Tests of General Relativity with GW150914
The LIGO detection of GW150914 provides an unprecedented opportunity to study the two-body motion of a compact-object binary in the large-velocity, highly nonlinear regime, and to witness the final merger of the binary and the excitation of uniquely relativistic modes of the gravitational field. We...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Abbott, B P [verfasserIn] |
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Artikel |
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| Sprache: |
Englisch |
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2016 |
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| Übergeordnetes Werk: |
Enthalten in: Physical review letters - Ridge, NY : American Physical Society, 1958, 116(2016), 22 |
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| Übergeordnetes Werk: |
volume:116 ; year:2016 ; number:22 |
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| DOI / URN: |
10.1103/PhysRevLett.116.221101 |
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OLC1976633176 |
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| 520 | |a The LIGO detection of GW150914 provides an unprecedented opportunity to study the two-body motion of a compact-object binary in the large-velocity, highly nonlinear regime, and to witness the final merger of the binary and the excitation of uniquely relativistic modes of the gravitational field. We carry out several investigations to determine whether GW150914 is consistent with a binary black-hole merger in general relativity. We find that the final remnant's mass and spin, as determined from the low-frequency (inspiral) and high-frequency (postinspiral) phases of the signal, are mutually consistent with the binary black-hole solution in general relativity. Furthermore, the data following the peak of GW150914 are consistent with the least-damped quasinormal mode inferred from the mass and spin of the remnant black hole. By using waveform models that allow for parametrized general-relativity violations during the inspiral and merger phases, we perform quantitative tests on the gravitational-wave phase in the dynamical regime and we determine the first empirical bounds on several high-order post-Newtonian coefficients. We constrain the graviton Compton wavelength, assuming that gravitons are dispersed in vacuum in the same way as particles with mass, obtaining a 90%-confidence lower bound of 10^{13} km. In conclusion, within our statistical uncertainties, we find no evidence for violations of general relativity in the genuinely strong-field regime of gravity. | ||
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10.1103/PhysRevLett.116.221101 doi PQ20160719 (DE-627)OLC1976633176 (DE-599)GBVOLC1976633176 (PRQ)a1681-e3937563b1693d2d52e3a9b82063fcc78db8ca35122d6accb2c7d90f882c3d110 (KEY)0009201020160000116002200000testsofgeneralrelativitywithgw150914 DE-627 ger DE-627 rakwb eng 550 DNB UA 1000 AVZ rvk Abbott, B P verfasserin aut Tests of General Relativity with GW150914 2016 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier The LIGO detection of GW150914 provides an unprecedented opportunity to study the two-body motion of a compact-object binary in the large-velocity, highly nonlinear regime, and to witness the final merger of the binary and the excitation of uniquely relativistic modes of the gravitational field. We carry out several investigations to determine whether GW150914 is consistent with a binary black-hole merger in general relativity. We find that the final remnant's mass and spin, as determined from the low-frequency (inspiral) and high-frequency (postinspiral) phases of the signal, are mutually consistent with the binary black-hole solution in general