the repeating burst FRB121102 and a star-forming dwarf galaxy located at the cosmo- logical distance z = 0.19 was reported. These observations imply that at least some of the fast radio bursts indeed originate from the distant Universe and have to be associated with extremely violent events to explain their observed brightness. So far, the radiative processes powering the radio emission are unknown but efficient particle acceleration may occur in the vicinity of the progenitor. A multi-wavelength and a multi-messenger approach are therefore crucial to identify the nature of these acceleration mechanisms. In this context, a search for a high-energy neutrino signal from the most recent radio bursts has been performed with the ANTARES neutrino tele- scope. By design, ANTARES mainly observes the Southern sky (2π steradian at any time) and is perfectly suited to search for a neutrino signal from sources of transients that have been mainly detected at the Parkes observatory in Australia. In this contribution, we will present the results of our searches with ANTARES and their implications for hadronic models of FRBs.
Published: 2017

20. The SUrvey for Pulsars and Extragalactic Radio Bursts I: Survey Description and Overview

Author: Matthew Bailes, Shivani Bhandari, Michael Kramer, Caterina Tiburzi, N. D. R. Bhat, V. Morello, Ewan Barr, Simon Johnston, Cherry Ng, W. van Straten, E. Petroff, A. Jameson, Evan Keane, F. Jankowski, Ralph Eatough, M. Caleb, M. Burgay, Chris Flynn, Sarah Burke-Spolaor, Lina Levin, A. Possenti, and V. Venkatraman Krishnan
Subjects: media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, Binary number, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Electromagnetic interference, Radio telescope, Pulsar, surveys, Millisecond pulsar, 0103 physical sciences, Eccentricity (behavior), 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), media_common, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Orbital period, methods: data analysis, Orbit, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, methods: observational, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: We describe the Survey for Pulsars and Extragalactic Radio Bursts (SUPERB), an ongoing pulsar and fast transient survey using the Parkes radio telescope. SUPERB involves real-time acceleration searches for pulsars and single-pulse searches for pulsars and fast radio bursts. We report on the observational setup, data analysis, multi-wavelength/messenger connections, survey sensitivities to pulsars and fast radio bursts and the impact of radio frequency interference. We further report on the first 10 pulsars discovered in the project. Among these is PSR~J1306$-$40, a millisecond pulsar in a binary system where it appears to be eclipsed for a large fraction of the orbit. PSR~J1421$-$4407 is another binary millisecond pulsar; its orbital period is $30.7$ days. This orbital period is in a range where only highly eccentric binaries are known, and expected by theory; despite this its orbit has an eccentricity of $10^{-5}$., Accepted for publication in MNRAS, 21 pages, 18 figures, 6 tables
Published: 2017

