Exploring the Ultrahigh-Energy Universe with the ANITA Long ...

Exploring the Ultrahigh-Energy Universewith the ANITA Long-Duration-Balloon Experiment

Cosmin Deaconu

University of Chicago /Enrico Fermi Institute/ Kavli Institute for Cosmological Physics

Northwestern/COFI WebinarJune 24, 2020

Outline

Introduction: Ultrahigh energy (UHE) neutrinos and how to detect them

The ANITA Experiment

Results from ANITA

The future of ANITA (PUEO!)

Cosmin Deaconu (UChicago/EFI/KICP) Exploring the UHE Universe with ANITA Northwestern/COFI 2 / 50

What do I mean by Ultrahigh-Energy (UHE)?

Neutrinos cover a wide energyrange (From µeV to EeV)

I’ll be talking about looking forneutrinos at energies ofO(1EeV) and higher.

1 EeV = 1018 eV = 109 GeV =106 TeV = 1000 PeV

For reference, Most energeticcosmic ray ever detected is 300EeV.

1 ZeV

1 PeV

1 TeV

1 GeV

1 EeV

1 MeV

1 keV

1 eV

highest-energy CR

Fastball

Mosquito

highest-energy IC ν

Cosmogenic νs

Astrophysical νs

Atmospheric νs

SN νs

Accelerator νs

Solarνs

Reactor νs

geoνs

Cosmological νs


Cosmogenic and Astrophysical νs

????

???

???

????

?UHE Cosmic Ray

NASA/H

ST ESA/Planck

JPL

CosmicAccelerators

Cosmic Accelerators


Cosmogenic νs

p,Nπ ν

NASA/WMAP

For protons, typically 5% of initial energy goes to ν in GZK process (threshold ∼ 50 EeV).

p + γCMB → ∆+ → π → νs (1)

Heavier nuclei also produce ν’s via photodisintegration, but with lower energy yield.

We know both UHECR and the CMB exist, so these neutrinos are “guaranteed” at somelevel, although they have not yet been detected.


Cosmogenic ν flux

Ballpark cosmogenic interaction estimate is < 1 / km3 of stuff / century, but large uncertainty.

1 Unconstrained UHECR composition at highest energiesI TA and Auger measure Xmax , which has a distribution related to

the UHECR composition (albeit with large systematics and messyhadronic physics).

I Auger prefers a heavier CR composition at the highest energies,implying lower UHE ν flux. TA composition more favorable.

2 Unknown source evolutionI Since we haven’t identified the UHECR sources, don’t know how

they evolve with redshift.I Because of GZK, TA and Auger can only probe the local universe.I Some sources classes are much more abundant outside GZK

horizon (z ≈ 0.03).

3 Unknown maximum UHECR energyI UHECR get downcoverted by CMB, so cannot constrain Emax


Astrophysical ν?

NASA

νπ

p

These are the neutrinos produced directly in astrophysical sources (p + γ, p + p, etc.),rather than during propagation.

Have been measured up ∼ 10 PeV by IceCube (sources unclear).Note that sources of astrophysical ν not necessarily good sources of UHECR (because theparticles can’t be accelerated to the highest energy if they produce neutrinos within thesource).

I Typically, need both an acceleration zone and an interaction zone.I Usually will also get γ-rays.

Some sources (e.g. GRB’s, FSRQ) may produce neutrinos at EeV energies.


Some flux predictionsNote that y-axis is scaled by E 2!

101 103 105 107 109 1011

Particle energy [GeV]

10 10

10 9

10 8

10 7

10 6

E2 (a

ll-fla

vor)[

GeV

cm2 s

1 sr

1 ] high-energy neutrinos (IceCube)

cosmic rays (Auger)

-ray background(Fermi)

Neutrino flux predictionsFang & Murase, ClustersFang et a.s, PulsarsBoncioli et al., LL GRBsMurase, GRB afterglowRodrigues et al., BlazarsMurase et al., AGNHeinze et al., Auger best fitvan Vliet et al., Auger UHECRvan Vliet et al., TA UHECR

Neutrino flux predictionsFang & Murase, ClustersFang et a.s, PulsarsBoncioli et al., LL GRBsMurase, GRB afterglowRodrigues et al., BlazarsMurase et al., AGNHeinze et al., Auger best fitvan Vliet et al., Auger UHECRvan Vliet et al., TA UHECR

A. Nelles.


More speculative sources?

