Sound waves in the early universe that left imprints on the distribution of galaxies.Acoustic oscillations are sound waves that propagated through the hot, dense plasma of the early universe before recombination. These waves were driven by the competition between gravitational attraction and radiation pressure, creating alternating regions of higher and lower density. After the universe cooled enough for neutral atoms to form, these density variations were frozen into the distribution of matter, leaving a characteristic imprint on the cosmic microwave background and on the large-scale structure of galaxies.
The theory was developed in the 1970s and 1980s, with key contributions from P.J.E. Peebles and others. The first clear detection of the acoustic peaks in the cosmic microwave background was made by the BOOMERanG experiment in 2000, followed by more precise measurements from WMAP and Planck.
In the early universe, photons and baryons were tightly coupled, forming a single fluid. Perturbations from quantum fluctuations created pressure waves that traveled at about half the speed of light. Regions where the waves compressed matter became slightly denser, attracting more matter, while rarefactions became voids. When electrons and protons combined to form neutral hydrogen, the photons decoupled and the waves stopped propagating, leaving a characteristic scale — the sound horizon — imprinted in the matter distribution.
The study of acoustic oscillations, particularly baryon acoustic oscillations (BAO), is used as a standard ruler to measure the expansion history of the universe and constrain dark energy properties.
The characteristic scale of these oscillations is about 150 megaparsecs, which means that galaxies are slightly more likely to be separated by that distance than by other scales — a pattern that has been used to map the universe's expansion.












