Future Radio Astronomy Instrumentation and Future SETI Dan

Future Radio Astronomy Instrumentation and Future SETI Dan Werthimer and 800 CASPER Collaborators and 8, 000 SETI@home Collaborators http: //casper. berkeley. edu http: //seti. Berkeley. edu

Why you should be nice to instrument designers: Nobel Prizes with Better Instrumentation: • Gravitational Wave Detection (pulsar timing) • Black Hole Physics (Event Horizon Telescope…) • How did the First Stars and Galaxies Form ? (EOR) • What is Dark Matter ? • What is Dark Energy ? • Discover ET

Design Observatories with Plan for Exponential Growth in Digital Processing • Digital Backend should be replaced every 5 years (keep software, toss old - buy new hardware) • DSP Part of Operating Costs, not construction costs

The Original Moore’s Law Plot • In 1965 Gordon Moore (cofounder of Intel) noted that the transistor density of semiconductor chips doubled roughly every 18 months. Extrapolation accurate for another 50 years!

1960 – First Radio Astronomy Digital Correlator 21 lags 300 k. Hz clock discrete transistors $19, 000 Sandy Weinreb

Correlator processing power 107 SKA EVLA 106 GFlops ALMA LOFAR SMA 105 109 . EVN/WSRT 104 103 106 VLA DXB 102 DLB DAS DCB 10 1 103 70 75 80 85 90 95 2000 05 10 2015 source: Arnold van Ardenne

Ray Escoffier “With correlator performance having gone up by a factor of 922, 000 over the last 30 years, its only fair that correlator design engineers' salaries should have gone up by a similar factor!!”

ng. VLA correlator 2015 cost $28 M commercial off the shelf 2015 boards (assumes 256 antenna, 50 GHz bandwidth) ADC’s boards 2000 x $3 K/26 Gsps $6 M F engine boards: 512 x XCKU 11 P $2 M X engine boards: 1200 x XCVU 13 $4 M Switches (50 128 port QSFP) $5 M 51, 200 DWDM transceivers (80 km) $5 M racks, power, UPS, cables, cooling $1 M labor $5 M

Radio Telescope Sensitivity doubles every 3. 6 years

Moores Law – Instruments using FPGA’s: 2 X per year (1, 000 over 20 years)

13

expect (plan for) • 100 GHz bandwidth • 1000 to 1 M antenna arrays • 1000 to 1 M beams (commensal experiments) • 6: 1 or 20: 1 ? Feeds and receivers • phased array feeds with low Tsys ? • Observatory removes RFI (part of instrument)

New Hardware

Phased Array Feed – 64 beams

Dual 26 Gsps ADC and FPGA board

ADC’s 26 Gsps 55 Gsps 80 Gsps 160 Gsps 240 Gsps 3. 5 bit Hittite 8 bit Fujitsu 8 bit Berkeley 8 bit Keysight 8 bit Teledyne Lecroy

The end of hard disks in 2020 solid state (flash) disk cost coming down fast

New Instrument Architectures • Scalable • Upgradeable • Flexible • General Purpose • Fault Tolerant

Simultaneous Digital Backends Piggyback, Commensal, Sky Surveys Pulsar Spectrometer Signal Splitte r Galactic Spectromet er Extra Galactic Spectromet er SETI Spectromet er Baseband Data Recorder Analog Power Splitters or Digital Data Splitter

CASPER General Purpose Architechture Dynamic Allocation of Resources, need not be FPGA based

VEGAS/DIBAS Multi-beam Spectrometer + Pulsar Timing/Searching John Ford, Dan Werthimer, David Mac. Mahon, Richard Prestage VG 25

GBT spectrometer, pulsar, seti…

SETI and FRB search at Arecibo/GBT SERENDIP VI and ALFABURST Lorimer, Werthimer, Siemion, Mac. Mahon, Dexter, Cobb, Chennamangalam, Armour, Karastergiou

CASPER FXB Correlator/Beamformer (correlator needed to calibrate beamformer)

Board Interconnect - Upgradable • Problem: Backplanes are short lived (S 100, Multibus, VME, ISA, EISA, PCIx, PCIe 2. 0, compact. PCIe, ATCA…) • Solution: Use 10, 40 or 100 Gbit/sec Ethernet since 1973 – likely to stay around !

