the iss peter dornan imperial college london. 16 march 2006p dornan - mutac 20062...

The ISS

Peter Dornan

Imperial College London

16 March 2006 P Dornan - MUTAC 2006 2

`atmospheric’ `solar’ `cross/reactor’

3,2,1,, itaumuonelectronU iMNS

Oscillation defined by 3 mixing angles,

phase

ijijijij sc sin,cos

Neutrino Oscillation


Where are we?from: Maltoni, Schwetz, Tortola, Valle (’04)

Also know m2 > m1from matter effects in the sun


Unanswered – Oscillation Expts

Is 23 maximal?

How small is 13? CP Violation in the lepton sector? Mass hierarchy?

m3 < or > m2

Is the MNS approach correct? CPT violation? The ultimate accuracy on the mixing angles and the

mass differences What accuracy is needed?

(LSND? Sterile neutrino(s)? )


The Precision Era - after T2K and Nova

Around 2012 - 2015 We shall have good measurements of

12, 23, m212, m2

23

Probably have a measurement of 13

Possibly know the mass hierarchy

So can now plan for the ultimate neutrino measurements Refine all parameters Check consistency Measure CP Violation

This is the aim of the ISS


Neutrino source – options:

Second generation super-beam CERN, FNAL, BNL,

J-PARC II

Beta-beam

Neutrino Factory


The International Scoping Study

International scoping study of a future Neutrino Factory and super-beam facility

Motivation

Organisation Status

Physics Group Accelerator Group Detector Group

ISS: next steps


ISS: motivation

Neutrino Factory – prior to launch of ISS Several studies at the turn of the century

US Studies I, II, IIa ECFA/CERN Study NuFact-J Study

established feasibility & R&D programme MUCOOL, MICE, MERIT….

But there have been advances since then Also appreciation of the need for an integrated

accelerator-detector-physics approach and an international approach


ISS: motivation

Preparation for design study Review physics case

Critical comparison of options Review options for accelerator complex:

Prepare concept-development and hardware-R&D roadmaps for design-study phase

Review options for neutrino-detection systems Emphasis: identify concept-development and hardware-R&D

roadmaps for design-study phase Establish the Cost Drivers & Optimize

Physics/$ - where there are alternatives Absolute scientific value - where only one method


ISS: organisation


Meetings

Plenary meetings to date: CERN: 22 – 24 September 2005

Attendance: 92 Americas: 15 Asia: 12 Europe 65

KEK: 23 – 26 January 2006 Attendance: 67 Americas: 11 Asia: 28 Europe 28

RAL 25 – 28 April 2006 Attendance 70

Final Plenary Meeting Irvine, Aug 21 – 22 Just before NuFact06


Physics Group

Theory subgroup : What is the new physics Need to distinguish between alternative theories Establish the case for high-precision, high-sensitivity neutrino-

oscillation programme Phenomenological subgroup

Review models of neutrino oscillations Identify measurables that distinguish them and assess the

precision required Experimental subgroup:

Use realistic assumptions on the performance of accelerator and detector to: Evaluate performance of the super-beam, beta-beam and Neutrino

Factory alone or in combination Make meaningful comparisons

Muon physics subgroup: Lepton-flavour violating processes – clear synergy with neutrino

oscillations – possibly the next major discovery


Some Theoretical Ideas

Quark-lepton complementarity

Intriguing Relations Coincidence fundamental

GUTs motivate relationships between the quark and lepton mixing matrices

Measurable relations Need Precision

41212 CKMMNS

42323 CKMMNS


Quark-lepton complementarity


A Possible Neutrino Sum Rule

cos26.35 1312

%10313

%10313

20

5.012


Towards a performance comparison

A Major Goal of the ISS Now many options Must be reduced if there is to be a realistic design for

a ‘precision era’ neutrino facility Requires justifiable assumptions:

Accelerator: flux, energy spectrum Detector: Ethresh, ERes (background, x-sect.

uncertainty…)

and optimised facility (accelerator, baseline, & detectors)

Already a very substantial amount of work


Cases under Consideration

Off axis super-beam: T2HK taken as example

Plan to explore different options (essentially vary E and L)

Beta beam: Low : = 100 and L = 130 km

High flux (~1018 decays per year) and high flux (1019 dpy) High : = 350 and L = 700 km

High flux (~1018 decays per year) and high flux (1019 dpy) Also Beta beam abd superbeam combination

Neutrino Factory Performance studied as a function of:

E and L Ethresh and ERes


Sample - CP sensitivity v. sin2213

Work in progress

But highlights the importance of 13 in defining a strategy

Huber, Lindner, Rolinec, Winter


CPT & the MNS Theory

In the Quark sector the CP violation parameters are determined in many ways

Can we do the same in the neutrino sector?

