IceCube)and)high)energy) neutrino)astronomy)
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1 IceCube)and)high)energy) neutrino)astronomy) Albrecht)Karle) University)of)Wisconsin/Madison) Lecture,)March)4,)) Physics)734)) Albrecht)Karle,)UW/Madison)
2 High)energy)parEcles)in)the)Universe) Cosmic)Rays) Observed)up)to)10^21) ev) Diffuse,)mass) composieon) Gamma)Rays) Observed)up)to)~100) TeV) Numerous)TeV)point) sources)resolved) Neutrinos) Atmospheric)neutrinos) observed)up)to)300)tev) Solar)neutrinos)and) SN1987a)at)lower)energies) Albrecht)Karle,)UW/Madison)
3 ))Cosmic)Rays)and)Neutrino)Sources) Candidate sources (from acceleration region): Cosmic ray related: SN remnants Active Galactic Nuclei Gamma Ray Bursts Other: Dark Matter Exotics T. Gaisser 2005! Cosmic rays! Guaranteed)sources)(known)targets):) )Atmospheric)neutrinos)(from)π)and)K) decay)) )GalacEc)plane:))CR)interacEng)with)ISM,) concentrated)on)the)))disk) )GZK)(cosmogenic)neutrinos)) knee! 1 part m -2 yr -1! Ankle! 1 part km -2 yr -1! 3)
4 pp NN + pions; pγ pπ 0,nπ + π + µ + + ν µ µ + e + + ν e + ν µ 4) Fermi))AcceleraEon) Predicts)E /2)) Spectrum) 4)
5 Highest)energy)cosmic)rays)can)produce) neutrinos)during)interglacec)propagaeon) 411 photons / cm K InteracEon)with)) microwave)background)photons) 5)
6 ))Neutrinos) MeV energy neutrino astrophysics High energy neutrino astronomy: Small fluxes, Need large detectors, Note wide energy range 6)
7 Neutrinos)as)Cosmic)Messengers) p) Protons:)deflected)by) magne7c)fields.)) γ" Photons:)easily) absorbed)by)cmb)and)ir) backgrounds.)em/ Hadronic)discrimina7on) difficult)) ν Neutrinos:)not) deflected)by)magne7c) fields.)low)interac7on) crossgsec7on.) 7)
8 Cosmic)rays,)muons) and)neutrinos)in)the) atmosphere) a constant rain of muons and neutrinos is produced by cosmic rays crashing into the atmosphere IceCube)measures)about)100000) neutrinos/year)generated)by)the) rain)of)cosmic)rays)hibng)the) Earth.)
9 Cosmic)rays)and) atmosphere) Cosmic)rays)bombarding)Earth s) atmosphere)produce)energeec) secondary)parecles.))important)for) underground)detectors:)muons)and) neutrinos) π + µ + + ν µ µ + e + + ν e + ν µ ) )and)the)same)for)) π ν e ν µ Why)are)there)fewer)))))))than)))))))?)) Electron)neutrinos)have)lower)energy) Muon)decay)is)increasingly)suppressed)at) high)energies.)life)eme)of)2.2µsec)much) longer)due)to)eme)dilataeon) (Lorentzfactors)of)>)1000).)) π 0 γ + γ For)completeness:)) )make)e.m.)showers,)which)can)be)nicely) used)for)ground)based)detectors) graphic:) B.)Louis)
10 Muons)and)neutrinos)at)depth) Neutrino/induced) muons)from)all) direceons) 50000)/)day) Downward) atmospheric) muons) 300)million)/)day) Neutrinos:)Use)Earth)as)filter;)look)for)neutrinos)from)below)(GeV)to)PeV)) Cosmic)ray)muons:)) 10)
11 How)to)detect)high)energy)neutrinos) ) the)challenge:) Rates)are)small!) The) cross)seceon )is)small!) Backgrounds)from)cosmic)ray)muons)are)high)
12 deep)detector) shielded)by)water) or)ice) Muon) neutrino)travels) through)the)earth) and) ) someemes)interacts)to)make)a)muon) )that)travels)through)the)detector) Neutrino)
13 Cherenkov)light)emission) Charged particles, eg muons, when traveling faster than c_medium, emit light at a characteristic angle where coherent superposition takes place. In ice: n = 1.33 Cherenkov angle: cosθ = 1 nβ = 41 β = 1 Yield ( nm): dn/dx 200photons/cm 2x10^7 photons/km for a minimum ionizing muon. About 0.01% of all energy deposited will be radiated in Cherenkov photons Example: A high energy cascade of 10^14 ev will produce about 10^10 photons in visible range.
