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Future supernova neutrino detectors Kate Scholberg, Duke University - - PowerPoint PPT Presentation
Future supernova neutrino detectors Kate Scholberg, Duke University - - PowerPoint PPT Presentation
Future supernova neutrino detectors Kate Scholberg, Duke University TAUP 2009 OUTLINE Brief summary of current detectors Near and medium term detectors Farther future mega-detectors What GW coincidence can add Current supernova neutrino
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Current supernova neutrino detectors
Detector Type Location Mass (kton) Events @ 8 kpc Status Super-K Water Japan 32 8000 Running (SK IV) LVD Scintillator Italy 1 300 Running KamLAND Scintillator Japan 1 300 Running Borexino Scintillator Italy 0.3 100 Running IceCube Long string South Pole 0.4/PMT N/A Running Baksan Scintillator Russia 0.33 50 Running Mini- BOONE Scintillator USA 0.7 200 Running
νe + p e+ + n
Primary sensitivity is to electron antineutrinos via inverse beta decay
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νe + 40Ar → e- + 40K*
- Tag modes with gamma
- spectrum (or lack thereof)
- Excellent electron
neutrino sensitivity
νe,x + e- → νe,x + e- νx + 40Ar → νx + 40Ar* CC NC ES
Ethr=1.5 MeV Ethr=7.48 MeV Ethr=1.46 MeV
Near term future experiments (~5 years)
ICARUS: 600 ton LAr
νe + 40Ar → e- + 40Cl* _
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Relative rates depend
- n ν energy
⇒ spectral sensitivity
νe + 208Pb → 208Bi* + e-
1n, 2n emission CC
νx + 208Pb → 208Pb* + νx
1n, γ emission NC
HALO at SNOLab
SNO 3He counters + 76 tons of Pb: ~85 events @ 10 kpc
from
- T. Massicotte
thesis
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NOνA: long baseline oscillation experiment (Ash River, MN)
15 kton scintillator, near surface
- K. Arms, CIPANP ‘09
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SNO+: SNO vessel filled with scintillator
~300 inverse beta decay events @ 10 kpc
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Current and near-future supernova neutrino detectors
Detector Type Location Mass (kton) Events @ 8 kpc Status Super-K Water Japan 32 8000 Running (SK IV) LVD Scintillator Italy 1 300 Running KamLAND Scintillator Japan 1 300 Running Borexino Scintillator Italy 0.3 100 Running IceCube Long string South Pole 0.4/PMT N/A Running Baksan Scintillator Russia 0.33 50 Running Mini- BOONE Scintillator USA 0.7 200 Running HALO Lead Canada 0.076 85 Under construction Icarus Liquid argon Italy 0.6 230 Almost ready NOνA Scintillator USA 15 3000 Construction started SNO+ Scintillator Canada 1 300 Funded
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- Ap. J, .669:519-524,2007, arXiv:0706.2283
Distant burst search:E> 17 MeV,≥ 2 ev/20 s Low threshold burst search: E>~ 7 MeV, ≥ 3 ev/0.5 s OR ≥ 4 ev/2 s OR ≥ 8 ev/10 s
Farthest distance reach: Super-K
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Current best neutrino detectors sensitive out to ~ few 100 kpc.. mostly just the Milky Way 3±1 per century
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How requiring a GW coincidence with a single SK event affects SK sensitivity: current SK burst search (require double) SK single event (bg: 1 ev/day) Improves probability of detection of supernova in Andromeda from 8% to 30% (and one could optimize search parameters to possibly do better)
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SK Mton
doubles singles{
Looking beyond: number of sources α D3
With Mton scale detector, probability of detecting 1-2 events reasonably close to ~1 at distances where rate is <~1/year Tagging signal over background becomes the issue ⇒ require double ν's or grav wave/optical coincidence
- S. Ando et al., PRL 95:171101, 2005:
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Next generation mega-detectors (10-20 years)
Megaton-scale water detector concepts
Memphys
100 kton-scale scintillator detector concepts 5-100 kton-scale LAr detector concepts
LENA, HanoHano Hyper-K
DUSEL LBNE
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Possible WC detector design: 100 kton modules
Studies underway to optimize detector parameters e.g. PMT coverage, Gd solute (for SN, want low threshold)
Zoom in on LBNE water Cherenkov detector
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Expected signal at 7 MeV threshold SN burst signal
CR µ (unvetoed)
- ther bg, scaled from SK
Clean signal out to Andromeda @ 4290 mwe
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Distance sensitivity for early alert (not physics) depends on:
Mass Background
rate λ λ
Eth~ 5 MeV ΔT = 10 s (ignoring correlated background like spallation)
Could provide early alert for SN in Andromeda assuming reasonable bg rejection
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Reach with GW coincidence Sensitivity enhancement from external trigger SK doubles 300 kt doubles 300 kt singles
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Elastic scattering off electrons is the best bet
POINTING from Cherenkov cone: (slightly degraded by isotropic bg)
νe,x + e- → νe,x + e-
In water Cherenkov few % of total rate
νe,x e-
POINTING
Individual experiments can use ASYMMETRIC REACTIONS (triangulation is hard)
- G. Raffelt
SK: expect ~200 ES for 8.5 kpc SN (5-10 from breakout) ⇒ ~ 4o pointing
DUSEL WC: <~ 1o pointing
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Summary of supernova neutrino detectors
G a l a c t i c s e n s i t i v i t y Extragalactic
Detector Type Location Mass (kton) Events @ 8 kpc Status Super-K Water Japan 32 8000 Running (SK IV) LVD Scintillator Italy 1 300 Running KamLAND Scintillator Japan 1 300 Running Borexino Scintillator Italy 0.3 100 Running IceCube Long string South Pole 0.4/PMT N/A Running Baksan Scintillator Russia 0.33 50 Running Mini- BOONE Scintillator USA 0.7 200 Running HALO Lead Canada 0.076 85 Under construction Icarus Liquid argon Italy 0.6 230 Almost ready NOνA Scintillator USA 15 3000 Construction started SNO+ Scintillator Canada 1 300 Funded DUSEL LAr Liquid argon USA 5 1900 Proposed DUSEL WC Water USA 300 78,000 Proposed MEMPHYS Water Europe 440 120,000 Proposed Hyper-K Water Japan 500 130,000 Proposed LENA Scintillator Europe 50 15,000 Proposed GLACIER Liquid argon Europe 100 38,000 Proposed
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