Results from MINOS and NOA - NuPHYS - London

Results from MINOS and NOνA

NuPHYS - London

Christopher Backhouse

California Institute of Technology

December 19, 2013

C. Backhouse (Caltech) MINOS & NOνA December 19, 2013 1 / 33

Introduction

◮ NuMI: produce neutrino beamstarting with 120GeV protonsfrom Fermilab Main Injector

◮ Main Injector NeutrinoOscillation Search

◮ NuMI Off-axis νe Appearance

◮ Both use two-detector techniqueto cancel systematic effects

◮ NOνA is off-axis for moresharply peaked flux


MINOS

MINOS detector technology

◮ Magnetized steel-scintillator trackingsampling calorimeters

◮ Alternate planes of scintillator and steel

◮ WLS fibres embedded in 4.1x1cm strips ofextruded polystyrene scintillator

◮ Read out by Hamamatsu multi-pixel PMTs

◮ ∼1T magnetic field for charge ID

REFLECTIVE SEAL

TiO2 LOADED POLYSTYRENE CAP

41mm

CLEAR POLYSTYRENE SCINTILLATOR

WLS FIBER

UP TO 8m

10mm

MINOS SCINTILLATOR STRIP


MINOS detector technology

Near Detector

◮ 1 kton

◮ 1km from target

◮ Running since 2005

Far Detector

◮ 5.4 kton

◮ 735km from target

◮ Running since 2003

REFLECTIVE SEAL

TiO2 LOADED POLYSTYRENE CAP

41mm

CLEAR POLYSTYRENE SCINTILLATOR

WLS FIBER

UP TO 8m

10mm

MINOS SCINTILLATOR STRIP


MINOS datasets

Date2005/05/02 2006/05/29 2007/06/26 2008/07/23 2009/08/20 2010/09/17 2011/10/15 2012/11/11 2013/12/09

Pro

tons

per

wee

k (E

18)

0

2

4

6

8

10

Total NuMI protons

Tot

al P

roto

ns (

E20

)

0

2

4

6

8

10

12

14

16

18

◮ 10.7 × 1020 POT in (LE) neutrino running◮ 3.36 × 1020 POT in antineutrino running◮ 37.9 kton years of FD atmospheric neutrinos◮ NOνA/MINOS+ running ongoing


Far Detector beam samples

Neutrinos

Energy (GeV)µν Reconstructed

Eve

nts

/ GeV

0

100

200

300

400

500

600

0 2 4 6 8 10 12

MINOS PRELIMINARY POT)20 10×Neutrino beam (10.71

µνcontained-vertex

MINOS dataBest fit oscillationsNo oscillationsNC background

Antineutrinos

Energy (GeV)µν Reconstructed E

vent

s / G

eV

0

20

40

60

80

0 2 4 6 8 10 12 14

MINOS PRELIMINARY POT)20 10×Antineutrino beam (3.36


MINOS dataBest fit oscillationsNo oscillationsNC background

◮ Three-flavour oscillations fit data well◮ 18% of pseudo-experiments have worse fit

CC νµ CC ν̄µPred 3201 363Obs 2579 312


Far Detector beam samples

Neutrinos

Energy (GeV)µν Reconstructed

Rat

io to

No

Osc

illat

ions

0.0

0.5

1.0

1.5

2.0

0 2 4 6 8 10 12

MINOS PRELIMINARY POT)20 10×Neutrino beam (10.71


MINOS dataBest fit oscillations

Antineutrinos

Energy (GeV)µν Reconstructed R

atio

to N

o O

scill

atio

ns

0.0

0.5

1.0

1.5

2.0

0 2 4 6 8 10 12 14

MINOS PRELIMINARY POT)20 10×Antineutrino beam (3.36


MINOS dataBest fit oscillations

◮ Three-flavour oscillations fit data well◮ 18% of pseudo-experiments have worse fit

CC νµ CC ν̄µPred 3201 363Obs 2579 312


Far Detector atmospheric samples

)zθcos(-1.0 -0.5 0.0 0.5 1.0

Eve

nts

0

10

20

30

40

50 = 1-3 GeVνEµν

MINOS PRELIMINARY

)zθcos(-1.0 -0.5 0.0 0.5 1.0

Eve

nts

0

10

20

30 Atmospheric neutrinosµν and µνcontained-vertex

= 3-10 GeVνEµν

)zθcos(-1.0 -0.5 0.0 0.5 1.0

Eve

nts

0

5

10

15

20 = 10-30 GeVνEµνMINOS data (37.88 kt-yr)Best fit, normal hierarchyBest fit, inverted hierarchyNo oscillationsCosmic-ray muons