“Top-down models” (don’t accelerate particles, produce them directly):I Ultra-heavy dark matterI Topological defectsI Many of these have already been constrained by UHE neutrino data.

High-redshift-only sourcesI Accelerators outside of GZK horizon (z ≈ 0.03) largely unconstrained by UHECR or γ data

(since both downconvert into more abundant lower-energy particles).I Not so crazy to imagine some sources just don’t exist within our GZK horizon, for example,

there are no known FSRQs within GZK horizon.I Anything can happen out there and we might only find out through neutrinos.

???I If found, UHE neutrinos may not be consistent with any of the predictions and suggest

something entirely.


So what? Why bother trying to detect them?

p,N

ν

NASA/WMAPγ

Because they’re (maybe) there!

To better understand cosmic accelerators:I Neutrinos are the ideal messengers since they don’t interact or get deflected on the way here.I Even though cosmogenics are produced away from the sources, on cosmologlical distances,

that’s unresolveable, so if there are few enough sources, could find them.I Astrophysical ν may appear coincident with transients from other messengers (γs, GW).I Even non-detection can provide insight on how cosmic accelerators work (and things like

mass composition)


So what? (for particle physicists): Most energetic neutrinos available!

Verify Standard Model ν −N cross-section at anew energy scale by using Earth as a filter.

Phys. Rev. D 83, 113009

BSM models could enhance or suppresscross-sections at high energies

Can also probe Lorentz invariance, sterileneutrinos, etc.


https://journals.aps.org/prd/abstract/10.1103/PhysRevD.83.113009

Problem: how do you build a detector large enough?

Due to low predicted interaction rate, needto instrument some existing dense volume.

Optical Cerenkov detectors like IceCube orKm3NeT limited in size by opticaltransparency of detection medium

I glacial ice and water have attenuationlengths . 100 m

Scaling IceCube up by large factors iscost-prohibitive


Solution: Radio-detection via Askaryan Effect

High-energy cascade in dielectric medium develops O(20%) negative charge excess.

From far away, at wavelengths longer than shower width (O(10cm), appears as singlemoving charge going faster than light velocity in medium.

Potential media: glacial ice, sand, salt, lunar regolith (yes, people have pointed radiotelescopes at the moon to look for this!)


Askaryan Effect in IceDemonstrated in SLAC beam test!

Attenuation length ∼ 1 kmCosmin Deaconu (UChicago/EFI/KICP) Exploring the UHE Universe with ANITA Northwestern/COFI 14 / 50

Some ice-based Askaryan ν experiments

ANITA/PUEO*

Antennas on ahigh-altitude balloon

over Antarctica

ARA*

Antennas buried inice near the South

Pole

ARIANNA

Near surfaceantennas on Ross Ice

Shelf

RNO-G*

New project inGreenland!

*denotes an experiment I work on.


Another method (also with radio): Detect upward-going showers from ντ

Extensive air showers (EAS) also produce radio signal (mostly from charge-separation byEarth’s magnetic field, although also an Askaryan component)

Technique widely used to measure air showers from cosmic rays (e.g. AERA, LOFAR).

But, a ντ interacting in the Earth can produce a τ that escapes the Earth which can thendecay in the atmosphere to produce an apparent upward-going air shower.


Some radio experiments searching for ντ channel

ANITA*

Antennas on ahigh-altitude balloon

over Antarctica

BEACON*

Antenna array inWhite Mountains of

California

GRAND

(Eventually)thousands of

antennas in the TienShan Mountains of

China

TAROGE

Antennas onmountains inAntarctica.

*denotes an experiment I work on.


