Observations of Atmospheric Neutrinos Importance in Particle and Astroparticle Physics
Antoine Kouchner
University Paris 7 Diderot- AstroParticle and Cosmology
Multiple Messengers and Challenges in Astroparticle Physics” GSSI, october 6-17, 2014
Focus on: • the Neutrino Mass Hierarchy • Next Generation Detectors Biases toward: • Cherenkov Techniques
Feel free to interrupt me!
Atmospheric Neutrino Connection
Cosmic-ray Induced particle physics
Particle physics Astroparticle
physics
Strong connection
Atmospheric neutrinos
Accelerator based
neutrino physics
Neutrino astronomy
I will focus on atmospheric neutrinos, but the link with particle physics and astroparticle physics is obvious through the detectors themselves. These detectors can also probe:
Nucleon decays Cosmic neutrinos Indirect search for dark matter
Accelerator neutrinos Monopoles …
2
Neutrinos 3
Introduction
Historical aspects
Atmospheric Neutrinos
The Atmospheric sector
Measuring the Neutrino Mass Hierarchy with Atmospheric Neutrinos
Current Knowledge on Neutrino Mixing
Phenomenological considerations
Detectors (mostly future project)
Water/Ice Cherenkov
Magnetized Trackers
Liquid Argon TPCs
High Energy Atmospheric Neutrinos
Spectrum measurement
Prompt component
Outline 4
Covered by T. Gaisser & F Halzen + WG discussion.
First atmospheric neutrinos
Physics Letters 18, (1965) 196, dated 15th Aug 1965 PRL 15, (1965), 429, dated 30th Aug. 1965
Kol
ar�G
old�F
ield
Eas
t R
and g
old m
ine
5
The first neutrino skymap?
Link to AstroParticle Physics
Link to Particle Physics
One of the main motivations: cross-section and mass of W propagator. Does the neutrino cross section saturate >1 GeV?
Mw
Predictions Halprin and Oakes 1978
6
First atmospheric neutrinos
First atmospheric neutrinos
Was the deficit due to oscillations? Or instrumental artifact?
7
Oscillation’s basic
Mixing in the
leptonic sector (θ)
Non-degenerate mass
spectrum (Δm2)
Oscillation Probability
P=ƒ(θ,Δm2)
Quantum interference
(macroscopic)
UPMNS matrix
(à la CKM)
⊕ ! =!
8
9
Experimental setup
P(Lo,ΔΕ)→ƒ(θ,Δm2)
theory!experiment!
rate & shape!(if resolution)!
rate only!
What is measured?
Source is far ! large statistics implies
large detectors
L not accurately known ! Not ultimate measurement
of Δm2
If Energy small ! Average measurement
9
Atmospheric neutrinos
~1 particle/(cm2 sec sr)
10
Flux predictions
" P. Lipari, Introduction to Neutrino Physics
Rely on a mix of measurements and MC techniques. Many ingredients in the simulation:
µµ νννν+
+= eeR
Absolute neutrino flux 20-30% uncertainties
⇓ Measure Up/Down &
Up/down symmetry if No oscillation
No Earth magnetic field No relief
11
Flux predictions
" P. Lipari, Introduction to Neutrino Physics
Rely on mix of measurements and MC techniques. Many ingredients in the simulation:
pp cross section versus center of mass energy. Average number of charged hadrons produced in pp collisions versus center of mass energy
Link to Particle Physics Accelerator ! Recent LHC data
12
Flux predictions
" P. Lipari, Introduction to Neutrino Physics
Rely on mix of measurements and MC techniques. Many ingredients in the simulation:
• high precision 3D calculations, • refined geomagnetic cut-off treatment (also geomagnetic field in atmosphere) • elevation models of the Earth • different atmospheric profiles • Detector’ environment (mountain)
13
Flux predictions
Remaining uncertainties ? Normalisation
Shape
INO site
" M.S. Athar et al. arXiv:1210.5154
Honda et al. ICRC2007
WG discussion item?
14
Nucleon decay detectors ! At the beginning of the ’80s, some theories (GUT) predicted the proton
decay with measurable livetime
! Detector size: 103 m3, and mass 1kt (=1031 p target)
! The main background for the detection of proton decay were atmospheric neutrinos interacting inside the experiment
# Water Cerenkov Experiments (IMB, Kamiokande) Kamioka Nucleon Decay Experiment Super-Kamioka Neutrino Detection Experiment # Tracking calorimeters (NUSEX, Frejus, KGF) # Result: NO proton decay ! (Some GUT ruled out) But some anomalies on the neutrino measurement!
