High-energy neutrino interactions: first cross section measurements at TeV and above
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1 High-energy neutrino interactions: first cross section measurements at TeV and above Mauricio Bustamante TeVPA 2017 August 10, 2017
2 Two seemingly unrelated questions 1 Where are the most energetic particles coming from? 2 What is the structure of matter at the smallest scales? Mauricio Bustamante (OSU) 2
3 SYMMETRY MAGAZINE
4 Neutrino interactions are weak but we are persistent At center-of-mass energy of 1 GeV: σ pp cm 2 σ γp cm 2 σ νp cm 2 Mauricio Bustamante (OSU) 4
5 Neutrino interactions: what we (do not) know < 1 MeV Not observed Coherent neutrino-nucleus scattering (just measured!), capture on radionuclei 1 MeV 350 GeV Lots of data Quasi-elastic scattering, resonance production, deep inelastic scattering > 350 GeV / GeV) cm 2-38 (10 cross section / E QE DIS RES TOTAL 2 10 E (GeV) Not observed No high-energy neutrino beam available... til now Cross section [cm 2 ] νn NC Connolly 11 fit νn CC Connolly 11 fit νn NC Gandhi 98 νn CC Gandhi Neutrino energy [GeV] Mauricio Bustamante (OSU) 5
6 / GeV) cm 2-38 (10 cross section / E QE DIS RES TOTAL 2 10 E (GeV) E PARTICLE DATA GROUP Mauricio Bustamante (OSU) 6
7 / GeV) cm 2 1? TOTAL QE? DIS -38 (10 cross section / E RES E (GeV) E PARTICLE DATA GROUP Mauricio Bustamante (OSU) 6
8 ν l + n l + p ν l + p l + + n / GeV) cm 2-38 (10 cross section / E QE DIS RES TOTAL 2 10 E (GeV) E PARTICLE DATA GROUP Mauricio Bustamante (OSU) 6
9 ν l + n l + p ν l + p l + + n / GeV) cm 2-38 (10 cross section / E QE DIS RES ν l + N l + N l + π + N TOTAL 2 10 E (GeV) E PARTICLE DATA GROUP Mauricio Bustamante (OSU) 6
10 ν l + n l + p ν l + p l + + n / GeV) cm 2-38 (10 cross section / E QE DIS RES ν l + N l + N l + π + N TOTAL 2 10 E (GeV) E ν l + N l + X ν l + N l + + X PARTICLE DATA GROUP Mauricio Bustamante (OSU) 6
11 How does DIS probe nucleon structure? What you see Beneath the hood ν l (p ν ) l (p l ) ν l (p ν ) l (p l ) W + (q) W + (q) u(p f ) d(p i ) X(p X ) N(p N ) N(p N ) Plus the equivalent neutral-current process (Z -exchange) GIUNTI & KIM, Fundamentals of Neutrino Physics & Astrophysics Mauricio Bustamante (OSU) 7
12 FERMILAB TODAY
13 Peeking inside a proton (Parton distribution function) xf 1 sea quarks Extrapolation xs ( 0.05) H1 and ZEUS HERAPDF1.0 exp. uncert. model uncert. parametrization uncert. xg ( 0.05) gluons 2 2 Q = 10 GeV xu v xd v valence up quark valence down quark A. COOPER-SARKAR (Fraction of momentum carried by parton) Mauricio Bustamante (OSU) 9 x
14 Extrapolating the neutrino cross section Cross section [cm 2 ] νn NC Connolly 11 fit νn CC Connolly 11 fit νn NC Gandhi 98 νn CC Gandhi Neutrino energy [GeV] Mauricio Bustamante (OSU) 10
15 Extrapolating the neutrino cross section Extrapolation Cross section [cm 2 ] νn NC Connolly 11 fit νn CC Connolly 11 fit νn NC Gandhi 98 νn CC Gandhi Neutrino energy [GeV] Mauricio Bustamante (OSU) 10
16 What can IceCube do? Neutrino-nucleon CC cross section σ νn CC [cm2 ] Gandhi 98 Connolly 11 Cooper-Sarkar 11 Block 14 Arguelles 15 Testable by IceCube Testable by ANITA Neutrino energy E ν [GeV] Mauricio Bustamante (OSU) 11
