Properties of the binary neutron star merger GW170817

Abbott, B. P. et al. (2019) Properties of the binary neutron star merger GW170817. Physical Review X, 9(1), 011001. (doi:10.1103/PhysRevX.9.011001)

Abbott, B. P. et al. (2019) Properties of the binary neutron star merger GW170817. Physical Review X, 9(1), 011001. (doi:10.1103/PhysRevX.9.011001)

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Abstract

On August 17, 2017, the Advanced LIGO and Advanced Virgo gravitational-wave detectors observed a low-mass compact binary inspiral. The initial sky localization of the source of the gravitational-wave signal, GW170817, allowed electromagnetic observatories to identify NGC 4993 as the host galaxy. In this work, we improve initial estimates of the binary’s properties, including component masses, spins, and tidal parameters, using the known source location, improved modeling, and recalibrated Virgo data. We extend the range of gravitational-wave frequencies considered down to 23 Hz, compared to 30 Hz in the initial analysis. We also compare results inferred using several signal models, which are more accurate and incorporate additional physical effects as compared to the initial analysis. We improve the localization of the gravitational-wave source to a 90% credible region of 16     deg 2 . We find tighter constraints on the masses, spins, and tidal parameters, and continue to find no evidence for nonzero component spins. The component masses are inferred to lie between 1.00 and 1.89     M ⊙ when allowing for large component spins, and to lie between 1.16 and 1.60     M ⊙ (with a total mass 2.73 + 0.04 − 0.01     M ⊙ ) when the spins are restricted to be within the range observed in Galactic binary neutron stars. Using a precessing model and allowing for large component spins, we constrain the dimensionless spins of the components to be less than 0.50 for the primary and 0.61 for the secondary. Under minimal assumptions about the nature of the compact objects, our constraints for the tidal deformability parameter ˜ Λ are (0,630) when we allow for large component spins, and 300 + 420 − 230 (using a 90% highest posterior density interval) when restricting the magnitude of the component spins, ruling out several equation-of-state models at the 90% credible level. Finally, with LIGO and GEO600 data, we use a Bayesian analysis to place upper limits on the amplitude and spectral energy density of a possible postmerger signal.

Item Type:Articles
Status:Published
Refereed:Yes
Glasgow Author(s) Enlighten ID:Grant, Mr Alastair and Spencer, Mr Andrew and Pascucci, Daniela and Messenger, Dr Christopher and Masso Reid, Ms Mariela and Isa, Hafizah Noor Binti and Bell, Dr Angus and Williams, Mr Daniel and Toland, Mr Karl and Hammond, Professor Giles and Hild, Professor Stefan and Barr, Dr Bryan and Sorazu Lucio, Dr Borja and Keitel, David and Steinlechner, Dr Jessica and Veitch, Dr John and Tornasi, Mr Zeno and Phelps, Ms Margot and Heng, Professor Ik Siong and Wright, Ms Jennifer and van Veggel, Dr Marielle and Tait, Mr Simon and Houston, Mr Ewan and Graef, Dr Christian and Zhang, Mr Teng and Pearlstone, Mr Brynley and Hendry, Professor Martin and Scott, Dr Jamie and Rowan, Professor Sheila and Martin, Dr Iain and Robertson, Professor Norna and Chan, Mr Man Leong and Robie, Mr Raymond and Gabbard, Mr Hunter and Dupej, Mr Peter and Cumming, Dr Alan and Hennig, Mr Jan-Simon and Cunningham, Dr Liam and Barclay, Miss Sheena and Woan, Professor Graham and Steinlechner, Dr Sebastian and Mangano, Miss Valentina and Hough, Professor James and Huttner, Dr Sabina and Bayley, Mr Joseph and Strain, Professor Kenneth and Jones, Mr Russell and Haughian, Dr Karen and HART, Martin and Pitkin, Dr Matthew and Murray, Dr Peter and Fletcher, Mr Mark
Authors: Abbott, B. P., Abbott, R., Abbott, T. D., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R. X., Adya, V. B., Affeldt, C., Agarwal, B., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, B., Allen, G., Allocca, A., Aloy, M. A., Altin, P. A., Amato, A., Ananyeva, A., Anderson, S. B., Anderson, W. G., Angelova, S. V., Antier, S., Appert, S., Arai, K., Araya, M. C., Areeda, J. S., Arène, M., Arnaud, N., Arun, K. G., Ascenzi, S., Ashton, G., Ast, M., Aston, S. M., Astone, P., Atallah, D. V., Aubin, F., Aufmuth, P., Aulbert, C., AultONeal, K., Austin, C., Avila-Alvarez, A., Babak, S., Bacon, P., Badaracco, F., Bader, M. K. M., Bae, S., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Banagiri, S., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barkett, K., Barnum, S., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Batch, J. C., Bawaj, M., Bayley, J. C., Bazzan, M., Bécsy, B., Beer, C., Bejger, M., Belahcene, I., Bell, A. S., Beniwal, D., Bensch, M., Berger, B. K., Bergmann, G., Bernuzzi, S., Bero, J. J., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhandare, R., Bilenko, I. A., Bilgili, S. A., Billingsley, G., Billman, C. R., Birch, J., Birney, R., Birnholtz, O., Biscans, S., Biscoveanu, S., Bisht, A., Bitossi, M., Bizouard, M. A., Blackburn, J. K., Blackman, J., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bock, O., Bode, N., Boer, M., Boetzel, Y., Bogaert, G., Bohe, A., Bondu, F., Bonilla, E., Bonnand, R., Booker, P., Boom, B. A., Booth, C. D., Bork, R., Boschi, V., Bose, S., Bossie, K., Bossilkov, V., Bosveld, J., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Bramley, A., Branchesi, M., Brau, J. E., Briant, T., Brighenti, F., Brillet, A., Brinkmann, M., Brisson, V., Brockill, P., Brooks, A. F., Brown, D. D., Brunett, S., Buchanan, C. C., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. L., Cabero, M., Cadonati, L., Cagnoli, G., Cahillane, C., Calderón Bustillo, J., Callister, T. A., Calloni, E., Camp, J. B., Canepa, M., Canizares, P., Cannon, K. C., Cao, H., Cao, J., Capano, C. D., Capocasa, E., Carbognani, F., Caride, S., Carney, M. F., Carullo, G., Casanueva Diaz, J., Casentini, C., Caudill, S., Cavaglià, M., Cavalier, F., Cavalieri, R., Cella, G., Cepeda, C. B., Cerdá-Durán, P., Cerretani, G., Cesarini, E., Chaibi, O., Chamberlin, S. J., Chan, M., Chao, S., Charlton, P., Chase, E., Chassande-Mottin, E., Chatterjee, D., Chatziioannou, K., Cheeseboro, B. D., Chen, H. Y., Chen, X., Chen, Y., Cheng, H.-P., Chia, H. Y., Chincarini, A., Chiummo, A., Chmiel, T., Cho, H. S., Cho, M., Chow, J. H., Christensen, N., Chu, Q., Chua, A. J. K., Chua, S., Chung, K. W., Chung, S., Ciani, G., Ciobanu, A. A., Ciolfi, R., Cipriano, F., Cirelli, C. E., Cirone, A., Clara, F., Clark, J. 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College/School:College of Science and Engineering > School of Physics and Astronomy
Journal Name:Physical Review X
Publisher:American Physical Society
ISSN:2160-3308
ISSN (Online):2160-3308
Published Online:02 January 2019
Copyright Holders:Copyright © 2019 American Physical Society
First Published:First published in Physical Review X 9(1): 011001
Publisher Policy:Reproduced under a Creative Commons License

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