ASIC needs for “observational cosmology” · ASIC needs for “observational cosmology” Gary...
Transcript of ASIC needs for “observational cosmology” · ASIC needs for “observational cosmology” Gary...
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ASIC needs for “observational cosmology”
Gary S. Varner University of Hawai’i
HEPIC 2013 LBNL
May 30th, 2013
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What’s in & out • Very broad topic; minimize overlap with 2
following talks
• Focus on UHE ν, CR detection in Radio
• To better clarify needs: – State of the art – Current developments – Future (anticipated) needs
• WFS in TeV gamma (CTA) [DRS, SAM, TARGET]
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Neutrinos: The only known messengers at PeV energies and above
• Photons lost above 30 TeV: pair production on IR & µwave background
• Charged particles: scattered by B-fields or GZK process at all energies
• Sources extend to 109 TeV ! • => Study of the highest
energy processes and particles throughout the universe requires PeV-ZeV neutrino detectors
• To guarantee EeV neutrino detection, design for the GZK neutrino flux
Region not observable In photons or Charged particles
Courtesy: Peter Gorham [U. Hawaii]
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Why Radio?? (Ultra-)High Energy Physics of Cosmic rays & Neutrinos
• Neither origin nor acceleration mechanism known for cosmic rays above 1019 eV
• A paradox: – No nearby sources observed – distant sources excluded due to
process below
• Neutrinos at 1017-19 eV
required by standard-model physics
galactic
extragalactic
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Radio Observation in dense media
1960’s: Askaryan predicted that the resultant compact cascade shower (1962 JETP 14, 144; 1965 JETP 21, 658): • would develop a local, relativistic net negative charge excess • would be coherent (Prf ~ E2) for radio frequencies • for high energy interactions, well above thermal noise:
• detectable at a distance (via antennas) • polarized – can tell where on the Cherenkov cone
neutrino Cascade: ~10m length
air
solid
RF Cherenkov
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In the last decade or so… radio detection techniques finally flourishing
1. Radio Constraints on UHE neutrinos 2. ANtarctic Impulsive Transient Antenna (ANITA) 3. Serendipitous observation of UHE CR 4. Tera-ton Initiatives (ARA, ARIANNA, …)
Won’t cover low E CR, other radio, Atmospheric Molecular Bremsstrahlung
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Detector Energy Scales – the tonne
(total weight 7,000 tons, but sensitive elements much less)
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Detector Energy Scales – the kT
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Detector Energy Scales – the MT
Pushing bounds of civil
construction
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Detector Energy Scales – the GT
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Detector Energy Scales – the TeraTonne
IceCube ~200M$
Simply scaling up??
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Initial Round of Experiments • PRL 93:041101 (2004) limits published
Radio Ice Experiment (RICE) @ South Pole
Greenland Ice
• PRD 69:0133008 (2004) • Astropart.Phys.20:195 (2003)
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Design for cosmogenic ν flux discovery
• Huge Volume of solid, RF-transparent medium: Antarctic Ice Sheet
• Broadband antennas, low noise amplifiers and high-speed digitizers to observe them
• A high vantage point, but not too high nor too far away
• First realization: ANITA (balloon altitude)
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ANITA concept
Ice RF clarity: ~1.2km(!) attenuation length
Effective “telescope” aperture: • ~250 km3 sr @ 1018 eV • ~104 @ km3 sr 1019 eV (compare to ~1 km3 at lower E)
~4km deep ice!
