physics of atmospheric neutrinos (introductory...

27
V. A. Naumov Physics of Atmospheric Neutrinos Abstract The lecture reviews the physics of neutrino production in the atmosphere, the detection methods, and the results obtained with large underground neutrino detectors. Contents of the lecture. 1. Introduction. The role of atmospheric neutrinos (AN) in astroparticle physics. 2. Mechanisms and the main features of neutrino production in the earth's atmosphere at low, intermediate, and high energies. 3. A short review of calculational methods. 4. Sketch of numerical results. Comparison between different models and analysis of uncertainties. 5. Verification of the AN flux calculations with the cosmic-ray secondaries in the atmosphere and ground level. 6. Underground muons as a tool for the AN flux normalization. 7. Detection methods. Description of the largest underground neutrino detectors. Neutrino-induced events classification. 8. Search for neutrino oscillations in underground experiments. 9. Results from the detectors Kamiokande, IMB, NUSEX, Frejus, SOUDAN 2, MACRO, and Super-Kamiokande. Interpretation of the data in terms of neutrino oscillations. 10. Other explanations (proton decay, neutrino decay, FCNC, neutron background, etc). 11. Conclusions.

Upload: others

Post on 03-Oct-2020

4 views

Category:

Documents


0 download

TRANSCRIPT

Page 1: Physics of atmospheric neutrinos (introductory overview)hep.fi.infn.it/PAMELA/naumov/Rus/Papers/Baikal1_067_1998... · 2005. 10. 22. · 0.5 0.0 0.5 1 φ(7Be) / φ(7Be) SSM 0.0 0.5

file:///G|/Works/BSFPh98/Lecture/Misc/Abstract%20to%20Lecture%20at%20KIAS.txt

V. A. Naumov

Physics of Atmospheric Neutrinos

Abstract

The lecture reviews the physics of neutrino production in the atmosphere, the detection methods, and the results obtained with large underground neutrino detectors.

Contents of the lecture.

1. Introduction. The role of atmospheric neutrinos (AN) in astroparticle physics. 2. Mechanisms and the main features of neutrino production in the earth's atmosphere at low, intermediate, and high energies. 3. A short review of calculational methods. 4. Sketch of numerical results. Comparison between different models and analysis of uncertainties. 5. Verification of the AN flux calculations with the cosmic-ray secondaries in the atmosphere and ground level. 6. Underground muons as a tool for the AN flux normalization. 7. Detection methods. Description of the largest underground neutrino detectors. Neutrino-induced events classification. 8. Search for neutrino oscillations in underground experiments. 9. Results from the detectors Kamiokande, IMB, NUSEX, Frejus, SOUDAN 2, MACRO, and Super-Kamiokande. Interpretation of the data in terms of neutrino oscillations.10. Other explanations (proton decay, neutrino decay, FCNC, neutron background, etc).11. Conclusions.

file:///G|/Works/BSFPh98/Lecture/Misc/Abstract%20to%20Lecture%20at%20KIAS.txt10/10/2005 12:28:48 AM

Page 2: Physics of atmospheric neutrinos (introductory overview)hep.fi.infn.it/PAMELA/naumov/Rus/Papers/Baikal1_067_1998... · 2005. 10. 22. · 0.5 0.0 0.5 1 φ(7Be) / φ(7Be) SSM 0.0 0.5

10-1

1

10

102

10 -3 10 -2 10 -1 1sin2 2

∆m2

[eV

2 ]

BNL E776

LSND93-97

CCFR

BUGEY

KARMEN2Feb.97-Apr.9890 % CL exclusion

KARMEN2Feb.97-Apr.98sensitivity

Page 3: Physics of atmospheric neutrinos (introductory overview)hep.fi.infn.it/PAMELA/naumov/Rus/Papers/Baikal1_067_1998... · 2005. 10. 22. · 0.5 0.0 0.5 1 φ(7Be) / φ(7Be) SSM 0.0 0.5

0.5 0.0 0.5 1φ(7Be) / φ(7Be)SSM

0.0

0.5

1.0φ(

8 B)

/ φ(8 B

) SS

MMonte Carlo SSMsTL SSMLow ZLow opacityWIMPLarge S11Small S 34Large S33Mixing modelsDarShaviv modelCummingHaxton model

T C power law

BP SSM

Smaller S17Combined fit90, 95, 99% C.L.

