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Volumn 66, Issue 10, 2002, Pages

Time-frequency detection algorithm for gravitational wave bursts

Author keywords

[No Author keywords available]

Indexed keywords

ACCURACY; ALGORITHM; ANALYTIC METHOD; ANALYTICAL ERROR; ARTICLE; CLUSTER ANALYSIS; GRAVITY; INTERFEROMETER; MATHEMATICAL MODEL; SIGNAL DETECTION; TIME;

EID: 0037113862     PISSN: 15507998     EISSN: 15502368     Source Type: Journal    
DOI: 10.1103/PhysRevD.66.102004     Document Type: Article
Times cited : (74)

References (41)
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    • An arbitrary random process can always be reduced to a set of uncorrelated coefficients (“whitened”) by the Karhunen-Loève expansion. Signals are affected by the whitening; however, the only place where this could have an adverse effect here is if the whitening were reducing the amount of clustering of astrophysical signals.
    • An arbitrary random process can always be reduced to a set of uncorrelated coefficients (“whitened”) by the Karhunen-Loève expansion. Signals are affected by the whitening; however, the only place where this could have an adverse effect here is if the whitening were reducing the amount of clustering of astrophysical signals.
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    • The Neyman-Pearson lemma shows that Eq. (3) is optimal when choosing between Eqs. (1) and (2); for the model (Formula presented) with (Formula presented) Eq. (3) is the most efficient estimator for A, in the sense of being unbiased and of achieving the minimum possible mean square error (from the Fisher information, this is (Formula presented): (Formula presented)
    • The Neyman-Pearson lemma shows that Eq. (3) is optimal when choosing between Eqs. (1) and (2); for the model (Formula presented) with (Formula presented) Eq. (3) is the most efficient estimator for A, in the sense of being unbiased and of achieving the minimum possible mean square error (from the Fisher information, this is (Formula presented): (Formula presented)
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    • Rules to use the Itô integral (Formula presented) are similar to those for normal integration, except that second order terms in the increment (Formula presented) are preserved, corresponding to the fact the these increments are (Formula presented) for a Wiener process. See Sec. II of 20 for a pedagogical introduction.
    • Rules to use the Itô integral (Formula presented) are similar to those for normal integration, except that second order terms in the increment (Formula presented) are preserved, corresponding to the fact the these increments are (Formula presented) for a Wiener process. See Sec. II of 20 for a pedagogical introduction.
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    • That is, the proof of Mallat’s heuristic, i.e., that wavelet bases are optimal for representing functions containing singularities, in D.L. Donoho, Appl. Comput. Harmon. Anal. 1, 100 (1993).
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    • Compare Eq. (3.11) with (Formula presented) in 6
    • Compare Eq. (3.11) with (Formula presented) in 6.
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    • That is, Eq. (B16) in 16
    • That is, Eq. (B16) in 16.
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    • An interesting fact about the distribution of sizes of connected clusters is the existence of a critical black pixel probability (Formula presented) such that an infinite (spanning) connected cluster occurs when (Formula presented) see A.R. Conway and A.J. Guttmann, J. Phys. A 28, 891 (1995).
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    • B. Allen et al., Numerical Algorithms Library Specification and Style Guide, LIGO technical note LIGO-T990030-E, 2001; See also http://www.lsc-group.phys.uwm.edu/lal/index.html
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* 이 정보는 Elsevier사의 SCOPUS DB에서 KISTI가 분석하여 추출한 것입니다.