veniceXIII
francis halzen
University of Wisconsinhttp://icecube.wisc.edu
• it’s the technology !• cosmic accelerators• neutrinos associated with
Galactic cosmic raysextragalactic cosmic rays
• status of neutrino astronomy• to lower energies• to higher energies• conclusions
menu
1960
M. Markov B. Pontecorvo
M.Markov :we propose to install detectors deep in a lake or in the sea and
to determine the direction of charged particles with the help
of Cherenkov radiation.
• lattice of photomultipliers
• shielded and optically transparent medium
Requires Kilometer-ScaleNeutrino Detectors
F. Reines K. Greissen
kilometer-scale neutrino detectors
1987: DUMAND test string
Camp
Lake Baikalice as a naturaldeployment platform
neutrinos!
1993 AMANDAdeconstructing astronomy
mediterranean detectors
Nestor
March 29, 20031 of 12 floors deployed4000 m deep
Antares
March 17, 20032 strings connected2400 m deep start 2006
Nemo
towards
KM3NeT
2008
Baikal
ANTARES
AMANDA
IceCube59 out of 86 strings
2006-2007:
13 Strings
2005-2006:
8 Strings
2004-2005 :
1 String
2007-2008:18 Strings
1450 m
2450 m
2008-2009:
18+1 Strings
since jan 09
59 out of 86
Ferraro Choi Associates LTD
National Science Foundation Office of Polar Programs United States Antarctic Program
IceCube Neutrino Observatory IceCube Neutrino Observatory
South Pole Drilling SeasonsSouth Pole Drilling Seasons
• Avg. time to deep drill hole 41hrs• Avg. hole depth 2452 m• Avg. drilling rate 1.7 m/min • Avg. fuel per hole 5 ,520 gal• Drill thermal power output 4.7 MW• Avg. string deployment time 8 hrs
1996/2000 Seasons - AMANDAAMANDA 2008/2009 Season - 18 Strings2005/2006 Season - First String 2009/2010 Season - 16 to 19 Strings2006/2007 Season - 8 Strings 2010/2011 Season - 18 to 20 Strings2007/2008 Season - 13 Strings 2011/2012 Season - Remaining 6 to 15 Strings
simple 8-foldmajority trigger
neutrino area
predicted performance level 2 (red)Astroparticle Physics 20, 507 (2004)
deep core
IceCube
thenandnow
back to neutrinos…
50 years later
• we have detected neutrinos, in ice and in water• we know how to build kilometer-scale detectors• an impressive achievement
separate neutrinos (filtered by the Earth) from down- going cosmic ray muons at a level of much less than one per million
p
atm
p
the challenge:
IceCube 22
one in 106 muon tracks is produced by a neutrino
within trigger time window
downdowndown
up
IceCube
background:downgoing cosmic
ray muons
~ 2000 per second
signal:upgoing muons
initiated byneutrinos
~ 10 per hour
IceCube (40) turns the corner at the horizon
ANTARES EVENT DISPLAY
26
Neu
trino
Astro
no
my
AN
TA
RE
SA
NT
AR
ES
An
alysis of th
e5Lin
e data
Heig
ht
of
hit
OM
Time of hit
EXAMPLE OF NEUTRINO CANDIDATE
Example of a reconstructed up-going muon (i.e. a neutrino candidate) detected in 5/12 detector lines.
Dornic, Moriond 2009
ANTARES
is the background more interesting ?the muon sky is not isotropic
Tibet array: northern hemisphere
the 100 TeV cosmic ray sky is not isotropic
IceCube 4x109 muons of 14TeV
Milagro cosmic ray sky between a few and 30 degrees
3 degree point source
50 years later
• we have detected neutrinos, in ice and in water• we know how to build kilometer-scale detectors• an impressive achievement, but after 10,000 ’s
• we have still not detected a cosmic neutrino
after early 1990’s days of irrational exhuberance the predictions have been stable and the goals defined
• it’s the technology !• cosmic accelerators• neutrinos associated with
Galactic cosmic raysextragalactic cosmic rays
• status of neutrino astronomy• to lower energies• to higher energies• conclusions
menu
protons > 108 TeVphotons > 102 TeVneutrinos > 102 TeV
nature’s accelerators ?
shock acceleration (solar flare)
coronal mass
ejection
10 GeVparticles
cassiopeia A supernova remnant in X-rays
shock fronts
acceleration whenparticles crosshigh B-fields
large magnetic field inyoung supernova remnants
and when the star collapses to a black hole …
collapse of massivestar produces a
gamma rayburst
’s and protons
(cosmic rays)
coexist
produce ’s
spinning black hole
active galaxyparticle flowspowered by thegravity ofsupermassiveblack hole
RadiationEnvelopingBlack Hole
Black Hole
p + 0
~ cosmic ray + gamma
NEUTRINO BEAMS: HEAVEN & EARTHNeutrino Beams: Heaven & Earth
p + n + +
~ cosmic ray + neutrino
and beams : heaven and earth
• it’s the technology !• cosmic accelerators• neutrinos associated with cosmic rays
Galactic cosmic raysextragalactic cosmic rays
• status of neutrino astronomy• to lower energies• to higher energies• conclusions
menu
galacticandextragalacticcosmic rays
galactic extragalactic
galactic cosmic rays
10-41 erg/cm3
/////////////////
Rad
io
CM
B
Vis
ible
GeV
-r
ays
energy (eV)
flu
x
410 photonsof 2.7 K
or 10-12 erg/cm3
galactic cosmic rays10-12 erg/cm3
extragalactic cosmic rays10-19 erg/cm3
2x1052 erg per gamma ray burst
energy in cosmic rays ~ photons
energy in extra-galactic cosmic rays is ~ 3x10-19 erg/cm3
~ neutrinos
3x1044 erg/s per active galaxy
neutrinos associated with extragalactic cosmic rays
AMANDA
IceCube
supermassive supermassive black holeblack hole
active galaxy
•accretion disk
•jet
Centaurus AM87Fornax A
…
Auger : the sources revealed ?
