Large Magellanic Cloud, 1987 (51.4 kparsec) SN 1987a after before 2006 Hubble

Large Magellanic Cloud, 1987 (51.4 kparsec)

SN 1987a

after before

2006Hubble

Precursor of Superkamiokande

H2O

8 more events in IMB

Crab, 1054

About 1 SN every 30 years in our galaxy

Einstein satellite (X)

Where does the acceleration take place?

Cosmic rays

Look for the neutrals, not deflected in B fields, to identify, the sites of acceleration

HE gamma and neutrino astronomy

: created by synchrotronstrahlung, decay

from decay:

or very high energy charged particles

Candidates: Fermi (SN remnants…)

AGN, pulsars, …

0

K,

From a presentation by: Paul Mantsch Auger Project Manger

Building the Pierre Auger Observatory (Argentina)

Adventures in Cosmic Ray Physics

The Design

The Observatory Plan

Surface Array 1600 detector stations 1.5 km spacing 3000 km2

Fluorescence Detectors 4 Telescope enclosures 6 Telescopes per

enclosure 24 Telescopes total

The Surface Array Detector Station

Communications antenna

Electronics enclosure

3 – nine inchphotomultipliertubes

Solar panels

Plastic tank with 12 tons of water

Battery box

GPS antenna

EGRET on Compton Gamma Ray Observatory (NASA)

ee

Galactic view

Active Galactic Nucleus (AGN)

Matter accreting on supermassive black hole at center of galaxy

Gamma ray burst (GRB)

must be « small » size sources

Microquasar: binary systems with a black hole

Ground based: look for electromagnetic shower induced in the upper atmosphere, measure Cerenkov light E>10 GeV

HESS in Namibia

(others: MAGIC in Mallorca,

future (CTA))

shower hadron shower

HESS, stereoscopic view

Look for upward going muons

Neutrino astronomy principles

Antares

Mediterranean, off Toulon, 3000 m deep, 0.1 km2

42:1n

1cos35.1nm60

Cerenkov light

t

height

Downward going muon

Antares, 0.1 km2 at the bottom of the Mediterreanean (3000 m deep),

Starting to take data

But: needs 1 km3!!!