21. A polarized fast radio burst at low Galactic latitude

Author: M. de Jong, Michael Punch, Mansi M. Kasliwal, T. A. Pritchard, S. Galatà, K. Egberts, S. Loucatos, C. Tönnis, S. Öttl, G. Pelletier, Ivan Felis, Mitchell B. Mickaliger, Jacek Niemiec, G. Cologna, Robert Wagner, A. Gleixner, C. Racca, P. J. Meintjes, Thomas Lohse, Jamie Farnes, Olaf Reimer, F. Ait Benkhali, L. O'c. Drury, P. de Wilt, R. Chalme-Calvet, I. Salvadori, Kay Graf, Karel Melis, A. Vizzoca, I. El Bojaddaini, G. Heinzelmann, C. B. Rulten, Bruny Baret, Heinrich J. Völk, Manami Sasaki, S. Schwemmer, Q. Piel, Andrea Santangelo, Thomas Vuillaume, Guillaume Dubus, A. Jacholkowska, Simon Johnston, J. Chevalier, Julien Lefaucheur, M. Renaud, K. Dutson, F. Spies, D. Dornic, C. Farnier, A. Trovato, E. Leser, Tanya Edwards, Jean-Pierre Macquart, L. Tibaldo, Thomas Murach, C. Lachaud, A. Marinelli, I. D. Davids, Ramin Marx, M. Panter, U. Katz, Silvia Celli, Timothée Grégoire, D. Kiessling, Antoine Kouchner, Marco Padovani, Matthias Kadler, Francois Brun, A. Ivascenko, E. D. Barr, C. W. James, Daniela Hadasch, C. Perrina, Maria Tselengidou, G. Hermann, Regis Terrier, D. Klochkov, Johan Bregeon, W. Kluzniak, M. Kieffer, P. Vincent, Y. Cui, S. Bernhard, L. Stawarz, A. Ziegler, M.C. Bouwhuis, C. Romoli, Dieter Horns, Mateusz Janiak, B. van Soelen, B. Rudak, T. Michael, Nachiketa Chakraborty, Caterina Tiburzi, N. Zywucka, Alison Mitchell, B. Degrange, Santiago Pita, R. Blackwell, Reinhard Schlickeiser, I. Kreykenbohm, Annarita Margiotta, Jutta Schnabel, M. Jingo, R. J. White, Thomas Eberl, H. Laffon, M. Lotze, Christo Venter, Tommaso Chiarusi, M. Anghinolfi, Maura McLaughlin, Zorawar Wadiasingh, B. Condon, D. A. Sanchez, M. Mayer, V. Lefranc, H. Abdalla, M. A. Kastendieck, S. Bourret, G. Vasileiadis, Iryna Lypova, Yvonne Becherini, G. Illuminati, Clemens Hoischen, A. A. Zdziarski, S. Geisselsoder, I. Shilon, E. O. Angüner, Domenico Tiziani, K. Kosack, Konrad Bernlöhr, A. Enzenhöfer, R. Moderski, V. S. Dhillon, Evan Keane, G. Lamanna, Riaan Steenkamp, Matthew Bailes, M. Füssling, A. Zech, V. Van Elewyck, M. Taiuti, J. Decock, Ullrich Schwanke, Monica Barnard, D. Zaborov, O. Kalekin, M. Circella, Y. A. Gallant, N. D. R. Bhat, A. Creusot, Victor Zabalza, Th. Stolarczyk, B. Vallage, N. Maxted, Dominique Lefèvre, L. Dirson, E. Petroff, D. Jankowsky, M.-H. Grondin, C. Perennes, Markus Böttcher, E. Nezri, A. G. Akhperjanian, Maria Haupt, Jürgen Brunner, G. Pühlhofer, S. Klepser, A. Wörnlein, Denis Wouters, Armin Rest, A. Possenti, R. C. G. Chaves, C. Mueller, P. Coyle, F. Zefi, Poonam Chandra, F. Niederwanger, R. D. Parsons, Anne Deschamps, T. Seitz, Daniele Vivolo, D. J. Champion, C. Sieger, J. Dyks, F. Schüssler, L. Caramete, A. Reimer, Felix Spanier, Dominik Elsässer, H. van Haren, S. R. Bernard, T. Garrigoux, K. Morå, I. Di Palma, L. K. Hardy, David Salek, E. Moulin, Justine Devin, Michal Ostrowski, Tomasz Bulik, J.-P. Lenain, Luigi Antonio Fusco, Thomas Tavernier, Matteo Sanguineti, A. Sánchez-Losa, M. Capasso, S. J. Fegan, A. Djannati-Ataï, G. Riccobene, Gianluca Giavitto, Benjamin Stappers, Gilles Maurin, I. Oya, L. Quinn, Axel Donath, Jacco Vink, A. W. Chen, J. Zúñiga, A. S. Seyffert, R. Miller, Pierre-Henri Aubert, Nu. Komin, Sabrina Casanova, Andrew M. Taylor, Jörn Wilms, M. Kreter, Mark Sullivan, Michael Kramer, S. Krakau, V. Sahakian, R. Bruijn, Andreas Quirrenbach, J-J. Aubert, R. Borrnuth, M. Saldaña, Aion Viana, C. Mariaud, Joao A B Coelho, J. P. Lees, P. Migliozzi, D. J. van der Walt, M. Settimo, C. Vallée, Christian Stegmann, Stefan Wagner, Gisela Anton, Bruno Khelifi, Jan Conrad, M. Marcelin, V. Giordano, M. Lorentz, M. Kraus, D. Kerszberg, T. Avgitas, Rachel Simoni, Helen Poon, J.A. Martínez-Mora, Alexis Coleiro, Antonia Rowlinson, S. Raab, Stefan Funk, Alicja Wierzcholska, B. Peyaud, Yasunobu Uchiyama, R. J. Tuffs, L. Mohrmann, Juan José Hernández-Rey, T. Jogler, D.A. Prokhorov, Michel André, Frank M. Rieger, J.D. Zornoza, A. Schulz, T. Pradier, S. Wagner, A. Abramowski, R. Mele, S. Rosier-Lees, G. Spengler, Yann Hello, J. Lau, C. van Rensburg, M. Holler, R. Coniglione, Arnauld Albert, Emanuele Leonora, A. Balzer, Michael Zacharias, M. Mohamed, Yahya Tayalati, J. Carr, I. Jung-Richardt, A. Mathieu, A. Fiasson, Roberta Zanin, P. Willmann, Hervé Glotin, K. Geyer, K. Roensch, Michael Backes, Alexandre Marcowith, J. King, J. Hofestädt, P. P. Krüger, K. Stycz, Jeff Cooke, S. P. Littlefair, H. Odaka, Felix Jankowsky, N. Shafi, M. de Naurois, Krzysztof Katarzynski, Jim Hinton, Matteo Cerruti, P. Bordas, Robert Lahmann, F. Krayzel, V. Bertin, J. Barrios-Martí, R. Liu, Stefan Ohm, W. van Straten, Christoph Deil, J. Hossl, P. Jaroenjittichai, Léa Jouvin, R. Gracia-Ruiz, T. Andersson, W. Domainko, Gerard Fontaine, Felix Aharonian, J. F. Glicenstein, Maurizio Spurio, V. Popa, Catherine Boisson, D. Drouhin, Paolo Piattelli, Olivier Hervet, Pierre Brun, F. Voisin, M. Jongen, D. Kolitzus, C. Trichard, M. Arrieta, Utane Sawangwit, Heike Prokoph, P. T. O'Brien, Paolo Sapienza, A. Förster, Ruben Lopez-Coto, M. Lemoine-Goumard, Abdelilah Moussa, S. Eschbach, M. V. Fernandes, A.J. Heijboer, Steffen Hallmann, C. Hugon, Ruizhi Yang, D. Turpin, Werner Hofmann, Stefano Gabici, S.F. Biagi, P. Wagner, V. Marandon, Jean-Pierre Ernenwein, C. Distefano, S. Colafrancesco, D. F. E. Samtleben, Vladimir Kulikovskiy, Marek Jamrozy, I. Andreoni, Corinne Donzaud, Vikram Ravi, Joachim Hahn, Shivani Bhandari, L. Oakes, Johannes Veh, M. Tluczykont, M. Caleb, Gilles Henri, J. Bolmont, J. Hawkes, I. Sushch, S. Basa, M. Chrétien, Sarah Burke-Spolaor, M. Gajdus, G.E. Păvălaş, C. Pellegrino, H. Costantini, Peter Eger, F. Stinzing, C. van Eldik, D. Berge, G. De Bonis, B. Giebels, A. Capone, Helene Sol, J. Busto, J. Becker Tjus, J.-P. Tavernet, Gavin Rowell, M. Bryan, R. de los Reyes, P.-O. Petrucci, N. W. Pekeur, Manuel Meyer, A. Goya, M. Burgay, Miguel Ardid, D. Gottschall, Anne Lemiere, Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, 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), 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), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Petroff, E, Burke-Spolaor, S, Keane, Ef, Mclaughlin, Ma, Miller, R, Andreoni, I, Bailes, M, Barr, Ed, Bernard, Sr, Bhandari, S, Bhat, Ndr, Burgay, M, Caleb, M, Champion, D, Chandra, P, Cooke, J, Dhillon, V, Farnes, J, Hardy, Lk, Jaroenjittichai, P, Johnston, S, Kasliwal, M, Kramer, M, Littlefair, Sp, Macquart, Jp, Mickaliger, M, Possenti, A, Pritchard, T, Ravi, V, Rest, A, Rowlinson, A, Sawangwit, U, Stappers, B, Sullivan, M, Tiburzi, C, van Straten, W, Albert, A, Andre, M, Anghinolfi, M, Anton, G, Ardid, M, Aubert, Jj, Avgitas, T, Baret, B, Barrios-Marti, J, Basa, S, Bertin, V, Biagi, S, Borrnuth, R, Bourret, S, Bouwhuis, Mc, Bruijn, R, Brunner, J, Busto, J, Capone, A, Caramete, L, Carr, J, Celli, S, Chiarusi, T, Circella, M, Coelho, Jab, Coleiro, A, Coniglione, R, Costantini, H, Coyle, P, Creusot, A, Deschamps, A, De Bonis, G, Distefano, C, Di Palma, I, Donzaud, C, Dornic, D, Drouhin, D, Eberl, T, El Bojaddaini, I, Elsasser, D, Enzenhofer, A, Felis, I, Fusco, La, Galata, S, Gay, P, Geisselsoder, S, Geyer, K, Giordano, V, Gleixner, A, Glotin, H, Gregoire, T, Gracia-Ruiz, R, Graf, K, Hallmann, S, van Haren, H, Heijboer, Aj, Hello, Y, Hernandez-Rey, Jj, Hossl, J, Hofestadt, J, Hugon, C, Illuminati, G, James, Cwcw, de Jong, M, Jongen, M, Kadler, M, Kalekin, O, Katz, U, Kiessling, D, Kouchner, A, Kreter, M, Kreykenbohm, I, Kulikovskiy, V, Lachaud, C, Lahmann, R, Lefevre, D, Leonora, E, Lotze, M, Loucatos, S, Marcelin, M, Margiotta, A, Marinelli, A, Martinez-Mora, Ja, Mathieu, A, Mele, R, Melis, K, Michael, T, Migliozzi, P, Moussa, A, Mueller, C, Nezri, E, Pavalas, Ge, Pellegrino, C, Perrina, C, Piattelli, P, Popa, V, Pradier, T, Quinn, L, Racca, C, Riccobene, G, Roensch, K, Sanchez-Losa, A, Saldana, M, Salvadori, I, Samtleben, Dfe, Sanguineti, M, Sapienza, P, Schnabel, J, Seitz, T, Sieger, C, Spurio, M, Stolarczyk, T, Taiuti, M, Tayalati, Y, Trovato, A, Tselengidou, M, Turpin, D, Tonnis, C, Vallage, B, Vallee, C, Van Elewyck, V, Vivolo, D, Vizzoca, A, Wagner, S, Wilms, J, Zornoza, Jd, Zuniga, J, Abdalla, H, Abramowski, A, Aharonian, F, Benkhali, Fa, Akhperjanian, Ag, Andersson, T, Anguner, Eo, Arrieta, M, Aubert, P, Backes, M, Balzer, A, Barnard, M, Becherini, Y, Tjus, Jb, Berge, D, Bernhard, S, Bernlohr, K, Blackwell, R, Bottcher, M, Boisson, C, Bolmont, J, Bordas, P, Bregeon, J, Brun, F, Brun, P, Bryan, M, Bulik, T, Capasso, M, Casanova, S, Cerruti, M, Chakraborty, N, Chalme-Calvet, R, Chaves, Rcg, Chen, A, Chevalier, J, Chretien, M, Colafrancesco, S, Cologna, G, Condon, B, Conrad, J, Cui, Y, Davids, Id, Decock, J, Degrange, B, Deil, C, Devin, J, de Wilt, P, Dirson, L, Djannati-Atai, A, Domainko, W, Donath, A, Drury, Lo, Dubus, G, Dutson, K, Dyks, J, Edwards, T, Egberts, K, Eger, P, Ernenwein, Jp, Eschbach, S, Farnier, C, Fegan, S, Fernandes, Mv, Fiasson, A, Fontaine, G, Forster, A, Funk, S, Fussling, M, Gabici, S, Gajdus, M, Gallant, Ya, Garrigoux, T, Giavitto, G, Giebels, B, Glicenstein, Jf, Gottschall, D, Goya, A, Grondin, Mh, Hadasch, D, Hahn, J, Haupt, M, Hawkes, J, Heinzelmann, G, Henri, G, Hermann, G, Hervet, O, Hinton, Ja, Hofmann, W, Hoischen, C, Holler, M, Horns, D, Ivascenko, A, Jacholkowska, A, Jamrozy, M, Janiak, M, Jankowsky, D, Jankowsky, F, Jingo, M, Jogler, T, Jouvin, L, Jung-Richardt, I, Kastendieck, Ma, Katarzynski, K, Kerszberg, D, Khelifi, B, Kieffer, M, King, J, Klepser, S, Klochkov, D, Kluzniak, W, Kolitzus, D, Komin, N, Kosack, K, Krakau, S, Kraus, M, Krayzel, F, Kruger, Pp, Laffon, H, Lamanna, G, Lau, J, Lees, Jp, Lefaucheur, J, Lefranc, V, Lemiere, A, Lemoine-Goumard, M, Lenain, Jp, Leser, E, Lohse, T, Lorentz, M, Liu, R, Lopez-Coto, R, Lypova, I, Marandon, V, Marcowith, A, Mariaud, C, Marx, R, Maurin, G, Maxted, N, Mayer, M, Meintjes, Pj, Meyer, M, Mitchell, Amw, Moderski, R, Mohamed, M, Mohrmann, L, Mora, K, Moulin, E, Murach, T, de Naurois, M, Niederwanger, F, Niemiec, J, Oakes, L, O'Brien, P, Odaka, H, Ottl, S, Ohm, S, Ostrowski, M, Oya, I, Padovani, M, Panter, M, Parsons, Rd, Pekeur, Nw, Pelletier, G, Perennes, C, Petrucci, Po, Peyaud, B, Piel, Q, Pita, S, Poon, H, Prokhorov, D, Prokoph, H, Puhlhofer, G, Punch, M, Quirrenbach, A, Raab, S, Reimer, A, Reimer, O, Renaud, M, de los Reyes, R, Rieger, F, Romoli, C, Rosier-Lees, S, Rowell, G, Rudak, B, Rulten, Cb, Sahakian, V, Salek, D, Sanchez, Da, Santangelo, A, Sasaki, M, Schlickeiser, R, Schulz, A, Schussler, F, Schwanke, U, Schwemmer, S, Settimo, M, Seyffert, A, Shafi, N, Shilon, I, Simoni, R, Sol, H, Spanier, F, Spengler, G, Spies, F, Stawarz, L, Steenkamp, R, Stegmann, C, Stinzing, F, Stycz, K, Sushch, I, Tavernet, Jp, Tavernier, T, Taylor, Am, Terrier, R, Tibaldo, L, Tiziani, D, Tluczykont, M, Trichard, C, Tuffs, R, Uchiyama, Y, van der Walt, Dj, van Eldik, C, van Rensburg, C, van Soelen, B, Vasileiadis, G, Veh, J, Venter, C, Viana, A, Vincent, P, Vink, J, Voisin, F, Volk, Hj, Vuillaume, T, Wadiasingh, Z, Wagner, Sj, Wagner, P, Wagner, Rm, White, R, Wierzcholska, A, Willmann, P, Wornlein, A, Wouters, D, Yang, R, Zabalza, V, Zaborov, D, Zacharias, M, Zanin, R, Zdziarski, Aa, Zech, A, Zefi, F, Ziegler, A, Zywucka, N, PSL Research University (PSL)-PSL Research University (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), Petroff, E., Burke-Spolaor, S., Keane, E. F., Mclaughlin, M. A., Miller, R., Andreoni, I., Bailes, M., Barr, E. D., Bernard, S. R., Bhandari, S., Bhat, N. D. R., Burgay, M., Caleb, M., Champion, D., Chandra, P., Cooke, J., Dhillon, V. S., Farnes, J. S., Hardy, L. K., Jaroenjittichai, P., Johnston, S., Kasliwal, M., Kramer, M., Littlefair, S. P., Macquart, J. P., Mickaliger, M., Possenti, A., Pritchard, T., Ravi, V., Rest, A., Rowlinson, A., Sawangwit, U., Stappers, B., Sullivan, M., Tiburzi, C., van Straten, W., Albert, A., André, M., Anghinolfi, M., Anton, G., Ardid, M., Aubert, J.-J., Avgitas, T., Baret, B., Barrios-Martí, J., Basa, S., Bertin, V., Biagi, S., Bormuth, R., Bourret, S., Bouwhuis, M.C., Bruijn, R., Brunner, J., Busto, J., Capone, A., Caramete, L., Carr, J., Celli, S., Chiarusi, T., Circella, M., Coelho, J.A.B., Coleiro, A., Coniglione, R., Costantini, H., Coyle, P., Creusot, A., Deschamps, A., De Bonis, G., Distefano, C., Palma, I. Di, Donzaud, C., Dornic, D., Drouhin, D., Eberl, T., El Bojaddaini, I., Elsässer, D., Enzenhöfer, A., Felis, I., Fusco, L.A., Galatà, S., Gay, P., Geißelsöder, S., Geyer, K., Giordano, V., Gleixner, A., Glotin, H., Grégoire, T., Gracia-Ruiz, R., Graf, K., Hallmann, S., van Haren, H., Heijboer, A.J., Hello, Y., Hernández-Rey, J.J., Hößl, J., Hofestädt, J., Hugon, C., Illuminati, G., James, C.W, de Jong, M., Jongen, M., Kadler, M., Kalekin, O., Katz, U., Kießling, D., Kouchner, A., Kreter, M., Kreykenbohm, I., Kulikovskiy, V., Lachaud, C., Lahmann, R., Lefèvre, D., Leonora, E., Lotze, M., Loucatos, S., Marcelin, M., Margiotta, A., Marinelli, A., Martínez-Mora, J.A., Mathieu, A., Mele, R., Melis, K., Michael, T., Migliozzi, P., Moussa, A., Mueller, C., Nezri, E., Păvălaş, G.E., Pellegrino, C., Perrina, C., Piattelli, P., Popa, V., Pradier, T., Quinn, L., Racca, C., Riccobene, G., Roensch, K., Sánchez-Losa, A., Saldaña, M., Salvadori, I., Samtleben, D. F. E., Sanguineti, M., Sapienza, P., Schnabel, J., Seitz, T., Sieger, C., Spurio, M., Stolarczyk, Th., Taiuti, M., Tayalati, Y., Trovato, A., Tselengidou, M., Turpin, D., Tönnis, C., Vallage, B., Vallée, C., Van Elewyck, V., Vivolo, D., Vizzoca, A., Wagner, S., Wilms, J., Zornoza, J.D., Zúñiga, J., Abdalla, H., Abramowski, A., Aharonian, F., Benkhali, F. Ait, Akhperjanian, A.G., Andersson, T., Angüner, E.O., Arrieta, M., Aubert, P., Backes, M., Balzer, A., Barnard, M., Becherini, Y., Becker Tjus, J., Berge, D., Bernhard, S., Bernlöhr, K., Blackwell, R., Böttcher, M., Boisson, C., Bolmont, J., Bordas, P., Bregeon, J., Brun, F., Brun, P., Bryan, M., Bulik, T., Capasso, M., Casanova, S., Cerruti, M., Chakraborty, N., Chalme-Calvet, R., Chaves, R.C.G., Chen, A., Chevalier, J., Chrétien, M., Colafrancesco, S., Cologna, G., Condon, B., Conrad, J., Cui, Y., Davids, I.D., Decock, J., Degrange, B., Deil, C., Devin, J., Dewilt, P., Dirson, L., Djannati-Ataï, A., Domainko, W., Donath, A., Drury, L.O’C., Dubus, G., Dutson, K., Dyks, J., Edwards, T., Egberts, K., Eger, P., Ernenwein, J.-P., Eschbach, S., Farnier, C., Fegan, S., Fernandes, M.V., Fiasson, A., Fontaine, G., Förster, A., Funk, S., Füßling, M., Gabici, S., Gajdus, M., Gallant, Y.A., Garrigoux, T., Giavitto, G., Giebels, B., Glicenstein, J.F., Gottschall, D., Goyal, A., Grondin, M.-H., Hadasch, D., Hahn, J., Haupt, M., Hawkes, J., Heinzelmann, G., Henri, G., Hermann, G., Hervet, O., Hinton, J.A., Hofmann, W., Hoischen, C., Holler, M., Horns, D., Ivascenko, A., Jacholkowska, A., Jamrozy, M., Janiak, M., Jankowsky, D., Jankowsky, F., Jingo, M., Jogler, T., Jouvin, L., Jung-Richardt, I., Kastendieck, M.A., Katarzyński, K., Kerszberg, D., Khélifi, B., Kieffer, M., King, J., Klepser, S., Klochkov, D., Kluźniak, W., Kolitzus, D., Komin, Nu., Kosack, K., Krakau, S., Kraus, M., Krayzel, F., Krüger, P.P., Laffon, H., Lamanna, G., Lau, J., Lees, J.-P., Lefaucheur, J., Lefranc, V., Lemière, A., Lemoine-Goumard, M., Lenain, J.-P., Leser, E., Lohse, T., Lorentz, M., Liu, R., López-Coto, R., Lypova, I., Marandon, V., Marcowith, A., Mariaud, C., Marx, R., Maurin, G., Maxted, N., Mayer, M., Meintjes, P.J., Meyer, M., Mitchell, A.M.W., Moderski, R., Mohamed, M., Mohrmann, L., Morå, K., Moulin, E., Murach, T., de Naurois, M., Niederwanger, F., Niemiec, J., Oakes, L., O’Brien, P., Odaka, H., Öttl, S., Ohm, S., Ostrowski, M., Oya, I., Padovani, M., Panter, M., Parsons, R.D., Pekeur, N.W., Pelletier, G., Perennes, C., Petrucci, P.-O., Peyaud, B., Piel, Q., Pita, S., Poon, H., Prokhorov, D., Prokoph, H., Pühlhofer, G., Punch, M., Quirrenbach, A., Raab, S., Reimer, A., Reimer, O., Renaud, M., Reyes, R. de lo, Rieger, F., Romoli, C., Rosier-Lees, S., Rowell, G., Rudak, B., Rulten, C.B., Sahakian, V., Salek, D., Sanchez, D.A., Santangelo, A., Sasaki, M., Schlickeiser, R., Schulz, A., Schüssler, F., Schwanke, U., Schwemmer, S., Settimo, M., Seyffert, A.S., Shafi, N., Shilon, I., Simoni, R., Sol, H., Spanier, F., Spengler, G., Spies, F., Stawarz, Ł., Steenkamp, R., Stegmann, C., Stinzing, F., Stycz, K., Sushch, I., Tavernet, J.-P., Tavernier, T., Taylor, A.M., Terrier, R., Tibaldo, L., Tiziani, D., Tluczykont, M., Trichard, C., Tuffs, R., Uchiyama, Y., Walt, D.J. van der, van Eldik, C., van Rensburg, C., van Soelen, B., Vasileiadis, G., Veh, J., Venter, C., Viana, A., Vincent, P., Vink, J., Voisin, F., Völk, H.J., Vuillaume, T., Wadiasingh, Z., Wagner, S.J., Wagner, P., Wagner, R.M., White, R., Wierzcholska, A., Willmann, P., Wörnlein, A., Wouters, D., Yang, R., Zabalza, V., Zaborov, D., Zacharias, M., Zanin, R., Zdziarski, A.A., Zech, A., Zefi, F., Ziegler, A., Żywucka, N., High Energy Astrophys. & Astropart. Phys (API, FNWI), KM3NeT (IHEF, IoP, FNWI), Faculty of Science, Gravitation and Astroparticle Physics Amsterdam, ATLAS (IHEF, IoP, FNWI), GRAPPA (ITFA, IoP, FNWI), 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, Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Andre, M., Aubert, J. -J., Barrios-Marti, J., Bouwhuis, M. C., Coelho, J. A. B., Di Palma, I., Elsasser, D., Enzenhofer, A., Fusco, L. A., Galata, S., Geisselsoder, S., Gregoire, T., Heijboer, A. J., Hernandez-Rey, J. J., Hobl, J., Hofestadt, J., James, C. W., Kiebling, D., Lefevre, D., Martinez-Mora, J. A., Pavalas, G. E., Sanchez-Losa, A., Saldana, M., Stolarczyk, T., Tonnis, C., Vallee, C., Zornoza, J. D., Zuniga, J., Ait Benkhali, F., Akhperjanian, A. G., Anguner, E. O., Bernlohr, K., Bottcher, M., Chaves, R. C. G., Chretien, M., Davids, I. D., Djannati-Atai, A., Drury, L. O'C., Ernenwein, J. -P., Fernandes, M. V., Forster, A., Fubling, M., Gallant, Y. A., Glicenstein, J. F., Grondin, M. -H., Hinton, J. A., Kastendieck, M. A., Katarzynski, K., Khelifi, B., Kluzniak, W., Komin, N., Kruger, P. P., Lees, J. -P., Lemiere, A., Lenain, J. -P., Lopez-Coto, R., Meintjes, P. J., Mitchell, A. M. W., Mora, K., O'Brien, P., Ottl, S., Parsons, R. D., Pekeur, N. W., Petrucci, P. -O., Puhlhofer, G., de los Reyes, R., Rulten, C. B., Sanchez, D. A., Schussler, F., Seyffert, A. S., Stawarz, L., Tavernet, J. -P., Taylor, A. M., van der Walt, D. J., Volk, H. J., Wagner, S. J., Wagner, R. M., Wornlein, A., Zdziarski, A. A., Zywucka, N., Centre Tecnològic de Vilanova i la Geltrú, and Universitat Politècnica de Catalunya. LAB - Laboratori d'Aplicacions Bioacústiques
Subjects: Astrofísica, Astronomy, Astrophysics, Surveys, ISM: structure, Methods: data analysis, Polarization, Astronomy and Astrophysics, Space and Planetary Science, 01 natural sciences, Radio telescopes, data analysis [Methods], 010303 astronomy & astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Line-of-sight, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Linear polarization, Fast radio burst, Galactic Center, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, Astrophysics - High Energy Astrophysical Phenomena, polarization–methods, dataanalysis–surveys–ISM, structure, Milky Way, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Radio telescope, 0103 physical sciences, Neutrins, Neutrinos, Astrophysics::Galaxy Astrophysics, Astroparticle physics, Telescopis, 010308 nuclear & particles physics, Galactic plane, Física::Astronomia i astrofísica [Àrees temàtiques de la UPC], FISICA APLICADA, ddc:520, polarization – methods: data analysis – surveys – ISM: structure, structure [ISM], Methods: data analysi
Abstract: Monthly notices of the Royal Astronomical Society 469(4), 4465 – 4482 (2017). doi:10.1093/mnras/stx1098, We report on the discovery of a new fast radio burst (FRB), FRB 150215, with the Parkes radio telescope on 2015 February 15. The burst was detected in real time with a dispersion measure (DM) of 1105.6 ± 0.8 pc cm$^{−3}$, a pulse duration of 2.8 $^{+1.2}_{-0.5}$ ms, and a measured peak flux density assuming that the burst was at beam centre of 0.7$^{+0.2}_{-0.1}$ Jy. The FRB originated at a Galactic longitude and latitude of 24.66°, 5.28° and 25° away from the Galactic Center. The burst was found to be 43 ± 5 per cent linearly polarized with a rotation measure (RM) in the range −9, Published by Oxford Univ. Press, Oxford
Published: 2017