Page 4: Physics of atmospheric neutrinos (introductory overview)hep.fi.infn.it/PAMELA/naumov/Rus/Papers/Baikal1_067_1998... · 2005. 10. 22. · 0.5 0.0 0.5 1 φ(7Be) / φ(7Be) SSM 0.0 0.5

Energy (GeV/particle)

m-2 s

sr

(GeV

/par

ticle

)-1

-11.

75 [

]

E

dF/

dE2.

75

10 10 10 10 10 10 10 10 103 4 5 6 7 8 9 10 11

4

5

6

10

10

10

103

Grigorov et al.Ichimura et al.JACEETien ShanNorikura

Tibet AS EAS-TOPDiceTunkaAkeno

SUGARHaverah ParkYakutskFly’s EyeAGASA

"All-particle" spectrumof primary cosmic rays

direct data

γ

these two pointsare senseless

-1-1

(GeV

/nuc

leon

) ]

[ms

srdF

/dE

-1

-24

Kinetic Energy [GeV/nucleon]10-1 100 101 102 10310-4

10-3

10-2

10-1

100

101

102

103

10

Solar mid.Solar min.

Solar max.

Smith et al., 1973

Ananda et al., 1968

Verma et al., 1972

Balasubrahmanyan et al., 1973Julisson, 1973

Ormes & Webber, 1965Webber et al., 1973

Ryan et al., 1972

He

CNO

H

Page 5: Physics of atmospheric neutrinos (introductory overview)hep.fi.infn.it/PAMELA/naumov/Rus/Papers/Baikal1_067_1998... · 2005. 10. 22. · 0.5 0.0 0.5 1 φ(7Be) / φ(7Be) SSM 0.0 0.5

H He

CNO Ne-S

Fe

Log (Energy [GeV/nucleon])10

1 2 3 4 5 6

1 2 3 4 5 61 2 3 4 5 6

1 2 3 4 5 6

1 2 3 4 5 6Log (Energy [GeV/nucleon])

10

10

10

10

1

0

-1

10

10

10

2

1

0

10

10

10

1

0

-1

10 2

10

10

10

3

2

1

10

10

10

4

3

2

Log (Energy [GeV/nucleon])10

Log (Energy [GeV/nucleon])10

Log (Energy [GeV/nucleon])10

E

dF/d

E [m

s

sr

(GeV

/nuc

leon

) ]

2.5

-2-1

-11.

5

Page 6: Physics of atmospheric neutrinos (introductory overview)hep.fi.infn.it/PAMELA/naumov/Rus/Papers/Baikal1_067_1998... · 2005. 10. 22. · 0.5 0.0 0.5 1 φ(7Be) / φ(7Be) SSM 0.0 0.5

1

10 2

10 3

µ µν ν+

e eν ν+

10

Neutrino Energy (GeV)10 -1 100 10

HKKMBGSBNLK

10 -2

E d

F /d

E2

νν

ν(m

srs

GeV

)-1

-1-1

+

+

νµνµ

νeνe

νeνe

Flux

Rat

ios

10 -2 10 -1 100 1010 -2 10 -1 100 1010 -2 10 -1 100 1010 -2 10 -1 100 10

2.5

2.0

1.5

1.0

LKBNBGSHKKM

νµνµ

Neutrino Energy (GeV)

νeνe

νµνµ

νeνe

νµνµ

νeνe

νµνµ

+

+

νµνµ

νeνe

+

+

νµνµ

νeνe

+

+

νµνµ

νeνe

Page 7: Physics of atmospheric neutrinos (introductory overview)hep.fi.infn.it/PAMELA/naumov/Rus/Papers/Baikal1_067_1998... · 2005. 10. 22. · 0.5 0.0 0.5 1 φ(7Be) / φ(7Be) SSM 0.0 0.5

a) b)

x dN

/dx

0

0.2

0.4

0.6

0.8

1

0

0.2

0.4

0.6

0.8

1

0 0.2 0.4 0.6 0.8x

1 0 0.2 0.4 0.6 0.8x

1

BGSBNHKHM

π+ π-

π

BGSBNHKHM

Page 8: Physics of atmospheric neutrinos (introductory overview)hep.fi.infn.it/PAMELA/naumov/Rus/Papers/Baikal1_067_1998... · 2005. 10. 22. · 0.5 0.0 0.5 1 φ(7Be) / φ(7Be) SSM 0.0 0.5

νµνµ +

Near Vertical

Neutrino Energy (GeV)100 10 1 10 2 10 3 10 4

10

10 3

2

Near Horizontal

νν +e e

Lipari

VolkovaMitsui et al.Butkevich et al.

