( ( ( ( ( Cosmic(rays( Photons( Neutrinos( Only(ν(propagate( freely(through( the(cosmos( Multi-messenger astronomy
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1 Lezioni 19 e 20 The IceCube Detector Motivation o Neutrinos: a new probe of the High Energy Universe Neutrino properties and how to detect them Construction of IceCube o Optical Modules, Ice Properties o The surface detector: IceTop o The pointing capability (Moon observation ) Evidence for astrophysical neutrinos at high energy Significance, implications, the Cosmic-Ray connection Cosmic Ray anisotropy: results from IceCube and other experiment in the Northern hemisphere Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 1
2 Cosmic(rays( Photons( Neutrinos( Only(ν(propagate( freely(through( the(cosmos( Multi-messenger astronomy ( ( ( ( ( Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 2
3 Cosmic ray neutrino connection Cosmic(rays(are(accelerated(( in#galac(c#sources#such#as#supernova#remnants# In#extragalac(c#sources#such#as#ac(ve#galaxies#and# gamma6ray#bursts# Cosmic(ray(sources(produce(γ8rays(in(two(ways( From#radia(on#by#accelerated#electrons# From#decay#of#π 0 #produced#by#interac(ons#of#accelerated# cosmic6ray#protons#or#nuclei#with#gas#or#photons# High(energy(ν are(produced(only(in(hadronic(collisions:( From#decay#of#π/K#produced#when#cosmic#rays#interact# with#gas#in#or#near#their#sources# Or#from#photo6pion#produc(on#on#CMB#or#EBL # Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 3
4 Implications of astrophysical neutrinos Observa9ons(of(γ rays(are(oten(ambiguous( Electrons#radiate#efficiently#and#usually#explain#the# observa(ons# Signatures#of#hadronic#origin#of#photons#are#difficult# to#iden(fy#and#prove# Neutrinos(have(a(unique(implica9on( Observa(on#of#high#energy#extraterrestrial#ν requires#a#hadronic#origin# Neutrinos#can#emerge#from#deep#inside#a#compact# source#without#degrada(on#by#electromagne(c# cascading# Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 4
5 Cosmic Rays Energies and rates of the cosmic-ray particles Energy(content(of(CR( determines(possible( sources(of(neutrinos( Extra8galac9c(origin(is(likely( Loca9on(of(transi9on(from( galac9c(to(extra8galac9c( affects(energy(es9mate( E 2 dn/de (GeV cm -2 sr -1 s -1 ) 10 0 protons only electrons positrons antiprotons Grigorov Akeno MSU KASCADE Tibet KASCADE-Grande IceTop73 all-particle HiRes1&2 TA2013 Auger2013 Model H4a CREAM all particle Galactic E dn d ln E (at GeV (10 19 ev) GeV cm 2 srs 10-8 Fixed target HERA RHIC TEVATRON LHC Extra-Galactic E (GeV / particle) Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 5
6 and neutrinos Φ ν dn de 1 E Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 6
7 ( ( ( ( Detecting neutrinos in H 2 O Proposed#by#Greisen,#Reines,#Markov#in#1960# ( (DUMAND( (IMB( (Kamiokande( Baikal( AMANDA( Super8K( SNO( IceCube' ANTARES( Neutrino'must'interact' 'to'be'detected' Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 7
8 A'36D'cosmic6ray'detector:' Two different kinds of events Closely related scientifically: Cosmic rays after propagation Neutrinos from cosmic ray sources ν e :ν µ :ν τ = 1:2:0! 1:1:1 Cosmic(ray(showers(from( above( South(Pole( (2835(m.a.s.l.( IceTop Neutrinos(from(all(direc9ons( #ν µ 6induced#µ#(from#below)# #all#flavors#star(ng#inside#detector# 1450 m IceCube ( 2450 m Atmospheric(muons( Roma,(28/01/2014( Tom(Gaisser( 8( Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 8
9 Deployment*history* 2002:'proposal' 'staging' ''''1'''''4' ''''9'''16' ''22'''26' ''40'''40' ''59'''59' ''79'''73' '''86'''81( Deep(strings( Surface(sta9ons( Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 9
