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Bicocca Open Archive
Isolated neutron stars that are asymmetric with respect to their spin axis are possible sources of detectable continuous gravitational waves. This paper presents a fully coherent search for such signals from eighteen pulsars in data from LIGO and Virgo's third observing run (O3). For known pulsars, efficient and sensitive matched-filter searches can be carried out if one assumes the gravitational radiation is phase-locked to the electromagnetic emission. In the search presented here, we relax this assumption and allow both the frequency and the time derivative of the frequency of the gravitational waves to vary in a small range around those inferred from electromagnetic observations. We find no evidence for continuous gravitational waves, and set upper limits on the strain amplitude for each target. These limits are more constraining for seven of the targets than the spin-down limit defined by ascribing all rotational energy loss to gravitational radiation. In an additional search, we look in O3 data for long-duration (hours-months) transient gravitational waves in the aftermath of pulsar glitches for six targets with a total of nine glitches. We report two marginal outliers from this search, but find no clear evidence for such emission either. The resulting duration-dependent strain upper limits do not surpass indirect energy constraints for any of these targets.
Abbott, R., Abbott, T., Acernese, F., Ackley, K., Adams, C., Adhikari, N., et al. (2022). Narrowband Searches for Continuous and Long-duration Transient Gravitational Waves from Known Pulsars in the LIGO-Virgo Third Observing Run. THE ASTROPHYSICAL JOURNAL, 932(2) [10.3847/1538-4357/ac6ad0].
Narrowband Searches for Continuous and Long-duration Transient Gravitational Waves from Known Pulsars in the LIGO-Virgo Third Observing Run
R. Abbott;T. D. Abbott;F. Acernese;K. Ackley;C. Adams;N. Adhikari;R. X. Adhikari;V. B. Adya;C. Affeldt;D. Agarwal;M. Agathos;K. Agatsuma;N. Aggarwal;O. D. Aguiar;L. Aiello;A. Ain;P. Ajith;T. Akutsu;S. Albanesi;A. Allocca;P. A. Altin;A. Amato;C. Anand;S. Anand;A. Ananyeva;S. B. Anderson;W. G. Anderson;M. Ando;T. Andrade;N. Andres;T. Andri??;S. V. Angelova;S. Ansoldi;J. M. Antelis;S. Antier;S. Appert;Koji Arai;Koya Arai;Y. Arai;S. Araki;A. Araya;M. C. Araya;J. S. Areeda;M. Ar??ne;N. Aritomi;N. Arnaud;S. M. Aronson;K. G. Arun;H. Asada;Y. Asali;G. Ashton;Y. Aso;M. Assiduo;S. M. Aston;P. Astone;F. Aubin;C. Austin;S. Babak;F. Badaracco;M. K. M. Bader;C. Badger;S. Bae;Y. Bae;A. M. Baer;S. Bagnasco;Y. Bai;M. Bailes;L. Baiotti;J. Baird;R. Bajpai;M. Ball;G. Ballardin;S. W. Ballmer;A. Balsamo;G. Baltus;S. Banagiri;D. Bankar;J. C. Barayoga;C. Barbieri;B. C. Barish;D. Barker;P. Barneo;F. Barone;B. Barr;L. Barsotti;M. Barsuglia;D. Barta;J. Bartlett;M. A. Barton;I. Bartos;R. Bassiri;A. Basti;M. Bawaj;J. C. Bayley;A. C. Baylor;M. Bazzan;B. B??csy;V. M. Bedakihale;M. Bejger;I. Belahcene;V. Benedetto;D. Beniwal;T. F. Bennett;J. D. Bentley;M. BenYaala;F. Bergamin;B. K. Berger;S. Bernuzzi;D. Bersanetti;A. Bertolini;J. Betzwieser;D. Beveridge;R. Bhandare;U. Bhardwaj;D. Bhattacharjee;S. Bhaumik;I. A. Bilenko;G. Billingsley;S. Bini;R. Birney;O. Birnholtz;S. Biscans;M. Bischi;S. Biscoveanu;A. Bisht;B. Biswas;M. Bitossi;M. -A. Bizouard;J. K. Blackburn;C. D. Blair;D. G. Blair;R. M. Blair;F. Bobba;N. Bode;M. Boer;G. Bogaert;M. Boldrini;L. D. Bonavena;F. Bondu;E. Bonilla;R. Bonnand;P. Booker;B. A. Boom;R. Bork;V. Boschi;N. Bose;S. Bose;V. Bossilkov;V. Boudart;Y. Bouffanais;A. Bozzi;C. Bradaschia;P. R. Brady;A. Bramley;A. Branch;M. Branchesi;J. E. Brau;M. Breschi;T. Briant;J. H. Briggs;A. Brillet;M. Brinkmann;P. Brockill;A. F. Brooks;J. Brooks;D. D. Brown;S. Brunett;G. Bruno;R. Bruntz;J. Bryant;T. Bulik;H. J. Bulten;A. Buonanno;R. Buscicchio;D. Buskulic;C. Buy;R. L. Byer;L. Cadonati;G. 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Ramirez;A. Ramos-Buades;J. Rana;P. Rapagnani;U. D. Rapol;A. Ray;V. Raymond;N. Raza;M. Razzano;J. Read;L. A. Rees;T. Regimbau;L. Rei;S. Reid;S. W. Reid;D. H. Reitze;P. Relton;A. Renzini;P. Rettegno;M. Rezac;F. Ricci;D. Richards;J. W. Richardson;L. Richardson;G. Riemenschneider;K. Riles;S. Rinaldi;K. Rink;M. Rizzo;N. A. Robertson;R. Robie;F. Robinet;A. Rocchi;S. Rodriguez;L. Rolland;J. G. Rollins;M. Romanelli;R. Romano;C. L. Romel;A. Romero-Rodr??guez;I. M. Romero-Shaw;J. H. Romie;S. Ronchini;L. Rosa;C. A. Rose;D. Rosi??ska;M. P. Ross;S. Rowan;S. J. Rowlinson;S. Roy;Santosh Roy;Soumen Roy;D. Rozza;P. Ruggi;K. Ryan;S. Sachdev;T. Sadecki;J. Sadiq;N. Sago;S. Saito;Y. Saito;K. Sakai;Y. Sakai;M. Sakellariadou;Y. Sakuno;O. S. Salafia;L. Salconi;M. Saleem;F. Salemi;A. Samajdar;E. J. Sanchez;J. H. Sanchez;L. E. Sanchez;N. Sanchis-Gual;J. R. Sanders;A. Sanuy;T. R. Saravanan;N. Sarin;B. Sassolas;H. Satari;S. Sato;T. Sato;O. Sauter;R. L. Savage;T. Sawada;D. Sawant;H. L. Sawant;S. Sayah;D. Schaetzl;M. Scheel;J. Scheuer;M. Schiworski;P. Schmidt;S. Schmidt;R. Schnabel;M. Schneewind;R. M. S. Schofield;A. Sch??nbeck;B. W. Schulte;B. F. Schutz;E. Schwartz;J. Scott;S. M. Scott;M. Seglar-Arroyo;T. Sekiguchi;Y. Sekiguchi;D. Sellers;A. S. Sengupta;D. Sentenac;E. G. Seo;V. Sequino;A. Sergeev;Y. Setyawati;T. Shaffer;M. S. Shahriar;B. Shams;L. Shao;A. Sharma;P. Sharma;P. Shawhan;N. S. Shcheblanov;S. Shibagaki;M. Shikauchi;R. Shimizu;T. Shimoda;K. Shimode;H. Shinkai;T. Shishido;A. Shoda;D. H. Shoemaker;D. M. Shoemaker;S. ShyamSundar;M. Sieniawska;D. Sigg;L. P. Singer;D. Singh;N. Singh;A. Singha;A. M. Sintes;V. Sipala;V. Skliris;B. J. J. Slagmolen;T. J. Slaven-Blair