# Presentation: 095803

## Neutrino Experiments

- Status, recent progress, prospects
- Steve Brice
- Fermilab

## Mixing Matrix and Masses

******m****2****32**

******m****2****21**

- (m3)2

- (m2)2

- (m1)2

- Normal hierarchy

******m****2****21**

- (m2)2

- (m1)2

- (m3)2

******m****2****31**

- Inverted hierarchy

******e**

********

********

**3********Ranges**
******m****2****21**** ****	****: (7.0 - 9.1) × 10****-5**** eV****2**
**TAN****2********12**** ****	****: 0.34 – 0.62**
******m****2****32**** ****	****: (1.9 – 2.98) × 10****-3**** eV****2**** **
**TAN****2********23**** ****	****: 0.49 – 2.2**
**SIN****2********13 ****≤ 0.045**
****** ****unknown**
**Hierarchy unknown**
**m****lightest**** < 2.2 eV**
**Dirac or Majorana unknown**
**         **[updated from Gonzalez-Garcia PASI 2006]

**m****2****lightest**

**m****2****lightest**

## Talk Overview

- Intro
**More than 3 neutrino types?**
- 12 Sector
- 23 Sector
**Is ********23**** maximal?**
- 13 Sector
**What is the value of ********13****?**
**How are the mass eigenstates ordered?**
**Is CP violated?**
- Mass
**What are the values of the neutrino masses?**
**Are neutrinos their own anti-particles?**
- Summary

- Philosophy:- Describe the status of the field, highlighting progress
- made in the last 2 years (since last EPS HEP conference), and
- outlining prospects for the near (~5 year) future.

**Connections to the parallel talks given last week will be** **highlighted in red**

## Not Covered in this Talk

- Theoretical developments – see next talk
- Cosmic ray neutrinos (e.g. IceCube) – see previous talk
- Neutrinos in cosmology
- Neutrino magnetic moment searches
- Recent result: A.G. Beda et al., "The first result of the neutrino magnetic moment measurement in GEMMA", arXiv:0705.4576
- < 5.8 x 10^{-11} B 90% CL
- BB Relic neutrinos
**M. Messina parallel talk Fri AM**
- Experiments more than ~5 years distant
- Superbeams beyond NOA and T2K
- Neutrino Factory
- Beta Beams
**C. Espinoza parallel talk Thu PM (EC Beam)**
**T. Tabarelli parallel talk Thu PM (Beta Beam and Atmospheric)**
**C. Orme parallel talk Thu PM (Beta Beam)**

## LSND

- LSND:
**Excess of ********e**** events in a ************ beam**
**87.9 ± 22.4 ± 6.0 over background**
**~4******** evidence for ******** oscillation**

**L/E dictates ********m****2 ****be very different**
**from the well established solar and **
**atmospheric ********m****2****s.**
**Z width dictates 3 light, active**
**neutrinos and therefore only**
**2 independent ********m****2****s**
**Therefore is the LSND result evidence for a sterile neutrino?**

## MiniBooNE

- Keep L/E same as LSND
- while changing systematics, energy & event signature

- Order of magnitude
- higher energy (~500 MeV)
- than LSND (~30 MeV)

- Order of magnitude
- longer baseline (~500 m)
- than LSND (~30 m)

## MiniBooNE Result

- Two independent analyses show
- no evidence for   e
- appearance-only oscillations.

- No e excess in oscillation signal region
- but 96 ± 17 ± 20 events above background, for 300<EnQE<475MeV

**M. Sorel parallel talk Fri AM**

**M. Maltoni parallel talk Fri AM**

## The 12 Sector

******m****2****32**

******m****2****21**

- (m3)2

- (m2)2

- (m1)2

- Normal hierarchy

******m****2****21**

- (m2)2

- (m1)2

- (m3)2

******m****2****31**

- Inverted hierarchy

******e**

********

********

**3********Ranges**
******m****2****21**** ****	****: (7.0 - 9.1) × 10****-5**** eV****2**
**TAN****2********12**** ****	****: 0.34 – 0.62**
******m****2****32**** ****	****: (1.9 – 2.98) × 10****-3**** eV****2**** **
**TAN****2********23**** ****	****: 0.49 – 2.2**
**SIN****2********13 ****≤ 0.045**
****** ****unknown**
**Hierarchy unknown**
**m****lightest**** < 2.2 eV**
**Dirac or Majorana unknown**
**         **[updated from Gonzalez-Garcia PASI 2006]

