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; T.S. Bauer; F. Beauville; S. Bigotta; S. Birindelli; M.A. Bizouard; C. Boccara; F. Bondu; L. Bosi; C. Bradaschia; S. Braccini; J.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

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, T.S. Bauer, F. Beauville, S. Bigotta, S. Birindelli, M.A. Bizouard, C. Boccara, F. Bondu, L. BosiC. Bradaschia, S. Braccini, J.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

^*Corresponding author for this work

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

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
Pages (from-to)	S617-S625
Number of pages	9
Journal	Classical and Quantum Gravity
Volume	24
Issue number	19
DOIs	https://doi.org/10.1088/0264-9381/24/19/S24
Publication status	Published - 7 Oct 2007
Externally published	Yes

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10.1088/0264-9381/24/19/S24

Cite this

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., ... Dujardin, B. (2007). Improving the timing precision for inspiral signals found by interferometric gravitational wave detectors. Classical and Quantum Gravity, 24(19), S617-S625. https://doi.org/10.1088/0264-9381/24/19/S24

@article{2b0db43a23544a2ba837f130474baf95,

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 T.S. Bauer and F. Beauville and S. Bigotta and S. Birindelli and M.A. Bizouard and C. Boccara and F. Bondu and L. Bosi and C. Bradaschia and S. Braccini and {van den Brand}, J.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 A.C. Clapson and F. Cleva and J.P. Coulon 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",

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, JFJ, 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 2007, 'Improving the timing precision for inspiral signals found by interferometric gravitational wave detectors', Classical and Quantum Gravity, vol. 24, no. 19, 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, T.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, J.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.

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.

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

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

M3 - Article

SN - 0264-9381

VL - 24

SP - S617-S625

JO - Classical and Quantum Gravity

JF - Classical and Quantum Gravity

IS - 19

ER -