A Search for Evidence of Advanced Extraterrestrial Life on Kepler Planets
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A Search for Evidence of Advanced Extraterrestrial Life on Kepler Planets. Matt Lebofsky Arielle Little Ron Maddalena Geoff Marcy Jill Tarter Dan Werthimer. Jeff Cobb Paul Demorest John Ford Andrew Howard Eric Korpela Glen Langston. Andrew Siemion, University of California, Berkeley.

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A Search for Evidence of Advanced Extraterrestrial Life on Kepler Planets

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A Search for Evidence of Advanced Extraterrestrial Life on Kepler Planets

Matt Lebofsky

Arielle Little

Ron Maddalena

Geoff Marcy

Jill Tarter

Dan Werthimer

Jeff Cobb

Paul Demorest

John Ford

Andrew Howard

Eric Korpela

Glen Langston

Andrew Siemion, University of California, Berkeley


Graphic: Wendy Stenzel / NASA


Narrowband Radio Signals


Broadband Radio Pulses

e

p

e

e

p

p

e

p

p

e

e

p

e

e

p

p

p

e


Observing Plan


Observing Plan

5 minute targeted observation of especially interesting KOIs:


Observing Plan

5 minute targeted observation of especially interesting KOIs:

‘Traditional’ HZ:

-50 C < Teq< 100 C


Observing Plan

5 minute targeted observation of especially interesting KOIs:

‘Traditional’ HZ:

-50 C < Teq< 100 C

Ncandidates > 4


Observing Plan

5 minute targeted observation of especially interesting KOIs:

‘Traditional’ HZ:

-50 C < Teq< 100 C

Ncandidates > 4

Small, long period

P > 50d && Rp < 3 RE


Observing Plan

11 hour raster scan of the entire Kepler field.

5 seconds

per 10’ beam


Radio SETI


H2O

O2

Galactic Synchrotron

Background

Ionospheric Reflection


18 cm

hyperfine OH

21 cm

hyperfine H

“Water Hole”


Kepler SETI Band

16 to 27 cm

1.1 to 1.9 GHz


Green Bank, West Virginia


Single Dish Radio Astronomy

Incoming Radiation

Processing

Analog / Digital Conversion

Prime Focus

Receiver /

Amplifier

Receiver


Green Bank Ultimate Pulsar Machine (GUPPI)


Green Bank Ultimate Pulsar Machine (GUPPI)

8 bit sampling ➡ 2 bit quantization

Raw ‘baseband’ recording

800 MHz bandwidth, 2 polarizations

~ 1 gigabyte/second to disk


Narrowband Signals

Fast Fourier Transform

Dynamic Spectrum

FREQUENCY

TIME


Narrowband Signals

POWER

FREQUENCY


Broadband Pulses

FREQUENCY (MHz)

Assuming a model of free electron density in the ISM, we can infer a distance of ~2000 pc.

TIME (mS)


Broadband Pulses

Dedispersion

FREQUENCY (MHz)

Thresholding


What could we detect?


What could we detect?

Broadband Pulses

Narrowband Signals


What could we detect?

Broadband Pulses

Narrowband Signals


What could we detect?

at 10σ:

Broadband Pulses

~1 ly

Narrowband Signals


What could we detect?

at 10σ:

Broadband Pulses

~1 ly

Narrowband Signals

~1650 ly


What could we detect?

at 10σ:

Broadband Pulses

~1 ly

Narrowband Signals

~1650 ly

SEFD = 10 Jy tintegration=150s tpulse=10s


Status


Status

Observations completed May 22, 2011

Total Data set ~50 TB


Status

Total Data set ~50 TB


SETI@Home

Status

Total Data set ~50 TB

AstroPulse


SETI@Home

Status

Questions?

Total Data set ~50 TB

AstroPulse


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