FermilabFermilab Plan Plan...FermilabFermilab Plan Plan with I t it F ti A l tith an Intensity Frontier Accelerator Young-Kee Kim Young-Kee Kim Fermilab Strategic Plan Slide 1 0. What

FermilabFermilab PlanPlanith I t it F ti A l tith I t it F ti A l twith an Intensity Frontier Acceleratorwith an Intensity Frontier Accelerator

Young-Kee Kim

Young-Kee Kim Fermilab Strategic Plan Slide 1

Colloquium, Thomas Jefferson LabAugust 27, 2008

0. What is the origin of mass for fundamental particles? 1. Are there undiscovered principles of nature:

new symmetries, new physical laws?new symmetries, new physical laws? 2. Are there extra dimensions of space? 3. Do all the forces become one? 4. Why are there so many kinds of particles? y y p5. What are neutrinos telling us? 6. What happened to the antimatter? 7. What is dark matter? How can we make it in the laboratory? 8. How can we solve the mystery of dark energy? 9. How did the universe come to be?

Based on "The Quantum Universe“Based on "The Quantum Universe“HEPAP 2004

FermilabFermilabTevatron (CDF, DZero)LHC (Accelerator, CMS)ILCILCMuon Collider

Booster, Main Injector, Project X:

Dark Matter:CDMS COUPPoject

NeutrinosMiniBooNE, SciBooNE, MicroBooNE

CDMS, COUPP

Dark Energy:SDSS, DES, SNAP

MINOS, NOvA, MINERvA, DUSEL

Precision2 ( 2 k )

, ,

HE Cosmic Rays:Pierre Auger


mu2e, (muon g-2, kaons)

P5 (Particle Phys. Proj. Prioritization Panel) RoadmapFY07 Level

FY07 FY08 FY09 FY10 FY11 FY12 FY13 FY14 FY15 FY16 FY17 FY18 FY19

1. The Energy Frontier1.1 Tevatron collider1.2.1 Initial LHC

Roadmap for the Scenario w ith Constant level of Effort at the FY2007 Level

Fermilab

1.2.2 SuperLHC--Phase 11.2.3 SuperLHC--Phase 21.3 ILC / Lepton Collider

2. The Intensity Frontier2.1 Neutrino Physics

2.1.1 Mini and SciBOONE2.1.2 MINOS2.1.3 DoubleCHOOZ2.1.4 T2K2.1.5 Daya Bay2.1.6 MINERvA2.1.7 NOvA2.1.8 Beamline to DUSEL2.1.9 First Section Large Detg2.1.10 Dbl Beta Dec-Current2.1.11 Dbl Beta Dec-New Init.

2.2 Precision Measurements2.2.1 Offshore B Factory2.2.2 Mu-e Conv Expt2.2.3 Rare K Decays

2.3 DUSEL2.4 High Intens Proton Sce Fermilab

3. The Cosmic Frontier3.1 Dark Matter-Current Expts3.2 Dark Matter-New Initiatives3.3 Dark Energy-DES3.4 Dark Energy-JDEM3.5 Dark Energy-LSST

Project X


gy3.6 High Energy Particles from Space

4. Accelerator and Detector R&D

Key R&D Construction Operation

Project X: High Intensity Proton AcceleratorProject X: High Intensity Proton Accelerator8 GeV ILC-like Linac + Recycler + Main Injectory j

National Project with International Collaboration

> 2 MW over the range 60 – 120 GeV for neutrinos (Main Injector)> 2 MW over the range 60 – 120 GeV for neutrinos (Main Injector)Simultaneous with > 100 kW at 8 GeV for precision measurements (Recycler)

Compatible with future upgrades to >2 MW at 8 GeV


Project X: Naming Contesthttp://www.fnal.gov/directorate/Longrange/Steering_Public/Name-ProjectX.html

Project X

DUSEL (Deep Underground Science and Engineering Lab.)

