Search for gravitational wave radiation associated with the pulsating tail of the SGR 1806-20 hyperflare of 27 December 2004 using LIGO

Search for gravitational wave radiation associated with the pulsating tail of the SGR 1806-20 hyperflare of 27 December 2004 using LIGO. Abbott, B., Drever, R. W. P., Brown, D. A., Savov, P., Siemens, X., Thorne, K. S., Vallisneri, M., Abbott, R., Adhikari, R. X., Agresti, J., Anderson, S. B., Araya, M., Armandula, H., Ballmer, S., Barish, B. C., Bhawal, B., Billingsley, G., Black, E., Blackburn, K., Bork, R., Boschi, V., Busby, D., Cardenas, L., Cepeda, C., Chatterji, S., Coyne, D., Creighton, T. D., D'Ambrosio, E., DeSalvo, R., Dupuis, R. J., Ehrens, P., Espinoza, E., Etzel, T., Evans, M., Fairhurst, S., Fazi, D., Goggin, L., Heefner, J., Ivanov, A., Kells, W., Keppel, D. G., King, P., Kondrashov, V., Kozak, D., Lazzarini, A., Lei, M., Libbrecht, K., Lindquist, P., Mageswaran, M., Mailand, K., Mandic, V., Maros, E., Marx, J. N., Meshkov, S., Messaritaki, E., Meyers, D., Miyakawa, O., Nash, T., Patel, P., Pedraza, M., Robertson, N. A., Russell, P., Samidi, M., Sannibale, V., Sears, B., Smith, M. R., Sutton, P. J., Tarallo, M., Taylor, R., Tinto, M., Tyler, W., Varvella, M., Vass, S., Villar, A., Waldman, S. J., Wallace, L., Ward, R., Webber, D., Weinstein, A. J., Whitcomb, S. E., Willems, P. A., Yamamoto, H., Zhang, L., & Zweizig, J. Physical Review D, 76(6):Art. No. 062003, American Physical Society, September, 2007. o̧pyright 2007 American Physical Society. Received 9 April 2007. Published 27 September 2007. We are indebted to Gianluca Israel and Anna Watts for frequent and fruitful discussions. 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 Educacion y Ciencia, the National Aeronautics and Space Administration, the John Simon Guggenheim Foundation, the Alexander von Humboldt Foundation, the Leverhulme Trust, the David and Lucile Packard Foundation, the Research Corporation, the Alfred P. Sloan Foundation, and Columbia University in New York City.

Paper abstract bibtex

We have searched for gravitational waves (GWs) associated with the SGR 1806?20 hyperflare of 27 December 2004. This event, originating from a Galactic neutron star, displayed exceptional energetics. Recent investigations of the x-ray light curve?s pulsating tail revealed the presence of quasiperiodic oscillations (QPOs) in the 30?2000 Hz frequency range, most of which coincides with the bandwidth of the LIGO detectors. These QPOs, with well-characterized frequencies, can plausibly be attributed to seismic modes of the neutron star which could emit GWs. Our search targeted potential quasimonochromatic GWs lasting for tens of seconds and emitted at the QPO frequencies. We have observed no candidate signals above a predetermined threshold, and our lowest upper limit was set by the 92.5 Hz QPO observed in the interval from 150 s to 260 s after the start of the flare. This bound corresponds to a (90% confidence) root-sum-squared amplitude h\^ (90%)_(rss-det) =4.5$\times$10\^ (?22) strain Hz\^ (?1/2) on the GW waveform strength in the detectable polarization state reaching our Hanford (WA) 4 km detector. We illustrate the astrophysical significance of the result via an estimated characteristic energy in GW emission that we would expect to be able to detect. The above result corresponds to 7.7$\times$10\^ (46) erg (=4.3$\times$10\^ (?8) M_$\odot$c\^ 2), which is of the same order as the total (isotropic) energy emitted in the electromagnetic spectrum. This result provides a means to probe the energy reservoir of the source with the best upper limit on the GW waveform strength published and represents the first broadband asteroseismology measurement using a GW detector.

