review article measurement of atmospheric neutrino...

Review ArticleMeasurement of Atmospheric Neutrino Oscillations withVery Large Volume Neutrino Telescopes

J P Yaacutentildeez1 and A Kouchner2

1DESY 15735 Zeuthen Germany2Laboratoire AstroParticule et Cosmologie (APC) Universite Paris Diderot CNRSIN2P3 CEAIRFUObservatoire de Paris Sorbonne Paris Cite 75205 Paris France

Correspondence should be addressed to J P Yanez juanpabloyanezdesyde

Received 18 September 2015 Accepted 1 November 2015

Academic Editor Vincenzo Flaminio

Copyright copy 2015 J P Yanez and A Kouchner This is an open access article distributed under the Creative Commons AttributionLicense which permits unrestricted use distribution and reproduction in any medium provided the original work is properlycited The publication of this article was funded by SCOAP3

Neutrino oscillations have been probed during the last few decades using multiple neutrino sources and experimental set-ups Inthe recent years very large volume neutrino telescopes have started contributing to the field First ANTARES and then IceCubehave relied on large and sparsely instrumented volumes to observe atmospheric neutrinos for combinations of baselines andenergies inaccessible to other experiments Using this advantage the latest result from IceCube starts approaching the precision ofother established technologies and is paving the way for future detectors such as ORCA and PINGU These new projects seek toprovide better measurements of neutrino oscillation parameters and eventually determine the neutrino mass ordering The resultsfrom running experiments and the potential from proposed projects are discussed in this review emphasizing the experimentalchallenges involved in the measurements

1 Introduction

Massive mixed neutrinos inferred from the phenomenonof oscillations remain until this day the only physics foundbeyond the original formulation of the Standard ModelWhile the Standard Model can be extended to accountfor these experimental facts precise measurements of theparameters involved in the phenomenon are necessary to

constrain the different theories that attempt to explainit

The current knowledge favors the existence of three activeneutrinos (flavor eigenstates ]

119890 ]120583 and ]

120591) whose mixing

can be fully determined by the PMNS (Pontecorvo-Maki-Nakagawa-Sakata) matrix 119880 The matrix is often parameter-ized as the product of three rotation matrices related to themixing angles 120579

12 12057913 and 120579

23 and a complex CP phase 120575

119880 = (

1 0 0

0 11988823

11990423

0 minus11990423

11988823

)(

11988813

0 119890minus119894120575

11990413

0 1 0

minus119890119894120575

11990413

0 11988813

)(

11988812

11990412

0

minus11990412

11988812

0

0 0 1

)(

1198901198941205881 0 0

0 1198901198941205882 0

0 0 1

) (1)

where 119888119894119895

equiv cos 120579119894119895and 119904119894119895

equiv sin 120579119894119895 The last matrix in the

multiplication does not affect neutrino oscillations and onlyexists if neutrinos are Majorana particles [1]

The three angles that determine the mixing matrix areknown to a precision of 10 or better [2ndash4] The absolutedifferences of the square of the masses (mass splittings

Hindawi Publishing CorporationAdvances in High Energy PhysicsVolume 2015 Article ID 271968 24 pageshttpdxdoiorg1011552015271968

2 Advances in High Energy Physics

Δ1198982

119894119895= 1198982

119894minus 1198982

119895with 119894 119895 = 1 2 3) which play a role in

oscillations are known to a precision better than 5 Whilethe sign of themass splitting between the states 1-2 (119898

2gt 1198981)

is known from matter effects in solar neutrino oscillationsthe relative difference between119898

3and119898

1remains unknown

The relative values of the neutrino masses are commonlyreferred to as the neutrino mass ordering (NMO) (thedetermination of the mass ordering is sometimes confusedwith the determination of the neutrino ldquomass hierarchyrdquowhich requires additional information on the absolute scaleof the neutrino masses [5]) which has two possible optionsthe normal ordering (NO) with 119898

1lt 1198982

lt 1198983 and

the inverted ordering (IO) with 1198983

lt 1198981

lt 1198982 The

determination of the NMO is important as the parametercan discriminate between flavor symmetry models [6] Alsothe sensitivity of experiments attempting to determine theneutrino nature depends on theNMO [7 8] Finally knowingthe NMO would help to measure the value of the 120575 phasewhich in turn would be an important step forward towardssolving the fundamental question of the prevalence of matterover antimatter in the Universe Better measurements of allthe parameters involved in neutrino oscillations are thereforenecessary to understand if the current model is correct andhow to incorporate it to the Standard Model

In this view atmospheric neutrinos remain a promisingtool for studying oscillations they cover a wide energy rangefrom MeV to TeV and can reach a detector after travelingdistances from a few to about 12700 km when they cross theEarth No man-made beam covers a similar parameter spaceHowever the flux strongly decreases with energy Detectingit implies building large detectors such as very large volumeneutrino telescopes (VLVNTs) to study atmospheric neutrinooscillations

In the recent years first ANTARES and then Ice-CubeDeepCore have proven that these studies are feasibleby analyzing interactions of neutrinos with energy as low as15GeVThe current result from IceCube on sin2120579

23and Δ1198982

32

reaches a precisionwhich is only a factor of three to four timesless stringent than global fits which combine all available data[2 3 9] Building upon the success of these studies proposalsof new more densely instrumented telescopes as extensionsor part of new projects have appeared PINGU and ORCAaim to improve the precision of these measurements andreduce the energy threshold to a fewGeVwherematter effectsare strong and use these effects to measure the NMO

This review begins by covering in Section 2 the currentknowledge on atmospheric neutrinos and how oscillationsaffect their flux Section 3 describes the design and operationof VLVNTs Special attention is paid to relevant sources ofuncertainty The neutrino oscillation results produced bythese experiments until this date are covered in Section 4Section 5 discusses the possible studies with future detectorsand a short summary is given in Section 6

2 Atmospheric Neutrino Oscillations

The flux of atmospheric neutrinos in the energies relevant fora VLVNT together with how the flux is modified by neutrino

oscillations for those neutrinos that cross the Earth is thetopics covered in this section

21 A Neutrino Beam from Cosmic Rays Cosmic rays (CR)continuously arrive at the Earth from all directions andinteract with nuclei in the atmosphere at altitudes of about25 km above sea level and initiate showers of particles Duringthe shower development charged mesons are produced thateventually decay in comparable numbers of muons andneutrinos

CR + 119873 997888rarr 119883 + 120587∓

119870∓

120587minus

119870minus

997888rarr 120583minus

+ ]120583

120587+

119870+

997888rarr 120583+

+ ]120583

120583minus


+ ]119890+ ]120583

120583+

997888rarr 119890+

+ ]119890+ ]120583

(2)

The atmospheric muons produced in air showers cantravel long distances before they decay They are able topenetrate deep into the Earth depending on their energyand the material that they are crossing [1] and constitute thedominant background in the measurement of atmosphericneutrinos

Atmospheric neutrinos have been measured over a wideenergy range [10ndash18] and multiple models predict their flux[19ndash21] (see Figure 1)Themost noticeable difference betweenthe models is the absolute flux which changes by up to 20both for electron and for muon (anti)neutrinos Apart fromthat the models agree that atmospheric neutrinos follow apower-law energy spectrum with a spectral index close to 3in the energy range 119864] = [3ndash100]GeV Measurements from[11] estimate an uncertainty of plusmn004 on the spectral index ofatmospheric neutrinos A similar uncertainty has been alsoderived from varying the underlying cosmic ray model inneutrino flux calculations [22]

Muon neutrinos dominate the flux and also havethe hardest spectral index (see Figure 1) Since electron(anti)neutrinos mainly come from muons that lose energybefore decaying (see (2)) their spectral index is softer andtheir relative contribution to the total neutrino flux dependson energy and direction The direction-averaged flux of ]

120583is

between 11 and 13 times smaller than that of ]120583 depending

on the energyThe electron (anti)neutrino direction-averagedflux at a few GeV is about 25 times smaller than its muon(anti)neutrino counterpart Figure 2 shows isocontours of theneutrino flux flavor ratio as a function of energy and zenithangle for neutrinos that cross the Earth The flux differencebetween ]

120583and ]

119890grows with both energy and | cos 120579

119911|

Already at 40GeV the direction-averaged ratio is close tofour

Above 10GeV the neutrino flux as a function of zenithangle is almost symmetric around cos 120579

119911= 0 The angular

dependence of the flux at the detection site is influenced byhadronization processes the local atmospheric density andgeomagnetic effects at the interaction pointTheuncertaintiesassociated with these processes result in energy-dependent

Advances in High Energy Physics 3

400

300

200

100

0

120601E3

(mminus2

secminus

1srminus1

GeV

2)

e

e

120583

120583

HKKM15

BartolFluka

4 6 8 10 20 30 40

E (GeV)

Figure 1 Comparison of predicted atmospheric neutrino fluxesper flavor for the energy range relevant for neutrino oscillationmeasurements with VLVNT Reproduced from [19 23]

00

minus02

minus04

minus06

minus08

minus10

30

70

20

40

50

60

80

90

100

110

4 6 8 10 20 30 40

E (GeV)

cos(120579z)

(u + u)(e + e)

Figure 2 Isocontours of the ratio of (]120583+ ]120583)(]119890+ ]119890) as a function

of energy and neutrino arrival direction for neutrinos that cross theEarth as predicted by the latest HKKM model [23] The ratio isnearly up-down symmetric

modeling errors of the arrival zenith angle by up to 20on the ratio ]] for muon neutrinos and 8 for electronneutrinos [22]

22 Neutrino Oscillations at 119864] ge 5GeV The flux of atmos-pheric neutrinos at a detection site ismodified by oscillationsThe oscillations that act over the 119871119864 parameter spaceaccessible with atmospheric neutrinos that cross the Earth(119871119864 sim 10

1ndash103 kmGeV) aremainly driven by the largemasssplitting Δ1198982

32≃ Δ119898

2

31 and the mixing angles 120579

13 12057923 These

are therefore parameters that VLVNTs are sensitive toNeutrinos propagating inmatter are subject to a potential

due to coherent forward scattering with the particles in themedium [24] For explanatory purposes we consider the caseof neutrinos traveling through matter with constant electron

density that results in a potential 119860 = plusmn2radic2119866119865119899119890(119909)119864]

where 119866119865is the Fermi constant and the plus (minus) sign

corresponds to neutrinos (antineutrinos) Computation ofneutrino oscillation probabilities for the relevant energies hasbeen done in [25] fromwherewe take the approximations forthe ]120583to ]119890transition given by

119875120583119890

≃ sin212057923sin22120579119872

13sin2 [Δ119872 119871

4119864] (3)

while the survival probability of ]120583is a somewhat more

complicated expression

119875120583120583

≃ 1 minus sin212057911987213sin22120579

23sin2 [(Δ minus Δ

119872

+ 119860)119871

8119864]

minus cos212057911987213sin22120579

23sin2 [(Δ + Δ

119872

+ 119860)119871

8119864]

minus sin412057923sin22120579119872

13sin2 [Δ119872 119871

4119864]

(4)

and the transitions to ]120591are simply

119875120583120591

≃ 1 minus 119875120583119890minus 119875120583120583 (5)

In these expressions Δ equiv Δ1198982

31and Δ

119872 is the effective masssplitting in matter given by

Δ119872

≃ radic(Δ1198982

31cos 2120579

13minus 119860)2

+ (Δ1198982

31sin 2120579

13)2

(6)

The superscript 119872 also accompanies 12057913 whose effective

value in matter is

sin 212057911987213

≃Δ1198982

31sin 2120579

13

Δ119872 (7)

The mixing angle 12057923

is known to be close to maximal(sim1205874) and |Δ119898

2

31| is of the order of 10minus3 eV2 [1] The angle

12057913

has been recently measured and found to be small butnonzero [26ndash28] It is then the case that 120579119872

13can acquire any

value depending on the neutrino energy and the electrondensity of the material being crossed as shown in (7) Fora low electron density or neutrino energy the parameters(and equations) in vacuum are recovered A particularlyinteresting case appearswhen119860 = Δ119898

2

31cos 2120579

13 which gives

120579119872

13= 1205874 maximizing the mixing between states 1ndash3 that is

a resonance appears [29]The effectivemass splitting acquiresits minimum value under this condition and is reduced by afactor sin 2120579

13

The resonance that leads to maximal 1ndash3 mixing canonly happen if the potential 119860 and the mass difference Δ1198982

31

have the same sign and so for neutrinos in the case of NOand antineutrinos in the case of IO Identifying whether theresonance takes place in neutrinos or antineutrinos is a wayto identify the NMO

For 119860 ≫ Δ1198982

31cos 2120579

13a saturation effect occurs where

the effective angle in matter goes to 1205872 and the effectivemass splitting is thenwell approximated by119860 In the saturatedregime transitions of the type ]

119890rarr ]

120583 given in (3)


00

minus02

minus04

minus06

minus08

minus104 6 8 10 20 30 40 50

cos(120579z)

10

08

06

04

02

00

E (GeV)

e rarr e (NO)

(a)

10

08

06

04

02

00

00

minus02

minus04

minus06

minus08

minus104 6 8 10 20 30 40 50

cos(120579z)

E (GeV)

120583 rarr 120583 (NO)

(b)

Figure 3 Survival probabilities for ]119890(a) and ]

120583(b) as a function of neutrino energy and arrival direction for Earth crossing trajectories

affected by oscillations (cos(120579119911) le 0) Calculated using the values in [3] assuming a normal mass ordering Resonant matter effects produce

the large disappearance of ]119890around 6GeV and cos 120579

119911sim minus08 as well as the discontinuities on the survival pattern of ]

120583below 15GeV The

abrupt changes observed at cos 120579119911sim minus085 minus045 are due to sharp jumps in the electron density profile of the EarthThe dashed line indicates

the connection between these figures and Figure 4

are suppressed by the factor sin2212057911987213 The effective matter

parameters also modify 119875120583120583

by making the last two terms in(4) go to zero resulting in the simpler expression

119875120583120583

= 1 minus sin2212057923sin2 [Δ 119871

4119864] (8)

with all the oscillated ]120583turning into ]

120591

The CP-violating phase 120575 is not present in the approx-imate formulas shown The reason is that the parameter 120575always appears in oscillation probabilities accompanied bya factor Δ1198982

21Δ1198982

31 which suppresses its contribution [30]

Note however that the approximations presented here servethe purpose of explaining the main features of neutrinooscillations in matter Figures contained in this review aswell as the latest data analyses discussed use numericalcalculations of oscillation probabilities that do not rely onsimplified analytical expressions

23 An Oscillating Atmospheric Neutrino Flux The atmo-spheric neutrinos under consideration of a few GeV aremostly ]

120583+ ]120583produced around a height of 25 km in the

atmosphere where the matter density is low enough tobe approximated as vacuum For most production anglesthe neutrinos proceed to cross the Earth which has anonnegligible matter density

Earthrsquos matter profile can be well explained as concentricshells each onewith a constant density [31] To study the tran-sitions that take place consider the oscillation parametersfrom [3] and the electron number density of the mantle119899119890

= 25 cmminus3119873119860 where 119873

119860is Avogadrorsquos number Neu-

trinos crossing the mantle experience the resonance around119864] ≃ 6GeV (see (7)) while the saturation condition 119860 ≫

Δ1198982

31cos 2120579

13is fulfilled already at 119864] sim 12GeV Neutrinos

measured by VLVNTs then experience oscillations in eitherthe resonant or saturated regime depending on the energythreshold of the detector

Another interesting effect takes place on neutrinos thatcross the Earthrsquos core These neutrinos experience a symmet-ric electron density profile that changes abruptly For the rightcombination of neutrino energy and electron densities a so-called parametric resonance can appear [32ndash35] The effecthowever is not the dominant one at the energies to whichfuture projects (Section 5) will be sensitive

In the saturated regime atmospheric neutrino oscillationsare independent of the mass ordering dominated by ]

120583rarr

]120591transitions and well described by (8) Near the resonance

condition transitions involving electron (anti)neutrinos alsoplay a role and patterns become complex Figure 3 shows thesurvival probabilities of ]

119890and ]120583for neutrinos and normal

mass orderingThe original electron neutrino flux is expectedto fully disappear due to matter effects over 119864] = [5 8]GeVand cos 120579

119911= [minus09 minus05] The suppression of these oscilla-

tions due to saturation can be observed at about 10GeV Thesurvival probability of ]

120583shows abrupt changes that are due to

the effects of matter Muon neutrinos oscillate even if the res-onance conditions are not fulfilled which makes the effectsof the resonance less obvious than for electron neutrinosResonant matter effects appear in the ]

120583survival probability

asmodifications on the otherwise smooth andperiodic disap-pearance pattern as shown in Figure 3 Saturation is reachedabove 15GeV and the survival probability becomes smooth

Figure 4 shows the transition probabilities of ]119890and ]

120583

into different flavors for the arrival direction cos 120579119911= minus07

assuming a normal mass orderingThey correspond to a one-dimensional projection of Figure 3 along the dashed lineThebands demonstrate how the uncertainties on the oscillationparameters impact the expected probabilities For ]

119890it is

easy to observe the same disappearance as in Figure 3 withneutrinos oscillating equally into ]

120583and ]120591 Transitions of ]

120583

to other flavors are complicated bymatter effects which openthe ]120583harr ]119890channel and thus modify the survival probability

of ]120583


Measurements of neutrino fluxes above the saturationenergy of about 15GeV are largely independent of 120579

13 the

neutrinoantineutrino admixture of the sample and theordering of neutrino masses They provide excellent data fordetermining sin2120579

23as well as |Δ1198982

31|

The NMO can only be accessed with neutrinos below15GeV where matter induced resonances occur either forneutrinos or for antineutrinos The survival probability ofmuon (anti)neutrinos the main component of atmosphericneutrinos is modified by matter effects by about 20 As willbe discussed in Section 3 VLVNT cannot separate neutrinosfrom antineutrinos event-wise and instead rely on the ]]fluxratio and the difference in cross sections to identify whetheroscillation probabilities of neutrinos or antineutrinos aremodified by matter effects

An interesting feature introduced by matter effects isthat instead of oscillating fully into ]

120591 muon neutrinos also

change into ]119890 Transitions of these type are almost symmetric

between the two flavors (see Figure 4) but since the flux of ]120583

is several times that of ]119890at the energy and zenith angle of

interest (see Figure 2) the net effect is a significant excess ofelectron neutrinos with respect to the original ]

119890flux In the

NO the ]119890flux is enhanced while for an IO the enhancement

is realized for ]119890 Because of the initial ]

120583]120583flux ratio and

the differences in the ]119890]119890cross sections different orderings

result in a different number of detected events Figure 5 showsthe ratio between expected interaction rates of ]

119890+ ]119890for

normal and inverted orderings including all of the oscillationchannels A factor of 21 is applied to neutrinos to accountfor the difference in cross sectionsThe normalmass orderingpredicts up to 30 more events in the region 119864] = [5 8]GeVand cos 120579

119911= [minus09 minus05] Measurements of the flux of

atmospheric electron neutrinos thus provide suitable data fordetermining the NMO

The VLVNTs currently in operation are presented indetail in the next section With an energy threshold ofabout 15GeV they operate in the saturated regime They canmeasuremuonneutrino disappearance aswell as tau neutrinoappearance and thus 120579

23and |Δ119898

2

31| Measuring the sign of

Δ1198982

31 on the other hand requires measuring differences in

oscillation probabilities below this threshold (see Figures 3and 4) This is the main goal of the next-generation detectorsdiscussed in Section 5

3 Very Large Volume Neutrino Telescopes

A generic VLVNT is a three-dimensional array of photo-sensors detecting the Cherenkov light of charged particlesproduced after a neutrino interaction The secondaries ofneutrino interactions above a few GeV produce enough lightso that they can be observed by sensors several meters apartThe spacing between the optical sensors defines the energythreshold of VLVNTs which is approximately 15GeV incurrently operating detectors

31 VLVNTs in Operation The optical sensors of VLVNTsare deployed at depths of 1 km or more in an opticallytransparent naturally occurringmedium Sensors are laid outin lines or strings that are operationally independent The

10

08

06

04

02

005 7 10 20 50

E (GeV)

Tran

sitio

n pr

obab

ility

e rarr 120583e rarr 120591

e rarr e

(a)

5 7 10 20 50

E (GeV)

10

08

06

04

02

00

Tran

sitio

n pr

obab

ility

120583 rarr 120583120583 rarr 120591

120583 rarr e

(b)

Figure 4 Transition probabilities for electron (a) and muon (b)neutrinos that arrive at a detector from cos 120579

119911= minus07 (mantle-

crossing trajectory marked by a dashed line in Figure 3) The bandsencompass the results of the calculation once the uncertaintieson the oscillation parameters from [3] are included Normal massordering is assumed If the resonance was absent (inverted massordering or transitions for antineutrinos) (a) would show oscil-lations with amplitudes smaller than 01 while (b) would showtransitions only between muon and tau neutrinos

spacing between sensors is uneven being considerably largerin the119909-119910 plane (in between linesstrings) than in the 119911 planeThe sensors also have a preferred acceptance for light comingfrom below although this might change for future detectors

The neutrino telescopes currently in operation are Ice-Cube in Antarctica [42] ANTARES in the MediterraneanSea [43] and the prototype of the Gigaton Volume Detectorin Lake Baikal [44] Both ANTARES and IceCube have


140

125

110

095

080

065

050

cos(120579z)

00

minus02

minus04

minus06

minus08

minus104 6 8 10 20 30 5040

E (GeV)

(21 times Φ(e) + Φ(e) NO) (21 times Φ(e) + Φ(e) IO)

Figure 5 Expected interaction rate of electron neutrinos andantineutrinos predicted by a NO over the rate predicted assumingan IO Using the oscillation parameters in [3] Because of the fluxratio ]

120583]120583and the cross section difference estimated to be 21 times

larger for neutrinos than antineutrinos more electron neutrinointeractions are expected for a NO

published studies of neutrino oscillations and are thereforethe only ones discussed in this review

311 Detector Design and Layout ANTARES is locatedbetween depths of 2025ndash2475m 20 km away from Toulon(French Riviera) in the Mediterranean Sea [43] It comprises885 optical modules (OMs) [45] distributed along 12 flexiblelines OMs are grouped in triplets with 25 triplets per lineThe distance between triplets is 145m and the separationbetween lines ranges from 60 to 70m as sketched in Figure 6Acoustic devices tiltmeters and compasses are used tomonitor the shape of the detector which is influenced by seacurrents

IceCube is located at depths between 1450 and 2450m atthe geographic South Pole [42] The in-ice part of IceCubeconsists of 5160 downward-facing digital optical modules(DOMs) [46] The detector has 86 strings each holding 60DOMs Of these 78 strings are arranged in a hexagonal gridwith a typical distance of 125m (horizontal spacing) and 17m(vertical spacing) between DOMs A sketch of the detectorlayout is shown in Figure 7

