Radio Detec+on of High-Energy Neutrinos
Christian Glaser
Christian Glaser, Chiba, October2020

High Energy Universe§ Origin of cosmic rays is a century long mystery§ Observation of ultra-high energy cosmic rays (1 Joule in a single proton)

ycosmic ra

Christian Glaser, Chiba, October2020

Sources of 1020 eV Particles

Need accelerator of size of Mercury ś orbit
to reach 1020 eV with LHC technology

Christian Glaser, Chiba, October2020

High Energy Universe§ Origin of cosmic rays is a century long mystery§ Observa;on of ultra-high energy cosmic rays (1 Joule in a single proton)§ Insights into most violent phenomena in our universe§ Measured extensively over decades but no hint of source§ Cosmic rays are deﬂected ~ Z/E§ anisotropy with high energy protons

ycosmic ra

Christian Glaser, Chiba, October2020

use

Neutrinos instead of cosmic rays

§ Created by cosmic rays at the source§ Electrically neutral, (almost) no mass, small interaction cross section§ No deflection§ Excellent messenger particle

ycosmic raneu
trino

Christian Glaser, Chiba, October2020

better useNeutrinos instead of cosmic rays

§ Created by cosmic rays at the source§ Electrically neutral, (almost) no mass, small interac;on cross sec;on§ No deﬂec;on§ Excellent messenger par0cle§ Coincident detec;on with EM and gravita;onal waves (mul0 messenger)

gam
ma
ray

neu
gratrinvitoation
al waves

Chris4an Glaser, Chiba, October2020

ycosmic raExperimental Challenges§ Low interaction cross section of neutrinos

neutrino spectrum§ Very low neutrino flux
→Very large volumes needed for reasonablerates

optical7Chris4an Glaser, Chiba, October2020

IceCubeExperimental Challenges§ Low interaction cross section of neutrinos

neutrino spectrum§ Very low neutrino flux
→Very large volumes needed for reasonablerates§ Solution: radio technique§ Large volumes at no cost: Antarctic ice§ Ice transparent to radio waves (L ~ 1km)
§ A single radio station has 1km³ effective
volume (comparable to IceCube)

op;cal8

Chris&an Glaser, Chiba, October2020

IceCuberadioRadio Emission of Particle Showers§ Askaryan effect: Time varying negative charge excess in the shower front§ Macroscopic: Longitudinal current

v=c/ n§ Microscopic: Acceleration and creation of charge§ Cherenkov-like time compression effect§ Shower is faster than its emissionv/nc=§ Constructive interference at the Cherenkovangle§ In ice: arccos(1/n) = 56 deg
v=c

9Chris&an Glaser, Chiba, October2020

Radio Emission of Particle Showers§ Askaryan effect: Negative charge excess in the shower front

10

Chris&an Glaser, Chiba, October2020

Radio Emission of Par+cle Showers§ Askaryan effect: Negative charge excess in the shower front§ No neutrino detected yet because current detectors are toosmall but§ Askaryan pulse measured in lab§ Feasibility shown with cosmic-ray detectors
misco11ayrc§ Radio signals very similar§ Mature and competitive detection technique§ Knowledge transfer to neutrinos

Chris&an Glaser, Chiba, October2020

Air Shower Experiments§ Radio detection is establishedtechnique for cosmic-ray detection§ Most achievements can be transferred
to neutrino detection

12

Chris&an Glaser, Chiba, October2020

Image by Tim Huege

Achievements of Radio Detection of Cosmic Rays
Cosmic-ray quantities of interest

directionenergy~10% energy resolution~10% systematic uncertainty< 1 degree

Pierre Auger Collaboration, PRL 116 241101 (2016), PRD
93 122005 (2016), JINST 12 T10005 (2017), Gottowik et al.,Astro Part. 103 87-93 (2018)

mass/charge

16 g/cm2 Xmax resolu;on
Buitink et al., PRD 90 082003 (2014)
Buitink et al., Nature 531 70-73 (2016)

