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

menu

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