Upper limit map of a background of gravitational waves

Abbott, B. P.; Abbott, R.; Adhikari, R. X.; Agresti, J.; Ajith, P.; Allen, B.; Amin, R.; Anderson, S. B.; Anderson, W. G.; Arain, M. A.; Araya, M. C.; Armandula, H.; Ashley, M. C. B.; Aston, S. M.; Aufmuth, P.; Aulbert, C.; Babak, S.; Ballmer, S. W.; Bantilan, H.; Barish, B. C.; Barker, C.; Barker, D.; Barr, B.; Barriga, P.; Barton, M. A.; Bayer, K.; Belczyński, Krzysztof; Betzwieser, J.; Beyersdorf, P. T.; Bhawal, B.; Bilenko, I. A.; Billingsley, G.; Biswas, R.; Black, E.; Blackburn, K.; Blackburn, L.; Blair, David; Bland, B.; Bogenstahl, J.; 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.; Bullington, A.; Bunkowski, A.; Buonanno, A.; Burmeister, O.; Busby, D.; Byer, Robert L.; Cadonati, L.; Cagnoli, G.; Camp, J. B.; Cannizzo, J. K.; Cannon, K. C.; Cantley, C. A.; Cao, Junwei; Cardenas, L.; Casey, M. M.; Castaldi, G.; Cepeda, C.; Chalkey, E.; Charlton, P.; Chatterji, S.; Chelkowski, S.; Chen, Y.; Chiadini, F.; Chin, D.; Chin, E.; Chow, J. H.; Christensen, N.; Clark, J. A.; Cochrane, P.; Cokelaer, Thomas; Colacino, C. N.; Coldwell, R. L.; Conte, R.; Cook, D.; Corbitt, T. R.; Coward, D. M.; Coyne, D. C.; Creighton, J. D. E.; Creighton, T. D.; Croce, R. P.; Crooks, D. R. M.; Cruise, A. M.; Cumming, A.; Dalrymple, James; D’Ambrosio, E.; Danzmann, K.; Davies, G. S.; DeBra, D.; Degallaix, J.; Degree, M.; Demma, T.; Dergachev, V.; Desai, S.; DeSalvo, R.; Dhurandhar, S.; Díaz, M. C.; Dickson, J.; Credico, A. Di; Diederichs, G.; Dietz, A.; Doomes, E. E.; Drever, R. W. P.; Dumas, J. C.; Dupuis, R. J.; Dwyer, J. G.; Ehrens, P.; Espinoza, Eduardo; Etzel, T.; Evans, M.; Evans, T. M.; Fairhurst, S.; Fan, Y.; Fazi, D.; Fejer, M. M.; Finn, L. S.; Fiumara, V.; Fotopoulos, N.; Franzen, A.; Franzen, K. Y.; Freise, A.; Frey, R.; Fricke, T. T.; Fritschel, P.; Frolov, V. V.; Fyffe, M.; Galdi, Vincenzo; Garofoli, J.; Gholami, I.; Giaime, J. A.; Giampanis, S.; Giardina, K. D.; Goda, Keisuke; Goetz, E.; Goggin, L. M.; González, Gabriela; Goßler, S.; Grant, A.; Gras, S.; Gray, C.; Gray, Malcolm B.; Greenhalgh, J.; Gretarsson, A. M.; Grosso, R.; Grote, H.; Grünewald, S.; Guenther, M.; Gustafson, R.; Hage, B.; Hammer, D. A.; Hanna, C.; Hanson, J.; Harms, J.; Harry, G. M.; Harstad, E. D.; Hayler, T.; Heefner, J.; Heng, I. S.; Heptonstall, A.; Heurs, M.; Hewitson, M.; Hild, S.; Hirose, E.; Hoak, D.; Hosken, D. J.; Hough, J.; Howell, E. J.; Hoyland, D.; Huttner, S. H.; Ingram, D. R.; Innerhofer, E.; Ito, Masahiro; Itoh, Y.; Ivanov, A.; Jackrel, D.; Johnson, B.; Johnson, W. W.; Jones, D. I.; Jones, Gareth; Jones, R.; Li, Ju; Kalmus, P.; Kalogera, V.; Kasprzyk, Dimitri; Katsavounidis, E.; Kawabe, K.; Kawamura, Seiji; Kawazoe, F.; Kells, W.; Keppel, D. G.; Khalili, F. Y.; Kim, C.; King, P. J.; Kissel, J. S.; Klimenko, S.; Kokeyama, K.; Kondrashov, V.; Kopparapu, R.; Kozak, D. B.; Krishnan, B.; Kwee, P.; Lam, Ping Koy; Landry, M.; Lantz, B.; Lazzarini, A.; Lee, B.; Lei, M.; Leiner, J.; Leonhardt, V.; Leonor, I.; Libbrecht, Kenneth