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Overview of the Ferm

ilab Neutrino

Program

Steve Brice

PPD Neutrino Department

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Mixing Matrix and Masses

23

2

1

iα/2

2

iα/

iδ

13

13

-iδ

13

3

23

213

12

12

12

12

2+iβ

µ τe

33

c0

s1

00

0c

10

0ν

=0

e

e

01

0

-se

cs

0

-sc

0

0

0ν

00

s

0-

00

sc

νc

eννν

1

∆ ∆∆∆m232

∆ ∆∆∆m221

(m3)2

(m2)2

(m1)2

Norm

al hierarchy

∆ ∆∆∆m221

(m2)2

(m1)2

(m3)2

∆ ∆∆∆m231

Inverted hierarchy

ν ννν e ν ννν µ µµµ ν ννν τ τττ

3σ

σ

σ

σ Ranges

∆ ∆∆∆m221

: (7.0 -9.1) ×10-5eV2

TAN2θ θθθ 12: 0.34 –0.62

∆ ∆∆∆m232

: (1.9 –2.98) ×10-3eV2

TAN2θ θθθ 23: 0.49 –2.2

SIN2θ θθθ 13 ≤0.045

δ δδδunknown

Hierarchy unknown

mlightest< 2.2 eV

Dirac or Majoranaunknown

[updated from Gonzalez-Garcia PASI 2006]

m2lightest

m2lightest

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Open Questions in Neutrino Physics

•General

Is the picture more complex? MiniBooNE, MicroBooNE

What are the cross-sections?

MiniBooNE, SciBooNE,

MINERν νννA, MicroBooNE

•12 Sector

•23 Sector

–Is θ θθθ23maximal? MINOS, NOν νννA

•13 Sector

–What is the value of θ θθθ 13? NOν νννA, LBNE

–How are the mass eigenstatesordered? NOν νννA, LBNE

–Is CP violated? LBNE

•Mass

–What are the neutrino masses? No plans to

–Are neutrinos their own anti-particles? address at FNAL

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FNAL Neutrino Program

•8 GeV protons from the Booster

–Neutrinos from Booster Neutrino Beam (BNB) to…

•MiniBooNE (running)

•SciBooNE(completed in 2008)

•MicroBooNE(approved, design phase)

•120 GeV protons from the Main Injector

–Neutrinos from NuMIto…

•MINOS (running)

•ArgoNeut(being installed)

•MINERvA(under construction)

•NOvA(passed CD2, CD3a, awaiting funding)

–Neutrinos from a new beamlineto…

•LBNE (pre CD0)

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Keep L/E same as LSND

while changing systematics, energy & event signature

P(ν

µν e)= sin

2 2θ sin2 (1.27∆m

2 L/Ε)

Booster

K+

targ

et and h

orn

dete

cto

rdirt

decay

regio

nabsorb

er

prim

ary

beam

tertia

ry b

eam

secondary

beam

(pro

tons)

(mesons)

(neutrin

os)

π+ν µ

→ν e

???

Order of magnitude

higher energy (~500 MeV)

than LSND (~30 MeV)

Order of magnitude

longer baseline (~500 m

)than LSND (~30 m

)

MiniBooNE

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Main MiniBooNE Result

Two independent analyses show

no evidence for ν

µ→ν e

appearance-only oscillations.

No ν

eexcess in oscillation signal region

but 96 ±

17 ±

20 events above

background, for 300<EnQE<475MeV

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MiniBooNE Status

•Taken ~6.6 x 1020POT in neutrino m

ode

–Making suite of cross-section m

easurements

–Searching for various neutrino oscillations

–Found interesting excess of low energy ν

ecandidates

–Publications coming out

•Taken ~4.5 x 1020POT in anti-neutrino m

ode

–Making suite of cross-section m

easurements

–Searching for anti-neutrino appearance and disappearance

–No evidence of a low energy ν

ecandidate excess

–Request to PAC for 10.0 x 1020POT with further running

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SciBooNE

SciBooNETimeline

•2005, Summer -Collaboration form

ed

•2005, Dec -Proposal

•2006, Jul -Detectors m

ove to FNAL

•2006, Sep -Groundbreaking

•2006, Nov -EC Assembly

•2007, Feb -SciBarAssembly

•2007, Mar -MRD Assembly

•2007, Mar -Cosmic Ray Data

•2007, Apr -Detector Installation

•2007, May –

Commissioning

•2007, Jun -Neutrino Data Run

•2008, Aug –

Run Ends

Idea: Put well developed

K2K SciBardetector into

the well understood FNAL

Booster Neutrino Beamline

•Precision measurement of xsecsfor T2K

•BNB beam well m

atched to T2K beam

•Low cost (<$1M)