National Project with International Collaboration

8 GeV slow spill 120 GeV fast extraction8 GeV slow spill200 kW2.2 x 1014 protons/1.4 sec

120 GeV fast extraction2.3 MW1.7 x 1014 protons/1.4 sec

Precision / Recycler

3 linac pulse / fill Main Injector1.4 sec cycle

Rare Decays

ILC Style 8 GeV H- Linac:

Stripping Foil1.4 sec cycle

Single turn transfer

0.4 GeV Front End

0.4 - 8 GeV ILC style linac


ILC Style 8 GeV H Linac:9 mA x 1 msec x 5 Hz

Single turn transfer @ 8 GeV

Project X Accelerator R&D Goals

FY FY08 FY09 FY10 FY11 FY12

Form R&D Collaboration

Start project documentation

CD-0

Fi i h CDR F ll b tiCD-1

Start project documentation (including CDR), and

accompanying R&D program

Finish CDR. Form collaboration to undertake construction project CD-2

Establish project baseline ( t h d l )

R&D Plan: http://projectx.fnal.gov/RnDplanDraft MOU circulating to possible collaborating institutions

(scope, cost, schedule)


Draft MOU circulating to possible collaborating institutions.Collaboration meeting on November 21-22, 2008

AIP’s Ten Top Physics Stories for 2007

• Three out of ten are from HEP:

– The Energy Frontier: The Tevatron in its quest to observeThe Energy Frontier: The Tevatron, in its quest to observe the Higgs boson, updated the top quark mass and observed several new types of collision events, such as those in which only a single top quark is made and those inthose in which only a single top quark is made, and those in which a W and Z boson or two Z bosons are made simultaneously.

– The Intensity Frontier: The MiniBooNE experiment at Fermilab solves a neutrino mystery, apparently dismissing the possibility of a fourth species of neutrino.p y p

– The Cosmic Frontier: Based on data recorded at the Auger Observatory, astronomers conclude that the highest


energy cosmic rays come from active galactic nuclei.

More than 100 Ph.D.s per yearwith Experiments at Fermilab

1240 Ph.D.s in 2007 in US Physics1240 Ph.D.s in 2007 in US Physics

The Energy FrontierThe Energy Frontier

The Tevatron ProgramThe Tevatron ProgramCollisions since 1985Collisions since 1985

Tevatron

CDFDZero

Tevatron

y (p

b-1 )

ty (p

b-1 )

50

55

60

5000

5500

6000Total and Weekly Luminosity

Lum

inos

ity

Lum

inos

it

30

35

40

45

50

3000

3500

4000

4500

5000

7.3 – 8.8 fb-1

Expected by FY2010

nteg

rate

d

Inte

grat

ed

10

15

20

25

30

1000

1500

2000

2500

3000Expected by FY2010


Tota

l I

Wee

kly

I

0

5

10

0 20 40 60 80 100 120 140 160 180 200 220 240 260 280 300 320 340 360 380 400Week #

0

500

1000

Mar.01 Aug.08


Rich Program indicated by PublicationsP bli ti / Y ( f M h 2008)

itted DZero

Publications / Year (as of March 2008)

CDF

Zero

Sub

m

30Published

Submitted

DZ

20

1

0

1993 1998 2004 2008

CDF – another 50+ in internal review Similar number for DZero

0


CDF another 50+ in internal review, Similar number for DZero.~2 paper submissions / week!

Bosons at the Tevatron

W Z Wγ Zγ WW WZ ZZ H WW


Similar Results from the CDF

Origin of Mass

Top Quark172.6 + 1.4 GeV/c2

Z gluons172.6 1.4 GeV/c

W

cτc .νμ

b.ντ

Where could Higgs be found?


gg

Origin of Mass: via Electroweak Precision

68% CL Direct MeasurementsTop Mass: Tevatron

W Mass: Tevatron + LEP268% CL IndirectMeasurementsLEP1, SLC, …

Top Mass (GeV)


Prefer Light Higgs (< ~180 GeV) where Tevatron has sensitivity.

Origin of Mass: SM Higgs Searches

Tevatron PreliminaryL = 2 ~ 3 fb-11 – CLs

2~3 fb-1: Tevatron excludes ~170 GeV Higgs at 95% CL

Higgs Mass

2~3 fb 1: Tevatron excludes ~170 GeV Higgs at 95% CL.~7 fb-1: Tevatron could exclude 110-180 GeV Higgs at 95% CL.


HEP world: the LHC will dominate


LHC and Fermilab• LHC – single most important component of the US HEP program• Contribution to the accelerator. We are now helping to commission LHC.• Built major components of CMS. Support “US CMS” and “LHC” Community

CMS

• US & Fermilab will continue to contribute to detector and accelerator improvements.

Fermilab’s Remote Operations Center

Support the Tevatron and LHC Community

Supporting “US CMS” d “LHC” C i“US CMS” and “LHC” Community:

Remote Operations CenterTier-1 Center, Physics Center

30 WH Offices for US CMS Univ s


~30 WH Offices for US CMS Univ.sCERN-FNAL Annual Summer School

International Linear Collider (0.5–1.0 TeV)

ILCInternational

e- e+

ILCLinear Collider (ILC)

LHCLHC

p p


The ILC

• Strong world-wide collaboration on ILCgby far the easiest machine beyond the LHC.

