Abstract
One unanswered question about the binary neutron star coalescence GW170817 is the nature of its post-merger remnant. A previous search for post-merger gravitational waves targeted high-frequency signals from a possible neutron star remnant with a maximum signal duration of 500 s. Here, we revisit the neutron star remnant scenario and focus on longer signal durations, up until the end of the second Advanced LIGO-Virgo observing run, which was 8.5 days after the coalescence of GW170817. The main physical scenario for this emission is the power-law spindown of a massive magnetar-like remnant. We use four independent search algorithms with varying degrees of restrictiveness on the signal waveform and different ways of dealing with noise artefacts. In agreement with theoretical estimates, we find no significant signal candidates. Through simulated signals, we quantify that with the current detector sensitivity, nowhere in the studied parameter space are we sensitive to a signal from more than 1 Mpc away, compared to the actual distance of 40 Mpc. However, this study serves as a prototype for post-merger analyses in future observing runs with expected higher sensitivity.
Original language | English |
---|---|
Article number | 160 |
Number of pages | 19 |
Journal | The Astrophysical Journal |
Volume | 875 |
Issue number | 2 |
DOIs | |
Publication status | Published - 20 Apr 2019 |
Keywords
- gravitational waves
- methods: data analysis
- stars: neutron
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Search for Gravitational Waves from a Long-lived Remnant of the Binary Neutron Star Merger GW170817. / The LIGO Scientific Collaboration and the Virgo Collaboration.
In: The Astrophysical Journal, Vol. 875, No. 2, 160, 20.04.2019.Research output: Contribution to journal › Article › Research › peer-review
TY - JOUR
T1 - Search for Gravitational Waves from a Long-lived Remnant of the Binary Neutron Star Merger GW170817
AU - Abbott, B. P.
AU - Abbott, R.
AU - Abbott, T. D.
AU - Acernese, F.
AU - Ackley, K.
AU - Adams, C.
AU - Adams, T.
AU - Addesso, P.
AU - Adhikari, R. X.
AU - Adya, V. B.
AU - Affeldt, C.
AU - Agarwal, B.
AU - Agathos, M.
AU - Agatsuma, K.
AU - Aggarwal, N.
AU - Aguiar, O. D.
AU - Aiello, L.
AU - Ain, A.
AU - Ajith, P.
AU - Allen, B.
AU - Allen, G.
AU - Allocca, A.
AU - Aloy, M. A.
AU - Altin, P. A.
AU - Amato, A.
AU - Ananyeva, A.
AU - Anderson, S. B.
AU - Anderson, W. G.
AU - Angelova, S. V.
AU - Antier, S.
AU - Appert, S.
AU - Arai, K.
AU - Araya, M. C.
AU - Areeda, J. S.
AU - Arène, M.
AU - Arnaud, N.
AU - Ascenzi, S.
AU - Ashton, G.
AU - Ast, M.
AU - Aston, S. M.
AU - Astone, P.
AU - Atallah, D. V.
AU - Aubin, F.
AU - Aufmuth, P.
AU - Aulbert, C.
AU - Aultoneal, K.
AU - Austin, C.
AU - Avila-Alvarez, A.
AU - Babak, S.
AU - Bacon, P.
AU - Badaracco, F.
AU - Bader, M. K.M.
AU - Bae, S.
AU - Baker, P. T.
AU - Baldaccini, F.
AU - Ballardin, G.
AU - Ballmer, S. W.
AU - Banagiri, S.
AU - Barayoga, J. C.
AU - Barclay, S. E.
AU - Barish, B. C.
AU - Barker, D.
AU - Barkett, K.
AU - Barnum, S.
AU - Barone, F.
AU - Barr, B.
AU - Barsotti, L.
AU - Barsuglia, M.
AU - Barta, D.
AU - Bartlett, J.
AU - Bartos, I.
AU - Bassiri, R.
AU - Basti, A.
AU - Batch, J. C.
AU - Bawaj, M.
AU - Bayley, J. C.