The lower center region of IceCube from 1760m downto 2450m houses DeepCore [47] a region of denser instru-mentation (7m DOM vertical spacing) where eight stringsare separated by 40ndash70m Some 50 of the PMTs in thisregion have 35 higher quantum efficiency than the standardIceCube PMTs The DeepCore fiducial volume used for dataanalysis is defined by a cylinder with a height of 350m and aradius of approximately 150m that starts below a dust layerwhere the light transparency is reduced as shown in Figure 7This volume which corresponds to roughly 25 times that ofANTARES encloses about 550 DOMs with reduced spacingand results in a threshold for detection and reconstruction ofneutrinos of about 15GeV

The optical modules of both IceCube and ANTARESare glass spheres enclosing a ten-inch PMT optical couplinggel and a 120583-metal cage for magnetic shielding The IceCube

Buoy

IL07

sim480

m

145m

100m

sim180m

Anchorsim180m

Junction box

(a)

Glass spherePenetrator

LED

Optical gelPhotomultiplier

Vacuum value

Base

Magnetic shield

(b)

Figure 6 The ANTARES detector configuration (a) The 12 detec-tion lines are connected to a single junction box providing powerand transferring all data recorded by the OMs to the shore stationthrough a main electrooptical cable (b) shows the OM and thecomponents it houses including a 1010158401015840 photomultiplier tube

OM digitizes the waveforms detected by the PMT inside themodule before transmission [46] while the ANTARES OMkeeps the readout to a minimum and only transmits the timeand amplitude of a signal above threshold [53] ANTARESoptical modules have a baseline noise rate of 70 kHz at singlephoton level [54] while for IceCube (DeepCore) OMs thenoise is 045 kHz (065 kHz) [55]

312 OpticalMediumandCalibration Theoptical propertiesof the medium affect the time of arrival and the numberof detected Cherenkov photons At the ANTARES site (saltwater) the absorption length which is 60m for blue light(120582 ≃ 470 nm) and 26m for UV light (120582 ≃ 375 nm) reducesthe number of photons observed The effective scatteringlength which is 256m for blue light and 122m for UVlight is considerably larger than the spacing between sensors[56] In the clear ice in which DeepCore is located theabsorption length of UV light (120582 ≃ 400 nm) is of the orderof 200m which is larger than the spacing between sensorsThe effective scattering length in the deep Antarctic ice is


10 DOMrsquos10m spacing1750ndash1860m

(in red)

Dust layer


(in green)

minus1450

minus1550

minus1650

minus1750

minus1850

minus1950

minus2150

minus2050

minus2250

minus2350

minus2450

75m

40m

DeepCore volume

125m

600m

Figure 7 IceCube Top and side schematic projections of thedetector The DeepCore volume used for analysis is highlighted inboth figures

approximately 50m comparable to the string distance ofDeepCore thus significantly modifying the expected time ofarrival of photons [57 58]

Water offers the advantage of being a homogeneousmedium Nonetheless sea currents can deviate the detectorlines so the position of the lines needs to be monitored con-stantlyThis is achieved by combining acoustic triangulationswith tilt and compass measurements yielding a precisionbetter than 10 cmwhich does not affect the angular resolution[59] High sea currents can also trigger bioluminescencebursts that must be accounted for in the optical backgroundsimulation in addition to the stable optical noise arisingfor 40K decays The latter can be used for determining theabsolute detection efficiency of the optical modules

In ice the positions of the optical modules are fixed andknown to be within a few cm Noise levels are constant and ahundred times lower than in salt water after the detector hasstabilized A disadvantage of using ice is that the medium isnot homogeneous and its structure has to be modeled Thisis particularly challenging in the immediate surroundingsof the optical modules Columns of the original glacier aremelted to deploy the instrumentationThe refreezing processleaves behind clear ice near to the boundaries of the hole

and a cylinder of ice of about 10 cm in diameter with a highconcentration of bubbles towards the center of the columnThese changes in ice properties modify the DOM angularacceptance measured in the laboratory Future detectors inice will consider the possibility of degassing thewater to avoidtrapping air bubbles inside the hole ice and with that reducethe impact of the medium

The absolute optical efficiency of the optical modulesas well as their angular acceptance must be determinedin situ after deployment ANTARES and IceCube use bothcontrolled light sources and minimum ionizing muons tocalibrate the efficiency and timing accuracy of their opticalmodules [60ndash62] Relative arrival times are known with aprecision better than 3 ns and 15 ns for IceCube [46] andANTARES respectively

32 Neutrino Interactions The dominant neutrino interac-tion for most of the energy range that VLVNTs can accessis neutrino-nucleon deep inelastic scattering (DIS) withother processes being only a subdominant contributionNonetheless below 15GeV the region of interest to search formatter effects in neutrino oscillations and the NMO quasi-elastic scattering and production of resonances competewithDIS processes Figure 8 shows a calculation of the competing]119873 cross sections around the GeV region together with thedata available

Most of the knowledge of neutrino-nucleon cross sectionsbetween 1 and 15GeV comes from bubble chambers or sparkchamber detectors which collected comparatively small datasamples Thus the constraints on the models that describethem are rather weak [36] The uncertainty with the largestimpact on the neutrino cross sections for quasi-elastic andresonant interactions which changes them by up to 40is the value of the axial mass that effectively describes thenucleon form factor and has an estimated error of 15ndash25[36 63] DIS interactions in the crossover region have a smallmomentum transfer Nonperturbative QCD calculations arerequired [64] and the estimated errors are as well of the orderof 20 [65]

Deep inelastic scattering accounts for 90 or more ofthe total cross section of neutrinos and antineutrinos abovean energy of roughly 12GeV as shown in Figure 8 DIS inthe perturbative regime is comparatively better understoodthan the processes discussed so far with uncertainties comingmainly from the determination of the parton distributionfunctions (PDFs) of the nucleons The uncertainties on thePDFs change the total cross section by 5 or less [65]

At these energies the neutrino-nucleon DIS chargedcurrent (CC) cross section is quasi-independent of theinelasticity 119910 (119910 = 1 minus 119864lepton119864]) of the interaction whilefor antineutrinos the cross section is accompanied by a factor(1 minus 119910

2

) which suppresses kinematic configurations wherethe hadronic part of the interaction takes most of the energyThe inelasticity dependence makes the total ]119873 cross sectionabout one-half of that of ]119873

While the neutrino-nucleon DIS CC cross sections for ]119890

and ]120583are equal the ]

120591119873 one is suppressed due to themass of

the tau lepton It is only at 119864] sim 40GeV that the cross sectionreaches half of the value of the other neutrino flavors [66]


1 100

02

04

06

08

1

12

14

Total

QE

DIS

RES

cr

oss s

ectio

nE(10minus38

cm2G

eV)

10minus1 102

E (GeV)

(a)

0

005

01

015

02

025

03

035

04

1 1010minus1 102

E (GeV)

cros

s sec

tionE(10minus38

cm2G

eV)

Total

QEDIS

RES

(b)

Figure 8 Collection of existingmuon neutrino (a) and antineutrino(b) charged current cross sectionmeasurements and predictions as afunction of neutrino energy (see [36] for details on the experimentscontributing to the data points and [37] for a description of themodel used) The contributing processes in this energy regioninclude quasi-elastic (QE) scattering resonance production (RES)and deep inelastic scattering (DIS) Taken from [36]

In neutral current interactions (NC) one or severalhadrons are produced initiating a hadronic shower Incharged current (CC) interactions a hadronic shower is alsopresent but now the neutrino transforms into a chargedlepton Electrons and taus also initiate a shower of particlesafter they are produced (the tau lepton has a 17 probabilityto decay into a muon However due to energy losses andother particles involved in the processes muons from taudecays with a range larger than a fewmeters are uncommon)Muons on the other hand travel practically undisturbedand lose energy at a quasi-constant rate For muons passingthrough water 119889119864119889119909 sim 025GeVm up to a few hundredGeV [1] Once they travel distances comparable to thedetector spacing they can be identified and charged current]120583interactions can be tagged

33 Event Reconstruction Neutrino interactions are recon-structed using the number of photons recorded by the optical

module (or time over threshold) as well as the time at whichthey arrive For the energy range under consideration themost general hypothesis is an interaction which produces ahadronic shower (all interaction types) an electromagneticshower (]

119890CC) or a long rangemuon (]

120583CC)The direction

in which these particles are produced is reconstructed fromthe arrival times of the emitted photonsThe Cherenkov lightof muons is produced almost perfectly in a cone The lightcoming from the cascade is also beamed in the Cherenkovangle but the smearing due tomultiple particle contributionsto it is larger which degrades the achievable precision ofdirectional reconstructions This smearing effect is strongerfor hadronic showers

The energy reconstruction of showers is primarily givenby the number of photons detected from a given interac-tion and its accuracy depends mainly on the reconstructedposition of the interaction vertex To estimate the energyan assumption has to be made on whether the shower ishadronic or electromagnetic The energy of muons can beestimated by the observed range in the detector

In principle it is possible to fit the directions of bothcascade and track components in an interaction The sparseinstrumentations of the detectors however make it chal-lenging In the simplest approach tracks and cascades areassumed to be collinear

34 Simulation Tools The measurement of diffuse fluxes inVLVNTs such as the one required to determine oscillationparameters relies fully on the correct modeling of the exper-imental set-up Atmospheric muons the leading source ofbackground are simulated in IceCube using full showers andparameterizations obtained from CORSIKA [69] ANTARESuses the MUPAGE program which produces muons basedon a parameterization tuned to MACRO data [70]

Neutrino interactions in IceCube are simulated using theGENIE package [71] (119864] le 200GeV) and NuGenANIS[72] (119864] ge 50GeV) Besides GENIE ANTARES uses an in-house neutrino generator based on LEPTO [73] for the fullenergy range with the PYTHIA package [74] handling thehadronization processes The neutrinos produced are thenweighted to match the flux predictions of the Honda andorBartol groups [20 75]

The propagation of short-ranged particles produced inthe interaction is done both in IceCube andANTARES usingtheGeant software [76] as basis Parameterizations of the lightyield of these particles are produced by both experiments andused to obtain the detector response to high-energy hadronselectrons and photons [77] while low-energy hadrons (119864 le

30GeV) are propagated individually Muons are propagatedusing code optimized for simulation of long ranged leptonsnamelyMUSIC [78] andMUM [79] in ANTARES andMMC[80] in IceCube

The Cherenkov photons produced during the propaga-tion of charged particles are individually traced through theice in IceCubeDeepCore while ANTARES uses expectationfrom tables Low-energy future projects (Section 5) plan touse individual photon tracing to assure that the opticalproperties of the medium are included in detail After thephotons are propagated the response of the optical module is


recreated and events from simulation and experimental dataare treated equally

35 Large Statistics versus Precise Reconstruction Thecurrentknowledge on the oscillation parameters in the atmosphericsector comes from experiments which differ from VLVNTssubstantially they are Super-Kamiokande [81] T2K [82]MINOS [83] which is no longer in operation and the recentlycommissioned NOvA [84] Table 1 contains a qualitativecomparison of the detectors and neutrino sources used bythese experiments and VLVNTs

Super-Kamiokande which also measures atmosphericneutrinos has about twenty (ten) times the number of opticalsensors as DeepCore (ANTARES) separated by a few cmplaced on a cylindrical tank with a diameter similar to theinterstring distance in ANTARESDeepCore Neutrinos aredetected using the rings produced after the Cherenkov lightof the charged products of the interaction hits the walls of thedetector Muons electrons and pions can be identified by thedifferences in the ring pattern they produce Because of itsconsiderable smaller size and the steepness of the spectrumof atmospheric neutrinos its operating energy is lower thanthat of VLVNTs

Long baseline experiments such as T2K MINOS andNOvA use neutrinos fromparticle accelerators andhave nearand far detectors While T2K uses Super-Kamiokande as afar detector MINOS and NOvA follow an experimental set-up where the far detector is smaller than Super-Kamiokandebut is more densely instrumented can be magnetized andobserves the path of individual particles coming from a neu-trino interaction These set-ups benefit from their controlledneutrino source and detailed event reconstruction Unlikethe case of atmospheric neutrino experiments long baselineexperiments have a unique baseline and cover a narrowenergy range allowing for better precision but also limitingthe 119871119864 region that they can access It should also be notedthat as stated in Section 32 the poor knowledge of neutrinointeractions at energies of a few GeV introduces significantuncertainties in the data analysis of long baseline oscillationexperiments

VLVNTs have become competitive with accelerator basedexperiments thanks to the possibility of observing multiplecombinations of baseline and energy (119871119864) and with Super-Kamiokande becauseVLVNTs can collect large event samplesand in an energy range where most events are DIS which canbe modeled with high accuracy The sparse instrumentationdoes not permit observation of small details of the interactionbut in the same way reduces the impact from uncertaintiesin the hadronization processes one of the leading systematicuncertainties for MINOS [87] and T2K [4] Reconstructionaccuracy and proper handling of systematic uncertaintiesare the most important points to consider for precisionmeasurements with VLVNT

4 Neutrino Oscillation Measurements fromRunning VLVNTs

The ANTARES and IceCube collaborations have publishedmeasurements of oscillations studying the muon neutrino

disappearance channel Above 15GeV where these detectorsoperate muon neutrinos oscillate into tau neutrinos follow-ing (8) Signal neutrinos that is ]

120583interacting via CC with

119864] sim 25GeV are typically recorded by a handful of opticalmodules both for ANTARES and for IceCubersquos DeepCoreThe events develop over a distance of order of 100m and thuscan be fully contained in both detectors

The measurement of neutrino oscillations in VLVNTsfollows a general strategy which begins with the reductionof the dominant sources of background that is atmosphericmuons and pure noise Straight cuts are applied on variablesof which the distribution for neutrinos differs from that ofbackground sourcesThey generally aim for a neutrino purityhigher than 95

For the currently published results of both experimentsthe presence of a muon in a neutrino interaction is requiredfor an event to be selected for analysis The analyses aredone by comparing the histograms of data and simula-tion as a function of the reconstructed variable(s) usedThe simulation is modified by the physics parameters ofinterest 120579

23and Δ119898

2

32 and by nuisance parameters which

absorb the systematic uncertainties involved in the mea-surement Errors are derived from a scan of the likeli-hood landscape andor directly using a 120594

2 approxima-tion

The results of ANTARES and IceCube that have beenmade public until now use only events coming below thehorizonANTARES removes the downgoing region because itis dominated by atmosphericmuons IceCube uses the instru-mentation outside DeepCore to veto atmospheric muonsnevertheless the contribution of these muons in the down-going region is still significant so the region is alsoremoved from analysis This situation is different for Super-Kamiokande where events from the entire zenith range areused in oscillation studies and top-down ratios are used toreduce uncertainties Ongoing studies within IceCube areexploring the possibility of using neutrinos coming fromabove the horizon in future results [88]

41 First Measurements of Oscillations from ANTARES TheANTARES collaboration presented the first results on thestudy of neutrino oscillations from VLVNTs [38] The analy-sis relied on themuon track reconstruction described in [89]which fits the depth at which the Cherenkov cone of lightarrives at the OMs as a function of time This correspondsto a hyperbola of which the orientation of the asymptotesdepends on the zenith angle An algorithm that searchesfor these patterns without assuming any knowledge on thearrival angle of the emitter was implemented The algorithmis capable of rejecting noise hits and keeping events down toenergies of 20GeV (119877

120583= 100m)with photons in a single line

and 50GeV (119877120583= 250m) inmultiple linesMisreconstructed

muons that appear upgoing are removed by selecting onlyevents which have a good fit quality This cut also effectivelyreduces the contribution of NC interactions from all flavorsand ]119890CC interactions

The median zenith angle resolution with respect to theneutrino direction of single-line events is 30∘ and it reducesto 08∘ for multiline events The energy of the neutrino is


estimated solely by the muon range resulting in a lower limitto the neutrino energy where 119864reco = (50 plusmn 22)119864]

The analysis is done by comparing data and simulationas a function of 119864reco cos 120579reco by means of a 1205942 combiningsingle- and multiline selections Only events below the hori-zon (cos 120579reco lt minus015) are considered Systematic uncertain-ties are implemented using two normalization coefficientsfor single- and multiline events as pull factors in the 120594

2

following the method presented in [90] These factors absorbthe effects of changes in the average quantum efficiency(plusmn10) optical properties of sea water (plusmn10) the spectralindex of atmospheric neutrinos (plusmn003) and disagreementsbetween data and simulation during the selection (varyingcut values) The overall normalization of the ]

120583flux and

detector efficiency are left unconstrainedThe data analyzed were taken between March 2007 and

December 2010 corresponding to a detector live time of863 days A total of 2126 neutrino candidates were selectedThe measured oscillation parameters which were found tobe compatible with the worldrsquos average are indicated inFigure 13 Data and simulation were in good agreement asit can be seen in Figure 9 which results in a 120594

2NDF =17121 The case of no oscillations could be rejected at the 3120590confidence level The ANTARES collaboration will proceedto an updated analysis of this kind with the full data samplecollected until the end of the data taking circa 2017

42 First Measurements from IceCube DeepCore To this dateIceCube has reported results of four neutrino oscillationanalyses of the low-energy DeepCore data The selectionreconstruction and analysis methods have been refined ineach step The low-energy data for all studies comes from theDeepCore filter and trigger [47] The main source of back-ground at this stage are triggers due to sensor self-noise andatmosphericmuonsThe instrumentation outside the fiducialvolume of DeepCore (see Section 21 and Figure 7) is usedto tag atmospheric muons Low-energy neutrino interactionsare required to start within the DeepCore fiducial volumewhile no requirement is imposed for full containment

Systematic uncertainties are accounted for using addi-tional parameters which modify the expected number ofevents An energy-dependent term (119864minus120574 120574 plusmn 005) and a freeoverall normalization absorb total cross section uncertaintiesand the uncertainties on the spectral index of the neutrinoflux The electron neutrino flux is varied by plusmn20 aroundthe predicted value The cosmic ray models which predictthe cosmic muon contamination are varied to obtain a robustestimateThe effects of changing the optical description of thepristine ice as well as the refrozen ice around the DOMs arestudied by producing multiple simulation sets

The initial three oscillation studies from DeepCorepresented first herein were restricted to a single year ofdetector live time Two used a partial configuration (IC79twoDeepCore strings missing) and one used the full detector(IC86) The first analysis [39] from here on IC79-A used aDeepCore low-energy sample where the effect of oscillationsis expected (119864] lt 100GeV 719 events) and an IceCube high-energy sample where oscillations play no role to constrain

Num

ber o

f eve

nts

0

20

40

60

80

100

120

140

160

180

200

ERcosΘR (GeV)0 20 40 60 80 100 120 140

Figure 9 Distribution of 119864reco cos 120579reco for events selected inthe oscillation analysis of ANTARES Data are shown in blacksimulation without oscillations is in blue and simulation with thefit parameters is given in red From [38]

6

5

4

3

2

1

minus1 minus09 minus08 minus07 minus06 minus05 minus04 minus03 minus02 minus01 0

cos(reconstructed zenith angle)

Rate

(Hz)

times10minus6 Low-energy sample

Figure 10 Data and simulation expectation at world averageoscillation parameters (in black) and the case of no oscillations(in red) for the low-energy sample of IceCubersquos IC79-A analysisSystematic uncertainties are split into a fully correlated part (hatchedbands) and uncorrelated part (shaded bands) From [39]

flux and detection uncertainties (119864] ≃ 1TeV 39638 events)The measurement was done by analyzing the distribution ofevents as a function of zenith angle in the low-energy sample(see Figure 10) The zenith angle of both samples was esti-mated using themuon track reconstruction described in [92]Atmospheric muons were mainly removed by reconstructingall events as upgoing and making cuts on parameters relatedto the quality of the reconstruction (without muon tagging)

The data were analyzed using a 1205942 optimization with

pulls also following the method in [90] The results obtainedfor the atmospheric oscillation parameters were compatiblewith contemporary global fits [93] although the errors werea factor 4 to 9 larger (see Figure 13)

Two subsequent analyses of the data from here on IC79-B and IC86-A created new event selections based on therejection of atmospheric muons by using the veto separating


Nonoscillation curvenormalized to

oscillation curvein first three bins

Total simulation

IceCube preliminary

Total simulation no oscExp data

Ratio

120

115

110

105

100

095

090

085

08005 10 15 2520

Log10((L osckm)(L recom))

Figure 11 Ratio of the distribution of oscillation length overreconstructed track length to the no oscillation hypothesis fromsimulation in the IC79-B analysis The best fit is also shown From[40]

the background rejection from the reconstruction of events[40 48] In both cases only the low-energy DeepCore datawere analyzed

The data used for IC79-B were acquired during the sameperiod of time as for IC79-A however due to the change inthe selection of events the final sample studied was a factor10 larger The zenith angle of events was reconstructed witha similar method as in IC79-A [40] A second observablethe reconstructed muon range 119871muon [94] was used as anenergy proxy and the data were analyzed as a functionof both observables The ratio of events with respect tothe no oscillation scenario together with the best fit isshown as a function of reconstructed 119871osc119871 reco in Figure 11where 119871osc is the distance the neutrino traveled and 119871 recois the reconstructed length of the muon produced in theinteraction The best fit and estimated errors of this methodwere similar to those of IC79-A

The first analysis of data from the full detector con-figuration [48] IC86-A was performed using a selectionof photons and event reconstruction based on the methodpublished by ANTARES [89] The selection of photons wasmodified to remove multiply scattered photons instead ofnoise Unscattered or direct photons were identified byrestricting their possible arrival times to those given bythe hyperbolic pattern that Cherenkov light produces as afunction of time as it crosses a string About 70 of theneutrino interactions which trigger the detector do not havea clear core of direct photons and thus are removed

The direct photons found are used to fit track and cascadehypothesesThe zenith angle from the track fit was used as anobservable and the ratio of the 1205942 of the track and cascadefits was used to separate track-like from cascade-like eventsAn estimator of the total energy of the neutrino was alsoimplemented which takes the muon range estimator fromIC79-A and also fits a hadronic cascade at the vertex

In IC79-B and IC86-A the datawere analyzed using a like-lihood optimization with nuisance parameters to account forsystematic uncertainties For IC86-A uncertainties relatedto the detector were also included as nuisance parametersSimulation sets with varied detector settings were producedand interpolated at the final level of the analysis allowing thefitter to make arbitrary modifications to them

In similar live time as IC79-A and IC79-B IC86-Aselected 1487 neutrino events for analysis While the bestfit obtained was in agreement with the other results theerror in Δ119898

2

32was reduced by about 20 with respect to

IC79-A while maintaining a similar precision on sin2212057923

Figure 12 shows a comparison of data and best fit simulationin projections in energy of the two-dimensional histogramused in the analysis A comparison of the confidence regionsin sin2120579

23and Δ119898

2

32of the single year analyses of IceCube

DeepCore together with the result fromANTARES is shownin Figure 13

43 Precision Measurements with IceCube DeepCore Thelatest result from IceCube DeepCore [9] is an update tothe IC86-A analysis introduced before now with almosta thousand days of detector live time The measurementdemonstrates the potential for VLVNTs to become relevantexperiments in the field of neutrino oscillations

