Related Experiment Video
Updated: May 5, 2026
13:43
Correlative Microscopy for 3D Structural Analysis of Dynamic Interactions
Published on: June 24, 2013
13.5K
A correlation between the cosmic microwave background and large-scale structure in the Universe
Stephen Boughn1, Robert Crittenden
1Department of Astronomy, Haverford College, Haverford, Pennsylvania 19041, USA.
Nature
|January 1, 2004
Summary
Dark energy influences the Universe's expansion and structure formation. Researchers detected correlations between cosmic microwave background (CMB) data and large-scale structures, supporting dark energy's role in cosmic evolution.
Area of Science:
- Cosmology
- Astrophysics
Background:
- Cosmic microwave background (CMB) fluctuations and distant supernovae suggest accelerating universal expansion driven by dark energy.
- Dark energy dominates the Universe, impacting expansion rate and slowing matter density fluctuations, thus affecting gravitational collapse.
Purpose of the Study:
- To investigate the influence of dark energy on the growth of cosmic structures.
- To detect correlations between CMB data and large-scale structures as evidence for dark energy's effects.
Main Methods:
- Analyzing fluctuations in cosmic microwave background (CMB) photon temperatures.
- Correlating CMB data with large-scale structure probes: X-ray background and radio galaxy distribution.
Main Results:
- Detected significant correlations between recent CMB data and large-scale structure probes.
- Observed correlations are consistent with predictions for dark energy's influence on structure formation.
Conclusions:
- The study provides observational evidence for dark energy's imprint on the growth of cosmic structure.
- Findings support the existence and effects of dark energy on the Universe's evolution and structure formation.
Related Concept Videos
01:062D NMR: Homonuclear Correlation Spectroscopy (COSY)
1.9K
Homonuclear correlation spectroscopy, or COSY, is a 2-dimensional NMR technique that provides information about coupled protons. Typically, the geminal and vicinal coupling are observed. For example, consider the COSY spectrum of ethyl acetate, where its 1D proton NMR spectrum is plotted along the vertical and horizontal axes with their corresponding chemical shift scale. Three spots on the diagonal corresponding to the three peaks in the 1D proton spectrum are called diagonal peaks. The COSY...
1.9K
01:10Detection of Black Holes
1.7K
Although black holes were theoretically postulated in the 1920s, they remained outside the domain of observational astronomy until the 1970s.
Their closest cousins are neutron stars, which are composed almost entirely of neutrons packed against each other, making them extremely dense. A neutron star has the same mass as the Sun but its diameter is only a few kilometers. Therefore, the escape velocity from their surface is close to the speed of light.
Not until the 1960s, when the first neutron...
Their closest cousins are neutron stars, which are composed almost entirely of neutrons packed against each other, making them extremely dense. A neutron star has the same mass as the Sun but its diameter is only a few kilometers. Therefore, the escape velocity from their surface is close to the speed of light.
Not until the 1960s, when the first neutron...
1.7K
01:17Space-Time Curvature and the General Theory of Relativity
4.4K
In 1905, Albert Einstein published his special theory of relativity. According to this theory, no matter in the universe can attain a speed greater than the speed of light in a vacuum, which thus serves as the speed limit of the universe.
This has been verified in many experiments. However, space and time are no longer absolute. Two observers moving relative to one another do not agree on the length of objects or the passage of time. The mechanics of objects based on Newton's laws of...
This has been verified in many experiments. However, space and time are no longer absolute. Two observers moving relative to one another do not agree on the length of objects or the passage of time. The mechanics of objects based on Newton's laws of...
4.4K
01:09Correlation
12.2K
In statistics, two variables are said to be correlated if the values of one variable are associated with the other variable. Depending on the relationship between two variables, correlation can be of three types– positive correlation, negative correlation, and zero correlation.
Two variables, for example, a and b, are said to be positively correlated if both variables move in the same direction. In other words, a positive correlation exists between two variables, a and b, if:
Two variables, for example, a and b, are said to be positively correlated if both variables move in the same direction. In other words, a positive correlation exists between two variables, a and b, if:
12.2K
01:11Calculating and Interpreting the Linear Correlation Coefficient
6.5K
The correlation coefficient, r, developed by Karl Pearson in the early 1900s, is numerical and provides a measure of strength and direction of the linear association between the independent variable, x, and the dependent variable, y. Hence, it is also known as the Pearson product-moment correlation coefficient. It can be calculated using the following equation:
6.5K
01:10Calibration Curves: Correlation Coefficient
5.0K
In a linear calibration curve, there is a value called the calibration coefficient, denoted by 'r,' which measures the strength and the direction of association between two variables. The correlation coefficient value ranges from −1 to +1. A value of +1 indicates a perfect positive linear correlation, −1 denotes a perfect negative correlation, and 0 implies no correlation between the two variables. A positive correlation value establishes that as one variable increases, the...
5.0K