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PoS(ICRC2019)006 http://pos.sissa.it/ ∗ ‡ †1 Rosa Coniglione [email protected] INFN - Laboratori Nazionali del Sud (LNS), Via Santa Sofia 62, 95123 Catania, for collaboration list see PoS(ICRC2019)1177 Speaker. 1 Since 2007 the ANTARES highranean energy Sea, detector, is installed taking inabout data. the depths 0.01 It of cubic is the kilometers. Mediter- locatedof 40 The astrophysical km main off aim as the ofcan a French observe the diffuse coast in ANTARES flux real instrumenting neutrino time or a telescopemessenger neutrinos coming volume approach) is correlated from of providing in the valuable astrophysical space search informations and sources. fromWith time the the with Northern ANTARES aim sky. other to cosmic enlarge probesgive the (multi- valuable effective responses areas in for the the neutrinoing detection physics two of detectors domain, high in the the energy Mediterranean KM3NeT neutrinos Sea: collaborationobservation and KM3NeT/ARCA is of also mainly construct- neutrinos devoted to to from the Active discovery Galactic and devoted Nuclei to and the Galactic study sources of and theIn KM3NeT/ORCA fundamental this properties work of the the neutrino. mainperspectives recent as well results the achieved first by results the from the ANTARES deployed collaboration KM3NeT and Detection the UnitsCorresponding will KM3NeT author: be reported. ∗ † Copyright owned by the author(s) under the terms of the Creative Commons http://antares.in2p3.fr/Collaboration/index2.html https://www.km3net.org/km3net-author-list-for-icrc-2019 c Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0). 36th International Cosmic Ray Conference -IceCubeRC2019- July 24th - August 1st, 2019 Madison, WI, U.S.A. ‡ E-mail: The KM3NeT and ANTARES‡ Collaborations Results from the Mediterranean neutrino detectors PoS(ICRC2019)006 - γ ] and . The . The 4 4 5 ]. This, 2 , 1 together with 3 Rosa Coniglione ], has confirmed 3 -rays (E>300 TeV) are absorbed by cosmic γ . The recent results achieved in the searches for 1 2 -rays can be produced at the sources or in the encountered γ ] offer a unique opportunity to observe the neutrino sky from a 5 . Results from studies and perspectives are reported 6 GeV, focuses on the high-energy neutrino astrophysics while the KM3NeT/ORCA 8 The ANTARES results collected in 11 years of data taking cover many aspects of the neutrino The detectors will be described in Section The study of astrophysical high-energy neutrinos can add relevant pieces of information to The existence of neutrinos of cosmic origin has been demonstrated by IceCube with the detec- offers an optimal location for the observation of the Southern sky, where indirect search for dark matterbe is presented also in one Section of the main results of the collaboration and results will the future KM3NeT detectors [ results from transient sources and the alert system of ANTARES will be covered in Section point-like sources also in a joint analysis with IceCube will be reported in Section physics. Currently, ANTARES is providing an active real-timethe monitoring best of the sensitivity Southern in Sky the with 1-300studies TeV of domain. astrophysical This transients is including of also fundamental gravitational waves. importance for the follow-up complmentary field of view w.r.t. IceCube.unprecedented Thanks angular to resolution, the which optical is a water crucial properties,KM3NeT parameter they will for provide be the an a pointing distributed of infrastructure neutrinosearch comprising sources. with two telescopes: Cosmic in ARCA the (Astroparticle Abyss), Re- ORCA located (Oscillation at a Research depth with of CosmicToulon 3500 (). m in offshore the Capo The Abyss), Passero (Italy), KM3NeT/ARCA located100 and GeV at detector, to a optimized 10 depth for ofdetector, the 2500 optimized neutrino for m energy neutrino offshore range energiesdamental from from few neutrino GeV properties. to 100 Withneutrino GeV, the focuses energies on with two high the detectors effective study KM3NeT areas. of will fun- cover a very wide range of the perspectives for the future KM3NeT/ARCAand detector. from extended The regions search proposed of as neutrinos hadronic from acceleration the sites will all be sky shown in Section the understanding of production mechanisms of primary cosmic rays (CRs) and high energy tion of a diffuse fluxbulk exceeding of the these expected neutrinos background from of thetion more full with sky than is other 5 yet astrophysical sigma. unknown. messengers Only the The thanks first origin to neutrino of the source the simultaneous has observa- been discovered [ the Galactic center and most of the Galactic Plane are located. The ANTARES telescope [ Mediterranean neutrino detectors 1. Introduction rays. Neutrinos, CR and highdense energy source environment. Unlikethe intergalactic CRs, magnetic which fields in orcollisions, their absorbed neutrinos as path travel they towards undisturbed. interact the High withmicrowave energy matter background or are radiation. radiation deflected via Only by inelastic we by be combing able to information to from achieve aGravitational all complete Waves three picture have of messengers, been non added will thermal processes tophenomena in the in the the number Universe. cosmos. of Recently also probes that can be associated to energetic together with the observation ofthat counterparts multi-messenger astronomy of is a the gravitationalcommunities. future waves key source objective [ of the astrophysical and astronomical PoS(ICRC2019)006 . 3 48’ ◦ 48’ N ◦ ]. 5 Rosa Coniglione 2 06’ E at about 80 km off-shore the Sicilian coast in front of ◦ the KM3NeT construction status will be presented together with 8 downwards to optimize the detection of light for up-going neutrinos. . 3 ◦ 16’ N 16 ◦ ], has been the first operating . It is installed at 42 4 . Finally in Section 7 10’ E at about 40 km off shore the French coast at a depth of about 2500 m, and is contin- ANTARES [ An innovative optical sensor, the Digital Optical Modules (DOM), has been developed by the The ARCA and ORCA detectors will share the same technology for the construction and With the aim to enlarge the effective areas for the detection of high energy neutrinos and to ◦ 02’ E at about 40 km off the coast of Toulon, France, at a depth of about 2450m. The ORCA ◦ detector is located at about 10 km west the site of ANTARES. 