PoS(ICRC2021)048 International th 12–23 July 2021 July 12–23 37 SICS CONFERENCE SICS CONFERENCE Berlin | Germany Berlin Berlin | Germany Cosmic Ray Conference Ray Cosmic ICRC 2021 THE ASTROPARTICLE PHY ICRC 2021 THEASTROPARTICLE PHY https://pos.sissa.it/ ONLINE ∗ 0,1, [email protected] International Cosmic Ray Conference (ICRC 2021) Presenter ∗ th This contribution attempts to summarizepresented the at status the ICRC of 2021, the the first field online-onlybuilds edition of on of neutrinos 212 this contributions conference. from with This the pre-recorded rapporteur cosmos talks report Furthermore, and as many posters, of as well the as session 11 conveners discussion provided sessions. valuable input to this summary. DESY, Platanenallee 6, 15738 Zeuthen, Germany ECAP, Friedrich-Alexander-University Erlangen-Nuremberg, Erwin-Rommel-Str. 1, 91058 Erlangen, Germany E-mail: Copyright owned by the author(s) under the terms of the Creative Commons 0 1 © Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0). 37 July 12th – 23rd, 2021 Online – Berlin, Germany Anna Nelles Rapporteur ICRC 2021: Neutrinos and Muons PoS(ICRC2021)048 Anna Nelles in cascade mode. 3 2 The field of neutrino astronomy already provides exciting results, however,it is still dominated The field is driven by ideas, both in further developing experiments and theoretical models. 10 years after its completion, IceCube is still only scratching the surface of neutrino astronomy Baikal-GVD, exploiting the waters of lake Baikal, is still under12 construction. KM3NeT detection units Currently are now operational in the Mediterranean sea. It is planned to With RNO-G (Radio Neutrino Observatory Greenland) the first large scale implementation of a A successor to ANITA, PUEO [7], has been selected as balloon mission to fly over Antarctica. The Pacific Ocean Neutrino Experiment Explorer (P-ONE) deployed the second pathfinder by very low statistics inbeen astrophysical discussed neutrino in detections. the multi-messengeropportunity The context for [1] most all and transformative clearly results experiments neutrinosbooming have with are with a becoming new potential a ideas sensitivity target forand of detectors to systematic and them. detector has reached calibration The acommunity are neutrino maturity the is field in order doing which itself of their detailed is community business. data homework is analysis excited to about. To get summarize ready the for sentiment: many the more neutrinos,1. which the broader Ideas 1.1 Established players, upgrading or under construction [2]. The IceCube Upgrade, targeting lowerand energies optical and an modules improved are detector currently calibration being issensitivity produced. funded across IceCube-Gen2, the an energy order range ofThe is magnitude IceCube-Gen2 better proposed collaboration in published for a construction comprehensivemore after whitepaper details that completion and can of an be the overview referred of Upgrade. to the for science case [3]. 8 clusters are operational, corresponding to an effective volume of 0.4complete the km ORCA115 array (focusing onon neutrino astrophysical oscillations) neutrinos) in in 2025 2027 and]. [5 ARCA230 (focusing Antares data analysis is ongoing1.2 with 10 New years players of under data. construction radio neutrino array is currently being deployedplanned at and Summit Station fully-funded in [6]. its first The season.RNO-G radio will 35 in-ice have stations techniques are to targets show neutrino theexperiments. energies scalability above of 10 the PeV. radio detection technique from smaller pathfinder It will improve on ANITAfactor of by 10. lowering It the is energy scheduled to threshold fly and in December increasing1.3 2024. the sensitivity New by players in a pathfinder mode string [8]. The site offarray, the as coast the of infrastructure Vancouver is has alreadypromising the in [9] potential (see place to also and develop2 Figure first intoright). measurements a of third the large attenuation water length are Rapporteur: Neutrinos and Muons Completion of the detector with 14 clusters is scheduled for 2024 [4]. PoS(ICRC2021)048 Anna Nelles -interactions. The g a stemming from g 3 will be placed in a service tunnel close to ATLAS, targeting the muon excess a -induced air showers. To this end, one can either blanket large areas with simple g through What is discovered first: new physics or secondary corrections toDo our we models? have too many fudge factors in our models, tuned to data? A demonstrator Cherenkov telescope for Trinity has been funded [10, 11], which will look The various EUSO missions combine the Cherenkov with the Fluorescence approach. EUSO- There are various proposed radio air shower arrays in pathfinder mode aiming at the detection It has been 25 years since Super Kamiokande has started taking data. Gadolinium-sulfate It was also reported about JUNO, a reactor neutrino experiment under construction in China Valuable input for the neutrino and muon field is expected from two experiments at CERN. In general the neutrino field tends to think in areas of fundamental physics and astrophysics, • • C0D a at the rim of the Earth from a mountain top for upcoming SPB2, scheduled to fly in 2023 onworks