Author: "A. G. Lyne" / Topic: pulsar - Searchworks@Jio Institute Digital Library Search Results

Your search keyword '"A. G. Lyne"' showing total 37 results

Start Over Author "A. G. Lyne" Topic pulsar

37 results on '"A. G. Lyne"'

1. Strong-Field Gravity Tests with the Double Pulsar

Author: M. Kramer, I. H. Stairs, R. N. Manchester, N. Wex, A. T. Deller, W. A. Coles, M. Ali, M. Burgay, F. Camilo, I. Cognard, T. Damour, G. Desvignes, R. D. Ferdman, P. C. C. Freire, S. Grondin, L. Guillemot, G. B. Hobbs, G. Janssen, R. Karuppusamy, D. R. Lorimer, A. G. Lyne, J. W. McKee, M. McLaughlin, L. E. Münch, B. B. P. Perera, N. Pol, A. Possenti, J. Sarkissian, B. W. Stappers, G. Theureau, 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), Institut des Hautes Etudes Scientifiques (IHES), IHES, 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)), and 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)
Subjects: higher-order, Astronomy, QC1-999, Astrophysics::High Energy Astrophysical Phenomena, deflection, binary, FOS: Physical sciences, General Physics and Astronomy, General Relativity and Quantum Cosmology (gr-qc), spin, 01 natural sciences, General Relativity and Quantum Cosmology, strong field, 0103 physical sciences, propagation, general relativity, 010306 general physics, neutron star, 010303 astronomy & astrophysics, orbit, equation of state, pulsar, High Energy Astrophysical Phenomena (astro-ph.HE), Quantum Physics, effect, precision measurement, Physics, photon, formation, deformation, gravitational radiation, Condensed Matter Physics, moment, gravitation, relativistic, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astronomical and Space Sciences
Abstract: Continued observations of the Double Pulsar, PSR J0737-3039A/B, consisting of two radio pulsars (A and B) that orbit each other with a period of 2.45hr in a mildly eccentric (e=0.088) binary system, have led to large improvements in the measurement of relativistic effects in this system. With a 16-yr data span, the results enable precision tests of theories of gravity for strongly self-gravitating bodies and also reveal new relativistic effects that have been expected but are now observed for the first time. These include effects of light propagation in strong gravitational fields which are currently not testable by any other method. We observe retardation and aberrational light-bending that allow determination of the pulsar's spin direction. In total, we have detected seven post-Keplerian (PK) parameters, more than for any other binary pulsar. For some of these effects, the measurement precision is so high that for the first time we have to take higher-order contributions into account. These include contributions of A's effective mass loss (due to spin-down) to the observed orbital period decay, a relativistic deformation of the orbit, and effects of the equation of state of super-dense matter on the observed PK parameters via relativistic spin-orbit coupling. We discuss the implications of our findings, including those for the moment of inertia of neutron stars. We present the currently most precise test of general relativity's (GR's) quadrupolar description of gravitational waves, validating GR's prediction at a level of $1.3 \times 10^{-4}$ (95% conf.). We demonstrate the utility of the Double Pulsar for tests of alternative theories by focusing on two specific examples and discuss some implications for studies of the interstellar medium and models for the formation of the Double Pulsar. Finally, we provide context to other types of related experiments and prospects for the future., 56 pages, 23 Figures. Published by Physical Review X. Uploaded ArXiv version is authors' (pre-proof) version with abbreviated abstract. Resubmission for updated acknowledgement information. For final published version see https://link.aps.org/doi/10.1103/PhysRevX.11.041050
Published: 2021

2. Erratum: 'Searches for Gravitational Waves from Known Pulsars at Two Harmonics in 2015–2017 LIGO Data' (2019, ApJ, 879, 10)

