SETI: Searches So-far

While interest in the question of extraterrestrial life is at least as old as historical civilizations, the modern SETI era can be defined as beginning in 1959. In that year, Cornell physicists Giuseppi Cocconi and Philip Morrison published an article in Nature in which they pointed out the potential for using microwave radio to communicate between the stars.

A young radio astronomer, Frank Drake, had independently reached the same conclusion, and in the spring of 1960 conducted the first microwave radio search for signals from other solar systems. For two months Drake aimed an 85-foot West Virginia antenna in the direction of two nearby Sun-like stars. His single-channel receiver was tuned to the "magic" frequency of the 21 cm (1,420 MHz) line of neutral hydrogen, a spot on the radio dial also favored by Cocconi and Morrison because of its astronomical significance. While he didn't detect any signal of extraterrestrial origin, Drake's Project Ozma spurred the interest of others in the astronomical community, most immediately the Russians.
In the 1960's, the Soviet Union dominated SETI, and it frequently adopted bold strategies. Rather than searching the vicinities of nearby stars, the Soviets used nearly-omnidirectional antennas to observe large chunks of sky, counting on the existence of at least a few very advanced civilizations capable of radiating enormous amounts of transmitter power.

At the beginning of the 1970's, NASA's Ames Research Center in Mountain View, California began to consider the technology required for an effective search. A team of outside experts, under the direction of Bernard Oliver, on leave from the Hewlett-Packard Corporation, produced a comprehensive study for NASA known as Project Cyclops. The Cyclops report provided an analysis of SETI science and technology issues that is the foundation upon which much subsequent work is based.

As the perception grew that SETI had a reasonable prospect for success, the Americans once again began to observe. During the 1970's, many radio astronomers conducted searches, using existing antennas and receivers. Some of the efforts, employing improved technology, have continued to the present time. Foremost among these are the Planetary Society's Project META, the University of California's SERENDIP project, and a long-standing observing program at Ohio State University.

By the late-1970's, SETI programs had been established at NASA's Ames Research Center and at the Jet Propulsion Laboratory (JPL) in Pasadena, California. These groups arrived at a dual-mode strategy for a large-scale SETI project. Ames would examine 1,000 Sun-like stars in a Targeted Search, capable of detecting weak or sporadic signals. JPL would systematically sweep all directions in a Sky Survey. In 1988, after a decade of study and preliminary design, NASA Headquarters formally adopted this strategy, and funded the program. Four years later, on the 500th anniversary of Columbus' arrival in the New World, the observations began. Within a year, Congress terminated funding.

With NASA no longer involved, both researchers and interested members of the public saw a diminished chance to answer, within their lifetimes, the profound question addressed by SETI. Consequently the SETI Institute raised private funds to continue the targeted search portion of NASA’s large-scale program as Project Phoenix.

Project Phoenix concentrated efforts on that component of the NASA SETI project known as the Targeted Search. Its strategy was to carefully examine the regions around 1,000 nearby Sun-like stars. The world's largest antennas were used, committing observing time for SETI.  Phoenix used the 64 meter Parkes telescope in Australia to scrutinize about 200 selected southern stars. 

The most sensitive observations, covering a few hundred stars in one third of the sky used the 305 meter telescope of the Arecibo Observatory.

Phoenix observed another few hundred stars in the northern skies with the 140 Foot Telescope of NRAO Green Bank, just a short distance from the site of Project Ozma.

Project Phoenix was orders of magnitude more comprehensive than any experiment yet performed. Frequently, the successful attainment of an elusive goal requires nothing less than a systematic and thorough effort. Over the span of a decade, the project examined about 800 stars within 200 light years, searching for signals in  about 1.5 billion channels for each star.  The search was sensitive to the equivalent of strong terrestrial radars, but found no evidence of extraterrestrial signals of that strength.

Other long-term SETI projects are underway. Among these is Project SERENDIP operated by the University of California, Berkeley at the Arecibo telescope. A second major project is conducted in Australia by an independent group, the SETI Australia Centre at the University of Western Sydney. The Australians have bought the SERENDIP technology to run their own 58 million-channel experiment on the Parkes radio telescope.  The popular screensaver/distributed computing software project known as SETI@home, run by UC Berkeley, has brought SETI to millions.

In the meantime the SETI Institute has been focusing on the future. In a joint project with UC Berkeley, it is building a SETI-dedicated array of telescopes that will equal a 100-meter radio telescope, the Allen Telescope Array.

It is the forerunner of other larger radio astronomy arrays planned for later in the decade. It is possible that as telescope and SETI technology advance it may be possible to detect intelligence not by directed message but by the same kind of 'noise' we accidentally broadcast to the cosmos via radio, television and radar signals. SETI truly is a long-term project and setiQuest is part of that long term strategy.

There are two ways of searching with the ATA – SETI searches done at the same time as radio astronomy surveys – we call this commensal.

And surveys of areas of the sky where there are many potential target stars, so close together that we do not separate them.


History of SETI searches

For a detailed History of SETI searches list see: