The ATA Galactic Center Survey: SETI Observations in 2009

Details The ATA Galactic Center Survey: SETI Observations in 2009 The ATA Galactic Center Survey: SETI Observations in 2009

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21540302b&link_type=abstract

American Astronomical Society, AAS Meeting #215, #403.02; Bulletin of the American Astronomical Society, Vol. 42, p.223

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Scientific paper

We report on SETI observations of a region near the Galactic Center during 2009 with the Allen Telescope Array. The survey covers galactic longitude 357° to 7° and latitude ± 1° with a grid of 3500 positions corresponding to a synthesized beam of 8’ by 3'. For each position, we searched the "Water Hole” portion of the microwave spectrum (1420 - 1720 MHz) with a resolution of 0.7 Hz for continuous and pulsed signals with frequency drift rates of up to ±1 Hz/sec and bandwidths less than 10 Hz. In order to preserve the coherence of narrow band signals, we avoid pointing within 60° of the Sun. In its current stage, the Allen Telescope Array (ATA-42) is an array of 42 six-meter dishes with three dual-polarization beamformers. The beams observe independent positions within the field of view at the same frequency allowing each to serve as an "off” position for the other beam. This is a new approach to RFI mitigation. While SETI observations proceed, two independently tunable correlators are used to image the field of view. These "commensal” observations are discussed in another poster in this session ("The ATA Galactic Center Survey: Slow Radio Transients” by P. Williams).
The first phase of the ATA was funded through generous grants from the Paul G. Allen Family Foundation. UC Berkeley, the SETI Institute, the National Science Foundation (Grant No. 0540599), Sun Microsystems, Xilinx, Nathan Myhrvold, Greg Papadopoulos, and other corporations and individual donors contributed additional funding.

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