Beyond Standard Model
Physics with IceCube
Anna Pollmann

South Pole
IceTop Array
81 stations

IceCubeIceCube Laboratory

Working principle•Particles interact with the deepclear ice•
Emitted light is detected bysensors

1450m –

InIce Array
86 strings,
each with 60
optical sensors

2450m –

anna.pollmann@uni-wuppertal.de22

South Pole
IceTop Array
81 stations

IceCubeIceCube Laboratory

Working principle•
Particles interact with the deepclear ice•
Emitted light is detected bysensors
Digital Optical
Module (DOM)
1450m –Readout
electronics

InIce Array
86 strings,
each with 60optical sensors

Photomultiplier

2450m –anna.pollmann@uni-wuppertal.de22Particle types in IceCube
Atmospheric Muons (~108 per day)•cosmic HE particles interact withatmosphere (cosmic ray)•a particle shower develops through theatmosphere (air shower)•
muons reach IceCube

atmospheric μ
cosmic ray
3

Particle types in IceCube
Atmospheric Muons (~108 per day)•cosmic HE particles interact withatmosphere (cosmic ray)•a particle shower develops through theatmosphere (air shower)•
muons reach IceCube
Atmospheric Neutrinos (~200 per day)•cosmic ray induces air shower•
neutrino is created in shower•
neutrino interacts in Earth or ice•
visible muon or shower in IceCube•
energy threshold ~10 GeV

cosmic ray

atmospheric ν

atmospheric μ
cosmic ray
3

Particle types in IceCube
Atmospheric Muons (~108 per day)•cosmic HE particles interact withatmosphere (cosmic ray)•a particle shower develops through theatmosphere (air shower)•muons reach IceCube
Atmospheric Neutrinos (~200 per day)•cosmic ray induces air shower•
neutrino is created in shower•
neutrino interacts in Earth or ice•
visible muon or shower in IceCube•
energy threshold ~10 GeV

Astrophysical Neutrinos (~10 per year)•neutrino from outer space passes
through Earth•neutrino interacts in Earth or ice•
visible muon or shower in IceCube

cosmic ray

astrophysical ν

atmospheric ν

atmospheric μ
cosmic ray3

Outline•

Introduction of IceCube•

Beyond Standard Model physics with IceCube- Direct detection of exotic particles‣ Standard detection channels‣ Development of new detection channels- Development of new detector modules

4Beyond Standard Model physics with IceCube
Indirect detection
••

•

•

exotic source of particles
contributes to particle flux
exotic interactions/particles
contribute to propagationof particle fluxes

Direct detection••

exotic particle (or interactionsecondary) passes throughthe detector
often distinct event signature
expected

unexpected particle
properties at
unprecedentedly highenergies
different fundamental lawsof physics appear at longscales

5Relic Magnetic Monopoles•

elemental magnetic charge (Dirac)
gD = e / 2 α ≈ 68.5 e•with huge mass created•-shortly after the Big Bang (GUT)1013 GeV ≦ MMM ≦ 1019 GeV-in intermediate stages of symmetry
breaking (IMM)
107 GeV ≦ MMM ≦ 1013 GeV

acceleration in magnetic fields forMMM ≦ 1014 GeV to Ekin ≦ 1015 GeV•trapping around galaxy, sun, Earthv ~ 10-3 / 10-4 / 10-5 c
Gluesenkamp ´10anna.pollmann@uni-wuppertal.de6

Light production in water-Cherenkov telescopes
Relativistic speeds•
Continuous light emission- Cherenkov Lightrofdila- Cherenkov light from also v ardStandsecondariesledoM•
Stochastic lossesselcitr
pa- Bremsstrahlung- Pair production- Photonuclear interactions

Cherenkov light emission pattern

Monopole light yield

directtecr
idni

particlematterphotons7

Light production in water-Cherenkov telescopes
exotic scenarios

Slow speeds•
catalysis of proton decay•
thermal shock waves (not used yet)Monopole light yieldmodel dependent

