Abstract
We present a directed search for continuous gravitational wave (CW) signals emitted by spinning neutron stars located in the inner parsecs of the Galactic Center (GC). Compelling evidence for the presence of a numerous population of neutron stars has been reported in the literature, turning this region into a very interesting place to look for CWs. In this search, data from the full O3 LIGO-Virgo run in the detector frequency band [10,2000] Hz have been used. No significant detection was found and 95% confidence level upper limits on the signal strain amplitude were computed, over the full search band, with the deepest limit of about 7.6×10-26 at ≃142 Hz. These results are significantly more constraining than those reported in previous searches. We use these limits to put constraints on the fiducial neutron star ellipticity and r-mode amplitude. These limits can be also translated into constraints in the black hole mass-boson mass plane for a hypothetical population of boson clouds around spinning black holes located in the GC.
| Original language | English |
|---|---|
| Article number | 042003 |
| Journal | Physical Review D |
| Volume | 106 |
| Issue number | 4 |
| DOIs | |
| Publication status | Published - 15 Aug 2022 |
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- Abbott et al 2022 Search for continuous gravitational wave emission from the Milky Way center in O3 LIGO-Virgo dataFinal published version, 903 KBLicence: Other
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In: Physical Review D, Vol. 106, No. 4, 042003, 15.08.2022.
Research output: Contribution to journal › Article › peer-review
TY - JOUR
T1 - Search for continuous gravitational wave emission from the Milky Way center in O3 LIGO-Virgo data
AU - The LIGO Scientific Collaboration, the Virgo Collaboration, and the KAGRA Collaboration
AU - Abbott, R.
AU - Abe, H.
AU - Acernese, F.
AU - Ackley, K.
AU - Adhikari, N.
AU - Adhikari, R. X.
AU - Adkins, V. K.
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 - Akutsu, T.
AU - Albanesi, S.
AU - Alfaidi, R. A.
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 - Ando, M.
AU - Andrade, T.
AU - Andres, N.
AU - Andrés-Carcasona, M.
AU - Andrić, T.
AU - Angelova, S. V.
AU - Ansoldi, S.
AU - Antelis, J. M.
AU - Antier, S.
AU - Apostolatos, T.
AU - Appavuravther, E. Z.
AU - Appert, S.
AU - Apple, S. K.
AU - Arai, K.
AU - Araya, A.
AU - Araya, M. C.
AU - Areeda, J. S.
AU - Arène, M.
AU - Aritomi, N.
AU - Arnaud, N.
AU - Arogeti, M.
AU - Aronson, S. M.
AU - Arun, K. G.
AU - Asada, H.
AU - Asali, Y.
AU - Ashton, G.
AU - Aso, Y.
AU - Assiduo, M.
AU - De Souza Melo, S. Assis
AU - Aston, S. M.
AU - Astone, P.
AU - Aubin, F.
AU - Aultoneal, K.
AU - Austin, C.
AU - Babak, S.
AU - Badaracco, F.
AU - Bader, M. K.M.
AU - Badger, C.
AU - Bae, S.
AU - Bae, Y.
AU - Baer, A. M.
AU - Bagnasco, S.
AU - Bai, Y.
AU - Baird, J.
AU - Bajpai, R.
AU - Baka, T.
AU - Ball, M.
AU - Ballardin, G.
AU - Ballmer, S. W.
AU - Balsamo, A.
AU - Baltus, G.
AU - Banagiri, S.
AU - Banerjee, B.
AU - Bankar, D.
AU - Barayoga, J. C.
AU - Barbieri, C.
AU - Barish, B. C.
AU - Barker, D.
AU - Barneo, P.
AU - Barone, F.
AU - Barr, B.
AU - Barsotti, L.
AU - Barsuglia, M.
AU - Barta, D.
AU - Bartlett, J.
AU - Barton, M. A.
AU - Bartos, I.
AU - Basak, S.
AU - Bassiri, R.
AU - Basti, A.