While the analysis strategy is still to focus on the selectionon clear tracks for which a core of direct photons can beidentified three large improvements are introduced namely

(i) an optimization of the event selection which resultsin 40 more events

(ii) the cosmic muon background derived from data(tagged muons) avoiding the need of computation-ally expensive model-dependent simulation

(iii) an improved estimator of the energy deposited at theinteraction point which reduces the error on the totalneutrino energy by more than 30 at 20GeV

A demonstration of how the data-derived backgroundis used can be seen in Figure 14 where the distribution ofevents as a function of reconstructed zenith angle at the finallevel and two earlier stages of the event selection is shownAt each step the cosmic muon background is more stronglysuppressed The contribution of atmospheric muons in thedowngoing region can be seen at all steps including the finalsample to be analyzed

For their IC86-B result the IceCube collaboration hasexpanded the list of possible sources of uncertainties con-sidered Non-DIS events are a nonnegligible fraction of thesample at119864reco le 20GeV and additional cross sections uncer-tainties on these interactions (about 20) were also includedA possible shift of 5 in the energy scale of hadronic showerswas also taken into account

In 950 days of live time a total of 5174 events wereobserved while 6830 were expected without oscillationsNote that the energy range of the search was reduced incomparison with IC86-A to 119864reco = [7 56]GeV The datawere analyzed in a full three-neutrino oscillation formalism


DataMC with oscMC no osc


Ereco = [7ndash10] GeV







0

20

40

60

IceCube preliminary


cos(120579reco)

minus10 minus08 minus06 minus04 minus02 000

20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band


0

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40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band


20

40

60

cos(120579reco)


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60

cos(120579reco)


20

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60

cos(120579reco)

Even

ts pe

r ene

rgy

band


0

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60

cos(120579reco)

Even

ts pe

r ene

rgy

band


20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band

Even

ts pe

r ene

rgy

band

Even

ts pe

r ene

rgy

band

Even

ts pe

r ene

rgy

band


Figure 12 Comparison between data and simulation for the two-dimensional histogram used in the IC86-A analysis of IceCube The dataare shown as a function of the zenith angle for the energy bins studied Bands indicate the impact of the estimated systematic uncertaintiesFigure taken from [41]

including the effects induced by matter as neutrinos cross theEarth The parameters that best describe the data assuminga normal mass ordering are sin2120579

23= 053

+009

minus012and Δ119898

2

32=

272+019

minus020times 10minus3 eV2 No significant preference was found for

either the normal or inverted mass orderings Purely sta-tistical uncertainties are +006

minus008for sin2120579

23 and +014

minus015times10minus3 eV2

for Δ1198982

32 from which it is deduced that statistical and

systematic uncertainties have an almost equal impact on theresult

Data and simulation are in good agreement with a1205942NDF=54956 for the energy-zenith angle histogramused

in the fit Figure 15 compares the 119871 reco119864reco distributions ofdata and best fit simulation where the agreement can beobserved (note that the analysis is not done on this variablebut in a two-dimensional energy-zenith angle histograminstead) The 90 confidence contours on the atmospheric

oscillation parameters obtained are shown in Figure 16together with the results from the other experiments leadingthe field

The results from VLVNTs will be further improved byadding statistics to the analyzed data sample and refiningthe reconstruction methods However the most decisiveimprovements will come with the construction of the next-generation VLVNTs presented in the next section

5 Neutrino Oscillations with the NextGeneration of VLVNTs

After the measurements from ANTARES and IceCubeDeepCore in the atmospheric sector the next goal of VLVNTsis to further decrease the energy threshold below the 15GeVdomain in order to improve the sensitivity to the PMNS


Table 1 Qualitative comparison of experimentsmeasuring the atmospheric neutrino oscillation parametersThe table is divided into detectorand flux characteristics Note that the far detector of T2K is Super-Kamiokande but uses accelerator neutrinos Detector performances takenfrom [4 9 38 43 49 83 95] Expected neutrino events quoted from published results of ]

120583disappearance at analysis level (note that for

VLVNTs this number can vary significantly depending on the studied range in energy zenith angle and topology) COH refers to coherentpion production For details on the other interaction channels and energy ranges see Figure 8

Parameter VLVNT SK MINOS T2K and NOvAANTARES DeepCore

Detector (far)

Instrumentation density (mminus3) 91 times 10minus5OMs 23 times 10minus5 DOMs 02OMs 15 channelsDetection principle Cherenkov light over tens of meters Cherenkov rings Trackerscalorimeters

119864] resolution 50plusmn 22 25 at 20GeV 3 at 1 GeV 10ndash15 at 10GeV120579] resolution 3∘ at 20GeV 8∘ at 20GeV 2-3∘ mdash

Particle ID capabilities Muonno muon in interaction 119890 120583 120587 (rings) Individual particles charge

Neutrino flux

Source of neutrinos Atmosphere mix of ]119890 ]119890 ]120583 and ]

120583Accelerator ]

120583]120583modes

Baseline 10ndash12700 km 300ndash800 kmFlux determination Atm ]models self-fit +topdown ratios Nearfar detector

Energy range 10ndash100GeV Few MeVndashfew GeV Few GeVMain interaction channel DIS QE QE RES COH and DIS] events expected with osc 530 1800 2000 30 (T2K) 900 (MINOS)and without osc (per year) 660 2300 2300 120 (T2K) 1050 (MINOS)

50

45

40

35

30

25

20

15

10060 065 070 075 080 085 090 095 100

sin2(212057923)

|Δm2 32|

(10minus3

eV2)

MINOS 2012 90Super-K 2012 90ANTARES 90

ICeCube-79 2012 90ICeCube-79 2013 90 prelICeCube-86 2013 90 prel

Figure 13 90 CL contours from ANTARES [38] and IceCubersquossingle year measurements [39 40 48] compared to earlier mea-surements by MINOS [49] T2K [50] and Super-Kamiokande [51]Taken from [52]

matrix elements and determine the NMO Measuring theneutrino mass ordering is the main objective of the forth-coming ORCA (Oscillation Research with Cosmics in theAbyss) [85] and PINGU (Precision IceCubeNext-GenerationUpgrade) [86 96] detectors as part of the KM3NeT [97] andIceCube Gen2 [98] infrastructures respectively

51 Design of Future Detectors Both ORCA and PINGUwill be more densely equipped than the currently operatingdetectors and should reach several megatons in instrumentedvolume Their concepts are similar in many ways withthe most significant differences coming from the detectionmedium the proposed detector layout and the (default)optical module design

511 Hardware and Detector Geometry The PINGU opticalmodule will most likely be a simplified and modernizedversion of that of IceCube which has demonstrated itsstability and reliability over almost ten years of operationThe PINGU DOM design removes components that areno longer required such as the local coincidence logicand the multiple amplification modes while providing alarger dynamic range than the original IceCube DOM andimproved time resolution of 2 ns [86] A schematic view ofthe IceCube and PINGU (Gen2)DOMs is shown in Figure 17By maintaining the basic IceCube design the PINGU DOMminimizes risk and cost The ORCA optical module willfollow the KM3NeT design [97] with each DOM housing 31small (310158401015840) PMTs arranged in a 1710158401015840 glass sphere together withthe associated electronics as can be seen from Figure 18Thisdesign offers the possibility of creating coincidences withinthe OM to suppress the large 40K decay background as well asthe thermal noise of the PMTs The orientation of the PMTswithin the OM is also used in the reconstruction of eventsalthough not yet at its full potential A single sphere housesthree to four times the photo cathode area of an ANTARESOMwith an almost uniform angular coverage improving thecost effectiveness by a factor four Several prototypes of sucha multi-PMT OM have been successfully tested in situ [99]

The final layouts of ORCA and PINGU are still underoptimization (preliminary results tend to indicate that thebest vertical spacing between OM is around 10m for ORCAwhile similar studies in the PINGU case favor a vertical


102

101

100

Even

ts

minus10 minus05 00 05 10

cos(120579reco)

DataNeutrino simulation

Atmospheric muons (from data)Neutrinos + atmospheric muons

102

101

100

Even

ts


cos(120579reco)



102

101

100

Even

ts


cos(120579reco)



Figure 14 Zenith angle distributions of neutrino simulation and atmospheric muons derived from data for three subsequent steps in theevent selection with increasing veto cuts in IceCubersquos IC86-B analysis A comparison is also made to a 10 control sample of the data Notethat the region cos 120579

119911gt 0 is not used in the final analysis of the data Taken from [9]

spacing of about 3m close to the adopted benchmark)The current benchmark geometries used for establishingthe detector performances consist of 40 (115) strings with ahorizontal spacing ofsim20m for PINGU (ORCA)The verticalspacing is set to 6m for ORCA and 3m for PINGU While aPINGU string will hold up to 96 DOMs there are 18 DOMsin a default ORCA string The maximum number of DOMsthat a PINGU string can hold is given by themechanical con-straints of the downhole cable and the appearance of shad-owing effects while for ORCA the constraint comes from thelauncher vehicle (a large spherical frame in which the DOMsslot into dedicated cavities) used for string deployments Theseparation between the sensors of both detectors is smallerthan the absorption and scattering lengths of their respective

media making the optical properties of ice and salt water lessrelevant than for ANTARES and IceCubeDeepCore

The footprints of the ORCA and PINGU detectors areshown in Figure 19The instrumented mass of both detectorsis of order 35 to 4Mt and their effective masses reach thesame value for neutrinos of energy above 10GeV While thePINGU extension is foreseen to be embedded inside thecurrent IceCubeDeepCore detector (which will be used forbackground vetoing) the ORCA detector will be locatedaround 10 km west from the ANTARES site at a depth of2475m

512 Costs and Timescale PINGU estimates a cost of 48M$for hardware and 23M$ for logistics [100]The estimated cost


800

600

400

200

0

101 102 103

LrecoEreco (kmGeV)

Even

ts

Expectation best fitExpectation no oscData

(a)

14

12

10

08

06

04101 102 103

LrecoEreco (kmGeV)

Ratio

to n

o os

c


(b)

Figure 15 Distribution of events as a function of reconstructed 119871119864of IceCubersquos IC86-B analysis Data are compared to the best fit andexpectation with no oscillations (a) and the ratio of data and bestfit to the expectation without oscillations is also shown (b) Bandsindicate estimated systematic uncertainties From [9]

of ORCA is 40MC Funding request processes are currentlydriving the possible time line of the projects

PINGU will be built as part of the IceCube Gen2 projectFrom a technical point of view the installation of the detectorat South Pole could start by the end of 2020 [101] Basedon the experience gained with the IceCube the deploymentis expected to take only three years The first constructionphase of ORCA a demonstrator array of 6-7 strings (alreadyfunded) started in late 2014 with the deployment of themain electrooptical cable followed by the deployment of ajunction box in April 2015 The demonstrator is expected tobe deployed by the end of 2016 and will be used to carryout studies of detector-related systematic effects and eventreconstructions In an optimistic case the deployment of thefull detector case could happen by 2020 Both PINGU andORCA plan to take data during their construction phase

52 Projected Performance The determination of the NMOthe main physics goal of these projects relies on a detailedanalysis of deviations of the order of sim10 and sim30 in therates of detected atmospheric muon and electron neutrinos(see Figures 3 4 and 5) as a function of energy and arrival

zenith angle Therefore the key parameters that characterizethe potential of a detector are its effective mass the energyand zenith angle resolutions achievable and its particle(mis)identification capabilities In the following discussionthe latest preliminary studies from ORCA [85 102] andPINGU [86 91] are presented

These studies are based on full Monte Carlo simulationsadapted from IceCube and ANTARES All ORCA resultsaccount for an optical background induced by 40K decays of5ndash10 kHz per PMT and a time-correlated hit rate of 500Hzper OM (two coincident hits in different PMTs inside thesame OM) Since PINGU DOMs will follow closely thedesign used for IceCube the typical in situ behaviour of theIceCubeDeepCore DOMs with a noise rate of 650Hz isused in the simulations

The published results of ANTARES and IceCube have sofar focused on ]

120583disappearance and therefore only selected

events where a muon was observed The sensitivity to theNMO on the other hand also comes from oscillations thatinvolve ]

119890 It is therefore useful to detect all neutrino flavors

placing them in two categories depending on their topologytracks and cascades (see Section 522)

521 Reconstruction of Tracks and Cascades Track-likeevents are those where a muon is observed coming outof the interaction vertex Track-like topologies are CC ]

120583

interactions as well as the ]120591CC interactions when the

decay of the tau lepton produces a muon The cascade-liketopologies are CC ]

119890interactions CC ]

120591interactions without

a muon in the final state and NC interactions from allflavors Independent studies indicate that after accounting forreasonable detector resolution effects the cascade channelprovides more sensitivity to the effects of the NMO Notehowever that the two channels are complementary as track-like events can provide better precision in sin2120579

23 It is

consequently important to be able to distinguish the twotopologies with high efficiency and purity

The event reconstruction in PINGU is a simultaneousglobal likelihood fit of the interaction vertex position andtime the zenithal and azimuthal angles the energy of thecascade at the vertex and the length of the daughter muontrack The event hypothesis assumes that tracks and cascadesare collinear The likelihood is calculated using the time ofarrival of single photons and the expected noise in the timewindows analyzed The expectations for minimum ionizingmuon tracks and electromagnetic cascades needed for thelikelihood are stored in tables obtained from direct simula-tion of particle and photon propagation as it is already donefor IceCube [62] An event is reconstructed by comparingphoton expectation for a given event hypothesis to thephotons observed All the DOMs in PINGU as well as thosein IceCubeDeepCore are used in the reconstruction [86]

Fitting eight parameters at once while simultaneouslylooking up expectations from tables makes the reconstruc-tion CPU intensive but in return it provides robust resultsand similar resolutions for track-like and cascade-like topolo-gies While it would be possible to use the informationprovided by this reconstruction to obtain an estimate of theinelasticity of the event this has not been explored so far


IceCube 2014 [NH]MINOS watm [NH]

90 CL contours

T2K 2014 [NH]SK IV 2015 [NH]

43210

38

36

34

32

30

28

26

24

22

20

|Δm2 32|

(10minus3

eV2)

38

36

34

32

30

28

26

24

22

20

|Δm2 32|

(10minus3

eV2)

minus2ΔlnL

minus2Δ

lnL

03 04 05 06 07 0 1 2 3 4

sin2(12057923)

03 04 05

(a)

(b) (c)

06 07

sin2(12057923)

Figure 16 90 confidence contours of the latest result from IceCube (IC86-B) in the sin212057923minus Δ119898

2

32plane in comparison with the ones of

the most sensitive experiments [49 67 68] The log-likelihood profiles for individual oscillation parameters are also shown (a c) A normalmass ordering is assumed Updated from [9]

Penetrator

PMT baseHV supply

Flasher boardMain boardDelay board

Waist band

Pressure sphere

Mu-metal cageSilicone gel

PMT photocathode

Gen2 (PINGU) DOMIceCube DOM

Figure 17 Comparison between the currently operating IceCube DOM and the updated PINGUGen2 DOM

Energy and zenith angle resolutions for different interactionsare shown in Figures 20 and 21 together with those obtainedby ORCA with the methods explained hereunder

ORCA uses two distinct algorithms for tracks and cas-cades The track reconstruction is directly adapted fromthe main reconstruction of ANTARES [103] and focuses onthe muon direction using the combined information of thePMT spatial positions and the Cherenkov photon arrivaltimes The neutrino energy estimation is mainly given by thereconstructed muon track length which is complementedby the number of hits used in the track reconstructionalgorithm Muon tracks produced in neutrino interactionsat 119864] ge 15 GeV are not always fully contained which turns

the estimate into a lower limit above these energies as shownin Figure 20 The time residuals under a spherical emissionprofile (shower-like) or according to a Cherenkov cone(track-like) are used to obtain sensitivity to the inelasticity inthe track channel

The cascade reconstruction in ORCA takes advantageof the long scattering length in sea water which preservesthe structure of the Cherenkov light cone and tries toidentify the leading lepton in the cascade An example ofthe distribution of the expected number of photons as afunction of emission angle for different inelasticity intervals isshown in Figure 22 A peak is always visible at the Cherenkovangle (42∘) whose height with respect to the off-peak region


Penetrator

Top hemisphere

Pressure gauge

Nanobeacon

PMT supportstructure (top)

Cooling system (13)

Cooling system (23)

Power board(and thermal sheet)

Cooling system (33)

CLBCompass and tiltmeter

Piezosensor

PMT and base

Light collection device

Valve

Signal collection boards(top and bottom)

DOM collar and rope anchor inpoints (external to DOM)

PMT supportstructure (bottom)

Bottom hemisphere

Figure 18 An exploded view of the multi-PMT optical module of KM3NeTORCA

depends on 119910 Cascades are reconstructed in two separatesteps using maximum likelihood fits First the interactionvertex is obtained with a resolution of about 05ndash1m by analgorithm based on hit time residuals It is then followed bya fit of the direction energy and inelasticity of the event Theperformances of the cascade reconstruction are summarizedin Figures 20 and 21

In ORCA the inelasticity of about 60 of the tracks withtrue 119910 le 025 or 119910 ge 075 is reconstructed correctly theaccuracy of the inelasticity estimator of cascades is slightlyworse The inelasticity could be used for potential statisticalseparation between neutrinos and antineutrinos which canbe exploited for the mass ordering measurement [104] It canalso be tested to separate charged current interactions fromneutral current interactions While both PINGU and ORCAare studying this possibility inelasticity estimates are not yetpart of the current analyses that are discussed in the followingsections

522 Particle Identification and Background RejectionVLVNTs measuring atmospheric neutrinos should beable to identify and reject atmospheric muons the largestsource of background and differentiate between events withtrack-like and cascade-like topologies PINGU plans to tagatmospheric muons following the strategy developed inDeepCore that is using the outer detector strings to identifyparticles that enter the fiducial volume and restrictingthe analysis to starting and upgoing events (see [9] andFigure 14) The cosmic muon background is expected to beon the level of a few percent similar to DeepCore Eventreconstruction and selection in PINGU do not rely ondirect hits the single largest impact on signal efficiencyin the latest DeepCore results Signal efficiency in PINGUtherefore is expected to beminimally affected by backgroundrejection and reconstruction methods and largely definedby the number of photons observed from an interac-tion


minus100 minus50 0 50 100 150 200minus200

minus150

minus100

minus50

0

50

100

IceCubeDeepCorePINGU

Preliminary

Y(m

)

X (m)

(a)

minus100

minus50

0

50

100

KM3NeTORCA preliminary

minus100 minus50 0 50 100x (m)

y(m

)

107m

115 strings-dav = 20m

(b)

Figure 19 (a) An envisaged 40-string PINGU layout (blue strings)The black circles refer to the standard IceCube strings and the redtriangles to the DeepCore strings (b) ORCA benchmark detectorfootprint

The ORCA detector does not rely on an outer detectorto tag muons Current analyses reduce the impact of thesemuons by selecting only upgoing events and rejecting themisreconstructed ones using variables such as their recon-struction quality and the position of their reconstructedinteraction vertex The topology of neutrino interactionstrack-like or cascade-like is identified using the distributionof hit time residuals distances between reconstructed verticesat various reconstruction steps the quality of the recon-structions and topological variables among others A single

PINGU e + eORCA e + e

PINGU 120583 + 120583ORCA 120583 + 120583

E (GeV)

040

035

025

030

020

015

010

005

0005 10 15 20 25 30

Med

ian

frac

tiona

l ene

rgy

reso

lutio

n

ORCAPINGU preliminary

Figure 20 Expected median fractional energy resolution for elec-tron and muon neutrinos in PINGU (solid) and ORCA (dashed)Reproduced from [85 86]

PINGU e + eORCA eORCA e

PINGU 120583 + 120583ORCA 120583ORCA 120583

20

15

10

5

05 10 15 20 25 30

E (GeV)

Med

ian

zeni

th an

gle r

es (∘ )


Figure 21 Expected median zenith angle resolution for electronand muon neutrinos in PINGU (solid) and ORCA (dashed) ForORCA individual resolutions for neutrinos and antineutrinos areshown while a mixture of both is given for PINGU Resolutions arebetter for antineutrinos than for neutrinos due to the smaller averageinelasticity leading to a smaller intrinsic scattering angle betweenthe neutrino and the leading lepton Values taken from [85 86]

multivariate method which incorporates the parameterslisted above is applied to the data and classifies eventsas tracks showers or atmospheric muons The procedureachieves sim1 muon contamination in the final sample with-out a severe signal loss

The approach followed in PINGU to separate tracksfrom cascades also uses a multivariate method with variablesdescribing the reconstruction quality of the event under thetrack versus cascade hypothesis as well as the reconstructed


Angle with respect to electron (deg)0 20 40 60 80 100 120 140

Mea

n nu

mbe

r of p

hoto

ns p

er D

OM 1

KM3NeT preliminary

07 lt y lt 08

05 lt y lt 06

02 lt y lt 03

00 lt y lt 01

Bjorken y

e and e CC8 lt E (GeV) lt 9

40 lt d (m) lt 5010minus1

10minus2

Figure 22 Number of expected photons as a function of theemission angle between the shower direction and the directionfrom the vertex to the DOM for different intervals of interactioninelasticity 119910

10

08

06

04

02

002 4 6 8 10 12 14 16 18

E (GeV)

Frac

tion

class

ified

as tr

ack-

like


P e + eO e + eP 120583 + 120583O 120583O120583

P 120591 + 120591O 120591 + 120591P + (NC)O + (NC)

Figure 23 Fraction of events selected as tracks for differentcategories of simulated events for ORCA (dashed lines labeled asO) and PINGU (solid lines labeled as P) As expected ]

120583performs

better because of their average lower inelasticity From [88]

muon track length as input Figure 23 shows a comparison ofthe performance of these classification methods for neutrinointeractions around the energies relevant for mass orderingmeasurements for PINGU and ORCA Current methodsdiffer at low energies with PINGU showing a bias towardsclassifying low-energy tracks as cascades and ORCA exhibit-ing the opposite behavior Above 10GeV both classificationschemes result in a similar outcome The results suggest

Table 2 List of the uncertainties studied by ORCA and PINGUwhich have the largest impact on their respective NMO analyses(more systematic uncertainties have been studied see text) Sourcesof uncertainty are additional parameters in the fit Studies areperformed for a set of true oscillation parameters The best knownvalues for all other parameters are injected for creating the datatemplates PINGU uses priors to penalize deviations while fittingthese parameters ORCA does not use priors and instead reports thestandard deviation of the fit results

Uncertainties ORCA PINGU120590 (fit yield) 120590(prior)

12057923 Δ119898231

Unconstrained12057913

Integrated plusmn1∘ 02∘

12057912 Δ119898221

Fixed120575CP Fixed at zeroa

Overall rate factor 20 Unconstrained119864minus120574 (slope spectral index) 05 plusmn005

