10 August 2004Vth Rencontres du Vietnam - L. Sulak1 New Neutrino Detectors for Astro and Particle Physics...a “Bright” Future …a selected overview... L

10 August 2004 Vth Rencontres du Vietnam - L. Sulak 1

New Neutrino Detectors

for Astro and Particle Physics

...a “Bright” Future

…a selected overview...

L. R. Sulak

CPPM Marseille and Boston University

now in a new era, well past the 1998 advent of neutrino mass and oscillations

next a panoply of key, very difficult, experiments measuring precision neutrino oscillation parameters Kayser, Farine

...the search for CP violation in the second sector of nature Kobayashi, Lasserre, Wong

absolute mass scale...the problem of mass

zero neutrino double β decay...neutrino = antineutrino? Thomas

neutrino astronomy Connolly, Houghey, Kouchner, Olinta,Tomas

all point to high energy scale, possibly Grand Unification scale each physics goal has very different challenges

neutrino sources...flux, energy, baseline Blondel, Wagner

detectors...shielding, depth, volume

neutrinos...physics, as critical as searching for electroweak scale ...astronomy, may become important as light

... neutrinos merit the many required new detectors

...consider a few selected future operations... IceCube Km3 Mediterranean astrophysical observatory...complement to IceCube

12 string Antares detector well underway...counterpart to Amanda first data from Nestor prototype “star”Km3 design study in approval process (10 M Euro request)

3 sites and 2 technologies

SNOLab... a “new” international lab, in transitionexpansion program to accommodate many experiments ($50 M) SNO detector evolution...it, and KamLAND...have done there duty

Frejus Lab...a home for Megaton? next step in search for proton decay...key to early universe, 1016 GeV

...grand unificationwith potential ideal oscillation distance, energy, and beams from CERN

Neutrino facilities planning in the US


...the future...

Evolution of Major Neutrino Research Worldwide

Facility Detectors Neutrino Source

SNOLab SNO → SNO+ → SNO++ Bruce Reactor + , Dark Matter, ...

Soudan Lab Minos→NOA NuMI → p driver+

Kamioka Lab K2K → T2K KEK → JPARC SK→ Hyper-K

Gran Sasso Lab Opera, Icarus CNGS → SPL Modane Lab → Megaton CERN → SPL+ South Pole Amanda → IceCube cosmic

Radio Č → Anita Mediterranean Antares/Nemo/Nestor → Km3 cosmic

→ Acoustic Detection


...viewing the heavens below each detector...

AMANDA (South Pole)ANTARES (43° North)

Never seenPSR B1706-44

RXJ 1713.7-39

Mkn 421

Mkn 501

PKS 2155-30

SN1006

VELA

CRAB

CasA

1ES2344+514

galactic center only seen by Antares60% overlap in coverage...systematic checks

...neutrino telescopes necessary in both hemispheres

~Never seen

PSR B1706-44

RXJ 1713.7-39

Mkn 421

Mkn 501

PKS 2155-30

SN1006

VELA

CRAB

CasA

1ES2344+514

“Proc. Dumand Summer Workshop,” 1976, LRS

with Markov & Zheleznykh’s inspiration,

ultra high energy neutrino signatures

for Dumand (and successors)

1) long penetrating muon tracks,

mostly with minimal light

2) short bright hadronic showers

if vertex “nearby”

signature, & light attenuation length,

set spacing & size of light sensors

Dumand array concept:

~ as realized in Amanda

the same in Antares

...but 4 km depth

“Proc. Dumand Summer Workshop,” 1976


Amanda technology80 strings / 60 OM’s each17 m OM spacing125 m between strings1 km2 hexagonal pattern

Surface array: 2 OMs each string topcalibrate angular response 100 tagged TeV /day

installation, operation 2005-2010

Eµ=6 PeV, 1000 hits

Am

anda

II

IceCubeSimulation

0.6° resolution

20m scattering length


Antares: install, operate ‘05-’07, 60 m sea water, 2.1-2.4 km depth 900 pms, 12 lines, 25 stories/line, 3 pms/story, ~0.1 km2 , 0.2° above 10 TeV, x2-3 energy resolution above 1 TeV

