Sci Ne GHE Pisa 2016 ANTARES Results M

Sci. Ne. GHE- Pisa 2016 ANTARES Results - M. Spurio Results from the ANTARES Neutrino Telescope Maurizio Spurio University of Bologna and INFN on behalf of the ANTARES collaboration Sci. Ne. GHE– Pisa 19/10/2016 1

• Running since 2007 • 885 10” PMTs • 12 lines • 25 storeys/line • 3 PMTs / storey Details: see ar. Xiv 1409. 4552 450 m 40 km to shore ANTARES Results - M. Spurio ANTARES Sci. Ne. GHE- Pisa 2016 2500 m Junction Box 70 m 2 Interlink cables

Details: see ar. Xiv 1409. 4552 Sci. Ne. GHE- Pisa 2016 2500 m ANTARES Results - M. Spurio 450 m 40 km to shore Junction Box 70 m 3 Interlink cables

Details: see ar. Xiv 1409. 4552 Sci. Ne. GHE- Pisa 2016 2500 m ANTARES Results - M. Spurio 450 m 40 km to shore Junction Box 70 m 4 Interlink cables

The scientific goals of ANTARES Dark Matter searches Study of atmospheric neutrinos, oscillations Particle searches: nuclearites, monopoles Acoustic detection Sea sciences Not covered in this talk ANTARES Results - M. Spurio • • • Sci. Ne. GHE- Pisa 2016 • Neutrino astrophysics • Multi-messenger studies 5

HESE – 4 years Sci. Ne. GHE- Pisa 2016 Isotropic, diffuse ANTARES Results - M. Spurio On the quest for the origin of the Ice. Cube astrophysical n’s 6

• Evidence for astrophysical neutrinos (HESE, MESE, …) from partially contained events. Upgoing and downgoing events • Evidence for Astrophysical Muon Neutrinos nm from the Northern Sky [PRL 115 (2015) 081102]. Results updated: ar. Xiv: 1607. 08006 • • M. Spurio, PRD 90 (2014) 10, 103004 A. Neronov, D. Semikoz, APP 75(2016)60 D. Gaggero et al. APJ L 25(2015) 815 Palladino, F. Vissani, Ap. J. 826 (2016) 185 • …. ar. Xiv: 1607. 08006 ANTARES Results - M. Spurio • A 3. 2 tension among the two samples (HESE…, nm) • This tension can be solved assuming e. g. a two-component origin of the IC signal (one galactic, one extragalactic) Sci. Ne. GHE- Pisa 2016 The Ice. Cube spectral anomaly 7 G, Astrophysical n spectral index

ANTARES Results - M. Spurio Sci. Ne. GHE- Pisa 2016 Down in IC = Up in ANTARES 8 Almost in scale

Sci. Ne. GHE- Pisa 2016 1. Searches for a diffuse flux 2. Searches for point-like sources 3. Searches for «enhanced» diffuse flux (extended regions) 4. Transient/multimessenger studies ANTARES Results - M. Spurio ANTARES searches for astrophysical neutrinos 9

1. ANTARES diffuse flux (tracks) Sci. Ne. GHE- Pisa 2016 preliminary Reconstructed Energy preliminary Above Ecut: • Observed: 19 events • Background: 13. 5 3 • IC-like signal: 3 events Plot: ANTARES upper limits and sensitivity ANTARES Results - M. Spurio • Search for excess of reconstructed HE events w. r. t atmospheric n’s • Data: 2007 -2015 (2451 livedays) • Optimization based on IC best fit flux (spectral index Γ = 2 and 2. 5) • Variables used checked with burn sample (‘ 0’ ending runs) 10

preliminary Reconstructed Energy preliminary Above Ecut: • Observed: 7 evts • Background: 5 2 • IC-like signal: 1. 5 evts Plot: ANTARES combined upper limits and sensitivity (2007 -2015) for traks+showers ANTARES Results - M. Spurio • Search for excess of reconstructed HE events w. r. t atmospheric n’s • Data: 2007 -2013 (1405 livedays) • Optimization based on IC best fit flux (spectral index Γ = 2 and 2. 5) • Variables used checked with burn sample (‘ 0’ ending runs) Sci. Ne. GHE- Pisa 2016 1. ANTARES diffuse flux (cascades) 11

