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Review of experimental results on atmospheric neutrinos. Univ. of Tokyo, Kamioka Observatory Masato Shiozawa. Introduction Super-Kamiokande MACRO Soudan 2 Summary. C Scientific American. Super-Kamiokande detector. Water Cherenkov detector. 1000 m underground - PowerPoint PPT Presentation
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Jan.-2002 @CERN
Review of experimental results on atmospheric neutrinos
Introduction Super-Kamiokande MACRO Soudan 2 Summary
Univ. of Tokyo, Kamioka ObservatoryMasato Shiozawa
Jan.-2002 @CERN
Super-Kamiokande detector
39.3 m
42 m
Water Cherenkovdetector
1000 m underground 50,000 ton (22,500 ton fid.) 11,146 20 inch PMTs 1,885 anti-counter PMTs
C Scientific American
Jan.-2002 @CERN
Phase-1 quick restart of K2K rebuild SK with about half PMT density by autumn of 2002 atmospheric ν, proton decay search solar ν, SN watch with higher energy threshold PMT vessel to prevent from chain reaction of explosion
Phase-2 full detector before the time of commissioning of JHF
Rebuilding Super-K
acrylic vessel acrylic+(FRP or stainless steel)
Jan.-2002 @CERN
Event classification of atmospheric ν
e/e/
Fully Contained (FC) Partially Contained (PC)
Upward through-going
Upward stopping
Contained event(sub-GeV, multi-GeV sample)
Eν ~ 1 GeV Eν ~ 10 GeV
Eν ~ 10 GeV (stop μ ) 100 GeV (through μ )
Jan.-2002 @CERNZenith angle distributions(FC+PC+up-μ)
No oscillation (χ2
=393.4/172 d.o.f)
Best fit (m2=2.5x10-3eV2,sin22=1.00 χ2
min=157.5/170 d.o.f)νμ⇔ντ 2-flavor oscillations
~ 15km~ 13000km~ 500km ~ 13000km ~ 500km
Jan.-2002 @CERN
Combined allowed regions
→
Super-KamiokandeBest fit(Δm2=2.5×10-3,sin22θ=1.0
χ2min=157.5/170 d.o.f)
No oscillation
(χ2 =393.4/172 d.o.f)
Δm2 = (1.6 ~ 3.6)x10-3eV2
sin22θ > 0.9 @ 90%CL
Jan.-2002 @CERN
νμ⇔ντorνμ⇔νsterile?
Using MSW effect and enriched NC sample
→: No matter effect / NC interaction
→s : With matter effect / No NC interactionNeutrino oscillation in matter:
( ) = ( cosm
s
sinm
- sinm cosm ) 1 2( ) sin22m
sin22=
(cos2sin22= 2 GFnnE / m2 √
For sin22= 1
sin22m1~ + 1
And for E = 30~100 GeV ≫1 andsin22m≪1 Suppression !
Test zenith angle of NC enriched events, high energy PC and through-going muon events.
A
llow
ed
reg
ion
fro
m F
C s
ing
le-r
ing
sam
ple
Jan.-2002 @CERN
νμ⇔ντorνμ⇔νsterile?
→s
→Evis> 5 GeV
<E>=~25 GeV
Zenith angle of high-E PC
up
/dow
n r
ati
o
cosΘ
→s
→
1 checking matter effect (partially contained events)
Up/down ratio of high-E PC
10-3 10-2
Δm2
Jan.-2002 @CERN
νμ⇔ντorνμ⇔νsterile?
→s
→
2 checking matter effect (upward through going μ)
Zenith angle of up through μ
cosΘ
vert
ical/
hori
zon
tal ra
tio
→
→s
V/H ratio of up through μ
10-3 10-2
Δm2
Jan.-2002 @CERN
νμ⇔ντorνμ⇔νsterile?