AU - Bazzan, M.
AU - Bécsy, B.
AU - Beer, C.
AU - Bejger, M.
AU - Belahcene, I.
AU - Bell, A. S.
AU - Beniwal, D.
AU - Bensch, M.
AU - Berger, B. K.
AU - Bergmann, G.
AU - Bernuzzi, S.
AU - Bero, J. J.
AU - Berry, C. P.L.
AU - Bersanetti, D.
AU - Bertolini, A.
AU - Betzwieser, J.
AU - Bhandare, R.
AU - Bilenko, I. A.
AU - Bilgili, S. A.
AU - Billingsley, G.
AU - Billman, C. R.
AU - Birch, J.
AU - Birney, R.
AU - Birnholtz, O.
AU - Biscans, S.
AU - Biscoveanu, S.
AU - Bisht, A.
AU - Bitossi, M.
AU - Bizouard, M. A.
AU - Blackburn, J. K.
AU - Blackman, J.
AU - Blair, C. D.
AU - Blair, D. G.
AU - Blair, R. M.
AU - Bloemen, S.
AU - Bock, O.
AU - Bode, N.
AU - Boer, M.
AU - Boetzel, Y.
AU - Bogaert, G.
AU - Bohe, A.
AU - Bondu, F.
AU - Bonilla, E.
AU - Bonnand, R.
AU - Booker, P.
AU - Boom, B. A.
AU - Booth, C. D.
AU - Bork, R.
AU - Boschi, V.
AU - Bose, S.
AU - Bossie, K.
AU - Bossilkov, V.
AU - Bosveld, J.
AU - Bouffanais, Y.
AU - Bozzi, A.
AU - Bradaschia, C.
AU - Brady, P. R.
AU - Bramley, A.
AU - Branchesi, M.
AU - Brau, J. E.
AU - Briant, T.
AU - Brighenti, F.
AU - Brillet, A.
AU - Brinkmann, M.
AU - Brisson, V.
AU - Brockill, P.
AU - Brooks, A. F.
AU - Brown, D. D.
AU - Brunett, S.
AU - Buchanan, C. C.
AU - Buikema, A.
AU - Bulik, T.
AU - Bulten, H. J.
AU - Buonanno, A.
AU - Buskulic, D.
AU - Buy, C.
AU - Byer, R. L.
AU - Cabero, M.
AU - Cadonati, L.
AU - Cagnoli, G.
AU - Cahillane, C.
AU - Bustillo, J. Calderón
AU - Callister, T. A.
AU - Calloni, E.
AU - Camp, J. B.
AU - Canepa, M.
AU - Canizares, P.
AU - Cannon, K. C.
AU - Cao, H.
AU - Cao, J.
AU - Capano, C. D.
AU - Capocasa, E.
AU - Carbognani, F.
AU - Caride, S.
AU - Carney, M. F.
AU - Diaz, J. Casanueva
AU - Casentini, C.
AU - Caudill, S.
AU - Cavaglià, M.
AU - Cavalier, F.
AU - Cavalieri, R.
AU - Cella, G.
AU - Cepeda, C. B.
AU - Cerdá-Durán, P.
AU - Cerretani, G.
AU - Cesarini, E.
AU - Chaibi, O.
AU - Chamberlin, S. J.
AU - Chan, M.
AU - Chao, S.
AU - Charlton, P.
AU - Chase, E.
AU - Chassande-Mottin, E.
AU - Chatterjee, D.
AU - Cheeseboro, B. D.
AU - Chen, H. Y.
AU - Chen, X.
AU - Chen, Y.
AU - Cheng, H. P.
AU - Chia, H. Y.
AU - Chincarini, A.
AU - Chiummo, A.
AU - Chmiel, T.
AU - Cho, H. S.
AU - Cho, M.
AU - Chow, J. H.
AU - Christensen, N.
AU - Chu, Q.
AU - Chua, A. J.K.
AU - Chua, S.
AU - Chung, K. W.
AU - Chung, S.