~70 m

350 m

100 m

14.5 m

Submarine links

JunctionBox

40 km toshore

Line anchor


...deployment of Antares preproduction prototype string, 5 storys 2002


underwater connections for prototype:

manned sub, 1 of 4 from Ifremer, based at shore station, Toulon


plugging line for prototype string into the junction box


junction box at depth, with prototype string cable connected


Antares:

unreeling cable

from

junction box

to

string bottom

...Cu for power

fiber for signals


plugging-in the pre-production prototype at 2.4 km depth

master local control module

LED beacon local control module

string control module andstring power module

interlink cable withwet-mateable connector

acoustic beacon

acoustic receiver

3 optical modules

acoustic receiver

12m

100m

acousticreleases

Antares preproduction prototype (2002-3)...redeploy in October

Nestor preprototype deployment rigid “star” architecture

March 2003 4 km depth

6 blue optical modules

2 pm’s, up & down

6 yellow floats

above pix:

white lines to bouy

red to LED beacon

below, unseen:

lines to junction box

Kouchner


Run: 63_37 Event: 396

Track Candidate

Number of Hits

Number of Used

Hits

Number of Degrees

of Freedom

Zenith Angle

(Degrees)

Azimuth Angle

(Degrees)

Impact Parameter

(m)

Pseudovertexχ2 -lnLch

Vx (m) Vy (m) Vz (m)

1 7 7 2 30 (± 35)

82 ±3) 11 11(± 21)

30 (± 23)

42(± 9)

3 36.5

2 7 7 2 101(± 10)

33(± 29)

9 43(± 15)

32(± 16)

-4(± 8)

2.7 30.3

Nestor: 800 events from 106 4-fold triggers


Zenith Angle (degrees)

(1/N

)dN

/dco

s(θ)

M.C. Prediction

Data Points

Angular Fits to

Nestor Raw Data


Nestor measurement of atmospheric muon flux

with Dumand and Antares prototypes,

3 existence proofs for deep underwater technology

...other neutrino detectors...

beside geography,

why so many facilities?

for Megaton...

the bigger cavity, the better.

for solar and

background sensitive exp’ts

the deeper, the better

e.g. impossible for IMB

consider SNO at Sudbury,

then Modane at Frejus

...Letters of Intent, presentations from this May…

Prospective Experiments at New SNOLab Int’l Facility

6 kmwe, deepest int’l facility: 70 muons/day vs. 26,000/day at Kamioka

2 new halls, 30m x 15m, approved (~1/2 size vs. Gran Sasso), $50 M upgrades

potentially in new halls, starting ‘07:

Dark Matter Searches Chardin

CDMS vs Soudan, SNO depth minimizes muon-induced fast neutrons

ZEPLIN dark matter with liquid scintillator, if Boulby is not deep enough

CLEAN 1 T (10 T for solar ) self-shielded, scintillating liquid Ne/Xe*

XENON drifting charge dark matter search - R & D

DRIFT dark matter with pointing using low pressure TPC:

PICASSO acoustic detection of nuclear recoil with superheated bubbles in gel

Neutrino Experiments

HALO SNO 3He detectors with Pb, supernova neutrinos

Noble Liquid Tracking Detectors for solar neutrinos with He or Xe


Double Beta Decay searches

Majorana 500 kg of Ge detectors for : scale up of known technology

GERDA (~GENIUS) 1 T Ge crystals in clean Liq N2, no housings, self-shielded

EXO Xe TPC, with laser fluorescence tag of Ba upon decay

COBRA CdZnTe...semiconductor, all 3 candidates

recyling SNO Detector or Cavity

after 3He neutral current work is done, SNO Phase III over, D2O comes out in ’07

SNO+ geo and reactor neutrinos: fill with scintillator

with n tag, get 700 kT fiducial

SNO++ Decay: scintillator + 1 Ton of Te or Nb nanocrystals

or + 2 Ton Xe dissolved gas

SNO best facility in world for almost all experiments?