Energy scale Not used plusmn10]] ratio 40 plusmn10120583119890 flavor ratio 12 plusmn3NC cross section scaling 110 GENIE modelaBoth projects have studied how 120575CP impacts their sensitivity but the resultsare not yet reflected in the projections given in this review

that the behavior of the particle identification algorithms atlow energy can be tuned for optimizing sensitivity to theNMOmeasurement In both cases the final performances aresubject to further optimization

53 Physics Potential and Systematics The preliminary per-formances described above are used by the PINGU andORCA collaborations as inputs to estimate the confidencelevel with which the projected experiments will be ableto reject a given NMO This is done by drawing severalthousands of pseudoexperiments generated under each massordering hypothesis as outlined in [105] The analysis isconducted by comparing the two-dimensional histograms ofpseudodata and simulation as a function of the reconstructedenergy and zenith The pseudo-data sets are generated usingdifferent input parameters such as the values of the mixingangles in order to study the impact of degeneracies in themeasurement

A full log-likelihood ratio (LLR) method is used by bothcollaborations to report their expected sensitivity In thismethod each pseudoexperiment is analyzed by performinga log-likelihood fit with the oscillation parameters as freeparameters (mostly 120579

23 Δ119898232 and 120579

13) and assuming both

hierarchies in turn Sources of systematic uncertainty areincorporated as additional parameters in the fit (see Table 2)

As such methods can be quite CPU expensive in par-ticular when studying various sources of systematics thePINGU collaboration also implemented a simplified Δ120594

2-based approach This method is a parametric analysis basedon the Fisher information matrix which relies on the partialderivatives of the event counts in each bin with respectto all parameters under study Inverting the Fisher matrixyields the full covariancematrix between the parametersThe


covariance matrix of the mixing angle 12057923

is calculated atseveral values to overcome the limitations of themethodTheresults obtained with the Fisher matrix are in agreement withthe LLR method and are also used to report the projectedsensitivity of PINGU

The parameters of the fits performed by ORCA andPINGU presented in Table 2 are the oscillation parametersof interest plus a set of parameters related to uncertainties onthe detection process neutrino fluxes cross sections and theremaining oscillation parametersThe oscillation parametersin particular 120579

23 have the largest impact on the achievable

precision The overall normalization has the second largestimpact on the precision This absorbs uncertainties on theefficiency of the detector the absolute atmospheric neutrinoflux and interaction cross sections PINGU has recentlystudied uncertainties on the neutrino flux by using a morerefined description which involves a set of 18 parameters[22] The impact found was a reduction of the three-yearsensitivity by 02120590 [106] (not yet included in Figure 24) Crosssections have been also studied in more detail by modifyingthe six most relevant parameters of the model implementedin GENIE The reduction in sensitivity was found to benegligible Studies within ORCA and PINGU have tested theimpact of 120575CP and found an additional reduction of up to 05120590at the three-year benchmark [85 88] Note that all figures inthis review do not include this effect

The LLR (and Δ1205942 for PINGU) resulting from fits to

the pseudoexperiments are used to calculate the separabilityof the two possible mass orderings The median (ie with50 statistical power) sensitivities to the NMO are shownin Figure 24(a) after 3 years of data taking The results areobtained by fixing 120575CP to zero and are shown as a functionof 12057923 Both collaborations observe that constraining 120579

23to

either octant while doing a fit artificially increases the sensi-tivity to the NMO thus the parameter is left unconstrainedin these studies

Though ORCA and PINGU sensitivities should be com-pared with caution as the various inputs are slightly differentboth studies find a better sensitivity to the NMO for a truevalue of 120579

23in the second octant in the case of normal mass

ordering For the case of inverted ordering the sensitivityhas a much weaker dependence on the value of 120579

23 The

consistency of the two results is encouraging as they havebeen obtained with completely independent analysis chains

The expected improvement in sensitivities with runningtime which does not yet include the effects of 120575CP nor thereconstructed inelasticity is shown in Figure 24(b) Oncemore the discrimination power of both detectors is compa-rable

The identification of the mass ordering devised by bothcollaborations also produces a measurement of 120579

23and the

absolute value of the atmospheric mass splitting Projectionsof the sensitivity to sin2120579

23have a strong dependence on the

assumed true values For sin212057923

= 045 both PINGU andORCA expect to achieve errors of the order of 005 afterthree years of operation The precision achievable on theabsolute value of the mass splitting is roughly independentof the true value and the expected error on the measurementfor both projects is about 005 times 10

minus3 Both experiments are

7

6

5

4

3

2

1

0040 045 050 055 060

sin212057923

120590(3

year

s)


PINGU NOORCA NO

PINGU IOORCA IO

(a)

45

40

35

30

25

20

15

100 1 2 3 4 5

Operation time (3 yrs)


PINGU NOORCA NO

PINGU IOORCA IO

NO 12057923 = 42∘

IO 12057923 = 49∘

Expe

cted

sens

itivi

ty (120590

)

(b)

Figure 24 (a) Significance of ORCA and PINGU for rejectinga given hypothesis for the neutrino mass ordering plotted as afunction of 120579

23 after 3 years of data taking (b) Median significance

as a function of time for the benchmark detectors described in thetext The oscillation parameters injected are close to those found in[3] (120579

23= 42∘ for a NMO 120579

23= 49∘ for an IMO) From [85 91]

expected to produce measurements with better precision tothose projected for NOvA and T2K by the year 2020

The results shown in the present paper are a compilationof the most recent publicly shown projections of bothcollaborations and include most leading systematics effects[85 88 91 107] Recently a thorough study of the interplaybetween the oscillations parameters has been reported in[108] consistent with the recent results from ORCA andPINGU The authors also introduced uncertainties in theestimated energy and zenith resolutions as well as additional(conservative) uncorrelated uncertainties Their results showthat after 5 years of data taking the loss in sensitivity ranges


from 24 to 40 under pessimistic assumptions (such asfully uncorrelated errors in each analysis bin) thus leavingroom for a measurement of the NMO by ORCA and PINGUon a reasonable time scale

6 Summary

Atmospheric neutrinos are a versatile tool to study neutrinooscillations This naturally occurring beam covers baselinesas large as Earthrsquos diameter and has an energy range whichspans over the regimes of oscillations in vacuum and withresonant and saturated matter effects Current VLVNTsANTARES and IceCube can detect neutrinos in the latterregime and have already produced measurements of theatmospheric oscillation parameters 120579

23and |Δ1198982

32| Constant

improvements in the understanding and modeling of thedetector and media as well as more sophisticated dataanalysis techniques have led to promising results whichhave started to become comparable with those of other moremature experimental set-ups

Proposed VLVNTs ORCA and PINGU aim to lowerthe energy threshold and access the resonant regime withthe goal of measuring the sign of Δ119898

2

31and completely

determining the neutrinomass orderingWhile both projectsare on the way of optimizing their detector geometriesandor analysis techniques current studies are neverthelessmature and indicate that they could provide a significantmeasurement (ge3120590 depending on the true value of 120579

23) of

the neutrino mass ordering after 3-4 years of operation

Conflict of Interests

The authors declare that there is no conflict of interestsregarding the publication of this paper

Acknowledgments

Theauthors are grateful to J BrunnerM Jongen J HofestadtW Winter D Cowen S Boser and T DeYoung for usefuldiscussions and clarifications on both the theoretical andexperimental aspects covered in this paper

References

[1] K Olive ldquoParticle Data Grouprdquo Chin Phys C vol 38 noParticle Article ID 090001 2014

[2] D V Forero M Tortola and J W F Valle ldquoNeutrino oscil-lations refittedrdquo Physical Review D vol 90 no 9 Article ID093006 2014

[3] M Gonzalez-Garcia M Maltoni and T Schwetz ldquoUpdatedfit to three neutrino mixing status of leptonic CP violationrdquoJournal of High Energy Physics vol 2014 no 11 article 052 2014

[4] K Abe J Adam H Aihara et al ldquoMeasurements of neutrinooscillation in appearance and disappearance channels by theT2K experiment with 66 times 10

20 protons on targetrdquo PhysicalReview D vol 91 no 7 Article ID 072010 2015

[5] WWinter ldquoNeutrinomass hierarchy theory and phenomenol-ogyrdquo in Proceedings of the 26th International Conference onNeutrino Physics and Astrophysics (Neutrino rsquo14) vol 1666Boston Mass USA June 2014

[6] C H Albright and M-C Chen ldquoModel predictions for neu-trino oscillation parametersrdquo Physical Review D vol 74 no 11Article ID 113006 2006

[7] M Lindner A Merle and W Rodejohann ldquoImproved limit on12057913and implications for neutrinomasses in neutrinoless double

beta decay and cosmologyrdquo Physical Review D vol 73 no 5Article ID 053005 2006

[8] A Garfagnini ldquoNeutrinoless double beta decay experimentsrdquoInternational Journal of Modern Physics Conference Series vol31 Article ID 1460286 2014 (In 12th Conference on FlavorPhysics and CP Violation (FPCP rsquo14) Marseille France May2014)

[9] M G Aartsen M Ackermann J Adams et al ldquoDetermin-ing neutrino oscillation parameters from atmospheric muonneutrino disappearance with three years of IceCube DeepCoredatardquo Physical Review D vol 91 no 7 Article ID 072004 2015

[10] M Aglietta G Battistoni E Bellotti et al ldquoExperimental studyof atmospheric neutrino flux in the NUSEX experimentrdquo Euro-physics Letters vol 8 no 7 pp 611ndash614 1989

[11] K Daum W Rhode P Bareyre et al ldquoDetermination ofthe atmospheric neutrino spectra with the Frejus detectorrdquoZeitschrift fur Physik C Particles and Fields vol 66 no 3 pp417ndash428 1995

[12] W W M Allison G J Alner D S Ayres et al ldquoMeasurementof the atmospheric neutrino flavour composition in Soudan 2rdquoPhysics Letters B vol 391 no 3-4 pp 491ndash500 1997

[13] R Clark R Becker-Szendy C B Bratton et al ldquoAtmosphericmuon neutrino fraction above 1 GeVrdquo Physical Review Lettersvol 79 no 3 pp 345ndash348 1997

[14] S Hatakeyama T Hara Y Fukuda et al ldquoMeasurement ofthe flux and zenith-angle distribution of upward through-goingmuons in Kamiokande 119868119868 + 119868119868119868rdquo Physical Review Letters vol 81no 10 pp 2016ndash2019 1998

[15] Y Fukuda T Hayakawa E Ichihara et al ldquoStudy of the atmos-pheric neutrino flux in the multi-GeV energy rangerdquo PhysicsLetters B vol 436 no 1-2 pp 33ndash41 1998

[16] R Abbasi Y Abdou M Ackermann et al ldquoDetermination ofthe atmospheric neutrino flux and searches for newphysicswithAMANDA-IIrdquo Physical Review D vol 79 no 10 Article ID102005 15 pages 2009

[17] S Adrian-Martinez A Albert I Al Samarai et al ldquoMeasure-ment of the atmospheric ]

120583energy spectrum from 100GeV to

200 TeV with the ANTARES telescoperdquo The European PhysicalJournal C vol 73 article 2606 2013

[18] M G Aartsen M Ackermann J Adams et al ldquoDevelopmentof a general analysis and unfolding scheme and its applicationto measure the energy spectrum of atmospheric neutrinos withIceCuberdquo The European Physical Journal C vol 75 article 1162015

[19] MHonda TKajita KKasahara and SMidorikawa ldquoImprove-ment of low energy atmospheric neutrino flux calculation usingthe JAM nuclear interaction modelrdquo Physical Review D vol 83no 12 Article ID 123001 34 pages 2011

[20] G Barr T Gaisser P Lipari S Robbins and T Stanev ldquoThree-dimensional calculation of atmospheric neutrinosrdquo PhysicalReview D vol 70 Article ID 023006 2004

[21] G Battistoni A Ferrari T Montaruli and P R Sala ldquoTheFLUKA atmospheric neutrino flux calculationrdquo AstroparticlePhysics vol 19 no 2 pp 269ndash290 2003

[22] G D Barr S Robbins T K Gaisser and T Stanev ldquoUncertain-ties in atmospheric neutrino fluxesrdquo Physical Review D vol 74no 9 Article ID 094009 2006


[23] M Honda M S Athar T Kajita K Kasahara and SMidorikawa ldquoAtmospheric neutrino flux calculation using theNRLMSISE-00 atmospheric modelrdquo Physical Review D vol 92Article ID 023004 2015

[24] L Wolfenstein ldquoNeutrino oscillations in matterrdquo PhysicalReview D vol 17 no 9 pp 2369ndash2374 1978

[25] S Choubey and P Roy ldquoProbing the deviation from maximalmixing of atmospheric neutrinosrdquo Physical Review D vol 73no 1 Article ID 013006 2006

[26] F P An J Z Bai A B Balantekin et al ldquoObservation of elec-tron-antineutrino disappearance at daya bayrdquo Physical ReviewLetters vol 108 no 17 Article ID 171803 7 pages 2012

[27] J K Ahn S Chebotaryov J H Choi et al ldquoObservation of reac-tor electron antineutrinos disappearance in the RENO experi-mentrdquo Physical Review Letters vol 108 no 19 Article ID 1918022012

[28] Y Abe J C dos Anjos J C Barriere et al ldquoImproved measure-ments of the neutrino mixing angle 120579

13with the Double Chooz

detectorrdquo Journal of High Energy Physics vol 2014 no 10 article086 2014 Erratum in Journal of High Energy Physics vol 2015no 2 article 074 2015

[29] S P Mikheev and A Y Smirnov ldquoResonance amplificationof oscillations in matter and spectroscopy of solar neutrinosrdquoSoviet Journal of Nuclear Physics vol 42 pp 913ndash917 1985Yadernaya Fizika vol 42 p 1441 1985

[30] M Freund ldquoAnalytic approximations for three neutrino oscil-lation parameters and probabilities in matterrdquo Physical ReviewD vol 64 no 5 Article ID 053003 12 pages 2001

[31] A M Dziewonski and D L Anderson ldquoPreliminary referenceEarth modelrdquo Physics of the Earth and Planetary Interiors vol25 no 4 pp 297ndash356 1981

[32] V A T V K Ermilova F V A Chechin and K Soob ldquoPara-metric enhancement of neutrino oscillations in matterrdquo ShortNotices of the Lebedev Institute vol 5 p 26 1986

[33] E K Akhmedov ldquoOn neutrino oscillations in a nonhomoge-neous mediumrdquo Soviet Journal of Nuclear Physics vol 47 no 2pp 301ndash302 1988

[34] P I Krastev and A Y Smirnov ldquoParametric effects in neutrinooscillationsrdquo Physics Letters B vol 226 no 3-4 pp 341ndash3461989

[35] S T Petcov ldquoDiffractive-like (or parametric-resonance-like)enhancement of the Earth (day-night) effect for solar neutrinoscrossing the Earth corerdquo Physics Letters B vol 434 no 3-4 pp321ndash332 1998

[36] J A Formaggio and G P Zeller ldquoFrom eV to EeV neutrinocross sections across energy scalesrdquo Reviews of Modern Physicsvol 84 no 3 pp 1307ndash1341 2012

[37] D Casper ldquoThe nuance neutrino physics simulation and thefuturerdquo Nuclear Physics BmdashProceedings Supplements vol 112no 1ndash3 pp 161ndash170 2002

[38] S Adrian-Martinez I Al Samarai A Albert et al ldquoMeasure-ment of atmospheric neutrino oscillations with the ANTARESneutrino telescoperdquo Physics Letters B vol 714 no 2ndash5 pp 224ndash230 2012

[39] M G Aartsen R Abbasi Y Abdou et al ldquoMeasurementof atmospheric neutrino oscillations with IceCuberdquo PhysicalReview Letters vol 111 no 8 Article ID 081801 2013

[40] M G Aartsen R Abbasi Y Abdou et al ldquoThe IceCube neu-trino observatory part V neutrino oscillations and super-nova searchesrdquo in Proceedings of the 33nd International Cos-mic Ray Conference Rio de Janeiro Brazil July 2013 httparxivorgabs13097008

[41] J P Yanez Proceedings 26th International Conference on Neu-trino Physics and Astrophysics (Neutrino 2014) Boston Mas-sachusetts United States June 2ndash7 2014 vol 1666 of AIPConference Proceedings 2015

[42] A Achterberg M Ackermann J Adams et al ldquoFirst yearperformance of the IceCube neutrino telescoperdquo AstroparticlePhysics vol 26 no 3 pp 155ndash173 2006

[43] MAgeron J AAguilar I Al Samarai et al ldquoANTARES the firstundersea neutrino telescoperdquoNuclear Instruments andMethodsin Physics Research A vol 656 no 1 pp 11ndash38 2011

[44] A D Avrorin A V Avrorin V M Aynutdinov et al ldquoTheprototypingearly construction phase of the BAIKAL-GVDprojectrdquo Nuclear Instruments and Methods in Physics ResearchSection A Accelerators Spectrometers Detectors and AssociatedEquipment vol 742 pp 82ndash88 2014 Proceedings of the4th Roma International Conference on Astroparticle Physics(RICAP rsquo13)

[45] P Amram M Anghinolfi S Anvar et al ldquoThe ANTARESoptical modulerdquo Nuclear Instruments and Methods in PhysicsResearch Section A Accelerators Spectrometers Detectors andAssociated Equipment vol 484 no 1ndash3 pp 369ndash383 2002

[46] R Abbasi M Ackermann J Adams et al ldquoThe IceCube dataacquisition system signal capture digitization and timestamp-ingrdquo Nuclear Instruments and Methods in Physics ResearchSection A Accelerators Spectrometers Detectors and AssociatedEquipment vol 601 no 3 pp 294ndash316 2009

[47] R Abbasi Y Abdou T Abu-Zayyad et al ldquoThe design andperformance of IceCube DeepCorerdquo Astroparticle Physics vol35 no 10 pp 615ndash624 2012

[48] J P Yanez G Yodh S Yoshida et al ldquoThe IceCube neu-trino observatory part V neutrino oscillations and supernovasearchesrdquo in Proceedings of the International Cosmic Ray Con-ference Rio de Janeiro Brazil 2013

[49] P Adamson I Anghel C Backhouse et al ldquoMeasurementof neutrino and antineutrino oscillations using beam andatmospheric data in MINOSrdquo Physical Review Letters vol 110no 25 Article ID 251801 2013

[50] K Abe N Abgrall Y Ajima et al ldquoFirst muon-neutrino dis-appearance studywith an off-axis beamrdquo Physical ReviewD vol85 no 3 Article ID 031103 8 pages 2012

[51] Y Itow ldquoRecent results in atmospheric neutrino oscillations inthe light of large 120579

13rdquo Nuclear Physics BmdashProceedings Supple-

ments vol 235-236 pp 79ndash86 2013 the XXV InternationalConference on Neutrino Physics and Astrophysics (Neutrino2012)

[52] J Brunner ldquoMeasurement of neutrino oscillations with neu-trino telescopesrdquo Advances in High Energy Physics vol 2013Article ID 782538 16 pages 2013

[53] J A Aguilar I Al Samarai A Albert et al ldquoPerformance ofthe front-end electronics of the ANTARES neutrino telescoperdquoNuclear Instruments and Methods in Physics Research Section Avol 622 no 1 pp 59ndash73 2010

[54] C Tamburini S Martini B Al Ali et al ldquoEffects of hydro-static pressure on growth and luminescence of a moderately-piezophilic luminous bacteria Photobacterium phosphoreumANT-2200rdquo PLoS ONE vol 8 no 6 Article ID e66580 2013

[55] R Abbasi Y Abdou T Abu-Zayyad et al ldquoCalibration andcharacterization of the IceCube photomultiplier tuberdquo NuclearInstruments and Methods in Physics Research Section A Accel-erators Spectrometers Detectors and Associated Equipment vol618 no 1ndash3 pp 139ndash152 2010


[56] J A Aguilar A Albert P Amram et al ldquoTransmission of lightin deep sea water at the site of the Antares neutrino telescoperdquoAstroparticle Physics vol 23 no 1 pp 131ndash155 2005

[57] M G Aartsen R Abbasi Y Abdou et al ldquoMeasurement ofSouth Pole ice transparency with the IceCube LED calibrationsystemrdquo Nuclear Instruments and Methods in Physics ResearchSection A Accelerators Spectrometers Detectors and AssociatedEquipment vol 711 pp 73ndash89 2013

[58] D Chirkin R Abbasi Y Abdou et al ldquoThe IceCube neutrinoobservatory part VI ice properties reconstruction and futuredevelopmentsrdquo in Proceedings of the the 33nd InternationalCosmic Ray Conference Rio de Janeiro Brazil 2013

[59] J A Aguilar I Al Samarai A Albert et al ldquoAMADEUSmdashtheacoustic neutrino detection test system of the ANTARES deep-sea neutrino telescoperdquo Nuclear Instruments and Methods inPhysics Research Section A vol 626-627 pp 128ndash143 2011

[60] J A Aguilar I Al Samarai A Albert et al ldquoTime calibrationof the ANTARES neutrino telescoperdquo Astroparticle Physics vol34 no 7 pp 539ndash549 2011

[61] S Adrian-Martınez A Albert M Andre et al ldquoTime cali-bration with atmospheric muon tracks in the ANTARES neu-trinotelescoperdquo httparxivorgabs150704182

[62] M G Aartsen R Abbasi M Ackermann et al ldquoEnergy recon-struction methods in the IceCube neutrino telescoperdquo Journalof Instrumentation vol 9 Article ID P03009 2014

[63] T Kajita Ed Proceedings of the International Workshop on Sub-Dominant Oscillation Effects in Atmospheric Neutrino Experi-ments held on December 9ndash11 2004 in Kashiwa Japan 2005

[64] A Bodek andU K Yang ldquoHigher twist 120585119908scaling and effective

LO PDFs for lepton scattering in the few GeV regionrdquo Journalof Physics G Nuclear and Particle Physics vol 29 no 8 p1899 2003 Neutrino factories Proceedings 4th InternationalWorkshop NuFactrsquo02 London UK July 1ndash6 2002

[65] A Cooper-Sarkar P Mertsch and S Sarkar ldquoThe high energyneutrino cross-section in the Standard Model and its uncer-taintyrdquo Journal of High Energy Physics vol 2011 no 8 article42 2011

[66] K Kodama N Ushida C Andreopoulos et al ldquoFinal tau-neutrino results from the DONuT experimentrdquo Physical ReviewD vol 78 no 5 Article ID 052002 20 pages 2008

[67] K Abe J Adam H Aihara et al ldquoPrecise measurement ofthe neutrino mixing parameter 120579

23from muon neutrino dis-

appearance in an off-axis beamrdquoPhysical ReviewLetters vol 112no 18 Article ID 181801 8 pages 2014

[68] M Nakahata ldquoRecent results from super-kamiokanderdquo in Pre-sented at 16th International Workshop on Neutrino TelescopesVenice Italy 2015