2. Point Sources Sci. Ne. GHE- Pisa 2016 2007 -2013: 1690 days (+2014 -2015 next weeks) 6490 tracks , 172 cascades Unbinned all-sky search 54 candidate sources + 8 HESE m Unsurpassed limits for E<100 Te. V HESS Pe. Vatron ANTARES Results - M. Spurio • • • 12 Nature 531 (2016) 476

Galactic Plane H S ANTARES Results - M. Spurio Fermi Bubbles Sci. Ne. GHE- Pisa 2016 3. “Enhanced” diffuse flux ? 13

3. The Galactic ridge • • • Search for nm , data 2007 -2013 Search region |l|<30° , |b|<4° Cuts optimized for G=2. 4 -2. 5 Counts in the signal/off zones No excess in the HE neutrinos 90% c. l. upper limits: 3<En<300 Te. V ANTARES Results - M. Spurio Sci. Ne. GHE- Pisa 2016 • n’s and g-rays produced by CR propagation • PLB 760 (2016) 143 14

15 ANTARES Results - M. Spurio Sci. Ne. GHE- Pisa 2016 • The simple extrapolation of the Fermi-LAT γ-ray measurement to the IC n flux in the Galactic Plane area excluded • For a neutrino flux ∝E− 2. 5 3 HESE originating in this region excluded at 90% c. l. • More information soon (tracks up to 2015+cascades) and maxlikelihood analysis Seen as a shower l pre ry na imi Seen as a track • n’s yield (positions and E): KRAγ model y pre ar n i m li

4. Multimessenger program Multi wavelength follow-up of neutrinos Radio Visible X-ray Ge. V-ray Te. V-ray MWA TAROT Swift Fermi-LAT HESS ZADKO HAWC MASTER Alerts 12/yr 30/yr 6/yr (Offline) (1 -10/yr) GW n Ligo IC Virgo (Offline) ANTARES Results - M. Spurio Sci. Ne. GHE- Pisa 2016 • A way to better understand the related physics mechanisms • A way to increase the detector sensitivities 16

4. Multimessenger program ANTARES Results - M. Spurio Real-time (follow-up of the selected neutrino events): • optical telescopes [TAROT, ROTSE, ZADKO, MASTER] • X-ray telescope [Swift/XRT] • Ge. V-Te. V 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] Sci. Ne. GHE- Pisa 2016 • A way to better understand the related physics mechanisms • A way to increase the detector sensitivities 17

Real-time follow-up (TATo. O) • APP 35 (2012) 530 (method) • JCAP 02 (2016) 062 (optical) • AJ 820 (2016) L 24 (radio) • single HE n (~10 Te. V) • single n correlated to local galaxies for SNe (~1 Te. V) • doublet of n’s Performances: • Time to send an alert: ~ 5 s • Median angular resolution: 0. 3 o - 0. 4 o • First image of the follow-up: <20 s • Dedicated optical image analysis ANTARES Results - M. Spurio ANTARES trigger Sci. Ne. GHE- Pisa 2016 External server 18

Multifrequency observations: 16 ATEL + 6 GCN CIRCULAR NUMBER: 18236 (Optical + NIR spectroscopy from NOT). . All this points to USNO-B 1. 0 0626 -0501169 being a young accreting G-K star, undergoing a flaring episode that produced the X-ray emission. We also note that this object is close to the nearby Rho Ophiuchi star forming region, being probably associated with it. ANTARES Results - M. Spurio Sci. Ne. GHE- Pisa 2016 A particular event: ANT 150901 19