06 KM3NeT collaboration. Each DOM is31 a 3-inch 17-inch diameter PMTs pressure-resistant together glasscontains with sphere 19 housing the PMTs, associated which electronics. areEighteen thus DOMs downward-looking, The are whereas lower suspended the by hemisphere other meanstion of 12 of Unit PMTs each two (DU). look ropes DOM The upwards. along DUs aby are vertical submerged flexible structure, buoys. structures called An anchored the electro-optical to Detec- backboneallows cable, the running for sea along floor power the and feeding full kept length andnetwork almost of data each of vertical transmission. DU, electro-optical Each cables DUoptical and cable is junction connecting connected boxes, to at shore. which The itsall converges readout base analogue in is signals to based a from on a single the the sea PMTs "all-data-to-shore" maindigitised floor concept that and electro- in pass all which a digital preset data thresholdits (typically are integration 0.3 sent and photo-electrons) deployment, to are each shore DUdeposited where is on they wrapped the are on seabed. processed a 2.5 in Thearray m DU real of diameter is 115 time. spherical DUs then frame To will unfurled which simplify constitute until is a it detector reaches building its block. operatingdeployment configuration. of An the main componentsdetector of will the comprise detectors, two although building withm blocks different and (230 granularity. DUs) with ARCA with a DUs vertical horizontally spacing spaced between by DOMs about of 90 about 36 m for a total volume of about 1 km Mediterranean neutrino detectors in Section the first results obtained. 2. The Detectors N, 6 uously taking data in itsANTARES complete consists configuration since of May about 2008(PMT), 885 with arranged optical a in duty modules, groups cycle of each of threeof one about (a each 95%. storey) storey housing and are a facing distributed 45 along 10-inchThe 12 strings photomultiplier vertical are anchored strings. on The the PMTs distance sea of floor, about arranged 60 in m, an and octagonal keptdetector configuration vertical is with by a of a inter-string about submerged 0.01 buoy. km The total volume of the ANTARES study the neutrino oscillation propertiestion detecting has atmospheric started the neutrino, construction the ofthe KM3NeT two Abyss) collabora- detectors: and ARCA the (Astroparticle ORCA Research (Oscillation with Research Cosmics with in Cosmic in the Abyss) detectors [ It will be installed atCapo 36 Passero, Italy, at awith depth DOMs vertically of spaced 3500m. onof average ORCA about by will 20m. about comprise The 9 one detector m instruments building and about blocks with 8 DUs (115 Mton with DUs) of an sea horizontal water. distance It will be located at 42 PoS(ICRC2019)006 ) ]. σ δ 8 , ). α σ Rosa Coniglione ]. In the full sky 7 ) and 1 shower event ◦ (1 ◦ bins to search for clusters ◦ 1 × ◦ ] has been recently updated adding two ] were investigated. 6 ]. The post-trial value is of 16% (1.4 7 6 ]) is the optimal detector to look for extragalactic 3 5 and a post-trial value of 0.23 corresponding to 1.2 6 − ] and more recently updated with the addition of 5 more 6 . No new events in the sample of data from 2015 to 2017 ◦ at 1 PeV [ ◦ =343.5 α . Another interesting source among the Fermi 3LAC BL Lacs popula- ] using 11 years of ANTARES data. The different source populations con- σ 9 )) unchanged w.r.t. the analysis in Ref.[ ◦ the upper limit for the selected sources and the sensitivity, assuming a spectrum with 1 and right ascension were found. The same position in the sky was found with the same pre-trial value when ,5.81 ◦ ◦ ◦ , where all the sources are assumed to have the same flux. The most significant source dependence, are shown as a function of the source declination. Also reported (green line) σ 2 To increase the significance that would be observed for a single source, a stacking analysis An alternative approach is to search in the directions of a pre-selected list of candidate sources. The search for Galactic and extragalactic neutrino sources is one of the primary goals of an The ANTARES 9 years analysis presented in Ref.[ In Fig. The neutrino source detected by IceCube, the blazar TXS0506+056, was also investigated in − =+23.6 has been performed [ =(98.24 No excess of eventssteady was mode search found adding in two more bothdirection years of analyses of the ANTARES and blazar data and no upper upper further limits limits events were were in set found assuming in the different the flux spectral indexes. were set. In the This analysis has been presented in Ref. [ sources in a wide field of view. sources, recently observed, reaching aThe total highest of number 111 of Galactic cluster and extragalactic events candidate was sources. found at the location of HESSJ0632+057 (at ( sidered are: Fermi3LAC catalog containing414 1420 FSRQ, blazar, 15 a Dust sub-sample obscured offield AGN BL of and Lacs 65 (604 view sources), Radio-Galaxies. ofthe ANTARES Moreover, most 56 were significant IceCube population also events is considered. inof represented the by 1.6 the The Radio-Galaxies results withamong of a post-trial this the significance analysis FSRQ has populationRadio-Galaxies shown is of that the 2.5 3C403tion with is a the chance MG3J225517+2409J2255.1+2411) to that and classified has be as been casually BL Lac measured found and by LSP among (Low Fermi Synchrotron the (corresponding Peak) 56 and to with Fermi unknown red- 3FG a E is the sensitivity ofafter the 6 KM3NeT/ARCA years detector, of that observation.the will optimal allow The angular for KM3NeT/ARCA resolution (<0.1 detector an thanks increase to of the a high factor sensitivity 20 and to more years of data (up to December 2017) for a total live time of 3125 days [ high energy neutrino telescope.acceleration sites Different able to type produce of asearch neutrino for astrophysical neutrino flux objects sources through has have hadronic been interactions. been performed In following proposed ANTARES several the as approaches. steady mode with 9 years of data and time-dependent search and the results are reported in Ref.[ Mediterranean neutrino detectors 3. Point-like neutrino searches search all the sky in theof field neutrinos. of For view each of bin ANTARES is theis scanned significance, estimated. in based 1 on The the point likelihoodsδ in of the the signal sky and with background, the higher significance remains unchanged at declination was found and the pre-trial valuewas of assigned. 1.5 Around 10 the most significantwithin direction 5 18(3) tracks within 5 the directions of 75 IceCube track neutrino candidates [ PoS(ICRC2019)006 (right)). 1 ] and those ) was found 6 σ Rosa Coniglione (5.2 7 − and post trial value of 0.18. Moreover, ◦ ] (red dashed line) and the 6 years sensitivity 6 . Without including the IceCube ID3 event ◦ ]. This joined analysis increased of 30% the from the location of this source (Fig. 12 ◦ 4 (black) angular distances to the source. The nearby Fermi ◦ 1 δ ), extension 0 ). The probability to found by chance a similar excess ◦ σ ] were joined and analyzed to increase the sensitivity for sin 0.8 ). To explore more in details this source the emission light 11 (3.8 σ ]. With this sample of events different searches for cosmic 0.6 4 (red) and 5 12 − ◦ ,-40.798 ◦ 0.4 , 2 ◦ 0.2 ] lies at a distance of 1.1 10 0 ]). 9 ) =(213.51 ANTARES 9 years Sensitivity ANTARES 9 years Sensitivity ANTARES 11 years Limits (astrophysical candidates) ANTARES 11 years KM3NeT/ARCA 6 years Sensitivity 0.2 δ − , α 0.4 − the most significant sources identified in the different ANTARES analyses are re- 0.6 1 − -rays above 100 MeV has been analyzed. It was found that in a 5 months period (around Left - ANTARES upper limits for the investigated astrophysical candidates (blue dots) as a func- γ 0.8 − 1 The events in the Southern sky resulting from the ANTARES nine-years analysis [ In Tab. − 7 8 9 10 − − − −