a super-pressure as balloon, technology targets the demonstrator observation of forneutrinos UHECRs the, [12 and proposed13]. POEMMA mission targeting (also) transient of antennas as proposed foroverlooking GRAND large areas, [14, like proposed15] for or BEACONboth [16, approaches one]17 are or can currently TAROGE operational. [18]. set-up Demonstrators smaller for arrays on mountain1.4 tops The low energy regime is now being released for better[19]. neutrino anti-neutrino Its distinction successor andconstruction improving Hyper-Kamiokande has the has already performance begun, been and approved operations are for envisioned construction to begin in in 2020, 2027[21], [20]. the which tunnel is particularlyORCA or intriguing IceCube-Upgrade. for Also, BAKSAN, cosmic ageo-neutrinos multi-purpose neutrinos and liquid in neutrinos scintillator detector from combination targeting the withmass CNO of cycle sensitivities 10 is kt of currently [22]. in an R&D stage of 51.5 t with a Other target experimental endeavors NA61/SHINE, a fixed-target experiment,simulations. has Planned been are detector and[23, upgrades will24]. and be the FASER investigation delivering ofproblems heavy input particle in to fragmentation air cosmic-ray showersproduction). and It is predictions scheduled to for start prompt data taking neutrinos in 2022 (through [25, 1.626]. forward charm Ideas of meson what to target which has been reflected atNext this conference to in comprehensive two summaries discussiondiscussion sessions of panels that on-going raised are some research worth provocative re-watching. questions and such new as theoretical developments, the Rapporteur: Neutrinos and Muons Cherenkov technique has the potential to bridge theand energy gap the between radio optical technique. in air or water arrays PoS(ICRC2021)048 Anna Nelles 4 Are we clear enough aboutclasses? assumptions (such as identical sources) when rulingAre out there source enough precautions against over-interpreting correlations and bias? The larger ideas as presented in the first chapter, were complimented with reports about hands- Since many experiments rely on photo(n) detectors, a whole discussion session was reserved Overall, there were rather few contributions dedicated to hardware only, with many from the The extended discussion session about detector calibration is indicative of the fact that the field Similarly, considerable effort is being undertaken to better model and understand the detection • • on detector development and calibration.able to In better particular or more calibration tightly is interpret gaining the in signals detected. importance2.1 to be Hardware development for this topic. The general trendlike seems multi-PMT to go modules towards used more complexcalibration in and plans. KM3NeT. segmented Also, These photodetectors given complex the increase sensors,about also in however, the size require of suitability optimized the overall for experiments,scalability many mass-production discussions were of on the morecomplex table, sensors. complex with sensors, one standardization or needs the and other voiceradio arguing domain, for which is simpler still more rather inunder than construction. the nuts more It and can bolts be phase, concluded with that fiber the optics first are large here array2.2 to only stay just and now no Detector longer calibration controversial. has grown up. A pointconsiderable has effort been is reached being where made studiesdespite to are not reduce starting being these to put systematic be forward effects. systematics forinto limited, a being It so successfully neutrino should used a detector be for anymore, positioning highlighted the1). in that all acoustic large detection arrays has with matured strings [27–29] (see also Figure 2.3 Media properties media ice and water.tenuation In length, many scattering coefficients experiments and the media systematicAlso, impurities given uncertainties are the starting carried long to duration forward dominate of the from calibrationment progress. efforts at- devices, presented dedicated (development measurement of campaigns), specialized it measure- resource’s should are not being be allocated underestimated to that thisselves significant aspect. in However, this also context. interesting opportunities A present new them- approach has been presented measuring the luminescence properties Rapporteur: Neutrinos and Muons It seems of utmostresults, importance so that that the bold fields claimsinto keeps reality that critically without are scrutiny. questioning being In the particular madewhere when advances in assumptions it and comes proposals such to new as or sources, "all high-impact we sources seem papers are to the do be same" reaching not a can blend point no longer2. reasonably be defended. 