# Presentation: 088993

## The Fermilab Neutrino Program – Status and Challenges Ahead

- Eric Prebys*
- Fermilab Accelerator Division/MiniBooNE

- *with acknowledgements to everyone who leaves talks where I can find them

## Preface

- The turn-on of the LHC in ~2007 will mark the end of the Fermilab Tevatron’s unprecedented 20+ year reign as the world’s highest energy collider.
- With the cancellation of the BTeV (B physics) project, the collider program is scheduled to be terminated in 2009, possibly sooner.
- The lab has a strong commitment to the International Linear Collider, but physics results are at least 15 years away.
- -> Neutrino physics will be the centerpiece of Fermilab science for at least a decade.

## Luckily, neutrinos are very interesting

- Many unanswered questions
- Type: Dirac vs. Majorana
- Generations: 3 active, but possibly sterile
- Masses and mass differences
- Mixing angles
- CP and possibly even CPT violation
- Multi-disciplinary
- Study
- Solar
- Atmospheric
- Reactor
- Lab based (beta-decay)
- Accelerator Based
- Application
- Particle physics
- Astrophysics
- Cosmology
- Trying to coordinate the effort and priorities
- See “APS Multidivisional Neutino Study”
- http://www.aps.org/neutino/

## This Talk

**A Brief History of Neutrinos**
- Background
- Neutrino “problem”
- Neutrino oscillations
**Some Key Experimental Results**
- SuperKamiokande
- SNO
- Reactor Summary
- K2K
- LSND (????)
- Where do we stand?
**Major Fermilab Experiments**
- MiniBooNE
- NuMI/Minos
- Nova
**Meeting the Needs of these Experiments**
- Existing Complex
- Post-Collider
- Longer Term

## A Brief History of Neutrinos: The Beginning

- Electron Energy

- Expected monoenergetic electrons

- Observed electron spectrum

- In “beta decay”, one element changes to another when the nucleus emits an electron (or positron). Looked like a 2-body decay, but energy spectrum wrong.

- In 1930, Wolfgang Pauli suggested a *“desperate remedy”,* in which an “invisible” particle was carrying away  the missing energy. He called this particle a “neutron”.

- Enrico Fermi changed the name to “neutrino” in 1933, and it became an integral part of his **extremely  successful** weak decay theory.
**In 1956, Reines and Cowen observe first direct evidence of neutrinos – 26 years after their prediction!**

## The Question of Mass, the Standard Model

- All observed kinematics of neutrino interactions are consistent with **zero mass** to within the limits of sensitivity.
- In Fermi model (and later Standard Model), neutrinos are massless *by definition**.*
- In 1956, Bruno Pontecorvo first shows that it might be possible for neutrinos to *oscillate *from one type to another if they have a small – **but nonzero** – mass*.*
**Other important developments:**
- 1962: Lederman, Steinberger, and Schwartz show that that there are at least two distinct “flavors” of neutrinos (e)
- 1970’s: “Standard Model” completed – with *massless* neutrinos.
- 1989: LEP experiments prove there are **only three flavors** of active neutrino (e ,, and )

## Neutrinos in the Standard Model

- Each Generation lepton has an associated neutrino

- The weak interaction causes a charged lepton to “flip” to a neutrino and vice versa

- The weak interaction conserves “lepton number”

## The “Neutrino Problem”

- 1968: Experiment in the Homestake Mine first observes neutrinos from the Sun, **but there are far fewer than predicted**.  Possibilities:
- Experiment wrong?
- Solar Model wrong? *(**** believed by most not involved)*
- Enough created, but maybe oscillated (or decayed to something else) along the way.
- ~1987: Also appeared to be too few atmospheric muon neutrinos.  Less uncertainty in prediction.  Similar explanation.
- Both results confirmed by numerous experiments over the years.
- 1998:  SuperKamiokande observes clear oscillatory behavior in signals from atmospheric neutrinos.  For most, this establishes neutrino oscillations “beyond a reasonable doubt”.

