Upper limit map of a background of gravitational waves

B. Abbott, R. Abbott, R. Adhikari, J. Agresti, P. Ajith, B. Allen, R. Amin, S.B. Anderson, W.G. Anderson, M. Arain, M. Araya, H. Armandula, M. Ashley, S. Aston, P. Aufmuth, C. Aulbert, S. Babak, S. Ballmer, H. Bantilan, B.C. BarishC. Barker, D. Barker, B. Barr, Pablo Barriga, M.A. Barton, K. Bayer, K. Belczynski, J. Betzwieser, P.T. Beyersdorf, B. Bhawal, I.A. Bilenko, G. Billingsley, R. Biswas, E. Black, K. Blackburn, L. Blackburn, David Blair, B. Bland, J. Bogenstahl, L. Bogue, R. Bork, V. Boschi, S. Bose, P.R. Brady, V.B. Braginsky, J.E. Brau, M. Brinkmann, A. Brooks, D.A. Brown, A. Bullington, A. Bunkowski, A. Buonanno, O. Burmeister, D. Busby, R.L. Byer, L. Cadonati, G. Cagnoli, J.B. Camp, J. Cannizzo, K. Cannon, C.A. Cantley, J. Cao, L. Cardenas, M.M. Casey, G. Castaldi, C. Cepeda, E. Chalkey, P. Charlton, S. Chatterji, S. Chelkowski, Y. Chen, F. Chiadini, D. Chin, E. Chin, J. Chow, N. Christensen, J. Clark, P. Cochrane, T. Cokelaer, C.N. Colacino, R. Coldwell, R. Conte, D. Cook, T. Corbitt, David Coward, D. Coyne, J.D.E. Creighton, T.D. Creighton, R.P. Croce, D.R.M. Crooks, A.M. Cruise, A. Cumming, J. Dalrymple, E. D'Ambrosio, K. Danzmann, G. Davies, D. Debra, Jerome Degallaix, M. Degree, T. Demma, V. Dergachev, S. Desai, R. Desalvo, S. Dhurandhar, M. Diaz, J. Dickson, A. Di Credico, G. Diederichs, A. Dietz, E.E. Doomes, R.W.P. Drever, Jean-Charles Dumas, R.J. Dupuis, J.G. Dwyer, P. Ehrens, E. Espinoza, T. Etzel, M. Evans, T. Evans, S. Fairhurst, Y. Fan, D. Fazi, M.M. Fejer, L.S. Finn, V. Fiumara, N. Fotopoulos, A. Franzen, K.Y. Franzen, A. Freise, R. Frey, T. Fricke, P. Fritschel, V.V. Frolov, M. Fyffe, V. Galdi, J. Garofoli, I. Gholami, J.A. Giaime, S. Giampanis, K.D. Giardina, K. Goda, E. Goetz, L.M. Goggin, G. Gonzalez, S. Gossler, A. Grant, Slawomir Gras, C. Gray, M. Gray, J. Greenhalgh, A.M. Gretarsson, R. Grosso, H. Grote, S. Grunewald, M. Guenther, R. Gustafson, B. Hage, D. Hammer, C. Hanna, J. Hanson, J. Harms, G. Harry, E. Harstad, T. Hayler, J. Heefner, I.S. Heng, A. Heptonstall, M. Heurs, M. Hewitson, S. Hild, E. Hirose, D. Hoak, D. Hosken, J. Hough, Eric Howell, D. Hoyland, S.H. Huttner, D. Ingram, E. Innerhofer, M. Ito, Y. Itoh, A. Ivanov, D. Jackrel, B. Johnson, W.W. Johnson, D.I. Jones, G. Jones, R. Jones, Li Ju, P. Kalmus, V. Kalogera, D. Kasprzyk, E. Katsavounidis, K. Kawabe, S. Kawamura, F. Kawazoe, W. Kells, D.G. Keppel, F.Y. Khalili, C. Kim, P. King, J.S. Kissel, S. Klimenko, K. Kokeyama, V. Kondrashov, R.K. Kopparapu, D. Kozak, B. Krishnan, P. Kwee, P.K. Lam, M. Landry, B. Lantz, A. Lazzarini, B.H. Lee, M. Lei, J. Leiner, V. Leonhardt, I. Leonor, K. Libbrecht, P. Lindquist, N.A. Lockerbie, M. Longo, M. Lormand, M. Lubinski, H. Luck, B. Machenschalk, M. Macinnis, M. Mageswaran, K. Mailand, M. Malec, V. Mandic, S. Marano, S. Marka, J. Markowitz, E. Maros, I. Martin, J.N. Marx, K. Mason, L. Matone, V. Matta, N. Mavalvala, R. Mccarthy, D.E. Mcclelland, S.C. Mcguire, M. Mchugh, K. Mckenzie, J.W.C. Mcnabb, S. Mcwilliams, T. Meier, A. Melissinos, G. Mendell, R.A. Mercer, S. Meshkov, E. Messaritaki, C.J. Messenger, D. Meyers, E. Mikhailov, S. Mitra, V.P. Mitrofanov, G. Mitselmakher, R. Mittleman, O. Miyakawa, S. Mohanty, G. Moreno, K. Mossavi, C. Mowlowry, A. Moylan, D. Mudge, G. Mueller, S. Mukherjee, H. Muller-Ebhardt, J. Munch, P. Murray, E. Myers, J. Myers, G. Newton, A. Nishizawa, K. Numata, B. O'Reilly, R. O'Shaughnessy, D.J. Ottaway, H. Overmier, B.J. Owen, Y. Pan, M.A. Papa, V. Parameshwaraiah, P. Patel, M. Pedraza, S. Penn, V. Pierro, I.M. Pinto, M. Pitkin, H. Pletsch, M.V. Plissi, F. Postiglione, R. Prix, V. Quetschke, F. Raab, D. Rabeling, H. Radkins, R. Rahkola, N. Rainer, M. Rakhmanov, K. Rawlins, S. Ray-Majumder, V. Re, H. Rehbein, S. Reid, D.H. Reitze, L. Ribichini, R. Riesen, K. Riles, B. Rivera, N.A. Robertson, C. Robinson, E.L. Robinson, S. Roddy, A. Rodriguez, A.M. Rogan, J. Rollins, J.D. Romano, J. Romie, R. Route, S. Rowan, A. Rudiger, L. Ruet, P. Russell, K. Ryan, S. Sakata, M. Samidi, L. Sancho De La Jordana, V. Sandberg, V. Sannibale, S. Saraf, P. Sarin, B.S. Sathyaprakash, S. Sato, P.R. Saulson, R. Savage, P. Savov, Sascha Schediwy, R. Schilling, R. Schnabel, R. Schofield, B.F. Schutz, P. Schwinberg, S.M. Scott, A.C. Searle, B. Sears, F. Seifert, D. Sellers, A.S. Sengupta, P. Shawhan, D.H. Shoemaker, A. Sibley, J.A. Sidles, X. Siemens, D. Sigg, S. Sinha, A.M. Sintes, B.J.J. Slagmolen, J. Slutsky, J.R. Smith, M.R. Smith, K. Somiya, K.A. Strain, D.M. Strom, A. Stuver, T.Z. Summerscales, K.X. Sun, M. Sung, P.J. Sutton, H. Takahashi, D.B. Tanner, M. Tarallo, R. Taylor, J. Thacker, K.A. Thorne, K.S. Thorne, A. Thuring, K.V. Tokmakov, C. Torres, C. Torrie, G. Traylor, M. Trias, W. Tyler, D. Ugolini, C. Ungarelli, K. Urbanek, H. Vahlbruch, M. Vallisneri, C. Van Den Broeck, M. Varvella, S. Vass, A. Vecchio, J. Veitch, P. Veitch, A. Villar, C. Vorvick, S.P. Vyachanin, S.J. Waldman, L. Wallace, H. Ward, R. Ward, K. Watts, D. Webber, A. Weidner, M. Weinert, A. Weinstein, R. Weiss, S. Wen, K. Wette, J.T. Whelan, D.M. Whitbeck, S.E. Whitcomb, B.F. Whiting, C. Wilkinson, P.A. Willems, L. Williams, B. Willke, I. Wilmut, W. Winkler, C.C. Wipf, S. Wise, A.G. Wiseman, G. Woan, D. Woods, R. Wooley, J. Worden, W. Wu, I. Yakushin, H. Yamamoto, Z. Yan, S. Yoshida, N. Yunes, M. Zanolin, J. Zhang, L. Zhang, Chunnong Zhao, N. Zotov, M. Zucker, H. Zur Muhlen, J. Zweizig

