Home News About Us Contact Contributors Disclaimer Privacy Policy Help FAQ

Home
Search
Quick Search
Advanced
Fulltext
Browse
Collections
Persons
My eDoc
Session History
Login
Name:
Password:
Documentation
Help
Support Wiki
Direct access to
document ID:


          Institute: MPI für Gravitationsphysik     Collection: Laser Interferometry & Gravitational Wave Astronomy     Display Documents



  history
ID: 372162.0, MPI für Gravitationsphysik / Laser Interferometry & Gravitational Wave Astronomy
All-sky search for periodic gravitational waves in LIGO S4 data
Authors:Abbott, B.; Abbott, R.; Adhikari, R.; Agresti, Juri; Ajith, P.; Allen, Bruce; Amin, R.; Anderson, S. B.; Anderson, W. G.; Arain, M.; Araya, M.; Armandula, H.; Ashley, M.; Aston, S.; Aufmuth, Peter; Aulbert, Carsten; Babak, Stanislav; Ballmer, S.; Bantilan, H.; Barish, B. C.; Barker, C.; Barker, D.; Barr, B. W.; Barriga, P.; Barton, M. A.; Bayer, K.; Belczynski, K.; Betzwieser, J.; Beyersdorf, P. T.; Bhawal, B.; Bilenko, I. A.; Billingsley, G.; Biswas, R.; Black, E.; Blackburn, K.; Blackburn, L.; Blair, D.; Bland, B.; Bogenstahl, Johanna; Bogue, L.; Bork, Rolf; Boschi, V.; Bose, Sukanta; Brady, Patrick R.; Braginsky, V. B.; Brau, J. E.; Brinkmann, Marc; Brooks, A.; Brown, Duncan A.; Bullington, A.; Bunkowski, Alexander; Buonanno, Alessandra; Burmeister, Oliver; Busby, D.; Byer, R. L.; Cadonati, L.; Cagnoli, G.; Camp, J. B.; Cannizzo, J.; Cannon, K.; Cantley, C. A.; Cao, J.; Cardenas, L.; Casey, Morag M.; Castaldi, G.; Cepeda, C.; Chalkley, E.; Charlton, P.; Chatterji, S.; Chelkowski, Simon; Chen, Yanbei; Chiadini, F.; Chin, D.; Chin, E.; Chow, J.; Christensen, Nelson; Clark, James; Cochrane, Paul; Cokelaer, T.; Colacino, Carlo Nicola; Coldwell, R.; Conte, R.; Cook, D.; Corbitt, Thomas; Coward, D.; Coyne, D.; Creighton, Jolien D. E.; Creighton, Teviet D.; Croce, R. P.; Crooks, D. R. M.; Cruise, A. M.; Cumming, A.; Dalrymple, J.; D'Ambrosio, Erika; Danzmann, Karsten; Davies, G.; DeBra, D.; Degallaix, Jerome; Degree, M.; Demma, T.; Dergachev, V.; Desai, S.; DeSalvo, R.; Dhurandhar, Sanjeev; Diaz, M.; Dickson, J.; Di Credico, A.; Diederichs, G.; Dietz, A.; Doomes, E. E.; Drever, R. W. P.; Dumas, J. C.; Dupuis, R. J.; Dwyer, J. G.; Ehrens, P.; Espinoza, E.; Etzel, T.; Evans, M.; Evans, T.; Fairhurst, Stephen; Fan, Y.; Fazi, D.; Fejer, M. M.; Finn, Lee S.; Fiumara, V.; Fotopoulos, N.; Franzen, Alexander; Franzen, K. Y.; Freise, Andreas; Frey, R.; Fricke, T.; Fritschel, P.; Frolov, V. V.; Fyffe, M.; Galdi, V.; Garofoli, J.; Gholami, Iraj; Giaime, J. A.; Giampanis, S.; Giardina, K. D.; Goda, Keisuke; Goetz, E.; Goggin, Lisa M.; Gonzalez, Gabriela; Gossler, Stefan; Grant, A.; Gras, S.; Gray, C.; Gray, M.; Greenhalgh, J.; Gretarsson, A. M.; Grosso, R.; Grote, Hartmut; Grunewald, Steffen; Guenther, Mathias; Gustafson, R.; Hage, Boris; Hammer, D.; Hanna, Chad; Hanson, J.; Harms, Jan; Harry, G.; Harstad, E.; Hayler, T.; Heefner, J.; Heng, Ik Siong; Heptonstall, A.; Heurs, Michele; Hewitson, Martin; Hild, Stefan; Hirose, E.; Hoak, D.; Hosken, D.; Hough, J.; Howell, E.; Hoyland, D.; Huttner, S. H.; Ingram, D.; Innerhofer, Edith; Ito, M.; Itoh, Yousuke; Ivanov, A.; Jackrel, D.; Johnson, B.; Johnson, W. W.; Jones, David