Outline



Results from ANITA



ANITA CollaborationANtarctic Impulsive Transient Antenna

12 institutes, 3 countries, 4 continents


ANITA experiment concept


The UHECR EAS signalEarth’s magnetic field separates charges in EASs, produces radio emission

I “Direct” ∼horizontal CR’s: miss ground.I “Reflected” down-going CR’s: point to ground, opposite polarity (phase)


The ντ EAS signalCan tell apart from UHECR because direction consistent with reflected UHECR, butphase with direct UHECR


Ballooning in Antarctica

Antarctica not only has abundant ice but also hoststhe NASA long duration balloon program!

At float (35-40 km), balloon expands to size offootball stadium.

Wind patterns over Antarctica


The ANITA instrument

ANITA is an oscilloscope connected to a bunch ofantennas dangled from a balloon

ANITA’s antenna layout is driven by the launchenvelope.

0.18-1.2 GHz signal split into digitizer and trigger pathI Tunnel diode square-law detector first-level trigger.

Combinatorics between channels take O(105−6 Hz)singles rate → O(50 Hz) global rate that we canreasonably record

I Switched capacitor array digitizers for high sampling rateand low power consumption.

Telemetry via line-of-sight and satellite, but mostly relyon recovering payload for data.

I On-board prioritizer does try to telemeter the “best”events, but fortunately we’ve never had to rely on it.


Timeline of completed ANITA flights

ANITA-Lite ANITA-I ANITA-II ANITA-III ANITA-IV

2003-2004 2006-2007 2008-2009 2014-2015 2016

18 days, 2antennas

35 days, 32antennas

30 days, 40antennas

22 days, 48antennas

29 days, 48antennas

Piggy-back onTIGER

Multi-band,Pol-independent

trigger

Multi-band,VPol trigger

Full-band HPol+ VPol trigger

Full-band,Lin-Pol trigger


ANITA-III (2014-2015) and ANITA-IV (2016)Ic

e thic

kness

(m

)

Flight Path

WAIS Divide

LDB Facility

3000

4500

1500

0

ANITA-III:I Independent H + V triggerI Complications from new military comm satellites → loss of volume,

significant improvements to data analysis required.

ANITA-IV:I Tunable notch filters to reduce CW, increase livetimeI New trigger uses phase shifters to convert H+V to LCP and RCP;

requires coincidence of LCP and RCP, ensuring linear polarizationI Lower noise figure front-end design


ANITA-IV Launch (December 2016, 7 miles from McMurdo)


Example raw data (from calibration pulser)

48dual-polarizationhorn antennas

Sampled at ≈2.6 GHz’s

100 ns perevent

50 Hz globaltrigger rate

O(107) RFtriggers perflight (ANITA-IIIand IV)


Calibration

Use ground-based calibrationpulsers in a field camp (WAIS,for ANITA-III and -IV):

I Calibrate as-flown antennaphase centers (effectivepositions)

I Understand efficiency asfunction of SNR

I Estimate pointing resolutionI Measure payload tilt

Hi-Cal trailing balloon providedballoon-borne calibration signalfor part of flight (ANITA-III and-IV)

I Also better understand iceproperties!

Expected azimuth - measured azimuth1.5− 1− 0.5− 0 0.5 1 1.5

0

1000

2000

3000

4000

5000

6000

° = 0.46σ

Expected elevation - measured elevation1− 0.8− 0.6− 0.4− 0.2− 0 0.2 0.4 0.6 0.8 1

0

500

1000

1500

2000

2500

3000

3500

4000°

= 0.23σ


Signals

Askaryan emission from ν’s

Impulsive signal (few ns)

Broadband

Linearly polarized; mostlyvertically-polarized (VPol) due tointeraction geometry (Earth opaque toEeV ν’s) and transmission throughair-ice boundary (Fresnel coefficients).


Signals



Broadband


Geomagnetic emission from EAS

Impulsive signal

More low-frequency weighted

Linearly polarized; due to Earth’smagnetic field and ~v × ~B, primarilyhorizontally-polarized (HPol)


Signals and backgrounds (fake νs)



Broadband


Geomagnetic emission from EAS

Impulsive signal

More low-frequency weighted

Linearly polarized; due to Earth’smagnetic field and ~v × ~B, primarilyhorizontally-polarized (HPol)

Continuous wave (CW) signals

Anthropogenic narrow-band signals (from satellites andbases) contaminate most data so must be filtered.