Neutrino Energy (GeV)100 10 1 10 2 10 3

10 1

10 2

10 3

Near Vertical

HKKMLipari

VolkovaMitsui et al.Butkevich et al.

HKKM

Near Horizontal

E d

F /d

E3

νν

ν(m

srs

GeV

)

-1-1

-12

Page 9: Physics of atmospheric neutrinos (introductory overview)hep.fi.infn.it/PAMELA/naumov/Rus/Papers/Baikal1_067_1998... · 2005. 10. 22. · 0.5 0.0 0.5 1 φ(7Be) / φ(7Be) SSM 0.0 0.5

10-3

10-2

10-1

10

102

103

104

105

103 104 105

a)

0 o

conventional νe + ν⎯e

prompt νe + ν⎯e

from K0e3 decays

from K–e3 decays

from µe3 decays

c)conventional νµ + ν⎯µprompt νµ + ν⎯µfrom Kµ2 decaysfrom πµ2 decaysfrom Kµ3 decaysfrom µe3 decays

b)

90o

conventional νe + ν⎯eprompt νe + ν⎯efrom K

0e3 decays

from K–e3 decays

from µe3 decays

d)conventional νµ + ν⎯µprompt νµ + ν⎯µfrom Kµ2 decaysfrom πµ2 decaysfrom Kµ3 decaysfrom µe3 decays

Eν (GeV)

0 o

90o

RQPMQGSM

pQCD RQPM

QGSM

pQCD

RQPM

QGSM

pQCD

RQPMQGSM

pQCD

ν-2

s-1 s

r-1 G

eV2

νE

dF

/dE

(

m3

ν-2

s-1 s

r-1 G

eV2

νE

dF

/dE

(

m3

(ν µ + ν⎯ µ

)/(ν e

+ ν⎯ e

)

pQCD

RQPM

QGSM

pQCD

RQPM

QGSM

π,K neutrinosπ,K + prompt neutrinos

π,K neutrinosπ,K + prompt neutrinos

10

1

0

103 104 105

10-3

10-2

10-1

10

102

103

104

105

10

1

0

10-2

10-1

10

102

103

104

105

10

1

0

106

103 104 105

Eν (GeV)103 104 105

10-2

10-1

10

102

103

104

105

10

1

0

106

a) b) 90o0 o

Eν (GeV)103 104 105

Eν (GeV)103 104 105

10

102

10

1

0

10

102

10

1

0

Page 10: Physics of atmospheric neutrinos (introductory overview)hep.fi.infn.it/PAMELA/naumov/Rus/Papers/Baikal1_067_1998... · 2005. 10. 22. · 0.5 0.0 0.5 1 φ(7Be) / φ(7Be) SSM 0.0 0.5

νdI dE

ν ν

3[G

eV /

cm /

s/sr

]2

2

γp ,pp π ν

pp π ν

pA ΛD, c ν

νpA π,Κ

E

AKENO ZHVa

VFGS

BNSZ

GGHVZZHVeTIG

TeV PeV EeV

10

10

1

3

-3

Dar, Shav

iv

Man

nhei

m

Proth

eroe

blazars

interstellar mediumgalactic pole

galactic center

vert.

atmospheric

atmospheric

horiz.MACRO

Selected predictions for high-energy neutrino fluxes (from P. Gondolo, Proc. of the 4th SFB-375 Ringberg Workshop on Neutrino Astrophysics, Oct. 20-24, 1997)

Page 11: Physics of atmospheric neutrinos (introductory overview)hep.fi.infn.it/PAMELA/naumov/Rus/Papers/Baikal1_067_1998... · 2005. 10. 22. · 0.5 0.0 0.5 1 φ(7Be) / φ(7Be) SSM 0.0 0.5

0.05

0.1

0.15

0.2

0.25

0.3

0.35

0.4

10 102

103

a)