...except potential cavity size too small for Megaton


...the other lab with a rebirth...

Modane Megaton detector: two possible sites, both ~130 km to CERN

Fréjus I required second tunnel, near the present lab, ’05-’08

deep covering, 4800 mwe

dry rock, good quality, well known

question: 5m diameter safety tunnel or 10m roadway?

Fréjus II 15 km experimental tunnel for new Lyon-Torino TGV train

(actual train tunnel to be longest and deepest in Europe)

endorsed by Chirac and Berlusconi on Monday

covering of 7000 mwe

rock expected to be hard, but not yet studied

potentially water, since glaciers above

problem: regional support for lab if no entry in France?

≈ 13 km (12 870 m)

1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 18 19 20 21 22 23 24 25 26 27 28 29 30 31 32 33 34

70 m x 70 m x 250 m

France Italy

Future Lab.

Present road Tunnel at Fréjus (grey)andfuture Tunnel (black) for safety with 34 bypasses (shelters)connecting the two Tunnels

In Europe, build Megaton for proton decay and supernova while tunneling,

super and beta beams later

JPARC/T2K: Hyper-K and 2 MW proton source upgrade tentative, pending

proton decay hint at Super-K, or

favorable θ13 measurement in T2K...Hyper-K could be much later


...under study Modane “Megaton,” 2 detector technologies, 3 geometries

1 MT water Cherenkov à la Hyper-K

100 kT liquid argon Messina

...meanwhile in the USA?

Neutrino Physics Planning Processes

American Physical Society Neutrino Study (Kayser, co-chair)

recommending high priority neutrino experiments: atmospheric and solar (pp?) astrophysical reactor

superbeams neutrino factories and beta

beams double beta decay

NSF Initiative: A “Deep Engineering and Science Underground Laboratory”7 potential sites: Henderson, Homestake, Icicle Creek,

Kimbleton, San Jacinto, Soudan, WIPP3 solicitations for proposals:

1) site independent physics justification and requirements (out)2) site specific proposals, a few to be chosen3) full proposals, limited to the NSF selected sites

...conclusions...

new recognition of importance of neutrino physics and astrophysics relative to electroweak symmetry breakingfor pointing, where photons cannot penetrate

necessity of coupled source / detector facilities to optimize S/B

synergism other needs for proton drivers at CERN, FNAL, JPARC increased luminosity and intensity for other experimentsradioactive ion beams...nuclear, biology, medicine all naturally lend themselves to hot neutrino beams

within a few years...results expected fromAntares, Minos...as well as other experiments

longer term: significant promise for IceCube...Km3, Megaton...T2K...Hyper-K

...bright future for neutrino detectors


this talk is dedicated to Tran

hommage for all those Rencontres

theory godfather to particle and astroparticle physics

and the legacy of neutrino detectors that have followed

...and to Kim...we all wouldn’t be here if it weren’t for them



…wither this next step in neutrino physics in Europe?

Future European Neutrino Sources and Detectors

Coordinated Accelerator Research in Europe for Hi Intensity Proton Pulsed Injector

CERN accelerator projects: Multi-MegaWatt Proton Linac

RFQ preinjector 3MeV @ 50 mA... a project of CEA, CNRS, IN2P3

Linac 4 3 MeV → 160MeV…5-10 x more protons...R&D

Superconducting Proton Linac (SPL at CERN, Proton Driver at FNAL)

160 MeV → 2 GeV x 2 mA = 4 MW goal for 2014

the promise for neutrino physics:

Super-intense CERN Neutrinos to Gran Sasso (SCNGS)

2 x more neutrinos (limited by other elements in complex)

Super (but conventional) Neutrino Beams...many more neutrinos

(Advantages for LHC (robust operation, hi luminosity for UltraLHC, rare K decays, etc3-4 x more protons on target)


...using the great depth...