Author: P. Kumar, B. R. Hall, R. Cavalieri, A. K. Srivastava, A. E. Pace, A. Fernandez-Galiana, A. Basti, Ryan N. Lang, J.-P. Coulon, T. Hardwick, D. Steinmeyer, E. A. Chase, Z. Frei, Piotr Jaranowski, V. Sequino, S. Caride, Jordan Camp, J. Liu, F. Travasso, Michał Bejger, A. Pasqualetti, J.-D. Fournier, M. Croquette, Philip F. Hopkins, Christian Pedersen, H. M. Lee, L. Xiao, Milan Gupta, P. Fulda, P. T.H. Pang, T. Etzel, G. Mendell, C. S. Unnikrishnan, J. Jiang, I. Fiori, S. J. Jadhav, B. C. Pant, Sourav Ghosh, Imre Bartos, V. Germain, V. Quetschke, Martin M. Fejer, R. Bork, S. Ghonge, Shawn Rosofsky, T. Di Girolamo, K. AultONeal, A. Perreca, S. M. Scott, G. Gemme, L. van der Schaaf, S. A. Pai, Cody Messick, M. Drago, L. E. Wade, Rebecca Fisher, K. S. Phukon, J. Li, J. Eichholz, Guenakh Mitselmakher, Zhihui Du, I. Belahcene, S. E. Barclay, M. Fyffe, R. Kirchhoff, R. Colgan, B. L. Pearlstone, D. M. Macleod, Charalampos Markakis, Archana Pai, W. Z. Korth, Gabriela Gonzalez, K. R. Corley, Christopher P. L. Berry, J. L. Willis, M. Eisenmann, Ofek Birnholtz, Archisman Ghosh, F. Paoletti, B. A. Boom, Samuel Deléglise, B. L. Swinkels, A. M. Sergeev, Torrey Cullen, G. Vedovato, L. E. H. Datrier, Samuele Cortese, Charlie Hoy, A. M. Holgado, G. Ciani, D. B. Kozak, A. D. Silva, J. Suresh, M. C. Milovich-Goff, J. L. Wright, Sebastiano Bernuzzi, P. Booker, S. Mastrogiovanni, Nicolas Sanchis-Gual, P. Ruggi, A. Parida, R. K. Lanza, S. S. Eikenberry, R. Pedurand, Benno Willke, S. T. Countryman, Michael E Zucker, A. Grado, Andrew Matas, C. D. Booth, D. Stocks, Surabhi Sachdev, Christopher J. Moore, Alessandra Corsi, Sanjay Kumar, V. V. Frolov, M. Fitz-Axen, Eric Howell, A. Singhal, P. Thomas, M. Arène, A. Mullavey, T. J. N. Nelson, V. Fafone, J. Betzwieser, C. Vorvick, G. Kang, Daniel E. Holz, B. J. J. Slagmolen, P. Dupej, Alena Ananyeva, Stanislav Babak, M. Constancio, C. Cahillane, Debnandini Mukherjee, C. Pankow, P. M. Meyers, S. Doravari, M. Muratore, M. C. Heintze, P. J. Sutton, Alyssa Garcia, B. Patricelli, F. Carbognani, D. S. Wu, Margaret Millhouse, J. H. Romie, G. D. O'Dea, Bruno Giacomazzo, A. Pal-Singh, S. Leavey, Hai-Ping Cheng, A. Iess, L. K. Nuttall, Erik Katsavounidis, R. Macas, G. Billingsley, S. Macfoy, O. Halim, K. W. Tsang, Kendall Ackley, R. K. Nayak, B. D. Lackey, P. Grassia, Kipp Cannon, M. Steinke, Xiaohui Fan, Richard O'Shaughnessy, B. Barr, J. Worden, Rana X. Adhikari, F. Donovan, R. Kennedy, Geoffrey Lovelace, S. G. Gaonkar, Antoine Heidmann, D. Töyrä, David Jones, Marco Cavaglia, Sascha Husa, G. Venugopalan, D.B. DeBra, A. K. Zadrożny, H. Estelles, K. Siellez, J. Derby, K. A. Thorne, Isabel Cordero-Carrión, Sung-Po Chao, H. Overmier, Eric B. Flynn, B. Gateley, G. Kuehn, Haixing Miao, H. Ohta, G. Bogaert, J. J. Bero, F. J. Raab, N. Mukund, S. Marsat, V. Tiwari, Yann Bouffanais, V. Avendano, Xiuling Li, Matthew Evans, K. L. Dooley, R. Inta, L. R. Cominsky, Rosa Poggiani, V. Frey, A. K. Mehta, S. Farinon, A. Pele, E. J. Daw, Maurizio Canepa, P. H. Nguyen, Antonio Marquina, T. A. Ferreira, M. Rakhmanov, P. Oppermann, Aaron Buikema, J. Hennig, V. Gayathri, S. Walsh, Miriam Cabero, Alessandra Buonanno, R. Metzdorff, C.-J. Haster, Gabrielle Allen, D. M. Wilken, S. Klimenko, Leo Tsukada, P. T. Baker, A. Avila-Alvarez, K. Gill, J. Palfreyman, Fangchen Feng, B. Lantz, B. Irwin, C. C. Yancey, W. G. Anderson, G. Cella, H. Vahlbruch, J. C. Mills, K. Riles, R. Mittleman, Francesco Pannarale, Soichiro Morisaki, Paul J. Groot, M. Zevin, N. A. Holland, K. Rao, Podila Satya Venkata Narasimha Sharma, K. D. Giardina, P. J. Veitch, R. De Rosa, I. Nardecchia, D. Sellers, H. Radkins, Lisa Barsotti, H. Y. Chia, Fl Linde, F. Magaña-Sandoval, M. F. Carney, C. Whittle, R. Gustafson, H. J. Bulten, Anirban Dasgupta, E. Z. Hamilton, Walter Winkler, B. P. Abbott, A. Bozzi, R. J. G. Jonker, J. K. Wofford, M. A. Page, J. Y. Vinet, H. Middleton, J. B. Kanner, Michael Keith, Robert J. McCarthy, C. C. Wipf, E. J. King, Nelson Christensen, Linqing Wen, P. Raffai, L. Naticchioni, Salvatore Vitale, A. Cumming, F. Di Renzo, Lee McCuller, N. Mazumder, J. D. E. Creighton, E. K. Gustafson, M. Weinert, H. A. G. Gabbard, S. V. Angelova, John Veitch, J. Lehmann, T. D. Abbott, J. Meidam, A. W. Heptonstall, Pablo Cerdá-Durán, Vivien Raymond, Peter R. Saulson, Alessandro Corongiu, S. Vass, S. Raja, E. Genin, J. Zhang, F. Baldaccini, L. F. Ortega, A. Rocchi, A. S. Markosyan, S. E. Strigin, J. V. Van Heijningen, H. Fong, G. Greco, J. S. Lange, F. Fidecaro, G. M. Guidi, Harald Lück, F. Marion, J. McIver, Z. Tornasi, M. J. Cowart, P. Puppo, A. L. Urban, D. Ugolini, P. Clearwater, K. E. Ramirez, D. W. Yeeles, Zoheyr Doctor, A. Malik, S. Gaudio, E. J. Fauchon-Jones, R. M. S. Schofield, R. Coyne, Fabrice Matichard, H. N. Isa, N. Arnaud, Maggie Tse, L. Wallace, A. Królak, Riccardo Sturani, J. Hanks, M. Lormand, R. Abbott, A. Ain, R. J. Trudeau, D. Moffa, J. Zweizig, C. De Rossi, D. Verkindt, C. Cocchieri, B. Goncharov, R. Birney, F. Frasconi, E. L. Merilh, M. Kinley-Hanlon, M. C. Tringali, S. Hochheim, N. A. Robertson, M. Cho, David Coward, D. Tuyenbayev, E. A. Huerta, D. J. Stops, J. S. H. Lee, Felix Wellmann, R. Flaminio, J. Warner, J. J. McCann, T. J. Slaven-Blair, S. ShyamSundar, C. Stachie, R. Frey, Duncan Meacher, N. V. Keerthana, Moritz Mehmet, Benjamin J. Owen, R. Passaquieti, J. F. J. van den Brand, E. A. Muñiz, K. Y. Ng, S. Brunett, Marco Romanelli, E. K. Wessel, Vijay Varma, M. MacInnis, C. Rajan, J. K. Blackburn, Bala R. Iyer, Terry G. McRae, E. Chassande-Mottin, S. P. Stevenson, Sebastian Steinlechner, Sheila Rowan, S. Caudill, G. Gaur, S. C. McGuire, J. F. Read, Chris A. Collins, J. G. Bartlett, Márton Tápai, W. Ren, Mandar Patil, Abhirup Ghosh, Sheon Chua, S. Sunil, M. Tacca, Martin Hendry, Cecilio García-Quirós, R. Bonnand, S. Di Pace, Mariana Fazio, A. Dmitriev, G. Koekoek, A. J. Weinstein, R. Goetz, S. Katsanevas, V. Boschi, Marcus E. Lower, Tarun Souradeep, M. Yvert, S. Ponrathnam, B. U. Gadre, M. Pürrer, S. Kwang, C. L. Romel, M. C. Díaz, Sebastien Biscans, G. A. Prodi, J. C. Barayoga, S. McCormick, P. Rapagnani, T. Mistry, A. L. Stuver, D. Hoak, D. Sentenac, A. Bisht, R. DeSalvo, Karsten Danzmann, N. Letendre, L. G. Prokhorov, Patrick Brady, Nikhil Sarin, D. Passuello, Odylio D. Aguiar, I. W. Martin, C. F. Da Silva Costa, Hua Wang, M. van Beuzekom, Liam Cunningham, M. Punturo, Leopoldo Milano, K. Haris, Madeline Wade, M. Di Giovanni, P. Leaci, L. Glover, S. A. Bilgili, Jay D. Tasson, S. Mitra, A. W. Jones, H. S. Chen, M. Landry, R. De Pietri, S. Biscoveanu, Rocco Romano, A. Cirone, P. Couvares, F. Garufi, David H. Shoemaker, S. Karki, Junwei Cao, O. V. Palashov, Sean T. McWilliams, Y. Boetzel, Hongyu Shen, Nicholas Demos, J. D. Lough, D. C. Coyne, Colm Talbot, Andreas Freise, M. Boer, M. A. Okada, Shubhanshu Tiwari, A. F. Brooks, P. J. Quinonez, F. Piergiovanni, Slawomir Gras, D. Lumaca, M. Haney, K. Mason, L. Di Fiore, B. Mours, Jingbo Wang, Soma Mukherjee, E. C. Ferreira, Sanjeev Dhurandhar, G. Wang, Hyun Lee, S. W. S. Ng, John D. Scott, M. Standke, Otto A. Hannuksela, Surendra Nadh Somala, C. Austin, N. Radulescu, Patrick Godwin, R. A. Mercer, M. Barsuglia, Jan Harms, A. S. Sengupta, J. Calderón Bustillo, K. Izumi, T. Sadecki, Paul D. Lasky, Kiran Prasai, J. W. Westhouse, T. A. Callister, Matthew Pitkin, Denis Martynov, Marco Bazzan, Xin Chen, R. M. Martin, David A. Nichols, W. Katzman, S. Grunewald, R. Prasanna, Edward K. Porter, D. Buskulic, G. Giordano, K. Toland, D. J. Hofman, C. Ingram, L. Pinard, G. L. Mansell, I. Maksimovic, S. Ossokine, Jinsook Kim, R. L. Ward, G. Hemming, C. Affeldt, L. Matone, M. Davier, M. C. Araya, Srishti Tiwari, C. Lazzaro, Patricia Schmidt, V. Brisson, M. J. Yap, Lindsay DeMarchi, C. K. Cheong, Hyang Woon Lee, A. Grant, John R. Smith, C. Palomba, S. Privitera, Matthew Kerr, M. Khursheed, A. Possenti, Federico Ferrini, F. Brighenti, Jade Powell, B. B. Lane, A. Viceré, Lucas Guillemot, C. Messenger, L. Kuo, H. Yamamoto, Lijing Shao, G. Vajente, E. Capocasa, S. M. Gaebel, José A. Font, N. Singh, J. P. Zendri, G. Rutins, Graham Woan, R. Taylor, Robert L. Byer, Stuart Reid, M. S. Shahriar, Tyson Littenberg, T. D. Creighton, L. Zhang, J. H. Klika, S. Barnum, James Healy, P. A. Altin, Haocun Yu, M. Hulko, V. Mangano, Riccardo Ciolfi, Yi Chen, B. W. Schulte, M. Granata, J. C. Driggers, A. Schönbeck, Alexander C. Jenkins, B. Rajbhandari, P. Brockill, M. Nery, Ettore Majorana, A. A. Ciobanu, S. A. Usman, Y. K. Lecoeuche, G. M. Harry, Maya Fishbach, K. W. Chung, S. Ascenzi, V. Kringel, F. J. Hayes, M. Agathos, M. Kasprzack, E. Cuoco, Jacob Scheuer, Binlei Ding, S. M. Koehlenbeck, Gregorio Carullo, G. Pagano, S. Appert, Y. Setyawati, Roman Schnabel, L. Sammut, Daniel Wysocki, J. E. Brau, A. A. van Veggel, D. Fiorucci, A. K. Prajapati, A. Gupta, S. Meshkov, Seog Oh, N. Leroy, R. L. Savage, Efim A. Khazanov, G. Ballardin, A. S. Bell, M. Laxen, D. Barker, A. Samajdar, Michael L. Gorodetsky, Vuk Mandic, Minchuan Zhou, H. K. Gulati, David H. Reitze, Rahul Kashyap, A. Markowitz, Ryan Lynch, J. Prasad, Alessandro Ridolfi, B. Bécsy, M. Bawaj, Alessandro Bertolini, Q. Chu, Bernard F. Schutz, Li Ju, C. Buy, M. Oliver, Daniel A. Shaddock, Brittany Kamai, G. Dálya, A. Giazotto, P. Shawhan, Lionel London, F. Aubin, A. R. Wade, I. Ferrante, G. Stratta, C. M. Mow-Lowry, Sergey P. Vyatchanin, F. Y. Khalili, D. C. Vander-Hyde, Alejandro Torres-Forné, A. Allocca, P. Ehrens, Paul M. Ricker, Jesper Munch, H. Khan, G. Valdes, Steven Bloemen, R. Tso, K. Venkateswara, R. Cotesta, D. J. McManus, Jonathan R. Gair, C. Horst, F. Lin, Alice K. Harding, Tania Regimbau, S. B. Anderson, J.-G. Ducoin, Tim Dietrich, C. V. Kalaghatgi, J. Hanson, A. Miller, N. Koper, L. Mereni, B. Idzkowski, V. Loriette, L. Aiello, M. Gosselin, R. Green, Vivishek Sudhir, Rico K. L. Lo, E. E. Cowan, B. F. Whiting, E. Schreiber, J. Casanueva Diaz, S. D. Linker, B. Pang, R. Robie, A. Hreibi, Tristan Briant, V. Skliris, L. Sun, Marta Colleoni, William Parker, N. A. Lockerbie, R. C. Walet, Patrick M. Koch, J. Neilson, P. Charlton, J. A. Giaime, Kejia Lee, Mark A. Scheel, F. Clara, A. K. Lenon, Alberto Vecchio, Y. M. Kim, J. M. Fishner, Maher Yazback, Zachariah B. Etienne, V. P. Mitrofanov, S. Kaufer, S. Banagiri, H. Qi, L. Magaña Zertuche, Lili Yang, Hang Yu, N. Bode, P. Schale, Leo Singer, Achamveedu Gopakumar, C. Van Den Broeck, E. Sowell, A. M. Sintes, M. A. Aloy, M. Bitossi, G. Bergmann, K. Wette, M. De Laurentis, W. Del Pozzo, P. F. Cohadon, H. Heitmann, Carlos O. Lousto, T. Prestegard, T. L. Lam, O. J. Piccinni, Keith C. Gendreau, J. S. Areeda, K. Bossie, Tomasz Bulik, Will M. Farr, M. Montani, Jennifer Watchi, Miftar Ganija, T. P. Downes, Rainer Weiss, K. A. Santiago, F. Ricci, M. Branchesi, Gilles Theureau, M. Was, D. Huet, S. H. Huttner, M. H. Wimmer, A. Effler, Dániel Barta, A. Kumar, V. Srivastava, M. Fays, M. M. Hanke, Alessandro Longo, Hartmut Grote, Chandra Kant Mishra, R. Bhandare, Ryan Magee, John J. Oh, Timothy Evans, C. North, Thomas Dent, P. Corban, M. C. Edwards, S. C. Tait, Nancy Aggarwal, Zahoor Ali Khan, M. Pedraza, M. Chan, Richard J. Oram, L. Trozzo, D. Y. T. Pong, E. Massera, A. Di Lieto, Matthew Bailes, S. J. Chamberlin, M. Vasúth, Zifan Zhou, P. Ajith, Jonathan Cripe, C-H. Lee, Andrew Melatos, M. Lorenzini, I. A. Bilenko, L. Haegel, G. Losurdo, David J. Ottaway, E. Bonilla, Robert Stone, Rory Smith, C. Adams, Kazuhiro Agatsuma, Alessandro Nagar, A. Mishkin, A. Paoli, F. Cavalier, T. Enoto, H. Vocca, S. J. Kapadia, P. B. Covas, Frank Ohme, Eugeniy E. Mikhailov, V. Bossilkov, D. B. Tanner, Edward Seidel, Albert Lazzarini, O. E. S. Sauter, J. H. Briggs, Mark Hannam, F. Thies, X. Liu, R. M. Blair, D. Sigg, S. W. Ballmer, D. M. Shoemaker, M. Tonelli, François Bondu, A. Gennai, Rahul Kumar, Harald P. Pfeiffer, J. M. Gonzalez Castro, I. Dave, B. D. Cheeseboro, G. Cerretani, P. J. Easter, Kevin M. Ryan, M. Korobko, J. Woehler, Tanja Hinderer, F. Badaracco, Michelle E. Walker, Samaya Nissanke, M. Fletcher, B. Hughey, Zaven Arzoumanian, A. Ramos-Buades, A. R. Williamson, A. Strunk, S. L. Danilishin, M. Rizzo, B. K. Berger, Olivier Minazzoli, Devon S. Johnson, David Cohen, David E. McClelland, T. Huynh-Dinh, P. Weltervrede, Chunglee Kim, David Blair, S. D'Antonio, S. Chung, N. Kijbunchoo, Sheelu Abraham, G. Moreno, W. A. Campbell, A. Kontos, K. Rose, N. N. Janthalur, N. V. Krishnendu, J. Junker, S. Sitmukhambetov, Ismaël Cognard, J. S. Kissel, H. Cao, D. J. Vine, S. Penn, A. C. Green, Neil J. Cornish, D. Rosińska, M. Razzano, P. G. Murray, G. Mo, B. Sassolas, C. Fee, Andrew Lundgren, G. Cho, W. S. Kim, Marc Favata, Xing-Jiang Zhu, Patrice Hello, Kevin Barkett, J. Birch, S. Bae, S. E. Gossan, Roger Jones, V. J. Roma, C. J. Richardson, J. M. Isac, A. P. Spencer, Fausto Acernese, A. Chiummo, V. Dattilo, Edwin J. Son, E. Coccia, C. Graef, B. A. Weaver, J. G. Rollins, L.-W. Wei, Felice Sorrentino, D. Moraru, C. Gray, G. H. Ogin, D. D. Brown, Gianpietro Cagnoli, Fabien Kéfélian, J. H. Hough, P. W. F. Forsyth, Anthony A. Amato, N. van Bakel, Stefan Hild, Y. Ma, I. Dorrington, S. R. Thondapu, J. R. Palamos, I. Di Palma, F. Martelli, Karan Jani, R. Shink, E. Goetz, Giuseppe Intini, R. A. Eisenstein, T. J. Shaffer, A. Masserot, Yuri Levin, M. Mantovani, E. A. Quintero, A. Brillet, K. Kawabe, S. M. Aston, A. Trovato, Luca Gammaitoni, M. B. Shaner, L. Rei, Huang-Wei Pan, Gijs Nelemans, S. B. Coughlin, Jessica Steinlechner, A. Neunzert, F. Vetrano, R. Gray, S. Antier, E. D. Hall, Michael W. Coughlin, I. Khan, M. Heurs, Reed Essick, S. Kandhasamy, S. E. Dwyer, David Keitel, Hee-Suk Cho, Michele Zanolin, Benjamin Stappers, G. D. Meadors, S. J. Cooper, B. Sorazu, A. Kutynia, A. Lartaux-Vollard, Suvadeep Bose, R. Gouaty, Andrea Chincarini, M. K. M. Bader, T. Z. Summerscales, K. Holt, Z. Márka, S. Koley, M. Brinkmann, E. Cesarini, T. Zelenova, M. Merzougui, Riccardo Bassiri, Magnus Manske, D. Pascucci, T. J. Massinger, T. Vo, O. Chaibi, V. Kalogera, V. Sandberg, Koh Ueno, S. Frasca, E. Maros, Jonathan Richardson, S. Márka, N. Sennett, Kai Staats, L. Conti, G. D. Hammond, Javed Rana, M. Chaturvedi, Jimin George, M. Sieniawska, Martin Obergaulinger, Wynn C. G. Ho, P. Weßels, T. Dal Canton, Stephen Fairhurst, Carl Blair, K. Chakravarti, Fabio Marchesoni, S. G. Crowder, J. Bosveld, Kyungmin Kim, Debarati Chatterjee, B. O'Reilly, P. Gruning, L. Rolland, Fabrizio Barone, N. Man, K. A. Strain, Peter Aufmuth, K. Haughian, László Á. Gergely, A. Macquet, Daichi Tsuna, D. Talukder, David A. Williams, I. W. Harry, Z. A. Warden, K. Mogushi, John A. Clark, Ben Farr, P. J. King, J. T. Whelan, K. H. Lai, Aaron Viets, J. Feicht, Christophe Collette, C. J. Perez, B. D. O'Brien, O. Puncken, Joey Shapiro Key, J. R. Sanders, Marek Szczepanczyk, C. Bradaschia, Ik Siong Heng, A. Rüdiger, A. L. Miller, K. S. Karvinen, P. Astone, Mairi Sakellariadou, G. Pillant, S. H. R. Yuen, O. de Varona, Tenglin Li, I. Kowalska, D. Estevez, Marie-Anne Bizouard, Fabian Jankowski, Nergis Mavalvala, Jerome Degallaix, C. Casentini, Sebastian Khan, B. C. Barish, V. Kondrashov, Arunava Mukherjee, Y. Minenkov, P. Bacon, J. C. Bayley, H. Wittel, M. Deenadayalan, S. G. Schwalbe, M. Phelps, R. G. Ormiston, F. Cipriano, Michael Thomas, P. Popolizio, Koji Arai, E. J. Sanchez, A. G. Lyne, M. Vardaro, F. Robinet, F. Cleva, M. P. Ross, T. B. Edo, M. Pichot, Maximiliano Isi, E. M. Gretarsson, Ying Guo, D. Beniwal, Peter Fritschel, Wenxiao Wang, M. Masso-Reid, L. E. Sanchez, Enrico Calloni, G. Traylor, Thomas Corbitt, L. Salconi, C. A. Costa, Paulo C. C. Freire, Slavko Bogdanov, Laura Cadonati, D. A. Steer, L. Kleybolte, Daniel R. George, Chad Hanna, A. Bramley, C. Kimball, J. Oberling, M. Pirello, S. R.P. Mohapatra, J. Bidler, F. Nocera, C. Zhao, Kun Li, T. Zhang, Thibaut Jacqmin, C. I. Torrie, M. Saleem, Douglas Davis, Geraint Pratten, H. Fair, Andrea Taracchini, D. Bersanetti, G. Ashton, Yu Wang, Francisco Hernandez Vivanco, Eric Thrane, C. Michel, T. D. Knowles, R. Quitzow-James, V. B. Adya, Laser Interferometer Gravitational-Wave Observatory (LIGO), Louisiana State University, Baton Rouge, Inter-University Centre for Astronomy and Astrophysics (IUCAA), Università di Salerno, School of Physics, Monash University, Max Planck Institute for Gravitational Physics, University of Cambridge, University of Birmingham, Instituto Nacional de Pesquisas Espaciais (INPE), Gran Sasso Science Institute, INFN, International Centre for Theoretical Sciences, Tata Institute of Fundamental Research, Bengaluru 560089, India, NCSA, University of Illinois at Urbana-Champaign, Urbana, IL 61801, USA, Universita di Pisa, I-56127 Pisa, Italy, Universitat de València (UV), Australian National University, Laboratoire des matériaux avancés (LMA), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), University of Wisconsin-Milwaukee, Milwaukee, WI 53201, USA, Scottish Universities Physics Alliance (SUPA), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), California State University Fullerton, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), European Gravitational Observatory (EGO), Università di Roma Tor Vergata, INFN, Sezione di Roma, I-00185 Roma, Italy, Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Institut für Erdmessung, Leibniz Universität Hannover, Embry-Riddle Aeronautical University (ERAU), Montclair State University, Montclair, NJ 07043, USA, National Institute for Subatomic Physics (NIKHEF), Korea Advanced Institute of Science and Technology, Swinburne University of Technology, Department of Physics, West Virginia University (WVU), Università degli Studi di Perugia = University of Perugia (UNIPG), Syracuse University, University of Minnesota, California Institute of Technology, Department of Astronomy (CALTECH), KFKI Research Institute for Particle and Nuclear Physics (KFKI-RMKI), University of Florida, Stanford University, Istituto Nazionale di Fisica Nucleare, Sezione di Perugia (INFN), Dipartimento di Fisica e Astronomia G. Galilei, Università di Padova, Department of Physics, Montana State University, Centrum Astronomiczne im. M. Kopernika, Warszawa (CAMK), University of Adelaide, Friedrich-Schiller-Universität Jena, Rochester Institute of Technology, Center for Interdisciplinary Exploration and Research in Astrophysics, Department of Physics and Astronomy, Northwestern University, Istituto Nazionale di Fisica Nucleare, Sezione di Genova (INFN), RRCAT, Indore, Madhya Pradesh 452013, India, Faculty of Physics, M.V. Lomonosov Moscow State University, Istituto Nazionale di Fisica Nucleare, Sezione di Pisa (INFN), The University of Western Australia (UWA), Institute for Mathematics, Astrophysics, and Particle Physics, Department of Astrophysics, Radboud University (IMAPP), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Physik-Institut, Universität Zürich, Centre National de la Recherche Scientifique (CNRS), Cardiff University, Department of Physics, University of Oregon, Laboratoire Kastler Brossel (LKB (Jussieu)), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Urbino 'Carlo Bo', Astronomical Observatory, Warsaw University, Center for Relativistic Astrophysics, School of Physics, Georgia Institute of Technology, Université de Lyon, Istituto Nazionale di Fisica Nucleare, Sezione di Napoli (INFN), NASA/Goddard Space Flight Center (NASA/GSFC), University of Tokyo, Tsinghua University, Texas Tech University, Lubbock, TX 79409, USA, University of Mississippi, Istituto Nazionale di Fisica Nucleare, Sezione di Roma Tor Vergata (INFN), The Pennsylvania State University, University Park, PA 16802, USA, University of New South Wales, University of Chicago, Department of Physics, University of Hong Kong, Department of Physics and Astronomy, Seoul National University, Pusan National University, University of Maryland, Carleton College, Northfield, INAF, Osservatorio Astronomico di Padova, I-35122 Padova, Italy, School of Physics, University of Melbourne, Columbia University, New York, Department de Física, Universitat de les Illes Balears, Université Libre de Bruxelles, Department of Physics and Astronomy, Sonoma State University, Istituto Nazionale di Fisica Nucleare, Sezione di Padova (INFN), Departamento de Matematicas, Universitat de Valencia, E-46100 Burjassot, Valencia, Spain, University of Rhode Island, Kingston, RI 02881, USA, The University of Texas Rio Grande Valley, Brownsville, TX 78520, USA, Bellevue College, Bellevue, WA 98007, USA, Eötvös Loránd University (ELTE), Raman Research Institute, Duke University [Durham], INFN, Sezione di Milano Bicocca, Gruppo Collegato di Parma, I-43124 Parma, Italy, California State University, San Bernardino, INFN, Trento Institute for Fundamental Physics and Applications, I-38123 Povo, Trento, Italy, Colorado State University, Fort Collins, Kenyon College, Gambier, OH 43022, USA, National Astronomical Observatory of Japan (NAOJ), Canadian Institute for Theoretical Astrophysics, McLennan Physical Laboratories, University of Toronto (CITA), University of Edinburgh, Indian Institute of Technology, University of Szeged [Szeged], Tata Institute of Fundamental Research (TIFR), University of Michigan, Washington State University, Washington University in Saint Louis (WUSTL), Department of Physics and Astronomy, University of Missouri, Directorate of Construction, Services & Estate Management, Mumbai 400094, India, Bialystok University, Physics Department, King's College London, Strand, University of Southampton, Institute of Applied Physics, Ewha Womans University, Inje University Gimhae, South Gyeongsang 50834, Republic of Korea, National Institute for Mathematical Sciences, Daejeon 34047, Republic of Korea, Institut für Theoretische Physik, Universität Hamburg, Chennai Mathematical Institute, National Centre for Nuclear Research (NCBJ), Center for Radiophysics and Space Research, Cornell University (CRSR), Hillsdale College, Hillsdale, MI 49242, USA, Korea Astronomy and Space Science Institute (KASI), Marshall Space Flight Center, NASA, Dipartimento di Matematica e Fisica, Università del Salento, Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL), University of Portsmouth, Portsmouth, PO1 3FX, UK, Southern University and A& M College, Baton Rouge, LA 70813, USA, College of William and Mary, Williamsburg, Centre Scientifique de Monaco, 8 quai Antoine Ier, MC-98000, Monaco, Museo Storico della Fisica e Centro Studi e Ricerche ?Enrico Fermi,? I-00184 Roma, Italyrico Fermi, I-00184 Roma, Italy, Institut des Hautes Études Scientifiques (IHES), IHES, Department of Physics, University of North Bengal, Illinois College, Institute of Mathematics, Polish Academy of Sciences, Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Hobart and William Smith Colleges, University of Washington [Seattle], Laboratoire d'Astrophysique Expérimentale (LAE), Observatoire du Mont Mégantic, Departamento de Física, Universidade Federal do Rio Grande do Norte, Department of Astronomy and Astrophysics, Villanova University, Andrews University, Albert-Einstein-Institut, Trinity University, San Antonio, TX 78212, USA, X-Ray Astrophysics Laboratory, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA, Columbia Astrophysics Laboratory, Columbia University, New York, Unité Scientifique de la Station de Nançay (USN), 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 d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Osservatorio Astronomico di Cagliari, Astrochemistry Group (INAF), Hakubi Center, Max-Planck-Institut für Radioastronomie at Effelsberg, CRESST/NASA GSFC, Astrophysics Science Division, Jodrell Bank Centre for Astrophysics (JBCA), Space Science Division (NRL-SSD), Department of Physical Sciences, University of Tasmania, Private Bag 37, Hobart, Tasmania 7001, Australia, 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 Cité (UPCité), Abbott, Bp, Abbott, R, Abbott, Td, Abraham, S, Acernese, F, Ackley, K, Adams, C, Adhikari, Rx, Adya, Vb, Affeldt, C, Agathos, M, Agatsuma, K, Aggarwal, N, Aguiar, Od, Aiello, L, Ain, A, Ajith, P, Allen, G, Allocca, A, Aloy, Ma, Altin, Pa, Amato, A, Anand, S, Ananyeva, A, Anderson, Sb, Anderson, Wg, Angelova, Sv, Antier, S, Appert, S, Arai, K, Araya, Mc, Areeda, J, Arene, M, Arnaud, N, Aronson, Sm, Ascenzi, S, Ashton, G, Aston, Sm, Astone, P, Aubin, F, Aufmuth, P, Aultoneal, K, Austin, C, Avendano, V, Avila-Alvarez, A, Babak, S, Bacon, P, Badaracco, F, Bader, Mkm, Bae, S, Baird, J, Baker, Pt, Baldaccini, F, Ballardin, G, Ballmer, Sw, Bals, A, Banagiri, S, Barayoga, Jc, Barbieri, C, Barclay, Se, Barish, Bc, Barker, D, Barkett, K, Barnum, S, Barone, F, Barr, B, Barsotti, L, Barsuglia, M, Barta, D, Bartlett, J, Bartos, I, Bassiri, R, Basti, A, Bawaj, M, Bayley, Jc, Bazzan, M, Becsy, B, Bejger, M, Belahcene, I, Bell, A, Beniwal, D, Benjamin, Mg, Berger, Bk, Bergmann, G, Bernuzzi, S, Berry, Cpl, Bersanetti, D, Bertolini, A, Betzwieser, J, Bhandare, R, Bidler, J, Biggs, E, Bilenko, Ia, Bilgili, Sa, Billingsley, G, Birney, R, Birnholtz, O, Biscans, S, Bischi, M, Biscoveanu, S, Bisht, A, Bitossi, M, Bizouard, Ma, Blackburn, Jk, Blackman, J, Blair, Cd, Blair, Dg, Blair, Rm, Bloemen, S, Bobba, F, Bode, N, Boer, M, Boetzel, Y, Bogaert, G, Bondu, F, Bonnand, R, Booker, P, Boom, Ba, Bork, R, Boschi, V, Bose, S, Bossilkov, V, Bosveld, J, Bouffanais, Y, Bozzi, A, Bradaschia, C, Brady, Pr, Bramley, A, Branchesi, M, Brau, Je, Breschi, M, Briant, T, Briggs, Jh, Brighenti, F, Brillet, A, Brinkmann, M, Brockill, P, Brooks, Af, Brooks, J, Brown, Dd, Brunett, S, Buikema, A, Bulik, T, Bulten, Hj, Buonanno, A, Buskulic, D, Buy, C, Byer, Rl, Cabero, M, Cadonati, L, Cagnoli, G, Cahillane, C, Bustillo, Jc, Callister, Ta, Calloni, E, Camp, Jb, Campbell, Wa, Cannon, Kc, Cao, H, Cao, J, Carapella, G, Carbognani, F, Caride, S, Carney, Mf, Carullo, G, Diaz, Jc, Casentini, C, Caudill, S, Cavaglia, M, Cavalier, F, Cavalieri, R, Cella, G, Cerda-Duran, P, Cesarini, E, Chaibi, O, Chakravarti, K, Chamberlin, Sj, Chan, M, Chao, S, Charlton, P, Chase, Ea, Chassande-Mottin, E, Chatterjee, D, Chaturvedi, M, Cheeseboro, Bd, Chen, Hy, Chen, X, Chen, Y, Cheng, Hp, Cheong, Ck, Chia, Hy, Chiadini, F, Chincarini, A, Chiummo, A, Cho, G, Cho, H, Cho, M, Christensen, N, Chu, Q, Chua, S, Chung, Kw, Chung, S, Ciani, G, Cieslar, M, Ciobanu, Aa, Ciolfi, R, Cipriano, F, Cirone, A, Clara, F, Clark, Ja, Clearwater, P, Cleva, F, Coccia, E, Cohadon, Pf, Cohen, D, Colleoni, M, Collette, Cg, Collins, C, Colpi, M, Cominsky, Lr, Constancio, M, Conti, L, Cooper, Sj, Corban, P, Corbitt, Tr, Cordero-Carrion, I, Corezzi, S, Corley, Kr, Cornish, N, Corre, D, Corsi, A, Cortese, S, Costa, Ca, Cotesta, R, Coughlin, Mw, Coughlin, Sb, Coulon, Jp, Countryman, St, Couvares, P, Covas, Pb, Cowan, Ee, Coward, Dm, Cowart, Mj, Coyne, Dc, Coyne, R, Creighton, Jde, Creighton, Td, Cripe, J, Croquette, M, Crowder, Sg, Cullen, Tj, Cumming, A, Cunningham, L, Cuoco, E, Dal Canton, T, Dalya, G, D'Angelo, B, Danilishin, Sl, D'Antonio, S, Danzmann, K, Dasgupta, A, Costa, Cfd, Datrier, Leh, Dattilo, V, Dave, I, Davier, M, Davis, D, Daw, Ej, Debra, D, Deenadayalan, M, Degallaix, J, De Laurentis, M, Deleglise, S, Del Pozzo, W, Demarchi, Lm, Demos, N, Dent, T, De Pietri, R, De Rosa, R, De Rossi, C, Desalvo, R, de Varona, O, Dhurandhar, S, Diaz, Mc, Dietrich, T, Di Fiore, L, Difronzo, C, Di Giorgio, C, Di Giovanni, F, Di Giovanni, M, Di Girolamo, T, Di Lieto, A, Ding, B, Di Pace, S, Di Palma, I, Di Renzo, F, Divakarla, Ak, Dmitriev, A, Doctor, Z, Donovan, F, Dooley, Kl, Doravari, S, Dorrington, I, Downes, Tp, Drago, M, Driggers, Jc, Du, Z, Ducoin, Jg, Dupej, P, Durante, O, Dwyer, Se, Easter, Pj, Eddolls, G, Edo, Tb, Effler, A, Ehrens, P, Eichholz, J, Eikenberry, S, Eisenmann, M, Eisenstein, Ra, Errico, L, Essick, Rc, Estelles, H, Estevez, D, Etienne, Zb, Etzel, T, Evans, M, Evans, Tm, Fafone, V, Fairhurst, S, Fan, X, Farinon, S, Farr, B, Farr, Wm, Fauchon-Jones, Ej, Favata, M, Fays, M, Fazio, M, Fee, C, Feicht, J, Fejer, Mm, Feng, F, Fernandez-Galiana, A, Ferrante, I, Ferreira, Ec, Ferreira, Ta, Fidecaro, F, Fiori, I, Fiorucci, D, Fishbach, M, Fisher, Rp, Fishner, Jm, Fittipaldi, R, Fitz-Axen, M, Fiumara, V, Flaminio, R, Fletcher, M, Floden, E, Flynn, E, Fong, H, Font, Ja, Forsyth, Pwf, Fournier, Jd, Vivanco, Fh, Frasca, S, Frasconi, F, Frei, Z, Freise, A, Frey, R, Frey, V, Fritschel, P, Frolov, Vv, Fronze, G, Fulda, P, Fyffe, M, Gabbard, Ha, Gadre, Bu, Gaebel, Sm, Gair, Jr, Gammaitoni, L, Gaonkar, Sg, Garcia-Quiros, C, Garufi, F, Gateley, B, Gaudio, S, Gaur, G, Gayathri, V, Gemme, G, Genin, E, Gennai, A, George, D, George, J, Gergely, L, Ghonge, S, Ghosh, A, Ghosh, S, Giacomazzo, B, Giaime, Ja, Giardina, Kd, Gibson, Dr, Gill, K, Glover, L, Gniesmer, J, Godwin, P, Goetz, E, Goetz, R, Goncharov, B, Gonzalez, G, Castro, Jmg, Gopakumar, A, Gossan, Se, Gosselin, M, Gouaty, R, Grace, B, Grado, A, Granata, M, Grant, A, Gras, S, Grassia, P, Gray, C, Gray, R, Greco, G, Green, Ac, Green, R, Gretarsson, Em, Grimaldi, A, Grimm, Sj, Groot, P, Grote, H, Grunewald, S, Gruning, P, Guidi, Gm, Gulati, Hk, Guo, Y, Gupta, A, Gupta, P, Gustafson, Ek, Gustafson, R, Haegel, L, Halim, O, Hall, Br, Hall, Ed, Hamilton, Ez, Hammond, G, Haney, M, Hanke, Mm, Hanks, J, Hanna, C, Hannuksela, Oa, Hansen, Tj, Hanson, J, Harder, T, Hardwick, T, Haris, K, Harms, J, Harry, Gm, Harry, Iw, Hasskew, Rk, Haster, Cj, Haughian, K, Hayes, Fj, Healy, J, Heidmann, A, Heintze, Mc, Heitmann, H, Hellman, F, Hello, P, Hemming, G, Hendry, M, Heng, I, Hennig, J, Heurs, M, Hild, S, Hinderer, T, Hochheim, S, Hofman, D, Holgado, Am, Holland, Na, Holt, K, Holz, De, Hopkins, P, Horst, C, Hough, J, Howell, Ej, Hoy, Cg, Huang, Y, Hubner, Mt, Huerta, Ea, Huet, D, Hughey, B, Hui, V, Husa, S, Huttner, Sh, Huynh-Dinh, T, Idzkowski, B, Iess, A, Inchauspe, H, Ingram, C, Inta, R, Intini, G, Irwin, B, Isa, Hn, Isac, Jm, Isi, M, Iyer, Br, Jacqmin, T, Jadhav, Sj, Jani, K, Janthalur, Nn, Jaranowski, P, Jariwala, D, Jenkins, Ac, Jiang, J, Johnson, D, Jones, Aw, Jones, Di, Jones, Jd, Jones, R, Jonker, Rjg, Ju, L, Junker, J, Kalaghatgi, Cv, Kalogera, V, Kamai, B, Kandhasamy, S, Kang, G, Kanner, Jb, Kapadia, Sj, Karki, S, Kashyap, R, Kasprzack, M, Katsanevas, S, Katsavounidis, E, Katzman, W, Kaufer, S, Kawabe, K, Keerthana, Nv, Kefelian, F, Keitel, D, Kennedy, R, Key, J, Khalili, Fy, Khan, I, Khan, S, Khazanov, Ea, Khetan, N, Khursheed, M, Kijbunchoo, N, Kim, C, Kim, Jc, Kim, K, Kim, W, Kim, Ym, Kimball, C, King, Pj, Kinley-Hanlon, M, Kirchhoff, R, Kissel, J, Kleybolte, L, Klika, Jh, Klimenko, S, Knowles, Td, Koch, P, Koehlenbeck, Sm, Koekoek, G, Koley, S, Kondrashov, V, Kontos, A, Koper, N, Korobko, M, Korth, Wz, Kovalam, M, Kozak, Db, Kramer, C, Kringel, V, Krishnendu, N, Krolak, A, Krupinski, N, Kuehn, G, Kumar, A, Kumar, P, Kumar, R, Kuo, L, Kutynia, A, Kwang, S, Lackey, Bd, Laghi, D, Lai, Kh, Lam, Tl, Landry, M, Lane, Bb, Lang, Rn, Lange, J, Lantz, B, Lanza, Rk, Lartaux-Vollard, A, Lasky, Pd, Laxen, M, Lazzarini, A, Lazzaro, C, Leaci, P, Leavey, S, Lecoeuche, K, Lee, Ch, Lee, Hk, Lee, Hm, Lee, Hw, Lee, J, Lee, K, Lehmann, J, Lenon, Ak, Leroy, N, Letendre, N, Levin, Y, Li, A, Li, J, Li, Kjl, Li, Tgf, Li, X, Lin, F, Linde, F, Linker, Sd, Littenberg, Tb, Liu, J, Liu, X, Llorens-Monteagudo, M, Lo, Rkl, London, Lt, Longo, A, Lorenzini, M, Loriette, V, Lormand, M, Losurdo, G, Lough, Jd, Lousto, Co, Lovelace, G, Lower, Me, Luck, H, Lumaca, D, Lundgren, Ap, Lynch, R, Ma, Y, Macas, R, Macfoy, S, Macinnis, M, Macleod, Dm, Macquet, A, Hernandez, Im, Magana-Sandoval, F, Magee, Rm, Majorana, E, Maksimovic, I, Malik, A, Man, N, Mandic, V, Mangano, V, Mansell, Gl, Manske, M, Mantovani, M, Mapelli, M, Marchesoni, F, Marion, F, Marka, S, Marka, Z, Markakis, C, Markosyan, A, Markowitz, A, Maros, E, Marquina, A, Marsat, S, Martelli, F, Martin, Iw, Martin, Rm, Martinez, V, Martynov, Dv, Masalehdan, H, Mason, K, Massera, E, Masserot, A, Massinger, Tj, Masso-Reid, M, Mastrogiovanni, S, Matas, A, Matichard, F, Matone, L, Mavalvala, N, Mccann, Jj, Mccarthy, R, Mcclelland, De, Mccormick, S, Mcculler, L, Mcguire, Sc, Mcisaac, C, Mciver, J, Mcmanus, Dj, Mcrae, T, Mcwilliams, St, Meacher, D, Meadors, Gd, Mehmet, M, Mehta, Ak, Meidam, J, Villa, Em, Melatos, A, Mendell, G, Mercer, Ra, Mereni, L, Merfeld, K, Merilh, El, Merzougui, M, Meshkov, S, Messenger, C, Messick, C, Messina, F, Metzdorff, R, Meyers, Pm, Meylahn, F, Miani, A, Miao, H, Michel, C, Middleton, H, Milano, L, Miller, L, Millhouse, M, Mills, Jc, Milovich-Goff, Mc, Minazzoli, O, Minenkov, Y, Mishkin, A, Mishra, C, Mistry, T, Mitra, S, Mitrofanov, Vp, Mitselmakher, G, Mittleman, R, Mo, G, Moffa, D, Mogushi, K, Mohapatra, Srp, Molina-Ruiz, M, Mondin, M, Montani, M, Moore, Cj, Moraru, D, Morawski, F, Moreno, G, Morisaki, S, Mours, B, Mow-Lowry, M, Muciaccia, F, Mukherjee, A, Mukherjee, D, Mukherjee, S, Mukund, N, Mullavey, A, Munch, J, Muniz, Ea, Muratore, M, Murray, Pg, Nagar, A, Nardecchia, I, Naticchioni, L, Nayak, Rk, Neil, Bf, Neilson, J, Nelemans, G, Nelson, Tjn, Nery, M, Neunzert, A, Nevin, L, Ng, Ky, Ng, S, Nguyen, C, Nguyen, P, Nichols, D, Nichols, Sa, Nissanke, S, Nocera, F, North, C, Nuttall, Lk, Obergaulinger, M, Oberling, J, O'Brien, Bd, Oganesyan, G, Ogin, Gh, Oh, Jj, Oh, Sh, Ohme, F, Ohta, H, Okada, Ma, Oliver, M, Oppermann, P, Oram, Rj, O'Reilly, B, Ormiston, Rg, Ortega, Lf, O'Shaughnessy, R, Ossokine, S, Ottaway, Dj, Overmier, H, Owen, Bj, Pace, Ae, Pagano, G, Page, Ma, Pagliaroli, G, Pai, A, Pai, Sa, Palamos, Jr, Palashov, O, Palomba, C, Pan, H, Panda, Pk, Pang, Pth, Pankow, C, Pannarale, F, Pant, Bc, Paoletti, F, Paoli, A, Parida, A, Parker, W, Pascucci, D, Pasqualetti, A, Passaquieti, R, Passuello, D, Patil, M, Patricelli, B, Payne, E, Pearlstone, Bl, Pechsiri, Tc, Pedersen, Aj, Pedraza, M, Pedurand, R, Pele, A, Penn, S, Perego, A, Perez, Cj, Perigois, C, Perreca, A, Petermann, J, Pfeiffer, Hp, Phelps, M, Phukon, K, Piccinni, Oj, Pichot, M, Piergiovanni, F, Pierro, V, Pillant, G, Pinard, L, Pinto, Im, Pirello, M, Pitkin, M, Plastino, W, Pong, Dyt, Ponrathnam, S, Popolizio, P, Porter, Ek, Powell, J, Prajapati, Ak, Prasad, J, Prasai, K, Prasanna, R, Pratten, G, Prestegard, T, Principe, M, Prodi, Ga, Prokhorov, L, Punturo, M, Puppo, P, Purrer, M, Qi, H, Quetschke, V, Quinonez, Pj, Raab, Fj, Raaijmakers, G, Radkins, H, Radulesco, N, Raffai, P, Raja, S, Rajan, C, Rajbhandari, B, Rakhmanov, M, Ramirez, Ke, Ramos-Buades, A, Rana, J, Rao, K, Rapagnani, P, Raymond, V, Razzano, M, Read, J, Regimbau, T, Rei, L, Reid, S, Reitze, Dh, Rettegno, P, Ricci, F, Richardson, Cj, Richardson, Jw, Ricker, Pm, Riemenschneider, G, Riles, K, Rizzo, M, Robertson, Na, Robinet, F, Rocchi, A, Rolland, L, Rollins, Jg, Roma, Vj, Romanelli, M, Romano, R, Romel, Cl, Romie, Jh, Rose, Ca, Rose, D, Rose, K, Rosinska, D, Rosofsky, Sg, Ross, Mp, Rowan, S, Rudiger, A, Ruggi, P, Rutins, G, Ryan, K, Sachdev, S, Sadecki, T, Sakellariadou, M, Salafia, O, Salconi, L, Saleem, M, Samajdar, A, Sammut, L, Sanchez, Ej, Sanchez, Le, Sanchis-Gual, N, Sanders, Jr, Santiago, Ka, Santos, E, Sarin, N, Sassolas, B, Saulson, Pr, Sauter, O, Savage, Rl, Schale, P, Scheel, M, Scheuer, J, Schmidt, P, Schnabel, R, Schofield, Rm, Schonbeck, A, Schreiber, E, Schulte, Bw, Schutz, Bf, Scott, J, Scott, Sm, Seidel, E, Sellers, D, Sengupta, A, Sennett, N, Sentenac, D, Sequino, V, Sergeev, A, Setyawati, Y, Shaddock, Da, Shaffer, T, Shahriar, M, Shaner, Mb, Sharma, A, Sharma, P, Shawhan, P, Shen, H, Shink, R, Shoemaker, Dh, Shoemaker, Dm, Shukla, K, Shyamsundar, S, Siellez, K, Sieniawska, M, Sigg, D, Singer, Lp, Singh, D, Singh, N, Singhal, A, Sintes, Am, Sitmukhambetov, S, Skliris, V, Slagmolen, Bjj, Slaven-Blair, Tj, Smith, Jr, Smith, Rje, Somala, S, Son, Ej, Soni, S, Sorazu, B, Sorrentino, F, Souradeep, T, Sowell, E, Spencer, Ap, Spera, M, Srivastava, Ak, Srivastava, V, Staats, K, Stachie, C, Standke, M, Steer, Da, Steinke, M, Steinlechner, J, Steinlechner, S, Steinmeyer, D, Stevenson, Sp, Stocks, D, Stone, R, Stops, Dj, Strain, Ka, Stratta, G, Strigin, Se, Strunk, A, Sturani, R, Stuver, Al, Sudhir, V, Summerscales, Tz, Sun, L, Sunil, S, Sur, A, Suresh, J, Sutton, Pj, Swinkels, Bl, Szczepanczyk, Mj, Tacca, M, Tait, Sc, Talbot, C, Tanner, Db, Tao, D, Tapai, M, Tapia, A, Tasson, Jd, Taylor, R, Tenorio, R, Terkowski, L, Thomas, M, Thomas, P, Thondapu, Sr, Thorne, Ka, Thrane, E, Tiwari, S, Tiwari, V, Toland, K, Tonelli, M, Tornasi, Z, Torres-Forne, A, Torrie, Ci, Toyra, D, Travasso, F, Traylor, G, Tringali, Mc, Tripathee, A, Trovato, A, Trozzo, L, Tsang, Kw, Tse, M, Tso, R, Tsukada, L, Tsuna, D, Tsutsui, T, Tuyenbayev, D, Ueno, K, Ugolini, D, Unnikrishnan, C, Urban, Al, Usman, Sa, Vahlbruch, H, Vajente, G, Valdes, G, Valentini, M, van Bakel, N, van Beuzekom, M, van den Brand, Jfj, Van Den Broeck, C, Vander-Hyde, Dc, van der Schaaf, L, Vanheijningen, Jv, van Veggel, Aa, Vardaro, M, Varma, V, Vass, S, Vasuth, M, Vecchio, A, Vedovato, G, Veitch, J, Veitch, Pj, Venkateswara, K, Venugopalan, G, Verkindt, D, Vetrano, F, Vicere, A, Viets, Ad, Vinciguerra, S, Vine, Dj, Vinet, Jy, Vitale, S, Vo, T, Vocca, H, Vorvick, C, Vyatchanin, Sp, Wade, Ar, Wade, Le, Wade, M, Walet, R, Walker, M, Wallace, L, Walsh, S, Wang, H, Wang, Jz, Wang, S, Wang, Wh, Wang, Yf, Ward, Rl, Warden, Za, Warner, J, Was, M, Watchi, J, Weaver, B, Wei, Lw, Weinert, M, Weinstein, Aj, Weiss, R, Wellmann, F, Wen, L, Wessel, K, Wessels, P, Westhouse, Jw, Wette, K, Whelan, Jt, Whiting, Bf, Whittle, C, Wilken, Dm, Williams, D, Williamson, Ar, Willis, Jl, Willke, B, Winkler, W, Wipf, Cc, Wittel, H, Woan, G, Woehler, J, Wofford, Jk, Wright, Jl, Wu, D, Wysocki, Dm, Xiao, S, Xu, R, Yamamoto, H, Yancey, Cc, Yang, L, Yang, Y, Yang, Z, Yap, Mj, Yazback, M, Yeeles, Dw, Yu, H, Yu, Hc, Yuen, Shr, Zadrozny, Ak, Zadrozny, A, Zanolin, M, Zelenova, T, Zendri, Jp, Zevin, M, Zhang, J, Zhang, L, Zhang, T, Zhao, C, Zhao, G, Zhou, M, Zhou, Z, Zhu, Xj, Zimmerman, Ab, Zucker, Me, Zweizig, J, (Astro)-Particles Physics, Arzoumanian, Z, Bogdanov, S, Cognard, I, Corongiu, A, Enoto, T, Freire, P, Gendreau, Kc, Guillemot, L, Harding, Ak, Jankowski, F, Keith, Mj, Kerr, M, Lyne, A, Palfreyman, J, Possenti, A, Ridolfi, A, Stappers, B, Theureau, G, Weltervrede, P, Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Institut 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)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon, Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), 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 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)
Subjects: Known Pulsars, 010504 meteorology & atmospheric sciences, Astronomy, Astrophysics, Table (information), Vela, gravitational waves, pulsars, 01 natural sciences, Pulsar, 0103 physical sciences, Limit (mathematics), 010303 astronomy & astrophysics, gravitational wave, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Physics, [PHYS]Physics [physics], Gravitational wave, Two Harmonics, Astronomy and Astrophysics, Gravitational Waves, Known Pulsars, Two Harmonics, Erratum, LIGO, Amplitude, Space and Planetary Science, Erratum, Glitch (astronomy), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: Two analysis errors have been identified that affect the results for a handful of the high-value pulsars given in Table 1 of Abbott et al. (2019). One affects the Bayesian analysis for the five pulsars that glitched during the analysis period, and the other affects the 5n-vector analysis for J0711-6830. Updated results after correcting the errors are shown in Table 1, which now supersedes the results given for those pulsars in Table 1 of Abbott et al. (2019). Updated versions of figures can be seen in Figures 1-4. Bayesian analysis.-For the glitching pulsars, the signal phase evolution caused by the glitch was wrongly applied twice and was therefore not consistent with our expected model of the pulsar phase. This error did not affect the F/G-statistic or 5n-vector analysis. Analyses of the five pulsars PSR J0205+6449, PSR J0534+2200, PSR J0835-4510, PSR J1028-5819, and PSR J1718-3825 have been repeated after correcting for the error. There are small quantitative differences in the results, but the changes do not affect the main conclusions of the paper. The largest differences are for PSR J0835-4510 (the Vela pulsar), for which the updated upper limits from the Bayesian method are found to be between 1.1 and 2 times larger than those obtained when the error was present. This appears primarily to be due to the error leading to the decohering of a strong spectral line in the LIGO Livingston detector and thus lowering the amplitude limit. 5n-vector analysis.-An error was also identified in the settings of the 5n-vector analysis, which affected the upper limit computation at the rotation frequency for C21 95% of J0711-6830. Specifically, we found an incorrect choice for the range of amplitudes used to inject simulated signals in the O2 data. The updated upper limit is about 2.5 times worse than that obtained when the error was present. This error did not affect the Bayesian or F/G-statistic results. (Table Presented) (Figure Presented).
Published: 2020

