Improving the timing precision for inspiral signals found by interferometric gravitational wave detectors

F. Acernese; P. Amico; M. Alshourbagy; F. Antonucci; S. Aoudia; P. Astone; S. Avino; D. Babusci; G. Ballardin; F. Barone; L. Barsotti; M. Barsuglia; Th S. Bauer; F. Beauville; S. Bigotta; S. Birindelli; M. A. Bizouard; C. Boccara; F. Bondu; L. Bosi; C. Bradaschia; S. Braccini; F. J. Van Den Brand; A. Brillet; V. Brisson; D. Buskulic; E. Calloni; E. Campagna; F. Carbognani; F. Cavalier; R. Cavalieri; G. Cella; E. Cesarini; E. Chassande-Mottin; N. Christensen; C. Corda; A. Corsi; F. Cottone; A. C. Clapson; F. Cleva; J. P. Coulon; E. Cuoco; A. Dari; V. Dattilo; M. Davier; M. Del Prete; R. De Rosa; L. Di Fiore; A. Di Virgilio; B. Dujardin; A. Eleuteri; M. Evans; I. Ferrante; F. Fidecaro; I. Fiori; R. Flaminio; J. D. Fournier; S. Frasca; F. Frasconi; L. Gammaitoni; F. Garufi; E. Genin; A. Gennai; A. Giazotto; G. Giordano; L. Giordano; R. Gouaty; D. Grosjean; G. Guidi; S. Hamdani; S. Hebri; H. Heitmann; P. Hello; D. Huet; S. Karkar; S. Kreckelbergh; P. La Penna; M. Laval; N. Leroy; N. Letendre; B. Lopez; Lorenzini; V. Loriette; G. Losurdo; J. M. MacKowski; E. Majorana; C. N. Man; M. Mantovani; F. Marchesoni; F. Marion; J. Marque; F. Martelli; A. Masserot; M. Mazzoni; L. Milano; F. Menzinger; C. Moins; J. Moreau; N. Morgado; B. Mours; F. Nocera; C. Palomba; F. Paoletti; S. Pardi; A. Pasqualetti; R. Passaquieti; D. Passuello; F. Piergiovanni; L. Pinard; R. Poggiani; M. Punturo; P. Puppo; S. Van Der Putten; K. Qipiani; P. Rapagnani; V. Reita; A. Remillieux; F. Ricci; I. Ricciardi; P. Ruggi; G. Russo; S. Solimeno; A. Spallicci; M. Tarallo; M. Tonelli; A. Toncelli; E. Tournefier; F. Travasso; C. Tremola; G. Vajente; D. Verkindt; F. Vetrano; A. Viceré; J. Y. Vinet; H. Vocca; M. Yvert

doi:10.1088/0264-9381/24/19/S24

Improving the timing precision for inspiral signals found by interferometric gravitational wave detectors

F. Acernese, P. Amico, M. Alshourbagy, F. Antonucci, S. Aoudia, P. Astone, S. Avino, D. Babusci, G. Ballardin, F. Barone, L. Barsotti, M. Barsuglia, Th S. Bauer, F. Beauville, S. Bigotta, S. Birindelli, M. A. Bizouard, C. Boccara, F. Bondu, L. BosiC. Bradaschia, S. Braccini, F. J. Van Den Brand, A. Brillet, V. Brisson, D. Buskulic, E. Calloni, E. Campagna, F. Carbognani, F. Cavalier, R. Cavalieri, G. Cella, E. Cesarini, E. Chassande-Mottin, N. Christensen, C. Corda, A. Corsi, F. Cottone, A. C. Clapson, F. Cleva, J. P. Coulon, E. Cuoco, A. Dari, V. Dattilo, M. Davier, M. Del Prete, R. De Rosa, L. Di Fiore, A. Di Virgilio, B. Dujardin, A. Eleuteri, M. Evans, I. Ferrante, F. Fidecaro, I. Fiori, R. Flaminio, J. D. Fournier, S. Frasca, F. Frasconi, L. Gammaitoni, F. Garufi, E. Genin, A. Gennai, A. Giazotto, G. Giordano, L. Giordano, R. Gouaty, D. Grosjean, G. Guidi, S. Hamdani, S. Hebri, H. Heitmann, P. Hello, D. Huet, S. Karkar, S. Kreckelbergh, P. La Penna, M. Laval, N. Leroy, N. Letendre, B. Lopez, Lorenzini, V. Loriette, G. Losurdo, J. M. MacKowski, E. Majorana, C. N. Man, M. Mantovani, F. Marchesoni, F. Marion, J. Marque, F. Martelli, A. Masserot, M. Mazzoni, L. Milano, F. Menzinger, C. Moins, J. Moreau, N. Morgado, B. Mours, F. Nocera, C. Palomba, F. Paoletti, S. Pardi, A. Pasqualetti, R. Passaquieti, D. Passuello, F. Piergiovanni, L. Pinard, R. Poggiani, M. Punturo, P. Puppo, S. Van Der Putten, K. Qipiani, P. Rapagnani, V. Reita, A. Remillieux, F. Ricci, I. Ricciardi, P. Ruggi, G. Russo, S. Solimeno, A. Spallicci, M. Tarallo, M. Tonelli, A. Toncelli, E. Tournefier, F. Travasso, C. Tremola, G. Vajente, D. Verkindt, F. Vetrano, A. Viceré, J. Y. Vinet, H. Vocca, M. Yvert

Physics

Research output: Contribution to journal › Article › peer-review

11 Scopus citations

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.

