…a selected overview...
New Neutrino Detectors
for Astro and Particle Physics
...a “Bright” Future
L. R. Sulak
CPPM Marseille and Boston University
10 August 2004
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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?
neutrino astronomy
Thomas
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 transition
expansion 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 unification
with potential ideal oscillation distance, energy, and beams from CERN
Neutrino facilities planning in the US
...the future...
Evolution of Major Neutrino Research Worldwide
Facility
SNOLab
Soudan Lab
Kamioka Lab
Gran Sasso Lab
Modane Lab
South Pole
Mediterranean
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Detectors
SNO → SNO+ → SNO++
+ bb, Dark Matter, ...
Minos→NOnA
K2K → T2K
SK→ Hyper-K
Opera, Icarus
→ Megaton
Amanda → IceCube
Radio Č → Anita
Antares/Nemo/Nestor → Km3
→ Acoustic Detection
Vth Rencontres du Vietnam - L. Sulak
Neutrino Source
Bruce Reactor
NuMI → p driver+
KEK → JPARC
CNGS → SPL
CERN → SPL+
cosmic
cosmic
4
...viewing the heavens below each detector...
ANTARES (43° North)
AMANDA (South Pole)
Mkn 421
Mkn 421
Mkn 501
~Never seen
Mkn 501
RXJ 1713.7-39
SN1006
RXJ 1713.7-39
CRAB
SN1006
CRAB
Never seen
CasA
CasA
PSR B1706-44
1ES2344+514
VELA
PSR B1706-44
1ES2344+514
PKS 2155-30
VELA
PKS 2155-30
galactic center only seen by Antares
60% overlap in coverage...systematic checks
...neutrino telescopes necessary in both hemispheres
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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
“Proc. Dumand Summer Workshop,” 1976, LRS
Dumand array concept:
~ as realized in Amanda
the same in Antares
...but 4 km depth
“Proc. Dumand Summer Workshop,” 1976
Amanda technology
80 strings / 60 OM’s each
17 m OM spacing
125 m between strings
1 km2 hexagonal pattern
Surface array:
2 OMs each string top
calibrate angular response
100 tagged TeV  /day
installation, operation
2005-2010
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Eµ=6 PeV, 1000 hits
0.6° resolution
20m scattering
length
Amanda II
IceCube
Simulation
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
14.5 m
350 m
40 km to
shore
100 m
Junction
Box
~70 m
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Line
anchor
10
Submarine links
...deployment of Antares preproduction prototype string, 5 storys
2002
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underwater connections
for prototype:
manned sub,
1 of 4 from Ifremer,
based at shore station,
Toulon
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plugging line for prototype string into the junction box
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junction box at depth, with prototype string cable connected
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Antares:
unreeling cable
from
junction box
to
string bottom
...Cu for power
fiber for signals
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plugging-in the pre-production prototype at 2.4 km depth
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Antares preproduction prototype (2002-3)...redeploy in October
acoustic
receiver
3 optical modules
12m
local control module
LED beacon
acoustic
receiver
acoustic
beacon
acoustic
releases
master local control module
100m
string control module and
string power module
interlink cable with
wet-mateable connector
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
Nestor: 800 events from 106 4-fold triggers
Track
Candidate
Number
of Hits
Number
of Used
Hits
Number of
Degrees
of
Freedom
Pseudovertex
Zenith
Angle
(Degrees)
Azimuth
Angle
(Degrees)
χ2
Impact
Parameter
(m)
Vx (m)
Vy (m)
Vz (m)
-lnLch
Run: 63_37 Event: 396
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
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Nestor Raw Data
(1/N)dN/dcos(θ)
Angular Fits to
M.C. Prediction
Data Points
Zenith Angle (degrees)
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Nestor measurement of
atmospheric muon flux
with Dumand and Antares
prototypes,
3 existence proofs for deep
underwater technology
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...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
CDMS
Chardin
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 n) 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 bb : 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 bb 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++
bb 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
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...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?
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- 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 2425 26 2728 293031 323334
70mx 70
mx 250
m
France
Italy
Future Lab.
In Europe,
build Megaton for proton decay and supernova while tunneling,
super at
and
beta(grey)
beams later
Present road Tunnel
Fréjus
and
JPARC/T2K:
Hyper-K and 2 MW proton source upgrade tentative, pending
future Tunnel (black) for safety with 34 bypasses (shelters)
decay hint at Super-K, or
connecting theproton
two Tunnels
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
10 August 2004
Messina
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...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, WIPP
3 solicitations for proposals:
1) site independent physics justification and requirements (out)
2) site specific proposals, a few to be chosen
3) full proposals, limited to the NSF selected sites
...conclusions...
new recognition of importance of neutrino physics and astrophysics
relative to electroweak symmetry breaking
for 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 experiments
radioactive ion beams...nuclear, biology, medicine
all naturally lend themselves to hot neutrino beams
within a few years...results expected from
Antares, 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
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…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, etc
3-4 x more protons on target)
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...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
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An « 0ptimal » schedule for a Megaton Physics Project in Europe
Year
Procedure :
2003 2004
EoI
LoI
Safety Tunne l
Large Cavity
R&D PMT’s, etc.
2007 2008
Prop
2012
2015
Approv.
excavation
Pre-study
study
excavation
R&D PMT’s, etc
PMT’s produc tion
Detector installation
PMT’s production
Detector inst.
Start Megaton Physics ………………...
………………….
Start Megaton Phys ics
SPL + Supe r-beam realization
Beta-beam realization
10 August 2004
2020
SPL+Super-beam realization
?
Beta-beam realization
?
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EeV neutrinos...e.g. from GKZ pions produced by protons on CMB photons
Satellite-based Air Cherenkov telescopes
EUSO and OWL
>1000 GTon mass
Radio Cherenkov seen by balloon above South polar cap
Anita
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...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
n 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 n at <2.6 MeV
confused with 2nd oscillation minimum at 3 MeV
...hard to extract geo n since reactor n spectrum distorted just there
and only ~ 40 geo neutrinos per year
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consider geo signal to noise for KamLAND:
...but geo-neutrinos and reactor neutrinos difficult to separate
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...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 MeV
reactor flux is max
no geo n signal >3.4 MeV
...clean for reactor neutrinos
narrower 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 out
64 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
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KamLAND
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D. Casper’s n Oscillator
40
SNO+
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D. Casper’s n Oscillator
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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 n
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/po/g 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?
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