10 10 10 ν

ν

d E s cm [GeV /dE ] ] 10

Φ

-1 2 -2 of the IceCube seven-years analysisthe [ search in theneutrinos Southern were sky performed. [ Inhas the coordinates full ( sky search57 the preselected most known significant cosmic pointNo objects in excess were was the selected found Southern and and sky a upper search limits in were these set directions [ performed. sensitivity of ANTARES that, despite thesearch limited of size, neutrinos from remains point-like the sources best in neutrino the telescope Southern for sky. the The IceCube EHE ID3 [ the pre-trial probability is 1.4 10 (for more details see [ Figure 1: tion of the source declination.from the The nine red years solid ANTARES line point-like shows source the analysis median [ sensitivity. For comparison, the curve shift. Five ANTARES events were found within 1 for KM3NeT/ARCA (green solid line)is are represented also by reported. a Right filledthe - circle event Blazar is with MG3 indicated a J225517+2409. by radius(black star the equal Each marker) color to event indicate code. the its 1 angularsource The 3FGL error concentric J2258.8+2437 estimate. circles is indicated (dashed The as lines)red-hashed a estimated circle centered empty energy with star around of a marker, the and black the diamond source range position marker. of of The the the ANTARES available events IceCube Fermi that track blazar do by light have the curve arrival are times circled within by the a bold black line. among the 1255 blazars iscurve 0.16 for (1.4 July 2010) the intensity hasthe flaring increased period of while about the adependent IceCube factor analysis EHE 5. combining ID3 the is No ANTARESflux detected ANTARES and is inside events produced IceCube were the continuously p-values, flaring found by assuming the period. in that source, a From the global a neutrino pre-trial time value of 2.2 10 Mediterranean neutrino detectors PoS(ICRC2019)006 ]). ) σ 12 ] for a (2.5) (1.4) (1.4) ∗ ∗ ∗ 14 post-trial ( Rosa Coniglione ] and even softer ], has evidenced a ) 15 σ 10 ( (4.8)(2.4) 0.23 (1.2) (4.8) 0.16 (1.4) 0.015 (2.4) (2.8)(3.7) 0.10 (1.6) (1.7) 0.013 (3.8) 0.64 (0.5) (3.7) 0.16 (5.2) 0.16 - (2.1)(4.3 ) 0.87 (0.16) 0.18 (1.3) (0.84) spectrum is assumed in 2 6 2 6 3 4 2 4 4 7 5 1 − ]. The sensitivity of the − − − − − − − − − 2 − − − 0.09) [ 13 ± pre-trial 3.4 10 1.5 10 1.5 10 1.5 10 4.8 10 2.3 10 8.8 10 1.4 10 1.4 10 2.2 10 1.3 10 4.0 10 ]. 9 =2.5 ] Γ (right)). ◦ [ - - 2 +2.5 δ -40.8 +23.6 +5.81 +23.6 +5.69 -39.75 +24.19 +24.19 +24.19 discovery potential for several Galactic , as well the pre-trial and post-trial values, σ α ] ◦ [ - - α 343.5 98.24 343.5 77.36 213.2 258.25 298.06 343.78 343.78 343.78 5 -rays and sites of proton acceleration as evidenced in γ ]. An alternative explanation is based on a two-component 3C403 Source 17 EHE ID3 , and right ascension, δ HESSJ0632+057 MG3J225517+2409 MG3J225517+2409 MG3J225517+2409 (left). The SNR RXJ1713.7-3946 can be observed with a significance are evaluated with the formula reported in [ 2 0.13 while in the analysis where high energy events are selected from all ∗ ± ]. No point-sources have been associated to date and since candidate source =2.13 Γ 16 observation can be achieved in 2.5 years (Fig. σ full sky ) in [ Analysis 33 9 candidate list Results from the ANTARES point-like search analyses. For each analysis the most significant . . Time Analysis TXS0506+056 IceCube tracks 0 3 + − within 5.5 years. Stacking the two most intense SNR sources the RXJ1713.7-3946 and the stacking Radio-galaxies stacking Radio-galaxies The detection of neutrino from Galactic sources is challenging for a neutrino telescope because Observed with statistically high significance in several IceCube analyses, a diffuse flux of ANT-IceCube RXJ1713 stacking 3LAC BL Lacs stacking 3LAC BL Lacs σ ANT-IceCube Southern sky =2.9 Time Analysis ANT-IceCube Γ selection of sources from the TeVCat catalogue. The 3 ( populations, as AGN and GRB cannot explainwas the suggested observed as excess, a an high explanation. number of [ weak sources of 3 Vela Jr. the 3 of their spacial extension andneutrino the energy spectrum. presence of The an mostThese energy promising are cutoff neutrino intense in Galactic emitters candidate the of sources TeV high are range energy the in SNR. the expected cosmic neutrinos can be now consideredup-going as tracks, a that mainly guaranteed look flux. for The neutrinos from results the obtained Northern by Hemisphere IceCube [ for are reported. Theall significance the (two-side analyses except convention) forperformed is assuming the also a RXJ1713 indicated. neutrino ANTARES-IceCube energy combinedThe spectrum analysis post-trial A with values (ANT-IceCube) slope E with that a 2.06 was and energy cutoff of 8.04 TeV (seeported [ together with the pretwo-sided and convention. post-trial probabilities and the correspondent sigma value in the 2013 by Fermi-LAT observations of theKM3NeT/ARCA SNRs neutrino W44 telescope and IceCube to 443 Galactic [ neutrino sources hassources is been reported evaluated in [ Fig. 4. Diffuse neutrino searches flux with a slope sky (mainly cascade events) a softer spectrum was evidenced ( Table 1: point in the sky, with declination, Mediterranean neutrino detectors PoS(ICRC2019)006 10 in the ] model σ . 8 1 22 − as a function ν sr 1 Φ Rosa Coniglione 6 − s 2 − ] adding data collected 4 cm 1 20 − Observation time [years] 2 GeV 18 − to the expectation flux KM3NeT σ 0 3 2 1 010

