PoS(ICRC2015)002 http://pos.sissa.it/ ∗ [email protected] Speaker. With the recent discovery of high-energy neutrinostrino of observatory, extra-terrestrial origin neutrino-astronomy by is the entering IceCubeserved neu- a to date new exceed era. 1 PeV in The energy,point a highest back regime to of energy the particular neutrinos interest still because elusive ob- the acceleratorsrays. neutrinos of should the This highest review energy will Galactic and coverresults extragalactic currently from cosmic operating searches neutrino for telescopes a in fluxsteady of water and transient extra-terrestrial and neutrino neutrinos ice, point and the sources. currentMediterranean latest In efforts Sea addition, in and future the plans detectors for search such IceCube for as detector KM3NeT upgrades in will the be discussed. ∗ Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-ShareAlike Licence. c

The 34th International Cosmic Ray Conference, 30 July- 6 August, 2015 The Hague, The Netherlands C. Kopper Department of Physics, CCIS 4-181, UniversityCanada of Alberta, Edmonton, Alberta T6GE-mail: 2E1, Recent Results in Neutrino Astronomy PoS(ICRC2015)002 ) ]. γ 7 2 ]. It 5 → . Vari- 1 0 − C. Kopper π sr 1 − s 2 − GeVcm 8 − 10 · 3 ≈ Φ 2 E ] and a full overview of highlight results in decays in the atmosphere above a detector 3 K of 1 : 2 : 0 is expected. Due to oscillations, this and 2 τ ν ]. π 6 : µ ν : e . While neutral pions decay into two gammas ( 0 ν π p → γ p ], neutrino-astronomy is entering a new era. Even long before this discov- 2 and , ] can be found later in these proceedings. 1 + 4 π n → γ p All backgrounds to astrophysical neutrino detection are due to interactions of cosmic ray air Given the abundant number of observed high-energy hadronic cosmic rays, a flux of neutrinos A rough estimate of the neutrino flux expected (assuming a proton-only cosmic ray injec- With the recent discovery of high-energy neutrinos of extra-terrestrial origin by the IceCube This article will give a brief overview of neutrino flux expectations, of current and future detec- The flavor composition of the atmospheric neutrino flux is heavily biased towards muon neutrinos and create a flux ofcharged-pion high-energy decay, gamma a rays, flavor charged ratio pions of eventually decay to neutrinos. From showers. ‘Atmospheric muons’, produced by from interactions of these cosmic raysinteractions with can ambient either matter and happen radiation ata fields a high-energy is proton source expected. interacting or These with duringcesses a propagation target like through photon space. will yield As charged an and neutral example, pions in pro- 2. Neutrino Flux Expectation sets an upper bound for the all-flavor flux of neutrinos at can penetrate to reach thesame detector, interactions also even produce through neutrinos substantialmospheric that amounts neutrinos’ enter are of the seen shielding detector at a material. from lower above rate The and due below. to the These lower ‘at- neutrino interaction cross-section [ tion, a purely extra-galactic origininto and neutrons considering and only a charged single pions) interaction is of provided protons by converted the so-called ‘Waxman-Bahcall bound’ [ neutrino astronomy [ corresponds to a flavor ratiolarger at than Earth the of oscillation approximately length 1environments scale. : such 1 as The : in expected 1 the ratio presence assuming can of a strong change source magnetic in distance fields. case much of different source neutrino observatory[ ery, neutrinos have been targetedthus as escape ideal from cosmic dense messengers: astrophysicalThey environments they are that only not are interact affected opaque weakly by to andpaths, Galactic electro-magnetic can and pointing radiation. intergalactic back magnetic to fields theirEarth and sources. provides will insight thus Measuring into travel high-energy in aexplosions straight astrophysical large to neutrinos number acceleration arriving of processes at astrophysicalhadronic in phenomena, processes, active ranging galactic they from can nuclei. supernova cosmic also rays. Because help Finding they to a are solve classsmoking only the of guns created 100-year for Galactic the in and/or old acceleration extra-galactic mystery sites neutrino of of sources cosmic the