SNO+ as low energy solar neutrino detector

7Be 0.86 MeV line

10% calculational, 40% experimental uncertainty...difficult

pep 1.44 MeV line...a precision measurement

1% predicted uncertainty...3000/year oscillated

muon-induced 11C → e+ gives 1 MeV within 20 minutes

untenable background in KamLAND , Borexino

SNO+ : with only 70 muons/day

track muon and veto 1 m radius around it


An « 0ptimal » schedule for a Megaton Physics Project in Europe

Safety Tunnel

Large Cavity

R&D PMT’s, etc.

PMT’s production

2003 2004 2007 2008 2012 2015 2020

Detector installation

Start Megaton Physics

SPL + Super-beam realization

Procedure :

Beta-beam realization

excavation

excavation

R&D PMT’s, etc

PMT’s production

Detector inst.

Start Megaton Physics ………………...………………….

SPL+Super-beam realization

Beta-beam realization

EoI

Year

?

?

studyPre-study

LoI Prop Approv.


Satellite-based Air Cherenkov telescopes

EUSO and OWL

>1000 GTon mass

Radio Cherenkov seen by balloon above South polar cap

Anita

EeV neutrinos...e.g. from GKZ pions produced by protons on CMB photons

...astro successes of water Cherenkov detectors...

first physics beyond standard model from cosmic neutrinos

mass and oscillation...most cited exp’tal paper of all time

first extra-terrestrial neutrinos, imaging sun with them

first extra-galactic neutrinos – SN 1987A

the truly early universe, and grand unification still an ultimate goal,

...but awaiting discovery

annihilations of susy particles in sun, galactic center

high energy point sources (e.g. active galactic nuclei, grbs)


...potential future of SNO+ Detector, for geo and reactor neutrinos...

A Closer Look at SNO+

infrastructure for low background work

e.g. low Rn cover gas (N2), 1 neutron capture/day from U&Th

1 kT of low background liquid scintillator, as in KamLAND w/ 10-17

Geological electron anti-neutrinos

energy = 3.4 MeV - 1.8 MeV Q = 1.6 MeV positron + 1 MeV e+e- annihilation = 2.6 MeV deposited

for KamLAND: at 180 km from reactors, looking for geo at <2.6 MeV

confused with 2nd oscillation minimum at 3 MeV

...hard to extract geo since reactor spectrum distorted just there

and only ~ 40 geoneutrinos per year


...but geo-neutrinos and reactor neutrinos difficult to separate

consider geo signal to noise for KamLAND:


...how important is distance from reactor? SNO+ vs. KamLAND

SNO+ is 240 km from 14 GW Bruce vs KamLAND at 180 km from 80 GW

2nd reactor oscillation minimum moves up x 1.5 to 5 MeVreactor flux is max

no geo signal >3.4 MeV ...clean for reactor neutrinosnarrower dip sharper spectral distortion

a notch at 5 MeV 80 events / year, if no reactor oscillations

note subtle difference in pattern with Casper’s Oscillator

for geo-neutrinos, look < 2.6 MeV, at SNO+ many fewer reactor neutrinos (1 reactor, further away)

oscillation pattern smeared out64 geo-neutrino events / year vs. 29 at KamLAND & 10 at Borexino

U/Th neutrino source thick continental crust, vs. the thin coastal crust in Japan

SNO+... ideal to separate geo from reactor neutrinos


KamLAND

D. Casper’s Oscillator


D. Casper’s Oscillator

SNO+


Advantages of either Frejus Site

independent, horizontal access

neutrino super-beams and beta beams likely upgrades to CERN

at “magic distance” and right L/E (130 km/0.3 GeV) for those beams

if LEP RF cavities recycled, 2.2 GeV protons give 0.3 GeV higher energy, muon/pion discrimination a problem

lower energy, muons don’t make enough Cherenkov light in water

(further away, higher E, as in US, e/o/ separation a problem for Č

French and Italian joint initiative

“extension” of Gran Sasso Lab... water prevents a Megaton cavity

preliminary study of large cavity (106 m3) at both Fréjus sites

maximum possible size of cavity for each of 3 shapes?

cost and time of excavation?

Documents

10 August 2004Vth Rencontres du Vietnam - L. Sulak1 New Neutrino Detectors for Astro and Particle Physics...a “Bright” Future …a selected overview... L