Paper abstract bibtex

We present a LIGO search for short-duration gravitational waves (GWs) associated with soft gamma ray repeater (SGR) bursts. This is the first search sensitive to neutron star f modes, usually considered the most efficient GW emitting modes. We find no evidence of GWs associated with any SGR burst in a sample consisting of the 27 Dec. 2004 giant flare from SGR 1806-20 and 190 lesser events from SGR 1806-20 and SGR 1900+14. The unprecedented sensitivity of the detectors allows us to set the most stringent limits on transient GW amplitudes published to date. We find upper limit estimates on the model-dependent isotropic GW emission energies (at a nominal distance of 10 kpc) between 3$\times$10\^ (45) and 9$\times$10\^ (52) erg depending on waveform type, detector antenna factors and noise characteristics at the time of the burst. These upper limits are within the theoretically predicted range of some SGR models.

@article{caltechauthors15998, volume = {101}, number = {21}, month = {November}, author = {B. Abbott and R. Abbott and Rana X. Adhikari and P. Ajith and B. Allen and G. Allen and R. Amin and S. B. Anderson and W. G. Anderson and M. A. Arain and M. Araya and H. Armandula and P. Armor and Y. Aso and S. Aston and P. Aufmuth and C. Aulbert and S. Babak and S. Ballmer and H. Bantilan and B. C. Barish and C. Barker and D. Barker and B. Barr and P. Barriga and M. A. Barton and I. Bartos and M. Bastarrika and K. Bayer and J. Betzwieser and P. T. Beyersdorf and I. A. Bilenko and G. Billingsley and R. Biswas and E. Black and K. Blackburn and L. Blackburn and D. Blair and B. Bland and T. P. Bodiya and L. Bogue and R. Bork and V. Boschi and S. Bose and P. R. Brady and V. B. Braginsky and J. E. Brau and M. Brinkmann and A. Brooks and D. A. Brown and G. Brunet and A. Bullington and A. Buonanno and O. Burmeister and R. L. Byer and L. Cadonati and G. Cagnoli and J. B. Camp and J. Cannizzo and K. Cannon and J. Cao and L. Cardenas and T. Casebolt and G. Castaldi and C. Cepeda and E. Chalkley and P. Charlton and S. Chatterji and S. Chelkowski and Y. Chen and N. Christensen and D. Clark and J. Clark and T. Cokelaer and R. Conte and D. Cook and T. Corbitt and D. Coyne and J. D. E. Creighton and A. Cumming and L. Cunningham and R. M. Cutler and J. Dalrymple and K. Danzmann and G. Davies and D. DeBra and J. Degallaix and M. Degree and V. Dergachev and S. Desai and R. DeSalvo and S. Dhurandhar and M. D{\'i}az and J. Dickson and A. Dietz and F. Donovan and K. L. Dooley and E. E. Doomes and R. W. P. Drever and I. Duke and J.-C. Dumas and R. J. Dupuis and J. G. Dwyer and C. Echols and A. Effler and P. Ehrens and E. Espinoza and T. Etzel and T. Evans and S. Fairhurst and Y. Fan and D. Fazi and H. Fehrmann and M. M. Fejer and L. S. Finn and K. Flasch and N. Fotopoulos and A. Freise and R. Frey and T. Fricke and P. Fritschel and V. V. Frolov and M. Fyffe and J. Garofoli and I. Gholami and J. A. Giaime and S. Giampanis and K. D. Giardina and K. Goda and E. Goetz and L. Goggin and G. Gonz{\'a}lez and S. Gossler and R. Gouaty and A. Grant and S. Gras and C. Gray and M. Gray and R. J. S. Greenhalgh and A. M. Gretarsson and F. Grimaldi and R. Grosso and H. Grote and S. Grunewald and M. Guenther and E. K. Gustafson and R. Gustafson and B. Hage and J. M. Hallam and D. Hammer and C. Hanna and J. Hanson and J. Harms and G. Harry and E. Harstad and K. Hayama and T. Hayler and