AntaresInauguration

1
discovering neutrinos from the
earth...the sun... our sister galaxy...
...next a galactic center?
L. R. Sulak CPPM Marseille and Boston University
2
an experimenters tribute to Maury Shapiro...
from Dumand IMB... thru Super
K ...and onto Antares
today, the first of two talks
L. R. Sulak CPPM Marseille and Boston University
3
...homage to Maury, godfather to
Dumand, IMB, the legacy of detectors
that followed ...even those still on
their way for precocious support of neutrino
astrophysics... water Cherenkov and acoustic
detection techniques, proton decay neutrino
oscillation searches MS born the year of
Einsteins General Relativity...destined for
physics off to Los Alamos in 44,
with all the greats, Val Fitch Cosmic Ray Lab
at Naval Research Lab...Navy funds my
PhD stimulating water C detection since 76 study
of Dumand inspiring young scientists for gt 28
years when I met him
4
...a retrospective on ? detection by Cherenkov
light in water, and a perspective for the
next 4 years invention of technology massive,
pixellated, time and amplitude Dumand
IMB evolution Kamioka to Super-K astro
discoveries! terrestrial neutrinos confirmed
IMB extra-terrestrial neutrinos...solar
K extra-galactic neutrinos...Magellanic Cloud
IMB K particle physics! neutrino
oscillation and mass yet to come? AGN BZS
neutrinos (Amanda) Antares
(IceCube Km3) proton decay, CP
violation (Megaton)
5
...a personal commentary...evolution of neutrino
astrophysics... Retrospective of 4 ring-imaging
Cherenkov Detectors muon telescope,
prematurely terminated (with SSC), then reborn
Dumand 76-93 0.1 km2 ? 1 km3 7
countries, off Hawaii Antares 05
8 countries, off France worlds
largest calorimeters IMB 81 10
kilotons 2k pms salt mine, Ohio
Kamiokande 83 3 kilotons 1k pms heavy
metal mine, Japan Super-K 96 50
kilotons 13k pms 2nd Kamioka site
detectors color-coded
throughout talks see other talks for
details and other experiments e.g.
Goodman, Kuzmin, Mikheyev, Migneco, Postnov,
Silvestri, Stanev...
6
IMB 1981 2000 - 5 EMI pms, time pe 25 Mev
threshold reverse osmosis water, worlds purist
water, gt 50m
7
Kamiokande 1983 1000 - 20 inch pms 40
photocathode coverage outer veto 7 MeV
threshold, for sun 1 km underground...for
sun 2.7 km of water, Antares depth, 2x
Amanda initially no timing, minimal water
filtering remedied in Kamioka III, 1986
8
Super-K 1996 half way up first filling inner
detector 11,000 20 inch pms outer detector
(not visible) reconfigured IMB III 2,000 8
inch pms with wavelength-shifting
light collectors
9
Dumand (1987) 7 - 15 photomultipliers in
17 Benthos spheres short prototype string
deployment 1 week operation to 4.5 km
depth
10
Antares (2004-6) 900 pms, 12 lines, 25
stories/line, 3 pms/story
Submarine links
11
with Markov Zheleznykhs 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
12
the challenge... reconstructing energy and
direction of particle tracks using
light intensity
arrival time
Proc. Dumand Summer Workshop, 1976, LRS
13
Dumand array concept the same in
Antares similar in IMB, Amanda...
Proc. Dumand Summer Workshop, 1976
14
the Dumand site same distance to shore as
Antares 4.8 km deep atm ? shielding 2x
Antares, 4x Amanda ...we were conservative in
76 Proc. Dumand Summer
Workshop, 1976
15
an optical module photomultipler
housing, precursor for Amanda, Antares without
Benthos spheres, similar for IMB, then
Kamioka and Super-K
16
Dumand concept line deployment
17
...conclusion of Dumand 76 Workshop
...stage was set...for a massive land-based
prototype...IMB
18
...when PDK impetus came, 10 kiloton prototype
design study immersed hemispherical pms
single photoelectrons (1/4 pe lsb) 2-scale
waveform digitization 1 ns for
directionality 0.1 ms, muon decay deadtimeless
calibration LED ball, N2 laser, muon
decay Cortez, Foster, Levi,
LoSecco LRS Madison Meeting on Proton
Stability, D. Cline, ed., December 1978
19
...a 0.5 MeV muon track... what does it look
like?
LRS Erice 1980,
Neutrino 79, Bergen FWOGU, 1980
20
...why is timing so important? Cherenkov light is
directiona 1 ns resolution ? few degrees
LRS Erice 1980, Neutrino 79, Bergen
FWOGU, 1980
21
IMB Status at Erice 1980 Proton decay
detector details and First proposal of
neutrino oscillation search over baseline of
earth via up/down ?/e asymmetry critical in
securing DOE funding
LRS also FWOGU 1980
22
IMB I after 1 year operation, 5 of pms
crack ...reverse osmosis too clean IMB II
replace 5 EMI pms with 8 Hamamatsu pms...
designed using IMB photoelectron tracing
code IMB III add wavelength shifting light
collector plates
23
IMB III (1983) 2000 - 8 inch pms and light
collectors dry suit diver/physicist
24
IMB best proton decay candidate...pm code
timing in color, 1 pe/slash
25
(No Transcript)
26
Nucleon Lifetime Limits IMB 45 decay modes
mass is everything, MEGATON is needed
McGrew 2003
27
atm ?s up-going ?, as well as contained
events...red entry, yellow exit...
28
IMB Do the neutrino-induced up-going muons point
back to a source?
Galactic Latitude
Galactic Longitude
sun, moon, galactic center? with 496 IMB
events, no ...with Super-K? no, see Shantanu
Desais recent PhD too small! need Amanda,
Antares, IceCube, Km3
29
Supersymmetry... has generated so many
thousands of papers it must be correct
Shelly Glashow
30
at 073535 UTbamb-bam bam bam8 times in IMB