would rays. make acceleration them of tors, the detection principle andrecent various results detection and channels. briefly touch It on future willof detectors. then the A highlight high-energy discussion astrophysical a of neutrino the few observation multi-messenger important [ connection Recent Results in Neutrino Astronomy 1. Introduction ous detailed model predictions aregamma-ray available bursts for and active a galactic wide nuclei range [ of potential source classes, such as PoS(ICRC2015)002 charged- C. Kopper µ ν ]. At higher energies 8 higher than the rate expected from CC interactions, a high-energy muon 6 τ ν 10 ]. For equal neutrino fluxes of all flavors ≈ 10 , 50% CL in ice, better in water) than for those ◦ 1 3 . ]. 11 , 50% CL in ice, better in water) [ mesons decay overwhelmingly to muons rather than electrons. Because of the ◦ K 15 ]. ∼ 13 CC events make up only 20% of interactions. Tau neutrinos can have other signatures, , and µ π 12 at lower energies are on-going [ ν ]. This ‘prompt’ atmospheric neutrino flux has not yet been observed and is only poorly τ 9 ν [ In order to detect a flux on the order of the Waxman-Bahcall bound within a few years, detec- Because muons at the relevant energies can travel over distances of several kilometers, one K / (1:1:1), such as “double-bang” events withbe two detectable showers close at to the each PeVfrom other. level, Such have not signatures, yet expected to been observed. Searches for double-pulse signatures tors on the scale of a cubicof kilometer natural are transparent necessary. Building medium, such such detectorsdetectors: requires as Neutrinos large water are amounts detected or by ice.created observing when the The neutrinos Cherenkov principle interact. light of These produced particles detection byindividually generally charged is and travel particles similar the distances too for particle small all shower to (or be ‘cacade’) resolved is observed only in aggregate. In way to look for neutrinoswhelming is to number search of for down-going track atmospheric events muons entering ( the detector. To suppress the over- of about 100TeV a similarpected flux to of become muons important. and Because of neutrinosinteraction the from before shorter the lifetime decay decay of is these of expected, particles, leading charmedπ no to mesons suppression an is from expected ex- cross-over with the neutrino flux from 3. Detection Principle current (CC) interactions, however, as well as ais minority produced of that leaves a visible trackAlthough (unless the produced deposited on energy the resolution detector boundary iscontaining heading similar visible outward). for muon all tracks events, is the much angular better resolution ( for events neutrinos) only up-going events in the detectoragainst are selected. the This atmospheric effectively muon uses the background. Earthin to Atmospheric this shield case. neutrinos They are need an to be irreduciblespectrum included background and in angular analyses on distribution. a statistical Thesample basis other and is main described to by way use their to the energy select outeratmospheric a layers muons reasonably of will pure the be neutrino detector rejected as event pass while an the neutrinos anti-coincidence veto. veto. interacting inside Incoming This tracks thechannel from significantly detector described will reduces above be but the it able effective allows to The detection to veto volume detect will compared all even suppress three to some flavors thetriggered of and by “track” the allows muons down-going for traveling atmospheric all-sky in neutrino observation. coincidence flux withshower because [ the the neutrino veto generated is in the same cosmic ray air constrained at the moment. that do not ( Recent Results in Neutrino Astronomy because increasing lifetime of the parent mesonsatmosphere with increases. increasing energy, This their leads interaction probability toimately in a one the suppression power at steeper high than energies the producing original a primary spectrum cosmic approx- ray spectrum [ PoS(ICRC2015)002 C. Kopper ]. 