SELECTED RESULTS OF THE ANTARES TELESCOPE AND PERSPECTIVES FOR KM3NET. D. Dornic (CPPM) on behalf the ANTARES Coll.

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1 SELECTED RESULTS OF THE ANTARES TELESCOPE AND PERSPECTIVES FOR KM3NET D. Dornic (CPPM) on behalf the ANTARES Coll. MORIOND La Thuile, March 2017

2 Neutrino telescopes: science scope Low$Energy$$ MeV$<$E ν $<$100$GeV$ ν$oscilla?ons$ ν$mass$hierarchy$ Supernova$$ Medium$Energy$$ 10$GeV$<$E ν $<$1$TeV$ Dark$maEer$search$ Monopoles,$nuclearites, $ High$Energy$$ E ν $>$1$TeV$ ν $from$extrakterrestrial$ sources$ Origin$and$produc?on$ mechanism$of$he$cr$ ANTARES$ +$oceanography,$biology,$seismology, $$ 2 3$

3 Multi-messenger paradigm Neutrinos: smoking gun for cosmic-ray interactions! GeV: atmospheric neutrinos, dark matter! 100 GeV - 30 TeV: various galactic (TeV gamma) sources! 30 TeV 3 PeV: IceCube signal (astrophysical flux) ORCA ANTARES ARCA 3

4 Neutrino fluxes: from MeV-PeV 4

5 ANTARES 5

6 ANTARES in numbers ANTARES in numbers: 12-line data taking since 2008 o(11000) detected neutrinos Angular resolution: (median) Effective area: 1m 30 TeV Visibility: ¾ of the sky, most of the galactic plane Real-time data processing Mkn 501 SS433 RX J Galactic Centre GX339-4 CRAB VELA 6

7 Neutrino event topologies Tracks: Angular resol: ~0.3 o Energy resol: factor 3 Large detection volume => Ideal for astronomy => but large atm bkg Cascades: Angular resol: ~3 o Energy resol: 5-10% Contained event => Almost no atm bkg Not to scale 7

8 ANTARES => KM3NeT 3 Building Blocks on 2 sites: 3*115 lines, ~6210 OMs, ~45200 PMTs 12 lines, 885 OMs 8

9 DOM KM3NeT technologies String LOM 31 x 3 PMTs Transmission Gbit/s on optical fibre Synchro with Hybrid White Rabbit Calib LED flasher & acoustic piezo Position Tiltmeter/compass Uniform angular coverage Directional information Digital photon counting Wide angle of view Background rejection All data to shore ~ 700#or#200##m# 9 2 Dyneema ropes VEOC: Oil filled PVC tube Low drag Low cost Rapid / safe deployment Multiple strings / campaign Auto/ROV unfurling Re-useable

10 ORCA detector:! 115 lines! 20 m horizontal spacing! 9 m vertical DOM spacing! 18 DOMs / string! ~6 Mt instrumented volume KM3NeT ORCA Located closed to ANTARES at a depth of ~2475m Shore station La Seyne sur Mer Infrastructure already deployed 2 new ORCA lines will be deployed before summer 10

11 KM3NeT ARCA ARCA detector! ARCA: 2 blocks! 115 strings per block! 90m horizontal spacing! 36m spacing! 18 optical modules ~1 km 11! Total volume: 1.2 km3! Site: 3.5 km depth! Shore station: Capo Passero (Sicily) 2 ARCA strings working for more than a year

12 1st string KM3NeT 12

13 Performances KM3NeT ARCA Tracks: Direction: Gal. sources: 0.2 o at 10TeV Extra-gal. sources: 0.1 o at 100TeV Energy: 0.27 in Log10(E) Cascades: Vertex: 6-8m (long), 0.5m (perp) Direction: ~1.5 o Energy: 5% 13

14 Method: looking for a cosmic signal ANTARES: experiment dominated by the backgrounds: atm muon: 10/s, atm neutrino: 4-5/day, cosmic neutrino: 1-2/year (?) => Atm muons: quite "easy" to remove (zenith +quality cuts) => Atm neutrinos: irreducible isotropic background, low energy Point-like neutrino sources => looking for cluster in direction Diffuse neutrino flux => looking for excess at HE 14

15 IceCube signal 4 year HESE analysis (ICRC 2015) 15 track+39 shower Hemipshere North and South Eth: 60 TeV 6 year upgoing muon Eth: 100 TeV Eevent >5 PeV! Significance: 6.5 sigma Spectra: E Significance: 5.9 sigma Spectra: E Indication of a break in spectrum? (energy threshold different) Indication of galactic and extra-galactic components? (different hemispheres) 15

