From setiquest wiki
(→Collection: add RF converter board image.)
(convert navigation table to template format)
|Line 44:||Line 44:|
Revision as of 20:29, 30 March 2011
Allen Telescope Array
The Allen Telescope Array (ATA) is a joint effort by the SETI Institute and the Radio Astronomy Laboratory (RAL) at the University of California, Berkeley to construct a Radio Interferometer that will be dedicated to astronomical and simultaneous search for extra-terrestrial intelligence observations.
It is being built at the existing Hat Creek Radio Observatory (HCRO) is run by the RAL at Berkeley (UCB). Hat Creek is located in the Cascades just north of Mt. Lassen at an elevation of 1280m (4200 ft) above sea level. Hat Creek is 290 miles northeast of San Francisco, California.
The ATA is being constructed in stages. The initial array has 42 six-meter antennas and the final configuration will have 350 of these relatively small antennas. The ATA-42 is complete and became operational on 11 October 2007. The total collecting area of the ATA-42 is 1100 square meters with an aperture efficiency of 63%. The ATA-42 has the equivalent collecting area of a larger sqrt(42 * (6m/2)^2)) = 19.4m single dish.
An innovative feed and cryogenic receiver system on each antenna provides continuous frequency coverage from 0.5 to 11 GHz. This entire bandwidth is brought from each antenna over fiber optic cables to the control building, and there as much of the bandwidth as possible is digitized, with current-epoch ADCs (104.8576 MHz, dual-polarization in 4 independent frequency channels today). The digitized signals received from individual antennas are combined in two ways; to form a radio map or image of the entire field of view of the array using a spectral-imaging correlator, and to form a synthesized, full-resolution beam for pointing at a specific target on the sky using a phased-up beamformer. There are four independent IF tunings available at the ATA. Today two correlators are attached to two of the frequency tunings, and three beamformers work from the other two tunings. Eventually multiple beamformers and correlators could populate all of the IF tunings, if the scientific case for such commensal observations is strong enough. The three beamformers used by SETI currently each produce 104.8576 MHz bandwidth dual-polarization beams.
The ATA is a shared resource between the RAL at Berkeley and the SETI Institute. Observation proposals are sent to the ATA steering committee. The committee approves or rejects proposals and allocates telescope time accordingly.
In general either one astronomical survey or one SETI survey (SonATA) will control the pointing of the array as the primary user, with other secondary users able to access different IF tunings, correlators, beamformers, or other backend processors for their observations. This is what is meant by commensal observing at the ATA; the direction on the sky must be shared, but the multiple back end instruments and the frequency agility of the array permit many different science programs to be conducted at one time utilizing that same piece of sky.
The antennas are grouped into 5 "nodes", 1,2,3,4,5. Each antenna in a node has a set of antennas that are assigned a letter. The naming convention is node:letter. There are 42 antennas. Here is a list of all the antennas:
Each antenna has 2 pols, x and y. The convention for referring to a particular antenna pol is node:letter:pol. Example: 1ax, 1ay, etc.
Occasionally antennas are referred to as "ant3a" or "ant2e".
The term "ant" or "ants" is commonly used to mean "antenna" or "antennas".
|← Backend Server||Index||Beamformer →|