Andrew Norman for the NOºA Collaboration

NuFACT07, Okayama JapanAugust 11, 2007

NONOººAAThe NuMI Offaxis The NuMI Offaxis ººee Appearance Appearance

ExperimentExperiment

NNOOººAA CCoollllaabboorraattiioonn

Over 140 Physicists and Engineers from 28 institutions

IntroductionIntroductionPhysics MotivationSensitivities

Detector DesignR&D Progress

Status

Ash River

Minneapolis

Duluth

International Falls

Fermilab

Ash River

Minneapolis

Duluth

International Falls

Fermilab

Overview: NOvA Today Overview: NOvA Today (Baseline)(Baseline) NOvA is an 18kTon far detector +

218Ton near detector + NuMI beam upgrade project.

Both detectors are “totally active” liquid scintillator designs

The detectors are 14mrad off the primary beam axis to achieve narrow º¹ energy spectrum, peaked at 2GeV.

The far detect sits on a 810km baseline between Chicago and Northern Minnesota at the first oscillation maximum

Designed to use the 320KW then 700KW NuMI beam with final upgrade to the 1.2MW “super-NuMI” beam from the Fermilab main injector.

Integrate ultimately 10£1020 pot/yr

Ash River

Minneapolis

Duluth

International Falls

Fermilab

Ash River

Minneapolis

Duluth

International Falls

Fermilab

The NOºA experimental program goals:Observe º¹ ! ºe oscillationsMeasure µ13Or improve the current limit on µ13 by a factor of

20.Measure sin2(2µ23) to a precision of 0.5-1%.Resolve the neutrino mass hierarchyMeasure the CP violating phase ±Measurement of NC cross section at 2 GeV

Detection of near galactic supernova

Physics ProgramPhysics Program

The Effect of Going Off-The Effect of Going Off-AxisAxis

By going off-axis, the neutrino flux from ¼ ! ¹ + º is reduced at a distance z to:

But the energy narrows as µ2:

For NOνA, moving 14 mrad off axis makes the NuMI beam energy peak at 2 GeVEº width narrows to 20%

This corresponds to the first the oscillation maximum

6

F = ( 2°1+° 2µ2 )2 A

4¼z2

E º = 0:43E ¼1+° 2µ2

1st Osc. Max

• This suppresses the high energy tail (NC background)• Significantly reduces the Kaon background contribution by shifting the neutrino energy away from the signal band

• Energy spectrum in the signal region becomes almost insensitive to the /K ratio

• Results in a neutrino peak primarily from decays

The Effect of Going Off-The Effect of Going Off-AxisAxis

7

E ºK = 0:96E K1+° 2µ2

º’s from K’s well above signal band

º’s from ¼’s in 2GeV band

Measuring a ºe excess in the NuMI º¹ beam will give evidence for º¹! ºe transitions and a non-zero Ue3 component to ¢ m232

This is done through the ºe CC channel

The º¹ NC is the dominant background, Controlled through the identification of

initial vertex and displaced shower conversion point.

NOºA’s energy (2GeV) and baseline (810km) and segmentation (0.15X0) are chosen to maximize the physics reach of accessing these transitions

Electron neutrino’s role in the º¹ flavor transitions is given an upper bound by CHOOZ limit at 5-10% of the total state.

P(P(ºº¹¹ !! ººee) and ) and UUe3e3

º1

º2

º3

¢ m2atm

The Ue3 contribution to the third mass state is small,

requiring a precision measurement of ºe appearance

Event ParametersReaction:

Eº = 2.5GeVEp = 1.1GeVE¼ = 0.2GeVEe = 1.9GeV

Shower spans »65 of the 1178 planes

ººee Charged Current Charged Current ChannelChannel

ºep! p¼+e¡

Localized E&M Shower

Primary Vertex

Event ParametersReaction:

Eº = 10.6GeVEp = 1.04GeVE¼ = 1.97GeV

Suppressed by vertex/shower displacement identification

ºº¹¹ Neutral Current Neutral Current BackgroundBackground

ºeN ! p¼0º¹

Localized E&M Shower

Primary Vertex

Displacement

Sensitivity at 3Sensitivity at 3¾¾ for for µµ1313 from from ºº¹¹ !! ººee

For the current 18kTon detector, with 700kW (dashed) and 1.2MW (solid) beam.

