All-Sky LIGO Search for Periodic Gravitational Waves in the Early Fifth-Science-Run Data

Abbott, B. P.; Abbott, R.; Adhikari, R. X.; Ajith, P.; Allen, B.; Allen, G.; Amin, R. S.; Anderson, S. B.; Anderson, W. G.; Arain, M. A.; Araya, M. C.; Armandula, H.; Armor, P.; Aso, Y.; Aston, S. M.; Aufmuth, P.; Aulbert, C.; Babak, S.; Baker, P. T.; Ballmer, S. W.; Bantilan, H.; Barish, B. C.; Barker, C.; Barker, D.; Barr, B.; Barriga, P.; Barsotti, L.; Barton, M. A.; Bartos, I.; Bassiri, R.; Bastarrika, M.; Behnke, B.; Benacquista, M.; Betzwieser, J.; Beyersdorf, P. T.; Bilenko, I. A.; Billingsley, G.; Biswas, R.; Black, E.; Blackburn, J. K.; Blackburn, L.; Blair, David; Bland, B.; Bodiya, T. P.; Bogue, L.; Bork, R.; Boschi, V.; Bose, S.; Brady, P. R.; Braginsky, V. B.; Brau, J. E.; Brinkmann, M.; Brooks, A. F.; Brown, D. A.; Brunet, G.; Bullington, A.; Buonanno, A.; Burmeister, O.; Byer, Robert L.; Cadonati, L.; Cagnoli, G.; Camp, J. B.; Cannizzo, J. K.; Cannon, K. C.; Cao, Junwei; Cardenas, L.; Cardoso, Vítor; Caride, S.; Casebolt, T.; Castaldi, G.; Caudill, S.; Cavaglià, M.; Cepeda, C.; Chalkley, E.; Charlton, P.; Chatterji, S.; Chelkowski, S.; Chen, Y.; Christensen, N.; Clark, D.; Clark, J. A.; Clayton, J. H.; Cokelaer, Thomas; Conte, R.; Cook, D.; Corbitt, T. R.; Cornish, N.; Coyne, D. C.; Creighton, J. D. E.; Creighton, T. D.; Cruise, A. M.; Cumming, A.; Cunningham, L.; Cutler, R. M.; Danzmann, K.; Daudert, B.; Davies, G. S.; DeBra, D.; Degallaix, J.; Dergachev, V.; Desai, S.; DeSalvo, R.; Dhurandhar, S.; Díaz, M. C.; Dickson, J.; Dietz, A.; Donovan, F.; Dooley, K. L.; Doomes, E. E.; Drever, R. W. P.; Duke, I.; Dumas, J. C.; Dwyer, J. G.; Echols, C.; Edgar, M.; Effler, A.; Ehrens, P.; Ely, Gabriela Zenatti; Espinoza, Eduardo; Etzel, T.; Evans, M.; Evans, T. M.; Fairhurst, S.; Faltas, Y.; Fan, Y.; Fazi, D.; Fejer, M. M.; Finn, L. S.; Flasch, Kurt; Foley, S.; Forrest, C.; Fotopoulos, N.; Franzen, A.; Frei, Z.; Freise, A.; Frey, R.; Fricke, T. T.; Fritschel, P.; Фролов, В. В.; Fyffe, M.; Garofoli, J.; Gholami, I.; Giaime, J. A.; Giampanis, S.; Giardina, K. D.; Goda, Keisuke; Goetz, E.; Goggin, L. M.; González, Gabriela; Goßler, S.; Gouaty, R.; Grant, A.; Gras, S.; Gray, C.; Gray, Malcolm B.; Greenhalgh, R. J. S.; Gretarsson, A. M.; Grimaldi, F.; Grosso, R.; Grote, H.; Grünewald, S.; Guenther, M.; Gustafson, E. K.; Gustafson, R.; Hage, B.; Hallam, J. M.; Hanna, C.; Hanson, J.; Harms, J.; Harry, G. M.; Harstad, E. D.; Haughian, E.; Hayama, K.; Hayler, T.; Heefner, J.; Heng, I. S.; Heptonstall, A. W.; Hewitson, M.; Hild, S.; Hirose, E.; Hoak, D.; Holt, K.; Hosken, D. J.; Hough, J.; Huttner, S. H.; Ingram, D. R.; Ito, Masahiro; Ivanov, A.; Johnson, B.; Johnson, W. W.; Jones, D. I.; Jones, Gareth; Jones, R.; Li, Ju; Kalmus, P.; Kalogera, V.; Kamat, S.; Kanner, J. B.; Kasprzyk, Dimitri; Katsavounidis, E.; Kawabe, K.; Kawamura, Seiji; Kawazoe, F.; Kells, W.; Keppel, D. G.; Khalaidovski, A.; Khalili, F. Y.; Khan, R.; Хазанов, Е. А.; King, Peter; Kissel, J. S.; Klimenko, S.; Kocsis, Bence; Kokeyama, K.; Kondrashov, V.; Kopparapu, R.; Koranda, S.; Kozak, D. B.; Kozhevatov, I. E.; Krishnan, B.; Kwee, P.; Landry, M.; Lantz, B.; Lazzarini, A.; Lei, M.; Leonor, I.; Li, C.; Lin, H.; Lindquist, P.; Littenberg, T. B.; Lockerbie, N. A.; Lodhia, D.; Lormand, M.; Lu, P.; Łubiński, M.; Lucianetti, Antonio; Lück, H.; Machenschalk, B.; MacInnis, M.; Mageswaran, M.; Mailand, K.; Mandel, Ilya; Mandic, V.; Márka, S.; Márka, Z.; Markosyan, A. S.; Markowitz, J.; Maros, E.; Martin, Ian; Martin, R. M.; Marx, J. N.; Mason, K.; Matichard, F.; Matone, L.; Matzner, R. A.; Mavalvala, N.; McCarthy, R.; McClelland, D. E.; McGuire, S. C.; McHugh, M.; McIntyre, G.; McKechan, D. J. A.; McKenzie, Kirk; Mehmet, M.; Melissinos, Adrian