16 Diffuse neutrino flux Track events Cascade events Preliminary All-sky / All-flavor neutrino search Look for excess above a given Eth 9 (7) yrs of data for tracks (cascades) Bkg expectation Signal exceptation => Small excess (not significant) Track+Cascade U.L. Nb events measured Track 13+/ Shower 5+/ Preliminary 16

17 Diffuse neutrino KM3NeT Track channel: Analysis for up-going events based on maximum likelihood Pre-cuts on θzen >80 o, reconstruction quality parameter and Nhit (proxy for muon energy) Cascade channel: Containment cut on reconstructed vertex to remove atm. muons (excludes upper 100m layer) Full sky analysis based on BDT and maximum likelihood. Final ANTARES sensitivity ~ IC flux Event in 5yrs 17

18 Reduced search window: enhanced flux 18

19 Reduced search window: Fermi Bubbles Fermi Bubbles: (1765 days) track only 3 OFF-zone regions (sideral time shift) Off-zone: Av. exp. bkg : 19.7 Observed in the ON-region : 28 => Excess reduced to 1.5 σ Similar expected sensitivity with cascades 19

20 Reduced search window: Galactic plane Testing KRAγ model (Astropart. Phys. 55 (2014) 37-50) Phenomenological model of Cosmic Ray diffusion in the Galaxy Radial dependence of the slope of the diffusion coefficient and the advective wind => This models predicts the ν energy and spatial distribution on the sky 9 years of ANTARES Data ( ) all flavor (7300 tracks+208 cascades) Likelihood analysis 20

21 Reduced search window: Galactic plane Results: Sensitivity: median U.L. (90% CL) = 1.1 ΦKRAγ => No significant excess => Upper Limit = 1.3 ΦKRAγ => Bkg p-value = 0.5 => Will be combined with IceCube data 21

22 Search for neutrino point-like sources 9 years of ANTARES data ( , 2424 days) All flavor dataset: tracks + cascades 7269 tracks 180 cascades 3 analysis based on a likelihood ratio: Full sky search Search around the galactic plane Candidate list search (105 sources including 13 IC tracks HESE ) Results: No significant excess found All-sky: 1.9σ at RA:311.7 δ:-48.3 Candidate list: 1.6σ for HESS J

23 results PS: most significant cluster Preliminary All-sky (1.9σ) Cand. list HESSJ (1.6σ) Search for point-source in the GC region: Track Cascade Excludes any single PS (Γ=-2.5;-2) close togc as producing more than 2-6 HESE (3yrs) Preliminary Preliminary 23

24 Combined IC/ANT point-like sources Combined search with IceCube: ANT: 6 yrs + IceCube: 4 yrs Southern hemisphere Track only => No significant excess => Combined 90% CL sensitiv. => To be updated with new data Astrophys. J. 823 (2016) no. 1, 65 24

25 Point-like KM3NeT Discovery potential (5sigma) for 3yrs of observation with full ARCA! Broad coverage! Fills southern gap! Galactic sources! 25

26 Specific KM3NeT Specific source templates: RXJ1713, Vela X, GC Neutrino flux prescriptions: RX J1713: Kelner et al, Phys. Rev. D74, (2006) VelaX: Villante & Vissani, Phys. Rev. D78, (2008). 26

27 KM3NeT 2.0: Letter of Intent J. Phys. G: Nucl. Part. Phys. 43 (2016)

28 Dark Sun Gravitational trapping and accumulation of DM particles in the centre of astro. objects (Sun and GC, dwarf, Galaxy clusters ) DM annihilation => HE neutrino flux with almost no significant astro bkg Neutrino WIMPSIM [Blennow, Edsjö,Ohlsson,arXiv: ] with masses 50 GeV - 5 TeV Bkg estimated from time scrambled data. Sun analysis ( , 6yrs, track only): - dedicated low-energy reconstruction algos - No excess observed - Limits on the spin dependent WIMP nucleon scattering cross section Physic Letters B 759 (2016)

29 Galactic Center WIMP + WIMP bƀ, τ+τ, W+W, μ+μ-, νν ν Search for an excess of ν close to the Galactic Center 9 years of ANTARES data ( ): track only GC: good visibility by ANTARES (>66%) => No significant excess found => Limit on the thermally averaged annihilation cross section <σv> 29 arxiv:

30 Summary: - 10 years of continuous data-taking - Small excess in all diffuse analysis (final ANTARES sensitivity <=> IC signal flux) - Update with 2016 ICRC - Competitive results on the Southern sky - Huge multi-messenger effort (Cf Talk A. Coleiro) - ANTARES will be decommissioned end of 2017, then smooth transition to KM3NeT - KM3NeT is under construction in Europe (2 sites South of Italy and South of France).

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