22. Dispersion measure variations in a sample of 168 pulsars

Author: Simon Johnston, W. van Straten, Ryan Shannon, E. Petroff, and Michael Keith
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Scattering, Gamma ray, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, Astrophysics, Galactic plane, Astrophysics - Astrophysics of Galaxies, Pulsar wind nebula, Supernova, Pulsar, Space and Planetary Science, Millisecond pulsar, Astrophysics of Galaxies (astro-ph.GA), Astrophysics - High Energy Astrophysical Phenomena, Fermi Gamma-ray Space Telescope
Abstract: We analyse dispersion measure (DM) variations in six years of radio observations of more than 160 young pulsars, all gamma ray candidates for the Fermi gamma ray telescope mostly located close to the Galactic plane. DMs were fit across 256 MHz of bandwidth for observations centred at 1.4 GHz and across three frequencies -- 0.7 GHz, 1.4 GHz, and 3.1 GHz -- where multifrequency observations were available. Changes in dispersion measure, dDM/dt, were calculated using a weighted linear fit across all epochs of available DMs. DM variations were detected at a 3\sigma level in 11 pulsars, four of which were above 5\sigma: PSRs J0835-4510, J0908-4913, J1824-1945, and J1833-0827. We find that after 28 years of gradual decline, the DM of PSR J0835-4510 is now increasing. The magnitude of variations in three of the four (PSRs J0835-4510, J0908-4913, and J1833-0827) are above what models would predict for an ISM dominated by Kolmogorov turbulence. We attribute this excess as likely due to the pulsar's local environment - the supernova remnants near PSRs J0835-4510 and J1833-0827 and the pulsar wind nebula around PSR J0908-4913. Upper limits were determined for all pulsars without detectable values of dDM/dt, most limits were found to lie above the levels of variations predicted by ISM theory. We find our results to be consistent with scattering estimates from the NE2001 model along these lines of sight., Comment: 9 pages, 6 figures, 2 tables, Accepted for publication in MNRAS
Published: 2013

23. Diagnostic des ruptures du subscapulaire : nos tests diagnostiques sont-ils pertinents pour le diagnostic positif ?

Author: C E Thelu, Arnaud Godenèche, E Petroff, Nicolas Graveleau, Bruno Toussaint, N. Solignac, Laurent Nové-Josserand, la Société française d’arthroscopie, S. Audebert, T. Joudet, Yves Lefebvre, J Barth, Michel Pitermann, C Scymanski, and Christophe Charousset
Subjects: Orthopedics and Sports Medicine, Surgery
Abstract: Resume Hypothese Les ruptures du subscapulaire peuvent etre evoquees cliniquement devant une rotation externe passive augmentee en comparatif par rapport au cote oppose, des manœuvres de rotation interne contrariee (Lift-Off test [LOT], Belly-Press test [BPT], Napoleon test et Bear-Hug test [BHT]) et des signes de rappel automatique positifs (Internal Rotation Lag Sign et Belly-Off Sign). Le biceps est frequemment associe aux lesions du subscapulaire car ce dernier participe a la formation de la poulie mediale. Le Palm-Up test [PUT] est utilise pour le biceps comme le test de Jobe pour le supraepineux. Patients et methode Dans le cadre d’une etude multicentrique, nous avons souhaite evaluer la valeur diagnostique positive des tests cliniques LOT, BPT, BHT, PUT et de Jobe, pour les lesions du subscapulaire et leur importance anatomique. Les relations entre les differents parametres etudies ont ete comparees statistiquement en utilisant une analyse de la variance. Cette etude prospective multicentrique de janvier 2009 a fevrier 2010 comprenait 208 cas de lesions du subscapulaire isolees ou associees a une atteinte partielle (Ellman 1, 2, 3) ou transfixiante (stade 1 de la SFA) du supraepineux. Resultats La severite de l’atteinte du subscapulaire a ete quantifiee selon la classification de la SFA (en quatre stades) et selon la hauteur de l’atteinte (tiers proximal et tiers superieur). Les trois tests LOT, BPT et BHT etaient correles a severite des lesions observees (p Conclusion Malgre la realisation des trois tests (LOT, BPT, BHT), 24 % des lesions du subscapulaire n’etaient diagnostiquees qu’en peroperatoire. L’apport des signes de rappel automatique dans l’amelioration du diagnostic lesionnel n’a pas ete etudie dans ce travail. Niveau de preuve II.
Published: 2012