• ILC will be itprovided LHC tells us the richness is there.provided LHC tells us the richness is there.

• Fermilab and US community will continue with• Fermilab and US community will continue with ILC and SCRF R&D

on stretched timescale


on stretched timescale.

ILC: SCRF Technology (Broadly Applicable)at Fermilab

Vertical Test Standcavitiesat Fermilab

Horizontal Test Stand

First cryomodule


NML Test Facility

1.5 – 4 TeV Muon (μ+μ-) Collider P j X Li d (HINS)Project X – Linac upgrade (HINS)

Muon Cooling (MuCool, MICE)

detector

μμ

Muon Collider


Energy Frontier Strategy

• Alignment of Project X with the ILC will position us for the ILC and give us command of the technolog b mid decadetechnology by mid-decade.

• If the ILC energy is too low, then Project X will be the first step of development towards muonthe first step of development towards muon colliders (and a neutrino factory).


The Cosmic FrontierThe Cosmic Frontier

Particle Astrophysics: Quarks to CosmosParticle Astrophysics: Quarks to Cosmos


The Cosmic Frontier

• Dark Matter– CDMS

The UniverseThe Universe

– COUPP

• Dark Energy– SDSS– DES– SNAP(JDEM): LBNL led, Science Ops. Center at FNAL

• High Energy Particles from Space


– Pierre Auger

Dark Matter:WIMPs (Weekly-Interacting Massive Particles)

• Leading dark matter candidateC ld l f l t di• Could solve some of long standing SM problems

CDMS COUPPCDMSLow temp. Ge / Si crystals

near MINOS far detector (Soudan Mine)Results with 5 towers

Room temp. CF3I Bubble Chamberin the MINOS near detector Hall

Results with 2 kg (1 liter)

COUPP

Results with 5 towers Results with 2 kg (1 liter)


Dark Matter (WIMP): Present and FutureCDMS 5 towers (4 kg) COUPP 2 kg

Spin Independent Spin Dependent

10 102 103 104

CDMS (2008)COUPP (2007)

10 102 103

2 kg with better muon vetoin operation

15 kg at Soudan (2010 Ops)100 kg at SNOLAB

WIMP mass [GeV/c2] WIMP mass [GeV/c2]


in operation~100 kg under construction

100 kg at SNOLAB1 ton at DUSEL (?)

SDSS Impact(Sl Di it l Sk S )(Sloan Digital Sky Survey)

Power Spectrum of Galaxies


Power Spectrum of Galaxies Constrain Dark Energy Density Parameter

Dark Energy: SDSS DES SNAP

Blanco 4-meter at CTIO

Dark Energy Survey will probe much deeper than SDSS.

DECamBigger telescope, better CCD’s, photometric redshifts

Construction has begun. Operation: 2011 2016Operation: 2011 – 2016

SNAP (Joint Dark Energy Mission)SNAP(led by LBNL)

Spectra of thousands of SupernovaeMap the Universe out to even higher redshift

Weak Lensing from space


Weak Lensing from space

Science Operations Center at Fermilab

The Intensity FrontierThe Intensity Frontier

Physics of Flavor

• Flavor phenomenaEssential to shaping ph sics– Essential to shaping physicsbeyond the SM.

• SM is incomplete:– Neutrino Masses (flavor)Neutrino Masses (flavor)

• The only new physics seen so far in the laboratory

– Baryon Asymmetry of the Universe (flavor)– Dark Matter


– Dark Energy

Neutrinos

The enigmatic neutrinos are among the most abundantThe enigmatic neutrinos are among the most abundant of the tiny particles that make up our universe.

To understand the universe, must understand neutrinos.

Behavior is so different from other particles.

O i “ ” i d


Opening a “new” window

Neutrinos

• Neutrino masses– via See-Saw mechanism, point to mνM = (mquark)2

pnew physics at a very high mass scale (unification scale).

• Baryon Asymmetry of the Universey y y– Possible scenarios as the source

• Electroweak baryogenesis – LHC and ILC.• Leptogenesis Neutrino CP violation would support it• Leptogenesis – Neutrino CP violation would support it.