L3, 1993MASS, 1993Nottingham, 1984MARS, 1975, 1977

Durgapur, 1972Kiel, 1971Texas, 1971Nottingham, 1968

MACRO best fit, 1995

Muon Momentum [ GeV/c ]

Bugaev et al., 1998Agrawal et al., 1996

10-2

10-1

103

104

105

b)

MACRO best fit, 1995Moscow University, 1994Frejus, 1994Baksan, 1992Artyomovsk, 1985Nottingham, 1984MARS, 1977Durgapur, 1972

Muon Momentum [ GeV/c ]

Bugaev et al., 1998Bugaev et al., 1989Volkova et al., 1987

1 - π ,K-muons2 - π ,K-muons + PM (QGSM) 3 - π ,K-muons + PM (RQPM) 4 - π ,K-muons + PM (VFGS)

4

3

21

LVD, 1998

µ-2

s-1sr

-1(G

eV/c

)2

]

µµ

p d

F /d

p [

cmµ

-2s-1

sr-1

(GeV

/c)2

µp

dF

/dp

[cm

Page 12: Physics of atmospheric neutrinos (introductory overview)hep.fi.infn.it/PAMELA/naumov/Rus/Papers/Baikal1_067_1998... · 2005. 10. 22. · 0.5 0.0 0.5 1 φ(7Be) / φ(7Be) SSM 0.0 0.5

10-3

10-2

10-1

103

104

105

4

3

2

1

EAS-TOP, 1995Baksan, 1992Baksan, 1990KGF, 1990 [X=0]KGF, 1990 [X=9 10 ]KGF, 1964

Muon Momentum [ GeV/c ]

1 - π ,K-muons2 - π ,K-muons + PM (QGSM) 3 - π ,K-muons + PM (RQPM) 4 - π ,K-muons + PM (VFGS)

b)Bugaev et al., 1998Bugaev et al., 1989Volkova et al., 1987

10-2

10-1

10 102

103

a)

MASS, 1993Nottingham, 1984MARS, 1975Durgapur, 1972Nottingham, 1968KGF, 1964Durham, 1963

Muon Momentum [ GeV/c ]

Bugaev et al., 1998

-4

p2 F

µ(p

) [

cm-2

s-1sr

-1(G

eV/c

)

]

µµ

p2 F

µ(p

) [

cm-2

s-1sr

-1(G

eV/c

)

]

µµ

+

Page 13: Physics of atmospheric neutrinos (introductory overview)hep.fi.infn.it/PAMELA/naumov/Rus/Papers/Baikal1_067_1998... · 2005. 10. 22. · 0.5 0.0 0.5 1 φ(7Be) / φ(7Be) SSM 0.0 0.5

10-13

10-12

10-11

10-10

10-9

10-8

10-7

2 4 6 8 10 12

LVDData converted to standard rockData for Gran Sasso rock (x 10-1)

π,K-muonsπ,K-muons + Iµ

ν

π,K-muons + Iµν + PM (RQPM)

π,K-muons + Iµν + PM (VFGS)

Iµν =2.98x10-13 cm-2s-1sr-1

Inte

nsity

( c

m-2

s-1sr

-1 )

Depth (km w.e.)

Muo

n

Page 14: Physics of atmospheric neutrinos (introductory overview)hep.fi.infn.it/PAMELA/naumov/Rus/Papers/Baikal1_067_1998... · 2005. 10. 22. · 0.5 0.0 0.5 1 φ(7Be) / φ(7Be) SSM 0.0 0.5

0

0.1

0.2

0.3

0.4

0.5

0.6

0.7

0.8

0.9

1

0 5 10 15 20 25 30 35 40

BEBC (1979-1982)

BNL (1980-1981)

CRS (1980-1981)

FNAL (1977-1983)

GGM (1979-1981)

IHEP-ITEP (1979-1983) SKAT (1979)

IHEP-JINR (1995)

ν N

ν– N

0

0.1

0.2

0.3

0.4

0.5

0.6

0.7

0.8

0.9

1

50 75 100 125 150 175 200

BEBC (1979-1982)

FNAL (1977-1983) CCFRR (1984) 20-200 GeV average

ν N

ν N

IHEP-ITEP (1979-1983)

Eν (GeV)225

Eν (GeV)

σC

Cto

t10

-38

(cm

/G

eV )