10 south pole 2000 AMANDA South Pole Dome 1500 m 2000 m [not to scale] Amundsen-Scott south pole station Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 10
11 The South Pole n telescope: ICECUBE equipment on the surface Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 11
12 The South Pole n telescope: ICECUBE equipment on the surface The(drill(heaHng(plant IceCube(Site Thermal(power:(5(MW Pressure:(140(bar Flow:(800(L/m((90 C) 24(h(to(drill(to(2500m Most(importantly: (an(excellent(crew(of(drillers! Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 12 11
13 IceCube Digital Optical Module and deployment ( LED'Flasher'board' HV'board' Main'board'for'digiLzing'&'Lme'stamping' Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 13
14 architecture of independent DOMs 10 inch pmt LED flasher board main board HV board Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 14
15 each Digital Optical Module independently collects light signals like this, digitizes them, time stamps them with 2 nanoseconds precision, and sends them to a computer that sorts them events Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 15
16 DOMs during construction Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 16
17 Roma,(28/01/2014( Tom(Gaisser( 13( Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 17
18 IceCube IceTop: dimensions Example... 5(μs( Tom(Gaisser( Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 18
19 Properties of ice vary with depth Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 19
20 Ice Properties ( ( IceCube,(NIM(A(711,(73,(2013( charge on near and far strings [ p.e. ] DOM number on string 63 Figure 6: Charge collected by DOMs on the six nearest strings ( m away, triangles) and six next-to-nearest strings ( m away, circles), observed when flashing at the same position on string 63. eff. scattering b e (400 nm) [ m -1 ] absorption a(400 nm) [ m -1 ] 0.2 SPICE MIE AHA depth [ m ] 0.05 SPICE MIE AHA λ e (400 nm) [ m ] λ a (400 nm) [ m ] depth [ m ] Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 20
21 Primary spectrum from IceTop Phys.(Rev.(D(88,(042004((2013).((( sr -1 s -1 ] m [GeV dn de da d dt 2.7 E 4 10 IceTop 73, SIBYLL 2.1, H4a composition assumption KASCADE-Grande, SIBYLL 2.1 KASCADE, SIBYLL 2.1 GAMMA 2008 Tunka-133 Tibet III, SIBYLL log (E/GeV) ( (10 8( GeV(sets(normaliza9on(for(PeV(ν$ Directly(for(background(atmospheric(ν(( At(sources(for(astrophysical(ν( 10 7 ( (10 9( GeV:(transi9on(from(galac9c(to(extragalac9c(( Model(dependent( ( ( ( ( ( Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 21
22 Neutrino Interactions - 1 Charged(current(ν µ :( ν µ µ Force(carrier( q Also charged current ν e e and charged current ν τ τ and neutral current ν α ν α Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 22
23 Neutrino Interactions - 2 Tracks( (because(of(µ)( ν µ µ Force(carrier( q Cascades( Also charged current ν e e and charged current ν τ τ and neutral current ν α ν α Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 23
24 IceCube Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 24
25 IceCube Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 25
26 Upward neutrinos in IceCube be( S.P.( Cross sections proton-nucleon cross section (cm -2 ) E (GeV) neutrino-nucleon E Ν GeV Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 26 Nup Ndown Ν e Ν e Passing(frac9on( P.(Lipari,( ( Frac9on(absorbed( r( 21(
27 IceCube Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 27
28 IceCube: check of track angular reconstruction capability Moon(Shadow(of(Cosmic(Rays(using(muons in(the(icecube(detector Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 28
