Ultra-High Energy Cosmic Rays & Neutrinos above the Terascale

Transcription

1 Ultra-High Energy Cosmic Rays & Neutrinos above the Terascale Angela V. Olinto A&A, KICP, EFI The University of Chicago

2 Nature sends ev particles QuickTime and a YUV420 codec decompressor are needed to see this picture.

3 Origin of Ultra High Energy Cosmic Rays? Galaxy Jets from Black Holes? Gamma Ray Bursts? QuickTime and a Photo decompressor are needed to see this picture. Neutron Stars? Magnetars?

4 Super Heavy Relics in the Dark Halo of our Galaxy Topological Defects Dark Matter = 23% Universe (85 % matter in U) baryons only 4%

5 Pierre Auger Observatory Goal to determine the origin of Ultra High Energy Cosmic Rays Where are the Sources? SM BHs? NSs? Shocks? Jets? DM? TD? Extragalactic? Galactic? DM halo? Space? What are the sources? Acceleration or Decay? Injection Spectrum? Composition? Protons, Mixed Nuclei? Any Gammas? Neutrinos? Interactions with? cosmic background radiations Atmosphere 100 TeV - 1PeV CM

6 Cosmic Ray Observables SPECTRUM ANISOTROPIES in Sky COMPOSITION MULTIPARTICLE INFO: Gamma rays Neutrinos

7 Cosmic Ray Observables SPECTRUM ANISOTROPIES in Sky COMPOSITION MULTIPARTICLE INFO: Gamma rays Neutrinos

8 Cosmic Ray Spectrum E cm = PeV (E uhecr /ZeV) 1/2 (2A) 1/ discovered by Victor Hess 1938 Pierre Auger discovered Extensive Air Showers (EAS) Energy range: ~10 9 ev to > ev 32 orders of magnitude E -2.7 E -3.1 Ankle (1 particle /km 2 yr) Fixed target RHIC Tevatron LHC 12 orders of magnitude

9 HE Proton sees Cosmic Microwave Background as HE Gamma Rays! p+γ cmb + p + π 0 n + π + Proton Horizon QuickTime and a TIFF (Uncompressed) decompressor are needed to see this picture. WMAP GZK Cutoff Greisen 66, Zatsepin & Kuzmin 66

10 Energy losses for protons Berezinsky et al. 03 redshift pair GZK modification factor: J obs (E,z) = η(e,z) x J injec (E)

11 AGASA High Resolution Fly s Eye No GZK cutoff Consistent w/ GZK cutoff (see PM)

12 AGASA Ground Array High Resolution Fly s Eye 100 km 2 scintillators + muon detectors 2 fluorescence telescopes QuickTime and a GIF decompressor are needed to see this picture.

13 Low Statistics + Systematic Errors sr -1 ] 2 s -1 m -2 [ev AGASA AGASA γ= E>10 : E>10 : ± E>10 : 2.02 ± 1.35 AGASA-15% flux E HiRes +15% sr -1 ] s -1 m no 2.5 σ 18.5 DDM, Blasi, 19 Olinto 2003, 19.5 AP in 20 press log10(e) [ev] HiRes HiRes γ= E>10 : E>10 : ± E>10 : 1.92 ± 1.39 sr -1 ] 2 s -1 m -2 [ev 3 flux E AGASA γ= E>10 : E>10 : ± E>10 : 2.25 ± [ev 3 flux E σ log10(e) [ev] log10(e) [ev] E max = ev DDeMarco, Blasi, AO 03

14 Statistical Challenge To reach > km 2 sr yr Past experiments ~ 10 3 km 2 sr yr AGASA (100 km 2 array scintillators) exposure ~ km 2 sr yr HiRes (Binocular Fluorescence Telescopes) exposure ~ km 2 sr yr PIERRE AUGER Observatory (South) 3,000 km 2 array + 4 Fluorescence Telescopes Aperture 6,600 km 2 sr - reach > 10 4 in 2 years