Original language	English
Article number	S24
Pages (from-to)	S617-S625
Journal	Classical and Quantum Gravity
Volume	24
Issue number	19
DOIs	https://doi.org/10.1088/0264-9381/24/19/S24
State	Published - Oct 7 2007

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10.1088/0264-9381/24/19/S24

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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, T. S., Beauville, F., Bigotta, S., Birindelli, S., Bizouard, M. A., Boccara, C., Bondu, F., ... Yvert, M. (2007). Improving the timing precision for inspiral signals found by interferometric gravitational wave detectors. Classical and Quantum Gravity, 24(19), S617-S625. [S24]. https://doi.org/10.1088/0264-9381/24/19/S24

@article{d7a516d5d2af47e7b0181be2bab65a1f,

title = "Improving the timing precision for inspiral signals found by interferometric gravitational wave detectors",

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.",

author = "F. Acernese and P. Amico and M. Alshourbagy and F. Antonucci and S. Aoudia and P. Astone and S. Avino and D. Babusci and G. Ballardin and F. Barone and L. Barsotti and M. Barsuglia and Bauer, {Th S.} and F. Beauville and S. Bigotta and S. Birindelli and Bizouard, {M. A.} and C. Boccara and F. Bondu and L. Bosi and C. Bradaschia and S. Braccini and {Van Den Brand}, {F. J.} and A. Brillet and V. Brisson and D. Buskulic and E. Calloni and E. Campagna and F. Carbognani and F. Cavalier and R. Cavalieri and G. Cella and E. Cesarini and E. Chassande-Mottin and N. Christensen and C. Corda and A. Corsi and F. Cottone and Clapson, {A. C.} and F. Cleva and Coulon, {J. P.} and E. Cuoco and A. Dari and V. Dattilo and M. Davier and {Del Prete}, M. and {De Rosa}, R. and {Di Fiore}, L. and {Di Virgilio}, A. and B. Dujardin and A. Eleuteri and M. Evans and I. Ferrante and F. Fidecaro and I. Fiori and R. Flaminio and Fournier, {J. D.} and S. Frasca and F. Frasconi and L. Gammaitoni and F. Garufi and E. Genin and A. Gennai and A. Giazotto and G. Giordano and L. Giordano and R. Gouaty and D. Grosjean and G. Guidi and S. Hamdani and S. Hebri and H. Heitmann and P. Hello and D. Huet and S. Karkar and S. Kreckelbergh and {La Penna}, P. and M. Laval and N. Leroy and N. Letendre and B. Lopez and Lorenzini and V. Loriette and G. Losurdo and MacKowski, {J. M.} and E. Majorana and Man, {C. N.} and M. Mantovani and F. Marchesoni and F. Marion and J. Marque and F. Martelli and A. Masserot and M. Mazzoni and L. Milano and F. Menzinger and C. Moins and J. Moreau and N. Morgado and B. Mours and F. Nocera and C. Palomba and F. Paoletti and S. Pardi and A. Pasqualetti and R. Passaquieti and D. Passuello and F. Piergiovanni and L. Pinard and R. Poggiani and M. Punturo and P. Puppo and {Van Der Putten}, S. and K. Qipiani and P. Rapagnani and V. Reita and A. Remillieux and F. Ricci and I. Ricciardi and P. Ruggi and G. Russo and S. Solimeno and A. Spallicci and M. Tarallo and M. Tonelli and A. Toncelli and E. Tournefier and F. Travasso and C. Tremola and G. Vajente and D. Verkindt and F. Vetrano and A. Vicer{\'e} and Vinet, {J. Y.} and H. Vocca and M. Yvert",

year = "2007",

month = oct,

day = "7",

doi = "10.1088/0264-9381/24/19/S24",

language = "English",

volume = "24",

pages = "S617--S625",

journal = "Classical and Quantum Gravity",

issn = "0264-9381",

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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, TS, Beauville, F, Bigotta, S, Birindelli, S, Bizouard, MA, Boccara, C, Bondu, F, Bosi, L, Bradaschia, C, Braccini, S, Van Den Brand, FJ, 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, AC, Cleva, F, Coulon, JP, 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, JD, 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, JM, Majorana, E, Man, CN, 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, Viceré, A, Vinet, JY, Vocca, H & Yvert, M 2007, 'Improving the timing precision for inspiral signals found by interferometric gravitational wave detectors', Classical and Quantum Gravity, vol. 24, no. 19, S24, pp. S617-S625. https://doi.org/10.1088/0264-9381/24/19/S24

TY - JOUR

T1 - Improving the timing precision for inspiral signals found by interferometric gravitational wave detectors

AU - Acernese, F.