With 3 flavours and CPT CP violation related in

e ->

->

e ->

Needs tau modes

Murayama


Physics Report

How important – gold, silver, platinum?

In the ideal scenario should we measure

e→e

→e

Specifically - how important are the tau channels?


Neutrino Factory: optimisation

Study performance as a function of muon energy and baseline

Detector: 100 kton, magnetised iron Importance of threshold

sensitivity

Can trade muon energy against detector threshold and resolution


Muon Physics & the Factory

Intense muon beams are needed for muon physics

Could be the place for the next major advance

But - is a Factory suitable for muon experiments?


ISS status: Accelerator Group

Most work on -Factory Subsystems

& subgroups Proton driver Target and capture Front end

Bunching and phase rotation

Cooling

Acceleration Decay ring

Decay Channel

Linear Cooler

Buncher

1-4 MWProtonSource

Hg-Jet Target

Pre-Accelerator

Acceleration

DecayRing ~

1 km5-10 GeV

10-20GeV

1.5-5 GeV

Decay Channel

Linear Cooler

Buncher

1-4 MWProtonSource

Hg-Jet Target

Pre-Accelerator

Acceleration

DecayRing ~

1 km5-10 GeV

10-20GeV

1.5-5 GeV


Towards a Baseline -Factory

RF Frequency: Baseline is 201 MHz• Phase Rotation: Baseline is Neuffer bunched beam rotation• Phase Rotation: Baseline RMS bunch length 2 ns• Amount of Cooling: Baseline is 50 m• Target: Baseline is Liquid Mercury• Pion Collection: 20 T Solenoid• Repetition Rate: 50 (Hz)• Proton bunch structure: 4 bunches spaced by 16 μsec• Proton energy: 5-15 (GeV)• Final acceleration: No decision yet• Storage Ring: Choice is site dependent


ISS status: Detector Group

Detector options and subgroups Large water Cherenkov

ISS activity focuses on consideration of R&D required: Photo tubes Front-end electronics

Liquid argon Emulsion Magnetic sampling calorimeter Near detector

Further instrumentation issues: Flux, muon-polarisation measurement


Detector Questions

Which can effectively be magnetised?

Iron calorimeter, Emulsion, Hybrid Emulsion-Scintillator, Totally active scintillator

Liquid Argon??

How low can one reduce the threshold?

Can the Detector be on the surface

Which can identify taus?This must tie in with the relevance of gold, silver platinum

Usefulness for non-oscillation physics

Define the necessary R&D Programme


Neutrino Factory Future Development Following ISS there needs to be a Design Study

for a Neutrino Factory It will need engineering effort And therefore resources Where can these come from?

Funding Agencies, Labs, EU

At the BENE/ISS meeting tomorrow planning for a request to the EU FP7 programme will start

But funding from this source will not come until mid-end 2007 Activity must start before then - it should start this

year And maintain the momentum of the ISS study


Era ofsensitivity &

precision

Factory Beam

But Factory and beam can be on same timescale as superbeam upgrades

Timescale – the Challenges


ISS – Summary The ISS was launched at NuFact05 and is now over half

way through its one year programme Conclude at NuFact06 and a report early fall

It has demonstrated a strong desire to have an internationally coordinated effort for future neutrino research (c.f linear collider) New ideas Many clarifications

It has brought together accelerator & detector scientists with their experimental and theoretical physics colleagues in a very productive way

It has built up a momentum which must be used as a springboard for the next phase

the iss peter dornan imperial college london. 16 march 2006p dornan - mutac 20062...

Documents

p dornan mutac

iss slide

organisation slide

nufact06 slide

international approach

motivation neutrino

neutrino source options

physics approach