RFI from payload (“payload blasts”)

Timing between antennas not plane wave-y.

Thermal noiseIncoherent random noise, that sometimes by chance looksimpulsive (but not correlated between antennas).

Impulsive anthropogenic emissionTransformers, engines, etc. produce broadband impulsiveemission that can mimic ν’s. Dominant background.


Sketch of analysis: Part 1, identify impulsive events

Three independent blind ν analyses forANITA-III, two for ANITA-IV. Basic flow:

1 Filter waveforms (reduce CW) and removeevents failing quality cuts

2 Form correlation map, where we calculatechannel cross-correlations with differentdirection assumptions

3 From peaks of correlation map, formcoherent waveforms, generate features(e.g. impulsivity, linear polarizationfraction) used to cut out thermal noise,payload RFI.

Calibration pulser event

0 20 40 60 80 100

80-

60-

40-

20-

0

20

40

60 HPol

VPol

Coherently-Averaged

0 20 40 60 80 100ns100-

80-

60-

40-

20-

0

20

40

60

80

mV

HPol

VPol

Coherently-Dedispersed

nsmV


Sketch of analysis: Part 2, reject Anthropogenics

We assume anthropogenic emission is spatiallyclustered on the continent, so we only considerisolated events as candidates.

For each signal-like event, we measure adirection with some pointing resolution.

One example clustering algorithm:I Project all interesting events to continent and

accumulate to form a “clustering map.” Useto compute overlap integral of each eventwith all other events.

I Isolated events will have overlap integralsclose to zero

Other methods to tackle anthropogenicsinclude pairwise event clustering or a binnedcontinent analysis.


Outline



Results from ANITA



Diffuse Askaryan ν results

ANITA-III: (Phys.Rev. D98 (2018) no.2, 022001)

Most sensitive search found one candidate on abackground of 0.7+0.5

−0.3 events.

ANITA-IV: (Phys.Rev. D99 (2019) no.12, 122001)

Most sensitive search found one candidate on abackground of 0.64+0.69

−0.45 events.

ANITA-III candidate: ANITA-IV candidate:

1800 2000 2200 2400 2600 2800Easting (km)

600−

400−

200−

0

200

No

rth

ing

(km

)

ANITA

Event83139414

Event Location

Mirny (RUS)

Edgeworth David (AUS)

10− 0 10 20 30 40 50 60time (ns)

40−

20−

0

20

40

am

plit

ude a

t dig

itizer

(mV

)

VPol

HPol

Coherently-Dedispersed

0 20 40 60 80 10080−

60−

40−

20−

0

20

40VPol

HPol

0 20 40 60 80 100

30−

20−

10−

0

10

20

30

40

50 VPol

HPol

am

plit

ude a

t dig

itiz

er

(mV

)am

plit

ude a

t dig

itiz

er

(mV

)

time (ns)

time (ns)

Event number = 36019849

Event number = 69261214

1710 1810 1910 2010 2110E (eV)

19−10

18−10

17−10

16−10

15−10

14−10

13−10

12−10 )-1

s-1

sr

-2 d

t (cm

ΩE

dN

/dE

dA

d

Auger 2017IceCube 2018ANITA-IIIANITA IVANITA I-IV

GZK, Kotera '10

eV18.5=10min

Ahlers '12, E


https://doi.org/10.1103/PhysRevD.98.022001

https://doi.org/10.1103/PhysRevD.99.122001

Work in progress: Non-diffuse Askaryan analyses

Searches for neutrinos in coincidence with sources ongoing in ANITA-III and ANITA-IV

Consider e.g. putative IceCube sources, flaring blazars, andGRBs

By constraining time and direction, reduce backgrounds andanalysis threshold. Also set explicit limits on sources.

Using polarization information, simulations preliminarilyindicate RA and dec resolution of a few degrees.

Intriguingly, the IceCube “neutrino burst” from TXS0506+056 occured during ANITA-III flight


EAS searches

Due to potential for upgoing showers,searches performed blind to polarity.

