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Published April 15, 2004 | Published
Journal Article Open

Setting upper limits on the strength of periodic gravitational waves from PSR J1939+2134 using the first science data from the GEO 600 and LIGO detectors

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, É.
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

Data collected by the GEO 600 and LIGO interferometric gravitational wave detectors during their first observational science run were searched for continuous gravitational waves from the pulsar J1939+2134 at twice its rotation frequency. Two independent analysis methods were used and are demonstrated in this paper: a frequency domain method and a time domain method. Both achieve consistent null results, placing new upper limits on the strength of the pulsar's gravitational wave emission. A model emission mechanism is used to interpret the limits as a constraint on the pulsar's equatorial ellipticity.

Additional Information

© 2004 The American Physical Society. Received 17 September 2003; published 30 April 2004. The authors gratefully acknowledge the support of the U.S. 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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