C.; Mendell, G.; Mercer, R. A.; Meshkov, S.; Messenger, C.; Meyers, D.; Miller, A.; Miller, John M.; Minelli, J.; Mitra, S.; Mitrofanov, V. P.; Mitselmakher, G.; Mittleman, R.; Miyakawa, O.; Moe, B.; Mohanty, S. D.; Moreno, G.; Mors, K.; Mossavi, K.; Mow–Lowry, C. M.; Mueller, G.; Muhammad, D.; Mukherjee, Soma; Mukhopadhyay, H.; Mullavey, A.; Müller‐Ebhardt, H.; Münch, J.; Murray, P. G.; Myers, E.; Myers, J.; Nash, T.; Nelson, J.; Newton, G.; Nishizawa, A.; Numata, Kenji; Ochsner, E.; O’Dell, J.; Ogin, G. H.; O’Reilly, B.; O’Shaughnessy, R.; Ottaway, D. J.; Ottens, R. S.; Overmier, H.; Owen, B. J.; Pan, Y.; Pankow, C.; Papa, M. A.; Parameshwaraiah, V.; Patel, P.; Pedraza, M.; Penn, S.; Perraca, A.; Pétrie, T.W.; Pinto, I. M.; Pitkin, M.; Pletsch, H. J.; Plissi, M. V.; Postiglione, F.; Principe, M.; Prix, R.; Quetschke, V.; Raab, F. J.; Rabeling, D. S.; Radkins, H.; Raffai, P.; Rainer, N.; Rakhmanov, M.; Ramsunder, M.; Reed, T.; Rehbein, H.; Reid, S.; Reitze, D. H.; Riesen, Rolf; Riles, K.; Rivera, B.; Robertson, N. A.; Robinson, C.; Robinson, E. L.; Roddy, S.; Rogan, A. M.; Rollins, J. G.; Romano, Joseph D.; Romie, J. H.; Rowan, S.; Rüdiger, A.; Ruet, Laurent; Russell, P.; Ryan, K.; Sakata, S.; Jordana, L. Sancho De La; Sandberg, V.; Sannibale, V.; Santamaría, L.; Saraf, S.; Sarin, P.; Sathyaprakash, B. S.; Sato, S.; Saulson, P. R.; Savage, R. L.; Savov, P.; Scanlan, M.; Schediwy, Sascha; Schilling, R.; Schnabel, R.; Schofield, R. M. S.; Schutz, B. F.; Schwinberg, P.; Scott, John D.; Scott, S. M.; Searle, A. C.; Sears, B.; Seifert, F.; Sellers, D.; Sengupta, A. S.; Sergeev, A.; Shapiro, B.; Shawhan, P.; Shoemaker, D. H.; Sibley, A.; Siemens, X.; Sigg, D.; Sinha, S.; Sintes, A. M.; Slagmolen, B. J. J.; Slutsky, J.; Smith, J. R.; Smith, M. R.; Smith, N. D.; Somiya, K.; Sorazu, B.; Stein, L. C.; Strain, K. A.; Stuver, A. L.; Summerscales, T. Z.; Sun, K. X.; Sung, M.; Sutton, P. J.; Takahashi, Hideya; Tanner, D. B.; Taylor, Robert W.; Thacker, John G.; Thorne, K. A.; Thorne, Kip S.; Thüring, A.; Tokmakov, K. V.; Torres, C.; Torrie, C. I.; Traylor, G.; Trias, M.; Ugolini, D.; Urbánek, Karel; Vahlbruch, H.; Broeck, C. Van Den; Sluys, Monique Van; Veggel, A. A. van; Vass, S.; Vaulin, R.; Vecchio, A.; Veitch, J.; Veitch, P. J.; Villar, A.; Vorvick, C.; Vyachanin, S. P.; Waldman, S. J.; Wallace, L.; Ward, H.; Ward, R. L.; Weinert, M.; Weinstein, A. J.; Weiss, R.; Wen, L.; Wen, S.; Wette, K.; Whelan, J. T.; Whitcomb, S. E.; Whiting, B. F.; Wilkinson, C.; Willems, P. A.; Williams, H. R.; Williams, L.; Willke, B.; Wilmut, Ian; Winkler, W.; Wipf, C. C.; Wiseman, Alan; Woan, G.; Wooley, R.; Worden, J.; Wu, W.; Yakushin, I.; Yamamoto, H.; Yan, Z.; Yoshida, S.; Zanolin, M.; Zhang, J.; Zhang, L.; Zhao, C.; Zotov, N.; Zucker, M. E.; Mühlen, Heribert; Zweizig, J.

