John Beacom, The Ohio State University · Many surprised; Laha+ (2013) demystified and showed...

JohnBeacom,TheOhioStateUniversity BaryonandLeptonNumberViolation,CaseWestern,May2017

TestingNewPhysicsWithNeutrinoAstrophysics

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JohnBeacom,TheOhioStateUniversity

JohnBeacom,TheOhioStateUniversity BaryonandLeptonNumberViolation,CaseWestern,May2017 2

PlanoftheTalk

Neutrinoastronomy— whytry?

WhatisIceCube?WhathasIceCube discovered?

Whatdoesitmeanforparticlephysics?

Concludingperspectives


NeutrinoAstronomy—WhyTry?


FirstGoal:NewAstrophysics

Whathappensdeepinsideastrophysicalsystems?Useknowledgeofsubatomicphysics…listentotheorists

Examplesuccesses:solarandsupernovaneutrinosExamplesearches:GRBneutrinos;CRsourcesinMW

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SecondGoal:NewParticlePhysics

Examplesuccesses:numberofflavors;neutrinomassissmallExamplesearches:neutrinoexotica;darkmatter

Whatarethepropertiesoffamiliarandofunmetparticles?Useknowledgeofastrophysics…listentotheorists

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ThirdGoal:NewSurprises

Examplesuccesses:neutrinomixing;cosmicrayanisotropiesExamplesearches:unknownunknowns!

Whathaven’twethoughtof?Developflexible,powerfulsearches…don’tlistentotheorists

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WhatisIceCube?


TheLocation


TheConstruction


TheDesign

Needs86stringsofPMTsburiedin1km3 ofclearice


TheDetectionPrinciples

ve + n→ e− + pvτ + n→ τ − + p

Cascade(shower)eventsFewminlengthSeeBeacomandCandia(2004)

e.g.,vµ + n→ µ− + p

TrackeventsFewkminlengthPlannedfocusofIceCube

e.g.,


FirstDifficulty:BeseechingNature

Requires:sourcesthatreachhighenergiessourcesthatareluminoussourcesofdifferenttypesparticlesthatcanreachusparticlesthatcanpointbackparticlesthatcanbedetectedresultsthatcanbeunderstood Ourpart

eV keV MeV GeV TeV PeV EeV ZeV

atomic nuclear accelerator ?????????????????????????

106 eV 1012 eV 1018 eV


Nevents ~ 4p . Ntargets s . T . F ~ 4p . Aeffective . T . F

Volume~ 1km3 Aeffective ~ 1m2 at100TeV

Formanysources,~ 1km3 istheminimumrequired

SecondDifficulty:MeasuringSignals


ThirdDifficulty:RejectingBackgroundsAtmosphericmuons:enormousbutgreatlyreduciblebackground

Atmosphericneutrinos:bigbutreducible(Schonert+2008)foreground

[GeV]ν E10

log2 3 4 5 6 7 8 9 10

-1 s

r-1

s-2

GeV

cm

ν/d

Eν

dN

ν2 E

-910

-810

-710

-610

-510

-410

-310

1387 dµνAMANDA-II Atmospheric Bartol + Naumov RQPM

unfolding (2000-2003)µνAMANDA-II Honda + Enberg Min

807 dµνAMANDA-II Waxman Bahcall Prompt GRB

07-09µνANTARES Blazars Stecker

µνIC40 Atmospheric Waxman Bahcall 1998 x 1/2

UnfoldingµνIC40 Atmo. Becker AGN

375.5 dµνIC40 Mannheim AGNs

1)2)3)4)5)6)7)

(10

(8(9

(11(12

(13(14

1

5

14

12

6 23

4

7

10 89

13

11

IceCube 2011:

Atm.numeasuredupto~ 200TeV

Astro.nustronglimitsathigherenergies


WhathasIceCube Discovered?


ThePevatrons Uncloak

2011: ~ 1 PeV cascade 2012: ~ 1 PeV cascade

Greatfortuneinfindingtheseeventsinthissearch(2013)

Manysurprised;Laha+(2013)demystifiedandshowedtests


NowComestheFlood

-80

-60

-40

-20

0

20

40

60

80

102 103

Decl

inatio

n (

degre

es)

Deposited EM-Equivalent Energy in Detector (TeV)

ShowersTracks

2014IceCube TeV-PeV search,using2010—2013data

Conservativeanalysis:37candidates,~ 15background,5.7s

Myopinion:focusabove100TeV on“CleanDozen”eventswithnegligibleatmosphericbackgrounds


WhatDoestheEnergySpectrumTellUs?Sumofcascade(allflavors),startingtrack(muon)channels

Truesignificanceismuch higherthanreported

Easytosee(!):astrophysicalneutrinoswithspectrum~ E-2

For“CleanDozen”events,ignorethebackgroundsshownbecausecascadechanneldominates


WhatDoestheAngularDistributionTellUs?FirstHEneutrinoskymap;somecaveatsforinterpretation

Easytosee(!):sourcesmostlyisotropic,extragalactic

Isolating“CleanDozen”changespicture

Onlytrack


Certainties,Probabilities,MysteriesSignalorigin:definitelyobservedextraterrestrialneutrinos

likelynoUHE,Galactic,orexoticsources

Energyspectrum:E2F ~ 10^-8GeV cm-2s-1 sr-1shapeE^-2withcutofforabitsteeper

Angulardistribution: likelyisotropicwithEarthattenuationnoobviousclusteringorcorrelations

Flavorratios:maybeconsistentwith1:1:1,butalittleweirdwherearethemuon tracksathighenergy?