J. Heefner and I. S. Heng and M. Hennessy and A. Heptonstall and M. Hewitson and S. Hild and E. Hirose and D. Hoak and D. Hosken and J. Hough and S. H. Huttner and D. Ingram and M. Ito and A. Ivanov and B. Johnson and W. W. Johnson and D. I. Jones and G. Jones and R. Jones and L. Ju and P. Kalmus and V. Kalogera and S. Kamat and J. Kanner and D. Kasprzyk and E. Katsavounidis and K. Kawabe and S. Kawamura and F. Kawazoe and W. Kells and D. G. Keppel and F. Ya. Khalili and R. Khan and E. Khazanov and C. Kim and P. King and J. S. Kissel and S. Klimenko and K. Kokeyama and V. Kondrashov and R. K. Kopparapu and D. Kozak and I. Kozhevatov and B. Krishnan and P. Kwee and P. K. Lam and M. Landry and M. M. Lang and B. Lantz and A. Lazzarini and M. Lei and N. Leindecker and V. Leonhardt and I. Leonor and K. Libbrecht and H. Lin and P. Lindquist and N. A. Lockerbie and D. Lodhia and M. Lormand and P. Lu and M. Lubinski and A. Lucianetti and H. L{\"u}ck and B. Machenschalk and M. MacInnis and M. Mageswaran and K. Mailand and V. Mandic and S. M{\'a}rka and Z. M{\'a}rka and A. Markosyan and J. Markowitz and E. Maros and I. Martin and R. M. Martin and J. N. Marx and K. Mason and F. Matichard and L. Matone and R. Matzner and N. Mavalvala and R. McCarthy and D. E. McClelland and S. C. McGuire and M. McHugh and G. McIntyre and G. McIvor and D. McKechan and K. McKenzie and T. Meier and A. Melissinos and G. Mendell and R. A. Mercer and S. Meshkov and C. J. Messenger and D. Meyers and J. Miller and J. Minelli and S. Mitra and V. P. Mitrofanov and G. Mitselmakher and R. Mittleman and O. Miyakawa and B. Moe and S. Mohanty and G. Moreno and K. Mossavi and C. MowLowry and G. Mueller and S. Mukherjee and H. Mukhopadhyay and H. M{\"u}ller-Ebhardt and J. Munch and P. Murray and E. Myers and J. Myers and T. Nash and J. Nelson and G. Newton and A. Nishizawa and K. Numata and J. O'Dell and G. Ogin and B. O'Reilly and R. O'Shaughnessy and D. J. Ottaway and R. S. Ottens and H. Overmier and B. J. Owen and Y. Pan and C. Pankow and M. A. Papa and V. Parameshwaraiah and P. Patel and M. Pedraza and S. Penn and A. Perreca and T. Petrie and I. M. Pinto and M. Pitkin and H. J. Pletsch and M. V. Plissi and F. Postiglione and M. Principe and R. Prix and V. Quetschke and F. Raab and D. S. Rabeling and H. Radkins and N. Rainer and M. Rakhmanov and M. Ramsunder and H. Rehbein and S. Reid and D. H. Reitze and R. Riesen and K. Riles and B. Rivera and N. A. Robertson and C. Robinson and E. L. Robinson and S. Roddy and A. Rodriguez and A. M. Rogan and J. Rollins and J. D. Romano and J. Romie and R. Route and S. Rowan and A. R{\"u}diger and L. Ruet and P. Russell and K. Ryan and S. Sakata and M. Samidi and L. Sancho de la Jordana and V. Sandberg and V. Sannibale and S. Saraf and P. Sarin and B. S. Sathyaprakash and S. Sato and P. R. Saulson and R. Savage and P. Savov and S. W. Schediwy and R. Schilling and R. Schnabel and R. Schofield and B. F. Schutz and P. Schwinberg and S. M. Scott and A. C. Searle and B. Sears and F. Seifert and D. Sellers and A. S. Sengupta and P. Shawhan and D. H. Shoemaker and A. Sibley and X. Siemens and D. Sigg and S. Sinha and A. M. Sintes and B. J. J. Slagmolen and J. Slutsky and J. R. Smith and M. R. Smith and N. D. Smith and K. Somiya and B. Sorazu and L. C. Stein and A. Stochino and R. Stone and K. A. Strain and D. M. Strom and A. Stuver and T. Z. Summerscales and K.