Light emission from proton decay
photons

oninotprdirectdirect➡

yca

demonopoleatom

8Signatures of fast Magnetic Monopoles
Background

Magnetic Monopolesmuonbundles fromair showers

0.50 cneutrinos

0.8 ccoincident
eventsColor ≙ time (red -> blue)
Size ≙ light amount

EPJ C76 (2016) 1339

Mapping the parameter space of Magnetic Monopoles

PRELIMINARY

Catalysis ofproton decay

Indirect
Cherenkov
radiation

DirectCherenkov
radiation

EPJ C76 (2016) 133 &EPJ C74 (2014) 2938 10

Mapping the parameter space of Magnetic Monopoles

No sensitivity withrecent detectors yet
PRELIMINARY

Catalysis ofproton decay

Luminescence

Indirect
Cherenkov
radiation

DirectCherenkov
radiation

EPJ C76 (2016) 133 &EPJ C74 (2014) 2938 10

Light production by (exotic) particles in water and ice
Relativistic speeds•
continuous lightemission•
stochastic losses

Intermediate speed➡ not covered yet

Idea: Luminescence light•ionising radiation passes throughmatter•it excites atoms/molecules•
relaxation with light emission‣‣

Slow particle speed (< 0.1 c)•catalysis of proton decay•
thermal shock waves

Luminescence light emission patternparticleworks for all speeds
works for all ionising particles

Light yield defines detectability!

matterlight11

Luminescence light measurement
Characterisation via•
light yield•decay kinetics•
emission spectrum•
quenching

Few existing measurementswith very different setups and results

Dependencies•
temperature•
impurities / solubles•
radiation type•pressure

Note:•sample quality varies significantly
between measurements•
different radiation causes different
amount of quenching12

Luminescence light measurement

rect
ditlumdirececnec
ines

onot
pr

Dependencies•
temperature•
impurities / solubles•
radiation type•pressureFew existing measurementswith very different setups and resultsin

Characterisation via•
light yield•decay kinetics•
emission spectrum•
quenchingyca

deNote:•sample quality varies significantly
between measurements•
different radiation causes different
amount of quenching12

Laboratory measurements
•

•

•

•

•

ultra-purified water degassed in
vacuum (frozen to bubble free ice)induced luminescence light with
α-particles from 241Am
measured single photons withphotomultiplierprobed background (temperaturedependent)
calibrated & calculated optics

temperature
peraturegauge

over cup

photomultiplier

photomultiplier
α-source
source atfrozen
ultra-purified
ice
into ice surface

arxiv:1710.01197 13

Previous light yield measurements

Note:•sample quality varies significantly
between measurements•
different radiation causes different
amount of quenching

Comment:•
uncertainties of new laboratory
measurement originates from water quality•”Trofimenko” is the only in-situ
measurement, all others use cleaned water
arxiv:1710.01197 14

Previous light yield measurements
First laboratory measurement at temperatures of neutrino telescopes

Note:•sample quality varies significantly
between measurements•
different radiation causes different
amount of quenching

Comment:•
uncertainties of new laboratory
measurement originates from water quality•”Trofimenko” is the only in-situ
measurement, all others use cleaned water
arxiv:1710.01197 14

South Pole

Neutrino Observatory

Boreholet

650 m 350 m

Ice layer til

SPICEcore borehole•
filled with anti-freeze / drilling grease (Estisol)•measurements in 2018 / 201915

anna.pollmann@uni-wuppertal.de∅ 12,7 cm

IceCubeSPICEcore

1.5 km

1 km

1.75 km

Antarctica

South PoleAntarctica

1 km

SPICEcore
Boreholet

650 m 350 m

Ice layer til

SPICEcore borehole•
filled with anti-freeze / drilling grease (Estisol)•measurements in 2018 / 201915