. the distribution for the energy estimator

Φ

1.8 1.6 1.4 1.2 0.8 0.6 0.4

1 ν σ 3 Φ / Φ 3 ± 5 . 1 (left) is the diffuse flux spectrum assumed in the 4 6 ) = 20 (left) (red band) together with the IceCube diffuse fluxes 4 100 TeV 8.7 events. In Fig. ( 0 ± Φ 15 and Galactic Centre Vela X Vela Jr HESS J1614-518 (1) HESS J1614-518 (2) RXJ1713.7-3946 ]. Recently the data set has been extended [ 4 4 . . 0 0 19 − + 10 3 ]. ] model for the conventional component and the Enberg et al. [ . 2 18 21 . For the cosmic flux the best fit parameters obtained for an unbroken power = σ Observation time [years] Γ 5 Energy estimator distributions for track-like events (left) and shower-like events (right) for the KM3NeT Ratio of the discovery potential for KM3NeT/ARCA 0 1 2

1.8 1.6 0.8 0.6 0.4 1.4 1.2

0 σ 3 Φ / Φ This spectrum is reported in Fig. ANTARES has already observed a small excess of neutrino with a significance of 1.6 from two different analyses. The redKM3NeT/ARCA line analysis in for Fig. the estimate of the number of years needed to observe an excess at from January 2016 toanalysis June of track 2018 and for shower events, a hasevents) selected as total 50 cosmic events livetime neutrino (27 candidates. of track-like The events 3350 and Monteassuming 23 Carlo days. the shower-like expectation Honda for [ the The background, analysis, simulated for the based prompt on component, is the offor 36.1 track like events (left) anda the significance shower-like of events (right) 1.8 are reported. The excess observed has law spectrum are: Figure 3: selected events. The red line showsthe the background cosmic contribution. flux as The estimated bluesimulation. in band this represents analysis the and systematic the uncertainties blue line of represents the MC background analysis of 9 years of data [ Figure 2: Mediterranean neutrino detectors of the observation time for theRX sources J1713.7-3946 reported and Vela in Jr the (right). legend (right) and for the stacking analysis including spectrum, with a softerextragalactic diffuse sources component [ of Galactic origin and a harder one originating from PoS(ICRC2019)006 level 3 -2 σ cm -1 s -1 ] and more sr -1 2.5 ]. No excess 24 Rosa Coniglione 28 2 combined track+shower - 2 blocks combined track+shower - 1 blocks exp(-E/3 PeV) GeV -2 1.5 Observation time [years] KM3NeT (E/1 GeV) -8 1 ]. The red line represents the diffuse 20 0.5 at 90% confidence level. flux per flavour 1.2 10 KRA 0

1

6 5 4 3 2 0

Φ ] [ Significance σ ]. The bubbles are large regions of the sky × 27 ] has been constrained. In the KRA model a (right). This estimate, based on combined track 4 ]. In this analysis the diffuse emission from the -ray emission along the whole Galactic Plane, as 26 7 γ 25 ], the green band from the IceCube 8 years up-going track 16 ]. The atmospheric neutrino flux is also reported (black dashed line). 5 , from this region has been tested assuming a 5 PeV and 50 PeV cutoffs KRA Φ ] and the red band from the ANTARES 11 years analysis [ Left - Diffuse signal fluxes as a function of the neutrino energy. The blue band represents the flux 23 The region around the Galactic Plane is an interesting region accessible with high visibility To explain the astrophysical high energy neutrino flux observed by IceCube, neutrino emission recently in a joint analysis with IceCube data [ by a neutrino telescope located inin the particular Mediterranean Sea. near Diffuse the flux GalacticConstraints from the on Center Galactic the is plane emission and expected from to the be Galactic enhanced plane has due been to set a from larger ANTARES [ matter density. for CR primaries. Noneutrino excess flux with of a events normalization has factor of been about observed 1.1 and thefrom upper the limits Local have superbubble excluded wall a was hypothesized [ Right - Significance as athe function red line of in time the forARCA right the detector figure, detection (2 for building of cascade-like blocks a and - track-like diffuse 330 combined flux DUs) events. and of the The neutrinos black blue corresponding line line to for is one for building the block full (115 DUs). Galactic plane estimated with the KRA model [ well as the hardening of CR spectraThe measured neutrino at signal, 250 GeV and the possible cutoffs of Galactic CRs. estimated from the IceCube HESE analysis [ nonuniform cosmic-ray (CR) transport scenario withbeen a adopted radially to dependent explain diffusion the coefficient high-energy has diffuse originated by the stellar wind from massivemedium stars creating that expanding an collides expanding with low thematter gas density density of bubble. interstellar and higher The magnetic wallsuperbubble fields. of that the overlaps The superbubble with presents theCosmic is higher nearby rays located Loop inside generated I a by superbubble superbubblegenerated sources forming neutrino. called a inside Local A wall the search of superbubble forcollected dense neutrinos can by material. from interact the the with ANTARES Loop1 neutrino region the telescope has wall over been region 11 carried out years and using of data data acquisition [ Figure 4: analysis [ and cascade events, hasdetector been made calculated of 2 for building two blockscan different (330 be DUs) detector reached and in configurations: only about one 1 the building year block complete of (115 data DUs). taking A with 5 the first block of 115DUs. flux assumed in the KM3NeT LoI [ Mediterranean neutrino detectors different significance levels that is reported in Fig. PoS(ICRC2019)006 - γ ] have been ]. This alert 29 31 Rosa Coniglione )[ ◦ 4 ) of the known Fermi < 1 hour around the GW ◦ | b ± | 10 < | and b | ◦ ] can be discovered with a large 30 500 s and and 26 < ◦ ± | ` | 15 < | ` | -ray satellites and to the H.E.S.S. high-energy 8 γ ]. Neutrinos from sub-threshold events (events with low signal ] as the expected neutrino flux from this region has a higher cutoff 34 ]. No counterpart has been detected until now. Also for the binary 30 35 ]. These real-time analyses have been developed to react in short time to the public 33 ]. 32 The real time searches of neutrino candidates in coincidence with Swift, Fermi, IceCube high ANTARES has implemented since 2009 a follow-up program of neutrino alerts [ The simultaneous observation in space and time by neutrino telescopes, gravitational waves The region around the Galactic Plane will also be a target for KM3NeT/ARCA. The expected . More than 300 alerts have been issued since 2009 and no counterpart detected in the different ◦ alerts sent by the Gamma-ray Coordinatedspecial Network (GCN) channels. or by Sources private alerts of transmittedwith neutrinos through the and following strategy: GW temporal have coincidence between been the searched from the O2 Ligo/Virgo run system consists of real-time triggerscurrently and implemented an are on-line based track onneutrino reconstruction (HE); the a algorithm. detection very high of The energy one (VHE)the triggers neutrino; sky; following a at events: neutrino least associated a two with neutrinos single specificof coming these directions high criteria, in from an energy close alert directions. is issued Whenand to SWOM) one robotic which event optical immediately telescopes satisfies start (MASTER, at the ROTSE, TAROT, ZDKO observation leastweeks. and one schedule the About observation 25 in the alerts following them per (about year 6 are per year) sent that tosatellites, satisfy these the to optical VHE the trigger ground Swift are based and alsoray telescopes. sent INTEGRAL telescope. to X-ray/ A the The MWA fraction low-frequency system radio of is0.5 able to send insearches about [ 6 s alerts for events with a resolution of about alert and a spacial overlap betweenregion the at 90% the GW time probability of contourto GW and noise the alert ratio) ANTARES [ from visibility Ligo O1and run IceCube were collaborations searched recently [ using HENneutron events star detected by merger ANTARES GW170817, for which electromagnetic counterparts have been observed, no energy neutrinos and Gravitational Wave (GW) eventspresented performed in with [ the ANTARES detector are reported for the track channelof and observation for the the neutrino cascade flux channel. predicted in In the both KRA the model channels [ after four years interferometers and multi-wave detectors (multi-messangerfuture astronomy) the is key and approach will forcosmos. be the in understanding the of next the most remote and extreme phenomena in the 5. Multimessenger and transient sources w.r.t the neutrino flux from theit entire has bubbles been region. estimated Considering that only theblock up-going expected of track-like flux KM3NeT/ARCA, events will even be considering observable the with case 5 of years a of pessimistic data cutoff of at one 100 building TeV. sensitivities for this region are really promising.flux The expectations from for a a diffuse Galactic high-energy Plane neutrino region near the Galactic Center ( Mediterranean neutrino detectors has been found and an upper limit 6.5 times larger than the reference flux was set. significance. The Low Latitude Bubble (LLB)Bubbles region was ( also considered [ PoS(ICRC2019)006 ≤ ]. M (left). 33 5 ≤ K decay. 40 ] has shown 37 Rosa Coniglione is achieved for a CCSN σ ]. With MC simulations and 36 is negligible for M> 3. As shown K 40 9 .

