2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind...

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2006-01-07 Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University [email protected]

Transcript of 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind...

Page 1: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

Cosmic Neutrinos and

High Energy Neutrino Telescopes

Spåtind 2006 lecture 1

Per Olof Hulth

Stockholm University

[email protected]

Page 2: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

Neutrino sky 5-40 MeV

Page 3: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

Neutrino sky > 1 GeV

Nothing seen so far…….

Page 4: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

Outline

• Lecture 1– Why do we expect to see cosmic neutrinos?

• Cosmic rays• Dark matter

– Neutrino detection principles

• Lecture 2– Running High Energy Neutrino telescopes

• Some physics results

– Near future telescopes

Page 5: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

+CMB -> e+ + e-

p+CMB -> +->n+

+ GZK - neutrinos

(Greisen, Zatsepin, Kusmin)

P. Gorham

Universe is not transparent for HE photons or nuclei!

Protons deflected by magnetic field in space for

E < 1019 eV!

Not pointing back to the source!

Page 6: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

Page 7: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

Page 8: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

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Page 9: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

Page 10: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

Page 11: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

Page 12: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

Page 13: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

photonselectrons/positrons

muons neutrons

Page 14: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

photonselectrons/positrons

muons neutronsIn the same time also atmospheric neutrinos from meson and muon decays!!

Page 15: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

LHC

~E-2.7

~E-2.7

~E-3

Ankle

1 part km-2 yr-1

knee

1 part m-2 yr-1

T. Gaisser 2005

- The accelerators?

Nature accelerates particles 10 7 times the energy of LHC!

What are the sources?

Cosmic rays

Page 16: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

The size of the Universe “LHC” accelerator?

R

To use LHC magnets to deliver 1020 eV we need a radius of the

accelerator to be about 1.5 times the distance Earth -Sun

Page 17: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

Galactic sources

• Supernova are assumed to be able to accelerate particles up 1016 eV

• But the observed gammas could have electromagnetic orgin and not hadronic.

• If gammas are from 0 decays you expect about the same flux of neutrinos!

• MicroquasarHESS gamma flux

Page 18: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

Very High Energy Gamma sources

Page 19: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

Ultra High Energy Cosmic Rays

• UHECR are assumed to be extra galactic

• There are still uncertainties about flux.

• No obvious sources for the particles > 1019.5 eV within 20 Mpc…?

• GZK effect observed?Shigeru Yoshida, ICRC 2005, Pune

Page 20: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

Possible sources of UHE Cosmic Rays

Page 21: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

Active galaxies

Galaxy 3C296

Page 22: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

Gamma Ray Bursts

Cosmological sources!!

But what is it??

Source 9000 Million light years away!

Page 23: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

Gamma Ray Burst ?

Page 24: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

• We expect to have neutrinos produced when the accelerated UHECR collides with matter or light in the vicinity of the source!

• Detect the neutrinos!

Page 25: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

Observing neutrinos

Fermi acceleration of protons gives particle spectrum

dNp/dE~ E-2

Neutrino production at source: p+ or p+p collisions gives pionse- + e

Neutrino flavors:e : : 1:2:~0 at source1:1:1 at detector (?)

Page 26: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

NGC 2300

Page 27: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

Dark matter searchThere exists about 5 times more dark matter in the universe than our baryonic matter

“Best” dark matter candidate: neutralino

Neutralinos are trapped in large objects like the Sun and Earth and self-annihilate.

Search for neutrinos from the centers of Earth and Sun

See talks by Thomas Burgess and Gustav Wikström today

Page 28: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

Neutrino Astronomy

• + Neutrinos penetrate the whole Universe • + Neutrinos direction points back to the source• + Neutrinos are produced at the sources of the cosmic rays• + Neutrinos are not reprocessed at the sources• + Neutrinos expected from dark matter particle

annihilation

• - Low expected flux of extragalactic neutrinos • - Small cross section• - Needs gigantic detector volumes

Page 29: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

Backgrounds

• Atmospheric muons– Produced in cosmic ray interactions above the

telescope. In AMANDA there are 106 downward going atmospheric muons for every upward going atmospheric neutrino induced muon -> select only upward going muons as neutrino candidates. The Earth acts as a filter.

• Atmospheric neutrinos

Page 30: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

log

[E2

· flu

x(E

) / G

eV c

m-2 s

-1 s

r-1]

-9

-7

-8

-6

-5

atmospheric

2 43 5 8 109 log (E /GeV)6 7

AGN

core

(SS)

AGN Jet (

MPR)

GRB (WB)

WB bound GZK

Required sensitivity

many specific models fornon-resolved sources ...

