Cosmic voids are regions in the large-scale structure of space that have very low cosmic mean densities. These zones have less than one-tenth of the average density of matter abundance that is considered typical for the observable Universe. This serves as a working definition even though there is no single agreed upon definition of what constitutes a void. The matter density value used for describing the cosmic mean density is usually based on a ratio of the number of galaxies per unit volume rather than the total mass of the matter contained in a unit volume.
- 1 Introduction
- 2 History and Discovery
- 3 Methods for Finding Voids
- 4 Methods for Testing an Algorithm's Robustness
- 5 Significance of Voids
- 6 See also
- 7 References
- 8 External links
The structure of the Universe can be broken down into components that can help describe the characteristics of individual regions of the cosmos. These are the main structural components of the cosmic web:
- Voids – vast regions with very low cosmic mean densities, usually larger than 10 megaparsecs (Mpc) in diameter.
- Walls – the regions that contain the typical cosmic mean density of matter abundance. Walls can be further broken down into two smaller structural features:
History and Discovery
Cosmic voids are a relatively new topic of study in astrophysics, originating only within the past 40 years. The field began in the mid 1970s when redshift surveys became more popular and led two separate teams of astrophysicists in 1978 to identifying superclusters and voids in the distribution of galaxies and Abell clusters in a large region of space. The new redshift surveys revolutionized the field of astronomy by adding depth to the two-dimensional maps of cosmological structure, which were often densely packed and overlapping, allowing for the first three-dimensional mapping of the Universe. The redshift surveys based the depth component on each grouping of galaxies individual redshift resulting from the accelerating expansion of the Universe as noted by Edwin Hubble in the early 1900s.
A summarized timeline of important events in the field of cosmic voids from its beginning to recent times is listed below:
- 1961 – Large scale structural features such as "second order clusters", a specific type of supercluster, were brought to the astronomical community's attention.
- 1978 – The first two papers on the topic of voids in the large scale structure were published referencing voids found in the foreground of the Coma/A1367 clusters.
- 1981 – Discovery of a large void in the Bootes region of the sky that was nearly 50 h−1 Mpc in diameter (which was later recalculated to be about 34 h−1 Mpc).
- 1983 – Computer simulations sophisticated enough to provide relatively reliable results of growth and evolution of the large scale structure emerged and yielded insight on key features of the large scale galaxy distribution.
- 1985 – Details of the supercluster and void structure of the Perseus-Pisces region were surveyed.
- 1989 – The Center for Astrophysics Redshift Survey revealed that large voids, sharp filaments, and the walls that surround them dominate the large-scale structure of the Universe.
- 1991 – The Las Campanas Redshift Survey confirmed the abundance of voids in the large-scale structure of the Universe (Kirshner et al. 1991).
- 1995 – Comparisons of optically selected galaxy surveys indicate that the same voids are found regardless of the sample selection.
- 2001 – The completed two-degree Field Galaxy Redshift Survey adds a significantly large amount of voids to the database of all known cosmic voids.
- 2009 – The latest SDSS (Sloan Digital Sky Survey) data combined with previous large scale surveys now provide the most complete view of the detailed structure of cosmic voids.
Methods for Finding Voids
There exist a number of ways for finding voids with the results of large-scale surveys of the Universe. Of the many different algorithms, virtually all fall into one of three general categories . The first class consists of void finders that try to find empty regions of space based on local galaxy density. The second class are those which try to find voids via the geometrical structures in the dark matter distribution as suggested by the galaxies. The third class is made up of those finders which identify structures dynamically by using gravitationally unstable points in the distribution of dark matter. The three most popular methods through the study of cosmic voids are listed below:
This first class method uses each galaxy in a catalog as its target and then uses the Nearest Neighbor Approximation to calculate the cosmic density in the region contained in a spherical radius determined by the distance to the third closest galaxy. El Ad & Piran introduced this method in 1997 to allow a quick and effective method for standardizing the cataloging of voids. Once the spherical cells are mined from all of the structure data, each cell is expanded until the underdensity returns to average expected wall density values. One of the helpful features of void regions is that their boundaries are very distinct and defined, with a cosmic mean density that starts at 10% in the body and quickly rises to 20% at the edge and then to 100% in the walls directly outside the edges. The remaining walls and overlapping void regions are then gridded into respectively distinct and intertwining zones of filaments, clusters, and near-empty voids. Any overlap of more than 10% with already known voids are considered to be subregions within those known voids. All voids admitted to the catalog had a minimum radius of 10 Mpc in order to ensure all identified voids were not accidentally cataloged due to sampling errors.