Typical balloon field of regard
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Flight Payload Design
• Quad-ridged horn antennas provide superb impulse response & bandwidth (200-1200 MHz)
• Interferometry & beam gradiometry from multiple overlapped antenna measurements
A radio “feedhorn array” for the Antarctica Continent
~320ps Measured
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Major Hurdles • No commercial waveform recorder solution (power/resolution)
• 3σ thermal noise fluctuations occur at MHz rates (need ~2.3σ)
• Without being able to record or trigger efficiently, there is no experiment
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Strategy: Divide and Conquer
• Split signal: 1 path to trigger, 1 for digitizer • Digitizer runs ONLY when triggered to save power
Three key technologies:
1. Very low-noise (low power) amplifiers 2. Efficient, thermal-noise limited triggering 3. Low power, Gsa/s waveform sampling
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Switched Capacitor Array Sampling
Input
Channel 1
Channel 2 Few 100ps delay
• Write pointer is ~4-6 switches closed @ once
20fF
Tiny charge: 1mV ~ 100e-
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Example: LABRADOR performance (similar to other ASICs)
• Excellent linearity, noise • Sampling rates up to 4 GSa/s with voltage overdrive
2.6GSa/s
12-bit ADC
• 10 real bits (1.3V/1.3mV noise)
1.3mV
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A solar powered, airborne HEP experiment
Raw Signals
80 RF channels @ 1.5By * 2.6GSa/s
= 312 Gbytes/s
Level-1
Antenna
3-of-8
100-200kHz @ 36kBy/evt
= 3.6-7.2Gby/s
Level-2
Cluster
2-of-5
Few kHz @ 36kBy/evt = 36-72Mby/s
Level-3 Phi
2-of-2
5-10Hz @ 36kBy/evt
= 180-360kBy/s To disk
Prioritizer (+compress)
Few
eve
nts/
min
TD
RSS
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After full calibration – 100’s km downrange
<30ps timing
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A. Vieregg
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Warning!!! Log Plot!
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ANITA3 – the “last” round
• Rebuild “space flight” readout instrumentation (half a decade old technology) • Threshold limited – new trigger ASIC (RITC) • New digitizer (LAB4) to go to longer waveforms • “going for broke” – ARA is successor
For December 2014 Flight New SURF & TURF
RITC LAB4 25
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How to “go big” ?
• Salt – Salt domes
• Ice – In situ (RICE AURA IceRayARA/ARIANNA) – Overflight (satellite) [high threshold]
• Silica sand – Lunar regolith (GLUE) [high threshold]
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Askaryan Radio Array (ARA)
• Gusev and Zheleznykh proposed in 1983! • 100’s of km3 volume at GZK nu range • Inexpense extention to IceCube
Physics Goals
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ARA Readout Electronics (similar to ARIANNA)
• Uplink bandwidth (~1Mbit/s [wireless]) – First (test station) this season
– 1 detector station each of next 2 seasons after (building more) 28
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Askaryan Radio Array
• ANITA trigger/digitizer electronics to ARA • “array crossing” waveform sampler (IRS) • Built “testbed” in mid-2000’s …. • Finally deployed in January 2011, taking data • First “station” January 2012
Development Milestones IRS, IRS2, IRS3 ASIC
ARA Test Bed
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Neutrino Flavor/Current ID
• Charged/neutral current & flavor ID possible on subset of SalSA events • At least 20% of GZK CC events will get first order flavor ID • Detailed initial studies – looks very promising [BLAB ASIC – 64us deep
version of LABRADOR makes possible [NIM A591 (2008) 534]
Charged current (SM: 80%)
Neutral current (SM: 20%)
e 25% hadronic + 75% EM shower at primary vertex; LPM on EM shower
Single hadronic shower at vertex
µ 25% hadronic at primary, 2ndary lepton showers, mainly EM
Single hadronic shower at vertex
τ 25% hadronic at vertex, 2ndary lepton showers, mainly hadronic
Single hadronic shower at vertex
~2 km
1018 eV νµ
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Directions for future ASIC R&D • Low noise amplifiers
– Lower noise figure, lower power
• Better triggering – Only a couple bits needed – Real-time noise correlator
• Deeper waveform sampling – Already at ~100us analog storage – Higher frequency?
• Lower power! – Solar, wind, ??? – Autonomous, robust comm links – Design for manufacture**
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Why nattering on about power?!?