Radio is compe,,ve to tradi,onal techniques
13

Chris&an Glaser, Chiba, October2020

Auger Prime Upgrade§ All 1600 surface detectors will be upgraded with scin5llators and radio antennas§ Combine radio with par5cle measurement -> cosmic-ray charge/mass§ Anisotropy analysis with protons only -> chance of source discovery

14

Christian Glaser, Chiba, October2020

Detection of High-Energy Neutrinos

not to scale
15

Christian Glaser, Chiba, October2020

Detection of High-Energy Neutrinos
:
1EGR
ENO
LTL
CA
E
CHET
DGNI
W O RK§ Two pilot detectors§ ARA (South Pole)§ ARIANNA (Moor’s Bay + South Pole)§ Size 1%- 5% of required size
§ no neutrino measured yet but§ Hardware proven reliable§ Technology ready for large scale detector

16

Christian Glaser, Chiba, October2020

harsh Antarctic conditions

Development of wind power system§ Autonomous stations have many advantages§ Wind power system required for dark wintermonths§ Pioneered at Uppsala§ current prototype survives harsh Antarctic conditions
and powers station for ~50% of the time

17

Christian Glaser, Chiba, October2020

ARIANNA collaboration, JCAP 03(2020)053

:N2OI
ETGA
N
ICLEFILTANHECID
Example: ARIANNA signal searchONIRTNEUsignal in detector