)zθcos(-1.0 -0.5 0.0 0.5 1.0

Eve

nts

0

5

10

15

20

25 = 1-3 GeVνEµν

)zθcos(-1.0 -0.5 0.0 0.5 1.0

Eve

nts

0

5

10

15 = 3-10 GeVνEµν

)zθcos(-1.0 -0.5 0.0 0.5 1.0

Eve

nts

0

2

4

6

8

10 = 10-30 GeVνEµν

◮ Additional sensitivity from atmospheric sample◮ Predict 1100 events, observe 905◮ Showing contained muon-selected events◮ Partially-contained and showering events also included


νe appearance

ν ν̄

θ13 = 0 69.1 10.5θ13 = 0.1 95.1 13.6

Obs. 88 12

◮ Combine with reactorconstraints

◮ Gives some sensitivity tohierarchy and octant


νe appearance

ν ν̄

θ13 = 0 69.1 10.5θ13 = 0.1 95.1 13.6

Obs. 88 12

◮ Combine with reactorconstraints

◮ Gives some sensitivity tohierarchy and octant


Combined contours

2.2

2.4

2.6

2.8 MINOS PRELIMINARY appearanceeν disappearance + µν

-mode,µν POT 2010×-mode, 3.36 µν POT 2010×10.71 37.88 kt-yr atmospheric neutrinos

Normal hierarchy

23θ2sin0.3 0.4 0.5 0.6 0.7

-2.8

-2.6

-2.4

-2.2Inverted hierarchy

68% C.L.90% C.L.

Best fit

)2eV

-3 (

102 32

m∆

log(

L)∆

-2

0

2

4

6

)2 eV-3| (10232m∆|

2.2 2.3 2.4 2.5 2.6

68% C.L.

90% C.L.

Profile of likelihood surfaceNormal hierarchyInverted hierarchy

23θ2sin0.3 0.4 0.5 0.6 0.7

log(

L)∆

-2

0

2

4

6

68% C.L.

90% C.L.


◮ Solar parameters fixed◮ θ13 nuisance parameter, constrained by reactor results◮ δCP, θ23, ∆m2

32 unconstrained◮ Major systematics included as nuisance parameters


Combined resultslo

g(L)

∆

-2

0

1

2

3

4

5

π / CPδ0.0 0.5 1.0 1.5 2.0

68% C.L.

90% C.L.

/4π<23θ<0, 232m∆

/4π>23θ<0, 232m∆

/4π<23θ>0, 232m∆

/4π>23θ>0, 232m∆

MINOS PRELIMINARY appearanceeν disappearance + µν


◮ Disfavour normalhierarchy, upper octantat 81% C.L.

◮ Maximal mixingdisfavoured at 79% C.L.

◮ Best measurement of|∆m2

32|


MINOS sterile neutrinos

◮ See no deficit of NC events◮ In fact a small excess

◮ Interpret in terms of oscillationsat ∆m2 ∼ 0.5eV2

◮ Expect flat deficit in FD, noeffect in ND

◮ sin2 2θµe < 7.1× 10−3 90% C.L.


MINOS+

◮ Continue to operate MINOSdetectors in the NOνA beam

◮ Flux reduced in the oscillationregion

◮ But large increase in stats at highenergy

◮ ∼ 4000 νµ CC / year expected

◮ Test oscillation paradigm, look forexotic signals


MINOS+

◮ First event observed in MINOS+ FD in the NOνA-era beam


MINOS+

2.2

2.4

2.6

2.8 MINOS PRELIMINARY appearanceeν disappearance + µν


Normal hierarchy

23θ2sin0.3 0.4 0.5 0.6 0.7

-2.8

-2.6

-2.4


68% C.L.90% C.L.

Best fit

)2eV

-3 (

102 32

m∆

log(

L)∆

-2

0

2

4

6

)2 eV-3| (10232m∆|

2.2 2.3 2.4 2.5 2.6

68% C.L.

90% C.L.


23θ2sin0.3 0.4 0.5 0.6 0.7

log(

L)∆

-20

2

4

6

68% C.L.

90% C.L.


