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We report results of a wideband search for periodic gravitational waves from isolated neutron stars within the Orion spur towards both the inner and outer regions of our Galaxy. As gravitational waves interact very weakly with matter, the search is unimpeded by dust and concentrations of stars. One search disk (A) is 6.87° in diameter and centered on 20h10m54.71s+33°33′25.29′′, and the other (B) is 7.45° in diameter and centered on 8h35m20.61s−46°49′25.151′′. We explored the frequency range of 50–1500 Hz and frequency derivative from 0 to −5×10−9 Hz/s. A multistage, loosely coherent search program allowed probing more deeply than before in these two regions, while increasing coherence length with every stage. Rigorous follow-up parameters have winnowed the initial coincidence set to only 70 candidates, to be examined manually. None of those 70 candidates proved to be consistent with an isolated gravitational-wave emitter, and 95% confidence level upper limits were placed on continuous-wave strain amplitudes. Near 169 Hz we achieve our lowest 95% C.L. upper limit on the worst-case linearly polarized strain amplitude h0 of 6.3×10−25, while at the high end of our frequency range we achieve a worst-case upper limit of 3.4×10−24 for all polarizations and sky locations.
Aasi, J., Abbott, B. ., Abbott, R., Abbott, T. ., Abernathy, M. ., Acernese, F., et al. (2016). Search of the Orion spur for continuous gravitational waves using a loosely coherent algorithm on data from LIGO interferometers. PHYSICAL REVIEW D, 93(4), 042006-1-042006-14 [10.1103/PhysRevD.93.042006].
Search of the Orion spur for continuous gravitational waves using a loosely coherent algorithm on data from LIGO interferometers
Aasi, J.;Abbott, B. .p.;Abbott, R.;Abbott, T. .d.;Abernathy, M. .r.;Acernese, F.;Ackley, K.;Adams, C.;Adams, T.;Addesso, P.;Adhikari, R. .x.;Adya, V. .b.;Affeldt, C.;Agathos, M.;Agatsuma, K.;Aggarwal, N.;Aguiar, O. .d.;Ain, A.;Ajith, P.;Allen, B.;Allocca, A.;Amariutei, D. .v.;Andersen, M.;Anderson, S. .b.;Anderson, W. .g.;Arai, K.;Araya, M. .c.;Arceneaux, C. .c.;Areeda, J. .s.;Arnaud, N.;Ashton, G.;Aston, S. .m.;Astone, P.;Aufmuth, P.;Aulbert, C.;Babak, S.;Baker, P. .t.;Baldaccini, F.;Ballardin, G.;Ballmer, S. .w.;Barayoga, J. .c.;Barclay, S. .e.;Barish, B. .c.;Barker, D.;Barone, F.;Barr, B.;Barsotti, L.;Barsuglia, M.;Bartlett, J.;Barton, M. .a.;Bartos, I.;Bassiri, R.;Basti, A.;Batch, J. .c.;Baune, C.;Bavigadda, V.;Behnke, B.;Bejger, M.;Belczynski, C.;Bell, A. .s.;Berger, B. .k.;Bergman, J.;Bergmann, G.;Berry, C. .p. .l.;Bersanetti, D.;Bertolini, A.;Betzwieser, J.;Bhagwat, S.;Bhandare, R.;Bilenko, I. .a.;Billingsley, G.;Birch, J.;Birney, R.;Biscans, S.;Bitossi, M.;Biwer, C.;Bizouard, M. .a.;Blackburn, J. .k.;Blair, C. .d.;Blair, D.;Bloemen, S.;Bock, O.;Bodiya, T. .p.;Boer, M.;Bogaert, G.;Bojtos, P.;Bond, C.;Bondu, F.;Bonnand, R.;Bork, R.;Born, M.;Boschi, V.;Bose, Sukanta;Bradaschia, C.;Brady, P. .r.;Braginsky, V. .b.;BRANCHESI, MARICA;Branco, V.;Brau, J. .e.;Briant, T.;Brillet, A.;Brinkmann, M.;Brisson, V.;Brockill, P.;Brooks, A. .f.;Brown, D. .a.;Brown, D.;Brown, D. .d.;Brown, N. .m.;Buchanan, C. .c.;Buikema, A.;Bulik, T.;Bulten, H. .j.;Buonanno, A.;Buskulic, D.;Buy, C.;Byer, R. .l.;Cadonati, L.;Cagnoli, G.;Bustillo, J. Calderón;Calloni, E.;Camp, J. .b.;Cannon, K. .c.;Cao, J.;Capano, C. .d.;Capocasa, E.;Carbognani, F.;Caride, S.;Diaz, J. Casanueva;Casentini, C.;Caudill, S.;Cavaglià, M.;Cavalier, F.;Cavalieri, R.;Celerier, C.;Cella, G.;Cepeda, C.;CERBONI