24. Nouvelle classification endoscopique des lésions du sub-scapulaire

Author: Nicolas Graveleau, Arnaud Godenèche, Carlos Maynou, C E Thelu, N. Solignac, P. Hardy, Pascal Boileau, Laurent Nové-Josserand, la Société française d’arthroscopie, C Scymanski, Yves Lefebvre, J Barth, Christophe Charousset, Bruno Toussaint, S. Audebert, E Petroff, and T. Joudet
Subjects: Orthopedics and Sports Medicine, Surgery
Abstract: Resume L’absence d’un systeme coherent de classification des lesions du sub-scapularis a rendu difficile la communication en matiere de traitement et de pronostic pour les differents types de rupture du sub-scapularis. En outre, une classification fiable fournit un moyen de comparaison des donnees epidemiologique et therapeutiques. Les classifications jusqu’alors proposees n’integraient pas les constatations radiologiques et peroperatoires de la coulisse du biceps et le degre de clivage du tendon du sub-scapulaire. Cette etude propose une nouvelle classification basee sur les constatations arthroscopiques a visee therapeutique et pronostic. Methode Il s’agit d’une etude prospective multicentrique promue par la Societe francaise d’arthroscopie de mars 2010 a janvier 2011. Cent cinquante cas de lesions isolees du sub-scapularis et d’atteinte anterosuperieure limitee ont ete etudies. La coulisse du biceps et l’insertion du feuillet profond du sub-scapularis ont ete explorees systematiquement par arthroscopie avec enregistrement video. Chaque lesion a ete classee par une analyse realisee par quatre chirurgiens et par convergence entre eux des conclusions lesionnelles. Resultats Quatre types lesionnels ont ete definis et sont bases sur les lesions constatees au niveau de la coulisse bicipitale. Le type I comprenait les lesions partielles de desinsertion des fibres du sub-scapularis de la petite tuberosite, sans lesion de la coulisse bicipitale. Le type II correspondait aux lesions partielles des fibres du sub-scapularis sur la petite tuberosite associees a une lesion partielle du mur anterieur de la coulisse bicipitale, mais avec conservation du ligament gleno-humeral superieur. Le type III correspondait a une desinsertion complete des fibres du sub-scapulaire de la petite tuberosite associee a une large fente de la coulisse bicipitale. Le stade IV correspondait a la desinsertion complete des fibres du sub-scapulaire, pouvant s’associer au « comma sign » par la reunion de fibres du sub-scapulaire et du supraepineux. Toutes les lesions constatees en peroperatoire pouvaient etre classees dans un de ces types a quelques exceptions pres. Discussion Une classification reproductible permet une description homogene des lesions entre les chirurgiens et a alors un interet therapeutique et/ou pronostique. Cette nouvelle classification permet de definir quatre types lesionnels facilement identifiables en cas de lesions du sub-scapularis isolee ou associee a une lesion antero-superieure de la coiffe des rotateurs. Cette classification peut etre completee en integrant des elements concernant la longue portion du biceps et l’infiltration graisseuse du muscle. Une etude de reproductibilite intra- et interobservateur reste necessaire pour completer la validation de son interet diagnostique ou pronostique. Niveau de preuve Niveau 2.
Published: 2012

25. Réparation arthroscopique du sous-scapulaire : résultats préliminaires d’une étude prospective multicentrique

Author: Bruno Toussaint, E Petroff, Arnaud Godenèche, M Pitermann, S. Audebert, T. Joudet, P. Hardy, Nicolas Graveleau, Société française d’arthroscopie, C Scymanski, Christophe Charousset, Yves Lefebvre, J Barth, Carlos Maynou, C E Thelu, Laurent Nové-Josserand, Pascal Boileau, and N. Solignac
Subjects: Orthopedics and Sports Medicine, Surgery
Abstract: Resume Introduction Jusqu’a l’utilisation de l’arthroscopie dans la chirurgie de la coiffe des rotateurs, la frequence des lesions du subscapulaire est restee longtemps sous-estimee. Par ailleurs, leur traitement meme sous controle arthroscopique reste difficile. L’absence de classification reellement specifique des lesions du subscapulaire a rendu difficile la communication en matiere de traitement et de pronostic pour les differents types de rupture du sous-scapulaire. Le but de cette etude prospective multicentrique etait de valider la pertinence du traitement arthroscopique des lesions du subscapulaire en analysant les resultats a court terme, en fonction de l’importance initiale des lesions anatomiques. Methode Il s’agit d’une etude prospective multicentrique menee sous l’egide de la Societe francaise d’arthroscopie de mars 2010 a janvier 2011. Deux cent-huit cas de lesions isolees du subscapulaire ou associees a une d’atteinte antero-superieure limitee. Une evaluation des resultats cliniques (Score de Constant et University of California Los Angeles rating scale [UCLA]), anatomiques et du pronostic tenant compte de l’examen clinique, de l’imagerie pre- et postoperatoire et des lesions anatomiques mises en evidence a ete possible pour les donnees cliniques, sur un groupe de 103 patients ayant un recul d’un an et pour les donnees radiologiques, sur un groupe de 129 patients ayant au moins six mois de recul. Resultats Les resultats cliniques preliminaires portent sur 103 patients revus au recul minimal d’un an. Il existait une amelioration globale, statistiquement significative des scores de Constant et UCLA, avec dans ces cas une disparition des signes cliniques. Cette amelioration semblait augmenter avec le recul. Apres, classification en quatre groupes lesionnels des patients, en fonction des lesions anatomiques observees, il existait egalement une difference significative des resultats cliniques entre les differents types lesionnels. Les resultats anatomiques, apprecies par une imagerie postoperatoire chez tous les patients ayant au moins six mois de recul (n = 129) comportaient 92 % de cicatrisation tendineuse, mais associee dans 18,6 % a une amyotrophie de la partie superieur du subscapulaire et une majoration de l’infiltration graisseuse du corps musculaire. Discussion Notre etude confirme les bons resultats cliniques et radiologiques deja publies dans la litterature. L’utilisation d’une classification des lesions en quatre groupes a montre qu’elle etait utilisable des le bilan d’imagerie. Cette classification permettait surtout de differencier les resultats entre les types II et III. La tendance a l’amelioration des resultats avec le recul doit etre confirmee par une evaluation a plus long terme, de meme que l’absence de caractere pejoratif de l’aggravation de l’amyotrophie superieure du subscapulaire et de l’infiltration graisseuse. Niveau de preuve 3.
Published: 2012

26. Limits on the TeV gamma-ray afterglow of fast radio bursts with H.E.S.S

Author: Francois Brun, E. Petroff, F. Schüssler, G. Pühlhofer, Gavin Rowell, Evan Keane, Robert Wagner, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), H.E.S.S., SUPERB, and Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Electromagnetic spectrum, Astrophysics::High Energy Astrophysical Phenomena, absorption: effect, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, spectrum, energy dependence, Pulsar, X-shaped radio galaxy, Observatory, HESS, 0103 physical sciences, 010303 astronomy & astrophysics, pulsar, Physics, radio wave, 010308 nuclear & particles physics, background, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Galaxy, Afterglow, observatory, electromagnetic, Extragalactic background light, gamma ray, galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], burst, Radio wave
Abstract: International audience; We here present the H.E.S.S. follow-up of Fast Radio Bursts (FRBs), millisecond-long, very strong radio pulses of yet unknown origin. The SUPERB (SUrvey for Pulsars and Extragalactic Radio Bursts) project at the Parkes radio observatory is able to detect these enigmatic events almost in real-time which allows triggering follow-up observations covering the full electromagnetic spectrum. The H.E.S.S. gamma-ray observatory is taking active part in this endeavor. Here we focus on data taken within hours of FRB 150418, which allow us to derive the first limits on gamma-ray afterglow emission of FRBs. Based on the identification of the potential host galaxy of this burst we are able to discuss absorption effects due to the extragalactic background light (EBL) and derive intrinsic, energy dependent limits on the gamma-ray afterglow.
Published: 2016

27. Five new Fast Radio Bursts from the HTRU high latitude survey at Parkes: first evidence for two-component bursts

Author: Caterina Tiburzi, N. D. R. Bhat, Andrew Jameson, Matthew Bailes, E. Petroff, David J. Thornton, W. van Straten, Chris Flynn, Sarah Burke-Spolaor, Ben Stappers, Samuel Bates, Andrew Lyne, Michael Kramer, Lina Levin, E. D. Barr, Michael Keith, Simon Johnston, D. J. Champion, Cherry Ng, M. Burgay, and A. Possenti
Subjects: media_common.quotation_subject, Population, Multiple component, FOS: Physical sciences, Astrophysics, 01 natural sciences, surveys, pulsars: general, High latitude, 0103 physical sciences, education, 010303 astronomy & astrophysics, media_common, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, education.field_of_study, 010308 nuclear & particles physics, Fast radio burst, Single component, Canadian Hydrogen Intensity Mapping Experiment, scattering, Astronomy, Astronomy and Astrophysics, Time resolution, Space and Planetary Science, Sky, intergalactic medium, Astrophysics - High Energy Astrophysical Phenomena
Abstract: The detection of five new fast radio bursts (FRBs) found in the High Time Resolution Universe high latitude survey is presented. The rate implied is 6$^{+4}_{-3}\times~10^3$ (95%) FRBs sky$^{-1}$ day$^{-1}$ above a fluence of between 0.13 and 5.9 Jy ms for FRBs between 0.128 and 262 ms in duration. One of these FRBs has a clear two-component profile, each component is similar to the known population of single component FRBs and are separated by 2.4(4) ms. All the FRB components appear to be unresolved following deconvolution with a scattering tail and accounting for intra-channel smearing. The two-component FRB also has the highest dispersion measure (1629 pc cm$^{-3}$) of any FRB to-date. Many of the proposed models to explain FRBs use a single high energy event involving compact objects (such as neutron star mergers) and therefore cannot easily explain a two-component FRB. Models that are based on extreme versions of flaring, pulsing or orbital events however could produce multiple component profiles. The compatibility of these models and the FRB rate implied by these detections is discussed., Comment: 5 pages, 1 figure, 1 table, submitted to MNRAS
Published: 2016