AU - Bawaj, M.
AU - Bayley, J. C.
AU - Bazzan, M.
AU - Becher, B. R.
AU - Bécsy, B.
AU - Bedakihale, V. M.
AU - Beirnaert, F.
AU - Bejger, M.
AU - Belahcene, I.
AU - Benedetto, V.
AU - Beniwal, D.
AU - Benjamin, M. G.
AU - Bennett, T. F.
AU - Bentley, J. D.
AU - Benyaala, M.
AU - Bera, S.
AU - Berbel, M.
AU - Bergamin, F.
AU - Berger, B. K.
AU - Bernuzzi, S.
AU - Bersanetti, D.
AU - Bertolini, A.
AU - Betzwieser, J.
AU - Beveridge, D.
AU - Bhandare, R.
AU - Bhandari, A. V.
AU - Bhardwaj, U.
AU - Bhatt, R.
AU - Bhattacharjee, D.
AU - Bhaumik, S.
AU - Bianchi, A.
AU - Bilenko, I. A.
AU - Billingsley, G.
AU - Bini, S.
AU - Birney, R.
AU - Birnholtz, O.
AU - Biscans, S.
AU - Bischi, M.
AU - Biscoveanu, S.
AU - Bisht, A.
AU - Biswas, B.
AU - Bitossi, M.
AU - Bizouard, M. A.
AU - Blackburn, J. K.
AU - Blair, C. D.
AU - Blair, D. G.
AU - Blair, R. M.
AU - Bobba, F.
AU - Bode, N.
AU - Boër, M.
AU - Bogaert, G.
AU - Boldrini, M.
AU - Bolingbroke, G. N.
AU - Bonavena, L. D.
AU - Bondu, F.
AU - Bonilla, E.
AU - Bonnand, R.
AU - Booker, P.
AU - Boom, B. A.
AU - Bork, R.
AU - Boschi, V.
AU - Bose, N.
AU - Bose, S.
AU - Bossilkov, V.
AU - Boudart, V.
AU - Bouffanais, Y.
AU - Bozzi, A.
AU - Bradaschia, C.
AU - Brady, P. R.
AU - Bramley, A.
AU - Branch, A.
AU - Branchesi, M.
AU - Brau, J. E.
AU - Breschi, M.
AU - Briant, T.
AU - Briggs, J. H.
AU - Brillet, A.
AU - Brinkmann, M.
AU - Brockill, P.
AU - Brooks, A. F.
AU - Brooks, J.
AU - Brown, D. D.
AU - Brunett, S.
AU - Bruno, G.
AU - Bruntz, R.
AU - Bryant, J.
AU - Bucci, F.
AU - Bulik, T.
AU - Bulten, H. J.
AU - Buonanno, A.
AU - Burtnyk, K.
AU - Buscicchio, R.
AU - Buskulic, D.
AU - Buy, C.
AU - Byer, R. L.
AU - Davies, G. S.Cabourn
AU - Cabras, G.
AU - Cabrita, R.
AU - Cadonati, L.
AU - Caesar, M.
AU - Cagnoli, G.
AU - Cahillane, C.
AU - Bustillo, J. Calderón
AU - Callaghan, J. D.
AU - Callister, T. A.
AU - Calloni, E.
AU - Cameron, J.
AU - Camp, J. B.
AU - Canepa, M.
AU - Canevarolo, S.
AU - Cannavacciuolo, M.
AU - Cannon, K. C.
AU - Cao, H.
AU - Cao, Z.
AU - Capocasa, E.
AU - Capote, E.
AU - Carapella, G.
AU - Carbognani, F.
AU - Carlassara, M.
AU - Carlin, J. B.
AU - Carney, M. F.
AU - Carpinelli, M.
AU - Carrillo, G.
AU - Carullo, G.
AU - Carver, T. L.
AU - Diaz, J. Casanueva
AU - Casentini, C.
AU - Castaldi, G.
AU - Caudill, S.
AU - Cavaglià, M.