11 in Kamioka
an entire sun implodes, explodes...in 13 seconds
31
Super Novaall heavy elements are born....iodine,
silver, gold...
the night before 23 Feb gt 4 hours
after neutrino burst
32
each with a beautiful Cherenkov ring
all detectors hit at the same timetime
encoded in color
33
with your eye at the vertex of the 3rd event...
...100 billion neutrinos per cm2
34
SuperNova! Cover Story
35
IMB anomaly see only 75 of expected
muon-neutrinos...
...but Kamioka found no muon anomaly (e.g.Kajita
PhD 86)...until 88
36
conclusion... Technology driven by the
science pixelated, ring-imaging Cherenkov
calorimetry...proven submersible,
depth-tolerant pms and electronics single
photoelectron operation pattern recognition
and directionality Astro-neutrino physics
discoveries first physics beyond standard
model neutrino mass and oscillation...most
cited paper of all time first
extra-terrestrial neutrinos, imaging sun with
them first extra-galactic neutrinos SN
1987A grand unification still the ultimate
goal, ...and annihilations, high energy
point sources etc. await discovery!
37
pursuing cosmic ray and neutrino astrophysics...
Maury, on behalf of your experimental
friends, and me, from Dumand, IMB, Super-K
and Antares, we thank you for your seminal
cosmic ray work and for your intellectural
support of our experiments
38
(No Transcript)
39
(No Transcript)
40
(No Transcript)
41
...dedicated to you, the new generation of ?
astrophysicists... discovering neutrinos
from the earth...the sun... our sister
galaxy... ...next a galactic center?
L. R. Sulak CPPM Marseille and Boston University
42
an experimenters view of technical details
from Dumand IMB... thru Super
K ...and onto Antares
today, the second of two talks
L. R. Sulak CPPM Marseille and Boston University
43
...a retrospective on ? detection by Cherenkov
light in water, and a perspective for the
next 4 years ? invention of technology
massive, pixellated, time, amplitude
? IMB Dumand to Antares evolution
Kamioka and Super-K astro discoveries!
? terrestrial neutrinos confirmed
IMB ? extra-galactic neutrinos...Magellanic
Cloud IMB K extra-terrestrial
neutrinos...solar K particle physics!
neutrino oscillation and mass yet to
come? AGN BZS neutrinos Amanda,
IceCube Silvestri Km3
Migneco acoustic detection proton
decay, CP violation Megaton
44
Kamioka II 1987 with timing by U. Penn Cortez,
Rn purification ...low energy
electron-neutrino events point back to the sun!
...with hi statistics, Super-K sees only 47 of
expected solar model flux
22,400 solar neutrino events 15 events/day
Direction cosine to the sun
45
pointing neutrinos from the peak back to find
their origin...
Kamioka and Super-K see the suna neutrino
heliograph from Svoboda
46
...but tubes from Kamioka not tested at Super-K
depth!!!
47
Super-K II (2003) a typical muon-neutrino event
...in time with beam pulse from KEK
accelerator 300 km away
...sharp ring edges characteristic of a muon track
48
typical electron track...fuzzy at edges
49
(No Transcript)
50
but 30 of muon neutrinos missing...those coming
up through the earth
...six other different samples of neutrino data
behave similarly
51
(No Transcript)
52
neutrinos are missing with high statistical
significance...
...consistent with original IMB anomaly and later
Kamiokande results ...but not with
much smaller iron detectors
53
Dumand 1987 Optical Module Fabrication
...magnetic shielding and Boston
electronics visible
54
Dumand Short Prototype String Assembly 0.5 km
optical and electrical cables kevlar support
cables
55
String controller distribution box...power
(black) and optic fibers (red)
56
Dumand 87 deployment of string controller
view of middle of string with power
converters 1 GHz digitizer optical
multiplexer/demultiplexer 1 of the 7 optical
modules seen in front
57
Dumand 87 laying of cable
58
Dumand winch laying cable and junction box
59
Junction box deployment, with cable to shore
60
Dumand 87 junction box resting on the
bottom at 4.8 km now ...fast forward to
Antares
61
...why 2 detectors? viewing the heavens below
each detector...
ANTARES (43 North)
AMANDA (South Pole)
Mkn 421
Mkn 421
Mkn 501
Mkn 501
Never seen
SN1006
SN1006
CRAB
CRAB
Never seen
CasA
CasA
VELA
1ES2344514
VELA
1ES2344514
PKS 2155-30
PKS 2155-30
galactic center only seen by Antares, but good
overlap... sun, and any SUSY anihilations from
it, always at Amandas horizon ...complementary
? telescopes necessary in both hemispheres
62
Antares preproduction prototype (2002-3)...1 of
20 sea campaigns