15
Kamiokande results " Y. Fukuda et al., Phys. Lett. B335, 237 (1994).
4.5 kton detector
16
SuperKamiokande νµ
atmospheric ν results
GeV νatm & the imaging Cherenkov technique
Position & angular reconstruction
PID: separate νµ from νe
Record PMT charge and timing
µ
17
SK results 1998
The announcement of the discovery* of neutrino oscillation at Neutrino 98 by T. Kajita. * What about solar neutrinos?
" P
hys
.Rev
.Let
t.81:1
562-1
567,1
998
18
Consequences ? 19
! Atmospheric Neutrino Oscillations ! we ‘see’ the oscillation
! ! Credit to the oscillation solution to the solar anomaly
! Dramatic consequences in astroparticle physics
! MSW effect in the Sun, in Supernovae
! Oscillation of cosmic neutrinos
! But no Nobel Prize for oscillation
MACRO experiment Main features of Macro as ν detector
• Large acceptance (~10000 m2sr for an isotropic flux)
• Low downgoing µ rate (~10-6 of the surface rate )
• ~600 tons of liquid scintillator to measure T.O.F. (time resolution ~500psec)
• ~20000 m2 of streamer tubes (3cm cells) for tracking (angular resolution < 1° )
More details in Nucl. Inst. and Meth. A324 (1993) 337.
Data taking period: 1989 – 1994 construction 1994 – 2000 full
"Physics Letters B 434 1998. 451–457
20
SOUDAN II experiment
Soudan Mine Northern Minnesota 2100 mwe depth 963 t iron-tracking calorimeter Proportional counters veto shield • Single track event with a dE/dX compatible with a muon ( νµ CC) • Single shower events (νe CC)
224 calorimeter modules
νe νµ $
Ear
l A
Pet
erso
n –
Neu
trin
o 98
21
Situation circa 2002
End of the calorimetric tracking device (FREJUS, NUSEX) vs Cherenkov devices (SK, IMB) controversy. Further confirmation with Long BaseLine accelerator experiments. ! Exploring the atmospheric sector
22
LBL & the atmospheric sector det km GeV start
Japan KEK K2K SuperK 250 1.4 1999
Japan Tokai T2K SuperK 290 1.5 (on) 2009
US NuMI Soudan MINOS 730 17 2005
US NuMI Ash River NovA 810 2 (off) 2014
EU CERN GS Opera 732 17 2006
Sensitivity Δm2 > 10-3 eV2
23
Observation of tau neutrinos 24
SK: Evidence for appearance of τ neutrinos
" Phys. Rev. Lett. 110, 181802 (2013)
Signal: extra pions from tau decay ! More spherically symmetric ! Analysis based on Neural Network ! Maximum likelihood fit
Should allow for studies of ντ interaction physics with oscillation produced ντ
22,5 kt – 2806 days
25
Introduction
Historical aspects
Atmospheric Neutrinos
The Atmospheric sector
Measuring the Neutrino Mass Hierarchy with Atmospheric Neutrinos
Current Knowledge on Neutrino Mixing
Phenomenological considerations
Detectors (mostly future project)
Water/Ice Cherenkov
Magnetized Trackers
Liquid Argon TPCs
High Energy Atmospheric Neutrinos
Spectrum measurement
Prompt component
Outline 26
Covered by T. Gaisser & F Halzen + WG discussion.
Massive neutrinos • Neutrinos have distinct masses => why so light?
• Often considered as first evidence of physics beyond the Standard Model. Are neutrinos fundamentally different from other particles? • Neutrinos mix like quarks ⟹ why so similar/different?
Ue3 = sinθ13 e-iδ$UPMNS! UCKM!
27
Oscillations of Massive Neutrinos
Atmospheric θA~45°
Reactor θ13~9°
$%CP violating phase δCP
Solar θ&~30°
Majorana
28
All parameters measured to fair precision except: mass hierarchy octant of θ23
CP phase
Current Status of unknowns E. Li
si, La
rge
Neu
trin
o In
fras
truct
ure
, P
aris
, Ju
ne
2014
29
Why knowing the mass hierarchy? • Help measuring the CP phase • Absolute mass scale • Nature (Dirac vs Majorana) • Origin of neutrino mass and flavor • Core-Collapse Supernovae Physics
Walter Winter Neutrino 2014
WG discussion item
Impact of direct mass ordering measurement
30
! « Standard approach » :probe νµ νe governed by Δm231
! Insensitive to the sign of Δm213 at leading order.