29 IceCube: use the Moon to check the track angular reconstruction Moon(shadow(observed(in(muons( Check(on(IceCube(poinHng Center(of(moon(is(spot(on( to(a(precision(of(<0.1(degrees.( Sta>s>cal&significance&with& IC&59:&&>&10&sigma Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 29
30 IceCube, as an example: search for neutrinos from Galactic Sources - 1 galactic plane in 10 TeV gamma rays : supernova remnants in star forming regions Southern Hemisphere Sky Standard(DeviaHons Milagro il Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics
31 IceCube, as an example: search for neutrinos from Galactic Sources - 2 cygnus region : Milagro Milagro translahon(of TeV(gamma(rays into TeV(neutrinos 3(±(1(ν per(year(in(icecube(per(source Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 31
32 IceCube, as an example: search for neutrinos from Galactic Sources - 3 5σ(in(5(years(of(IceCube IceCube(image(of(our Galaxy(>(10(TeV 3σ 5σ time in years M.(C.(Gonzalez[Garcia,(F.(Halzen,(and(S.(Mohapatra,(Astropart.(Phys.(31,(437(2009;(e[print arxiv: Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 32
33 Upward neutrinos in IceCube Must(have(low(enough(energy(to(get(through( the(earth((depends(on(direc9on)( Must(produce(a(signal(in(the(detector((((((( ν µ a. (((((( (induced(muon(from(neutrino(interac9on(in( the(rock(or(ice(below(the(detector((highest(rate)( b. Neutrino(of(any(flavor(interacts(inside(detector( 1kmice= = nucleons/cm 2 σ ν cm 2 at 10 5 GeV Product( (10 85 (is(frac9on(of(ν(of(this(energy(that(interact(in(detector( ( ( ( ( ( Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 33
34 energy measurement ( > 1 TeV ) convert the amount of light emitted to measurement of the muon energy (number of optical modules, number of photons, de/dx, ) Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 34
35 Neutrino Events (ν8induced(µ( entering(from( below( PeV(=(10 6 (GeV(=(10 15 (ev.((these(are(the(highest(energy(neutrinos(ever(detected!( Two(PeV(cascades( star9ng(inside(the( detector(( PRL#111,#021103#(2013)' Large(energy(!(atmospheric( origin(unlikely(( 20( 14( ( ( ( ( ( Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 35
36 Starting n µ à µ events ((((((((((((((((( ( Event(starts(in(fiducial(volume( Light(from(vertex(spreads( spherically(with(v=c/1.31( Muon(moves(ahead(with(v(=(c( ID(confirma9on(by(9ming( Jakob(van(Santen( Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 36
37 ( / / ( ( ( Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 37
38 Most events are not astrophysical neutrinos!!! 2.5(kHz( Astrophysical(ν( ~(1(per(million( ~(1(per(billion( Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 38
39 Search strategy for astrophysical neutrinos 1. Look(for(a(hard,(high8energy(component( above(the(atmospheric(background( Upward(ν µ (induced(muons( Highest(rate( Events(star9ng(in(the(detector( Lower(rate,(but( Atmospheric(ν(background(is(lower( 2. Look(for(excess(of(events(in(the(ν µ (skymap( Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 39
40 ( ( ( ( ( Results from IC-59 ( ) events Analysis(of(ν µ induced(µ(from(below(( 1 experimental data conv. atms. ν (HKKMS07 + H3a) conv. atms. ν (best fit) prompt atms. ν (90%CL upper limit) astrophysical ν (best fit) astrophysical ν (90%CL upper limit) Cascade(search( with(ic59(finds(8( events((expected( background(of(4).( Prompt(ν?( #" ' ICRC(paper(0662( %' log10(de/dx [GeV/m]) reco Sugges9on(of(hard((astrophysical?)(component( ~0.25(x(10 88 (GeV(cm 82 (sr 81 (s 81 (( (arxiv: ( Most(energe9c(event.( '1;;.*&)+*&<0.&!=.">-.&"+(('-+*'?+3& ( / / ( ( ( ( Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 40