2/ –

Page 15: Physics of atmospheric neutrinos (introductory overview)hep.fi.infn.it/PAMELA/naumov/Rus/Papers/Baikal1_067_1998... · 2005. 10. 22. · 0.5 0.0 0.5 1 φ(7Be) / φ(7Be) SSM 0.0 0.5

Through-going muons

Stopping muons

Kamiokande multi-GeV

Contained events ( x1/10 )

10 10 10 10 10 10 10-1 0 1 2 3 4 5

E (GeV)

E d

N /d

En

n n

nM

uon-

neut

rino

resp

onse

(Bar

tol,

11/1

1/19

96)

50

45

40

35

30

25

20

15

10

5

0

Page 16: Physics of atmospheric neutrinos (introductory overview)hep.fi.infn.it/PAMELA/naumov/Rus/Papers/Baikal1_067_1998... · 2005. 10. 22. · 0.5 0.0 0.5 1 φ(7Be) / φ(7Be) SSM 0.0 0.5

Distance

under ground

1.6 km

SUPERKAMIOKANDE DETECTORCatching NeutrinosAbout once every 90 minutes, a neutrino interacts in the detectorchamber, generating Cherenkov radiation. This optical equivalent ofa sonic boom creates a cone of light that is registered on thephotomultipliers that line the tank. Characteristic ring patterns tellphysicists what kind of neutrinos interacted and in which directionthey were headed.

The light isdetected byphoto sensorsthat line thetank, andtranslated into adigital image.

Electronicstrailers

Controlroom

Accesstunnel(2 km)

12.5 million gallontank of ultra-purewater

Mt. Ikena Yama

Mountains filter out other signalsthat mask neutrino detection.

A few neutrinos interactwithin the huge tank of superpure water, generating acone of light.

University of Hawai’i media graphic

Page 17: Physics of atmospheric neutrinos (introductory overview)hep.fi.infn.it/PAMELA/naumov/Rus/Papers/Baikal1_067_1998... · 2005. 10. 22. · 0.5 0.0 0.5 1 φ(7Be) / φ(7Be) SSM 0.0 0.5

a)Fr

om w

ithin

Sup

er-K

amio

kand

e

detector wall

Cherenkov ring

θ

Cherenkov cone

c

PMTparticle track

Cherenkovgeometry

39.3 m

SK T

ank

b)

ν µ

ν (ν ) µ e

ν (ν ) µ e

µ (e)

µ (e)

µ

µ USFC

PCν µ

UT

41.4

m

Page 18: Physics of atmospheric neutrinos (introductory overview)hep.fi.infn.it/PAMELA/naumov/Rus/Papers/Baikal1_067_1998... · 2005. 10. 22. · 0.5 0.0 0.5 1 φ(7Be) / φ(7Be) SSM 0.0 0.5

RUN 1743EVENT 188DATE 96-May-31TIME 21:43:51TOT PE: 74546.4MAX PE: 251.8NMHIT : 8374ANT-PE: 1719.3ANT-MX: 43.0NMHITA: 239

RunMODE:NORMALTRG ID :00001011T diff.:0.467E+05us : 46.7 msFSCC: 0TDC0: -1129.0Q thr. : 0.0BAD ch.: maskedSUB EV : 0/ 0

NUM 33

Page 19: Physics of atmospheric neutrinos (introductory overview)hep.fi.infn.it/PAMELA/naumov/Rus/Papers/Baikal1_067_1998... · 2005. 10. 22. · 0.5 0.0 0.5 1 φ(7Be) / φ(7Be) SSM 0.0 0.5

electron

muon

Page 20: Physics of atmospheric neutrinos (introductory overview)hep.fi.infn.it/PAMELA/naumov/Rus/Papers/Baikal1_067_1998... · 2005. 10. 22. · 0.5 0.0 0.5 1 φ(7Be) / φ(7Be) SSM 0.0 0.5

SK50

100

150

200

250

0

60

120

180

240

300

e-likep > 0.4 GeV/c

µ-likep > 0.4 GeV/c

b)

d)

10

20

30

40

50

15

30

45

60

75

0

20

40

60

80

100

e-likep < 2.5 GeV/c

e-likep > 2.5 GeV/c

µ-like FC

0

25

50

75

100

125µ-like PC

e) f)

g) h)