63
deployment of Antares preproduction prototype 2002
64
underwater connection to prototype manned
sub 1 of 4 from Ifremer based at Toulon, FR
65
Antares prototype spool out cable from
string bottom to junction box
66
plugging the pre-production string at 2.4 km
depth
67
plugging line from prototype string into the
junction box
68
junction box at depth, with prototype string
connected
69
Nestor prototype...off of Greece Star
Deployment March 2003
6 blue optical modules 2 pms each 6 yellow
floats above pix white lines to bouy
red line to LED beacon below, unseen lines
to junction box
70
Nestor 800 events from 106 4-fold triggers
Track Candidate Number of Hits Number of Used Hits Number of Degrees of Freedom Zenith Angle (Degrees) Azimuth Angle (Degrees) Impact Parameter (m) Pseudovertex Pseudovertex Pseudovertex ?2 -lnLch
Track Candidate Number of Hits Number of Used Hits Number of Degrees of Freedom Zenith Angle (Degrees) Azimuth Angle (Degrees) Impact Parameter (m) Vx (m) Vy (m) Vz (m) ?2 -lnLch
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
Run 63_37 Event 396
71
Angular Fits to Nestor Raw Data

72
Nestor measurement of atmospheric muon flux
...another existence proof for deep underwater
technology
73
conclusions for the water Cherenkov
detectors... Technology driven by the
science pixelated, ring-imaging Cherenkov
calorimetry...proven submersible,
depth-tolerant pms and electronics single
photoelectron operation to maximize
sensitivity directionality from
timing pattern recognition for electron/muon
discrimination Astro-neutrino physics
discoveries first physics beyond standard
model neutrino mass and oscillation...most
cited paper of all time first
extra-terrestrial neutrinos, imaging sun with
them first extra-galactic neutrinos SN
1987A grand unification still an ultimate goal,
...and annihilations, high energy point
sources etc await discovery too!
74
a new era since 1998, the discovery of neutrino
mass and oscillations now a panoply of
key, very difficult, neutrino physics
experiments precision neutrino oscillation
parameters ...search for CP
violation in a new sector of nature
neutrinoless double beta decay is the neutrino
its own antiparticle? absolute mass scale of
neutrinos...the problem of mass neutrino
astronomy all point to a high energy scale,
possibly Grand Unification scale each
goal has very different needs neutrino
sources...flux, energy, baseline
detectors...shielding, depth, volume neutrino
physics as important as searching for
electroweak scale at LHC!
... neutrinos merit the many required
new facilities ...
75
...in your future... Evolution of Neutrino
Research Worldwide Facility
Detectors Neutrino Source
SNOLab SNO?SNO ?SNO
Bruce Reactor bb, Dark Matter ...
Soudan Lab Minos ? NOnA NuMI ?
p driver Kamioka Lab SK ? Hyper-K
K2K ? T2K KEK ? JPARC
Kamland ? new reactor Gran Sasso Lab
Opera, Icarus CNGS ?
SPL Modane Lab ? Megaton CERN ?
SPL South Pole Amanda ?
IceCube astro-neutrinos
Mediterranean Antares/Nemo/Nestor ? Km3
astro-neutrinos
76
...time limits talk to selected future
operations SNOLab... new international
lab, in transition 50 M expansion program to
accommodate many experiments SNO detector
evolution Km3 astrophysical
observatory... 3 sites and 2 technologies
Migneco first data from Nestor prototype
star construction of 12 string Antares
underway Km3 engineering, site study (10 M
Euro) in approval process Frejus Lab...a
home for Megaton...an Italian/French initiative
potentially with ideal beams from CERN
77
beside my back yard, why so many
facilities? for Megaton... the bigger the
cavity better, deeper not necessarily
better for solar sensitive expts the
deeper, the better e.g. spallation from muons
impossible for IMB to do
solar neutrinos ...consider SNO at Sudbury