◮ Continue to add stats to conventional analyses


MINOS+

2.2

2.4

2.6

2.8 MINOS+ SIMULATION appearanceeν disappearance + µν: MINOS data

disappearanceµν: MINOS+ simulation)ν-mode, 27 kt-yr atmospheric µν POT 2010×(16

Normal hierarchy

23θ2sin0.3 0.4 0.5 0.6 0.7

-2.8

-2.6

-2.4


68% C.L.90% C.L.

Best fit

)2eV

-3 (

102 32

m∆

log(

L)∆

-2

0

2

4

6

)2 eV-3| (10232m∆|

2.2 2.3 2.4 2.5 2.6

68% C.L.

90% C.L.


23θ2sin0.3 0.4 0.5 0.6 0.7

log(

L)∆

-20

2

4

6

68% C.L.

90% C.L.


◮ Continue to add stats to conventional analyses


MINOS+

Extra dimensions Sterile oscillations

◮ Sterile analysis with joint fit to NC and CC spectra

◮ Lots of stats away from the main oscillation maximum

◮ Other signals of exotic physics possible in the high energy region too


NOνA

NOνA detector technology

◮ Fine-grained low-Z, highly active, tracking calorimeter

◮ 64% liquid scintillator by mass

◮ WLS fibres looped in 4x6cm cells of PVC extrusion

◮ Each to one of 32 pixels of Hamamatsu APD


NOνA detector technology

Far Detector

◮ 14 kton

◮ 344,000 channels

◮ 810km from target

Near Detector

◮ 0.3 kton

◮ 18,000 channels

◮ 1km from target


Far Detector construction status

◮ Block assembly and placement, scintillator filling, and electronicsinstallation proceeding in parallel

◮ Over 10,000 modules and 2 million gallons of scintillator so farC. Backhouse (Caltech) MINOS & NOνA December 19, 2013 18 / 33

Near Detector construction status

◮ Rapid progress on the Near Detector

◮ Installation of final block in the New Year

◮ Then filling and completion of electronics outfitting


Accelerator and NuMI upgrades

◮ NuMI being upgraded from350kW to 700kW

◮ Beam returned September 2013

◮ Convert Recycler to protonsfrom antiprotons

◮ Shorten Main Injector cycle2.2s→1.33s

◮ Overhaul of NuMI target station

◮ 7.2 × 1019 POT delivered so far

◮ Maximum power 500kW untilBooster RF upgrades completed

0

20

40

60

80

0 2 4 6 8 10Eν (GeV)

ν C

C e

ven

ts /

kt

/ 1E

21 P

OT

/ 0

.2 G

eV

Medium Energy Tune

on-axis7 mrad off-axis14 mrad off-axis21 mrad off-axis

μ

14mrad off-axis beam peaks sharply at 2GeV


NDOS beam peak

◮ NDOS is the Near Detector prototype on the surface at Fermilab

◮ Clearly see the NuMI beam peak

◮ Validates the timing synchronization


Event topologies

◮ Very good granularity, especially considering scale◮ X0 = 38cm (6 cell depths, 10 cell widths)


Far Detector data

NOvA - FNAL E929

Run: 11900 / 62Event: 263639 / CAL

UTC Mon Dec 9, 201305:53:50.922771008 sec)µt (

0 100 200 300 400 500

hits

110

210

q (ADC)10 210 310

hits

110

210310

0 1000 2000 3000 4000 5000 6000

x (c

m)

-800

-600

-400

-200

0

200

400

600

800

z (cm)0 1000 2000 3000 4000 5000 6000

y (c

m)

-800

-600

-400

-200

0

200

400

600

800

◮ Commissioning Far Detector blocks as they are instrumented◮ Showing one 500µs cosmic ray spill (beam window is ∼ 10µs)


Far Detector data

NOvA - FNAL E929

Run: 11900 / 62Event: 263639 / CAL

UTC Mon Dec 9, 201305:53:50.922771008 sec)µt (

0 100 200 300 400 500

hits

110

210

q (ADC)10 210 310

hits

110

210310

0 500 1000 1500 2000

x (c

m)

-800

-600

-400

-200

0

200

400

600

800

z (cm)0 500 1000 1500 2000

y (c

m)

-800

-600

-400

-200

0

200

400

600

800



Far Detector data

NOvA - FNAL E929

Run: 11900 / 62Event: 263639 / CAL

UTC Mon Dec 9, 201305:53:50.922771008 sec)µt (

0 100 200 300 400 500

hits

110

210

q (ADC)10 210 310

hits

110

210310

0 500 1000 1500 2000

x (c

m)

-800

-600

-400

-200

0

200

400

600

800

z (cm)0 500 1000 1500 2000

y (c

m)