! Matter effects (MSW) come to the rescue
! Earth density variations (e.g. mantle-core) also affect the oscillations (parametric resonance)
[Neglecting solar (> a few GeV and >1000’s km) and CP violation effects]
Through matter, neutrinos interact acquiring an effective mass (forward scattering) Only electron neutrinos interact through CC with electrons ! Additional potential A in the Hamiltonian
m!m!
! Modify the oscillation probability
(�)+ for (anti-)neutrinos
MH with LBL experiments 31
Matter resonance: A ' Δ13cos2θ13 - Effective mixing maximal - Effective osc. frequency minimal
Resonance energy Earth: - Mantle Eres ~ 7 GeV - Core Eres ~ 3 GeV
Same signs
Opposite signs
Requirements: • Δ13 ~ A matter potential must be significant but not overwhelming • L large enough – matter effects are absent near the origin • Distinction between neutrinos and anti-neutrinos
! different flux and cross-sections!
(Constant Density) Matter Effects 32
Phenomenological Summary
cosθ = �1 Inverted Hierachy
Normal Hierachy
In each case, CP-phase is varied in steps of 30 degrees
cosθ = �0.6
• Hierarchy differences disappear at around 15 GeV
• P(νµ!νe) < 2% at 20 GeV
GLoBES
GLoBES
P(νµ! νµ), NH
33
Phenomenological Summary
cosθ = �1 Inverted Hierachy
Normal Hierachy
In each case, CP-phase is varied in steps of 30 degrees
cosθ = �0.6
• Hierarchy differences disappear at around 15 GeV
• P(νµ!νe) < 2% at 20 GeV
GLoBES
GLoBES
Degeneracies due to parameter uncertainties must be carefully considered!
cosθ = �0.6
34
Muon versus Electron channels " Agarwalla et al. arXiv:1212.2238
±10% Earth density
Muons provide more statistics Electron channel is more robust against detector resolutions… Brings additional sensitivity to the mass hierarchy Lately considered by PINGU and ORCA while main channel for HK
" Honda et al. PRD 83:123001,2011
“Screening effect” r~2 & sin2θ23~0.5
But enhancement possible: - r increases with energy - Larger effect for second octant
35
Fluxes and cross sections
σ/Ε
(10
-38 G
eV-1
cm
-2)
! Use external measurements and regions without oscillations
Different cross sections for ν and ν !$ Three main contributions: Quasi-elastic, Resonant, DIS
σ (ν ) ≈ 2σ (ν )
cosθ = �0.6
φ x
E-2
(GeV
cm
-1 s
r-1 s
-1)
" M.S. Athar et al. arXiv:1210.5154
Calculations now
made as a function of the position on Earth and the time
in year
x
" Kajita, New J. Phys. 6 (2004) 194
x
A beam for free !
• Produce neutrinos and anti-neutrinos • Broad energy range: Steeply falling spectrum
! Requires good energy resolution • Broad path-length range
! Requires good direction resolution
36
WG discussion item
" Akhmedov et al. JHEP 02 (2013) 082 With exceedingly large PINGU effective volume
Uncorrelated systematics
S=45.5σ (f=0%) S=28.9σ (f=5%) S=18.8σ (f=10%)
In 5 years
Oscillograms & sensitivity for NT
Perfect resolutions
S=7.2σ (f=0%) S=4.5σ (f=5%) S=3.0σ (f=10%)
σE=4 GeV, σθ= 22.5°
37
Introduction
Historical aspects
Atmospheric Neutrinos
The Atmospheric sector
Measuring the Neutrino Mass Hierarchy with Atmospheric Neutrinos
Current Knowledge on Neutrino Mixing
Phenomenological considerations
Detectors (mostly future project)
Water/Ice Cherenkov
Magnetized Trackers
Liquid Argon TPCs
High Energy Atmospheric Neutrinos
Spectrum measurement
Prompt component
Outline 38
Covered by T. Gaisser & F Halzen + WG discussion.
