The characterization of Virgo data and its impact on gravitational-wave searches

Aasi, J.; Abadie, J.; Abbott, B. P.; Abbott, R.; Abbott, T. D.; Abernathy, M. R.; Accadia, T.; Acernese, F.; Adams, C.; Adams, T.; Addesso, P.; Adhikari, R. X.; Affeldt, C.; Agathos, M.; Agatsuma, K.; Ajith, P.; Allen, B.; Allocca, A.; Ceron, E. Amador; Amariutei, D.; Anderson, S. B.; Anderson, W. G.; Arai, K.; Araya, M. C.; Ast, S.; Aston, S. M.; Astone, P.; Atkinson, D.; Aufmuth, P.; Aulbert, C.; Aylott, B. E.; Babak, S.; Baker, P. T.; Ballardin, G.; Ballinger, Thomas J.; Ballmer, S. W.; Bao, Yiliang; Barayoga, J. C.; Barker, D.; Barone, F.; Barr, B.; Barsotti, L.; Barsuglia, M.; Barton, M. A.; Bartos, I.; Bassiri, R.; Bastarrika, M.; Basti, A.; Batch, J. C.; Bauchrowitz, J.; Bauer, Th.; Bebronne, M.; Beck, D.; Behnke, B.; Bejger, M.; Beker, M. G.; Bell, A. S.; Bell, C.; Belopolski, Ilya; Benacquista, M.; Berliner, J. M.; Bertolini, A.; Betzwieser, J.; Beveridge, N.; Beyersdorf, P. T.; Bhadbade, T.; Bilenko, I. A.; Billingsley, G.; Birch, J.; Biswas, R.; Bitossi, M.; Bizouard, M. A.; Black, E.; Blackburn, J. K.; Blackburn, L.; Blair, David; Bland, B.; Blom, M.; Böck, O.; Bodiya, T. P.; Bogan, C.; Bond, C.; Bondarescu, Ruxandra; Bondu, F.; Bonelli, L.; Bonnand, R.; Bork, R.; Born, M.; Boschi, V.; Bose, S.; Bosi, L.; Bouhou, B.; Braccini, S.; Bradaschia, C.; Brady, P. R.; Braginsky, V. B.; Branchesi, M.; Brau, J. E.; Breyer, J.; Briant, T.; Bridges, D. O.; Brillet, A.; Brinkmann, M.; Brisson, V.; Britzger, M.; Brooks, A. F.; Brown, D. A.; Bulik, T.; Bulten, H. J.; Buonanno, A.; Burguet–Castell, J.; Buskulic, D.; Buy, C.; Byer, R. L.; Cadonati, L.; Cagnoli, G.; Calloni, E.; Camp, J. B.; Campsie, P.; Cannon, K. C.; Canuel, B.; Cao, J.; Capano, C. D.; Carbognani, F.; Carbone, L.; Caride, S.; Caudill, S.; Cavaglià, M.; Cavalier, F.; Cavalieri, R.; Cella, G.; Cepeda, C.; Cesarini, E.; Chalermsongsak, T.; Charlton, P.; Chassande–Mottin, E.; Chen, W.; Chen, X.; Chen, Y.; Chincarini, A.; Chiummo, A.; Cho, H. S.; Chow, J. 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P.; Moraru, D.; Moreno, G.; Morgado, N.; Morgia, A.; Mori, Toshiyuki; Morriss, S. R.; Mosca, S.; Mossavi, K.; Mours, B.; Mow–Lowry, C. M.; Mueller, C. L.; Mueller, G.; Mukherjee, S.; Mullavey, A.; Müller‐Ebhardt, H.; Münch, J.; Murphy, D.; Murray, P. G.; Mytidis, A.; Nash, T.; Naticchioni, L.; Necula, V.; Nelson, J.; Neri, I.; Newton, G.; Nguyen, T.; Nishizawa, A.; Nitz, A.; Nocera, F.; Nolting, D.; Normandin, M. E. N.; Nuttall, L. K.; Ochsner, E.; O’Dell, J.; Oelker, E.; Ogin, G. H.; Oh, J. J.; Oh, Sang Hoon; Oldenberg, R. G.; O’Reilly, B.; O’Shaughnessy, R.; Osthelder, C.; Ott, Christian D.; Ottaway, D. J.; Ottens, R. S.; Overmier, H.; Owen, B. J.; Page, Amanda J.; Palladino, L.; Palomba, C.; Pan, Y.; Pankow, C.; Paoletti, F.; Paoletti, R.; Papa, M. A.; Parisi, M.; Pasqualetti, A.; Passaquieti, R.; Passuello, D.; Pedraza, M.; Penn, S.; Perreca, A.; Persichetti, G.; Phelps, M.; Pichot, M.; Pickenpack, M.; Piergiovanni, F.; Pierro, V.; Pihlaja, M.; Pinard, L.; Pinto, I. 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Z.; Sung, M.; Susmithan, S.; Sutton, P. J.; Swinkels, B. L.; Szeifert, G.; Tacca, M.; Taffarello, L.; Talukder, D.; Tanner, D. B.; Tarabrin, S. P.; Taylor, Robert W.; Braack, A. P. M. ter; Thomas, P.; Thorne, K. A.; Thorne, Kip S.; Thrane, E.; Thüring, A.; Titsler, C.; Tokmakov, K. V.; Tomlinson, C.; Toncelli, A.; Tonelli, M.; Torre, O.; Torres, C.; Torrie, C. I.; Tournefier, E.; Travasso, F.; Traylor, G.; Tse, M.; Tucker, Evan; Ugolini, D.; Vahlbruch, H.; Vajente, G.; Brand, J. van den; Broeck, C. Van Den; Putten, S. van der; Veggel, A. A. van; Vass, S.; Vasúth, M.; Vaulin, R.; Vavoulidis, M.; Vecchio, A.; Vedovato, G.; Veitch, J.; Veitch, P. J.; Venkateswara, K.; Verkindt, D.; Vetrano, F.; Viceré, A.; Villar, A.; Vinet, J.-Y.; Vitale, Salvatore; Vocca, H.; Vorvick, C.; Vyatchanin, S. P.; Wade, A. R.; Wade, L. E.; Wade, M.; Waldman, S. J.; Wallace, L.; Wan, Y.; Wang, M.; Wang, X.; Wanner, A.; Ward, R. L.; Was, M.; Weinert, M.; Weinstein, A. 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doi:10.1088/0264-9381/29/15/155002