To be an air shower candidate, in additionto being isolated, impulsive and primarilyHPol, must:

I Match expected air shower shape (whichwe know, since we’ve detected EASbefore)

I Have polarization angle consistent withlocal magnetic field

O(30) EAS candidates identified in eachof ANITA-III and ANITA-IV.

ANITA-III event map:

3000− 2000− 1000− 0 1000 2000 3000Easting (km)

3000−

2000−

1000−

0

1000

2000

3000

Nor

thin

g (k

m)

EAS Candidates

VPol Candidate

Flight path


Upward-going showers?

Top-Left: Anomalous ANITA-III eventTop-Right, Bottom-Left: Direct UHECR candidates

Bottom-Right: A reflected UHECR candidate

An anomalous event found in ANITA-III(Phys.Rev.Lett. 121 (2018) no.16, 161102),similar to event found in ANITA-I.

Mostly HPol, matches UHECR template,polarity consistent with direct cosmic rayevent, but clearly points to ice, so consistentwith an upward going air shower.

Each event is ∼ 3σ unlikely to be ananthropogenic background.

Phenomenologically “looks like” a ντ → τcandidate, but it can’t be an SM neutrino.


https://doi.org/10.1103/PhysRevLett.121.161102

Why these can’t be a ντ

Auger, IceCube have much larger exposures at implied energy of O(1 EeV).Due to Earth opacity at UHE, not even self-consistent for diffuse flux, even accounting forτ regeneration.Very hard to produce a transient flux that IceCube or Auger would not have seen.

I IceCube not running during ANITA-I event, and had a run change at time of ANITA-III event,and Auger wasn’t sensitive to that part of the sky at the time, but... how lucky could we get?


These “ANITA anomalous events” have generated quite a lot of interest


Including of the wrong kind (tabloids!)...


...and the REALLY wrong kind (Ancient Aliens!)


Some Mundane-ish explanations

Funny ice reflections (Shoemaker et al, arxiv:1905.02846)I Possible, but ice would need to have special structure over a wide area (Fresnel zone

convolved with beam on ground)I Would need a massive underice cavern, shallow or surface lake, or something unexpected like

that in order to not be overly contrived (dielectric constrast from underice layers would havea very hard time explaining the observations).

I Lack of non-inversion from HiCal suggests that any such reflection can’t be common

Funny EAS emissionI Maybe there is a class of atypical EAS that produce signals that look differentI In particular, some air showers may not terminate before hitting the ice (de Vries and

Prohira, arxiv:1903.08750), which could potentially make an event appear to be non-inverted.I Whether or not this works will require more detailed simulations


More fun explanations: new physics!

Many exotic particle or exotic neutrino explanations that eventually produce a τ -inducedEAS (See Anchordoqui et al. arxiv:1907.06308 for a summary)

I +Compatible with observed effectI -Non-trivial to evade IceCube or Auger bounds

Maybe it’s actually Askaryan emission, not from an EAS (e.g. Hooper et al.,arxiv:1904.12865)

I +Not in tension with other experimentsI +Observed polarization and polarity possible if Askaryan shower from some deeply

penetrating particle (not a ν).I -But the observed polarization and polarity would be a coincidence

Some other radio emission mechanism entirely (e.g. axions in ionosphere, Esteban et al.arXiv:1905.10372).

I +Not in tension with other experimentsI +Testable by looking for other evidence of same mechanism in existing dataI -Unclear if could produce observed signal without more work.


What about upward showers in ANITA-IV?

Due to time-dependent system responsefrom tunable notch filters, polaritydetermination significantly morecomplicate in ANITA-IV

We’ve very recently unblinded polarity ...I For real this time! Had to re-blind

polarity after significant errors found indetermining system response

... but I don’t have permission to shareresults with you.

However, results should be revealedTuesday at Stephanie Wissel’sNeutrino2020 talk!


