21/06/2017. Weak Interactions and Neutrinos (WIN2017) - University of California, Irvine, USA - Antonio Capone 1

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1 Weak Interactions and Neutrinos (WIN2017) - University of California, Irvine, USA - Antonio Capone 1

2 Search for a diffuse flux Search for point-like sources Search for enhanced diffuse flux from the SUN, the Galactic Plane, the Earth Weak Interactions and Neutrinos (WIN2017) - University of California, Irvine, USA - Antonio Capone 2

From Traditional Astronomy (Optics) to Multi-Wavelength Astronomy:

(1858), fresco by Giuseppe Bertini (1825 1898) and to Multi-Messengers

3 From Traditional Astronomy (Optics) to Multi-Wavelength Astronomy: observations of light in the visible band are complemented by radio, X-ray and g astronomy Galileo Galilei showing the Doge of Venice how to use the telescope (1858), fresco by Giuseppe Bertini ( ) and to Multi-Messengers Astronomy: HE-CR, photons, neutrinos, GW Weak Interactions and Neutrinos (WIN2017) - University of California, Irvine, USA - Antonio Capone 3

Search for neutrino induced events, mainly v µ N µ X, deep underwater Down-going µ from atm.

Search for neutrinos with E n >1 TeV - ~TeV muons propagate in water for several km before being

long µ tracks allow good angular reconstruction For E ν 1TeV θ µν ~ 0.

Telescope µ direction reconstructed from the arrival time of Cherenkov photons on the Optical

4 Search for neutrino induced events, mainly v µ N µ X, deep underwater Down-going µ from atm. showers S/N ~ -6 at 3500m w.e. depth p, nuclei - Atmospheric neutrino flux ~ E n -3 - Neutrino flux from cosmic sources ~ E n -2 Search for neutrinos with E n >1 TeV - ~TeV muons propagate in water for several km before being stopped go deep to reduce down-going atmospheric µ backg. long µ tracks allow good angular reconstruction For E ν 1TeV θ µν ~ 0.7 E ν [TeV ] p, nuclei Neutrinos from cosmic sources induce 1-0 muon evts/y in a km 3 Neutrino Telescope µ direction reconstructed from the arrival time of Cherenkov photons on the Optical Modules: needed good measurement of PMT hits, s(t)~1ns, and good knowledge of PMT positions: (s ~cm) Cherenkov Neutrino Telescope Up-going µ from neutrinos generated in atm. showers S/N ~ -4 charge current interactions up-going neutrino 43 µ water/ice rock Picture from ANTARES Weak Interactions and Neutrinos (WIN2017) - University of California, Irvine, USA - Antonio Capone 4

5 m 40 km to shore String-based detector

vertical 0 m ~70 m 12 detection lines 25

5 The Largest Neutrino Detector in the Northern Hemisphere Nucl. Instr. and Meth.A 656 (2011) Total Instrum. Volume ~ -2 km3 25 storeys 350 m 14.5 m 40 km to shore String-based detector Downward-looking PMTs axis at 45º to vertical 0 m ~70 m 12 detection lines 25 storeys / line 3 PMTs / storey ~900 PMTs Junction Box ~2500 m depth 5

~ factor 3 Events contained in the detector: smaller Effective Volume, Energy resolution ~ 5-% Median angular resolution ~ 33

6 Tracks: CC νν μμ or νν ττ μμ Electronic or hadronic showers: NC and CC νν ee or νν ττ showers Interaction can occur far from the detector providing a large Effective Volume Angular resol. < for EE νν > 1111 TTTTTT Energy resol. ~ factor 3 Events contained in the detector: smaller Effective Volume, Energy resolution ~ 5-% Median angular resolution ~ 33 angular resoluton ( ) tracks angular resoluton ( ) showers 4 Weak Interactions and Neutrinos (WIN2017) - University of California, Irvine, USA - Antonio Capone 6

Search for point-like cosmic Neutrino Sources

Remnants Microquasars Active Galactic Nuclei GRB

73946HESS Their identification requires a detector

5 for E ν 1TeV Experimental signal : statistical

7 Search for point-like cosmic Neutrino Sources Extragalactic Pulsar Wind Nebulae Galactic Supernova Remnants Microquasars Active Galactic Nuclei GRB RX J HESS Their identification requires a detector with accurate angular reconstruction For transient sources the time meas. improves the signal detection σ (ϑ ) 0.5 for E ν 1TeV Experimental signal : statistical evidence of an excess of events coming from the same direction Weak Interactions and Neutrinos (WIN2017) - University of California, Irvine, USA - Antonio Capone 7

