Abstract
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 Me) 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 ≤ 0.3 at 16.9 Gpc−3 yr−1 at the 90% confidence level.
| Original language | English |
|---|---|
| Article number | ad65ce |
| Journal | Astrophysical Journal |
| Volume | 973 |
| Issue number | 2 |
| DOIs | |
| Publication status | Published - 1 Oct 2024 |
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In: Astrophysical Journal, Vol. 973, No. 2, ad65ce, 01.10.2024.
Research output: Contribution to journal › Article › peer-review
TY - JOUR
T1 - Search for Eccentric Black Hole Coalescences during the Third Observing Run of LIGO and Virgo
AU - The LIGO Scientific Collaboration, the Virgo Collaboration, and the KAGRA Collaboration
AU - Abac, A. G.
AU - Abbott, R.
AU - Abe, H.
AU - Acernese, F.
AU - Ackley, K.
AU - Adamcewicz, C.
AU - Adhicary, S.
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 - Aguiar, O. D.
AU - Aguilar, I.
AU - Aiello, L.
AU - Ain, A.
AU - Ajith, P.
AU - Akutsu, T.
AU - Albanesi, S.
AU - Alfaidi, R. A.
AU - Al-Jodah, A.
AU - Alléné, C.
AU - Allocca, A.
AU - Almualla, M.
AU - Altin, P. A.
AU - Álvarez-López, S.
AU - Amato, A.
AU - Amez-Droz, L.
AU - Amorosi, A.
AU - Anand, S.
AU - Ananyeva, A.
AU - Andersen, R.
AU - Anderson, S. B.
AU - Anderson, W. G.
AU - Andia, M.
AU - Ando, M.
AU - Andrade, T.
AU - Andres, N.
AU - Andrés-Carcasona, M.
AU - Andrić, T.
AU - Ansoldi, S.
AU - Antelis, J. M.
AU - Antier, S.
AU - Aoumi, M.
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 - Aritomi, N.
AU - Armato, F.
AU - Arnaud, N.
AU - Arogeti, M.
AU - Aronson, S. M.
AU - Arun, K. G.
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 - Ault O'Neal, K.
AU - Babak, S.
AU - Badalyan, A.
AU - Badaracco, F.
AU - Badger, C.
AU - Bae, S.
AU - Bagnasco, S.
AU - Bai, Y.
AU - Baier, J. G.
AU - Bajpai, R.
AU - Baka, T.
AU - Ball, M.
AU - Ballardin, G.
AU - Ballmer, S. W.
AU - Baltus, G.
AU - Banagiri, S.
AU - Banerjee, B.
AU - Bankar, D.
AU - Baral, P.
AU - Barayoga, J. C.
AU - Barber, J.
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 - Barthelmy, S. D.
AU - Barton, M. A.
AU - Bartos, I.
AU - Basak, S.
AU - Basalaev, A.
AU - Bassiri, R.
AU - Basti, A.
AU - Bawaj, M.
AU - Baxi, P.
AU - Bayley, J. C.
AU - Baylor, A. C.
AU - Bazzan, M.
AU - Bécsy, B.
AU - Bedakihale, V. M.
AU - Beirnaert, F.
AU - Bejger, M.
AU - Bell, A. S.
AU - Benedetto, V.
AU - Beniwal, D.
AU - Benoit, W.
AU - Bentley, J. D.
AU - Ben Yaala, M.
AU - Bera, S.
AU - Berbel, M.
AU - Bergamin, F.
AU - Berger, B. K.
AU - Bernuzzi, S.
AU - Beroiz, M.
AU - Berry, C. P.L.
AU - Bersanetti, D.
AU - Bertolini, A.
AU - Betzwieser, J.
AU - Beveridge, D.
AU - Bevins, N.
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 - Bilicki, M.
AU - Billingsley, G.
AU - Binetti, A.
AU - Bini, S.
AU - Birnholtz, O.
AU - Biscans, S.
AU - Bischi, M.