doi:10.1103/physrevlett.102.111102

Cited by 84 publications

(70 citation statements)

References 16 publications

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“…where F þ and F × characterize the detector responses to signals with "þ" and "×" quadrupolar polarizations [12,14,16], the sky location is described by right ascension α 0 and declination δ 0 , ψ is the polarization angle of the projected source rotation axis in the sky plane, and the inclination of the source rotation axis to the detector line of sight is ι. The phase evolution of the signal is given by the formula…”

Section: A Signal Modelmentioning

confidence: 99%

“…In summary, (a) The PowerFlux pipeline has been used in previous searches of initial LIGO data from the S4, S5 and S6 Science Runs [12,14,16,20]. The program uses a Loosely Coherent method for following up outliers [24], and also a new universal statistic that provides correct upper limits regardless of the noise distribution of the underlying data, but which yields near-optimal performance for Gaussian data [25].…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

All-sky search for periodic gravitational waves in the O1 LIGO data

Abbott¹,

Abbott²,

Abbott³

et al. 2017

Phys. Rev. D

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178

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We report on an all-sky search for periodic gravitational waves in the frequency band 20-475 Hz and with a frequency time derivative in the range of ½−1.0; þ0.1 × 10 −8 Hz=s. Such a signal could be produced by a nearby spinning and slightly nonaxisymmetric isolated neutron star in our galaxy. This search uses the data from Advanced LIGO's first observational run, O1. No periodic gravitational wave signals were observed, and upper limits were placed on their strengths. The lowest upper limits on worst-case (linearly polarized) strain amplitude h 0 are ∼4 × 10 −25 near 170 Hz. For a circularly polarized source (most favorable orientation), the smallest upper limits obtained are ∼1.5 × 10 −25 . These upper limits refer to all sky locations and the entire range of frequency derivative values. For a population-averaged ensemble of sky locations and stellar orientations, the lowest upper limits obtained for the strain amplitude are ∼2.5 × 10 −25 .

