Op#mizing ARIANNA Design (all-nu, nu-tau, cosmic ray) US, Sweden, - - PowerPoint PPT Presentation

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Op#mizing ARIANNA Design (all-nu, nu-tau, cosmic ray) US, Sweden, - - PowerPoint PPT Presentation

Feb 18, 2023 136 likes •579 views

Op#mizing ARIANNA Design (all-nu, nu-tau, cosmic ray) US, Sweden, Taiwan, Germany, Denmark S. Barwick, UC Irvine PoS(ICRC2017) 1042 Why go to Polar Regions? Radio Quiet, but Noisy near bases and/or experiments Noise from satellites

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SLIDE 1

Op#mizing ARIANNA Design

(all-nu, nu-tau, cosmic ray)

US, Sweden, Taiwan, Germany, Denmark

  • S. Barwick, UC Irvine

PoS(ICRC2017) 1042

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SLIDE 2

Why go to Polar Regions?

  • Radio Quiet, but

– Noisy near bases and/or experiments – Noise from satellites in case of ANITA-III

  • Thick cold, Radio transparent, (free) material
  • Ice provides a dense target for neutrinos
  • Surprisingly good infrastructure

TeraTon detectors at modest cost

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SLIDE 3

Science Mo#va#on

  • ARIANNA 5 year sensi#vi#es for 1296 sta#ons

(including published live#mes and analysis efficiency)

Reach minimum all proton cosmogenic flux

C Persichilli PoS(ICRC2017)977

IceCube ARIANNA baseline ARIANNA with wind

IC EHE

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SLIDE 4

Science Mo#va#on

  • ARIANNA 5 year sensi#vi#es for 1296 sta#ons

(including published live#mes and analysis efficiency)

Extend measurement of IceCube Flux

C Persichilli PoS(ICRC2017)977

IceCube ARIANNA baseline ARIANNA with wind

IC EHE

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SLIDE 5

Science Mo#va#on

  • ARIANNA 5 year sensi#vi#es for 1296 sta#ons

(including published live#mes and analysis efficiency)

Improve search at 1020 eV by order of magnitude

C Persichilli PoS(ICRC2017)977

IceCube ARIANNA baseline ARIANNA with wind

IC EHE

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SLIDE 6

Hexagonal Radio Array (HRA):

2012-present

Moore’s Bay, 110 km from McMurdo Station

Deployed 2012 Deployed 2014 1 km A B C D E F G

CR 1 CR 2 HCR

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SLIDE 7

Current status of ARIANNA - HRA HRA

7

7 regular sta1ons “Cosmic Ray” sta1on 1 “Cosmic Ray” sta1on 2

All sta#ons run reliably since deployment - technology is ready

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SLIDE 8

Event ID: Template Matching

Template Observed CR Candidate Predicted waveforms confirmed by Cosmic Ray “calibra#on beam”

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SLIDE 9

>200 Cosmic Ray Candidates

Nelles PoS(ICRC2017)399 and Wang PoS(ICRC2017)358

2015-2016 2016-2017 Horizontal CR tower 2016-2017

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SLIDE 10

Neutrino Search 2015-2017

CR candidate

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SLIDE 11

Horizontal Propaga#on at ARIANNA site

1 km A B C D E F G

CR 1 CR 2 HCR

Vpol Dipole pulser buried at depth of 20m Despite non-op#mal antenna geometry, signals observed

  • n all sta#ons to 1.4 km

X D C B A

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SLIDE 12

Horizontal Propaga#on also seen at South Pole

Antarc#c data compa#ble with simple model |E|~ (e-r/Lajen)/r ARIANNA site

  • S. Pole (D. Besson)

Lajen= 508 m Lajen= 501 +-168 m

Distance(m) 1600 Ln(r*V)

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SLIDE 13

Modeling Horizontal Propaga#on-ray paths

Realis#c Firn Idealis#c Firn

ARIANNA

No signals propagate to ARIANNA sta#on

ARIANNA

TRX TRX

Large amplitudes in 100m studies suggests ~50% of signal is trapped; modeling consistent with this

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SLIDE 14

Poten#al Improvement with Horizontal Propaga#on

No geometric reason to bury antennas at S. Pole Combina#on sta#on with both dipoles and LPDA gives best results with horizontal propaga#on 5x increase is possible! As few as 169 ARIANNA sta#ons at South Pole can reach science goal 5x increase

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SLIDE 15

Commentary

  • IceCube neutrinos, especially those above

1015 eV provide strong incen#ve to probe to higher energies with larger detectors.