28. Polarization Gradient Study of Interstellar Medium Turbulence Using The Canadian Galactic Plane Survey

Author: E. Petroff, C. A. Herron, Bryan Gaensler, Naomi McClure-Griffiths, Roland Kothes, Joern Geisbuesch, Geraint F. Lewis, and T. L. Landecker
Subjects: Physics, 010504 meteorology & atmospheric sciences, Turbulence, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galactic plane, Polarization (waves), Astrophysics - Astrophysics of Galaxies, 01 natural sciences, Galaxy, Interstellar medium, symbols.namesake, Mach number, Space and Planetary Science, Skewness, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, symbols, Kurtosis, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences
Abstract: We have investigated the magneto-ionic turbulence in the interstellar medium through spatial gradients of the complex radio polarization vector in the Canadian Galactic Plane Survey (CGPS). The CGPS data cover 1300 square-degrees, over the range ${53^{\circ}}\leq{\ell}\leq{192^{\circ}}$, ${-3^{\circ}}\leq{b}\leq{5^{\circ}}$ with an extension to ${b}={17.5^{\circ}}$ in the range ${101^{\circ}}\leq{\ell}\leq{116^{\circ}}$, and arcminute resolution at 1420 MHz. Previous studies found a correlation between the skewness and kurtosis of the polarization gradient and the Mach number of the turbulence, or assumed this correlation to deduce the Mach number of an observed turbulent region. We present polarization gradient images of the entire CGPS dataset, and analyze the dependence of these images on angular resolution. The polarization gradients are filamentary, and the length of these filaments is largest towards the Galactic anti-center, and smallest towards the inner Galaxy. This may imply that small-scale turbulence is stronger in the inner Galaxy, or that we observe more distant features at low Galactic longitudes. For every resolution studied, the skewness of the polarization gradient is influenced by the edges of bright polarization gradient regions, which are not related to the turbulence revealed by the polarization gradients. We also find that the skewness of the polarization gradient is sensitive to the size of the box used to calculate the skewness, but insensitive to Galactic longitude, implying that the skewness only probes the number and magnitude of the inhomogeneities within the box. We conclude that the skewness and kurtosis of the polarization gradient are not ideal statistics for probing natural magneto-ionic turbulence., Comment: 21 pages, 15 figures, accepted by ApJ
Published: 2016
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29. Radio light curve of the galaxy possibly associated with FRB150418

Author: Michael Kramer, Ewan Barr, Shivani Bhandari, C. G. Bassa, Evan Keane, Jean-Pierre Macquart, Hajime Sugai, Robert Beswick, E. Petroff, Steven Tingay, A. Possenti, Mareki Honma, Benjamin Stappers, Poonam Chandra, Simon Johnston, and M. Burgay
Subjects: Active galactic nucleus, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, Flux, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, law.invention, Jansky, Telescope, X-shaped radio galaxy, law, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, Light curve, Astrophysics - Astrophysics of Galaxies, Galaxy, Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA), Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present observations made with the Australia Telescope Compact Array (ATCA), the Jansky Very Large Array (JVLA) and the Giant Metre-Wave Telescope of the radio source within the galaxy WISE~J071634.59-190039.2, claimed to be host of FRB~150418 by Keane et al. (2016). We have established a common flux density scale between the ATCA and JVLA observations, the main result of which is to increase the flux densities obtained by Keane et al. At a frequency of 5.5 GHz, the source has a mean flux density of 140uJy and is variable on short timescales with a modulation index of 0.36. Statistical analysis of the flux densities shows that the variations seen are consistent with refractive interstellar scintillation of the weak active galactic nucleus at the centre of the galaxy. It may therefore be the case that the FRB and the galaxy are not associated. However, taking into account the rarity of highly variable sources in the radio sky, and our lack of knowledge of the progenitors of FRBs as a class, the association between WISE~J071634.59-190039.2 and FRB~150418 remains a possibility., Comment: Accepted by MNRAS, 9 pages, 4 figures
Published: 2016
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30. A survey of FRB fields: limits on repeatability

Author: M. Caleb, E. Petroff, Michael Kramer, Cherry Ng, W. van Straten, A. Jameson, C.M.L. Flynn, Andrea Possenti, B. R. Barsdell, Ewan Barr, Ben Stappers, Simon Johnston, Matthew Bailes, Sarah Burke-Spolaor, D. J. Champion, and Evan Keane
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Millisecond, Canadian Hydrogen Intensity Mapping Experiment, media_common.quotation_subject, Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, Time resolution, Astrophysics, Repeatability, Magnetar, Methods observational, Universe, Pulsar, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena, media_common
Abstract: Several theories exist to explain the source of the bright, millisecond duration pulses known as fast radio bursts (FRBs). If the progenitors of FRBs are non-cataclysmic, such as giant pulses from pulsars, pulsar-planet binaries, or magnetar flares, FRB emission may be seen to repeat. We have undertaken a survey of the fields of eight known FRBs from the High Time Resolution Universe survey to search for repeating pulses. Although no repeat pulses were detected the survey yielded the detection of a new FRB, described in Petroff et al. (2015a). From our observations we rule out periodic repeating sources with periods P $\leq$ 8.6 hours and rule out sources with periods 8.6 < P < 21 hours at the 90% confidence level. At P $\geq$ 21 hours our limits fall off as ~1/P. Dedicated and persistent observations of FRB source fields are needed to rule out repetition on longer timescales, a task well-suited to next generation wide-field transient detectors., 6 pages, 1 figure; accepted for publication in MNRAS
Published: 2015

31. The High Time Resolution Universe Pulsar Survey X: Discovery of four millisecond pulsars and updated timing solutions of a further 12

Author: Caterina Tiburzi, N. D. R. Bhat, L. Guillemot, E. Petroff, C. G. Bassa, Cherry Ng, David J. Thornton, Ryan Shannon, Simon Johnston, P. Coster, W. van Straten, Paulo C. C. Freire, Matthew Bailes, Samuel Bates, Thomas M. Tauris, D. J. Champion, Marta Burgay, Sarah Burke-Spolaor, Michael Kramer, Andrew Lyne, Benjamin Stappers, Michael Keith, Norbert Wex, Lina Levin, Andrea Possenti, Max-Planck-Institut für Radioastronomie ( MPIFR ), Centre for Astrophysics and Supercomputing, Swinburne University of Technology [Melbourne], West Virginia University [Morgantown], International Centre for Radio Astronomy Research ( ICRAR ), Government of Western Australia-The University of Western Australia ( UWA ) -Curtin University [Perth], Planning and Transport Research Centre ( PATREC ) -Planning and Transport Research Centre ( PATREC ), INAF-ORA-Osservatorio Astronomico di Cagliari, Jet Propulsion Laboratory ( JPL ), NASA-California Institute of Technology ( CALTECH ), Australia Telescope National Facility, CSIRO ( CSIRO ), Commonwealth Scientific and Industrial Research Organisation [Canberra] ( CSIRO ), Jodrell Bank Centre for Astrophysics, University of Manchester [Manchester], Max-Planck-Institut für Radioastronomie, INAF-Osservatorio di Cagliari, Netherlands Institute for Radio Astronomy ( ASTRON ), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace ( LPC2E ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Université d'Orléans ( UO ) -Centre National de la Recherche Scientifique ( CNRS ), Unité Scientifique de la Station de Nançay ( USN ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université d'Orléans ( UO ) -Centre National de la Recherche Scientifique ( CNRS ), Max-Planck-Institut für Radioastronomie (MPIFR), International Centre for Radio Astronomy Research (ICRAR), Government of Western Australia-The University of Western Australia (UWA)-Curtin University [Perth], Planning and Transport Research Centre (PATREC)-Planning and Transport Research Centre (PATREC), INAF - Osservatorio Astronomico di Cagliari (OAC), Istituto Nazionale di Astrofisica (INAF), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Australia Telescope National Facility (ATNF), Commonwealth Scientific and Industrial Research Organisation [Canberra] (CSIRO), Jodrell Bank Centre for Astrophysics (JBCA), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Unité Scientifique de la Station de Nançay (USN), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), and Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)
Subjects: Proper motion, Astrophysics::High Energy Astrophysical Phenomena, Population, Pulsar planet, FOS: Physical sciences, Astrophysics, 01 natural sciences, Binary pulsar, PSR J1811−2405, Pulsar, Millisecond pulsar, 0103 physical sciences, stars: neutron -pulsars: general -pulsars: individual: PSR J1017−7156 -pulsars, 010306 general physics, education, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Physics, High Energy Astrophysical Phenomena (astro-ph.HE), education.field_of_study, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astronomy, White dwarf, Astronomy and Astrophysics, individual: PSR J1543−5149 -pulsars: individual: PSR J1801−3210 -pulsars: individual, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena, [ SDU.ASTR.SR ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], X-ray pulsar
Abstract: We report on the discovery of four millisecond pulsars (MSPs) in the High Time Resolution Universe (HTRU) pulsar survey being conducted at the Parkes 64-m radio telescope. All four MSPs are in binary systems and are likely to have white dwarf companions. In addition, we present updated timing solutions for 12 previously published HTRU MSPs, revealing new observational parameters such as five proper motion measurements and significant temporal dispersion measure variations in PSR J1017-7156. We discuss the case of PSR J1801-3210, which shows no significant period derivative after four years of timing data. Our best-fit solution shows a period derivative of the order of $10^{-23}$, an extremely small number compared to that of a typical MSP. However, it is likely that the pulsar lies beyond the Galactic Centre, and an unremarkable intrinsic period derivative is reduced to close to zero by the Galactic potential acceleration. Furthermore, we highlight the potential to employ PSR J1801-3210 in the strong equivalence principle test due to its wide and circular orbit. In a broader comparison with the known MSP population, we suggest a correlation between higher mass functions and the presence of eclipses in `very low-mass binary pulsars', implying that eclipses are observed in systems with high orbital inclinations. We also suggest that the distribution of the total mass of binary systems is inversely-related to the Galactic height distribution. Finally, we report on the first detection of PSRs J1543-5149 and J1811-2404 as gamma-ray pulsars., Comment: 21 pages, 9 figures, 2 tables, MNRAS accepted
Published: 2014
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32. A 24 HR GLOBAL CAMPAIGN TO ASSESS PRECISION TIMING OF THE MILLISECOND PULSAR J1713+0747