relativity. Furthermore, the data following the peak of GW150914 are consistent with the least-damped quasinormal mode inferred from the mass and spin of the remnant black hole. By using waveform models that allow for parametrized general-relativity violations during the inspiral and merger phases, we perform quantitative tests on the gravitational-wave phase in the dynamical regime and we determine the first empirical bounds on several high-order post-Newtonian coefficients. We constrain the graviton Compton wavelength, assuming that gravitons are dispersed in vacuum in the same way as particles with mass, obtaining a 90%-confidence lower bound of 10^{13} km. In conclusion, within our statistical uncertainties, we find no evidence for violations of general relativity in the genuinely strong-field regime of gravity. General Relativity and Quantum Cosmology Abbott, R oth Abbott, T D oth Abernathy, M R oth Acernese, F oth Ackley, K oth Adams, C oth Adams, T oth Addesso, P oth Adhikari, R X oth Adya, V B oth Affeldt, C oth Agathos, M oth Agatsuma, K oth Aggarwal, N oth Aguiar, O D oth Aiello, L oth Ain, A oth Ajith, P oth Allen, B oth Allocca, A oth Altin, P A oth Anderson, S B oth Anderson, W G oth Arai, K oth Araya, M C oth Arceneaux, C C oth Areeda, J S oth Arnaud, N oth Arun, K G oth Ascenzi, S oth Ashton, G oth Ast, M oth Aston, S M oth Astone, P oth Aufmuth, P oth Aulbert, C oth Babak, S oth Bacon, P oth Bader, M K M oth Baker, P T oth Baldaccini, F oth Ballardin, G oth Ballmer, S W oth Barayoga, J C oth Barclay, S E oth Barish, B C oth Barker, D oth Barone, F oth Barr, B oth Barsotti, L oth Barsuglia, M oth Barta, D oth Bartlett, J oth Bartos, I oth Bassiri, R oth Basti, A oth Batch, J C oth Baune, C oth Bavigadda, V oth Bazzan, M oth Behnke, B oth Bejger, M oth Bell, A S oth Bell, C J oth Berger, B K oth Bergman, J oth Bergmann, G oth Berry, C P L oth Bersanetti, D oth Bertolini, A oth Betzwieser, J oth Bhagwat, S oth Bhandare, R oth Bilenko, I A oth Billingsley, G oth Birch, J oth Birney, R oth Birnholtz, O oth Biscans, S oth Bisht, A oth Bitossi, M oth Biwer, C oth Bizouard, M A oth Blackburn, J K oth Blair, C D oth Blair, D G oth Blair, R M oth Bloemen, S oth Bock, O oth Bodiya, T P oth Boer, M oth Bogaert, G oth Bogan, C oth Bohe, A oth Bojtos, P oth Bond, C oth Bondu, F oth Bonnand, R oth Boom, B A oth ... oth Enthalten in Physical review letters Ridge, NY : American Physical Society, 1958 116(2016), 22 (DE-627)129503959 (DE-600)208853-8 (DE-576)014907267 0031-9007 nnns volume:116 year:2016 number:22 http://dx.doi.org/10.1103/PhysRevLett.116.221101 Volltext http://www.ncbi.nlm.nih.gov/pubmed/27314708 http://arxiv.org/abs/1602.03841 GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY GBV_ILN_21 GBV_ILN_22 GBV_ILN_40 GBV_ILN_47 GBV_ILN_55 GBV_ILN_59 GBV_ILN_60 GBV_ILN_70 GBV_ILN_130 GBV_ILN_2004 GBV_ILN_2016 GBV_ILN_2095 GBV_ILN_2192 GBV_ILN_2279 GBV_ILN_2286 UA 1000 AR 116 2016 22 |
| spelling |
10.1103/PhysRevLett.116.221101 doi PQ20160719 (DE-627)OLC1976633176 (DE-599)GBVOLC1976633176 (PRQ)a1681-e3937563b1693d2d52e3a9b82063fcc78db8ca35122d6accb2c7d90f882c3d110 (KEY)0009201020160000116002200000testsofgeneralrelativitywithgw150914 DE-627 ger DE-627 rakwb eng 550 DNB UA 1000 AVZ rvk Abbott, B P verfasserin aut Tests of General Relativity with GW150914 2016 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier The LIGO detection of GW150914 provides an unprecedented opportunity to study the two-body motion of a compact-object binary in the large-velocity, highly nonlinear regime, and to witness the final merger of the binary and the excitation of uniquely relativistic modes of the gravitational field. We carry out several investigations to determine whether GW150914 is consistent with