Gravitational waves are tiny ripples in the fabric of spacetime. These waves interact very weakly with matter, allowing the information imprinted in these signals to travel over billions of light years without distortion from dust or galaxies. This signal clarity offers unprecedented tests of fundamental physics through the laboratory of cosmic collisions and explosions.

Gravitational waves were first predicted by Einstein's general theory of relativity. General relativity tells us that what we feel as gravity is the curvature of spacetime; three-dimensional space and time woven into a four-dimensional mathematical description of our reality. General relativity describes the relationship between the distribution of mass and energy with the curvature of spacetime. Matter both follows the curvature of spacetime and induces spacetime curvature.

Gravitational waves stretch and squeeze spacetime as they pass. This spacetime *strain* is generated by the asymmetric acceleration of matter. Gravitational waves ripple outward from their source at the speed of light.

Below is an illustration of the effect of passing gravitational waves on spacetime strain. A gravitational wave passing through the series of hoops will stretch and squeeze them in perpendicular directions. A gravitational wave detector should be able to sense this perpendicular relative change in length.

ESA.

The Laser Interferometer Gravitational-wave Observatory (LIGO) detectors are designed to sense the orthogonal stretching and squeezing of spacetime produced by gravitational waves. Input laser light is split by a beam splitter so that 50% of the light travels down each of two orthogonal 4 kilometer long arms. Any relative change in length between the two perpendicular arms induced by passing gravitational waves will cause an interference pattern in the light that is read out at the output port.

We can directly sense the relative change in length between the interferometer arms as a time series.

LIGO/Caltech.

The twin LIGO gravitational wave detectors are located in Livingston, Louisiana and Hanford, Washington. There are currently two LIGO detectors in the U.S., with another LIGO detector planned to be built in India.

The LIGO interferometers are the most precise measurement devices ever constructed. The video below shows the measurement of the relative change in length between the 4 kilometer long orthogonal interferometer arms to scale. The LIGO instruments can sense changes in length up to 10,000 times smaller than the width of a proton. This is equivalent to sensing a change in length the width of a human hair between the Earth and the nearest star, Alpha Centauri.

LIGO/Caltech.

Love LIGO? Help gravitational wave astrophysicists discover more signals! Citizen scientists all over the world are contributing to LIGO research with Gravity Spy. This Zooniverse project crowd-sources critical LIGO glitch classifications and helps researchers uncover the noise sources that are interfering with our ability to detect a wider range of astrophysical gravitational wave signals. Gravity Spy users that have helped us solve noise mysteries have been featured in the public LIGO electronic logbooks.

The LIGO Scientific Collaboration (LSC) has more than 1200 members from over 100 instituons all over the world.

If you're an undergraduate student majoring in physics or a closely related field, consider applying for the LIGO Laboratory Summer Undergraduate Research Fellowship program at Caltech. If you're interested in applying for physics Ph.D. programs, many LSC institutions offer top graduate-level research opportunities.

** Learn more! **Excellent resources to explore:

The LIGO Laboratory home page

Amber Stuver's blog Living LIGO

Take me back to the top!