-1 -0.6 -0.2 0.2 0.6 1 -1 -0.6 -0.2 0.2 0.6 1 -1 -0.6 -0.2 0.2 0.6 1cos θ

10-1 10 10-1

-0.5

0

0.5

1

-1

-0.5

0

0.5

1

e - like(U

-D)/(

U+D

)

Momentum (GeV/c)

µ - like

100 1 2 10-1 10100 1

10 102 103 104 1050

0.5

1

1.5

L/Eν (km/GeV)

Dat

a / M

onte

Car

lo

e-likeµ-like

SK (33 kt/year)

ν ντµ∆m = 2.2 102 -3 eV2

sin 2 = 12

sin 2

∆m

(eV

)

νµ ντ

Kamiokande

Super-Kamiokande

68% CL90% CL99% CL

0 0.2 0.4 0.6 0.8 110-4

10-3

10-2

10-1

22

2

�90% CL

10 10

100

cos θcos θ

50

100

150

200

250

-1 -0.6 -0.2 0.2 0.6 10

40

80

120

160

200

e-likep < 0.4 GeV/c

µ-likep < 0.4 GeV/c

a)

c)

cos θ

Even

ts

FC PC

Page 21: Physics of atmospheric neutrinos (introductory overview)hep.fi.infn.it/PAMELA/naumov/Rus/Papers/Baikal1_067_1998... · 2005. 10. 22. · 0.5 0.0 0.5 1 φ(7Be) / φ(7Be) SSM 0.0 0.5

νµ ↔ ντ 90% C.L. contour10 -4

10 -3

10 -2

10 -1

1

0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1

SK through-going

CDHSW

K contained

IMB stoppingthroughgoing

sin 2 2

∆m

2 (eV

2)

0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1

SK through-going

K containedGosgen

Bugey

Chooz

SK best fit

SK b.f.

10 -4

10 -3

10 -2

10 -1

1

∆m

(eV

)

sin 2 2

νe ↔ νµ 90% C.L. contour

22

Page 22: Physics of atmospheric neutrinos (introductory overview)hep.fi.infn.it/PAMELA/naumov/Rus/Papers/Baikal1_067_1998... · 2005. 10. 22. · 0.5 0.0 0.5 1 φ(7Be) / φ(7Be) SSM 0.0 0.5

Drift Tubes Gas TightSteel Skin

CathodeSignalCables

Drift HVConnector

Gas Supply

AnodeSignalCables

2.7 m

1.0 m1.1 m

SOUDAN 2SOUDAN 2El

ectro

nics

UT IU

US ID

MA

CR

O

z

y

Eve

nts/

year

1

2

6

5

4

3

0

E (GeV)-1 0 1 2 3 4

ν

10 10 10 10 10 10

UTID + USIUAbsorber

StreamerScintillatorTrack-Etch

MA

CR

O

Page 23: Physics of atmospheric neutrinos (introductory overview)hep.fi.infn.it/PAMELA/naumov/Rus/Papers/Baikal1_067_1998... · 2005. 10. 22. · 0.5 0.0 0.5 1 φ(7Be) / φ(7Be) SSM 0.0 0.5

-1 - 0.8 - 0.6 - 0.4 - 0.2 00

1

2

3

4

5

cos θ

Baksan, 1991IMB, 1990

Kamiokande, 1992

F (E

>3

GeV

) [1

0

cm

s s

r ]

-13

µµ

-2

-1-1

Experiment Threshold 10 F (E > 3 GeV)

(GeV) (cm s sr )

IMB 2 1.92 0.11 Baksan 1 2.08 0.14 Kamiokande 3 2.04 0.13

–––

µ µ-13

-2 -1 -1

Measured rates

Page 24: Physics of atmospheric neutrinos (introductory overview)hep.fi.infn.it/PAMELA/naumov/Rus/Papers/Baikal1_067_1998... · 2005. 10. 22. · 0.5 0.0 0.5 1 φ(7Be) / φ(7Be) SSM 0.0 0.5

cos θ

0

1

2

3

4

5

6

7

8

9

-1 -0.9 -0.8 -0.7 -0.6 -0.5 -0.4 -0.3 -0.2 -0.1 0

MACRO data (UT, 451 events)

Bartol flux∆ m = 2.5 10 eV , sin 2� = 12 2 2-3

10-5

10-4

10-3

10-2

10-1

0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1

sin22�

90%

99%Sensitivity

∆m

(eV

)