19 . ANTARES and the 3 01km . ] and the ANTARES neutrino tele- 15 4 ]. The discovery of two PeV energy cascades in a two-year 21 ]. ]. It was deployed between 2005 and 2010 and consists of 86 strings with 17 ]. ], the NEMO project close to Sicily [ 18 16 14 ] and in the cascade channel [ Before the discovery of the astrophysical neutrino flux mentioned earlier, hints of it had been Another neutrino detector, NT200, is deployed in Lake Baikal using the frozen lake surface Currently, the largest neutrino telescope is the IceCube neutrino telescope, located at the geo- Several large-scale neutrino telescopes are currently in operation around the world. All of In the Mediterranean sea, several efforts were started at different sites: the NESTOR project off 20 seen in various analyses of data ofnel the [ partially completed IceCube detector, both in the track chan- 5. Neutrino Searches 5.1 Diffuse Neutrino Flux Searches search for GZK neutrinos (from cosmic raysground) interacting provided on the photons first of concrete the evidence cosmicwere for microwave back- too an astrophysical low flux. for Theprovided a detected further event GZK evidence energies for flux an but unaccountedfor component higher in events than the with expected measured the flux. from neutrino A atmospheric vertex dedicated inside search backgrounds the and detector thus using the outer layer of optical modules as 5160 optical modules in total.1450m The and instrumented 2450m. volume isantarctic Unlike a glacier. the cubic water-based The kilometer detectors at detectorthreshold described a contains for previously depth a neutrino it between denser physics is sub-array studies deployedcomplemented called by using in DeepCore an the the lowering air-shower atmospheric array the on neutrino energy the flux surface as of the a glacier source. called IceTop It [ also is during the winter as awith 192 deployment optical platform. modules in total This wasstrings version completed with of in 12 1998. the modules An detector upgrade, eachthan NT200+, consisting was adding ANTARES, of three deployed but 8 more in a strings 2005. futuredeployed in gigaton The early upgrade currently 2015 operating is [ detector planned is and smaller a first cluster of this upgrade was scope off the coast of France.and While future the deep-sea first neutrino two detector projects technology, madea the significant large-scale ANTARES contributions collaboration detector to has current in been operating stable12 conditions vertical “strings” for with several 25 years.mented storeys volume of The of consisting ANTARES the of detector detector, three completed consistsfuture optical in of Mediterranean 2008, modules cubic-kilometer is each. detector approximately The KM3NeT 0 are totalin highlighted instru- these in prcoeedings a [ separate contribution graphical South Pole [ these use the samenatural detection water principle or ice for with Cherenkovpressure-resistant a light: glass three-dimensional housings, array they of so-called instrument photomultiplier ‘opticalarrival time tubes a modules’. and (PMTs) large amplitude contained These volume of in optical photons. of of modules Dedicated water record algorithms or use the ice a (scattering,energy model absorption in of and the the detector. noise) optical to properties reconstruct the event direction, topologythe and coast of Greece [ Recent Results in Neutrino Astronomy 4. Neutrino Detectors PoS(ICRC2015)002 ]. 24 (5.1) C. Kopper . 1 − sr 1 − s 2 − level against the atmospheric- σ IceCube IceCube Preliminary GeVcm 3 25 . > 0 ± 58 . 0 − ) 5 100TeV . Assuming a 1:1:1 flavor ratio and a 1:1 neutrino to / 1 E ( 8 shows limits set on the flavor composition by this global − 3 10 × 7 . 0 ]. Fig. ± 2 25 . 2 ]. A follow-up extending this analysis to three years of data increased the 1 ) = ), 6 total years of IceCube data have now been analyzed and results will be 2 E . Continuing this analysis with a fourth year of data increases this significance ( σ φ 7 2 . ] in these proceedings). A total of 54 events are detected in the whole 4-year sam- E ]. 