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P 5 Attenuation length vs. wavelength from the simultaneous multi-wavelength fit of all available The optical properties of the water at the P-ONE site are critical for the success of the ex- The DAQ system of the sDOM records timestamps of the pulse trigger times and time-over- For the analysis of STRAW data, a Bayesian approach has been chosen because it facilitates , the average fraction of flashes that cause the detector to record a photon hitfraction ]. ph position method 7 # This number is an easily accessiblehas therefore and been reliably used measurable for observable deriving for the the attenuation STRAW length. setup and the consideration of systematic uncertainties as nuisance parameters. Using this approach, the PoS(ICRC2021)1083Optical characterization of the P-ONE site Figure 1: STRAW data. Measurements fromAlso various the other results neutrino from telescope a[ sites study are of attenuation shown lengths shown as in the well clearest [ ocean waters are shown for2. comparison Attenuation Length Measurements periment. One of theattenuation fundamental length, quantities this that property strongly setsmooring influence lines the as the scale well design as for the how of distanceusing far P-ONE between the the the is POCAM lines. flashers optical the and The modules attenuation locking will measurement into is be the performed pulse set frequency on signal the inthreshold the (TOT), sDOM this data. level ofThe information is flasher not intensities well used suited fornumber for of the resolving photons attenuation multiple recorded length in photon an pulses. analysis sDOMfor are an PMT average is adjusted intensity < in such 1. terms that of From photons the Poisson hitting statistics average and it being can detected be by derived theexpressed that photo as sensor, follows. per flash 7 Detection Line Fit position reconstruction with top-view in three dierent moments: at the Detection Line Fit position reconstruction with top-view for each line with respect to their position The results presented here show that the developed DU line fit model looks promising using 7. Conclusions AHRS data with the of compass value uncertainties. Another importantwhere aspect there is is that a the strong modeltion. sea can be current These used results that on show can periods the displacedetector possibility the independently to DUs of reconstruct the a the acoustic few positions positioning meters of system. from the the main components vertical of posi- the Figure 5: beginning of the considered period (left plot), in the middle (plot in the middle), at the end (plot on the right). Figure 4: on the sea bed KM3NeT Detection Unit Line Fit ]. Similar to the Q-balls these Big Bang relics are assumed to be very in comparison to a bare muon passing through ice. 10 A.D. Avrorin 20 10 . (original pictures of this composed picture are taken from Ref. [ 4 137 Light yield of dierent emissions for magnetic monopoles carrying one Dirac charge and Planar coordinates Top view of string positions as reconstructed through acoustic modules. Left: Baikal-GVD Left: Light yield of different emissions for magnetic monopoles carrying one Dirac charge and (b) Luminescence light also contributes to the total light emission of Standard Model particles, In this work various measurents of luminescence of water and ice in laboratory and in-situ are Another particle, which can be searched for using luminescence, is a magnetic monopole. The first search ever using luminescence light as detection channel for Magnetic Monopoles An overall highlight of a conference like this is to see all the hands behind the scenes involved presented and compared. A clear indication of the influence of the radiation type as well as the ice passing through the IceCube detector at low relativisticof speeds has this been finalised analysis [ exceeds previousThe limits exclusion in limit this therefore region catches bycurrently up approximately World with leading. two orders the of IceCube magnitude. limits at other speed rangesespecially which the are interaction products ofenergy, ultra signature topology high or energy particle neutrinos. IDcould reconstruction improve This because accuracy taking has of luminescence consequences these into by for account uo the to 10%. 5. Summary and outlook massive, however monopoles can befields. accelerated to At relativistic low and speedsdecay high by via speeds inter-galactic the magnetic detection Rubakov-Callan channels eectspeeds are and as the well (in-) as model direct low dependent speeds Cherenkov no catalysis light. (model of in-dependent) nucleon light However, at emission was intermediate known before. Figure 6: Left: Q-balls with a charge of a Q-ball simulated with luminescenceelectric emission. charge The of Q-ball has a speed of which hides the track in noise which can be removed in theThese analysis [ are predicted byisolated Grand-Unified magnetic charge theories [ and others to be particles carrying at least one Luminescence of water and ice in getting the best out of theusual data chance of to the detectors. shine in Regrettably, thethis person, online important format but did the work. not discussion provide A the sessions flurryhave did been of at presented studies least and try that new to futurefraction developments attempt measurements can in to and be reconstruction highlight highlighted science and here. results simulations will benefit from. Only a tiny 3. Reconstruction and simulations of ice and water resulting from movingparticles charges, in a neutrino potential new telescopes detection [30] channel (see for also exotic “slow” 2). Figure Figure 2: Q-balls with a charge oflength 1020 vs. in wavelength from comparison the to simultaneous a multi-wavelength fit bare obtained muon at passing the through P-ONE ice site [9]. [30]. Right: Attenuation Figure 1: Beacon No. 306 drift between MayDetection 1 Unit and Line May Fit 12 position 2020, reconstructionthe during sea with a bed top-view regular [28]. for drift each period line [29]. with Right: respect KM3NeT to their position on Rapporteur: Neutrinos and Muons ] and corresponds to a subnanosecond 4

