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@Article{AasiAAAAAAAAAAAAAAAAACAAAAAAAAAAAAAAABBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBCCBCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCDDDDDDDDDDDDDDRDDDDDDDDDDDDDDDDDDDDDDDDDDDDEEEEEEEEEEEEFFFFFFFFFFFFFFFFFFFFFFFFFFFFFFFFFFFFFGGGGGGGGGGGGGGGGGGGGGGGGGGGGGGGGGGGGGGGGGGGHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHIIIIIIIJJJJJJJJJJJJHKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKLLLLLLLLLLLLLLLLLLLLLLLLLLLLLLLLLLLLLLLLLLLLLMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMNKNNNNNNNNNNNNNNNOOOOOOOOOLOOOOOOOPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPQQQRRRRRRRRRRRRRRRRRRRRRRRRRRRRRRRRRRRRRRSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSTTTTTTBTTTTTTTTTTTTTTTTTUUVVVVVPSHVVVVVVVVVVVVVVVVVVVVVVVWWWWWWWWWWWWWWWWWWWWWWWWWWWWWWWWWWWWWWWWWWWYYYYYYYYYZZZZZZZZZZZCC:2013:DiSeCo,
               author = "Aasi, J. and Abadie, J. and Abbott, B. P. and Abbott, R. and 
                         Abbott, T. and Abernathy, M. R. and Accadia, T. and Acernese, F. 
                         and Adams, C. and Adams, T. and Adhikari, R. X. and Affeldt, C. 
                         and Agathos, M. and Aggarwal, N. and Aguiar, O. D. and Ajith, P. 
                         and Allen, B. and Allocca, A. and Ceron, E. Amador and Amariutei, 
                         D. and Anderson, R. A. and Anderson, S. B. and Anderson, W. G. and 
                         Arai, K. and Araya, M. C. and Arceneaux, C. and Areeda, J. and 
                         Ast, S. and Aston, S. M. and Astone, P. and Aufmuth, P. and 
                         Aulbert, C. and Austin, L. and Aylott, B. E. and Babak, S. and 
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                         C. and Barker, D. and Barnum, S. H. and Barone, F. and Barr, B. 
                         and Barsotti, L. and Barsuglia, M. and Barton, M. A. and Bartos, 
                         I. and Bassiri, R. and Basti, A. and Batch, J. and Bauchrowitz, J. 
                         and Bauer, Th. S. and Bebronne, M. and Behnke, B. and Bejger, M. 
                         and Beker, M. G. and Bell, A. S. and Bell, C. and Belopolski, I. 
                         and Bergmann, G. and Berliner, J. M. and Bertolini, A. and Bessis, 
                         D. and Betzwieser, J. and Beyersdorf, P. T. and Bhadbhade, T. and 
                         Bilenko, I. A. and Billingsley, G. and Birch, J. and Bitossi, M. 
                         and Bizouard, M. A. and Black, E. and Blackburn, J. K. and 
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                         T. P. and Boer, M. and Bogan, C. and Bond, C. and Bondu, F. and 
                         Bonelli, L. and Bonnand, R. and Bork, R. and Born, M. and Bose, S. 
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                         Zweizig, J. and Collaboration, LIGO Sci and Collaboration, Virgo",
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                         and {} and {} and {} and {Instituto Nacional de Pesquisas 
                         Espaciais (INPE)}",
                title = "Directed search for continuous gravitational waves from the 
                         Galactic center",
              journal = "Physical Review D",
                 year = "2013",
               volume = "88",
               number = "10",
                month = "Nov.",
             keywords = "gravitational waves, galactic center, LIGO.",
             abstract = "We present the results of a directed search for continuous 
                         gravitational waves from unknown, isolated neutron stars in the 
                         Galactic center region, performed on two years of data from LIGO's 
                         fifth science run from two LIGO detectors. The search uses a 
                         semicoherent approach, analyzing coherently 630 segments, each 
                         spanning 11.5 hours, and then incoherently combining the results 
                         of the single segments. It covers gravitational wave frequencies 
                         in a range from 78 to 496 Hz and a frequency-dependent range of 
                         first-order spindown values down to -7.86 x 10(-8) Hz/s at the 
                         highest frequency. No gravitational waves were detected. The 
                         90\\% confidence upper limits on the gravitational wave 
                         amplitude of sources at the Galactic center are similar to 3.35 x 
                         10(-25) for frequencies near 150 Hz. These upper limits are the 
                         most constraining to date for a large-parameter-space search for 
                         continuous gravitational wave signals.",
                  doi = "10.1103/PhysRevD.88.102002",
                  url = "http://dx.doi.org/10.1103/PhysRevD.88.102002",
                 issn = "1550-2368 and 1550-7998",
                label = "isi 2014-01",
           targetfile = "PhysRevD.88.102002.pdf",
        urlaccessdate = "21 jan. 2021"
}


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