On-line set-up ANTARES run control ANTARES Results - M. Spurio Alert trigger On-line analysis ANTARES on-line data Sci. Ne. GHE- Pisa 2016 External input External server • Private Mo. U with all the observatories • Different transfer protocols (mail, GCN socket, VO Event…) 20

4. Multimessenger program ANTARES Results - M. Spurio Real-time (follow-up of the selected neutrino events): • optical telescopes [TAROT, ROTSE, ZADKO, MASTER] • X-ray telescope [Swift/XRT] • Ge. V-Te. V 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] Sci. Ne. GHE- Pisa 2016 • A way to better understand the related physics mechanisms • A way to increase the detector sensitivities 21

ANTARES visibility ANTARES Results - M. Spurio 3 alerts sent by LIGO during the run 01 (2015/09 2016/01): • GW 150914: merging of 2 BHs (M= 36/29 Ms - 410 Mpc - 5. 1 ) • LVT 151012: merging of 2 BHs (M= 23/13 Ms - 1000 Mpc - 1. 7 ) • GW 151226: merging of 2 BHs (M= 14/7 Ms - 440 Mpc - >5 ) Sci. Ne. GHE- Pisa 2016 Neutrino follow-up of GWs 22

Neutrino follow-up of GW 150914 • • • No ANTARES events in ± 500 s from the GW time (0. 015 expected) Limits from ANTARES dominates for En < 100 Te. V U. L. from IC dominated above 100 Te. V Size of GW 150914 : 590 deg 2 ANTARES resolution: <0. 5 deg 2 Limits on total energy radiated in neutrinos: <10% GW Future: Receive / send alerts in real time ANTARES Results - M. Spurio Sci. Ne. GHE- Pisa 2016 a joint ANTARES/Ice. Cube/Ligo. SC/Virgo. Phys. Rev. D 93 (2016), 122010 23

4. Multimessenger program ANTARES Results - M. Spurio Real-time (follow-up of the selected neutrino events): • optical telescopes [TAROT, ROTSE, ZADKO, MASTER] • X-ray telescope [Swift/XRT] • Ge. V-Te. V 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] ar. Xiv: 1608. 08840, JCAP 1303 (2013) 006 • Micro-quasar and X-ray binaries [Fermi/LAT, Swift, RXTE] ar. Xiv: 1609. 07372 • Gamma-ray binaries [Fermi/LAT, IACT] • Blazars [Fermi/LAT, IACT, TANAMI…] JCAP 1512 (2015), 014; A&A 576 (2015) L 8 • Crab [Fermi/LAT] • Supernovae Ib, c [Optical telescopes] in preparation • Fast radio burst [radio telescopes] in preparation Sci. Ne. GHE- Pisa 2016 • A way to better understand the related physics mechanisms • A way to increase the detector sensitivities 24

ANTARES Results - M. Spurio • Search for n’s (2008 -2012) 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 (paper in prep. ) • No significant excess (best post-trial 72% for GX 1+4). • Upper limits on n fluence and model parameters constrain Sci. Ne. GHE- Pisa 2016 nm associated with Ge. V and Te. V g-ray flaring blazars and X-ray binaries 25

• Searches for a possible nm excess due to DM annihilation from the Galactic center, the Sun core, the Earth nucleus ANTARES Results - M. Spurio DM n Sci. Ne. GHE- Pisa 2016 Dark Matter searches 26

ANTARES Results - M. Spurio • DM particles scatter with Sun’s nuclei and accumulate in its centre. • Among the final products, only neutrinos could escape. • HE n’s from the Sun would be a very clean indication of DM (no significant astrophysical backgrounds expected) • For the Earth and the Sun analyses the DM, the nm spectrum calculated with WIMPSIM [Blennow, Edsjö, Ohlsson, ar. Xiv: 0709. 3898] • Annihilations into: b b, t+t-, W+W-, m+m- (and non-SUSY) n n used as benchmark • Background estimated from time scrambled data. • The sensitivities optimized w. r. t. a search cone and reconstruction quality No excess observed • Most restrictive limits for spin-dependent cross section Sci. Ne. GHE- Pisa 2016 Search from the Sun 27