• The Four Measurementsl f i 22θ– value of sin22θ13

– Are neutrino masses Dirac or Majorana? (ν = ν)– Is the mass ordering normal or inverted? (mass ordering)


– CP violation

The Intensity Frontier: PresentThe Intensity Frontier: Present

17 kW at 8 GeV

Tevatron MiniBooNESciBooNEMINOS

17 kW at 8 GeVfor neutrinos

MI beam power at 120 GeVCollider

250 kW at 120 GeV

since multi-batch slip stackingbecome operational

for neutrinos

Jan May


Jan. May

The Intensity Frontier: Early Next DecadeThe Intensity Frontier: Early Next Decade

20 kW at 8 GeV~20 kW at 8 GeVfor neutrinos & precision

MINOS MicroBooNE

700 kW at 120 GeV

NOvA MINERvA

for neutrinos


Neutrino OscillationNeutrino Oscillation

MiniBooNEMINOSNOvA

MiniBooNE: νμ νeMiniBooNEMiniBooNE

8 GeV Proton Beam

SciBooNE

from Booster

The LSND result?

requires the 4th ν.

MiniBooNE ruled it outMiniBooNE ruled it out


MINOS: νμ νX (Disappearance)Near

Detector

νμ

FarDetector

1 kmat Fermilab

νμ 735 kmat Soudan

best Δm232 measurement32

K2K

MINOS

Super K


Reconstructed neutrino energy (GeV)

MINOS: νμ νe for θ13 (Appearance)Near

Detector

νμ

FarDetector

1 kmat Fermilab

νμ 735 kmat Soudan

MINOS could provide an early glimpse on θ13.


NOvA for θ13, ν mass ordering

15 kton Liquid Scintillator

NOvA could provide the first glimpse of the mass ordering for l th l t b f hi h i th ldlarge θ13 - the only near term probe of hierarchy in the world.


Neutrino’s Interactionswith Matter

SciBooNESciBooNEMINERvA

How do neutrinos interact with matter?

• We are entering– a precision era in neutrino oscillation physics.a precision era in neutrino oscillation physics.

It requires• It requires– precise determination of the neutrino reaction

and production cross sectionsand production cross sections.


SciBooNE

SciBooNEMiniBooNE

8 GeV Proton Beam8 GeV Proton Beamfrom Booster

νμ μ−μ

p (n)

π+

p (n)


MINERvA (under construction)

MINOS

MINERvAMINERvA


The Intensity Frontier: FutureThe Intensity Frontier: FutureToward DUSEL for Neutrino CP ViolationToward DUSEL for Neutrino CP Violation

Phase 1 (700 kW power, ~100 kt WC detector)

20 kW at 8 GeV

MINOS

~20 kW at 8 GeVfor neutrinos & precision

MicroBooNE

700 kW at 120 GeV

NOvA MINERvA

for neutrinos


The Intensity Frontier: FutureThe Intensity Frontier: FutureToward DUSEL for Neutrino CP ViolationToward DUSEL for Neutrino CP Violation

Phase 2 (> 2MW power, ~300 kt WC or ~100 kt LAr TPC detector)

Project X:Project X:Project X:Project X:


Neutrino / Proton Decay “Massive” DetectorsOptions under consideration:

~300 kt WC, ~100 kt LAr, or some combination of the two.Fermilab supports both technologies

• Water CerenkovKnown technology

• Liquid Argon TPCsGreat promise (x 3 4)

Fermilab supports both technologies.

– Known technology – Great promise (x 3-4)


MicroBooNE with ~170 ton

NOvANOvA(off-axis)

NSF’s proposedUnderground Lab.

DUSEL

MINOS (on-axis)

DUSEL

1300 km

735 km

Ph 1 D t tPh 1 D t tMiniBooNESciBooNE

MicroBooNE

1300 kmPhase 1 DetectorPhase 1 DetectorFull size Detector Full size Detector (( Proton Decay,Proton Decay,

Supernova)Supernova)MINERvA

Phase 1: 700 kWPhase 1: 700 kWPhase 2: Project XPhase 2: Project X


Precision Measurementswith Muons

Neutrinos change from one kind to another.Neutrinos change from one kind to another.Do charged leptons do, too?

