Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 1. Hermann Kolanoski Humboldt-Universität zu Berlin and DESY
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1 Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 1 Hermann Kolanoski Humboldt-Universität zu Berlin and DESY
2 Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 2 What I want to tell you: Cosmic rays (CR) How to measure cosmic rays What we know and don t know about CR Neutrinos as messengers of cosmic accelerators Neutrino Observatory IceCube The IceCube Muppet Show... Do not talk about e.g. exotic searches (wimps, )
3 Cosmic Rays 100 years after their discovery not yet understood faster discharge of an electrometer with increasing height interpreted due to radiation from space: Höhenstrahlung Viktor Hess 1912 ion pairs / (cm 3 s) 5 km height Kernfragmente Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 3
4 Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 4 Zwicky s proposal for the CR Origin In Los Angeles Times, Jan Cosmic rays are caused by exploding stars which burn with a fire equal to 100 million suns and then shrivel from ½ million mile diameters to little spheres 14 miles thick., says Fritz Zwicky, Swiss Physicist. since then we are trying to prove it
5 Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 5 Cosmic Ray Spectrum ~ 32 decades ~ 32 decades ~E -2.7 very different detection methods very different detector sizes LHC(p) LHC(pp) cut-off?
6 Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 6 Cosmic Ray Spectrum ~ 32 decades ~ 32 decades ~E -2.7 very different detection methods very different detector sizes Where and how are the highest LHC(p) energies LHC(pp) produced??? What is the elemental composition? Galactic and/or extragalactic? cut-off?
7 Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 7 Extensive Air Showers Use the atmosphere as calorimeter
8 Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 8 IceTop 1 km 2 Air Shower Detectors IceTop distance 125 m size 1 km 2 energies PeV EeV Pierre Auger Observatory 3000 km 2 distance 1500 m size 3000 km 2 energies EeV 100 EeV
9 Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 9 PeV to EeV The fine structure in the spectrum M.G. Aartsen et al, Physical Review D88 (2013) ! γ= F = E γ
10 Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 10 Rigidity : Confinement in the Galaxy R = p z e = ρ B H O Fe 10 kpc E max ~ Z E max (Fe) 26 E max (H) CR in galaxy: mean lifetime 10 7 years Energy has to be refueled. Where, how?
11 Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 11 Origin and Physics of the knee(s) p knee Fe knee If the knee is due to the diffusion out of the galaxy we expect a change in composition towards heavier elements spectrum below the knee: well known by direct measurements; above the knee: indirect measurements via air showers, difficult
12 Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 12 Cosmic Ray Anisotropy 5 TeV IceCube 17 TeV The orientation of the dipole moment does not correspond to the relative motion (~200 km/s) in the Galaxy (Compton-Getting effect) Diffusive transport in galactic magnetic field from nearby sources?
13 Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 13 Energy Dependence of CR Anisotropy 17 TeV 590 TeV 41 TeV 1.2 PeV 75 TeV 4.5 PeV 140 TeV 240 TeV Anisotropy changes in position, size Above 400 TeV there s indication of an increase in strength.
14 Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 14 Large and Small Scale Anisotropies diffusive transport from nearby sources? observed small scale (10 ) structures few pc distance
15 UHECR Results Auger Observatory Cen A direction correlation with AGN? cut-off at ev definitely observed GZK or source power limited? (GZK = Greisen-Zatsepin-Kuzmin) 28/84 = 33% isotropic background = 21% <1 % chance probability Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 15
16 Cosmic Rays, CMB Photons and Neutrinos Cosmic Microwave Background (CMB): perfect blackbody at 2.74 K CMB 2.7 K threshold E p ev GZK horizon ~160 Mly Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 16
17 Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 17 Nature of the Cutoff? Is this the GZK cutoff? Energy loss by collison with CMB photons? Or do accelerators run out of steam? composition becomes heavier Fe Auger: X max with florescence detectors data suggest change of composition from light to heavy Not GZK cutoff? Clarification from other messengers? Are there GZK neutrinos?
18 Where could particles possibly be accelerated? B Hillas diagram L E max ev z β s (L / kpc) (B / μg) supernova remnants (SNR) gamma ray bursts (GRB) active galactic nuclei (AGN) black holes Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 18
19 Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 19 Cosmic Accelerators Supernova Remnants (SNR) Fermi acceleration at shock front 1 % of the energy of all SN explosions can explain energy density of cosmic rays in galaxy (~ 0.5 MeV/m 3 ) Crab Nebula (explosion 1054) However: No SNR has been clearly pinned down as source
20 Twisted and Straight Paths Charged Particle Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 20
21 Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 21 Absorption of γ s by γ γ -> e + e - γ γ e + e - σ γγ 1 ~ s 2m e I know! I did γ γ hadrons s
22 Cosmic Rays, Gammas and Neutrinos CR ν connection accelerator p π ± μ ± ν ν ν target π 0 γ γ the γ ν connection for hadron accelerators ν spectrum ~ E -2 assumed CR γ connection Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 22
23 Neutrino fluxes Cosmic neutrinos should have a hard spectrum E -3.7 F ~ E -2 E -2 atmospheric ν F ~ E -3.7 Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 23
24 How to detect cosmic high energy neutrinos? quite difficult Absorption small detection probability small large target volume Most efficient: Cherenkov light from charged ν products Mediterranean Sea Lake Baikal transparent water or ice Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 24
25 Amundsen Scott Station Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 25
26 Approaching the Pole these Days Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 26
27 Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 27
28 Arriving at Pole Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 28
29 IceCube Neutrino Observatory air shower array IceTop neutrino telescope 86 Strings, 2450 m deep 5160 Optical Modules IceCube Instrumented: 1 km 3 IceTop: 1 km 2 DeepCore 1000 m Installation: Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 29
30 The Drill Camp Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 30