a binary black-hole merger in general relativity. We find that the final remnant's mass and spin, as determined from the low-frequency (inspiral) and high-frequency (postinspiral) phases of the signal, are mutually consistent with the binary black-hole solution in general relativity. Furthermore, the data following the peak of GW150914 are consistent with the least-damped quasinormal mode inferred from the mass and spin of the remnant black hole. By using waveform models that allow for parametrized general-relativity violations during the inspiral and merger phases, we perform quantitative tests on the gravitational-wave phase in the dynamical regime and we determine the first empirical bounds on several high-order post-Newtonian coefficients. We constrain the graviton Compton wavelength, assuming that gravitons are dispersed in vacuum in the same way as particles with mass, obtaining a 90%-confidence lower bound of 10^{13} km. In conclusion, within our statistical uncertainties, we find no evidence for violations of general relativity in the genuinely strong-field regime of gravity. General Relativity and Quantum Cosmology Abbott, R oth Abbott, T D oth Abernathy, M R oth Acernese, F oth Ackley, K oth Adams, C oth Adams, T oth Addesso, P oth Adhikari, R X oth Adya, V B oth Affeldt, C oth Agathos, M oth Agatsuma, K oth Aggarwal, N oth Aguiar, O D oth Aiello, L oth Ain, A oth Ajith, P oth Allen, B oth Allocca, A oth Altin, P A oth Anderson, S B oth Anderson, W G oth Arai, K oth Araya, M C oth Arceneaux, C C oth Areeda, J S oth Arnaud, N oth Arun, K G oth Ascenzi, S oth Ashton, G oth Ast, M oth Aston, S M oth Astone, P oth Aufmuth, P oth Aulbert, C oth Babak, S oth Bacon, P oth Bader, M K M oth Baker, P T oth Baldaccini, F oth Ballardin, G oth Ballmer, S W oth Barayoga, J C oth Barclay, S E oth Barish, B C oth Barker, D oth Barone, F oth Barr, B oth Barsotti, L oth Barsuglia, M oth Barta, D oth Bartlett, J oth Bartos, I oth Bassiri, R oth Basti, A oth Batch, J C oth Baune, C oth Bavigadda, V oth Bazzan, M oth Behnke, B oth Bejger, M oth Bell, A S oth Bell, C J oth Berger, B K oth Bergman, J oth Bergmann, G oth Berry, C P L oth Bersanetti, D oth Bertolini, A oth Betzwieser, J oth Bhagwat, S oth Bhandare, R oth Bilenko, I A oth Billingsley, G oth Birch, J oth Birney, R oth Birnholtz, O oth Biscans, S oth Bisht, A oth Bitossi, M oth Biwer, C oth Bizouard, M A oth Blackburn, J K oth Blair, C D oth Blair, D G oth Blair, R M oth Bloemen, S oth Bock, O oth Bodiya, T P oth Boer, M oth Bogaert, G oth Bogan, C oth Bohe, A oth Bojtos, P oth Bond, C oth Bondu, F oth Bonnand, R oth Boom, B A oth ... oth Enthalten in Physical review letters Ridge, NY : American Physical Society, 1958 116(2016), 22 (DE-627)129503959 (DE-600)208853-8 (DE-576)014907267 0031-9007 nnns volume:116 year:2016 number:22 http://dx.doi.org/10.1103/PhysRevLett.116.221101 Volltext http://www.ncbi.nlm.nih.gov/pubmed/27314708 http://arxiv.org/abs/1602.03841 GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY GBV_ILN_21 GBV_ILN_22 GBV_ILN_40 GBV_ILN_47 GBV_ILN_55 GBV_ILN_59 GBV_ILN_60 GBV_ILN_70 GBV_ILN_130 GBV_ILN_2004 GBV_ILN_2016 GBV_ILN_2095 GBV_ILN_2192 GBV_ILN_2279 GBV_ILN_2286 UA 1000 AR 116 2016 22 |
| allfields_unstemmed |