First achievements with Neutrino Telescopes
450 m
40 km Off Shore, French Riviera
12 line detector completed 2008
Oscillations maximal at 24 GeV for vertical neutrinos (muon range~120m) Larger effect on
low energy than
higher energy events
South Pole
IceCube (86 strings)+ DeepCore (8 strings)
Single lines
Multi lines
DeepCore
IceCube
" Phys. Lett. B 714 (2012) 22. " Phys. Rev. Lett. 111, 081801 (2013)
39
First achievements with Neutrino Telescopes
MC truth
2008-2010 data (863 days)
No oscill Oscill
IC79 data (319 days)
All results statistically limited
Other analyses have been recently presented
40
Latest results with DeepCore
J. Koskinen , NOW14
41
Latest results with DeepCore
IceCube now competes with SK and LBL experiments !
Great confidence for next steps
42
Proposed Low Energy Extensions
450 m
ORCA*
115 lines, 20m spaced, 18 OM/line 6m spaced
Instrumented volume ~3.8 Mt, 2070 OM
40 strings, 20-25m spaced, 96 OM/string 3m spaced
Instrumented volume ~ 6 Mt, 3840 OM
" S. Galata et al, VHEPU 2014 " A. Gross et al, ICRC13 proc 0555
PINGU#
Optimized layouts still under study
*First performances evaluated with a 50 string detector
43
31 3” PMTs " arXiv:1405.0839
#First performances evaluated 60 OMs/string
KM3NeT already taking data from an ANTARES line since April 2013
… and sees muons!
Coincidence in a DOM $
hits in different PMTs in a time window of 20ns
PMT down-looking PMT up-looking
Ncoinc θPMT (deg)
Events with Ncoinc>6 selected
PRELIMINARY PRELIMINARY
In situ tests of new Optical Module
" KM3NeT, arXiv:1405.0839
44
Event topologies
Track-like
Shower-like
45
Track-like contains both a cascade and one track
No track is identified
Not to scale
Preliminary performances (νµ)
450 m Water is a better tracker
Estimated with µ path length Should be improved
46
Preliminary performances (νe)
450 m
Water is a better tracker
47
Sensitivity studies To optimally distinguish between IH and NH: likelihood ratio test with nuisance parameters → deal with degeneracies by fitting!
LLR used to check FIM approach
1) fit mixing parameters assuming NH 2) fit mixing parameters assuming IH 3) compute ΔlogL = log( L(NH)/L(IH) ) θ23 , Δm2 and δCP can be fitted from data.
48
Current Sensitivities
Tracks Cascades
Combined
Quite similar results Both collaboration currently investigating details
Preliminary PiD included
49
Further on-going studies ( Reconstruction
“With the inelasticity, the total significance of establishing mass hierarchy may increase by
(20 - 50)%” " Ribordy & Smirnov arXiv:1303.0758v1
Try to separate track-like (ν) to shower-like events (ν)
( Atmospheric muons
Can use Veto from IceCube/Deepcore In addition to quality cuts
( Inelasticity
Neutrinos Eν<20 GeV Muons (all energies)
No need for veto
Cut on reconstructed
vertex
Investigate sensitivity to Bjorken y
50
Studies of systematics
Earth Model Almost negligible impact
Atmospheric neutrinos flux • Shape • Normalization Large impact but normalization from data
Moderate impact
PMNS uncertainties
Several other studies point to the same conclusions e.g " W. Winter, Physical Review D, vol. 88, Issue 1, id. 013013 + PINGU LoI
" D. Franco et al, JHEP 04 (2013) 008
Method: extended unbinned log-likelihood ratio
Negligible impact varying combinations of {θ12, Δm221} (± 1σ)
Large impact varying combinations of {θ13, θ23, Δm231} (± 1σ)
Small impact varying CP phase
51
Project timelines Both project are subject to funding approval
Similar timelines
“Detector construction can be completed five years after funding starts, or as early as 2020.” “The PINGU share of the facility cost is roughly $55M (US cost, including contingency) plus $25M (foreign contribution) for a total of 80M$.” " arXiv:1409.5755v2 P5 report: “[…]cannot go forward as major projects at this time, due to concept maturity and/or program cost considerations. However, further development of PINGU is recommended […]” “…we encourage continued work to understand systematics. PINGU could play a very important role as part of a larger upgrade of IceCube, or as a separate upgrade, but more work is required.”
ORCA is part of the KM3NeT program A Possible scenario, subject to collaboration approval: Phase 1 (funded) : deploy a 6-7 string array In the ORCA configuration to demonstrate detection method in the GeV range. Phase 2 (40 M€) : deploy 1 building block 115 strings. Completion in 2019
52
Neutrino beam to PINGU/ORCA?