AU - Cavalier, F.
AU - Cavalieri, R.
AU - Chatterjee, C.
AU - Chen, X.
AU - Choudhary, R. K.
AU - Chu, Q.
AU - Coward, D. M.
AU - Howell, E. J.
AU - JaberianHamedan, V.
AU - Jones, A. W.
AU - Ju, L.
AU - Kaur, T.
AU - Kovalam, M.
AU - Liu, J.
AU - McCann, J. J.
AU - Neil, B. F.
AU - Page, M. A.
AU - Panther, F. H.
AU - Satari, H.
AU - Slaven-Blair, T. J.
AU - Wen, L.
AU - Zhao, C.
N1 - Funding Information: 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 U.S. 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 work was supported by MEXT, JSPS Leading-edge Research Infrastructure Program, JSPS Grant-in-Aid for Specially Promoted Research 26000005, JSPS Grant-in-Aid for Scientific Research on Innovative Areas 2905: JP17H06358, JP17H06361, and JP17H06364, JSPS Core-to-Core Program A. Advanced Research Networks, JSPS Grant-in-Aid for Scientific Research (S) 17H06133 and 20H05639, JSPS Grant-in-Aid for Transformative Research Areas (A) 20A203: JP20H05854, the joint research program of the Institute for Cosmic Ray Research, University of Tokyo, National Research Foundation (NRF), Computing Infrastructure Project of KISTI-GSDC, Korea Astronomy and Space Science Institute (KASI), and Ministry of Science and ICT (MSIT) in Korea, Academia Sinica (AS), AS Grid Center (ASGC), and the Ministry of Science and Technology (MoST) in Taiwan under grants including AS-CDA-105-M06, Advanced Technology Center (ATC) of NAOJ, and Mechanical Engineering Center of KEK. Publisher Copyright: © 2022 American Physical Society. All rights reserved.
PY - 2022/8/15
Y1 - 2022/8/15
N2 - We present a directed search for continuous gravitational wave (CW) signals emitted by spinning neutron stars located in the inner parsecs of the Galactic Center (GC). Compelling evidence for the presence of a numerous population of neutron stars has been reported in the literature, turning this region into a very interesting place to look for CWs. In this search, data from the full O3 LIGO-Virgo run in the detector frequency band [10,2000] Hz have been used. No significant detection was found and 95% confidence level upper limits on the signal strain amplitude were computed, over the full search band, with the deepest limit of about 7.6×10-26 at ≃142 Hz. These results are significantly more constraining than those reported in previous searches. We use these limits to put constraints on the fiducial neutron star ellipticity and r-mode amplitude. These limits can be also translated into constraints in the black hole mass-boson mass plane for a hypothetical population of boson clouds around spinning black holes located in the GC.
AB - We present a directed search for continuous gravitational wave (CW) signals emitted by spinning neutron stars located in the inner parsecs of the Galactic Center (GC). Compelling evidence for the presence of a numerous population of neutron stars has been reported in the literature, turning this region into a very interesting place to look for CWs. In this search, data from the full O3 LIGO-Virgo run in the detector frequency band [10,2000] Hz have been used. No significant detection was found and 95% confidence level upper limits on the signal strain amplitude were computed, over the full search band, with the deepest limit of about 7.6×10-26 at ≃142 Hz. These results are significantly more constraining than those reported in previous searches. We use these limits to put constraints on the fiducial neutron star ellipticity and r-mode amplitude. These limits can be also translated into constraints in the black hole mass-boson mass plane for a hypothetical population of boson clouds around spinning black holes located in the GC.
UR - http://www.scopus.com/inward/record.url?scp=85137883577&partnerID=8YFLogxK
U2 - 10.1103/PhysRevD.106.042003
DO - 10.1103/PhysRevD.106.042003
M3 - Article
AN - SCOPUS:85137883577
SN - 2470-0010
VL - 106
JO - Physical Review D
JF - Physical Review D
IS - 4
M1 - 042003
ER -