Some other things ANITA can measureMeasure ice reflectivity / roughness (with HiCal, reflection of sun, EAS)(arxiv:1801.08909)Look for some other exotics that can produce radio signatures

I Monopoles (arXiv:1008.1282)I Antiquark Nuggets (arXiv:1208.3697)

Lorentz Invariance (arXiv:1207.6425)


Outline



Results from ANITA



Future of ANITA: Payload for Ultrahigh Energy Observations (PUEO)

PUEO

pueo

More antennas (120 instead of48), but with a higher cutofffrequency (300 vs. 180 MHz).

Much lower trigger threshold

24 antennas canted down to fillgap in ANITA elevation coverage(and further investigate steep airshower events)

Improved digitizers, front-endelectronics

Up to 10X more sensitive thanANITA-IV

Projected PUEO sensitivity:

1810

1910

2010 10

1

10

210

Eff

ectiv

e V

olu

me

Ra

tio

PUEO / ANITA-IV

1810 1910 2010E (eV)

19−10

18−10

17−10

16−10

15−10

14−10

13−10

12−10

)-1 s

-1sr

-2

dt

(cm

ΩE

dN

/dE

dA

d

ANITA-III

ANITA IV

Auger 2017

IceCube 2018

Projected PUEO Sensitivity (30 days)

KKSS '02

Takami et al '09

eV18.5

=10min

Ahlers '12, E

GZK, Kotera '10


How to reduce threshold? Beamforming Trigger!

Abandon analog combinatoric trigger, switch to adigital beam-forming trigger

Low-bit Streaming DigitizerAntenna Signals Beamform (Delay-and-Sum) Trigger on Power Envelope

Use streaming digitizers (mostly likely a low-bitcustom ASIC, for power reasons) to record signalsfrom each channel in real time, then delay and sumaccording to causal plane-wave hypotheses(“beams”).

Technique demonstrated in-situ at the South Pole,this would use more channels and higher-gainantennas to achieve an even lower threshold.

0 1 2 3 4 50.0

0.2

0.4

0.6

0.8

1.0

Tri

gger

Eff

icie

ncy

PUEO16-antennacoherenttriggersimulation

ANITA-IVtrigger[measured]

NuPhase7-antennacoherenttrigger[simulated]

[measured]


See my PUEO poster at Neutrino2020!

Poster 486, presented at poster session that just happened(so you’ll need access to the parallel universe to see it)

Video: https://www.youtube.com/watch?v=uCy6mKr_d2E


https://www.youtube.com/watch?v=uCy6mKr_d2E

Conclusions

Ultrahigh-energy (UHE) neutrinos can teach us alot about the universe and neutrinos.

Radio detectors can be used to search for UHEneutrinos.

ANITA I-IV combined set the best limits on UHE νflux above 1019.5 eV.

ANITA has detected EAS candidates consistentwith an upward-going air shower, but unclearintepretation.

Stay tuned for ANITA-IV polarity unblinding andANITA-III and ANITA-IV source searches!

The proposed PUEO will have substantial hardwareand sensitivity improvements.

Thank You!

Questions?


Backup Slides


ANITA-III Block DiagramSe

avey

Ant

enna

(x4

8)

180-1200 MHz bandpass

Bias Tee

Front-end Amplification

HPol

40 ft LMR-240

40 dB LNA

Bias Tee

Second-Stage Amplification3 dB attenuator

Instrument Box

180-1200 MHz bandpass

trigger path

Square-LawDetector

digitizer path

cPCI Crate

Disk Storage (Helium Drives)

SURF

cPCI backplane

discriminator

DAC

FPGAL1 + L2 Triggers

TURF FPGAL3

Trigger

LAB3 (x4)2.6 GSa/s

40 dB LNA

hold/digitize

Flight Computer

GPS Antennas, NASA SIP, Sun Sensors, etc.

(identical to VPol)

VPol

amp


ANITA-IV Block DiagramSe

avey

Ant

enna

(x4

8)

1200 MHzlowpass

Front-end Amplification

HPol

20 ft SFX-500

Second-Stage Amplification

3 dB attenuator

Instrument Box

180-1200 MHzbandpass

trigger path

Square-LawDetector

digitizer path

cPCI Crate

Disk Storage (Helium Drives)

SURF cPCI backplane

discriminator

DAC

TURF

LAB3 (x4)2.6 GSa/s

35 dB LNA

hold/digitize

Flight Computer

GPS Antennas, NASA SIP,Sun Sensors, etc.