[69] D Heck J Knapp J N Capdevielle G Schatz and T ThouwCORSIKA a Monte Carlo Code to Simulate Extensive AirShowers Forschungszentrum Karlsruhe GmbH 1998 httpinspirehepnetrecord469835filesFZKA6019pdf

[70] G Carminati M Bazzotti S Biagi et al ldquoMUPAGE a fastatmospheric MUon generator for neutrino telescopes based onparametric formulasrdquo in Proceedings of the International CosmicRay Conference Lodz Poland July 2009

[71] C Andreopoulos A Bell D Bhattacharya et al ldquoThe GENIEneutrino Monte Carlo generatorrdquo Nuclear Instruments andMethods in Physics Research Section A vol 614 no 1 pp 87ndash1042010

[72] A Gazizov and M P Kowalski ldquoANIS high energy neutrinogenerator for neutrino telescopesrdquo Computer Physics Commu-nications vol 172 no 3 pp 203ndash213 2005

[73] G Ingelman A Edin and J Rathsman ldquoLEPTO 65mdasha MonteCarlo generator for deep inelastic lepton-nucleon scatteringrdquoComputer Physics Communications vol 101 no 1-2 pp 108ndash1341997

[74] T Sjostrand P Eden C Friberg et al ldquoHigh-energy-physicsevent generation with PYTHIA61rdquo Computer Physics Communi-cations vol 135 no 2 pp 238ndash259 2001

[75] M Sajjad Athar M Honda T Kajita K Kasahara and SMidorikawa ldquoAtmospheric neutrino flux at INO South Poleand Pyhasalmirdquo Physics Letters B vol 718 no 4-5 pp 1375ndash1380 2013

[76] S Agostinelli J Allison K Amako et al ldquoGeant4mdasha simulationtoolkitrdquo Nuclear Instruments and Methods in Physics ResearchSection A Accelerators Spectrometers Detectors and AssociatedEquipment vol 506 no 3 pp 250ndash303 2003

[77] J Brunner ldquoAntares simulation toolsrdquo in Proceedings of the 1stVLVnTWorkshop AmsterdamTheNetherlands October 2003

[78] P Antonioli C Ghetti E V Korolkova V A Kudryavtsev andG Sartorelli ldquoA three-dimensional code for muon propagationthrough the rockMUSICrdquoAstroparticle Physics vol 7 no 4 pp357ndash368 1997

[79] I A Sokalski E V Bugaev and S I Klimushin ldquoMUM flexibleprecise Monte Carlo algorithm for muon propagation throughthick layers of matterrdquo Physical Review D vol 64 no 7 ArticleID 074015 2001

[80] D Chirkin and W Rhode ldquoPropagating leptons throughmatter with Muon MonteCarlo (MMC)rdquo httparxivorgabshep-ph0407075

[81] S Fukuda Y Fukuda T Hayakawa et al ldquoThe Super-Kamiokande detectorrdquo Nuclear Instruments and Methods inPhysics Research Section A Accelerators Spectrometers Detec-tors and Associated Equipment vol 501 no 2-3 pp 418ndash4622003

[82] K Abe N Abgrall H Aihara et al ldquoThe T2K experimentrdquoNuclear Instruments and Methods in Physics Research SectionA Accelerators Spectrometers Detectors and Associated Equip-ment vol 659 no 1 pp 106ndash135 2011

[83] D G Michael P Adamson T Alexopoulos et al ldquoThe mag-netized steel and scintillator calorimeters of the MINOS exper-imentrdquo Nuclear Instruments and Methods in Physics ResearchSection A Accelerators Spectrometers Detectors and AssociatedEquipment vol 596 no 2 pp 190ndash228 2008

[84] ldquoThe NOvA technical design reportrdquo Tech RepFERMILAB-DESIGN-2007-01 2007 httplssfnalgovarchivedesignfermilab-design-2007-01pdf

[85] J Brunner ldquoMeasuring neutrino oscillations and the neutrinomass hierarchy in the Mediterranean seardquo in Proceedings ofthe 34th International Cosmic Ray Conference (ICRC rsquo15) TheHague The Netherlands July-August 2015

[86] M Aartsen K AbrahamM Ackermann et al ldquoLetter of intenttheprecision IceCube next generation upgrade (PINGU)rdquohttparxivorgabs14012046

[87] P Adamson C Andreopoulos K E Arms et al ldquoMeasurementof neutrino oscillations with theMINOS detectors in the NuMIbeamrdquo Physical Review Letters vol 101 Article ID 131802 2008

[88] J P Yanez ldquoFromDeepCore to PINGUmeasuring atmosphericneutrino oscillations at the South Polerdquo in Proceedings of theVery Large Volume Neutrino Telescope Workshop (VLVnT rsquo15)Rome Italy September 2015

[89] J A Aguilar I Al Samarai A Albert et al ldquoA fast algorithm formuon track reconstruction and its application to the ANTARES


neutrino telescoperdquoAstroparticle Physics vol 34 no 9 pp 652ndash662 2011

[90] G L Fogli E Lisi A Marrone D Montanino and A PalazzoldquoGetting the most from the statistical analysis of solar neutrinooscillationsrdquo Physical ReviewD vol 66 no 5 Article ID 05301022 pages 2002

[91] K Clark ldquoStatus of the PINGU detectorrdquo in Proceedings ofthe International Cosmic Ray Conference The Hague TheNetherlands July 2015

[92] J Ahrens X Bai R Bay et al ldquoMuon track reconstruction anddata selection techniques in AMANDArdquo Nuclear Instrumentsand Methods in Physics Research Section A vol 524 no 1ndash3 pp169ndash194 2004

[93] M Gonzalez-Garcia M Maltoni J Salvado and T SchwetzldquoGlobal fit to three neutrino mixing critical look at presentprecisionrdquo Journal of High Energy Physics vol 2012 no 12article 123 2012

[94] S Euler ldquoAtmospheric neutrino oscillations with DeepCorerdquo inProceedings of the International Cosmic Ray Conference vol 4p 67 2011

[95] R Wendell C Ishihara K Abe et al ldquoAtmospheric neu-trino oscillation analysis with subleading effects in Super-Kamiokande I II and IIIrdquo Physical Review D vol 81 no 9Article ID 092004 16 pages 2010

[96] D J Koskinen ldquoIcecube-DeepCore-PINGU fundamental neu-trino and darkmatter physics at the South PolerdquoModern PhysicsLetters A vol 26 no 39 p 2899 2011

[97] P Bagley J Craig A Holford et al ldquoTechnical Design ReportrdquoTech Rep 2010

[98] M G Aartsen M Ackermann J Adams et al ldquoIceCube-Gen2a vision for thefuture of neutrino astronomy in Antarcticardquohttparxivorgabs14125106

[99] S Adrian-Martinez M Ageron F Aharonian et al ldquoDeep seatests of a prototype of the KM3NeT digital optical modulerdquoTheEuropean Physical Journal C vol 74 article 3056 2014

[100] T DeYoung ldquoNeutrino physics prospects with PINGUrdquo inPresented at the Meeting of the APS Division of Particles andFields (DPF rsquo15) Ann Arbor Mich USA August 2015

[101] K Hanson and IceCube-Gen2 Collaboration ldquoIceCube-Gen2the science the detector drilling and logisticsrdquo in Proceedingsof theVery LargeVolumeNeutrinoTelescopes (VLVnT rsquo15) RomeItaly September 2015

[102] M Jongen ldquoSensitivity to the neutrino mass hierarchy ofKM3NeTORCArdquo in Proceedings of the 34th InternationalCosmic RayConference (ICRC rsquo15)TheHagueTheNetherlandsJuly-August 2015

[103] S Adrian-Martinez I Al Samarai A Albert et al ldquoSearch forcosmic neutrino point sources with four years of data fromthe antares telescoperdquo The Astrophysical Journal vol 760 no1 article 53 2012

[104] M Ribordy and A Y Smirnov ldquoImproving the neutrinomass hierarchy identification with inelasticity measurement inPINGU and ORCArdquo Physical Review D vol 87 no 11 ArticleID 113007 20 pages 2013

[105] D Franco C Jollet A Kouchner et al ldquoMass hierarchy dis-crimination with atmospheric neutrinos in large volume icewater Cherenkov detectorsrdquo Journal of High Energy Physics vol2013 no 4 article 008 2013

[106] J Sandroos ldquoAtmospheric flux uncertainties and the neutrinomass hierarchyrdquo in Proceedings of the VLVnT Workshop RomeItaly September 2015

[107] J P A M de Andre J Pedro and IceCube-PINGU Collabora-tion ldquoAtmospheric neutrino status and prospectsrdquo in Proceed-ings of the 17th International Workshop on Neutrino Factoriesand Future Neutrino Facilities (NuFact rsquo15) Rio de JaneiroBrazil August 2015

[108] F Capozzi E Lisi and A Marrone ldquoPINGU and the neutrinomass hierarchy statistical and systematic aspectsrdquo PhysicalReview D vol 91 no 7 Article ID 073011 18 pages 2015

Submit your manuscripts athttpwwwhindawicom

Hindawi Publishing Corporationhttpwwwhindawicom Volume 2014

High Energy PhysicsAdvances in

The Scientific World JournalHindawi Publishing Corporation httpwwwhindawicom Volume 2014


FluidsJournal of

Atomic and Molecular Physics

Journal of



Advances in Condensed Matter Physics

OpticsInternational Journal of



AstronomyAdvances in

International Journal of


Superconductivity


Statistical MechanicsInternational Journal of


GravityJournal of


AstrophysicsJournal of


Physics Research International


Solid State PhysicsJournal of

Computational Methods in Physics

Journal of



Soft MatterJournal of

Hindawi Publishing Corporationhttpwwwhindawicom

AerodynamicsJournal of

Volume 2014


PhotonicsJournal of


Journal of

Biophysics


ThermodynamicsJournal of


Δ1198982

119894119895= 1198982

119894minus 1198982

119895with 119894 119895 = 1 2 3) which play a role in

oscillations are known to a precision better than 5 Whilethe sign of themass splitting between the states 1-2 (119898

2gt 1198981)

is known from matter effects in solar neutrino oscillationsthe relative difference between119898

3and119898

1remains unknown

The relative values of the neutrino masses are commonlyreferred to as the neutrino mass ordering (NMO) (thedetermination of the mass ordering is sometimes confusedwith the determination of the neutrino ldquomass hierarchyrdquowhich requires additional information on the absolute scaleof the neutrino masses [5]) which has two possible optionsthe normal ordering (NO) with 119898

1lt 1198982

lt 1198983 and

the inverted ordering (IO) with 1198983

lt 1198981

lt 1198982 The

determination of the NMO is important as the parametercan discriminate between flavor symmetry models [6] Alsothe sensitivity of experiments attempting to determine theneutrino nature depends on theNMO [7 8] Finally knowingthe NMO would help to measure the value of the 120575 phasewhich in turn would be an important step forward towardssolving the fundamental question of the prevalence of matterover antimatter in the Universe Better measurements of allthe parameters involved in neutrino oscillations are thereforenecessary to understand if the current model is correct andhow to incorporate it to the Standard Model

In this view atmospheric neutrinos remain a promisingtool for studying oscillations they cover a wide energy rangefrom MeV to TeV and can reach a detector after travelingdistances from a few to about 12700 km when they cross theEarth No man-made beam covers a similar parameter spaceHowever the flux strongly decreases with energy Detectingit implies building large detectors such as very large volumeneutrino telescopes (VLVNTs) to study atmospheric neutrinooscillations

In the recent years first ANTARES and then Ice-CubeDeepCore have proven that these studies are feasibleby analyzing interactions of neutrinos with energy as low as15GeVThe current result from IceCube on sin2120579

23and Δ1198982

32

reaches a precisionwhich is only a factor of three to four timesless stringent than global fits which combine all available data[2 3 9] Building upon the success of these studies proposalsof new more densely instrumented telescopes as extensionsor part of new projects have appeared PINGU and ORCAaim to improve the precision of these measurements andreduce the energy threshold to a fewGeVwherematter effectsare strong and use these effects to measure the NMO

This review begins by covering in Section 2 the currentknowledge on atmospheric neutrinos and how oscillationsaffect their flux Section 3 describes the design and operationof VLVNTs Special attention is paid to relevant sources ofuncertainty The neutrino oscillation results produced bythese experiments until this date are covered in Section 4Section 5 discusses the possible studies with future detectorsand a short summary is given in Section 6

2 Atmospheric Neutrino Oscillations

The flux of atmospheric neutrinos in the energies relevant fora VLVNT together with how the flux is modified by neutrino

oscillations for those neutrinos that cross the Earth is thetopics covered in this section

21 A Neutrino Beam from Cosmic Rays Cosmic rays (CR)continuously arrive at the Earth from all directions andinteract with nuclei in the atmosphere at altitudes of about25 km above sea level and initiate showers of particles Duringthe shower development charged mesons are produced thateventually decay in comparable numbers of muons andneutrinos

CR + 119873 997888rarr 119883 + 120587∓

119870∓

120587minus

119870minus


+ ]120583

120587+

119870+

997888rarr 120583+

+ ]120583

120583minus


+ ]119890+ ]120583

120583+

997888rarr 119890+

+ ]119890+ ]120583

(2)

The atmospheric muons produced in air showers cantravel long distances before they decay They are able topenetrate deep into the Earth depending on their energyand the material that they are crossing [1] and constitute thedominant background in the measurement of atmosphericneutrinos

Atmospheric neutrinos have been measured over a wideenergy range [10ndash18] and multiple models predict their flux[19ndash21] (see Figure 1)Themost noticeable difference betweenthe models is the absolute flux which changes by up to 20both for electron and for muon (anti)neutrinos Apart fromthat the models agree that atmospheric neutrinos follow apower-law energy spectrum with a spectral index close to 3in the energy range 119864] = [3ndash100]GeV Measurements from[11] estimate an uncertainty of plusmn004 on the spectral index ofatmospheric neutrinos A similar uncertainty has been alsoderived from varying the underlying cosmic ray model inneutrino flux calculations [22]

Muon neutrinos dominate the flux and also havethe hardest spectral index (see Figure 1) Since electron(anti)neutrinos mainly come from muons that lose energybefore decaying (see (2)) their spectral index is softer andtheir relative contribution to the total neutrino flux dependson energy and direction The direction-averaged flux of ]

120583is

between 11 and 13 times smaller than that of ]120583 depending

on the energyThe electron (anti)neutrino direction-averagedflux at a few GeV is about 25 times smaller than its muon(anti)neutrino counterpart Figure 2 shows isocontours of theneutrino flux flavor ratio as a function of energy and zenithangle for neutrinos that cross the Earth The flux differencebetween ]

120583and ]

119890grows with both energy and | cos 120579

119911|

Already at 40GeV the direction-averaged ratio is close tofour

Above 10GeV the neutrino flux as a function of zenithangle is almost symmetric around cos 120579

119911= 0 The angular

dependence of the flux at the detection site is influenced byhadronization processes the local atmospheric density andgeomagnetic effects at the interaction pointTheuncertaintiesassociated with these processes result in energy-dependent


400

300

200

100

0

120601E3

(mminus2

secminus

1srminus1

GeV

2)

e

e

120583

120583

HKKM15

BartolFluka

4 6 8 10 20 30 40

E (GeV)


00

minus02

minus04

minus06

minus08

minus10

30

70

20

40

50

60

80

90

100

110

4 6 8 10 20 30 40

E (GeV)

cos(120579z)

(u + u)(e + e)






32≃ Δ119898

2


13 12057923 These






119875120583119890

≃ sin212057923sin22120579119872

13sin2 [Δ119872 119871

4119864] (3)



119875120583120583

≃ 1 minus sin212057911987213sin22120579


119872

+ 119860)119871

8119864]

minus cos212057911987213sin22120579

23sin2 [(Δ + Δ

119872

+ 119860)119871

8119864]

minus sin412057923sin22120579119872

13sin2 [Δ119872 119871

4119864]

(4)


119875120583120591

≃ 1 minus 119875120583119890minus 119875120583120583 (5)


31and Δ


Δ119872

≃ radic(Δ1198982

31cos 2120579

13minus 119860)2

+ (Δ1198982

31sin 2120579

13)2

(6)


value in matter is

sin 212057911987213

≃Δ1198982

31sin 2120579

13

Δ119872 (7)



2


12057913


13can acquire any


2

31cos 2120579

13 which gives

120579119872



13


31


For 119860 ≫ Δ1198982

31cos 2120579



119890rarr ]

120583 given in (3)


00

minus02

minus04

minus06

minus08

minus104 6 8 10 20 30 40 50

cos(120579z)

10

08

06

04

02

00

E (GeV)

e rarr e (NO)

(a)

10

08

06

04

02

00

00

minus02

minus04

minus06

minus08

minus104 6 8 10 20 30 40 50

cos(120579z)

E (GeV)

120583 rarr 120583 (NO)

(b)












119875120583120583

= 1 minus sin2212057923sin2 [Δ 119871

4119864] (8)


120591


21Δ1198982







= 25 cmminus3119873119860 where 119873



Δ1198982

31cos 2120579





120583rarr












120583



119890it is



120583


of ]120583



13 the



31|








119890flux In the






119890+ ]119890for





23and |Δ119898

2


Δ1198982






10

08

06

04

02

005 7 10 20 50

E (GeV)

Tran

sitio

n pr

obab

ility

e rarr 120583e rarr 120591

e rarr e

(a)

5 7 10 20 50

E (GeV)

10

08

06

04

02

00

Tran

sitio

n pr

obab

ility

120583 rarr 120583120583 rarr 120591

120583 rarr e

(b)







140

125

110

095

080

065

050

cos(120579z)

00

minus02

minus04

minus06

minus08

minus104 6 8 10 20 30 5040

E (GeV)










Buoy

IL07

sim480

m

145m

100m

sim180m

Anchorsim180m

Junction box

(a)


LED


Vacuum value

Base

Magnetic shield

(b)






(in red)

Dust layer


(in green)

minus1450

minus1550

minus1650

minus1750

minus1850

minus1950

minus2150

minus2050

minus2250

minus2350

minus2450

75m

40m

DeepCore volume

125m

600m











2







1 100

02

04

06

08

1

12

14

Total

QE

DIS

RES

cr

oss s

ectio

nE(10minus38

cm2G

eV)

10minus1 102

E (GeV)

(a)

0

005

01

015

02

025

03

035

04

1 1010minus1 102

E (GeV)

cros

s sec

tionE(10minus38

cm2G

eV)

Total

QEDIS

RES

(b)




























23and Δ119898

2



2 approxima-tion










2


120583flux and







Num

ber o

f eve

nts

0

20

40

60

80

100

120

140

160

180

200

ERcosΘR (GeV)0 20 40 60 80 100 120 140


6

5

4

3

2

1



Rate

(Hz)










Total simulation

IceCube preliminary


Ratio

120

115

110

105

100

095

090

085

08005 10 15 2520









2




23and Δ119898

2





















0

20

40

60

IceCube preliminary


cos(120579reco)


20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band


0

20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band


20

40

60

cos(120579reco)


0

20

40

60

cos(120579reco)


20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band


0

20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band


20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band

Even

ts pe

r ene

rgy

band

Even

ts pe

r ene

rgy

band

Even

ts pe

r ene

rgy

band




23= 053

+009


2

32=

272+019




23 and +014


for Δ1198982














Detector (far)




Neutrino flux


120583Accelerator ]

120583]120583modes



50

45

40

35

30

25

20

15

10060 065 070 075 080 085 090 095 100

sin2(212057923)

|Δm2 32|

(10minus3

eV2)









102

101

100

Even

ts


cos(120579reco)



102

101

100

Even

ts


cos(120579reco)



102

101

100

Even

ts


cos(120579reco)










800

600

400

200

0

101 102 103

LrecoEreco (kmGeV)

Even

ts


(a)

14

12

10

08

06

04101 102 103

LrecoEreco (kmGeV)

Ratio

to n

o os

c


(b)













120583






23 It is






90 CL contours

T2K 2014 [NH]SK IV 2015 [NH]

43210

38

36

34

32

30

28

26

24

22

20

|Δm2 32|

(10minus3

eV2)

38

36

34

32

30

28

26

24

22

20

|Δm2 32|

(10minus3

eV2)

minus2ΔlnL

minus2Δ

lnL

03 04 05 06 07 0 1 2 3 4

sin2(12057923)

03 04 05

(a)

(b) (c)

06 07

sin2(12057923)


2



Penetrator

PMT baseHV supply


Waist band

Pressure sphere


PMT photocathode








Penetrator

Top hemisphere

Pressure gauge

Nanobeacon


Cooling system (13)

Cooling system (23)


Cooling system (33)


Piezosensor

PMT and base


Valve




Bottom hemisphere







minus150

minus100

minus50

0

50

100


Preliminary

Y(m

)

X (m)

(a)

minus100

minus50

0

50

100



y(m

)

107m


(b)




PINGU 120583 + 120583ORCA 120583 + 120583

E (GeV)

040

035

025

030

020

015

010

005

0005 10 15 20 25 30

Med

ian

frac

tiona

l ene

rgy

reso

lutio

n




PINGU 120583 + 120583ORCA 120583ORCA 120583

20

15

10

5

05 10 15 20 25 30

E (GeV)

Med

ian

zeni

th an

gle r

es (∘ )







Mea

n nu

mbe

r of p

hoto

ns p

er D

OM 1

KM3NeT preliminary

07 lt y lt 08

05 lt y lt 06

02 lt y lt 03

00 lt y lt 01

Bjorken y



10minus2


10

08

06

04

02

002 4 6 8 10 12 14 16 18

E (GeV)

Frac

tion

class

ified

as tr

ack-

like


P e + eO e + eP 120583 + 120583O 120583O120583

P 120591 + 120591O 120591 + 120591P + (NC)O + (NC)


120583performs





12057923 Δ119898231



12057912 Δ119898221







23 Δ119898232 and 120579













23to





23 The




23and the






7

6

5

4

3

2

1

0040 045 050 055 060

sin212057923

120590(3

year

s)


PINGU NOORCA NO

PINGU IOORCA IO

(a)

45

40

35

30

25

20

15

100 1 2 3 4 5



PINGU NOORCA NO

PINGU IOORCA IO

NO 12057923 = 42∘

IO 12057923 = 49∘

Expe

cted

sens

itivi

ty (120590

)

(b)




23= 42∘ for a NMO 120579

23= 49∘ for an IMO) From [85 91]





6 Summary


23and |Δ1198982

32| Constant



2

31and completely


23) of




Acknowledgments


References

































































































































FluidsJournal of


Journal of










Superconductivity




GravityJournal of








Journal of






Volume 2014


PhotonicsJournal of


Journal of

Biophysics




400

300

200

100

0

120601E3

(mminus2

secminus

1srminus1

GeV

2)

e

e

120583

120583

HKKM15

BartolFluka

4 6 8 10 20 30 40

E (GeV)


00

minus02

minus04

minus06

minus08

minus10

30

70

20

40

50

60

80

90

100

110

4 6 8 10 20 30 40

E (GeV)

cos(120579z)

(u + u)(e + e)






