1. Italy
Pizza, Mozzarella di Buffala
Switzerland
Roesti, Cheese Fondue
Netherland
Stampot, Croquetten
Spain
Paella, Jamon

2. Italy
Capri, Vesuvio, Pompei
Switzerland
Matterhorn
Netherland
Reichshaus, Grachten
Spain
Fallas,

3. Italy
Calcio and Physics
Switzerland
Fussball and Physics
Netherland
Voetbal and Physics
Spain
Futbol and Physics

4. Italy
OPERA
Switzerland
HERA
Netherland
ANTARES
Spain

5. OPERA
Momentum measurement based on detection of multiple Coulomb scattering
Emulsion Cloud Chamber: sandwiches of lead plates and nuclear emulsion sheets

6. HERA
Member of H1 collaboration

7. Heavy Quarks Charm and beauty production in Neutral Current
Motivation: experimental test of Standard Model and perturbativ QCD

8. Lifetime
Distinguish heavy quarks from light quarks using variables sensitive to longer livetime

11. HERA:H1 Charm production in Charged Current
Measurements of strange distribution

13. Neutrino Astrononomy Photons: Interact with CMB
Protons: Deflect by magnetic fields (E<1019 eV
Interact with CMB (E>1019 eV => <50 Mpc)
Neutrinos: Unambiguous probe of hadronic processes
Not deflected by magnetic fields -> point back to the source of emission
Not absorbed by dust
Horizon not limited by interaction with CMB
Detectable over full energy range (GeV-PeV)

14. Sky Observable by Neutrino Telescope
AMANDA/IceCube
(South Pole)
ANTARES/KM3
(North Hemispher)

15. Scientific scope Origin of cosmic rays
Hadronic vs. leptonic signatures
Limitation at low energies:
Detector density
Low light yield
Limitation at high energies:
Detector size
Fast decreasing fluxes
Supernova Oscillations Dark matter Astrophysical
neutrinos
~MeV GeV GeV-TeV TeV-EeV > EeV

17. How to measure neutrinos?
Detection lines
with PMTs
Cherenkov light
from muon
Cheap high quality sea water
Sea floor
Muon
Weak interaction
Time and position from PMTs
=> muon trajectory
Neutrino

18. What does ANTARES measure?
107 atmospheric
muons per year
103 atmospheric
neutrinos per year
Detector
Earth shielding rejects
atmospheric muons
upward going muon = neutrino-induced
event
??? exotic
neutrino per year
1019
??? cosmic
neutrino per year

19. How to measure neutrinos?
Detection lines
with PMTs
Cherenkov light
from muon
Cheap high quality sea water
Sea floor
Muon
Weak interaction
Time and position from PMTs
=> muon trajectory
Neutrino

20. What is ANTARES? In the Mediterranean Sea 2.1 km
Installed off French coast
2.5 km under water
12 Lines (885 PMTs)
Completed in May 2008
Data taking started soon
after installation of the
first line in 2006
2.1 km
2.5 km

23. Results and ongoing analysis
Astroparticle Physics:
Diffuse flux
Point sources
Neutrino oscillation
Searches:
Dark matter
Multi messenger astronomy
Magnetic monopoles/Nuclearites
Particle physics:
Atmospheric muon flux
Cosmic rays anisotropy/composition
Electromagnetic showers
Detector related:
Timing/positioning
Water absorption length/refractive index
Acoustic /

24. Muon energy loss Below 1 TeV: Continuous energy loss Above 1 TeV:
Discrete energy loss
Large energy fluctuation
=>Electromagnetic showers

25. Phenomenology Cerenkov photons emitted:
1. Continuously along muon path
2. At Cerenkov angle
3. Arrive earlier than shower photons
Shower photons emitted:
1. From one point
2. Almost isotropically
3. Arrive later than Cerenkov photons

26. Identification Method
Simple Idea:
1. Reconstruct
muon trajectory
2. Project photons
onto
muon track
3. Peak signals
shower position

27. Photon emission position along MC muon track
All reconstructed detected photons
along the projected muon track
Peaks selected by the algorithm
Position of generated showers
along the muon track

28. Algorithm Take muon direction Calculate photon emission (weight=1)
Search shower candidate
Eliminate background
Fit 3-dimensional position
Muons with shower multiplicity

29. Down going muon with two showers
Result of muon recontruction
Result of the 3D shower reconstruction
Detected photon
Peak=Shower position on muon track

30. Muon event rate as function of shower multiplicity
MC shows:
Shower energy TeV
Muon energy with shower 3.7TeV
Position resolution m
Shower Efficiency %
Shower Purity %
Systematic errors from MC
No reconstruction efficiency
included

31. An application:

32. Cosmic Ray energies in Antares
Primary energies measured by Antares between
10^13 eV and 10^16 eV (knee region included)
Does the composition change at the knee region?

33. Pure proton primaries or pure iron primaries versus data
No way to explain data with only proton or iron primaries

34. Fit MC templates from two different mass groups to data
How much light nuclei (proton) and heavy nuclei (iron) do we need to reproduce data distribution?
MC proton distribution = f_p(x)
MC iron distribution = f_Fe(x)
Data distribution = f(x)
Fit data with this two MC templates (chi²-fit)
f(x) = a * f_p(x) + b * f_Fe(x)
Fit parameter: a, b

35. Light nuclei primaries or heavy nuclei primaries versus data
Exclusive light nuclei primaries describe better
the data than exclusive heavy nuclei primaries

36. Fit light and heavy nuclei to data
High shower multiplicity dominated by heavy nuclei
Low shower multiplicity domination by light nuclei
Fit says data contains 91% light and 9% heavy nuclei

37. Conclusion Feasibility
Goal: Distinguish light and heavy primary ray composition in different energy ranges
Need: more statistics, energy estimator, independent variable (SRF,...)
Composition measurements are hadronic interaction model dependent. How stable is the shower multiplicity method under different hadronic interaction models? (Chiariusi & Margiotta in Erlangen)

38. Backup sildes

39. OPERA Method

40. HERA

41. CC polarised cross sections
No right handed CC