neutrino signal

hardwareresponse

simulation
template
correlation

18

Christian Glaser, Chiba, October2020

datano neutrino found-> limit on neutrino ﬂux

3:NEOIGTNCEUL
CHAL RECONSTR
TEVEN
Neutrino quan00es of interest

direction

19

Christian Glaser, Chiba, October2020

energyflavor

C. Glaser, PoS(ICRC2019)899

Neutrino Direc+on§ The neutrino direc5on depends on the§ signal arrival direc;on "⃗§ signal polariza;on #⃗§ viewing angle Θ§ distance to neutrino interac;on to correct for bending in ﬁrn<latexit sha1_base64="VNYg5CblcxyNYeM4KIzxGk0COSQ=">AAAB7nicbVBNS8NAEJ3Ur1q/qh69LBbBU0mqoMeiF48V7Ae0oWy2k3bpZhN2N4US+iO8eFDEq7/Hm//GbZuDtj4YeLw3w8y8IBFcG9f9dgobm1vbO8Xd0t7+weFR+fikpeNUMWyyWMSqE1CNgktsGm4EdhKFNAoEtoPx/dxvT1BpHssnM03Qj+hQ8pAzaqzU7k2QZcmsX664VXcBsk68nFQgR6Nf/uoNYpZGKA0TVOuu5ybGz6gynAmclXqpxoSyMR1i11JJI9R+tjh3Ri6sMiBhrGxJQxbq74mMRlpPo8B2RtSM9Ko3F//zuqkJb/2MyyQ1KNlyUZgKYmIy/50MuEJmxNQSyhS3txI2oooyYxMq2RC81ZfXSatW9a6qtcfrSv0uj6MIZ3AOl+DBDdThARrQBAZjeIZXeHMS58V5dz6WrQUnnzmFP3A+fwCnCY/G</latexit><latexit sha1_base64="VNYg5CblcxyNYeM4KIzxGk0COSQ=">AAAB7nicbVBNS8NAEJ3Ur1q/qh69LBbBU0mqoMeiF48V7Ae0oWy2k3bpZhN2N4US+iO8eFDEq7/Hm//GbZuDtj4YeLw3w8y8IBFcG9f9dgobm1vbO8Xd0t7+weFR+fikpeNUMWyyWMSqE1CNgktsGm4EdhKFNAoEtoPx/dxvT1BpHssnM03Qj+hQ8pAzaqzU7k2QZcmsX664VXcBsk68nFQgR6Nf/uoNYpZGKA0TVOuu5ybGz6gynAmclXqpxoSyMR1i11JJI9R+tjh3Ri6sMiBhrGxJQxbq74mMRlpPo8B2RtSM9Ko3F//zuqkJb/2MyyQ1KNlyUZgKYmIy/50MuEJmxNQSyhS3txI2oooyYxMq2RC81ZfXSatW9a6qtcfrSv0uj6MIZ3AOl+DBDdThARrQBAZjeIZXeHMS58V5dz6WrQUnnzmFP3A+fwCnCY/G</latexit><latexit sha1_base64="VNYg5CblcxyNYeM4KIzxGk0COSQ=">AAAB7nicbVBNS8NAEJ3Ur1q/qh69LBbBU0mqoMeiF48V7Ae0oWy2k3bpZhN2N4US+iO8eFDEq7/Hm//GbZuDtj4YeLw3w8y8IBFcG9f9dgobm1vbO8Xd0t7+weFR+fikpeNUMWyyWMSqE1CNgktsGm4EdhKFNAoEtoPx/dxvT1BpHssnM03Qj+hQ8pAzaqzU7k2QZcmsX664VXcBsk68nFQgR6Nf/uoNYpZGKA0TVOuu5ybGz6gynAmclXqpxoSyMR1i11JJI9R+tjh3Ri6sMiBhrGxJQxbq74mMRlpPo8B2RtSM9Ko3F//zuqkJb/2MyyQ1KNlyUZgKYmIy/50MuEJmxNQSyhS3txI2oooyYxMq2RC81ZfXSatW9a6qtcfrSv0uj6MIZ3AOl+DBDdThARrQBAZjeIZXeHMS58V5dz6WrQUnnzmFP3A+fwCnCY/G</latexit>~l~v⌫<latexit sha1_base64="k3k4By9SOWioOdnL7BKnTWB3Ths=">AAAB7nicbVBNS8NAEJ3Ur1q/qh69LBbBU0mqoMeiF48V7Ae0oWy2k3bpZhN2N4US+iO8eFDEq7/Hm//GbZuDtj4YeLw3w8y8IBFcG9f9dgobm1vbO8Xd0t7+weFR+fikpeNUMWyyWMSqE1CNgktsGm4EdhKFNAoEtoPx/dxvT1BpHssnM03Qj+hQ8pAzaqzU7k2QZWLWL1fcqrsAWSdeTiqQo9Evf/UGMUsjlIYJqnXXcxPjZ1QZzgTOSr1UY0LZmA6xa6mkEWo/W5w7IxdWGZAwVrakIQv190RGI62nUWA7I2pGetWbi/953dSEt37GZZIalGy5KEwFMTGZ/04GXCEzYmoJZYrbWwkbUUWZsQmVbAje6svrpFWrelfV2uN1pX6Xx1GEMziHS/DgBurwAA1oAoMxPMMrvDmJ8+K8Ox/L1oKTz5zCHzifP6D1j8I=</latexit><latexit sha1_base64="gf7R24uxlFwC2mw9oShPRWeaF/k=">AAAB8nicbVBNS8NAEJ3Ur1q/qh69LBbBU0mqoMeiF48V7AckoWy2m3bpZjfsbgol9Gd48aCIV3+NN/+N2zYHbX0w8Hhvhpl5UcqZNq777ZQ2Nre2d8q7lb39g8Oj6vFJR8tMEdomkkvVi7CmnAnaNsxw2ksVxUnEaTca38/97oQqzaR4MtOUhgkeChYzgo2V/GBCST6Z9QOR9as1t+4ugNaJV5AaFGj1q1/BQJIsocIQjrX2PTc1YY6VYYTTWSXINE0xGeMh9S0VOKE6zBcnz9CFVQYolsqWMGih/p7IcaL1NIlsZ4LNSK96c/E/z89MfBvmTKSZoYIsF8UZR0ai+f9owBQlhk8twUQxeysiI6wwMTalig3BW315nXQade+q3ni8rjXvijjKcAbncAke3EATHqAFbSAg4Rle4c0xzovz7nwsW0tOMXMKf+B8/gDF+5GS</latexit>~ int
X<latexit sha1_base64="4+x9NZsI47i6AQRd0Ta8tbFYMFA=">AAAB/XicbVDLSsNAFJ34rPUVHzs3g0VwVZIq6LLoxmUF+4AmhMl00g6dmYSZSaGG4K+4caGIW//DnX/jpM1CWw8MHM65lzn3hAmjSjvOt7Wyura+sVnZqm7v7O7t2weHHRWnEpM2jlkseyFShFFB2ppqRnqJJIiHjHTD8W3hdydEKhqLBz1NiM/RUNCIYqSNFNjH3oTgrJcHHkd6JHlGhc4Du+bUnRngMnFLUgMlWoH95Q1inHIiNGZIqb7rJNrPkNQUM5JXvVSRBOExGpK+oQJxovxslj6HZ0YZwCiW5gkNZ+rvjQxxpaY8NJNFRrXoFeJ/Xj/V0bVvDkpSTQSefxSlDOoYFlXAAZUEazY1BGFJTVaIR0girE1hVVOCu3jyMuk06u5FvXF/WWvelHVUwAk4BefABVegCe5AC7QBBo/gGbyCN+vJerHerY/56IpV7hyBP7A+fwCCn5Xo</latexit>

