measuring the low energy solar neutrino spectrum lens-sol snolab workshop, sudbury, aug 15, 2005
Post on 15-Jan-2016
23 Views
Preview:
DESCRIPTION
TRANSCRIPT
Measuring the Low Energy Solar Neutrino SpectrumLENS-Sol
SNOLAB Workshop, Sudbury, Aug 15, 2005
R. S. RaghavanVirginia Tech
LENS-Sol GOAL: Experimental Measurement of the Neutrino Luminosity of the Sun (3-4%)
Measure the low energy neutrino spectrum (pp, Be, …) in real time & with precision
Exptal Tool: Tagged CC Nu Capture in Indium
νe + 115In e- + (delay) 2 γ + 115Sn
solar signal tag
115In ( 95.7%) = 6.4x1014 y
115Sn
B(GT) = 0.17; Q=114
e1
(e/)2 115.6 (e/ = 0.96)
3 497.3
115 In(p,n)100.8 (e/ =5.7)
= 4.76 s
max = 498.8
= 16 ps
= 231s
9/2+
1/2+
3/2+
7/2+
11/2-
0
497.3
612.8
713.6
7/2+ 1857
B(GT) ~0.01; Q =1362
e
115In ( 95.7%) = 6.4x1014 y
115Sn
B(GT) = 0.17; Q=114
e1
(e/)2 115.6 (e/ = 0.96)
3 497.3
115 In(p,n)100.8 (e/ =5.7)
= 4.76 s
max = 498.8
= 16 ps
= 231s
9/2+
1/2+
3/2+
7/2+
11/2-
0
497.3
612.8
713.6
7/2+ 1857
B(GT) ~0.01; Q =1362
e
The Indium Low Energy Neutrino Tag
115In ( 95.7%) = 6.4x1014 y
115Sn
B(GT) = 0.17; Q=114
e1
(e/)2 115.6 (e/ = 0.96)
3 497.3
115 In(p,n)100.8 (e/ =5.7)
= 4.76 s
max = 498.8
= 16 ps
= 231s
9/2+
1/2+
3/2+
7/2+
11/2-
0
497.3
612.8
713.6
7/2+ 1857
B(GT) ~0.01; Q =1362
e
115In ( 95.7%) = 6.4x1014 y
115Sn
B(GT) = 0.17; Q=114
e1
(e/)2 115.6 (e/ = 0.96)
3 497.3
115 In(p,n)100.8 (e/ =5.7)
= 4.76 s
max = 498.8
= 16 ps
= 231s
9/2+
1/2+
3/2+
7/2+
11/2-
0
497.3
612.8
713.6
7/2+ 1857
B(GT) ~0.01; Q =1362
e
The Indium Low Energy Neutrino Tag
LENS-Sol-- Low Energy Solar Nu Spectroscopy via Indium --Basics
CC Nu Capture in 115In to excited isomer in 115Sn
Tag: Delayed emission of 2 γ’s
Threshold: 114 keV pp Nu
115In abundance: ~96%
Basic Bgd Challenge:Natural β-radioactivity of In•In β-Spectrum overlaps pp signal (Be, CNO not affected• β max energy = tag energy
R.S.Raghavan/VT/June05
LENS-Sol Signal= [SSM(low CNO)+LMA] xDetection Efficiency:
pp ~40%; Be 85%; pep 90%Rate: pp 25 /y /t In
For pp ± 3%, need 2000 ev. / 5y
Signal Electron Energy (MeV)
Expected Result:
Nu- capture Signature: Isomeric Coincidence decay with τ =4.76 µsBgd measured concurrently with signal
S/N~1 AdequateFor Precision Flux
S/N=1
S/N=3
2000 pp events (0-10 µs) generated:Fit S=2044±62; (3.1%) S/N=1 (in 0-10µs)Fit S=2031±51; ( 2.5%) S/N=3
Random coinc bgd signal
pp 7Be
pepCNO
Detector ResolutionIncluded (800 pe/MeV)
~10 keV det. threshold
LENS: Studied world wide since 1976 !- Dramatic Progress in 2005-
2004 2005
Longitudinal modules + hybrid design
• In: 30 ton for 1900 pp’s /5y
• Total mass LS: 6000 ton
• PMTs: ~200,000
or
Cube lattice or non-hybrid longitudinal modular design
• In: 14 ton for 1970 pp’s /5y
• Total mass In LS : ~175 ton
• PMTs: ~6,500 ( MPIK Talk at DPG 03/2004)
LENS Progress- - How?--
Major Advances in Scintillator Chemistry Absorption length ~ 1.5m @ 5% In > 10m @ 8% In Module size: ~ 1.5m ~ 6m Photoelectron yield:~ 230 pe/MeV ~ 900 pe/MeV + high energy resolution:
• Structure of internal 115In Bgd: partial study (1 component) complete study (5-6 comps.) only single- decay with BS multi- decays with or w/o BS considered 498keV from decay to 115Sn*
(single- decay not dominant!)