Author: Sourav Chatterjee, Gemma H. Janssen, G. Jones, Fredrick A. Jenet, Christine Jordan, J. W. T. Hessels, I. H. Stairs, Ryan Shannon, T. J. W. Lazio, L. Guillemot, Kang Liu, C. G. Bassa, P. Lazarus, Nipuni Palliyaguru, Michael Kramer, D. R. Madison, E. Petroff, M. A. McLaughlin, J. M. Cordes, Bhaswati Bhattacharyya, Joanna M. Rankin, D. J. Champion, Benjamin Stappers, Kevin Stovall, Michael Keith, Kuan Jin Lee, Joris P. W. Verbiest, Timothy Dolch, Shi Dai, W. W. Zhu, V. I. Kondratiev, A. G. Lyne, Kathryn Crowter, Delphine Perrodin, R. Smits, G. Desvignes, Ramesh Karuppusamy, Benetge Perera, Ismaël Cognard, Paul Demorest, Scott M. Ransom, Jayashree Roy, Michael T. Lam, Oberlin College, Cornell University, Jodrell Bank Centre for Astrophysics, University of Manchester [Manchester], Inter-University Centre for Astronomy and Astrophysics, Max-Planck-Institut für Radioastronomie (MPIFR), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Unité Scientifique de la Station de Nançay (USN), Université d'Orléans (UO)-Observatoire des Sciences de l'Univers en région Centre (OSUC), PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), University of British Colombia, National Radio Astronomy Observatory [Socorro] (NRAO), National Radio Astronomy Observatory (NRAO), Netherlands Institute for Radio Astronomy (ASTRON), University of Amsterdam [Amsterdam] (UvA), Center for Advanced Radio Astronomy (CARA), University of Texas Rio Grande Valley [Brownsville, TX] (UTRGV), ARC Centre of Excellence for Coral Reef Studies (CoralCoE), James Cook University (JCU), CSIRO Astronomy and Space Science, Commonwealth Scientific and Industrial Research Organisation [Canberra] (CSIRO), Vrije Universiteit Medical Centre (VUMC), Vrije Universiteit Amsterdam [Amsterdam] (VU), Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft, Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), School of Medical Sciences - Institute of Medical Sciences, University of Aberdeen, Department of Physics, West Virginia University, West Virginia University, Department of Physics and Astronomy, University of British Columbia, University of British Columbia (UBC), Center for Gravitational Wave Astronomy (CGWA), Department of Physics [Rolla], Missouri University of Science and Technology (Missouri S&T), University of Missouri System-University of Missouri System, INAF - Osservatorio Astronomico di Cagliari (OAC), Istituto Nazionale di Astrofisica (INAF), Laboratory of Infrared Material and Devices, Ningbo University, Centre de Physique des Particules de Marseille (CPPM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), University of Vermont [Burlington], European Project: 337062,EC:FP7:ERC,ERC-2013-StG,DRAGNET(2014), European Project: 227947,EC:FP7:ERC,ERC-2008-AdG,LEAP(2009), Cornell University [New York], Inter-University Centre for Astronomy and Astrophysics [Pune] (IUCAA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Jodrell Bank Centre for Astrophysics (JBCA), Ningbo University (NBU), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO), and High Energy Astrophys. & Astropart. Phys (API, FNWI)
Subjects: media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, ISM: structure, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Radio telescope, Pulsar, Millisecond pulsar, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, media_common, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Scintillation, Gravitational wave, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, LOFAR, gravitational waves, Space and Planetary Science, Sky, [SDU]Sciences of the Universe [physics], pulsars: individual: PSR J1713+0747, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, Noise (radio)
Abstract: The radio millisecond pulsar J1713+0747 is regarded as one of the highest-precision clocks in the sky, and is regularly timed for the purpose of detecting gravitational waves. The International Pulsar Timing Array collaboration undertook a 24-hour global observation of PSR J1713+0747 in an effort to better quantify sources of timing noise in this pulsar, particularly on intermediate (1 - 24 hr) timescales. We observed the pulsar continuously over 24 hr with the Arecibo, Effelsberg, GMRT, Green Bank, LOFAR, Lovell, Nancay, Parkes, and WSRT radio telescopes. The combined pulse times-of-arrival presented here provide an estimate of what sources of timing noise, excluding DM variations, would be present as compared to an idealized root-N improvement in timing precision, where N is the number of pulses analyzed. In the case of this particular pulsar, we find that intrinsic pulse phase jitter dominates arrival time precision when the S/N of single pulses exceeds unity, as measured using the eight telescopes that observed at L-band/1.4 GHz. We present first results of specific phenomena probed on the unusually long timescale (for a single continuous observing session) of tens of hours, in particular interstellar scintillation, and discuss the degree to which scintillation and profile evolution affect precision timing. This paper presents the data set as a basis for future, deeper studies., Published in the Astrophysical Journal
Published: 2014

33. Characterization of thick lead zirconate titanate films fabricated using a new sol gel based process

Author: D. A. Barrow, T. E. Petroff, R. P. Tandon, and Michael Sayer
Subjects: Materials science, General Physics and Astronomy, Dielectric, Coercivity, Lead zirconate titanate, Ferroelectricity, Piezoelectricity, chemistry.chemical_compound, chemistry, visual_art, visual_art.visual_art_medium, Ceramic, Thin film, Composite material, Sol-gel
Abstract: Lead zirconate titanate (PZT) films 60 μm in thickness have been fabricated using a new sol gel based process. PZT powders are dispersed in a sol gel matrix to form a 0–3 ceramic/ceramic composite. The dielectric properties of these films have been studied as a function of powder concentration, frequency, and temperature. The characteristic Curie point is observed at 420 °C. The ferroelectric behavior measured in terms of the remanant polarization (Pr=35 μC/cm2) and coercive field (Ec=20 kV/cm) was an improvement over values quoted for thin PZT films but lower than that of bulk ceramic. The piezoelectric properties d33 (325 pC/N) and d31 (−80 pC/N) were comparable with those of the bulk ceramic.
Published: 1997

34. Thick ceramic coatings using a sol gel based ceramic-ceramic 0–3 composite

Author: T. E. Petroff, D. A. Barrow, and Michael Sayer
Subjects: Materials science, Composite number, Surfaces and Interfaces, General Chemistry, engineering.material, Condensed Matter Physics, Lead zirconate titanate, Surfaces, Coatings and Films, Thermal barrier coating, chemistry.chemical_compound, chemistry, Coating, visual_art, Materials Chemistry, engineering, visual_art.visual_art_medium, Cubic zirconia, Ceramic, Composite material, Yttria-stabilized zirconia, Sol-gel
Abstract: A sol gel based coating technology has been developed for making high quality, thick ceramic coatings. The films are ceramic-ceramic 0–3 composites made by dispersing ceramic powders in a sol gel solution. The resulting system has all the benefits of sol gel, i.e. ease of fabrication, ability to coat complex geometries and relative cost effectiveness, but is not limited in film thickness. Lead zirconate titanate (PZT), yttria- and ceria-stabilized zirconia, titania, silica and alumina films have been fabricated in the 5–200 μm thickness range. The electrical properties of the PZT films are comparable with those of the bulk ceramic, and the zirconia and alumina films exhibit excellent potential as corrosion- and wear-resistant coatings as well as thermal barrier and performance enhancing coatings.
Published: 1995

35. Diagnosis of subscapularis tendon tears: Are available diagnostic tests pertinent for a positive diagnosis?

Author: S. Audebert, Arnaud Godenèche, Johannes Barth, Christophe Charousset, Bruno Toussaint, E Petroff, Laurent Nové-Josserand, Nicolas Graveleau, N. Solignac, T. Joudet, Charles-Edouard Thelu, Michel Pitermann, Christophe Scymanski, Yves Lefebvre, Pouchoulin, Gilles, Institut Paoli-Calmettes, Fédération nationale des Centres de lutte contre le Cancer (FNCLCC), Centre Hospitalier Régional Universitaire de Nancy (CHRU Nancy), Unité épaule, Centre Orthopedique Santy, Centre Orthopedique Santy, Centre de consultation orthopédique et sportive, Clinique du sport de Bordeaux-Mérignac, Laboratoire Parole et Langage (LPL), and Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Adult, Male, Diagnosis value, Clinical tests, medicine.medical_specialty, education, Physical examination, Biceps, Jobe's test, Rotator Cuff Injuries, 03 medical and health sciences, 0302 clinical medicine, Tendon Injuries, medicine, Humans, Orthopedics and Sports Medicine, Prospective Studies, Physical Examination, Aged, 030222 orthopedics, [SDV.MHEP] Life Sciences [q-bio]/Human health and pathology, medicine.diagnostic_test, business.industry, Diagnostic test, 030229 sport sciences, Middle Aged, Subscapularis tendon, Surgery, Multicenter study, Clinical exam, Tears, Female, Subcapularis, business, [SDV.MHEP]Life Sciences [q-bio]/Human health and pathology
Abstract: SummaryHypothesisClinically, subscapularis tendon tears are suggested by the presence of increased passive external rotation compared to the opposite side, resisted internal rotation manoeuvres (Lift-Off test [LOT], Belly-Press test [BPT], Napoleon test and Bear-Hug test [BHT] and positive Internal Rotation Lag Sign and/or Belly-Off Signs). Associated bicipital involvement is frequent with subscapularis tendon tears, because it participates in the formation of the biceps pulley. The Palm-Up test (PUT) is used for the biceps, and the Jobe test for the supraspinatus.Material and methodsIn this multicenter study, we evaluated the positive diagnostic value of the clinical tests, LOT, BPT, BHT, PUT, and the Jobe test for subscapularis tears as well as their anatomical value. The relationships of the different parameters studied were compared statistically by analysis of variance (ANOVA). This prospective multicenter study was performed from January 2009 to February 2010 and included 208 cases of subscapularis tendon tears, isolated or associated with partial (Ellman 1, 2 or 3) or full thickness (SFA stage 1) supraspinatus tears.ResultsThe severity of the subscapularis tear was quantified according to the SFA classification into four stages and according to the level of injury (the lower 1/3 and upper 2/3). The three tests LOT, BPT and BHT were correlated to the severity of observed tears (P
Published: 2012

36. Arthroscopic repair of subscapularis tears: Preliminary data from a prospective multicentre study

Author: Johannes Barth, Christophe Charousset, Pascal Boileau, Carlos Maynou, T. Joudet, Arnaud Godenèche, Philippe Hardy, C E Thelu, E Petroff, N. Solignac, S. Audebert, Christophe Scymanski, Yves Lefebvre, Bruno Toussaint, Nicolas Graveleau, Laurent Nové-Josserand, Michel Pitermann, Centre Hospitalier Régional Universitaire de Nancy (CHRU Nancy), Institut Paoli-Calmettes, Fédération nationale des Centres de lutte contre le Cancer (FNCLCC), Unité épaule, Centre Orthopedique Santy, Centre Orthopedique Santy, Hôpital Ambroise Paré [AP-HP], PremUp Foundation, Institut National de la Santé et de la Recherche Médicale (INSERM)-Sorbonne Université (SU)-Université Paris Descartes - Paris 5 (UPD5)-CHI Créteil-Institut de Recherche pour le Développement (IRD)-Université Paris-Sud - Paris 11 (UP11)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Université Paris Diderot - Paris 7 (UPD7), Service de Pédiatrie et Réanimations néonatales [Béclère], Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-AP-HP - Hôpital Antoine Béclère [Clamart], Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP), Laboratoire Parole et Langage (LPL), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS), Centre de consultation orthopédique et sportive, Clinique du sport de Bordeaux-Mérignac, Institut de Recherche pour le Développement (IRD)-Université Paris-Sud - Paris 11 (UP11)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Université Paris Diderot - Paris 7 (UPD7)-CHI Créteil-Université Paris Descartes - Paris 5 (UPD5)-Institut National de la Santé et de la Recherche Médicale (INSERM), Hôpital Ambroise Paré, Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Assistance publique - Hôpitaux de Paris (AP-HP) (APHP), Institut National de la Santé et de la Recherche Médicale (INSERM)-Sorbonne Universités-Université Paris Descartes - Paris 5 (UPD5)-CHI Créteil-Institut de Recherche pour le Développement (IRD)-Université Paris-Sud - Paris 11 (UP11)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Université Paris Diderot - Paris 7 (UPD7), Université Paris-Sud - Paris 11 (UP11)-Assistance publique - Hôpitaux de Paris (AP-HP) (APHP)-Hôpital Antoine Béclère, and Centre National de la Recherche Scientifique (CNRS)-Aix Marseille Université (AMU)
Subjects: Adult, Male, medicine.medical_specialty, Physical examination, Lesion, Arthroscopic repair, 03 medical and health sciences, Arthroscopy, Rotator Cuff, 0302 clinical medicine, Tendon Injuries, medicine, Humans, Rotator cuff, Orthopedics and Sports Medicine, Prospective Studies, Prospective cohort study, Aged, Aged, 80 and over, 030222 orthopedics, medicine.diagnostic_test, business.industry, Subscapularis muscle, 030229 sport sciences, Preliminary results, Middle Aged, 3. Good health, Surgery, medicine.anatomical_structure, Radiological weapon, Tears, Female, Subcapularis, medicine.symptom, business, [SDV.MHEP]Life Sciences [q-bio]/Human health and pathology
Abstract: SummaryBackgroundUntil the introduction of arthroscopic-assisted surgery for rotator cuff repair, the frequency of subscapularis tears was underestimated. These tears remain challenging to treat even with arthroscopy. The absence of a specific classification system has hampered communication about the treatment and outcomes of the various types of subscapularis tears. The objective of this prospective multicentre study was to validate the relevance of arthroscopic subscapularis tendon repair based on an assessment of short-term outcomes according to the initial extent of the anatomic lesions.MethodsA prospective multicentre study sponsored by the French Society for Arthroscopy was conducted from March 2010 to January 2011 in 208 patients with subscapularis lesions that were either isolated or associated with limited anterosuperior tears. The Constant and UCLA scores were used to assess clinical outcomes. Anatomic and prognostic results were evaluated based on the physical examination, preoperative and postoperative imaging study findings, and anatomic lesions. Clinical data were available for 103 patients after at least 1year of follow-up and radiological data for 129 patients after at least 6months.ResultsThe preliminary clinical results in 103 patients with at least 1year of follow-up showed overall statistically significant improvements in the Constant and UCLA scores, with resolution of the clinical manifestations. The degree of improvement seemed to increase over time. The clinical results varied significantly across patient groups based on a classification system distinguishing four lesion types. Postoperative imaging studies to assess the anatomic results in all patients with at least 6months of follow-up (n=129) showed tendon healing in 92% of cases but also indicated muscle wasting of the upper subscapularis muscle in 18.6% of cases and increased fatty degeneration of the muscle belly.DiscussionOur study confirms the good clinical and radiological results reported in the literature. Our classification system distinguishing four lesion patterns was applicable during the imaging workup. The main finding from this classification system was the difference in results between Type 2 and Type 3 lesions. The trend towards improvements over time requires confirmation by longer-term studies, which will also have to establish that the increased wasting of the upper subscapularis muscle and fatty degeneration of the muscle belly have no adverse effects.Level of evidenceLevel 3.
Published: 2012

