Calibration of the LIGO gravitational wave detectors in the fifth science run

Abadie, J.; Abbott, B. P.; Abbott, R.; Abernathy, M. R.; Adams, C.; Adhikari, R. X.; Ajith, P.; Allen, B.; Allen, G.; Ceron, E. Amador; Amin, R. S.; Anderson, S. B.; Anderson, W. G.; Arain, M. A.; Araya, M. C.; Aronsson, M.; Aso, Y.; Aston, S. M.; Atkinson, D.; Aufmuth, P.; Aulbert, C.; Babak, S.; Baker, P. T.; Ballmer, S. W.; Barker, D.; Barnum, S.; Barr, B.; Barriga, P.; Barsotti, L.; Barton, M. A.; Bartos, I.; Bassiri, R.; Bastarrika, M.; Bauchrowitz, J.; Behnke, B.; Benacquista, M.; Bertolini, A.; Betzwieser, J.; Beveridge, N.; Beyersdorf, P. T.; Bilenko, I. A.; Billingsley, G.; Birch, J.; Biswas, R.; Black, E.; Blackburn, J. K.; Blackburn, L.; Blair, David; Bland, B.; Böck, O.; Bodiya, T. P.; Bondarescu, Ruxandra; Bork, R.; Born, M.; Bose, S.; Boyle, Michael; Brady, P. R.; Braginsky, V. B.; Brau, J. E.; Breyer, J.; Bridges, D. O.; Brinkmann, M.; Britzger, M.; Brooks, A. F.; Brown, D. A.; Buonanno, A.; Burguet–Castell, J.; Burmeister, O.; Byer, R. 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C.; Effler, A.; Ehrens, P.; Engel, R.; Etzel, T.; Evans, M.; Evans, T. M.; Fairhurst, S.; Fan, Y.; Farr, B.; Fazi, D.; Fehrmann, H.; Feldbaum, D.; Finn, L. S.; Flanigan, Meghan E.; Flasch, Kurt; Foley, S.; Forrest, C.; Forsi, E.; Fotopoulos, N.; Frede, M.; Frei, M.; Frei, Z.; Freise, A.; Frey, R.; Fricke, T. T.; Friedrich, Daniel; Fritschel, P.; Frolov, V. V.; Fulda, P.; Fyffe, M.; Garofoli, J.; Gholami, I.; Ghosh, S.; Giaime, J. A.; Giampanis, S.; Giardina, K. D.; Gill, C.; Goetz, E.; Goggin, L. M.; Gonzlez, G.; Gorodetsky, M. L.; Goßler, S.; Graef, C.; Grant, A.; Gras, S.; Gray, C.; Greenhalgh, R. J. S.; Gretarsson, A. M.; Grosso, R.; Grote, H.; Grünewald, S.; Gustafson, E. K.; Gustafson, R.; Hage, B.; Hall, Peter; Hallam, J. M.; Hammer, D. A.; Hammond, G.; Hanks, J.; Hanna, C.; Hanson, J.; Harms, J.; Harry, G. M.; Harry, I. W.; Harstad, E. D.; Haughian, K.; Hayama, K.; Hayler, T.; Heefner, J.; Heng, I. S.; Heptonstall, A. W.; Hewitson, M.; Hild, S.; Hirose, E.; Hoak, D.; Hodge, K. 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I.; Traylor, G.; Trias, M.; Tseng, K.; Turner, L.; Ugolini, D.; Urbánek, Karel; Vahlbruch, H.; Vaishnav, B.; Vallisneri, Michele; Broeck, C. Van Den; Sluys, Monique Van; Veggel, A. A. van; Vass, S.; Vaulin, R.; Vecchio, A.; Veitch, J.; Veitch, P. J.; Veltkamp, C.; Villar, A.; Vorvick, C.; Vyachanin, S. P.; Waldman, S. J.; Wallace, L.; Wanner, A.; Ward, R. L.; Wei, Peng; Weinert, M.; Weinstein, A. J.; Weiss, R.; Wen, L.; Wen, S.; Weßels, P.; West, M.; Westphal, T.; Wette, K.; Whelan, J. T.; Whitcomb, S. E.; White, D. J.; Whiting, B. F.; Wilkinson, C.; Willems, P. A.; Williams, L.; Willke, B.; Winkelmann, L.; Winkler, W.; Wipf, C. C.; Wiseman, Alan; Woan, G.; Wooley, R.; Worden, J.; Yakushin, I.; Yamamoto, H.; Yamamoto, K.; Yeaton-Massey, D.; Yoshida, S.; Yu, P.; Zanolin, M.; Zhang, L.; Zhang, Z.; Zhao, C.; Zotov, N.; Zucker, M. E.; Zweizig, J.

doi:10.1016/j.nima.2010.07.089

Cited by 129 publications

(115 citation statements)

References 27 publications

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“…Calibration errors, which can influence the reconstructed amplitude, phase, and timing of the data [31], have the potential to affect parameter-estimation results. An analysis of the effect of calibration errors, which considered mock errors similar to those expected during the S6 and VSR2/3 runs, concluded that such errors are unlikely to cause a significant deterioration in parameter-estimation accuracy [33] at the moderate SNRs considered in this paper.…”

