Search of the Orion spur for continuous gravitational waves using a loosely coherent algorithm on data from LIGO interferometers

verfasst von: J. Aasi, B. P. Abbott, R. Abbott, T. D. Abbott, M. R. Abernathy, F. Acernese, K. Ackley, C. Adams, T. Adams, P. Addesso, R. X. Adhikari, V. B. Adya, C. Affeldt, M. Agathos, K. Agatsuma, N. Aggarwal, O. D. Aguiar, A. Ain, D. A. Brown, Y. Chen, S. L. Danilishin, Karsten Danzmann, T. T. Fricke, M. M. Hanke, J. Hennig, Michele Heurs, F. Kawazoe, H. M. Lee, Harald Lück, J. Luo, T. T. Nguyen, J. H. Poeld, P. Schmidt, M. Shaltev, Daniel Steinmeyer, L. Sun, Henning Fedor Cornelius Vahlbruch, M. Wang, X. Wang, L. W. Wei, Benno Willke, Holger Wittel, L. Zhang, Y. Zhang, M. Zhou, Bruce Allen, Peter Aufmuth, J. Hölscher-Obermaier, Stefan Kaufer, Christian Krüger, A. Sawadsky
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.
Organisationseinheit(en): Institut für Gravitationsphysik
Abt. Nanostrukturen
Externe Organisation(en): California Institute of Technology (Caltech)
Louisiana State University
Universita di Salerno
Università degli Studi di Napoli Federico II
University of Florida
Cardiff University
Universite de Savoie
University of Sannio
Max-Planck-Institut für Gravitationsphysik (Albert-Einstein-Institut)
Nationaal instituut voor subatomaire fysica (Nikhef)
LIGO Laboratory
Instituto Nacional de Pesquisas Espaciais
Inter-University Centre for Astronomy and Astrophysics India
University of Birmingham
University of Western Australia
University of Glasgow
Seoul National University
Carleton College
Australian National University
University of Melbourne
Tsinghua University
Universite de Nice-Sophia Antipolis
Rochester Institute of Technology
Northwestern University
University of Wisconsin Milwaukee
Typ: Artikel
Journal: Physical Review D
Band: 93
ISSN: 2470-0010
Publikationsdatum: 17.02.2016
Publikationsstatus: Veröffentlicht
Peer-reviewed: Ja
ASJC Scopus Sachgebiete: Physik und Astronomie (sonstige)
Elektronische Version(en): https://doi.org/10.1103/PhysRevD.93.042006 (Zugang: Geschlossen)
https://doi.org/10.15488/12017 (Zugang: Offen)

BibTeX

@article{7ee23c8820254fb2a05ca6100161b6f5,
title = "Search of the Orion spur for continuous gravitational waves using a loosely coherent algorithm on data from LIGO interferometers",
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.",
author = "J. Aasi and Abbott, {B. P.} and R. Abbott and Abbott, {T. D.} and Abernathy, {M. R.} and F. Acernese and K. Ackley and C. Adams and T. Adams and P. Addesso and Adhikari, {R. X.} and Adya, {V. B.} and C. Affeldt and M. Agathos and K. Agatsuma and N. Aggarwal and Aguiar, {O. D.} and A. Ain and Brown, {D. A.} and Y. Chen and Danilishin, {S. L.} and Karsten Danzmann and Fricke, {T. T.} and Hanke, {M. M.} and J. Hennig and Michele Heurs and F. Kawazoe and Lee, {H. M.} and Harald L{\"u}ck and J. Luo and Nguyen, {T. T.} and Poeld, {J. H.} and P. Schmidt and M. Shaltev and Daniel Steinmeyer and L. Sun and Vahlbruch, {Henning Fedor Cornelius} and M. Wang and X. Wang and Wei, {L. W.} and Benno Willke and Holger Wittel and L. Zhang and Y. Zhang and M. Zhou and Bruce Allen and Peter Aufmuth and J. H{\"o}lscher-Obermaier and Stefan Kaufer and Christian Kr{\"u}ger and A. Sawadsky",
note = "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 Educaci{\'o}n y Ciencia, the Conselleria d''Economia Hisenda i Innovaci{\'o} 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.",
year = "2016",
month = feb,
day = "17",
doi = "10.1103/PhysRevD.93.042006",
language = "English",
volume = "93",
journal = "Physical Review D",
issn = "2470-0010",
publisher = "American Institute of Physics",
number = "4",
}