**m****2****lightest**

**m****2****lightest**

## How to Measure the 12 Sector

- Probed by measuring neutrino disappearance
- in solar neutrino experiments

- Also probed by measuring anti-neutrino
- disappearance with the Kamland reactor
- neutrino experiment

**E******** > ~5 MeV**
**E******** < ~2 MeV**

**For E********/L = O(********m****12****2****)**

**L(km), E(MeV), ********m****2****(10****-3****eV****2****)**

- A. De Gouvea NUSS 07

## SNO

- Solved the solar neutrino problem
- Charged current measurement of electron flavour coupled with neutral current measurement of all active flavours provides conclusive proof of flavour transformation

**S. Peeters parallel talk Fri AM**

## Kamland

- S. Enomoto WIN05

- Use                        in 1000 tons of liquid
- scintillator to measure disappearance of e
- produced by large number of Japanese reactors

- Clear evidence for oscillation
- not merely disappearance

## State of 12 Sector

- Schwetz hep/ph 0606060

**Dashed = 90% CL**
**Solid and shaded = 99.73% CL**

- sin212

- 10-5

- 10-4

- m221 [eV2]

- Crucial input also from the Chlorine, Super-K, SAGE, and GALLEX solar  experiments

## SNO
Phase 3 (NCDs) results expected soon
Kamland II (Solar Neutrino Phase)
Scintillator purification ongoing
Borexino
Detector complete
Data taking started May 16
Kamland and Borexino plan to use neutrino scattering from electrons to measure Ev~1-2 MeV
See the change in                   from MSW effect

Other efforts to measure 1-2 MeV solar neutrinos
SNO+, LENA
Several collaborations looking to measure solar neutrinos below ~1 MeV using inverse beta decay
LENS(115In), MOON(100Mo), SIREN(160Gd)

- SNO
- Phase 3 (NCDs) results expected soon
- Kamland II (Solar Neutrino Phase)
- Scintillator purification ongoing
- Borexino
- Detector complete
- Data taking started May 16
- Kamland and Borexino plan to use neutrino scattering from electrons to measure Ev~1-2 MeV
- See the change in                   from MSW effect
- Other efforts to measure 1-2 MeV solar neutrinos
- SNO+, LENA
- Several collaborations looking to measure solar neutrinos below ~1 MeV using inverse beta decay
- LENS(115In), MOON(100Mo), SIREN(160Gd)

- Upcoming 12 Sector Measurements

- Shimizu DBD07

## The 23 Sector

******m****2****32**

******m****2****21**

- (m3)2

- (m2)2

- (m1)2

- Normal hierarchy

******m****2****21**

- (m2)2

- (m1)2

- (m3)2

******m****2****31**

- Inverted hierarchy

******e**

********

********

**3********Ranges**
******m****2****21**** ****	****: (7.0 - 9.1) × 10****-5**** eV****2**
**TAN****2********12**** ****	****: 0.34 – 0.62**
******m****2****32**** ****	****: (1.9 – 2.98) × 10****-3**** eV****2**** **
**TAN****2********23**** ****	****: 0.49 – 2.2**
**SIN****2********13 ****≤ 0.045**
****** ****unknown**
**Hierarchy unknown**
**m****lightest**** < 2.2 eV**
**Dirac or Majorana unknown**
**         **[updated from Gonzalez-Garcia PASI 2006]

**m****2****lightest**

**m****2****lightest**

## How to Measure the 23 Sector

- Probed by measuring muon neutrino disappearance
- in atmospheric neutrino experiments

- The same oscillations can also be measured by measuring
- muon neutrino disappearance from beam created at accelerators

- L(km), E(GeV), m(eV)

## Atmospheric Neutrinos at SuperK

- “Atmospheric Neutrino Anomaly” caused by muon neutrinos oscillating away. Presumably into tau neutrinos
- SuperK has some evidence for tau neutrino appearance – Need CNGS confirmation

- Kajita NuSS 2007

**K. Kaneyuki parallel talk Fri AM**

## K2K: Confirming Atmospheric Oscilllations

- First accelerator confirmation
- of atmospheric neutrino
- oscillations came from K2K

|  | Nskobs | Nskpred |
| --- | --- | --- |
| All | 112 | 155.9 |
| 1 ring | 67 | 99.0 |
| -like | 58 | 90.8 |
|       e-like | 9 | 8.2 |
| multi-ring | 45 | 56.8 |

## MINOS

- Far detector

- Near detector

- Far Detector:
- Soudan, Minnesota, 735 km from target
- 5.4 kton mass
- 484 steel/scintillator planes, 8x8x30 m3