around the IceCube alert coordinate. Up to now IceCube ◦ (right)). ]. This trigger is already implemented and will assure, when ARCA and 5 36 ]. 3 decay and from atmospheric . The number of PMTs in a DOM with hits K 40 at 25kpc (Fig. (left), where also the signal expectation is reported for two different hypothesis of mass

5 An online trigger, based on the number of DOMs detecting a coincidence and passing the Consensus on the existence of is now shared between different communities but its Since 2016 IceCube also sends alerts when a high-energy starting events (HESE) or extremely From the experience gained in ANTARES the implementation of an alert system in KM3NeT The atmospheric rejection isM>4 operated at the selecting microsecond coincidence scale. between Thein different contribution DOMs Fig. of hits with from progenitors at 10kpc, the multiplicity range where the signal is expected is in the range of 6 M>4 selection, has been developedthe for SNEWS network the [ generation ofORCA real-time will alerts be and competed, the theGalactic participation participation CCSN to at of the mass SNEWS higher than network 27 with M the capability to detect a that high values of MAfter are due the to rejection atmospheric of muons atmospheric while low muons values the of multiplicity M distribution are due is to reported in Fig. 10. If we take intofor account all a the fixed DOMs progenitor inKM3NeT the mass detectors, detector as for a a a detection total significance function ofof can about of 27 be 6000 M the evaluated DOMs, CCSN a significance distance. of 5 Combining the two complete existence has not yet beenthe proved. direct The search experimental techniques and are theof grouped indirect dark in searches. matter two contributing main Indirect to classes: experiments chargedtrinos. search cosmic rays, for In photons particular, in or neutrino a decay wide telescopes range are of good energies, and tools neu- for the search of neutrinos produced in has issued 27 alerts, 11 of which have been followed by ANTARES without any detection [ 6. Indirect dark matter searches high energy track candidates (EHE) arethis observed. case, too The look ANTARES for strategy each fortime IceCube the alert of follow whose the up position alert is, is in and below the inside horizon a for cone ANTARES at of the 3 has already started. In particularsites the and online studies reconstruction for has theof been setting Core-collapse already of SuperNovae implemented specific (CCSN) in triggers has both among started. started the and In most the particular energetic online phenomena a trigger inneutrinos. study implemented. the The for Universe. CCSN optical the outburst are They detection begins are onlycenter intense hours transient of after sources the the of actual star onset MeV and ofthe neutrinos the are explosion "engine". a in the unique A very probe studydetect to to MeV get neutrinos prove direct from that and CCSN KM3NeT, immediate explosion thanks has information to been about the reported DOM in structure, [ is able to Mediterranean neutrino detectors neutrino counterpart was found by theAuger ANTARES Observatory and [ IceCube neutrino telescopes and the Pierre with the data collected with thehits first from strings CCSN deployed signal a from technique the that,are backgrounds in has hits each been from single developed. DOM, The selects backgrounds in this context in a time window of 10ns is called "multiplicity" (M). Data analysis reported in [ PoS(ICRC2019)006 (right) ]. The 6 channel 41 ¯ ν ν Rosa Coniglione ). At high WIMP γ - γ ] data. Very competi- ]. The neutrino energy ] and recently also first ]. The search was done 40 39 43 38 and the neutrino energy spectra ¯ ν ν , − ] track events, is shown in Fig. µ + 40 µ , − channel are reported. This limit is compared W − + τ 10 + W τ , − ] for the range of WIMP masses from 15 to 100 GeV τ ] and IceCube [ + channel yields as final product also 44 τ 42 , − ¯ b τ b limits on the thermally averaged cross-section for WIMP pair + τ 6 progenitors at 10kpc. Right - Detection significance for ORCA and ARCA