41 ( ( ( ( ( ( Search for cosmogenic neutrinos (also known as GZK n ) p + γ CMB n + π + nµ + ν µ Limits(from(IC879(+(IC886,(May(20108May2012( This(search(discovered(( two(pev(cascade(events,( each(with(just(over(1(pev( deposited(energy88lower( than(expected(for( cosmogenic(neutrinos.(( The(events(were(just(at(the( threshold(of(the(search.( Engel,(Seckel,(Stanev( ( ( ( ( ( Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 41
42 ( ( ( ( ( ( HESE: follow-up analysis of PeV events HESE(=(High(Energy(Star9ng(Events( Looks(at(same(662(days(of(data((June(2010( (May(2012),((Science,(22(Nov(2013( Require(event(to(start(inside(fiducial(volume( 6000(p.e.(threshold((((((((((((((((((((((deposited(energy,( 30 TeV lower(than(ehe(search(( Accept' 10 3 IceCube 4 averaged e (anti- e ) effective areas 10 2 EHE analysis HESE analysis A eff (m 2 ) Comparison(of(effec9ve(areas( Roma,(28/01/2014( Tom(Gaisser( 30( Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 42 E (GeV)
43 High Energy Starting Event Analysis 210 TeV 70 TeV 250 TeV 220 TeV 2-year analysis: Science 342, ( Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 43
44 High Energy Starting Event Analysis 210 TeV Require that event: - Does not start in veto region - Has at least 6000 photoelectrons μ ν μ 70 TeV 220 TeV Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 44
45 3-Year Analysis PRL 113, (2014) 36 events in 3 years Three > PeV events seen in three years, including a 2-PeV neutrino High Energy Starting Event Analysis Big Bird Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 45
46 Significance of astrophysical flux: 5.7 σ High Energy Starting Event Analysis Of the 36 events, ~ half are expected to be bkg (atm. muons and atm. neutrinos) Astrophysical fit (and its significance) depends on number, direction, and energy Shape (energy and zenith distribution) of signal and background is different Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 46
47 Comments on backgrounds Atmospheric(muons(passing(the(veto( This(background(is(determined(experimentally(by( defining(a((smaller,(inner(veto(region(and(checking( the(rate(at(which(tagged(muons(leak(through( Atmospheric(neutrinos( Conven9onal (ν (from(k(and(π(decay)(( Prompt (ν (from(decay(of(charm)( Muons(produced(in(the(same(shower(as(ν(provide( a(par9al(self8veto(in(southern(sky( Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 47
48 Atmospheric neutrino self veto Two(cases( 1.(Stefan(Schönert(et(al.( Phys.(Rev.(D79((2009)(043009( Can(be(evaluated(analy9cally( 2.(Veto(by(an(unrelated(μ( 88also(applies(to(ν e( Requires(Monte(Carlo(or( numerical(integra9on( Roma,(28/01/2014( Tom(Gaisser( 37( Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 48
49 The rate of events passing the veto condition depends on n flavor Passing rate per 1 Veto(=(1( (Passing( ( Veto(is(more( effec9ve(for(ν µ than( for(ν e (and(prompt(ν((( Passing fraction solid: includes correlated!: for! dashed: uncorrelated! only: for e & prompt cos = 0.35 cos = 0.55 cos = 0.75 cos = E (GeV) ( ( ( ( ( Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 49
50 Atmospheric neutrino self-veto Interactions km 3 sr 1 yr 1 E > 100 TeV 10 1 astrophysical Some neutrinos are absorbed in the Earth conventional µ conventional e sin(δ) = cos( ) at the South Pole 1.5 km of ice An active muon veto removes down-going atmospheric neutrinos. Primary cosmic ray μ π- νμ Schönert, Resconi, Schulz, Phys. Rev. D, 79: (2009) Gaisser, Jero, Karle, van Santen, Phys. Rev. D, 90: (2014) Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics Jakob van Santen - ISVHECRI 2014, CERN 50