10.1103/PhysRevLett.116.221101 doi PQ20160719 (DE-627)OLC1976633176 (DE-599)GBVOLC1976633176 (PRQ)a1681-e3937563b1693d2d52e3a9b82063fcc78db8ca35122d6accb2c7d90f882c3d110 (KEY)0009201020160000116002200000testsofgeneralrelativitywithgw150914 DE-627 ger DE-627 rakwb eng 550 DNB UA 1000 AVZ rvk Abbott, B P verfasserin aut Tests of General Relativity with GW150914 2016 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier The LIGO detection of GW150914 provides an unprecedented opportunity to study the two-body motion of a compact-object binary in the large-velocity, highly nonlinear regime, and to witness the final merger of the binary and the excitation of uniquely relativistic modes of the gravitational field. We carry out several investigations to determine whether GW150914 is consistent with a binary black-hole merger in general relativity. We find that the final remnant's mass and spin, as determined from the low-frequency (inspiral) and high-frequency (postinspiral) phases of the signal, are mutually consistent with the binary black-hole solution in general relativity. Furthermore, the data following the peak of GW150914 are consistent with the least-damped quasinormal mode inferred from the mass and spin of the remnant black hole. By using waveform models that allow for parametrized general-relativity violations during the inspiral and merger phases, we perform quantitative tests on the gravitational-wave phase in the dynamical regime and we determine the first empirical bounds on several high-order post-Newtonian coefficients. We constrain the graviton Compton wavelength, assuming that gravitons are dispersed in vacuum in the same way as particles with mass, obtaining a 90%-confidence lower bound of 10^{13} km. In conclusion, within our statistical uncertainties, we find no evidence for violations of general relativity in the genuinely strong-field regime of gravity. General Relativity and Quantum Cosmology Abbott, R oth Abbott, T D oth Abernathy, M R oth Acernese, F oth Ackley, K oth Adams, C oth Adams, T oth Addesso, P oth Adhikari, R X oth Adya, V B oth Affeldt, C oth Agathos, M oth Agatsuma, K oth Aggarwal, N oth Aguiar, O D oth Aiello, L oth Ain, A oth Ajith, P oth Allen, B oth Allocca, A oth Altin, P A oth Anderson, S B oth Anderson, W G oth Arai, K oth Araya, M C oth Arceneaux, C C oth Areeda, J S oth Arnaud, N oth Arun, K G oth Ascenzi, S oth Ashton, G oth Ast, M oth Aston, S M oth Astone, P oth Aufmuth, P oth Aulbert, C oth Babak, S oth Bacon, P oth Bader, M K M oth Baker, P T oth Baldaccini, F oth Ballardin, G oth Ballmer, S W oth Barayoga, J C oth Barclay, S E oth Barish, B C oth Barker, D oth Barone, F oth Barr, B oth Barsotti, L oth Barsuglia, M oth Barta, D oth Bartlett, J oth Bartos, I oth Bassiri, R oth Basti, A oth Batch, J C oth Baune, C oth Bavigadda, V oth Bazzan, M oth Behnke, B oth Bejger, M oth Bell, A S oth Bell, C J oth Berger, B K oth Bergman, J oth Bergmann, G oth Berry, C P L oth Bersanetti, D oth Bertolini, A oth Betzwieser, J oth Bhagwat, S oth Bhandare, R oth Bilenko, I A oth Billingsley, G oth Birch, J oth Birney, R oth Birnholtz, O oth Biscans, S oth Bisht, A oth Bitossi, M oth Biwer, C oth Bizouard, M A oth Blackburn, J K oth Blair, C D oth Blair, D G oth Blair, R M oth Bloemen, S oth Bock, O oth Bodiya, T P oth Boer, M oth Bogaert, G oth Bogan, C oth Bohe, A oth Bojtos, P oth Bond, C oth Bondu, F oth Bonnand, R oth Boom, B A oth ... oth Enthalten in Physical review letters Ridge, NY : American Physical Society, 1958 116(2016), 22 (DE-627)129503959 (DE-600)208853-8 (DE-576)014907267 0031-9007 nnns volume:116 year:2016 number:22 http://dx.doi.org/10.1103/PhysRevLett.116.221101 Volltext http://www.ncbi.nlm.nih.gov/pubmed/27314708 http://arxiv.org/abs/1602.03841 GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY GBV_ILN_21 GBV_ILN_22 GBV_ILN_40 GBV_ILN_47 GBV_ILN_55 GBV_ILN_59 GBV_ILN_60 GBV_ILN_70 GBV_ILN_130 GBV_ILN_2004 GBV_ILN_2016 GBV_ILN_2095 GBV_ILN_2192 GBV_ILN_2279 GBV_ILN_2286 UA 1000 AR 116 2016 22 |