8 9 years of ANTARES data searching for all neutrino flavours: 7629 tracks shower events passed the selection criteria ττ lllllll ssssss:bbbbbb = > > llllll[μμ F ττ ττ ssssss PP ssssss,ii (EE ii ) + NN BB ττ ττ PP bbbbbb,ii (EE ii )] μμ ssssss SSKtttt.,ssss. ττkss ANTARES arxiv: v1, 6 June 2017 Blue: Tracks Red: Cascades Candidate Sources IC HESE tracks GC region equatorial coordinates so far. no significant excess has been found Weak Interactions and Neutrinos (WIN2017) - University of California, Irvine, USA - Antonio Capone 8

The visible sky of ANTARES divided on a 1 R 1 R (r.a x decl.) boxes. Maximum Likelihood analysis searching for clusters ANTARES arxiv:1706.

9 The visible sky of ANTARES divided on a 1 R 1 R (r.a x decl.) boxes. Maximum Likelihood analysis searching for clusters ANTARES arxiv: v1, 6 June 2017 equatorial coordinates The most significant cluster: decl. δ = , r.a. α = has a pre-trial p-value of à 22 ddφφ U. L. from this sky location EE = 33. dddd 88 10X88 GeV cm -2 s -1 Weak Interactions and Neutrinos (WIN2017) - University of California, Irvine, USA - Antonio Capone 9

10 s -1 ] -2 [GeV cm 90%CL Φ 2 E 5 ANTARES sensitivity ANTARES sensitivity (E < 0 TeV) ν ANTARES limits (candidate list) ANTARES limits (candidate list for HESE events) 90% U.L. 6 ANTARES limits (1 declination bands) IceCube 7 years sensitivity [ApJ 835(2017)2 151] IceCube 3 years MESE sensitivity (E < 0 TeV) [ApJ 824(2016)2 L28] ν IceCube 7 years limits [ApJ 835(2017)2 151] years of ANTARES data : 7629 tracks shower ANTARES arxiv: v1, 6 June sinδ Weak Interactions and Neutrinos (WIN2017) - University of California, Irvine, USA - Antonio Capone

11 Skymap of pre-trial p-values for the combined ANTARES 2007/12 and IceCube 40, 59, 79 point-source analyses. The red circle indicates the location of the most significant cluster: (0.7σ post-trial significance) Weak Interactions and Neutrinos (WIN2017) - University of California, Irvine, USA - Antonio Capone 11

12 Neutrinos from: Unresolved AGN "Z-bursts" "GZK like" proton-cmb interactions Top-Down models Neutrinos. Their identification out of the more intense background of atmospheric neutrinos (and µ) is possible at very high energies (E µ >> TeV) and requires good energy reconstruction. number of events 2 1 arxiv: v1 Search here!!! atm. ν atm. µ astrophys. flux Data Found 8 shower events for TeV<E SH <0 TeV when 5 expected. Compatible with IceCube signal ANTARES, 6 years reconstructed shower energy [GeV] Weak Interactions and Neutrinos (WIN2017) - University of California, Irvine, USA - Antonio Capone 12

Tracks Data: 2007-2015 (2451 live-days) Above E cut : Bkg: 13.

13 Tracks Data: (2451 live-days) Above E cut : Bkg: 13.5 ± 3 evts, IC-like signal: 3 evts Observed: 19 evts Cascades Data: (1405 live-days) Above E cut : Bkg: 5 ± 2 evts, IC-like signal: 1.5 evts Observed: 7 evts PRELIMINARY PRELIMINARY Energy Estimator sr -1 cm -2 ] 6 Reconstructed Energy Atmospheric neutrinos IceCube flux ANTARES combined upper limits and sensitivities for 9 years data sample ( ) tracks + cascades -1 /de [GeV s 1f dφ 2 E Γ = 2.5 PRELIMINARY ANTARES sensitivity ( ) ANTARES upper limit (this analysis) log (E /GeV) ν Weak Interactions and Neutrinos (WIN2017) - University of California, Irvine, USA - Antonio Capone 13 Γ = 2