15 Systematic off-set

16 LARGE QUANTITY Pierre Auger Project HYBRID DETECTOR - use both techniques HIGH QUALITY

17 Auger South Under Construction > 1120 surface detector stations deployed (~930 with electronics and sending triggers) 3 fluorescence buildings complete each with 6 telescopes

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19 tanks aligned seen from Los Leones (zoomed)

20 Auger Water Cherenkov Detector

21 view of Los Leones Fluorescence

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23 corrector lens (aperture x2) segmented spherical mirror ure box er UV pass y curtain 440 PMT camera 1.5 per pixel

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31 electrons/positrons photons muons neutrons

32 A clear Hybrid Event

33 Event Θ = 83 φ = -102 E = 55.2 R= 22 km χ/dof =2.3 NTanks = 61

34 Example Event 1 A moderate angle event Zenith angle ~ 48º, Energy ~ 70 EeV Typical flash ADC trace Detector signal (VEM) vs time (ns) Lateral density distribution Flash Flash ADC ADC traces traces

35 Example Event 2 A high zenith angle event Zenith angle ~ 60º, Energy ~ 86 EeV Flash ADC Trace for detector late in the shower Lateral density distribution Flash ADC traces

36 Event Θ = 87.6 φ = E = 49.2 R= 19 km χ/dof =1.7 NTanks = 37

37 Auger Appetizers SPECTRUM ANISOTROPIES in Sky COMPOSITION MULTIPARTICLE INFO: Gamma rays Neutrinos

38 First Auger South Energy Spectrum Appetizer dn/d(lne) = E*dN/dE E/E~30% E/E~50% 1 Jan 2004 to 5 June 2005 Zenith angles º Current rate - 18,000 / month 10,000 hybrids Total - 150,000 Surface array events (after quality cuts) Total Exposure 1750 km 2 sr yr (~ 1.07 * AGASA)

39 Comparison with HiRes1, AGASA

40 Comparison w/ HiRes1, AGASA-25%

41 Auger (S) x AGASA DeMarco, Blasi, A.O. 03

42 Auger Appetizers SPECTRUM ANISOTROPIES in Sky COMPOSITION MULTIPARTICLE INFO: Gamma rays Neutrinos

43 Sky Map of Data set Galactic coordinates E > ev latitude = -36. Coverage: South + limited North Jan 2004 to June ,000 events - 2,000 Hybrids

44 Cosmic Magnetic Fields Larmor radius: r L = 0.1 Mpc Z -1 (E / ev) (B / 1 µg) -1 Source Extra-galactic B? B < 10-2 µg 0.1 Mpc? γ weak deflection E > ev Halo B? Milky way B ~ µg 10 kpc strong deflection E < ev 1 kpc

45 Charged Particle Astronomy Window of opportunity to ev Maximize the Statistics in this window

46 Expect Anisotropies at Highest Energies Auger-S >60 o Auger-N >60 o Cronin, astro-ph/

47 Angular Correlation Function E > ev 10-6 Mpc Mpc Mpc Mpc -3 Source densities from galaxies to clusters DeMarco et al 06

48 Stronger EG Magnetic Fields E > ev DeMarco et al 06 Source density 10-3 Mpc Mpc Mpc Mpc -3

49 Spectrum DeMarco et al 06

50 Future Entree SPECTRUM ANISOTROPIES in Sky COMPOSITION MULTIPARTICLE INFO: Gamma rays Neutrinos

51 GZK Feature Shape depends on Injection Spectrum, Composition, Magnetic Fields, E max, Source Distribution & Evolution Allard et al 05

52 protons Galactic Cosmic Rays iron Extragalactic Protons Extragalactic Mixed Composition