22 22 Deposited energies of the observed events in four years of the high-energy starting event search ] (see Fig. 23 [ Searches using the track channel using incoming muons entering the detector from below have σ 7 . fit. Some source flavor compositionneutrinos is models expected such at as the neutron source, decay, are where already excluded a by pure this flux analysis. of electron now also confirmed this result inyears an of almost IceCube independent data channel. which Starting3 found from a an component analysis beyond of atmospheric two background expectations of anti-neutrino ratio, the best fit per-neutrino flux for a sample of four years of data is The choice of 100TeV as thethe pivot normalization. point minimizes It the should correlationBahcall between also bound, the be although spectral the noted index spectral and that index the and normalization detected are flux still is uncertain. on the order of the Waxman- published soon. Results fromAll a these 3-year searches sub-sample confirm canuncertainties be the on found the flux spectral later detected shapes in and inIceCube these on the flavor analyses proceedings composition. starting has [ A event dedicated been “global channel. performedto fit” in answer to There multiple order these are to questions still use [ as large much available information as possible ple. Their energy spectrum is shown in Fig. Figure 1: in IceCube. [ a veto (as explained above) finally provided evidence on the significance to 5 further (see [ Recent Results in Neutrino Astronomy only null-hypothesis [ PoS(ICRC2015)002 C. Kopper 6 10 5 10 Astrophysical ). Although not significant, the apparent Experimental data Experimental Sum of predictions 5 Prompt atmospheric 4 Conventional atmospheric 6 10 ] 23 Muon Energy Proxy (arb. units) 3 10 ], but neither has found significant clustering at any position on the sky. An near the galactic center has been studied in detail by ANTARES. Their field of 27 , 5 1 0 4 3 2 -2 -1 26

10 10 10 10 10 10 10 Events Distribution of a muon energy proxy variable of the final event sample used in a two-year track- . Note that these point-source samples are dominated by atmospheric backgrounds in order 4 The next step after detection of an astrophysical neutrino flux is to attribute it to sources or view for track-like events includes thislower region energies. and None allows of them these to searches extend have searches found for significant clustering. clustering to More recent point-source clustering in Fig. source classes. The moreclustering traditional in way the sky. to These do searchesand this are atmospheric is dominated neutrinos by to atmospheric for use muonssuch the up-going for searches down-going “track” events. [ events channel and Both search ANTARES for and IceCube have performed 5.2 Point Source Searches overview of current limits on neutrino pointin sources Fig. from both ANTARES and IceCube canto be seen allow as much low-energysitivity signal to as clustering possible (under to the belaws). accepted, assumption In which that principle, in neutrino searches for turn source point maximizesportional spectra sources to the are in the sen- neutrinos steeply-falling square should power root have of theirthan observation sensitivities that time. scale because Up pro- of improvements to in this analysis pointreconstruction technique in techniques (such time as (mostly the the improvements inclusion scaling in of has reconstruction eventhas been quality/angular energy) faster also and error). performed IceCube a clusteringlier. study Even though using this the sample should high-energy beangular starting-event signal-dominated, resolution sample the of described limited shower-type amount ear- events of limits statisticsany the and significant sensitivity poor clustering of after this trial-correction search which (see has Fig. not yielded Figure 2: based study of thephysical diffuse component neutrino are flux. shown as Best-fitseen colored at contributions lines. the of high-energy atmospheric An end excess of backgrounds the above and distribution. atmospheric an [ expectations astro- can clearly be Recent Results in Neutrino Astronomy PoS(ICRC2015)1066PoS(ICRC2015)002 -ray γ ] C. Kopper ]. 25 14 15 8 7 8 7 6 0 5 4 ...... 30 0 0 0 1 0 0 2 0 7 1 + + + + + 6 7 0 7 as measured at Earth. . . . . 35 τ ]. Also point sources . 3 3 0 ν : 2 29 µ , as measured ν ’. Composi- : 28 t L. Mohrmann e ⇥ ]. It should be noted, however, ν n 08 08 7 5 7 6 4 0 : . . 32 ...... 0 0 0 0 2 0 0 1 69 0 µ . + + + + n 1 2 3 0 : ], respectively. The . . . 53 , where we focus on e + . 