BAIARDI, LORENZO;Cerretani, G.;Cesarini, E.;Chakraborty, R.;Chalermsongsak, T.;Chamberlin, S. .j.;Chao, S.;Charlton, P.;Chassande Mottin, E.;Chen, X.;Chen, Y.;Cheng, C.;Chincarini, A.;Chiummo, A.;Cho, H. .s.;Cho, M.;Chow, J. .h.;Christensen, N.;Chu, Q.;Chua, S.;Chung, S.;Ciani, G.;Clara, F.;Clark, J. .a.;Cleva, F.;Coccia, E.;Cohadon, P. F.;Colla, A.;Collette, C. .g.;Colombini, M.;Constancio, M.;Conte, A.;Conti, L.;Cook, D.;Corbitt, T. .r.;Cornish, N.;Corsi, A.;Costa, C. .a.;Coughlin, M. .w.;Coughlin, S. .b.;Coulon, J. P.;Countryman, S. .t.;Couvares, P.;Coward, D. .m.;Cowart, M. .j.;Coyne, D. .c.;Coyne, R.;Craig, K.;Creighton, J. .d. .e.;Creighton, T.;Cripe, J.;Crowder, S. .g.;Cumming, A.;Cunningham, L.;Cuoco, E.;Canton, T. Dal;Damjanic, M. .d.;Danilishin, S. .l.;D’Antonio, S.;Danzmann, K.;Darman, N. .s.;Dattilo, V.;Dave, I.;Daveloza, H. .p.;Davier, M.;Davies, G. .s.;Daw, E. .j.;Day, R.;Debra, D.;Debreczeni, G.;Degallaix, J.;De Laurentis, M.;Deléglise, S.;Del Pozzo, W.;Denker, T.;Dent, T.;Dereli, H.;Dergachev, V.;De Rosa, R.;Derosa, R. .t.;Desalvo, R.;Dhurandhar, S.;Díaz, M. .c.;Di Fiore, L.;Di Giovanni, M.;Di Lieto, A.;Di Palma, I.;Di Virgilio, A.;Dojcinoski, G.;Dolique, V.;Dominguez, E.;Donovan, F.;Dooley, K. .l.;Doravari, S.;Douglas, R.;Downes, T. .p.;Drago, M.;Drever, R. .w. .p.;Driggers, J. .c.;Du, Z.;Ducrot, M.;Dwyer, S. .e.;Edo, T. .b.;Edwards, M. .c.;Edwards, M.;Effler, A.;Eggenstein, H. 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.m.;Pitkin, M.;Poeld, J. .h.;Poggiani, R.;Post, A.;Powell, J.;Prasad, J.;Predoi, V.;Premachandra, S. .s.;Prestegard, T.;Price, L. .r.;Prijatelj, M.;Principe, M.;Privitera, S.;Prix, R.;Prodi, G. .a.;Prokhorov, L.;Puncken, O.;Punturo, M.;Puppo, P.;Pürrer, M.;Qin, J.;Quetschke, V.;Quintero, E. .a.;Quitzow James, R.;Raab, F. .j.;Rabeling, D. .s.;Rácz, I.;Radkins, H.;Raffai, P.;Raja, S.;Rakhmanov, M.;Rapagnani, P.;Raymond, V.;Razzano, M.;Re, V.;Reed, C. .m.;Regimbau, T.;Rei, L.;Reid, S.;Reitze, D. .h.;Ricci, F.;Riles, K.;Robertson, N. .a.;Robie, R.;Robinet, F.;Rocchi, A.;Rodger, A. .s.;Rolland, L.;Rollins, J. .g.;Roma, V. .j.;Romano, R.;Romanov, G.;Romie, J. .h.;Rosińska, D.;Rowan, S.;Rüdiger, A.;Ruggi, P.;Ryan, K.;Sachdev, S.;Sadecki, T.;Sadeghian, L.;Saleem, M.;Salemi, F.;Sammut, L.;Sanchez, E.;Sandberg, V.;Sanders, J. .r.;Santiago Prieto, I.;Sassolas, B.;Saulson, P. .r.;Savage, R.;Sawadsky, A.;Schale, P.;Schilling, R.;Schmidt, P.;Schnabel, R.;Schofield, R. .m. .s.;Schönbeck, A.;Schreiber, E.;Schuette, D.;Schutz, B. .f.;Scott, J.;Scott, S. .m.;Sellers, D.;Sentenac, D.;Sequino, V.;Sergeev, A.;Serna, G.;Sevigny, A.;Shaddock, D. .a.;Shaffery, P.;Shah, S.;Shahriar, M. .s.;Shaltev, M.;Shao, Z.;Shapiro, B.;Shawhan, P.;Shoemaker, D. .h.;Sidery, T. .l.;Siellez, K.;Siemens, X.;Sigg, D.;Silva, A. .d.;Simakov, D.;Singer, A.;Singer, L. .p.;Singh, R.;Sintes, A. .m.;Slagmolen, B. .j. .