anna.pollmann@uni-wuppertal.de∅ 12,7 cm

Neutrino Observatory

1.75 km

IceCube1.5 km

Setup
Winch tower
DeviceHole
Bottom Camera @ 114m

Luminescence Logger
Goal•

ElectronicBoard

irradiate ice with β-source andmeasure back-scattered light

MiniOscilloscope

Method••press source against ice
guide scattered light onto
photomultiplier

SideCamera

Details•diameter: max 92 mm•

length: 1.30 m

Mirrorcommercial mini USBoscilloscope for readout

Photomultiplier

•

•

•

light detection withphotomultiplier tube

Low
temperature
Batteries

several sensors: i.e.
temperature, gyro,
IR camera
16

BottomCameraLuminescence Logger
Goal•

irradiate ice with β-source andmeasure back-scattered lightMethod••

press source against ice•

diameter: max 92 mm•

length: 1.30 m••

Spring& wire

guide scattered light onto
photomultiplier

Details•

Motor &Slow control

commercial mini USBoscilloscope for readoutMiniOscilloscope

SideCamera

Magnets
36Cl-Mirror

SourcePhotomultiplier

light detection withphotomultiplier tube
several sensors: i.e.
temperature, gyro,IR camera

ElectronicBoard

Low
temperature
Batteries

Photomultiplier
16

BottomCameraLuminescence Logger
Goal•

irradiate ice with β-source andmeasure back-scattered light

Method••press source against ice•

diameter: max 92 mm•

length: 1.30 m••

Spring& wire

guide scattered light onto
photomultiplier

Details•

Motor &Slow control

commercial mini USBoscilloscope for readout

MiniOscilloscope

SideCamera

Magnets
36Cl-Mirror

SourcePhotomultiplier

light detection withphotomultiplier tube
several sensors: i.e.
temperature, gyro,IR camera

ElectronicBoard

Low
temperature
Batteries

Photomultiplier
16

BottomCameraResults: Luminescence light measurement

arXiv:1908.07231

17Results: Luminescence light measurement

arXiv:1908.07231
Decay times
2.44 ± 2.07 ns
196.1 ± 39.1 ns
5.03 ± 0.06 μs
56.1 ± 6.29 μs
17Results: Luminescence light measurement

arXiv:1908.07231
Decay times

Publication under preparation
Spectrum of luminescence

2.44 ± 2.07 ns
196.1 ± 39.1 ns
5.03 ± 0.06 μs
56.1 ± 6.29 μs
17Applications of ice luminescence••••searches for exotic particles incl. neutral particles
calibration of ultra high energy neutrinos
particle identification
ice classification on icy moons in the solar system
Magnetic monopole exclusion limits
1yMonopole
0.30 cQ-ball0.001 c,
Z=13718

IceCube Upgrade(construction end 2022)

IceCube Gen2
(starting ~2025)

Towards more sensitive & larger particle detectors
mDOM: new detector module for
the Upgrade (2022)•
24 instead of 1 PMT•
better signal/noise ratio•
directional sensitivity•
450 modules to be build in Berlinand Michigan

Mechanical integration•
low coverage of sensors•
safety at extreme environment
Current status:- prototype reviewed- test productionof 10 modules

20Towards more sensitive & larger particle detectors
WOM: new detector module for
the Generation 2 (>2025)•
1 prototype on its way to theocean network canada (ONC)•
15 modules for the Upgrade2022•
O(1000) modules for Generation
2 >2025

Prototype for ONC
Electronics based on logger21

Towards more sensitive & larger particle detectors
WOM: new detector module for
the Generation 2 (>2025)•
1 prototype on its way to theocean network canada (ONC)•15 modules for the Upgrade2022•
O(1000) modules
for Generation 2>2025

Physics to improve sensor

Tasks (Sept. 2021)•overall mechanicalintegration•pressure vessel•
electronics development•
calibration (with others)•production (with others)

22

Back to beyond standard model physics

••

•

•

fractionally charged particles
Q-balls (via standard methods andusing luminescence)nuclearites (via thermal shocks,maybe experiments needed)… and many more

23

Back to beyond standard model physics

••

•

•

fractionally charged particles
Q-balls (via standard methods andusing luminescence)nuclearites (via thermal shocks,maybe experiments needed)… and many more

23

Summary•••large neutrino
detectors aresensitive to any
ionising particles
large detection volume
facilitates unprecedented
sensitivities to new physics
many channels to probe new physics➡ Lots to discover!