20

Christian Glaser, Chiba, October2020

p~p~p~firn
deep ice

ARIANNA collabora;on, JINST 15 (2020) P09039

In-situ measurement at South Pole§ Radio emitter lowered into ~2 km deep borehole§ signal direction: sub-degree resolution achieved(including ice correction)

21

Christian Glaser, Chiba, October2020

ARIANNA collabora;on, JINST 15 (2020) P09039

In-situ measurement at South Pole§ Radio emitter lowered into ~2 km deep borehole§ signal direction: sub-degree resolution achieved(including ice correction)§ polarization: 2.7 degree resolution-> dominates neutrino
direction

22

Christian Glaser, Chiba, October2020

3:
NEOI
GTNCEULCHAL RECONSTR
TEVEN
Neutrino quan00es of interest

direction

23

Christian Glaser, Chiba, October2020

energyflavorGeHng the Neutrino Energy§ Electric ﬁeld dependenceFrom measured voltage via
antenna unfolding, requires
RF direction and polarization

Viewing angle via
Frequency spectrum ->broadband antennas and/orMapping of Cherenkov cone

distance to shower

Neutrino energy to shower energy
Neutral Current Interaction (NC)!
!
undetected§ Irreducible uncertainty fromneutrino -> shower energy§ Sets requirements for othercontributions to energy resolution(~factor of 2)§ No need to be much better thanuncertainty from inelasticity
24

Christian Glaser, Chiba, October2020

Z

nucleus

quark
quark
quark

quark
quark
quark

C. Glaser, PoS(ICRC2019)899

hadronicshower

D’n’R Technique§ Antenna observes direct and reflected pulse§ Time difference ~ 1 / distance§ Efficiency + resolution~ depth of antenna

25

Chris&an Glaser, Chiba, October2020

ARIANNA collaboration, JCAP 11(2019)030

First Experimental Results§ Measurement at Moore’s Bay§ 40m deep transmi\er§ 10m deep receiver§ thanks to EnEX/Aachen drill

26

Chris&an Glaser, Chiba, October2020

ARIANNA collaboration, JCAP 11(2019)030

ARIANNA collabora;on, JCAP 11(2019)030

Monitoring of Snow Accumulation~1 mmprecision

27Chris&an Glaser, Chiba, October2020

3:NEOIGT
NCEU
L
CHAL RECONSTR
TEVEN
Neutrino quantities of interest

directionenergyflavorjust star;ng to explore ﬂavor physics-> D. Garcia, C. Glaser, A. Nelles,
Phys. Rev. D 102, 083011 (2020)28