AU - Amico, P.

AU - Alshourbagy, M.

AU - Antonucci, F.

AU - Aoudia, S.

AU - Astone, P.

AU - Avino, S.

AU - Babusci, D.

AU - Ballardin, G.

AU - Barone, F.

AU - Barsotti, L.

AU - Barsuglia, M.

AU - Bauer, Th S.

AU - Beauville, F.

AU - Bigotta, S.

AU - Birindelli, S.

AU - Bizouard, M. A.

AU - Boccara, C.

AU - Bondu, F.

AU - Bosi, L.

AU - Bradaschia, C.

AU - Braccini, S.

AU - Van Den Brand, F. J.

AU - Brillet, A.

AU - Brisson, V.

AU - Buskulic, D.

AU - Calloni, E.

AU - Campagna, E.

AU - Carbognani, F.

AU - Cavalier, F.

AU - Cavalieri, R.

AU - Cella, G.

AU - Cesarini, E.

AU - Chassande-Mottin, E.

AU - Christensen, N.

AU - Corda, C.

AU - Corsi, A.

AU - Cottone, F.

AU - Clapson, A. C.

AU - Cleva, F.

AU - Coulon, J. P.

AU - Cuoco, E.

AU - Dari, A.

AU - Dattilo, V.

AU - Davier, M.

AU - Del Prete, M.

AU - De Rosa, R.

AU - Di Fiore, L.

AU - Di Virgilio, A.

AU - Dujardin, B.

AU - Eleuteri, A.

AU - Evans, M.

AU - Ferrante, I.

AU - Fidecaro, F.

AU - Fiori, I.

AU - Flaminio, R.

AU - Fournier, J. D.

AU - Frasca, S.

AU - Frasconi, F.

AU - Gammaitoni, L.

AU - Garufi, F.

AU - Genin, E.

AU - Gennai, A.

AU - Giazotto, A.

AU - Giordano, G.

AU - Giordano, L.

AU - Gouaty, R.

AU - Grosjean, D.

AU - Guidi, G.

AU - Hamdani, S.

AU - Hebri, S.

AU - Heitmann, H.

AU - Hello, P.

AU - Huet, D.

AU - Karkar, S.

AU - Kreckelbergh, S.

AU - La Penna, P.

AU - Laval, M.

AU - Leroy, N.

AU - Letendre, N.

AU - Lopez, B.

AU - Lorenzini,

AU - Loriette, V.

AU - Losurdo, G.

AU - MacKowski, J. M.

AU - Majorana, E.

AU - Man, C. N.

AU - Mantovani, M.

AU - Marchesoni, F.

AU - Marion, F.

AU - Marque, J.

AU - Martelli, F.

AU - Masserot, A.

AU - Mazzoni, M.

AU - Milano, L.

AU - Menzinger, F.

AU - Moins, C.

AU - Moreau, J.

AU - Morgado, N.

AU - Mours, B.

AU - Nocera, F.

AU - Palomba, C.

AU - Paoletti, F.

AU - Pardi, S.

AU - Pasqualetti, A.

AU - Passaquieti, R.

AU - Passuello, D.

AU - Piergiovanni, F.

AU - Pinard, L.

AU - Poggiani, R.

AU - Punturo, M.

AU - Puppo, P.

AU - Van Der Putten, S.

AU - Qipiani, K.

AU - Rapagnani, P.

AU - Reita, V.

AU - Remillieux, A.

AU - Ricci, F.

AU - Ricciardi, I.

AU - Ruggi, P.

AU - Russo, G.

AU - Solimeno, S.

AU - Spallicci, A.

AU - Tarallo, M.

AU - Tonelli, M.

AU - Toncelli, A.

AU - Tournefier, E.

AU - Travasso, F.

AU - Tremola, C.

AU - Vajente, G.

AU - Verkindt, D.

AU - Vetrano, F.

AU - Viceré, A.

AU - Vinet, J. Y.

AU - Vocca, H.

AU - Yvert, M.

PY - 2007/10/7

Y1 - 2007/10/7

N2 - 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.

AB - 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.

UR - http://www.scopus.com/inward/record.url?scp=34748842695&partnerID=8YFLogxK

U2 - 10.1088/0264-9381/24/19/S24

DO - 10.1088/0264-9381/24/19/S24

M3 - Article

AN - SCOPUS:34748842695

SN - 0264-9381

VL - 24

SP - S617-S625

JO - Classical and Quantum Gravity

JF - Classical and Quantum Gravity

IS - 19

M1 - S24

ER -

Improving the timing precision for inspiral signals found by interferometric gravitational wave detectors

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