Abstract
| Original language | English |
|---|---|
| Article number | 082005 |
| Number of pages | 25 |
| Journal | Physical Review D |
| Volume | 105 |
| Issue number | 8 |
| DOIs | |
| Publication status | Published - 28 Apr 2022 |
Keywords
- COMPACT CENTRAL OBJECT
- MOUNTAINS
- NEUTRON-STAR
- RADIATION
Access to Document
- 10.1103/PhysRevD.105.082005Licence: Free access - publisher
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In: Physical Review D, Vol. 105, No. 8, 082005, 28.04.2022.
Research output: Contribution to journal › Article › Academic › peer-review
TY - JOUR
T1 - Search of the early O3 LIGO data for continuous gravitational waves from the Cassiopeia A and Vela Jr. supernova remnants
AU - Abbott, R.
AU - Abbott, T.D.
AU - Acernese, F.
AU - Ackley, K.
AU - Adams, C.
AU - Adhikari, N.
AU - Adhikari, R.X.
AU - Adya, V.B.
AU - Affeldt, C.
AU - Agarwal, D.
AU - Agathos, M.
AU - Agatsuma, K.
AU - Aggarwal, N.
AU - Aguiar, O.D.
AU - Aiello, L.
AU - Ain, A.
AU - Ajith, P.
AU - Albanesi, S.
AU - Allocca, A.
AU - Altin, P.A.
AU - Amato, A.
AU - Anand, C.
AU - Anand, S.
AU - Ananyeva, A.
AU - Anderson, S.B.
AU - Anderson, W.G.
AU - Andrade, T.
AU - Andres, N.
AU - Angelova, S.V.
AU - Ansoldi, S.
AU - Antelis, J.M.
AU - Antier, S.
AU - Appert, S.
AU - Arai, K.
AU - Araya, M.C.
AU - Areeda, J.S.
AU - Arene, M.
AU - Arnaud, N.
AU - Aronson, S.M.
AU - LIGO Scientific Collaboration
AU - Virgo Collaboration
AU - Danilishin, S.
AU - Hennig, J.
AU - Hennig, M.H.
AU - Hild, S.
AU - Koekoek, G.
AU - Singha, A.
AU - Spagnuolo, V.
AU - Steinlechner, J.
AU - Steinlechner, S.
AU - Utina, A.
AU - van den Brand, J.F.J.
N1 - Funding Information: We thank the anonymous journal referee for helpful comments, especially concerning the treatment of the third frequency derivative which led to a refinement of the analysis. This material is based upon work supported by NSF’s LIGO Laboratory which is a major facility fully funded by the National Science Foundation. The authors also gratefully acknowledge the support of 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 GEO 600 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 Netherlands Organization for Scientific Research (NWO), 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 and Engineering Research Board (SERB), India, the Ministry of Human Resource Development, India, the Spanish Agencia Estatal de Investigación (AEI), the Spanish Ministerio de Ciencia e Innovación and Ministerio de Universidades, the Conselleria de Fons Europeus, Universitat i Cultura and the Direcció General de Política Universitaria i Recerca del Govern de les Illes Balears, the Conselleria d’Innovació, Universitats, Ciència i Societat Digital de la Generalitat Valenciana and the CERCA Programme Generalitat de Catalunya, Spain, the National Science Centre of Poland and the European Union—European Regional Development Fund; Foundation for Polish Science (FNP), the Swiss National Science Foundation (SNSF), the Russian Foundation for Basic Research, the Russian Science Foundation, the European Commission, the European Social Funds (ESF), 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 French Lyon Institute of Origins (LIO), the Belgian Fonds de la Recherche Scientifique (FRS-FNRS), Actions de Recherche Concertées (ARC) and Fonds Wetenschappelijk Onderzoek—Vlaanderen (FWO), Belgium, the Paris Île-de-France Region, the National Research, Development and Innovation Office Hungary (NKFIH), the National Research Foundation of Korea, the Natural Science and Engineering Research Council Canada, Canadian Foundation for Innovation (CFI), the Brazilian Ministry of Science, Technology, and Innovations, 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, the United States Department of Energy, and the Kavli Foundation. The authors gratefully acknowledge the support of the NSF, STFC, INFN and CNRS for provision of computational resources. This document has been assigned LIGO Laboratory document number LIGO-P2100298-v8 . Publisher Copyright: © 2022 American Physical Society. All rights reserved.
PY - 2022/4/28
Y1 - 2022/4/28
N2 - We present directed searches for continuous gravitational waves from the neutron stars in the Cassiopeia A (Cas A) and Vela Jr. supernova remnants. We carry out the searches in the LIGO detector data from the first six months of the third Advanced LIGO and Virgo observing run using the WEAVE semicoherent method, which sums matched-filter detection-statistic values over many time segments spanning the observation period. No gravitational wave signal is detected in the search band of 20-976 Hz for assumed source ages greater than 300 years for Cas A and greater than 700 years for Vela Jr. Estimates from simulated continuous wave signals indicate we achieve the most sensitive results to date across the explored parameter space volume, probing to strain magnitudes as low as similar to 6.3 x 10(-26) for Cas A and similar to 5.6 x 10(-26) for Vela Jr. at frequencies near 166 Hz at 95% efficiency.
AB - We present directed searches for continuous gravitational waves from the neutron stars in the Cassiopeia A (Cas A) and Vela Jr. supernova remnants. We carry out the searches in the LIGO detector data from the first six months of the third Advanced LIGO and Virgo observing run using the WEAVE semicoherent method, which sums matched-filter detection-statistic values over many time segments spanning the observation period. No gravitational wave signal is detected in the search band of 20-976 Hz for assumed source ages greater than 300 years for Cas A and greater than 700 years for Vela Jr. Estimates from simulated continuous wave signals indicate we achieve the most sensitive results to date across the explored parameter space volume, probing to strain magnitudes as low as similar to 6.3 x 10(-26) for Cas A and similar to 5.6 x 10(-26) for Vela Jr. at frequencies near 166 Hz at 95% efficiency.
KW - COMPACT CENTRAL OBJECT
KW - MOUNTAINS
KW - NEUTRON-STAR
KW - RADIATION
U2 - 10.1103/PhysRevD.105.082005
DO - 10.1103/PhysRevD.105.082005
M3 - Article
SN - 1550-7998
VL - 105
JO - Physical Review D
JF - Physical Review D
IS - 8
M1 - 082005
ER -