and 11 M

-ray detectors (the γ Left - DOM rates after muon rejection as a function of the multiplicity for background and signal (left) where the sensitivity is reported (dashed red line). 6 Limits for Dark Matter from the Sun has been set by ANTARES [ An effort to unify the analysis methods and the expected neutrino spectra was done in the com- Track events collected in 11 years of ANTARES data have been analyzed to search for neu- ORCA sensitivity have been estimatedshowing [ that the ORCA detector after only one year of data is a competitive detector. selecting the highest-yield channelsneutrinos. of The annihilation channel of selected are: WIMPs that lead directly or indirectly to upper limit, obtained from ANTARES [ for all the channels analyzedments and for the the NFW WIMP mass halo range model. froming 50 different The GeV data first to samples combined 1 and limits TeV. Further improving improvements show the are improve- analysis expected method. select- bined search for neutrinos from the Galactic Center with ANTARES and IceCube data [ annihilation set with 11 years of data for the for each annihilation and forspectra each depend on annihilation the channel assumed WIMP are mass, takenTeV. constrained Moreover, in from predictions this [ analysis of to the a maximum neutrinodepends value fluxes of on 100 deriving the from parameterization dark of matterconsidered the annihilation (NFW, dark Burkert, strongly matter McMillan) density. and In theand most our the stringent analysis NFW limit three halo is halo model. obtained models In for are Fig. the with limits of tive limits are expected for ARCAin full Fig. detector (230 DUs) after one year of observation as shown Figure 5: the annihilation of Weakly Interacting Particles (WIMPs)density accumulated such in as cosmic the regions Galactic with Center high (GC) and the Sun. trinos originated in the annihilation of WIMPs in the Galactic Center [ expected for a 27 M detectors as a function of the CCSN distance. Mediterranean neutrino detectors masses the most stringent limitsIceCube are upper that limit one was obtained of with HESS 3 collected years in of 10 IceCube86/DeepCore years [ of observation. The PoS(ICRC2019)006 ]) for ]. The 45 ◦ , 50 ◦ Rosa Coniglione [40 appearance have ]. In this region 5 ∈ CC τ ν 23 θ 25% and a zenith angle ≈ was assigned as prior. The 13 θ and for ] and Non-Standard Interactions π 46 = CP δ 0 and ), for direct and inverse mass ordering reaches µ = 11 ν , e CP ν δ and the normalization factor of the has been also determined (for analysis details see [ ) (x= 23 23 µ θ were fixed during fitting and θ ν 2 2 12 → θ x channel he obtained limits are also compared with current similar searches ν and and sin and sin − τ 2 21 2 32 2 32 + = 10 GeV for shower and track events. The identification between track m τ (left) for three years of observation show that the highest sensitivity (about m m -ray telescopes. The sensitivity for the KM3NeT/ARCA detector is also reported ν 7 ∆ ∆ γ ∆ at E ] as well as the sensitivity for [ ◦ ) for the rejection of the other ordering is seen if normal ordering is assumed with 5 45 ◦ ≈ 50 = ]. Left - Limits on the thermally averaged cross-section for WIMP pair annihilation set with 11 years 23 θ 47 The sensitivity to The energy range of interest for the NMO is between about 5-15 GeV [ The main aim of the KM3NeT/ORCA detector is the study of the fundamental properties of = 0. for σ CP the oscillation probability, P( 5 δ three years of observation with thewith ORCA the full detector ORCA (115 7 DUs)upper and DU limits for detectors, from one other year that experiments of are is observation reported. planned After to only three be years deployed of observation the ORCA next can year. For comparison (NSI) [ its maximal difference. Theenergy key and ingredients zenith angular related resolutions to and thetrack-like the ability events. detector to experimental ORCA distinguish features the will shower-like are provide events the from a the neutrino energy resolution of Figure 6: of ANTARES data for the Mediterranean neutrino detectors from IceCube and from been estimated [ resolution of oscillation parameters for 1 year of observation. Rightfor - the Limits combined on analysis the thermally ANTARES IceCube averaged cross-section for for all WIMP the pair channels annihilation analyzed. 7. Neutrino oscillation studies the neutrinos through the measurementEarth. of The expected the performance oscillation for the of measurementsoscillation atmospheric of parameters the neutrinos Neutrino traversing Mass Ordering the (NMO), the and shower events is performed with aof Random 80% Decision of the Forest track resulting events in and awhere 90% correct for the identification shower hypothesis events. The of analysis Normal isvice based Ordering on versa. (NO) pseudo was experiments tested The against calculation the was Inverse done Ordering (IO) for and results reported in Fig. PoS(ICRC2019)006 τ σ ν . Devi- CC τ ν N Rosa Coniglione ] and sensitivities from 0 can be excluded at 3 48 = normalization, CC τ ν CC τ N ν ]. Significant distortions in the atmo- ]. 46 45 3 neutrino mixing matrix and then a hint × the full ORCA detector after 3 years of observation and 12 23 5. For ORCA 7 DUs ), experimentally is observed as an excess of shower . θ τ 0 2 ν − → < µ θ and sin ν 2 32 cos m ∆ space significantly and even if with a small detector first additional 20-30 GeV. Upper limits from ANTARES [ 23 ≈ θ ν 2 E appearance, P( 20 GeV and - sin 1 indicates a non unitarity of the 3 τ ≈ ν 2 32 = ν m CC τ ∆ ν N ] to sterile neutrinos in the (3+1) model show that ANTARES has excluded values of the Left - Sensitivity for the NMO measurement of the KM3NeT/ORCA detector after 3 years of 46 Building on the experience gained with the ANTARES neutrino telescope and other projects The first DU (DU1) of the ARCA detector was deployed in December 2015, followed by two A study to search for the existence of sterile neutrinos with ANTARES and the estimate of An interesting results is also the estimated sensitivity for the like events for E spheric neutrino oscillation pattern in the presencesignal of in light the sterile ANTARES neutrinos and are expected. ORCAin The detectors the main energy is range an of expectedORCA excess [ of up-going track-like events in the Mediterranean Sea, the KM3NeTof collaboration, innovative optical after sensors an and R&D Detection programand Units, for ORCA started the sites. to construction deploy the first strings on both ARCA in May 2016. One ofIn the the units period deployed May in 2016problems May April 2016 in 2017 was the the recovered detector network for was infrastructurehave inspection operational been in at with on July the two hold 2016. DUs. seabed, since(DU1) April the Due working. 