Status of IceCube Upgrade Program and KM3NeT Joshua Hignight August 9th, 2019 Joshua Hignight IC Upgrase/KM3NeT August 9th, 2019 1 / 22 Why have VLVNTs? The Universe is opaque to EM radiation at high energies can only explore with neutrinos! ! Joshua Hignight IC Upgrase/KM3NeT August 9th, 2019 2 / 22 Where are HE neutrinos coming from? Are there single (point) sources? Joshua Hignight IC Upgrase/KM3NeT August 9th, 2019 3 / 22 Measuring the EHE Spectrum Diffuse γ (Fermi LAT) IceCube (ApJ 2015) 5 10− Cosmic rays (Auger) ] 2 Cosmic rays (TA) − 6 10− Understand the evolution cm 1 of the spectral index − sr 7 1 10− − I Does it soften at low 8 energies? 10− I High energy cut-off? Φ [GeV s 9 10− × 2 Connect the neutrino E 10 spectrum to the cosmic 10− ray spectrum 100 101 102 103 104 105 106 107 108 109 1010 1011 E [GeV] Joshua Hignight IC Upgrase/KM3NeT August 9th, 2019 4 / 22 Measuring the EHE Spectrum Diffuse γ (Fermi LAT) IceCube (ApJ 2015) 5 10− Cosmic rays (Auger) Gen2 (15 years) ] 2 Cosmic rays (TA) − 6 10− Understand the evolution cm 1 of the spectral index − sr 7 1 10− − I Does it soften at low 8 energies? 10− I High energy cut-off? Φ [GeV s 9 10− × 2 Connect the neutrino E 10 spectrum to the cosmic 10− ray spectrum 100 101 102 103 104 105 106 107 108 109 1010 1011 E [GeV] Joshua Hignight IC Upgrase/KM3NeT August 9th, 2019 4 / 22 Measuring the EHE Spectrum Diffuse γ (Fermi LAT) IceCube (ApJ 2015) 5 10− Cosmic rays (Auger) Gen2 (15 years) ] 2 Cosmic rays (TA) − Understand the evolution 6 10− cm of the spectral index 1 − sr 7 1 10− I Does it soften at low − energies? 8 10− I High energy cut-off? Φ [GeV s 9 10− × Connect the neutrino 2 E 10 spectrum to the cosmic 10− ray spectrum 100 101 102 103 104 105 106 107 108 109 1010 1011 E [GeV] Joshua Hignight IC Upgrase/KM3NeT August 9th, 2019 4 / 22 Flavor Ratio Production Mechanism fe : fµ : fτ at source fe : fµ : fτ at detector π decay 1 : 2 : 0 0.93 : 1.05 : 1.02 µ cooling 0 : 1 : 0 0.6 : 1.3 : 1.1 n decay 1 : 0 : 0 1.6 : 0.6 : 0.8 Joshua Hignight IC Upgrase/KM3NeT August 9th, 2019 5 / 22 Flavor Ratio Production Mechanism fe : fµ : fτ at source fe : fµ : fτ at detector π decay 1 : 2 : 0 0.93 : 1.05 : 1.02 µ cooling 0 : 1 : 0 0.6 : 1.3 : 1.1 n decay 1 : 0 : 0 1.6 : 0.6 : 0.8 Joshua Hignight IC Upgrase/KM3NeT August 9th, 2019 5 / 22 Multi-Messenger Astronomy Joshua Hignight IC Upgrase/KM3NeT August 9th, 2019 6 / 22 Landscape of VLVNTs Joshua Hignight IC Upgrase/KM3NeT August 9th, 2019 7 / 22 KM3NeT Joshua Hignight IC Upgrase/KM3NeT August 9th, 2019 8 / 22 KM3NeT Joshua Hignight IC Upgrase/KM3NeT August 9th, 2019 9 / 22 IceCube-Gen2 IceCube-Gen2 is a versatile facility for future South Pole physics Radio Array Surface Array High Energy Array I 120 strings 90 × sensors/string 2 I 8 km area with wider ∼ string spacing PINGU I Low energy infill Joshua Hignight IC Upgrase/KM3NeT August 9th, 2019 10 / 22 IceCube Upgrade: Stepping Stone to Gen2 7 new strings 22m spacing ∼ between strings 3m vertical module spacing