Improving the timing precision for inspiral signals found by interferometric gravitational wave detectors
Year: 2007
Authors: Acernese F., Amico P., Alshourbagy M., Antonucci F., Aoudia S., Astone P., Avino S., Babusci D., Ballardin G., Barone F., Barsotti L., Barsuglia M., Bauer Th S., Beauville F., Bigotta S., Birindelli S., Bizouard M. A., Boccara C., Bondu F., Bosi L., Bradaschia C., Braccini S., van den Brand F. J., Brillet A., Brisson V., Buskulic D., Calloni E., Campagna E., Carbognani F., Cavalier F., Cavalieri R., Cella G., Cesarini E., Chassande-Mottin E., Christensen N., Corda C., Corsi A., Cottone F., Clapson A-C, Cleva F., Coulon J-P, Cuoco E., Dari A., Dattilo V., Davier M., del Prete M., De Rosa R., Di Fiore L., Di Virgilio A., Dujardin B., Eleuteri A., Evans M., Ferrante I., Fidecaro F., Fiori I., Flaminio R., Fournier J-D, Frasca S., Frasconi F., Gammaitoni L., Garufi F., Genin E., Gennai A., Giazotto A., Giordano G., Giordano L., Gouaty R., Grosjean D., Guidi G., Hamdani S., Hebri S., Heitmann H., Hello P., Huet D., Karkar S., Kreckelbergh S., La Penna P., Laval M., Leroy N., Letendre N., Lopez B., Lorenzini, Loriette V., Losurdo G., Mackowski J-M, Majorana E., Man C. N., Mantovani M., Marchesoni F., Marion F., Marque J., Martelli F., Masserot A., Mazzoni M., Milano L., Menzinger F., Moins C., Moreau J., Morgado N., Mours B., Nocera F., Palomba C., Paoletti F., Pardi S., Pasqualetti A., Passaquieti R., Passuello D., Piergiovanni F., Pinard L., Poggiani R., Punturo M., Puppo P., van der Putten S., Qipiani K., Rapagnani P., Reita V., Remillieux A., Ricci F., Ricciardi I., Ruggi P., Russo G., Solimeno S., Spallicci A., Tarallo M., Tonelli M., Toncelli A., Tournefier E., Travasso F., Tremola C., Vajente G., Verkindt D., Vetrano F., Vicere A., Vinet J-Y, Vocca H., Yvert M.
Autors Affiliation: Ist Nazl Fis Nucl, Sez Napoli, I-80125 Naples, Italy
Abstract: As they take data and improve their sensitivities, interferometric gravitational wave detectors will eventually detect signals emitted by inspiralling compact binary systems. Determining the sky position of the source will require that the signal be recorded in several detectors. The precision of the source direction determination will be driven by that of the time-of-flight measurements between detectors, and ultimately by the timing precision at the level of each detector. The latter is limited by the noise of the detector and the use of template banks, which introduce some mismatches between the parameters of the signal and the parameters of the template used to detect it. The standard way for signal timing is based on referring to the end time of the signal. In this paper we show that this is not an optimal choice and the timing precision can be improved referring to a time when the signal crosses some reference frequency, whose optimal value depends on the detector sensitivity.
Journal/Review: CLASSICAL AND QUANTUM GRAVITY
Volume: 24 (19) Pages from: S617 to: S625
KeyWords: Gravitational waves; Laser interferometry; DOI: 10.1088/0264-9381/24/19/S24ImpactFactor: 2.846Citations: 10data from “WEB OF SCIENCE” (of Thomson Reuters) are update at: 2024-11-24References taken from IsiWeb of Knowledge: (subscribers only)Connecting to view paper tab on IsiWeb: Click hereConnecting to view citations from IsiWeb: Click here