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G. V
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Det
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“Obs Cosmo” Summary
ASICs as the way Forward: • Further discoveries will depend upon evolutionary improvements in the basic instrumentation, of which ASICs play a crucial role
• Interesting problems with much overlap in other disciplines (low noise, high speed, low power)
• “Funding problems” are often mass manufacturing or operations cost issues – room for further ‘enabling technologies’
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Back-up slides
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A great idea that took a while to catch on
– 1962: G. Askaryan predicts coherent radio Cherenkov from particle showers in solid dielectrics – His applications? Ultra-high energy cosmic rays &
neutrinos
– Mid-60’s: Jelley & collaborators see radio impulses from high energy cosmic ray air showers – -- from geo-sychrotron emission, NOT radio
Cherenkov – Renewed interest: LOPES/Codelema
– 1970-2000: Askaryan’s hypothesis
remained unconfirmed – 2000-2001: Argonne & SLAC beamtests
confirm strong radio Cherenkov from showers in silica sand
– Salt (2004) & ice (2006) also tested, all confirmed
Saltzberg, et al PRL 2001
Gorham, et al PRD 2004
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Particle Physics: Energy Frontier
• GZK ν spectrum is an energy-frontier beam: – up to 300 TeV center of
momentum particle physics
– Search for large extra dimensions and micro-black-hole production at scales beyond reach of LHC
� ν Lorentz factors of γ=1018-21
Std. model
Large extra dimensions
Anchordoqui et al. Astro-ph/0307228
GZK ν
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Particle Physics: Neutrinos • GZK neutrinos are the
“longest baseline” neutrino experiment: – Longest L/E (proper time) for:
sterile ν admixtures & anomalous ν decays
• SUN: L/E ~ 30 m/eV • GZK: L/E ~ 109 m/eV
• Measured flavor ratios of νe:νµ:ντ can identify non-standard physics at source
νe:νµ:ντ
(1:1:1)! (5-6):1:1
Neutrino decay leaves a strong imprint on flavor ratios at Earth
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Differential GPS Antennas
Solar cells for NASA equipment
32 Quad-ridge horn antennas - 200 MHz to 1200 MHz - 10 degree downward angle
8 low gain antennas to monitor payload-generated noise
ANITA electronics box
Solar panels for science mission
Battery box
ANITA-1 pieces
“instrument paper” arXiv:0812.1920 [astro-ph]
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9 x 260 samples = 2340 storage cells
Convert all 2340 samples in parallel,
transfer out on common 12-bit data bus
256 + 4 “tail” samples
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G. Varner -- Challenges in Radio Detection, Detector R&D WS @ FNAL 40
Large Analog Bandwidth Recorder and Digitizer with Ordered Readout [LABRADOR]
8+1 chan. * 256+4 samples
Straight Shot
RF inputs
Random access:
• Common STOP acquisition
• 3.2 x 2.9 mm • Conversion in
31µs (all 2340 samples)
• Data transfer takes 80µs
• Ready for next event in <150µs
• Switched Capacitor Array (SCA)
• Massively parallel ADC array
• Similar to other WFS ASICs analog bandwidth
NIM A583:447-460, 2007
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Bandwidth Evaluation
Transient Impulse
FFT Difference
Frequency [GHz]
f3dB ~ 1GHz
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Sampling Unit for RF (SURF) board
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G. Varner -- Challenges in Radio Detection, Detector R&D WS @ FNAL 43
SURFv3 Board
Trigger Inputs
Programming/ Monitor Header
RF Inputs
LAB3
J4 to TURF J1 to CPU
(SURF = Sampling Unit for RF) (TURF = Trigger Unit for RF)
Flies in space – all components heat sunk
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Quiet, but are we sensitive?
Ground pulser
Dipole
Bore hole pulser
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Validation data: borehole pulser
• RF Impulses from borehole antenna at Williams field
• Detected at payload out to 300-400 km, consistent with expected sensitivity
• Allows trigger & pointing calibration
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S. Hoover
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Askaryan Radio Array (ARA)
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Cluster Station
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