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SETI on the SKA

SETI on the SKA. Dan Werthimer University of California, Berkeley. http://seti.berkeley.edu/. SETI history SETI today SETI future (SKA) Signal processing. NOT FUNDED. NOT FUNDED. NOT FUNDED. Porno in space: FUNDED!. First Radio SETI. Nikola Tesla (1899)

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SETI on the SKA

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  1. SETI on the SKA Dan Werthimer University of California, Berkeley http://seti.berkeley.edu/

  2. SETI history • SETI today • SETI future (SKA) • Signal processing

  3. NOTFUNDED

  4. NOTFUNDED

  5. NOTFUNDED

  6. Porno in space: FUNDED!

  7. First Radio SETI • Nikola Tesla (1899) • Announces “coherent signals from Mars” • Guglielmo Marconi (1920) • Strange signals from ET • Frank Drake (1960) • Project Ozma • one channel, 1420-1420.4 MHz

  8. Traditional SETI dogma: ultra narrow band sine waves barycentric, beacons, FGK stars 21 cm Future dogma: many bandwidths, frequencies, drifting signals, pulses, M stars, galaxies

  9. It’s naïve to think we know how best to search today, given our history of changing SETI fashion. • Multiple strategy is best (IR, Vis, Radio, pulse, continuous, targetted sky survey…) • Half of astronomy discoveries are serendipitous • Examine glitches in data • Data Mining Experiments

  10. OPTICAL SETI 1961 Charlie Townes Paper largely ingored until 1999 1971 Cyclops report calculates radio >> optical Today’s lasers can communicate across galaxy

  11. Optical SETI experiments • Lick Observatory (Lick, Seti Institute, Berkeley) • Harvard (targetted  sky survey) • Princeton • Berkeley

  12. 10-meter Keck Telescope Survey: 650 F8 – M5 V, IV Hipparcos V < 8.5 B-V > 0.55 (F8V) Sep > 2 arcsec Age > 2 Gyr

  13. Keck Optical SETI – Data Mining • Geoff Marcy, Amy Reines • 650 stars (planet data) • Echelle Spectrometer • Can detect 10KW narrow band signal (10 KW laser on 10 meter telescope)

  14. SETI GOAL: SkyCoverage * FreqCoverage * Sensitivity^-3/2 * Nsignaltypes solid angle vs number of nearby FGK stars? FreqCoverage vs Noctaves? Pulses vs sinewaves vs drifting vs broadband…? FreqCoverage, SkyCoverage, signal types: other telescopes sensitivity: SKA

  15. Radio SETI Targetted Search Strategy Project Phoenix - Seti Institute Sky Survey Strategy Serendip, SETI@home - UC Berkeley Southern Serendip - Australia Meta II - Argentina Seti Italia - Bologna

  16. SETI Programs at the University of California

  17. University of California, Berkeley SETI Program • Graduate Students Chen Chang, Karl Chen, Paul Demorest, Nia Imara, P. Monat, A. Parsons • Undergraduate Students Noaa Avital, Brian Boshes, Henry Chen, Charlie Conroy, Chris Day, Daniel Hsu, Wonsop Sim, Ryo Takahashi • Astronomers and Computer Scientists David Anderson, Bob Bankay, Jeff Cobb, Court Cannick, Eric Korpela, Matt Lebofsky, Jeff Mock, Dan Werthimer, Rom Walton • Administrative Staff - None

  18. SERENDIP IV Photos Courtesy NAIC Arecibo Observatory, a facility of the NSF • 168M channels • 100 MHz Band centered on 1420 MHz • Carriage House 1 line feed • Operating since 1997

  19. Why SETI@home? • Coherent Doppler drift correction • Narrower Channel Width->Higher Sensitivity • Variable bandwidth/time resolution • Search for multiple signal types • Gaussian beam fitting • Search for repeating pulses Problem: Requires TFLOP/s processing power. Solution: Distributed Computing

  20. The SETI@home Client

  21. SETI@home Statistics TOTAL RATE

  22. SETI@home in Canada • 255,426 participants (0.8% of population) • 112,000 years of computer time • 72 million work units

  23. Web site: 2 million hits/day 200,000 visitors/day(stats & games popular; science less popular)100,000 children, families(including congress members and their kids)> 7,000 schools

  24. Desired SKA Parameters • Wide bandwidth • 1 M beams • fat beams • short dwell times (~ 100 seconds)

  25. Gaussian Candidates

  26. BOINC • Berkeley Open Infrastructure for Network Computing • General-purpose distributed computing framework. • Open source. • Will make distributed computing accessible to those who need it. (Starting from scratch is hard!)

  27. BOINC Projects • SETI@home (Berkeley)) • Astropulse (Berkeley) • ClimateModeling@home (Oxford) • Einstein@home (Caltech) • Folding@home (Stanford) • ParticlePhysics@home (CERN) • Stardust@home (U. Wa, Berkeley)

  28. AstroPulse • Sky survey • Covers decs 0 to 30 • ~3 years of data recorded so far. • Good time resolution • Sensitive to 0.4 µs radio pulses at 21 cm • DM range • -1000 to +1000 pc/cm3 • Sensitivity • 10-18 W/m2 peak (Coherent de-dispersion)

  29. Piggyback ALFA Sky Survey • Improved sensitivity • Tsys, integration time • Uniform sky sampling • galactic plane concentration • Multibeam RFI rejection • Larger Bandwidth

  30. Search for Optical/Radio Signals from Dyson Sphere Candidates| Charlie Conroy Looked for IR excess from >500 stars All stars had age > 1 Gigayear 33 stars found with 12m excess Searched for anomalous radio detection using SETI@home and SERENDIP IV databases Searched for optical pulse emission using OSETI experiment Thus far, none of the 33 sources have shown anomalous optical or radio emission Color excess using 2MASS K band data and 12, 25, 60, & 100 micron IRAS data. An excess at K-[12] is clearly visible and disappears by K-[25]. Dotted lines are Gaussian fits to the distributions. The 33 IR excess candidates have K-[12] > 3 above the mean.

  31. ‘Prelude’ Precedes SonATAIn Fall 2004For Use On The ATA-32 3 beams with 30 MHz each – PCs with accelerator cards

  32. Future SETI Spectrometers

  33. Moore’s Law in FPGA world 100X More efficient than micro-processors! 3X improvement per year!

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