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Neutrino astronomy with Antares Aart Heijboer. Research to fundamental building blocks of matter Research on the Universe using those particles.

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Presentation on theme: "Neutrino astronomy with Antares Aart Heijboer. Research to fundamental building blocks of matter Research on the Universe using those particles."— Presentation transcript:

1 Neutrino astronomy with Antares Aart Heijboer

2 Research to fundamental building blocks of matter Research on the Universe using those particles

3 muon discovered in 'cosmic radiation' Particles from space

4 protons same particles that the LHC accelerates The universe contains particle accelerators times more powerful than the LHC we don't know what they are E LHC = 7000 GeV 10 bilion GeV

5 protons are deflected by magnetic fields in the universe M87: galaxy with supermassive black hole at the center, emitting a relativistic jet of particles.

6 protons are deflected by magnatic fields in the universe ns1006a: remnant of a supernova

7 protons are deflected by magnetic fields in the universe ns1006a: remnant of a supernova photon

8 protons are deflected by magnetic fields in the universe High energy photons can be seen from galactic objects GeV energies (~LHC) Not sure they have to do with the protons Absorbed over larger distances ns1006a: remnant of a supernova photon Hess telescope Namibia

9 New messenger particle: The Neutrino 'Neutrinos are the closest thing to nothing you can study' - Italian for 'little neutral thingy' - no size - no electric charge - no mass (almost) - no interaction with matter (almost / weak) … but rising with the energy of the neutrino don't notice anything ← very small chance of an interaction

10 protons are deflected by magnetic fields in the universe photon high energy neutrinos: travel in straight lines → point to their source are tell-tale signs of proton acceleration are not absorbed on their way here but: very hard to detect; most of them fly right trough the Earth.

11 Uppsala 2000Ivo van Vulpen11 neutrino muon High energy neutrinos interaction probability proportional to E n muon goes 5 km for E = 10 TeV Cherenkov radiation (35000 photons/metre) → huge volume with sparse detector deep -> shielding from down-going particles clear water → good pointing accuracy (< 0.5 o )

12 Uppsala 2000Ivo van Vulpen12 Junction box ~60-75 m Buoy 350 m 100 m total volume ~ 200 x 200 x 300 meter 3

13 Bucarest 40 km to detector shore station 7 countries 29 institutes ~150 scientists+ engineers

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20 since May 2008: All cables plugged in... What do we see?

21 Neutrinos!

22 (atmospheric)

23 Searching for cosmic sources. scrambled 2007 & 2008 data

24 Searching for cosmic sources. scrambled 2007 & 2008 data Neutrino's from same spot in the sky... A cosmic source or a random fluke?

25 The next step. KM3NeT - plan for an even bigger Detector - at least 1 km 3 - Project in 'Preperatory phase' - Lots of discussions on design/site location - Nikhef thinking hard about design... - hopefully start building in few years.

26 Close connections between particle physics and study of The universe Antares is one example: looking for cosmic particle accelerators with neutrinos First neutrinos have been seen: the search for cosmic sources is on. Summary


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