-800

-600

-400

-200

0

200

400

600

800



Far Detector data

NOvA - FNAL E929

Run: 11900 / 62Event: 263639 / CAL

UTC Mon Dec 9, 201305:53:50.922771008 sec)µt (

0 100 200 300 400 500

hits

110

210

q (ADC)10 210 310

hits

110

210310

0 500 1000 1500 2000

x (c

m)

-800

-600

-400

-200

0

200

400

600

800

z (cm)0 500 1000 1500 2000

y (c

m)

-800

-600

-400

-200

0

200

400

600

800



Far Detector data

NOvA - FNAL E929

Run: 11900 / 62Event: 263639 / CAL

UTC Mon Dec 9, 201305:53:50.922771008 sec)µt (

0 100 200 300 400 500

hits

110

210

q (ADC)10 210 310

hits

110

210310

0 500 1000 1500 2000

x (c

m)

-800

-600

-400

-200

0

200

400

600

800

z (cm)0 500 1000 1500 2000

y (c

m)

-800

-600

-400

-200

0

200

400

600

800



Far Detector data

Distance to Readout End of Cell (cm)0 500 1000 1500

Mea

n A

DC

/Pat

hlen

gth

0

20

40

60

A PreliminaryνNO

Far Detector Data

Simulation

Hit ADC100 200 300 400

Fre

quen

cy

0

0.01

0.02

0.03

0.04

0.05

A PreliminaryνNO

Far Detector Data

Simulation

◮ Fairly good data/MC agreement

◮ Currently searching for neutrino events to confirm beam timing


Far Detector data - containment variables

Minimum X-coordinate (cm)-500 0 500

Eve

nts

410

510

610

Far Detector Data

Cosmic Simulation

A PreliminaryνNO

Maximum X-coordinate (cm)-500 0 500

Eve

nts

310

410

510

610

Far Detector Data

Cosmic Simulation

A PreliminaryνNO

Minimum Y-coordinate (cm)-500 0 500

Eve

nts

210

310

410

510

610

Far Detector Data

Cosmic Simulation

A PreliminaryνNO

Maximum Y-coordinate (cm)-500 0 500

Eve

nts

10

210

310

410

510

610

Far Detector Data

Cosmic Simulation

A PreliminaryνNO


Far Detector data - direction variables

Y Direction Cosine-1 -0.5 0 0.5 1

Eve

nts

0

200

400

600

800

Far Detector Data

Cosmic Simulation

A PreliminaryνNO

NuMIθCosine

-1 -0.5 0 0.5 1

Eve

nts

0

100

200

300

400

500

Far Detector Data

Cosmic Simulation

A PreliminaryνNO

◮ Fairly good data/MC agreement

◮ Currently searching for neutrino events to confirm beam timing


NOνA sensitivities

◮ Assuming 18× 1020 POT neutrinos + 18× 1020 POT antineutrinos◮ 6× 1020/yr for 3+3 years

◮ Assuming sin2 2θ13 = 0.095, sin2 2θ23 = 0.95 or 1.0◮ ∆m2

32 = 2.35× 10−3eV2

Representative event counts for analyses:

νe selected ν ν̄

NC 19 10νµ CC 5 < 1

Beam νe 8 5

Tot bkg 32 15Signal 68 32

νµ selected ν ν̄

QE signal 82 49NC bkg < 1 < 1

non-QE signal 168 78NC bkg 14 6

Uncont. signal 233 134NC bkg 6 3

(0-5GeV visible energy)