5

. As can be seen from this analysis, the mean upper bound 8 ], the immediate interpolation error during active drift periods can reach 0.5 Coordinate scans 5 (a) Beacon #306 drift between May 1 and May 12 2020, during a regular drift period. Figure 7: The Baikal-GVD acoustic positioning system is currently in operation. Following an improve- OM positions are interpolated from beacon coordinates using a piecewise-linear string model. ment in the polling algorithm in May 2020, the median polling interval in 2021 is 180 seconds. The string segment betweenstring beacons segments, 3 compounding and linear 4 interpolationon also error. this exhibits worst-case error, greater In two order curvature calibration tobetween beacons compared were obtain regular to installed experimental beacons in lower bounds the 3 middlecluster and of 3 the in 4. string 2018, and segment calibration Calibration beaconCalibration #2 beacon beacon was installed #1 coordinates on were a was peripheral then installedand string linearly of on 4. interpolated cluster 5 the from in The the central 2019. distance coordinatesacoustic string between of trilateration of calibration beacons then 3 beacon provides an positionsthese upper obtained dierences bound are with on provided linear on OM Figure interpolation positioningon error. and OM The positioning distributions of errorbound is is possible below because 15 GVD strings cm areof largely (note nearly a vertical. that previous This the study, is done consistent photocathode with overtime the the diameter calibration results course error. is of While 25 season the cm). 2018 meanin error [ similar over This detectors three [ years is comparablemeters to due the to positioning high error beacon mobilitybeacon and coordinates string to curvature. a This physical, can rather only then be piecewise-linear ameliorated string by model. applying 4. Conclusion 3.4 Positioning precision In this approach, the interpolation errorbeacons, string will curvature, vary and with beacon mobility, the which is distancethe decreases between with season. OM depth and and varies The interpolation throughout biggestbeacons interpolation 3 error and is 4. expected for OMs These installed beacons in are the middle the between most mobile due to their relatively shallow position. Positioning system for Baikal-GVD PoS(ICRC2021)1065 PoS(ICRC2021)048 Anna Nelles ] and the newly 4 -coordinate of the cascade z ], a CNN based method [ 1 interactions for a typical cascade event selection is 4 a 7 6 The pulse arrival time PDF, approximated by the generative model, is shown for three dierent The angular resolution of charged-current NuE interactions for a typical cascade event selection The angular resolution of charged-current With the detection of the first likely neutrino sources, combined with the fact that event statistics KM3NeT will likely reach sub-degree resolution for single cascades [31], and IceCube has, In the overall event reconstruction, a clear trend towards more modern machine learning Figure 6: is compared between IceCube’s defaultdeveloped reconstruction hybrid (MLE) method. [ The hybridwhole method energy leads range. to The a plateau significantly towards higher improved angular energies is resolution induced over by the systematic uncertainties. Figure 5: DOMs of the sameinteraction event. vertex, while the The right left panel illustrates panel the shows change the due to eect the of varying zenith modifying angle. the Combining Maximum-Likelihood with Deep Learning Figure 3: are still very low, aincrease significant the effort fidelity is of being events, madecascade-like which events. to are intrinsically better harder reconstruct to arrival reconstruct directions a and direction to for suchfor as example, reported on checks of theresolve pointing the accuracy rim using of the the shadow moon ofthe angular the [32]. resolution moon, of While starting in-ice to likely radio arrays not are4), competitive starting which in to will be angular be more pointing, useful concrete predictions to [33, and]34 evaluate of (see physics get also cases the Figure of theory the community upcoming thinking and of proposed particular in-ice models radio to arrays test in the3.2 highest energy range. Event reconstruction techniques is observable, however, establishedlittle bit are too much techniques inertia in still using the going formerof techniques. strong; By machine now, the possibly learning characteristics and with performance tools a areaspects in well which understood they are and good one (theto true could use pdf also parameterizations) is consider unknown, and too to notdoes many parameters use for not to those them need efficiently where be only to able for theestimation be physics with trained, modeling a as convolutional is neural for solid network example [35] and (see shown the also in analysis 3). Figure an analysis combing maximum likelihood compared between IceCube’s default reconstruction (MLE), amethod. CNN The based hybrid method, method leads and to theThe a presented significantly plateau hybrid improved towards angular higher resolution over energies the is whole induced energy range. by systematic uncertainties]. [35 3.1 Neutrino pointing Rapporteur: Neutrinos and Muons PoS(ICRC2021)1151 , 3