AU - Biscoveanu, S.
AU - Bisht, A.
AU - Bitossi, M.
AU - Bizouard, M. A.
AU - Blackburn, J. K.
AU - Blair, C. D.
AU - Blair, D. G.
AU - Bobba, F.
AU - Bode, N.
AU - Boër, M.
AU - Bogaert, G.
AU - Boileau, G.
AU - Boldrini, M.
AU - Bolingbroke, G. N.
AU - Bonavena, L. D.
AU - Bondarescu, R.
AU - Bondu, F.
AU - Bonilla, E.
AU - Bonilla, G. S.
AU - Bonnand, R.
AU - Booker, P.
AU - Boschi, V.
AU - Bose, S.
AU - Bossilkov, V.
AU - Boudart, V.
AU - Bozzi, A.
AU - Bradaschia, C.
AU - Brady, P. R.
AU - Braglia, M.
AU - Branch, A.
AU - Branchesi, M.
AU - Breschi, M.
AU - Briant, T.
AU - Brillet, A.
AU - Brinkmann, M.
AU - Brockill, P.
AU - Brooks, A. F.
AU - Brown, D. D.
AU - Brozzetti, M. L.
AU - Brunett, S.
AU - Bruno, G.
AU - Bruntz, R.
AU - Bryant, J.
AU - Bucci, F.
AU - Buchanan, J.
AU - Bulashenko, O.
AU - Bulik, T.
AU - Bulten, H. J.
AU - Buonanno, A.
AU - Burtnyk, K.
AU - Buscicchio, R.
AU - Buskulic, D.
AU - Buy, C.
AU - Davies, G. S.Cabourn
AU - Cabras, G.
AU - Cabrita, R.
AU - Cadonati, L.
AU - Cagnoli, G.
AU - Cahillane, C.
AU - Cain, H. W.
AU - Bustillo, J. Calderón
AU - Callaghan, J. D.
AU - Callister, T. A.
AU - Calloni, E.
AU - Camp, J. B.
AU - Canepa, M.
AU - Santoro, G. Caneva
AU - Cannavacciuolo, M.
AU - Cannon, K. C.
AU - Cao, H.
AU - Cao, Z.
AU - Capistran, L. A.
AU - Capocasa, E.
AU - Capote, E.
AU - Carapella, G.
AU - Carbognani, F.
AU - Carlassara, M.
AU - Carlin, J. B.
AU - Carpinelli, M.
AU - Carter, J. J.
AU - Carullo, G.
AU - Chen, Y.
AU - Choudhary, S.
AU - Coward, D. M.
AU - Danilishin, S.
AU - Degallaix, J.
AU - Diamond, P. Z.
AU - Di Fronzo, C.
AU - Gould, D. W.
AU - Howell, E. J.
AU - JaberianHamedan, V.
AU - Ju, L.
AU - Kaur, T.
AU - Kovalam, M.
AU - Liu, Jian
AU - McLeod, A.
AU - Neil, B. F.
AU - Page, M. A.
AU - Panther, F. H.
AU - Satari, H.
AU - Slaven-Blair, T. J.
AU - van Heijningen, J. V.
AU - Veitch, P. J.
AU - Wen, L.
AU - Zhao, C.
N1 - Publisher Copyright: © 2024. The Author(s). Published by the American Astronomical Society.
PY - 2024/10/1
Y1 - 2024/10/1
N2 - 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 Me) 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 ≤ 0.3 at 16.9 Gpc−3 yr−1 at the 90% confidence level.
AB - 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 Me) 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 ≤ 0.3 at 16.9 Gpc−3 yr−1 at the 90% confidence level.
UR - http://www.scopus.com/inward/record.url?scp=85210770411&partnerID=8YFLogxK
U2 - 10.3847/1538-4357/ad65ce
DO - 10.3847/1538-4357/ad65ce
M3 - Article
AN - SCOPUS:85210770411
SN - 0004-637X
VL - 973
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 2
M1 - ad65ce
ER -