Project OZMA, 1959 85ft Tatel Telescope Frank Drake Project OZMA, - - PowerPoint PPT Presentation

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Project OZMA, 1959 85ft Tatel Telescope Frank Drake Project OZMA, - - PowerPoint PPT Presentation

Nov 05, 2022 118 likes •501 views

T HE M ODERN R ADIO S EARCH FOR E XTRA T ERRESTRIAL I NTELLIGENCE Glen Langston - National Radio Astronomy Observatory Hong Chen - University of California, Berkeley Sebastien Lepine - Georgia State University Jayanth Chennamangalam - West

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Hong Chen - University of California, Berkeley Jayanth Chennamangalam - West Virginia University Jeff Cobb - University of California, Berkeley Jim Cordes - Cornell University Paul Demorest - National Radio Astronomy Observatory Heino Falcke - Radboud University, Nijmegen John Ford - National Radio Astronomy Observatory Mike Garrett - ASTRON Abhimat Gautam - University of California, Berkeley Jason Hessels - ASTRON Andrew Howard - University of Hawaii Glenn Jones - Columbia University Eric Korpela - University of California, Berkeley Glen Langston - National Radio Astronomy Observatory Sebastien Lepine - Georgia State University Ron Maddalena - National Radio Astronomy Observatory Alessio Magro - University of Malta Geoff Marcy - University of California, Berkeley Erik Petigura - University of California, Berkeley Andrew Siemion - UC Berkeley / ASTRON / Radboud Laura Spitler - MPIfR Jill Tarter - SETI Institute Joeri van Leeuwen - ASTRON Mark Wagner - University of California, Berkeley Dan Werthimer - University of California, Berkeley Kristian Zarb-Adami - University of Oxford

THE MODERN RADIO SEARCH FOR EXTRATERRESTRIAL INTELLIGENCE

http://seti.berkeley.edu http://casper.berkeley.edu

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85ft Tatel Telescope

Frank Drake

Project OZMA, 1959

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85ft Tatel Telescope

Frank Drake Single 100 Hz manually tuned channel 400 kHz band around 1420.4 MHz

Project OZMA, 1959

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Frank Drake

N = R* ⋅ fp ⋅ ne ⋅ fl ⋅ fi ⋅ fc ⋅ L

R* = the average rate of star formation per year in our galaxy fp = the fraction of those stars that have planets ne = the average number of planets that can potentially support life per star

that has planets

fl = the fraction of the above that actually go on to develop life

at some point

fi = the fraction of the above that actually go on to develop intelligent life fc = the fraction of civilizations that develop a technology that releases

detectable signs of their existence into space

L = the length of time such civilizations release detectable signals into space

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Graphics Courtesy NRAO, Bill Saxton AUI

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PLANETS ARE EVERYWHERE

Petigura et al, 2013

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Noise Temperature (Kelvin) Frequency (GHz) 1 10 100 1000 0.1 10 1 100 1000

Galactic Synchrotron Background

H2O O2

Atmospheric Rotational Transitions

Terrestrial Microwave Window H2O O2

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Intentional Signals...

Low energy - Radio photons are cheap Easy to generate, easy to receive - Earth technology makes photons look attractive As fast as possible - c Easily distinguished from natural sources - narrowest astrophysical sources 100s of Hz wide (masers) Robust to the interstellar medium - Narrow band signals encounter limited broadening by the ISM, viz. Drake and Helou 1977, Cordes and Lazio, 1991 ~ 0.1 Hz at 1.4 GHz

✴ ✴ ✴ ✴ ✴

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NAIC Arecibo Observatory, Puerto Rico

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2006 2008 2010 2012 2000 4000 6000 8000 10000 6 hours per day 3 hours per day Year Total Time Observed (Hours)

Total G-ALFA Observing (40 sec/beam)

Adapted from a graphic courtesy J.E.G. Peek

Arecibo L-band Feed Array (ALFA) Receiver System: ~1.3 GHz band center 7 dual-polarization feeds 300 MHz Bandwidth

  • ALFA Receiver (courtesy NAIC)
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X Pol Y Pol

Arecibo ALFA Receiver ALFA Splitter / Beam Selector iBOB

Beam Selector Signal

⊗ DDC 212 polyphase filterbank

matrix transpose

217 complex FFT

threshold

  • utput

∑

∝

∫ ∫

BEE2

SERENDIP V.v

XAUI Digital Link 100 Mbit Ethernet Control 10 Gbit Ethernet Spectral Data 100 Mbit Ethernet Control

iADC

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Operational since Sept 2009 Approximately 6000 hours

  • bserved

SERENDIP V.v

X polarization Y polarization

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Search for Extraterrestrial Radio Emissions from Nearby Developed Intelligent Populations Sky Coverage 2009-2012

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SETI@Home

Polyphase Channelization Coherent Doppler Drift Search Narrowband Pulse Search Gaussian Drift Search Autocorrelation <insert your algorithm here>