3 3 0 n 24 3(a) 7 2 2 2 ]. Triggers are (or were) sent to networks of small 34 , cm cm cm 33 1 1 1 sr sr sr 1 1 1 ]. s s s 1 1 1 26 —2 Results on the flavor composition, using hy- PeV — 2 ] and Enberg et al. [ confidence level. s 23 GeV GeV GeV 18 18 18 Constraints on flavor composition of the astrophysical neutrino flux from a global fit of various Figure 2: pothesis B for the energy spectrum.triangle Each corresponds to point a on ratio the at Earth. The besttions fit expected is for three marked different with sourceindicated. ‘ scenarios are 6 10 10 10 One of the most prominent transient sources discussed as candidates for the production of Best-fit results for the flavor composition fit. The quoted astrophysical neutrinos are gamma-ray bursts (GRBs). These objects generate very bright searches using a joint sample of IceCube and ANTARES data have been performed [ 5.3 Limits on Transient Sources signals within a short durationrelevant of background typically from 1 atmospheric to neutrinos 100 toneutrino seconds. GRBs observations is Because significantly within of reduced a this and shortinterest. short even time single No time span, such window the coincidence coincident hasGRBs been to as reported the a so sources GRB far, of which cosmic would places rays be stringent of the limits of reported on significant neutrino models flux of [ robotic telescopes (ROTSE and TAROT), the Palomar Transient Factory (PTF), the SWIFT X-ray Figure 3: other IceCube analyses. Each point on the triangle corresponds to a ratio searches in IceCube andto ANTARES are the beginning usual to track use channel to the improve starting sensitivity event to channel lower in energies addition [ that other transient phenomena such as off-axis orthe failed progenitor GRBs star) (GRBs and where several the other jet modelstive does are to not not escape a ruled wide out range by of this transientin non-observation. phenomena, direction both To and be ANTARES time. and sensi- IceCube Versions of search thesewith for searches event other are clusters run observatories in are real-time so possible that [ follow-up observations Recent Results in Neutrino Astronomy Compositions expected for three different source scenarios (before oscillations) are indicated. [ L ln e t µ cut g f D f f

with 10 years of data. Note that a single isotropic cosmic E 2

Param. Unit Hyp. A Hyp. B s

Table 3: uncertainties are at 1

3 ⇠ . In con- ) is mainly 2 1 confidence, i.e. well above the current best-fit value of 2.7 PeV. On the other hand, s The projected sensitivity to the energy spectrum is illustrated in fig. In order to derive the future sensitivity The impact of the newly ). We weight the simulated cosmic neutrino rejected with a significance of neutrino flux is assumed in all cases. the sensitivity to the presence ofpanels an show exponential expected high-energy limits cut-off on to the the energyspectrum spectrum. of of The such two hypothesis an large exponential A cut-off, and whererespectively. the B If current is no best-fit assumed cut-off is to present, be6.7 the PeV the expected at true lower 2 spectrum limit in withfor 10 the a years top true of and full cut-off bottom detector energy panel, data at is the current best fit, the non-existence of an exponential cut-off can be flux to the current best-fit energy spectrumhypothesis of A or B (cf.scale previous the section) expected and signal up to mimic thelection col- of additional data. Fora the flux conventional at and the prompt level atmospheric ofsensitivity neutrino the is flux, then predictions we derived by assume using Honda the et approach al. described in [ [ of the IceCube detector tothe cosmic the neutrino properties flux, of we useanalysis a that prototype is based on theof event samples selections T2, H2,1 DP, and US (cf. Table plied to new data thatThe are resulting already expected sensitivity recorded. toergy the spectrum en- and flavor compositionvestigated is in the in- following section. 6. Projected Sensitivities fect the energy spectrumcontribute and to the slight preference ofnential an cut-off. expo- The samples DP andresent US rep- new event signaturesviously that not were considered in pre- most the all analysis. of Al- the event selections can be ap- visible in the flavor composi- tion fit, seetrast, fig. the newof event uncontained showers sample (US) and the extended eventple sam- of analysis H1 mainly af- Combined Analysis of the High-Energy Cosmic Neutrino Flux at the IceCube Detector added tau search eventple (DP, sam- cf. table PoS(ICRC2015)002 ]. 