10 August 2004Vth Rencontres du Vietnam - L. Sulak1 New Neutrino Detectors for Astro and Particle...
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Transcript of 10 August 2004Vth Rencontres du Vietnam - L. Sulak1 New Neutrino Detectors for Astro and Particle...
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
10 August 2004 Vth Rencontres du Vietnam - L. Sulak 4
...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
10 August 2004 Vth Rencontres du Vietnam - L. Sulak 5
...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
10 August 2004 Vth Rencontres du Vietnam - L. Sulak 8
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
10 August 2004 Vth Rencontres du Vietnam - L. Sulak 10
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
10 August 2004 Vth Rencontres du Vietnam - L. Sulak 11
...deployment of Antares preproduction prototype string, 5 storys 2002
10 August 2004 Vth Rencontres du Vietnam - L. Sulak 12
underwater connections for prototype:
manned sub, 1 of 4 from Ifremer, based at shore station, Toulon
10 August 2004 Vth Rencontres du Vietnam - L. Sulak 13
plugging line for prototype string into the junction box
10 August 2004 Vth Rencontres du Vietnam - L. Sulak 14
junction box at depth, with prototype string cable connected
10 August 2004 Vth Rencontres du Vietnam - L. Sulak 15
Antares:
unreeling cable
from
junction box
to
string bottom
...Cu for power
fiber for signals
10 August 2004 Vth Rencontres du Vietnam - L. Sulak 16
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
10 August 2004 Vth Rencontres du Vietnam - L. Sulak 19
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
10 August 2004 Vth Rencontres du Vietnam - L. Sulak 20
Zenith Angle (degrees)
(1/N
)dN
/dco
s(θ)
M.C. Prediction
Data Points
Angular Fits to
Nestor Raw Data
10 August 2004 Vth Rencontres du Vietnam - L. Sulak 21
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
10 August 2004 Vth Rencontres du Vietnam - L. Sulak 24
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
10 August 2004 Vth Rencontres du Vietnam - L. Sulak 25
...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
10 August 2004 Vth Rencontres du Vietnam - L. Sulak 27
...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
10 August 2004 Vth Rencontres du Vietnam - L. Sulak 30
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
10 August 2004 Vth Rencontres du Vietnam - L. Sulak 31
10 August 2004 Vth Rencontres du Vietnam - L. Sulak 32
…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)
10 August 2004 Vth Rencontres du Vietnam - L. Sulak 33
...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
10 August 2004 Vth Rencontres du Vietnam - L. Sulak 34
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.
10 August 2004 Vth Rencontres du Vietnam - L. Sulak 35
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)
10 August 2004 Vth Rencontres du Vietnam - L. Sulak 37
...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
10 August 2004 Vth Rencontres du Vietnam - L. Sulak 38
...but geo-neutrinos and reactor neutrinos difficult to separate
consider geo signal to noise for KamLAND:
10 August 2004 Vth Rencontres du Vietnam - L. Sulak 39
...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
10 August 2004 Vth Rencontres du Vietnam - L. Sulak 40
KamLAND
D. Casper’s Oscillator
10 August 2004 Vth Rencontres du Vietnam - L. Sulak 41
D. Casper’s Oscillator
SNO+
10 August 2004 Vth Rencontres du Vietnam - L. Sulak 42
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?