✴ ✴ ✴ ✴ ✴ ✴

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AstroPulse

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AstroPulse

Coherent Dedispersion Broadband Pulse Searching

✴ ✴

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KEPLER PLANET CANDIDATE SURVEY

The Robert C. Byrd Green Bank Telescope

NASA/Kepler

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Ncandidates > 4 ‘Traditional’ HZ:

  • 50 C < Teq

< 100 C

Small, long period P > 50d && Rp < 3 RE 5 minute targeted

  • bservation of potentially

‘hospitable’ KOIs

Kepler Field Observations

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11 hour raster scan of the entire Kepler field. 5 seconds per 10’ beam

Kepler Field Observations

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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

26

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SETI@Home Astropulse

Kepler Search Analysis

Locally Performed

Synthesized coarse filterbank Incoherent dispersed pulse search Synthesized high resolution spectrometer Incoherent Doppler drift search

Siemion et al, 2013 ApJ 767 94

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Time (Seconds) KOI 1199 400 300 200 100 100 200 300 400 50 100 Frequency (Fcntr +/ Hz) 400 300 200 100 100 200 300 400

MJD: 55696.1692 RA: 19:34:58.488 DEC: +38:56:21.48 Fctr: 1424.9660701 MHz Drift: 0.2788 Hz/sec SNR: 25.2578

Time (Seconds) KOI 1372 400 300 200 100 100 200 300 400 50 100 150 Frequency (Fcntr +/ Hz) 400 300 200 100 100 200 300 400

MJD: 55696.2171 RA: 19:45:35.856 DEC: +42:23:13.92 Fctr: 1424.7873276 MHz Drift: 0.50555 Hz/sec SNR: 36.5513

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1100 1200 1300 1400 1500 1600 1700 1800 1900 10 10

2

10

4

10

6

10

8

Number of Detections Frequency (MHz) Kepler Field Targeted Observations 02/2011 04/2011 Aircraft Radar 12001330 MHz Filter All Detections Peak Detections Final Candidates

Siemion et al, 2013 ApJ 767 94

Fewer than 10-4 FGK stars are radio loud in orbital plane radio emission at the ~5 LAO level Number of Kardashev Type II civilizations less than ~ 10-6 M⨀

  • 1
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SETI WITH LOFAR

Analysis pipeline leveraging existing pulsar capabilities (DSPSR) Complex baseband recording of ~8-10 phased beams over ~32 MHz bandwidth Pilot survey of 150 nearby M- dwarfs accepted for Cycle 0

  • bservations
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NEW OBSERVING STRATEGIES

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NEW OBSERVING STRATEGIES EPIC-SETI: EXOPLANET INTERPLANETARY COMMUNICATION SEARCHES FOR EXTRATERRESTRIAL INTELLIGENCE

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NEW OBSERVING STRATEGIES EPIC-SETI: EXOPLANET INTERPLANETARY COMMUNICATION SEARCHES FOR EXTRATERRESTRIAL INTELLIGENCE

Kepler multi-planet ephemerides allow accurate prediction of conjunction times 100s of multi-planet systems provide frequent conjunction events (many per day)

  • D. Fabrycky 2012

24 total hours of

  • bservations w/ GBT

Aug-Sep 2013, L, S, X bands

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DETECTABILITY OF THE MOST ENERGETIC TERRESTRIAL PHENOMENA

Frequency (GHz) Detectable Range (Ly)

10

2

10

1

10 10

1

10

2

10

2

10

3

10

4

10

5

LOFARcore HBA Arecibo GBT SKA1low SKA1mid

L ~ 10 x AO Planetary Radar D ~ 300m

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DETECTABILITY OF THE MOST ENERGETIC TERRESTRIAL PHENOMENA

Frequency (GHz) Detectable Range (Ly)

10

2

10

1

10 10

1

10

2

10

2

10

3

10

4

10

5

LOFARcore HBA Arecibo GBT SKA1low SKA1mid

L ~ 10 x AO Planetary Radar D ~ 300m

Based on Kepler ~5-50% of stars host an ~Earth like planet. e.g. Dressing et al 2013, Kopparapu 2013, Petigura et al 2013

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DETECTABILITY OF THE MOST ENERGETIC TERRESTRIAL PHENOMENA

Frequency (GHz) Detectable Range (Ly)

10

2

10

1

10 10

1

10

2

10

2

10

3

10

4

10

5

LOFARcore HBA Arecibo GBT SKA1low SKA1mid

L ~ 10 x AO Planetary Radar D ~ 300m

  • 1. at least 10-100 billion ~Earth like

worlds in the Galaxy.

  • 2. With the SKA, we will for the first time

have confidence that we are sensitive to ~Earth-level ~isotropic leakage radiation from an Earth-like planet.*

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LOOKING FORWARD TO SETI ON THE SKA SKA-low and SKA-mid are equally interesting from a SETI perspective, and each could be the preeminent facility for targeted SETI in their respective bands. For the foreseeable future, large single dish telescopes will be best for sky surveys. As of now, there is no provision for a SETI

  • bserving capability with SKA-low, -mid or
  • survey.