Section: Data Descriptionmentioning

confidence: 99%

“…The fact that gravitational waveforms used in the analysis are an approximation to the actual radiation produced by astrophysical sources and that the measured strain is affected by the uncertainties in the instrument calibration [31][32][33] represent additional challenges for making robust inferences on the underlying physics. To study parameter estimation in this regime, we have analyzed several artificial compact binary coalescence (CBC) signals added to real detector data, including the ''blind'' injection described above, added both in hardware and software to the data collected by the two LIGO instruments (Hanford and Livingston) and the Virgo detector during the most recent joint science run, S6/VSR2-3.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Parameter estimation for compact binary coalescence signals with the first generation gravitational-wave detector network

Aasi¹,

Abadie²,

Abbott³

et al. 2013

Phys. Rev. D

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149

128

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Compact binary systems with neutron stars or black holes are one of the most promising sources for ground-based gravitational-wave detectors. Gravitational radiation encodes rich information about source physics; thus parameter estimation and model selection are crucial analysis steps for any detection candidate events. Detailed models of the anticipated waveforms enable inference on several parameters, such as component masses, spins, sky location and distance, that are essential for new astrophysical studies of these sources. However, accurate measurements of these parameters and discrimination of models describing the underlying physics are complicated by artifacts in the data, uncertainties in the waveform models and in the calibration of the detectors. Here we report such measurements on a selection of simulated signals added either in hardware or software to the data collected by the two LIGO instruments and the Virgo detector during their most recent joint science run, including a "blind injection" where the signal was not initially revealed to the collaboration. We exemplify the ability to extract information about the source physics on signals that cover the neutron-star and black-hole binary parameter space over the component mass range 1 MâŠ™-25 MâŠ™ and the full range of spin parameters. The cases reported in this study provide a snapshot of the status of parameter estimation in preparation for the operation of advanced detectors. © 2013 American Physical Society

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Section: Data Descriptionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Parameter estimation for compact binary coalescence signals with the first generation gravitational-wave detector network

Aasi¹,

Abadie²,

Abbott³

et al. 2013

Phys. Rev. D

Self Cite

149

128

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“…Black hole (BH)-neutron star (NS) binary coalescences are among the prime sources of gravitational waves (GWs) for ground-based detectors, such as Advanced LIGO, Advanced Virgo, and KAGRA [1][2][3]. Gravitaional waves from BH-NS binaries will enable us to probe the supranuclear-density matter [4,5] and cosmological expansion [6] via the NS tidal effect even without electromagnetic (EM) observation.…”

Section: Introductionmentioning

confidence: 99%

Anisotropic mass ejection from black hole-neutron star binaries: Diversity of electromagnetic counterparts

Kyutoku

Ioka²,

Shibata³

2013

Phys. Rev. D

147

178

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The merger of black hole-neutron star binaries can eject substantial material with the mass ∼ 0.01-0.1M⊙ when the neutron star is disrupted prior to the merger. The ejecta shows significant anisotropy, and travels in a particular direction with the bulk velocity ∼ 0.2c. This is drastically different from the binary neutron star merger, for which ejecta is nearly isotropic. Anisotropic ejecta brings electromagnetic-counterpart diversity which is unique to black hole-neutron star binaries, such as viewing-angle dependence, polarization, and proper motion. The kick velocity of the black hole, gravitational-wave memory emission, and cosmic-ray acceleration are also discussed.

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“…Uncertainty in the calibration of GW detectors (Abadie et al 2010a;Accadia et al 2011) may impact the ability to correctly choose the right fields to observe with EM instruments. To estimate the potential detriment to pointing, we generated a second set of simulated burst signals, with each signal including some level of miscalibration corresponding to realistic calibration errors.…”

Section: Calibration Uncertaintymentioning

confidence: 99%

Implementation and testing of the first prompt search for gravitational wave transients with electromagnetic counterparts

Abadie

Abbott

et al. 2012

A&A

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Article published by EDP Sciences A124, page 1 of 15 A&A 539, A124 (2012) ABSTRACT Aims. A transient astrophysical event observed in both gravitational wave (GW) and electromagnetic (EM) channels would yield rich scientific rewards. A first program initiating EM follow-ups to possible transient GW events has been developed and exercised by the LIGO and Virgo community in association with several partners. In this paper, we describe and evaluate the methods used to promptly identify and localize GW event candidates and to request images of targeted sky locations. Methods. During two observing periods (Dec. 17, 2009 to Jan. 8, 2010 and Sep. 2 to Oct. 20, 2010, a low-latency analysis pipeline was used to identify GW event candidates and to reconstruct maps of possible sky locations. A catalog of nearby galaxies and Milky Way globular clusters was used to select the most promising sky positions to be imaged, and this directional information was delivered to EM observatories with time lags of about thirty minutes. A Monte Carlo simulation has been used to evaluate the low-latency GW pipeline's ability to reconstruct source positions correctly.Results. For signals near the detection threshold, our low-latency algorithms often localized simulated GW burst signals to tens of square degrees, while neutron star/neutron star inspirals and neutron star/black hole inspirals were localized to a few hundred square degrees. Localization precision improves for moderately stronger signals. The correct sky location of signals well above threshold and originating from nearby galaxies may be observed with ∼50% or better probability with a few pointings of wide-field telescopes.

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Calibration of the LIGO gravitational wave detectors in the fifth science run

Cited by 129 publications

References 27 publications

Parameter estimation for compact binary coalescence signals with the first generation gravitational-wave detector network

Parameter estimation for compact binary coalescence signals with the first generation gravitational-wave detector network

Anisotropic mass ejection from black hole-neutron star binaries: Diversity of electromagnetic counterparts

Implementation and testing of the first prompt search for gravitational wave transients with electromagnetic counterparts

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