$n s and g-rays produced by CR propagation pp Z[ + pp \]^ ππ R ππ ± ππ R γγγγ EEEE cccccccccccccc ππ ± νν μμ, νν ee Search for n µ, data 2007-2013 Search$ upper limits: 3<E n <300 TeV Physics Letters B 760 (2016) 143 148 E µ cut applied Distribution of the reconstructed E µ of up-going muons in the Galactic

upper limits: 3<E n <300 TeV Physics Letters B 760 (2016) 143 148 E µ cut applied Distribution of the reconstructed E µ of up-going muons in the Galactic

14 n s and g-rays produced by CR propagation pp Z[ + pp \]^ ππ R ππ ± ππ R γγγγ EEEE cccccccccccccc ππ ± νν μμ, νν ee Search for n µ, data Search region l <30, b <4 Cuts optimized for neutrino energy spectrum ~E -g (g= ) Counts in the signal/off zones No excess in the HE neutrinos 90% C.L. upper limits: 3<E n <300 TeV Physics Letters B 760 (2016) E µ cut applied Distribution of the reconstructed E µ of up-going muons in the Galactic Plane (black crosses) and average of the offzone regions (red histogram). Weak Interactions and Neutrinos (WIN2017) - University of California, Irvine, USA - Antonio Capone 14

15 j j New analysis on tracks and showers, based on Max. Lik. ττ ττ ττ ττ L ssssss:bbbbbb = f f[μμ pppppp ssssss (EE ii, αα ii, δδ ii ) + μμ pppppp bbbbbb (EE ii, αα ii, δδ ii )] ττ tttt,ssss ii ττ ANTARES arxiv: v1 1 May 2017 New ANTARES 90% UL, 50 PeV cutoff ANTARES 90% UL 2016 IceCube n KRA g new model to describe the C.R. transport in our galaxy. It agrees with C.R. measurements (KASCADE, Pamela, AMS, Fermi-LAT, HESS). FERMI-LAT diffuse g flux from along the galactic plane (ππ R γγγγ) well explained above few GeV. KRA g allows to predict the n flux by ππ ± decays induced by galactic CR interactions KRA g 50PeV cut-off for CR KRA g 5PeV cut-off for CR KRA g assuming a neutrino flux E -2.5 and a CR spectrum with 50 PeV cut-off can explain ~20% of the IceCube observed HESE. ANTARES, with an good visibility of the Galactic Plane well suited to observe these fluxes or to put competitive limits: no signal found à set 90%C.L. upper limits. Weak Interactions and Neutrinos (WIN2017) - University of California, Irvine, USA - Antonio Capone 15

16 also open problems in particle physics Dark Matter searches: Neutralino annihilation in Sun, Earth, Galactic Center Magnetic Monopoles Particle acceleration mechanisms Multi-messenger searches Neutrino Oscillations Search for Sterile Neutrinos Neutralino search: cc n+ Weak Interactions and Neutrinos (WIN2017) - University of California, Irvine, USA - Antonio Capone 16

6 years of ANTARES data: 2007-2012 Distribution of the angular distance between reconstructed the track direction of events and the Sun position for two different track reconstruction algorithms in

17 6 years of ANTARES data: Distribution of the angular distance between reconstructed the track direction of events and the Sun position for two different track reconstruction algorithms in order to maximize the event reconstruction for single line and multi-lines events. No excess observed over the expected backg. µ Y Neutralino search: cc n+ Neutrino fluxes from WWWWWWWW + WWWWWWWW bbbbp, WW : WW X, ττ : ττ X Neutrino spectrum from WIMPSIM (M. Blennow, J. Edsjö, T. Ohlsson, J. Cosmol. Astropart. Phys (2008) 021. ) Background estimated from time-scrambled data. evaluated for 50 GeV/c 2 < M WIMP < 5 TeV/c 2 ννp νν + à limits to n fluxes and to WIMP-nucleon cross sections Weak Interactions and Neutrinos (WIN2017) - University of California, Irvine, USA - Antonio Capone 17