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SciBooNEOutlook

•First Result

–No evidence for CC coherent pionproduction found

–Confirm

s K2K result, sets stronger limit

–σCoh/σCC < 0.67x10-2 (90% CL) at 1.1 GeV

–Also have small higher energy sample

–σCoh/σCC < 1.36x10-2 (90% CL) at 2.2 GeV

•Outlook

•11 current PhD students

•Up to 8 new results in the next year

•Shooting for NuInt09 workshop in m

ost cases

•Will maintain strong presence at Ferm

ilab until spring 2009

•Maintain analysis center at Ferm

ilab for several more years

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10

MINOS

Far detector

Near detector

Far Detector:

Soudan, Minnesota, 735 km from target

5.4 ktonmass

484 steel/scintillatorplanes, 8x8x30 m

3

Near Detector:

Ferm

ilab, 1km from target

1 ktonmass

282 steel planes

153 scintillatorplanes, 3.8x4.8x15 m

3

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Main MINOS Result

322.

4100

.1

2sin

eV 10

38

.2

2

08

.0

23

2

23

20

.0

16

.0

2 23

==Θ

×=

∆

−

−+ −

DoF

N

m χ

2.50 POT analyzed ≈

2x statistics of 2006 result

Also improved m

odeling, reconstruction, and PID

Comparison of

new and old

MINOS results

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MINOS Near Term

Outlook

•Expect data set of 7 x 1020POT by summer 2009.

–This doubles the currently published CC sample.

•Electron neutrino appearance

–First result with 3.25 x 1020POT two weeks ago

–Analysis of doubled dataset to follow

•Neutral currents

–Extended analysis of 3.25 x 1020POT by early 2009

–Analysis of doubled dataset by end 2009

•Muon Antineutrino disappearance

–3.2 x 1020POT exposure result nearly completed. Expect results early 2009.

–Using 6% intrinsic beam antineutrinos

•Total cross-section from Near Detector

–Low m

odel dependence flux determ

ination

–Expect end of 2008

•Request to switch to anti-neutrino running after the 2009 shutdown

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13

MINERνA

MINOS near detector(muon spectrometer)(

Fully

Active S

cin

tilla

tor Targ

et R

egio

n8.3

tons (~3 tons fid

ucia

l)(

Veto

Wall

NuM

IBeam

Liq

uid

He

0.2

5to

n

Nucle

ar Targ

et R

egio

n w

ith P

b, Fe, C

6.2

tons (in

clu

din

g 4

0%

Scin

tilla

tor)

EC

AL

HC

AL

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MINERνA

Physics Program

•Quasi-elastic scattering

•Resonance Production -1pi

•Resonance/transition Region –npi

resonance to DIS

•Deep-Inelastic Scattering

•Coherent Pion Production

•Strange & Charm Particle Production

•sT, Structure Functions and PDFs

–s(x) and c(x)

–High-x parton distribution

functions

•Nuclear Effects

•Generalized Parton Distributions

MIN

ERνA

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MINERνA

Proposed Schedule

•Continue construction and commissioning, with cosmics, of the

Tracking Prototype at WideBand Hall.

•If successful, install in NuMI beam early in CY2009 to check

response to neutrino beam.

•Continue commissioning of tertiary test beam through end

CY2008.

•Install and commission test beam detector as well as test beam

physics runs in CY2009.

•Complete construction of full MINERnA detector and install in

stages throughout CY2009, partial commissioning as we install.

•Begin commissioning of full detector toward end of CY2009.

•Begin physics data taking end-CY2009/beginning-CY2010.

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16

How to Measure the 13 Sector

21.27

/ij

ijmLE

∆≡

∆L(km), E(M

eV), m

(10-3eV)

Probed by m

easuring the

disappearance of reactor produced

electron anti-neutrinos.