3. The LOFAR Tied-Array All-Sky Survey (LOTAAS): Characterization of 20 pulsar discoveries and their single-pulse behavior

Author: V. I. Kondratiev, Benjamin Stappers, S. Sanidas, C. G. Bassa, Jean-Mathias Grießmeier, Daniele Michilli, C. M. Tan, Joris P. W. Verbiest, Patrick Weltevrede, S. Cooper, Jason W. T. Hessels, J. van Leeuwen, Ismaël Cognard, A. G. Lyne, High Energy Astrophys. & Astropart. Phys (API, FNWI), Netherlands Institute for Radio Astronomy (ASTRON), McGill University = Université McGill [Montréal, Canada], Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Jodrell Bank Centre for Astrophysics (JBCA), University of Manchester [Manchester], P. N. Lebedev Physical Institute of the Russian Academy of Sciences [Moscow] (LPI RAS), Russian Academy of Sciences [Moscow] (RAS), 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), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Universität Bielefeld, Max-Planck-Institut für Radioastronomie (MPIFR), The Nançay Radio Observatory is operated by the Paris Observatory, associated with the French Centre National de la Recherche Scientifique(CNRS) and Université d’Orléans., European Project: 337062,EC:FP7:ERC,ERC-2013-StG,DRAGNET(2014), European Project: 617199,EC:FP7:ERC,ERC-2013-CoG,ALERT(2014), 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: media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, observational [methods], FOS: Physical sciences, Flux, Ephemerides, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Ephemeris, general [pulsars], 01 natural sciences, law.invention, Radio telescope, Rotating radio transient, Telescope, Pulsar, law, pulsars: general, 0103 physical sciences, ephemerides, 010303 astronomy & astrophysics, media_common, [PHYS]Physics [physics], High Energy Astrophysical Phenomena (astro-ph.HE), Physics, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, LOFAR, Space and Planetary Science, Sky, methods: observational, Astrophysics - High Energy Astrophysical Phenomena
Abstract: We are using the LOw-Frequency ARray (LOFAR) to perform the LOFAR Tied-Array All-Sky (LOTAAS) survey for pulsars and fast transients. Here, we present the astrometric and rotational parameters of 20 pulsars discovered as part of LOTAAS. These pulsars have regularly been observed with LOFAR at 149 MHz and the Lovell telescope at 1532 MHz, supplemented by some observations with the Lovell telescope at 334 MHz and the Nançay Radio Telescope at 1484 MHz. Timing models are calculated for the 20 pulsars, some of which are among the slowest spinning pulsars known. PSR J1236 − 0159 rotates with a period P ∼ 3.6 s, while five additional pulsars show P > 2 s. Also, the spin-down rates P˙P˙ are, on average, low, with PSR J0815 + 4611 showing P˙∼4×10−18. Some of the pulse profiles, generically single-peaked, present complex shapes evolving with frequency. Multifrequency flux measurements show that these pulsars have generically relatively steep spectra but exceptions are present, with values ranging between ∼−4 and −1. Among the pulsar sample, a large fraction shows large single-pulse variability, with four pulsars being undetectable more than 15 per cent15 per cent of the time and one tentatively classified as a Rotating Radio Transient. Two single-peaked pulsars show drifting sub-pulses.
Published: 2020

4. Rotating Radio Transients: new discoveries, timing solutions and musings

Author: Maura McLaughlin, Michael Kramer, Evan Keane, A. G. Lyne, and Benjamin Stappers
Subjects: Physics, education.field_of_study, Field (physics), Astrophysics::High Energy Astrophysical Phenomena, Population, Astronomy and Astrophysics, Astrometry, Astrophysics, Parameter space, Rotating radio transient, Neutron star, Pulsar, Space and Planetary Science, education
Abstract: We describe observations of Rotating RAdio Transients (RRATs) that were discovered in a re-analysis of the Parkes Multi-beam Pulsar Survey (PMPS). The sources have now been monitored for sufficiently long to obtain seven new coherent timing solutions, to make a total of 14 now known. Furthermore we announce the discovery of 7 new transient sources, one of which may be extragalactic in origin (with $z\sim0.1$) and would then be a second example of the so-called `Lorimer burst'. The timing solutions allow us to infer neutron star characteristics such as energy-loss rate, magnetic field strength and evolutionary timescales, as well as facilitating multi-wavelength followup by providing accurate astrometry. All of this enables us to consider the question of whether or not RRATs are in any way special, i.e. a distinct and separate population of neutron stars, as has been previously suggested. We see no reason to consider 'RRAT' as anything other than a detection label, the subject of a selection effect in the parameter space searched. However, single-pulse searches can be utilised to great effect to identify pulsars difficult, or impossible, to find by other means, in particular those with long-periods (half of the PMPS RRATs have periods greater than 4 seconds), high-magnetic field strengths ($B\gtrsim 10^{13}$ G) and pulsars approaching the 'death valley'. The detailed nulling properties of such pulsars are unknown but the mounting evidence suggests a broad range of behaviour in the pulsar population. The group of RRATs fit in to the picture where pulsar magnetospheres switch between stable configurations.
Published: 2011

5. OBSERVATIONS AND MODELING OF RELATIVISTIC SPIN PRECESSION IN PSR J1141–6545

Author: M. Burgay, Michael Kramer, George Hobbs, John Reynolds, W. van Straten, A. G. Lyne, I. H. Stairs, R. N. Manchester, Maura McLaughlin, Fernando Camilo, Christie A. McPhee, D. R. Lorimer, and A. Possenti
Subjects: Physics, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Position angle, Polarization (waves), Astrophysics - Astrophysics of Galaxies, 01 natural sciences, Binary pulsar, Radio telescope, Recoil, Pulsar, Space and Planetary Science, Total angular momentum quantum number, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, 010306 general physics, 010303 astronomy & astrophysics, Circular polarization
Abstract: Observations of the binary pulsar PSR J1141-6545 using the Parkes radio telescope over 9.3 years show clear time-variations in pulse width, shape and polarization. We interpret these variations in terms of relativistic precession of the pulsar spin axis about the total angular momentum vector of the system. Over the nine years, the pulse width at the 50% level has changed by more than a factor of three. Large variations have also been observed in the 1400-MHz mean flux density. The pulse polarization has been monitored since 2004 April using digital filterbank systems and also shows large and systematic variations in both linear and circular polarization. Position angle variations, both across the pulse profile and over the data span, are complex, with major differences between the central and outer parts of the pulse profile. Modelling of the observed position angle variations by relativistic precession of the pulsar spin axis shows that the spin-orbit misalignment angle is about 110 deg and that the precessional phase has passed through 180 deg during the course of our observations. At the start of our observations, the line-of-sight impact parameter was about 4 deg in magnitude and it reached a minimum very close to 0 deg around early 2007, consistent with the observed pulse width variations. We have therefore mapped approximately one half of the emission beam, showing that it is very asymmetric with respect to the magnetic axis. The derived precessional parameters imply that the pre-supernova star had a mass of about 2 Msun and that the supernova recoil kick velocity was relatively small. With the reversal in the rate of change of the impact parameter, we predict that over the next decade we will see a reversed "replay" of the variations observed in the past decade., 45 pages, 19 figures, 6 tables, accepted by Astrophysical Journal
Published: 2010

6. Simultaneous multifrequency single-pulse properties of AXP XTE J1810-197

Author: Christine Jordan, K. Lazaridis, Benjamin Stappers, M. Serylak, Axel Jessner, Patrick Weltevrede, J. A. Zensus, A. G. Lyne, and Michael Kramer
Subjects: Physics, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Phase (waves), Single pulse, Modulation index, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Magnetar, Intensity (physics), Pulse (physics), Radio telescope, Pulsar, Space and Planetary Science, Astrophysics::Galaxy Astrophysics
Abstract: We have used the 76-m Lovell, 94-m equivalent WSRT and 100-m Effelsberg radio telescopes to investigate the simultaneous single-pulse properties of the radio emitting magnetar AXP XTE J1810-197 at frequencies of 1.4, 4.8 and 8.35 GHz during May and July 2006. We study the magnetar's pulse-energy distributions which are found to be very peculiar as they are changing on time-scales of days and cannot be fit by a single statistical model. The magnetar exhibits strong spiky single giant-pulse-like subpulses, but they do not fit the definition of the giant pulse or giant micropulse phenomena. Measurements of the longitude-resolved modulation index reveal a high degree of intensity fluctuations on day-to-day time-scales and dramatic changes across pulse phase. We find the frequency evolution of the modulation index values differs significantly from what is observed in normal radio pulsars. We find that no regular drifting subpulse phenomenon is present at any of the observed frequencies at any observing epoch. However, we find a quasi-periodicity of the subpulses present in the majority of the observing sessions. A correlation analysis indicates a relationship between components from different frequencies. We discuss the results of our analysis in light of the emission properties of normal radio pulsars and a recently proposed model which takes radio emission from magnetars into consideration., 15 pages, 11 figures, accepted for publication by MNRAS
Published: 2009

7. Arecibo Pulsar Survey Using ALFA. IV. Mock Spectrometer Data Analysis, Survey Sensitivity, and the Discovery of 40 Pulsars

Author: F. Cardoso, J. M. Cordes, Fernando Camilo, Khee-Gan Lee, E. C. Madsen, Ryan Lynch, J. W. T. Hessels, Fronefield Crawford, A. Venkataraman, P. Scholz, Xavier Siemens, Robert D. Ferdman, A. G. Lyne, C. Karako-Argaman, Scott M. Ransom, Kevin Stovall, Sourav Chatterjee, Adam Brazier, Joseph K. Swiggum, Julia S. Deneva, W. W. Zhu, Fredrick A. Jenet, I. H. Stairs, V. M. Kaspi, Maura McLaughlin, Benjamin William Allen, C. Patel, J. van Leeuwen, Paulo C. C. Freire, Slavko Bogdanov, Laura Spitler, Benjamin Knispel, D. R. Lorimer, P. Lazarus, and High Energy Astrophys. & Astropart. Phys (API, FNWI)
Subjects: Physics, Spectrometer, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics, Galactic plane, 01 natural sciences, Galaxy, Pulsar, Space and Planetary Science, Millisecond pulsar, Colors of noise, 0103 physical sciences, Arecibo Observatory, 010303 astronomy & astrophysics, Data reduction
Abstract: The on-going PALFA survey at the Arecibo Observatory began in 2004 and is searching for radio pulsars in the Galactic plane at 1.4 GHz. Observations since 2009 have been made with new wider-bandwidth spectrometers than were previously employed in this survey. A new data reduction pipeline has been in place since mid-2011 which consists of standard methods using dedispersion, searches for accelerated periodic sources, and search for single pulses, as well as new interference-excision strategies and candidate selection heuristics. This pipeline has been used to discover 41 pulsars, including 8 millisecond pulsars (MSPs; P < 10 ms), bringing the PALFA survey's discovery totals to 145 pulsars, including 17 MSPs, and one Fast Radio Burst (FRB). The pipeline presented here has also re-detected 188 previously known pulsars including 60 found in PALFA data by re-analyzing observations previously searched by other pipelines. A comprehensive description of the survey sensitivity, including the effect of interference and red noise, has been determined using synthetic pulsar signals with various parameters and amplitudes injected into real survey observations and subsequently recovered with the data reduction pipeline. We have confirmed that the PALFA survey achieves the sensitivity to MSPs predicted by theoretical models. However, we also find that compared to theoretical survey sensitivity models commonly used there is a degradation in sensitivity to pulsars with periods P >= 100 ms that gradually becomes up to a factor of ~10 worse for P > 4 s at DM < 150 pc/cc. This degradation of sensitivity at long periods is largely due to red noise. We find that 35 +- 3% of pulsars are missed despite being bright enough to be detected in the absence of red noise. This reduced sensitivity could have implications on estimates of the number of long-period pulsars in the Galaxy.
Published: 2015

8. The European Pulsar Timing Array

Author: B. Stappers, Michael Kramer, N. D'Amico, A. G. Lyne, and A. Jessner
Subjects: Physics, Gravitational-wave observatory, Gravitational wave, Astrophysics::High Energy Astrophysical Phenomena, Timing data, Astronomy, Astronomy and Astrophysics, Astrophysics, Gravitational-wave astronomy, Binary pulsar, European Pulsar Timing Array, Pulsar, Space and Planetary Science, Range (statistics)
Abstract: The timing of radio pulsars provides a tool for studying a wide range of fundamental physical and astrophysical problems. The best results are obtained by regular, frequent timing observations of a large number of sources at various frequencies. We describe a project which aims to improve on all of the above parameters by combining timing data from the pulsar timing programs of 4 European groups to form the so-called EPTA. These data will be used to study, amongst other things, relativistic binaries and gravitational waves.
Published: 2006

9. Pulsar Birthrates from the Parkes Multibeam Survey

Author: N. Vranesevic, R. N. Manchester, D. R. Lorimer, G. B. Hobbs, A. G. Lyne, M. Kramer, F. Camilo, I. H. Stairs, V. M. Kaspi, N. D'Amico, A. Possenti, F. Crawford, A. J. Faulkner, and M. A. McLaughlin
Subjects: Physics, Dipole, Pulsar, Space and Planetary Science, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, Multi beam, Astrophysics::Solar and Stellar Astrophysics, Astronomy and Astrophysics, Astrophysics, Magnetic field
Abstract: We report on calculations of the pulsar birthrate based on the results of the Parkes multibeam survey. From the observed sample of more than 800 pulsars, we compute the pulsar current, accounting as accurately as possible for all known selection effects. The main goal of this work is to understand the pulsar birthrate as a function of the surface dipole magnetic field strengths. We show that pulsars with magnetic fields greater than 10**12.5 G account for about half of the total birthrate.
Published: 2004

10. The Parkes Multibeam Pulsar Survey - III. Young pulsars and the discovery and timing of 200 pulsars

Author: Duncan R. Lorimer, Fronefield Crawford, A. Possenti, Andrew Faulkner, Michael Kramer, George Hobbs, Fernando Camilo, R. N. Manchester, Bhal Chandra Joshi, N. D'Amico, A. G. Lyne, V. M. Kaspi, Maura McLaughlin, D. J. Morris, J. F. Bell, and Ingrid H. Stairs
Subjects: Physics, education.field_of_study, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Population, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galactic plane, Vela, 01 natural sciences, Neutron star, Pulsar, Space and Planetary Science, 0103 physical sciences, Statistical analysis, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: The Parkes multibeam pulsar survey has unlocked vast areas of the Galactic plane which were previously invisible to earlier low-frequency and less-sensitive surveys. The survey has discovered more than 600 new pulsars so far, including many that are young and exotic. In this paper we report the discovery of 200 pulsars for which we present positional and spin-down parameters, dispersion measures, flux densities and pulse profiles. A large number of these new pulsars are young and energetic, and we review possible associations of $\gamma$-ray sources with the sample of about 1300 pulsars for which timing solutions are known. Based on a statistical analysis, we estimate that about $19\pm6$ associations are genuine. The survey has also discovered 12 pulsars with spin properties similar to those of the Vela pulsar, nearly doubling the known population of such neutron stars. Studying the properties of all known `Vela-like' pulsars, we find their radio luminosities to be similar to normal pulsars, implying that they are very inefficient radio sources. Finally, we review the use of the newly discovered pulsars as Galactic probes and discuss the implications of the new NE2001 Galactic electron density model for the determination of pulsar distances and luminosities., Comment: accepted for publication in MNRAS, 31 pages, 10 figures (figure 1 in reduced quality, find original version at ftp://ftp.jb.man.ac.uk/pub/psr/papers/kbm+03.ps.gz)
Published: 2003

11. Fast Radio Burst Discovered in the Arecibo Pulsar ALFA Survey

Author: A. Brazier, C. Aulbert, Duncan R. Lorimer, J. van Leeuwen, Benjamin Knispel, Scott M. Ransom, Fredrick A. Jenet, Laura Spitler, C. Karako-Argaman, Ingrid H. Stairs, Kejia Lee, A. Venkataraman, James M. Cordes, H. Fehrmann, Jason W. T. Hessels, Benjamin William Allen, Julia S. Deneva, Sourav Chatterjee, Robert Wharton, Victoria M. Kaspi, Fernando Camilo, Maura McLaughlin, A. G. Lyne, Weiwei Zhu, Fronefield Crawford, Kevin Stovall, Paulo C. C. Freire, Slavko Bogdanov, P. Lazarus, J. K. Swiggum, X. Siemens, P. Scholz, R. S. Lynch, and High Energy Astrophys. & Astropart. Phys (API, FNWI)
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), education.field_of_study, Brightness, 010308 nuclear & particles physics, Fast radio burst, Canadian Hydrogen Intensity Mapping Experiment, Astrophysics::High Energy Astrophysical Phenomena, Population, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Radio telescope, Pulsar, Space and Planetary Science, 0103 physical sciences, Dispersion (optics), Arecibo Observatory, Astrophysics - High Energy Astrophysical Phenomena, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: Recent work has exploited pulsar survey data to identify temporally isolated, millisecond-duration radio bursts with large dispersion measures (DMs). These bursts have been interpreted as arising from a population of extragalactic sources, in which case they would provide unprecedented opportunities for probing the intergalactic medium; they may also be linked to new source classes. Until now, however, all so-called fast radio bursts (FRBs) have been detected with the Parkes radio telescope and its 13-beam receiver, casting some concern about the astrophysical nature of these signals. Here we present FRB 121102, the first FRB discovery from a geographic location other than Parkes. FRB 121102 was found in the Galactic anti-center region in the 1.4-GHz Pulsar ALFA survey with the Arecibo Observatory with a DM = 557.4 $\pm$ 3 pc cm$^{-3}$, pulse width of $3\; \pm 0.5$ ms, and no evidence of interstellar scattering. The observed delay of the signal arrival time with frequency agrees precisely with the expectation of dispersion through an ionized medium. Despite its low Galactic latitude ($b = -0.2^{\circ}$), the burst has three times the maximum Galactic DM expected along this particular line-of-sight, suggesting an extragalactic origin. A peculiar aspect of the signal is an inverted spectrum; we interpret this as a consequence of being detected in a sidelobe of the ALFA receiver. FRB 121102's brightness, duration, and the inferred event rate are all consistent with the properties of the previously detected Parkes bursts., Comment: 9 pages, 3 figures, submitted to ApJ
Published: 2014

12. 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

13. Timing and Interstellar Scattering of 35 Distant Pulsars Discovered in the PALFA Survey

Author: J. M. Cordes, J. W. T. Hessels, D. R. Lorimer, Fredrick A. Jenet, Scott M. Ransom, Ryan Lynch, Benjamin Knispel, E. Altiere, Julia S. Deneva, Fernando Camilo, Yuzhuo Wang, Benjamin William Allen, Khee-Gan Lee, L. Popa, G. Desvignes, David J. Nice, Benjamin Stappers, I. H. Stairs, V. M. Kaspi, P. Lazarus, Maura McLaughlin, Fronefield Crawford, Kevin Stovall, S. Sanpa-arsa, Sourav Chatterjee, P. Scholz, N. D. R. Bhat, Xavier Siemens, A. Venkataraman, J. van Leeuwen, D. Farrington, Adam Brazier, D. J. Champion, W. W. Zhu, Paulo C. C. Freire, Slavko Bogdanov, A. G. Lyne, and High Energy Astrophys. & Astropart. Phys (API, FNWI)
Subjects: Physics, education.field_of_study, 010504 meteorology & atmospheric sciences, Scattering, Astrophysics::High Energy Astrophysical Phenomena, Population, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Jodrell Bank Observatory, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Pulsar wind nebula, Pulsar, Space and Planetary Science, 0103 physical sciences, Arecibo Observatory, Glitch (astronomy), education, 010303 astronomy & astrophysics, Noise (radio), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences
Abstract: We have made extensive observations of 35 distant slow (non-recycled) pulsars discovered in the ongoing Arecibo PALFA pulsar survey. Timing observations of these pulsars over several years at Arecibo Observatory and Jodrell Bank Observatory have yielded high-precision positions and measurements of rotation properties. Despite being a relatively distant population, these pulsars have properties that mirror those of the previously known pulsar population. Many of the sources exhibit timing noise, and one underwent a small glitch. We have used multifrequency data to measure the interstellar scattering properties of these pulsars. We find scattering to be higher than predicted along some lines of sight, particularly in the Cygnus region. Finally, we present XMM-Newton and Chandra observations of the youngest and most energetic of the pulsars, J1856+0245, which has previously been associated with the GeV-TeV pulsar wind nebula HESS J1857+026.
Published: 2013

