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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!!!