51 Atmospheric neutrino self-veto Interactions km 3 sr 1 yr 1 E > 100 TeV 10 1 astrophysical Some neutrinos are absorbed in the Earth conventional µ conventional e sin(δ) = cos( ) at the South Pole 1.5 km of ice An active muon veto removes down-going atmospheric neutrinos. Primary cosmic ray μ π- νμ Schönert, Resconi, Schulz, Phys. Rev. D, 79: (2009) Gaisser, Jero, Karle, van Santen, Phys. Rev. D, 90: (2014) Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics Jakob van Santen - ISVHECRI 2014, CERN 51
52 Atmospheric neutrino self-veto Interactions km 3 sr 1 yr 1 E > 100 TeV 10 1 astrophysical Some neutrinos are absorbed in the Earth prompt µ + e conventional conventional µ conventional conventional e sin(δ) = cos( ) at the South Pole An Prompt active atmospheric muon veto neutrinos removes are down-going vetoed, too. atmospheric neutrinos. 1.5 km of ice K 0 Primary cosmic ray μ π- D - νμ Schönert, Resconi, Schulz, Phys. Rev. D, 79: (2009) Gaisser, Jero, Karle, van Santen, Phys. Rev. D, 90: (2014) Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics Jakob van Santen - ISVHECRI 2014, CERN 52
53 Atmospheric neutrino self-veto Interactions km 3 sr 1 yr 1 E > 100 TeV 10 1 astrophysical Some neutrinos are absorbed in the Earth atmospheric prompt µ + e conventional conventional µ conventional conventional e sin(δ) = cos( ) at the South Pole The zenith distributions of high-energy Primary cosmic ray astrophysical and An Prompt active atmospheric muon veto neutrinos removes are down-going vetoed, too. atmospheric neutrinos. π- atmospheric D - K neutrinos 0 are νμ 1.5 km! of ice μ fundamentally different.! Schönert, Resconi, Schulz, Phys. Rev. D, 79: (2009) Gaisser, Jero, Karle, van Santen, Phys. Rev. D, 90: (2014) Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics Jakob van Santen - ISVHECRI 2014, CERN 53
54 3-Year High Energy Starting Event Analysis Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 54
55 3-Year High Energy Starting Event Analysis Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 55
56 3-Year High Energy Starting Event Analysis Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 56
57 3-Year High Energy Starting Event Analysis Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 57
58 3-Year High Energy Starting Event Analysis Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 58
59 High Energy Starting Event Analysis Assuming unbroken E -2 spectrum, best-fit astrophysical normalization is: Lack of events above 2 PeV (3.1 expected in this analysis; more in the EHE analysis, PRL 111, (2013)) suggests unbroken E -2 disfavored Best power-law fit yields a spectral index of -2.3 (and fits 0 charm component): Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 59
60 where do they come from (3 year data)? hottest spot 7.2%: consistent with diffuse flux with fllavor 1:1:1? Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 60
61 diamonds: muon tracks (0.4 degree resolution) circles : electromagnetic showers : energy : angular resolution angular resolution Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 61
62 too few ν µ? no, in an all flavor search ν µ tracks are rare length of τ track = 50m E ν PeV a muon track is relatively rare Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 62
63 mostly showers PeV showers: volume ~ 5 m 3 isotropic after 25~ 50 m Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 63
64 Muon Neutrino Diffuse Analysis Northern Sky Complementary analysis to Starting Event analysis Northern sky allow events to enter from outside detector, use Earth as filter against muons from cosmic rays Track events from muon neutrinos Good pointing: ~ 0.5 log 10 muon energy resolution ~ 0.3 (at energies ~ 100 TeV) events in 2-year analysis Data Astrophysical Prompt IceCube Preliminary Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 64