" Lujan-Peschard et al, Eur. Phys. J. C (2013) 73:2439 ; Tang & Winter, JHEP 1202 (2012) 028
• Muon counting experiment - Optimum 6-8 GeV 6000-8000 km but beam inclination
1 Mt mass
! 9 σ separation on purely statistical ground in one year
• Electron counting experiment - Protvino-ORCA L=2588 km, beam inclined by 11.7° " J. Brunner, AHEP, Volume 2013 (2013), Article ID 782538.
1021 pot -- 3 years 7 σ stat. separation 3 σ with 3-4% sys
No need for
energy reconstruction
53
CP band 2nd octant
1st octant
NH
IH
CP band
Globes
Prospects with HyperKamiokande
Proposal for ~500 kT multi-purpose Water Cherenkov facility 295 km from JPARC and 8km off from SK. 1750 mwe overburden.
• Well-known technology • Sensitive to νe and νµ (and ντ )$• Good control of systematics
Status: • Among top priorities in Japan (with ILC) : 800 M$ estimated cost (without beam) • If funded, access tunnel work should start in 2016 • Excavation works in 2018 • Detector operation in 2023
54
Prospect for the MH (atm)
After 10 years, determine MH at >3σ for values of sin2 θ23 > 0.4. Improved sensitivity is expected by adding beam data (>1σ sensitivity alone,
depending on δCP) ! >3σ in all cases.
Bands correspond to δCP range of
values NH IH
sin2 2θ13 =0.1 sin2 2θ13 =01
Ratio of oscillated νe rate over no oscillation case in sub-GeV and Multi-GeV channels. Statistical separation of νe and anti-νe.
" HK letter of Intent, arXiv:1109.3262v1
SK Sensitivity (σ)�
sin2θ23� now� +10 yrs�
0.4� 0.70� 0.98�
0.6� 1.50� 2.10 �
55
Prospects for θ23 octant and δCP
" From C. Walter, Neutrino Telescopes 2013
50% δCP fraction can be excluded at 3 σ after 10 yrs
Octant sensitivity 10 years of data
SK Sensitivity (σ)�
sin2θ23� now� +10 yrs�
0.4� 2.00 � 2.60�
0.6� 1.61� 2.10�
Bands correspond to δCP range of
values
With beam Atmospheric data
56
INO: India-based Neutrino Observatory
• 115 km west of Madurai (internat. airport) • Pottipuram Village, Theni District, Tamil Nadu State • 1.9 km access tunnel • Indian collab (~20 institutes) + Hawaii Univ (USA) • Several other experiments when operational (ββ0ν, DM)
50 kton ICAL (room for additional 50kton)
1 km
Current Status: • Fencing work started for facilities near portal and Madurai Center for HE Physics • Waiting for full project approval by Indian Government
22
The INO-ICAL detector
[NB: Slightly different numbers exist]
Construction of RPC
Pickup strips
2 mm thick spacer
Glass plates Resistive coating on the outer surfaces of glass
2m x 2m glass RPC test stand
Cosmic –ray tracks are
seen…
Current Status: • RPCs: help from Industry expected • Electronics: ASIC (2nd batch being tested) and DAQ under development
• Magnet: Prototype running at VECC Engineering module (800 ton) will be constructed by 2014.