31 m deep Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 31
32 Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 32.. what you see down there
33 When the Season is over Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 33
34 The Last Flight at the End of the Season Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 34
35 Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 35
36 Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 36 Detection of High Energy Neutrinos atmosph. Muons mean free path ν µ µ atmosph. Neutrinos km lightyear 10 ν 12 µ +N µ + X Radius Earth orbit Earth diameter density of Universe ρ(h 2 O) extraterr. Neutrinos MeV GeV TeV PeV EeV ZeV Energy Earth as filter even for neutrinos the Earth becomes opaque above about 1 PeV look upward atm. background becomes less
37 Detecting a Neutrino Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 37
38 Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 38
39 Particle Signatures up-going ν µ point sources l ± W ± X ν l Z 0 X ν l N ν l N CC NC CR shower in IceTop ν µ µ ν e cascade all flavours µ - muon tracks - em + had. shower background & physics µ bundle ν e Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 39
40 Search for Diffuse Astrophysical Neutrino Flux Background: Atmospheric Neutrinos ~ 100,000 events per year prompt ν s: from (semi-) leptonic decays of heavy hadrons (mainly charm). Flatter spectrum than conventional ν s large uncertainty for astro-ν s IceCube has now constrained to ~ ERS model (Enberg et al.) E -2 astrophysical? Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 40
41 Atmos. ν s: background for one Signal for the other Neutrino Oscillation ν μ disappearence Atmospheric Neutrinos Detector Different direction = different pass length Survival probability in the 2ν scheme E ν GeV in DeepCore 41
42 Neutrino Oscillation arxiv: Disappearance atmospheric νμ with 3 years of data (for the normal hierarchy): sin 2 (θ23) = m 2 32 = Ultimate goal: measure mass hierarchy with a densely instrumented extension: PINGU 42
43 Search for Pointsources: The Method 4282 events (small sample) Source background 2-3 background: atmospheric ν Search for event excess within 2-3 somewhere in the Northern sky from list of candidate sources Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 43
44 The Statistics Problem If you search long enough you will for sure get an excess at some point I only believe in statistics that I doctored myself Winston Churchill Example: Expect 3 events background in a search window, but see 7. How significant is this? 0.25 <n> = w(n>6) = 3,3 % Already for about 30 search windows the probability to see 7 or more events in any window is about 60% for background only. Significance is determined by ~10000-fold simulation of measurement Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 44
45 Point Source Search IC Hottest spot in South: p-value * 10-6 (pre-trial) Ra: Dec: N s =16.16 γ =2.34 p-value * ~ 9.3% (post-trial) * p-value for background only Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 45
46 Improving Statistical Significance pre-defined source positions pre-defined time-window stacking of pre-defined sources Pre-Definition with multi-messenger information of optical, gamma, X-ray, radio telescopes Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 46
47 Intense flashes of gamma rays Duration some seconds highly-relativistic jet ( fireball ) Search for neutrinos which are in time and direction consistent with GRB GCN: The Gamma-ray Coordinates Network Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 47
48 Are GRBs the main sources of Cosmic Rays? 225 GRB... no coincidences observed Standard Fireball Models excluded [Nature 484 (2012) 351] Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 48
49 Extremly High Energy (EHE) Neutrinos GZK threshold ~ ev Search for high number of Cherenkov photons = NPE θ = zenith angle Search region upward downward up-going down-going Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 49
50 Search for cosmogenic neutrinos with data. Aug. 8, ± 0.14 PeV deposited Jan. 3, ± 0.14 PeV energies Two shower type events found in 616 days of IceCube observations. Neutrino energies could be higher than deposited energies, if neutral current interaction. Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 50
51 The Muppet Show 1.04 ± 0.14 PeV 1.14 ± 0.14 PeV 2.00 ± 0.26 PeV A theoreticians view (Francis Halzen, IceCube PI) : A detection of 1 neutrino is interesting 2 is evidence and 3 is a spectrum! Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 51
52 Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 52. Follow-up Search for contained and semi-contained events find contained events below the energy threshold of the Bert-and-Ernie analysis same dataset, 662 days of livetime Use outer IceCube layers as incoming track veto Additional atmospheric muon veto Sensitive to all flavors in region above ~ 60TeV Muon background can be estimated from data μ Veto νμ Effective volume μ
53 Some example events declination: deposited energy: 82TeV declination: -0.4 deposited energy: 71TeV declination: 40.3 deposited energy: 253TeV Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 53
54 Excess of HE Starting Tracks Phys. Rev. Lett. 113, Significance about 5.7 σ First observation of astrophysical flux of high energy neutrinos Starting events depositing >60 TeV using 3 years of data, events up to ~2 PeV Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 54
55 Global Fit to 6 Different Measurements Simplest model: flux and flavor ratio Results: Flavor ratio compatible with prompt < 2 ERS Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 55
56 no significant correlation with galactic plane p-value: 7% Skymap equatorial coordinates Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 56
57 Blazars or GRB as Sources? Compare directions of the high energy ν μ with directions of Blazars observed by Fermi Satellite at high γ luminosity 17% atmost from Blazars Even more stringent for GRB: from analysis of 506 GRBs in four years it was found that no more than 1% of the high energy neutrinos could come from GRB 1% atmost from GRBs Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 57
58 Anything new down there? Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory
59 CONCLUSION? Alles Wissen und alle Vermehrung unseres Wissens endet nicht mit einem Schlußpunkt, sondern mit Fragezeichen Hermann Hesse. imagine Sisyphos to be happy» il faut imaginer Sisyphe heureux«a.camus Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 59
60 Coll. Ljubljana, H.Kolanoski - IceCube Neutrino Observatory 60
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