The ANTARES deep-sea neutrino telescope TeVPA 2010 JP Ernenwein, - - PowerPoint PPT Presentation

TeVPA 2010 Paris 20/07/2010

JP Ernenwein, for the ANTARES collaboration Univ Aix-Marseille CPPM

The ANTARES deep-sea neutrino telescope

Neutrino

µ

ν

MeV GeV TeV PeV EeV Astrophysical neutrinos Dark Matter Oscillations Supernovae GZK, topological defects Fast decrease

• f

fluxes E-2, E-3 short muon path weak light

40K

Principle & Physics

Active Galactic Nuclei Gamma Ray Bursts Dark Matter Microquasar

1 a.l. 1 a.l.

SNR Pulsars

Magnetic Monopoles

Exotic physics

Nuclearites

M 87, HST

SNR RX J1713.7-3946

Aharonian et al, A.A. 449 (2006) 223-242

Potential sources of neutrinos

2475m, 3 PMT/floor 12 lines of 25 floors 885 PMTs

floor

350 m 70 m 14.5 m

100 m

ANTARES

Junction box

Cable to shore station (Toulon, France) ~40 km

JUNCTION box

Connection

• f a line

Optical Module 10” PMT

floor

Mar: MILOM

2005 2006 2007 2008

Mar: L1 Sep: L2 Jan : L3-5 MILOM recovery Dec: L6-10 IL07 Jun: L11,12

L11 L9 L10 L12 L7 L8 L6 L4 L2 L3 L5 L1 IL07 sismomètre

100 m N

Boîte de jonction Câble sous marin (vers la côte)

Connection of lines

µ

42°

γ č

Cherenkov light (µ)

3D matrix

Measurements time (O(ns)), amplitude (30%) & hit position(O(10 cm))

Muon track or shower measurement

νµ

Detection principle

νe

Charged current interaction (W) shower

track:

good energy resolution (O(30%)), poor angular resolution (O(10°))

Good angular resolution (~0.3 degrees @ E>10 TeV), Poor energy resolution (factor 2-3)

1 photo-electron

Dynamic range : 20pe/40ns

threshold ~1/3 pe required sensitivity: photo-electron

2475 m 1 2 3 4 5 6 7 8 9 10

p ν µ ν µ µ p, α γ

sea atmosphere Up going background (muons from neutrinos) Cosmic neutrinos Down going background events (atm muons and muons from neutrinos)

10-7

cos θµ

Atm muons Muons from atm neutrinos

106

dΦ/dΩ cm-2 s-1 sr-1 10-9 10-11 10-13 10-15 10-17

Profondeur 2400 m E > 1 TeV

Signal & background

µ

Atmospheric muons & neutrinos

Neutrino Candidate (up-going muon) Time (ns) Z hit PMT (m)

bullet= hit triggering the event Square= hit in the fit

χ2 method (no alignment)

Muon bundle (down-going event) Time (ns) Z hit PMT (m)

bullet= hit triggering the event Square= hit in the fit

χ2 method (no alignment)

Elevation(°)

5-line data (May-Dec. 2007) + 9-12 line data (2008)= 341 days detector live time

DATA Upgoing: 1062 neutrino candidates: 3.1 ν candidates/day Monte Carlo: atmospheric neutrinos: 916 (30% syst. error) Wrong reco atmospheric µ : 40 (50% syst. error)

Scrambled ANTARES Sky map of 1000 ν

Galactic Coordinates

Muon depth-intensity relation

Equivalent depth

µ µ

Electromagnetic showers induced by atmospheric muons

Time (ns) Z hit PMT (m) Muon(s) down-going event

Electromagnetic showers induced by atmospheric muons

Time (ns) Z hit PMT (m) Muon(s) down-going event

Electromagnetic showers induced by atmospheric muons

Preliminary

Sensitive to primary

Ongoing combined searches

• Receive GRB alerts from Satellites

search for coincident neutrinos within time window (~100 s)

• Send neutrino cluster alert for optical follow-up

Trigger: multiple or ”HE single” neutrino event; Reconstruction “on-line” (<10ms). Alert message to T arot T elescope in La Silla and to the ROTSE system (4 telescopes)

• Correlation with AUGER source distribution

investigate directional correlation of neutrinos and UHE particles

• Correlation with VIRGO-LIGO signals

investigate correlation of neutrinos and gravitational waves

Point source search

DATA on 5 lines (2007) 140 days equivalent

χ2

Events Events Events Track quality ~ Track energy Number

• f hits

Zenith distribution

Event reconstruction and selection

Selected neutrino Candidate (up-going muon)

Declination distribution

Selected events

Sky map Blue: selected sources from catalog Point spread function

• f the reconstruction

used in this analysis (χ2) No significant excess neither in all-sky No significant excess neither in all-sky search nor in selected source directions. search nor in selected source directions. limit Galactic coordinates

See next talk (JDD Zornoza)

Diffuse flux

• f

muon neutrinos

DATA on 9-10-12 lines (Dec. 2007, 2008, 2009) 334 days equivalent

Energy estimator

µ direct photons + µ scattered photons + light from EM showers

Cut

• ptimized

by MRF method

• n MC

Energy estimator= Repetition (R) of integration gate on the same Optical Module

Diffuse νµ flux – Upper limits (E-2)

E2Φ(E)90%= 4.8×10-8 GeV cm-2 s-1 sr-1 20 T eV<E<2.5 PeV

334 days

9 observed events for 10.5±2 expected background

Magnetic Monopole search

DATA on 9-10-12 lines (Dec.2007-2008) 116 days equivalent

Reconstruction:

Same as for muon studies but velocity β is a free parameter. Reconstruction of trajectory + velocity. Selection of high energy up-going events: Above Cherenkov threshold: large amount of light (~8500 more photons than for a muon) Below Cherenkov threshold: Delta rays (from β~0.55)

Reconstructed β

DATA/MC comparison before unblinding (small sample)

g from d-rays g from MM g from m Cherenkov γ from delta-rays. x 8 5 Cherenkov γ from a µ . Direct Cherenkov γ from a MM with g=gD.

Time (ns) Z hit PMT (m) Simulated MM (beta=0.7)

Expected sensitivity for 116 days (90% C.L.)

Preliminary unblinding in progress

Dark Matter search

χχ ν µ

• Atm. ν bkg
• Atm. µ bkg

misreconstucted (10% of ν)

3° half aperture cone Background: ~7 events/3 yrs

3 years, 12 lines

mSugra parameters

Summary, outlook

• Antares is taking data since 2007 in its different

configurations (5, 9, 10, 12 lines)

• The detector and its environment are now well

understood: good agreement DATA/MC

• First physics results are now available after unblinding:

Point sources for the 5-line stage, Diffuse Fluxes

• For other topics the unblinding is in progress

(Magnetic Monopoles) or the studies are on-going (Point sources with more than 5 lines, showers)