1. SETI@Arecibo Jim Cordes and Dan Werthimer And Five Milliion SETI@home Volunteers in 226 countries http://http://seti.berkeley.edu http://

2. Warning Why you might not want to do SETI at Arecibo

8. SERENDIP IV 168M channels 100 MHz Band centered on 1420 MHz Photos Courtesy NAIC Arecibo Observatory, a facility of the NSF

9. Why you might want to do SETI at Arecibo

11. Piggyback ALFA Sky Survey Improved sensitivityImproved sensitivity –Tsys Uniform sky samplingUniform sky sampling –galactic plane concentration Multibeam RFI rejectionMultibeam RFI rejection Larger Bandwidth (SERENDIP V coming soon)Larger Bandwidth (SERENDIP V coming soon) Piggyback on Palfa, Galfa, EgalfaPiggyback on Palfa, Galfa, Egalfa Automatic recording during ALFA useAutomatic recording during ALFA use (no more operator manual switch for observations) (no more operator manual switch for observations)

13. SETI Figure of Merit Drake, Gulkis FOM = Sky Coverage * Frequency Coverage * Sensitivity -1.5

14. Arecibo SETI Figure of Merit Arecibo SETI Figure of Merit SearchDateTelescope MHzSky Cover W /m^2FOM Phoenix2000Arecibo 18001E-53 E-26 2.5 SETI@home1999-Arecibo 100.251.4 E-26 300 SERENDIP V2008Arecibo 3000.25 10 E-26 300 SETI@h II2009 ?Arecibo 3000.251.4 E-2610,000 Prelude2008ATA 4210000.001200 E-26 0.5 Sonata2010ATA 350 ???100000.001 40 E-26 50 Square Km2020SKA100000.001 1 E-2515,000

15. SETI on Single Dish vs Arrays? Arrays OK for targetted searches, but horrible for sky surveys due to tiny synthesized beam: SKA would require millions of beamformers and millions of spectrometers to cover the area in one single Arecibo beam SETI on Single Dish vs Arrays? Arrays OK for targetted searches, but horrible for sky surveys due to tiny synthesized beam: SKA would require millions of beamformers and millions of spectrometers to cover the area in one single Arecibo beam

16. s Radio - Targeted Search Strategy Project Phoenix - Seti Institute – Arecibo Project Phoenix - Seti Institute – Arecibo Prelude, Sonata – Seti Institute – Allen Telescope Array Prelude, Sonata – Seti Institute – Allen Telescope Array Radio - Sky Survey Strategy Serendip, SETI@home - Arecibo Serendip, SETI@home - Arecibo Meta II - Argentina Meta II - Argentina Seti Italia - Bologna Seti Italia - Bologna Optical - Targeted UC Berkeley - Pulse and Continuous UC Berkeley - Pulse and Continuous Lick Observatory – Pulse Lick Observatory – Pulse Harvard – Pulse Sky survey Harvard – Pulse Sky survey

17. UC Berkeley SETI Programs Name Time Scale Search Type SERENDIPseconds radio sky survey SETI@home mS - seconds radio sky survey Astropulse nS - mS radio sky survey SEVENDIPnS visible targetted SPOCK 1000 seconds visible targetted DYSON IR targetted

18. SETI Group (Berkeley and Cornell) SETI Group (Berkeley and Cornell) David Anderson, Bob Bankay, Daniel Chapman, David Anderson, Bob Bankay, Daniel Chapman, Henry Chen, Jeff Cobb, Jim Cordes, Jonah Hare, Andrew Howard Henry Chen, Jeff Cobb, Jim Cordes, Jonah Hare, Andrew Howard Josh Von Korff, Eric Korpela, Matt Lebofsky, Andrew Siemion, Laura Spitler, Dan Werthimer NSF, NASA, Individual Donors Agilent, Fujitsu, HP, Intel, Sun, Xilinx

19. The SETI@home Client

20. SETI@home Statistics TOTAL RATE

27. 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

28. Desired SKA Parameters Wide bandwidthWide bandwidth 1 M beams1 M beams fat beamsfat beams short dwell times (~ 100 seconds)short dwell times (~ 100 seconds)

