Whole Earth Blazar Telescope
The Whole Earth Blazar Telescope (WEBT) is an international group of astronomers founded in 1997 to study blazars, a type of active galactic nucleus that can vary in brightness very quickly, sometimes in hours or less. The collaboration brings together many telescopes that observe in optical, near-infrared, and radio wavelengths. Because the observatories are spread around the world, they can monitor a target almost continuously as the Earth turns, with coverage moving from east to west. WEBT observations are often combined with higher-frequency observations—from ultraviolet to gamma rays—made by space and ground-based facilities, giving a view of blazar emission across nearly the entire electromagnetic spectrum. The goal is to understand the physical processes behind the variable emission, which comes from a jet of plasma pointing close to our line of sight, powered by a supermassive black hole at the galaxy’s center.
WEBT began in autumn 1997, founded by John Mattox of Boston University as a collaboration among optical observers. In 2000, Massimo Villata of the Turin Observatory became the leader. A formal charter outlined aims and management, and soon radio and near-infrared observers joined. By February 2009, WEBT had organized 24 observing campaigns with more than 100 telescopes. Each campaign targets a specific blazar and is led by a Campaign Manager responsible for planning the observations, collecting and analyzing data, and helping publish the results.
Over the years, WEBT campaigns have covered many well-known blazars. In 2007, the project launched the GLAST-AGILE Support Program (GASP) to provide long-term, multi-wavelength monitoring that complements gamma-ray satellites. GASP monitors 28 bright blazars with periodic data collection and analysis. Examples include 3C 273, 3C 279, BL Lacertae, Markarian 421, OJ 287, PKS 2155-304, and 1ES 2344+514, among others.
Since its start, WEBT has contributed to more than 160 scientific publications, helping scientists better understand how blazars emit and vary over time.
This page was last edited on 3 February 2026, at 13:32 (CET).