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CRIS Current Research Information System
We employ gravitational-wave radiometry to map the stochastic gravitational wave background expected from a variety of contributing mechanisms and test the assumption of isotropy using data from the Advanced Laser Interferometer Gravitational Wave Observatory’s (aLIGO) first observing run. We also search for persistent gravitational waves from point sources with only minimal assumptions over the 20–1726 Hz frequency band. Finding no evidence of gravitational waves from either point sources or a stochastic background, we set limits at 90% confidence. For broadband point sources, we report upper limits on the gravitational wave energy flux per unit frequency in the range
F(α,Θ)(f)<(0.1–56)×10^−8 erg cm−2 s−1 Hz−1 (f/25 Hz)^(α−)
depending on the sky location Θ and the spectral power index α. For extended sources, we report upper limits on the fractional gravitational wave energy density required to close the Universe of Ω(f, Θ) <(0.39–7.6)×10^−8 sr^−1 (f/25 Hz)^α depending on Θ and α. Directed searches for narrowband gravitational waves from astrophysically interesting objects (Scorpius X-1, Supernova 1987 A, and the Galactic Center) yield median frequency-dependent limits on strain amplitude of h0 < (6.7, 5.5, and 7.0) × 10^−25, respectively, at the most sensitive detector frequencies between 130–175 Hz. This represents a mean improvement of a factor of 2 across the band compared to previous searches of this kind for these sky locations, considering the different quantities of strain constrained in each case.
Abbott, B. .p., Abbott, R., Abbott, T. .d., Abernathy, M. .r., Acernese, F., Ackley, K., et al. (2017). Directional Limits on Persistent Gravitational Waves from Advanced LIGO’s First Observing Run. PHYSICAL REVIEW LETTERS, 118(12), 121102-1-121102-13 [10.1103/PhysRevLett.118.121102].
Directional Limits on Persistent Gravitational Waves from Advanced LIGO’s First Observing Run
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.;Aiello, L.;Ain, A.;Ajith, P.;Allen, B.;Allocca, A.;Altin, P. .a.;Ananyeva, A.;Anderson, S. .b.;Anderson, W. .g.;Appert, S.;Arai, K.;Araya, M. .c.;Areeda, J. .s.;Arnaud, N.;Arun, K. .g.;Ascenzi, S.;Ashton, G.;Ast, M.;Aston, S. .m.;Astone, P.;Aufmuth, P.;Aulbert, C.;Avila Alvarez, A.;Babak, S.;Bacon, P.;Bader, M. .k. .m.;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.;Barta, D.;Bartlett, J.;Bartos, I.;Bassiri, R.;Basti, A.;Batch, J. .c.;Baune, C.;Bavigadda, V.;Bazzan, M.;Beer, C.;Bejger, M.;Belahcene, I.;Belgin, M.;Bell, A. .s.;Berger, B. .k.;Bergmann, G.;Berry, C. .p. .l.;Bersanetti, D.;Bertolini, A.;Betzwieser, J.;Bhagwat, S.;Bhandare, R.;Bilenko, I. .a.;Billingsley, G.;Billman, C. .r.;Birch, J.;Birney, R.;Birnholtz, O.;Biscans, S.;Biscoveanu, A. .s.;Bisht, A.;Bitossi, M.;Biwer, C.;Bizouard, M. .a.;Blackburn, J. .k.;Blackman, J.;Blair, C. .d.;Blair, D. .g.;Blair, R. .m.;Bloemen, S.;Bock, O.;Boer, M.;Bogaert, G.;Bohe, A.;Bondu, F.;Bonnand, R.;Boom, B. .a.;Bork, R.;Boschi, V.;Bose, S.;Bouffanais, Y.;Bozzi, A.;Bradaschia, C.;Brady, P. .r.;Braginsky, V. .b.;BRANCHESI, MARICA;Brau, J. .e.;Briant, T.;Brillet, A.;Brinkmann, M.;Brisson, V.;Brockill, P.;Broida, J. .e.;Brooks, A. .f.;Brown, D. .a.;Brown, D. .d.;Brown, N. .m.;Brunett, S.;Buchanan, C. .c.;Buikema, A.;Bulik, T.;Bulten, H. .j.;Buonanno, A.;Buskulic, D.;Buy, C.;Byer, R. .l.;Cabero, M.;Cadonati, L.;Cagnoli, G.;Cahillane, C.;Calderón Bustillo, J.;Callister, T. .a.;Calloni, E.;Camp, J. .b.;Campbell, W.;Canepa, M.;Cannon, K. .c.;Cao, H.;Cao, J.;Capano, C. .d.;Capocasa, E.;Carbognani, F.;Caride, S.;Casanueva Diaz, J.;Casentini, C.;Caudill, S.;Cavaglià, M.;Cavalier, F.;Cavalieri, R.;Cella, G.;Cepeda, C. .b.;CERBONI BAIARDI, LORENZO;Cerretani, G.;Cesarini, E.;Chamberlin, S. .j.;Chan, M.;Chao, S.;Charlton, P.;Chassande Mottin, E.;Cheeseboro, B. .d.;Chen, H. .y.;Chen, Y.;Cheng, H. P.;Chincarini, A.;Chiummo, A.;Chmiel, T.;Cho, H. .s.;Cho, M.;Chow, J. .h.;Christensen, N.;Chu, Q.;Chua, A. .j. .k.;Chua, S.;Chung, S.;Ciani, G.;Clara, F.;Clark, J. .a.;Cleva, F.;Cocchieri, C.;Coccia, E.;Cohadon, P. F.;Colla, A.;Collette, C. .g.;Cominsky, L.;Constancio, M.;Conti, L.;Cooper, S. .j.;Corbitt, T. .r.;Cornish, N.;Corsi, A.;Cortese, S.;Costa, C. .a.;Coughlin, E.;Coughlin, M. .w.;Coughlin, S. .b.;Coulon, J. 