Semi-analytic treatment of the power spectrum with the approximation of constant linear bias provides a way to compare cosmological models to a large amount of data, as Peacock & Dodds (1994, 1996; hereafter PD94 and PD96, respectively) have shown. By applying the appropriate corrections to the observational power spectrum it is possible to recover the underlying linear power spectrum for any g...

Non-relativistic potential models are considered of the pure power V (r) = sgn(q)r and logarithmic V (r) = ln(r) types. It is shown that, from the spectral viewpoint, these potentials are actually in a single family. The log spectra can be obtained from the power spectra by the limit q → 0 taken in a smooth representation Pnl(q) for the eigenvalues Enl(q). A simple approximation formula is deve...

In this paper, a novel method is developed for computing formulae for the power spectra associated with run-length-limited (RLL) codes. Explicit use is made of a compact description of the run-length process associated with the RLL code. This association simplifies the general derivation of the power spectrum. The calculation of the spectra of several RLL codes popular in data storage applicati...

A feature estimation technique is proposed for speech signals that are corrupted by both additive and convolutive noises via combining channel identification with power spectrum estimation. A correlation-matching algorithm is developed for channel identification, and a Gaussian mixture density model of speech DFT spectra is formulated for estimation of speech power spectra. Cepstral features of...

Power spectra of an extensive set of natural images were analysed. Both the total power in a spectrum (corresponding to image contrast) and its dependence on spatial frequency vary considerably between images, and also within images when considered as functions of orientation. A series of probabilistic models for power spectra enabled calculating the information obtained from prior knowledge of...

Theoretically calculated power spectra are compares with observed solar p-mode velocity power spectra over a range of mode degree and frequency. The depth for the sources responsible for exciting p-modes of frequency 2.0 mHz is determined from the asymmetry of their power spectra and found to be about 800 km below the photosphere for quadrupole sources and 150 km if sources are dipole. The sour...

In this work we present experimental and calculated two-dimensional electronic spectra for a 5,15-bisalkynyl porphyrin chromophore. The lowest energy electronic Qy transition couples mainly to a single 380 cm(-1) vibrational mode. The two-dimensional electronic spectra reveal diagonal and cross peaks which oscillate as a function of population time. We analyze both the amplitude and phase distr...

Published galaxy power spectra from the 2dFGRS and SDSS are not in good agreement. We revisit this issue by analyzing both the 2dFGRS and SDSS DR5 catalogues using essentially identical techniques. We confirm that the 2dFGRS exhibits relatively more large scale power than the SDSS, or, equivalently, SDSS has more small scale power. We demonstrate that this difference is due to the r-band select...

21 We present suggestive evidence for an inverse energy cascade within Jupiter’s 22 atmosphere through a calculation of the power spectrum of its kinetic en23 ergy and its cloud patterns. Using Cassini observations, we composed full24 longitudinal mosaics of Jupiter’s atmosphere at several wavelengths. We 25 also utilized image pairs derived from these observations to generate full26 longitudin...

The solar acoustic p-mode line profiles are asymmetric. Velocity spectra have more power on the low-frequency sides, whereas intensity profiles show the opposite sense of asymmetry. Numerical simulations of the upper convection zone have resonant p-modes with the same asymmetries and asymmetry reversal as the observed modes. The temperature and velocity power spectra at optical depth τ cont = 1...