- Near Detector:
- Fermilab, 1km from target
- 1 kton mass
- 282 steel planes
- 153 scintillator planes, 3.8x4.8x15 m3

## New MINOS Result Last Thursday

- 2.50 POT analyzed ≈ 2x statistics of 2006 result
- Also improved modeling, reconstruction, and PID

- Comparison of new and old MINOS results

**A. Weber parallel talk Thu PM**

## Current State of 23 Sector

## Opera

- Hall B

****** ****spectrometer: Dipolar magnet + RPC chambers**

**Target Trackers**
**Pb/Em. target**

**Precision tracker: Drift tubes**

- 

- brick
- (56 Pb/Em. “cells”)

**8 cm ****(****10X****0****)**

- scintillator strips

- brick wall

- module

- A hybrid emulsion
- and tracking detector
- Goal: Verify that the 
- are oscillating into 

- Pb target 1.8 kton
- CNGS:
- Beam <E> ≈ 17 GeV
- Baseline 732 km
- Expected event rate:
- ~3600  NC+CC /kton/year
- ~16  CC /kton/year
- (for sin2223=1, m322=2.5x10-3 eV2)

**G. Wilquet parallel talk Thu PM**

**A. Murst Guler  parallel talk Thu PM (Assoc. Charm Prod.)**

## Opera Latest

- Tracking tested with CNGS runs in Aug and Oct 2006
- Brick installation started Sep 2006 (~20000 currently stored)
- May 2007 cosmic ray test with 15000 bricks.
- 	Tested chain:
- 	Prediction / Brick Extraction / Development / Scanning
- 	Worked well
- Sep 2007 CNGS neutrino beam on 50000-60000 bricks.
- Full (170,000 Bricks) planned for Mar 2008.

- Sato DBD07

## The 13 Sector

******m****2****32**

******m****2****21**

- (m3)2

- (m2)2

- (m1)2

- Normal hierarchy

******m****2****21**

- (m2)2

- (m1)2

- (m3)2

******m****2****31**

- Inverted hierarchy

******e**

********

********

**3********Ranges**
******m****2****21**** ****	****: (7.0 - 9.1) × 10****-5**** eV****2**
**TAN****2********12**** ****	****: 0.34 – 0.62**
******m****2****32**** ****	****: (1.9 – 2.98) × 10****-3**** eV****2**** **
**TAN****2********23**** ****	****: 0.49 – 2.2**
**SIN****2********13 ****≤ 0.045**
****** ****unknown**
**Hierarchy unknown**
**m****lightest**** < 2.2 eV**
**Dirac or Majorana unknown**
**         **[updated from Gonzalez-Garcia PASI 2006]

**m****2****lightest**

**m****2****lightest**

## How to Measure the 13 Sector

- L(km), E(MeV), m(10-3eV)

- Probed by measuring the disappearance of reactor produced
- electron anti-neutrinos.
- Need to work at an L/E matched to the  atmospheric m2
- (C.F. Kamland measurement at solar m2)

## How to Measure the 13 Sector (cont)

- L(km), E(GeV), m(eV)

- Matter effect

- Also probed by measuring electron neutrino appearance from
- accelerator produced muon neutrinos
- Need to have an L and E such that interference between solar and
- atmospheric scales can bee seen

## Current State of 13 Sector

- Schwetz hep/ph 0606060

- sin213

- 10-3

- 10-2

- m231 [eV2]

## How to Improve on Chooz

**Increase statistics:**
- Use more powerful nuclear reactors
- Utilize larger target mass, hence larger detectors
**Suppress background:**
- Go deeper underground to gain overburden for reducing cosmogenic background
**Reduce systematic uncertainties:**
- Reactor-related:
- Optimize baseline for best sensitivity and smaller reactor-related errors
- Near and far detectors to minimize reactor-related errors
- Detector-related:
- Use “Identical” pairs of detectors to do *relative *measurement
- Comprehensive program in calibration/monitoring of detectors
- Interchange near and far detectors (optional)

- Peng DBD07

**G. Mention parallel talk Thu AM**

## Double Chooz

- Near

- Far

- 0.28 km

- 1.05 km

- Suekane DBD07

**I. Gil Botella parallel talk Thu AM**

## Daya Bay

**V. Vorobel parallel talk Thu AM**

## Double Chooz Latest

- Final stages of R&D
- Detector construction starts this year
- First data taking expected to start in 2008 with far detector
- Get down to sin2213 < 0.06 in 1.5 years
- Start taking data with both detectors in 2010
- Get down to sin2213 < 0.025 in 3 years

