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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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slide1

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

slide4

Broadband Radio Pulses

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p

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p

p

e

p

p

e

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p

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p

p

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e

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Observing Plan

5 minute targeted observation of especially interesting KOIs:

slide7

Observing Plan

5 minute targeted observation of especially interesting KOIs:

‘Traditional’ HZ:

-50 C < Teq< 100 C

slide8

Observing Plan

5 minute targeted observation of especially interesting KOIs:

‘Traditional’ HZ:

-50 C < Teq< 100 C

Ncandidates > 4

slide9

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

slide10

Observing Plan

11 hour raster scan of the entire Kepler field.

5 seconds

per 10’ beam

slide13

H2O

O2

Galactic Synchrotron

Background

Ionospheric Reflection

slide14

18 cm

hyperfine OH

21 cm

hyperfine H

“Water Hole”

slide15

Kepler SETI Band

16 to 27 cm

1.1 to 1.9 GHz

slide18

Single Dish Radio Astronomy

Incoming Radiation

Processing

Analog / Digital Conversion

Prime Focus

Receiver /

Amplifier

Receiver

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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

slide21

Narrowband Signals

Fast Fourier Transform

Dynamic Spectrum

FREQUENCY

TIME

slide22

Narrowband Signals

POWER

FREQUENCY

slide23

Broadband Pulses

FREQUENCY (MHz)

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

TIME (mS)

slide24

Broadband Pulses

Dedispersion

FREQUENCY (MHz)

Thresholding

slide26

What could we detect?

Broadband Pulses

Narrowband Signals

slide27

What could we detect?

Broadband Pulses

Narrowband Signals

slide28

What could we detect?

at 10σ:

Broadband Pulses

~1 ly

Narrowband Signals

slide29

What could we detect?

at 10σ:

Broadband Pulses

~1 ly

Narrowband Signals

~1650 ly

slide30

What could we detect?

at 10σ:

Broadband Pulses

~1 ly

Narrowband Signals

~1650 ly

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

slide32

Status

Observations completed May 22, 2011

Total Data set ~50 TB

slide33

Status

Total Data set ~50 TB

slide34

[email protected]

Status

Total Data set ~50 TB

AstroPulse

slide35

[email protected]

Status

Questions?

Total Data set ~50 TB

AstroPulse

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