14 Simulated)µ/track)of)energy)1.2)TeV)) propagated)through)1km)of)south)pole)ice)) 1)%)of)all)photons)are)shown)unEl)they)are)absorbed.) AbsorbEon)length:)100/200m) EffecEve )Scasering)length:)20) )50m)
15 Photomultiplier Tube Principle:)) Photoelectric)effect) +)electron)muleplicaeon) A)beser)name)would)be)) secondary)electron)mul7plier) IceCube)PMT)(Hamamatsu)) Diameter)25cm^2) quantum)efficiency:)25%)(35)) Gain:)10^7)) (Single)photoelectrons) )10mV)) Eme)resoluEon)spe:)3)ns) Dynamic)range:)300pe/10ns) 1 cm
16 The)IceCube)Digital)OpEcal)Module)
17 Digital)OpEcal)Module)(DOM)) Each)sensor)is)almost)an)independent)detector) PMT:)10)inch)Hamamatsu) Power)consumpEon:)3)W) DigiEze)at)300)MHz) Dynamic))rang:)1) )10000)photelectrons) Flasherboard)with)12)LEDs) Local)HV) Clock stability: nsec / sec" Synchronized to GPS time every 10 sec " Time calibration resolution = 2 nsec " Digitized Waveform
18 Time)resoluEon:)) ~1ns)for)bright)pulses) Time)difference)between) neighboring)doms)fired)with) (bright))flasher)pulses:)~1)ns.) )(this)includes)clock)eming))) For)SPE)pulses)add)jiser)(3)nsec))) Single)photoelectron)pulse) resolueon)limited)by)pmt.) RMS)in)the)peak:)~2ns) Lab)measurement)with)laser.)) FWHM)=)5)ns)
19 IceCube) Total)of)86)strings) and)160)icetop) tanks;) CompleEon)with)86) strings:)january) 2011) Full)operaEon)with) all)strings)since)may) 2011.) A.)Karle,)UW/Madison) 19)
20 IceCube)Laboratory) OperaEonal)support:)) ICL)maintenance) ~60)kW)power)to)electronics) 90)GB/day)over)satellite) 2)winterovers) summer)populaeon)(around)5/7)pop)dec)/)jan)))
21 Flasher)events)used)for)calibraEon) All)sensors)are)equipped)) with)a)set)of)12)led)flashers.)) A)30)ns)pulse)of)only)) 10)billion)photons)(400nm)) is)visible)to)a)distance)of)600m.) These)measurements)are)used)) to)calibrate)the)detector)) /)Eme)) / )geometry)) / )opecal)properees)of)the)ice)
22 Topology)of)neutrino)interac7ons) neutrinoginduced)showers) Mixed )showers)) <E electromagne7c) >) )80%)E ) <E hadronic) >) )20%)E nu )) Hadronic)showers)) <E>) )20%)E ) EM)or)Hadronic) graphics:)jaime)alvarez)
23 Event)types) Throughgoing)muons) )the)workhorse) for)neutrino)astronomy.) Vertex)can)be)far)outside)the)detector.) Increased)effecEve)volume!)) Cascade)events:) ν e,ν τ )))))))))))))))))and)neutral)current) High)energy)resoluEon)(fully)acEve) calorimeter,)all)energy)gets)deposieed) in)the)deteceon)volume))) StarEng)tracks:)downgoing)neutrino) astronomy)(reject)background)of) throughgoing)cosmic)ray)muons))
24 Rare)and)complex)event)types:) ν τ Tau)events))) ν τ + N τ + X The)tau)will)decay) Tau _ decay τ ν τ + X γ ct τ At)low)energies)(<1TeV),)the)tau)will) decay) instantly ) At)high)energies)the)decay)length)is) long)enough)for)a))the)second) interaceon)to)become)detectable) l τ = γ ct τ 50 (E τ /PeV) m Double)bang )signature) Also)possible,)parEally)contained)first)or) second)interaceon)only.) Energy)loss)of)tau)is)smaller)than)that)of) a)muon.)