29. Triplets Three evenly spaced spikes above 7.75X the mean power. (5.3X10 -25 W/m 2 )Three evenly spaced spikes above 7.75X the mean power. (5.3X10 -25 W/m 2 )

30. Pulses Modified Fast folding algorithm w/ dynamic thresholdModified Fast folding algorithm w/ dynamic threshold Logarithmically spaced periods from 3ms to 35sLogarithmically spaced periods from 3ms to 35s Sensitivity as low as 10 - 26 J/m 2Sensitivity as low as 10 - 26 J/m 2

31. Gaussians Weighted  2 fit to beam profile (vs time).Weighted  2 fit to beam profile (vs time). Gaussian must exceed a power and  2 thresholdGaussian must exceed a power and  2 threshold Score inversely proportional to probability of arising due to noiseScore inversely proportional to probability of arising due to noise Sensitivity 8.4x10 -25 W/m 2Sensitivity 8.4x10 -25 W/m 2

34. Gaussian Candidates

35. Arecibo SETI@home led to Public Participation Supercomputing David Anderson, Rom Walton, SETI Group David Anderson, Rom Walton, SETI Group aka Distributed Computingaka Distributed Computing aka “edge resource aggregation”)aka “edge resource aggregation”)

36. BOINC: NSF Berkeley Open Infrastructure for Network ComputingBerkeley 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!)

37. Projects AstronomyAstronomy –SETI@home (Berkeley) –Astropulse (Berkeley) –Einstein@home: gravitational pulsar search (Caltech,…) –PlanetQuest (SETI Institute) –Stardust@home (Berkeley, Univ. Washinton,…) Earth scienceEarth science –Climateprediction.net (Oxford) Biology/MedicineBiology/Medicine –Folding@home, Predictor@home (Stanford, Scripts) –FightAIDSathome: virtual drug discovery PhysicsPhysics –LHC@home (Cern) OtherOther –Web indexing/search –Internet Resource mapping (UC Berkeley)

41. Where's the computing power? ● 2010: 1 billion Internet-connected PCs ● 55% privately owned ● If 100M participate: – 100 PetaFLOPs, 1 Exabyte (10^18) storage your computers academic business home PCs

42. AstroPulse (Josh Vonkorff, Eric Korpela) Sky survey – –SETI@home I and piggyback ALFA data Good time resolution – –Sensitive to 0.4 µs radio pulses at 21 cm DM range – –-830 to +830 pc/cm 3 (but not -50 to +50) Sensitivity – –10 -18 W/m 2 peak (Coherent de-dispersion)

45. Future SETI at Arecibo Open Data to the community (SETI consortium?)Open Data to the community (SETI consortium?) (both raw 200TB and signals data base) (both raw 200TB and signals data base) Astropulse (uS dispersed pulses)Astropulse (uS dispersed pulses) SERENDIP V Spectrometer (14*256M channels)SERENDIP V Spectrometer (14*256M channels) SETI@home II (300 MHz – ALFA) SETI@home II (300 MHz – ALFA) New Multibeam Receiver ArraysNew Multibeam Receiver Arrays New wavelengths, More Bandwidth New wavelengths, More Bandwidth

46. Data storage: NERSC HPSS (Naional Energy Research Scientific Computing Center)‏

49. Arecibo SETI “Spin Offs” Public Participation Distributed ComputingPublic Participation Distributed Computing (Edge resource aggregation) (Edge resource aggregation) SetHI Hydrogen MapSetHI Hydrogen Map Transient Sky Survey for uS pulses (Astropulse)Transient Sky Survey for uS pulses (Astropulse) Instrumentation at 20 ObservatoriesInstrumentation at 20 Observatories (open source hardware and software for spectometers, correlators, beamformers, pulsars) (open source hardware and software for spectometers, correlators, beamformers, pulsars) Education, Public OutreachEducation, Public Outreach Commensal Observing ConceptCommensal Observing Concept

51. Moores Law – Instruments using FPGA’s: 2X per year (1,000,000 over 20 years)

52. Future Spectrometers

53. SETI HAIKU

54. Searching for life Answers are revealed About ourselves Paula Cook, Duke University

55. One million earthlings Bounded by optimism Leave their PC’s on Dan Seidner