18 Maximization of a likelihood function based on the knowledge of the probability density functions, for the contribution of a background event, B(Y, N hit, b), or a signal event, S(Y, N hit, b), to the observed distribution. L nn ss NN tttttt = ee X(nn ss:nn bbbb ) f(nn ss SS(ψψ ii, NN hhhhhh,ii, ββ ii ) + (nn ss SS(ψψ ii, NN hhhhhh,ii, ββ ii ) iik11 N hit = number of hit used for the track reconstruction b = the angular error estimate for the reconstructed track N tot = tot. Number of reconstructed events n s and N bg are the number of signal and background events in the maximization procedure B(Y, N hit, b) obtained by the collected data randomising the right ascension of the event S(Y, N hit, b) obtained from MC simulation using the n energy spectra given by WIMPSIM High statistics Pseudo-MC experiments are performed for each combination of M WIMP, annihilation channel: with only background n s = 0 à allow to evaluate L(0) with a given value of simulated signal-like events n s > 0. For each one of these pseudo-mc experiment a maximum likelihood analysis is performed searching for the value of n s that maximize the likelihood. We then get L nn stu We can now evaluate a Test Statistic TTTT = llllll 1111 LL(00) LL nn mmmmmm that gives us a measure of the probability to assume a fluctuation of the background as a distribution of events with n s 0. Weak Interactions and Neutrinos (WIN2017) - University of California, Irvine, USA - Antonio Capone 18

19 No excess observed over the expected background: evaluate 90% C.L. upper limits for expected signal Limits on the spin-dependent WIMP-nucleon scattering cross-section as a function of WIMP mass for the bb, τ+τ and W+W channels. assumptions: capture and annihilations in equilibrium local D.M. density =0.4 GeV cm -3 Ä^ υυ ]~ according to Maxwell distr. 270 km s -1 r,m.s. Limits on the spin-independent WIMP-nucleon scattering cross-section as a function of WIMP mass for the different channels considered. Limits on a neutrino flux coming from the Sun as a function of the WIMP masses for the different channels considered. Weak Interactions and Neutrinos (WIN2017) - University of California, Irvine, USA - Antonio Capone 19

9 years of ANTARES data: 2007-2015 - ANTARES observes the G.

20 9 years of ANTARES data: ANTARES observes the G.C > 66% time Search performed for: 50 GeV/c 2 < M WIMP < 0 TeV/c 2 WWWWWWWW + WWWWWWWW bbbbp, WW : WW X, ττ : ττ X, μμ : μμ X, ννννp ddφφ νν μμíννìμμ ddee νν μμíννìμμ = îσσσσï ddnn ννμμíννìμμ WWWWWWWW ddee νν μμíννìμμ µ JJ iiiiii (ΔΔΔΔ) The expected n flux depends on the DM distribution around the GC. 3 halo models have been considered Parameter NFW Burkert McMillan r s [kpc] ± 7.5 ρ local [GeV/cm 3 ] ± No excess found over the expected backg. à limits to < σσσσ > J int ( ) = ρ 2 DM dl d Distribution of measured angles between reconstructed tracks and the Galactic Centre (crosses). The red line describes what is expected from background event. The integrated J-Factor, J int, for a cone-shaped region centred on the G.C. with an opening angle Y Weak Interactions and Neutrinos (WIN2017) - University of California, Irvine, USA - Antonio Capone 20

21 No excess found over the expected background limits to ddφφ νν μμíννìμμ ddee νν μμíννìμμ = îσσσσï ddnn ννμμíννìμμ WWWWWWWW ddee νν JJ iiiiii (ΔΔΔΔ) DM density profile from NFW 90% C.L. limits on the thermally averaged annihilation cross-section σv from WIMP annihil. in the Milky Way 90% C.L. limits on the thermally averaged annihilation crosssection, σ v, as a function of M WIMP. The results from IceCube and ANTARES were obtained with the NFW profile. DM density profile from NFW 90% C.L. upper limits on the neutrino flux from WIMP annihilations in the Milky Way. Weak Interactions and Neutrinos (WIN2017) - University of California, Irvine, USA - Antonio Capone 21

22 90% C.L. limits on the thermally averaged annihilation cross-section σ v obtained only for the channel WWWWWWWW + WWWWWWWW ττ : ττ X but for different models of the DM halo around the G.C. Weak Interactions and Neutrinos (WIN2017) - University of California, Irvine, USA - Antonio Capone 22