Chris&an Glaser, Chiba, October2020

The future part I: RNO-G(Radio Neutrino Observatory – Greenland)

RNO-G collaboration, arXiv:2010.12279§ 35 autonomous stations

29

Chris&an Glaser, Chiba, October2020

ARIANNA collaboration, arXiv:2004.09841

The future part I: ARIANNA-200 (proposal)§ 200 autonomous surface stations on theRoss Ice Shelf§ Advantage: large sky coverage§ Not funded yet

30

Chris&an Glaser, Chiba, October2020

Science Poten+al

RNO-G collaboration, arXiv:2010.12279
ARIANNA collaboration, arXiv:2004.09841

Diffuse neutrino flux
RNO-G

31

Chris&an Glaser, Chiba, October2020

ARIANNA-200

The future part II: IceCube-Gen2§ Large radio detector is part ofIceCube-Gen2§ to increase sensitivity for E>1016eV§ >200 radio detector stations

32

Chris&an Glaser, Chiba, October2020

IceCube-Gen2 collaboration, arXiv:2008.04323

IceCube-Gen2 collaboration, arXiv:2008.04323

Science Potential IceCube-Gen2 Radio
Explosive sources
Diffuse neutrino flux

33

Chris&an Glaser, Chiba, October2020

IceCube-Gen2 collaboraQon, arXiv:2008.04323

Science Potential IceCube-Gen2 Radio
Explosive sources
Diffuse neutrino flux

34

Chris&an Glaser, Chiba, October2020

NS-NS merger follow up

Summary§ Radio detection is an intriguing (new) technique to detect neutrinosof the highest energies§ Emission properties well understood§ Technology proven in pilot arrays§ Future:§ RNO-G: 35 stations in Greenland§ Radio component of IceCube-Gen2: 200+ stations at the South Pole

35

Chris&an Glaser, Chiba, October2020

NuRadioMC

Simulating the radio emission ofneutrinos from interaction to detector
Christian Glaser, Daniel García-Fernández, Anna Nelles, Jaime Alvarez-Muñiz, Steven W.
Barwick, Dave Z. Besson, Brian A. Clark, Amy Connolly, Cosmin Deaconu, Krijn de Vries, Jordan C.
Hanson, Ben Hokanson-Fasig, R. Lahmann, Uzair Latif, Stuart A. Kleinfelder, Christopher
Persichilli, Yue Pan, Carl Pfender, Ilse Plaisier, Dave Seckel, Jorge Torres, Simona Toscano, Nick vanEijndhoven, Abigail Vieregg, Christoph Welling, Tobias Winchen, Stephanie A. Wissel
European Physics Journal C 80, 77 (2020) arXiv:1906.01670+NuRadioReco: A reconstruction framework for radio neutrino detectors
C. Glaser, A. Nelles, I. Plaisier, C. Welling et al., Eur. Phys. J. C (2019) 79: 464
36

Chris&an Glaser, Chiba, October2020

NuRadioMC Overview§ Modular python code (C++ modules for time critical operations)§ Open source: github.com/nu-radio/NuRadioMC§ Community wide effort (InIceMC group)

EventGeneration§ Cross sec;on§ Flavor-ra;o§ Arrival direc;on
§ …

wen37

multiple interactions
e.g. tau decaysinterference between
showers

Chris&an Glaser, Chiba, October2020

SignalGeneration

Signal
Propaga,onDetector
Simulation§ Phase andfrequency§ LPM eﬀect§ …

§ Ice models§ (analytic) raytracing§ …

§ Frequency and phase
response§ Flexible station layout§ Trigger simulation§ …

time domain calculation
with realistic LPM

fast + precise analy;cray tracer

NuRadioReco:
Detector simulation andevent reconstruction

Event Generation§ HDF5 input file
§ List of§ shower direction§ shower energy§ shower position§ Easy to write custom event generator for e.g.
§ BSM physics§ monopoles§ calibration measurements

