Abstract
We present a search for gravitational waves from 222 pulsars with rotation frequencies 10 Hz. We use advanced LIGO data from its first and second observing runs spanning 2015-2017, which provides the highest-sensitivity gravitational-wave data so far obtained. In this search we target emission from both the l = m = 2 mass quadrupole mode, with a frequency at twice that of the pulsar's rotation, and the l = 2, m = 1 mode, with a frequency at the pulsar rotation frequency. The search finds no evidence for gravitational-wave emission from any pulsar at either frequency. For the l = m = 2 mode search, we provide updated upper limits on the gravitational-wave amplitude, mass quadrupole moment, and fiducial ellipticity for 167 pulsars, and the first such limits for a further 55. For 20 young pulsars these results give limits that are below those inferred from the pulsars' spin-down. For the Crab and Vela pulsars our results constrain gravitational-wave emission to account for less than 0.017% and 0.18% of the spin-down luminosity, respectively. For the recycled millisecond pulsar J0711-6830 our limits are only a factor of 1.3 above the spin-down limit, assuming the canonical value of 1038 kg m2 for the star's moment of inertia, and imply a gravitational-wave-derived upper limit on the star's ellipticity of 1.2 × 10-8. We also place new limits on the emission amplitude at the rotation frequency of the pulsars.
| Original language | English |
|---|---|
| Article number | 10 |
| Number of pages | 36 |
| Journal | The Astrophysical Journal |
| Volume | 879 |
| Issue number | 1 |
| DOIs | |
| Publication status | Published - 1 Jul 2019 |
Keywords
- Gravitational Waves
- Pulsars: General
- Stars: Neutron Supporting Material: Machine-Readable Table
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In: The Astrophysical Journal, Vol. 879, No. 1, 10, 01.07.2019.
Research output: Contribution to journal › Article › Research › peer-review
TY - JOUR
T1 - Searches for Gravitational Waves from Known Pulsars at Two Harmonics in 2015-2017 LIGO Data
AU - Abbott, B. P.
AU - Abbott, R.
AU - Abbott, T. D.
AU - Abraham, S.
AU - Acernese, F.
AU - Ackley, K.
AU - Adams, C.
AU - Adhikari, R. X.
AU - Adya, V. B.
AU - Affeldt, C.
AU - Agathos, M.
AU - Agatsuma, K.
AU - Aggarwal, N.
AU - Aguiar, O. D.
AU - Aiello, L.
AU - Ain, A.
AU - Ajith, P.
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 - Arene, M.
AU - Arnaud, N.
AU - Ascenzi, S.
AU - Ashton, G.
AU - Aston, S. M.
AU - Astone, P.
AU - Aubin, F.
AU - Aufmuth, P.
AU - Aultoneal, K.
AU - Austin, C.
AU - Avendano, V.
AU - Avila-Alvarez, A.
AU - Babak, S.
AU - Bacon, P.
AU - Badaracco, F.
AU - Bader, M. K.M.
AU - Bae, S.
AU - Bailes, M.
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 - Bawaj, M.
AU - Bayley, J. C.
AU - Bazzan, M.
AU - Bécsy, B.
AU - Bejger, M.
AU - Belahcene, I.
AU - Bell, A. S.
AU - Beniwal, D.
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 - Bidler, J.
AU - Bilenko, I. A.
AU - Bilgili, S. A.
AU - Billingsley, G.
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 - Blair, C. D.
AU - Blair, D. G.
AU - Blair, R. M.
AU - Bloemen, S.
AU - Bode, N.
AU - Boer, M.
AU - Boetzel, Y.
AU - Bogaert, G.
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 - Briggs, J. H.
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 - 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 - Campbell, W. A.
AU - Canepa, M.
AU - Cannon, K. C.
AU - Cao, H.
AU - Cao, J.
AU - Capocasa, E.
AU - Carbognani, F.
AU - Caride, S.
AU - Carney, M. F.
AU - Carullo, G.
AU - Diaz, J. Casanueva
AU - Casentini, C.
AU - Caudill, S.
AU - Cavaglia, M.
AU - Cavalier, F.
AU - Cavalieri, R.
AU - Cella, G.
AU - Cerdá-Durán, P.
AU - Cerretani, G.
AU - Cesarini, E.
AU - Chaibi, O.
AU - Chakravarti, K.
AU - Chamberlin, S. J.
AU - Chan, M.
AU - Chao, S.
AU - Charlton, P.
AU - Chase, E. A.
