Details
| Original language | English |
|---|---|
| Article number | 042006 |
| Journal | Physical Review D |
| Volume | 93 |
| Issue number | 4 |
| Publication status | Published - 17 Feb 2016 |
Abstract
We report results of a wideband search for periodic gravitational waves from isolated neutron stars within the Orion spur towards both the inner and outer regions of our Galaxy. As gravitational waves interact very weakly with matter, the search is unimpeded by dust and concentrations of stars. One search disk (A) is 6.87° in diameter and centered on 20h10m54.71s+33°33′25.29′′, and the other (B) is 7.45° in diameter and centered on 8h35m20.61s-46°49′25.151′′. We explored the frequency range of 50-1500 Hz and frequency derivative from 0 to -5×10-9 Hz/s. A multistage, loosely coherent search program allowed probing more deeply than before in these two regions, while increasing coherence length with every stage. Rigorous follow-up parameters have winnowed the initial coincidence set to only 70 candidates, to be examined manually. None of those 70 candidates proved to be consistent with an isolated gravitational-wave emitter, and 95% confidence level upper limits were placed on continuous-wave strain amplitudes. Near 169 Hz we achieve our lowest 95% C.L. upper limit on the worst-case linearly polarized strain amplitude h0 of 6.3×10-25, while at the high end of our frequency range we achieve a worst-case upper limit of 3.4×10-24 for all polarizations and sky locations.
ASJC Scopus subject areas
- Physics and Astronomy(all)
- Physics and Astronomy (miscellaneous)
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In: Physical Review D, Vol. 93, No. 4, 042006, 17.02.2016.
Research output: Contribution to journal › Article › Research › peer review
}
TY - JOUR
T1 - Search of the Orion spur for continuous gravitational waves using a loosely coherent algorithm on data from LIGO interferometers
AU - Aasi, J.
AU - Abbott, B. P.
AU - Abbott, R.
AU - Abbott, T. D.
AU - Abernathy, M. R.
AU - Acernese, F.
AU - Ackley, K.
AU - Adams, C.
AU - Adams, T.
AU - Addesso, P.
AU - Adhikari, R. X.
AU - Adya, V. B.
AU - Affeldt, C.
AU - Agathos, M.
AU - Agatsuma, K.
AU - Aggarwal, N.
AU - Aguiar, O. D.
AU - Ain, A.
AU - Brown, D. A.
AU - Chen, Y.
AU - Danilishin, S. L.
AU - Danzmann, Karsten
AU - Fricke, T. T.
AU - Hanke, M. M.
AU - Hennig, J.
AU - Heurs, Michele
AU - Kawazoe, F.
AU - Lee, H. M.
AU - Lück, Harald
AU - Luo, J.
AU - Nguyen, T. T.
AU - Poeld, J. H.
AU - Schmidt, P.
AU - Shaltev, M.
AU - Steinmeyer, Daniel
AU - Sun, L.
AU - Vahlbruch, Henning Fedor Cornelius
AU - Wang, M.
AU - Wang, X.
AU - Wei, L. W.
AU - Willke, Benno
AU - Wittel, Holger
AU - Zhang, L.
AU - Zhang, Y.
AU - Zhou, M.
AU - Allen, Bruce
AU - Aufmuth, Peter
AU - Hölscher-Obermaier, J.
AU - Kaufer, Stefan
AU - Krüger, Christian
AU - Sawadsky, A.
N1 - Funding information: The authors gratefully acknowledge the support of the United States National Science Foundation for the construction and operation of the LIGO Laboratory, 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, and the Nucleare and the French Centre National de la Recherche Scientifique for the construction and operation of the Virgo detector. The authors also gratefully acknowledge the support of the research by these agencies and by the Australian Research Council, the International Science Linkages program of the Commonwealth of Australia, the Council of Scientific and Industrial Research of India, the Istituto Nazionale di Fisica Nucleare of Italy, the Spanish Ministerio de Educación y Ciencia, the Conselleria d''Economia Hisenda i Innovació of the Govern de les Illes Balears, the Foundation for Fundamental Research on Matter supported by the Netherlands Organisation for Scientific Research, the Polish Ministry of Science and Higher Education, the FOCUS Programme of Foundation for Polish Science, 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. This document has been assigned LIGO Laboratory document number LIGO-P1500034-v23.
PY - 2016/2/17
Y1 - 2016/2/17
N2 - We report results of a wideband search for periodic gravitational waves from isolated neutron stars within the Orion spur towards both the inner and outer regions of our Galaxy. As gravitational waves interact very weakly with matter, the search is unimpeded by dust and concentrations of stars. One search disk (A) is 6.87° in diameter and centered on 20h10m54.71s+33°33′25.29′′, and the other (B) is 7.45° in diameter and centered on 8h35m20.61s-46°49′25.151′′. We explored the frequency range of 50-1500 Hz and frequency derivative from 0 to -5×10-9 Hz/s. A multistage, loosely coherent search program allowed probing more deeply than before in these two regions, while increasing coherence length with every stage. Rigorous follow-up parameters have winnowed the initial coincidence set to only 70 candidates, to be examined manually. None of those 70 candidates proved to be consistent with an isolated gravitational-wave emitter, and 95% confidence level upper limits were placed on continuous-wave strain amplitudes. Near 169 Hz we achieve our lowest 95% C.L. upper limit on the worst-case linearly polarized strain amplitude h0 of 6.3×10-25, while at the high end of our frequency range we achieve a worst-case upper limit of 3.4×10-24 for all polarizations and sky locations.
AB - We report results of a wideband search for periodic gravitational waves from isolated neutron stars within the Orion spur towards both the inner and outer regions of our Galaxy. As gravitational waves interact very weakly with matter, the search is unimpeded by dust and concentrations of stars. One search disk (A) is 6.87° in diameter and centered on 20h10m54.71s+33°33′25.29′′, and the other (B) is 7.45° in diameter and centered on 8h35m20.61s-46°49′25.151′′. We explored the frequency range of 50-1500 Hz and frequency derivative from 0 to -5×10-9 Hz/s. A multistage, loosely coherent search program allowed probing more deeply than before in these two regions, while increasing coherence length with every stage. Rigorous follow-up parameters have winnowed the initial coincidence set to only 70 candidates, to be examined manually. None of those 70 candidates proved to be consistent with an isolated gravitational-wave emitter, and 95% confidence level upper limits were placed on continuous-wave strain amplitudes. Near 169 Hz we achieve our lowest 95% C.L. upper limit on the worst-case linearly polarized strain amplitude h0 of 6.3×10-25, while at the high end of our frequency range we achieve a worst-case upper limit of 3.4×10-24 for all polarizations and sky locations.
UR - http://www.scopus.com/inward/record.url?scp=84960193113&partnerID=8YFLogxK
U2 - 10.1103/PhysRevD.93.042006
DO - 10.1103/PhysRevD.93.042006
M3 - Article
AN - SCOPUS:84960193113
VL - 93
JO - Physical Review D
JF - Physical Review D
SN - 2470-0010
IS - 4
M1 - 042006
ER -