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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.
Abbott, B. ., Abbott, R., Abbott, T. ., Abraham, S., Acernese, F., Ackley, K., et al. (2019). Narrow-band search for gravitational waves from known pulsars using the second LIGO observing run. PHYSICAL REVIEW D, 99(12) [10.1103/physrevd.99.122002].
Narrow-band search for gravitational waves from known pulsars using the second LIGO observing run
B. P. Abbott;R. Abbott;T. D. Abbott;S. Abraham;F. Acernese;K. Ackley;C. Adams;R. X. Adhikari;V. B. Adya;C. Affeldt;M. Agathos;K. Agatsuma;N. Aggarwal;O. D. Aguiar;L. Aiello;A. Ain;P. Ajith;G. Allen;A. Allocca;M. A. Aloy;P. A. Altin;A. Amato;A. Ananyeva;S. B. Anderson;W. G. Anderson;S. V. Angelova;S. Antier;S. Appert;K. Arai;M. C. Araya;J. S. Areeda;M. Arène;N. Arnaud;S. Ascenzi;G. Ashton;S. M. Aston;P. Astone;F. Aubin;P. Aufmuth;K. AultONeal;C. Austin;V. Avendano;A. Avila-Alvarez;S. Babak;P. Bacon;F. Badaracco;M. K. M. Bader;S. Bae;P. T. Baker;F. Baldaccini;G. Ballardin;S. W. Ballmer;S. Banagiri;J. C. Barayoga;S. E. Barclay;B. C. Barish;D. Barker;K. Barkett;S. Barnum;F. Barone;B. Barr;L. Barsotti;M. Barsuglia;D. Barta;J. Bartlett;I. Bartos;R. Bassiri;A. Basti;M. Bawaj;J. C. Bayley;M. Bazzan;B. Bécsy;M. Bejger;I. Belahcene;A. S. Bell;D. Beniwal;B. K. Berger;G. Bergmann;S. Bernuzzi;J. J. Bero;C. P. L. Berry;D. Bersanetti;A. Bertolini;J. Betzwieser;R. Bhandare;J. Bidler;I. A. Bilenko;S. A. Bilgili;G. Billingsley;J. Birch;R. Birney;O. Birnholtz;S. Biscans;S. Biscoveanu;A. Bisht;M. Bitossi;M. A. Bizouard;J. K. Blackburn;C. D. Blair;D. G. Blair;R. M. Blair;S. Bloemen;N. Bode;M. Boer;Y. Boetzel;G. Bogaert;F. Bondu;E. Bonilla;R. Bonnand;P. Booker;B. A. Boom;C. D. Booth;R. Bork;V. Boschi;S. Bose;K. Bossie;V. Bossilkov;J. Bosveld;Y. Bouffanais;A. Bozzi;C. Bradaschia;P. R. Brady;A. Bramley;M. Branchesi;J. E. Brau;T. Briant;J. H. Briggs;F. Brighenti;A. Brillet;M. Brinkmann;V. Brisson;P. Brockill;A. F. Brooks;D. D. Brown;S. Brunett;A. Buikema;T. Bulik;H. J. Bulten;A. Buonanno;D. Buskulic;C. Buy;R. L. Byer;M. Cabero;L. Cadonati;G. Cagnoli;C. Cahillane;J. Calderón Bustillo;T. A. Callister;E. Calloni;J. B. Camp;W. A. Campbell;M. Canepa;K. C. Cannon;H. Cao;J. Cao;E. Capocasa;F. Carbognani;S. Caride;M. F. Carney;G. Carullo;J. Casanueva Diaz;C. Casentini;S. Caudill;M. Cavaglià;F. Cavalier;R. Cavalieri;G. Cella;P. Cerdá-Durán;G. Cerretani;E. Cesarini;O. Chaibi;K. Chakravarti;S. J. Chamberlin;M. Chan;S. Chao;P. Charlton;E. A. Chase;E. Chassande-Mottin;D. Chatterjee;M. Chaturvedi;B. D. Cheeseboro;H. Y. Chen;X. Chen;Y. Chen;H. -P. Cheng;C. K. Cheong;H. Y. Chia;A. Chincarini;A. Chiummo;G. Cho;H. S. Cho;M. Cho;N. Christensen;Q. Chu;S. Chua;K. W. Chung;S. Chung;G. Ciani;A. A. Ciobanu;R. Ciolfi;F. Cipriano;A. Cirone;F. Clara;J. A. Clark;P. Clearwater;F. Cleva;C. Cocchieri;E. Coccia;P. -F. Cohadon;D. Cohen;R. Colgan;M. Colleoni;C. G. Collette;C. Collins;L. R. Cominsky;M. Constancio;L. Conti;S. J. Cooper;P. Corban;T. R. Corbitt;I. Cordero-Carrión;K. R. Corley;N. Cornish;A. Corsi;S. Cortese;C. A. Costa;R. Cotesta;M. W. Coughlin;S. B. Coughlin;J. -P. Coulon;S. T. Countryman;P. Couvares;P. B. Covas;E. E. Cowan;D. M. Coward;M. J. Cowart;D. C. Coyne;R. Coyne;J. D. E. Creighton;T. D. Creighton;J. Cripe;M. Croquette;S. G. Crowder;T. J. Cullen;A. Cumming;L. Cunningham;E. Cuoco;T. Dal Canton;G. Dálya;S. L. Danilishin;S. D’Antonio;K. Danzmann;A. Dasgupta;C. F. Da Silva Costa;L. 