Located inside IceCube-DeepCore Joshua Hignight IC Upgrase/KM3NeT August 9th, 2019 11 / 22 IceCube Upgrade: Modules D-EGG: 2x8-inch PMTS, slimmer design, improved UV acceptance mDOM: 24x3-inch PMTs, better directional coverage pDOM: IceCube PMT and glass, improved electronics Joshua Hignight IC Upgrase/KM3NeT August 9th, 2019 12 / 22 IceCube Upgrade: Calibration POCAM Reduce primary systematic Piezo-module uncertainties I Better calibration of new and existing sensors I Improved knowledge of glacial ice Integrated devices I LED flashers I Acoustic sensors I Optical cameras CCD CMOS Stand-alone light sources I Precision Optical Calibration Module (POCAM) I ns-pulse LEDs with small opening angle Joshua Hignight IC Upgrase/KM3NeT August 9th, 2019 13 / 22 IceCube Upgrade: Calibration Will have better angular resolution I Median error not scaling with photon statistics in IceCube Will have better Ice modeling systematic uncertainties I Bubble column distorts angular acceptance I Anisotropy of photon scattering and/or absorption lengths in ice New calibrations will be applied to the entire accumulated IceCube data set Joshua Hignight IC Upgrase/KM3NeT August 9th, 2019 14 / 22 IceCube Upgrade: HE Science New calibration devices inside IceCube enhance HE science Can simulate tau neutrino “double bang” events with baselines of 20m Joshua Hignight IC Upgrase/KM3NeT August 9th, 2019 15 / 22 NMO with ORCA ORCA should be able to measure the NMO at 3σ or better after 3 years. The IceCube Upgrade will be able to reach 2σ in the same time scale. ≈ Joshua Hignight IC Upgrase/KM3NeT August 9th, 2019 16 / 22 ντ Appearance Both ORCA and the IC Upgrade can constrain the Nντ to 10% with 1 year of data. < 7% precision on the ντ normalization after 3 years. 10% precision needed ∼ for real tests of the unitarity of the PMNS mixing matrix. Very few experiments can do this measurement! Joshua Hignight IC Upgrase/KM3NeT August 9th, 2019 17 / 22 νµ Disappearance NOvA 2019 (90%) 0.0032 T2K 2018 (90%) SuperK 2018 (90%) 0.0030 MINOS 2016 (90%) DeepCore 3 yr 2018 (90%) IceCube Upgrade 3 yr sensitivity (90%) 0.0028 ] 2 V e [ 0.0026 2 2 3 m 0.0024 0.0022 0.0020 IceCube Work in Progress 0.30 0.35 0.40 0.45 0.50 0.55 0.60 0.65 0.70 2 sin ( 23) 2 2 Can reach 3-5% precision on ∆m32 and 4-10% on sin (θ23) after 3 years. Joshua Hignight IC Upgrase/KM3NeT August 9th, 2019 18 / 22 KM3NeT Deployment Joshua Hignight IC Upgrase/KM3NeT August 9th, 2019 19 / 22 IceCube Upgrade/Gen-2 Timeline Joshua Hignight IC Upgrase/KM3NeT August 9th, 2019 20 / 22 Joshua Hignight IC Upgrase/KM3NeT August 9th, 2019 21 / 22 KM3NeT Talks Used for Preporation J. Hofestädtm, ICRC 2019 (link) C. Distefano, ESP-HEP 2019(link) J. Brunner, PANE 2018 (link) KM3NeT LOI (link) Joshua Hignight IC Upgrase/KM3NeT August 9th, 2019 22 / 22 Backup Joshua Hignight IC Upgrase/KM3NeT August 9th, 2019 23 / 22 IceCube Gen2: Sunflower 240m Joshua Hignight IC Upgrase/KM3NeT August 9th, 2019 24 / 22 IceCube Upgrade DeepCore Upgrade Joshua Hignight