Need to work at an L/E m

atched to

the atm

ospheric ∆m

2

(C.F. Kamlandmeasurement at

solar ∆m

2)

3

1

42

2

22

12

23

1

22

1

1

12

12

3

2

32

()

1co

ssin

2sin

sin

2(cos

sin

sin

sin

)

ee

Pθ

ν

θθ

θ

θν

→=

−

+∆

∆

∆

−

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17

12

21

12

31

23

31

31

23

31

23

32

31

31 3

2

22

22

2

22

21

12

22

2

332

13

13

13

sin

()

()

sin

sin

2(

)

sin

()

cos

sin

2(

)

sin(

)sin(

)co

ssin2

sin2

sin2

cos

()

()

sin(

sin

sin2

sin2

sin2

sin

e

aL

PaL

aL

aL

aL

aL

aL

aL

µ

θθ

δθ

δθ

θ

ν

θ

ν

θ

θθ

θ→

= +

∆∆

∆

+

∆

∆∆

∆ ∆∆

∆

∆

+

∓

∓

∓

∓ 131

1

31

2

)sin(

)

()

()

aL

aL

aL

aL

∆

∆

∆

∓

∓

How to Measure the 13 Sector (cont)

1/

2(4000km)

Fe

aGN

−≡

≈

21.27

/ij

ijmLE

∆≡

∆L(km), E(GeV), m

(eV)

Matter effect

():

sin

sin

,e

Pa

aµ

δν

νδ

→→

−→

−

Also probed by m

easuring electron neutrino appearance from

accelerator produced m

uon neutrinos

Need to have an L and E such that interference between solar and

atm

ospheric scales can bee seen

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18

Matter Effects and CP

ν’s

and a

nd a

nti-ν

’scan b

e u

sed to d

istinguis

h a

mbig

uitie

s

Matter effect

CP e

ffect

Norm

al hierarchy

sin

2(2θ 1

3)= 0.04

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NOνA

Far detector:

18 kton, fully active segmented detector

12 km off NuMIbeamlineaxis

810 km baseline

optical

fibre

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NOνA

Near Detector

186 liquid scintillatorplanes in target

10 in m

uon ranger, 1m steel

Same cell size as far detector

Readout from one side per plane

with APDsplus faster electronics

than far detector

Requires some additional excavation in

NuMItunnel in order for detector to be at

proper 14 m

radangle

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NOνA

θ 13Sensitivity

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NOνA

Mass Hierarchy Sensitivity

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NOνA

Schedule

Best estimate of schedule:

–Apr 2009

Start of Construction (assumes FY09 funding final before March 6)

–Jun 2011

Far Detector Building Beneficial Occupancy

–Aug 2012

1st 2.5 kT of the Far Detector Online

–Jan 2014

Full Far Detector Online

Apr 3

0 2

008

Passed R

epeatC

D-2

/3a R

evi

ew

May

29 2

008

Re-recom

mended b

y P5 u

nder Scenario B

or better

July

1

2008

Supple

menta

l bill resto

res $

9.5

M N

OνA

fundin

gSep 1

5 2

008

CD

-2 G

rante

dO

ct 2

4 2

008

CD

-3a G

rante

d: $17.3

M for lo

ng-lead ite

ms:

$8.9

M for fa

r site p

rep -

road a

nd e

xcava

tion

$6.2

M for AN

U toolin

g, parts, and instrum

enta

tion

$2.1

M for scin

tilla

torw

ave

-shift

ers

(sin

gle

sourc

e)

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Neutrino Program Evolution

•Numerous studies over the past several years have laid out

options for further exploring the neutrino sector

•In particular, searching for CP violation

•i.e. BNL-FNAL US long baseline neutrino experiment study

(March 2006-June 2007) explored

–Beam options

–NuMI , newWide Band Beam at a longer baseline

–On and off axis detector locations

–Detector technology options

•Water cerenkov, liquid argon

•These studies m

ake sense in the context of a non-zero

determ

ination of θ13

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General Conclusions

•Future experiments using conventional* neutrino beams

can be designed to have 3-5σdiscovery potential for

measuring CP violation and the neutrino mass

hierarchyfor values of sin

22θ13as low as ~ 0.01

•These sensitivities are reached assuming :