@article{caltechauthors44547,
          volume = {76},
          number = {6},
           month = {September},
          author = {B. Abbott and R. W. P. Drever and D. A. Brown and P. Savov and X. Siemens and K. S. Thorne and M. Vallisneri and R. Abbott and Rana X. Adhikari and J. Agresti and S. B. Anderson and M. Araya and H. Armandula and S. Ballmer and B. C. Barish and B. Bhawal and G. Billingsley and E. Black and K. Blackburn and R. Bork and V. Boschi and D. Busby and L. Cardenas and C. Cepeda and S. Chatterji and D. Coyne and T. D. Creighton and E. D'Ambrosio and R. DeSalvo and R. J. Dupuis and P. Ehrens and E. Espinoza and T. Etzel and M. Evans and S. Fairhurst and D. Fazi and L. Goggin and J. Heefner and A. Ivanov and W. Kells and D. G. Keppel and P. King and V. Kondrashov and D. Kozak and A. Lazzarini and M. Lei and K. Libbrecht and P. Lindquist and M. Mageswaran and K. Mailand and V. Mandic and E. Maros and J. N. Marx and S. Meshkov and E. Messaritaki and D. Meyers and O. Miyakawa and T. Nash and P. Patel and M. Pedraza and N. A. Robertson and P. Russell and M. Samidi and V. Sannibale and B. Sears and M. R. Smith and P. J. Sutton and M. Tarallo and R. Taylor and M. Tinto and W. Tyler and M. Varvella and S. Vass and A. Villar and S. J. Waldman and L. Wallace and R. Ward and D. Webber and A. J. Weinstein and S. E. Whitcomb and P. A. Willems and H. Yamamoto and L. Zhang and J. Zweizig},
            note = {{\copyright} 2007 American Physical Society. Received 9 April 2007.    Published 27 September 2007. We are indebted to Gianluca Israel and Anna Watts for
frequent and fruitful discussions. 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 Educacion y Ciencia, the National Aeronautics and
Space Administration, the John Simon Guggenheim
Foundation, the Alexander von Humboldt Foundation,
the Leverhulme Trust, the David and Lucile Packard
Foundation, the Research Corporation, the Alfred P.
Sloan Foundation, and Columbia University in New York
City.},
           title = {Search for gravitational wave radiation associated with the pulsating tail of the SGR 1806-20 hyperflare of 27 December 2004 using LIGO},
       publisher = {American Physical Society},
            year = {2007},
         journal = {Physical Review D},
           pages = {Art. No. 062003},
             url = {http://resolver.caltech.edu/CaltechAUTHORS:20140328-102903046},
        abstract = {We have searched for gravitational waves (GWs) associated with the SGR 1806?20 hyperflare of 27 December 2004. This event, originating from a Galactic neutron star, displayed exceptional energetics. Recent investigations of the x-ray light curve?s pulsating tail revealed the presence of quasiperiodic oscillations (QPOs) in the 30?2000 Hz frequency range, most of which coincides with the bandwidth of the LIGO detectors. These QPOs, with well-characterized frequencies, can plausibly be attributed to seismic modes of the neutron star which could emit GWs. Our search targeted potential quasimonochromatic GWs lasting for tens of seconds and emitted at the QPO frequencies. We have observed no candidate signals above a predetermined threshold, and our lowest upper limit was set by the 92.5 Hz QPO observed in the interval from 150 s to 260 s after the start of the flare. This bound corresponds to a (90\% confidence) root-sum-squared amplitude h{\^{ }}(90\%)\_(rss-det) =4.5{$\times$}10{\^{ }}(?22)  strain  Hz{\^{ }}(?1/2) on the GW waveform strength in the detectable polarization state reaching our Hanford (WA) 4 km detector. We illustrate the astrophysical significance of the result via an estimated characteristic energy in GW emission that we would expect to be able to detect. The above result corresponds to 7.7{$\times$}10{\^{ }}(46)  erg (=4.3{$\times$}10{\^{ }}(?8)  M\_{$\odot$}c{\^{ }}2), which is of the same order as the total (isotropic) energy emitted in the electromagnetic spectrum. This result provides a means to probe the energy reservoir of the source with the best upper limit on the GW waveform strength published and represents the first broadband asteroseismology measurement using a GW detector.}
}

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