14. Radio and \gamma-ray Constraints on the Emission Geometry and Birthplace of PSR J2043+2740

Author: A. Noutsos, A. A. Abdo, M. Ackermann, M. Ajello, J. Ballet, G. Barbiellini, M. G. Baring, D. Bastieri, K. Bechtol, R. Bellazzini, B. Berenji, E. Bonamente, A. W. Borgland, J. Bregeon, A. Brez, M. Brigida, P. Bruel, R. Buehler, G. Busetto, G. A. Caliandro, R. A. Cameron, F. Camilo, P. A. Caraveo, J. M. Casandjian, C. Cecchi, Ö. Çelik, S. Chaty, A. Chekhtman, J. Chiang, S. Ciprini, R. Claus, I. Cognard, J. Cohen-Tanugi, S. Colafrancesco, S. Cutini, C. D. Dermer, F. de Palma, P. S. Drell, D. Dumora, C. M. Ea, C. Favuzzi, E. C. Ferrara, W. B. Focke, M. Frailis, P. C. C. Freire, Y. Fukazawa, S. Funk, P. Fusco, F. Gargano, S. Germani, N. Giglietto, F. Giordano, M. Giroletti, G. Godfrey, P. Grandi, I. A. Grenier, J. E. Grove, L. Guillemot, S. Guiriec, A. K. Harding, R. E. Hughes, M. S. Jackson, G. Jóhannesson, A. S. Johnson, T. J. Johnson, W. N. Johnson, S. Johnston, T. Kamae, H. Katagiri, J. Kataoka, J. Knödlseder, M. Kramer, M. Kuss, J. Lande, S.-H. Lee, F. Longo, F. Loparco, M. N. Lovellette, P. Lubrano, A. G. Lyne, A. Makeev, M. Marelli, M. N. Mazziotta, J. E. McEnery, J. Mehault, P. F. Michelson, T. Mizuno, C. Monte, M. E. Monzani, A. Morselli, I. V. Moskalenko, S. Murgia, M. Naumann-Godo, P. L. Nolan, E. Nuss, T. Ohsugi, A. Okumura, N. Omodei, E. Orlando, J. F. Ormes, J. H. Panetta, D. Parent, V. Pelassa, M. Pepe, M. Persic, M. Pesce-Rollins, F. Piron, T. A. Porter, S. Rainò, P. S. Ray, M. Razzano, A. Reimer, O. Reimer, T. Reposeur, R. W. Romani, H. F.-W. Sadrozinski, A. Sander, P. M. Saz Parkinson, C. Sgrò, E. J. Siskind, D. A. Smith, P. D. Smith, G. Spandre, P. Spinelli, B. W. Stappers, M. S. Strickman, D. J. Suson, H. Takahashi, T. Tanaka, G. Theureau, D. J. Thompson, S. E. Thorsett, O. Tibolla, D. F. Torres, A. Tramacere, T. L. Usher, J. Vandenbroucke, G. Vianello, N. Vilchez, M. Villata, V. Vitale, A. von Kienlin, A. P. Waite, P. Wang, K. Watters, P. Weltevrede, B. L. Winer, K. S. Wood, M. Ziegler, 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), Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de physique et chimie de l'environnement (LPCE), 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), 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 d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Théorique et Astroparticules (LPTA), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), 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), Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), 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), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université d'Orléans (UO)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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), 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), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Université d'Orléans (UO)-Observatoire des Sciences de l'Univers en région Centre (OSUC), 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)-Centre National de la Recherche Scientifique (CNRS), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Noutsos, A., Abdo, A. A., Ackermann, M., Ajello, M., Ballet, J., Barbiellini, G., Baring, M. G., Bastieri, D., Bechtol, K., Bellazzini, R., Berenji, B., Bonamente, E., Borgland, A. W., Bregeon, J., Brez, A., Brigida, M., Bruel, P., Buehler, R., Busetto, G., Caliandro, G. A., Cameron, R. A., Camilo, F., Caraveo, P. A., Casandjian, J. M., Cecchi, C., Celik, ., Chaty, S., Chekhtman, A., Chiang, J., Ciprini, S., Claus, R., Cognard, I., Cohen Tanugi, J., Colafrancesco, S., Cutini, S., Dermer, C. D., Palma, F., Drell, P. S., Dumora, D., C. M., Ea, Favuzzi, C., Ferrara, E. C., Focke, W. B., Frailis, M., P. C. C., Fukazawa, Y., Funk, S., Fusco, P., Gargano, F., Germani, S., Giglietto, N., Giordano, F., Giroletti, M., Godfrey, G., Grandi, P., Grenier, I. A., Grove, J. E., Guillemot, L., Guiriec, S., Harding, A. K., Hughes, R. E., Jackson, M. S., Johannesson, G., Johnson, A. S., Johnson, T. J., Johnson, W. N., Johnston, S., Kamae, T., Katagiri, H., Kataoka, J., Kn\odlseder, J., Kramer, M., Kuss, M., Lande, J., Lee, S., Longo, Francesco, Loparco, F., Lovellette, M. N., Lubrano, P., Lyne, A. G., Makeev, A., Marelli, M., Mazziotta, M. N., Mcenery, J. E., Mehault, J., Michelson, P. F., Mizuno, T., Monte, C., Monzani, M. E., Morselli, A., Moskalenko, I. V., Murgia, S., Naumann Godo, M., Nolan, P. L., Nuss, E., Ohsugi, T., Okumura, A., Omodei, N., Orlando, E., Ormes, J. F., Panetta, J. H., Parent, D., Pelassa, V., Pepe, M., Persic, M., Pesce Rollins, M., Piron, F., Porter, T. A., Rain\`o, S., Ray, P. S., Razzano, M., Reimer, A., Reimer, O., Reposeur, T., Romani, R. W., Sadrozinski, H. F., Sander, A., Saz, P. M., Sgr\`o, C., Siskind, E. J., Smith, D. A., Smith, P. D., Spandre, G., Spinelli, P., Stappers, B. W., Strickman, M. S., Suson, D. J., Takahashi, H., Tanaka, T., Theureau, G., Thompson, D. J., Thorsett, S. E., Tibolla, O., Torres, D. F., Tramacere, A., Usher, T. L., Vandenbroucke, J., Vianello, G., Vilchez, N., Villata, M., Vitale, V., Kienlin, A., Waite, A. P., Wang, P., Watters, K., Weltevrede, P., Winer, B. L., Wood, K. S., and Ziegler, M.
Subjects: Proper motion, 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, Magnetic dip, FOS: Physical sciences, Geometry, Astrophysics, 97.60.Gb, 97.10.Cv , 95.85, 95.30.Gv, 97.10.Ri, gamma rays: stars, 01 natural sciences, star [gamma rays], Pulsar, Gamma rays: stars, pulsars: individual (PSR J2043+2740), 0103 physical sciences, Very-long-baseline interferometry, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, pulsars: individual: PSR J2043 + 2740, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Gamma ray, individual: PSR J2043 + 2740 [pulsars], Astronomy and Astrophysics, Polarization (waves), Astrophysics - Astrophysics of Galaxies, pulsars: individual (PSR J2043 + 2740), Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Caustic (optics), Fermi Gamma-ray Space Telescope
Abstract: We report on the first year of Fermi gamma-ray observations of pulsed high-energy emission from the old PSR J2043+2740. The study of the gamma-ray efficiency of such old pulsars gives us an insight into the evolution of pulsars' ability to emit in gammma rays as they age. The gamma-ray lightcurve of this pulsar above 0.1 GeV is clearly defined by two sharp peaks, 0.353+/-0.035 periods apart. We have combined the gamma-ray profile characteristics of PSR J2043+2740 with the geometrical properties of the pulsar's radio emission, derived from radio polarization data, and constrained the pulsar-beam geometry in the framework of a Two Pole Caustic and an Outer Gap model. The ranges of magnetic inclination and viewing angle were determined to be {alpha,zeta}~{52-57,61-68} for the Two Pole Caustic model, and {alpha,zeta}~{62-73,74-81} and {alpha,zeta}~{72-83,60-75} for the Outer Gap model. Based on this geometry, we assess possible birth locations for this pulsar and derive a likely proper motion, sufficiently high to be measurable with VLBI. At a characteristic age of 1.2 Myr, PSR J2043+2740 is the third oldest of all discovered, non-recycled, gamma-ray pulsars: it is twice as old as the next oldest, PSR J0357+32, and younger only than the recently discovered PSR J1836+5925 and PSR J2055+25, both of which are at least 5 and 10 times less energetic, respectively., 17 pages, 6 figures, Accepted for publication in ApJ
Published: 2011

15. The evolution of PSR J0737−3039B and a model for relativistic spin precession

Author: B. B. P. Perera, M. A. McLaughlin, M. Kramer, I. H. Stairs, R. D. Ferdman, P. C. C. Freire, A. Possenti, R. P. Breton, R. N. Manchester, M. Burgay, A. G. Lyne, F. Camilo, Marta Burgay, Nicolò D’Amico, Paolo Esposito, Alberto Pellizzoni, and Andrea Possenti
Subjects: Physics, Neutron star, Pulsar, Millisecond pulsar, Astrophysics::High Energy Astrophysical Phenomena, Precession, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Spin (physics), Binary pulsar, Beam (structure), Pulse (physics)
Abstract: We present the evolution of the radio emission from the 2.8‐s pulsar of the double pulsar system PSR J0737−3039A/B. We describe the changes in the pulse profile and flux density over five years of observations, culminating in the B pulsar’s radio disappearance in 2008 March. Over this time, the flux density decreased by 0.177 mJy yr−1 at the brightest orbital phases and the pulse profile evolved from a single to a double peak. Relativistic spin precession, coupled with an elliptical beam, can model the pulse profile evolution well and the reappearance is expected to happen in ∼2035 with the same part of the beam or in ∼2014 if we assume a symmetric beam shape.
Published: 2011

16. Results from the latest re-analysis of the Parkes multi-beam pulsar survey

Author: R. P. Eatough, M. Kramer, A. G. Lyne, M. Keith, Marta Burgay, Nicolò D’Amico, Paolo Esposito, Alberto Pellizzoni, and Andrea Possenti
Subjects: Physics, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, Binary number, Astronomy, Astrophysics, Binary pulsar, Neutron star, symbols.namesake, Pulsar, Millisecond pulsar, Multi beam, symbols, Doppler effect, X-ray pulsar
Abstract: The Parkes multi‐beam pulsar survey (PMPS) [1] is the most successful pulsar survey ever undertaken, discovering 786 pulsars (including those from this work) and 30 RRATs (e.g. [2] and references therein). Previous analyses of the survey have not been fully sensitive to relativistic binary systems, where the spin period of the pulsar varies significantly over the duration of the 35 minute observations because of the Doppler effect. The aim of this latest re‐analysis was to partially combat such selection effects and to find any relativistic binary systems that were missed in previous searches. In total 16 pulsars have been discovered including one MSP binary and a possible intermittent pulsar.
Published: 2011

17. A search for the binary companion to PSR J1740-3052

Author: Ih Stairs, Cr Tam, Michael Kramer, S Wagner, Fernando Camilo, R. N. Manchester, N. D'Amico, and A. G. Lyne
Subjects: Physics, Intergalactic star, Pulsar planet, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Binary pulsar, Neutron star, Pulsar, Space and Planetary Science, Millisecond pulsar, Binary star, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, X-ray pulsar
Abstract: We present results of near-infrared spectroscopy of the late-type star coincident with the young pulsar PSR J1740-3052. High-spectral-resolution K-band (~2.2 μm) observations were obtained in 2003 with the Infrared Spectrometer and Array Camera instrument on the Very Large Telescope and with Phoenix on the Gemini Telescope. We find no consistent evidence of a radial velocity shift in the star compatible with the known pulsar orbit, setting a limit on the minimum mass of the star, if it is the companion, of 60 M ⊙ . We therefore conclude that the observed star is likely to be a foreground object. No sign of the previously reported Brackett-γ emission was found in this analysis. Our findings support previous suggestions that the companion to PSR J1740-3052 is most likely a massive B-type star that has been obscured by the bright late-type star in the foreground.
Published: 2010

18. Fermi Large Area Telescope Observations Of The Vela Pulsar

Author: A. A. Abdo, M. Ackermann, W. B. Atwood, R. Bagagli, L. Baldini, J. Ballet, D. L. Band, G. Barbiellini, M. G. Baring, J. Bartelt, D. Bastieri, B. M. Baughman, K. Bechtol, F. Bellardi, R. Bellazzini, B. Berenji, D. Bisello, R. D. Blandford, E. D. Bloom, J. R. Bogart, E. Bonamente, A. W. Borgland, A. Bouvier, J. Bregeon, A. Brez, M. Brigida, P. Bruel, T. H. Burnett, G. A. Caliandro, R. A. Cameron, F. Camilo, P. A. Caraveo, J. M. Casandjian, M. Ceccanti, C. Cecchi, E. Charles, A. Chekhtman, C. C. Cheung, J. Chiang, S. Ciprini, R. Claus, I. Cognard, J. Cohen-Tanugi, L. R. Cominsky, J. Conrad, R. Corbet, L. Corucci, S. Cutini, D. S. Davis, M. DeKlotz, C. D. Dermer, A. de Angelis, F. de Palma, S. W. Digel, M. Dormody, E. do Couto e Silva, P. S. Drell, R. Dubois, D. Dumora, C. Espinoza, C. Farnier, C. Favuzzi, D. L. Flath, P. Fleury, W. B. Focke, M. Frailis, P. C. C. Friere, Y. Fukazawa, S. Funk, P. Fusco, F. Gargano, D. Gasparrini, N. Gehrels, S. Germani, R. Giannitrapani, B. Giebels, N. Giglietto, F. Giordano, T. Glanzman, G. Godfrey, E. V. Gotthelf, I. A. Grenier, M.-H. Grondin, J. E. Grove, L. Guillemot, S. Guiriec, G. Haller, A. K. Harding, P. A. Hart, R. C. Hartman, E. Hays, G. Hobbs, R. E. Hughes, G. Jóhannesson, A. S. Johnson, R. P. Johnson, T. J. Johnson, W. N. Johnson, S. Johnston, T. Kamae, G. Kanbach, V. M. Kaspi, H. Katagiri, J. Kataoka, A. Kavelaars, N. Kawai, H. Kelly, M. Kerr, B. Kiziltan, W. Klamra, J. Knödlseder, M. Kramer, F. Kuehn, M. Kuss, J. Lande, D. Landriu, L. Latronico, B. Lee, S.-H. Lee, M. Lemoine-Goumard, M. Livingstone, F. Longo, F. Loparco, B. Lott, M. N. Lovellette, P. Lubrano, A. G. Lyne, G. M. Madejski, A. Makeev, R. N. Manchester, B. Marangelli, M. Marelli, M. N. Mazziotta, J. E. McEnery, S. McGlynn, M. A. McLaughlin, N. Menon, C. Meurer, P. F. Michelson, T. Mineo, N. Mirizzi, W. Mitthumsiri, T. Mizuno, A. A. Moiseev, M. Mongelli, C. Monte, M. E. Monzani, E. Moretti, A. Morselli, I. V. Moskalenko, S. Murgia, T. Nakamori, P. L. Nolan, A. Noutsos, E. Nuss, T. Ohsugi, N. Omodei, E. Orlando, J. F. Ormes, M. Ozaki, A. Paccagnella, D. Paneque, J. H. Panetta, D. Parent, M. Pearce, M. Pepe, M. Perchiazzi, M. Pesce-Rollins, L. Pieri, M. Pinchera, F. Piron, T. A. Porter, S. Rainò, R. Rando, S. M. Ransom, E. Rapposelli, M. Razzano, A. Reimer, O. Reimer, T. Reposeur, L. C. Reyes, S. Ritz, L. S. Rochester, A. Y. Rodriguez, R. W. Romani, M. Roth, F. Ryde, A. Sacchetti, H. F.-W. Sadrozinski, N. Saggini, D. Sanchez, A. Sander, P. M. Saz Parkinson, K. N. Segal, A. Sellerholm, C. Sgrò, E. J. Siskind, D. A. Smith, P. D. Smith, G. Spandre, P. Spinelli, M. Stamatikos, J.-L. Starck, F. W. Stecker, T. E. Stephens, M. S. Strickman, A. W. Strong, D. J. Suson, H. Tajima, H. Takahashi, T. Takahashi, T. Tanaka, A. Tenze, J. B. Thayer, J. G. Thayer, G. Theureau, D. J. Thompson, S. E. Thorsett, L. Tibaldo, O. Tibolla, D. F. Torres, A. Tramacere, M. Turri, T. L. Usher, L. Vigiani, N. Vilchez, V. Vitale, A. P. Waite, P. Wang, K. Watters, P. Weltevrede, B. L. Winer, K. S. Wood, T. Ylinen, M. Ziegler, Abdo, A. A., Ackermann, M., Atwood, W. B., Bagagli, R., Baldini, L., Ballet, J., Band, D. L., Barbiellini, G., Baring, M. G., Bartelt, J., Bastieri, D., Baughman, B. M., Bechtol, K., Bellardi, F., Bellazzini, R., Berenji, B., Bisello, D., Blandford, R. D., Bloom, E. D., Bogart, J. R., Bonamente, E., Borgland, A. W., Bouvier, A., Bregeon, J., Brez, A., Brigida, M., Bruel, P., Burnett, T. H., Caliandro, G. A., Cameron, R. A., Camilo, F., Caraveo, P. A., Casandjian, J. M., Ceccanti, M., Cecchi, C., Charles, E., Chekhtman, A., Cheung, C. C., Chiang, J., Ciprini, S., Claus, R., Cognard, I., Cohen Tanugi, J., Cominsky, L. R., Conrad, J., Corbet, R., Corucci, L., Cutini, S., Davis, D. S., Deklotz, M., Dermer, C. D., Angelis, A. d., Palma, F. d., Digel, S. W., Dormody, M., Silva, E. D. E., Drell, P. S., Dubois, R., Dumora, D., Espinoza, C., Farnier, C., Favuzzi, C., Flath, D. L., Fleury, P., Focke, W. B., Frailis, M., Friere, P. C. C., Fukazawa, Y., Funk, S., Fusco, P., Gargano, F., Gasparrini, D., Gehrels, N., Germani, S., Giannitrapani, R., Giebels, B., Giglietto, N., Giordano, F., Glanzman, T., Godfrey, G., Gotthelf, E. V., Grenier, I. A., Grondin, M. H., Grove, J. E., Guillemot, L., Guiriec, S., Haller, G., Harding, A. K., Hart, P. A., Hartman, R. C., Hays, E., Hobbs, G., Hughes, R. E., Johannesson, G., Johnson, A. S., Johnson, R. P., Johnson, T. J., Johnson, W. N., Johnston, S., Kamae, T., Kanbach, G., Kaspi, V. M., Katagiri, H., Kataoka, J., Kavelaars, A., Kawai, N., Kelly, H., Kerr, M., Kiziltan, B., Klamra, W., Knodlseder, J., Kramer, M., Kuehn, F., Kuss, M., Lande, J., Landriu, D., Latronico, L., Lee, B., Lee, S. H., Lemoine Goumard, M., Livingstone, M., Longo, Francesco, Loparco, F., Lott, B., Lovellette, M. N., Lubrano, P., Lyne, A. G., Madejski, G. M., Makeev, A., Manchester, R. N., Marangelli, B., Marelli, M., Mazziotta, M. N., Mcenery, J. E., Mcglynn, S., Mclaughlin, M. A., Menon, N., Meurer, C., Michelson, P. F., Mineo, T., Mirizzi, N., Mitthumsiri, W., Mizuno, T., Moiseev, A. A., Mongelli, M., Monte, C., Monzani, M. E., Moretti, E., Morselli, A., Moskalenko, I. V., Murgia, S., Nakamori, T., Nolan, P. L., Noutsos, A., Nuss, E., Ohsugi, T., Omodei, N., Orlando, E., Ormes, J. F., Ozaki, M., Paccagnella, A., Paneque, D., Panetta, J. H., Parent, D., Pearce, M., Pepe, M., Perchiazzi, M., Pesce Rollins, M., Pieri, L., Pinchera, M., Piron, F., Porter, T. A., Raino, S., Rando, R., Ransom, S. M., Rapposelli, E., Razzano, M., Reimer, A., Reimer, O., Reposeur, T., Reyes, L. C., Ritz, S., Rochester, L. S., Rodriguez, A. Y., Romani, R. W., Roth, M., Ryde, F., Sacchetti, A., Sadrozinski, H. F. W., Saggini, N., Sanchez, D., Sander, A., Parkinson, P. M. S., Segal, K. N., Sellerholm, A., Sgro, C., Siskind, E. J., Smith, D. A., Smith, P. D., Spandre, G., Spinelli, P., Stamatikos, M., Starck, J. L., Stecker, F. W., Stephens, T. E., Strickman, M. S., Strong, A. W., Suson, D. J., Tajima, H., Takahashi, H., Takahashi, T., Tanaka, T., Tenze, A., Thayer, J. B., Thayer, J. G., Theureau, G., Thompson, D. J., Thorsett, S. E., Tibaldo, L., Tibolla, O., Torres, D. F., Tramacere, A., Turri, M., Usher, T. L., Vigiani, L., Vilchez, N., Vitale, V., Waite, A. P., Wang, P., Watters, K., Weltevrede, P., Winer, B. L., Wood, K. S., Ylinen, T., and Ziegler, M.
Subjects: Photon, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, Magnetosphere, Fermi satellite, Astrophysics, Gamma rays: observations, pulsars: individual (PSR B0833-45), Astrophysics::Cosmology and Extragalactic Astrophysics, Vela, 01 natural sciences, Spectral line, High Energy Gamma-ray Astronomy, Pulsar, 0103 physical sciences, 010306 general physics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Pulsars, media_common, Physics, Nebula, Astronomy and Astrophysics, pulsars: individual: PSR B0833-45, Space and Planetary Science, Sky, gamma rays: observations, Fermi Gamma-ray Space Telescope
Abstract: 著者人数：235名, Accepted: 2009-02-09, 資料番号: SA1000979000
Published: 2009