37. Prothèse d'épaule à cupule mobile dans le traitement des omarthroses à coiffe détruite

Author: A. Mulliez, C. Maynou, E. Petroff, H. Mestdagh, S. Audebert, and S. Naudi
Subjects: medicine.medical_specialty, medicine.anatomical_structure, business.industry, medicine.medical_treatment, Arthropathy, medicine, Rotator cuff, medicine.disease, business, Arthroplasty, Surgery
Published: 2008

38. 263 Driving Patterns among Younger and Older Emergency Department Patients

Author: E. Petroff, Chris Carpenter, D. Balk, David B. Carr, and Marian E. Betz
Subjects: medicine.medical_specialty, business.industry, Emergency medicine, Emergency Medicine, medicine, Emergency department, Medical emergency, business, medicine.disease
Published: 2012

39. [Arthroplasty with a mobile cup for shoulder arthrosis with irreparable rotator cuff rupture: preliminary results and cineradiographic study]

Author: E, Petroff, H, Mestdagh, C, Maynou, and J M, Delobelle
Subjects: Male, Pain, Postoperative, Rotation, Rupture, Spontaneous, Shoulder Joint, Arthritis, Cineradiography, Videotape Recording, Middle Aged, Prosthesis Design, Rotator Cuff Injuries, Treatment Outcome, Activities of Daily Living, Humans, Female, Arthroplasty, Replacement, Range of Motion, Articular, Aged, Follow-Up Studies
Abstract: Management of patients with massive irreparable rotator cuff tears associated with severe glenohumeral joint degeneration presents a difficult clinical challenge. The present study reports on 24 patients with disabling shoulder pain due to rotator cuff arthropathy treated using a bipolar arthroplasty.Between 1995 and 1997, a bipolar shoulder arthroplasty (Biomet, Warsaw, In) was used in 24 patients (25 shoulders) with rotator cuff arthropathy. Patients were monitored for an average of 14.5 months (range 12 to 24 months). The coracoacromial ligament was maintained in all patients to provide anterosuperior stability. The rotator cuff was irreparable and no attempt was made to cover the superior defect. Postoperative results were reviewed with the Constant score and the Swanson score. In order to verify the head-shell motion and to analyze the dynamic comportement of bipolar arthroplasties, we recorded anterior active elevation and active rotations with video-fluoroscopy.At final the follow-up, 21 shoulders had no or slight pain. Average active flexion improved to 84.8 degrees after operation from 62.4 degrees beforehand. 13 patients achieved more than 90 degrees of active flexion after operation. Active external rotation improved from a mean 3 to 28.8 degrees. Before surgery the average Constant score was 17.62. Postoperatively, the average Constant score was 46.97 and the average Swanson score was 23.13. Complications requiring reoperation occurred in 2 cases: 1 component dislocation (Head-shell), 1 subluxation of the long head of the biceps. Radiographic evaluation at follow up demonstrated no humeral stem loosening or component migration and no bony erosion of the coracoacromial arch. Rupture of the infraspinatus tendon (absolute Constant score: p = 0.04, adjusted Constant score: p = 0.02, Swanson score: p = 0.03, Functional score: p = 0.04), preoperative anterior subluxation of the humeral head (absolute Constant score: p = 0.03, adjusted Constant score: p = 0.05, anterior elevation: p = 0.01, functional score: p = 0.04), preoperative narrowing of the acromio-humeral interval (adjusted Constant score: p = 0.02, overall mobility: p = 0.02, anterior elevation: p = 0.03) may jeopardize the subsequent success of bipolar shoulder arthroplasty. The results of this study suggest that the radius curvature of the shell must match that of the bony surface of the glenoid and the coracoacromial arch (absolute Constant score: p = 0.003, adjusted Constant score: p = 0.005, overall mobility: p = 0.002, anterior elevation: p = 0.0008, functional score: p = 0.002). Recording of anterior active elevation with video-fluoroscopy allowed to identify 3 different types of movements after bipolar shoulder arthroplasty. Recording of internal and external rotation allowed to distinguish 2 differents types of movements. Motion appeared to occur between the bipolar shell and the head. The amount of motion was variable and depended on the biomechanics.Bipolar shoulder arthroplasty is an effective surgical option for patients with massive irreparable tears of the rotator cuff with concomitant glenohumeral arthritis. Satisfactory pain relief and modest gains in motion result in significant functional improvement in this "low functional demand" population. Predictive factors have been identified and should be discussed before surgery.
Published: 1999

40. [Clinical and radiologic outcome of humeral implants in shoulder arthroplasty]

Author: C, Maynou, E, Petroff, H, Mestdagh, H H, Dubois, and O, Lerue
Subjects: Male, Treatment Outcome, Shoulder Joint, Arthritis, Humans, Female, Prostheses and Implants, Arthroplasty, Replacement, Humerus, Middle Aged, Shoulder Injuries
Abstract: The clinical and radiological evolution of the glenoid socket in total shoulder arthroplasty is well documented, whereas evaluation of the humeral component has received much less attention. The outcome of 40 humeral replacements performed in 39 patients was studied with a minimum follow-up of one year. There were 26 Neer prostheses, 9 Modular Shoulder prostheses and 5 Aequalis prostheses. Twenty-nine prostheses were implanted with cement and 11 were cementless. The clinical and radiological results were assessed according to the scoring system used for the 1994 symposium of SO.F.C.O.T. X rays in the coronal plane were used to assess the position of the stem, radiolucencies around the humeral component and the percentage of the cross-section of the diaphysis filled by the humeral stem. The average follow-up period was respectively 55.6 months for the Neer prostheses, 17.9 months for the Modular Shoulder prostheses and 12.4 months for the Aequalis prostheses. Radiolucent lines were noted in 20 cases, all with uncemented humeral components. Two prostheses were loose; however, none required revision. The underlying pathology, surgical approach, position of the humeral component, implant design or association with glenoid resurfacing were not correlated with the presence of radiolucent lines or with a loose implant. Cementless fixation was the only parameter statistically related with the presence of radiolucent lines. This report confirms the good results obtained with cemented humeral prostheses. Radiological evaluation of the smooth cementless humeral implant showed many progressive radiolucent lines, without clinical expression. The authors analyze the various studies in the literature and discuss the interest of cementless implants with ingrowth surface.
Published: 1999

41. [Is calcaneal osteotomy justified in Haglund's disease?]

Author: C, Maynou, H, Mestdagh, H H, Dubois, E, Petroff, and S, Elise
Subjects: Adult, Male, Reoperation, Pain, Postoperative, Adolescent, Arthritis, Bone Screws, Subtalar Joint, Bone Nails, Middle Aged, Achilles Tendon, Osteotomy, Shoes, Radiography, Weight-Bearing, Calcaneus, Postoperative Complications, Treatment Outcome, Bursitis, Recurrence, Activities of Daily Living, Humans, Female, Aged, Follow-Up Studies
Abstract: The authors report their experience of Zadek's wedge osteotomy in the treatment of posterior talalgia in adults and evaluate the various radiographical measurements for calcaneus deformity measurement....This procedure was performed in 27 patients with a total of 36 calcanea treated between 1985 and 1996. The sex ratio was 20 women for 7 men with an average age of 27 years. Prior to this osteotomy nine feet were operated by resection of the postero-superior tuberosity with recurrence of pain and disability, and two patients presented an inflammatory arthritis.For the surgical procedure, the patient was placed in lateral position. Skin incision was five to six centimeters long, curvilinear along the lateral side of the tendo achillis. Two dorsal pins were inserted, creating a triangle so that the apex pointed plantarly and the base dorsally. The sagittal saw was then used to create a wedge osteotomy with a dorsal base of seven to ten millimeters. A screw was then driven across the osteotomy site for ultimate fixation.Eighty per cent (29 osteotomies) of patients had been examined clinically and radiologically with a mean follow-up of 29 months. Considering pain, daily activity and discomfort with footwear, results were excellent in 12 cases, good in 10, fair in 5 and poor in two cases. No radiological criteria used for the diagnosis of Haglund's disease were absolutely reliable. The "total angle" of Ruch, the "c.l angle" of Chauveaux and the "parallel pitch lines" of Heneghan reflect the amount of deformation most accurately, but especially, the calcaneal inclination angle was always increased (16 cases between 18 degrees and 30 degrees, 6 cases30 degrees). All patients had a weight-bearing calcaneal talus, either alone or in the context of posterior pes cavus.This study confirms the responsibility of rearfoot morphostatic disorders in posterior talalgia and the goods results obtained by Zadek osteotomy.
Published: 1999

42. [Long-term results of proximal osteocartilaginous autografts in extensive cartilagenous destruction of the knee. Apropos of 5 cases]

Author: C, Maynou, H, Mestdagh, E, Beltrand, E, Petroff, and H, Dubois
Subjects: Adult, Cartilage, Articular, Male, Knee Joint, Knee Injuries, Transplantation, Autologous, Weight-Bearing, Arthroscopy, Osteoarthritis, Humans, Femur, Range of Motion, Articular, Wound Healing, Bone Transplantation, Tibia, Graft Survival, Osteonecrosis, Patella, Middle Aged, Osteochondritis Dissecans, Osteotomy, Radiography, Cartilage, Female, Osteosclerosis, Follow-Up Studies
Abstract: Five patients with a large defect in the articular cartilage at the knee joint were treated by transplantation of an autogenic osteochondral fragment. The graft was harvested from the posterior portion of the ipsilateral femoral condyle in 4 cases of osteochondritis dissecans, and from the lateral third of the patella pedicled on the patellar ligament in one case of posttraumatic necrotic collapse of the lateral tibial plateau. One patient underwent concomitant high tibial osteotomy. Two months postoperatively bony union was achieved in all cases but in one case, the grafted articular cartilage did not survive after weight bearing because of an overlooked varus deformity. At the follow-up examination (8 to 20 years) all 5 patients were asymptomatic ; the range of flexion was somewhat restricted (120 degrees) ; roentgenogram revealed slight narrowing of the articular space or at least flattening of the grafted zone and subchondral osteosclerosis. At arthroscopic exploration, the grafted zones were recognizable from the surrounding cartilage, and histologic examination of their border revealed fibrocartilage and proliferating vessels; late gonarthrosis might ensue over time. Therefore the procedure should be performed only in large osteochondral defects where neither reattachment of a loose body, nor hemiarthroplasty, nor isolated osteotomy are suitable and before degenerative changes have developed. Morever any associated varus deformity requires concomitant correction by high tibial osteotomy to relieve stress from the graft.
Published: 1998