53 Observed Composition vs. Injected Composition

54 X max x E Composition measurement Allard et al 05 (see Sakurai on PM)

55 Cosmic Rays Observables SPECTRUM COMPOSITION ANISOTROPIES in Sky MULTIPARTICLE INFO: Photons Neutrinos

56 Highest Energy Gamma-rays ~ to ev MAGIC QuickTime and a TIFF (Uncompressed) decompressor are needed to see this picture. Armengaud 06 HESS VERITAS QuickTime and a TIFF (Uncompressed) decompressor are needed to see this picture. QuickTime and a TIFF (Uncompressed) decompressor are needed to see this picture. (see PM)

57 Photon Limits

58 Cosmic Rays Observables SPECTRUM COMPOSITION ANISOTROPIES in Sky MULTIPARTICLE INFO: Photons Neutrinos

59 High Energy Proton sees Cosmic Microwave Background as High Energy Gamma Rays! WMAP p+γ cmb + p + π 0 n + π + n p + e - + ν e QuickTime and a π + µ + + ν TIFF are (Uncompressed) needed to see this decompressor picture. µ µ + e + + ν e +ν µ GZK, Photopion, or Cosmogenic Neutrinos

60 Photo-Pion Mean free paths IRB z=0 CMB z=5 CMB z=1 CMB z= λ(mpc) IRB high z (z>2) pair production + adiabatic loss propagated spectra log(e proton (ev)) Allard et al 06

61 Propagated spectra : Pure proton 10 Q(E) ~ E - β E max = ev protons only different sources evolution Φ(E) E 3 (10 24 ev 2 m -2 s -1 sr -1 ) 1 0,1 strong β=2.4 flat β=2.6 medium β=2.5 Madau et al. 96 β=2.5 HiRes 1 (mono) HiRes 2 (mono) 17 17, , , ,5 log 10 E (ev) Allard et al 06

62 Neutrino fluxes : Pure proton Different Flavors IRB important (Stanev et al 05) E Max (p)= ev TOTAL CMB IR/Optical/UVB En(E) (m -2.sr -1.s -1 ) log 10 E(eV) Allard et al 06

63 Propagated spectra : Mixed composition Q(E) ~ E - β HiRes 1 (mono) 10 E =Z* ev HiRes 2 (mono) max Φ(E) E 3 (10 24 ev 2 m -2 s -1 sr -1 ) 1 0,1 (c) (a) (b) Mixed composition different sources evolution (a) strong β=2.1 (b) madau et al. 96 β=2.1 (c) no evolution β= , , , ,5 log 10 E (ev) Allard et al 06

64 Neutrino fluxes: Mixed composition Strong source evolution Total ν µ from π prod ν e from π prod ν e from n decay Total Proton He Fe En(E) (m -2.sr -1.s -1 ) En(E) (m -2.sr -1.s -1 ) log(e) ev log(e) ev photo-pion flux mainly due to protons Neutron decay flux mainly due to nuclei Allard et al 06

65 Neutrino fluxes : Proton & Mixed E max (see PM) Allard et al 06

66 Earth Skimming ν τ Auger exposure to tau Neutrinos zenith angle > 90 o Neutrino events per year (Cosmogeni c) South 3,000 km 2 North Ext 10,000 Milles 2 North 4,000 Milles 2 Horizontal >~ 0.3 >~ 0.12 Earthskimming 1.3 >~ 5.5 >~ 2.15 Cazon 06 τ ν τ

67 TeV gravity & EHE Tau Neutrinos nice to be next to a Mountain range ν τ TeV Gravity τ τ Standard Model Ahn, Ave, Cavaglia, AO 03

68 Auger North Lamar Detectors in a mile Square Grid 10,000 sq km (4,000 sq miles) Springfield

69 North South Auger-N Auger-S Cronin, astro-ph/

70 Towards Auger North Auger South (3 yr) Auger South + North

71 Muons on the Side What is the problem? Incorrect Model of Detector? Incorrect Model of Showers? Hadronic Interactions? Heavy Primaries? New Physics?

72 Auger North Colorado site 10,000 mile 2 Lamar Springfield 4,000 sq miles

73 Pierre Auger Project South & North to discover Ultra-High Energy Cosmic Ray Sources Begin and Reach beyond Terascale