Sampling Detectors for e Detection and Identification Adam Para, Fermilab NuFact02 Imperial College...
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![Page 1: Sampling Detectors for e Detection and Identification Adam Para, Fermilab NuFact02 Imperial College Interest de jour: what is sin 2 2 13 oscillations.](https://reader036.fdocuments.net/reader036/viewer/2022062518/56649e725503460f94b7098e/html5/thumbnails/1.jpg)
Sampling Detectors for e Detection and Identification
Adam Para, Fermilab
NuFact02
Imperial College
Interest de jour: what is sin2213 • oscillations -> e
• ‘superbeams’
• ‘Current’ generation of experiments
• How can we do better
• Sampling detectors for e detection
![Page 2: Sampling Detectors for e Detection and Identification Adam Para, Fermilab NuFact02 Imperial College Interest de jour: what is sin 2 2 13 oscillations.](https://reader036.fdocuments.net/reader036/viewer/2022062518/56649e725503460f94b7098e/html5/thumbnails/2.jpg)
Different baselines: where the oscillation peaks are ?
L(km)/n 1 2 3
300 0.73 GeV
0.24 GeV
0.15 GeV
750 1.82 GeV
0.60 GeV
0.36 GeV
1500 3.64 GeV
1.21 GeV
0.73 GeV
E < 1 GeV (KEK/JHF to SuperK, CERN to Frejus
0.3 < E < 3 GeV (NuMI)
0.5< E < 6 GeV (CERN to Taranto, BNL to ?)
Flux/rates drop
![Page 3: Sampling Detectors for e Detection and Identification Adam Para, Fermilab NuFact02 Imperial College Interest de jour: what is sin 2 2 13 oscillations.](https://reader036.fdocuments.net/reader036/viewer/2022062518/56649e725503460f94b7098e/html5/thumbnails/3.jpg)
Neutrino Cross Sections
N+leptonN+l+
Many particles
![Page 4: Sampling Detectors for e Detection and Identification Adam Para, Fermilab NuFact02 Imperial College Interest de jour: what is sin 2 2 13 oscillations.](https://reader036.fdocuments.net/reader036/viewer/2022062518/56649e725503460f94b7098e/html5/thumbnails/4.jpg)
Det. 2
What will MINOS do?
Two functionally identical neutrino detectors
Det. 1
![Page 5: Sampling Detectors for e Detection and Identification Adam Para, Fermilab NuFact02 Imperial College Interest de jour: what is sin 2 2 13 oscillations.](https://reader036.fdocuments.net/reader036/viewer/2022062518/56649e725503460f94b7098e/html5/thumbnails/5.jpg)
e Interactions in MINOS?
NC, Eobs = 3 GeVe CC, Etot = 3 GeV
NC interactions:
Energy distributed over ‘large’ volume
Detector Granularity:
•Longitudinal: 1.5X0
•Transverse: ~RM
e CC interactions (low y) :•Electromagnetic shower:
•Short•Narrow
•Most of the energy in a narrow cluster
energy
![Page 6: Sampling Detectors for e Detection and Identification Adam Para, Fermilab NuFact02 Imperial College Interest de jour: what is sin 2 2 13 oscillations.](https://reader036.fdocuments.net/reader036/viewer/2022062518/56649e725503460f94b7098e/html5/thumbnails/6.jpg)
Needle in a Haystack ? NC Background
e (|Ue3|2 = 0.001)e background
NC (visible energy), no rejection
spectrumSpectrum mismatch: These neutrinos contribute to background, but no signal
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MINOS Limits on to e Oscillations
Sample of e candidates defined using topological cuts
10 kton-yr exposure,
m2=0.003 eV2, |Ue3|2=0.01:
Signal (= 25%) - 8.5 ev
e background - 5.6 ev
Other (NC,CC,) – 34.1 ev
M. Diwan,M. Mesier, B. Viren, L. Wai, NuMI-L-
714
90% CL: | Ue3|2< 0.01
Limit comparable to a far superior detector (ICARUS) in CNGS beam
![Page 8: Sampling Detectors for e Detection and Identification Adam Para, Fermilab NuFact02 Imperial College Interest de jour: what is sin 2 2 13 oscillations.](https://reader036.fdocuments.net/reader036/viewer/2022062518/56649e725503460f94b7098e/html5/thumbnails/8.jpg)
Receipe for a Better Experiment
More neutrinos in a signal region Less background Better detector (improved efficiency, improved rejection
against background) Bigger detector
Lucky coincidences:
• distance to Soudan = 735 km, m2=0.025-0.035 eV2
• Below the tau threshold! (BR(->e)=17%)
2 21.27 2.541.6 2.2
2
m L m LE GeV
E
![Page 9: Sampling Detectors for e Detection and Identification Adam Para, Fermilab NuFact02 Imperial College Interest de jour: what is sin 2 2 13 oscillations.](https://reader036.fdocuments.net/reader036/viewer/2022062518/56649e725503460f94b7098e/html5/thumbnails/9.jpg)
Two body decay kinematics
* * *
* *
( cos )
sin
L
T
p p E
p p
‘On axis’: E=0.43E
At this angle, 15 mrad, energy of produced neutrinos is 1.5-2 GeV for all pion energies very intense, narrow band beam
![Page 10: Sampling Detectors for e Detection and Identification Adam Para, Fermilab NuFact02 Imperial College Interest de jour: what is sin 2 2 13 oscillations.](https://reader036.fdocuments.net/reader036/viewer/2022062518/56649e725503460f94b7098e/html5/thumbnails/10.jpg)