## Neutrino Oscillations

- Neutrinos are produced as *weak eigenstates* (e ,, or ).
- In general, these can be represented as *linear combination of mass eigenstates*.
- If the above matrix is not diagonal *and* the masses are not equal, then the net weak flavor content will *oscillate *as the neutrinos propagate.
**Example: **if there is mixing between the e and :then the probability that a e will be detected as a  after a distance *L* is:

- Distance in *km*

- Energy in GeV

- Mass eigenstates

- Flavor eigenstates

- Only measure *magnitude* of the *difference* of the square of the masses!

- Problem: need a heck of a lot of neutrinos to study this!

## Sources of a Heck of a Lot of Neutrinos

- The sun:
- Mechanism: nuclear reactions
- Pros: free
- Cons: only electron neutrinos, low energy, exact flux hard to calculate, can’t turn it on and off.
- Atmosphere:
- Mechanism: Cosmic rays make pions, which decay to muons, electrons, and neutrinos.
- Pros: free, muon and electron neutrinos, higher energy than solar neutrinos, flux easier to calculate.
- Cons: flux fairly low, can’t turn it on and off.
- Nuclear Reactors:
- Mechanism: nuclear reactions.
- Pros: “free”, they do go on and off.
- Cons: only electron neutrinos, low energy, little control of on and off cycles.
- Accelerators:
- Mechanism: beam dumps -> particle decays + shielding -> neutrinos
- Pros: Can get all flavors of neutrinos, higher energy, can control source.
- Cons: NOT free

## Probing Neutrino Mass Differences

- & Reactors

- Accelerators use  decay to *directly* probe  e

- Reactors use use *disappearance* to probe  e  

- Cerenkov detectors directly measure  and e  content in atmospheric neutrinos. Fit to e mixing hypotheses

- Solar neutrino experiments typically measure the disappearance of e.

- Also probe with “long baseline” accelerator experiments

## SuperKamiokande Atmospheric Result

- Huge water Cerenkov detector can directly measure and  e  signals.
- Use azimuthal dependence to measure distance traveled (through the Earth)
- Positive result announced in 1998.
- Consistent with  mixing.

## SNO Solar Neutrino Result

- Looked for Cerenkov signals in a large detector filled with heavy water.
- Focus on 8B neutrinos
- Used 3 reactions:
* ****e*+*d**p+p+e**-*: only sensitive to ***e*
-  ***x*+*d**p+n+****x*: equally sensitive to ***e *,***** *,****
* ****x*+ *e**-* ***x*+ *e**-*: 6 times more sensitive to ***e *than ***** *,*****d*
- Consistent with initial full SSM flux of ***e*’s mixing to ***** *,******

- Just SNO

- SNO+others

## Reactor Experimental Results

- Single reactor experiments (Chooz, Bugey, etc).  Look for ***e* disappearance: all negative
- KamLAND (single scintillator detector looking at ALL Japanese reactors): ***e* disappearance consistent with mixing.

## K2K

- First “long baseline Experiment
- Beam from KEK PS to Kamiokande, 250 km away
- Look for nm disappearance (atmospheric “problem”)
- Results consistent with mixing

- Best fit

- No mixing

- Allowed Mixing Region

## LSND Experiment (odd man out)

- Looked for ****  ***e* and ****  ***e* in  decay from the 800 MeV LANSCE proton beam at Los Alamos
- Look for ***e* appearance via:
- Look for ***e* appearance via:
- Observe excess in both channels (higher significance in ***e*)
- Only exclusive *appearance* result to date.
- Doesn’t fit “nicely” with the other results!

## Full Mixing Picture (without LSND)

- General Mixing Parameterization

- CP violating phase

- Almost diagonal
- Third generation weakly coupled to first two
- “Wolfenstein Parameterization”

- Mixing large
- No easy simplification
- Think of mass and weak eigenstates as totally separate

## Neutrino Mixing (cont’d)

## Incorporating LSND

**Only 3 active ******

**- not a good fit to data**

**3 active+1 sterile ******

**- possible(?)**

- OR...