• New Insights in Analysis Strategy Old: pp-efficiency: ~ 20% New: ~ 45% Signal/Noise: ~ 1 ~ 3
• New Detector design: Design: Hybrid Hybrid design obsolete Longitudinal modules - Cube lattice - Event location analog- via PMT timing Event location digital
2004 2005
Components of Indium radioactive bgd
In115
Sn115
β0 , γ0 (BS) (Emax = 498 keV)
β1 (Emax< 2 keV)(1.2x10-6)*
498 keVBGD
0-300(e1)
116 (g2)
498(g3)
In SIGNAL
R.S.Raghavan/VT/June05
* Cattadori et al (2003) SnIn tag search volume around vertex of initial beta, occurrence ofa random event with minimum Nhit =3 1 beta decay: A1 = beta + BS gamma (Etot = 498 keV) A2 = 498 gamma 2 beta decays in random coinc: B = beta, BS or 498 in any
combination from each beta decay 3 beta decaysin random coinc : C = 3 betas mostly 4 beta decays in random coinc: DOnly A1 considered previously
* Cattadori et al: 2003
Signal
/ton In/y
In Bgd
/ton In/y
A1 A2 B
RAW 62.5
(singles)75x1011
(Singles)
Time, Space Coinc. (Granularity: 35g/ton)
62.5 2.8x105 8.5x104 3.3x103 1.9x105
+ Min 3 Hits 58 3x104 2.6x104 3x103 1.4x103
+Tag Energy 53.5 3x102 2 6 290
+Tag topology 32 10.6 1.6 5 4
Bgd Reduction Factor ~1011
Signal Loss Factor ~2
Role of Experimental Tools in Bgd Suppression in LENS-Sol
Basic Experimental Tools
•Detection Technology: In loaded liq. Scintillator (InLS) (E resln)Advances in Scint. Chemistry
•DetectorArchitecture: Segmented /Granularity ~1kg/100 tonNew Design
•Bgd Suppression at high Det. EfficiencyNew Analysis Strategy
1
10
100
1000
10000
0 50 100 150 200 250
InLS (PC:PBD/MSB): 10800 hν / MeV
BC505 Std12000 hν/MeV
In 8%-photo
Light Yield from Compton edges of 137Cs γ-ray Spectra
PCNEAT
ZVT27; Abs/10cm=0.004; L(1/e)=10.8 m
ZVT28,32: Abs/10cm=0.02; L(1/e)~20m
In LS Status (July ‘05) – Summary
1 Indium conc. ~8 wt% (higher may be viable)2.Scintillation signal eff (typical): 9000 hν/MeV3.Transparency at 430 nm: L(1/e) (typical): 10 m4.Chemical and Optical Stabililty: ~ 2 years5. InLS Chemistry Robust (>1000 syntheses )
Milestones unprecedented in metal LS technology
R.S.Raghavan/VT/Aug 05
Detector Design:---Segmented
Objective: Moderate Granularity (~1kg/100 T)
Two Approaches for close packed architecture: •Longitudinal Modules (“classical”)•Scintillation Lattice (3-D) (new)
Both Designs under studyScintillation Lattice Design Detailsin this talk
R.S.Raghavan/VT/June05
GEANT
NEW DETECTOR CONCEPT—SCINTILLATION LATTICE (RSR ’93)
Concept Simulation: ideal optics
•Light output 75% (6PMT) vs 50% (2PMT) in long. modules•Precise 3D Digital Event Localization ~10cm v. 60 cm (±2σ) in longitudinal modules•Event localization independent of event energy •Particle tracks, γ-ray shower structure directly seen
•reconstructed hit times reduced randoms
Perfect optical surfaces Ideal optics: 20 pe
rough optical surfaces:20% of light with non-ideal optics:12 pe in vertex + 4pe in “halo”
1211
1
10.750.75
0.75
0.75
11.75 1 0.751211
1
10.750.75
0.75
0.75
11.75 1 0.75
Vertex definition in non-smooth optical channels
12.5 cm cells in 4x4x4m cube
100 keV event /9000 pe/MeV
