High Energy Neutrino Astronomy
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1 High Energy Neutrino Astronomy VII International Pontecorvo School Prague, August 2017 Christian Spiering, DESY Zeuthen
2 Content Lecture 1 Scientific context Operation principles The detectors Atmospheric neutrinos Lecture 2 Search for steady point sources Search for transient sources and the multi-messenger concept The diffuse flux of cosmic neutrinos Search for Dark Matter (indirect) and magnetic monopoles A look to the future
3
4 Neutrinos: a synoptic spectrum underground optical: - deep water - deep ice - air showers - radio - acoustics
5 First ideas 1960 K. Greisen F. Reines M. Markov (with I. Zheleznykh) discuss ways to detect cosmic high-energy neutrinos deep underground or underwater.
6 Moisej Markov Bruno Pontecorvo M.Markov,1960: We propose to install detectors deep in a lake or in the sea and to determine the direction of charged particles with the help of Cherenkov radiation Proc ICHEP, Rochester, p. 578.
7 Physics with neutrino telescopes Search for the sources of high-energy cosmic rays with neutrinos Dark Matter and Exotic Physics WIMPs Magnetic Monopoles and other superheavies Violation of Lorentz invariance Neutrino and Particle Physics Neutrino oscillation studies Charm physics, cross sections at highest energies, Supernova Collapse Physics MeV neutrinos in bursts early SN phase, neutrino hierarchy,... Cosmic Ray Physics Spectrum, composition and anisotropies
8 Physics with neutrino telescopes Search for the sources of high-energy cosmic rays with neutrinos Dark Matter and Exotic Physics p + WIMPs target Magnetic Monopoles and other superheavies Violation of Lorentz invariance Neutrino and Particle Physics Neutrino oscillation studies Charm physics, cross sections at highest energies, Supernova Collapse Physics MeV neutrinos in bursts early SN phase, neutrino hierarchy,... Cosmic Ray Physics Spectrum, composition and anisotropies + + e + + e + at source: e : : = 1:2:0 at Earth: e : : = 1:1:1
9 Charged cosmic rays vs. gamma rays vs. neutrinos Charged particles,
10 Gamma Rays: hadronic or electromagnetic origin? Hadronic: Electromagnetic (Inverse Compton Scattering):
11 An electron-hadron accelerator -TeV
12 An electron accelerator -TeV
13 E 2 dn/de radio infrared visible light X-rays VHE -rays Proton Accelerators Electron Accelerators C telescopes Fermi Stars Dust 0 CMB Synchrotron Radiation Inverse Compton ln (E)
14 The viewing range 99% of the Universe AGN Nearby Clusters % of the Universe Local Group Milky Way
15
16 Detection deep under-ground/-water/-ice
17 Atmospheric neutrinos
18 Astrophysical ( cosmic ) neutrinos
19 How to detect high energy neutrinos The traditional way: muons from CC interactions
20 Neutrino cross sections
21 Neutrino cross sections
22 Neutrino cross sections W
23 Neutrino cross sections slide R. Nahnhauer
24 Neutrino cross sections Only way to distinguish and anti-!
25 Muon energy loss 0.002
26 Muon energy loss and range in water
27 Number of muon events per detection area A µ and observation time T E,min de E, P E,E e E N Z AT,min E N E,,min Neutrino flux spectrum tot A
28 Number of muon events per detection area A µ and observation time T E,min de E, P E,E e E N Z AT,min E N E,,min Neutrino flux spectrum tot A Probability to produce a detectable (E >E min ) muon P 10-3 E,min =1GeV E 1TeV,min 1 TeV LogE (GeV)
29 Number of muon events per detection area A µ and observation time T E,min de E, P E,E e E N Z AT,min E N E,,min Neutrino flux spectrum tot A Probability to produce a detectable (E >E min ) muon Earth transparency mto HE neutrinos P Earth 1 TeV 10 TeV 100 TeV deg