- Suekane DBD07

- Daya Bay Latest

- Oct 2006: Passed DOE scientific review
- Apr 2007
- Passed DOE CD-1 review
- Passed final nuclear safety review in China
- Began to receive 3 year project funding from Chinese agencies
- Jun 2007: Began civil construction
- Oct 2007: Anticipate DOE CD-2/3a review
- May 2009: Start data taking with 2 detectors at Daya Bay near hall
- Apr 2010: Start data taking with 8 detector final configuration

- Peng DBD07

- Other reactor efforts ongoing: Angra (Brazil), RENO (Korea)

## Off Axis Beams

********** **

**OA2°**

- m2=3x10-3eV2
- L=295km

- 

- Target

- Horns

- Decay Pipe

- Far
- Detector

- Near
- Detector

- Increases flux on osc. max.
- Reduces high-E tail, and thus NC backgrounds
- Reduces e contamination from K and  decay

## NOA

- Far detector:
- 18 kton, fully active segmented detector
- 12 km off NuMI beamline axis
- 810 km baseline

**optical**
**fibre**

## NOA Near Detector

- 186 liquid scintillator planes in target
- 10 in muon ranger, 1m steel
- Same cell size as far detector
- Readout from one side per plane
- with APDs plus faster electronics
- than far detector

- Requires some additional excavation in NuMI tunnel in order for detector to be at proper 14 mrad angle

## T2K

- Beam from JPARC to SuperK

**M. Zito parallel talk Thu AM**

## T2K Near Detector (@280m Offaxis)

- Near Detector @ 280m
- Built inside UA1/NOMAD magnet for p measurement
- Sandwich calorimeters/trackers and TPCs for precision beam spectrum and composition measurement.
- Particular attention paid to measuring 0 from neutral current interactions

- 0 detector

- tracker

- FGDs

- TPCs

- ECAL

- Magnet
- yoke

- Magnet
- coils

- beam

## NOA Latest

- Accelerator upgrades merged with NOA detector project Dec 20 2006 (upgrades for a 700kW source)
- Cap on total project cost of $260M put in place late Dec 2006
- DOE CD1 approval announced May 11
- Currently working to get cost below $260M
- Hoping to start detector construction in 2010 and have 700kW source on same timescale

- T2K Latest

- JPARC Linac beam commissioning Dec 2006
- First horn prototype operated successfully with 8.5x105 pulses
- JPARC Rapid Cycling Synchrotron Beam Commissioning Sep 2007
- JPARC Main Ring Beam Commissioning: May, 2008
- Hoping for first data April 2009
- Ramp up to 750kW source by 2012

## An Aside on GeV Neutrino Cross Sections

- Compilation of  CC Quasi-Elastic Cross-Section Measurements

- The CCQE xsec is
- the best known!!
- Background xsecs
- for NOa and T2K
- are known much
- more poorly
- If NOA and T2K
- are to perform as
- we hope then the
- xsecs need to be
- better constrained

**A. Bodek parallel talk Thu PM**

## Cross-Sections with MiniBooNE

**A. Blondel parallel talk Thu PM (HARP)**

**M. Wascko/B. Roe parallel talk Fri AM**

- By almost 2 orders of magnitude
- MiniBooNE has the largest ~1 GeV
- neutrino data set ever taken.
- A range of Cross-Section measurements
- are planned:-
- CC Quasi-elastic (MA, osc signal channel)
- NC elastic (compare to CC QE)
- CC  + (disapp. osc. bkgd, coh. prod.)
- NC 0 (osc bkgd., coh. prod.)
- CC 0 (compare to NC channel)

- Cross-Sections are also being
- published by the K2K collaboration

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

## Cross-Sections with SciBooNE

- SciBooNE Timeline
- • 2005, Summer - Collaboration formed
- • 2005, Dec - Proposal
- • 2006, Jul - Detectors move to FNAL
- • 2006, Sep - Groundbreaking
- • 2006, Nov - EC Assembly
- • 2007, Feb - SciBar Assembly
- • 2007, Mar - MRD Assembly
- • 2007, Mar - Cosmic Ray Data
- • 2007, Apr - Detector Installation
- • 2007, May - Commissioning
- • 2007, Jun - Neutrino Data Run

- Idea: Put well developed
- K2K SciBar detector into
- the well understood FNAL
- Booster Neutrino Beamline
- Precision  measurement of xsecs for T2K
- BNB beam well matched to T2K beam
- Low cost (<$1M)

