ANTARES Neutrino Telescope Recents results Neutrino Telescope Recents results 1. ... Junction Box Main Electro-optic Cable ... simulation package for different WIMP masses

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  • Pascal GayLPC Clermont

    Universit Blaise Pascal IN2P3-CNRS

    ANTARES Neutrino TelescopeRecents results

    1

  • P. Gay LIO12 LyonANTARES Results

    Introduction

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    1 ANTARES telescope 2 Relativistic magnetic monopoles!3 Neutrino oscillations!4 Dark matter 5 Outlook

  • P. Gay LIO12 LyonANTARES Results

    Multi messager astronomy

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    Why neutrino astronomyneutrinos point back to the sourceneutrinos travel cosmological distancesneutrinos escape optically thick sourcesneutrinos are a clear sign of hadron acceleration complementary to gamma and cosmic rays

    Some source candidates Galactic sources: supernova remnants, microquasars Extra-galactic sources: active galactic nuclei, gamma ray bursts Dark matter

  • P. Gay LIO12 LyonANTARES Results

    Neutrino telescope : detection principle

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    interaction

    43Sea floor

    Cherenkov light from

    3D PMTarray

    Reconstruction of trajectory (~ ) from timing and position PMT hits

  • P. Gay LIO12 LyonANTARES Results

    Background rates

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  • P. Gay LIO12 LyonANTARES Results

    Neutrino telescopes

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    galactic centre: 2/3 of the timeGalactic centre: not seennot

    observed

    notobserved

    Angular resolution(Ice: ~2/0.6)

    Angular resolution(water: ~0.2/0.1)

  • P. Gay LIO12 LyonANTARES Results 7

    ANTARES Detector

    14.5 m

    ~60-75 m

    350 m

    100 m

    JunctionBox

    Main Electro-optic Cable (~40

    km)

    Storey

    12 lines 25 storeys / line 3 PMs / storey 885 PMs

    Depth : 2500m

    Submarinelinks

    Buoy

  • P. Gay LIO12 LyonANTARES Results

    Some analysis topics

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    Environmental and marine scienceseismologymarine biologyin situ oxygen comsumption

    Cosmic neutrinosSteady sources

    full sky search candidate list

    Transient sources multi-messenger flare analysis (GRBs,

    microquasars, etc.) triggered search, optical

    follow-up gravitational waves

    Diffuse flux

    90%CL upper limits for neutrinos flux with an E-2

    spectrum for 51 candidates sources (blue points), sensitivity in blue

    Search for Point Sources

    Particle physics and exotic phenomenasuper-heavy particlesneutrino oscillationsindirect search of dark matter

    Preliminary

    Astro. J. Lett., 743:L14

    http://stacks.iop.org/2041-8205/743/L14http://stacks.iop.org/2041-8205/743/L14http://stacks.iop.org/2041-8205/743/L14http://stacks.iop.org/2041-8205/743/L14

  • P. Gay LIO12 LyonANTARES Results

    Relativistic Magnetic Monopoles

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    knock off electrons (rays) produced along its path

    gMM = k e2

    0.5 < < 0.75

    Magnetic monopolesrequired in many models via SSB [t Hooft, Polyakov]

    light yield > th = 0.75Cerenkov regime

    via -rays

  • P. Gay LIO12 LyonANTARES Results

    Relativistic Magnetic Monopoles

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    standard track reconstruction =1

    [0.825, 0.875]

    /~0.012

    [0.625, 0.675]

    Reconstruction algorithm developped for magnetic monopole, also below Cerenkov threshold, free parameter

  • = log[Q=1Q=free

    ]

    < th

    P. Gay LIO12 LyonANTARES Results

    Relativistic Magnetic Monopoles

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    Discriminante variables cut on numbers of hits cut on the ratio of reconstruction qualities

    15% of data used here

    >0 expected for monopole events

    [0.775, 0.825]

  • P. Gay LIO12 LyonANTARES Results

    Relativistic Magnetic Monopoles

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    cuts backg observed

    2007-2008 116 days

  • P. Gay LIO12 LyonANTARES Results

    Relativistic Magnetic Monopoles

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    Astroparticle Physics 35 (2012) 634640 [arXiv:1110.2656]

    Limits

    http://www.sciencedirect.com/science/article/pii/S0927650512000461http://www.sciencedirect.com/science/article/pii/S0927650512000461http://arxiv.org/abs/1110.2656http://arxiv.org/abs/1110.2656

  • E/ cos

    P(

    )

    P. Gay LIO12 LyonANTARES Results

    Neutrino oscillations

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    oscillations w/ atmospheric neutrinos

    Larger effect on single-line events (low energy)than multi-line events (higher energy)

    P ( ) = 1 sin2 232 sin2(16200m232 cos

    E)

    (muon range~120m)

    25 GeV

    25

  • P. Gay LIO12 LyonANTARES Results

    Neutrino oscillations

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    Special low energy fit for single-line events (>7storeys, do not fit azimuth)

    zenith angle resolution

    Multi-line Single-line

    track selection

    Select pure sample of atmospheric neutrinos (

  • P. Gay LIO12 LyonANTARES Results

    Neutrino oscillations

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    MC truth

    Analysis, low energynot easy! E > 50 GeV : multi-lines (65 m between lines)