Cited by 90 publications

(95 citation statements)

References 86 publications

(144 reference statements)

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“…Noise in interferometers arises from a combination of instrumental, environmental, and anthropomorphic noise sources that are extremely difficult to characterize precisely [50,[99][100][101]. Instrumental "glitches" can lead to large excursions over the time-averaged noise and may mimic the expected time-frequency content of an astrophysical signal [50,102].…”

Section: B the Duty Cycle Of The Detectors Is Not 100%mentioning

confidence: 99%

Observing gravitational waves from core-collapse supernovae in the advanced detector era

et al. 2016

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The next galactic core-collapse supernova (CCSN) has already exploded, and its electromagnetic (EM) waves, neutrinos, and gravitational waves (GWs) may arrive at any moment. We present an extensive study on the potential sensitivity of prospective detection scenarios for GWs from CCSNe within 5 Mpc, using realistic noise at the predicted sensitivity of the Advanced LIGO and Advanced Virgo detectors for 2015, 2017, and 2019. We quantify the detectability of GWs from CCSNe within the Milky Way and Large Magellanic Cloud, for which there will be an observed neutrino burst. We also consider extreme GW emission scenarios for more distant CCSNe with an associated EM signature. We find that a three-detector network at design sensitivity will be able to detect neutrino-driven CCSN explosions out to ∼5.5 kpc, while rapidly rotating core collapse will be detectable out to the Large Magellanic Cloud at 50 kpc. Of the phenomenological models for extreme GW emission scenarios considered in this study, such as long-lived bar-mode instabilities and disk fragmentation instabilities, all models considered will be detectable out to M31 at 0.77 Mpc, while the most extreme models will be detectable out to M82 at 3.52 Mpc and beyond.