;J. Smetana;J. R. Smith;R. J. E. Smith;J. Soldateschi;S. N. Somala;K. Somiya;E. J. Son;K. Soni;S. Soni;V. Sordini;F. Sorrentino;N. Sorrentino;H. Sotani;R. Soulard;T. Souradeep;E. Sowell;V. Spagnuolo;A. P. Spencer;M. Spera;R. Srinivasan;A. K. Srivastava;V. Srivastava;K. Staats;C. Stachie;D. A. Steer;J. Steinlechner;S. Steinlechner;D. J. Stops;M. Stover;K. A. Strain;L. C. Strang;G. Stratta;A. Strunk;R. Sturani;A. L. Stuver;S. Sudhagar;V. Sudhir;R. Sugimoto;H. G. Suh;T. Z. Summerscales;H. Sun;L. Sun;S. Sunil;A. Sur;J. Suresh;P. J. Sutton;Takamasa Suzuki;Toshikazu Suzuki;B. L. Swinkels;M. J. Szczepa??czyk;P. Szewczyk;M. Tacca;H. Tagoshi;S. C. Tait;H. Takahashi;R. Takahashi;A. Takamori;S. Takano;H. Takeda;M. Takeda;C. J. Talbot;C. Talbot;H. Tanaka;Kazuyuki Tanaka;Kenta Tanaka;Taiki Tanaka;Takahiro Tanaka;A. J. Tanasijczuk;S. Tanioka;D. B. Tanner;D. Tao;L. Tao;E. N. Tapia San Mart??n;C. Taranto;J. D. Tasson;S. Telada;R. Tenorio;J. E. Terhune;L. Terkowski;M. P. Thirugnanasambandam;M. Thomas;P. Thomas;J. E. Thompson;S. R. Thondapu;K. A. Thorne;E. Thrane;Shubhanshu Tiwari;Srishti Tiwari;V. Tiwari;A. M. Toivonen;K. Toland;A. E. Tolley;T. Tomaru;Y. Tomigami;T. Tomura;M. Tonelli;A. Torres-Forn??;C. I. Torrie;I. Tosta e Melo;D. T??yr??;A. Trapananti;F. Travasso;G. Traylor;M. Trevor;M. C. Tringali;A. Tripathee;L. Troiano;A. Trovato;L. Trozzo;R. J. Trudeau;D. S. Tsai;D. Tsai;K. W. Tsang;T. Tsang;J-S. Tsao;M. Tse;R. Tso;K. Tsubono;S. Tsuchida;L. Tsukada;D. Tsuna;T. Tsutsui;T. Tsuzuki;K. Turbang;M. Turconi;D. Tuyenbayev;A. S. Ubhi;N. Uchikata;T. Uchiyama;R. P. Udall;A. Ueda;T. Uehara;K. Ueno;G. Ueshima;C. S. Unnikrishnan;F. Uraguchi;A. L. Urban;T. Ushiba;A. Utina;H. Vahlbruch;G. Vajente;A. Vajpeyi;G. Valdes;M. Valentini;V. Valsan;N. van Bakel;M. van Beuzekom;J. F. J. van den Brand;C. Van Den Broeck;D. C. Vander-Hyde;L. van der Schaaf;J. V. van Heijningen;J. Vanosky;M. H. P. M. van Putten;N. van Remortel;M. Vardaro;A. F. Vargas;V. Varma;M. Vas??th;A. Vecchio;G. Vedovato;J. Veitch;P. J. Veitch;J. Venneberg;G. Venugopalan;D. Verkindt;P. Verma;Y. Verma;D. Veske;F. Vetrano;A. Vicer??;S. Vidyant;A. D. Viets;A. Vijaykumar;V. Villa-Ortega;J. -Y. Vinet;A. Virtuoso;S. Vitale;T. Vo;H. Vocca;E. R. G. von Reis;J. S. A. von Wrangel;C. Vorvick;S. P. Vyatchanin;L. E. Wade;M. Wade;K. J. Wagner;R. C. Walet;M. Walker;G. S. Wallace;L. Wallace;S. Walsh;J. Wang;J. Z. Wang;W. H. Wang;R. L. Ward;J. Warner;M. Was;T. Washimi;N. Y. Washington;J. Watchi;B. Weaver;S. A. Webster;M. Weinert;A. J. Weinstein;R. Weiss;C. M. Weller;F. Wellmann;L. Wen;P. We??els;K. Wette;J. T. Whelan;D. D. White;B. F. Whiting;C. Whittle;D. Wilken;D. Williams;M. J. Williams;A. R. Williamson;J. L. Willis;B. Willke;D. J. Wilson;W. Winkler;C. C. Wipf;T. Wlodarczyk;G. Woan;J. Woehler;J. K. Wofford;I. C. F. Wong;C. Wu;D. S. Wu;H. Wu;S. Wu;D. M. Wysocki;L. Xiao;W-R. Xu;T. Yamada;H. Yamamoto;Kazuhiro