Off-axis ‘magic’ ( D.Beavis at al. BNL Proposal E-889)
2
2
22 412
zA
Flux
1-3 GeV intense beams with well defined energy in a cone around the nominal beam direction
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NC/ e /0 detectors
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CHARM II (e scattering)
Challenges: Identify electrons Small cross section,
large background from NC interactions
Solution:
•Low Z, fine grained calorimeter
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Detector(s) Challenge
Surface (or light overburden) High rate of cosmic ’s Cosmic-induced neutrons
But: Duty cycle 0.5x10-5
Known direction Observed energy > 1 GeV
Principal focus: electron neutrinos identification
• Good sampling (in terms of radiation/Moliere length)
Large mass:
• maximize mass/radiation length
• cheap
![Page 14: Sampling Detectors for e Detection and Identification Adam Para, Fermilab NuFact02 Imperial College Interest de jour: what is sin 2 2 13 oscillations.](https://reader036.fdocuments.net/reader036/viewer/2022062518/56649e725503460f94b7098e/html5/thumbnails/14.jpg)
A possible detector: an example
Cheap low z absorber: recycled plastic pellets
Cheapest detector: glass RPC (?)
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Constructing the detector ‘wall’
Containment issue: need very large detector Engineering/assembly/practical issues
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On the Importance of the Energy Resolution
M. Messier, Harvard U.
Cut around the expected signal region too improve signal/background ratio
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Energy resolution vis-à-vis oscillation pattern
First oscillation minimum: energy resolution/beam spectrum ~ 20% well matched to the width of the structure
Second maximum: 20% beam width broader than the oscillation minimum, need energy resolution <10%. Tails??
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Energy Resolution of Digital Sampling Calorimeter
Digital sampling calorimeter:
1/3 X0 longitudinal 3 cm transverse
Energy = Cx(# of hits) DE ~ 15% @ 2 GeV DE ~ 10% 4-10 GeV ~15% non-linearity @
8 GeV, no significant non-gaussian tails
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Improve energy resolution?
Total Absorption Calorimeter: HPWF
Energy resolution limited by fluctuations of the undetected energy: nuclear binding energy, neutrinos and not by sampling fluctuations
‘Crude’ sampling calorimeter (CITFR), 10 cm steel, better energy resolution than total absorption one (HPWF)
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Neutrino energy, Quasi-elastics ?
E(reconstruct) – E (True) (MeV)
=80MeV
E(
reco
nst
ruct
)
events
cos
22
pEm
mEmE
N
N
+ n → + p
p
(E , p)
![Page 21: Sampling Detectors for e Detection and Identification Adam Para, Fermilab NuFact02 Imperial College Interest de jour: what is sin 2 2 13 oscillations.](https://reader036.fdocuments.net/reader036/viewer/2022062518/56649e725503460f94b7098e/html5/thumbnails/21.jpg)
~ 2 GeV: CC e / NC interactions
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~ 2 GeV: CC interaction
![Page 23: Sampling Detectors for e Detection and Identification Adam Para, Fermilab NuFact02 Imperial College Interest de jour: what is sin 2 2 13 oscillations.](https://reader036.fdocuments.net/reader036/viewer/2022062518/56649e725503460f94b7098e/html5/thumbnails/23.jpg)
~ 7 GeV: CC e / NC interactions
![Page 24: Sampling Detectors for e Detection and Identification Adam Para, Fermilab NuFact02 Imperial College Interest de jour: what is sin 2 2 13 oscillations.](https://reader036.fdocuments.net/reader036/viewer/2022062518/56649e725503460f94b7098e/html5/thumbnails/24.jpg)
CC e vs NC events: example
Electron candidate: Long track ‘showering’ I.e. multiple
hits in a road around the track
Large fraction of the event energy
‘Small’ angle w.r.t. beam
NC background sample reduced to 0.3% of the final electron neutrino sample (for 100% oscillation probability)
35% efficiency for detection/identification of electron neutrinos
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Detector questions/issues
What is the optimal absorber material (mostly an engineering/cost question, if X0 kept constant)
What longitudinal sampling (X0)? What is the desired density of the detector?
(containment/engineering/transverse segmentation) Containment issues: fiducial volume vs total volume,
engineering issues: what is the practical detector size? What is the detector technology (engineering/cost issue
if transverse segmentation kept constant) What is the optimal transverse segmentation (e/p0,
saturation,…) Can a detector cope with cosmic ray background? What
is the necessary timing resolution?