(identical to VPol)

VPol

amp

45 dBLNA

260, 375 & 460 MHz tunable notch filters

90° hybridcoupler

FPGAL0, L1 & L2

Trigger

FPGAL3

Trigger

HPol RCPol

LCPol


PUEO Block Diagram

NUMBER SHEET

TITLESUBTITLE

COMPANY NAME

_________

_________

_________

_________

_________

_________

_________

_________

_________

PUEO system diagram

3/13/2019

1 of 1Rev. 1

Ring 1

(top)

Ring 2

Ring 3

Ring 4

Ring 5

(drop-down)

Dual-Polarized Quad-Ridged

Horn Antennas

280-1200 MHz

120 total antennas

PHI-SECTOR N of 24

Vpol pre-amp

+ RFoF Tx

Hpol pre-amp

+ RFoF Tx

Vpol pre-amp

+ RFoF Tx

Vpol pre-amp

+ RFoF Tx

Vpol pre-amp

+ RFoF Tx

Vpol pre-amp

+ RFoF Tx

Hpol pre-amp

+ RFoF Tx

Hpol pre-amp

+ RFoF Tx

Hpol pre-amp

+ RFoF Tx

Hpol pre-amp

+ RFoF Tx

+4V DC

power

+4V DC

power

+4V DC

power

+4V DC

power

+4V DC

power

1 of 24

1 of 24

1 of 24

1 of 24

1 of 24

1

2

NOTES:

1

2

3

4

Legend

Digital link

Digital link - gigabit serial

DC Power

RF signal - coax

RF signal - optical fiber

PUEO Main Instrument Faraday Housing

RFoF

Receiver

Bank

240

total

H+V ch.

Pre-amp power

Distribution

PUEO CPCI Crate 3

48 ch.

Ring 5

(drop-

down)

192 ch

Rings

1-4

CPCI Back

plane

16 Ch.

DTA

4

12 boards

3 boards

Trigger

Unit

for Radio-

Freq.

(TURF)

board

Flight CPUXCOM-6400

10 GbEGPU Compute

Engine

(XMC

expansion)

Telemetry

House-

keeping &

Sensors

To CSBF SIP

Acc

elero

mete

r, T

empera

ture

,

Sun-Sensors

, Magneto

mete

r

HOUSEKEEPING S

ENSOR S

UITE:

Storage Servers &

Storage

[56 TB x 3]

Nav. Systems:

IMU (LN-251) &

Diff. GPS (Trimble ABX-2)

DC-DC power

Charge

Controller

10 GbE

Pre-flight

testing

3.7, 4.0, 12.0V

Navigation

Antenna Suite

Photovoltaic

Panel ArrayBatteriesRF-over optical fiber routed in 12-channel bundles

between pre-amps and the Main Instrument (TFOCA-II)

Power to pre-amps sent over LMR-240 coaxial cable.

One cable serves 12 pre-amp channels

CPCI crate is used for power (via backplane) and

heat sinking only. All data flow through separate

high-speed serial links.

The Digitizer and Trigger Assembly (DTA) is a two-

board stackup made from a Sampling Unit for RF

(SURF) board and a mezzanine Trigger Interferometric

Sum Correlator (TISC) board. The SURF includes a pair

of programmable notch filters per channel

16 Ch.

DTA


ANITA-III Trigger

VPol

HPol

digitizer

full band

full band

L2:multiple L1's in causal time window

independent H and V

L3: adjacent L2 phi sectors

?

?

hold

GPU prioritizer

telemeter

disk

L1: ʃv2 above threshold

dt


ANITA-IV Trigger

LCP

RCP

phase shifter

tunable notches

digitizer

full band

full band

L2: L3:adjacent L2 phisectors

?

?

holdGPU prioritizer

telemeter

disk

L0:ʃv2 abovethreshold

dt

VPol

HPol

L1:LCP-RCP coincidence

2 out of 3upgoing

AND


Exploring the Ultrahigh-Energy Universe with the ANITA Long ...

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