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10.1103/PhysRevLett.116.221101 doi PQ20160719 (DE-627)OLC1976633176 (DE-599)GBVOLC1976633176 (PRQ)a1681-e3937563b1693d2d52e3a9b82063fcc78db8ca35122d6accb2c7d90f882c3d110 (KEY)0009201020160000116002200000testsofgeneralrelativitywithgw150914 DE-627 ger DE-627 rakwb eng 550 DNB UA 1000 AVZ rvk Abbott, B P verfasserin aut Tests of General Relativity with GW150914 2016 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier The LIGO detection of GW150914 provides an unprecedented opportunity to study the two-body motion of a compact-object binary in the large-velocity, highly nonlinear regime, and to witness the final merger of the binary and the excitation of uniquely relativistic modes of the gravitational field. We carry out several investigations to determine whether GW150914 is consistent with a binary black-hole merger in general relativity. We find that the final remnant's mass and spin, as determined from the low-frequency (inspiral) and high-frequency (postinspiral) phases of the signal, are mutually consistent with the binary black-hole solution in general relativity. Furthermore, the data following the peak of GW150914 are consistent with the least-damped quasinormal mode inferred from the mass and spin of the remnant black hole. By using waveform models that allow for parametrized general-relativity violations during the inspiral and merger phases, we perform quantitative tests on the gravitational-wave phase in the dynamical regime and we determine the first empirical bounds on several high-order post-Newtonian coefficients. We constrain the graviton Compton wavelength, assuming that gravitons are dispersed in vacuum in the same way as particles with mass, obtaining a 90%-confidence lower bound of 10^{13} km. In conclusion, within our statistical uncertainties, we find no evidence for violations of general relativity in the genuinely strong-field regime of gravity. General Relativity and Quantum Cosmology Abbott, R oth Abbott, T D oth Abernathy, M R oth Acernese, F oth Ackley, K oth Adams, C oth Adams, T oth Addesso, P oth Adhikari, R X oth Adya, V B oth Affeldt, C oth Agathos, M oth Agatsuma, K oth Aggarwal, N oth Aguiar, O D oth Aiello, L oth Ain, A oth Ajith, P oth Allen, B oth Allocca, A oth Altin, P A oth Anderson, S B oth Anderson, W G oth Arai, K oth Araya, M C oth Arceneaux, C C oth Areeda, J S oth Arnaud, N oth Arun, K G oth Ascenzi, S oth Ashton, G oth Ast, M oth Aston, S M oth Astone, P oth Aufmuth, P oth Aulbert, C oth Babak, S oth Bacon, P oth Bader, M K M oth Baker, P T oth Baldaccini, F oth Ballardin, G oth Ballmer, S W oth Barayoga, J C oth Barclay, S E oth Barish, B C oth Barker, D oth Barone, F oth Barr, B oth Barsotti, L oth Barsuglia, M oth Barta, D oth Bartlett, J oth Bartos, I oth Bassiri, R oth Basti, A oth Batch, J C oth Baune, C oth Bavigadda, V oth Bazzan, M oth Behnke, B oth Bejger, M oth Bell, A S oth Bell, C J oth Berger, B K oth Bergman, J oth Bergmann, G oth Berry, C P L oth Bersanetti, D oth Bertolini, A oth Betzwieser, J oth Bhagwat, S oth Bhandare, R oth Bilenko, I A oth Billingsley, G oth Birch, J oth Birney, R oth Birnholtz, O oth Biscans, S oth Bisht, A oth Bitossi, M oth Biwer, C oth Bizouard, M A oth Blackburn, J K oth Blair, C D oth Blair, D G oth Blair, R M oth Bloemen, S oth Bock, O oth Bodiya, T P oth Boer, M oth Bogaert, G oth Bogan, C oth Bohe, A oth Bojtos, P oth Bond, C oth Bondu, F oth Bonnand, R oth Boom, B A oth ... oth Enthalten in Physical review letters Ridge, NY : American Physical Society, 1958 116(2016), 22 (DE-627)129503959 (DE-600)208853-8 (DE-576)014907267 0031-9007 nnns volume:116 year:2016 number:22 http://dx.doi.org/10.1103/PhysRevLett.116.221101 Volltext http://www.ncbi.nlm.nih.gov/pubmed/27314708 http://arxiv.org/abs/1602.03841 GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY GBV_ILN_21 GBV_ILN_22 GBV_ILN_40 GBV_ILN_47 GBV_ILN_55 GBV_ILN_59 GBV_ILN_60 GBV_ILN_70 GBV_ILN_130 GBV_ILN_2004 GBV_ILN_2016 GBV_ILN_2095 GBV_ILN_2192 GBV_ILN_2279 GBV_ILN_2286 UA 1000 AR 116 2016 22 |