PoS(ICRC2021)048shows 3 Steven W. Barwick , leading to improved 1 km Anna Nelles for each antenna type. This demonstrates that the 5 ° 05 . is booming. Clearly this 0 g a average shown in a darker red color. The red vertical line corresponds to average shown in a darker blue color. Red squares show the residuals using 10 m 10 m -propagation through the Earth, and g Dierence between measured and expected arrival directions (top plots:zenith angle, bottom plots: 7

PoS(ICRC2021)1153The linear polarization of the arriving radio pulse was determined as a function of depth and -related aspects did highlight the fact that currently consequence of the large signal toa noise. significant Neither oset the direction as nor athe polarization function measurement depth of show dependence depth of relative bothcomponent to indicates polarization expectation. good components. understanding The of right The icephi panel eects relatively component during of flat shows propagation. Fig. response a Only of variationmeasurement. the the with subdominant depth theta which Laboratory causes calibration the variation studies in of the the polarization angle SPice transmitter show strong dierences Figure 2: azimuth angle). Left plotsexpected show direction the includes depth the dependence; knownthe histogram geometry four LPDAs projections of along are with the a shown hole.the on four the Light dipoles right. blue along triangles with The a show a the reflection coecient residuals from using thecoecient snow of surface 0.5. of The 0.1, grayand while shaded thus the not area taking blue indicates data. vertical the The line periodson projected corresponds an where histograms (LPDAs:blue to event-by-event station basis dash, 51 a dipoles:solid (i.e. red) was reflection present without in the the communication residuals averaging). mode the detector station, which in turndirection. results in The a depth systematic uncertainty dependencezenith in has and the flattened azimuth predicted for resolutions signal depths by arrival roughly greaterangular reconstruction than by an ARIANNA stationcored is boreholes. sensitive to typical variation in the geometry of compared to expectation basedright). on There laboratory is measurements a slowly oferror varying in the systematic the error polarization transmitting as measurement pulser is a smaller function (Fig. than of 1 degree, depth but of the 2.7 excellent precision degrees. is partly Statistical a ARIANNA direction reconstruction g a Kaeli Hughes ]. 6 Eciency vs. SNR. (b) Left: Analysis efficiency resulting from an analysis of the phased array (PA) data compared to It was encouraging to observe that the radio technique is slowly but surely moving towards As already visible from the first section, the field of upward going The dedicated discussion session on

6 3.3 Radio reconstruction the mainstream and contributions dealing withgrouped the with event other reconstruction were radio no contributions. longergiven that exclusively However, radio some is discussions still are a step stillhas behind very been optical reported unique methods on all to in fronts, not radio, most having notably in detectedis being a able required neutrino to extract yet. to low-SNR neutrino Progress signals, reach which theamong proposed others, sensitivities by [36] studies (seereconstruct showing also flavor the4). [38]. Figure expected This energy was resolution complemented. [37] and first ideas of3.4 how to UHE tau-neutrinos the most recent ARA Station 2a efficiency, strong scaled improvement to at have low equalexperiment signal-to-noise definitions. sensitivities ratios, This [36]. which most was recent Right: anpulser analysis outstanding shows Difference study issue between with to measured ARIANNA. deliver and Light on10 expected promised blue m arrival triangles average directions shown show from in thewith a residuals a a using darker 10 the blue m four color. average[34]. shown LPDAs Together along in Red with with a squares the a darker show resolutiondirection. red on the polarization color. residuals [39], using The this the gray translates four into shaded dipoles a areas resolution along indicate on communication neutrinos periods arrival development has also been fueled bythe the "ANITA Cherenkov mystery events", camera which experiments of likeon. EUSO-SPB2, PUEO, Without or additional experimental ultimately evidence POEMMAcalmed the down, discussion will while about the have ANITA the collaboration an origin naturally keeps of excellent investigating different these handle scenarios events [40]. have 7 independent codes [41–43] areraised the