acoustic oscillation

These two effects compete to create acoustic oscillations which give the microwave background its characteristic peak structure.

Baryon acoustic oscillations, a signature of the early universe observed in galaxy surveys.

This is commonly used to observe so called standard rulers, for example in the context of baryon acoustic oscillations.

Baryon acoustic oscillations, also called galaxy clustering analysis, will serve as an independent measurement of dark energy.

Acoustic oscillations can be excited by thermal processes, such as the flow of hot air through a pipe or combustion in a chamber.

The acoustic oscillations arise because of a conflict in the photon-baryon plasma in the early universe.

For example, the peaks in the power spectrum due to acoustic oscillations are decreased in amplitude by diffusion damping.

Acoustic streaming is a steady current in a fluid driven by the absorption of high amplitude acoustic oscillations.

The baryonic acoustic oscillation signal should be evident in the power spectrum of Lyman-alpha emitters at high redshift.

The structure of the cosmic microwave background anisotropies is principally determined by two effects: acoustic oscillations and diffusion damping.

Other measurements of our physical cosmology rely upon fundamental physics and include techniques like gravitational lensing and baryonic acoustic oscillations.

Baryonic acoustic oscillations are imprints of sound waves on scales where radiation pressure stabilized the density perturbations against gravitational collapse in the early universe.

Baryon Acoustic Oscillations (BAO)

The acoustic oscillations are detectable on almost any time series of solar images, but are best observed by measuring the Doppler shift of photospheric absorption lines.

Note that the CMB data and the BAO data measure the acoustic oscillations at very different distance scales.

Baryon Acoustic Oscillations (BAO) refer to oscillations within the baryon-photon plasma that filled the early universe.

The 6dFGS survey is one of the few surveys which are big enough to allow a Baryon Acoustic Oscillation (BAO) signal to be detected.

Non-linear evolution erases the acoustic oscillations on small scales, while both non-linear mode coupling and scale-dependent bias can shift the positions of the BAO features.

Commonly, the set of observations fitted includes the cosmic microwave background anisotropy, the brightness/redshift relation for supernovae, and large-scale galaxy clustering including the baryon acoustic oscillation feature.

Voids are believed to have been formed by baryon acoustic oscillations in the Big Bang by collapses of mass followed by implosions of the compressed baryonic matter.

Cosmic microwave background anisotropies and baryon acoustic oscillations are only observations that redshifts are larger than expected from a "dusty" Friedmann-Lemaître universe and the local measured Hubble constant.

Furthermore, separate observations of baryon acoustic oscillations, both in the cosmic microwave background and large-scale structure of galaxies, set limits on the ratio of baryons to the total amount of matter.

The WMAP five-year data was combined with measurements from Type Ia supernova (SNe) and Baryon acoustic oscillations (BAO).

In 2013, Cassini data confirmed a 1993 prediction by Porco and Mark Marley that acoustic oscillations within the body of Saturn are responsible for creating particular features in the rings of Saturn.

It will map the spatial distribution of luminous red galaxies (LRGs) and quasars to map the spatial distribution and detect the characteristic scale imprinted by baryon acoustic oscillations in the early universe.