2017 operations to and electrical at successfully the restarted KM3NeT in January Italian 2019 site with only one DU parameter space not yet excluded bythree other years experiments of and data that taking the can ORCA constrain 115 significantly DUs the detector present after allowed phase space. 8. KM3NeT status and first results the expected sensitivity for ORCA has been presented in [ ation from interactions. The significance after approximately 6 months of data taking [ Figure 7: observation. Right - Sensitivity to ORCA sub-array of 7 DUs after 1 year. For comparison upper limits from other experiments are reported. Mediterranean neutrino detectors constrain the for new physics or significant deviations from the predicted cross-section for charged-current inputs can be provided. PoS(ICRC2019)006 ]. 50 (right)). 8 Rosa Coniglione ], testing the pro- 49 K backgrounds. The 40 8 (more than 8 PMTs with ≥ M ] and comparing MC simulations with the 50 ]. 49 ] among the large number of atmospheric muons. 13 52 ]. Moreover, even if data are collected with few strings it (left) the coincident rate as a function of the DOM depths 8 51 ]. In Fig. 37 8 coincidence rate of all DOMs as function of depth below the sea level. Left -The ≥ ] model predicting the depth dependence of atmospheric muons (Fig. 55 Multiplicity The features of a multi-PMTs sensor as the KM3NeT DOM (31 3-inch PMTs inside a glass The calibration of an instrument that cannot profit of calibrated sources or mono-energetic The first DU of ORCA (ORCA1) was installed in September 2017 and operated until mid- The first data collected has allowed checking the calibration procedures [ discriminating power is mainlythe achieved same by DOM. exploiting In coincidences thisa between analysis, time different a window PMTs coincidence of in is 15hits defined ns. as in a coincidence The sequence in coincidence ofa a rate hits DOM-by-DOM DOM) in for basis is a multiplicity [ DOM used within to select a high-purity sample of atmospheric muons on for ORCA and ARCA before thetection correction efficiency (blue (red points) points) and are afterdetection reported. the efficiency correction The has for been depth the evaluated range PMT onwith explored de- a the is Bugaev run-by-run about [ basis. 1.2 The km. corrected The values PMT are compared The number of photonsformation arriving are in used a to single discriminate DOM signals from together atmospheric with muons the and direction and the time in- coincidence rates for the ARCA2 andcorrection ORCA1 for detectors the are reported PMT as photon measuredreported detection (blue as efficiencies points) a (red and function after points). of the flux Right- the (black The depth line). corrected (red coincidence points) rate and is fitted with the Bugaev model of the atmospheric muon sphere) were exploited measuring the atmospheric muon rate as a function of the sea depth [ particle beams is a complex procedures.a good To angular achieve resolution, a the nanosecond in time situdescription accuracy, and of required off-shore the calibration to procedures procedure have are have reported been in optimized. Ref. The [ Figure 8: In this section some relevant results are reported. measured atmospheric muon events [ has been possible to select up-going neutrinos [ December 2017, when a failureunderwater of detector. the After main the electro-optical replacement cable oflatest made a one it part in impossible in June to 2019, the power 4 main the DUs cable are and now two being sea operated. campaigns, the Mediterranean neutrino detectors cedure to correct the data for the PMT inefficiency [ PoS(ICRC2019)006 8 . 0 < ) ] with elec- zenith 1 θ ( Rosa Coniglione cos (left) for the ORCA1 K decays, is verified. 9 40 ] and neutrinos [ 3 14 ]. The reconstructed zenith angle is shown in Fig. 52 Reconstructed zenith distribution of ORCA1 events (left) and ARCA2 events (right). Figure 9: The neutrino detectors located in the Mediterranean Sea can effectively contribute to a more The data collected with 2 DUs of ARCA (ARCA2) (livetime 53 days) and ORCA1 (livetime Due to their extremely low interaction cross section, neutrinos can escape from dense source precise observation of the high-energyvery good neutrino angular flux resolution thanks both to forneutrino telescope cascade their constructed and off wide track shore field the events. coast ofplete ANTARES of was Toulon view configuration (France) the and from and first it May their is undersea taking 2008. data in A its large com- variety of analyses has been carried out during these and right for ARCA2.from The MC measured distribution simulations. in data Forsample, is ORCA1, while in 77 67 good neutrino events agreement candidatesatmospheric are with are muon expectations expected simulations. observed from From in the atmospheric MC theevents neutrino simulation considered has have simulations been data an and shown that average 4 the energyneutrinos selected events is neutrino of from more a challenging due few to tens theeffective livetime higher analyzed. of neutrino For GeV. energy ARCA2 detection With 6 threshold neutrino ARCA2, and candidates the the with smaller reconstructed search for atmospheric tromagnetic radiation has enforcedmessenger the can belief shed light that on only the energetic a non-thermal sources detailed in observation the of Universe. all the cosmic 123 days) were reconstructed with a tracklect reconstruction up-going algorithm neutrinos and [ analyzed with the aim to se- environments and, being not deflectedoriginal direction. from Moreover, magnetic the field, simultaneous observation can of reach GW [ the Earth preserving their Mediterranean neutrino detectors The very good agreement (RMS ofable deviations to within distinguish 2%) muons proves that from a backgroundtime single and offsets DOM that and is the PMT a calibration "detector" detection procedure to efficiency, based estimate on the coincidence PMT hits from are found in the consideredsimulations data and sample 0 while events 3.3 from eventsa atmospheric are typical muon expected energies simulations. from of atmospheric The few neutrino selected hundredsa neutrino of very events low GeV. The number show results of of strings this the analysis selection of have candidate proven that neutrino events even is with 9. possible. Conclusions PoS(ICRC2019)006 Rosa Coniglione . A time dependent σ ) 5 ANTARES tracks lie and it is fully compatible ◦ 1 − sr 1 − s = 343.78 2 α ). The estimated spectrum has a slope − σ cm and 1 -sources can be achieved in few years. ◦ − γ GeV 15 (before 1.6 =+24.19 18 σ GeV. In this work the most relevant results achieved − δ 8 ]. A mild excess of neutrinos above the background level (full sky search). This point is coincident with the blazar 19 ◦ 1.0 10 ± = 343.5 α of some of the most intense and ◦ σ (100 TeV)=1.5 0 Φ will be instrumented with a geometry that has been optimized for the detection =+23.6 from the source. In addition, one IceCube high energy events was present within 3 δ and ◦ 4 4 ) for the chance coincidence of observing such an association between ANTARES and . . 