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Published June 15, 2004 | Published
Journal Article Open

Analysis of LIGO data for gravitational waves from binary neutron stars

Abbott, B.
Abbott, R.
Adhikari, Rana X. ORCID icon
Ageev, A.
Allen, B.
Amin, R.
Anderson, S. B.
Anderson, W. G.
Araya, M.
Armandula, H.
Asiri, F.
Aufmuth, P.
Aulbert, C.
Babak, S.
Balasubramanian, R.
Ballmer, S.
Barish, B. C.
Barker, D.
Barker-Patton, C.
Barnes, M.
Barr, B.
Barton, M. A.
Bayer, K.
Beausoleil, R.
Belczynski, K.
Bennett, R.
Berukoff, S. J.
Betzwieser, J.
Bhawal, B.
Bilenko, I. A.
Billingsley, G. ORCID icon
Black, E.
Blackburn, K.
Bland-Weaver, B.
Bochner, B.
Bogue, L.
Bork, R.
Bose, S. ORCID icon
Brady, P. R. ORCID icon
Braginsky, V. B.
Brau, J. E.
Brown, D. A. ORCID icon
Brozek, S.
Bullington, A.
Buonanno, A.
Burgess, R.
Busby, D.
Butler, W. E.
Byer, R. L. ORCID icon
Cadonati, L.
Cagnoli, G.
Camp, J. B.
Cantley, C. A.
Cardenas, L.
Carter, K.
Casey, M. M.
Castiglione, J.
Chandler, A.
Chapsky, J.
Charlton, P.
Chatterji, S.
Chen, Y. ORCID icon
Chickarmane, V.
Chin, D.
Christensen, N.
Churches, D.
Colacino, C.
Coldwell, R.
Coles, M.
Cook, D.
Corbitt, T. ORCID icon
Coyne, D. ORCID icon
Creighton, J. D. E.
Creighton, T. D.
Crooks, D. R. M.
Csatorday, P.
Cusack, B. J.
Cutler, C.
D'Ambrosio, E.
Danzmann, K.
Davies, R.
Daw, E.
DeBra, D.
Delker, T.
DeSalvo, R.
Dhurandhar, S.
Díaz, M.
Ding, H.
Drever, R. W. P.
Dupuis, R. J.
Ebeling, C.
Edlund, J.
Ehrens, P.
Elliffe, E. J.
Etzel, T.
Evans, M.
Evans, T.
Fallnich, C.
Farnham, D.
Fejer, M. M. ORCID icon
Fine, M.
Finn, L. S.
Flanagan, E.
Freise, A. ORCID icon
Frey, R.
Fritschel, P.
Frolov, V.
Fyffe, M.
Ganezer, K. S.
Giaime, J. A.
Gillespie, A.
Goda, K.
González, G.
Goßler, S.
Grandclément, P.
Grant, A.
Gray, C.
Gretarsson, A. M.
Grimmett, D.
Grote, H.
Grunewald, S.
Guenther, M.
Gustafson, E.
Gustafson, R.
Hamilton, W. O.
Hammond, M.
Hanson, J.
Hardham, C.
Harry, G.
Hartunian, A.
Heefner, J.
Hefetz, Y.
Heinzel, G.
Heng, I. S.
Hennessy, M.
Hepler, N.
Heptonstall, A.
Heurs, M.
Hewitson, M.
Hindman, N.
Hoang, P.
Hough, J.
Hrynevych, M.
Hua, W.
Ingley, R.
Ito, M.
Itoh, Y.
Ivanov, A.
Jennrich, O.
Johnson, W. W.
Johnston, W.
Jones, L.
Jungwirth, D.
Kalogera, V. ORCID icon
Katsavounidis, E.
Kawabe, K.
Kawamura, S.
Kells, W.
Kern, J.
Khan, A.
Killbourn, S.
Killow, C. J.
Kim, C.
King, C.
King, P.
Klimenko, S.
Kloevekorn, P.
Koranda, S.
Kötter, K.
Kovalik, J.
Kozak, D. ORCID icon
Krishnan, B.
Landry, M.
Langdale, J.
Lantz, B.
Lawrence, R.
Lazzarini, A.
Lei, M.
Leonhardt, V.
Leonor, I.
Libbrecht, K. ORCID icon
Lindquist, P.
Liu, S.
Logan, J.
Lormand, M.
Lubinski, M.
Lück, H.
Lyons, T. T.
Machenschalk, B.
MacInnis, M.
Mageswaran, M.
Mailand, K.
Majid, W.
Malec, M.
Mann, F.
Marin, A.
Márka, S.
Maros, E.
Mason, J.
Mason, K.
Matherny, O.
Matone, L.
Mavalvala, N.
McCarthy, R.
McClelland, D. E.
McHugh, M.
McNamara, P.
Mendell, G.
Meshkov, S.
Messenger, C.
Mitrofanov, V. P.
Mitselmakher, G.
Mittleman, R.
Miyakawa, O.
Miyoki, S.
Mohanty, S.
Moreno, G.
Mossavi, K.
Mours, B.
Mueller, G. ORCID icon
Mukherjee, S.
Myers, J.
Nagano, S.
Nash, T.
Naundorf, H.
Nayak, R.
Newton, G.
Nocera, F.
Nutzman, P.
Olson, T.
O'Reilly, B.
Ottaway, D. J. ORCID icon
Ottewill, A.
Ouimette, D.
Overmier, H.
Owen, B. J.
Papa, M. A.
Parameswariah, C.
Parameswariah, V.
Pedraza, M.
Penn, S.
Pitkin, M.
Plissi, M.
Pratt, M.
Quetschke, V. ORCID icon
Raab, F.
Radkins, H.
Rahkola, R.
Rakhmanov, M.
Rao, S. R.
Redding, D.
Regehr, M. W.
Regimbau, T.
Reilly, K. T.
Reithmaier, K.
Reitze, D. H.
Richman, S.
Riesen, R.
Riles, K.
Rizzi, A.
Robertson, D. I.
Robertson, N. A.
Robison, L.
Roddy, S.
Rollins, J.
Romano, J. D.
Romie, J.
Rong, H.
Rose, D.
Rotthoff, E.
Rowan, S.
Rüdiger, A.
Russell, P.
Ryan, K.
Salzman, I.
Sanders, G. H.
Sannibale, V.
Sathyaprakash, B.
Saulson, P. R.
Savage, R.
Sazonov, A.
Schilling, R.
Schlaufman, K.
Schmidt, V.
Schofield, R.
Schrempel, M.
Schutz, B. F.
Schwinberg, P.
Scott, S. M.
Searle, A. C.
Sears, B.
Seel, S.
Sengupta, A. S.
Shapiro, C. A.
Shawhan, P.
Shoemaker, D. H.
Shu, Q. Z.
Sibley, A.
Siemens, X.
Sievers, L.
Sigg, D.
Sintes, A. M.
Skeldon, K.
Smith, J. R.
Smith, M. ORCID icon
Smith, M. R.
Sneddon, P.
Spero, R.
Stapfer, G.
Strain, K. A.
Strom, D.
Stuver, A.
Summerscales, T.
Sumner, M. C.
Sutton, P. J.
Sylvestre, J.
Takamori, A.
Tanner, D. B. ORCID icon
Tariq, H.
Taylor, I.
Taylor, R.
Thorne, K. S.
Tibbits, M.
Tilav, S.
Tinto, M. ORCID icon
Tokmakov, K. V.
Torres, C.
Torrie, C.
Traeger, S.
Traylor, G.
Tyler, W.
Ugolini, D.
Vallisneri, M. ORCID icon
van Putten, M.
Vass, S.
Vecchio, A. ORCID icon
Vorvick, C.
Vyachanin, S. P.
Wallace, L.
Walther, H.
Ward, H.
Ware, B.
Watts, K.
Webber, D.
Weidner, A.
Weiland, U.
Weiss, R.
Welling, H.
Wen, L.
Wen, S.
Whelan, J. T.
Whitcomb, S. E.
Whiting, B. F. ORCID icon
Willems, P. A.
Williams, P. R.
Williams, R. ORCID icon
Willke, B.
Wilson, A.
Winjum, B. J.
Winkler, W.
Wise, S.
Wiseman, A. G.
Woan, G.
Wooley, R.
Worden, J.
Yakushin, I.
Yamamoto, H.
Yoshida, S.
Zawischa, I.
Zhang, L. ORCID icon
Zotov, N.
Zucker, M. ORCID icon
Zweizig, J. ORCID icon
Weinstein, Alan J. ORCID icon
LIGO Scientific Collaboration

