Spectrophotometric measurement of binding of S-peptide analogs to S-protein

Finn, Frances M.

doi:10.1021/bi00758a023

Cited by 11 publications

(2 citation statements)

References 17 publications

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“…is the Fourier transform of the time domain single frequency quasi-normal signal that following Berti et al (2006) we approximate using the delta-function (in frequency) approximation, and S h (f ) is the LISA noise spectral density. In practice we calculate S h (f ) using the approximation given by Finn & Thorne (2000) and by Larson et al (2000), which agrees well, except for oscillations at the high-frequency end, with the LISA Sensitivity Curve Generator results 1 . The amplitudes in the two polarization states are denoted by A ± ℓmn , and S ℓmn (ι, β) are the spin-weighted spheroidal harmonics of spin weight 2, which depend on j through the overtone index n. Also the amplitudes A ± ℓmn are functions of j, as…”

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confidence: 68%

Monte Carlo Approach for black hole quasinormal mode spectroscopy with LISA

Jadhav¹,

Burko²

2010

AIP Conference Proceedings

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The signal-to-noise ratio (SNR) for black hole quasinormal mode sources of low-frequency gravitational waves is estimated using a Monte Carlo approach that replaces the all-sky average approximation. We consider an eleven dimensional parameter space that includes both source and detector parameters. We find that in the black-hole mass range M ∼ 4-7×10 6 M ⊙ the SNR is significantly higher than the SNR for the all-sky average case, as a result of the variation of the spin parameter of the sources. This increased SNR may translate to a higher event rate for the Laser Interferometer Space Antenna (LISA). We also study the directional dependence of the SNR, show at which directions in the sky LISA will have greater response, and identify the LISA blind spots.

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