@Article{AasiAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAABBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBBCCBCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCCDCDDDDDDDDDDDDDDDDDDDRDDDDDDDDDDDDDDDDDDDDDDEEEEEEEEEEEEEFFFFFFFFFFFFFFFFFFFFFFFFFFFFFFFFGGGGGGGGGGGGGGGGGGGGGGGGGGGGGGGGGGGGGGGGGGHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHHIIIIIIJJJJJJJJJJJHKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKKLLLLLLLLLLLLLLLLLLLLLLLLLLLLLLLLLLLLLLLLLLLLMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMNNNNNNNNNNNNNNNOOOOOOOOOOOOOOPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPPQQQQQRRRRRRRRRRRRRRRRRRRRRRRRRRRRRRRRRRRRRSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSTTTTTTTTTTTTTTTTTTTTUUUUVVVVVVVVVVVVVVVVVVVVVVVVVVVVVVWWWWWWWWWWWWWWWWWWWWWWWWWWWWWWWWWWWWWWWWYYYYYYYYZZZZZZZZZZ:2014:SeGrWa,
author = "Aasi, J. and Abbott, B. P. and Abbott, R. and Abbott, T. and
Abernathy, M. R. and Acernese, F. and Ackley, K. and Adams, C. and
Adams, T. and Addesso, P. and Adhikari, R. X. and Affeldt, C. and
Agathos, M. and Aggarwal, N. and Aguiar, Odylio Denys de and Ain,
A. and Ajith, P. and Alemic, A. and Allen, B. and Allocca, A. and
Amariutei, D. and Andersen, M. and Anderson, R. and Anderson, S.
B. and Anderson, W. G. and Arai, K. and Araya, M. C. and
Arceneaux, C. and Areeda, J. and Aston, S. M. and Astone, P. and
Aufmuth, P. and Aulbert, C. and Austin, L. and Aylott, B. E. and
Babak, S. and Baker, P. T. and Ballardin, G. and Ballmer, S. W.
and Barayoga, J. C. and Barbet, M. and Barish, B. C. and Barker,
D. and Barone, F. and Barr, B. and Barsotti, L. and Barsuglia, M.
and Barton, M. A. and Bartos, I. and Bassiri, R. and Basti, A. and
Batch, J. C. and Bauchrowitz, J. and Bauer, T. H. S. and
Bavigadda, V. and Behnke, B. and Bejger, M. and Beker, M. G. and
Belczynski, C. and Bell, A. S. and Bell, C. and Benacquista, M.
and Bergmann, G. and Bersanetti, D. and Bertolini, A. and
Betzwieser, J. and Beyersdorf, P. T. and Bilenko, I. A. and
Billingsley, G. and Birch, J. and Biscans, S. and Bitossi, M. and
Bizouard, M. A. and Black, E. and Blackburn, J. K. and Blackburn,
L. and Blair, D. and Bloemen, S. and Bock, O. and Bodiya, T. P.
and Boer, M. and Bogaert, G. and Bogan, C. and Bond, C. and Bondu,
F. and Bonelli, L. and Bonnand, R. and Bork, R. and Born, M. and
Boschi, V. and Bose, S. and Bosi, L. and Bradaschia, C. and Brady,
P. R. and Braginsky, V. B. and Branchesi, M. and Brau, J. E. and
Briant, T. and Bridges, D. O. and Brillet, A. and Brinkmann, M.
and Brisson, V. and Brooks, A. F. and Brown, D. A. and Brown, D.
D. and Br{\"u}ckner, F. and Buchman, S. and Bulik, T. and Bulten,
H. J. and Buonanno, A. and Burman, R. and Buskulic, D. and Buy, C.
and Cadonati, L. and Cagnoli, G. and Bustillo, J. C. and Calloni,
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affiliation = "{} and {} and {} and {} and {} and {} and {} and {} and {} and {}
and {} and {} and {} and {} and {Instituto Nacional de Pesquisas
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{} and {} and {} and {} and {} and {Instituto Nacional de
Pesquisas Espaciais (INPE)}",
title = "Search for gravitational wave ringdowns from perturbed
intermediate mass black holes in LIGO-Virgo data from 2005-2010",
journal = "Physical Review D",
year = "2014",
volume = "89",
number = "10",
pages = "102006 (18pp.)",
abstract = "We report results from a search for gravitational waves produced
by perturbed intermediate mass black holes (IMBH) in data
collected by LIGO and Virgo between 2005 and 2010. The search was
sensitive to astrophysical sources that produced damped sinusoid
gravitational wave signals, also known as ringdowns, with
frequency 50df0/Hzd2000 and decay timescale 0.0001 {\"A}/s 0.1
characteristic of those produced in mergers of IMBH pairs. No
significant gravitational wave candidate was detected. We report
upper limits on the astrophysical coalescence rates of IMBHs with
total binary mass 50dM/M d450 and component mass ratios of either
1:1 or 4:1. For systems with total mass 100dM/M d150, we report a
90% confidence upper limit on the rate of binary IMBH mergers with
nonspinning and equal mass components of 6.9×10-8Mpc-3yr-1. We
also report a rate upper limit for ringdown waveforms from
perturbed IMBHs, radiating 1% of their mass as gravitational waves
in the fundamental, = m=2, oscillation mode, that is nearly three
orders of magnitude more stringent than previous results. © 2014
American Physical Society.",
doi = "10.1103/PhysRevD.89.102006",
url = "http://dx.doi.org/10.1103/PhysRevD.89.102006",
issn = "1550-2368 and 1550-7998",
label = "scopus 2014-07
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language = "en",
targetfile = "PhysRevD.89.102006.pdf",
urlaccessdate = "27 abr. 2024"
}