seti on the ska - arecibo observatorynaic.edu/~ska/ska_talks/11tarter.pdf · 2000. 4. 7. ·...
TRANSCRIPT
SETI on the SKA
US SKA Consortium Meeting
Feb 28, 2000
Jill TarterBernard M. Oliver ChairSETI Institute
For SETI, We Don’t Know...
• Where To Look
• At WhatFrequency
• When To Look
• For What Signal
• From How Far
For SETI, We Don’t Know...
• Where To Look
• At WhatFrequency
• When To Look
• For What Signal
• From How Far
• Stars!
For SETI, We Don’t Know...
• Where To Look
• At WhatFrequency
• When To Look
• For What Signal
• From How Far
As Much Of TheSpectrum AsPossible
(Terrestrial µWave
Window, Optical, IR)
For SETI, We Don’t Know...
• Where To Look
• At WhatFrequency
• When To Look
• For What Signal
• From How Far
Multiple Looks
(Scintillation, and
Time Varying Signals)
For SETI, We Don’t Know...
• Where To Look
• At WhatFrequency
• When To Look
• For What Signal
• From How FarTechnology Nature
(Compressed In
Frequency Or Time)
For SETI, We Don’t Know...
• Where To Look
• At WhatFrequency
• When To Look
• For What Signal
• From How Far All The Sensitivity WeCan Get!!!
SETI On Telescopes Today
• Sky SurveysSERENDIP IV
( SETI@home )
[BETA]META IISo. SERENDIPProject Argus
• Targeted SearchesProject Phoenix10 micron IRHarvard OpticalBerkeley OpticalColumbus OSETI
SERENDIP IV At Arecibo• 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 σ• 2.5 MHz time series data
to SETI@home
Dan WerthimerDavid Anderson
Project Phoenix At Arecibo
• Microwave search from 1.2 to 3 GHz
Real Time Signal DetectionFrequency
Tim
e
Fully samplefrequency-time plane
Drifting CWdetectionalgorithmMN2 →
MN logN
N
M
Real Time Signal DetectionFrequency
Tim
e
ThresholdedSparseData Set
TripletPulse DetectionAlgorithm
Unique to Project Phoenix
2 Antennaslinked as apseudo-interferometer
6700 km
Unique to Project Phoenix• Original selection of
candidate signal is basedon power detection withspectral resolution of 1Hz
• Coherent integration onfollow up with spectralresolution that may be asfine as 0.01 Hz
• Differential Dopplersignature is key to RFIexcision
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
Coverage of the Cosmic Haystack
Phoenix is
most comprehensive
but looks
at only 1000 stars
How, Most Comprehensive??
• Hard to compare targeted searches with sky surveys• If you assume starsstars 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(Figure = # of Stars x BW x log(FFhihi//FFlolo) x (1+ log q) ) x (1+ log q) of Merit of Merit where q = number of looks
Merit vs EIRP (watts )
-1
1
3
5
7
9
6 8 10 12 14 16 18
log(EIRP)
log
(Me
rit)
P hoenix
1kT
S IV
1hT S S
SERENDIP IVsearches forintrinsicallystrong sourcesin sky visiblefrom Arecibo
Phoenixseaches for faint sources nearby and intrisically strong sourcesin the background
Coverage of the Cosmic Haystack
Results: NothingTo Date
We Needa Better
Telescope!The First Step
The One Hectare Telescope (1hT)
Notes Added After Meeting:
The next slide is VERY IMPORTANT!
It shows that no matter where on the sky YOU ARE LOOKINGthere 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 traditionalradio 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 bean infrequent conflict.)
1hT Speeds Up SETIMultiplexing
For a target list of1 million stars(from GAIA mission)there will be morethan 1 star in the fieldof view of a 5m (orsmaller) dish up to 10GHz and
Increased BW
0
10
20
30
40
50
60
70
80
90
100
0 2 4 6 8 10 12
Frequency in GHz
Ta
rge
t S
tars
pe
r B
ea
m (
5m d
ish
)
100000 stars
1000000 stars
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
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
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
Improved Search Space
Merit vs EIRP (watts )
6 8 10 12 14 16 18
log(EIRP)
log
(Me
rit)
P hoenix
1kT
S IV
1hT S S
Me rit vs EIRP(watts )
-1
1
3
5
7
9
6 8 10 12 14 16 18
log(EIRP)
log
(Me
rit)
BETAmax S IV
1hT S S 1hT TS
Log (EIRP)
Log
(M
erit
)
Phoenix S IV 1hT TS 1hT SS
In 20 year arraylifetime, the1hT can do both:
TS with 12 beams
SS with 100 beams
For SETI, We Don’t Know...
• Where To Look
• At WhatFrequency
• When To Look
• For What Signal
• From How Far All The Sensitivity WeCan Get!!!
• Stars! A MillionOr More
This Is a Job For
SKA
SETI Observations with SKA
• Factor of 100 in sensitivity over the 1hTobservations
• Factor of 100 decrease in transmitter EIRPfor current target star list
• Factor of 10 in distance or 1000 times asmany stars for current limit of 1012 W EIRP
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)
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
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
Bets on Moore’s Law
Merit vs EIRP(watts )
0
2
4
6
8
10
6 8 10 12 14 16
log(EIRP)
log
(Me
rit)
P hoenix
1 kT
1hT TS
Conclusions:A sensitivesearch of amillion nearbystars will takeabout 10 yearswith the SKA
It can be donein parallel withtraditional RA,assuming - 10 beams 9 GHz BW
SKA