38

Chris&an Glaser, Chiba, October2020

Simula+on of secondary leptons: Tau decays

39

Chris&an Glaser, Chiba, October2020

generalization: Integration of PROPSAL
for lepton propagation

D. Garcia, C. Glaser, A. Nelles, Phys. Rev. D 102, 083011 (2020)

Possible event signature

40

Chris&an Glaser, Chiba, October2020

D. Garcia, C. Glaser, A. Nelles, Phys. Rev. D 102, 083011 (2020)

Lepton propaga+on through ice using PROPOSAL§ muons/taus stochasticallyloose energy§ inducing many showers along
their trajectory§ Example plot:§ 1 EeV muon propagation
almost horizontally throughthe ice§ Askaryan signal of eachshower in fiducial simulation
volume is calculated andpropagated to antennas

41

Chris&an Glaser, Chiba, October2020

D. Garcia, C. Glaser, A. Nelles, Phys. Rev. D 102, 083011 (2020)

First Lepton Results
Tau neutrino eﬀec0ve volume42

Chris&an Glaser, Chiba, October2020

Background from atmospheric neutrinos

Signal Generation§ Well tested reference implantation of all available models

43

Chris&an Glaser, Chiba, October2020

ARZ

Alvarez-Muñiz et al., Phys. Rev. D 101, 083005

5me domain calcula5on based on charge-excess shower library

44

Chris&an Glaser, Chiba, October2020

ARZ

Alvarez-Muñiz et al., Phys. Rev. D 101, 083005

time domain calculation based on charge-excess shower library

45

Chris&an Glaser, Chiba, October2020

ARZ

Alvarez-Muñiz et al., Phys. Rev. D 101, 083005

time domain calculation based on charge-excess shower library46

Chris&an Glaser, Chiba, October2020

Signal Propaga+on§ Analytic formula of signal path for exponential density profile§ Fast and precise calculation of signalpaths§ Analytic formulas for travel time+ distance§ Attenuation requires numericalintegration§ C++ implementation§ Interface to RadioPropa
47

Chris&an Glaser, Chiba, October2020

Detector Simulation§ NuRadioReco: Detector simulation and event reconstruction§ github.com/nu-radio/NuRadioReco§ Glaser et al., EPJC 79: 464 (2019) arXiv:1903.07023§ Flexible detector layout§ any antenna position and orientation§ Modular design

48

Chris&an Glaser, Chiba, October2020

Example 1: Calculation of the sensitivity of an Askaryan
neutrino detector
detector description

49

Chris&an Glaser, Chiba, October2020

configDetector simulation

50

Chris&an Glaser, Chiba, October2020

Results§ Full example: h\ps://github.com/nu-radio/NuRadioMC/wiki/Tutorial§ Plodng scripts part of NuRadioMC

51

Chris&an Glaser, Chiba, October2020

Debug Plots

52

Chris&an Glaser, Chiba, October2020

How to get started§ Tutorial: https://github.com/nu-radio/NuRadioMC/wiki/Tutorial§ Webinar on NuRadioMC/Reco§ https://www-zeuthen.desy.de/~anelles/NuRadioMC.mp4§ https://www-zeuthen.desy.de/~anelles/NuRadioReco.mp4§ https://github.com/nu-radio/NuRadioMC/tree/master/NuRadioMC/examples/06_webinar§ NuRadioMC paper: https://link.springer.com/article/10.1140/epjc/s10052-0207612-8§ NuRadioReco paper: https://link.springer.com/article/10.1140/epjc/s10052-0196971-5§ NuRadioMC slack channel: https://join.slack.com/t/nu-radio/shared_invite/zt5f9vka05-kYx3cw743Y7QxM4BOSV8dw

53

Chris&an Glaser, Chiba, October2020