    E 20 GeV : single-line

    Solid line : no oscill.dashed line : w/ oscill.

    blue : multi-line events

    Red: single-line events

  • E/ cos

    S = (zmax zmin)/ cosR

    P. Gay LIO12 LyonANTARES Results

    Neutrino oscillations

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    Energy estimator using approximate range Observable

    E! 0.45

    ER = 0.2(zmax zmin)/ cosRionisation energy loss 0.2GeV/m for @ mip in sea water

  • P. Gay LIO12 LyonANTARES Results

    Neutrino oscillations

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    Systematics:

    ER/ cosRTest the distribution of Absolute normalisation free(absorbs dominant uncertainties)

    2008-2010 data (863 days):

    (Absolute normalisation free)Absorption length: 10%Detector efficiency: 10%Spectral index of flux: 0.03

    No oscillation: 2/NDF = 40/24 (2.1%)Best fit: 2/NDF = 17.1/21 m2 = 3.1 10-3 eV2 sin22 =1.00

    best fit osc best fit osc

    no osc no osc

    Red: best fit w/ oscill. blue : atm.neutrinos w/o oscill. + atm. muons

  • P. Gay LIO12 LyonANTARES Results

    Neutrino oscillations

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    ANTARES K2K Super-K MINOS

    Assuming maximal mixing: m2=(3.10.9) 10-3 eV2

    Phys. Lett. B 714 (2012) 224 [arXiv:1206.0645v2]

    best fit point

    68% (90%) Confidence level contour

    90%CL

    68%CL

    http://www.sciencedirect.com/science/article/pii/S037026931200740Xhttp://www.sciencedirect.com/science/article/pii/S037026931200740Xhttp://arxiv.org/abs/1206.0645v2http://arxiv.org/abs/1206.0645v2

  • P. Gay LIO12 LyonANTARES Results 20

    Search for Dark Matter in the Sun

    The products of such annihilations would yield high energy neutrinos, which can be detected by neutrino telescopes

    In the Sun a signal would be very clean (compared with gammas from the Galactic Centre, for instance)

    WIMPs (neutralinos, Kuluza Klein particles) are among the most popular explanations for Dark Matter

    They would accumulate in massive objects like the Sun, the Galactic Center, dwarf galaxies

  • Integrated neutrino flux for E > 10 GeV

    Local : 0.3 GeV/cm3

    = 220 km/s

    Bulk

    Higgs funnel

    focus points

    P. Gay LIO12 LyonANTARES Results

    Neutralino annihilations in the Sun in CMSSMStudy of neutralino DM sensitivity within SUSY CMSSM framework

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    0 < m1/2 < 2000 GeV 0 < m0 < 8000 GeV 0 < tan < 60 -3 m0 < A0 < 3 m0

    Random scan within CMSSM parameter space

    DarkSUSY & ISASUGRA (RGE code) w/ mtop = 172.5 GeV/c2 Including oscillation effects in the Sun and in vacuum

    W

    W Z

    Z

    A

    f

    f

    Z

    f

    f

    f

    f

    Bulk low m0 and m1/2V. Bertin E. Nazri J. Orloff

  • P. Gay LIO12 LyonANTARES Results

    Neutralino annihilations in the Sun in CMSSM

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    Bulk

    Higgs funnel

    focus points

    Higgs funnel

  • P. Gay LIO12 LyonANTARES Results

    Sensitivity calculated for 3 years of data taking

    Detection rate with ANTARES in 3 years

    Neutralino annihilations in the Sun in CMSSM

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    Model with relic density within 2 of WMAP constraint are highlighted (0.094 < h2 < 0.129)

    Background from atmospheric neutrinos and misreconstructed atmospheric muons within 3 radius search cone around the Sun

  • P. Gay LIO12 LyonANTARES Results

    Exclusion capabilities of ANTARES for the CMSSM parameter space :mainly Focus Point region (good complementarity to direct search at LHC)

    Search for neutralino annihilations in the Sun

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    Excludable in 3 years at 90% CL: all some none (A0 varied between -3m0 and +3m0 and tan() within indicated slice)

    some

    h2>1

    No EWSB

    excluded by accelerator (LEP)

    LSP

  • P. Gay LIO12 LyonANTARES Results

    neutrino signal from WIMP annihilation

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    The WIMPSIM package (Blennow, Edsj, Ohlsson, 03/2008) is used to generate events in the Sun in a model-independent way

    Great statistics: with 3106 WIMPs annihilations Capture rate and annihilations in equilibrium at the Sun core Annihilations in c,b and t quarks, leptons and direct channels Interactions taken into account in the Sun medium Three flavors oscillations, regeneration of leptons in the Sun

    medium (Bahcall et al.)

    Available parameters: WIMPs mass, oscillations parameters...

    Signal energy spectrum derived from WIMPSIM simulation package for different WIMP masses

  • hard annihilation : -> W+W-

    : neutrino : anti-neutrino

    M = 1 TeV

    soft annihilation : -> bb

    M = 1 TeVM = 1 TeV

    P. Gay LIO12 LyonANTARES Results

    Neutrino spectra from neutralino annihilations

    hard annihilation : -> W+W-

    M = 100 GeV

    soft annihilation : -> bb

    solid : including