37 C. Kopper 2014). For sources in the flux at di↵erent declinations 2 et al. ]. IceCube and ANTARES alerts are 36 , 35 – 24 – 8 ]. 38 neutrino flux from individual point sources as a function of declina- discovery of a point source emitting an E 2 − E Sensitivity to an sensitivities and uppersouthern limits hemisphere, are ANTARES also constrains neutrino shown fluxes (Adri´an-Mart´ınez at lower energies than this work. combined four years of datais (40, the 59, flux 79, and required 86 forwhile string 5 the detector dashed configurations). line The is solid the black line median upper limit or sensitivity also for a 90% C.L. The ANTARES Fig. 11.— Muon neutrino upper limits with 90% C.L. evaluated for the 44 sources (dots), for the ]. The IceCube constraints are derived from the non-observation of clustering in data dominated by 31 IceCube is also able to constrain models (or discover fluxes from) neutrinos generated by in- With the existence of dark matter firmly established by a number of independent observations, teraction of the highest-energy cosmic rays on“cosmogenic” photons or of “GZK” the neutrino cosmic fluxes microwave are background. characterizeda Such by few broken PeV power-laws and above energies extend of upsuch to energies, mainly several hundred due EeV. to Because itssix IceCube large years has volume, of sensitivity it recorded to is IceCube neutrinos able dataproton of to composition are search of currently for the underway. these primary Under cosmic fluxes.first favorable rays), Studies conditions detection their of (such sensitivity of up is GZK as expected to neutrinos a to in be IceCube sufficient [ for the 5.4 GZK Neutrinos including anomalous rotation velocities ofanisotropy galaxies, in gravitational the lensing cosmic of microwaveremains background, distant elusive. the galaxies, Weakly direct Interacting and Massive evidence Particles ofmetric (WIMPs), its (SUSY) like particulate particle the (the nature lightest neutralino), stable still are supersym- particularly well motivated dark matter candidates and Figure 4: tion [ atmospheric muon neutrinos (Northerncorrespondingly hemisphere) and different atmospheric energy muons thresholds.observation (Southern of The hemisphere), clustering constraints with in a from sample ANTARES dominated are by atmospheric derived neutrinos. from the non- satellite and to IACTs such asalso MAGIC sent and through VERITAS the [ AMON network for distribution to various third-party experiments [ 5.5 Neutrino Physics and Dark Matter Recent Results in Neutrino Astronomy PoS(ICRC2015)002 25GeV C. Kopper ≈ ν ◦ E 0 38 8 1 - 41 5 Galactic 39 27 and those containing tracks 9 26 + 6 3 42 46 11 40 13.1 19 37 ]. 4 54 8 40 30 20 , 45 16 35 49 39 ] 7 43 48 23 52 22 ) are marked with 53 ◦ 15 14 12 9 to 15 10 2 ◦ 22 36 24 21 17 18 TS=2log(L/L0) 25

44 Southern Hemisphere Southern

33 Northern Hemisphere Northern . Colors show the test statistics (TS) for the point-source clustering × 29 34 47 0 ) with 50 ◦ 31 1 51 ◦ 0 ICECUBE PRELIMINARY ICECUBE 8 13 ]. The current results are statistically limited and on-going analyses predict reaching 1 Arrival directions of the high-energy starting event sample in galactic coordinates. Shower-like 41 Given the success of the IceCube detector and its DeepCore sub-array, a substantial detec- While the focus in this article is mostly on astrophysical neutrino sources, it should be noted tor upgrade to both lowernamed and IceCube-Gen2, higher energies will is consist currentlygrade. of being the planned. PINGU low-energy The will extension, upgraded consist PINGU, detector, of and a an high-energy even up- denser instrumentation of the region of deep glacial ice test at each location. No significant clustering was found. [ limits as sensitive as other projects like T2K. 6. Future Detectors (with resolutions better than 1 that the atmospheric neutrino fluxneutrino measured source by to neutrino study detectors effects canthreshold such of be about as used 10GeV neutrino as has oscillations. a made it long-baseline IceCube’s possible DeepCore to map array out with the oscillation its minimum at in