30 Neutrino effective area for IceCube cut against atm.
31 Pointing accuracy
32 Tracks, showers, double bang events
33 Two Detection Modes: tracks and cascades + A + e, e, + Angular resolution < 1 de/dx gives E within factor 2-3 X X + Angular resolution 100 TeV Energy resolution ~ 15%
34 Two Detection Modes + A + e, e, + Angular resolution < 1 de/dx gives E within factor 2-3 X X + Angular resolution 100 TeV Energy resolution ~ 15%
35
36 The (first) pioneer
37 1978: 1.26 km³ 22,698 OMs 1980: 0.60 km³ 6,615 OMs 1982: km³ 756 OMs 1988: km³ 216 OMs DUMAND-II
38 Operating neutrino telescopes Antares Baikal AMANDA IceCube
39
40 NT200 in Lake Baikal: the (second) pioneer 8 strings 192 PMTs Height 72 m Diameter 42 m
41 1994: The first Underwater Neutrino
42 A textbook underwater neutrino event 1996
43 V. Bertin - CPPM - Roma 2500m ANTARES 885 PMTs 12 strings Operating in final configuration since m 70 m
44 IceCube Neutrino Observatory IceTop air shower detector 81 pairs of water Cherenkov tanks 1450m 2450m 2820m IceCube 86 strings including 8 Deep Core strings 60 PMT per string DeepCore 8 closely spaced strings Threshold: IceCube DeepCore ~ 100 GeV ~10 GeV
45 IceCube Neutrino Observatory Events per year: - Downgoing muons ~ Atmospheric neutrinos ~ 100, m - Cosmic neutrinos ~ m 2820m Threshold: IceCube DeepCore ~ 100 GeV ~10 GeV
46 46 institutions from 12 countries
47 46 institutions from 11 countries
48 Neumayer Amundsen-Scott Vostok Mirny Mc Murdo Concordia Dumont D Urville
49
50 The Amundsen-Scott Station South Pole Station Building Astronomy Sector IceCube AMANDA skiway
51 Infrastructure and support: NSF / Raytheon Polar Services NSF/ Lockheed Martin (ASC)
52
53 The drill camp - 5 MW power - 16 m³ Kerosine per hole
54
55
56
57
58
59 Construction IC Season IC Season IC Season IC Season IC Season IC Season IC Season
60 Besseres Bild 18.Dec. 2010: the last string
61 The Digital Optical Module (DOM) Penetrator HV Divider DOM Mainboard LED Flasher Board Mu-metal grid Delay Board PMT RTV gel Glass Pressure Housing Failure rate < 2 DOM/year (out of > 5000!)
62 IceCube Laboratory and Data Center
63
64
65 Performance
66 Ice properties Scattering coefficient Much stronger scattering than in water! Absorption coefficient Up to 2 times less absorption than in water
67 CHERENKOV PHOTONS are quickly diffused by light scattering
68
69 Atmospheric neutrinos
70
71
72 SPECTRUM AT HIGH ENERGIES (> 100 GEV)
73 Atmospheric muon neutrinos in IceCube de /dx E E (0) E Measured de/dx Monte Carlo: Correlation between de/dx and E Phys.Rev.D83:012001,2011 and arxiv:1010:3980
74 IceCube: Spectrum of atmospheric neutrinos proton c,(b) prompt π e,μ νe,μ μ e νμ νμ νe conventional Phys.Rev. D91 (2015) )
75 IceCube: Spectrum of atmospheric neutrinos.. and ANTARES arxiv: Phys.Rev. D91 (2015) )
76 Measurement of atmospheric e Signature: cascade events Subtract NC events and background Phys. Rev. Lett. 110 (2013) and arxiv:
77 Impact of non-atmospheric (i.e. cosmic) neutrinos at > 100 TeV
78 Impact of non-atmospheric (i.e. cosmic) neutrinos at > 100 TeV
79 OSCILLATION PHYSICS
80 Oscillations of atmospheric neutrinos Vertically upward Muon neutrino survival probability cosmic ray Earth L q Horizontal
81 DeepCore: Oscillations for atmospheric neutrinos (E < GeV) Consistent and competitive with accelerator-based measurement Different energy range and baseline than for accelerator studies!
82 IceCube: search for sterile neutrinos (E > 1 TeV) MSW resonance-like transition of atm. to s at high energies Sensitive to mixing angle q 24
83 END OF LECTURE 1
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