Significance to resolve hierarchy

π / δ0 0.2 0.4 0.6 0.8 1 1.2 1.4 1.6 1.8 2

)σsi

gnifi

canc

e of

hie

rarc

hy r

esol

utio

n (

0

0.5

1

1.5

2

2.5

3

3.5

A hierarchy resolution, 3+3 yrνNO

=1.0023θ22=0.095, sin13θ22sin

<02m∆>02m∆

π / δ0 0.2 0.4 0.6 0.8 1 1.2 1.4 1.6 1.8 2

)σsi

gnifi

canc

e of

CP

vio

latio

n (

0

0.5

1

1.5

2

2.5

A CPV determination, 3+3 yrνNO

=1.0023θ22=0.095, sin13θ22sin

<02m∆>02m∆

)σSignificance of hierarchy resolution (0 0.5 1 1.5 2 2.5 3 3.5

δF

ract

ion

of

0

0.1

0.2

0.3

0.4

0.5

0.6

0.7

0.8

0.9

1


=1.0023θ22=0.095, sin13θ22sin

<02m∆>02m∆

)σSignificance of CP violation (0 0.5 1 1.5 2 2.5

δF

ract

ion

of

0

0.1

0.2

0.3

0.4

0.5

0.6

0.7

0.8

0.9

1


=1.0023θ22=0.095, sin13θ22sin

<02m∆>02m∆


Significance to resolve hierarchy including T2K

π / δ0 0.2 0.4 0.6 0.8 1 1.2 1.4 1.6 1.8 2

)σsi

gnifi

canc

e of

hie

rarc

hy r

esol

utio

n (

0

0.5

1

1.5

2

2.5

3

3.5


=1.0023θ22=0.095, sin13θ22sin POT2110×+ T2K at 5.5

<02m∆>02m∆

π / δ0 0.2 0.4 0.6 0.8 1 1.2 1.4 1.6 1.8 2

)σsi

gnifi

canc

e of

CP

vio

latio

n (

0

0.5

1

1.5

2

2.5



<02m∆>02m∆

)σSignificance of hierarchy resolution (0 0.5 1 1.5 2 2.5 3 3.5

δF

ract

ion

of

0

0.1

0.2

0.3

0.4

0.5

0.6

0.7

0.8

0.9

1



<02m∆>02m∆

)σSignificance of CP violation (0 0.5 1 1.5 2 2.5

δF

ract

ion

of

0

0.1

0.2

0.3

0.4

0.5

0.6

0.7

0.8

0.9

1



<02m∆>02m∆


νµ analysis

)θ(22sin0.75 0.80 0.85 0.90 0.95 1.00

)2 e

V-3

| / (

102

m∆|

1.5

2.0

2.5

3.0

3.5

4.0-310×

MINOS: 37.88 kt-y Atmospheric Modeµν POT 20 10× 10.71

3.36 Super-K zenith angle*Super-K L/E*T2K**

90% C.L.MINOS PRELIMINARY

Modeµν POT 20 10×

**PRD 85, 031103(R) (2012)*Neutrino 2012

◮ Current constraints on sin2 2θ23 & 0.9◮ Hints of non-maximal value from MINOS


νµ analysis

◮ Fit quasi-elastic, non-QE, and uncontained samples

◮ Percent level uncertainty on atmospheric parameters in 3+3 years

◮ Exclude maximal mixing at 90% in 1+1 years if sin2 2θ = 0.95


Octant sensitivity

π / δ0 0.2 0.4 0.6 0.8 1 1.2 1.4 1.6 1.8 2

)σsi

gnifi

canc

e of

oct

ant d

eter

min

atio

n (

0

0.5

1

1.5

2

2.5

3

3.5

4

A octant determination, 3+3 yrνNO

/4π<23θ=0.95, 23θ22=0.095, sin13θ22sin

<02m∆>02m∆

)σsignificance of octant determination (0 0.5 1 1.5 2 2.5 3 3.5 4

δF

ract

ion

of

0

0.1

0.2

0.3

0.4

0.5

0.6

0.7

0.8

0.9

1

A octant determination, 3+3 yrνNO

/4π<23θ=0.95, 23θ22=0.095, sin13θ22sin

<02m∆>02m∆

◮ Combine appearance and disappearance analyses

◮ For lower octant to match MINOS best-fit

◮ Upper octant slightly better


∆χ2 scans

MINOS result NOνA sensitivity

log(

L)

∆ -

2

0

1

2

3

4

5

π / CPδ0.0 0.5 1.0 1.5 2.0

68% C.L.

90% C.L.

/4π<23θ<0, 232m∆

/4π>23θ<0, 232m∆

/4π<23θ>0, 232m∆

/4π>23θ>0, 232m∆

MINOS PRELIMINARY appearanceeν disappearance + µν


π / δ0 0.2 0.4 0.6 0.8 1 1.2 1.4 1.6 1.8 2

2 χ∆

0

5

10

15

20

25

30

35

40

45

50

scans, 3+3 yr2χA νExample NO

/2π=δ/4, π<23θ<0, 2m∆=0.95, 23θ22=0.095, sin13θ22sin/4 π<

23θ<0, 2m∆

/4 π<23

θ>0, 2m∆

/4 π>23

θ<0, 2m∆

/4 π>23

θ>0, 2m∆

◮ Calculated For MINOS’s best-fit parameters (IH, lower octant, δ ∼ π2 )