AU - Chassande-Mottin, E.
AU - Chatterjee, D.
AU - Chaturvedi, M.
AU - Cheeseboro, B. D.
AU - Chen, H. Y.
AU - Chen, X.
AU - Chen, Y.
AU - Cheng, H. P.
AU - Cheong, C. K.
AU - Chia, H. Y.
AU - Chincarini, A.
AU - Chiummo, A.
AU - Cho, G.
AU - Cho, H. S.
AU - Cho, M.
AU - Christensen, N.
AU - Chu, Q.
AU - Chua, S.
AU - Chung, K. W.
AU - Chung, S.
AU - Ciani, G.
AU - Ciobanu, A. A.
AU - Ciolfi, R.
AU - Cipriano, F.
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 - Colgan, R.
AU - Colleoni, M.
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 - Covas, P. B.
AU - Cowan, E. E.
AU - Coward, D. M.
AU - Cowart, M. J.
AU - Coyne, D. C.
AU - Coyne, R.
AU - Creighton, J. D.E.
AU - Creighton, T. D.
AU - Cripe, J.
AU - Croquette, M.
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 - Hernandez Vivanco, Francisco Javier
AU - The LIGO Scientific Collaboration and the Virgo Collaboration
AU - Lin, Fuhui
AU - Sarin, Nikhil
PY - 2019/7/1
Y1 - 2019/7/1
N2 - We present a search for gravitational waves from 222 pulsars with rotation frequencies 10 Hz. We use advanced LIGO data from its first and second observing runs spanning 2015-2017, which provides the highest-sensitivity gravitational-wave data so far obtained. In this search we target emission from both the l = m = 2 mass quadrupole mode, with a frequency at twice that of the pulsar's rotation, and the l = 2, m = 1 mode, with a frequency at the pulsar rotation frequency. The search finds no evidence for gravitational-wave emission from any pulsar at either frequency. For the l = m = 2 mode search, we provide updated upper limits on the gravitational-wave amplitude, mass quadrupole moment, and fiducial ellipticity for 167 pulsars, and the first such limits for a further 55. For 20 young pulsars these results give limits that are below those inferred from the pulsars' spin-down. For the Crab and Vela pulsars our results constrain gravitational-wave emission to account for less than 0.017% and 0.18% of the spin-down luminosity, respectively. For the recycled millisecond pulsar J0711-6830 our limits are only a factor of 1.3 above the spin-down limit, assuming the canonical value of 1038 kg m2 for the star's moment of inertia, and imply a gravitational-wave-derived upper limit on the star's ellipticity of 1.2 × 10-8. We also place new limits on the emission amplitude at the rotation frequency of the pulsars.
AB - We present a search for gravitational waves from 222 pulsars with rotation frequencies 10 Hz. We use advanced LIGO data from its first and second observing runs spanning 2015-2017, which provides the highest-sensitivity gravitational-wave data so far obtained. In this search we target emission from both the l = m = 2 mass quadrupole mode, with a frequency at twice that of the pulsar's rotation, and the l = 2, m = 1 mode, with a frequency at the pulsar rotation frequency. The search finds no evidence for gravitational-wave emission from any pulsar at either frequency. For the l = m = 2 mode search, we provide updated upper limits on the gravitational-wave amplitude, mass quadrupole moment, and fiducial ellipticity for 167 pulsars, and the first such limits for a further 55. For 20 young pulsars these results give limits that are below those inferred from the pulsars' spin-down. For the Crab and Vela pulsars our results constrain gravitational-wave emission to account for less than 0.017% and 0.18% of the spin-down luminosity, respectively. For the recycled millisecond pulsar J0711-6830 our limits are only a factor of 1.3 above the spin-down limit, assuming the canonical value of 1038 kg m2 for the star's moment of inertia, and imply a gravitational-wave-derived upper limit on the star's ellipticity of 1.2 × 10-8. We also place new limits on the emission amplitude at the rotation frequency of the pulsars.
KW - Gravitational Waves
KW - Pulsars: General
KW - Stars: Neutron Supporting Material: Machine-Readable Table
UR - http://www.scopus.com/inward/record.url?scp=85070731082&partnerID=8YFLogxK
U2 - 10.3847/1538-4357/ab20cb
DO - 10.3847/1538-4357/ab20cb
M3 - Article
AN - SCOPUS:85070731082
SN - 0004-637X
VL - 879
JO - The Astrophysical Journal
JF - The Astrophysical Journal
IS - 1
M1 - 10
ER -