23 j j t WIMPS can be gravitationally bound to the Earth if υυ ú\^ù < υυ ûü t û υυ EEEEEEEEEE eeeeeeeeeeee ~1111 kkkk ; υυ ss WWWWWWWW = υυp following a Maxwell-Boltzmann distr. with r.m.s. velocity 270 km/s only a small fraction of WIMPS captured on the Earth. WIMPS-nucleons collision described by spin-independent cross section σσ SSSS pp. Fe and Ni most abundant in the Earth à effective capture for MM WWWWWWWW ~5555 GGGGGG. In the Earth the capture (Γ Z tt ) and annihilation (Γ tt ) rates would reach the equilibrium in t~ 11 y >> Earth age (t Earth = y) In these conditions: Γ (tt t ) Æ Ø ± µ. s µ p ª FF ª mm æ ø Æ ƒ ƒ s µ ør «û Needed to estimate the n fluxes with WimpSim ρρ æ R. =0.3 GeV/cm 3 Local D.M. density the capture is very effective when m WIMP ~ m target CC Z ø capture factor C A annih. factor Conversion factor = µ. Fe, Ni ~ GeV øs µ p ª FF ª mm æ Weak Interactions and Neutrinos (WIN2017) - University of California, Irvine, USA - Antonio Capone 23

24 6 years of ANTARES data: GeV/c 2 < M WIMP < 1 TeV/c 2 WWWWWWWW + WWWWWWWW bbbbp, WW : WW X, ττ : ττ X, ννννì No excess found over the expected background Limits on the WIMP-WIMP annihilation rate in the Earth Limits on the spin independent WIMP-nucleon cross-section Weak Interactions and Neutrinos (WIN2017) - University of California, Irvine, USA - Antonio Capone 24

25 90% C.L. upper limits on σ p SI as a function of σ A n Earth for m WIMP =52.5 GeV 90% C.L. upper limits on Γ A as a function of the WIMP mass. 90% C.L. upper limits on σ p SI as a function of the WIMP mass for ANTARES (Earth) and ANTARES (Sun), assuming σ A υυ Earth = 3 26 cm 3 s 1 and WIMP pair annihilation to 0% into either t + t - (blue), W + W - (green) or bbbbp (purple). 25 Gev/c 2 < M WIMP < 1 Tev/c 2 Weak Interactions and Neutrinos (WIN2017) - University of California, Irvine, USA - Antonio Capone 25

26 A common observation of the same source will allow to better understand the acceleration mechanisms, the physics inside the source A common observation will increase the detector sensitivities A long list of activities: Real-time (follow-up of the selected neutrino events): optical telescopes [TAROT, ROTSE, ZADKO, MASTER] X-ray telescope [Swift/XRT] GeV-TeV γ-ray telescopes [HESS, HAWC] radio telescope [MWA] Online search of fast transient sources [GCN, Parkes] Multi-messenger correlation with: Gravitational wave [Virgo/Ligo] UHE events [Auger] Time-dependent searches: GRB [Swift, Fermi, IPN] Micro-quasar and X-ray binaries [Fermi/LAT, Swift, RXTE] Gamma-ray binaries [Fermi/LAT, IACT] Blazars [Fermi/LAT, IACT, TANAMI ] Crab [Fermi/LAT] Supernovae Ib,c [Optical telescopes] Fast radio burst [radio telescopes] Weak Interactions and Neutrinos (WIN2017) - University of California, Irvine, USA - Antonio Capone 26

t =-250 s Search for neutrino-like tracks GCN coming alerts in trigger time the recording of all the low level coincidence with an observed triggers. GRB.