Ian; Jones, G.; Jones, R.; Ju, L.; Kalmus, P.; Kalogera, V.; Kasprzyk, D.; Katsavounidis, E.; Kawabe, Keita; Kawamura, Seiji; Kawazoe, Fumiko; Kells, W.; Keppel, D. G.; Khalili, F. Y.; Kim, C.; King, Peter; Kissel, J. S.; Klimenko, S.; Kokeyama, Keiko; Kondrashov, V.; Kopparapu, R. K.; Kozak, D.; Krishnan, Badri; Kwee, Patrick; Lam, Ping Koy; Landry, Michael; Lantz, B.; Lazzarini, Albert; Lee, Bum-Hoon; Lei, M.; Leiner, J.; Leonhardt, Volker; Leonor, I.; Libbrecht, K.; Lindquist, P.; Lockerbie, N. A.; Longo, M.; Lormand, M.; Lubinski, M.; Lück, Harald; Machenschalk, Bernd; MacInnis, M.; Mageswaran, M.; Mailand, K.; Malec, Michaela; Mandic, V.; Marano, S.; Marka, S.; Markowitz, J.; Maros, E.; Martin, Ian; Marx, J. N.; Mason, K.; Matone, L.; Matta, V.; Mavalvala, N.; McCarthy, R.; McClelland, D. E.; McGuire, S. C.; McHugh, Martin; McKenzie, K.; McNabb, J. W. C.; McWilliams, S.; Meier, Tobias; Melissinos, A.; Mendell, Gregory; Mercer, R. A.; Meshkov, S.; Messenger, Christopher; Meyers, D.; Mikhailov, E.; Mitra, S.; Mitrofanov, V. P.; Mitselmakher, G.; Mittleman, R.; Miyakawa, O.; Mohanty, Soumya; Moreno, G.; Mossavi, Kasem; MowLowry, C.; Moylan, A.; Mudge, D.; Müller, G.; Mukherjee, Soma; Müller-Ebhardt, Helge; Munch, J.; Murray, P.; Myers, E.; Myers, J.; Nash, T.; Newton, G.; Nishizawa, A.; Numata, K.; O'Reilly, B.; O'Shaughnessy, R.; Ottaway, D. J.; Overmier, H.; Owen, B. J.; Pan, Y.; Papa, Maria Alessandra; Parameshwaraiah, V.; Patel, P.; Pedraza, M.; Penn, S.; Pierro, V.; Pinto, I. M.; Pitkin, Matthew; Pletsch, Holger; Plissi, M. V.; Postiglione, F.; Prix, Reinhard; Quetschke, V.; Raab, F.; Rabeling, D.; Radkins, H.; Rahkola, R.; Rainer, N.; Rakhmanov, M.; Ramsunder, M.; Rawlins, K.; Ray-Majumder, S.; Re, V.; Rehbein, Henning; Reid, S.; Reitze, D. H.; Ribichini, L.; Riesen, R.; Riles, K.; Rivera, B.; Robertson, N. A.; Robinson, C.; Robinson, E. L.; Roddy, S.; Rodriguez, A.; Rogan, A. M.; Rollins, J.; Romano, J. D.; Romie, J.; Route, R.; Rowan, S.; Rüdiger, Albrecht; Ruet, L.; Russell, P.; Ryan, K.; Sakata, S.; Samidi, M.; de la Jordana, L. S.; Sandberg, V.; Sannibale, V.; Saraf, S.; Sarin, P.; Sathyaprakash, B. S.; Sato, S.; Saulson, P. R.; Savage, R.; Savov, P.; Schediwy, S.; Schilling, Roland; Schnabel, Roman; Schofield, R.; Schutz, Bernard F.; Schwinberg, P.; Scott, S. M.; Searle, A. C.; Sears, B.; Seifert, Frank; Sellers, D.; Sengupta, A. S.; 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.; Somiya, Kentaro; Strain, Kenneth A.; Strom, D. M.; Stuver, A.; Summerscales, T. Z.; Sun, K. X.; Sung, M.; Sutton, P. J.; Takahashi, H.; Tanner, D. B.; Tarallo, M.; Taylor, R.; Taylor, R.; Thacker, J.; Thorne, K. A.; Thorne, K. S.; Thüring, Andre; Tokmakov, K. V.; Torres, C.; Torrie, C.; Traylor, G.; Trias, M.; Tyler, W.; Ugolini, D.; Ungarelli, C.; Urbanek, K.; Vahlbruch, Henning; Vallisneri, M.; van den