→s
→
3 checking NC enriched sample (multi-ring events)
Zenith angle of NC sample Up/down ratio of NC sample
cosΘ
up
/dow
n r
ati
o →
→s
10-3 10-2
Δm2
pu
re ν
μ⇔
νste
rile o
scilla
tion
sare
dis
favore
d w
ith
ab
ou
t 9
9%
CL
99%
CL e
xclu
ded
90%
CL e
xclu
ded
E
xclu
ded
reg
ion
f
rom
th
ree t
est
sam
ple
s
Jan.-2002 @CERN
Neutrino Decay
Neutrino Decay is a possible solution of the atmospheric neutrino problem (V.Barger et al.)
2
3
322μμ ))
E
L
2τ
mexp(sin(cos)νP(ν Survival probability without
neutrino oscillation(Δm2<<1)
FC 1-ring + PC + up-μdata are consistentwith neutrino decayscenario χ2
min=147.0/152 dof
Jan.-2002 @CERNNeutrino Decay study with NC enriched sample
Deficit of up-going NCevents is expected forν decay scenario
)0.07(stat.1.06down
up
data
perform χ2 test to constrain neutrino decay parameters
Jan.-2002 @CERN
Result on neutrino decay study
The 99%CL allowed region by FC 1-ring+PC+up-μ sampleis excluded at 99%CL by the NC enriched sample.
Jan.-2002 @CERNUpdate of neutrino crosssection(very preliminary)
c22
F2N2
QE θcosGMdq
dσ
Update parameters GF=1.16639×10-5
sinθc=0.22 ↓σ is increased by 5.8% (energy indep.)
free proton target bound nucleon target
blue newMagenta old
μν
μν
μν
blue newMagenta old
Jan.-2002 @CERNUpdate of neutrino flux(very preliminary)
HONDA 1D (official)
Fluka 3D
HONDA 3D (new) 3D calculation dpmjet3 interaction model primary flux from BESS/AMS Ikenoyama effect
sub-GeV e
multi-GeV μmulti-GeV e
sub-GeV μ
Jan.-2002 @CERN
MACRO detector76.6m×12m×9.3m
streamer tubes
liq. scintillation counters(TOF system)
Jan.-2002 @CERN
Up throughgoing muons in MACRO
Obs. 863evObs. 809ev(BG sub.)Exp. 1122ev.(Bartol)
Obs./Exp.=0.721±0.026(stat)±0.043(sys)±0.123(th)
Jan.-2002 @CERN
90% allowed region from MACRO
χmin@(1.0,2.5×10-3eV2)
νμ⇔ντ
consistent with Super-K
Jan.-2002 @CERN
Low energy events in MACRO
Obs. 154ev.Exp. 285ev.Obs./Exp. = 0.54±0.04(stat)±0.05(sys)±0.13(th)
Obs. 262ev.(BG sub.)Exp. 375ev.Obs./Exp. = 0.70±0.04(stat)±0.07(sys)±0.17(th)
consistent with up throughgoing muon results
Th
e S
ou
dan
2
dete
cto
r
Fid
uci
al m
ass
: 7
70
ton
s
(Ar/
CO
2, 0.8
cm/μ
sec)
×224
Man
n@
neu
trin
o2
00
0
Jan.-2002 @CERN
HiRes event summary in Soudan 2
νμ νe
Obs. 114.0±10.7 140.0±11.8Obs.(Bgsub) 106.3±14.7 132.8±13.4Exp.(Bartol) 158.5±4.8 132.8±4.4 (renorm. to νe data)
HiRes sample Recoil proton + lepton(>150MeV/c) single lepton(>600MeV/c) multiprong (Evis>700MeV and |Σp|>450MeV/c)
R=(μ/e)data/ (μ/e)MC=0.67±0.12
Jan.-2002 @CERN
Soudan 2 allowed region
χmin@(0.9,7.9×10-3eV2)
consistent with Super-K
Jan.-2002 @CERNSummary of atmospheric ν observations
Atmospheric neutrinos are measured using various techniques in SK, MACRO, Soudan 2
→ all consistent with each other
Δm2=1.6 ~ 3.6×10-3, sin22θ>0.9 for νμ⇔ντ
sterile neutrino is disfavored as a prominent oscillation partner
neutrino decay scenario with Δm2<<1 is excluded at
99% C τ likelihood distributions