32≃ Δ119898

2


13 12057923 These






119875120583119890

≃ sin212057923sin22120579119872

13sin2 [Δ119872 119871

4119864] (3)



119875120583120583

≃ 1 minus sin212057911987213sin22120579


119872

+ 119860)119871

8119864]

minus cos212057911987213sin22120579

23sin2 [(Δ + Δ

119872

+ 119860)119871

8119864]

minus sin412057923sin22120579119872

13sin2 [Δ119872 119871

4119864]

(4)


119875120583120591

≃ 1 minus 119875120583119890minus 119875120583120583 (5)


31and Δ


Δ119872

≃ radic(Δ1198982

31cos 2120579

13minus 119860)2

+ (Δ1198982

31sin 2120579

13)2

(6)


value in matter is

sin 212057911987213

≃Δ1198982

31sin 2120579

13

Δ119872 (7)



2


12057913


13can acquire any


2

31cos 2120579

13 which gives

120579119872



13


31


For 119860 ≫ Δ1198982

31cos 2120579



119890rarr ]

120583 given in (3)


00

minus02

minus04

minus06

minus08

minus104 6 8 10 20 30 40 50

cos(120579z)

10

08

06

04

02

00

E (GeV)

e rarr e (NO)

(a)

10

08

06

04

02

00

00

minus02

minus04

minus06

minus08

minus104 6 8 10 20 30 40 50

cos(120579z)

E (GeV)

120583 rarr 120583 (NO)

(b)












119875120583120583

= 1 minus sin2212057923sin2 [Δ 119871

4119864] (8)


120591


21Δ1198982







= 25 cmminus3119873119860 where 119873



Δ1198982

31cos 2120579





120583rarr












120583



119890it is



120583


of ]120583



13 the



31|








119890flux In the






119890+ ]119890for





23and |Δ119898

2


Δ1198982






10

08

06

04

02

005 7 10 20 50

E (GeV)

Tran

sitio

n pr

obab

ility

e rarr 120583e rarr 120591

e rarr e

(a)

5 7 10 20 50

E (GeV)

10

08

06

04

02

00

Tran

sitio

n pr

obab

ility

120583 rarr 120583120583 rarr 120591

120583 rarr e

(b)







140

125

110

095

080

065

050

cos(120579z)

00

minus02

minus04

minus06

minus08

minus104 6 8 10 20 30 5040

E (GeV)










Buoy

IL07

sim480

m

145m

100m

sim180m

Anchorsim180m

Junction box

(a)


LED


Vacuum value

Base

Magnetic shield

(b)






(in red)

Dust layer


(in green)

minus1450

minus1550

minus1650

minus1750

minus1850

minus1950

minus2150

minus2050

minus2250

minus2350

minus2450

75m

40m

DeepCore volume

125m

600m











2







1 100

02

04

06

08

1

12

14

Total

QE

DIS

RES

cr

oss s

ectio

nE(10minus38

cm2G

eV)

10minus1 102

E (GeV)

(a)

0

005

01

015

02

025

03

035

04

1 1010minus1 102

E (GeV)

cros

s sec

tionE(10minus38

cm2G

eV)

Total

QEDIS

RES

(b)




























23and Δ119898

2



2 approxima-tion










2


120583flux and







Num

ber o

f eve

nts

0

20

40

60

80

100

120

140

160

180

200

ERcosΘR (GeV)0 20 40 60 80 100 120 140


6

5

4

3

2

1



Rate

(Hz)










Total simulation

IceCube preliminary


Ratio

120

115

110

105

100

095

090

085

08005 10 15 2520









2




23and Δ119898

2





















0

20

40

60

IceCube preliminary


cos(120579reco)


20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band


0

20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band


20

40

60

cos(120579reco)


0

20

40

60

cos(120579reco)


20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band


0

20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band


20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band

Even

ts pe

r ene

rgy

band

Even

ts pe

r ene

rgy

band

Even

ts pe

r ene

rgy

band




23= 053

+009


2

32=

272+019




23 and +014


for Δ1198982














Detector (far)




Neutrino flux


120583Accelerator ]

120583]120583modes



50

45

40

35

30

25

20

15

10060 065 070 075 080 085 090 095 100

sin2(212057923)

|Δm2 32|

(10minus3

eV2)









102

101

100

Even

ts


cos(120579reco)



102

101

100

Even

ts


cos(120579reco)



102

101

100

Even

ts


cos(120579reco)










800

600

400

200

0

101 102 103

LrecoEreco (kmGeV)

Even

ts


(a)

14

12

10

08

06

04101 102 103

LrecoEreco (kmGeV)

Ratio

to n

o os

c


(b)













120583






23 It is






90 CL contours

T2K 2014 [NH]SK IV 2015 [NH]

43210

38

36

34

32

30

28

26

24

22

20

|Δm2 32|

(10minus3

eV2)

38

36

34

32

30

28

26

24

22

20

|Δm2 32|

(10minus3

eV2)

minus2ΔlnL

minus2Δ

lnL

03 04 05 06 07 0 1 2 3 4

sin2(12057923)

03 04 05

(a)

(b) (c)

06 07

sin2(12057923)


2



Penetrator

PMT baseHV supply


Waist band

Pressure sphere


PMT photocathode








Penetrator

Top hemisphere

Pressure gauge

Nanobeacon


Cooling system (13)

Cooling system (23)


Cooling system (33)


Piezosensor

PMT and base


Valve




Bottom hemisphere







minus150

minus100

minus50

0

50

100


Preliminary

Y(m

)

X (m)

(a)

minus100

minus50

0

50

100



y(m

)

107m


(b)




PINGU 120583 + 120583ORCA 120583 + 120583

E (GeV)

040

035

025

030

020

015

010

005

0005 10 15 20 25 30

Med

ian

frac

tiona

l ene

rgy

reso

lutio

n




PINGU 120583 + 120583ORCA 120583ORCA 120583

20

15

10

5

05 10 15 20 25 30

E (GeV)

Med

ian

zeni

th an

gle r

es (∘ )







Mea

n nu

mbe

r of p

hoto

ns p

er D

OM 1

KM3NeT preliminary

07 lt y lt 08

05 lt y lt 06

02 lt y lt 03

00 lt y lt 01

Bjorken y



10minus2


10

08

06

04

02

002 4 6 8 10 12 14 16 18

E (GeV)

Frac

tion

class

ified

as tr

ack-

like


P e + eO e + eP 120583 + 120583O 120583O120583

P 120591 + 120591O 120591 + 120591P + (NC)O + (NC)


120583performs





12057923 Δ119898231



12057912 Δ119898221







23 Δ119898232 and 120579













23to





23 The




23and the






7

6

5

4

3

2

1

0040 045 050 055 060

sin212057923

120590(3

year

s)


PINGU NOORCA NO

PINGU IOORCA IO

(a)

45

40

35

30

25

20

15

100 1 2 3 4 5



PINGU NOORCA NO

PINGU IOORCA IO

NO 12057923 = 42∘

IO 12057923 = 49∘

Expe

cted

sens

itivi

ty (120590

)

(b)




23= 42∘ for a NMO 120579

23= 49∘ for an IMO) From [85 91]





6 Summary


23and |Δ1198982

32| Constant



2

31and completely


23) of




Acknowledgments


References

































































































































FluidsJournal of


Journal of










Superconductivity




GravityJournal of








Journal of






Volume 2014


PhotonicsJournal of


Journal of

Biophysics




00

minus02

minus04

minus06

minus08

minus104 6 8 10 20 30 40 50

cos(120579z)

10

08

06

04

02

00

E (GeV)

e rarr e (NO)

(a)

10

08

06

04

02

00

00

minus02

minus04

minus06

minus08

minus104 6 8 10 20 30 40 50

cos(120579z)

E (GeV)

120583 rarr 120583 (NO)

(b)












119875120583120583

= 1 minus sin2212057923sin2 [Δ 119871

4119864] (8)


120591


21Δ1198982







= 25 cmminus3119873119860 where 119873



Δ1198982

31cos 2120579





120583rarr












120583



119890it is



120583


of ]120583



13 the



31|








119890flux In the






119890+ ]119890for





23and |Δ119898

2


Δ1198982






10

08

06

04

02

005 7 10 20 50

E (GeV)

Tran

sitio

n pr

obab

ility

e rarr 120583e rarr 120591

e rarr e

(a)

5 7 10 20 50

E (GeV)

10

08

06

04

02

00

Tran

sitio

n pr

obab

ility

120583 rarr 120583120583 rarr 120591

120583 rarr e

(b)







140

125

110

095

080

065

050

cos(120579z)

00

minus02

minus04

minus06

minus08

minus104 6 8 10 20 30 5040

E (GeV)










Buoy

IL07

sim480

m

145m

100m

sim180m

Anchorsim180m

Junction box

(a)


LED


Vacuum value

Base

Magnetic shield

(b)






(in red)

Dust layer


(in green)

minus1450

minus1550

minus1650

minus1750

minus1850

minus1950

minus2150

minus2050

minus2250

minus2350

minus2450

75m

40m

DeepCore volume

125m

600m











2







1 100

02

04

06

08

1

12

14

Total

QE

DIS

RES

cr

oss s

ectio

nE(10minus38

cm2G

eV)

10minus1 102

E (GeV)

(a)

0

005

01

015

02

025

03

035

04

1 1010minus1 102

E (GeV)

cros

s sec

tionE(10minus38

cm2G

eV)

Total

QEDIS

RES

(b)




























23and Δ119898

2



2 approxima-tion










2


120583flux and







Num

ber o

f eve

nts

0

20

40

60

80

100

120

140

160

180

200

ERcosΘR (GeV)0 20 40 60 80 100 120 140


6

5

4

3

2

1



Rate

(Hz)










Total simulation

IceCube preliminary


Ratio

120

115

110

105

100

095

090

085

08005 10 15 2520









2




23and Δ119898

2





















0

20

40

60

IceCube preliminary


cos(120579reco)


20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band


0

20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band


20

40

60

cos(120579reco)


0

20

40

60

cos(120579reco)


20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band


0

20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band


20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band

Even

ts pe

r ene

rgy

band

Even

ts pe

r ene

rgy

band

Even

ts pe

r ene

rgy

band




23= 053

+009


2

32=

272+019




23 and +014


for Δ1198982














Detector (far)




Neutrino flux


120583Accelerator ]

120583]120583modes



50

45

40

35

30

25

20

15

10060 065 070 075 080 085 090 095 100

sin2(212057923)

|Δm2 32|

(10minus3

eV2)









102

101

100

Even

ts


cos(120579reco)



102

101

100

Even

ts


cos(120579reco)



102

101

100

Even

ts


cos(120579reco)










800

600

400

200

0

101 102 103

LrecoEreco (kmGeV)

Even

ts


(a)

14

12

10

08

06

04101 102 103

LrecoEreco (kmGeV)

Ratio

to n

o os

c


(b)













120583






23 It is






90 CL contours

T2K 2014 [NH]SK IV 2015 [NH]

43210

38

36

34

32

30

28

26

24

22

20

|Δm2 32|

(10minus3

eV2)

38

36

34

32

30

28

26

24

22

20

|Δm2 32|

(10minus3

eV2)

minus2ΔlnL

minus2Δ

lnL

03 04 05 06 07 0 1 2 3 4

sin2(12057923)

03 04 05

(a)

(b) (c)

06 07

sin2(12057923)


2



Penetrator

PMT baseHV supply


Waist band

Pressure sphere


PMT photocathode








Penetrator

Top hemisphere

Pressure gauge

Nanobeacon


Cooling system (13)

Cooling system (23)


Cooling system (33)


Piezosensor

PMT and base


Valve




Bottom hemisphere







minus150

minus100

minus50

0

50

100


Preliminary

Y(m

)

X (m)

(a)

minus100

minus50

0

50

100



y(m

)

107m


(b)




PINGU 120583 + 120583ORCA 120583 + 120583

E (GeV)

040

035

025

030

020

015

010

005

0005 10 15 20 25 30

Med

ian

frac

tiona

l ene

rgy

reso

lutio

n




PINGU 120583 + 120583ORCA 120583ORCA 120583

20

15

10

5

05 10 15 20 25 30

E (GeV)

Med

ian

zeni

th an

gle r

es (∘ )







Mea

n nu

mbe

r of p

hoto

ns p

er D

OM 1

KM3NeT preliminary

07 lt y lt 08

05 lt y lt 06

02 lt y lt 03

00 lt y lt 01

Bjorken y



10minus2


10

08

06

04

02

002 4 6 8 10 12 14 16 18

E (GeV)

Frac

tion

class

ified

as tr

ack-

like


P e + eO e + eP 120583 + 120583O 120583O120583

P 120591 + 120591O 120591 + 120591P + (NC)O + (NC)


120583performs





12057923 Δ119898231



12057912 Δ119898221







23 Δ119898232 and 120579













23to





23 The




23and the






7

6

5

4

3

2

1

0040 045 050 055 060

sin212057923

120590(3

year

s)


PINGU NOORCA NO

PINGU IOORCA IO

(a)

45

40

35

30

25

20

15

100 1 2 3 4 5



PINGU NOORCA NO

PINGU IOORCA IO

NO 12057923 = 42∘

IO 12057923 = 49∘

Expe

cted

sens

itivi

ty (120590

)

(b)




23= 42∘ for a NMO 120579

23= 49∘ for an IMO) From [85 91]





6 Summary


23and |Δ1198982

32| Constant



2

31and completely


23) of




Acknowledgments


References

































































































































FluidsJournal of


Journal of










Superconductivity




GravityJournal of








Journal of






Volume 2014


PhotonicsJournal of


Journal of

Biophysics





13 the



31|








119890flux In the






119890+ ]119890for





23and |Δ119898

2


Δ1198982






10

08

06

04

02

005 7 10 20 50

E (GeV)

Tran

sitio

n pr

obab

ility

e rarr 120583e rarr 120591

e rarr e

(a)

5 7 10 20 50

E (GeV)

10

08

06

04

02

00

Tran

sitio

n pr

obab

ility

120583 rarr 120583120583 rarr 120591

120583 rarr e

(b)







140

125

110

095

080

065

050

cos(120579z)

00

minus02

minus04

minus06

minus08

minus104 6 8 10 20 30 5040

E (GeV)










Buoy

IL07

sim480

m

145m

100m

sim180m

Anchorsim180m

Junction box

(a)


LED


Vacuum value

Base

Magnetic shield

(b)






(in red)

Dust layer


(in green)

minus1450

minus1550

minus1650

minus1750

minus1850

minus1950

minus2150

minus2050

minus2250

minus2350

minus2450

75m

40m

DeepCore volume

125m

600m











2







1 100

02

04

06

08

1

12

14

Total

QE

DIS

RES

cr

oss s

ectio

nE(10minus38

cm2G

eV)

10minus1 102

E (GeV)

(a)

0

005

01

015

02

025

03

035

04

1 1010minus1 102

E (GeV)

cros

s sec

tionE(10minus38

cm2G

eV)

Total

QEDIS

RES

(b)




























23and Δ119898

2



2 approxima-tion










2


120583flux and







Num

ber o

f eve

nts

0

20

40

60

80

100

120

140

160

180

200

ERcosΘR (GeV)0 20 40 60 80 100 120 140


6

5

4

3

2

1



Rate

(Hz)










Total simulation

IceCube preliminary


Ratio

120

115

110

105

100

095

090

085

08005 10 15 2520









2




23and Δ119898

2





















0

20

40

60

IceCube preliminary


cos(120579reco)


20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band


0

20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band


20

40

60

cos(120579reco)


0

20

40

60

cos(120579reco)


20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band


0

20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band


20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band

Even

ts pe

r ene

rgy

band

Even

ts pe

r ene

rgy

band

Even

ts pe

r ene

rgy

band




23= 053

+009


2

32=

272+019




23 and +014


for Δ1198982














Detector (far)




Neutrino flux


120583Accelerator ]

120583]120583modes



50

45

40

35

30

25

20

15

10060 065 070 075 080 085 090 095 100

sin2(212057923)

|Δm2 32|

(10minus3

eV2)









102

101

100

Even

ts


cos(120579reco)



102

101

100

Even

ts


cos(120579reco)



102

101

100

Even

ts


cos(120579reco)










800

600

400

200

0

101 102 103

LrecoEreco (kmGeV)

Even

ts


(a)

14

12

10

08

06

04101 102 103

LrecoEreco (kmGeV)

Ratio

to n

o os

c


(b)













120583






23 It is






90 CL contours

T2K 2014 [NH]SK IV 2015 [NH]

43210

38

36

34

32

30

28

26

24

22

20

|Δm2 32|

(10minus3

eV2)

38

36

34

32

30

28

26

24

22

20

|Δm2 32|

(10minus3

eV2)

minus2ΔlnL

minus2Δ

lnL

03 04 05 06 07 0 1 2 3 4

sin2(12057923)

03 04 05

(a)

(b) (c)

06 07

sin2(12057923)


2



Penetrator

PMT baseHV supply


Waist band

Pressure sphere


PMT photocathode








Penetrator

Top hemisphere

Pressure gauge

Nanobeacon


Cooling system (13)

Cooling system (23)


Cooling system (33)


Piezosensor

PMT and base


Valve




Bottom hemisphere







minus150

minus100

minus50

0

50

100


Preliminary

Y(m

)

X (m)

(a)

minus100

minus50

0

50

100



y(m

)

107m


(b)




PINGU 120583 + 120583ORCA 120583 + 120583

E (GeV)

040

035

025

030

020

015

010

005

0005 10 15 20 25 30

Med

ian

frac

tiona

l ene

rgy

reso

lutio

n




PINGU 120583 + 120583ORCA 120583ORCA 120583

20

15

10

5

05 10 15 20 25 30

E (GeV)

Med

ian

zeni

th an

gle r

es (∘ )







Mea

n nu

mbe

r of p

hoto

ns p

er D

OM 1

KM3NeT preliminary

07 lt y lt 08

05 lt y lt 06

02 lt y lt 03

00 lt y lt 01

Bjorken y



10minus2


10

08

06

04

02

002 4 6 8 10 12 14 16 18

E (GeV)

Frac

tion

class

ified

as tr

ack-

like


P e + eO e + eP 120583 + 120583O 120583O120583

P 120591 + 120591O 120591 + 120591P + (NC)O + (NC)


120583performs





12057923 Δ119898231



12057912 Δ119898221







23 Δ119898232 and 120579













23to





23 The




23and the






7

6

5

4

3

2

1

0040 045 050 055 060

sin212057923

120590(3

year

s)


PINGU NOORCA NO

PINGU IOORCA IO

(a)

45

40

35

30

25

20

15

100 1 2 3 4 5



PINGU NOORCA NO

PINGU IOORCA IO

NO 12057923 = 42∘

IO 12057923 = 49∘

Expe

cted

sens

itivi

ty (120590

)

(b)




23= 42∘ for a NMO 120579

23= 49∘ for an IMO) From [85 91]





6 Summary


23and |Δ1198982

32| Constant



2

31and completely


23) of




Acknowledgments


References

































































































































FluidsJournal of


Journal of










Superconductivity




GravityJournal of








Journal of






Volume 2014


PhotonicsJournal of


Journal of

Biophysics




140

125

110

095

080

065

050

cos(120579z)

00

minus02

minus04

minus06

minus08

minus104 6 8 10 20 30 5040

E (GeV)










Buoy

IL07

sim480

m

145m

100m

sim180m

Anchorsim180m

Junction box

(a)


LED


Vacuum value

Base

Magnetic shield

(b)






(in red)

Dust layer


(in green)

minus1450

minus1550

minus1650

minus1750

minus1850

minus1950

minus2150

minus2050

minus2250

minus2350

minus2450

75m

40m

DeepCore volume

125m

600m











2







1 100

02

04

06

08

1

12

14

Total

QE

DIS

RES

cr

oss s

ectio

nE(10minus38

cm2G

eV)

10minus1 102

E (GeV)

(a)

0

005

01

015

02

025

03

035

04

1 1010minus1 102

E (GeV)

cros

s sec

tionE(10minus38

cm2G

eV)

Total

QEDIS

RES

(b)




























23and Δ119898

2



2 approxima-tion










2


120583flux and







Num

ber o

f eve

nts

0

20

40

60

80

100

120

140

160

180

200

ERcosΘR (GeV)0 20 40 60 80 100 120 140


6

5

4

3

2

1



Rate

(Hz)










Total simulation

IceCube preliminary


Ratio

120

115

110

105

100

095

090

085

08005 10 15 2520









2




23and Δ119898

2





















0

20

40

60

IceCube preliminary


cos(120579reco)


20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band


0

20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band


20

40

60

cos(120579reco)


0

20

40

60

cos(120579reco)


20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band


0

20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band


20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band

Even

ts pe

r ene

rgy

band

Even

ts pe

r ene

rgy

band

Even

ts pe

r ene

rgy

band




23= 053

+009


2

32=

272+019




23 and +014


for Δ1198982














Detector (far)




Neutrino flux


120583Accelerator ]

120583]120583modes



50

45

40

35

30

25

20

15

10060 065 070 075 080 085 090 095 100

sin2(212057923)

|Δm2 32|

(10minus3

eV2)









102

101

100

Even

ts


cos(120579reco)



102

101

100

Even

ts


cos(120579reco)



102

101

100

Even

ts


cos(120579reco)










800

600

400

200

0

101 102 103

LrecoEreco (kmGeV)

Even

ts


(a)

14

12

10

08

06

04101 102 103

LrecoEreco (kmGeV)

Ratio

to n

o os

c


(b)













120583






23 It is






90 CL contours

T2K 2014 [NH]SK IV 2015 [NH]

43210

38

36

34

32

30

28

26

24

22

20

|Δm2 32|

(10minus3

eV2)

38

36

34

32

30

28

26

24

22

20

|Δm2 32|

(10minus3

eV2)

minus2ΔlnL

minus2Δ

lnL

03 04 05 06 07 0 1 2 3 4

sin2(12057923)

03 04 05

(a)

(b) (c)

06 07

sin2(12057923)


2



Penetrator

PMT baseHV supply


Waist band

Pressure sphere


PMT photocathode








Penetrator

Top hemisphere

Pressure gauge

Nanobeacon


Cooling system (13)

Cooling system (23)


Cooling system (33)


Piezosensor

PMT and base


Valve




Bottom hemisphere







minus150

minus100

minus50

0

50

100


Preliminary

Y(m

)

X (m)

(a)

minus100

minus50

0

50

100



y(m

)

107m


(b)




PINGU 120583 + 120583ORCA 120583 + 120583

E (GeV)

040

035

025

030

020

015

010

005

0005 10 15 20 25 30

Med

ian

frac

tiona

l ene

rgy

reso

lutio

n




PINGU 120583 + 120583ORCA 120583ORCA 120583

20

15

10

5

05 10 15 20 25 30

E (GeV)

Med

ian

zeni

th an

gle r

es (∘ )







