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

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Presentation transcript:

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

Precursor of Superkamiokande H2OH2O

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, …

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 km 2 Fluorescence Detectors 4 Telescope enclosures 6 Telescopes per enclosure 24 Telescopes total

The Surface Array Detector Station Communications antenna Electronics enclosure 3 – nine inch photomultiplier tubes Solar panels Plastic tank with 12 tons of water Battery box GPS antenna

EGRET on Compton Gamma Ray Observatory (NASA) 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 km 2 Cerenkov light

t height Downward going muon

Antares, 0.1 km 2 at the bottom of the Mediterreanean (3000 m deep), Starting to take data But: needs 1 km 3 !!!