43. [Effect of the rotator cuff condition on the results of shoulder arthroplasty]

Author: H, Mestdagh, E, Petroff, C, Maynou, P, Forgeois, and B, Singer
Subjects: Adult, Diagnostic Imaging, Male, Shoulder Joint, Middle Aged, Prognosis, Rotator Cuff Injuries, Rotator Cuff, Treatment Outcome, Humans, Female, Arthroplasty, Replacement, Range of Motion, Articular, Aged
Abstract: The purpose of this report was to study the repercussions of rotator cuff condition on unconstrained shoulder arthroplasty results.Between 1986 and 1993, 40 unconstrained shoulder prostheses were performed (24 total and 16 hemiarthroplasties). At the time of the operation, rotator cuff condition was reported to be normal in 15 shoulders, atrophic in 10, scarred in 3, torn in 12. Clinical and radiographical results were analyzed and supplemented with a rotator cuff echography. Postoperative follow-up averaged 42.25 months (12 to 97 months).When the rotator cuff was intact at the time of operation, clinical results were the best at the time of review. Constant score, overall mobility, forward elevation, external rotation with the elbow along the side were better for intact than for atrophic, scarred or torn rotator cuffs (p0.01). Ruptures repaired by local tissue transfer or trapezo deltoidal flap substitution (3 cases) gave satisfactory results, whereas two dacron cuff prostheses failed. In the non repaired ruptures (7 cases), arthroplasty resulted in 3/4 fair or poor results. At the time of review, the total incidence of postoperative rotator cuff tears was high (12 cases), functional repercussions were variable. Among the 15 rotator cuff tears observed at the time of the review, the long head of the biceps was present and in place in 9 cases and ruptured in 6 cases. In these latter cases, Constant score (p0.01), the forward elevation (p0.01), external rotation with elbow along side (p0.05) and overall mobility (p0.05) were worse; moreover, humeral head superior migration was greater (p0.01).Our study confirms the superiority of clinical results when the cuff was intact at the time of the operation. The repair of rotator cuff tears seems to be justified. When the rupture has not been repaired, clinical results were fair or poor in 5 cases out of 7, the initial rupture spread to the other tendons in 3 cases out of 7. Secondary ruptures were frequent (12 cases). No predictive factor was identified, but an overlapping of the greater tuberosity appears to be detrimental. Among rotator cuff tears present at the time of review, long head of the biceps rupture jeopardized clinical results and was associated with a proximal migration of the humeral head which was significantly more severe than with an intact non displaced long head of the biceps.During unconstrained shoulder prosthesis implantation, it is therefore recommend to systematically repair any associated rotator cuff rupture, in order to avoid any greater tuberosity overlap relative to the prosthetic head and to preserve the long head of the biceps tendon which limits upward migration of the humeral head and improves prosthetic kinetics.
Published: 1997

44. [Surgical treatment of the rheumatoid forefoot by realignment using th dorsal approach]

Author: C, Maynou, H, Mestdagh, E, Petroff, P, Forgeois, and E, Hue
Subjects: Arthritis, Rheumatoid, Foot Diseases, Foot Deformities, Acquired, Arthrodesis, Humans, Female, Bone Nails, Follow-Up Studies, Metatarsus, Osteotomy
Abstract: The aim of this study was to appreciate the results of the modified Fowler's procedure in the surgical treatment of forefoot deformities due to rheumatoid arthritis.If the principles of the metatarsophalangeal resection through a dorsal transverse incision were conserved, we progressively modified the initial procedure with renunciation to the plantar skin incision, preservation of a skin bridge between the medial and transverse dorsal approach, using centro medullary pins to hold in position toes alignment and making an arthrodesis of the first metatarsophalangeal joint. Ten patients (17 surgical procedures) were clinically and roentgenographically reviewed at an average follow-up of 27.3 months (Range : 12 and 53 months).Clinical results according to the Gainor scale showed an increase of the overall score from 3.4 points to 11.2 points at revision. Twelve foot were rated excellents and five goods. Seventy per cent of patients had no pain and 58 per cent used a normal footwear. Radiographical and clinical analysis showed that an egyptian foot remained in nine cases, podoscopic examination revealed frequently a lack of footrest on lateral toes without functional implications. Delayed wound healing were observed in four cases with good evolution.With this surgical procedure, our functional results were encouraging and we recommend it in severe deformities of the rheumatoid foot with fixed metatarsophalangeal dislocations and bone defect of the metatarsal heads.
Published: 1997

45. 366 Distracted Driving and Emergency Department Patients

Author: Marian E. Betz, E. Petroff, and D. Balk
Subjects: business.industry, Emergency Medicine, Distracted driving, Medicine, Emergency department, Medical emergency, business, medicine.disease
Published: 2012

46. Fabrication of Thick, Sol Gel Pzt Films: Applications to Macroscopic Piezoelectric Devices

Author: T. E. Petroff, D. A. Barrow, and Michael Sayer
Subjects: Materials science, Fabrication, Optical fiber, Dielectric, Lead zirconate titanate, Piezoelectricity, Ferroelectricity, law.invention, chemistry.chemical_compound, chemistry, law, Composite material, Coaxial, Sol-gel
Abstract: Lead zirconate titanate (PZT) films of up to 60 μm in thickness have been fabricated on a wide variety of substrates using a new sol gel process. The dielectric properties (∈ = 900), ferroelectric (Ec = 16 kV/cm and Pr = 35 μC/cm 2) and piezoelectric properties are comparable to bulk values. The characteristic Curie point of these films is at 420 °C. Piezoelectric actuators have been developed by depositing thick PZT films on both planar and coaxial substrates. Stainless steel cantilevers and optical fibres coated with a PZT film exhibit flexure mode resonant vibrations observable with the naked eye. A low frequency in-line fibre optic modulator has been developed using a PZT coated optical fibre. The high frequency resonance of a 60 μm film on a aluminum substrate has been observed.
Published: 1994

47. [The stay in the hospital]

Author: E, Bayle, G, Hatem-Gantzer, E, Petroff, D, Horassius, C, Dossantis, B, Arnaud, E, Benchetrit, L, Coussirou, J, Dufond, and I, Gérintes
Subjects: Hospitalization, Massage, Pregnancy, Pregnancy in Diabetics, Anesthesia, Obstetrical, Humans, Baths, Female, Emergencies, Relaxation Therapy
Published: 1993

48. [When a child is to be born, that is quite a story]

Author: E, Petroff
Subjects: Labor, Obstetric, Pregnancy, Anesthesia, Obstetrical, Humans, Female, Obstetrics and Gynecology Department, Hospital
Published: 1993

49. The SUrvey for Pulsars and Extragalactic Radio Bursts – III. Polarization properties of FRBs 160102 and 151230

Author: W. van Straten, E. Petroff, Matthew Bailes, M. Burgay, Caterina Tiburzi, Benjamin Stappers, Manisha Caleb, E. D. Barr, N. D. R. Bhat, Simon Johnston, A. Jameson, V. Venkatraman Krishnan, Evan Keane, Fabian Jankowski, Shivani Bhandari, Wael Farah, A. Possenti, Michael Kramer, and Jean-Pierre Macquart
Subjects: FOS: Physical sciences, Astrophysics, magnetic fields, 01 natural sciences, Radio telescope, surveys, Pulsar, 0103 physical sciences, data analysis [methods], 010303 astronomy & astrophysics, Circular polarization, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, polarization, 010308 nuclear & particles physics, Linear polarization, Scattering, Astronomy and Astrophysics, Polarization (waves), Position angle, methods: data analysis, Magnetic field, 13. Climate action, Space and Planetary Science, intergalactic medium, Astrophysics - High Energy Astrophysical Phenomena
Abstract: We report on the polarization properties of two fast radio bursts (FRBs): 151230 and 160102 discovered in the SUrvey for Pulsars and Extragalactic Radio Bursts (SUPERB) at the Parkes radio telescope. FRB 151230 is observed to be 6 $\pm$ 11% circularly polarized and 35 $\pm$ 13 % linearly polarized with a rotation measure (RM) consistent with zero. Conversely, FRB 160102 is observed to have a circular polarization fraction of 30 $\pm$ 11 %, linear polarization fraction of 84 $\pm$ 15 % for RM = -221(6) rad m$^{-2}$ and the highest measured DM (2596.1 $\pm$ 0.3 pc cm$^{-3}$) for an FRB to date. We examine possible progenitor models for FRB 160102 in extragalactic, non-cosmological and cosmological scenarios. After accounting for the Galactic foreground contribution, we estimate the intrinsic RM to be -256(9) rad m$^{-2}$ in the low-redshift case and $\sim 2.4 \times 10^{2}$ rad m$^{-2}$ in the high-redshift case. We assess the relative likeliness of these scenarios and how each can be tested. We also place constraints on the scattering measure and study the impact of scattering on the signal's polarization position angle., 12 pages, 7 figures, accepted for publication in MNRAS
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50. New endoscopic classification for subscapularis lesions

Author: P. Hardy, T. Joudet, Yves Lefebvre, S. Audebert, Pascal Boileau, Johannes Barth, B Toussaint, N. Solignac, Nicolas Graveleau, Christophe Scymanski, Carlos Maynou, Christophe Charousset, C E Thelu, Arnaud Godenèche, Laurent Nové-Josserand, and E Petroff
Subjects: medicine.medical_specialty, Sling (implant), Rotator Cuff Injuries, Lesion, Arthroscopy, Tendon Injuries, medicine, Humans, Orthopedics and Sports Medicine, Rotator cuff, Prospective Studies, Lesser Tuberosity, Anatomical lesions, medicine.diagnostic_test, business.industry, Rotator cuff injury, Subscapularis tears, medicine.disease, Classification, Surgery, medicine.anatomical_structure, Homogeneous, Tears, medicine.symptom, business
Abstract: Summary Background The absence of a coherent classification system has hampered communication about the treatment and outcomes of the various types of subscapularis tendon lesions. In addition, a reliable classification system allows comparisons of epidemiological and therapeutic data. The classification systems used until now fail to incorporate the radiological and intraoperative abnormalities of the bicipital sling, and they do not consider the degree of subscapularis tendon cleavage. Here, we describe a new arthroscopy-based classification system intended for therapeutic and prognostic purposes. Methods A prospective multicentre study sponsored by the French Society for Arthroscopy was conducted from March 2010 to January 2011 in 150 isolated subscapularis lesions with or without limited anterosuperior involvement. The bicipital sling and insertion of the deep subscapularis layer were routinely investigated by arthroscopy with video recording. Each lesion was classified after a consensus was reached among four surgeons. Results We identified four lesion types based on the bicipital sling findings. Type I was defined as partial separation of the subscapularis tendon fibres from the lesser tuberosity with a normal bicipital sling. Type II consisted of a partial subscapularis tear at the lesser tuberosity attachment combined with partial injury to the anterior wall of the bicipital sling, without injury to the superior glenohumeral ligament. Type III was complete separation of the subscapularis fibres from the lesser tuberosity with extensive cleavage of the bicipital sling. Finally, in Type IV, all the subscapularis fibres were detached and, in some cases, conjunction of the subscapularis and supraspinatus fibres produced the comma sign. Nearly all the lesions identified intraoperatively during the study fit one of these four types. Discussion A reproducible classification system that allows different surgeons to establish comparable homogeneous patient groups is useful for both therapeutic and prognostic purposes. We defined four types of subscapularis lesions that are easy to identify as either isolated lesions or combined with anterosuperior rotator cuff tears. Long head of biceps tendon abnormalities and fatty degeneration of the shoulder muscles can be added to our classification system. Studies of intraobserver and interobserver reproducibility are needed to complete the process of validating the diagnostic and/or prognostic usefulness of this new classification scheme. Level of evidence II.
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