**CPT violation******

**- possible(?)**

- OR...

- OR...

- Can fit three mass states quite well *without* LSND, but no a priori reason to throw it out.  Must check...

- We have 3 very different ***m**2*’s.  Very hard to fit with only three mass states...

## Enter the Fermilab Neutrino Program

- MiniBooNE-neutrinos from 8 GeV   Booster proton beam (L/E~1): absolutely confirm or refute the LSND result

- NuMI/Minos – neutrinos from 120 GeV Main Injector proton beam (L/E~100):precision measurement  of  oscillations as seen in atmospheric neutrinos.

## The Fermilab Accelerator Complex

- = ProtonSystem

- =Proton Customer

## Preac(cellerator) and Linac

**“****Preac” - **Static Cockroft-Walton generator accelerates H- ions from 0 to 750 KeV.

**“****Old linac”(LEL)-** accelerate H- ions from 750 keV to 116 MeV

**“****New linac” (HEL)-** Accelerate H- ions from 116 MeV to 400 MeV

## Booster

-  Accelerates the 400 MeV beam from the Linac to 8 GeV
- From the Booster, beam can be directed to
-  The Main Injector
-  MiniBooNE (switch occurs in the MI-8 transfer line).
-  The Radiation Damage Facility (RDF) – actually, this is the old main ring transfer line.
-  A dump.
- More or less original equipment

## Main Injector

-  The Main Injector can accept 8 GeV protons OR antiprotons from
-  Booster
-  The anti-proton accumulator
-  The Recycler (which shares the same tunnel)
-  It can accelerate protons to 120 GeV (in a minimum of 1.4 s) and deliver them to
-  The antiproton production target.
-  The fixed target area.
-  The NUMI beamline.
-  It can accelerate protons OR antiprotons to 150 GeV and inject them into the Tevatron.

## Producing Neutrinos At an Accelerator

- 8 GeV Proton beam

*Mostly *pions

- Target

- Mostly lower energy

- We will look for these to oscillate

- Pion sign determined whether it’s a neutrino or anti-neutrino

## Neutrino Horn – “Focusing” Neutrinos 

- Can’t focus neutrinos themselves, but they will go more or less where the parent particles go.

- Target

- Coaxial “horn” will focus particles of a particular sign in both planes

- p

- Horn current selects + ->  or  -> 

## So What’s So Hard?

- Probability that a 150 GeV proton on the antiproton target will produce an accumulated pbar:  			.000015 (1.5E-5)
- Probability that a proton on the MiniBooNE target will result in a detected neutrino:		 .000000000000004 (4E-15)
- Probability that a proton on the NUMI target will result in a detected neutrino at the MINOS far detector: 	     .000000000000000025 (2.5E-17)
*** **Need more protons in a year than Fermilab has produced in its lifetime!!*

## MiniBooNE Experiment

- Proton flux ~ 6E16 p/hr (goal 9E16 p/hr)
- ~ 1 detected neutrino/minute
- L/E ~ 1

**FNAL****Booster**

**Be Target****and Horn**

**“****Little Muon Counter” (LMC): to understand K flux**

**50 m Decay Region**

**500m dirt**

**Detector**

- 8 GeV protons

## Detector

- 950,000 l of pure mineral oil
- 1280 PMT’s in inner region
- 240 PMT’s outer veto region
- Light produced by Cerenkov radiation and scintillation

- Light barrier

- Trigger:
- All beam spills
- Cosmic ray triggers
- Laser/pulser triggers
- Supernova trigger

## Neutrino Detection/Particle ID

- Important Background!!!