GCN=Gamma Ray Burst Coordination Network t = 0 s Data taking triggered by a satellite (FERMI; SWIFT, INTEGRAL) t = 20 s All data written to disk t = 200 s t = 1 h Specific

27 t =-250 s Search for neutrino-like tracks GCN coming alerts in trigger time the recording of all the low level coincidence with an observed triggers. GRB. A continuous buffer ensures the The knowledge of the time and availability the source of the position: data before the alert reduces the background improves the sensitivity GCN=Gamma Ray Burst Coordination Network t = 0 s Data taking triggered by a satellite (FERMI; SWIFT, INTEGRAL) t = 20 s All data written to disk t = 200 s t = 1 h Specific data filtering and reconstruction by searching for an excess of events in the GRB direction (offline) Weak Interactions and Neutrinos (WIN2017) - University of California, Irvine, USA - Antonio Capone 27

28 data: alerts and data from FERMI SWIFT - GCN analysis of 296 long GRBs (total prompt emission 6.6 hours) Simulation of neutrino fluxes from GRB: NeuCosmA (Hümmer et al 20) à expected events Guetta (Guetta et al. 2004) à expected 0.48 events Expected background events No events found in stacked GRB search within window: Previous ANTARES result, 40 GRBs JCAP 1303 (2013) 006 ANTARES upper limits 90% C.L. for Guetta fluxes NeuCosmA fluxes IceCube upper limits 90% C.L. IC40+59 for 215 GRBs ].2 "F ν ""[GeV"cm 2 E (b) 5 Astronomy & Astrophysics 559, A9 (2013) E""[GeV] Weak Interactions and Neutrinos (WIN2017) - University of California, Irvine, USA - Antonio Capone 28 6 A&A 559, A9 (2013) ANTARES"2007 ANTARES"NeuCosmA ANTARES"Guetta IceCube"IC40+59 A&A 559, A9 (2013) "s.1 "sr.1 ].2 ν""[gev"cm 2 E

29 The search was performed for 4 bright GRBs: GRB080916C, GRB 1918A, GRB A and GRB A) observed between 2008 and The expected neutrino fluxes evaluated in the framework of: - the fireball model have with the internal shock scenario (EE νν ) - the photospheric scenario (EE νν < ) No events have been found: 90% C.L. upper limits to the neutrino fluence. ) -2 (GeV cm ν µ φ 2 E νµ Monthly Notices Royal Astronomical Society (2017) 469 (1): C fluence C ANTARES UL A fluence A ANTARES UL A fluence A ANTARES UL 1918A fluence 1918A ANTARES UL E 2 ν µ φ νµ (Gev cm 2 ) C fluence C ANTARES UL A fluence A ANTARES UL A fluence A ANTARES UL 1918A fluence 1918A ANTARES UL Internal Shock Scenario E νµ (GeV) 4 5 Photospheric Scenario E νµ (GeV) Weak Interactions and Neutrinos (WIN2017) - University of California, Irvine, USA - Antonio Capone 29

30 3 alerts sent by LIGO during the run 01 (2015/09 à 2016/01): o GW150914: merging of 2 BHs (M= 36/29 M s - 4 Mpc s) o LVT1512: merging of 2 BHs (M= 23/13 M s - 00 Mpc s) o GW151226: merging of 2 BHs (M= 14/7 M s Mpc - >5 s) ANTARES visibility Weak Interactions and Neutrinos (WIN2017) - University of California, Irvine, USA - Antonio Capone 30

Phys.Rev. D93 (2016), 1220 No ANTARES events in ±500 s from the GW time (0.015 expected) Limits from ANTARES dominates for En < 0 TeV U.L. from IC dominated above 0 TeV Size of GW150914 : 590 deg 2 ANTARES resolution: <0.

31 Phys.Rev. D93 (2016), 1220 No ANTARES events in ±500 s from the GW time (0.015 expected) Limits from ANTARES dominates for En < 0 TeV U.L. from IC dominated above 0 TeV Size of GW : 590 deg 2 ANTARES resolution: <0.5 deg 2 Limits on total energy radiated in neutrinos: <% GW Future: Receive / send alerts in real time Weak Interactions and Neutrinos (WIN2017) - University of California, Irvine, USA - Antonio Capone 31

