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September 2014 Neutrino Oscillation Workshop
Otranto, Lecce, Italy
IceCube Results & PINGU Perspectives
D. Jason Koskinen for the IceCube-PINGU Collaboration
D. Jason Koskinen - NOW 2014
IceCube Detector
2
ν
IceCube DOM
•~1km3 of instrumented ice
•Uses ~5k optical sensors across 86 vertical strings to detect Cherenkov radiation
•Deployed 1.5 - 2.5km below the surface
D. Jason Koskinen - NOW 2014
IceCube Detector
2
νµ
IceCube DOM
•~1km3 of instrumented ice
•Uses ~5k optical sensors across 86 vertical strings to detect Cherenkov radiation
•Deployed 1.5 - 2.5km below the surface
D. Jason Koskinen - NOW 2014
Event Movie
3
D. Jason Koskinen - NOW 2014
Event Movie
3
D. Jason Koskinen - NOW 2014 4
νμ + N μ + X “Track”
νX + X νX + X “Cascade”
Track topology (e.g. induced by muon neutrino) !Good pointing, 0.2° - 1° Lower bound on energy for through-going events
Cascade topology (e.g. induced by electron neutrino) !Good energy resolution, 15% Some pointing, 10° - 15°
D. Jason Koskinen - NOW 2014 4
νμ + N μ + X “Track”
νX + X νX + X “Cascade”
Track topology (e.g. induced by muon neutrino) !Good pointing, 0.2° - 1° Lower bound on energy for through-going events
Cascade topology (e.g. induced by electron neutrino) !Good energy resolution, 15% Some pointing, 10° - 15°
D. Jason Koskinen - NOW 2014
IceCube Classic
5
D. Jason Koskinen - NOW 2014
High Energy Starting Events (HESE)
6
D. Jason Koskinen - NOW 2014
• Follow-up to observation of two events > 1 PeV in IceCube search for Ultra-High Energy (GZK) neutrinos
High Energy Starting Events (HESE)
6
D. Jason Koskinen - NOW 2014
• Follow-up to observation of two events > 1 PeV in IceCube search for Ultra-High Energy (GZK) neutrinos
• Use outermost layer of IceCube as a veto region • Identifies possible muon background
• Enforces neutrino interaction containment
High Energy Starting Events (HESE)
6
D. Jason Koskinen - NOW 2014
• Follow-up to observation of two events > 1 PeV in IceCube search for Ultra-High Energy (GZK) neutrinos
• Use outermost layer of IceCube as a veto region • Identifies possible muon background
• Enforces neutrino interaction containment
• Focused on brightest events with > 6000 photoelectrons
High Energy Starting Events (HESE)
6
D. Jason Koskinen - NOW 2014
High Energy Neutrinos
7
•Ultra-high energy IceCube (GZK) astrophysical search found 2 anomalous background events in 2 years of data
1.04±0.16 PeV 1.14±0.17 PeV
D. Jason Koskinen - NOW 2014
High Energy Neutrinos
7
•Ultra-high energy IceCube (GZK) astrophysical search found 2 anomalous background events in 2 years of data
1.04±0.16 PeV 1.14±0.17 PeV
D. Jason Koskinen - NOW 2014
!
• 36(+1) events total • 8.4 ± 4.2 atm. muons
• 6.6+5.9-1.6 atm. neutrinos
!
• 5.7σ rejection of only atmospheric neutrino flux
!