65 Muon Neutrino Diffuse Analysis Events events in 2-year analysis Estimated 99.9% pure muon neutrino sample Energy estimate for the muon track. Only lower-bound on neutrino energy (interacted before reaching detector) Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 65
66 Muon Neutrino Diffuse Analysis Best fit for E -2 astrophysical spectrum is: 0.96 ± GeV -1 cm -2 s -1 sr σ evidence of astrophysical flux Starting Events Differential Spectrum Muon Neutrino E -2 fit (nearly) independent of starting track analysis Strengthens evidence that flux is allflavor and all-sky Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 66
67 Muon Neutrino Diffuse Analysis Events E -2 flux implies there are ~ 100 astrophysical muon neutrino events in sample at lower energies or much more, if spectrum is softer than E -2 These events are nearly hidden in diffuse analysis, but can stand out in point source analysis Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 67
68 the high energy neutrino flux: atmospheric and cosmic Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 68
69 Point Source Analysis 4 years of data including construction period arxiv: Optimization for point source search: looser cuts possible (typically ~ 90-95% neutrino purity) and lower energy events more useful N. sky N. sky diffuse point source sample sample events events (comparing same 2-year period) Background estimated robustly from off-source data at similar declination Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 69
70 Point Source Analysis Data: Livetime 1371 days upgoing neutrinos downgoing CR muons Perform a search looking for significant clustering of events above random background expectation (unbinned maximum likelihood analysis) Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 70
71 Point Source Analysis arxiv: Data: Livetime 1371 days 178k (upgoing neutrinos) 216k (downgoing muons) No significant excess seen Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 71
72 Point Source Analysis IceCube Preliminary (arxiv: ) Northern Sky sensitive for TeV PeV Southern Sky sensitive mainly > PeV ANTARES sensitive to TeV PEV in both skies Southern sky Northern sky Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 72
73 Point Source Analysis Point-source equivalent flux if the diffuse flux came from: one point in the sky 100 points in the sky Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 73
74 Point Source Analysis Point-source equivalent flux if the diffuse flux came from: one point in the sky 100 points in the sky 1000 points in the sky Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 74
75 Point Source Analysis Point-source equivalent flux if the diffuse flux came from: one point in the sky 100 points in the sky 1000 points in the sky Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 75
76 Papers(explaining(IceCube(neutrinos( (par9al(list)( F. Halzen: IceCube Neutrinos: From GeV to PeV Nuclear Physics B (Proc. Suppl.) (2014) 3 17 GalacLc' Galac9c(PeV(Neutrinos, (Gupta,(arXiv: ( Sub8PeV(Neutrinos(from(TeV(Uniden9fied( Sources(in(the(Galaxy, (Fox,(Kashiytama,( Mészarós,(arXiv: ( Pinning(down(the(cosmic(ray(source( mechanism(with(new(icecube(data, ( Anchordoqui(et(al.,(arXiv: ( The(Galac9c(Pevatron, (Neronov,(Semikoz,( Tchernin,(arXiv: ( ExtragalacLc' PeV(neutrinos(from(the(propaga9on(of(ultra8high( energy(cosmic(rays, (Roulet(et(al.,(arXiv: ( On(The(Origin(of(IceCube's(PeV(Neutrinos, (Cholis,( Hooper,(arXiv: (( Cosmic(PeV(Neutrinos(and(the(Sources(of(Ultrahigh( Energy(Protons, ((Kistler,(Stanev,(Yuksel(,(arXiv: ( PeV(neutrinos(from(intergalac9c(interac9ons(of( cosmic(rays(emied(by(ac9ve(galac9c(nuclei, ( Kalashev,(Kusenko,(Essey,(arXiv: ( Neutrinos(at(IceCube(from(Heavy(Decaying(Dark( Maer, (Feldstein(et(al.,(arXiv: ( Ice(Cube(Observed(PeV(Neutrinos(from(AGN( Cores, (Stecker,(arXiv: ( Demys9fying(the(PeV(Cascades(in(IceCube:(Less( (Energy)(is(More((Events)(, (Laha(et(al.,(arXiv: ( ( On(the(Hadronuclear(Origin(of(PeV(Neutrinos( Observed(with(IceCube, (Murase,(Ahlers,(Lacki,( arxiv: ( Photohadronic(Origin(of(the(TeV8PeV(Neutrinos( Observed(in(IceCube, (Winter,(arXiv: ( Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 76