IC Upgrase/KM3NeT August 9th, 2019 25 / 22 IceCube Upgrade: Science Goals DeepCore Better neutrino astronomy at high energies I Improved angular resolution and veto performance I ντ identification I Multi-messenger astronomy ντ appearance analysis I PMNS unitarity tests 2 2 Upgrade Precision measurements of sin (θ23) and ∆m32 I Octant/Maximal mixing I Complementary to LBL experiments Neutrino mass ordering at 1.5-2σ in 3 years Improvement on eV sterile ν searches, NSI, solar dark matter searches, and other BSM searches Joshua Hignight IC Upgrase/KM3NeT August 9th, 2019 26 / 22 IceCube Upgrade: Oscillation Physics ORCA KM3NeT-ARCA 1023 7 Solar Potential L̥ Latm 10 1022 PINGU IceCube DUNE (High Energy) 6 NO νA 10 MINOS/OPERA/ICARUS KamLAND T2K ] 21 10 K2K –1 105 JUNO Super-Kamiokande [m] RENO-50 L [GeV 1020 L tau production 104 DAE δALUS threshold 1019 Daya Bay 3 Double CHOOZ 10 RENO 1018 10-3 10-2 10-1 100 101 102 103 Eν [GeV] IceCube probes oscillation physics at baselines and energies inaccessible to LBL or reactor neutrino experiments. Joshua Hignight IC Upgrase/KM3NeT August 9th, 2019 27 / 22 PINGU 2.4m2.4m Joshua Hignight IC Upgrase/KM3NeT August 9th, 2019 28 / 22 PINGU: Science Goals Augmenting the low-energy program of the upgrade. I 70k up-going atmospheric neutrinos per year ∼ Neutrino mass ordering ντ appearance 2 sin (θ23) octant sensitivity Wide breadth of other science: I Dark matter searches I Earth tomography I SN I ... Joshua Hignight IC Upgrase/KM3NeT August 9th, 2019 29 / 22 PINGU: Neutrino Mass Ordering Neutrinos Anti-Neutrinos Normal hierarchy (NH) Inverted hierarchy (IH) Joshua Hignight IC Upgrase/KM3NeT August 9th, 2019 30 / 22 PINGU: Neutrino Mass Ordering PINGU cannot differentiate ν and ν¯: rely on difference in flux and cross-section I Large statistical samples: 33k νµ + ν¯µ CC per year, 25k νe + ν¯e CC per year ∼ ∼ Distinct ordering dependent signatures for tracks (mostly νµ CC) and cascades I Intensity is statistical significance of each bin with 1 year data I Particular expected “distortion pattern” helps mitigate impact of systematics Joshua Hignight IC Upgrase/KM3NeT August 9th, 2019 31 / 22 PINGU: Neutrino Mass Ordering 12 7 IO median sensitivity 68% CL (stat.) 95% CL (stat.) 11 NO median sensitivity 68% CL (stat.) 10 6 95% CL (stat.) 9 5 ) ) 8 r r y y 7 4 4 4 6 ( ( 5 σ σ 3 n n 4 3 2 2 1 1 NuFit v2.0 NO best NuFit v2.0 IO best 0 0 0.40 0.45 0.50 0.55 0.60 0.65 0.40 0.45 0.50 0.55 0.60 0.65 2 2 sin θ23 sin θ23 Sensitivities calculated with 2 different methods (LLR and ∆χ2) in agreement 2 NMO sensitivity strongly depends on true sin (θ23) Median sensitivity of 3σ with 4 years of data for current best-fit values ∼ I Current global best fit close to sensitivity minimum for both orderings! Joshua Hignight IC Upgrase/KM3NeT August 9th, 2019 32 / 22 PINGU: ντ Appearance Expected to reach 5σ exclusion of no ντ appearance with a month of data I Can even reach 5σ exclusion of no ντ appearance within a year if ντ normalization is 0.6.