AU - Ciani, G.
AU - Ciobanu, A. A.
AU - Ciolfi, R.
AU - Cipriano, F.
AU - Cirelli, C. E.
AU - Cirone, A.
AU - Clara, F.
AU - Clark, J. A.
AU - Clearwater, P.
AU - Cleva, F.
AU - Cocchieri, C.
AU - Coccia, E.
AU - Cohadon, P. F.
AU - Cohen, D.
AU - Colla, A.
AU - Collette, C. G.
AU - Collins, C.
AU - Cominsky, L. R.
AU - Constancio, M.
AU - Conti, L.
AU - Cooper, S. J.
AU - Corban, P.
AU - Corbitt, T. R.
AU - Cordero-Carrión, I.
AU - Corley, K. R.
AU - Cornish, N.
AU - Corsi, A.
AU - Cortese, S.
AU - Costa, C. A.
AU - Cotesta, R.
AU - Coughlin, M. W.
AU - Coughlin, S. B.
AU - Coulon, J. P.
AU - Countryman, S. T.
AU - Couvares, P.
AU - Easter, P. J.
AU - Lasky, P. D.
AU - Levin, Y.
AU - Meadors, G. D.
AU - Smith, R. J.E.
AU - Talbot, C.
AU - Zhu, X. J.
AU - The LIGO Scientific Collaboration and the Virgo Collaboration
AU - Goncharov, Boris
AU - Sammut, Letizia
AU - Sarin, Nikhil
AU - Thrane, Eric
PY - 2019/4/20
Y1 - 2019/4/20
N2 - One unanswered question about the binary neutron star coalescence GW170817 is the nature of its post-merger remnant. A previous search for post-merger gravitational waves targeted high-frequency signals from a possible neutron star remnant with a maximum signal duration of 500 s. Here, we revisit the neutron star remnant scenario and focus on longer signal durations, up until the end of the second Advanced LIGO-Virgo observing run, which was 8.5 days after the coalescence of GW170817. The main physical scenario for this emission is the power-law spindown of a massive magnetar-like remnant. We use four independent search algorithms with varying degrees of restrictiveness on the signal waveform and different ways of dealing with noise artefacts. In agreement with theoretical estimates, we find no significant signal candidates. Through simulated signals, we quantify that with the current detector sensitivity, nowhere in the studied parameter space are we sensitive to a signal from more than 1 Mpc away, compared to the actual distance of 40 Mpc. However, this study serves as a prototype for post-merger analyses in future observing runs with expected higher sensitivity.
AB - One unanswered question about the binary neutron star coalescence GW170817 is the nature of its post-merger remnant. A previous search for post-merger gravitational waves targeted high-frequency signals from a possible neutron star remnant with a maximum signal duration of 500 s. Here, we revisit the neutron star remnant scenario and focus on longer signal durations, up until the end of the second Advanced LIGO-Virgo observing run, which was 8.5 days after the coalescence of GW170817. The main physical scenario for this emission is the power-law spindown of a massive magnetar-like remnant. We use four independent search algorithms with varying degrees of restrictiveness on the signal waveform and different ways of dealing with noise artefacts. In agreement with theoretical estimates, we find no significant signal candidates. Through simulated signals, we quantify that with the current detector sensitivity, nowhere in the studied parameter space are we sensitive to a signal from more than 1 Mpc away, compared to the actual distance of 40 Mpc. However, this study serves as a prototype for post-merger analyses in future observing runs with expected higher sensitivity.
KW - gravitational waves
KW - methods: data analysis
KW - stars: neutron
UR - http://www.scopus.com/inward/record.url?scp=85066449138&partnerID=8YFLogxK
U2 - 10.3847/1538-4357/ab0f3d
DO - 10.3847/1538-4357/ab0f3d
M3 - Article
AN - SCOPUS:85066449138
VL - 875
JO - The Astrophysical Journal
JF - The Astrophysical Journal
SN - 1538-4357
IS - 2
M1 - 160
ER -