Abstract
Isolated spinning neutron stars, asymmetric with respect to their rotation axis, are expected to be sources of continuous gravitational waves. The most sensitive searches for these sources are based on accurate matched filtering techniques that assume the continuous wave to be phase locked with the pulsar beamed emission. While matched filtering maximizes the search sensitivity, a significant signal-to-noise ratio loss will happen in the case of a mismatch between the assumed and the true signal phase evolution. Narrow-band algorithms allow for a small mismatch in the frequency and spin-down values of the pulsar while coherently integrating the entire dataset. In this paper, we describe a narrow-band search using LIGO O2 data for the continuous wave emission of 33 pulsars. No evidence of a continuous wave signal is found, and upper limits on the gravitational wave amplitude over the analyzed frequency and spin-down ranges are computed for each of the targets. In this search, we surpass the spin-down limit, namely, the maximum rotational energy loss due to gravitational waves emission for some of the pulsars already present in the LIGO O1 narrow-band search, such as J1400-6325, J1813-1246, J1833-1034, J1952+3252, and for new targets such as J0940-5428 and J1747-2809. For J1400-6325, J1833-1034, and J1747-2809, this is the first time the spin-down limit is surpassed.
Original language | English |
---|---|
Article number | 122002 |
Number of pages | 20 |
Journal | Physical Review D |
Volume | 99 |
Issue number | 12 |
DOIs | |
Publication status | Published - 15 Jun 2019 |
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- 10.1103/PhysRevD.99.122002Licence: CC BY
- 287338357-oaFinal published version, 1.27 MB
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In: Physical Review D, Vol. 99, No. 12, 122002, 15.06.2019.
Research output: Contribution to journal › Article › Research › peer-review
TY - JOUR
T1 - Narrow-band search for gravitational waves from known pulsars using the second LIGO observing run
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 - Arène, 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 - 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 - Cavaglià, 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 - Crowder, S. G.
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 - Goncharov, Boris
AU - Lin, Fuhui
AU - Sammut, Letizia
AU - Sarin, Nikhil
AU - Thrane, Eric
PY - 2019/6/15
Y1 - 2019/6/15
N2 - Isolated spinning neutron stars, asymmetric with respect to their rotation axis, are expected to be sources of continuous gravitational waves. The most sensitive searches for these sources are based on accurate matched filtering techniques that assume the continuous wave to be phase locked with the pulsar beamed emission. While matched filtering maximizes the search sensitivity, a significant signal-to-noise ratio loss will happen in the case of a mismatch between the assumed and the true signal phase evolution. Narrow-band algorithms allow for a small mismatch in the frequency and spin-down values of the pulsar while coherently integrating the entire dataset. In this paper, we describe a narrow-band search using LIGO O2 data for the continuous wave emission of 33 pulsars. No evidence of a continuous wave signal is found, and upper limits on the gravitational wave amplitude over the analyzed frequency and spin-down ranges are computed for each of the targets. In this search, we surpass the spin-down limit, namely, the maximum rotational energy loss due to gravitational waves emission for some of the pulsars already present in the LIGO O1 narrow-band search, such as J1400-6325, J1813-1246, J1833-1034, J1952+3252, and for new targets such as J0940-5428 and J1747-2809. For J1400-6325, J1833-1034, and J1747-2809, this is the first time the spin-down limit is surpassed.
AB - Isolated spinning neutron stars, asymmetric with respect to their rotation axis, are expected to be sources of continuous gravitational waves. The most sensitive searches for these sources are based on accurate matched filtering techniques that assume the continuous wave to be phase locked with the pulsar beamed emission. While matched filtering maximizes the search sensitivity, a significant signal-to-noise ratio loss will happen in the case of a mismatch between the assumed and the true signal phase evolution. Narrow-band algorithms allow for a small mismatch in the frequency and spin-down values of the pulsar while coherently integrating the entire dataset. In this paper, we describe a narrow-band search using LIGO O2 data for the continuous wave emission of 33 pulsars. No evidence of a continuous wave signal is found, and upper limits on the gravitational wave amplitude over the analyzed frequency and spin-down ranges are computed for each of the targets. In this search, we surpass the spin-down limit, namely, the maximum rotational energy loss due to gravitational waves emission for some of the pulsars already present in the LIGO O1 narrow-band search, such as J1400-6325, J1813-1246, J1833-1034, J1952+3252, and for new targets such as J0940-5428 and J1747-2809. For J1400-6325, J1833-1034, and J1747-2809, this is the first time the spin-down limit is surpassed.
UR - http://www.scopus.com/inward/record.url?scp=85068965834&partnerID=8YFLogxK
U2 - 10.1103/PhysRevD.99.122002
DO - 10.1103/PhysRevD.99.122002
M3 - Article
AN - SCOPUS:85068965834
SN - 2470-0010
VL - 99
JO - Physical Review D
JF - Physical Review D
IS - 12
M1 - 122002
ER -