-X. Sun and M. Sung and P. J. Sutton and H. Takahashi and D. B. Tanner and R. Taylor and R. Taylor and J. Thacker and K. A. Thorne and K. S. Thorne and A. Th{\"u}ring and K. V. Tokmakov and C. Torres and C. Torrie and G. Traylor and M. Trias and W. Tyler and D. Ugolini and J. Ulmen and K. Urbanek and H. Vahlbruch and C. Van Den Broeck and M. van der Sluys and S. Vass and R. Vaulin and A. Vecchio and J. Veitch and P. Veitch and A. Villar and C. Vorvick and S. P. Vyachanin and S. J. Waldman and L. Wallace and H. Ward and R. Ward and M. Weinert and R. Weiss and S. Wen and K. Wette and J. T. Whelan and S. E. Whitcomb and B. F. Whiting and C. Wilkinson and P. A. Willems and H. R. Williams and L. Williams and B. Willke and I. Wilmut and W. Winkler and C. C. Wipf and A. G. Wiseman and G. Woan and R. Wooley and J. Worden and W. Wu and I. Yakushin and H. Yamamoto and Z. Yan and S. Yoshida and M. Zanolin and J. Zhang and L. Zhang and C. Zhao and N. Zotov and M. Zucker and J. Zweizig and Alan J. Weinstein}, note = {{\copyright} 2008 The American Physical Society. Received 1 September 2008; published 21 November 2008. The authors are grateful to the Konus-Wind team and to S. Mereghetti for information used in the S5 burst list, and to G. Lichti and D. Smith for information on the giant flare event time. The authors gratefully acknowledge the support of the United States National Science Foundation for the construction and operation of the LIGO Laboratory and the Science and Technology Facilities 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 Council of Scientific and Industrial Research of India, the Istituto Nazionale di Fisica Nucleare of Italy, the Spanish Ministerio de Educacion y Ciencia, the Conselleria d?Economia Hisenda i Innovacio of the Govern de les Illes Balears, the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, The National Aeronautics and Space Administration, the Carnegie Trust, the Leverhulme Trust, the David and Lucile Packard Foundation, the Research Corporation, and the Alfred P. Sloan Foundation. K. C. H. is grateful for support under JPL contracts 1282043 and 1268385, and NASA grants NAG5-11451 and NNG04GM50G.}, title = {Search for Gravitational-Wave Bursts from Soft Gamma Repeaters}, publisher = {American Physical Society}, year = {2008}, journal = {Physical Review Letters}, pages = {Art. No. 211102}, url = {http://resolver.caltech.edu/CaltechAUTHORS:20090922-145122645}, abstract = {We present a LIGO search for short-duration gravitational waves (GWs) associated with soft gamma ray repeater (SGR) bursts. This is the first search sensitive to neutron star f modes, usually considered the most efficient GW emitting modes. We find no evidence of GWs associated with any SGR burst in a sample consisting of the 27 Dec. 2004 giant flare from SGR 1806-20 and 190 lesser events from SGR 1806-20 and SGR 1900+14. The unprecedented sensitivity of the detectors allows us to set the most stringent limits on transient GW amplitudes published to date. We find upper limit estimates on the model-dependent isotropic GW emission energies (at a nominal distance of 10 kpc) between 3{$\times$}10{\^{ }}(45) and 9{$\times$}10{\^{ }}(52) erg depending on waveform type, detector antenna factors and noise characteristics at the time of the burst. These upper limits are within the theoretically predicted range of some SGR models. } }

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