Broeck, C.; Varvella, M.; Vass, S.; Vecchio, A.; Veitch, J.; Veitch, P.; Villar, A.; Vorvick, C.; Vyachanin, S. P.; Waldman, S. J.; Wallace, L.; Ward, H.; Ward, R.; Watts, K.; Webber, D.; Weidner, Andreas; Weinert, Michael; Weinstein, A.; Weiss, R.; Wen, S.; Wette, Karl; Whelan, J. T.; Whitbeck, D. M.; Whitcomb, S. E.; Whiting, B. F.; Wilkinson, C.; Willems, P. A.; Williams, L.; Willke, Benno; Wilmut, I.; Winkler, Walter; Wipf, C. C.; Wise, S.; Wiseman, A. G.; Woan, G.; Woods, D.; Wooley, R.; Worden, J.; Wu, W.; Yakushin, I.; Yamamoto, H.; Yan, Z.; Yoshida, S.; Yunes, N.; Zanolin, M.; Zhang, J.; Zhang, L.; Zhao, C.; Zotov, N.; Zucker, M.; zur Mühlen, H.; Zweizig, J.
Date of Publication (YYYY-MM-DD):2008-01
Title of Journal:Physical Review D
Volume:77
Issue / Number:2
Sequence Number of Article:022001
Review Status:not specified
Audience:Not Specified
Abstract / Description:We report on an all-sky search with the LIGO detectors for periodic gravitational waves in the frequency range 50-1000 Hz and with the frequency's time derivative in the range -1 x 10(-8) Hz s(-1) to zero. Data from the fourth LIGO science run (S4) have been used in this search. Three different semicoherent methods of transforming and summing strain power from short Fourier transforms (SFTs) of the calibrated data have been used. The first, known as StackSlide, averages normalized power from each SFT. A "weighted Hough" scheme is also developed and used, which also allows for a multi-interferometer search. The third method, known as PowerFlux, is a variant of the StackSlide method in which the power is weighted before summing. In both the weighted Hough and PowerFlux methods, the weights are chosen according to the noise and detector antenna-pattern to maximize the signal-to-noise ratio. The respective advantages and disadvantages of these methods are discussed. Observing no evidence of periodic gravitational radiation, we report upper limits; we interpret these as limits on this radiation from isolated rotating neutron stars. The best population-based upper limit with 95% confidence on the gravitational-wave strain amplitude, found for simulated sources distributed isotropically across the sky and with isotropically distributed spin axes, is 4.28 x 10(-24) (near 140 Hz). Strict upper limits are also obtained for small patches on the sky for best-case and worst-case inclinations of the spin axes.
External Publication Status:published
Document Type:Article
Communicated by:Karsten Danzmann
Affiliations:MPI für Gravitationsphysik/Laser Interferometry & Gravitational Wave Astronomy
MPI für Gravitationsphysik/Teilinstitut Hannover
MPI für Gravitationsphysik/Observational Relativity and Cosmology
MPI für Gravitationsphysik/Astrophysical Relativity
Identifiers:ISI:000252864000005 [ID No:1]
ISSN:1550-7998 [ID No:2]
URL:http://link.aps.org/abstract/PRD/v77/e022001
DOI:10.1103/PhysRevD.77.022001
LOCALID:arXiv:0708.3818v1 [gr-qc]
Full Text:
You have privileges to view the following file(s):
0708.3818v1.pdf  [1,00 Mb] [Comment:arXiv:0708.3818v1 [gr-qc]]  
 
372162.pdf  [6,00 Mb] [Comment:Online Journal]  
 
The scope and number of records on eDoc is subject to the collection policies defined by each institute - see "info" button in the collection browse view.