## Experimental Sensitivity (1E21 POT)

- No signal
- Can exclude most of LSND at 5

- Signal
- Can achieve good m2 separation

## Beam to MiniBooNE

- 6.3E20 to date
- Plan for ~2E20/year during NuMI running
- First results in early 2006

- NuMI

## MINOS: Main Injector Neutrino Oscillation Study

- _MINOS_: Main Injector Neutrino Oscillation S*tudy*

- 8 GeV Booster beam is injected into Main Injector.
- Accelerated to 120 GeV
- Transported to target
- Two detectors for understanding systematic
- Near detector: FNAL (L=1km)
- Far detector: Sudan Mine in Minesota (735 km away)

## NuMI beams

- Two horns (second moveable) -> adjustable beam energy

## Near – 1040 m away

- Near – 1040 m away

** ****veto - target - shower - ******** spectrometer (detect neutrinos by ******** appearance**
** ****1 kT**
** ****3.8 x 4.8 “squeezed” octagon**
** ****12,300 scint.strips**
** ****1-end readout**
** ****no-multiplexing**
** ****220 M64s**
** ****QIE-based front-end**
**282 steel planes**
**153 scintillator planes**
** ****65 km WLS fiber**
** ****51 km clear fiber**

**Near detector will provide high event **
**statistics for “mundane” neutrino physics**

## Far Detector – 735.3 km away

** ****2 Supermodules**
** ****5.4 kT**
** ****484 scint. planes**
** ****92,928 strips (4.1 x 1.0 cm)**
** ****8-fold MUXed 2-ended readout**
** ****1452 M16s**
** ****722 km of WLS fiber**
** ****794 km of ****clear fiber**

** ****B ~ 1.5T (R=2m)**
** ****HAD ~ 55% / E ****1/2**
** ****EM ~ 23% / E ****1/2**

- MINOS

- Soudan 2/CDMS II

**shaft**

## Minos Status

- Test Beam in December 2004
- Startup in March, 2005
- Collecting data steadily
- Detectors working well

- Near detector (different target positions)

- Far detector (fully contained event)

## Beam to NuMI/MINOS

- Accumulating data at ~2-2.5E20/yr
- Can do initial oscillation result at 1E20 (~end of year)

- Target water leak problems

- Caught up!

## MINOS Ultimate Sensitivity

- ~3 years

- ~7 years

## Beyond Minos – an Off-Axis experiment

- Putting a Detector Off the NuMI Axis probes a narrower neutrino energy distribution than an on-axis experiment (albeit at a lower total intensity)
- By constraining L/E, one is able to resolve different contributions to the signal by comparing neutrino and anti-neutrino events
- sin(13)
- Si*gn* of m2  (resolve hierarchy question)
- CP violation

## Noa Proposal

- Place a 30 kT fully active liquid scintillator detector about 14 mr off the NuMI beam axis

## Noa Sensitivity

- Noa Sensitivity

- Fraction of  covered

## Noa Status and Schedule

- Stage I approval: April, 2005
- Project Start: October, 2006
- First kton operational: October, 2009
- All 30 ktons operations: July, 2011
- Problems:
- Would really like a LOT of protons

## Proton Demands (in Perspective)

- Highest number I could find on a plot

## Limits to Proton Intensity

- Total proton rate from Proton Source (Linac+Booster):
- Booster batch size
- Typical ~5E12 protons/batch
- Booster repetition rate
- 15 Hz instantaneous
- Currently 7.5Hz average (limited by injection bump and RF cooling)
- Beam loss
- Damage and/or activation of Booster components
- Above ground radiation
- Total protons accelerated in Main Injector:
- Maximum main injector load
- Six “slots” for booster batches (3E13)
- Up to ~11 with slip stacking (5.5E13)
- RF stability limitations (under study)
- Cycle time:
- 1.4s + loading time (1/15s per booster batch)

