Cosmological Redshift

Introduction to Cosmological Redshift

Cosmological redshift is a key concept in astronomy, used to measure the expansion of the universe. It occurs when the wavelength of light from a distant source is stretched as the universe expands, shifting toward the red end of the spectrum. The formula for calculating cosmological redshift is given by z, where λ_observed is the observed wavelength and λ_initial is the initial (emitted) wavelength.

Parameter Usage:

• initialWavelength: Initial (emitted) wavelength of the light
• observedWavelength: Observed wavelength of the light

Output:

• z: Cosmological redshift

Data Validation

The wavelengths should be greater than zero.

Summary

This formula helps astronomers quantify the change in wavelength of light from distant celestial objects due to the expansion of the universe, allowing for the measurement of cosmological distances.