@Article{AbbottAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAABBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBCCCCBCCCCCCCCCCCDCCCCCCCBCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCDDDDDCDDDDDDDDDDDLDPDDDRDDDDDDFGGLPPVDDDDDDD?DDDDDDDEEEEEEEEEEEEEEFFFFFFFFFFFFFGFFFFFFFFFFFFFFFFFFFFFFFGGGGGGGGGGGGGGGGGGGGGGGGGGGGGGCGGGGGGGGGGGGGGGGGGGGGGGHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHIIIIIIIIIJJJJJJJJJJJKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKLLLLLLLLLLLLLLLLLLLLLLLLLLLLLLLLLLLLLLLLLLMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMNNNNNNNNNNNNNNNNNNNOOOOOOOOOOOOOOOPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPQQQQQQRRRRRRRRRRRRRRRRRRRRRRRRRRRRRRRRRRRRSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSTTTTTTTTTTTTTTTTTTTTTTTTTTTTTTTTUUUUVVVBBBBVSHVVVVVVVVVVVVVVVVVVVVVVVVVWWWWWWWWWWWWWWWWWWWWWWWWWWWWWWWWWWWWWWWWWYYYYYYYZZZZZZZZZZZZZZZAFGGHLMRSSKZ:2017:SeGrWa,
author = "Abbott, B. P. and Abbott, R. and Abbott, T. D. and Abernathy, M.
R. and Acernese, F. and Ackley, K. and Adams, C. and Adams, T. and
Addesso, P. and Adhikari, R. X. and Adya, V. B. and Affeldt, C.
and Agathos, M. and Agatsuma, K. and Aggarwal, N. and Aguiar,
Odylio Denys de and Aiello, L. and Ain, A. and Ajith, P. and
Allen, B. and Allocca, A. and Altin, P. A. and Ananyeva, A. and
Anderson, S. B. and Anderson, W. G. and Appert, S. and Arai, K.
and Araya, M. C. and Areeda, J. S. and Arnaud, N. and Arun, K. G.
and Ascenzi, S. and Ashton, G. and Ast, M. and Aston, S. M. and
Astone, P. and Aufmuth, P. and Aulbert, C. and Avila-Alvarez, A.
and Babak, S. and Bacon, P. and Bader, M. K. M. and Baker, P. T.
and Baldaccini, F. and Ballardin, G. and Ballmer, S. W. and
Barayoga, J. C. and Barclay, S. E. and Barish, B. C. and Barker,
D. and Barone, F. and Barr, B. and Barsotti, L. and Barsuglia, M.
and Barta, D. and Bartlett, J. and Bartos, I. and Bassiri, R. and
Basti, A. and Batch, J. C. and Baune, C. and Bavigadda, V. and
Bazzan, M. and B?csy, B. and Beer, C. and Bejger, M. and
Belahcene, I. and Belgin, M. and Bell, A. S. and Berger, B. K. and
Bergmann, G. and Berry, C. P. L. and Bersanetti, D. and Bertolini,
A. and Betzwieser, J. and Bhagwat, S. and Bhandare, R. and
Bilenko, I. A. and Billingsley, G. and Billman, C. R. and Birch,
J. and Birney, R. and Birnholtz, O. and Biscans, S. and Bisht, A.
and Bitossi, M. and Biwer, C. and Bizouard, M. A. and Blackburn,
J. K. and Blackman, J. and Blair, C. D. and Blair, David G and
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Bogaert, G. and Bohe, A. and Bondu, F. and Bonnand, R. and Boom,
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affiliation = "{} and {} and {} and {} and {} and {} and {} and {} and {} and {}
and {} and {} and {} and {} and {} and {Instituto Nacional de
Pesquisas Espaciais (INPE)}",
title = "Search for Gravitational Waves Associated with Gamma-Ray Bursts
during the First Advanced LIGO Observing Run and Implications for
the Origin of GRB 150906B",
journal = "The Astrophysical Journal Letters",
year = "2017",
volume = "841",
number = "89",
pages = "1--17",
note = "{Setores de Atividade: Pesquisa e desenvolvimento
cient{\'{\i}}fico.}",
keywords = "GRB 150906B, Gravitational Waves, Gamma-Ray Bursts.",
abstract = "We present the results of the search for gravitational waves (GWs)
associated with \γ-ray bursts detected during the first
observing run of the Advanced Laser Interferometer
Gravitational-Wave Observatory (LIGO). We find no evidence of a GW
signal for any of the 41 \γ-ray bursts for which LIGO data
are available with sufficient duration. For all \γ-ray
bursts, we place lower bounds on the distance to the source using
the optimistic assumption that GWs with an energy of 10-2M c2
\ were emitted within the 16500 Hz band, and we find a
median 90% confidence limit of 71 Mpc at 150 Hz. For the subset of
19 short/hard \γ-ray bursts, we place lower bounds on
distance with a median 90% confidence limit of 90 Mpc for binary
neutron star (BNS) coalescences, and 150\and 139 Mpc for
neutron starblack hole coalescences with spins aligned to the
orbital angular momentum and in a generic configuration,
respectively. These are the highest distance limits ever achieved
by GW searches. We also discuss in detail the results of the
search for GWs associated with GRB 150906B, an event that was
localized by the InterPlanetary Network near the local galaxy NGC
3313, which is at a luminosity distance of 54 Mpc
(z\=\0.0124). Assuming the \γ-ray emission
is beamed with a jet half-opening angle \30\, we
exclude a BNS and a neutron starblack hole in NGC\3313 as
the progenitor of this event with confidence >99%. Further, we
exclude such progenitors up to a distance of 102 Mpc and 170 Mpc,
respectively.",
doi = "10.3847/1538-4357/aa6c47",
url = "http://dx.doi.org/10.3847/1538-4357/aa6c47",
issn = "2041-8205",
label = "lattes: 3325984959083987 16
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language = "pt",
targetfile = "1611.07947.pdf",
urlaccessdate = "27 abr. 2024"
}