77 Power for extragalactic cosmic rays (assuming transition at the ankle) Energy(in(extra8galac9c(cosmic(rays(per(ln(E): ( 4π EdN c d ln E = 4π { } GeV 20 erg c cm s sr cm 3 Divide(by(Hubble(9me(to(es9mate(power(required:( ( dl ( d ln E erg Mpc 3 s 1 Power(required(>(10 37 (erg/mpc 3 /s( Es9mates(depend(on(cosmology(+(extragalac9c(magne9c(fields:( 3(x(10 83 (galaxies/mpc 3 (5(x(10 39 (erg/s/galaxy( 3(x(10 86 (clusters/mpc 3 (4(x(10 42 (erg/s/galaxy(cluster( (AGN/Mpc 3 ( (10 44 (erg/s/agn( ~300(GRB/(Gpc 3 yr)( (10 51 (erg/grb( ( ((( Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 77
78 New limit on n from GRB (IC-40/IC-59) Note(shape(due(to( photoproduc9on:( Both(low(and(high( cutoffs(in(region( of(interest.( IceCube:(Nature,(19(April(2012( 8(events(expected(if(observed(GRB(account(for(all(UHECR( (None(seen(in(correla9on(with(GRBs(of(SWIFT(&(Fermi(GBM( Different(class(of(low(luminosity(GRB?((Cholis(&(Hooper,( )(( ( ( ( ( ( ( Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 78
79 Generic(model(I( CR(accelera9on(occurs(in(jets(( AGN(or(GRB( Intense(radia9on(fields( Models(assume(photo8produc9on:( (p(+(γ(!(δ +(!(p(+(π 0(!(p(+(γ γ( (p(+(γ(!(δ +(!(n(+(π +(!(n(+(µ(+(ν$ Ideal(case(((~( Waxman8Bahcall(limit )( Strong(magne9c(fields(retain(protons(in(jets( Neutrons(escape,(decay(to(protons(&(become(UHECR( Extra8galac9c(cosmic(rays(observed(as(protons( Energy(content(in(neutrinos( (energy(in(uhecr( This(picture(disfavored(as(limits(go(below(W8B( ( /rieger/science.gif Waxman, Bahcall, PRD 59, (1998). Also TKG astro-ph/ v Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 79
80 Generic(model(II( UHECR(are(accelerated(in(external(shocks(analogous(to( SNR( See(E.G.(Berezhko,( (&( ( mixed(composi9on((accelerate(whatever(is(there)( Low(density(of(target(material(!((lower(level(of(TeV8PeV(neutrino(produc9on( Diagram from Begelman & Cioffi, Ap.J. (1989) L ( ( Univ. "La Sapienza" Dott. in Fisica -( High Energy ( Neutrino Astrophysics ( 80
81 IceCube: study of TeV-PeV Cosmic-Ray anisotropy Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 81
82 IceCube: study of TeV-PeV Cosmic-Ray anisotropy Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 82
83 IceCube: study of TeV-PeV Cosmic-Ray anisotropy Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 83
84 IceCube: study of TeV-PeV Cosmic-Ray anisotropy Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 84
85 IceCube: study of TeV-PeV Cosmic-Ray anisotropy Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 85
86 IceCube: study of TeV-PeV Cosmic-Ray anisotropy Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 86
87 IceCube: study of TeV-PeV Cosmic-Ray anisotropy Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 87
88 IceCube: study of TeV-PeV Cosmic-Ray anisotropy Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 88
89 Ideas(for(the(future(at(South(Pole( Sunflower(paern( minimizes(entry( channels( ( Average(spacing:( ~250(m(( ( ( ( ( ( ( Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 89
90 PINGU( Univ. "La Sapienza" Dott. in Fisica - High Energy Neutrino Astrophysics 90
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