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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 & Engineering Research Board (SERB), India, the Ministry of Human Resource Development, India, the Spanish Agencia Estatal de Investigacion (AEI), the Spanish Ministerio de Ciencia e Innovacion and Ministerio de Universidades, the Conselleria de Fons Europeus, Universitat i Cultura and the Direccio General de Politica Universitaria i Recerca del Govern de les Illes Balears, the Conselleria d'Innovacio Universitats, Ciencia 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 (FRSFNRS), Actions de Recherche Concertees (ARC) and Fonds Wetenschappelijk Onderzoek -Vlaanderen (FWO), Belgium, the Paris I<^>le-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 National Science and Technology Council (NSTC), 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 the 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-inAid 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 Global Science experimental Data hub Center (GSDC) at KISTI, 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 National Science and Technology Council (NSTC) in Taiwan under grants including the Rising Star Program and Science Vanguard Research Program, Advanced Technology Center (ATC) of NAOJ, and Mechanical Engineering Center of KEK.

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Search for Eccentric Black Hole Coalescences during the Third Observing Run of LIGO and Virgo

Publicado en:Astrophysical Journal. 973 (2): 132- - 2024-10-01 973(2), DOI: 10.3847/1538-4357/ad65ce

Autores: Abac, A G; Abbott, R; Abe, H; Acernese, F; Ackley, K; Adamcewicz, C; Adhicary, S; Adhikari, N; Adhikari, R X; Adkins, V K; Adya, V B; Affeldt, C; Agarwal, D; Agathos, M; Aguiar, O D; Aguilar, I; Aiello, L; Ain, A; Ajith, P; Akutsu, T; Albanesi, S; Alfaidi, R A; Al-Jodah, A; Allene, C; Allocca, A; Almualla, M; Altin, P A; Alvarez-Lopez, S; Amato, A; Amez-Droz, L; Amorosi, A; Anand, S; Ananyeva, A; Andersen, R; Anderson, S B; Anderson, W G; Andia, M; Ando, M; Andrade, T; Andres, N; Andres-Carcasona, M; Andric, T; Ansoldi, S; Antelis, J M; Antier, S; Aoumi, M; Apostolatos, T; Appavuravther, E Z; Appert, S; Apple, S K; Arai, K; Araya, A; Araya, M C; Areeda, J S; Aritomi, N; Armato, F; Arnaud, N; Arogeti, M; Aronson, S M; Arun, K G; Ashton, G; Aso, Y; Assiduo, M; Melo, S Assis de Souza; Aston, S M; Astone, P; Aubin, F; AultONeal, K; Babak, S; Badalyan, A; Badaracco, F; Badger, C; Bae, S; Bagnasco, S; Bai, Y; Baier, J G; Bajpai, R; Baka, T; Ball, M; Ballardin, G; Ballmer, S W; Baltus, G; Banagiri, S; Banerjee, B; Bankar, D; Baral, P; Barayoga, J C; Barber, J; Barish, B C; Barker, D; Barneo, P; Barone, F; Barr, B; Barsotti, L; Barsuglia, M; Barta, D; Barthelmy, S D; Barton, M A; Bartos, I; Basak, S; Basalaev, A; Bassiri, R; Basti, A; Bawaj, M; Baxi, P; Bayley, J C; Baylor, A C; Bazzan, M; Becsy, B; Bedakihale, V M; Beirnaert, F; Bejger, M; Bell, A S; Benedetto, V; Beniwal, D; Benoit, W; Bentley, J D; Ben Yaala, M; Bera, S; Berbel, M; Bergamin, F; Berger, B K; Bernuzzi, S; Beroiz, M; Berry, C P L; Bersanetti, D; Bertolini, A; Betzwieser, J; Beveridge, D; Bevins, N; Bhandare, R; Bhandari, A V; Bhardwaj, U; Bhatt, R; Bhattacharjee, D; Bhaumik, S; Bianchi, A; Bilenko, I A; Bilicki, M; Billingsley, G; Binetti, A; Bini, S; Birnholtz, O; Biscans, S; Bischi, M; Biscoveanu, S; Bisht, A; Bitossi, M; Bizouard, M -A; Blackburn, J K; Blair, C D; Blair, D G; Bobba, F; Bode, N; Boer, M; Bogaert, G; Boileau, G; Boldrini, M; Bolingbroke, G N; Bonavena, L D; Bondarescu, R; Bondu, F; Bonilla, E; Bonilla, G S; Bonnand, R; Booker, P; Boschi, V; Bose, S; Bossilkov, V; Boudart, V; Bozzi, A; Bradaschia, C; Brady, P R; Braglia, M; Branch, A; Branchesi, M; Breschi, M; Briant, T; Brillet, A; Brinkmann, M; Brockill, P; Brooks, A F; Brown, D D; Brozzetti, M L; Brunett, S; Bruno, G; Bruntz, R; Bryant, J; Bucci, F; Buchanan, J; Bulashenko, O; Bulik, T; Bulten, H J; Buonanno, A; Burtnyk, K; Buscicchio, R; Buskulic, D; Buy, C; Davies, G S Cabourn; Cabras, G; Cabrita, R; Cadonati, L; Cagnoli, G; Cahillane, C; Cain, H W, III; Bustillo, J Calderon; Callaghan, J D; Callister, T A; Calloni, E; Camp, J B; Canepa, M; Santoro, G Caneva; Cannavacciuolo, M; Cannon, K C; Cao, H; Cao, Z; Capistran, L A; Capocasa, E; Capote, E; Carapella, G; Carbognani, F; Carlassara, M; Carlin, J B; Carpinelli, M; Carter, J J; Carullo, G; Diaz, J Casanueva; Casentini, C; Castaldi, G; Castro-Lucas, S Y; Caudill, S; Cavaglia, M; Cavalieri, R; Cella, G; Cerda-Duran, P; Cesarini, E; Chaibi, W; Chalathadka-Subrahmanya, S; Chan, C; 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Resumen

Despite the growing number of binary black hole coalescences confidently observed through gravitational waves so far, the astrophysical origin of these binaries remains uncertain. Orbital eccentricity is one of the clearest tracers of binary formation channels. Identifying binary eccentricity, however, remains challenging due to the limited availability of gravitational waveforms that include the effects of eccentricity. Here, we present observational results for a waveform-independent search sensitive to eccentric black hole coalescences, covering the third observing run (O3) of the LIGO and Virgo detectors. We identified no new high-significance candidates beyond those that have already been identified with searches focusing on quasi-circular binaries. We determine the sensitivity of our search to high-mass (total source-frame mass M > 70 M-circle dot) binaries covering eccentricities up to 0.3 at 15 Hz emitted gravitational-wave frequency, and use this to compare model predictions to search results. Assuming all detections are indeed quasi-circular, for our fiducial population model, we place a conservative upper limit for the merger rate density of high-mass binaries with eccentricities 0 < e

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