• Consistent with 1:1:1 flavor ratio
3-year HESE Result
8
D. Jason Koskinen - NOW 2014
HESE-III Sky Map
9
arXiv:1405.5303
• No significant evidence for clustering
D. Jason Koskinen - NOW 2014
Natural Neutrino Flux (>1 GeV)
10
D. Jason Koskinen - NOW 2014
Natural Neutrino Flux (>1 GeV)
10
• Combination of conventional neutrino, high energy astrophysical, and possible prompt neutrinos from charm hadron decay
D. Jason Koskinen - NOW 2014
Natural Neutrino Flux (>1 GeV)
10
• Combination of conventional neutrino, high energy astrophysical, and possible prompt neutrinos from charm hadron decay
CosmicRay
D. Jason Koskinen - NOW 2014
Natural Neutrino Flux (>1 GeV)
10
• Combination of conventional neutrino, high energy astrophysical, and possible prompt neutrinos from charm hadron decay
CharmHadronX
CosmicRay
D. Jason Koskinen - NOW 2014
Natural Neutrino Flux (>1 GeV)
10
• Combination of conventional neutrino, high energy astrophysical, and possible prompt neutrinos from charm hadron decay
CharmHadronX
X
Neutrino
CosmicRay
D. Jason Koskinen - NOW 2014
Prompt Neutrino Flux
11
CharmHadronX
X
Neutrino
CosmicRay
D. Jason Koskinen - NOW 2014
Prompt Neutrino Flux
11
CharmHadronX
X
Neutrino
CosmicRay
• Prompt flux more closely follows the incident CR energy spectrum (E-2) than the conventional neutrino spectrum (E-2.7 to -3.7)
D. Jason Koskinen - NOW 2014
Prompt Neutrino Flux
11
CharmHadronX
X
Neutrino
CosmicRay
• Prompt flux more closely follows the incident CR energy spectrum (E-2) than the conventional neutrino spectrum (E-2.7 to -3.7)
• Prompt νe versus νµ channel is advantageous due to conventional νµ bkg
D. Jason Koskinen - NOW 2014
Prompt Component
12
D. Jason Koskinen - NOW 2014
• Prompt can be constrained by flux in the 10-50 TeV range • Higher energy is dominated by astrophysical flux
• Lower energy is dominated by conventional flux (pion/kaon decay)
Prompt Component
12
D. Jason Koskinen - NOW 2014
• Prompt can be constrained by flux in the 10-50 TeV range • Higher energy is dominated by astrophysical flux
• Lower energy is dominated by conventional flux (pion/kaon decay)
• Northern vs. Southern sky comparison weakly breaks the degeneracy between the astrophysical and prompt flux
Prompt Component
12
D. Jason Koskinen - NOW 2014
• Places upper limits on some prompt models (<1.4 ERS model)
A Prompt Result
13
Atm. NeutrinosAtm. Muons
D. Jason Koskinen - NOW 2014
Fundamental Physics with DeepCore
14
D. Jason Koskinen - NOW 2014
DeepCore
15
scattering
D. Jason Koskinen - NOW 2014
• Low-energy extension • Closer instrumentation
• Clearer Ice
• Higher efficiency PMTs
DeepCore
15
scattering
D. Jason Koskinen - NOW 2014
• Low-energy extension • Closer instrumentation
• Clearer Ice
• Higher efficiency PMTs
• Use surrounding IceCube as a veto volume
DeepCore
15
scattering
D. Jason Koskinen - NOW 2014
• Low-energy extension • Closer instrumentation
• Clearer Ice
• Higher efficiency PMTs
• Use surrounding IceCube as a veto volume
• Oscillation Physics
• νµ disappearance
• ντ appearance*
DeepCore
15
scattering
*Covered later for PINGU
D. Jason Koskinen - NOW 2014
Neutrino Oscillation
16
~12,700km
IceCube DeepCore
Mena, Mocioiu & Razzaque, Phys. Rev. D78, 093003 (2008)
νµ disappearance
ντ appearance
νµνµ
νµνµ
νµ
D. Jason Koskinen - NOW 2014
Neutrino Oscillation
16
•Northern Hemisphere νµ oscillating over one earth radii produces νµ (ντ) oscillation minimum (maximum) at ~25 GeV
~12,700km
IceCube DeepCore
Mena, Mocioiu & Razzaque, Phys. Rev. D78, 093003 (2008)
νµ disappearance
ντ appearance
νµνµ
νµνµ
νµ
D. Jason Koskinen - NOW 2014
Neutrino Oscillation
16
•Northern Hemisphere νµ oscillating over one earth radii produces νµ (ντ) oscillation minimum (maximum) at ~25 GeV
• Beam never turns off
~12,700km
IceCube DeepCore
Mena, Mocioiu & Razzaque, Phys. Rev. D78, 093003 (2008)
νµ disappearance
ντ appearance
νµνµ
νµνµ
νµ
D. Jason Koskinen - NOW 2014
Neutrino Oscillation
16
•Northern Hemisphere νµ oscillating over one earth radii produces νµ (ντ) oscillation minimum (maximum) at ~25 GeV
• Beam never turns off
• Samples all terrestrial baselines
~12,700km
IceCube DeepCore
Mena, Mocioiu & Razzaque, Phys. Rev. D78, 093003 (2008)
νµ disappearance
ντ appearance
νµνµ
νµνµ
νµ
D. Jason Koskinen - NOW 2014
• High-purity analysis selected 5293 events over 2011-2014
νµ Disappearance in DeepCore
17
MC Expectation (3-yr)
Type Osc. No Osc.3755 5900
273 -
678 650
418
Atm. µ 54
Total 5178 7022
νµ
ντνe
νNC
D. Jason Koskinen - NOW 2014
Oscillation Contours
18
D. Jason Koskinen - NOW 2014
Next?