Serendip VI & ALFABURST (Hemant Shukla, NSF) UCB, WVU, Oxford, Arecibo (and soon, GBT)

CASPER Collaboration for Radio Astronomy Signal Processing and Electronics Research Some of the CASPER Collaborators: Xilinx, Fujitsu, HP, Sun/Oracle, Nvidia, NSF, NASA, NRAO, NAIC, CFA (Havard/Smithsonian), Haystack (MIT), Caltech, Cornell, CSIRO/ATNF, JPL/DSN, South Africa KAT, Manchester/Jodrell Bank, GMRT (India), Oxford, Bologna, Metsahovi Observatory/Helsinki University, University of California, Berkeley; Swinburne University (Australia), Seti Institute, University of California, Santa Barbara; University of California, Los Angeles; CNRS (France), University of Maryland Nancay Observatory, University of Cape Town (South Africa), ASTRON (Netherlands), Academica Sinica (Taiwan), Cambridge, Brigham Young University, Rhodes University (South Africa)

32

Invitation to Eleventh Annual CASPER Workshop Capetown, South Africa January 25 -29, 2016 morning: talks afternoon: lab training, tutorials, working groups, get help designing an instrument….

SETI past and future

1924 navy search for martian radio

Berkeley SETI Group David Anderson, Hong Chen, Jeff Cobb, Steve Croft, Dave De. Boer, Matt Dexter, Walt Fitelson, Kara Gieseking, Jack Hickish, Eric Korpela, Matt Lebofsky, Geoff Marcy, Dave Mac. Mahon, Eric Petigura, Chris Schodt, Isaac Shivvers, Andrew Siemion, Nate Tellis, Ed Wishnow, Dan Werthimer Breakthrough Foundation, NSF , NASA, Templeton Foundation, Individual Donors Keysight, Intel, Seagate, Xilinx

SETI@Home

FAST Interplanetary eavesdropping (GBT Kepler) § Kepler has found numerous multiple planet systems § When planets are in conjunction with Earth the more distant planet is beaming its signals at us, giving us an opportunity to catch spillover. § Given the number of exoplanet systems, these conjunctions are frequent § 5 -10 minute obs (per band) § 1. 1 -1. 9 GHz § 1. 8 -3. 0 GHz § 7. 8 -11. 0 GHz § total of about 30 hours thus far

Breakthough Prize Foundation “LISTEN” SETI Project • $100 M over 10 years • Starting with Green Bank and Parkes Radio Telescopes • Lick Observatory (optical SETI) • 1, 000 stars; 1000 galaxies; galactic plane; all sky • New instrumentation: 10 GHz bandwidth (100 billion channels) • SETI@home participants will analyze interesting parts of data • Open source data, hardware, software, gpuware, gateware

The Breakthrough Listen Initiative: Telescopes Automated Planet Finder (Lick Observatory) • • Search for extremely narrow emission lines from artificial lasers Extremely high resolution “Levy Spectrometer” 374 - 950 nm, λ/Δλ= 105 Green Bank Telescope (Green Bank, WV) • • • Radio search focusing on targeted and raster observations Nearly continuous frequency coverage 300 MHz - 100 GHz Flexible IF system can deliver up to 10 GHz dual-pol analog bandwidth Parkes Telescope (New South Wales, Australia) • • • Radio search focusing on surveys Southern hemisphere location gives great access to galactic plane Multi-beam receiver allows very efficient L-band (1. 2 - 1. 5 GHz) sky surveys

The Breakthrough Listen Initiative: Technology Many-GHz processing capability Commodity Compute Elements 320 Gbps data recording 1010 channel spectroscopy FPGA Computing Boards GPU-accelerated multi-parameter search pipeline (dispersion, Doppler effects) Interference identification, classification High Speed Digitizers

LISTEN SETI Data Rates

Warning Why you might not want to do SETI at the NGVLA

Summary and Conclusion No ET so far Still working on it

SETI HAIKU

Searching for life Answers are revealed About ourselves Paula Cook, Duke University

One million earthlings Bounded by optimism Leave their PC’s on Dan Seidner