  • ARIANNA technology has operated robustly
  • Horizontal propaga#on has poten#al to

improve sensi#vity. It is worth inves#ga#ng I believe the Antarc#c neutrino projects will coalesce around common technique within the next year to produce a “mature” proposal supported by the community.

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SLIDE 16

Thank You

Thank You!

Shown: (Left to right) Joulien Tatar, Chris Persichilli, James Walker, Corey Reed

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SLIDE 17

Backup Slides

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SLIDE 18

Modeling Horizontal Propaga#on

Signal vs depth Signal vs Distance (2-4m below surface)

ARIANNA

TRX

Rays emijed between 38o-40o trapped within 5m

  • f surface

Lajen =500m Range (m) 500 2500 Depth (m) 40 ~50% signal trapped

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SLIDE 19

Quote from the recent IceCube paper (arXiv:1607.05886): The detec(on of cosmogenic neutrinos from sources with weak or no evolu(on, and of heavy-composi(on UHE-CRs requires a larger scale detector. Cost effec(ve radio Askaryan neutrino detectors, such as ARA or ARIANNA, will therefore be an important future op(on.

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SLIDE 20

EHE ν detectors: Comments

  • Contribute to ongoing quest to understand EHE CRs
  • Neutrino measurements provide independent confirma#on of GZK

mechanism

  • Combined with CR and photon measurements, can help to constrain

source class, evolu#on, Emax, and composi#on of CR

  • Direct measurements of CR
  • Search for new physics
  • Beam of EeV neutrinos can uncover new physics at ~5-10 x Ecm of LHC

through cross-sec#on and spectral modifica#ons

  • Search for new sources:
  • EeV neutrinos must point back to sources and direc#on can be measured

with good precision ( and current procedures can be improved).

EHE neutrino detectors:

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SLIDE 21

ARIANNA CR summary

Between December 2015 and mid-March 2016 42 Cosmic Ray candidates 3 involved a coincidence between 2 sta#ons 1 involved a coincidence between 3 sta#ons 1 involved a coincidence between 5 sta#ons Candidates

  • 1. Isolated in #me and similar characteris#cs
  • 2. Have smooth and con#nuous power in FFT
  • 3. More power in upward than downward LPDA
  • 4. Correlate with CR template
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SLIDE 22

Capabili#es

Angular resolution σθ~2.8o Down horizon cos(θ)

  • K. Dookayka, UCI PhD dissertation, 2011
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SLIDE 23

No evidence of dispersion by horizontal propaga#on for d= 100m

Excellent shape agreement between air to air studies in park and 100m through snow

Dipole to Dipole, air vs 100m of firn

Dipole (20m) to LPDA Air vs firn

In shadow zone!

Large intrinsic dispersion due to X-pol

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SLIDE 24

Capabili#es

Angular resolution σθ~2.8o Down horizon cos(θ)

  • K. Dookayka, UCI PhD dissertation, 2011
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SLIDE 25

ARIANNA can find new hard spectrum source if 0.1ΦWB

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SLIDE 26

SAVANT Wind Generator: 2016

Data 2016 Expecta#on 2016 Expecta#on 2017

  • H. Bernhoff et al., Uppsala, Department of Engineering Sciences, 2016

ARIANNA Site

HRA power requirement

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SLIDE 27

SAVANT Wind Generator: 2016

  • H. Bernhoff et al., Uppsala, Department of Engineering Sciences, 2016

ARIANNA Site Produced power consistent with design es#mate. Will it survive the Antarc#c winter? Does it produce RF noise? (anechoic chamber tests say no) Can Bajery management cope with Wind Gen and solar?