25 IceCube)) background:) downgoing)cosmic) ray)muons) ~)1500)per)second) signal:) upgoing)muons) inieated)by) neutrinos) ~)10)per)hour)
26 Events)
27 SimulaEon:)1)ms)of)µ s)and)noise) Trigger)rate:)3kHz)of)muons) Shown)are)also)muons)that)will)not)form)a)trigger) noise)rate:)only)300)photoelectrons/s)(at)/30 C))
28 SimulaEon:)1)milli)second)of)µ s)and)noise) Trigger)rate:)3kHz)of)muons) Shown)are)also)muons)that)will)not)form)a)trigger) noise)rate:)only)300)photoelectrons/s)(at)/30 C)) /))take)care)of)coincident) events )
29 Muon)energy)loss,)range) hsp://pdg.lbl.gov/2011/reviews/rpp2011/rev/passage/parecles/maser.pdf)
30 Muon)energy)loss,)range) hsp://pdg.lbl.gov/2011/reviews/rpp2011/rev/passage/parecles/maser.pdf)
31 Muon)energy)loss,)range)
32 Neutrino/nucleon)cross/secEon) Cross)secEon)rises)with) energy) Glashow/resonance )at) 6.3)PeV) νn ν e + e W X CC) NC) ν N
33 the)earth)as)) a)cosmic)ray) muon)filter.) a)neutrino)of)70)tev) )has)an)interaceon)length)l) equal)to)the)diameter)of) the)earth)
34 Neutrino)effecEve)areas) Why)can)neutrino)telescopes)operate)over) )such)a)huge)energy)range?) Area)at)100)TeV)(1TeV)) AMANDA/II:)3m 2) )(0.005) ) IceCube)86:)100m 2 )(0.3)) (trigger)) (trigger)) Deep)Core)lowers) threshold)from)100)gev) to)10)gev.)) EffecEve)area)for) ) Strong)rise)with) energy:)) )) Increase)of)muon) range)with)energy)up) to)pev)
35 Neutrino)fluxes)
36 Atmospheric)neutrinos) Neutrino)fluxes)
37 Neutrino)fluxes) Atmospheric)neutrinos) IceCube)59:)) >)30000)neutrinos)from)) 0.3)to)300)TeV)/)year) (full)detector)>)50k/yr))
38 Atmospheric)Neutrinos) Very)large)neutrino) sample:)>)50k)events)per) year)of)purity,)) Muon)neutrinos)into) 100 s)of)tev) Now)also)Electron) neutrinos)up)to)tev) energies)) arxiv: ) Approaching)the)ability) to)test)prompt)models))
39 40+59)String)all/sky)neutrino)map) Kolanoski)(IceCube)Coll))) ICRC)2011) E /2 )Signal) arxiv:) ) Northern)hemisphere) Background:)atmospheric)neutrinos) Southern)hemisphere) Background:)atmospheric)muons) Reduced)by)10 /5 )using)energy)cut) on)downgoing)events ) No excess found! Analyze)skymap)cosmic)neutrinos)using)) 1))energy,)) 2))point)sources) 3))transient)sources) or)all)three!)example:)grb) 39)
40 IceCube)diffuse)neutrino)searches) Look)for)neutrino)events)at)high)energy,)above)the)rapidly)falling)atmospheric) neutrino)spectrum.)) 1. ν μ )signal)looks)for)upward)going)tracks) IC)40///string)published)[Phys.)Rev.)D)84,)082001)(2011))arXiv:) v5)])) Results)from)IC)59)search))) 2. Cascade)search) )Cascade)events)(CC)ν e )and)ν) τ ),)NC)ν μ,τ,e ))contained)showers)) )updated)results)for)ic)40///string)search) 3. Extremely)high)energy)events,)downgoing)events)at)energies)above) downgoing)muons)background) 4. New)strategies)for)all)flavor)searches)with)contained)vertex))
41 1.)Search)for)diffuse)))))flux) ν µ ) Search)for)upward)going)tracks)at ) energies)above)atmospheric) neutrino)spectrum.) ) RelaEve)rates)in)IceCube)(at) trigger)level,)before)analysis)cuts)) ConvenEonal)νμ:)Honda)2006)) Prompt)νμ:)Engberg)et)al.) Astrophysical)E /2 :)at)ic40)limit)
42 IC)59)diffuse))))))flux) ν µ Data)from)2009/2010:)348)days)of)liveEme,)21943)events)) Number of Events" Anne)SchukraÉ) Data)from)2009/2010:)348)days)of)liveEme)with)~75%)complete)detector) Analysis)looks)for)deviaEon)from)the)expected)atmospheric)neutrino)flux)
43 IC)59highest)energy)events) Fised)muon)energy:)))84)TeV)
44 Diffuse) )flux)limits) IC59)limit) IC59)sensiEvity)
45 GZK/EHE)Neutrino)Search) Data)from)2010/2012:) )days)of)liveEme) with)90%/100%)complete) detector.) Analysis)looks)for)EHE) neutrinos)where)no) background)is)expected.) Two)very)interesEng)events) were)found)at)~1)pev do) not)appear)to)be)part)of)a) GZK)flux,)however)
