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Status of the UC-Berkeley SETI efforts

Korpela, E. J. and Anderson, D. P. and Bankay, R. and Cobb, J. and Howard, A. and Lebofsky, M. and Siemion, A. P. V. and von Korff, J. and Werthimer, D. (2011) Status of the UC-Berkeley SETI efforts. In: Instruments, Methods, and Missions for Astrobiology XIV. Proceedings of SPIE. No.8152. Society of Photo-Optical Instrumentation Engineers (SPIE) , Bellingham, WA, Art. No. 815212. ISBN 978-0-81948-762-9. https://resolver.caltech.edu/CaltechAUTHORS:20170627-080943843

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Abstract

We summarize radio and optical SETI programs based at the University of California, Berkeley. The SEVENDIP optical pulse search looks for ns time scale pulses at visible wavelengths. It utilizes an automated 30 inch telescope, three ultra fast photo multiplier tubes and a coincidence detector. The target list includes F, G, K and M stars, globular cluster and galaxies. The ongoing SERENDIP V.v sky survey searches for radio signals at the 300 meter Arecibo Observatory. The currently installed configuration supports 128 million channels over a 200 MHz bandwidth with ~1.6 Hz spectral resolution. Frequency stepping allows the spectrometer to cover the full 300MHz band of the Arecibo L-band receivers. The final configuration will allow data from all 14 receivers in the Arecibo L-band Focal Array to be monitored simultaneously with over 1.8 billion channels. SETI@home uses the desktop computers of volunteers to analyze over 160 TB of data at taken at Arecibo. Over 6 million volunteers have run SETI@home during its 10 year history. The SETI@home sky survey is 10 times more sensitive than SERENDIP V.v but it covers only a 2.5 MHz band, centered on 1420 MHz. SETI@home searches a much wider parameter space, including 14 octaves of signal bandwidth and 15 octaves of pulse period with Doppler drift corrections from -100 Hz/s to +100 Hz/s. SETI@home is being expanded to analyze data collected during observations of Kepler objects of interest in May 2011. The Astropulse project is the first SETI search for μs time scale pulses in the radio spectrum. Because short pulses are dispersed by the interstellar medium, and the amount of dispersion is unknown, Astropulse must search through 30,000 possible dispersions. Substantial computing power is required to conduct this search, so the project uses volunteers and their personal computers to carry out the computation (using distributed computing similar to SETI@home). Keywords: radio instrumentation, FPGA spectrometers, SETI, optical SETI, Search for Extraterrestrial Intelligence, volunteer computing, radio transients, optical transients.


Item Type:Book Section
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1117/12.894066DOIArticle
http://proceedings.spiedigitallibrary.org/proceeding.aspx?articleid=1342481PublisherArticle
https://arxiv.org/abs/1108.3134arXivDiscussion Paper
ORCID:
AuthorORCID
Howard, A.0000-0001-8638-0320
Additional Information:© 2011 Society of Photo-Optical Instrumentation Engineers. This work has been supported by the Planetary Society, the SETI Institute, the University of California, Sun Microsystems and donations from individuals around the planet. Key hardware was donated by Network Appliance, Xilinx, Fujifilm Computers, Toshiba, Quantum, Hewlett Packard, and Intel Corp. We receive excellent support from the staff of the Arecibo Observatory, a part of that National Astronomy and Ionosphere Center, which is operated by Cornell University under a cooperative agreement with the National Science Foundation. We would also like to thank the Allen Telescope Array, a facility of the SETI Institute. The National Radio Astronomy Observatory in Green Bank, WV is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This work has been supported in part by NSF Grants AST-0808175 and AST-0307956, and NASA Grant NNX09AN69.
Funders:
Funding AgencyGrant Number
Planetary SocietyUNSPECIFIED
SETI InstituteUNSPECIFIED
University of CaliforniaUNSPECIFIED
Sun MicrosystemsUNSPECIFIED
Network ApplianceUNSPECIFIED
XilinxUNSPECIFIED
Fujifilm ComputersUNSPECIFIED
ToshibaUNSPECIFIED
QuantumUNSPECIFIED
Hewlett-PackardUNSPECIFIED
Intel Corp.UNSPECIFIED
NSFAST-0808175
NSFAST-0307956
NASANNX09AN69
Subject Keywords:radio instrumentation, FPGA spectrometers, SETI, optical SETI, Search for Extraterrestrial Intelligence, volunteer computing, radio transients, optical transients
Series Name:Proceedings of SPIE
Issue or Number:8152
Record Number:CaltechAUTHORS:20170627-080943843
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20170627-080943843
Official Citation:E. J. Korpela ; D. P. Anderson ; R. Bankay ; J. Cobb ; A. Howard ; M. Lebofsky ; A. P. V. Siemion ; J. von Korff ; D. Werthimer; Status of the UC-Berkeley SETI efforts. Proc. SPIE 8152, Instruments, Methods, and Missions for Astrobiology XIV, 815212 (September 23, 2011); doi:10.1117/12.894066.
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:78591
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:27 Jun 2017 20:31
Last Modified:03 Oct 2019 18:10

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