17 How does IceCube see neutrinos? Two types of fundamental interactions... Charged-current ν l + N l + hadrons Neutral-current ν l + N ν l + hadrons... create two event topologies... these shower and make light Showers Made by CC ν e or ν τ ; or by NC ν x Tracks Made mainly by CC ν µ Bad angular resolution (10 s deg) Good angular resolution (< deg) 100 s m 100 s m few km Mauricio Bustamante (OSU) 12
18 How do we measure the cross section? By looking at the angular distribution of events Earth absorbs neutrinos Absorption factor: e D(θ z)/l int (E ν,θ z ) Interaction length: L int = m N σ CC+NC νn (E ν ) ρ (θ z ) Neutrino attenuation factor AνN, A νn 1.0 E ν = 10 TeV ν ν 100 TeV 1 PeV 10 PeV Neutrino zenith angle cos θ z Mauricio Bustamante (OSU) 13
19 Where does the sensitivity to σ come from? Number of contained events: N Φ ν σ νn e τ = Φ ν σ νn e Lσ νnn N Downgoing (no matter) N dn Φ ν σ νn Downgoing events fix the product Φ ν σ νn Upgoing (lots of matter) N up N dn e τ Upgoing events measure the cross section via τ Reality check: Few events (per energy bin), so we are limited by Poissonian statistics Mauricio Bustamante (OSU) 14
20 The IceCube HESE sample (6 years) Deposited energy E dep [GeV] Attenuation in Earth Shower Track Neutrino zenith angle cos θ z MB & A. Connolly, In prep. Mauricio Bustamante (OSU)
21 The IceCube HESE sample (6 years) Deposited energy E dep [GeV] Downgoing events constrain flux 0.7 cross section Attenuation in Earth Shower Track Neutrino zenith angle cos θ z MB & A. Connolly, In prep. Mauricio Bustamante (OSU)
22 The IceCube HESE sample (6 years) Deposited energy E dep [GeV] 10 6 Upgoing events constrain the cross section 10 5 Downgoing events constrain flux 0.7 cross section Attenuation in Earth Shower Track Neutrino zenith angle cos θ z MB & A. Connolly, In prep. Mauricio Bustamante (OSU)
23 Flux vs. cross section In each energy bin: Downgoing events (τ 0) N down Φ ν σ νn Upgoing events (0 < τ < 1) N up = N down e τ N down e σ νn Comparing N down to N up constrains the cross section Sensitivity to σ νn comes from attenuation, not detection Mauricio Bustamante (OSU) 16
24 Where is most of the sensitivity to σ νn? Deposited energy E dep [GeV] Attenuation in Earth Shower Track Neutrino zenith angle cos θ z MB & A. Connolly, In prep. 0.1 Mauricio Bustamante (OSU) 17
25 Where is most of the sensitivity to σ νn? Deposited energy E dep [GeV] Attenuation in Earth Shower Track Neutrino zenith angle cos θ z MB & A. Connolly, In prep. Energy too low: N up and N down comparable 0.1 Mauricio Bustamante (OSU) 17
26 Where is most of the sensitivity to σ νn? Deposited energy E dep [GeV] Energy too high: no upgoing events Attenuation in Earth Shower Track Neutrino zenith angle cos θ z MB & A. Connolly, In prep. 0.1 Mauricio Bustamante (OSU) 17
27 Where is most of the sensitivity to σ νn? 1.0 Deposited energy E dep [GeV] Goldilocks region Attenuation in Earth Shower Track Neutrino zenith angle cos θ z MB & A. Connolly, In prep. 0.1 Mauricio Bustamante (OSU) 17
28 Bin-by-bin analysis 1.0 Deposited energy E dep [GeV] Shower Track Neutrino zenith angle cos θ z Attenuation in Earth 18 TeV 100 TeV Mauricio Bustamante (OSU) 18
29 Bin-by-bin analysis 1.0 Deposited energy E dep [GeV] Shower Track Neutrino zenith angle cos θ z Attenuation in Earth 100 TeV 500 TeV 18 TeV 100 TeV Mauricio Bustamante (OSU) 18
30 Bin-by-bin analysis Deposited energy E dep [GeV] Shower Track Neutrino zenith angle cos θ z Attenuation in Earth 500 TeV 2 PeV 100 TeV 500 TeV 18 TeV 100 TeV Mauricio Bustamante (OSU) 18