46 Two)events)found)at)PeV)energies) Preliminary) Number)of)Photoelectrons) Error)on)vertex)posiEon:)~)5m)
47
48 Observed)neutrino)event)at)E=1.1x10 6 )GeV) Waveforms)provide)useful) informaeon) Shown)is)one)event)with) best)fit)(blue))and)forced) reverse)direceon)(red))) Event)contains)354) waveforms)and)a)total)of) >)105)photoelectrons) 48)
49 PeV)Events)Compared)to)Models) The)two)events)are)not)from)muon) background!) The)two)events)are)difficult)to) explain)as)conveneonal) atmospheric)origin.)(2.7)sigma) tension)to)conveneonal) atmospheric)neutrino)flux;)very) high)prompt)flux)would)be)needed) (15)Emes)Enberg).)) The)two)PeV)events)are)compaEble) with)the)diffuse)e /2 )limit,)but)such)a) spectrum)would)also)predict) addieonal)events)at)higher) energies.) Seeing)two)such)events)would)be) relaevely)surprising)for)gzk)fluxes) which)peak)at)higher)energies) Figure:)Aya)Ishihara)
50 Background)free) neutrino)astronomy?) Schoenert)et)al.) Phys.Rev.)D79)(2009))043009) arxiv: ) Atmospheric)neutrinos)are)made) in)air)showers.) Downgoing)energeEc)neutrinos) (100TeV,)zenith)less)then)50 )) are)almost)always)accompanied) by)muons)down)to)several)km)of) depth.))
51 Veto)probability)) vs)energy)and)zenith) angle) Schoenert)et)al.) Phys.Rev.)D79)(2009))043009) arxiv: )
52
53 Kinematics i = π or K c = 1 E > several GeV makes β~1 In CM Frame P = m, 0,0,0 P = E, p μ P = E, p ν P = P + P P = P P P = P P P = P + P 2P P P P = E E p i p μ = m E P = 0 0 = m + m 2m E E = m + m E = E E = m m + m E = m m 2m 2m 2m Boosting Into Lab Frame E = γ(e + βp ) E = γ(e + βp ) p = p CM cos θ p = p CM cos( θ π) = p CM cos θ E = γ p CM (1 + cos θ ) E = γ p CM ( m + m m m cos θ ) In the worst case cos θ = 1 E = 2γ p CM E = 2γ p CM ( E E ( m m m ) m m m )
54 Kinematics E E ( m m m ) E E for π E E for K Can also show that the neutrino and muon deviate less than 1m (10m) over a 10 km path for neutrino energies greater than 1 TeV originating from a pion (kaon) decay These calculations prove that a nearly collinear muon with at least TeV (48 GeV) in energy is created for almost all atmospheric muon neutrinos with energy over 1 TeV which originated from pion (kaon) decays
55 What Can Be Done With This Information? Using E, x = 0.73TeV (e... 1) from Muon Monte Carlo to give an estimate of the muon s energy at depth one can produce the plot below The plot shows that for neutrino energies above ~10 4 GeV and zenith angles less than ~55⁰ there exists a region where an atmospheric muon neutrino will have an accompanying muon To find events one searches for events that are starting tracks above a certain energy and below a certain zenith angle This is the basis for the search done by Nathan and Claudio
56 Strategy)to)remove)all)background) /)neutrino)telescope)going)up/side)down)at)e>100tev)) Goal)of)background)free)region)for)E)>)~100)TeV) (but:)need)to)fold)in)zenith)angle)resolueon))
57 Strategy)to)remove)all)background) /)neutrino)telescope)going)up/side)down)at)e>100tev)) Goal)of)background)free)region)for)E)>)~100)TeV) (but:)need)to)fold)in)zenith)angle)resolueon))
58 Strategy)to)remove)all)background) /)neutrino)telescope)going)up/side)down)at)e>100tev)) Goal)of)background)free)region)for)E)>)~100)TeV) (but:)need)to)fold)in)zenith)angle)resolueon))
59 Neutrino)oscillaEons)
