1 / 33

SETI on the SKA

SETI on the SKA. US SKA Consortium Meeting Feb 28, 2000. Jill Tarter Bernard M. Oliver Chair SETI Institute. Where To Look At What Frequency When To Look For What Signal From How Far. For SETI, We Don’t Know. Where To Look At What Frequency When To Look For What Signal From How Far.

tam
Download Presentation

SETI on the SKA

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. SETI on the SKA US SKA Consortium Meeting Feb 28, 2000 Jill Tarter Bernard M. Oliver Chair SETI Institute

  2. Where To Look At What Frequency When To Look For What Signal From How Far For SETI, We Don’t Know...

  3. Where To Look At What Frequency When To Look For What Signal From How Far Stars! For SETI, We Don’t Know...

  4. Where To Look At What Frequency When To Look For What Signal From How Far As Much Of The Spectrum As Possible (Terrestrial Wave Window, Optical, IR) For SETI, We Don’t Know...

  5. Where To Look At What Frequency When To Look For What Signal From How Far Multiple Looks (Scintillation, and Time Varying Signals) For SETI, We Don’t Know...

  6. Where To Look At What Frequency When To Look For What Signal From How Far Technology Nature (Compressed In Frequency Or Time) For SETI, We Don’t Know...

  7. Where To Look At What Frequency When To Look For What Signal From How Far All The Sensitivity We Can Get!!! For SETI, We Don’t Know...

  8. SETI On Telescopes Today • Sky Surveys SERENDIP IV( SETI@home ) [BETA] META II So. SERENDIP Project Argus • Targeted Searches Project Phoenix 10 micron IR Harvard Optical Berkeley Optical Columbus OSETI

  9. UC Berkeley SSL Piggyback (commensal) Almost 4 years of data 1420 MHz +/- 50 MHz 0.6 Hz resolution 12 seconds per beam Simple threshold @ 15  2.5 MHz time series data to SETI@home SERENDIP IV At Arecibo David Anderson Dan Werthimer

  10. Project Phoenix At Arecibo • Microwave search from 1.2 to 3 GHz

  11. Frequency Time Real Time Signal Detection M Fully sample frequency- time plane Drifting CW detection algorithm MN2  MN logN N

  12. Frequency Time Real Time Signal Detection Thresholded Sparse Data Set Triplet Pulse Detection Algorithm

  13. 6700 km Unique to Project Phoenix 2 Antennas linked as a pseudo- interferometer

  14. Unique to Project Phoenix • Original selection of candidate signal is based on power detection with spectral resolution of 1Hz • Coherent integration onfollow up with spectral resolution that may be as fine as 0.01 Hz • Differential Doppler signature is key to RFI excision

  15. Current Status of Project Phoenix • Arecibo and Jodrell Bank • 12 am +/- 6 hr, 40 d/yr • 500 stars down, 500 to go • BW = 20 MHz  100 MHz(RCP and LCP) • Sensitivity limits 1012 W EIRP @ 155 lt yr 8x10-27 W/m2  1 Jy

  16. Phoenix ismost comprehensive but looks at only 1000 stars Coverage of the Cosmic Haystack

  17. How, Most Comprehensive?? • Hard to compare targeted searches with sky surveys • If you assume stars are what matters (not interstellar spacecraft between the stars) • Can use sensitivity of the various searches to calculate the number of stars that are “accessible” within any given beam on the sky for both TS & SS • Comparison can then be made for any ETI power • Figure = # of Stars x BW x log(Fhi/Flo) x (1+ log q) • of Meritwhere q = number of looks

  18. SERENDIP IV searches for intrinsically strong sources in sky visible from Arecibo Phoenix seaches for faint sources nearby and intrisically strong sources in the background

  19. Coverage of the Cosmic Haystack Results: NothingTo Date We Need a Better Telescope! The First Step

  20. The One Hectare Telescope (1hT)

  21. Notes Added After Meeting: The next slide is VERY IMPORTANT! It shows that no matter where on the sky YOU ARE LOOKING there will be multiple SETI target stars in the large field of view of a small dish. Therefore for the cost of the beam-forming and backend SETI processing systems, SETI can observe all the time without interfering with scheduled observations of traditional radio astronomy sources. (There would have to be some small accommodation so that the field of view is not changed while an interesting candidate signal is being pursued, but that will be an infrequent conflict.)

  22. 1hT Speeds Up SETI Multiplexing For a target list of 1 million stars (from GAIA mission) there will be more than 1 star in the field of view of a 5m (or smaller) dish up to 10 GHz and Increased BW

  23. TS SETI Observations with 1hT • 100 m equivalent • Number of beams = 3 • Bin width = 0.01 Hz • Integration time = 400 sec • Threshold = 9 sigma = 1.7 E-23 W • Processing bandwidth = .5 GHz • Frequency range = 1 to 3 GHz • Number of relooks = 3 • Total time for search = 6.3 years # of targets = 100,000 stars

  24. TS SETI Observations with 1hT • 100 m equivalent • Number of beams = 12 • Bin width = 0.01 Hz • Integration time = 400 sec • Threshold = 9 sigma = 1.7 E-23 W • Processing bandwidth = .5 GHz • Frequency range = 1 to 10 GHz • Number of relooks = 3 • Total time for search = 8 years # of targets = 100,000 stars

  25. SS SETI Observations with 1hT • 100 m equivalent • Number of beams = 100 • Bin width = 0.01 Hz • Integration time = 150 sec • Threshold = 25 sigma = 9.3 E-23 W • Processing bandwidth = 1GHz • Frequency range = 1 to 3 GHz • Number of relooks = 1 • Total time for search = 11 years +30 to +60 Declination

  26. Improved Search Space

  27. In 20 year array lifetime, the 1hT can do both: TS with 12 beams SS with 100 beams Phoenix S IV 1hT TS 1hT SS Log (Merit) Log (EIRP)

  28. Where To Look At What Frequency When To Look For What Signal From How Far All The Sensitivity We Can Get!!! This Is a Job For SKA For SETI, We Don’t Know... • Stars! A Million Or More

  29. SETI Observations with SKA • Factor of 100 in sensitivity over the 1hT observations • Factor of 100 decrease in transmitter EIRP for current target star list • Factor of 10 in distance or 1000 times as many stars for current limit of 1012 W EIRP

  30. SETI Issues • Targeted searches prefer large FOV • multiplexing advantage • Sky surveys prefer all sky imaging • tiles or Luneberg lenses • probably can’t afford high resolution processing • transients are attractive possibility (OSS for strong transients - 1020 ops)

  31. SETI Issues • Targeted searches prefer large FOV • Sky surveys prefer all sky imaging • 1-10 thousand km maximum baselines? OK • pencil beams all too small for background stars • Maximum instantaneous BW • Frequency range 0.5-10 GHz

  32. Bets on Moore’s Law SETI Observations with SKA • Bin width = 0.01 Hz • Integration time = 1000 sec • Threshold = 11 sigma = 1.2 E-23 W • Processing bandwidth = 9 GHz • Number of beams = 10 • Frequency range = 1 to 10 GHz • Number of relooks = 3 • Total time for search = 10 years • Total number of targets= 1,000,000

  33. Conclusions:A sensitive search of amillion nearby stars will takeabout 10 yearswith the SKA • It can be donein parallel withtraditional RA,assuming - 10 beams 9 GHz BW SKA

More Related