Waxman, Bahcall (1999)

derive generic limits from limits on extragalactic p‘s -ray flux

... for discovering extraterrestrial neutrinos

TeV PeV EeV

E-2 flux

50 events/year/km2

Page 31: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

Page 32: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

MeV GeV Tev PeV EeV

Different energy range for detectors

Underground

Optical Cherenkov

deep in water and ice

Radio, acoustic,

air showers

Page 33: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

Neutrino interactions in ice and water

The muon can travel several km in e.g. ice

< 1 degree

eV

e

e

Hadronic shower length

logE (10th of metres)

CCCharge Current

NCNeutral Current

Page 34: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

275 GeV muon neutrino interaction in BEBC

1 m

Page 35: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

Muon range in ice

Muon propagator: MMC , Chirkin, D. 27th ICRC, HE 220, Hamburg 2001

The muon starts to loose energy above 500 GeV to pair production, bremstrahlung

The muon will be dressed up by many e+ and e-.

More Cherenkov light!

Page 36: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

e

low energy)“Cascades”

Length of cascades 10th of meters (L prop. logE)

Neutrino interactions in ice and water

CCCharge Current

Page 37: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

e

high energy)“Cascades”

Length of cascades 10th of meters (L prop. logE)

Neutrino interactions in ice and water

CCCharge Current

Page 38: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

Neutrino cross-section

σ tot (νN) = 7.84 ×10−36cm2 Eν

1GeV

⎝ ⎜

⎠ ⎟0.363

For E< 104 GeV the x-section rises linearly with the energy

For E> 104 GeV (due to the W-boson propagator:

Cross-section measured up to 300 GeV. Up to about 10 TeV based on structure functions from HERA. Above different extrapolations.

Page 39: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

Cross-section larger in e.g. -BH models

Standard Model

Strings

σ (m

b)

Micro black holes

Page 40: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

Shadowing effect of the Earth

Page 41: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

PeV acceptance around horizon

EeV acceptance above horizon

Shadowing effect of the Earth

Page 42: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

AMANDA-B10 efficiency for UHE neutrinos

upup

E-2 neutrino flux 2.5 1015eV -> 5.6 1018eV

Page 43: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

But for neutrinos the earth is transparent…

The tau neutrino will degrade in energy due to interactions in the Earth but will continue through.

Page 44: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

The y-distributions

0 y 1.0 0 y 1.0

N N

(1-y)2

υq,υ q υ q,υq

Muon energy is harder in antineutrino interactions!

hadrons

muon

y = (Ehad - MN)/E

Page 45: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

y = Ehadrons /E

lepton = (1-y)E

Page 46: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

Z-bursts

• From Big Bang there should be about 330 neutrinos/cm3 with an average energy of 0.0004 eV

• The ultimate neutrino experiment to detect these….

CNB-> Z0-> decays

This process has been proposed to explain the UHECR events.

But you need a neutrino with 1024 eV energy..

Page 47: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

up/down energy direction time

Atmospheric X

Diffuse neutrinos X X

Point sources; AGN, X X X

WIMPS

GRB X X X X

Reconstruction handles

X

XX

X

X X

X X X X

Page 48: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

Optical Cherenkov detection

Page 49: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

Detection principleO(km) long muon tracks

direction determination by Cherenkov light timing

15 m

O(10m) Cascades, e Neutral Current

Page 50: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

Spåtind Norway P.O.Hulth

2006-01-07neutrino

muon

Cherenkov

light cone

Detectorinteraction

•The muon radiates blue light in its wake

•Optical sensors capture (and map) the light

Page 51: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

Neutrino interaction in AMANDA QuickTime™ and a

GIF decompressorare needed to see this picture.

Page 52: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

Acoustic Detection

Page 53: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

d

R

Particle cascade ionization heat pressure wave

P

t

50s

Attenuation length of sea water at 15-30 kHz: a few km(light: a few tens of meters)

→ given a large initial signal, huge detection volumes can be achieved.

Threshold > 10 PeV

Maximum of emission at ~ 20 kHz

C. Spiering

Page 54: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

Radio Detection

Page 55: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

e + n p + e-

e- ... cascade

relativist. pancake ~ 1cm thick, ~10cm

each particle emits Cherenkov radiation

C signal is resultant of overlapping Cherenkov cones

for >> 10 cm (radio) coherence

C-signal ~ E2

nsec

negative charge is sweeped into developing shower, which acquiresa negative net chargeQnet ~ 0.25 Ecascade (GeV).

Threshold > 10 PeVC. Spiering

Page 56: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

The Future

• We should be optimistic !

• New York Times, December 29, 1932

Robert A. Millikan

From S. Westerhoff, Lepton Photon 2005

Page 57: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

• Since we are in Norway.

• And that the point of gravity for High Energy Neutrino telescopes is at the South Pole which I will talk about tomorrow morning…

• A short historical comment.

Page 58: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

Sydpolsfarare då och nu

Övervintra vid kusten

Page 59: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

Sydpolsfarare då och nu

Tre timmars flyg från kusten

Page 60: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

Sydpolen december 1911

Page 61: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

Sydpolen januari 1912

Page 62: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

Sydpolen november 2003

Page 63: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

Page 64: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

Page 65: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth

Page 66: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth Joakim Edsjö SU

Page 67: 2006-01-07Spåtind Norway P.O.Hulth Cosmic Neutrinos and High Energy Neutrino Telescopes Spåtind 2006 lecture 1 Per Olof Hulth Stockholm University Hulth@physto.se.

2006-01-07 Spåtind Norway P.O.Hulth