23
Mass Hierarchy Discrimination
Further improvements expected by adding hadron events " arXiv:1306.1423v1
10 yrs 20 yrs
3σ$
INO + Other experiments " Ghosh, Thakore & Choubey, arXiv:1212.1305 " Blennow & Schwetz, JHEP 1208 (2012) 058,
Erratum-ibid. 1211 (2012) 098
Expected performances are a bit worse for IH
4σ$
10 yrs 20 yrs
INO only
INO + beams and reactors
24
The Liquid Ar TPC detectors
• First achievements with ICARUS (760 tons at LNGS) ! Proof of technology. • Excellent particle identification with low threshold (MeV)
• Atmospheric neutrino studies • Tau neutrino appearance • Discrimination between νµ!ντ and νµ!νs
from upward/downward asymmetry " A. Stahl et al, LBNO, SPSC-EOI-007 (2012)
• Proposed detectors (LBNO/E): staged approach up to 100 kton • Sensitive to muons and electrons • Hadronic component can me measured
70 m
20 m
25
Fiducial Exposure (kt-yrs)0 200 400 600 800
)2 χ∆√=
σSe
nsiti
vity
(
0
2
4
6 LAr Detector SimulationAtmospheric Neutrinos
Mass Hierarchy Determination
Normal HierarchyInverted Hierarchy
Input Parameters:π=CPδ=0.0242, 13θ2=0.4, sin23θ2sin
2eV-310×2.4±)=231m∆+2
32m∆1/2(
31
35 kt x 10 yrs = 350 kt-yrs
Mass hierarchy & octant with Lar TPCs
23θ2sin0.4 0.5 0.6
)2χ
∆√=σ
Sens
itivi
ty (
0
2
4
6
8Atmospheric Neutrinos
LAr Detector Simulation350 kt-yrs
σ3
Octant Determinationπ=CPδNormal Hierarchy,
=0CPδNormal Hierarchy, π=CPδInverted Hierarchy,
=0CPδInverted Hierarchy,
"LBNE arXiv:1307.7335
Requires very large detectors
Magnetized Lar TPCs ? => ~5σ (3σ ) with 250 kton.year exposure on MH (θ23) " V. Barger et al, Phys.Rev.Lett.109:091801,2012
Physics topics (with atmospheric ν) ! Current and future atmospheric detectors are also mentioned for:
! Sensitivity to CP phase (Threshold <1GeV, MH known)
! Earth tomography
! Test NSI and other exotic physics
! Sterile Neutrinos (Δm2 ~eV2 with TeV neutrinos)
" Arman Esmaili, Alexei Yu. Smirnov, arXiv:1307.6824v1 " Nunokawa et al, Phys.Lett. B562 (2003) 279-290
" Ohlsson et al, Phys. Rev. D 88 (2013) 013001 " Gonzales-Garcia et al., Phys.Rev. D71 (2005) 093010
" Gonzales-Garcia et al.,Phys.Rev.Lett.100:061802,2008, " Agarwalla et al., arXiv:1212.2238v1
WG
dis
cuss
ion ite
ms
" Razzaque & Smirnov, arXiv:1406.1407
HE neutrinos
Introduction
Historical aspects
Atmospheric Neutrinos
The Atmospheric sector
Measuring the Neutrino Mass Hierarchy with Atmospheric Neutrinos
Current Knowledge on Neutrino Mixing
Phenomenological considerations
Detectors (mostly future project)
Water/Ice Cherenkov
Magnetized Trackers
Liquid Argon TPCs
High Energy Atmospheric Neutrinos
Spectrum measurement
Prompt component
Outline 63
Covered by T. Gaisser & F Halzen + WG discussion.
Atmospheric neutrinos
Low Energy High Energy
Conventional neutrinos dN/dE ~E-3.7
Pion/Kaon decay Mostly νµ$
Prompt neutrinos dN/dE ~E-2.7
Charm decay Isotropic ~Equal flavor
Atmospheric muon neutrino 2008-2011 data set Two different energy estimators: - dE/dX as evaluated from total collected charge - Combined likelihood for hit/no-hit for all OMs
L: length ε: efficiency
Atmospheric energy spectrum by unfolding measured spectrum averaged in 90°-180° zenith band
Ae = x A: response matrix E: true distribution
X: measured distribution )Good understanding of the detector
free param
" S. Adrian-Martinez et al., Eur. Phys. J.C (2013) 73:2006)
Atmospheric muon neutrino
" M. G. Aartsen et al, arXiv:1409.4535 " M.G. Aartsen, et al., Physical Review Letters 110 (15), 151105 (2013).
Prompt component to atmospheric spectrum
Several predictions exist + large theoretical uncertainties
Prompt neutrino contribution unknown but currently affecting astrophysical spectrum estimate (and viceversa)
Can Neutrino Telescopes probe Charm production? WG discussion item
Prompt component to atmospheric spectrum
Constraints from IceCube
J. Koskinen , NOW14
Constraints from IceCube
J. Koskinen , NOW14
Summary (LE) ! Atmospheric Neutrinos have still a major role to play for precision measurements
and determination of unknown parameters such as the mass hierarchy and the search for exotic phenomena.
! Proposed detectors include Iron Calorimeter, Liquid Argon and Cherenkov detectors. None of these projects being firmly funded.
! Low energy (GeV) extensions of Neutrino Telescopes may be faster and cheaper than other alternatives…
! …but challenging, as systematics must be carefully controlled. Key parameters are the size of the detector as well as the energy and angle resolutions.
! Preliminary ORCA/PINGU sensitivities are quite promising.
! Synergies/Combination with LBL/reactor experiments may provide the first high significance MH determination…
ORCA!
ORCA
But one should never trust a plot like this!