19
D. Jason Koskinen - NOW 2014
Two Directions
20
D. Jason Koskinen - NOW 2014
• Higher energy • Point sources
• Neutrino flavor ratios
• HEX - High Energy Extension
Two Directions
20
D. Jason Koskinen - NOW 2014
• Higher energy • Point sources
• Neutrino flavor ratios
• HEX - High Energy Extension
• Lower Energy - just past DeepCore at the O(1) GeV sensitivity: • Resolve the ordering of the Neutrino Mass Hierarchy
• Improve neutrino oscillation
• ντ appearance
• non-maximal θ23
• GeV mass Dark Matter
• PINGU
Two Directions
20
D. Jason Koskinen - NOW 2014
• Higher energy • Point sources
• Neutrino flavor ratios
• HEX - High Energy Extension
• Lower Energy - just past DeepCore at the O(1) GeV sensitivity: • Resolve the ordering of the Neutrino Mass Hierarchy
• Improve neutrino oscillation
• ντ appearance
• non-maximal θ23
• GeV mass Dark Matter
• PINGU
Two Directions
20
D. Jason Koskinen - NOW 2014
PINGU
21
D. Jason Koskinen - NOW 2014
Precision IceCube Next Generation Upgrade
22
IceCube
DeepCore
PINGU
Letter of Intent - arXiv:1401.2046
D. Jason Koskinen - NOW 2014
• Use existing and familiar technology to infill DeepCore
Precision IceCube Next Generation Upgrade
22
IceCube
DeepCore
PINGU
Letter of Intent - arXiv:1401.2046
D. Jason Koskinen - NOW 2014
• Use existing and familiar technology to infill DeepCore
• Improve rejection of cosmic ray muon background
Precision IceCube Next Generation Upgrade
22
IceCube
DeepCore
PINGU
Letter of Intent - arXiv:1401.2046
D. Jason Koskinen - NOW 2014
• Use existing and familiar technology to infill DeepCore
• Improve rejection of cosmic ray muon background
• Primary physics goal is resolving neutrino mass hierarchy
Precision IceCube Next Generation Upgrade
22
IceCube
DeepCore
PINGU
Letter of Intent - arXiv:1401.2046
D. Jason Koskinen - NOW 2014
PINGU Simulation Event
23
•9.28 GeV Neutrino, 4.9 GeV muon, 4.5 GeV cascade
DeepCore
DeepCore+PINGU
D. Jason Koskinen - NOW 2014
PINGU Simulation Event
23
•9.28 GeV Neutrino, 4.9 GeV muon, 4.5 GeV cascade
DeepCore
DeepCore+PINGU
D. Jason Koskinen - NOW 2014
PINGU Simulation Event
23
•9.28 GeV Neutrino, 4.9 GeV muon, 4.5 GeV cascade
•~20 vs. ~50 Hit Modules
DeepCore
DeepCore+PINGU
D. Jason Koskinen - NOW 2014
PINGU Neutrino Mass Hierarchy
24
D. Jason Koskinen - NOW 2014
PINGU Neutrino Mass Hierarchy
24
1
1
D. Jason Koskinen - NOW 2014
PINGU Neutrino Mass Hierarchy
24
1
1
2
2
D. Jason Koskinen - NOW 2014
PINGU Neutrino Mass Hierarchy
24
1
1
2
2
•Inverted/Normal hierarchy has up to a 20% difference in oscillation probability for specific energies and zenith angles (baselines)
D. Jason Koskinen - NOW 2014
Neutrino Mass Hierarchy by Eye
25
1-year exposurePreliminary
Track-Like Events (mainly CC νµ+νµ)
D. Jason Koskinen - NOW 2014
• Several of the main systematics have been examined
Systematics
26
Preliminary
D. Jason Koskinen - NOW 2014
Mass Hierarchy Bottom Line
27
D. Jason Koskinen - NOW 2014
ντ Appearance in PINGU
28
D. Jason Koskinen - NOW 2014
• Direct measure of |Uτ3|2
ντ Appearance in PINGU
28
D. Jason Koskinen - NOW 2014
• Direct measure of |Uτ3|2
ντ Appearance in PINGU
28
cos(Zen)-1 -0.8 -0.6 -0.4 -0.2 0
(GeV
)νE
0
10
20
30
40
50
60
70
80
all f
lavo
urs
N)/µν+ eν
-Nal
l fla
vour
s(N
0
1
2
3
4
5livetime: 1 yearPINGU
preliminary
D. Jason Koskinen - NOW 2014
• Direct measure of |Uτ3|2
• Energy and zenith angle excess in cascade channel
• PINGU plots currently use same initial Boosted Decision Tree as NMH, but secondary selection for `cascades’
ντ Appearance in PINGU
28
cos(Zen)-1 -0.8 -0.6 -0.4 -0.2 0
(GeV
)νE
0
10
20
30
40
50
60
70
80
all f
lavo
urs
N)/µν+ eν
-Nal
l fla
vour
s(N
0
1
2
3
4
5livetime: 1 yearPINGU
preliminary