centaurus A (variability !)
neutrino astronomy
kilometer scale detectors have the capability ofdetecting astrophysical neutrinos from cosmic sourceswith an energy density in neutrinos comparable totheir energy density in the observed cosmic rays
• this is the case for gamma ray bursts if they are the sources of the extragalactic cosmic rays• for active galaxies it is also the case but the uncertain- ties are very large because of the variability of the sources
• it is definitely the case for galactic supernova remnants
• it’s the technology !• cosmic accelerators• neutrinos associated with
Galactic cosmic raysextragalactic cosmic rays
• status of neutrino astronomy• to lower energies• to higher energies• conclusions
menu
galactic plane in 10 TeV gamma rays : supernova remnants in star forming regions
Southern HemisphereSky
Standard D
eviations
30°
210°
90° 65°
Pevatrons associated with the cosmic rays near the knee ?do the sources extend to ~100 TeV with a textbook E-2 ?
\
neutrinosfrom
supernova
densemolecularclouds as
beamdumps
TeV photons trace the density of the molecular clouds
the accelerator
+-
+
+ -
e+ e
e+ e-
e+
0
e-
e+
neutral pions
are observed as
gamma rays
charged pions
are observed as
neutrinos
= =
IceCube 5 years (E > 40 TeV)
arXiv:0902.3022 for detailed statistical analysis
are the predictions time-dependent ? answer: no
in a detector with 1 km instrumented volume
1 TeV signal events: 1.3 (atm backgr: ~ 2) per year 5 TeV signal events: .2 (atm backgr: ~.2) per year
• oscillations• new HESS fluxarXiv:0902.3022
• it’s the technology !• cosmic accelerators• neutrinos associated with
Galactic cosmic raysextragalactic cosmic rays
• status of neutrino astronomy• to lower energies• to higher energies• conclusions
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AMANDA skyplot 2000-2007
6695 events below horizon
data public at http://www.icecube.wisc.edu/science/data
atmospheric neutrino spectrum
zenith angle number of PMT
the hottest spot location is: Ra 153.5 , Dec 11.5 events: 11 background: 3.3-log10(p-value) : 6.14 (4.8 sigma)
happens in 63 out of 104 scrambled maps, or the
probability is ~ 0.01
IceCube 22 moves above the horizon
Binned search: 35% less sensitive in Northern hemisphere
• it’s the technology !• cosmic accelerators• neutrinos associated with
Galactic cosmic raysextragalactic cosmic rays
• status of neutrino astronomy• to lower energies• to higher energies• conclusions
menu
~MeVGeV –
100 GeVGeV - TeV TeV - PeV PeV - EeV > EeV
?
−Decreasing neutrino flux radio
−Less light−Smaller neutrino cross section IceCube Deep Core
• it’s the technology or the long march !• cosmic accelerators• neutrino associated with
Galactic cosmic raysextragalactic cosmic rays
• status of neutrino astronomy• to lower energies• to higher energies• conclusions
1 km2 year of datathis year
menu
1500
2500
low energy core for IceCube
AMANDA
Deep Core
fiducial volume: contained vertex with no hits in outer “veto” region is a candidate for a neutrino, including downward as well as upward events
Mtontenheightn scattstrings 2
ta
u
el
ectr
on
muo
n
matter effects in the Earth near first absorption dip sensitive to hierarchy
key > 10K per year statistics
sin2 213m
sin2 213
sin2 213 cos213 2GF Ne13
2
(mostly) neutrino + antineutrino -
sign 13 : hierarchy !
• it’s the technology !• cosmic accelerators• neutrinos associated with
Galactic cosmic raysextragalactic cosmic rays
• status of neutrino astronomy• to lower energies• to higher energies• conclusions
menu
Gurgen Askaryan (1962)
radio emission from neutrino induced showers
Cherenkov power is notproportional to frequency becauseof coherence at MHz to GHz wavelengthsshowers (photons and pairs) are not electrically neutral
confirmed by calculation and
experiment in 1990s
ANITA : new data soon
staged IceCube enhancements
Optical:
80 IceCube + 13 IceCube-Plus (astro-ph/0310152) holes at 1 km radius (2.5 km deep)
Radio/Acoustic:
determine GZK event rates with 6 + 12 radio detectors at the surface or at depth
calibration with IceCube!
overflow
oscillation probability vs neutrino energy (GeV)
disappearance
appearance
WIMP capture in the sun and annihilation in
neutrinos
DETECTOR
n
+ W + W +
sensitivity to wimpsspin-dependent interactions
dark matter annihilation in the sun vs CMSSM
dark discstandard halo
sensitivity to wimpsspin-independent interactions