Details
| Originalsprache | Englisch |
|---|---|
| Aufsatznummer | 024004 |
| Seitenumfang | 27 |
| Fachzeitschrift | Physical Review D |
| Jahrgang | 100 |
| Ausgabenummer | 2 |
| Publikationsstatus | Veröffentlicht - 8 Juli 2019 |
Abstract
We present results of an all-sky search for continuous gravitational waves (CWs), which can be produced by fast spinning neutron stars with an asymmetry around their rotation axis, using data from the second observing run of the Advanced LIGO detectors. Three different semicoherent methods are used to search in a gravitational-wave frequency band from 20 to 1922 Hz and a first frequency derivative from -1×10-8 to 2×10-9 Hz/s. None of these searches has found clear evidence for a CW signal, so upper limits on the gravitational-wave strain amplitude are calculated, which for this broad range in parameter space are the most sensitive ever achieved.
ASJC Scopus Sachgebiete
- Physik und Astronomie (insg.)
- Physik und Astronomie (sonstige)
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in: Physical Review D, Jahrgang 100, Nr. 2, 024004, 08.07.2019.
Publikation: Beitrag in Fachzeitschrift › Artikel › Forschung
}
TY - JOUR
T1 - All-sky search for continuous gravitational waves from isolated neutron stars using Advanced LIGO O2 data
AU - The LIGO Scientific Collaboration
AU - The Virgo Collaboration
AU - Abbott, B. P.
AU - Abbott, R.
AU - Abbott, T. D.
AU - Abraham, S.
AU - Acernese, F.
AU - Ackley, K.
AU - Adams, C.
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 - Aiello, L.
AU - Ain, A.
AU - Ajith, P.
AU - Allen, G.
AU - Allocca, A.
AU - Aloy, M. A.
AU - Altin, P. A.
AU - Amato, A.
AU - Ananyeva, A.
AU - Anderson, S. B.
AU - Anderson, W. G.
AU - Angelova, S. V.
AU - Antier, S.
AU - Appert, S.
AU - Arai, K.
AU - Araya, M. C.
AU - Areeda, J. S.
AU - Arène, M.
AU - Arnaud, N.
AU - Arun, K. G.
AU - Ascenzi, S.
AU - Ashton, G.
AU - Aston, S. M.
AU - Astone, P.
AU - Aubin, F.
AU - Danilishin, S. L.
AU - Danzmann, K.
AU - Heurs, M.
AU - Hreibi, A.
AU - Lück, H.
AU - Steinmeyer, D.
AU - Vahlbruch, H.
AU - Wei, L.-w.
AU - Wilken, D. M.
AU - Willke, B.
AU - Wittel, H.
AU - Bose, Sukanta
AU - Brown, D. D.
AU - Chen, H. Y.
AU - Hanke, Manuela
AU - Hennig, J.
AU - Kumar, Sanjeev
AU - Lang, R. N.
AU - Lee, H. K.
AU - Lee, H. M.
AU - Lee, H. W.
AU - Lee, J.
AU - Li, X.
AU - Sanders, J. R.
AU - Schmidt, Patricia
AU - Sun, L.
AU - Wang, Y. F.
AU - Wu, D. S.
AU - Zhang, L.
AU - Zhu, X. J.
AU - Zhou, Minchuan
AU - Bergmann, Gerald
AU - Bisht, Aparna
AU - Bode, Nina
AU - Booker, P.
AU - Brinkmann, Marc
AU - Cabero, M.
AU - de Varona, O.
AU - Hochheim, S.
AU - Dent, T.
AU - Doravari, S.
AU - Junker, J.
AU - Kaufer, Stefan
AU - Kirchhoff, R.
AU - Koch, Patrick
AU - Koper, N.
AU - Köhlenbeck, S. M.
AU - Kringel, Volker
AU - Kuehn, G.
AU - Karvinen, Kai S.
AU - Khan, S.
AU - Leavey, S.
AU - Lehmann, J.
AU - Lough, James
AU - Mehmet, Moritz
AU - Mukherjee, Arunava
AU - Mukund, Nikhil
AU - Nery, M.
AU - Ohme, F.
AU - Oppermann, P.
AU - Rüdiger, A.
AU - Phelps, M.
AU - Puncken, O.
AU - Schreiber, Emil
AU - Schulte, B. W.
AU - Setyawati, Y.
AU - Standke, M.
AU - Steinke, M.
AU - Thies, Fabian
AU - Weinert, Michael
AU - Wellmann, F.