detail [ Figure 5: events (with angular resolutions of the order of 10 the focus of dozens of directscale detection galactic experiments structure worldwide. is Given attributedtion that to the is the formation expected distribution of of near large- dark theobjects, matter, Milky like the the Way largest galactic Sun, local centre throughor concentra- (GC) gravitational annihilate capture. with with each predicted WIMPs other, enrichment thatSignals result in from decay in these massive with high WIMP very energy interactions long Standard andthe Model lifetimes, WIMP-nucleon their scattering particles measurements cross probe including section two and neutrinos. either fundamentalWIMP the properties: annihilation self-annihilation in cross section the or Sun, lifetime. thenature GC given and the dwarf expected spheroidal energy galaxies spectrum wouldcompetitive of provide limits the a on events. striking dark Both sig- matter IceCube signals and from ANTARES neutrinos are setting [ Recent Results in Neutrino Astronomy PoS(ICRC2015)002 C. Kopper ]. The high-energy 43 ]. On the other end of the 42 -rays should allow us to narrow down the γ 10 ]. Its densely-spaced ORCA ‘building block’ will also be able 16 arXiv:1312.0558. Since the first evidence of astrophysical neutrinos in 2013, the significance of the observed In the Mediterranean, the KM3NeT project has recently started construction and deployed its [1] M.G. Aartsen et al., Science 342,[2] 1242856 (2013) R. Abbasi et al., PRL 111[3] (2013) 021103 M. Ahlers, PoS(ICRC2015)022, these proceedings [4] A. Ishihara, PoS(ICRC2015)013, these proceedings [5] E. Waxman, 2013, Proceedings of Rencontres du Vietnam: Windows on the Universe[6] (2013), J. K. Becker, Phys. Rept. 458,[7] 173 (2008) P. Desiati, PoS(ICRC2015)028, these proceedings possibilities and eventually lead to the discovery of the sources. References signal has steadily increased with more andbeen more observed observed in data. multiple Astrophysical channels neutrinos (incomingtheir have tracks now flavor and composition starting to events), be allowing mappedflux details out. are such now With as being increasing studied. statistics While theis the detailed consistent distribution properties with of of an the the extragalactic detectedThe high-energy origin, absence neutrinos a of in a Galactic the point component sky source canfor discovery not has the started be flux to excluded constrain – at thegiven a this number the single of time. current sources source point responsible source responsible sensitivities.started for construction The the should future total soon KM3NeT/ARCA be flux telescopeservation able which would of to recently the already provide astrophysical an have neutrino independent been flux.at confirmation The discovered of this sources IceCube’s of time, ob- astrophysical but neutrinos ongoing arenation observations not with with obvious information current from and radio, optical, future X-rays neutrino and telescopes and the combi- to measure the neutrino massarray hierarchy should on be a able competitive time-scale to whilepointing confirm resolution the the in ARCA IceCube order high-energy detection to in help a find detector the with sources different of systematics the observed and 7. flux. Summary and Outlook first string of optical modules [ Recent Results in Neutrino Astronomy currently occupied by the DeepCore sub-array, loweringan the order energy of threshold magnitude. of the This detector opensa nearly up the very possibility competitive to measure time-scale the andenergy neutrino mass scale, for hierarchy a within comparatively high-energy modest detectortical cost upgrade modules [ to around IceCube the will currentrecently add detector, discovered significantly more high-energy increasing detector astrophysical the strings neutrino detectorimproved with flux. effective acceptance op- area This for and angular upgraded the resolution detector forarray will the will highest-energy have permit events an [ a significant increasethe addition in of the a statistics full of surface high-energy veto events, above improved the further array. by PoS(ICRC2015)002 C. Kopper 11 [8] M. Honda, et al., PRD75[9] (2007) 043006 R. Enberg, M. H. Reno, and I. 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