The physics reach for µ13 is shown for 3 years of running each on º and º-bar.

The reach of the 1.2MW is almost an order of magnitude beyond the CHOOZ bound, giving improvement over the 3¾ MINOS reach

NOºA can perform the disappearance measurement to a precision of 0.5-1%

Proceeds as a parameterized analysis of quasielastic º¹ CC events

If , then resolve quadrant (µ23 > ¼/4 or µ23 < ¼/4, )

Measure if º3 couples more to º¹ or º¿

Resolve ambiguity by comparing NOºA to Daya Bay.

Sensitivity to Sensitivity to sinsin22(2(2µµ2323))

Mass OrderingMass Ordering From solar and atmospheric

data we know: ¢ m2

23

• This leads to two possible mass hierarchies• A “natural” order which

follows the lepton mass ordering

• An “inverted” order where m3 is actually the lightest

• NOºA can solve this by measuring the sign of m23 using the MSW effect over the 810km baseline

¢ m2atm

¢ m2solar

¢ m212

Natural

Inverted

Sensitivities Sensitivities for for P(P(ºº¹¹ !! ººee) = ) = 0.020.02

Some CP phases create an ambiguity in the resolution of the mass hierarchy.

Combine with a second measurement to break ambiguities

CP ViolationCP ViolationLarge Mixing Angle (LMA) solution gives sensitivity in º¹ ! ºe

transitions to the CP violating phase ±. In vacuum, the transition probability is shifted with ±. At the

first oscillation maximum the shift is:

Since the shift is proportional to the importance of the sub-leading terms grow, as gets small.

The ultimate sensitivity of NOνA for resolving the CP ambiguities in matter depend on both sin θ13 and ±

Combining the NOºA result with other experiments lifts the ambiguities in some regions.

p sin22µ13sin22µ13

j¢ P±(º¹ ! ºe)j » 0:06%q

sin22µ130:05

Normal Inverted

Resolution of Mass Resolution of Mass Hierarchy (95% CL)Hierarchy (95% CL)

Far DetectorFar Detector18 kTons1178

alternating X-Y planes

Grouped into 38 modular half kiloton “blocks”

Over 450,000 independent detection cells

> 70% of total mass is active

The NOThe NOννA DetectorsA Detectors

IPNDIPNDThe “Integration Prototype Near Detector” will be built in Q1 2008 to show technological integration of all the NOvA subsystem

How big is this?How big is this?The NOvA far detector is big enough to fit Atlas, CMS, DØ, and CDF Inside it’s active volume.

15.6 m

78 m

2.9 m

4.2 m

14.3

m

2.9 m

4.2 m

8.4 m

15.7 m

78 m

2.9 m

4.2 m

14.3

m

2.9 m

4.2 m

2.9 m

4.2 m

14.3

m14

.3 m

2.9 m

4.2 m

8.4 m

2.9 m

4.2 m

8.4 m

2.9 m

4.2 m

8.4 m

15.0

m

NearNearDetectorDetector IPNDIPND HumpbackHumpback

WhaleWhale

FarFarDetectorDetector

45 tons45 tons88 tons88 tons

218 tons218 tons

18,000 tons18,000 tons

NuMI Beam OptionsNuMI Beam OptionsTwo intensity options

700 kW (ANU baseline)1.2MW (super-NuMI)

1 year of beam = 44 weeks of runningDuty factor = 0.6 (accel + NuMI down time)

Run 3 years each on º and º-barFor 700kW this is 36£1020 potFor 1.2MW this is 60£ 1020 pot

&Recycler

New Injection line from MI to Recycler

New extraction line from Recycler to MI

New RF stations added and

acceleration rate switched to 240GeV/s

Beamline UpgradeBeamline Upgrade• Proton source upgraded

from 320kW to 700kW• NuMI will deliver 4.9×1012

protons per pulse• 1.33s rep-rate.• This results in 6×1020 pot/yr.