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A. Usman;H. Vahlbruch;G. Vajente;G. Valdes;N. van Bakel;M. van Beuzekom;J. F. J. van den Brand;C. Van Den Broeck;D. C. Vander-Hyde;J. V. van Heijningen;L. van der Schaaf;A. A. van Veggel;M. Vardaro;V. Varma;S. Vass;M. Vasúth;A. Vecchio;G. Vedovato;J. Veitch;P. J. Veitch;K. Venkateswara;G. Venugopalan;D. Verkindt;F. Vetrano;A. Viceré;A. D. Viets;D. J. Vine;J. -Y. Vinet;S. Vitale;T. Vo;H. Vocca;C. Vorvick;S. P. Vyatchanin;A. R. Wade;L. E. Wade;M. Wade;R. Walet;M. Walker;L. Wallace;S. Walsh;G. Wang;H. Wang;J. Z. Wang;W. H. Wang;Y. F. Wang;R. L. Ward;Z. A. Warden;J. Warner;M. Was;J. Watchi;B. Weaver;L. -W. Wei;M. Weinert;A. J. Weinstein;R. Weiss;F. Wellmann;L. Wen;E. K. Wessel;P. Weßels;J. W. Westhouse;K. Wette;J. T. Whelan;B. F. Whiting;C. Whittle;D. M. Wilken;D. Williams;A. R. Williamson;J. L. Willis;B. Willke;M. H. Wimmer;W. Winkler;C. C. Wipf;H. Wittel;G. Woan;J. Woehler;J. K. Wofford;J. Worden;J. L. Wright;D. S. Wu;D. M. Wysocki;L. Xiao;H. Yamamoto;C. C. Yancey;L. Yang;M. J. Yap;M. Yazback;D. W. Yeeles;Hang Yu;Haocun Yu;S. H. R. Yuen;M. Yvert;A. K. Zadrożny;M. Zanolin;T. Zelenova;J. -P. Zendri;M. Zevin;J. Zhang;L. Zhang;T. Zhang;C. Zhao;M. Zhou;Z. Zhou;X. J. Zhu;M. E. Zucker;J. Zweizig;M. Keith;M. Kerr;L. Kuiper;A. K. Harding;A. Lyne;J. Palfreyman;B. Stappers;P. Weltervrede
2019-01-01
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.
Abbott, B. ., Abbott, R., Abbott, T. ., Abraham, S., Acernese, F., Ackley, K., et al. (2019). Narrow-band search for gravitational waves from known pulsars using the second LIGO observing run. PHYSICAL REVIEW D, 99(12) [10.1103/physrevd.99.122002].
Abbott, B ; Abbott, R; Abbott, T ; Abraham, S; Acernese, F; Ackley, K; Adams, C; Adhikari, R ; Adya, V ; Affeldt, C; Agathos, M; Agatsuma, K; Aggarwal...espandi
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/2108/251113
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simulazione ASN
Il report seguente simula gli indicatori relativi alla propria produzione scientifica in relazione alle soglie ASN 2023-2025 del proprio SC/SSD. Si ricorda che il superamento dei valori soglia (almeno 2 su 3) è requisito necessario ma non sufficiente al conseguimento dell'abilitazione. La simulazione si basa sui dati IRIS e sugli indicatori bibliometrici alla data indicata e non tiene conto di eventuali periodi di congedo obbligatorio, che in sede di domanda ASN danno diritto a incrementi percentuali dei valori. La simulazione può differire dall'esito di un’eventuale domanda ASN sia per errori di catalogazione e/o dati mancanti in IRIS, sia per la variabilità dei dati bibliometrici nel tempo. Si consideri che Anvur calcola i valori degli indicatori all'ultima data utile per la presentazione delle domande.
La presente simulazione è stata realizzata sulla base delle specifiche raccolte sul tavolo ER del Focus Group IRIS coordinato dall’Università di Modena e Reggio Emilia e delle regole riportate nel DM 589/2018 e allegata Tabella A. Cineca, l’Università di Modena e Reggio Emilia e il Focus Group IRIS non si assumono alcuna responsabilità in merito all’uso che il diretto interessato o terzi faranno della simulazione. Si specifica inoltre che la simulazione contiene calcoli effettuati con dati e algoritmi di pubblico dominio e deve quindi essere considerata come un mero ausilio al calcolo svolgibile manualmente o con strumenti equivalenti.