Muons: the Standard Model

W-γ

xνμ νeμ- e-

W

xUμi U*ei

μ e

virtual ν mixing

Br(μ eγ) < 10-54

Experimental reach ~ 10-13 (μ eγ), 10-17 (μN eN)


Muons: μ to e Conv.(μN eN) in New Physics

Supersymmetry Compositeness

Λ ~ 3000 TeV

LeptoquarkMLQ =

3000 (λ λ )1/2 TeV/c2rate ~ 10-15

μ- e-

μ- e-

χi0~

lj lj~~

Λc 3000 TeV

μ- d

L

3000 (λμdλed)1/2 TeV/c2

LQ

rate 10

q q

μ e

q q

Heavy Z’

d e-

L LQ

Heavy Neutrinos Second Higgs Doublet Heavy ZAnomal. Z Coupling

MZ’ = 3000 TeV/c2|UμNUeN|2 ~ 8x10-13 g(Hμe) ~ 10-4g(Hμμ)

μ- e-

He-

t

t t

μ- e-

γ,Z,Z’μ- e-

N

W

Z


q q q qq q

Muons: Energy – Intensity Connection

Energy Frontier Facility Intensity Frontier Facility

The Gauge SectorHiggs

The Flavor SectorMixings, Masses,

C C CEWSB CPV, FCNC, LFV, …

χ~

E

χ

I t it F ti b h i t l >> T V l


Intensity Frontier can probe new physics at a scale >> TeV scale.

mu2e Muon Beam and Detector

for every incident proton 0.0025 μ−’s are stopped in

h 1 0 2 Althe 17 0.2 mm Al target foils


MECO spectrometer design

The Intensity Frontier:The Intensity Frontier:Ph 1 P i i M tPhase 1 Precision Measurements

20 kW at 8 GeV

MINOS

~20 kW at 8 GeVfor neutrinos & precision

MicroBooNE

700 kW at 120 GeV

NOvA MINERvA

for Neutrinos


Ph 2 P i i M t ith P j t XThe Intensity Frontier:The Intensity Frontier:

Stretcher Possibilities:

Phase 2 Precision Measurements with Project X

Stretcher Possibilities:Accumulator / Debuncher, Recycler, Tevatron

high duty factorhigh availability

good beam structure

Project X:Project X:

upto 200 kW at 8 GeV for precision measurements from Recycler

Project X:Project X:

upto 200 kW at 8 GeV for precision measurements from Recyclerwhile Main Injector provides > 2 MW at 60-120 GeV for neutrinos


mu2e can probe 103 – 104 TeV.New PhysicsScale (TeV)

μ e Conv. Expt.at Fermilab

Project X

pre-Project X

χi0~

~~μ- e-

CompositenessSUSY


μ- e-

q q

lj lj~~

q qModel Parameter

Evolutionary Path to ν-Factory & μ+μ- Collider

Project XMuon ColliderTest Facility

NeutrinoFactoryFactory

1.5 TeVMuon Collider

Beam to DUSEL4 TeV


Beam to DUSELMuon Collider

Opportunities with Project X

NeutrinosNeutrinos: Oscillation: Oscillation(International Collaboration) ILCILC

MuonsMuonsμμ e conversione conversion

(Phase 2)(Phase 2)

MuonMuonColliderCollider

NeutrinoNeutrino

(Phase 2)(Phase 2)

MuonsMuons gg--22 Project XProject X

AntiprotonsAntiprotonsHyperon CPHyperon CP

NeutrinoNeutrinoFactoryFactory

KaonsKaonsKK++ ππ++νννν, K, KLL ππ00νννν

(Phase 1 expt.s can be done with pre-Project X)

νν’s’sEWKEWK

Hyperon CPHyperon CPAntihydrogen CPTAntihydrogen CPT

CharmCharmMixing, CPMixing, CP

Need international coordination & collab

Accelerator ScienceAccelerator Science


Need international coordination & collab.

Developed together with the US HEP community

FermilabFermilabTevatron (CDF, DZero)LHC (Accelerator, CMS)ILCILCMuon Collider

Booster, Main Injector, Project X:

Dark Matter:CDMS, COUPP

NeutrinosMiniBooNE, SciBooNE, MicroBooNEMINOS NO A MINER A DUSEL

Dark Energy:SDSS, DES, SNAP

MINOS, NOvA, MINERvA, DUSEL

Precisionmu2e (muon g-2 kaons)

HE Cosmic Rays:Pierre Auger


mu2e, (muon g-2, kaons)

The 3σ Reach of the Successive Phasessin22θ13 Mass Ordering CP Violation

Phase

1

1.5

22

3


Documents

FermilabFermilab Plan Plan...FermilabFermilab Plan Plan with I t it F ti A l tith an Intensity Frontier Accelerator Young-Kee Kim Young-Kee Kim Fermilab Strategic Plan Slide 1 0. What