32 P sg (t) -1 Photons s -1 Photons s -2 cm -1 Photons s -2 cm cm -2 Search for n s ( ) correlated with high activity state Blazars monitored by FERMI-LAT and IACTs (JCAP 1512 (2015), 014) 33 X-ray binaries during flares observed by Swift-BAT, RXTE-ASM and MAXI. Transition states from telegram alerts No significant excess (best post-trial 72% for GX 1+4), then à Upper limits on n fluence and model parameters constrain Swift/BAT (15 kev < E < 50 kev) Swift/BAT (15 kev < E < 50 kev) Modified Julian Date RXTE/ASM (2 kev < E < kev) RXTE/ASM (2 kev < E < kev) Modified Julian Date MAXI (2 kev < E < 20 kev) MAXI (2 kev < E < 20 kev) Modified Julian Date Time PDF for 4U Neutrino Time-PDF X-ray binary 4U JCAP04(2017)019 Weak Interactions and Neutrinos (WIN2017) - University of California, Irvine, USA - Antonio Capone Modified Julian Date P sg (t)

12 Lines, 885 OM ANTARES KM3NeT 3 Building

33 12 Lines, 885 OM ANTARES KM3NeT 3 Building Blocks on 2 Sites 3*115 lines, ~62 OMs, ~ 1925 PMTs Basic active element: Digital Optical Module 31 x 3 PMTs 18 OMs/line Weak Interactions and Neutrinos (WIN2017) - University of California, Irvine, USA - Antonio Capone 33

34 240 people 45 institutes or universities 13 different countries Weak Interactions and Neutrinos (WIN2017) - University of California, Irvine, USA - Antonio Capone 34

From Supernovae - Dark Matter search - Monopoles - Nuclearites - Neutrinos from extraterrestrial sources - Origin and production

35 Composite View of the Crab Nebula Low Energy Medium Energy High Energy MeV < E n < 0 GeV M ev < E n < 0 GeV E n > 1 TeV - Neutrino Oscillations - Neut. Mass Hierarchy - Sterile neutrinos - Neut. From Supernovae - Dark Matter search - Monopoles - Nuclearites - Neutrinos from extraterrestrial sources - Origin and production mechanism of HE CR KM3NeT-ORCA ANTARES KM3NeT-ARCA and synergies with Sea-Sciences: oceanography, biology, seismology, Weak Interactions and Neutrinos (WIN2017) - University of California, Irvine, USA - Antonio Capone 35

36 ORCA ARCA ARCA ORCA Location Italy Capo Passero France - Toulon Detector Lines distance 90m 20m DOM spacing 36m 9m Instrumented mass 500Mton 5,7 Mton Weak Interactions and Neutrinos (WIN2017) - University of California, Irvine, USA - Antonio Capone 36

L.O.I. KM3NeT ARCA and ORCA: J. Phys. G43 (2016) n. 8, 084001 arxiv: 1601.

37 L.O.I. KM3NeT ARCA and ORCA: J. Phys. G43 (2016) n. 8, arxiv: Weak Interactions and Neutrinos (WIN2017) - University of California, Irvine, USA - Antonio Capone 37

38 Weak Interactions and Neutrinos (WIN2017) - University of California, Irvine, USA - Antonio Capone 38

39 ARCA detector ARCA: 2 blocks 115 strings/block 90m horizontal spacing 18 Optical Modules/strings 36m vertical spacing ~1km3 Total Volume 1.2 km3 Weak Interactions and Neutrinos (WIN2017) - University of California, Irvine, USA - Antonio Capone 39

40 ANTARES studied the Southern sky with n µ competitive sensitivities and excellent angular resolution for both tracks and cascades; Upper limits on known GeV-TeV g-ray sources < -8 GeV/(cm 2 s) Sensitivity for a diffuse flux close to the level of the IC signal Detailed study of extended regions (Galactic plane, Fermi Bubbles) no n µ excess from the Galactic ridge/ic hot spot; A large multi-messenger effort EM radiation: radio (MWA), optical, X-ray, g-rays (LAT,IACTs) Gravitational Wave observatories and IceCube ANTARES contribute to the indirect searches for Dark Matter Most competitive limits for spin-dependent cross-section Competitive <sv> limits from the Galactic centre KM3NeT-Arca Neutrino Telescope under construction will soon be able to observe the neutrino sky with unprecedented sensitivities. Weak Interactions and Neutrinos (WIN2017) - University of California, Irvine, USA - Antonio Capone 40

Antonio Capone Univ. La Sapienza INFN - Roma

Observations of HE Neutrino and Multimessenger AstroParticle Physics Antonio Capone Univ. La Sapienza INFN - Roma 1 Talk outline High Energy Astrophysical Neutrino Detection in a multi-messenger scenario