Research output: Contribution to journalArticle

80 Citations (Scopus)

Abstract

We searched for an anisotropic background of gravitational waves using data from the LIGO S4 science run and a method that is optimized for point sources. This is appropriate if, for example, the gravitational wave background is dominated by a small number of distinct astrophysical sources. No signal was seen. Upper limit maps were produced assuming two different power laws for the source strain power spectrum. For an f(-3) power law and using the 50 Hz to 1.8 kHz band the upper limits on the source strain power spectrum vary between 1.2 x 10(-48) Hz(-1) (100 Hz/f)(3) and 1.2 x 10(-47) Hz(-1) (100 Hz/f)(3), depending on the position in the sky. Similarly, in the case of constant strain power spectrum, the upper limits vary between 8.5 x 10(-49) Hz(-1) and 6.1 x 10(-48) Hz(-1). As a side product a limit on an isotropic background of gravitational waves was also obtained. All limits are at the 90% confidence level. Finally, as an application, we focused on the direction of Sco-X1, the brightest low-mass x-ray binary. We compare the upper limit on strain amplitude obtained by this method to expectations based on the x-ray flux from Sco-X1.
Original languageEnglish
Pages (from-to)082003-1-11
JournalPhysical Review D
Volume76
Issue number8
DOIs
Publication statusPublished - 2007

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