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10.1103/PhysRevLett.116.221101 doi PQ20160719 (DE-627)OLC1976633176 (DE-599)GBVOLC1976633176 (PRQ)a1681-e3937563b1693d2d52e3a9b82063fcc78db8ca35122d6accb2c7d90f882c3d110 (KEY)0009201020160000116002200000testsofgeneralrelativitywithgw150914 DE-627 ger DE-627 rakwb eng 550 DNB UA 1000 AVZ rvk Abbott, B P verfasserin aut Tests of General Relativity with GW150914 2016 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier The LIGO detection of GW150914 provides an unprecedented opportunity to study the two-body motion of a compact-object binary in the large-velocity, highly nonlinear regime, and to witness the final merger of the binary and the excitation of uniquely relativistic modes of the gravitational field. We carry out several investigations to determine whether GW150914 is consistent with a binary black-hole merger in general relativity. We find that the final remnant's mass and spin, as determined from the low-frequency (inspiral) and high-frequency (postinspiral) phases of the signal, are mutually consistent with the binary black-hole solution in general relativity. Furthermore, the data following the peak of GW150914 are consistent with the least-damped quasinormal mode inferred from the mass and spin of the remnant black hole. By using waveform models that allow for parametrized general-relativity violations during the inspiral and merger phases, we perform quantitative tests on the gravitational-wave phase in the dynamical regime and we determine the first empirical bounds on several high-order post-Newtonian coefficients. We constrain the graviton Compton wavelength, assuming that gravitons are dispersed in vacuum in the same way as particles with mass, obtaining a 90%-confidence lower bound of 10^{13} km. In conclusion, within our statistical uncertainties, we find no evidence for violations of general relativity in the genuinely strong-field regime of gravity. General Relativity and Quantum Cosmology Abbott, R oth Abbott, T D oth Abernathy, M R oth Acernese, F oth Ackley, K oth Adams, C oth Adams, T oth Addesso, P oth Adhikari, R X oth Adya, V B oth Affeldt, C oth Agathos, M oth Agatsuma, K oth Aggarwal, N oth Aguiar, O D oth Aiello, L oth Ain, A oth Ajith, P oth Allen, B oth Allocca, A oth Altin, P A oth Anderson, S B oth Anderson, W G oth Arai, K oth Araya, M C oth Arceneaux, C C oth Areeda, J S oth Arnaud, N oth Arun, K G oth Ascenzi, S oth Ashton, G oth Ast, M oth Aston, S M oth Astone, P oth Aufmuth, P oth Aulbert, C oth Babak, S oth Bacon, P oth Bader, M K M oth Baker, P T oth Baldaccini, F oth Ballardin, G oth Ballmer, S W oth Barayoga, J C oth Barclay, S E oth Barish, B C oth Barker, D oth Barone, F oth Barr, B oth Barsotti, L oth Barsuglia, M oth Barta, D oth Bartlett, J oth Bartos, I oth Bassiri, R oth Basti, A oth Batch, J C oth Baune, C oth Bavigadda, V oth Bazzan, M oth Behnke, B oth Bejger, M oth Bell, A S oth Bell, C J oth Berger, B K oth Bergman, J oth Bergmann, G oth Berry, C P L oth Bersanetti, D oth Bertolini, A oth Betzwieser, J oth Bhagwat, S oth Bhandare, R oth Bilenko, I A oth Billingsley, G oth Birch, J oth Birney, R oth Birnholtz, O oth Biscans, S oth Bisht, A oth Bitossi, M oth Biwer, C oth Bizouard, M A oth Blackburn, J K oth Blair, C D oth Blair, D G oth Blair, R M oth Bloemen, S oth Bock, O oth Bodiya, T P oth Boer, M oth Bogaert, G oth Bogan, C oth Bohe, A oth Bojtos, P oth Bond, C oth Bondu, F oth Bonnand, R oth Boom, B A oth ... oth Enthalten in Physical review letters Ridge, NY : American Physical Society, 1958 116(2016), 22 (DE-627)129503959 (DE-600)208853-8 (DE-576)014907267 0031-9007 nnns volume:116 year:2016 number:22 http://dx.doi.org/10.1103/PhysRevLett.116.221101 Volltext http://www.ncbi.nlm.nih.gov/pubmed/27314708 http://arxiv.org/abs/1602.03841 GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY GBV_ILN_21 GBV_ILN_22 GBV_ILN_40 GBV_ILN_47 GBV_ILN_55 GBV_ILN_59 GBV_ILN_60 GBV_ILN_70 GBV_ILN_130 GBV_ILN_2004 GBV_ILN_2016 GBV_ILN_2095 GBV_ILN_2192 GBV_ILN_2279 GBV_ILN_2286 UA 1000 AR 116 2016 22 |