Total signal 6x16=96 pe
7.5cm cells 700 pe/MeV
12.5cm cells 950 pe/MeV
18cm cells—1100 pe/MeV
5x5x5m Cube
Analysis
Basic Constraining Tools: (key for (A1, A2)
1. Total Shower Energy of tag candidate (g2 energy in vertex wide open)
2. No. of hits in tag candidate shower
(key for B, C, D…) 3. Shower sphere radius 4. Maximum inter-hit distance 5. e1-g2 coincidence window 10µs
R.S.Raghavan/VT/June05
nu events
g2+g3
Total Tag Energy
BS>450 kev
498
Before Cuts
Nu
Bgd
After Cuts
Nu
Bgd
Surviving bgd different fordifferent Nhit showersNew Analysis Paradigm (VT)Apply progressively less tight cuts for larger NhitIncreased detection Efficiency and lower bgd
R.S.Raghavan/VT/June05
Analysis Strategies:
Basic selection: Events with given NhitEvery hit in candidate event is a possible vertex with a previous beta in that cell to mimic nu event
NEW ANALYSIS STRATEGYClassify events according to NHitOptimize cut conditions separately for each class
19.3
15.3
10
Mass for
2000 ev/5y
(pp flux3%)
T (In)
22
9
13
Bgd
Rate /T In/y
20.7
26
40
Nu Rate /T In/y
33.1
41.8
64
Det Eff
%
1801000
pe/MeV
125950pe/MeV
751000
pe/MeV
Cell
Size (mm x mm x
mm)
2401
1902.9
1253
S/N
T (InLS)
LENS-Sol: DESIGN FIGURES OF MERIT (Lattice Architecture)4mx4mx4m supermodules: InLS: 8% In; L(1/e) =1000cm; Y= 9000hν/MeV;
R.S.Raghavan/VT/June05
g2
g2+g3
Shower Rad.
R.S.Raghavan/VT/June05
NEW SCIENCE—Discovery Potential of LENSSolar Nu spectrum <5 MeV Yet UNOBSERVED after 40 y of solar nu’s !!!
APS Nu Study 2004 Lo Energy Solar Nu Spectrum: one of 3 Priorities
R.S.Raghavan/VT/June05
In First two years of Data (No source Calib needed)• Proof of MSW LMA Physics from Pee of pp & Be nu --No proof yet! (no d/n effect, spectral shape a problem?)• Non-standard Fundamental Interactions?• CPT Invariance of nus ?• RSFP/ Nu magnetic moments—Time dependence?
In Five Years (with source Calib): pp Be fluxes measured to 3%First Exptal test of Neutrino Luminosity Photon Luminosity Ultimate test of Neutrino Physics and Solar Astrophysics Neutrino Physics: Precision Measurement of θ12 θ13
Sterile Neutrinos?Astrophysics: Is the Sun getting Hotter? Hidden new source of energy of Sun?
Summary•Major breakthroughs in• In LS technoloy• Detector Design• Analysis and Background Simulations Conceptual feasibility of In-based LENS secure
•Simple Small ( < 10 t In /125 ton InLS)• LENS in view
•Next Steps—Work in Progress
•Chemical Technology of large scale InLS production•Detector construction technology•
R.S.Raghavan/VT/June05
VT-NRL Low Bgd Laboratory @ Kimballton Mine VA
VT-NRL Low Bgd Laboratory Floor Plan
LENS-Sol / LENS-Cal Collaboration (US-Russia) (2004---)
Russia:Institute of Nuclear Research (INR Mosow)I. Barabanov, L. Bezrukov, V. Gurentsov, V. Kornoukhov, E. YanovichINR (Troitsk)V. Gavrin et al; A. Kopylov et al
U. S.BNLA.Garnov, R. L. Hahn, M. YehORNL J. Blackmon, C. Rascoe, A. Galindo-UrribariPrinceton:J. BenzigerU. North CarolinaA.ChampagneV. T. Z. Chang, C. Grieb, M. Pitt, RSR, R.B. Vogelaar
R.S.Raghavan/VT/June05
Additional Slides
top related