31 What events do we use? σ νn varies with neutrino energy So, we should use events where deposited energy neutrino energy We use IceCube High-Energy Starting Events (HESE): νn interaction occurs inside the detector Showers: completely contained in the detector (E dep E ν ) Tracks: partially contained (E dep < E ν ) We use only 58 HESE showers (ICRC 6-year IceCube HESE sample) Mauricio Bustamante (OSU) 19
32 What goes into the (likelihood) mix? Free parameters varied inside each energy bin: N atm sh (showers from atmospheric neutrinos) Nsh st (showers from astrophysical neutrinos) γ (astrophysical spectral index) σ CC νn (neutrino-nucleon charged-current cross section) Neutral-current showers are subdominant we fix σ NC νn = σcc νn /3 Mauricio Bustamante (OSU) 20
33 The result Neutrino-nucleon CC cross section (σ νn CC + σcc νn )/2 [cm2 ] Center-of-mass energy s [GeV] Tevatron LHC FCC Large EDM Low-energy global avg. Bustamante 17 Gandhi 98 Connolly 11 Cooper-Sarkar 11 Block 14 ν Argüelles 15 ν Preliminary Neutrino energy E ν [GeV] MB & A. Connolly, In prep. Mauricio Bustamante (OSU) 21
34 Extending the cross section measurements Preliminary σ νn CC /E ν [10 38 cm 2 GeV 1 nucleon 1 ] ν ν T2K (Fe) 14 T2K (CH) 14 T2K (C) 13 ArgoNeuT 14 ArgoNeuT Neutrino energy E ν [GeV] MB & A. Connolly, In prep. Mauricio Bustamante (OSU) 22 ANL 79 BEBC 79 BNL 82 CCFR 97 CDHS 87 GGM-SPS 81 GGM-PS 79 IHEP-ITEP 79 IHEP-JINR 96 MINOS 10 NOMAD 08 NuTeV 06 SciBooNE 11 SKAT 79
35 Extending the cross section measurements Preliminary σ νn CC /E ν [10 38 cm 2 GeV 1 nucleon 1 ] ν ν T2K (Fe) 14 T2K (CH) 14 T2K (C) 13 ArgoNeuT 14 ArgoNeuT Neutrino energy E ν [GeV] MB & A. Connolly, In prep. Mauricio Bustamante (OSU) 22 ANL 79 BEBC 79 BNL 82 CCFR 97 CDHS 87 GGM-SPS 81 GGM-PS 79 IHEP-ITEP 79 IHEP-JINR 96 MINOS 10 NOMAD 08 NuTeV 06 SciBooNE 11 SKAT 79 IC HESE sh. 17
36 Extending the cross section measurements Preliminary σ νn CC /E ν [10 38 cm 2 GeV 1 nucleon 1 ] ν ν T2K (Fe) 14 T2K (CH) 14 T2K (C) 13 ArgoNeuT 14 ArgoNeuT 12 Avg. of ν, ν E 0.5 ν Neutrino energy E ν [GeV] MB & A. Connolly, In prep. Mauricio Bustamante (OSU) 22 ANL 79 BEBC 79 BNL 82 CCFR 97 CDHS 87 GGM-SPS 81 GGM-PS 79 IHEP-ITEP 79 IHEP-JINR 96 MINOS 10 NOMAD 08 NuTeV 06 SciBooNE 11 SKAT 79 IC HESE sh. 17
37 Caveats Limited statistics (for now) Solvable with more IceCube + IceCube-Gen2 + KM3NeT Large errors in arrival directions give errors in attenuation Solvable with improvements (talk by Tianlu Yuan) + KM3NeT Only constrains charged-current + neutral-current cross section Solvable (?) with muon and neutron echoes (Li, MB, Beacom 16) Cannot separate ν from ν Wait for Glashow resonance Use starting tracks (easy) + through-going muons (less so) Doable now by the Collaboration Mauricio Bustamante (OSU) 23
38 Quo vadis: IceCube vs. ANITA/ARA/ARIANNA Neutrino-nucleon CC cross section σ νn CC [cm2 ] Gandhi 98 Connolly 11 Cooper-Sarkar 11 Block 14 Arguelles 15 Testable by IceCube Testable by ANITA Neutrino energy E ν [GeV] Mauricio Bustamante (OSU) 24
39 Quo vadis: IceCube vs. ANITA/ARA/ARIANNA Neutrino-nucleon CC cross section σ νn CC [cm2 ] Gandhi 98 Connolly 11 Cooper-Sarkar 11 Block 14 Arguelles 15 Testable by IceCube Testable by ANITA Test predictions of deep inelastic scattering Neutrino energy E ν [GeV] Mauricio Bustamante (OSU) 24