Abstract

We report on a search for gravitational waves from coalescing compact binary systems in the Milky Way and the Magellanic Clouds. The analysis uses data taken by two of the three LIGO interferometers during the first LIGO science run and illustrates a method of setting upper limits on inspiral event rates using interferometer data. The analysis pipeline is described with particular attention to data selection and coincidence between the two interferometers. We establish an observational upper limit of R<1.7x10^(2) per year per Milky Way Equivalent Galaxy (MWEG), with 90% confidence, on the coalescence rate of binary systems in which each component has a mass in the range 1-3 M☉.

Additional Information

© 2004 The American Physical Society. Received 6 October 2003; published 2 June 2004. The authors gratefully acknowledge the support of the United States National Science Foundation for the construction and operation of the LIGO Laboratory and the Particle Physics and Astronomy Research Council of the United Kingdom, the Max-Planck-Society and the State of Niedersachsen/Germany for support of the construction and operation of the GEO600 detector. The authors also gratefully acknowledge the support of the research by these agencies and by the Australian Research Council, the Natural Sciences and Engineering Research Council of Canada, the Council of Scientific and Industrial Research of India, the Department of Science and Technology of India, the Spanish Ministerio de Ciencia y Tecnologia, the John Simon Guggenheim Foundation, the David and Lucile Packard Foundation, the Research Corporation, and the Alfred P. Sloan Foundation.

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