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Tests of General Relativity with GW150914 |
| abstract |
The LIGO detection of GW150914 provides an unprecedented opportunity to study the two-body motion of a compact-object binary in the large-velocity, highly nonlinear regime, and to witness the final merger of the binary and the excitation of uniquely relativistic modes of the gravitational field. We carry out several investigations to determine whether GW150914 is consistent with a binary black-hole merger in general relativity. We find that the final remnant's mass and spin, as determined from the low-frequency (inspiral) and high-frequency (postinspiral) phases of the signal, are mutually consistent with the binary black-hole solution in general relativity. Furthermore, the data following the peak of GW150914 are consistent with the least-damped quasinormal mode inferred from the mass and spin of the remnant black hole. By using waveform models that allow for parametrized general-relativity violations during the inspiral and merger phases, we perform quantitative tests on the gravitational-wave phase in the dynamical regime and we determine the first empirical bounds on several high-order post-Newtonian coefficients. We constrain the graviton Compton wavelength, assuming that gravitons are dispersed in vacuum in the same way as particles with mass, obtaining a 90%-confidence lower bound of 10^{13} km. In conclusion, within our statistical uncertainties, we find no evidence for violations of general relativity in the genuinely strong-field regime of gravity. |
| abstractGer |
The LIGO detection of GW150914 provides an unprecedented opportunity to study the two-body motion of a compact-object binary in the large-velocity, highly nonlinear regime, and to witness the final merger of the binary and the excitation of uniquely relativistic modes of the gravitational field. We carry out several investigations to determine whether GW150914 is consistent with a binary black-hole merger in general relativity. We find that the final remnant's mass and spin, as determined from the low-frequency (inspiral) and high-frequency (postinspiral) phases of the signal, are mutually consistent with the binary black-hole solution in general relativity. Furthermore, the data following the peak of GW150914 are consistent with the least-damped quasinormal mode inferred from the mass and spin of the remnant black hole. By using waveform models that allow for parametrized general-relativity violations during the inspiral and merger phases, we perform quantitative tests on the gravitational-wave phase in the dynamical regime and we determine the first empirical bounds on several high-order post-Newtonian coefficients. We constrain the graviton Compton wavelength, assuming that gravitons are dispersed in vacuum in the same way as particles with mass, obtaining a 90%-confidence lower bound of 10^{13} km. In conclusion, within our statistical uncertainties, we find no evidence for violations of general relativity in the genuinely strong-field regime of gravity. |
| abstract_unstemmed |