22

Best Fit Point (P = 17%)max

ν ντ��µ

0.01 Pmax

0.01 Pmax

0.1 P max

a) b)

F (E

>1

GeV

) [1

0

cm

s s

r ]

-13

µµ

-2-1

-1

+

Eve

nts

60

50

40

30

20

10

0

60

50

40

30

20

10

0

-|cos θ|

ID + US(120 events)

IU(85 events)

-0.8 -0.6 -0.4 -0.2 0-1cos θ

-0.8 -0.6 -0.4 -0.2 0-1

a) b)

MACRO

Event Ratio O/E without Stat. Syst. Teor. Ratio O/E withTopology ν oscillations Error Error Error ν oscillations

ID+US 0.75 0.07 0.08 0.19 0.98 IU 0.59 0.06 0.06 0.15 1.02 UT 0.74 0.036 0.046 0.13 1.05

100

Page 25: Physics of atmospheric neutrinos (introductory overview)hep.fi.infn.it/PAMELA/naumov/Rus/Papers/Baikal1_067_1998... · 2005. 10. 22. · 0.5 0.0 0.5 1 φ(7Be) / φ(7Be) SSM 0.0 0.5

-4

-3.5

-3

-2.5

-2

-1.5

-1

-0.5

0

0 0.2 0.4 0.6 0.8 1

νµ ↔ νe

68%90%95%99%

sin22

EXCLUDED

ALLOWED

-4

-3.5

-3

-2.5

-2

-1.5

-1

-0.5

0

0 0.2 0.4 0.6 0.8 1

νµ ↔ ντ

68%90%95%99%

sin22

ALLOWED

EXCLUDEDlog 10

∆m

2

a) b)

05

10152025303540

0 500 1000 1500 2000 2500

05

10152025303540

0 500 1000 1500 2000 2500

05

10152025303540

0 500 1000 1500 2000 2500

05

10152025303540

0 500 1000 1500 2000 2500

DataBackgroundMC

Tracks Showers

Backgroundsubstructed

BackgroundsubstructedE

vent

s / 1

00 M

eV

Energy (MeV)

DataBackgroundMC

a)

b)

c)

d)

SOUDAN 2

Page 26: Physics of atmospheric neutrinos (introductory overview)hep.fi.infn.it/PAMELA/naumov/Rus/Papers/Baikal1_067_1998... · 2005. 10. 22. · 0.5 0.0 0.5 1 φ(7Be) / φ(7Be) SSM 0.0 0.5

BGS, 1989

P, 1994

HKHM, 1990LK, 1990

BN, 1989

KM, 1991

1.2

1.4

0.6 0.8 1.0(µ/e)/(µ/e) =

0.4

BGS

0 0.5 1 1.5 20

0.5

1

1.5

2

µ/µ BGS

e/e B

GS

(For Kamiokande)

0

1

(µ/e

)

/ (µ/

e)da

taM

C

Supe

r - K

amio

kand

e

Kam

ioka

nde

IMB

SOUD

AN 2

Frej

us

mul

ti-Ge

V

mul

ti-Ge

V

sub-

GeV

sub-

GeV

NUSE

X

0.5

1.5Water detectors Iron detectors

Page 27: Physics of atmospheric neutrinos (introductory overview)hep.fi.infn.it/PAMELA/naumov/Rus/Papers/Baikal1_067_1998... · 2005. 10. 22. · 0.5 0.0 0.5 1 φ(7Be) / φ(7Be) SSM 0.0 0.5

0 0.5 1 1.5 20 0.5 1 1.5 2 0

0

0.5

1

1.5

0

0

0.5

1

1.5

0

0.5

1

1.5

0

0.5

1

1.5

2

0.5

1

1.5

2

0.5

1

1.5

NUSEX

FREJUS

SOUDAN 2 (prelim.)

IMB

KAMIOKANDE(sub-GeV range)

KAMIOKANDE(multi-GeV range)

Iron detectorsWater detectorsd)a)

e)

f)c)

b)

data MC

All

FC

Legend

0.990.55

0.870.61

0.640.59

FC FC+PC

data MC/

(µ/e) (µ/e)data MC /

µ µdata MC/µ µ

data

MC

/e

e