60 Low)energies,)1) )100)GeV,)PINGU)...) IceCube - DeepCore: DESIGN Eight special strings in filled in the bottom center of IceCube ~5x higher effective photocathode density than regular IceCube IceCube Result: ~20 MTon detector with ~10 GeV threshold, will collect O(100k) physics quality atmospheric ν/yr extra veto cap VETO AMANDA IceCube s top and outer layers of strings provide an active veto shield for DeepCore Effective μ-free depth much greater Atm. μ/ν trigger ratio is ~10 6 Vetoing algorithms expected to reach well beyond 10 6 level of background rejection (Muon flux after veto comparable to Sudbury depth) 60) 350 m 250 m Deep Core
61 DeepCore Atmospheric Muon Veto Overburden of 2.1 km water-equivalent is substantial, but not as large as at deep underground labs However, top and outer layers of IceCube provide an active veto shield for DeepCore ~40 horizontal layers of modules above; 3 rings of strings on all sides Effective μ-free depth much greater Can use to distinguish atmospheric μ from atmospheric or cosmological ν Atm. μ/ν trigger ratio is ~10 6 Vetoing algorithms expected to reach at least 10 6 level of background rejection
62
63 Water)Cherenkov)detectors) PMT)coverage)vs)threshold) Super/K) HyperK) LBNE) Define:) Photon)effec7ve)area)=)) )Number)of)PMT) )x)cathode)area) )x)quantum)efficiency) =)equivalent)area)of)100%)photon)detec7on.))) (colleceon)efficiency)not)included)here.)) PINGU) Deep)Core) ANTARES) AMANDA) Baikal)GVD4) KM3Net) IceCube) Photon)effecEve)area)prop.)~)1/Energy)threshold.))) Detector)arrangements)and))opEcal)properEes)of) water)and)ice)are)different,)yet)the)pmt) density)scales)well)with)energy)threshold.) IceCube DeepCore PINGU AMANDA ANTARES KM3Net BAIKAL GVD4 LBNE SuperK HyperK String spacing [m] PMT spacing [m] Instrumented mass [Mt] Total No of PMT, OMS Cathode area No. of PMT or OMs/Mton Photon eff. area/mass [m2/mt] Energy "threshold" [GeV] ) Footnote/Disclaimer:)Some)figures)are)esEmates.)DefiniEons)of)threshold)vary)somewhat)within)factor)of)two) in)some)cases.))threshold)for)nu)telescopes)above)deep)core)are)for)muon)neutrinos.)
64 PINGU Physics Probe lower mass WIMPs Gain sensitivity to second oscillation peak/trough enhanced sensitivity to neutrino mass hierarchy Gain increased sensitivity to supernova neutrino bursts Extension of current search for coherent increase in singles rate across entire detector volume Only 2±1 core collapse SN/century in Milky Way need to reach out to our neighboring galaxies Gain depends strongly on noise reduction via coincident photon detection (e.g., in neighbor DOMs) Ref.)on)Supernova)detec7on:))))) G)L.)Demiroers,)M.)Ribordy,)M.)Salathe) arxiv: ) G)Poster)30G3:)M.)Voge)et)al) Neutrino hierarchy (sin 2 (2θ13)=0.1) Mena, Mocioiu & Razzaque, Phys. Rev. D78, (2008) ντ appearance νµ disappearance Deep)Core)data) Resconi)et)al.)(Poster)) G.)Sullivan s)talk)
65 Mass)hierarchy) Figure)and)Analysis)from:)) Akhmedov,)Razzaque,)Smirnov,)arXiv:) ) See)poster)by)E.)Resconi)et)al.))(IceCube)and)PINGU)) Expected)significance)for)observed)number)of) events)for)ih)vs)nh)are)shown)in)energy)vs.) zenith)plot) If)required)energy)and)direcEonal)resoluEon) is)achievable:) )))))))))))) )high)staesecal)significance) GeV) 18) 14) 10) 6) [/1,08])))[/0.8,/0.5]))[/0.5,0.0]) cos)(theta))) Assumed)above:) )Energy)resolu7on:)4)GeV,)) )Angular)resolu7on:)0.3)in)cos(theta)) )Exposure:)10)Mt)yr) +6) +3) 0) /1) /2) Significance) Conclusion)(Akhmedov)et)al.):) Our)preliminary)es7mates)show)that)aHer)5)years)of)PINGU)20) opera7on)the)significance)of)the)determina7on)of)the)hierarchy)can) range)from))3)to)11)(without)taking)into)account)parameter) degeneracy),)depending)on)the)accuracy)of)reconstruc7on)of)neutrino) energy)and)direc7on. ) 65)
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