AU - Weßels, Peter
AU - Wimmer, Maximilian H.
AU - Winkler, W.
AU - Woehler, J.
AU - Aufmuth, Peter
N1 - Funding Information: The authors gratefully acknowledge the support of the United States National Science Foundation (NSF) for the construction and operation of the LIGO Laboratory and Advanced LIGO as well as the Science and Technology Facilities Council (STFC) of the United Kingdom, the Max-Planck-Society (MPS), and the State of Niedersachsen/Germany for support of the construction of Advanced LIGO and construction and operation of the GEO600 detector. Additional support for Advanced LIGO was provided by the Australian Research Council. The authors gratefully acknowledge the Italian Istituto Nazionale di Fisica Nucleare (INFN), the French Centre National de la Recherche Scientifique (CNRS) and the Foundation for Fundamental Research on Matter supported by the Netherlands Organisation for Scientific Research, for the construction and operation of the Virgo detector and the creation and support of the EGO consortium. The authors also gratefully acknowledge research support from these agencies as well as by the Council of Scientific and Industrial Research of India, the Department of Science and Technology, India, the Science & Engineering Research Board (SERB), India, the Ministry of Human Resource Development, India, the Spanish Agencia Estatal de Investigación, the Vicepresidència i Conselleria d’Innovació, Recerca i Turisme and the Conselleria d’Educació i Universitat del Govern de les Illes Balears, the Conselleria d’Educació, Investigació, Cultura i Esport de la Generalitat Valenciana, the National Science Centre of Poland, the Swiss National Science Foundation (SNSF), the Russian Foundation for Basic Research, the Russian Science Foundation, the European Commission, the European Regional Development Funds (ERDF), the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, the Hungarian Scientific Research Fund (OTKA), the Lyon Institute of Origins (LIO), the Paris Île-de-France Region, the National Research, Development and Innovation Office Hungary (NKFIH), the National Research Foundation of Korea, Industry Canada and the Province of Ontario through the Ministry of Economic Development and Innovation, the Natural Science and Engineering Research Council Canada, the Canadian Institute for Advanced Research, the Brazilian Ministry of Science, Technology, Innovations, and Communications, the International Center for Theoretical Physics South American Institute for Fundamental Research (ICTP-SAIFR), the Research Grants Council of Hong Kong, the National Natural Science Foundation of China (NSFC), the Leverhulme Trust, the Research Corporation, the Ministry of Science and Technology (MOST), Taiwan and the Kavli Foundation. The authors gratefully acknowledge the support of the NSF, STFC, MPS, INFN, CNRS, INFN-CNAF, PL-Grid, and the State of Niedersachsen/Germany for provision of computational resources. Work at SURFsara and Nikhef has been performed using resources of the Dutch e-Infrastructure, which is financially supported by the Nederlandse Organisatie voor Wetenschappelijk Onderzoek (Netherlands Organisation for Scientific Research, NWO) and the Dutch higher education and research partnership for network services and information and communication technology (SURF). This article has LIGO document number LIGO-P1900012-v7.
PY - 2019/7/8
Y1 - 2019/7/8
N2 - We present results of an all-sky search for continuous gravitational waves (CWs), which can be produced by fast spinning neutron stars with an asymmetry around their rotation axis, using data from the second observing run of the Advanced LIGO detectors. Three different semicoherent methods are used to search in a gravitational-wave frequency band from 20 to 1922 Hz and a first frequency derivative from -1×10-8 to 2×10-9 Hz/s. None of these searches has found clear evidence for a CW signal, so upper limits on the gravitational-wave strain amplitude are calculated, which for this broad range in parameter space are the most sensitive ever achieved.
AB - We present results of an all-sky search for continuous gravitational waves (CWs), which can be produced by fast spinning neutron stars with an asymmetry around their rotation axis, using data from the second observing run of the Advanced LIGO detectors. Three different semicoherent methods are used to search in a gravitational-wave frequency band from 20 to 1922 Hz and a first frequency derivative from -1×10-8 to 2×10-9 Hz/s. None of these searches has found clear evidence for a CW signal, so upper limits on the gravitational-wave strain amplitude are calculated, which for this broad range in parameter space are the most sensitive ever achieved.
UR - http://www.scopus.com/inward/record.url?scp=85072684605&partnerID=8YFLogxK
U2 - 10.1103/PhysRevD.100.024004
DO - 10.1103/PhysRevD.100.024004
M3 - Article
VL - 100
JO - Physical Review D
JF - Physical Review D
SN - 2470-0010
IS - 2
M1 - 024004
ER -