19. PSR J1410-6132: A young, energetic pulsar associated with EGRET source 3EG J1410-6147

Author: D. R. Lorimer, Simon Johnston, George Hobbs, Michael Kramer, Matthew Bailes, L. Guillemot, Maura McLaughlin, M. Burgay, A. Possenti, J.T. O'Brien, A. G. Lyne, and D. Parent
Subjects: Physics, biology, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galactic plane, biology.organism_classification, Radio telescope, Pulsar, Space and Planetary Science, Egret, Astrophysics::Galaxy Astrophysics
Abstract: We present the discovery of PSR J1410-6132, a 50-ms pulsar found during a high-frequency survey of the Galactic plane, using a 7-beam 6.3-GHz receiver on the 64-m Parkes radio telescope. The pulsar lies within the error box of the unidentified EGRET source 3EG J1410-6147, has a characteristic age of 26 kyr and a spin-down energy of 10^37 erg s^-1. It has a very high dispersion measure of 960+/-10 cm^-3 pc and the largest rotation measure of any pulsar, RM=+2400 +/- 30 rad m^-2. The pulsar is very scatter-broadened at frequencies of 1.4 GHz and below, making pulsed emission almost impossible to detect. Assuming a distance of 15 kpc, the pulsar's spin-down energy and a gamma-ray efficiency factor of ~10 per cent is sufficient to power the gamma-ray source. We therefore believe we have identified the nature of 3EG J1410-6147. This new discovery suggests that deep targeted high-frequency surveys of inner-galaxy EGRET sources could uncover further young, energetic pulsars., Accepted for publication in MNRAS
Published: 2008

20. The double pulsar: evolutionary constraints from the system geometry

Author: R. D. Ferdman, I. H. Stairs, M. Kramer, R. N. Manchester, A. G. Lyne, R. P. Breton, M. A. McLaughlin, A. Possenti, M. Burgay, C. Bassa, Z. Wang, A. Cumming, and V. M. Kaspi
Subjects: Physics, Angular momentum, Proper motion, Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, Astrophysics (astro-ph), FOS: Physical sciences, Geometry, Astrophysics, Orbital period, Neutron star, Supernova, Pulsar, Eccentricity (behavior), media_common, Spin-½
Abstract: The double pulsar system PSR J0737-3039A/B is a highly relativistic double neutron star (DNS) binary, with a 2.4-hour orbital period. The low mass of the second-formed NS, as well the low system eccentricity and proper motion, point to a different evolutionary scenario compared to other known DNS systems. We describe analysis of the pulse profile shape over 6 years of observations, and present the resulting constraints on the system geometry. We find the recycled pulsar in this system, PSR J0737-3039A, to have a low misalignment between its spin and orbital angular momentum axes, with a 68.3% upper limit of 6.1 degrees, assuming emission from both magnetic poles. This tight constraint lends credence to the idea that the supernova that formed the second pulsar was relatively symmetric, possibly involving electron-capture onto an O-Ne-Mg core., Comment: 5 page, 2 figures; To appear in the conference proceedings "40 Years of Pulsars: Millisecond Pulsars, Magnetars, and More", August 12-17, 2007, at McGill University, Montreal, Canada. Version with full-resolution figures can be found at http://www.phas.ubc.ca/~ferdman/ferdman.0737_geo.full.ps.gz; typos corrected, some rewording, and references added
Published: 2008

21. Parkes Observations of Radio Pulsars in Globular Clusters

Author: A. Corongiu, A. Possenti, N. D'Amico, M. Burgay, A. G. Lyne, R. N. Manchester, F. Camilo, J. M. Sarkissian, C. Bassa, Z. Wang, A. Cumming, and V. M. Kaspi
Subjects: Physics, Radio telescope, Neutron star, Pulsar, Millisecond pulsar, Astrophysics::High Energy Astrophysical Phenomena, Globular cluster, Astrophysics::Instrumentation and Methods for Astrophysics, Cluster (physics), Static timing analysis, Astronomy, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: Millisecond pulsars in southern globular clusters have been regularly observed for timing pourposes with the Parkes radio telescope. To date, several pulsars have data spanning more than 6 years, and their peculiarities are now recognisable via their timing analysis. In this paper we briefly summarise the state of the art of the timing for the eclipsing binary PSR J1701‐3006B in the clobular cluster NGC6266 and for all the millisecond pulsars in the globualr cluster NGC6752.
Published: 2008

22. Parkes 20-cm Multibeam Pulsar Surveys

Author: A. G. Lyne, C. Bassa, Z. Wang, A. Cumming, and V. M. Kaspi
Subjects: Interstellar medium, Physics, Neutron star, Pulsar, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astrophysics, X-ray pulsar
Abstract: The Parkes 20‐cm Multibeam Pulsar search system has been used by several groups of astronomers who have to date discovered between them no fewer than 953 pulsars, more than the 822 discovered by all other searches combined.
Published: 2008

23. PSR J1856+0245: Arecibo Discovery of a Young, Energetic Pulsar Coincident with the TeV Gamma-ray Source HESS J1857+026

Author: Benjamin Stappers, A. G. Lyne, Fronefield Crawford, N. D. R. Bhat, J. van Leeuwen, Fredrick A. Jenet, J. M. Cordes, Michael Kramer, D. R. Lorimer, P. Lazarus, I. H. Stairs, J. W. T. Hessels, A. Venkataraman, Fernando Camilo, Laura Kasian, Julia S. Deneva, Paulo C. C. Freire, David J. Nice, Victoria M. Kaspi, Maura McLaughlin, Ismaël Cognard, D. J. Champion, Bryan Gaensler, Scott M. Ransom, and High Energy Astrophys. & Astropart. Phys (API, FNWI)
Subjects: Physics, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Gamma ray, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Pulsar wind nebula, Luminosity, law.invention, Telescope, Pulsar, 13. Climate action, Space and Planetary Science, Coincident, law, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We present the discovery of the Vela-like radio pulsar J1856+0245 in the Arecibo PALFA survey. PSR J1856+0245 has a spin period of 81ms, a characteristic age of 21kyr, and a spin-down luminosity Edot = 4.6 x 10^36 ergs/s. It is positionally coincident with the TeV gamma-ray source HESS J1857+026, which has no other known counterparts. Young, energetic pulsars create wind nebulae, and more than a dozen pulsar wind nebulae have been associated with very-high-energy (100GeV-100TeV) gamma-ray sources discovered with the HESS telescope. The gamma-ray emission seen from HESS J1857+026 is potentially produced by a pulsar wind nebula powered by PSR J1856+0245; faint X-ray emission detected by ASCA at the pulsar's position supports this hypothesis. The inferred gamma-ray efficiency is epsilon_gamma = L_gamma/Edot = 3.1% (1-10TeV, for a distance of 9kpc), comparable to that observed in similar associations., Comment: 13 pages, 1 figure, accepted for publication in The Astrophysical Journal Letters
Published: 2008
Full Text: View/download PDF

24. The X-ray emission of the highly magnetic RRAT J1819–1458

Author: N. Rea, M. A. McLaughlin, B. Gaensler, S. Chatterjee, F. Camilo, M. Kramer, D. R. Lorimer, A. G. Lyne, G. L. Israel, A. Possenti, C. Bassa, Z. Wang, A. Cumming, and V. M. Kaspi
Subjects: Physics, Rotating radio transient, Neutron star, Dipole, Pulsar, Proton, Scattering, law, Astrophysics::High Energy Astrophysical Phenomena, Cyclotron, Astrophysics, Magnetic field, law.invention
Abstract: We present the XMM–Newton discovery of X‐ray pulsations and a ∼1 keV spectral feature from RRAT J1819–1458, a Rotating Radio Transient source with an inferred surface dipole magnetic field of 5×1013 G and a 4.26 s spin period. We detect pulsations at the period predicted by the radio ephemeris, providing an unambiguous identification with the radio source and confirmation of its neutron star nature. The X‐ray pulse has a 0.3–5 keV pulsed fraction of 34% and is aligned with the radio pulse. On the other hand, the X‐ray spectrum is well fit by an absorbed blackbody with kT = 0.14 keV with the addition of a broad absorption feature at 1 keV The nature of this absorption feature is still not settled, it might be due to atomic transitions in the atmosphere or to resonant proton cyclotron scattering. No evidence for any X‐ray bursts or aperiodic variability has been found.
Published: 2008

25. Timing the Young Pulsar at the Centre of SNR 3C 58

Author: Margaret A. Livingstone, Scott M. Ransom, Fernando Camilo, Victoria M. Kaspi, Andrew G. Lyne, Michael Kramer, Ingrid H. Stairs, C. Bassa, Z. Wang, A. Cumming, and V. M. Kaspi
Subjects: Physics, Supernova, Neutron star, Pulsar, Green Bank Telescope, Timing data, Astronomy, Jodrell Bank Observatory, Astrophysics, Noise (radio), Luminosity
Abstract: PSR J0205+6449 is a young, rotation‐powered pulsar located at the centre of the SNR 3C 58, widely believed to be the remnant of the historical supernova SN 1181. The neutron star is cooler than expected from standard cooling models [1] and the pulsar, though it has a very high spin‐down luminosity of Ė = 2.6×1037 ergs/s, has very low radio (L1400∼0.5 mJy kpc2 [2]) and X‐ray luminosities (LX = 2.06×1032 ergs/s [3]). We present 4 yrs of timing data spanning 5 yrs obtained with the Rossi X‐ray Timing Explorer, the Jodrell Bank Observatory and the Green Bank Telescope. We present phase‐coherent timing analyses showing significant timing noise that prevents a measurement of the ‘braking index’. In addition, we present two glitches observed in the source and discuss implications for the age and temperature of the neutron star.
Published: 2008

26. A 610-MHz Galactic Plane Pulsar Search with the Giant Meterwave Radio Telescope

Author: B. C. Joshi, M. A. McLaughlin, M. Kramer, A. G. Lyne, D. R. Lorimer, D. A. Ludovici, M. Davies, A. J. Faulkner, C. Bassa, Z. Wang, A. Cumming, and V. M. Kaspi
Subjects: Physics, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Jodrell Bank Observatory, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galactic plane, law.invention, Radio telescope, Telescope, Pulsar, Intermediate frequency, law, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We report on the discovery of three new pulsars in the first blind survey of the north Galactic plane (45 < l < 135 ; |b| < 1) with the Giant Meterwave Radio telescope (GMRT) at an intermediate frequency of 610 MHz. The timing parameters, obtained in follow up observations with the Lovell Telescope at Jodrell Bank Observatory and the GMRT, are presented., 2 pages, 1 figure, to be published in conference proceedings of "40 years of pulsars ..", replaced figure .
Published: 2007

27. Discovery of 14 radio pulsars in a survey of the Magellanic Clouds

Author: R. N. Manchester, G. Fan, A. G. Lyne, V. M. Kaspi, and F. Crawford
Subjects: Physics, Systematic survey, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Limiting, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy, Radio telescope, Pulsar, Space and Planetary Science, Free electron density, Astrophysics::Galaxy Astrophysics, Luminosity function (astronomy)
Abstract: A systematic survey of the Large and Small Magellanic Clouds for radio pulsars using the Parkes radio telescope and the 20-cm multibeam receiver has resulted in the discovery of 14 pulsars and the redetection of five of the eight previously known spin-powered pulsars believed to lie in the Magellanic Clouds. Of the 14 new discoveries, 12 are believed to lie within Clouds, three in the Small Cloud and nine in the Large Cloud, bringing the total number of known spin-powered pulsars in the Clouds to 20. Averaged over all positions within the survey area, the survey had a limiting flux density of about 0.12 mJy. Observed dispersion measures suggest that the mean free electron density in the Magellanic Clouds is similar to that in the disk of our Galaxy. The observed radio luminosities have little or no dependence on pulsar period or characteristic age and the differential luminosity function is consistent with a power-law slope of -1 as is observed for Galactic pulsars., In press, ApJ
Published: 2006

28. Proper motion, age and initial spin period of PSR J0538+2817 in S147

Author: Christine Jordan, George Hobbs, O. Löhmer, Paul Carr, A. Wolszczan, Michael Kramer, and A. G. Lyne
Subjects: Physics, Proper motion, Period (periodic table), Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Measure (mathematics), Pulse period, Pulsar, Transverse velocity, Space and Planetary Science, Supernova remnant, Spin-½
Abstract: We present results of timing observations of the 143-ms pulsar J0538+2817 that provide a proper motion measurement which clearly associates the pulsar with the supernova remnant S147. We measure a proper motion of 67$_{-22}^{+48}$ mas yr$^{-1}$, implying a transverse velocity of $v= 385^{+260}_{-130}$ km s$^{-1}$. We derive an age of the pulsar and S147 of only $30\pm4$ kyr which is a factor of 20 times less than the pulsar's characteristic age of $\tau_c = 620$ kyr. This age implies an initial spin period of $P_0=139$ ms, close to the present pulse period and a factor of several larger than what is usually inferred for birth periods. Implications for recent X-ray detections of this pulsar are discussed., Comment: accepted for publication in ApJ Letters, 13 pages, 3 figures
Published: 2003

29. A Search for Pulsars in Quiescent Soft X-Ray Transients. I

Author: M. Burgay, L. Burderi, A. Possenti, N. D’Amico, R. N. Manchester, A. G. Lyne, F. Camilo, and S. Campana
Subjects: Physics, Millisecond, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Phase (waves), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Core (optical fiber), Neutron star, Radiation pressure, Pulsar, Space and Planetary Science, Cylinder, Absorption (electromagnetic radiation)
Abstract: We have carried out a deep search at 1.4 GHz for radio pulsed emission from six soft X-ray transient sources observed during their X-ray quiescent phase. The commonly accepted model for the formation of the millisecond radio pulsars predicts the presence of a rapidly rotating, weakly magnetized neutron star in the core of these systems. The sudden drop in accretion rate associated with the end of an X-ray outburst causes the Alfv\`en surface to move outside the light cylinder, allowing the pulsar emission process to operate. No pulsed signal was detected from the sources in our sample. We discuss several mechanisms that could hamper the detection and suggest that free-free absorption from material ejected from the system by the pulsar radiation pressure could explain our null result., Comment: accepted by ApJ
Published: 2003

30. The Parkes Multibeam Pulsar Survey: I. Observing and Data Analysis Systems, Discovery and Timing of 100 Pulsars

Author: Fronefield Crawford, V. M. Kaspi, N. P. F. McKay, Michael Kramer, N. D'Amico, Fernando Camilo, A. G. Lyne, I. H. Stairs, R. N. Manchester, A. Possenti, J. F. Bell, and D. C. Sheppard
Subjects: Physics, education.field_of_study, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Population, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, Binary number, Flux, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galactic plane, 01 natural sciences, Rotating radio transient, Interstellar medium, Radio telescope, Pulsar, Space and Planetary Science, 0103 physical sciences, education, 010303 astronomy & astrophysics
Abstract: The Parkes multibeam pulsar survey is a sensitive survey of a strip along the Galactic plane with |b, 35 pages, 7 figures, 7 tables. Accepted by MNRAS
Published: 2001
Full Text: View/download PDF

31. DISCOVERY OF NINE GAMMA-RAY PULSARS INFERMILARGE AREA TELESCOPE DATA USING A NEW BLIND SEARCH METHOD

Author: M. T. Wolff, Holger J. Pletsch, Elizabeth C. Ferrara, Ewan Barr, M. Dormody, Matthew Kerr, C. Aulbert, H. Fehrmann, Michael Kramer, Ralph Eatough, Benjamin William Allen, L. Guillemot, Benjamin Stappers, P. Caraveo, Fernando Camilo, Omer Celik, Paul S. Ray, J. W. T. Hessels, P. M. Saz Parkinson, Michael Keith, A. G. Lyne, M. Razzano, Scott M. Ransom, D. Parent, W. Reich, D. J. Champion, M. Marelli, Maura McLaughlin, Andrea Belfiore, Paulo C. C. Freire, A. De Luca, and High Energy Astrophys. & Astropart. Phys (API, FNWI)
Subjects: Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, Population, Astrophysics, gamma rays: stars, 01 natural sciences, Radio spectrum, PSR J1746-3239, Pulsar, Millisecond pulsar, pulsars: general, 0103 physical sciences, PSR J1620-4927, education, 010303 astronomy & astrophysics, media_common, Physics, education.field_of_study, PSR J1803-2149, 010308 nuclear & particles physics, Gravitational wave, Astronomy, Astronomy and Astrophysics, Neutron star, Space and Planetary Science, Sky, Fermi Gamma-ray Space Telescope
Abstract: We report the discovery of nine previously unknown gamma-ray pulsars in a blind search of data from the Fermi Large Area Telescope (LAT). The pulsars were found with a novel hierarchical search method originally developed for detecting continuous gravitational waves from rapidly rotating neutron stars. Designed to find isolated pulsars spinning at up to kHz frequencies, the new method is computationally efficient and incorporates several advances, including a metric-based gridding of the search parameter space (frequency, frequency derivative, and sky location) and the use of photon probability weights. The nine pulsars have spin frequencies between 3 and 12 Hz, and characteristic ages ranging from 17 kyr to 3 Myr. Two of them, PSRs J1803-2149 and J2111+ 4606, are young and energetic Galactic-plane pulsars (spin-down power above 6 × 1035 erg s-1 and ages below 100 kyr). The seven remaining pulsars, PSRs J0106+4855, J0622+3749, J1620-4927, J1746-3239, J2028+3332, J2030+4415, and J2139+4716, are older and less energetic; two of them are located at higher Galactic latitudes (|b| > 10°). PSR J0106+4855 has the largest characteristic age (3 Myr) and the smallest surface magnetic field (2 × 1011 G) of all LAT blind-search pulsars. PSR J2139+4716 has the lowest spin-down power (3 × 1033 erg s-1) among all non-recycled gamma-ray pulsars ever found. Despite extensive multi-frequency observations, only PSR J0106+4855 has detectable pulsations in the radio band. The other eight pulsars belong to the increasing population of radio-quiet gamma-ray pulsars.
Published: 2011

32. HIGH-PRECISION TIMING OF FIVE MILLISECOND PULSARS: SPACE VELOCITIES, BINARY EVOLUTION, AND EQUIVALENCE PRINCIPLES

Author: I. H. Stairs, Paul Demorest, Paulo C. C. Freire, David J. Nice, Scott M. Ransom, M. E. Gonzalez, Fernando Camilo, Robert D. Ferdman, George Hobbs, Michael Kramer, A. G. Lyne, and R. N. Manchester
Subjects: Physics, Proper motion, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Binary number, White dwarf, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Binary pulsar, Pulsar, Space and Planetary Science, Millisecond pulsar, 0103 physical sciences, 010303 astronomy & astrophysics, Equivalence (measure theory)
Abstract: We present high-precision timing of five millisecond pulsars (MSPs) carried out for more than seven years; four pulsars are in binary systems and one is isolated. We are able to measure the pulsars' proper motions and derive an estimate for their space velocities. The measured two-dimensional velocities are in the range 70-210 km/s, consistent with those measured for other MSPs. We also use all the available proper motion information for isolated and binary MSPs to update the known velocity distribution for these populations. As found by earlier works, we find that the velocity distribution of binary and isolated MSPs are indistinguishable with the current data. Four of the pulsars in our observing program are highly recycled with low-mass white dwarf companions and we are able to derive accurate binary parameters for these systems. For three of these binary systems we are able to place initial constraints on the pulsar masses with best-fit values in the range 1.0-1.6 M_sun. The implications of the results presented here to our understanding of binary pulsar evolution are discussed. The updated parameters for the binary systems studied here, together with recently discovered similar systems, allowed us to update previous limits on the the violation of the strong equivalence principle through the parameter |Delta| to 4.6x10^-3 (95% confidence) and the violation of Lorentz-invariance/momentum-conservation through the parameter |hat{alpha}_3| to 5.5x10^-20 (95% confidence).
Published: 2011