Mea

n nu

mbe

r of p

hoto

ns p

er D

OM 1

KM3NeT preliminary

07 lt y lt 08

05 lt y lt 06

02 lt y lt 03

00 lt y lt 01

Bjorken y



10minus2


10

08

06

04

02

002 4 6 8 10 12 14 16 18

E (GeV)

Frac

tion

class

ified

as tr

ack-

like


P e + eO e + eP 120583 + 120583O 120583O120583

P 120591 + 120591O 120591 + 120591P + (NC)O + (NC)


120583performs





12057923 Δ119898231



12057912 Δ119898221







23 Δ119898232 and 120579













23to





23 The




23and the






7

6

5

4

3

2

1

0040 045 050 055 060

sin212057923

120590(3

year

s)


PINGU NOORCA NO

PINGU IOORCA IO

(a)

45

40

35

30

25

20

15

100 1 2 3 4 5



PINGU NOORCA NO

PINGU IOORCA IO

NO 12057923 = 42∘

IO 12057923 = 49∘

Expe

cted

sens

itivi

ty (120590

)

(b)




23= 42∘ for a NMO 120579

23= 49∘ for an IMO) From [85 91]





6 Summary


23and |Δ1198982

32| Constant



2

31and completely


23) of




Acknowledgments


References

































































































































FluidsJournal of


Journal of










Superconductivity




GravityJournal of








Journal of






Volume 2014


PhotonicsJournal of


Journal of

Biophysics





(in red)

Dust layer


(in green)

minus1450

minus1550

minus1650

minus1750

minus1850

minus1950

minus2150

minus2050

minus2250

minus2350

minus2450

75m

40m

DeepCore volume

125m

600m











2







1 100

02

04

06

08

1

12

14

Total

QE

DIS

RES

cr

oss s

ectio

nE(10minus38

cm2G

eV)

10minus1 102

E (GeV)

(a)

0

005

01

015

02

025

03

035

04

1 1010minus1 102

E (GeV)

cros

s sec

tionE(10minus38

cm2G

eV)

Total

QEDIS

RES

(b)




























23and Δ119898

2



2 approxima-tion










2


120583flux and







Num

ber o

f eve

nts

0

20

40

60

80

100

120

140

160

180

200

ERcosΘR (GeV)0 20 40 60 80 100 120 140


6

5

4

3

2

1



Rate

(Hz)










Total simulation

IceCube preliminary


Ratio

120

115

110

105

100

095

090

085

08005 10 15 2520









2




23and Δ119898

2





















0

20

40

60

IceCube preliminary


cos(120579reco)


20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band


0

20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band


20

40

60

cos(120579reco)


0

20

40

60

cos(120579reco)


20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band


0

20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band


20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band

Even

ts pe

r ene

rgy

band

Even

ts pe

r ene

rgy

band

Even

ts pe

r ene

rgy

band




23= 053

+009


2

32=

272+019




23 and +014


for Δ1198982














Detector (far)




Neutrino flux


120583Accelerator ]

120583]120583modes



50

45

40

35

30

25

20

15

10060 065 070 075 080 085 090 095 100

sin2(212057923)

|Δm2 32|

(10minus3

eV2)









102

101

100

Even

ts


cos(120579reco)



102

101

100

Even

ts


cos(120579reco)



102

101

100

Even

ts


cos(120579reco)










800

600

400

200

0

101 102 103

LrecoEreco (kmGeV)

Even

ts


(a)

14

12

10

08

06

04101 102 103

LrecoEreco (kmGeV)

Ratio

to n

o os

c


(b)













120583






23 It is






90 CL contours

T2K 2014 [NH]SK IV 2015 [NH]

43210

38

36

34

32

30

28

26

24

22

20

|Δm2 32|

(10minus3

eV2)

38

36

34

32

30

28

26

24

22

20

|Δm2 32|

(10minus3

eV2)

minus2ΔlnL

minus2Δ

lnL

03 04 05 06 07 0 1 2 3 4

sin2(12057923)

03 04 05

(a)

(b) (c)

06 07

sin2(12057923)


2



Penetrator

PMT baseHV supply


Waist band

Pressure sphere


PMT photocathode








Penetrator

Top hemisphere

Pressure gauge

Nanobeacon


Cooling system (13)

Cooling system (23)


Cooling system (33)


Piezosensor

PMT and base


Valve




Bottom hemisphere







minus150

minus100

minus50

0

50

100


Preliminary

Y(m

)

X (m)

(a)

minus100

minus50

0

50

100



y(m

)

107m


(b)




PINGU 120583 + 120583ORCA 120583 + 120583

E (GeV)

040

035

025

030

020

015

010

005

0005 10 15 20 25 30

Med

ian

frac

tiona

l ene

rgy

reso

lutio

n




PINGU 120583 + 120583ORCA 120583ORCA 120583

20

15

10

5

05 10 15 20 25 30

E (GeV)

Med

ian

zeni

th an

gle r

es (∘ )







Mea

n nu

mbe

r of p

hoto

ns p

er D

OM 1

KM3NeT preliminary

07 lt y lt 08

05 lt y lt 06

02 lt y lt 03

00 lt y lt 01

Bjorken y



10minus2


10

08

06

04

02

002 4 6 8 10 12 14 16 18

E (GeV)

Frac

tion

class

ified

as tr

ack-

like


P e + eO e + eP 120583 + 120583O 120583O120583

P 120591 + 120591O 120591 + 120591P + (NC)O + (NC)


120583performs





12057923 Δ119898231



12057912 Δ119898221







23 Δ119898232 and 120579













23to





23 The




23and the






7

6

5

4

3

2

1

0040 045 050 055 060

sin212057923

120590(3

year

s)


PINGU NOORCA NO

PINGU IOORCA IO

(a)

45

40

35

30

25

20

15

100 1 2 3 4 5



PINGU NOORCA NO

PINGU IOORCA IO

NO 12057923 = 42∘

IO 12057923 = 49∘

Expe

cted

sens

itivi

ty (120590

)

(b)




23= 42∘ for a NMO 120579

23= 49∘ for an IMO) From [85 91]





6 Summary


23and |Δ1198982

32| Constant



2

31and completely


23) of




Acknowledgments


References

































































































































FluidsJournal of


Journal of










Superconductivity




GravityJournal of








Journal of






Volume 2014


PhotonicsJournal of


Journal of

Biophysics




1 100

02

04

06

08

1

12

14

Total

QE

DIS

RES

cr

oss s

ectio

nE(10minus38

cm2G

eV)

10minus1 102

E (GeV)

(a)

0

005

01

015

02

025

03

035

04

1 1010minus1 102

E (GeV)

cros

s sec

tionE(10minus38

cm2G

eV)

Total

QEDIS

RES

(b)




























23and Δ119898

2



2 approxima-tion










2


120583flux and







Num

ber o

f eve

nts

0

20

40

60

80

100

120

140

160

180

200

ERcosΘR (GeV)0 20 40 60 80 100 120 140


6

5

4

3

2

1



Rate

(Hz)










Total simulation

IceCube preliminary


Ratio

120

115

110

105

100

095

090

085

08005 10 15 2520









2




23and Δ119898

2





















0

20

40

60

IceCube preliminary


cos(120579reco)


20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band


0

20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band


20

40

60

cos(120579reco)


0

20

40

60

cos(120579reco)


20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band


0

20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band


20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band

Even

ts pe

r ene

rgy

band

Even

ts pe

r ene

rgy

band

Even

ts pe

r ene

rgy

band




23= 053

+009


2

32=

272+019




23 and +014


for Δ1198982














Detector (far)




Neutrino flux


120583Accelerator ]

120583]120583modes



50

45

40

35

30

25

20

15

10060 065 070 075 080 085 090 095 100

sin2(212057923)

|Δm2 32|

(10minus3

eV2)









102

101

100

Even

ts


cos(120579reco)



102

101

100

Even

ts


cos(120579reco)



102

101

100

Even

ts


cos(120579reco)










800

600

400

200

0

101 102 103

LrecoEreco (kmGeV)

Even

ts


(a)

14

12

10

08

06

04101 102 103

LrecoEreco (kmGeV)

Ratio

to n

o os

c


(b)













120583






23 It is






90 CL contours

T2K 2014 [NH]SK IV 2015 [NH]

43210

38

36

34

32

30

28

26

24

22

20

|Δm2 32|

(10minus3

eV2)

38

36

34

32

30

28

26

24

22

20

|Δm2 32|

(10minus3

eV2)

minus2ΔlnL

minus2Δ

lnL

03 04 05 06 07 0 1 2 3 4

sin2(12057923)

03 04 05

(a)

(b) (c)

06 07

sin2(12057923)


2



Penetrator

PMT baseHV supply


Waist band

Pressure sphere


PMT photocathode








Penetrator

Top hemisphere

Pressure gauge

Nanobeacon


Cooling system (13)

Cooling system (23)


Cooling system (33)


Piezosensor

PMT and base


Valve




Bottom hemisphere







minus150

minus100

minus50

0

50

100


Preliminary

Y(m

)

X (m)

(a)

minus100

minus50

0

50

100



y(m

)

107m


(b)




PINGU 120583 + 120583ORCA 120583 + 120583

E (GeV)

040

035

025

030

020

015

010

005

0005 10 15 20 25 30

Med

ian

frac

tiona

l ene

rgy

reso

lutio

n




PINGU 120583 + 120583ORCA 120583ORCA 120583

20

15

10

5

05 10 15 20 25 30

E (GeV)

Med

ian

zeni

th an

gle r

es (∘ )







Mea

n nu

mbe

r of p

hoto

ns p

er D

OM 1

KM3NeT preliminary

07 lt y lt 08

05 lt y lt 06

02 lt y lt 03

00 lt y lt 01

Bjorken y



10minus2


10

08

06

04

02

002 4 6 8 10 12 14 16 18

E (GeV)

Frac

tion

class

ified

as tr

ack-

like


P e + eO e + eP 120583 + 120583O 120583O120583

P 120591 + 120591O 120591 + 120591P + (NC)O + (NC)


120583performs





12057923 Δ119898231



12057912 Δ119898221







23 Δ119898232 and 120579













23to





23 The




23and the






7

6

5

4

3

2

1

0040 045 050 055 060

sin212057923

120590(3

year

s)


PINGU NOORCA NO

PINGU IOORCA IO

(a)

45

40

35

30

25

20

15

100 1 2 3 4 5



PINGU NOORCA NO

PINGU IOORCA IO

NO 12057923 = 42∘

IO 12057923 = 49∘

Expe

cted

sens

itivi

ty (120590

)

(b)




23= 42∘ for a NMO 120579

23= 49∘ for an IMO) From [85 91]





6 Summary


23and |Δ1198982

32| Constant



2

31and completely


23) of




Acknowledgments


References

































































































































FluidsJournal of


Journal of










Superconductivity




GravityJournal of








Journal of






Volume 2014


PhotonicsJournal of


Journal of

Biophysics
















23and Δ119898

2



2 approxima-tion










2


120583flux and







Num

ber o

f eve

nts

0

20

40

60

80

100

120

140

160

180

200

ERcosΘR (GeV)0 20 40 60 80 100 120 140


6

5

4

3

2

1



Rate

(Hz)










Total simulation

IceCube preliminary


Ratio

120

115

110

105

100

095

090

085

08005 10 15 2520









2




23and Δ119898

2





















0

20

40

60

IceCube preliminary


cos(120579reco)


20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band


0

20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band


20

40

60

cos(120579reco)


0

20

40

60

cos(120579reco)


20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band


0

20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band


20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band

Even

ts pe

r ene

rgy

band

Even

ts pe

r ene

rgy

band

Even

ts pe

r ene

rgy

band




23= 053

+009


2

32=

272+019




23 and +014


for Δ1198982














Detector (far)




Neutrino flux


120583Accelerator ]

120583]120583modes



50

45

40

35

30

25

20

15

10060 065 070 075 080 085 090 095 100

sin2(212057923)

|Δm2 32|

(10minus3

eV2)









102

101

100

Even

ts


cos(120579reco)



102

101

100

Even

ts


cos(120579reco)



102

101

100

Even

ts


cos(120579reco)










800

600

400

200

0

101 102 103

LrecoEreco (kmGeV)

Even

ts


(a)

14

12

10

08

06

04101 102 103

LrecoEreco (kmGeV)

Ratio

to n

o os

c


(b)













120583






23 It is






90 CL contours

T2K 2014 [NH]SK IV 2015 [NH]

43210

38

36

34

32

30

28

26

24

22

20

|Δm2 32|

(10minus3

eV2)

38

36

34

32

30

28

26

24

22

20

|Δm2 32|

(10minus3

eV2)

minus2ΔlnL

minus2Δ

lnL

03 04 05 06 07 0 1 2 3 4

sin2(12057923)

03 04 05

(a)

(b) (c)

06 07

sin2(12057923)


2



Penetrator

PMT baseHV supply


Waist band

Pressure sphere


PMT photocathode








Penetrator

Top hemisphere

Pressure gauge

Nanobeacon


Cooling system (13)

Cooling system (23)


Cooling system (33)


Piezosensor

PMT and base


Valve




Bottom hemisphere







minus150

minus100

minus50

0

50

100


Preliminary

Y(m

)

X (m)

(a)

minus100

minus50

0

50

100



y(m

)

107m


(b)




PINGU 120583 + 120583ORCA 120583 + 120583

E (GeV)

040

035

025

030

020

015

010

005

0005 10 15 20 25 30

Med

ian

frac

tiona

l ene

rgy

reso

lutio

n




PINGU 120583 + 120583ORCA 120583ORCA 120583

20

15

10

5

05 10 15 20 25 30

E (GeV)

Med

ian

zeni

th an

gle r

es (∘ )







Mea

n nu

mbe

r of p

hoto

ns p

er D

OM 1

KM3NeT preliminary

07 lt y lt 08

05 lt y lt 06

02 lt y lt 03

00 lt y lt 01

Bjorken y



10minus2


10

08

06

04

02

002 4 6 8 10 12 14 16 18

E (GeV)

Frac

tion

class

ified

as tr

ack-

like


P e + eO e + eP 120583 + 120583O 120583O120583

P 120591 + 120591O 120591 + 120591P + (NC)O + (NC)


120583performs





12057923 Δ119898231



12057912 Δ119898221







23 Δ119898232 and 120579













23to





23 The




23and the






7

6

5

4

3

2

1

0040 045 050 055 060

sin212057923

120590(3

year

s)


PINGU NOORCA NO

PINGU IOORCA IO

(a)

45

40

35

30

25

20

15

100 1 2 3 4 5



PINGU NOORCA NO

PINGU IOORCA IO

NO 12057923 = 42∘

IO 12057923 = 49∘

Expe

cted

sens

itivi

ty (120590

)

(b)




23= 42∘ for a NMO 120579

23= 49∘ for an IMO) From [85 91]





6 Summary


23and |Δ1198982

32| Constant



2

31and completely


23) of




Acknowledgments


References

































































































































FluidsJournal of


Journal of










Superconductivity




GravityJournal of








Journal of






Volume 2014


PhotonicsJournal of


Journal of

Biophysics






2


120583flux and







Num

ber o

f eve

nts

0

20

40

60

80

100

120

140

160

180

200

ERcosΘR (GeV)0 20 40 60 80 100 120 140


6

5

4

3

2

1



Rate

(Hz)










Total simulation

IceCube preliminary


Ratio

120

115

110

105

100

095

090

085

08005 10 15 2520









2




23and Δ119898

2





















0

20

40

60

IceCube preliminary


cos(120579reco)


20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band


0

20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band


20

40

60

cos(120579reco)


0

20

40

60

cos(120579reco)


20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band


0

20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band


20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band

Even

ts pe

r ene

rgy

band

Even

ts pe

r ene

rgy

band

Even

ts pe

r ene

rgy

band




23= 053

+009


2

32=

272+019




23 and +014


for Δ1198982














Detector (far)




Neutrino flux


120583Accelerator ]

120583]120583modes



50

45

40

35

30

25

20

15

10060 065 070 075 080 085 090 095 100

sin2(212057923)

|Δm2 32|

(10minus3

eV2)









102

101

100

Even

ts


cos(120579reco)



102

101

100

Even

ts


cos(120579reco)



102

101

100

Even

ts


cos(120579reco)










800

600

400

200

0

101 102 103

LrecoEreco (kmGeV)

Even

ts


(a)

14

12

10

08

06

04101 102 103

LrecoEreco (kmGeV)

Ratio

to n

o os

c


(b)













120583






23 It is






90 CL contours

T2K 2014 [NH]SK IV 2015 [NH]

43210

38

36

34

32

30

28

26

24

22

20

|Δm2 32|

(10minus3

eV2)

38

36

34

32

30

28

26

24

22

20

|Δm2 32|

(10minus3

eV2)

minus2ΔlnL

minus2Δ

lnL

03 04 05 06 07 0 1 2 3 4

sin2(12057923)

03 04 05

(a)

(b) (c)

06 07

sin2(12057923)


2



Penetrator

PMT baseHV supply


Waist band

Pressure sphere


PMT photocathode








Penetrator

Top hemisphere

Pressure gauge

Nanobeacon


Cooling system (13)

Cooling system (23)


Cooling system (33)


Piezosensor

PMT and base


Valve




Bottom hemisphere







minus150

minus100

minus50

0

50

100


Preliminary

Y(m

)

X (m)

(a)

minus100

minus50

0

50

100



y(m

)

107m


(b)




PINGU 120583 + 120583ORCA 120583 + 120583

E (GeV)

040

035

025

030

020

015

010

005

0005 10 15 20 25 30

Med

ian

frac

tiona

l ene

rgy

reso

lutio

n




PINGU 120583 + 120583ORCA 120583ORCA 120583

20

15

10

5

05 10 15 20 25 30

E (GeV)

Med

ian

zeni

th an

gle r

es (∘ )







Mea

n nu

mbe

r of p

hoto

ns p

er D

OM 1

KM3NeT preliminary

07 lt y lt 08

05 lt y lt 06

02 lt y lt 03

00 lt y lt 01

Bjorken y



10minus2


10

08

06

04

02

002 4 6 8 10 12 14 16 18

E (GeV)

Frac

tion

class

ified

as tr

ack-

like


P e + eO e + eP 120583 + 120583O 120583O120583

P 120591 + 120591O 120591 + 120591P + (NC)O + (NC)


120583performs





12057923 Δ119898231



12057912 Δ119898221







23 Δ119898232 and 120579













23to





23 The




23and the






7

6

5

4

3

2

1

0040 045 050 055 060

sin212057923

120590(3

year

s)


PINGU NOORCA NO

PINGU IOORCA IO

(a)

45

40

35

30

25

20

15

100 1 2 3 4 5



PINGU NOORCA NO

PINGU IOORCA IO

NO 12057923 = 42∘

IO 12057923 = 49∘

Expe

cted

sens

itivi

ty (120590

)

(b)




23= 42∘ for a NMO 120579

23= 49∘ for an IMO) From [85 91]





6 Summary


23and |Δ1198982

32| Constant



2

31and completely


23) of




Acknowledgments


References

































































































































FluidsJournal of


Journal of










Superconductivity




GravityJournal of








Journal of






Volume 2014


PhotonicsJournal of


Journal of

Biophysics






Total simulation

IceCube preliminary


Ratio

120

115

110

105

100

095

090

085

08005 10 15 2520









2




23and Δ119898

2





















0

20

40

60

IceCube preliminary


cos(120579reco)


20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band


0

20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band


20

40

60

cos(120579reco)


0

20

40

60

cos(120579reco)


20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band


0

20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band


20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band

Even

ts pe

r ene

rgy

band

Even

ts pe

r ene

rgy

band

Even

ts pe

r ene

rgy

band




23= 053

+009


2

32=

272+019




23 and +014


for Δ1198982














Detector (far)




Neutrino flux


120583Accelerator ]

120583]120583modes



50

45

40

35

30

25

20

15

10060 065 070 075 080 085 090 095 100

sin2(212057923)

|Δm2 32|

(10minus3

eV2)









102

101

100

Even

ts


cos(120579reco)



102

101

100

Even

ts


cos(120579reco)



102

101

100

Even

ts


cos(120579reco)










800

600

400

200

0

101 102 103

LrecoEreco (kmGeV)

Even

ts


(a)

14

12

10

08

06

04101 102 103

LrecoEreco (kmGeV)

Ratio

to n

o os

c


(b)













120583






23 It is






90 CL contours

T2K 2014 [NH]SK IV 2015 [NH]

43210

38

36

34

32

30

28

26

24

22

20

|Δm2 32|

(10minus3

eV2)

38

36

34

32

30

28

26

24

22

20

|Δm2 32|

(10minus3

eV2)

minus2ΔlnL

minus2Δ

lnL

03 04 05 06 07 0 1 2 3 4

sin2(12057923)

03 04 05

(a)

(b) (c)

06 07

sin2(12057923)


2



Penetrator

PMT baseHV supply


Waist band

Pressure sphere


PMT photocathode








Penetrator

Top hemisphere

Pressure gauge

Nanobeacon


Cooling system (13)

Cooling system (23)


Cooling system (33)


Piezosensor

PMT and base


Valve




Bottom hemisphere







minus150

minus100

minus50

0

50

100


Preliminary

Y(m

)

X (m)

(a)

minus100

minus50

0

50

100



y(m

)

107m


(b)




PINGU 120583 + 120583ORCA 120583 + 120583

E (GeV)

040

035

025

030

020

015

010

005

0005 10 15 20 25 30

Med

ian

frac

tiona

l ene

rgy

reso

lutio

n




PINGU 120583 + 120583ORCA 120583ORCA 120583

20

15

10

5

05 10 15 20 25 30

E (GeV)

Med

ian

zeni

th an

gle r

es (∘ )







Mea

n nu

mbe

r of p

hoto

ns p

er D

OM 1

KM3NeT preliminary

07 lt y lt 08

05 lt y lt 06

02 lt y lt 03

00 lt y lt 01

Bjorken y



10minus2


10

08

06

04

02

002 4 6 8 10 12 14 16 18

E (GeV)

Frac

tion

class

ified

as tr

ack-

like


P e + eO e + eP 120583 + 120583O 120583O120583

P 120591 + 120591O 120591 + 120591P + (NC)O + (NC)


120583performs





12057923 Δ119898231



12057912 Δ119898221







23 Δ119898232 and 120579













23to





23 The




23and the






7

6

5

4

3

2

1

0040 045 050 055 060

sin212057923

120590(3

year

s)


PINGU NOORCA NO

PINGU IOORCA IO

(a)

45

40

35

30

25

20

15

100 1 2 3 4 5



PINGU NOORCA NO

PINGU IOORCA IO

NO 12057923 = 42∘

IO 12057923 = 49∘

Expe

cted

sens

itivi

ty (120590

)

(b)




23= 42∘ for a NMO 120579

23= 49∘ for an IMO) From [85 91]





6 Summary


23and |Δ1198982

32| Constant



2

31and completely


23) of




Acknowledgments


References

































































































































FluidsJournal of


Journal of










Superconductivity




GravityJournal of








Journal of






Volume 2014


PhotonicsJournal of


Journal of

Biophysics













0

20

40

60

IceCube preliminary


cos(120579reco)