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Section: B the Duty Cycle Of The Detectors Is Not 100%mentioning

confidence: 99%

Observing gravitational waves from core-collapse supernovae in the advanced detector era

et al. 2016

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“…The same challenge occurs in the analysis of data from the ground-based LIGO/Virgo interferometers [32,33], where studies have shown the noise to be both nonstationary and non-Gaussian [34][35][36], with frequent loud transient features, or glitches [37]. While it is not possible to remove gravitational wave signals from the data, it is possible to destroy signal coherence across the detector network by introducing artificial time delays between the detectors during the analysis [38].…”

Section: Sky Scramblesmentioning

confidence: 99%

Towards robust gravitational wave detection with pulsar timing arrays

Cornish¹,

Sampson²

2016

Phys. Rev. D

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Precision timing of highly stable milli-second pulsars is a promising technique for the detection of very low frequency sources of gravitational waves. In any single pulsar, a stochastic gravitational wave signal appears as an additional source of timing noise that can be absorbed by the noise model, and so it is only by considering the coherent response across a network of pulsars that the signal can be distinguished from other sources of noise. In the limit where there are many gravitational wave sources in the sky, or many pulsars in the array, the signals produce a unique tensor correlation pattern that depends only on the angular separation between each pulsar pair. It is this distinct fingerprint that is used to search for gravitational waves using pulsar timing arrays. Here we consider how the prospects for detection are diminished when the statistical isotropy of the timing array or the gravitational wave signal is broken by having a finite number of pulsars and a finite number of sources. We find the standard tensor-correlation analysis to be remarkably robust, with a mild impact on detectability compared to the isotropic limit. Only when there are very few sources and very few pulsars does the standard analysis begin to fail. Having established that the tensor correlations are a robust signature for detection, we study the use of "sky-scrambles" to break the correlations as a way to increase confidence in a detection. This approach is analogous to the use of "time-slides" in the analysis of data from ground based interferometric detectors.

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“…To remove from the analysis data segments likely to be significantly affected by nonstationary noise sources, the data was selected based on data-quality vetoes [37][38][39]. A combination of site activity and the absence of the fourth detector available during S5-VSR1, H2, meant that a higher rate of nonstationary noise events was observed during the S6-VSR2/3 run.…”

Section: A Data Setmentioning

confidence: 99%

Search for gravitational radiation from intermediate mass black hole binaries in data from the second LIGO-Virgo joint science run

Collaboration¹,

Collaboration²,

Aasi³

et al. 2014

Phys. Rev. D

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and was sensitive to IMBHBs with a range up to ∼200 Mpc, averaged over the possible sky positions and inclinations of the binaries with respect to the line of sight. No significant candidate was found. Upper limits on the coalescence-rate density of nonspinning IMBHBs with total masses between 100 and 450 M ⊙ and mass ratios between 0.25 and 1 were placed by combining this analysis with an analogous search performed on data from the first LIGO-Virgo joint science run (November 2005-October 2007). The most stringent limit was set for systems consisting of two 88 M ⊙ black holes and is equal to 0.12 Mpc −3 Myr −1 at the 90% confidence level. This paper also presents the first estimate, for the case of an unmodeled analysis, of the impact on the search range of IMBHB spin configurations: the visible volume for IMBHBs with nonspinning components is roughly doubled for a population of IMBHBs with spins aligned with the binary's orbital angular momentum and uniformly distributed in the dimensionless spin parameter up to 0.8, whereas an analogous population with antialigned spins decreases the visible volume by ∼20%.

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The characterization of Virgo data and its impact on gravitational-wave searches

Abstract: The characterization of Virgo data and its impact on gravitational-wave searches.

Cited by 90 publications

References 86 publications

Observing gravitational waves from core-collapse supernovae in the advanced detector era

Observing gravitational waves from core-collapse supernovae in the advanced detector era

Towards robust gravitational wave detection with pulsar timing arrays

Search for gravitational radiation from intermediate mass black hole binaries in data from the second LIGO-Virgo joint science run

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