–aproton sourceat the Megawatt level (or decades of running

time)

–a neutrino beam

optimized to the oscillation probability

(covering the 1st and 2nd oscillation m

aximum)

–an experiment baseline> 1000 km

(to improve the

sensitivity to determ

ine the m

ass hierarchy)

–aDetectorwith effective m

ass (mass*efficiency) > 100kT

•If nature has m

ade θ

13very small we m

ay need to consider

a non-conventional neutrino source, i.e. neutrino factory

from P5 report

from P5 report

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Ferm

ilab to HomestakeDUSEL (1290km)

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Advantage of the Longer Baseline

•Oscillation m

axima are m

oved to higher energy

•Matter effects are significantly larger

Plo

t by

Nik

i Saoulid

ou

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Neutrino Beam Requirements*

•The maximal possible neutrino fluxesto encompass at least the

1st and 2nd oscillation nodes, which occur at 2.4 and 0.8 GeV

respectively

•Since neutrino cross-sections scale with energy, larger fluxes at

lower energiesare desirable to achieve the physics sensitivities

using effects at the 2nd oscillation node

•To detect νµ→νeat the far detector, it is critical to minimize the

neutral-current contamination at lower energy, therefore

minimizing the fluxof neutrinos with energies greater than 5 GeV

where there is little sensitivity to the oscillation parameters is

highly desirable

•The irreducible background to νµ→νeappearance signal comes

from beam generated νeevents, therefore, a high purity νµbeam

with as low as possible νe contamination is required

*From “Simulation of a W

ide-Band Low-Energy Neutrino Beam for Very Long Baseline

Neutrino Oscillation Experiments”, Bishai, Heim, Lewis, Marino, Viren, Yumiceva

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Worldwide Concepts for a Large Detector

Gla

cie

r

FLAR

E

LA

NN

D

Water Cerenkov

Liquid Argon

Liquid Scintillator

100 k

T

Mem

phys

LE

NA

Hyp

er-

Kam

iokande

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WC-100 x 3 @

HomestakeDUSEL

25%

PM

T c

overa

ge

60,0

00 1

0 inch P

MT’s

per m

odule

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Liquid Argon Phased Program

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LBNE Collaboration Organisation

•Several workshops/m

eetings

–April 24 at Leed South Dakota

–June 20 at FNAL

–August 14 at FNAL

–October 14-15 at BNL

–February 26-28 at UC Davis

•Temporary Executive Committee form

ed

•Form

ed an Institutional Board of “interested groups”

•WC and LAr groups submitted Proposals for the NSF S4

solicitation

•Working Towards DOE CD-0

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Summary

•The last decade has been revolutionary in neutrino physics

•The next decade promises an even m

ore rapid development of our

understanding

•The m

asses and m

ixings are giving us hints of physics well

beyond the Standard Model

•Ferm

ilab has a vibrant current, near term

, and far term

program

at the heart of this global effort

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Cross-Sections with MiniBooNE

By almost 2 orders of magnitude

MiniBooNE has the largest ~1 GeV

neutrino data set ever taken.

A range of Cross-Section m

easurements

are planned:-

•CC Quasi-elastic (MA, oscsignal channel)

•NC elastic (compare to CC QE)

•CC π+

(disapp. osc. bkgd, coh. prod.)

•NC π

0 (oscbkgd., coh. prod.)

•CC π

0 (compare to NC channel)

Cross-Sections are also being

published by the K2K collaboration

First CCQE paper completed (arXiv:0706.0926 [hep-ex])

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Cross-Sections with MINERνA

The νSNSexperiment is planning to m

easure cross-sections of 10-50 MeVneutrinos

produced by stopped pionsand m

uonsat SNS. Necessary input to supernova calculations

High granularity detector in NuMIbeamline

Large physics program including xsecmeasurements at a few GeV

“Chewy center (active target), with a crunchy shell of muon, hadron, and EM absorbers”

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Off Axis Beams

ν ννν µ µµµOA2

∆m

2=3x1

0-3eV

2

L=295km

θTargetHorns

Dec

ay Pipe

Far

Detector

Near

Detector

•Increases flux on osc. max.

•Reduces high-E tail, and

thus NC backgrounds

•Reduces ν

econtamination

from K and µ

decay