NuMI Accelerator NuMI Accelerator UpgradeUpgrade

ChangesChanges•Recycler runs proton not anti-protons•New injection/extraction lines for Recycler to Main Injector transfers•Main Injector cycle time reduced from 2.2s to 1.5s (stack in the recycler)•Cycle time reduced again to 1.33s with 2 more RF stations at MI-60 and with transition of the MI from 204 GeV/s to it’s design acceleration rate of 240 GeV/s.•NuMI target redesign for high flux

Two 16 cell extrusionsTwo 16 cell extrusions

NONOννA ModulesA Modules The NOνA detector module

forms the base unit for the detector.

Each module is made from two 16 cell high reflectivity PVC extrusions bonded into a single 32 cell module

Includes readout manifold for fiber routing and APD housing

Combined 12 module wide X or Y measuring planes.

Each module is capped, and filled with the liquid scintillator.

These are the primary containment vessel for the 3.9 million gallons of scintillator material.

There are 14,136 detector modules with a total of 452,352 separate detection cells in the NOνA Far Detector.

Detector ModulesDetector Modules

PVC ExtrusionsPVC Extrusions

Each extrusion is a single 15.7m (51.5ft) long set of 6x3.9cm cells. Two extrusions are joined to form a single 1.3m wide module

6cm6cm

3.9cm3.9cm

15.7m1.3m

Single CellSingle Cell

One ModuleOne Module

NONOººA Approval A Approval StatusStatus

CD-1 completed and signed.Total project capped at $260M

Includes Accel. Upgrade to 700kWFNAL Director’s review (Part 1) June ’07

Baseline detector size 18ktonPhysics & detector sub systems reviewed -- PASSEDCosts rolled up

Initial estimate placed detector over project cap Included many obvious accounting errors

July/Aug costs for project “scrubbed” to remove anomalous entries, redundancies and errors…

FNAL Director’s review (Part 2) Aug. ‘07Primarily cost accounting review

DoE CD-2/CD-3a review scheduled for Oct. ’07

Now Now Electronics, PVC, Scint, DAQ, DCS, SIM R&D ongoing and continues through 2008/9

Q1/Q2 2008Q1/Q2 2008 IPND installation in MINOS assem. Building

Q1/Q2 2008Q1/Q2 2008 Far site infrastructure start20102010 Collider shutdown, NuMI upgrades20112011 Beneficial Occupancy at Far Site2011-132011-13

Installation/Commisioning/Production data taking occur in parallel

NONOººA Time LineA Time Line

The Far Site - Ash River, MNThe Far Site - Ash River, MNAsh River is chosen as the site for the massive 18kTon far detector because it is the farthest site from Fermilab that is still inside the United States and yet accessible by roadway. The site is 810.5km from Fermilab, 1.5 miles south of Voyageurs National Park, and 45minute away from the town of International Falls, known as “The Icebox of the Nation” for it’s record breaking winter time temperatures.

Off Axis?Off Axis?By placing the detector at Ash River, 14.6mrad off of the NuMI beam axis, we obtain a sharp peak at 2GeV in the neutrino energy spectrum.

Ash River

VoyageursNational Park

0 25 50 kmN

Ash River

VoyageursNational Park

0 25 50 km

Ash River

VoyageursNational Park

0 25 50 km0 25 50 kmN

NuMIat NONOννA A gives a gives a 2GeV 2GeV peakpeak

The NOThe NOννA Site TodayA Site Today