available question to whether this calculate was sustainable the communities for a are smallish community. using In the particular, sincecodes. codes other The and overall may opinion was be that interested a consolidation in has using to take the place most for the comprehensive sake of of comparability, all Figure 4: Rapporteur: Neutrinos and Muons ) but the maximum within 10 m of the surface should be equal or 2b Eciency vs. Energy. (a) Analysisciency e of this analysis compared to the most recent ARA Station 2 e ciency, scaled to There are two types of events that are universally removed from the analysis: calibration pulser The second variable is the ratio of the correlation within 10 m of the surface and the global all were removed. Software trigger events,were which also removed occur from once the analysis. per second Forthe each and run, expected are RMS the not software of triggers RF each were triggered, channel. only used to calculate events and software trigger events. ARAown Station string 5 about is 20 equipped m with away, which aa pulses local trigger on calibration the time pulser GPS cut, on second, its which and ismode thus 99.984% that can is ecient. be not easily Occasionally, tied removed the with to calibrationthe the pulser livetime. GPS is time; In these operated total, runs in there were a were tagged as 13 calibration of runs these and calibration removed runs from for a total of 1.6 days of livetime and comparable to the global maximum.corresponding The to boundary signals on in this which ratio the forwithin global the maximum 10 deep was m region more was of than set twice thesurface to that calibration surface. 0.5, of events, the fall correlation All comfortably into candidate the surface shallow region events using in3.2 this the method. 10%, Designing as Cuts well as a population of allowed. The boundary forconsidering the Snell’s deep law region at was a set depthcosmic to of ray 20 57 events, which m degrees, are below a expected the to conservative surface. penetrate boundary to This from 20 was m chosen maximally tomaximum [ avoid correlation. impacting This alsosurface strongly events correlates may correlate with to surface both events thecorrelation in surface the and map the 10% in deep sample. region Figure (as True shown in the rooftop pulser Figure 5: have equal definitions. The blue curve isno the shallow eciency region on neutrinos neutrinos are in recoverable, the aall deep conservative energies. region; estimate the that This red causes analysis curve is a assumes ecient 21%to. on loss events in with eciency low over SNR that the traditional ARA trigger is not sensitive Low-Threshold ARA Analysis PoS(ICRC2021)048 a Anna Nelles . While there Should we be like particle physics and 8 We are physicists and not software developers While no one was willing to answer this question with "Yes" there Muons are grouped with the neutrinos in a track, but are likely to suffer from underexposure, The most pressing current issues are and have been for a long while that (1) too many muons are On the simulation sides, a couple of codes has established themselves as dominant players, In the light of the still small event statistics, the discussion session about future neutrino This conference series covers the newest results about all known types of neutrinos from the despite being critical to understand forcourse backgrounds a and large production overlap with mechanisms. the Also, air there shower is track. of observed in air showers as compared to theneutrino predictions production in (and air the shower related simulations muon and production) thatpredictions is (2) rather prompt [44], uncertain, while lacking solid becoming quantitative moreBoth and of more these problems important are at likely energies to of obtain the fresh astrophysical input flux. from NA61/SHINE [23, 24] and FASER such as MCEq, which islepton-propagator widely [47]. used for The the arrivalcommunity. muon of flux CORSIKA predictions 8 e.g. [48] [46], is and also PROPOSAL eagerly a awaited3.6 by the Global neutrino and combined analysis telescopes resulted in the admittedly provocative question: cosmos from solar neutrinos to astrophysical neutrinos, as well as exotic particles showing a signal Rapporteur: Neutrinos and Muons while not burdening all softwarepurposes. developers with having to accommodate all experiments and all 3.5 Muons measurements [25, 26]. Small flux differencesfor neutrino to study telescopes, prompt-production but may need also a be dedicated observable effort, not a by-product of neutrino analyses [45]. have ONE BIG telescope only? was rising consensus that collaboration andJoint-analyses cooperation are between currently experiments has rather tointo cumbersome, be single-experiment increased. as analyses and likelihoods are and bothgain hard assumptions to was are extract pointed and baked to deep out, generalize.tool, Also, if but the not efficiency forces were everyservice joined. experiment tasks used would This for bebut would example shared. highly also their controversial lead statement: own This, towas source in more consensus correlation turn, sustainable that almost code educationand immediately development, in younger resulted