78
...Letters of Intent, presentations from May
Prospective Experiments at New SNOLab
International Facility 6 kmwe, deepest intl
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 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

79
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
with the 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
cavity size too small for Megaton
80
...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
UTh 1 kT of low background liquid
scintillator, as in KamLAND w/ 10-17 Geo
electron anti-neutrinos n energy 3.4
MeV - 1.8 MeV Q 1.6 MeV positron
1 MeV ee- annihilation 2.6 MeV
deposited KamLAND at 180 km from reactors looks
for geo n at lt2.6 MeV but overwhelmed by 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
81
...the geoneutrino signal to noise in KamLAND
...geo-neutrinos and reactor neutrinos
difficult to separate
82
... SNO vs. KamLAND how important is distance
from reactor? 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 gt3.4 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 Caspers Oscillator for
geo-neutrinos, look lt 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
83
KamLAND
D. Caspers n Oscillator
84
SNO
D. Caspers n Oscillator
85
...again 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 and Borexino due to lack of depth SNO
with only 70 muons/day track muon and veto 1 m
radius around it
86
...the other lab with a rebirth...
Modane Megaton detector two possible cavities,
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 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 last month
covering of 7000 mwe
rock expected to be hard, but not yet studied
potentially water, since glaciers above

87
EU 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,
wait for proton decay hint at Super-K,
or favorable ?13 measurement
in T2K ...Hyper-K could be much later than EU
detector
88
Advantages of Frejus Sites   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
dont make enough Cherenkov light in water
(further away, higher E, as in US, e/po/g
separation a problem for C Italian /
French joint initiative extension of Gran
Sasso Lab... water prevents a Megaton cavity
there 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?
89
...under study Modane Megaton, 2
detector technologies, 3 geometries 1 MT water
Cherenkov à la Hyper-K 100 kT liquid argon
90
...conclusions... new recognition of
importance of neutrino physics relative to
electroweak symmetry breaking necessity of
coupled source / detector facilities synergism
with proton drivers at CERN, FNAL, JPARC
increased luminosity and intensity for other
experiments radioactive ion beams...nuclear,
biology, medicine naturally lead to hot
neutrino beams in next two years
results expected from Antares, Minos...as well
as many other experiments longer
term significant promise for IceCube, Km3,
Megaton, Hyper-K ...bright future for
neutrino facilities, near, medium and long term
91
Acknowledgements It is a pleasure to express my
appreciation to my following collaborators for
contributing material for this review John
Learned Dumand photographs John LoSecco IMB
historical documentation Clark McGrew Proton
Decay Limits, 2003 Masayuki Nakahata Kamiokande
historical data and archives Robert
Svoboda Super-K neutrino heliograph
92
Cronological Milestones for the 5
Detectors
76 Dumand conceptually designed 78 10
kTon design study ? 79 IMB proposes PDK and
?e/?? ratio 81 IMB turns
on 83 IMB no proton
decay! no SU5 Grand Unification! Foster,Cortez
PhD Kamioka turns on
86 IMB anomaly 25 of atmospheric
muon-neutrinos missing 87 Dumand string of 7
optical modules down to 4.5 km depth for week
IMB Kamioka neutrinos from Supernova 1987a
88 Kamioka image sun in neutrino
light Nobel Prize 02
Kamioka confirms missing muon-neutrinos 89
Dumand funding approved for 0.1 km2 array 93
Dumand funding lapses along
with SSC
Antares RD
starts 96 Super-K turn-on, outer
detector IMB 98
Super-K establishes muon-neutrinos oscillate,
have mass 01 Super-K solar
electron-neutrinos oscillate too 04
Antares deployment starts