Baryon acoustic oscillations

In cosmology, baryon acoustic oscillations (BAO) refers to an overdensity or clustering of baryonic matter at certain length scales due to acoustic waves which propagated in the early universe. In the same way that supernova experiments providing a "standard candle" for astronomical observations, BAO matter clustering provides a "standard ruler" for length scale in cosmology. The length of this standard ruler (~150 Mpc in today's universe) can be measured by looking at the large scale structure of matter using astronomical surveys. BAO measurements help cosmologists understand more about the nature of dark energy (the acceleration of the universe) by constraining cosmological parameters.

The Early Universe

The early universe consisted of a hot, dense plasma of electrons and baryons (protons and neutrons). Photons (light particles) traveling in this universe were essentially trapped, unable to travel for any considerable distance before interacting with the plasma via Thomson scattering.[need ref] As the universe expanded, the plasma cooled to below 3000 K -- a low enough energy such that the electrons and protons in the plasma could combine to form neutral hydrogen atoms. This recombination happened when the universe was around 400,000 years old, or at a redshift of z = 1100.[need ref] Photons rarely interact with neutral matter, therefore at recombination the universe suddenly became transparent to photons, allowing them to decouple from the matter and free-stream through the universe.[need ref] In other-words, the mean free path of the photons became on the order of the size of the universe. The cosmic microwave background (CMB) radiation is light emitted after recombination which is only now reaching our telescopes. Therefore when we look at Wilkinson Microwave Anisotropy Probe (WMAP) data, we are looking back in time to see an image of the universe when it was only 400,000 years old.[need ref]

Figure 1: Temperature anisotropies of the CMB based on the five year WMAP data.

WMAP indicates (Figure 1) of a smooth, homogeneous universe with density anisotropies of one part in 10⁵.[need ref]. However, when we observe the universe today we find large amounts of structure and density fluctuations. Galaxies, for instance, are 10⁶ times more dense than the universe's mean density. The current belief is that the universe was built in a bottom-up fashion, meaning that the small anisotropies of the early universe acted as gravitational seeds for the structure we see today. Overdense regions attract more matter, while underdense regions attract less, and thus these small anisotropies we see in the CMB become the large scale structures we observe in the universe today.

Cosmic Sound

File:BAO soundwave.jpg

Figure 2: BAO soundwave propagating outward from a single overdensity over time. The baryon density is shown in the left-most column, the photon density is in the middle column, and a graph of the mass profiles are in the right-most column.

Imagine an overdense region of the primordial plasma. While overdensity gravitationally attracts matter towards it, the heat of photon-matter interactions creates a large amount of outward pressure, however there is also a large amount of pressure due to the heat of photon-matter interactions in the plasma. These counteracting forces of gravity and pressure create oscillations, analagous to sound waves created in air by pressure differences.

Consider a single wave originating from this overdense region in the center of the plasma. This region contains dark matter, baryons and photons. The pressure results in a spherical sound wave of both baryons and photons moving with a speed slightly over half the speed of light outwards from the overdensity (Figure 2, row 1). The dark matter only interacts gravitationally and so it stays at the center of the sound wave, the origin of the overdensity. Before decoupling, the photons and baryons move outwards together (Figure 2, rows 2-3). After decoupling (Figure 2, row 4) the photons are no longer interacting with the baryonic matter so they diffuse away (Figure 2, rows 5-6). This relieves the pressure on the system, leaving a shell of baryonic matter at a fixed radius. This radius is often referred to as the sound horizon. Without the photo-baryon pressure driving the system outwards, the only remaining force on the baryons is gravitational. Therefore, the baryons and dark matter (still at the center of the perturbation) form a configuration which includes overdensities of matter both at the original site of the anisotropy and in a shell at the sound horizon (Figure 2, row 7-8).

The ripples in the density of space (shown at the bottom of Figure 2) continue to attract matter and eventually galaxies formed in a similar pattern, therefore one would expect to see a greater number of galaxies separated by the sound horizon than by nearby length scales. This particular configuration of matter occurred at each anisotropy in the early universe, and therefore the universe is not composed of one sound ripple, but many overlapping ripples. As an analogy, imagine dropping many pebbles into a pond and watching the resulting wave patterns in the water. It is not possible to observe this preferred separation of galaxies on the sound horizon scale by eye, but one can measure this signal statistically by looking at the separations of large numbers of galaxies.

Standard Ruler

The physics of the propagation of the baryon waves in the early universe is fairly simple, so cosmologists can predict the size of the sound horizon at recombination. In addition the CMB provides a measurement of this scale to high accuracy. However in the time between present day and recombination the universe has been expanding. This expansion is well supported by observations and is one of the foundations of the Big Bang Model. In the late 90's, observations of supernova determined that not only is the universe expanding, it is expanding at an increasing rate. Better understanding the acceleration of the universe, or dark energy, has become one of the most important questions in cosmology today. In order to understand the nature of the dark energy, it is important to have a variety of ways of measuring this acceleration. BAO can add to the body of knowledge about this acceleration by comparing observations of the sound horizon today (using clustering of galaxies) to the sound horizon at the time of recombination (using the CMB). Thus BAO provides a measuring stick with which to better understand the nature of the acceleration, completely independent from the supernova technique.

BAO Signal in the Sloan Digital Sky Survey

The Sloan Digital Sky Survey (SDSS) is a 2.5-m wide-angle optical telescope at Apache Point Observatory in New Mexico. The goal of this five-year survey was to take images and spectra of millions of celestial objects. Sloan data is a three-dimensional map of the objects in the nearby universe. The SDSS catalog provides a picture of the distribution of matter such that one can search for a BAO signal by seeing if there is a larger number of galaxies separated at the sound horizon.

The Sloan Team looked at a sample of 46,748 luminous red galaxies (LRGs), over 3816 square-degrees of sky (approximately five billion light years in diameter) and out to a redshift of z = 0.47. They analyzed the clustering of these galaxies by calculating a two-point correlation function on the data. The correlation function ($\xi$) is a function of comoving galaxy separation distance (s) and describes the probability that one galaxy will be found within a given distance bin of another (See SDSS Detection Figure). One would expect a high correlation of galaxies at small separation distances (due to the clumpy nature of galaxy formation) and a low correlation at large differences. The BAO signal would show up as a bump in the correlation function at a comoving separation equal to the sound horizon. This signal was detected by the SDSS team in 2005.. SDSS confirmed the WMAP results that the sound horizon is ~150 Mpc in today's universe.

BAO and Dark Matter

The [BAO signal] is a standard ruler such that the length of the sound horizon can be measured as a function of cosmic time. This allows us to determine two cosmological distances: the Hubble parameter, $H(z)$, and the angular diameter distance, $d_{A}(z)$, as a function of redshift $(z)$. By measuring the subtended angle, $\Delta \theta$, of the ruler of length, $\Delta \chi$, these parameters are determined as follows:

$\Delta \theta ={\frac {\Delta \chi }{d_{A}(z)}}$

$d_{A}(z)\propto \int _{0}^{z}{\frac {dz'}{H(z')}}$

the redshift interval, $\Delta z$, can be measured from the data and thus determining the Hubble parameter as a function of redshift:

$c\Delta z=H(z)\Delta \chi$ ${\displaystyle }$

External links

• Martin White's Baryon Acoustic Oscillations and Dark Energy Web Page
• Daniel Eisenstein's Detection of the Baryon Acoustic Peak Web Page
• SDSS BAO Press Release
• Berkeley Astronomy Department BAO Links Page
• Baryon Oscillation Spectroscopic Survey Web Page