anna.pollmann@uni-wuppertal.deBackup25Dark Matter annihilation and decay
TeV WIMP increasingly disfavoured due to non observation at LHC/elsewhere
Search for annihilation / decay of DM in•
galactic DM (anisotropic)•
extra-galactic DM (isotropic, red shifted)
Decay

Annihilation

heavy Spin-0 particle annihilates into SM
particles such as mono-energetic neutrinos

heavy DM decays into SM particles (directlyor indirectly) with neutrinos in final state

Neutrino 2018 & arxiv:1804.03848 & 1705.08103 26

Beyond Standard Model physics with IceCube
Indirect detection••••exotic source of particles
contributes to particle flux
exotic interactions/partices
contribute to propagationof particle fluxes

Exlep
am

Neutrino crosssection•

atmospheric neutrinos passdifferent lengths of Earth~ different amount of matter

unexpected particle
properties atunprecedentedly highenergies
different fundamental lawsof physics appear at longscales
Nature 551 (2017) 596-600

27

Neutrino oscillation
Strategy•
atmospheric neutrinos from a wide range of baselines (~angles)•energies: few GeV to 100 TeV
Event histogram
Model expectation

νμ enriched sample

IceCubesensitive
νμ disappearanceντ disappearance
mass ordering

matter resonances

vacuum dominatedνμ disappearance(less up-goingtrack-like events)

Phys. Rev. Lett. 120, 071801 (2018) 28

Neutrino oscillation
Strategy•
atmospheric neutrinos from a wide range of baselines (~angles)•energies: few GeV to 100 TeV
Event histogram
Model expectation

νμ enriched sample

IceCubesensitive
νμ disappearanceντ disappearance
mass ordering

matter resonances

vacuum dominatedνμ disappearance(less up-goingtrack-like events)

Phys. Rev. Lett. 120, 071801 (2018) 28

Neutrino oscillation
Strategy•
atmospheric neutrinos from a wide range of baselines (~angles)•energies: few GeV to 100 TeV
Event histogram
Model expectation

νμ enriched sample

IceCubesensitiveνμ disappearanceντ disappearance
mass ordering

matter resonances

vacuum dominatedνμ disappearance(less up-goingtrack-like events)

Phys. Rev. Lett. 120, 071801 (2018) 28

Neutrino oscillation
Strategy•
atmospheric neutrinos from a wide
range of baselines (~angles)•energies: few GeV to 100 TeV•
distinctive pattern in energy / angle /particle ID histograms
Recent result•
improved handlingof systematics•
MC driven backgroundhandling•
consistent with previous
IceCube / long baseline
experiments within
statistical uncertainties(shift due to statisticalfluctuations)•maximal mixing preferred
Phys. Rev. D 99, 032007 (2019) 29

Sterile neutrinos
Strategy•for Δm241 ~ 1 eV2 sterile neutrino
states produce a change in thematter potential

passinghole Earth:cosθ=-1

Phys. Rev. D95, 112002 (2017) 30

Non-standard neutrino interactions
Strategy•
additional potential by nonstandard neutrino interactions
changes oscillation pattern

Phys. Rev. D 97, 072009 (2018) 31

Lorentz Invariance Violation
Strategy•
atmospheric neutrino sample•
Standard Model extension describes
different LIV effects as operators ofdifferent dimension•
these change the neutrino oscillation
probability•
signal: anomalous muon neutrino
disappearance•
using 30k > TeV scale muon neutrinos•
result: best limits on LIV for higher
dimensions

6
anna.pollmann@uni-wuppertal.de7

8
arXiv:1709.03434 32

Sterile neutrinos at high energies
Strategy•for Δm241 ~ 1 eV2 sterile neutrino
states try to identify the resonant
oscillation from νμ into νs

Phys. Rev. Lett. 117, 071801 (2016) 33

Sensitivity for Fractional Charges

Erlangen, ECAP-Seminar 01/201
9anna.pollmann@uni-wuppertal.deK. Helbing, Wuppertal - IceCube3448