j.;Smith, J. .r.;Smith, N. .d.;Smith, R. .j. .e.;Son, E. .j.;Sorazu, B.;Souradeep, T.;Srivastava, A. .k.;Staley, A.;Stebbins, J.;Steinke, M.;Steinlechner, J.;Steinlechner, S.;Steinmeyer, D.;Stephens, B. .c.;Steplewski, S.;Stevenson, S. .p.;Stone, R.;Strain, K. .a.;Straniero, N.;Strauss, N. .a.;Strigin, S.;Sturani, R.;Stuver, A. .l.;Summerscales, T. .z.;Sun, L.;Sutton, P. .j.;Swinkels, B. .l.;Szczepanczyk, M. .j.;Tacca, M.;Talukder, D.;Tanner, D. .b.;Tápai, M.;Tarabrin, S. .p.;Taracchini, A.;Taylor, R.;Theeg, T.;Thirugnanasambandam, M. .p.;Thomas, M.;Thomas, P.;Thorne, K. .a.;Thorne, K. .s.;Thrane, E.;Tiwari, S.;Tiwari, V.;Tokmakov, K. .v.;Tomlinson, C.;Tonelli, M.;Torres, C. .v.;Torrie, C. .i.;Travasso, F.;Traylor, G.;Trifirò, D.;Tringali, M. .c.;Tse, M.;Turconi, M.;Ugolini, D.;Unnikrishnan, C. .s.;Urban, A. .l.;Usman, S. .a.;Vahlbruch, H.;Vajente, G.;Valdes, G.;Vallisneri, M.;van Bakel, N.;van Beuzekom, M.;van den Brand, J. .f. .j.;van den Broeck, C.;van der Schaaf, L.;van der Sluys, M. .v.;van Heijningen, J.;van Veggel, A. .a.;Vansuch, G.;Vardaro, M.;Vass, S.;Vasúth, M.;Vaulin, R.;Vecchio, A.;Vedovato, G.;Veitch, J.;Veitch, P. .j.;Venkateswara, K.;Verkindt, D.;VETRANO, FLAVIO;VICERE', ANDREA;Vinet, J. 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2016
Abstract
We report results of a wideband search for periodic gravitational waves from isolated neutron stars within the Orion spur towards both the inner and outer regions of our Galaxy. As gravitational waves interact very weakly with matter, the search is unimpeded by dust and concentrations of stars. One search disk (A) is 6.87° in diameter and centered on 20h10m54.71s+33°33′25.29′′, and the other (B) is 7.45° in diameter and centered on 8h35m20.61s−46°49′25.151′′. We explored the frequency range of 50–1500 Hz and frequency derivative from 0 to −5×10−9 Hz/s. A multistage, loosely coherent search program allowed probing more deeply than before in these two regions, while increasing coherence length with every stage. Rigorous follow-up parameters have winnowed the initial coincidence set to only 70 candidates, to be examined manually. None of those 70 candidates proved to be consistent with an isolated gravitational-wave emitter, and 95% confidence level upper limits were placed on continuous-wave strain amplitudes. Near 169 Hz we achieve our lowest 95% C.L. upper limit on the worst-case linearly polarized strain amplitude h0 of 6.3×10−25, while at the high end of our frequency range we achieve a worst-case upper limit of 3.4×10−24 for all polarizations and sky locations.
Aasi, J., Abbott, B. ., Abbott, R., Abbott, T. ., Abernathy, M. ., Acernese, F., et al. (2016). Search of the Orion spur for continuous gravitational waves using a loosely coherent algorithm on data from LIGO interferometers. PHYSICAL REVIEW D, 93(4), 042006-1-042006-14 [10.1103/PhysRevD.93.042006].
Aasi, J.; Abbott, B. .p.; Abbott, R.; Abbott, T. .d.; Abernathy, M. .r.; Acernese, F.; Ackley, K.; Adams, C.; Adams, T.; Addesso, P.; Adhikari, R. ...espandi
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11585/865974
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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.