20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band


0

20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band


20

40

60

cos(120579reco)


0

20

40

60

cos(120579reco)


20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band


0

20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band


20

40

60

cos(120579reco)

Even

ts pe

r ene

rgy

band

Even

ts pe

r ene

rgy

band

Even

ts pe

r ene

rgy

band

Even

ts pe

r ene

rgy

band




23= 053

+009


2

32=

272+019




23 and +014


for Δ1198982














Detector (far)




Neutrino flux


120583Accelerator ]

120583]120583modes



50

45

40

35

30

25

20

15

10060 065 070 075 080 085 090 095 100

sin2(212057923)

|Δm2 32|

(10minus3

eV2)









102

101

100

Even

ts


cos(120579reco)



102

101

100

Even

ts


cos(120579reco)



102

101

100

Even

ts


cos(120579reco)










800

600

400

200

0

101 102 103

LrecoEreco (kmGeV)

Even

ts


(a)

14

12

10

08

06

04101 102 103

LrecoEreco (kmGeV)

Ratio

to n

o os

c


(b)













120583






23 It is






90 CL contours

T2K 2014 [NH]SK IV 2015 [NH]

43210

38

36

34

32

30

28

26

24

22

20

|Δm2 32|

(10minus3

eV2)

38

36

34

32

30

28

26

24

22

20

|Δm2 32|

(10minus3

eV2)

minus2ΔlnL

minus2Δ

lnL

03 04 05 06 07 0 1 2 3 4

sin2(12057923)

03 04 05

(a)

(b) (c)

06 07

sin2(12057923)


2



Penetrator

PMT baseHV supply


Waist band

Pressure sphere


PMT photocathode








Penetrator

Top hemisphere

Pressure gauge

Nanobeacon


Cooling system (13)

Cooling system (23)


Cooling system (33)


Piezosensor

PMT and base


Valve




Bottom hemisphere







minus150

minus100

minus50

0

50

100


Preliminary

Y(m

)

X (m)

(a)

minus100

minus50

0

50

100



y(m

)

107m


(b)




PINGU 120583 + 120583ORCA 120583 + 120583

E (GeV)

040

035

025

030

020

015

010

005

0005 10 15 20 25 30

Med

ian

frac

tiona

l ene

rgy

reso

lutio

n




PINGU 120583 + 120583ORCA 120583ORCA 120583

20

15

10

5

05 10 15 20 25 30

E (GeV)

Med

ian

zeni

th an

gle r

es (∘ )







Mea

n nu

mbe

r of p

hoto

ns p

er D

OM 1

KM3NeT preliminary

07 lt y lt 08

05 lt y lt 06

02 lt y lt 03

00 lt y lt 01

Bjorken y



10minus2


10

08

06

04

02

002 4 6 8 10 12 14 16 18

E (GeV)

Frac

tion

class

ified

as tr

ack-

like


P e + eO e + eP 120583 + 120583O 120583O120583

P 120591 + 120591O 120591 + 120591P + (NC)O + (NC)


120583performs





12057923 Δ119898231



12057912 Δ119898221







23 Δ119898232 and 120579













23to





23 The




23and the






7

6

5

4

3

2

1

0040 045 050 055 060

sin212057923

120590(3

year

s)


PINGU NOORCA NO

PINGU IOORCA IO

(a)

45

40

35

30

25

20

15

100 1 2 3 4 5



PINGU NOORCA NO

PINGU IOORCA IO

NO 12057923 = 42∘

IO 12057923 = 49∘

Expe

cted

sens

itivi

ty (120590

)

(b)




23= 42∘ for a NMO 120579

23= 49∘ for an IMO) From [85 91]





6 Summary


23and |Δ1198982

32| Constant



2

31and completely


23) of




Acknowledgments


References

































































































































FluidsJournal of


Journal of










Superconductivity




GravityJournal of








Journal of






Volume 2014


PhotonicsJournal of


Journal of

Biophysics








Detector (far)




Neutrino flux


120583Accelerator ]

120583]120583modes



50

45

40

35

30

25

20

15

10060 065 070 075 080 085 090 095 100

sin2(212057923)

|Δm2 32|

(10minus3

eV2)









102

101

100

Even

ts


cos(120579reco)



102

101

100

Even

ts


cos(120579reco)



102

101

100

Even

ts


cos(120579reco)










800

600

400

200

0

101 102 103

LrecoEreco (kmGeV)

Even

ts


(a)

14

12

10

08

06

04101 102 103

LrecoEreco (kmGeV)

Ratio

to n

o os

c


(b)













120583






23 It is






90 CL contours

T2K 2014 [NH]SK IV 2015 [NH]

43210

38

36

34

32

30

28

26

24

22

20

|Δm2 32|

(10minus3

eV2)

38

36

34

32

30

28

26

24

22

20

|Δm2 32|

(10minus3

eV2)

minus2ΔlnL

minus2Δ

lnL

03 04 05 06 07 0 1 2 3 4

sin2(12057923)

03 04 05

(a)

(b) (c)

06 07

sin2(12057923)


2



Penetrator

PMT baseHV supply


Waist band

Pressure sphere


PMT photocathode








Penetrator

Top hemisphere

Pressure gauge

Nanobeacon


Cooling system (13)

Cooling system (23)


Cooling system (33)


Piezosensor

PMT and base


Valve




Bottom hemisphere







minus150

minus100

minus50

0

50

100


Preliminary

Y(m

)

X (m)

(a)

minus100

minus50

0

50

100



y(m

)

107m


(b)




PINGU 120583 + 120583ORCA 120583 + 120583

E (GeV)

040

035

025

030

020

015

010

005

0005 10 15 20 25 30

Med

ian

frac

tiona

l ene

rgy

reso

lutio

n




PINGU 120583 + 120583ORCA 120583ORCA 120583

20

15

10

5

05 10 15 20 25 30

E (GeV)

Med

ian

zeni

th an

gle r

es (∘ )







Mea

n nu

mbe

r of p

hoto

ns p

er D

OM 1

KM3NeT preliminary

07 lt y lt 08

05 lt y lt 06

02 lt y lt 03

00 lt y lt 01

Bjorken y



10minus2


10

08

06

04

02

002 4 6 8 10 12 14 16 18

E (GeV)

Frac

tion

class

ified

as tr

ack-

like


P e + eO e + eP 120583 + 120583O 120583O120583

P 120591 + 120591O 120591 + 120591P + (NC)O + (NC)


120583performs





12057923 Δ119898231



12057912 Δ119898221







23 Δ119898232 and 120579













23to





23 The




23and the






7

6

5

4

3

2

1

0040 045 050 055 060

sin212057923

120590(3

year

s)


PINGU NOORCA NO

PINGU IOORCA IO

(a)

45

40

35

30

25

20

15

100 1 2 3 4 5



PINGU NOORCA NO

PINGU IOORCA IO

NO 12057923 = 42∘

IO 12057923 = 49∘

Expe

cted

sens

itivi

ty (120590

)

(b)




23= 42∘ for a NMO 120579

23= 49∘ for an IMO) From [85 91]





6 Summary


23and |Δ1198982

32| Constant



2

31and completely


23) of




Acknowledgments


References

































































































































FluidsJournal of


Journal of










Superconductivity




GravityJournal of








Journal of






Volume 2014


PhotonicsJournal of


Journal of

Biophysics




102

101

100

Even

ts


cos(120579reco)



102

101

100

Even

ts


cos(120579reco)



102

101

100

Even

ts


cos(120579reco)










800

600

400

200

0

101 102 103

LrecoEreco (kmGeV)

Even

ts


(a)

14

12

10

08

06

04101 102 103

LrecoEreco (kmGeV)

Ratio

to n

o os

c


(b)













120583






23 It is






90 CL contours

T2K 2014 [NH]SK IV 2015 [NH]

43210

38

36

34

32

30

28

26

24

22

20

|Δm2 32|

(10minus3

eV2)

38

36

34

32

30

28

26

24

22

20

|Δm2 32|

(10minus3

eV2)

minus2ΔlnL

minus2Δ

lnL

03 04 05 06 07 0 1 2 3 4

sin2(12057923)

03 04 05

(a)

(b) (c)

06 07

sin2(12057923)


2



Penetrator

PMT baseHV supply


Waist band

Pressure sphere


PMT photocathode








Penetrator

Top hemisphere

Pressure gauge

Nanobeacon


Cooling system (13)

Cooling system (23)


Cooling system (33)


Piezosensor

PMT and base


Valve




Bottom hemisphere







minus150

minus100

minus50

0

50

100


Preliminary

Y(m

)

X (m)

(a)

minus100

minus50

0

50

100



y(m

)

107m


(b)




PINGU 120583 + 120583ORCA 120583 + 120583

E (GeV)

040

035

025

030

020

015

010

005

0005 10 15 20 25 30

Med

ian

frac

tiona

l ene

rgy

reso

lutio

n




PINGU 120583 + 120583ORCA 120583ORCA 120583

20

15

10

5

05 10 15 20 25 30

E (GeV)

Med

ian

zeni

th an

gle r

es (∘ )







Mea

n nu

mbe

r of p

hoto

ns p

er D

OM 1

KM3NeT preliminary

07 lt y lt 08

05 lt y lt 06

02 lt y lt 03

00 lt y lt 01

Bjorken y



10minus2


10

08

06

04

02

002 4 6 8 10 12 14 16 18

E (GeV)

Frac

tion

class

ified

as tr

ack-

like


P e + eO e + eP 120583 + 120583O 120583O120583

P 120591 + 120591O 120591 + 120591P + (NC)O + (NC)


120583performs





12057923 Δ119898231



12057912 Δ119898221







23 Δ119898232 and 120579













23to





23 The




23and the






7

6

5

4

3

2

1

0040 045 050 055 060

sin212057923

120590(3

year

s)


PINGU NOORCA NO

PINGU IOORCA IO

(a)

45

40

35

30

25

20

15

100 1 2 3 4 5



PINGU NOORCA NO

PINGU IOORCA IO

NO 12057923 = 42∘

IO 12057923 = 49∘

Expe

cted

sens

itivi

ty (120590

)

(b)




23= 42∘ for a NMO 120579

23= 49∘ for an IMO) From [85 91]





6 Summary


23and |Δ1198982

32| Constant



2

31and completely


23) of




Acknowledgments


References

































































































































FluidsJournal of


Journal of










Superconductivity




GravityJournal of








Journal of






Volume 2014


PhotonicsJournal of


Journal of

Biophysics




800

600

400

200

0

101 102 103

LrecoEreco (kmGeV)

Even

ts


(a)

14

12

10

08

06

04101 102 103

LrecoEreco (kmGeV)

Ratio

to n

o os

c


(b)













120583






23 It is






90 CL contours

T2K 2014 [NH]SK IV 2015 [NH]

43210

38

36

34

32

30

28

26

24

22

20

|Δm2 32|

(10minus3

eV2)

38

36

34

32

30

28

26

24

22

20

|Δm2 32|

(10minus3

eV2)

minus2ΔlnL

minus2Δ

lnL

03 04 05 06 07 0 1 2 3 4

sin2(12057923)

03 04 05

(a)

(b) (c)

06 07

sin2(12057923)


2



Penetrator

PMT baseHV supply


Waist band

Pressure sphere


PMT photocathode








Penetrator

Top hemisphere

Pressure gauge

Nanobeacon


Cooling system (13)

Cooling system (23)


Cooling system (33)


Piezosensor

PMT and base


Valve




Bottom hemisphere







minus150

minus100

minus50

0

50

100


Preliminary

Y(m

)

X (m)

(a)

minus100

minus50

0

50

100



y(m

)

107m


(b)




PINGU 120583 + 120583ORCA 120583 + 120583

E (GeV)

040

035

025

030

020

015

010

005

0005 10 15 20 25 30

Med

ian

frac

tiona

l ene

rgy

reso

lutio

n




PINGU 120583 + 120583ORCA 120583ORCA 120583

20

15

10

5

05 10 15 20 25 30

E (GeV)

Med

ian

zeni

th an

gle r

es (∘ )







Mea

n nu

mbe

r of p

hoto

ns p

er D

OM 1

KM3NeT preliminary

07 lt y lt 08

05 lt y lt 06

02 lt y lt 03

00 lt y lt 01

Bjorken y



10minus2


10

08

06

04

02

002 4 6 8 10 12 14 16 18

E (GeV)

Frac

tion

class

ified

as tr

ack-

like


P e + eO e + eP 120583 + 120583O 120583O120583

P 120591 + 120591O 120591 + 120591P + (NC)O + (NC)


120583performs





12057923 Δ119898231



12057912 Δ119898221







23 Δ119898232 and 120579













23to





23 The




23and the






7

6

5

4

3

2

1

0040 045 050 055 060

sin212057923

120590(3

year

s)


PINGU NOORCA NO

PINGU IOORCA IO

(a)

45

40

35

30

25

20

15

100 1 2 3 4 5



PINGU NOORCA NO

PINGU IOORCA IO

NO 12057923 = 42∘

IO 12057923 = 49∘

Expe

cted

sens

itivi

ty (120590

)

(b)




23= 42∘ for a NMO 120579

23= 49∘ for an IMO) From [85 91]





6 Summary


23and |Δ1198982

32| Constant



2

31and completely


23) of




Acknowledgments


References

































































































































FluidsJournal of


Journal of










Superconductivity




GravityJournal of








Journal of






Volume 2014


PhotonicsJournal of


Journal of

Biophysics





90 CL contours

T2K 2014 [NH]SK IV 2015 [NH]

43210

38

36

34

32

30

28

26

24

22

20

|Δm2 32|

(10minus3

eV2)

38

36

34

32

30

28

26

24

22

20

|Δm2 32|

(10minus3

eV2)

minus2ΔlnL

minus2Δ

lnL

03 04 05 06 07 0 1 2 3 4

sin2(12057923)

03 04 05

(a)

(b) (c)

06 07

sin2(12057923)


2



Penetrator

PMT baseHV supply


Waist band

Pressure sphere


PMT photocathode








Penetrator

Top hemisphere

Pressure gauge

Nanobeacon


Cooling system (13)

Cooling system (23)


Cooling system (33)


Piezosensor

PMT and base


Valve




Bottom hemisphere







minus150

minus100

minus50

0

50

100


Preliminary

Y(m

)

X (m)

(a)

minus100

minus50

0

50

100



y(m

)

107m


(b)




PINGU 120583 + 120583ORCA 120583 + 120583

E (GeV)

040

035

025

030

020

015

010

005

0005 10 15 20 25 30

Med

ian

frac

tiona

l ene

rgy

reso

lutio

n




PINGU 120583 + 120583ORCA 120583ORCA 120583

20

15

10

5

05 10 15 20 25 30

E (GeV)

Med

ian

zeni

th an

gle r

es (∘ )







Mea

n nu

mbe

r of p

hoto

ns p

er D

OM 1

KM3NeT preliminary

07 lt y lt 08

05 lt y lt 06

02 lt y lt 03

00 lt y lt 01

Bjorken y



10minus2


10

08

06

04

02

002 4 6 8 10 12 14 16 18

E (GeV)

Frac

tion

class

ified

as tr

ack-

like


P e + eO e + eP 120583 + 120583O 120583O120583

P 120591 + 120591O 120591 + 120591P + (NC)O + (NC)


120583performs





12057923 Δ119898231



12057912 Δ119898221







23 Δ119898232 and 120579













23to





23 The




23and the






7

6

5

4

3

2

1

0040 045 050 055 060

sin212057923

120590(3

year

s)


PINGU NOORCA NO

PINGU IOORCA IO

(a)

45

40

35

30

25

20

15

100 1 2 3 4 5



PINGU NOORCA NO

PINGU IOORCA IO

NO 12057923 = 42∘

IO 12057923 = 49∘

Expe

cted

sens

itivi

ty (120590

)

(b)




23= 42∘ for a NMO 120579

23= 49∘ for an IMO) From [85 91]





6 Summary


23and |Δ1198982

32| Constant



2

31and completely


23) of




Acknowledgments


References

































































































































FluidsJournal of


Journal of










Superconductivity




GravityJournal of








Journal of






Volume 2014


PhotonicsJournal of


Journal of

Biophysics




Penetrator

Top hemisphere

Pressure gauge

Nanobeacon


Cooling system (13)

Cooling system (23)


Cooling system (33)


Piezosensor

PMT and base


Valve




Bottom hemisphere







minus150

minus100

minus50

0

50

100


Preliminary

Y(m

)

X (m)

(a)

minus100

minus50

0

50

100



y(m

)

107m


(b)




PINGU 120583 + 120583ORCA 120583 + 120583

E (GeV)

040

035

025

030

020

015

010

005

0005 10 15 20 25 30

Med

ian

frac

tiona

l ene

rgy

reso

lutio

n




PINGU 120583 + 120583ORCA 120583ORCA 120583

20

15

10

5

05 10 15 20 25 30

E (GeV)

Med

ian

zeni

th an

gle r

es (∘ )







Mea

n nu

mbe

r of p

hoto

ns p

er D

OM 1

KM3NeT preliminary

07 lt y lt 08

05 lt y lt 06

02 lt y lt 03

00 lt y lt 01

Bjorken y



10minus2


10

08

06

04

02

002 4 6 8 10 12 14 16 18

E (GeV)

Frac

tion

class

ified

as tr

ack-

like


P e + eO e + eP 120583 + 120583O 120583O120583

P 120591 + 120591O 120591 + 120591P + (NC)O + (NC)


120583performs





12057923 Δ119898231



12057912 Δ119898221







23 Δ119898232 and 120579













23to





23 The




23and the






7

6

5

4

3

2

1

0040 045 050 055 060

sin212057923

120590(3

year

s)


PINGU NOORCA NO

PINGU IOORCA IO

(a)

45

40

35

30

25

20

15

100 1 2 3 4 5



PINGU NOORCA NO

PINGU IOORCA IO

NO 12057923 = 42∘

IO 12057923 = 49∘

Expe

cted

sens

itivi

ty (120590

)

(b)




23= 42∘ for a NMO 120579

23= 49∘ for an IMO) From [85 91]





6 Summary


23and |Δ1198982

32| Constant



2

31and completely


23) of




Acknowledgments


References

































































































































FluidsJournal of


Journal of










Superconductivity




GravityJournal of








Journal of






Volume 2014


PhotonicsJournal of


Journal of

Biophysics





minus150

minus100

minus50

0

50

100


Preliminary

Y(m

)

X (m)

(a)

minus100

minus50

0

50

100



y(m

)

107m


(b)




PINGU 120583 + 120583ORCA 120583 + 120583

E (GeV)

040

035

025

030

020

015

010

005

0005 10 15 20 25 30

Med

ian

frac

tiona

l ene

rgy

reso

lutio

n




PINGU 120583 + 120583ORCA 120583ORCA 120583

20

15

10

5

05 10 15 20 25 30

E (GeV)

Med

ian

zeni

th an

gle r

es (∘ )







Mea

n nu

mbe

r of p

hoto

ns p

er D

OM 1

KM3NeT preliminary

07 lt y lt 08

05 lt y lt 06

02 lt y lt 03

00 lt y lt 01

Bjorken y



10minus2


10

08

06

04

02

002 4 6 8 10 12 14 16 18

E (GeV)

Frac

tion

class

ified

as tr

ack-

like


P e + eO e + eP 120583 + 120583O 120583O120583

P 120591 + 120591O 120591 + 120591P + (NC)O + (NC)


120583performs





12057923 Δ119898231



12057912 Δ119898221







23 Δ119898232 and 120579













23to





23 The




23and the






7

6

5

4

3

2

1

0040 045 050 055 060

sin212057923

120590(3

year

s)


PINGU NOORCA NO

PINGU IOORCA IO

(a)

45

40

35

30

25

20

15

100 1 2 3 4 5



PINGU NOORCA NO

PINGU IOORCA IO

NO 12057923 = 42∘

IO 12057923 = 49∘

Expe

cted

sens

itivi

ty (120590

)

(b)




23= 42∘ for a NMO 120579

23= 49∘ for an IMO) From [85 91]





6 Summary


23and |Δ1198982

32| Constant



2

31and completely


23) of




Acknowledgments


References

































































































































FluidsJournal of


Journal of










Superconductivity




GravityJournal of








Journal of






Volume 2014


PhotonicsJournal of


Journal of

Biophysics





Mea

n nu

mbe

r of p

hoto

ns p

er D

OM 1

KM3NeT preliminary

07 lt y lt 08

05 lt y lt 06

02 lt y lt 03

00 lt y lt 01

Bjorken y



10minus2


10

08

06

04

02

002 4 6 8 10 12 14 16 18

E (GeV)

Frac

tion

class

ified

as tr

ack-

like


P e + eO e + eP 120583 + 120583O 120583O120583

P 120591 + 120591O 120591 + 120591P + (NC)O + (NC)


120583performs





12057923 Δ119898231



12057912 Δ119898221







23 Δ119898232 and 120579













23to





23 The




23and the






7

6

5

4

3

2

1

0040 045 050 055 060

sin212057923

120590(3

year

s)


PINGU NOORCA NO

PINGU IOORCA IO

(a)

45

40

35

30

25

20

15

100 1 2 3 4 5



PINGU NOORCA NO

PINGU IOORCA IO

NO 12057923 = 42∘

IO 12057923 = 49∘

Expe

cted

sens

itivi

ty (120590

)

(b)




23= 42∘ for a NMO 120579

23= 49∘ for an IMO) From [85 91]





6 Summary


23and |Δ1198982

32| Constant



2

31and completely


23) of




Acknowledgments


References

































































































































FluidsJournal of


Journal of










Superconductivity




GravityJournal of








Journal of






Volume 2014


PhotonicsJournal of


Journal of

Biophysics











23to





23 The




23and the






7

6

5

4

3

2

1

0040 045 050 055 060

sin212057923

120590(3

year

s)


PINGU NOORCA NO

PINGU IOORCA IO

(a)

45

40

35

30

25

20

15

100 1 2 3 4 5



PINGU NOORCA NO

PINGU IOORCA IO

NO 12057923 = 42∘

IO 12057923 = 49∘

Expe

cted

sens

itivi

ty (120590

)

(b)




23= 42∘ for a NMO 120579

23= 49∘ for an IMO) From [85 91]





6 Summary


23and |Δ1198982

32| Constant



2

31and completely


23) of




Acknowledgments


References

































































































































FluidsJournal of


Journal of










Superconductivity




GravityJournal of








Journal of






Volume 2014


PhotonicsJournal of


Journal of

Biophysics





6 Summary


23and |Δ1198982

32| Constant



2

31and completely


23) of




Acknowledgments


References

































































































































FluidsJournal of


Journal of










Superconductivity




GravityJournal of








Journal of






Volume 2014


PhotonicsJournal of


Journal of

Biophysics









































































































FluidsJournal of


Journal of










Superconductivity




GravityJournal of








Journal of






Volume 2014


PhotonicsJournal of


Journal of

Biophysics



review article measurement of atmospheric neutrino...

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