◮ Reject parts of phase-space at high confidence


Conclusion

◮ MINOS has most precise measurement of |∆m232|

◮ And hints for hierarchy and octant

◮ Will continue taking data in the NOνA beam as MINOS+

◮ NOνA detector construction progressing well

◮ Analyzing FD data for neutrino candidates

◮ Good sensitivity for hierarchy and octant

◮ Exciting future for experiments in the NuMI beam


Backup


Neutrino oscillations – theory

|να〉 =∑

i

U⋆αi |νi〉

i = 1, 2, 3 α = e, µ, τ

◮ PMNS matrix. ∼CKM matrix

for neutrinos

Pαβ =

∣

∣

∣

∣

∣

∑

i

U⋆αie

−im2iL/2E

Uβi

∣

∣

∣

∣

∣

2

U =

[

cos θ sin θ− sin θ cos θ

]

Pµµ = 1− sin2 2θ sin2( |∆m2|L

4E

)

2

atmm?

2

23sin2 ?

2

atmm?

2

23sin 2θ

ν2

ν1

ν3

mass2

∆m2atm

Normal Hierarchy

ν3

∆m2atm

ν2

ν1

Inverted Hierarchy

νe

νµ

ντ

∆m2

∆m2


Neutrino oscillations – 3 flavours

U =

1 0 00 c23 s23

0 −s23 c23

c13 0 s13e−iδ

0 1 0−s13e

iδ 0 c13

c12 s12 0−s12 c12 00 0 1

=

c12c13 s12s13 s13e−iδ

−s12c23 − c12s23s13eiδ c12c23 − s12s23s13e

iδ s23c13

s12s23 − c12c23s13eiδ −c12s23 − s12c23s13e

iδ c23c13

◮ “atmospheric”×”reactor”×”solar”

◮ Effect of δ changes sign under CP

◮ Need all three angles nonzero for δ effect

◮ δ has no effect on survival probabilities◮ Only transition (appearance) probabilities

◮ Is δ 6= 0◦, 180◦?


Neutrino oscillations – matter effects

◮ Apparent source of CP violation (Earth is made of matter)◮ CC interactions change effective mass of neutrinos◮ Effect depends on hierarchy

◮ Is the most-νe state the lightest, or one of the heaviest?

∆m2M =

√

(∆m2 cos 2θ ∓ 2√2EGFNe)2 + (∆m2 sin 2θ)2

tan 2θM =tan 2θ

1∓ 2√2EGFNe

∆m2 cos 2θ


The NuMI beam


The NuMI beam

◮ 120 GeV protons from the Main Injector

◮ Strike graphite target

◮ Produce hadrons. Primarily π± and K±

◮ Focused by two magnetic horns

◮ Allow us to select charge sign for aneutrino or antineutrino beam

◮ 675m decay-pipe: π+ → µ+ + νµ

◮ Muons absorbed by rockC. Backhouse (Caltech) MINOS & NOνA December 19, 2013 39 / 33

The NuMI beam – off-axis

0

20

40

60

80

0 2 4 6 8 10Eν (GeV)

ν C

C e

ven

ts /

kt

/ 1

E2

1 P

OT

/ 0

.2 G

eVMedium Energy Tune

on-axis7 mrad off-axis14 mrad off-axis21 mrad off-axis

μ

Eπ (GeV)

Eν (

GeV

)

θ = 0

θ = 7 mrad

θ = 14 mrad

θ = 21 mrad

0

2

4

6

8

10

0 5 10 15 20 25 30 35 40

Flux ∼ 1

L2

(

1

1 + γ2θ2

)2

Eν =0.43Eπ

1 + γ2θ2

◮ Off-axis concept: neutrino energy ∼ independent of pion energy◮ → narrow-band beam, measure rate at oscillation max◮ Reduce NC feed-down from high energy tail


The NuMI beam – off-axis

10-2

10-1

1

10

102

0 1 2 3 4 5Eν (GeV)

Ev

ents

/ k

t/ 3

.7E

20P

OT

/ G

eV

neutral-current

νμ (no oscillation)

νμ (after oscillation)

beam νe

signal νe

Flux ∼ 1

L2

(

1

1 + γ2θ2

)2

Eν =0.43Eπ

1 + γ2θ2

◮ Off-axis concept: neutrino energy ∼ independent of pion energy◮ → narrow-band beam, measure rate at oscillation max◮ Reduce NC feed-down from high energy tail


θ13 results



NDOS beam peak


Documents

Results from MINOS and NOA - NuPHYS - London