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SLIDE 28

Radio Pulses by Cosmic Rays in Atmosphere

But primary effect in dense media

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SLIDE 29

Annual Rate of CRs in ARIANNA

(~3x105 /year triggered with upward antenna)

Ecr ~ 1020 eV ~ 1/year Majority of CR at highest energies arrive from direc#ons within 30 deg of horizon S.Barwick, et al. , arXiv:1612.04473v1 Look for anisotropies Energy spectrum with radio technique

Auger Spectrum

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SLIDE 30

Cosmic Rays

30

Raw electric field pulse 80 ns Raw electric field spectrum 500 MHz 0 MHz Antenna/amp response Signal through back

  • Air shower signals

through front-lobe of LPDA have a unique characteris1c

  • High frequency chirping

followed by lower frequencies

  • Due to short broadband

pulses and group delay of antenna

Gain and group-delay 150 ns Signal through front 200 ns 300 mV 30 mV COREAS

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SLIDE 31

A few words on Dispersive LPDA

Dispersion is beneficial to help iden#fy short (few ns) pulses. Chirping + envelope is unique, and efficient. No RF BG close at ARIANNA site. There is not much downside to dispersion since most of the voltage amplitude in #me domain is derived from lowest frequencies (50 to 200 MHz). Dispersion is small enough so components add almost coherently. Small inefficiency at trigger level compensated by improved analysis efficiency. In addi#on, LPDA gain is 4-6 over the en#re frequency band, so signals are large compared to e.g, dipole. LPDA are inexpensive ~ $100 US in bulk purchase –other electronic components dominate budget LPDA are direc#onal and excellent in Xpol rejec#on. ARIANNA LPDA very good at polariza#on measurement.

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SLIDE 32

Nu-tau Detec#on with Radio

Concept:

ντ sta#on consist of 3 towers with 2 dual pol LPDA

Dual-pol LPDA 6-8 m

  • J. Nam, NTU, 2017

Flavor ra1o is intriguing probe for ν 1) source physics 2) oscilla#on 3) decay 4)mass hierarchy

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SLIDE 33

Detector Concepts

ARIANNA ARA

20m 4m 1 sta#on of 37, 2km spacing 1 sta#on in array of 36 x36, 1km spacing

  • S. Barwick, et al., IEEE Trans. Nucl Sci. (2015)
  • P. Allison, et al, Astropart. Phys. 35 (2012)

200 m

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SLIDE 34

Horizontal Cosmic Ray (HCR) tower

(prototype installed November 2016)

  • Goals

1) Evalua#on construc#on/robustness 2) Long-term RFI survey 3) Evalua#on of angular resolu#on 4) Evalua#on of CR backgrounds 5) Measurement of CR Flux vs theta

  • 4 antennas (3 Hpol + 1 Vpol) poin1ng

to the mountain

Galac#c excess clearly seen! RF Power vs Time

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SLIDE 35

HiCal and Angular Resolu#on

600 km ~40 km HCR Tower All ARIANNA sta#ons observed signals from HiCal

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SLIDE 36

HiCal and Angular Resolu#on

HCR tower HiCal GPS

preliminary Launched December 2016 No pulses

  • bserved un#l

HiCal visible above Minna Bluff

S.Wang, NTU, 2016

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SLIDE 37

Bounce Tests

Pulser->Seavey TRX->Sta#on

water

Trx

ARIANNA Station

LPDA LPDA LPDA LPDA

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SLIDE 38

Field Ajenua#on Length in ice

1 km

  • S. Pole, Antarc#ca

Similar numbers for Greenland at 75MHz

  • S. Wissel, et al. (ICRC -2015)

ARIANNA site, Ross Ice Shelf Shorter, due to warmer ice along reflected path Reflec#vity ~ perfect mirror

  • J. Hanson, et al., J. Glac. 61 (2015)
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SLIDE 39

ARIANNA Site is RF Quiet

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SLIDE 40

Opera#onal Efficiency = 0.87

1 km A B C D E F G Losses due to :

  • 1. Data transfer
  • 2. Calibra#on runs
  • C. Persichilli, CHEAPR, 2016
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SLIDE 41

Long Term Opera#on ARIANNA HRA

Yearly average of 0.58 yr At the moment, opera#on only during sunlit periods of year. New effort to run off wind generators in winter

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SLIDE 42

Shadow regions

Volume of ice where interac#ons produce signals that cannot reach receiver antennas Blue medium has parabolic varia#on of index of refrac#on ν RF pulse Shadow Region Firn ice at top of ice sheet has approximate gradient (n=1.32 top, n=1.78 bot)