G.; Lindquist, P.; Lockerbie, N. A.; Longo, M.; Lormand, M.; Łubiński, M.; Lück, H.; Machenschalk, B.; MacInnis, M.; Mageswaran, M.; Mailand, K.; Malec, M.; Mandic, V.; Maranò, Stefano; Márka, S.; Markowitz, J.; Maros, E.; Martin, I. W.; Marx, J. N.; Mason, K.; Matone, L.; Matta, Vincenzo; Mavalvala, N.; McCarthy, R.; McClelland, D. E.; McGuire, S. C.; McHugh, M.; McKenzie, Kirk; McNabb, J. W.; McWilliams, S. T.; Meier, T.; Melissinos, A. C.; Mendell, G.; Mercer, R. A.; Meshkov, S.; Messaritaki, E.; Messenger, C.; Meyers, D.; Михайлов, Е. Е.; Mitra, S.; Mitrofanov, V. P.; Mitselmakher, G.; Mittleman, R.; Miyakawa, O.; Mohanty, Soumya D.; Moreno, G.; Mossavi, K.; Mow–Lowry, C. M.; Moylan, A.; Mudge, D.; Mueller, G.; Mukherjee, Sajal; Müller‐Ebhardt, H.; Münch, J.; Murray, P. G.; Myers, E.; Myers, J.; Newton, G.; Nishizawa, A.; Numata, Kenji; O’Reilly, B.; O’Shaughnessy, R.; Ottaway, D. J.; Overmier, H.; Owen, B. J.; Pan, Y.; Papa, M. A.; Parameshwaraiah, V.; Patel, P.; Pedraza, M.; Penn, S.; Pierro, V.; Pinto, I. M.; Pitkin, M.; Pletsch, H. J.; Plissi, M. V.; Postiglione, F.; Prix, R.; Quetschke, V.; Raab, F. J.; Rabeling, D. S.; Radkins, H.; Rahkola, R.; Rainer, N.; Rakhmanov, M.; Rawlins, K.; Ray‐Majumder, S.; Re, V.; Rehbein, H.; Reid, S.; Reitze, D. H.; Ribichini, L.; Riesen, Rolf; Riles, K.; Rivera, B.; Robertson, N. A.; Robinson, C.; Robinson, E. L.; Roddy, S.; Rodríguez, A.; Rogan, A. M.; Rollins, J. G.; Romano, J. D.; Romie, J. H.; Route, R.; Rowan, S.; Rüdiger, A.; Ruet, Laurent; Russell, P.; Ryan, K.; Sakata, S.; Samidi, M.; Jordana, L. Sancho De La; Sandberg, V.; Sannibale, V.; Saraf, S.; Sarin, P.; Sathyaprakash, B. S.; Sato, S.; Saulson, P. R.; Savage, R. L.; Savov, P.; Schediwy, Sascha; Schilling, R.; Schnabel, R.; Schofield, R. M. S.; Schutz, B. F.; Schwinberg, P.; Scott, S. M.; Searle, A. C.; Sears, B.; Seifert, F.; Sellers, D.; Sengupta, A. S.; Shawhan, P.; Shoemaker, D. H.; Sibley, A.; Sidles, John A.; Siemens, X.; Sigg, D.; Sinha, S.; Sintes, A. M.; Slagmolen, B. J. J.; Slutsky, J.; Smith, J. R.; Smith, M. R.; Somiya, K.; Strain, K. A.; Strom, D.; Stuver, A. L.; Summerscales, T. Z.; Sun, Ke‐Xun; Sung, M.; Sutton, P. J.; Takahashi, Hideya; Tanner, D. B.; Tarallo, M.; 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.; Tyler, W.; Ugolini, D.; Ungarelli, C.; Urbánek, Karel; Vahlbruch, H.; Vallisneri, Michele; Broeck, C. Van Den; Varvella, M.; Vass, S.; Vecchio, A.; Veitch, J.; Veitch, P. J.; Villar, A.; Vorvick, C.; Vyachanin, S. P.; Waldman, S. J.; Wallace, L.; Ward, H.; Ward, R. L.; Watts, K.; Webber, David; Weidner, A.; Weinert, M.; Weinstein, A. J.; Weiss, R.; Wen, S.; Wette, K.; Whelan, J. T.; Whitbeck, D. M.; Whitcomb, S. E.; Whiting, B. F.; Wilkinson, C.; Willems, P. A.; Williams, L.; Willke, B.; Wilmut, Ian; Winkler, W.; Wipf, C. C.; Wise, S.; Wiseman, Alan; Woan, G.; Woods, D.; Wooley, R.; Worden, J.; Wu, W.; Yakushin, I.; Yamamoto, H.; Yan, Z.; Yoshida, S.; Yunes, Nicolás; Zanolin, M.; Zhang, J.; Zhang, L.; Zhao, C.; Zotov, N.; Zucker, M. E.; Mühlen, Heribert; Zweizig, J.