- Operational Limit

## Staged Approach to Neutrino Program

- Stage 0 (now):
- Goal: deliver 2.5E13 protons per 2 second MI cycle to NuMI (~2E20 p/yr)
- Deliver 1-2E20 protons per year to Booster Neutrino Beam (currently MiniBooNE)
- Stage 1 (~2007):
- A combination of Main Injector RF improvements and operational loading initiatives will increase the NuMI intensity to ~5E13 protons per 2.2 second cycle (~3.5E20 p/yr)
- It is hoped we can continue to operate BNB at the 2E20 p/yr level during this period.
- Stage 2 (post-collider):
- Proton to NuMI will immediately increase by 20%
- Consider (for example) using the Recycler as a preloader to the Main Injector and reducing the Main Injector cycle time (~6.5E20 p/yr)
- The exact scope and potential of these improvements are under study
- Stage 3 (proton driver)
- Main Injector must accommodate 1.5E14 protons every 1.5 seconds
- NuMI beamline and target must also be compatible with these intensities.

## Re-tasking the Recycler

- At present, the Main Injector must remain at the injection energy while Booster “batches” are loaded.
- Booster batches are loaded at 15 Hz
- When we slip stack to load more batches, this will waste > 1/3 of the Main Injector duty factor.

- After the collider, we have the option of “preloading” protons into the Recycler while the Main Injector is ramping, thereby eliminating dead time.
- Small invenstment
- New beamline directly from Booster to Recycler
- Some new RF
- Big payoff
- At least 50% increase in protons to NuMI

## Thinking Big: A Proton Driver

## The Benefits of an 8 GeV Linac Proton Driver

- The Benefits of an 8 GeV Linac Proton Driver

**Anti-**
**Proton**

## Possible “budget” Alternative to Proton Driver

- Less Expensive than the Linear Proton Driver
- Can get to 2 MW
- None of the side benefits
- No synergy with ILC

- Retire Booster
- Build new transfer line
- Replace pBar Debuncher with new Booster
- Prestack in Accumulator
- Transfer to recycler/Main Injector

## Evolution of Proton Delivery

## Evolution of 13 discovery limit

- Bands show dependence on CP violation parameter 

## Other Activities at the lab (some very big)

- Other Neutrino:
- FLARE: Same physics motivation as Noa, but with a liquid Argon detector
- Cross section experiments as input to neutrino physics
- MIPP
- Minera
- Finese
- SciBar
- Fixed Target
- Active 120 GeV program, mostly test beams
- LHC
- Big player in CMS
- Level 2 Physics Center
- LARP accelerator collaboration
- ILC
- Major Commitment ramping up over the next few years
- Major superconducting RF effort
- Non-HEP
- Sloan Digital Sky Survey
- Auger
- Computing Grid development

## Conclusions

- It’s a little disorienting to see the end of the Fermilab collider program
- We are disappointed at the cancellation of the BTeV project, nevertheless
- Fermilab is poised to hold a leading position in neutrino research for the next 10-15 years.

## MiniBooNE Beamline

- 8GeV Beam from Booster

## Neutrino Horn – Cont’d

-  Horn will pulse with 170 kA 150 usec pulse!
-  Horn heating limits the average rep rate to 5 Hz.
- Horn fatigue is an issue.
- Under nominal MiniBooNE running conditions, it will pulse about 100 million times per year.
- Highest rate neutrino horn ever built!

## MiniBooNE Secondary “Beamline”

- 25m

- 25m

- Detector

- “Teletubby Hill”

- Counting House

- 50m Muon absorber

- removable25m Muon absorber

- Target vault

- Proton Beam

- Decay region

- NOT to scale!!!!!!

- 500 m

## Predicted Neutrino Flux at the Detector

- The L/E ~1 m/MeV is similar to that at LSND.

**p********Be ****************K************K****0****L******

************
**K**K0L

****ee
**K****+**ee  , K0Lee

**-**8 GeV protons on Be:

- -yield a high flux of  :

- -with a low background of e :

- Flux estimate is important!

## Nova dependence on 