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.c.;Moore, C. .j.;Moraru, D.;Moreno, G.;Morriss, S. .r.;Mours, B.;Mow Lowry, C. .m.;Mueller, G.;Muir, A. .w.;Mukherjee, Arunava;Mukherjee, D.;Mukherjee, S.;Mukund, N.;Mullavey, A.;Munch, J.;Muniz, E. .a. .m.;Murray, P. .g.;Mytidis, A.;Napier, K.;Nardecchia, I.;Naticchioni, L.;Nelemans, G.;Nelson, T. .j. .n.;Neri, M.;Nery, M.;Neunzert, A.;Newport, J. .m.;Newton, G.;Nguyen, T. .t.;Nielsen, A. .b.;Nissanke, S.;Nitz, A.;Noack, A.;Nocera, F.;Nolting, D.;Normandin, M. .e. .n.;Nuttall, L. .k.;Oberling, J.;Ochsner, E.;Oelker, E.;Ogin, G. .h.;Oh, J. .j.;Oh, S. .h.;Ohme, F.;Oliver, M.;Oppermann, P.;Oram, Richard J.;O’Reilly, B.;O’Shaughnessy, R.;Ottaway, D. .j.;Overmier, H.;Owen, B. .j.;Pace, A. .e.;Page, J.;Pai, A.;Pai, S. .a.;Palamos, J. .r.;Palashov, O.;Palomba, C.;Pal Singh, A.;Pan, H.;Pankow, C.;Pannarale, F.;Pant, B. .c.;Paoletti, F.;Paoli, A.;Papa, M. .a.;Paris, H. .r.;Parker, W.;Pascucci, D.;Pasqualetti, A.;Passaquieti, R.;Passuello, D.;Patricelli, B.;Pearlstone, B. .l.;Pedraza, 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2017
Abstract
We employ gravitational-wave radiometry to map the stochastic gravitational wave background expected from a variety of contributing mechanisms and test the assumption of isotropy using data from the Advanced Laser Interferometer Gravitational Wave Observatory’s (aLIGO) first observing run. We also search for persistent gravitational waves from point sources with only minimal assumptions over the 20–1726 Hz frequency band. Finding no evidence of gravitational waves from either point sources or a stochastic background, we set limits at 90% confidence. For broadband point sources, we report upper limits on the gravitational wave energy flux per unit frequency in the range
F(α,Θ)(f)<(0.1–56)×10^−8 erg cm−2 s−1 Hz−1 (f/25 Hz)^(α−)
depending on the sky location Θ and the spectral power index α. For extended sources, we report upper limits on the fractional gravitational wave energy density required to close the Universe of Ω(f, Θ) <(0.39–7.6)×10^−8 sr^−1 (f/25 Hz)^α depending on Θ and α. Directed searches for narrowband gravitational waves from astrophysically interesting objects (Scorpius X-1, Supernova 1987 A, and the Galactic Center) yield median frequency-dependent limits on strain amplitude of h0 < (6.7, 5.5, and 7.0) × 10^−25, respectively, at the most sensitive detector frequencies between 130–175 Hz. This represents a mean improvement of a factor of 2 across the band compared to previous searches of this kind for these sky locations, considering the different quantities of strain constrained in each case.
Abbott, B. .p., Abbott, R., Abbott, T. .d., Abernathy, M. .r., Acernese, F., Ackley, K., et al. (2017). Directional Limits on Persistent Gravitational Waves from Advanced LIGO’s First Observing Run. PHYSICAL REVIEW LETTERS, 118(12), 121102-1-121102-13 [10.1103/PhysRevLett.118.121102].
Abbott, B. . p.; Abbott, R.; Abbott, T. . d.; Abernathy, M. . r.; Acernese, F.; Ackley, K.; Adams, C.; Adams, T.; Addesso, P.; Adhikari, R. . x.; ...espandi
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11585/866035
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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.