33. The Proper Motions of Young Pulsars

Author: J. L. Horlock, B. Anderson, A. G. Lyne, and N. P. F. McKay
Subjects: Physics, Pulsar, Astronomy
Abstract: We report on a project to determine the proper motions of a sample of 13 young pulsars. Sky positions are measured with phase referencing using two elements of the MERLIN array, giving a baseline of 198km. This technique involves the concurrent observation of each pulsar with one or more extra-galactic reference sources located in the same primary beam. At an observing wavelength of 21 cm, this allows the measurement of pulsar positions to an accuracy greater than 1 mas.
Published: 2000

34. Pulsed high-energy γ-rays from the radio pulsar PSRI706–44

Author: K. T. S. Brazier, E. J. Schneid, Gottfried Kanbach, A. G. Lyne, R. N. Manchester, Simon Johnston, H. Rothermel, James Taylor, P. L. Nolan, D. A. Kniffen, C. E. Fichtel, N. D'Amico, R. C. Hartman, D. J. Thompson, Victoria M. Kaspi, K. Pinkau, H. A. Mayer-Hasselwander, Yiing Lin, D. L. Bertsch, J. M. Fierro, H. I. Nel, Peter F. Michelson, Stanley D. Hunter, P. Sreekumar, J. R. Mattox, David J. Nice, Zaven Arzoumanian, M. Sommer, and C. V. Montigny
Subjects: Physics, Multidisciplinary, Astrophysics::High Energy Astrophysical Phenomena, Gamma ray, Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Gamma-ray astronomy, Astrophysics, Binary pulsar, Neutron star, Pulsar, Millisecond pulsar, Radio frequency, Astrophysics::Galaxy Astrophysics, X-ray pulsar
Abstract: Gamma radiation above 100 MeV in energy has been detected from the radio pulsar PSR1706-44. The gamma emission forms a single broad peak within the pulsar period of 102 ms, in contrast to the two narrow peaks seen in the other three known high-energy gamma-ray pulsars. The emission mechanism in all cases is probably the same, the differences arising from the geometry of the magnetic and rotation axes and the line of sight. Gamma-ray emission accounts for as much as 1 percent of the total neutron star spindown energy in these pulsars, much more than emerges at optical or radio frequencies. Thus, study of this emission is important in understanding pulsar emission and evolution.
Published: 1992

35. Period evolution of PSR B1259-63: Evidence for propeller-torque spindown

Author: Luciano Nicastro, R. N. Manchester, Matthew Bailes, N. D'Amico, A. G. Lyne, and Simon Johnston
Subjects: Physics, Orbital elements, Pulsar, Space and Planetary Science, Binary star, Propeller, Torque, Astronomy and Astrophysics, Astrophysics, Stellar evolution
Published: 1995

36. Fermi-LAT Search for Pulsar Wind Nebulae around gamma-ray Pulsars

Author: Ackermann, M., Ajello, M., Baldini, L., Ballet, J., Barbiellini, G., Bastieri, D., Bechtol, K., Bellazzini, R., Berenji, B., Bloom, E. D., Bonamente, E., Borgland, A. W., Bouvier, A., Bregeon, J., Brez, A., Brigida, M., Bruel, P., Buehler, R., Buson, S., Caliandro, G. A., Cameron, R. A., Camilo, F., Caraveo, P. A., Casandjian, J. M., Cecchi, C., Celik, O., Charles, E., Chekhtman, A., Cheung, C. C., Chiang, J., Ciprini, S., Claus, R., Cognard, I., Cohen-Tanugi, J., Conrad, J., Dermer, C. D., de, Angelis A., de, Luca A., de, Palma F., Digel, S. W., do, Couto e Silva E., Drell, P. S., Dubois, R., Dumora, D., Favuzzi, C., Focke, W. B., Frailis, M., Funk, S., Fusco, P., Gargano, F., Germani, S., Giglietto, N., Giommi, P., Giordano, F., Giroletti, M., Glanzman, T., Godfrey, G., Grenier, I. A., Grondin, M.-H., Grove, J. E., Guillemot, L., Guiriec, S., Hadasch, D., Harding, A. K., Hayashi, K., Hays, E., Hobbs, G., Hughes, R. E., Johannesson, G., Johnson, A. S., Johnson, W. N., Johnston, S., Keith, M., Kerr, M., Knodlseder, J., Kramer, M., Kuss, M., Lande, J., Latronico, L., Lee, S.-H., Lemoine-Goumard, M., Longo, F., Loparco, F., Lovellette, M. N., Lubrano, P., Lyne, A. G., Makeev, A., Marelli, M., Mazziotta, M. N., McEnery, J. E., Mehault, J., Michelson, P. F., Moiseev, A. A., Monte, C., Monzani, M. E., Morselli, A., Moskalenko, I. V., Murgia, S., Nakamori, T., Naumann-Godo, M., Nolan, P. L., Noutsos, A., Nuss, E., Ormes, J. F., Paneque, D., Panetta, J. H., Parent, D., Pelassa, V., Pepe, M., Pesce-Rollins, M., Piron, F., Porter, T. A., Raino, S., Rando, R., Ransom, S. M., Ray, P. S., Razzano, M., Rea, N., Reimer, A., Reimer, O., Reposeur, T., Ripken, J., Ritz, S., Romani, R. W., Sadrozinski, H. F.-W., Sander, A., Saz, Parkinson P. M., Sgro, C., Siskind, E. J., Smith, D. A., Smith, P. D., Spandre, G., Spinelli, P., Strickman, M. S., Suson, D. J., Fukazawa, Y., Hanabata, Y., Kamae, T., Katagiri, H., Kataoka, J., Mizuno, T., Ohsugi, T., Okumura, Akira, Takahashi, H., Takahashi, Tadayuki, 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), Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de physique et chimie de l'environnement (LPCE), 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), 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 d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Théorique et Astroparticules (LPTA), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), 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), Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Fermi-LAT, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Université d'Orléans (UO)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université d'Orléans (UO)-Observatoire des Sciences de l'Univers en région Centre (OSUC), 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)-Centre National de la Recherche Scientifique (CNRS), 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), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), 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), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, M., Ackermann, M., Ajello, L., Baldini, J., Ballet, G., Barbiellini, D., Bastieri, K., Bechtol, R., Bellazzini, B., Berenji, E. D., Bloom, E., Bonamente, A. W., Borgland, A., Bouvier, J., Bregeon, A., Brez, M., Brigida, P., Bruel, R., Buehler, S., Buson, G. A., Caliandro, R. A., Cameron, F., Camilo, P. A., Caraveo, J. M., Casandjian, C., Cecchi, Celik, ., E., Charle, A., Chekhtman, C. C., Cheung, J., Chiang, S., Ciprini, R., Clau, I., Cognard, J., Cohen Tanugi, J., Conrad, C. D., Dermer, Angelis, A., Luca, A., Palma, F., S. W., Digel, E. d., C., P. S., Drell, R., Duboi, D., Dumora, C., Favuzzi, W. B., Focke, M., Fraili, Y., Fukazawa, S., Funk, P., Fusco, F., Gargano, S., Germani, N., Giglietto, P., Giommi, F., Giordano, M., Giroletti, T., Glanzman, G., Godfrey, I. A., Grenier, M., Grondin, J. E., Grove, L., Guillemot, S., Guiriec, D., Hadasch, Y., Hanabata, A. K., Harding, K., Hayashi, E., Hay, G., Hobb, R. E., Hughe, G., Johannesson, A. S., Johnson, W. N., Johnson, S., Johnston, T., Kamae, H., Katagiri, J., Kataoka, M., Keith, M., Kerr, J., Kn\odlseder, M., Kramer, M., Ku, J., Lande, L., Latronico, S., Lee, M., Lemoine Goumard, Longo, Francesco, F., Loparco, M. N., Lovellette, P., Lubrano, A. G., Lyne, A., Makeev, M., Marelli, M. N., Mazziotta, J. E., Mcenery, J., Mehault, P. F., Michelson, T., Mizuno, A. A., Moiseev, C., Monte, M. E., Monzani, A., Morselli, I. V., Moskalenko, S., Murgia, T., Nakamori, M., Naumann Godo, P. L., Nolan, A., Noutso, E., Nu, T., Ohsugi, A., Okumura, J. F., Orme, D., Paneque, J. H., Panetta, D., Parent, V., Pelassa, M., Pepe, M., Pesce Rollin, F., Piron, T. A., Porter, S., Rain\`o, R., Rando, S. M., Ransom, P. S., Ray, M., Razzano, N., Rea, A., Reimer, O., Reimer, T., Reposeur, J., Ripken, S., Ritz, R. W., Romani, H. F., Sadrozinski, A., Sander, P. M., Saz, C., Sgr\`o, E. J., Siskind, D. A., Smith, P. D., Smith, G., Spandre, P., Spinelli, M. S., Strickman, D. J., Suson, H., Takahashi, T., Takahashi, T., Tanaka, J. B., Thayer, J. G., Thayer, G., Theureau, D. J., Thompson, S. E., Thorsett, L., Tibaldo, D. F., Torre, G., Tosti, A., Tramacere, Y., Uchiyama, T., Uehara, T. L., Usher, J., Vandenbroucke, Etten, A., V., Vasileiou, N., Vilchez, V., Vitale, A. P., Waite, P., Wang, P., Weltevrede, B. L., Winer, K. S., Wood, Z., Yang, T., Ylinen, and M., Ziegler
Subjects: catalog, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, general [pulsars], 01 natural sciences, Pulsar wind nebula, Binary pulsar, Astronomi, astrofysik och kosmologi, Pulsar, Millisecond pulsar, pulsars: general, catalogs, gamma rays: general, 0103 physical sciences, Astronomy, Astrophysics and Cosmology, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, 97.60.Gb, 98.58.Mj, 98.58,.Hf, 95.55.Ka, 98.70.Rz, 97.10.Ex, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astronomy, Astronomy and Astrophysics, Crab Nebula, Space and Planetary Science, Spectral energy distribution, Astrophysics - High Energy Astrophysical Phenomena, general [gamma rays], X-ray pulsar, Fermi Gamma-ray Space Telescope
Abstract: 著者人数：171名, Accepted: 2010-10-28, 資料番号: SA1002649000
Published: 2011