ZOBOV (ZOne Bordering On Voidness) Algorithm
This particular second class algorithm uses a Voronoi tessellation technique and mock border particles in order to categorize regions based on a high density contrasting border with a very low amount of bias. Neyrinck introduced this algorithm in 2008 with the purpose of introducing a method that did not contain free parameters or presumed shape tessellations. Therefore, this technique can create more accurately shaped and sized void regions. Although this algorithm has some advantages in shape and size, it has been criticized often for sometimes providing loosely defined results. Since it has no free parameters, it mostly finds small and trivial voids although, the algorithm places a statistical significance on each void it finds. A physical significance parameter can be applied in order to reduce the number of trivial voids by including a minimum density to average density ratio of at least 1:5. Subvoids are also identified using this process which raises more philosophical questions on what qualifies as a void.
DIVA (DynamIcal Void Analysis) Algorithm
This third class method is drastically different from the previous two algorithms listed. The most striking aspect is that it requires a different definition of what it means to be a void. Instead of the general notion that a void is a region of space with a low cosmic mean density; a hole in the distribution of galaxies, it defines voids to be regions in which matter is escaping; which corresponds to the Dark Energy equation of state, w. Void centers are then considered to be the maximal source of the displacement field denoted as Sψ. The purpose for this change in definitions was presented by Lavaux and Wandelt in 2009 as a way to yield cosmic voids such that exact analytical calculations can be made on their dynamical and geometrical properties. This allows DIVA to heavily explore the ellipticity of voids and how they evolve in the large-scale structure, subsequently leading to the classification of three distinct types of voids. These three morphological classes are True voids, Pancake voids, and Filament voids. Another notable quality is that even though DIVA also contains selection function bias just as first class methods do, DIVA is devised such that this bias can be precisely calibrated, leading to much more reliable results. Multiple shortfalls of this Lagrangian-Eulerian hybrid approach exist. One example is that the resulting voids from this method are intrinsically different than those found by other methods, which makes an all-data points inclusive comparison between results of differing algorithms very difficult.
Methods for Testing an Algorithm's Robustness
Once an algorithm is presented to find what it deems to be cosmic voids, it is crucial that its findings approximately match what is expected by the current simulations and models of large-scale structure. In order to perform this, the number, size, and proportion as well as other features of voids found by the algorithm are then checked by placing mock data through a Smoothed Particle Hydrodynamic Halo simulation, ΛCDM model, or other reliable simulator. An algorithm is much more robust if its data is in concordance with the results of these simulations for a range of input criterion (Pan et al. 2011).
Significance of Voids
Since so much time is being dedicated to the study of voids, the question of why they matter to the scientific community arises. The applications of voids is broad and relatively impressive, ranging from shedding light on the current understanding of dark energy, to refining and constraining cosmological evolution models. Some popular applications are mentioned in detail below:
Dark energy equation of state
Voids act as bubbles in the Universe that are sensitive to background cosmological changes. This means that the evolution of a void's shape is largely in part the result of the expansion of the Universe. Since this acceleration is believed to be caused by dark energy, studying the changes of a void's shape over a period of time can further refine the Quintessence + Cold Dark Matter (QCDM) model and provide a more accurate dark energy equation of state.
Galactic formation and evolution models
Cosmic voids contain a mix of galaxies and matter that is slightly different than other regions in the Universe. This unique mix supports the biased galaxy formation picture that is predicted in Gaussian adiabatic cold dark matter models. This phenomena provides an opportunity to modify the morphology-density correlation that holds discrepancies with these voids. Such observations like the morphology-density correlation can help uncover new facets about how galaxies form and evolve on the large scale. On a more local scale, galaxies that reside in voids have differing morphological and spectral properties than those that are located in the walls. One feature that has been found is that voids have been shown to contain a significantly higher fraction of starburst galaxies of young, hot stars when compared to samples of galaxies in walls.
Anomalies in anisotropies
Cold spots, such as the one on the Wilkinson Microwave Anisotropy Probe cosmic microwave background (WMAP CMB) screening, could possibly be explained by an extremely large cosmic void that has a radius of ~120 Mpc, as long as the late integrated Sachs-Wolfe effect was accounted for in the possible solution. Anomalies in CMB screenings are now being potentially explained through the existence of large voids located down the line-of-sight in which the cold spot[s] lie.
Accelerating expansion of the Universe
Although dark energy is currently the most popular explanation for the Universe accelerating, another theory elaborates on the possibility of our galaxy being part of a very large, not-so-underdense, cosmic void. According to this theory, such an environment could naively lead to the demand for dark energy to solve the problem with our observations of Type Ia Supernovae. As more data has been released on this topic the chances of it being a realistic solution in place of the current ΛCDM interpretation has been largely diminished but not all together abandoned.
Void regions often seem to adhere to cosmological parameters which differ from those of the known universe. It is because of this unique feature that cosmic voids make for great laboratories to study the effects that gravitational clustering and growth rates have on local galaxies and structure when the cosmological parameters have different values from the outside universe. Due to the observation that larger voids predominately remain in a linear regime possessing a great deal of spherical symmetry in an underdense environment, testing models for voids can be performed with very high accuracy. The cosmological parameters that differ in these voids are Ωm, ΩΛ, and H0.
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