40 Quo vadis: IceCube vs. ANITA/ARA/ARIANNA Neutrino-nucleon CC cross section σ νn CC [cm2 ] Gandhi 98 Connolly 11 Cooper-Sarkar 11 Block 14 Arguelles 15 Opportunity to test unprobed nucleon structure! Testable by IceCube Testable by ANITA Neutrino energy E ν [GeV] Mauricio Bustamante (OSU) 24
41 Backup slides Mauricio Bustamante (OSU) 25
42 The world of PDFs is messy Different fitting groups Different QCD prescriptions xf xg ( 0.05) xs ( 0.05) HERAPDF1.5 MSTW08 CTEQ Q = 10 GeV xd v xu v x xf H1 and ZEUS HERA I+II PDF Fit xg ( 0.05) xs ( 0.05) HERAPDF1.5 NNLO (prel.) exp. uncert. model uncert. parametrization uncert. HERAPDF1.5f (prel.) Q = 10 GeV xu v xd v x A. COOPER-SARKAR 2012 HERAPDF Structure Function Working Group March 2011 Mauricio Bustamante (OSU) 26
43 Neutrino baseline inside the Earth 10 4 Detector depth: 1.5 km Baseline inside Earth [km] Approximate Exact cos µ z MB & A. Connolly, In prep. Mauricio Bustamante (OSU) 27
44 Earth density profile From the Preliminary Reference Earth Model 12 Matter density [g cm 3 ] x r=r Mauricio Bustamante (OSU) 28
45 Average Earth density 12 Detector depth: 1.5 km Average matter density [g cm 3 ] Interpolated Exact cos µ z MB & A. Connolly, In prep. Mauricio Bustamante (OSU) 29
46 Neutrino interaction length inside the Earth Neutrino Anti-neutrino Interaction length [km] NC CC E º =10 4 GeV 10 6 GeV 10 8 GeV GeV GeV Interaction length [km] NC CC E º =10 4 GeV 10 6 GeV 10 8 GeV GeV GeV ºN Connolly11, Detector depth: 1.5 km cos µ z ¹ºN Connolly11, Detector depth: 1.5 km cos µ z Mauricio Bustamante (OSU) 30
47 Neutrino absorption in the Earth exp( ) 1.0 E º =10 4 GeV ¹º º 10 5 GeV 10 6 GeV 10 8 GeV ºN, ¹ºN Connolly11 Detector depth: 1.5 km GeV GeV cos µ z MB & A. Connolly, In prep. Mauricio Bustamante (OSU) 31
48 Angle-averaged neutrino absorption in the Earth Angle-averaged attenuation factor AνN cos θz ν e, ν µ, ν τ ν µ, ν τ ν e Neutrino energy E ν [GeV] exp( ) cos µ z º e ¹º e ºN, ¹ºN Connolly11, Detector depth: 1.5 km E º [GeV] MB & A. Connolly, In prep. Mauricio Bustamante (OSU) 32
49 Angular probability distribution for 4-yr HESE events Angular probability distribution dp=dcos µ z ID #1 47:6 +6:5 5:4 TeV ID #9 63:2 8:0 +7:1 TeV 0.0 ID #15 57:5 7:8 +8:3 TeV 0.0 ID #21 30:2 3:3 +3:5 TeV ID #27 60:2 +5:6 5:6 TeV ID #34 42:1 6:3 +6:5 TeV 0.0 ID # :6 +8:4 10:0 TeV ID #2 117:0 +15:4 14:6 TeV ID #10 97:2 +10:4 12:4 TeV ID #16 30:6 +3:6 3:5 TeV ID #22 219:5 +21:2 24:4 TeV ID #29 32:7 +3:2 2:9 TeV ID # :7 +236:2 261:5 TeV ID #42 76:3 +10:3 11:6 TeV ID #4 165:4 +19:8 14:9 TeV ID #11 88:4 +12:5 10:7 TeV ID #17 199:7 +27:2 26:8 TeV ID #24 30:5 +3:2 2:6 TeV ID #30 128:7 +13:8 12:5 TeV ID #36 28:9 +3:0 2:6 TeV ID #46 158:0 +15:3 16:6 TeV ID #6 28:4 +2:7 2:5 TeV ID #12 104:1 +12:5 13:2 TeV ID #19 71:5 +7:0 7:2 TeV ID #25 33:5 +4:9 5:0 TeV ID #31 42:5 +5:4 5:7 TeV ID #39 101:3 +13:3 11:6 TeV ID #48 ID #50 ID #51 ID #52 ID #54 22:2 +2:3 66:2 +6:7 158:1 +16:3 54:5 +5:1 2:0 TeV 6:1 TeV 18:4 TeV ID #7 34:3 +3:5 4:3 TeV ID # :7 +131:6 144:4 TeV ID # :8 +142:8 132:8 TeV ID #26 210:0 +29:0 25:8 TeV ID #33 384:7 +46:4 48:6 TeV ID #40 157:3 +15:9 16:7 TeV ID #49 104:7 10:2 +13:5 TeV 59:9 7:9 +8:3 TeV :3 TeV cos µ z MB & A. Connolly, In prep. Mauricio Bustamante (OSU) 33
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