doi:10.1103/physrevd.76.082003

Cited by 123 publications

(176 citation statements)

References 11 publications

(16 reference statements)

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“…The LSC uses both fully coherent [1][2][3][4][5] and semi-coherent [6][7][8][9] methods to search for periodic gravitational waves. Semi-coherent methods are computationally cheaper than coherent methods, but coherent methods can achieve greater sensitivity if the cost is feasible.…”

Section: Search Methodsmentioning

confidence: 99%

“…The LIGO Scientific Collaboration (LSC) has so far published three types of searches for periodic gravitational waves (GWs): searches for known non-accreting pulsars [1][2][3][4], for the non-pulsing low-mass x-ray binary Sco X-1 [5,6] and all-sky searches for as yet unknown neutron stars [5,[7][8][9]. The first and last types of searches are approaching the indirect upper limits on gravitational wave emission inferred from the observed spindowns (spin frequency derivatives) of pulsars and supernova-based estimates of the neutron star population of the galaxy [5].…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Searching for gravitational waves from Cassiopeia A with LIGO

Wette

Owen

Allen

et al. 2008

Class. Quantum Grav.

156

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We describe a search underway for periodic gravitational waves from the central compact object in the supernova remnant Cassiopeia A. The object is the youngest likely neutron star in the Galaxy. Its position is well known, but the object does not pulse in any electromagnetic radiation band and thus presents a challenge in searching the parameter space of frequency and frequency derivatives. We estimate that a fully coherent search can, with a reasonable amount of time on a computing cluster, achieve a sensitivity at which it is theoretically possible (though not likely) to observe a signal even with the initial LIGO noise spectrum. Cassiopeia A is only the second object after the Crab pulsar for which this is true. The search method described here can also obtain interesting results for similar objects with current LIGO sensitivity.

show abstract

Section: Search Methodsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Searching for gravitational waves from Cassiopeia A with LIGO

Wette

Owen

Allen

et al. 2008

Class. Quantum Grav.

156

View full text Add to dashboard Cite

show abstract

“…S5 saw milestones including limits on GWs from the Crab pulsar surpassing those inferred from the Crab's spindown [11], as well as limits on the isotropic SGWB surpassing indirect limits from big bang nucleosynthesis and the cosmic microwave background [12]. This work builds on [12,13].…”

Section: à23mentioning

confidence: 99%

Directional Limits on Persistent Gravitational Waves Using LIGO S5 Science Data

Abadie¹,

Abbott²,

Abbott³

et al. 2011

Phys. Rev. Lett.

Self Cite

114

152

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“…Backgrounds from pulsars, magnetars, core-collapse supernovae, and various physical processes in the early universe are all possible as well [4][5][6], but their expected amplitudes are not as well constrained as the expected background due to compact binary coalescences. The potential for the contamination of searches for a SGWB is strong due to potential correlated environmental noise between detectors [5,[7][8][9][10][11], which would result in a systematic error in the searches. A related concern exists in searches for transient sources of gravitational waves, such as due to correlated magnetic transients from storms [12].…”

Section: Introductionmentioning

confidence: 99%

Measurement and subtraction of Schumann resonances at gravitational-wave interferometers

Coughlin¹,

Cirone²,

Meyers³

et al. 2018

Phys. Rev. D

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Correlated magnetic noise from Schumann resonances threatens to contaminate the observation of a stochastic gravitational-wave background in interferometric detectors. In previous work, we reported on the first effort to eliminate global correlated noise from the Schumann resonances using Wiener filtering, demonstrating as much as a factor of two reduction in the coherence between magnetometers on different continents. In this work, we present results from dedicated magnetometer measurements at the Virgo and KAGRA sites, which are the first results for subtraction using data from gravitational-wave detector sites. We compare these measurements to a growing network of permanent magnetometer stations, including at the LIGO sites. We show the effect of mutual magnetometer attraction, arguing that magnetometers should be placed at least one meter from one another. In addition, for the first time, we show how dedicated measurements by magnetometers near to the interferometers can reduce coherence to a level consistent with uncorrelated noise, making a potential detection of a stochastic gravitational-wave background possible.

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Upper limit map of a background of gravitational waves

Cited by 123 publications

References 11 publications

Searching for gravitational waves from Cassiopeia A with LIGO

Searching for gravitational waves from Cassiopeia A with LIGO

Directional Limits on Persistent Gravitational Waves Using LIGO S5 Science Data

Measurement and subtraction of Schumann resonances at gravitational-wave interferometers

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