F Acernese et al 2007 Class. Quantum Grav. 24 S491 doi:10.1088/0264-9381/24/19/S12
F Acernese1, P Amico2, M Alshourbagy3, F Antonucci4, S Aoudia5, P Astone4, S Avino1, D Babusci6, G Ballardin7, F Barone1, L Barsotti3, M Barsuglia8, Th S Bauer9, F Beauville10, S Bigotta3, S Birindelli3, M A Bizouard8, C Boccara11, F Bondu5, L Bosi2, C Bradaschia3, S Braccini3, F J van den Brand9, A Brillet5, V Brisson8, D Buskulic10, E Calloni1, E Campagna12, F Carbognani7, F Cavalier8, R Cavalieri7, G Cella3, E Cesarini12, E Chassande-Mottin5, N Christensen7, C Corda3, A Corsi4, F Cottone2, A-C Clapson8, F Cleva5, J-P Coulon5, E Cuoco7, A Dari2, V Dattilo7, M Davier8, M del Prete3, R De Rosa1, L Di Fiore1, A Di Virgilio3, B Dujardin5, A Eleuteri1, M Evans7, I Ferrante3, F Fidecaro3, I Fiori7, R Flaminio7,10, J-D Fournier5, S Frasca4, F Frasconi3, L Gammaitoni2, F Garufi1, E Genin7, A Gennai3, A Giazotto3, G Giordano6, L Giordano1, R Gouaty10, D Grosjean10, G Guidi12, S Hamdani7, S Hebri7, H Heitmann5, P Hello8, D Huet7, S Karkar10, S Kreckelbergh8, P La Penna7, M Laval5, N Leroy8, N Letendre10, B Lopez7, Lorenzini12, V Loriette11, G Losurdo12, J-M Mackowski13, E Majorana4, C N Man5, M Mantovani3, F Marchesoni2, F Marion10, J Marque7, F Martelli12, A Masserot10, M Mazzoni12, L Milano1, F Menzinger7, C Moins7, J Moreau11, N Morgado13, B Mours10, F Nocera7, C Palomba4, F Paoletti3,7, S Pardi1, A Pasqualetti7, R Passaquieti3, D Passuello3, F Piergiovanni12, L Pinard13, R Poggiani3, M Punturo2, P Puppo4, S van der Putten9, K Qipiani1, P Rapagnani4, V Reita11, A Remillieux13, F Ricci4, I Ricciardi1, P Ruggi7, G Russo1, S Solimeno1, A Spallicci5, M Tarallo3, M Tonelli3, A Toncelli3, E Tournefier10, F Travasso2, C Tremola3, G Vajente3, D Verkindt10, F Vetrano12, A Viceré12, J-Y Vinet5, H Vocca2 and M Yvert10
Show affiliationsIn this paper, we describe the analysis performed in the data of C6 and C7 commissioning runs of Virgo for the search of periodic sources of gravitational waves. The analysis is all-sky, covers the frequency range between 50 Hz and 1050 Hz and neutron star spin-down rate below 1.58 × 10−8 Hz s−1. Coincidences in the source parameter space between candidates found in the two data sets are required to reduce the false alarm probability. The procedure used to estimate the detection efficiency of the analysis pipeline, through the injection of simulated signals in the data, is also described.
04.30.Db Wave generation and sources
Issue 19 (7 October 2007)
Received 13 April 2007, in final form 29 May 2007
Published 19 September 2007
F Acernese et al 2007 Class. Quantum Grav. 24 S491
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