**M. Wascko parallel talk Fri AM**

## Cross-Sections with MINERA

- The SNS experiment is planning to measure cross-sections of 10-50 MeV neutrinos produced by stopped pions and muons at SNS. Necessary input to supernova calculations

- High granularity detector in NuMI beamline
- Large physics program including xsec measurements at a few GeV

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

## The Masses

******m****2****32**

******m****2****21**

- (m3)2

- (m2)2

- (m1)2

- Normal hierarchy

******m****2****21**

- (m2)2

- (m1)2

- (m3)2

******m****2****31**

- Inverted hierarchy

******e**

********

********

**3********Ranges**
******m****2****21**** ****	****: (7.0 - 9.1) × 10****-5**** eV****2**
**TAN****2********12**** ****	****: 0.34 – 0.62**
******m****2****32**** ****	****: (1.9 – 2.98) × 10****-3**** eV****2**** **
**TAN****2********23**** ****	****: 0.49 – 2.2**
**SIN****2********13 ****≤ 0.045**
****** ****unknown**
**Hierarchy unknown**
**m****lightest**** < 2.2 eV**
**Dirac or Majorana unknown**
**         **[updated from Gonzalez-Garcia PASI 2006]

**m****2****lightest**

**m****2****lightest**

## How to Measure the Masses

- Direct kinematic search: Look for a distortion at the end-point
- of a  decay spectrum.

- Low endpoint energy optimal therefore use tritium (18.6keV)
- 	(Also an effort to use 187Re with 7x lower endpoint)
- Existing limit from tritium endpoint measurement: m < 2.2eV 95% CL

- (Mainz and Troitsk groups)

## Katrin

- Spectrometer being transported Nov 2006

- Gaseous tritium source

- Transport section

- Pre-spectrometer

- Main spectrometer

- Detector

- 2005 vacuum tests of pre-spectrometer
- 2006 electromagn. tests of pre-spectrometer,      main spectrometer on site
- 2007 source demonstrator, inner electrode mounting
- 2008 commissioning of WGTS, tritium loops, em. test of spectrometers
- 2009 system integration & first tritium runs
- regular data taking for 5-6 years

- G. Drexlin

## How to Measure the Masses (cont)

- Search for 0**** double **** decay:
- In many even-even nuclei, **** decay
- is energetically forbidden.This leaves
**** as the allowed decay mode.
- 2**** decay has been observed in
- several nuclei, but 0**** has not yet.

- G0 = phase space factor (~Q5)
- M0= nuclear matrix element
- , are the Majorana phases

**0****νββ**

**2****νββ**

**(T****e1****+T****e2 ****) / Q****ββ**

- If observed it would imply a massive Majorana neutrino

## 0 Decay Measurements

**Soldner-Rembold parallel talk Thu AM (NEMO-3)**

- Survey of some past and present experiments

- A. Nucciotti arXiv:0707.2216 [nucl-ex]

- Timescales: 	t1/2(U,Th) ~ Tuniverse
- 		t1/2(2) ~ 1010Tuniverse
- 		t1/2(0) ~ 1017Tuniverse

## Ge Claim 

**Heidelberg-Moscow (in Gran Sasso)**
- Enriched Ge detectors
- Operating 1990-2003
- Total exposure ~71.7 kg·y
- Longest running 0 expt. by far
- Part of collaboration claim:
- T1/2 = (0.7 – 4.2)·1025 y (3 σ)
- m ≈ 0.44 eV

## Combining 0 and Oscillation Knowledge

- Switch “bases” from (m1,m2,m3)  to  (m212,m322,mlightest)
- m212,m322  come from oscillation experiments
- Majorana phases ****,**** completely unknown
- mlightest could be constrained by 0**** decay

- Very interesting distinction
- between the normal and
- inverted mass hierarchies
- Normal hierarchy:
- At least one neutrino has
**m****i****>√(********m****32****2****)≈0.05eV**
- Inverted hierarchy:
- At least _two_ neutrinos have
**m****i****>√(********m****32****2****)≈0.05eV**

- Ge claim

## Future 0 Prospects

**K. Kroeninger parallel talk Thu AM (GERDA)**

**I. Bandac parallel talk Thu AM (CUORE)**

- A sample of the proposed experiments

- A. Nucciotti arXiv:0707.2216 [nucl-ex]

## Summary

- The last decade has been revolutionary in neutrino physics
- The next decade promises an even more rapid development of our understanding
- The masses and mixings are giving us hints of physics well beyond the Standard Model
- Can we develop these hints?
- In the upcoming era of LHC physics the neutrino realm will provide a unique and independent source of knowledge