37. Searches for gravitational waves from known pulsars with science run 5 LIGO data

Author: Abbott, B. P., Abbott, R., Acernese, F., Adhikari, R., Ajith, P., Allen, B., Allen, G., Alshourbagy, M., Amin, R. S., Anderson, S. B., Anderson, W. G., Antonucci, F., Aoudia, S., Arain, M. A., Araya, M., Armandula, H., Armor, P., Arun, K. G., Aso, Y., Aston, S., Astonea, P., Aufmuth, P., Aulbert, C., Babak, S., Baker, P., Ballardin, G., Ballmer, S., Barker, C., Barker, D., Barone, F., Barr, B., Barriga, P., Barsotti, L., Barsuglia, M., Barton, M. A., Bartos, I., Bassiri, R., Bastarrika, M., Bauer, T. S., Behnke, B., Beker, M., Benacquista, M., Betzwieser, J., Beyersdorf, P. T., Bigotta, S., Bilenko, I. A., Billingsley, G., Birindelli, S., Biswas, R., Bizouard, M. A., Black, E., Blackburn, J. K., Blackburn, L., Blair, D., Bland, B., Boccara, C., Bodiya, T. P., Bogue, L., Bondub, F., Bonelli, L., Bork, R., Boschi, V., Bose, S., Bosi, L., Braccinia, S., Bradaschia, C., Brady, P. R., Braginsky, V. B., Brau, J. E., Bridges, D. O., Brillet, A., Brinkmann, M., Brisson, V., Den Broeck, C. V., Brooks, A. F., Brown, D. A., Brummit, A., Brunet, G., Budzynski, R., Bulik, T., Bullington, A., Bulten, H. J., Buonanno, A., Burmeister, O., Buskulic, D., Byer, R. L., Cadonati, L., Cagnoli, G., Calloni, E., Camp, J. B., Campagna, E., Cannizzo, J., Cannon, K. C., Canuel, B., Cao, J., Carbognani, F., Cardenas, L., Caride, S., Castaldi, G., Caudill, S., Cavaglia, M., Cavalier, F., Cavalieri, R., Cella, G., Cepeda, C., Cesarini, E., Chalermsongsak, T., Chalkley, E., Charlton, P., Chassande Mottin, E., Chatterji, S., Chelkowski, S., Chen, Y., Chincarini, A., Christensen, N., Chung, C. T. Y., Clark, D., Clark, J., Clayton, J. H., Cleva, F., Coccia, E., Cokelaer, T., Colacino, C. N., Colas, J., Colla, A., Colombini, M., Conte, R., Cook, D., Corbitt, T. R. C., Corda, C., Cornish, N., Corsi, A., Coulon, J. P., Coward, D., Coyne, D. C., Creighton, J. D. E., Creighton, T. D., Cruise, A. M., Culter, R. M., Cumming, A., Cunningham, L., Cuoco, E., Danilishin, S. L., D'Antonio, S., Danzmann, K., Dari, A., Dattilo, V., Daudert, B., Davier, M., Davies, G., Daw, E. J., Day, R., Rosa, R. D., Debra, D., Degallaix, J., Prete, M. d., Dergachev, V., Desai, S., Desalvo, R., Dhurandhar, S., Fiore, L. D., Lieto, A. D., Emilio, M. D. P., Virgilio, A. D., Diaz, M., Dietz, A., Donovan, F., Dooley, K. L., Doomes, E. E., Drago, M., Drever, R. W. P., Dueck, J., Duke, I., Dumas, J. C., Dwyer, J. G., Echols, C., Edgar, M., Effler, A., Ehrens, P., Espinoza, E., Etzel, T., Evans, M., Evans, T., Fafone, V., Fairhurst, S., Faltas, Y., Fan, Y., Fazi, D., Fehrmann, H., Ferrante, I., Fidecaro, F., Finn, L. S., Fiori, I., Flaminio, R., Flasch, K., Foley, S., Forrest, C., Fotopoulos, N., Fournier, J. D., Franc, J., Franzen, A., Frasca, S., Frasconi, F., Frede, M., Frei, M., Frei, Z., Freise, A., Frey, R., Fricke, T., Fritschel, P., Frolov, V. V., Fyffe, M., Galdi, V., Gammaitoni, Luca, Garofoli, J. A., Garufiab, F., Gemme, G., Genin, E., Gennai, A., Gholami, I., Giaime, J. A., Giampanis, S., Giardina, K. D., Giazotto, A., Goda, K., Goetz, E., Goggin, L. M., Gonzalez, G., Gorodetsky, M. L., Gossler, S., Gouaty, R., Granata, M., Granata, V., Grant, A., Gras, S., Gray, C., Gray, M., Greenhalgh, R. J. S., Gretarsson, A. M., Greverie, C., Grimaldi, F., Grosso, R., Grote, H., Grunewald, S., Guenther, M., Guidi, G., Gustafson, E. K., Gustafson, R., Hage, B., Hallam, J. M., Hammer, D., Hammond, G. D., Hanna, C., Hanson, J., Harms, J., Harry, G. M., Harry, I. W., Harstad, E. D., Haughian, K., Hayama, K., Heefner, J., Heitmann, H., Hello, P., Heng, I. S., Heptonstall, A., Hewitson, M., Hild, S., Hirose, E., Hoak, D., Hodge, K. A., Holt, K., Hosken, D. J., Hough, J., Hoyland, D., Huet, D., Hughey, B., Huttner, S. H., Ingram, D. R., Isogai, T., Ito, M., Ivanov, A., Jaranowski, P., Johnson, B., Johnson, W. W., Jones, D. I., Jones, G., Jones, R., de la Jordana, L. S., Ju, L., Kalmus, P., Kalogera, V., Kandhasamy, S., Kanner, J., Kasprzyk, D., Katsavounidis, E., Kawabe, K., Kawamura, S., Kawazoe, F., Kells, W., Keppel, D. G., Khalaidovski, A., Khalili, F. Y., Khan, R., Khazanov, E., King, P., Kissel, J. S., Klimenko, S., Kokeyama, K., Kondrashov, V., Kopparapu, R., Koranda, S., Kowalska, I., Kozak, D., Krishnan, B., Krolak, A., Kumar, R., Kwee, P., Penna, P. L., Lam, P. K., Landry, M., Lantz, B., Lazzarini, A., Lei, H., Lei, M., Leindecker, N., Leonor, I., Leroy, N., Letendre, N., Li, C., Lin, H., Lindquist, P. E., Littenberg, T. B., Lockerbie, N. A., Lodhia, D., Longo, M., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lu, P., Lubinski, M., Lucianetti, A., Luck, H., Machenschalk, B., Macinnis, M., Mackowski, J. M., Mageswaran, M., Mailand, K., Majorana, E., Mana, N., Mandel, I., Mandic, V., Mantovani, M., Marchesoni, F., Marion, F., Marka, S., Marka, Z., Markosyan, A., Markowitz, J., Maros, E., Marque, J., Martelli, F., Martin, I. W., Martin, R. M., Marx, J. N., Mason, K., Masserot, A., Matichard, F., Matone, L., Matzner, R. A., Mavalvala, N., Mccarthy, R., Mcclelland, D. E., Mcguire, S. C., Mchugh, M., Mcintyre, G., Mckechan, D. J. A., Mckenzie, K., Mehmet, M., Melatos, A., Melissinos, A. C., Mendell, G., Menendez, D. F., Menzinger, F., Mercer, R. A., Meshkov, S., Messenger, C., Meyer, M. S., Michel, C., Milano, L., Miller, J., Minelli, J., Minenkova, Y., Mino, Y., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Miyakawa, O., Moe, B., Mohan, M., Mohanty, S. D., Mohapatra, S. R. P., Moreau, J., Moreno, G., Morgado, N., Morgia, A., Morioka, T., Mors, K., Mosca, S., Moscatelli, V., Mossavi, K., Mours, B., Mowlowry, C., Mueller, G., Muhammad, D., Muhlen, H. z., Mukherjee, S., Mukhopadhyay, H., Mullavey, A., Muller Ebhardt, H., Munch, J., Murray, P. G., Myers, E., Myers, J., Nash, T., Nelson, J., Neri, I., Newton, G., Nishizawa, A., Nocera, F., Numata, K., Ochsner, E., O'Dell, J., Ogin, G. H., O'Reilly, B., O'Shaughnessy, R., Ottaway, D. J., Ottens, R. S., Overmier, H., Owen, B. J., Pagliaroli, G., Palomba, C., Pan, Y., Pankow, C., Paoletti, F., Papa, M. A., Parameshwaraiah, V., Pardi, S., Pasqualetti, A., Passaquieti, R., Passuello, D., Patel, P., Pedraza, M., Penn, S., Perreca, A., Persichetti, G., Pichot, M., Piergiovanni, F., Pierro, V., Pietka, M., Pinard, L., Pinto, I. M., Pitkin, M., Pletsch, H. J., Plissi, M. V., Poggiani, R., Postiglione, F., Prato, M., Principe, M., Prix, R., Prodi, G. A., Prokhorov, L., Puncken, O., Punturo, M., Puppo, P., Quetschke, V., Raab, F. J., Rabaste, O., Rabeling, D. S., Radkins, H., Raffai, P., Raics, Z., Rainer, N., Rakhmanov, M., Rapagnani, P., Raymond, V., Re, V., Reed, C. M., Reed, T., Regimbau, T., Rehbein, H., Reid, S., Reitze, D. H., Ricci, F., Riesen, R., Riles, K., Rivera, B., Roberts, P., Robertson, N. A., Robinet, F., Robinson, C., Robinson, E. L., Rocchi, A., Roddy, S., Rolland, L., Rollins, J., Romano, J. D., Romanoac, R., Romie, J. H., Rosinska, D., Rover, C., Rowan, S., Rudiger, A., Ruggi, P., Russell, P., Ryan, K., Sakata, S., Salemi, F., Sandberg, V., Sannibale, V., Santamaria, L., Saraf, S., Sarin, P., Sassolas, B., Sathyaprakash, B. S., Sato, S., Satterthwaite, M., Saulson, P. R., Savage, R., Savov, P., Scanlan, M., Schilling, R., Schnabel, R., Schofield, R., Schulz, B., Schutz, B. F., Schwinberg, P., Scott, J., Scott, S. M., Searle, A. C., Sears, B., Seifert, F., Sellers, D., Sengupta, A. S., Sentenac, D., Sergeev, A., Shapiro, B., Shawhan, P., Shoemaker, D. H., Sibley, A., Siemens, X., Sigg, D., Sinha, S., Sintes, A. M., Slagmolen, B. J. J., Slutsky, J., van der Sluys, M. V., Smith, J. R., Smith, M. R., Smith, N. D., Somiya, K., Sorazu, B., Stein, A., Stein, L. C., Steplewski, S., Stochino, A., Stone, R., Strain, K. A., Strigin, S., Stroeer, A., Sturani, R., Stuver, A. L., Summerscales, T. Z., Sun, K. X., Sung, M., Sutton, P. J., Swinkels, B., Szokoly, G. P., Talukder, D., Tang, L., Tanner, D. B., Tarabrin, S. P., Taylor, J. R., Taylor, R., Terenzi, R., Thacker, J., Thorne, K. A., Thorne, K. S., Uring, A. T. R., Tokmakov, K. V., Toncelli, A., Tonelli, M., Torres, C., Torrie, C., Tournefier, E., Travasso, F., Traylor, G., Trias, M., Trummer, J., Ugolini, D., Ulmen, J., Urbanek, K., Vahlbruch, H., Vajente, G., Vallisneri, M., van den Brand, J. F. J., der Putten, S. v., Vass, S., Vaulin, R., Vavoulidis, M., Vecchio, A., Vedovato, G., van Veggel, A. A., Veitch, J., Veitch, P., Veltkamp, C., Verkindt, D., Vetrano, F., Vicere, A., Villar, A., Vineta, J. Y., Vocca, Helios, Vorvick, C., Vyachanin, S. P., Waldman, S. J., Wallace, L., Ward, R. L., Was, M., Weidner, A., Weinert, M., Weinstein, A. J., Weiss, R., Wen, L., Wen, S., Wette, K., Whelan, J. T., Whitcomb, S. E., Whiting, B. F., Wilkinson, C., Willems, P. A., Williams, H. R., Williams, L., Willke, B., Wilmut, I., Winkelmann, L., Winkler, W., Wipf, C. C., Wiseman, A. G., Woan, G., Wooley, R., Worden, J., Wu, W., Yakushin, I., Yamamoto, H., Yan, Z., Yoshida, S., Yvert, M., Zanolin, M., Zhang, J., Zhang, L., Zhao, C., Zotov, N., Zucker, M. E., Zweizig, J., Begin, S., Corongiu, A., D'Amico, N., Freire, P. C. C., Hessels, J. W. T., Hobbs, G. B., Kramer, M., Lyne, A. G., Manchester, R. N., Marshall, F. E., Middleditch, J., Possenti, A., Ransom, S. M., Stairs, I. H., Stappers, B., Collaboration, L. S., Collaboration, V., The LIGO Scientific Collaboration, The Virgo Collaboration, Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux ( ARTEMIS ), Université Nice Sophia Antipolis ( UNS ), Université Côte d'Azur ( UCA ) -Université Côte d'Azur ( UCA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de la Côte d'Azur, Université Côte d'Azur ( UCA ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de l'Accélérateur Linéaire ( LAL ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ), APC - Cosmologie, Physique Corpusculaire et Cosmologie - Collège de France ( PCC ), Collège de France ( CdF ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ) -Collège de France ( CdF ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ) -AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Centre National de la Recherche Scientifique ( CNRS ) -Observatoire de Paris-Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), ESPCI ParisTech, Institut de Physique de Rennes ( IPR ), Université de Rennes 1 ( UR1 ), Université de Rennes ( UNIV-RENNES ) -Université de Rennes ( UNIV-RENNES ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire d'Annecy de Physique des Particules ( LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules ), Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Savoie Mont Blanc ( USMB [Université de Savoie] [Université de Chambéry] ) -Centre National de la Recherche Scientifique ( CNRS ), APC - Gravitation ( APC-Gravitation ), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Max-Planck-Institut für Gravitationsphysik (Albert-Einstein-Institut), Max-Planck-Institut-Max-Planck-Institut, Laboratoire des matériaux avancés ( LMA ), Université Claude Bernard Lyon 1 ( UCBL ), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), 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 ), Virgo, Université Paris-Sud - Paris 11 ( UP11 ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Paris-Sud - Paris 11 ( UP11 ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL), Institut de Physique de Rennes (IPR), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), APC - Gravitation (APC-Gravitation), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, Laboratoire des matériaux avancés (LMA), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon, Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université de Rennes (UR)-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)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), High Energy Astrophys. & Astropart. Phys (API, FNWI), (Astro)-Particles Physics, Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), B. P., Abbott, R., Abbott, F., Acernese, R., Adhikari, P., Ajith, B., Allen, G., Allen, M., Alshourbagy, R. S., Amin, S. B., Anderson, W. G., Anderson, F., Antonucci, S., Aoudia, M. A., Arain, M., Araya, H., Armandula, P., Armor, K. G., Arun, Y., Aso, S., Aston, P., Astone, P., Aufmuth, C., Aulbert, S., Babak, P., Baker, G., Ballardin, S., Ballmer, C., Barker, D., Barker, F., Barone, B., Barr, P., Barriga, L., Barsotti, M., Barsuglia, M. A., Barton, I., Barto, R., Bassiri, M., Bastarrika, Bauer, T. h. S., B., Behnke, M., Beker, M., Benacquista, J., Betzwieser, P. T., Beyersdorf, S., Bigotta, I. A., Bilenko, G., Billingsley, S., Birindelli, R., Biswa, M. A., Bizouard, E., Black, J. K., Blackburn, L., Blackburn, D., Blair, B., Bland, C., Boccara, T. P., Bodiya, L., Bogue, F., Bondu, L., Bonelli, R., Bork, V., Boschi, S., Bose, L., Bosi, S., Braccini, C., Bradaschia, P. R., Brady, V. B., Braginsky, J. E., Brau, D. O., Bridge, A., Brillet, M., Brinkmann, V., Brisson, C., Van Den Broeck, A. F., Brook, D. A., Brown, A., Brummit, G., Brunet, R., Budzyński, T., Bulik, A., Bullington, H. J., Bulten, A., Buonanno, O., Burmeister, D., Buskulic, R. L., Byer, L., Cadonati, G., Cagnoli, Calloni, Enrico, J. B., Camp, E., Campagna, J., Cannizzo, K. C., Cannon, B., Canuel, J., Cao, F., Carbognani, L., Cardena, S., Caride, G., Castaldi, S., Caudill, M., Cavaglià, F., Cavalier, R., Cavalieri, G., Cella, C., Cepeda, E., Cesarini, T., Chalermsongsak, E., Chalkley, P., Charlton, E., Chassande Mottin, S., Chatterji, S., Chelkowski, Y., Chen, A., Chincarini, N., Christensen, C. T. Y., Chung, D., Clark, J., Clark, J. H., Clayton, F., Cleva, E., Coccia, T., Cokelaer, C. N., Colacino, J., Cola, A., Colla, M., Colombini, R., Conte, D., Cook, T. R. C., Corbitt, C., Corda, N., Cornish, A., Corsi, J. P., Coulon, D., Coward, D. C., Coyne, J. D. E., Creighton, T. D., Creighton, A. M., Cruise, R. M., Culter, A., Cumming, L., Cunningham, E., Cuoco, S. L., Danilishin, S., D'Antonio, K., Danzmann, A., Dari, V., Dattilo, B., Daudert, M., Davier, G., Davie, E. J., Daw, R., Day, DE ROSA, Rosario, D., Debra, J., Degallaix, M., del Prete, V., Dergachev, S., Desai, R., Desalvo, S., Dhurandhar, L., Di Fiore, A., Di Lieto, M., Di Paolo Emilio, A., Di Virgilio, M., Díaz, A., Dietz, F., Donovan, K. L., Dooley, E. E., Doome, M., Drago, R. W. P., Drever, J., Dueck, I., Duke, J. C., Duma, J. G., Dwyer, C., Echol, M., Edgar, A., Effler, P., Ehren, E., Espinoza, T., Etzel, M., Evan, T., Evan, V., Fafone, S., Fairhurst, Y., Falta, Y., Fan, D., Fazi, H., Fehrmann, I., Ferrante, F., Fidecaro, L. S., Finn, I., Fiori, R., Flaminio, K., Flasch, S., Foley, C., Forrest, N., Fotopoulo, J. D., Fournier, J., Franc, A., Franzen, S., Frasca, F., Frasconi, M., Frede, M., Frei, Z., Frei, A., Freise, R., Frey, T., Fricke, P., Fritschel, V. V., Frolov, M., Fyffe, V., Galdi, L., Gammaitoni, J. A., Garofoli, Garufi, Fabio, G., Gemme, E., Genin, A., Gennai, I., Gholami, J. A., Giaime, S., Giampani, K. D., Giardina, A., Giazotto, K., Goda, E., Goetz, L. M., Goggin, G., González, M. L., Gorodetsky, S., Goßler, R., Gouaty, M., Granata, V., Granata, A., Grant, S., Gra, C., Gray, M., Gray, R. J. S., Greenhalgh, A. M., Gretarsson, C., Greverie, F., Grimaldi, R., Grosso, H., Grote, S., Grunewald, M., Guenther, G., Guidi, E. K., Gustafson, R., Gustafson, B., Hage, J. M., Hallam, D., Hammer, G. D., Hammond, C., Hanna, J., Hanson, J., Harm, G. M., Harry, I. W., Harry, E. D., Harstad, K., Haughian, K., Hayama, J., Heefner, H., Heitmann, P., Hello, I. S., Heng, A., Heptonstall, M., Hewitson, S., Hild, E., Hirose, D., Hoak, K. A., Hodge, K., Holt, D. J., Hosken, J., Hough, D., Hoyland, D., Huet, B., Hughey, S. H., Huttner, D. R., Ingram, T., Isogai, M., Ito, A., Ivanov, P., Jaranowski, B., Johnson, W. W., Johnson, D. I., Jone, G., Jone, R., Jone, L., Sancho de la Jordana, L., Ju, P., Kalmu, V., Kalogera, S., Kandhasamy, J., Kanner, D., Kasprzyk, E., Katsavounidi, K., Kawabe, S., Kawamura, F., Kawazoe, W., Kell, D. G., Keppel, A., Khalaidovski, F. Y., Khalili, R., Khan, E., Khazanov, P., King, J. S., Kissel, S., Klimenko, K., Kokeyama, V., Kondrashov, R., Kopparapu, S., Koranda, I., Kowalska, D., Kozak, B., Krishnan, A., Królak, R., Kumar, P., Kwee, P., La Penna, P. K., Lam, M., Landry, B., Lantz, A., Lazzarini, H., Lei, M., Lei, N., Leindecker, I., Leonor, N., Leroy, N., Letendre, C., Li, H., Lin, P. E., Lindquist, T. B., Littenberg, N. A., Lockerbie, D., Lodhia, M., Longo, M., Lorenzini, V., Loriette, M., Lormand, G., Losurdo, P., Lu, M., Lubinski, A., Lucianetti, H., Lück, B., Machenschalk, M., Macinni, J. M., Mackowski, M., Mageswaran, K., Mailand, E., Majorana, N., Man, I., Mandel, V., Mandic, M., Mantovani, F., Marchesoni, F., Marion, S., Márka, Z., Márka, A., Markosyan, J., Markowitz, E., Maro, J., Marque, F., Martelli, I. W., Martin, R. M., Martin, J. N., Marx, K., Mason, A., Masserot, F., Matichard, L., Matone, R. A., Matzner, N., Mavalvala, R., Mccarthy, D. E., Mcclelland, S. C., Mcguire, M., Mchugh, G., Mcintyre, D. J. A., Mckechan, K., Mckenzie, M., Mehmet, A., Melato, A. C., Melissino, G., Mendell, D. F., Menéndez, F., Menzinger, R. A., Mercer, S., Meshkov, C., Messenger, M. S., Meyer, C., Michel, Milano, Leopoldo, J., Miller, J., Minelli, Y., Minenkov, Y., Mino, V. P., Mitrofanov, G., Mitselmakher, R., Mittleman, O., Miyakawa, B., Moe, M., Mohan, S. D., Mohanty, S. R. P., Mohapatra, J., Moreau, G., Moreno, N., Morgado, A., Morgia, T., Morioka, K., Mor, S., Mosca, V., Moscatelli, K., Mossavi, B., Mour, C., Mowlowry, G., Mueller, D., Muhammad, H., zur Mühlen, S., Mukherjee, H., Mukhopadhyay, A., Mullavey, H., Müller Ebhardt, J., Munch, P. G., Murray, E., Myer, J., Myer, T., Nash, J., Nelson, I., Neri, G., Newton, A., Nishizawa, F., Nocera, K., Numata, E., Ochsner, J., O'Dell, G. H., Ogin, B., O'Reilly, R., O'Shaughnessy, D. J., Ottaway, R. S., Otten, H., Overmier, B. J., Owen, G., Pagliaroli, C., Palomba, Y., Pan, C., Pankow, F., Paoletti, M. A., Papa, V., Parameshwaraiah, S., Pardi, A., Pasqualetti, R., Passaquieti, D., Passuello, P., Patel, M., Pedraza, S., Penn, A., Perreca, G., Persichetti, M., Pichot, F., Piergiovanni, V., Pierro, M., Pietka, L., Pinard, I. M., Pinto, M., Pitkin, H. J., Pletsch, M. V., Plissi, R., Poggiani, F., Postiglione, M., Prato, M., Principe, R., Prix, G. A., Prodi, L., Prokhorov, O., Puncken, M., Punturo, P., Puppo, V., Quetschke, F. J., Raab, O., Rabaste, D. S., Rabeling, H., Radkin, P., Raffai, Z., Raic, N., Rainer, M., Rakhmanov, P., Rapagnani, V., Raymond, V., Re, C. M., Reed, T., Reed, T., Regimbau, H., Rehbein, S., Reid, D. H., Reitze, F., Ricci, R., Riesen, K., Rile, B., Rivera, P., Robert, N. A., Robertson, F., Robinet, C., Robinson, E. L., Robinson, A., Rocchi, S., Roddy, L., Rolland, J., Rollin, J. D., Romano, R., Romano, J. H., Romie, D., Rosińska, C., Röver, S., Rowan, A., Rüdiger, P., Ruggi, P., Russell, K., Ryan, S., Sakata, F., Salemi, V., Sandberg, V., Sannibale, L., Santamaría, S., Saraf, P., Sarin, B., Sassola, B. S., Sathyaprakash, S., Sato, M., Satterthwaite, P. R., Saulson, R., Savage, P., Savov, M., Scanlan, R., Schilling, R., Schnabel, R., Schofield, B., Schulz, B. F., Schutz, P., Schwinberg, J., Scott, S. M., Scott, A. C., Searle, B., Sear, F., Seifert, D., Seller, A. S., Sengupta, D., Sentenac, A., Sergeev, B., Shapiro, P., Shawhan, D. H., Shoemaker, A., Sibley, X., Siemen, D., Sigg, S., Sinha, A. M., Sinte, B. J. J., Slagmolen, J., Slutsky, M. V., van der Sluy, J. R., Smith, M. R., Smith, N. D., Smith, K., Somiya, B., Sorazu, A., Stein, L. C., Stein, S., Steplewski, A., Stochino, R., Stone, K. A., Strain, S., Strigin, A., Stroeer, R., Sturani, A. L., Stuver, T. Z., Summerscale, K. X., Sun, M., Sung, P. J., Sutton, B., Swinkel, G. P., Szokoly, D., Talukder, L., Tang, D. B., Tanner, S. P., Tarabrin, J. R., Taylor, R., Taylor, R., Terenzi, J., Thacker, K. A., Thorne, K. S., Thorne, A., Thüring, K. V., Tokmakov, A., Toncelli, M., Tonelli, C., Torre, C., Torrie, E., Tournefier, F., Travasso, G., Traylor, M., Tria, J., Trummer, D., Ugolini, J., Ulmen, K., Urbanek, H., Vahlbruch, G., Vajente, M., Vallisneri, J. F. J., van den Brand, S., van der Putten, S., Va, R., Vaulin, M., Vavoulidi, A., Vecchio, G., Vedovato, A. A., van Veggel, J., Veitch, P., Veitch, C., Veltkamp, D., Verkindt, F., Vetrano, A., Viceré, A., Villar, J. Y., Vinet, H., Vocca, C., Vorvick, S. P., Vyachanin, S. J., Waldman, L., Wallace, R. L., Ward, M., Wa, A., Weidner, M., Weinert, A. J., Weinstein, R., Wei, L., Wen, S., Wen, K., Wette, J. T., Whelan, S. E., Whitcomb, B. F., Whiting, C., Wilkinson, P. A., Willem, H. R., William, L., William, B., Willke, I., Wilmut, L., Winkelmann, W., Winkler, C. C., Wipf, A. G., Wiseman, G., Woan, R., Wooley, J., Worden, W., Wu, I., Yakushin, H., Yamamoto, Z., Yan, S., Yoshida, M., Yvert, M., Zanolin, J., Zhang, L., Zhang, C., Zhao, N., Zotov, M. E., Zucker, J., Zweizig, S., Bégin, A., Corongiu, N., D'Amico, P. C. C., Freire, J. W. T., Hessel, G. B., Hobb, M., Kramer, A. G., Lyne, R. N., Manchester, F. E., Marshall, J., Middleditch, A., Possenti, S. M., Ransom, I. H., Stair, B., Stapper, and Pinto, Innocenzo
Subjects: [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astrophysics::High Energy Astrophysical Phenomena, Astrophysics, Ephemeris, 01 natural sciences, LIMIT, [ PHYS.GRQC ] Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Pulsar, Millisecond pulsar, pulsars: general, 0103 physical sciences, gravitational waves, Limit (mathematics), 010303 astronomy & astrophysics, QC, Physics, 010308 nuclear & particles physics, Crab Pulsar, Gravitational wave, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astrophysics::Instrumentation and Methods for Astrophysics, [ PHYS.ASTR.HE ] Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astronomy and Astrophysics, LIGO, Amplitude, Space and Planetary Science, DISCOVERY, DISTANCE, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], SPIN-DOWN, [ SDU.ASTR.HE ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE]
Abstract: 39 pages, 5 figures, Accepted in The Astrophysical Journal; International audience; We present a search for gravitational waves from 116 known millisecond and young pulsars using data from the fifth science run of the LIGO detectors. For this search ephemerides overlapping the run period were obtained for all pulsars using radio and X-ray observations. We demonstrate an updated search method that allows for small uncertainties in the pulsar phase parameters to be included in the search. We report no signal detection from any of the targets and therefore interpret our results as upper limits on the gravitational wave signal strength. The most interesting limits are those for young pulsars. We present updated limits on gravitational radiation from the Crab pulsar, where the measured limit is now a factor of seven below the spin-down limit. This limits the power radiated via gravitational waves to be less than ~2% of the available spin-down power. For the X-ray pulsar J0537-6910 we reach the spin-down limit under the assumption that any gravitational wave signal from it stays phase locked to the X-ray pulses over timing glitches, and for pulsars J1913+1011 and J1952+3252 we are only a factor of a few above the spin-down limit. Of the recycled millisecond pulsars several of the measured upper limits are only about an order of magnitude above their spin-down limits. For these our best (lowest) upper limit on gravitational wave amplitude is 2.3x10^-26 for J1603-7202 and our best (lowest) limit on the inferred pulsar ellipticity is 7.0x10^-8 for J2124-3358.
Published: 2010

Catalog

Books, media, physical & digital resources

See catalog results

Searchworks

Select search scope, currently: Articles Catalog books, media & more in Jio Institute collections Articles journal articles & other e-resources

Search

Search Constraints

Refine your results

Search Limiters

Topic

Publication Year Range

Language

Journal

Database

Publisher

37 results on '"A. G. Lyne"'

Search Results

Catalog

Select search scope, currently: Articles

Catalog

books, media & more in Jio Institute collections

Articles

journal articles & other e-resources