0 0 σ − + level can be achieved after less than one year of observation. (5.2 from the source center. The estimated post trial significance is of 1.4 σ The search for neutrinos from point-like sources was also addressed by ANTARES with sev- The discovery of Galactic neutrino sources can be addressed by KM3NeT/ARCA detector. ANTARES has also an intense activity in the multi-messenger physics, which will be further KM3NeT is taking data with the first 4 DUs installed in the ORCA site and 1 DUANTARES will in continue the data-taking until end of 2020 when KM3NeT will start to have a In the search for neutrinos from a diffuse flux the analysis adding two further years of data =2.3 7 ◦ Γ − eral analyses. Even if nosky significant has excess been of events put has in beendeclination evidence found, and of one studied interesting more region in of detail. the This region is located in the north sky at 1.1 Thanks to the high effective areas andsignificance the of good about visibility 3 of the Galactic plane the discovery with a extended by KM3NeT. A real-time follow up programand of also the many alerts analyses from for GCN counterpart is already searches well have tested been already published. ARCA site. Analyzing the firstthe data detector, has a proved validity the of robustness the ofresponse. simulation procedures chain for and the in calibration general of a good understanding of the detector significant instrumented volume thus assuringNorthern a hemisphere. continue monitoring of the neutrino sky from the of with the IceCube measurements. The diffuseconfirmed flux with will a be high one significance by of KM3NeT/ARCA.the the It 5 first was measurements estimated that that can with be the full detector MG3 J225517+2409. Around thisat source less than ( 1 analysis for this source has provided10 a preliminary estimation of a pre-trialIceCube probability neutrinos of in about space 2.2 and time correlation with the blazar. has been observed with a significance of 1.8 Mediterranean neutrino detectors years spanning from neutrino oscillation studies tothe searches next for future neutrinos to from continue different sources. andis improve In constructing the two measurements neutrinos of detectors neutrinos in theof the KM3NeT Mediterranean collaboration about Sea. 1 With km KM3NeT/ARCA a volume of neutrinos of astrophysical origin.deployed off A shore denser the instrumented Toulonneutrino coasts detector, oscillation far KM3NeT/ORCA, properties. about is 10 being With kma these from wide two the energy detectors ANTARES range it detector, from will to be few study possible GeV the to to study 10 neutrinos in has reinforced the results presented in [ by ANTARES after 11 yearsKM3NeT of neutrino data detectors taking also have reported. been presented and the expectation for the next PoS(ICRC2019)006 43 , Rosa Coniglione 031101 (2017). 119 , L20 (2018) , Number 7 (2018). 868 853 , 807 (2013). 11 (2011). Phys Rev. Lett. 100 (2019). 339 , L19 (2018). 656 Astrophys.J. 111 , Number 2 (2017). 861 043005 (2008). , 2 (2017). 98 (2015). 848 3 (2016). , 78 082001 (2017). 835 809 833 96 , 147-151 (2018). 103006 (2016). 16 , L30 (2018). 94 361 Journal of Physics G: Nuclear and 863 615 (2018). Phys. Rev. D Astrophys. J. Astrophys. J. Science Nucl. Instrum. Meth. A Astrophys. J. ApJL Phys. Rev. D The Astrophysical Journal Letters 043006 (2077). A168 062001 (2017). Phys. Rev. D 75 96 A.A. The Astrophysical Journal Letters The Astrophysical Journal Letters Phys. Rev. D Phys. Rev. D , eaat1378 (2018). 361 084001 (2016). Kiso, Kapteyn, Liverpool telescope, Subaru, Swift/NuSTAR,Science VERITAS, and VLA/17B-403 teams, [5] Adrian-Martinez S. et al., (KM3NeT coll.) [4] Ageron A. et al., (ANTARES coll.) [6] Albert A. et al. (ANTARES Coll.) [7] ANTARES Coll. PoS(ICRC2019)920. [8] Albert A. et al., (ANTARES Coll.) [9] ANTARES Coll. PoS(ICRC2019)840 [3] Abbott B.P. et al., [1] The IceCube, Fermi-LAT, MAGIceCube, AGILE, ASAS-SN, HAWC, H.E.S.S, INTEGRAL, Kanata, [2] Aartsen M.G. et al. (IceCube Coll.) [11] Aartsen M.G. et al. (IceCube Coll.) [12] ANTARES and IceCube Coll. PoS(ICRC2019)919. [13] Ackermann M., et al., (Fermi-LAT Collaboration) it Science [22] Enberg R., Reno M.H. and Sarcevic I. [10] Aartsen M.G. et al. (IceCube Coll.) [14] Aiello S. et al., (Km3NeT Coll.)[15] itAartsen Astroparticle M.G. Physics et al. (IceCube Coll.) [20] ANTARES Coll. PoS(ICRC2019)891. [21] Honda M. et al., [16] IceCube Coll. POS(ICRC2017)981. [17] Murase K. and Eli Waxman E. [18] Palladino A. and Winter W. [19] Albert A. et al. (ANTARES Coll.) Mediterranean neutrino detectors References [23] Icecube Coll. PoS(ICRC2017)1005. [24] Albert A.et al., [25] Albert A. et al. (ANTARES and[26] IceCube Collaborations), Gaggero D., Grasso D., Marinelli A.,[27] Taoso M. andAndersen Urbano K.J. A. et al., [28] ANTARES Coll. PoS(ICRC2019)892. [29] KM3NeT Coll. PoS(ICRC2017)998. [30] KM3NeT Coll. PoS(ICRC2017)870. PoS(ICRC2019)006 Eur. Phys, 014016 (2019) Rosa Coniglione 64 Phys.Lett.B Phys. Rev. D 69-75 (2016). 122010 (2016). ANTARES, IceCube 76:54 (2016). 113 (2019). (2017). 759 93 06 , 5530-536 (2012). 249 (2017). Erratum: 77.627 35 769 17 Phys. Lett. B 915 (2008). Eur. Phys. J. C Phys Rev. D. 179 022005 (2017), Albert A. et al. (ANTARES Coll.) Eur. Phys. J. C 96 Astropart.Phys. J. High Energ. Phys. , Phys. Lett. B 054001 (1998). Klimushin S.I. et al., 58 051 (2011). [Erratum: JCAP1210,E01(2012)]. Phys Rev. D. 1103 Comp. Phys. Comm. Phys.Rev.D JCAP 77 (2017). ANTARES Coll. (PoSIceCubeRC2019)856. 911 (2001) . PoS(ICRC2019)943. and LIGO-Virgo Coll. J. C [43] Adrian-Martinez S. et al., (ANTARES Coll.[44] ) KM3NeT Coll. PoS(ICRC2019)536 [45] KM3NeT Coll. PoS(ICRC2019)1019 [46] KM3NeT Coll. PoS(ICRC2019)870 [47] KM3NeT Coll. PoS(ICRC2019)931 [48] Albert A. et al., (ANTARES Coll.), [49] KM3NeT Coll. PoS(ICRC2019)932. [50] Ageron M. et al., (KM3NeT Coll.) https://arxiv.org/pdf/1906.02704.pdf and KM3NeT Coll. [51] KM3NeT Coll. PoS(ICRC2019)927. [52] KM3NeT Coll. PoS(ICRC2019)910. [53] Carminati M. et al., [54] CORSIKA web page. Available on http://www.ikp.kit.edu/corsika/. [55] Bugaev E.V. et al., [35] ANTARES Coll. PoS(ICRC2019)984. [36] KM3NeT Coll. PoS(ICRC2019)857 [37] Adrian-Martinez S. et al., (KM3NeT Coll. ) Mediterranean neutrino detectors [31] Ageron M. et al. (ANTARES Coll.) [32] ANTARES Coll. PoS(ICRC2019)871. [33] ANTARES Coll. PoS(ICRC2019)872. [34] ANTARES, IceCube and LIGO-Virgo Coll. [38] ANTARES and KM3NeT Coll. PoS(ICRC2019)552 [39] Cirelli M et al., [40] Aartsen M. G. et al. (IceCube[41] Coll.), ANTARES Coll. PoS(ICRC2019)522 [42] Albert A. et al. (ANTARES Coll.),