Timedistribution:appearstobeconstant,notbursty


WhatDoesitMeanforParticlePhysics?


DarkMatterAnnihilationDMlikelyshouldannihilatewithapredictedcrosssection

natural scale – expectation for DM as thermal relic

νν

νν

Super-K

IceCube

νν W+W-

bb

Fermi (γ)

µ+µ-

P.Mijakowski,Super-Kpreliminary2012

FirstuseofneutrinostoprobehaloDMbyBeacom+(2006)

IceCube 2014


DarkMatterDecayDMmaydecay(slowly),butthereisnopredictedlifetime

ExcitementthatDMdecaymayexplainGalacticCenterpeakandspectrumdipFeldstein+(2013);Esmaili+(2013);Bai+(2013);Ema+(2014);Bhattacharya+(2014)

Re-examinationisneededusingnewIceCube data,carewithotherneutrino,gamma-raycascadelimitsMurase,Beacom(2012);Ibarra+(2013)


SpectrumDistortionsfromSecretInteractions

0

0.5

1

1 PeV line w/ SFRw/ regeneration

w/o regeneration

Eres = 5 PeV

0

0.5

1

Eres = 0.5 PeV

0

0.5

1

103

104

105

106

E2J

[10

-8 G

eV c

m-2

s-1

sr-1

]

E [ GeV ]

Eres = 0.05 PeV E2J

[10

-8 G

eV c

m-2

s-1

sr-1

]

E [ GeV ]

no-interactionModel AModel BModel CModel D

0

1

2

103

104

105

106

107

108

Linespectruminjection Continuumspectruminjection

Newtest:n+nà n+n (Ng,Beacom2014;Ioka,Murase 2014;Cherry+2014)

Mustincludeattenuation,regeneration,multiplescattering

Ng,Beacom(2014) Ng,Beacom(2014)


ParameterSpaceforSecretInteractionsg

M [ MeV ]

10-3

10-2

10-1

100

10-2

10-1

100

101

102

103

104

105

Non-perturbative regime

gατ

gαµ

gαe

SN1987A

BB

N

CMB

Z-decay

G=10-5

GeV-2

G=10+1

GeV-2

G=10+7

GeV-2

τ(1 P

eV)=

1

τ(0.1

PeV

)=1

τ(0.0

1 PeV

)=1 A

BC

D

Ng,Beacom(2014)

Musttakecaretoseparatemass,couplingofnewmediator

IceCube sensitivityiscomplementarytootherconstraints


FlavorCompositionofMassEigenstates

Bustamante,Beacom,Winter(2015,PRL)

Neutrinomixinganglesarealllarge,wellknown

(andsimilarforbothhierarchies)


FlavorRatios– NoNewPhysics

Fornonewneutrinophysicsbeyondstandardmixing:

ThefullspaceofflavorratiosatEarthistightlyrestrictedforallinitialratios

Bustamante,Beacom,Winter(2015,PRL)


FlavorRatios– BroadClassofNewPhysics

Fornewneutrinophysicsthatonlyincoherentlymixesmasseigenstates:

ThefullspaceofflavorratiosatEarthisalso tightlyrestrictedforallinitialratiosBustamante,Beacom,Winter(2015,PRL)


FlavorRatios– AllPossibilitiesofNewPhysics

Arguelles,Katori,Salvado(2015,PRL)

Tofilltheremainderofthespace,thenewphysicsmustpreservecoherenceand/orchangethemixingparameters


ConcludingPerspectives


TheTimeforNeutrinoAstronomyisNow

NeutrinoAstronomy

MeV—GeVn

Efforts:HKandmore

Targets:Solar,SN,moreSurprises

TeV—PeV n

Efforts:IceCube andmore

Targets:GRBs,AGN,moreSurprises

EeV—ZeV n

Efforts:ANITAandmore

Targets:GZKprocessSurprises

Neutrinoastronomymustbebroad


TheTimeforNeutrinoScienceisNow

NeutrinoScience

Laboratoryn

Efforts:Fermilab andmore

Context:PrecisionPhysics,BSMreach

Cosmology n

Efforts:CMBandmore

Context:PrecisionCosmology,BSMreach

Astronomyn

Efforts:IceCube andmore

Context:TransientAstronomy,Multi-messenger

Neutrinosaremulti-frontierscience


TeVPA 2017

tevpa2017.osu.edu

I August 7–11, Columbus, OH

I Registration and abstractsubmission are open

I Pre-meeting mini-workshopson Sunday, August 7


CenterforCosmologyandAstroParticle Physics

Columbus,Ohio:1 millionpeople(city),2millionpeople(city+metro)OhioStateUniversity:56,000studentsPhysics: 55faculty,Astronomy: 20facultyCCAPP: 20faculty,10postdocsfrombothdepartmentsPlacements:In2014alone,12CCAPPalumnigotpermanent-trackjobs

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Recentfacultyhires:AntonioBoveia,LindaCarpenter,ChrisHirata,AdamLeroy,LauraLopez,AnnikaPeterRecentpostdochires: AmiChoi,AlexiaLewis,NiallMacCrann,Tuguldur Sukhbold,MichaelTroxel,YingZu,FrancescoCapozzi

ccapp.osu.edu

John Beacom, The Ohio State University · Many surprised; Laha+ (2013) demystified and showed...

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