colleagues as software in find development themselves theastroparticle ill-prepared is physics, well-known, opinions for lacking diverged the on from whether task encouraging of people ALLrecommendable. to simulation focus physics The on or (broader) programming curricula data community is still analysis undervaluesin in contributions career to decisions. software frameworks Thiswithout is despite software, the good fact no softwaresimplifies result speeds cross-instrument at verification up this and conference collaboration. results, would improves have been everyone’s work possible satisfaction, and 4. Cosmic Physics PoS(ICRC2021)1090 PoS(ICRC2021)048 ) of X , U , and the ] with and X 11 , angles, and : _ Anna Nelles . , declination, ) . ) X U : sin 2 - ) X, 89 ,B8=q , and longitude, : : XC q cos )/ ) W 2>Bq - of each detector pair. : U ,8 9 ( <0C2⌘ 89 0 ) XC - sin ) - ,B8=_ : : X, W U,X ( 4 cos 89 2>Bq ) C : W (( - 9 ) coincide with the equatorial coordinates of the CCSN . U X = 1 ( , 2>B_ ) U ( determination. The best estimate for the angles ( cos U,X ( ( ⇢0AC⌘ 2 89 ,8 9 <0C2⌘ = 0 ' j ) Æ = can be inferred from its latitude, = : : function: Æ A 2 j : ⇢0AC⌘ ' Comparison of the confidence areas obtained by the CCSN triangulation method [ neutrinos [54]. Illustrating the power of a multi-detector experiment for the determination of the location of 8 In this section, we describe the combination of the predicted light curves seen in KM3NeT, When it comes to supernova neutrinos, everyone is getting ready to see "the ONE". A Searches for the diffuse background of supernovae remain consistent with background at this Atmospheric neutrinos are the background for some and the signal for others. The measured Per definition solar neutrinos reside on the border between the solar physics track and the ratios or asymmetries between the number of events that would be detected in these three detectors DUNE, and DarkSide-20k. Each of these detectorsflavor. is predominantly sensitive The to a combination dierent of neutrino emission the during recorded the dierent light phases curves of may the CCSN. provide The a goal global of this view study on is the to use neutrino variables such as Figure 1: without using the prior for a CCSN located at the Galactic Center. 4. Multi-detector approach for enhancing the scientific output telescopes which is used, as shown in Fig depends on the uncertainty of theTo measured further time delay develop this approach,potential CCSN we through studied a the Bayesianstar impact approach. density of distribution The using in tested the a prior Milkyarea was prior Way. a of on This map approach the the of allows position source us GAIA to showing of localization reduce the the the by 90% more confidence than 55%, depending on the combination of neutrino The probability that the scanned angles ( is given by the following with no systematic shift inthe the searched CCSN location in the sky is given by the minimum of the function. The performance Greenwich mean sidereal time expressed as angle, The position of the detector the Earth radius, Multi-Detector Analyses for Core-Collapse Supernova Neutrino Detection geographic horizontal coordinate system from the CCSN right ascension, supernova in our own Galaxy willit! certainly The be supernova a Early Warning game System changeris (SNEWS) for will coming the alert and field, the astronomical so all community we[55–59] neutrino to better (see what telescopes not also are miss 5). Figure (in the process of) joiningpoint forces [61–63]. through the network 4.3 Atmospheric neutrinos atmospheric spectra keep improvingmeasurement of with the increasing prompt statistics neutrinoincrease precision flux and as seems well new within [66–69]. players reach, [64, putting pressure65], on so the a models to 4.2 Supernova neutrinos neutrino track. ItCNO has cycle been]. [49 reported All thatconsistent other Borexino with searches sees background for the solar at first neutrinos, thisresolve evidence point including B [50–53]. of those from neutrinos For solar from the flares, the future, remain JUNO is expected to be able to a supernova. Comparisonmethod of with the and without confidence using areas the prior obtained for by a location the at core-collapse the Galactic supernovain Center triangulation [60]. neutrino detectors.shown. It is of course almost impossible to4.1 do justice Solar to neutrinos all experimental results Figure 5: Rapporteur: Neutrinos and Muons PoS(ICRC2021)1123PoS(ICRC2021)048 ] 1 and ⇢ / ! is shown 2 31 Anna Nelles < Lodewijk Nauta , and the 90% CL (stat.+syst.), where 1 and . The best fit values 2 31 22 24 . 23 . 0 0 < \ + 95 . 1 and = 23 \ 2 31 2 is fitted to the data set in terms of < sin < , while having a dierence with Nu-Fit f 9 . 3 5 No oscillations Nu-Fit 5.0 Fit ORCA data 10 vs. cascades, etc.). of the model is calculated and the significance of [km/GeV] ` 6 2 a reco 10 j /E (stat.+syst.) and reco L 10 10 . . 0 0 + 50 . 2 0 10 for the former. At every point in the contour the log-likelihood is ORCA6 (355 days) KM3NeT preliminary = 23 distribution of the ORCA6 data, where the excellent agreement can be 1 23 0 \

\ 0.4 0.2 1.6 1.4 1.2 0.8 0.6