Phys. Lett. B 759 (2016) 69 -74 ANTARES Results - M. Spurio Spin dependent cross section • Equilibrium assumed between capture and annihilation in the Sun 2 G Sci. Ne. GHE- Pisa 2016 Search from the Sun (result) 28

DM from the Galactic Center Sci. Ne. GHE- Pisa 2016 Particle physics DM distribution x pre limi nary ANTARES Results - M. Spurio • ANTARES in the North hemisphere: very good visibility of the GC (Ice Cube: veto used) • J-factor s calculated with CLUMPY 29

• Upper limits on known Ge. V-Te. V g-ray sources <10 -8 Ge. V/(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 nm excess from the Galactic ridge/IC hot spot; • A large multimessenger effort • EM radiation: radio (MWA), optical, X-ray, g-rays (LAT, IACTs) • Gravitational Wave observatories and Ice. Cube • ANTARES contribute to the indirect searches for Dark Matter • Most competitive limits for spin-dependent cross-section • Competitive < v> limits from the Galactic center ANTARES Results - M. Spurio • ANTARES is significantly contributing to understand the origin of cosmic neutrinos observed by Ice. Cube; • Southern sky: studied with nm competitive sensitivities and excellent angular resolution for both tracks and cascades; Sci. Ne. GHE- Pisa 2016 Summary 30

Thank you! Sci. Ne. GHE- Pisa 2016 n ANTARES Results - M. Spurio • ANTARES demonstrate the great potential of deep-sea Neutrino Telescopes • … the future is today: see next talk 31

ANTARES Results - M. Spurio Sci. Ne. GHE- Pisa 2016 Spares 32

How limits on fluence are deduced? ANTARES Results - M. Spurio Sci. Ne. GHE- Pisa 2016 • • When integrated in different energy ranges we get (for E-2 spectrum): 33

ANTARES Results - M. Spurio Sci. Ne. GHE- Pisa 2016 IC-HESE vs. ANTARES Aeff • Comparisons among experiments must be done using the effective areas, which depend on the particular analysis 35

ANTARES Results - M. Spurio ANTARES angular resolution vs En. • Black line: median resolution • dark-blue 1 region • light-blue 2 region Sci. Ne. GHE- Pisa 2016 Tracks (nm. CC) in ANTARES • Tracks best suited for astronomy • Median <0. 4° above 10 Te. V • 90% purity 36

• Shower confined within 10 m • Angular resolution 3° Better measurement of the neutrino energy ANTARES Results - M. Spurio Cascade events (upgoing) also used for astronomy Sci. Ne. GHE- Pisa 2016 Cascades (ne. CC, NC) in ANTARES • Energy resolution better than 10% in a wide energy range 37

ANTARES Results - M. Spurio Sci. Ne. GHE- Pisa 2016 3 C 279 Blazar 38

ANTARES Results - M. Spurio Sci. Ne. GHE- Pisa 2016 3 C 279 Blazar 39

ANTARES Results - M. Spurio • The nm channel allows a proxy estimate of the energy • of reconstructed nm within 0. 4° (for E-2 spectrum) Sci. Ne. GHE- Pisa 2016 Atmospheric neutrinos 40

Cosmic Signal F 0 E-G Ice. Cube Coll. ar. Xiv: 1409. 4535 v 3 ANTARES EPJ C (2013) 73: 2606 • The search methods rely on the event-by-event estimate of the nm energy (the muon light yield gives a proxy) • Comparison between the signal region and off-signal zones ANTARES Results - M. Spurio • The expected signal spectrum is harder than the background of atmospheric neutrinos Sci. Ne. GHE- Pisa 2016 • Atmospheric neutrinos irreducible background 41