2007/05/31 by Takeshi Chiba, Y. Himemoto, Yoshiaki Himemoto +3 · 10 citations
Mathematics · Physics and Astronomy · #Amplitude #Artificial intelligence #Astrophysics #Black Holes and Theoretical Physics #Computer science #Cosmology and Gravitation Theories #Feature (linguistics) #Geometry #Gravitational wave #Gravitational wave background #Inflation (cosmology) #Mathematics #Noise (video) #Optics #Physics #Pulsars and Gravitational Waves Research #Quantum mechanics #SIGNAL (programming language) #Sensitivity (control systems) #Signature (topology) #Spectral density #Spectral signature #Spectrum (functional analysis) #Statistical physics #Statistics #Template #Theoretical physics #astro-ph #gr-qc #hep-ph
paper · pdf · doi:10.1103/physrevd.76.043516
published in Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields 76(4) (American Physical Society) · 13 pages, 4 figures, final version to be published in PRD
openalex publication_date 2007/08/20 · arxiv created 2007/08/21 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We calculate the signal-to-noise ratio (SNR) of the stochastic gravitational-wave background in an extreme case that its spectrum has a sharp falloff with its amplitude close to the detection threshold. Such a spectral feature is a characteristic imprint of the change in the number of relativistic degrees of freedom on the stochastic background generated during inflation in the early Universe. We find that, although SNR is maximal with the correct template which is proportional to the assumed real spectrum, its sensitivity to the shape of template is fairly weak indicating that a simple power-law template is sufficient to detect the signature.