Yamamoto;Kohei Yamamoto;T. Yamamoto;K. Yamashita;R. Yamazaki;F. W. Yang;L. Yang;Y. Yang;Yang Yang;Z. Yang;M. J. Yap;D. W. Yeeles;A. B. Yelikar;M. Ying;K. Yokogawa;J. Yokoyama;T. Yokozawa;J. Yoo;T. Yoshioka;Hang Yu;Haocun Yu;H. Yuzurihara;A. Zadro??ny;M. Zanolin;S. Zeidler;T. Zelenova;J. -P. Zendri;M. Zevin;M. Zhan;H. Zhang;J. Zhang;L. Zhang;T. Zhang;Y. Zhang;C. Zhao;G. Zhao;Y. Zhao;Yue Zhao;R. Zhou;Z. Zhou;X. J. Zhu;Z. -H. Zhu;M. E. Zucker;J. Zweizig;D. Antonopoulou;Z. Arzoumanian;A. Basu;S. Bogdanov;I. Cognard;K. Crowter;T. Enoto;C. M. Espinoza;C. M. L. Flynn;E. Fonseca;D. C. Good;L. Guillemot;S. Guillot;A. K. Harding;M. J. Keith;L. Kuiper;M. E. Lower;A. G. Lyne;J. W. McKee;B. W. Meyers;C. Ng;J. L. Palfreyman;R. M. Shannon;B. Shaw;I. H. Stairs;B. W. Stappers;C. M. Tan;G. Theureau;P. Weltevrede
2022
Abstract
Isolated neutron stars that are asymmetric with respect to their spin axis are possible sources of detectable continuous gravitational waves. This paper presents a fully coherent search for such signals from eighteen pulsars in data from LIGO and Virgo's third observing run (O3). For known pulsars, efficient and sensitive matched-filter searches can be carried out if one assumes the gravitational radiation is phase-locked to the electromagnetic emission. In the search presented here, we relax this assumption and allow both the frequency and the time derivative of the frequency of the gravitational waves to vary in a small range around those inferred from electromagnetic observations. We find no evidence for continuous gravitational waves, and set upper limits on the strain amplitude for each target. These limits are more constraining for seven of the targets than the spin-down limit defined by ascribing all rotational energy loss to gravitational radiation. In an additional search, we look in O3 data for long-duration (hours-months) transient gravitational waves in the aftermath of pulsar glitches for six targets with a total of nine glitches. We report two marginal outliers from this search, but find no clear evidence for such emission either. The resulting duration-dependent strain upper limits do not surpass indirect energy constraints for any of these targets.
Abbott, R., Abbott, T., Acernese, F., Ackley, K., Adams, C., Adhikari, N., et al. (2022). Narrowband Searches for Continuous and Long-duration Transient Gravitational Waves from Known Pulsars in the LIGO-Virgo Third Observing Run. THE ASTROPHYSICAL JOURNAL, 932(2) [10.3847/1538-4357/ac6ad0].
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/10281/393248
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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.
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