The LIGO detection of GW150914 provides an unprecedented opportunity to study the two-body motion of a compact-object binary in the large-velocity, highly nonlinear regime, and to witness the final merger of the binary and the excitation of uniquely relativistic modes of the gravitational field. We carry out several investigations to determine whether GW150914 is consistent with a binary black-hole merger in general relativity. We find that the final remnant's mass and spin, as determined from the low-frequency (inspiral) and high-frequency (postinspiral) phases of the signal, are mutually consistent with the binary black-hole solution in general relativity. Furthermore, the data following the peak of GW150914 are consistent with the least-damped quasinormal mode inferred from the mass and spin of the remnant black hole. By using waveform models that allow for parametrized general-relativity violations during the inspiral and merger phases, we perform quantitative tests on the gravitational-wave phase in the dynamical regime and we determine the first empirical bounds on several high-order post-Newtonian coefficients. We constrain the graviton Compton wavelength, assuming that gravitons are dispersed in vacuum in the same way as particles with mass, obtaining a 90%-confidence lower bound of 10^{13} km. In conclusion, within our statistical uncertainties, we find no evidence for violations of general relativity in the genuinely strong-field regime of gravity. |
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Tests of General Relativity with GW150914 |
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Abbott, R Abbott, T D Abernathy, M R Acernese, F Ackley, K Adams, C Adams, T Addesso, P Adhikari, R X Adya, V B Affeldt, C Agathos, M Agatsuma, K Aggarwal, N Aguiar, O D Aiello, L Ain, A Ajith, P Allen, B Allocca, A Altin, P A Anderson, S B Anderson, W G Arai, K Araya, M C Arceneaux, C C Areeda, J S Arnaud, N Arun, K G Ascenzi, S Ashton, G Ast, M Aston, S M Astone, P Aufmuth, P Aulbert, C Babak, S Bacon, P Bader, M K M Baker, P T Baldaccini, F Ballardin, G Ballmer, S W Barayoga, J C Barclay, S E Barish, B C Barker, D Barone, F Barr, B Barsotti, L Barsuglia, M Barta, D Bartlett, J Bartos, I Bassiri, R Basti, A Batch, J C Baune, C Bavigadda, V Bazzan, M Behnke, B Bejger, M Bell, A S Bell, C J Berger, B K Bergman, J Bergmann, G Berry, C P L Bersanetti, D Bertolini, A Betzwieser, J Bhagwat, S Bhandare, R Bilenko, I A Billingsley, G Birch, J Birney, R Birnholtz, O Biscans, S Bisht, A Bitossi, M Biwer, C Bizouard, M A Blackburn, J K Blair, C D Blair, D G Blair, R M Bloemen, S Bock, O Bodiya, T P Boer, M Bogaert, G Bogan, C Bohe, A Bojtos, P Bond, C Bondu, F Bonnand, R Boom, B A . |
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Abbott, R Abbott, T D Abernathy, M R Acernese, F Ackley, K Adams, C Adams, T Addesso, P Adhikari, R X Adya, V B Affeldt, C Agathos, M Agatsuma, K Aggarwal, N Aguiar, O D Aiello, L Ain, A Ajith, P Allen, B Allocca, A Altin, P A Anderson, S B Anderson, W G Arai, K Araya, M C Arceneaux, C C Areeda, J S Arnaud, N Arun, K G Ascenzi, S Ashton, G Ast, M Aston, S M Astone, P Aufmuth, P Aulbert, C Babak, S Bacon, P Bader, M K M Baker, P T Baldaccini, F Ballardin, G Ballmer, S W Barayoga, J C Barclay, S E Barish, B C Barker, D Barone, F Barr, B Barsotti, L Barsuglia, M Barta, D Bartlett, J Bartos, I Bassiri, R Basti, A Batch, J C Baune, C Bavigadda, V Bazzan, M Behnke, B Bejger, M Bell, A S Bell, C J Berger, B K Bergman, J Bergmann, G Berry, C P L Bersanetti, D Bertolini, A Betzwieser, J Bhagwat, S Bhandare, R Bilenko, I A Billingsley, G Birch, J Birney, R Birnholtz, O Biscans, S Bisht, A Bitossi, M Biwer, C Bizouard, M A Blackburn, J K Blair, C D Blair, D G Blair, R M Bloemen, S Bock, O Bodiya, T P Boer, M Bogaert, G Bogan, C Bohe, A Bojtos, P Bond, C Bondu, F Bonnand, R Boom, B A . |
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| doi_str |
10.1103/PhysRevLett.116.221101 |
| up_date |
2024-07-03T16:15:38.944Z |
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