D. Jason Koskinen - NOW 2014
• Direct measure of |Uτ3|2
• Energy and zenith angle excess in cascade channel
• PINGU plots currently use same initial Boosted Decision Tree as NMH, but secondary selection for `cascades’
ντ Appearance in PINGU
28
Livetime (months)1 2 3 4 5 6
)σ
app
eara
nce
(τν
no
Sign
ifica
nce
to e
xclu
de
0
2
4
6
8
10
expectedσ1±σ2±
limitβ=αGaussian approximation
norm=1τνtrue PINGU
preliminary
cos(Zen)-1 -0.8 -0.6 -0.4 -0.2 0
(GeV
)νE
0
10
20
30
40
50
60
70
80
all f
lavo
urs
N)/µν+ eν
-Nal
l fla
vour
s(N
0
1
2
3
4
5livetime: 1 yearPINGU
preliminary
D. Jason Koskinen - NOW 2014
Measuring ντ Appearance
29
D. Jason Koskinen - NOW 2014
Measuring ντ Appearance
29
cos(Zen)-1.0 -0.8 -0.6 -0.4 -0.2 0.0
Events/year
0
200
400
600
800
1000
1200
eν
µν
τν
PINGUEν∈[1,80] GeVpreliminary
νµνe
ντ
D. Jason Koskinen - NOW 2014
Measuring ντ Appearance
29
Livetime (months)1 2 3 4 5 6
nor
mal
izat
ion
τνTr
ue
0.0
0.5
1.0
1.5
σ5expectedσ1±σ2± norm=1τνmeasured
PINGU
preliminary
cos(Zen)-1.0 -0.8 -0.6 -0.4 -0.2 0.0
Events/year
0
200
400
600
800
1000
1200
eν
µν
τν
PINGUEν∈[1,80] GeVpreliminary
νµνe
ντ
D. Jason Koskinen - NOW 2014
• IceCube is opening a new window on neutrino astronomy with 5.7σ observation of astrophysical neutrinos and probing atmospheric charm meson production
!
• Potential with PINGU to quickly resolve the ordering of the neutrino mass hierarchy in addition to enhancing other physics (ντ appearance, non-maximal θ23, O(1) GeV dark matter,…)
Conclusions
30
D. Jason Koskinen - NOW 2014 31
• IceCube is opening a new window on neutrino astronomy with 5.7σ observation of astrophysical neutrinos and probing atmospheric charm hadron production
• Potential with PINGU to quickly resolve the ordering of the neutrino mass hierarchy in addition to enhancing other physics (ντ appearance, non-maximal θ23, O(1) GeV dark matter,…)
D. Jason Koskinen - NOW 2014
D. Jason Koskinen - NOW 2014 31
• IceCube is opening a new window on neutrino astronomy with 5.7σ observation of astrophysical neutrinos and probing atmospheric charm hadron production
• Potential with PINGU to quickly resolve the ordering of the neutrino mass hierarchy in addition to enhancing other physics (ντ appearance, non-maximal θ23, O(1) GeV dark matter,…)
D. Jason Koskinen - NOW 2014
32
D. Jason Koskinen - NOW 2014
Backup
33
D. Jason Koskinen - NOW 2014
•Measurements • Cosmic Ray Anisotropy - arXiv:1105.2326
• Diffuse Neutrino Flux - arXiv:1104.5187
• Atmospheric Neutrino Spectrum - arXiv:1010.3980
• Neutrino Oscillation - arXiv:1305.3909
• Atmospheric Electron Neutrino Flux - arXiv:1212.4760
•Searches • Supernova 2008D - arXiv:1101.3942
• Neutrino Induced Cascades - arXiv:1101.1692
• Neutrino Emission Constraints on 2010 Crab Flare - arXiv:1106.3484
• Point Sources - arXiv:1406.6757, 1307.6669
• Gamma Ray Burst Neutrino Emission - arXiv:1204.4219
• Slow Magnetic Monopole - arXiv:1402.3460
• Dark Matter - arXiv:1406.6868, 1303.3473, 1212.4097
Science Portfolio (Partial)
34
D. Jason Koskinen - NOW 2014
HESE-III Event Breakdown
35
D. Jason Koskinen - NOW 2014 36
Potential High Energy Extension (HEX)DeepCoreIceCubeDecaCube (1/2/3)
Spacing 1 (120m): IceCube (1 km3) + 98 strings (1,3 km3) = 2,3 km3
!Spacing 2 (240m):
IceCube (1 km3) + 99 strings (5,3 km3) = 6,3 km3
!Spacing 3 (360m):
IceCube (1 km3) + 95 strings (11,6 km3) = 12,6 km3
Chosen geometry not optimum (i.e. for HESE) … historically chosen to demonstrate that we do respect boundary conditions
*courtesy of C. Wiebusch (RTWH Aachen)
D. Jason Koskinen - NOW 2014
• Probes lower mass region
!
• Independent test of Spin-Independent results from direct detection experiments
Dark Matter in PINGU
37