2 ⇢ Ratio to no-oscillations to Ratio 2 / ! sin sin . 5 . shows the 1-D scans of the profile likelihood with best fit values for the oscillation shows the contour of the analysis of ORCA6. The Nu-Fit best fit point is within the shows the f 4 5 3 9 , in terms of . L/E distribution for the ORCA6 data and expected number of events relative to the “no oscillation” 5 First oscillation results from KM3Net ORCA. L/E distribution for the ORCA6 data and expected 1 Figure Finally the contour with the sensitivity to the oscillation parameters The phase-space of oscillation parameters has also been scanned and profiledFigure in terms of Figure As a first step to find neutrino oscillations, the model In terms of an astrophysical neutrino flux, IceCube remains the only player in the field, albeit Since last ICRC, IceCube has reported the observation of a firstThere identifiable was electron-anti- no shortage in terms for theoretical models [85–89], motivating different searches Using the improved measurements of the atmospheric neutrinos, results of oscillation physics ORCA detector. minimized relative to all nuisancecontour parameters is including drawn through the the priors recovered from likelihood landscape. table confidence level of 90% for this result.order With of almost year magnitude of as data competing for ORCA6 experiments, the showing result promise is in for the future same measurements with the for the parameters are the statistical and systematic errorcontour is in given figure in its entirety. This best fit valuein is figure also shown in the the negative log-likelihood, tosensitivity provide of 1-dimensional the ORCA scans detector and towards neutrino a oscillations. 2-dimensional contour ofparameters the added at the bottom. This is done for parameters seen for oscillations. From the fitno results oscillations the compared to oscillations is estimatedof at about Figure 3: hypothesis. The binning is chosennu-fit such curves that in similar this statistics figure is do present not in include each systematic bin. uncertainties as The modelled no for oscillations the and ‘Fit’ curve. values or “no oscillations” values while only marginalising the nuisance parameters. reconstructed energy and incoming angle.normalised The compared outcome to of the the fitis “no is also oscillations” then fitted hypothesis transformed against for to the visualisation data while purposes. constraining the The oscillation model parameters to either Nu-Fit 5.0 [ First neutrino oscillation measurement in KM3NeT/ORCA 3.2 Results increasing evidence is tangible thatsignificant KM3NeT detection [77, of78] an orprovide excess Baikal-GVD the flux [79, community before80] with the one may next[81–83], report estimate which ICRC. is of on IceCube in the a particular is astrophysical valuable increasingfor as spectrum studies the the and spectrum of effort consistent is sources needed/used reporting to or asbut new input fundamental for with many physics estimates the [84]. new Sodifference methods far, observed presented, no between different new it data global should sets fit ( also has been be shown clear soonneutrino whether at there the is Glashow aspectrum resonance significant and [2], will influence which combined leads fits of to the a spectral index very and accurate flavor. for neutrinos flux in point correlation in with astrophysical thedata sources. energy is Models combined are continuously from beingthe multiple refined multi-messenger and observatories track [1]). to Similarly, predictfor various interesting correlations, searches are objects time-variability conducted to or atdetection look other experiments, or looking at multi-messenger still aspects, (see hunting coming also there flukes close is [90–105]. to currently observing no However, “knock-it-out-of a itfact the-park” that seems suggestion and the that one sources in mayinitially of the have stated astrophysical absence to several neutrinos content of interesting with are clear multi-messenger the both data, associations variable were and reported intrinsically on, different. such as As Tidal [70, 71], mass orderingparticular the72, [ arrival73 ] of andresults the may other first be data available neutrino (see from6). Figure properties ORCA [74–76] shows the keep potential in how lock-step. soon4.4 new oscillation In Astrophysical neutrinos Figure 6: number of events relative tofigure the do not “no include oscillation” systematic uncertainties hypothesis. as modeled The for no the ‘Fit’ oscillations curve and [70]. nu-fit curves in this Rapporteur: Neutrinos and Muons PoS(ICRC2021)048 , in , J. Phys. , , vol. 395, , in , vol. 395, , in Anna Nelles PoS(ICRC2021) PoS(ICRC2021) , in PoS(ICRC2021) , vol. 395, p. 1160, 2021, Trinity’s Sensitivity to , vol. 395, p. 050, 2021, . DOI , in , in , vol. 395, p. 1234, 2021, DOI. , vol. 395, p. 1029, 2021, DOI. PoS(ICRC2021) PoS(ICRC2021) , in , in 11 PoS(ICRC2021) Science and mission status of EUSO-SPB2 , in ]. PoS(ICRC2021) IceCube-Gen2: the window to the extreme Universe , in , vol. 395, p. 1179, 2021, DOI. 2008.04323 Neutrino Telescope in Lake Baikal: Present and Nearest Future collaboration, , vol. 395, p. 404, 2021, DOI. , vol. 395, p. 002, 2021, . 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