show abstract

Section: A Signal Modelmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

All-sky search for periodic gravitational waves in the O1 LIGO data

Abbott¹,

Abbott²,

Abbott³

et al. 2017

Phys. Rev. D

Self Cite

178

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show abstract

“…Neutron stars with periods T < 200 ms emit gravitational waves (GWs) [3][4][5][6][7] in the ∼10-2000 Hz analysis band of current GW detectors such as Laser Interferometer Gravitational-Wave Observatory (LIGO) [8] and Virgo [9]. GW observatories have placed limits on GW emission from known pulsars [10][11][12][13], from nearby neutron stars with unknown phase evolution [14,15], and from electromagnetically quiet neutron stars [16][17][18][19]. For nearby pulsars, direct GW searches have bounded neutron star ellipticities to be as low as ϵ ≲ 7 × 10 −8 at 95% confidence level [11].…”

Section: Introductionmentioning

confidence: 99%

Measuring neutron-star ellipticity with measurements of the stochastic gravitational-wave background

et al. 2014

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Galactic neutron stars are a promising source of gravitational waves in the analysis band of detectors such as Laser Interferometer Gravitational-Wave Observatory (LIGO) and Virgo. Previous searches for gravitational waves from neutron stars have focused on the detection of individual neutron stars, which are either nearby or highly nonspherical. Here, we consider the stochastic gravitational-wave signal arising from the ensemble of Galactic neutron stars. Using a population synthesis model, we estimate the single-sigma sensitivity of current and planned gravitational-wave observatories to average neutron star ellipticity ϵ as a function of the number of in-band Galactic neutron stars N tot . For the plausible case of N tot ≈ 53000, and assuming one year of observation time with colocated initial LIGO detectors, we find it to be σ ϵ ¼ 2.1 × 10 −7 , which is comparable to current bounds on some nearby neutron stars. (The current best 95% upper limits are ϵ ≲ 7 × 10 −8 .) It is unclear if Advanced LIGO can significantly improve on this sensitivity using spatially separated detectors. For the proposed Einstein Telescope, we estimate that σ ϵ ¼ 5.6 × 10 −10 . Finally, we show that stochastic measurements can be combined with measurements of individual neutron stars in order to estimate the number of in-band Galactic neutron stars. In this way, measurements of stochastic gravitational waves provide a complementary tool for studying Galactic neutron stars.

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“…Glitches and wandering lines can be problematic for searches for bursts / compact binary coalescences and for pulsars respectively, see, e.g., [104][105][106][107]. (They also produce non-Gaussian noise for our crosspower statistic.)…”

Section: Application To Environmental Noise Identification a Envmentioning

confidence: 99%

Long gravitational-wave transients and associated detection strategies for a network of terrestrial interferometers

et al. 2011

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Searches for gravitational waves (GWs) traditionally focus on persistent sources (e.g., pulsars or the stochastic background) or on transients sources (e.g., compact binary inspirals or core-collapse supernovae), which last for timescales of milliseconds to seconds. We explore the possibility of long GW transients with unknown waveforms lasting from many seconds to weeks. We propose a novel analysis technique to bridge the gap between short O(s) "burst" analyses and persistent stochastic analyses. Our technique utilizes frequency-time maps of GW strain cross-power between two spatially separated terrestrial GW detectors. The application of our cross-power statistic to searches for GW transients is framed as a pattern recognition problem, and we discuss several patternrecognition techniques. We demonstrate these techniques by recovering simulated GW signals in simulated detector noise. We also recover environmental noise artifacts, thereby demonstrating a novel technique for the identification of such artifacts in GW interferometers. We compare the efficiency of this framework to other techniques such as matched filtering.PACS numbers: 95.55.Ym

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All-Sky LIGO Search for Periodic Gravitational Waves in the Early Fifth-Science-Run Data

Cited by 84 publications

References 16 publications

All-sky search for periodic gravitational waves in the O1 LIGO data

All-sky search for periodic gravitational waves in the O1 LIGO data

Measuring neutron-star ellipticity with measurements of the stochastic gravitational-wave background

Long gravitational-wave transients and associated detection strategies for a network of terrestrial interferometers

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