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TeV II Particle Astrophysics

TeV II Particle Astrophysics. Summary comments. Outline. Introduction: Cosmic-ray spectrum Multi-messenger astronomy TeV astronomy g -ray astronomy n astronomy Gravitational-wave astronomy New detectors. Extra-galactic component ?. n F( n ) for cosmic rays. Air Showers. DIRECT.

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TeV II Particle Astrophysics

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  1. TeV II Particle Astrophysics Summary comments Tom Gaisser

  2. Outline • Introduction: Cosmic-ray spectrum • Multi-messenger astronomy • TeV astronomy • g-ray astronomy • n astronomy • Gravitational-wave astronomy • New detectors Tom Gaisser

  3. Extra-galactic component ? nF(n) for cosmic rays Air Showers DIRECT Knee Ankle Tevatron LHC Tom Gaisser

  4. 1020 eV proton 16 joules energy Kinetic energy of Yanick Noah’s second serve But momentum of a snail Macroscopic energy in a microscopic particle No known astrophysical sources “seem” able to produce such enormous energies 1/ km2/ century 3000 km2 -> 30 events / year Simon Swordy University of Chicago J. Cronin, Aug 29

  5. Observations I: Spectrum Observations – I: Spectrum Knee 2nd Knee Dip GZK? P. Blasi, Aug 28

  6. B. Peters, Nuovo Cimento 22 (1961) 800 B. Peters on the knee and ankle <A> should begin to decrease again for E > 30 x Eknee Peters cycle: systematic increase of < A > approaching Emax

  7. 30 Rigidity-dependence • Acceleration, propagation • depend on B: rgyro = R/B • Rigidity, R = E/Ze • Ec(Z) ~ Z Rc • rSNR ~ parsec •  Emax ~ Z * 1015 eV • 1 < Z < 30 (p to Fe) • Slope change should occur within factor of 30 in energy • With characteristic pattern of increasing A • Problem: continuation of smooth spectrum to EeV

  8. KASCADE composition at the knee

  9. UHECR J. Cronin, Aug 29

  10. GZK feature recovery (depends on source density) Distant sources Contribution depends on evolution and propagation in Bextra-galactic Nearby sources clustering, anisotropy? (de) constructing the extra-galatic spectrum dip (due to pair production) End of Galactic population (not shown) Doug Bergman et al. (HiRes), Proc 29th ICRC, 7 (2005) 315

  11. Transition < 1018 eV Transition at 1019 eV N Busca, WG-4, Aug 29 Allard et al. astro-ph/0605327

  12. HiRes new composition result: transition occurs before ankle Original Fly’s Eye (1993): transition coincides with ankle Stereo or 0.3 EeV ? 3 EeV G. Archbold, P. Sokolsky, et al., Proc. 28th ICRC, Tsukuba, 2003 Where is transition to extragalactic CR?

  13. A & B galactic components + extra-galactic Hillas, J.Phys.G 31 (2005) R95-131 B E-G A

  14. De Marco, Blasi and Olinto 2006 15 years of Operation of Auger South Density of sources of extra-galactic cosmic rays determines post-GZK flux

  15. UHE/EHEn fluxes GZK (hard, high Emax) - Kalashev et al 2002 GZK (strong evolution) - ibid GZK (standard) - Yoshida Teshima 1993 TD - Sigl et al 1999 Zburst – Yoshida et al 1998

  16. Multi-messenger Astronomy • Particle, Nuclear & Gravitational Wave Astrophysics in the decadal survey (2000) • Theme: multi-messenger astronomy (Barwick) • Cosmic rays (Blasi, Cronin) • Gamma-ray astronomy (Lorenz, Krennrich) • Neutrino astronomy (Coyle, Hanson) • Gravitational waves (Cornish, Weiss) • Dark Matter

  17. Future: … transition to a ‘multi-messengers’ approach • -IceCube as a ( half ) – All-Sky-Monitor in neutrino: • - Filed of view: northern sky • - High duty cycle • Idea: use neutrinos in order to trigger gamma-ray telescopes • (see E. Bernardini, “The multimessenger approach..” Barcelona, 07.06) • -Critical points under discussion: • - selection of the sources: the phenomenology is limited • - statistical interpretation of possible coincidences: • -ray flare rate, catalogue … • - blindness of the data: • minimal impact with off-line analysis • Status: TEST run between AMANDA and Magic of 3 months approved. Elisa Resconi, WG-4, Aug 29

  18. KIFUNE PLOT E Lorenz, Aug 28 2006 Mkn180 PG1553 NOT ALL SOURCES IN INNER GALACTIC PLANE SHOWN ALL SOURCES HAVE SPECTRA EXTENDING ABOVE 1 TEV RARELY SPECTRA EXTEND ABOVE 10 TEV (CRAB->80 GEV MANY AGNS HAVE A SOFT SPECTRUM

  19. Study of Galactic Sources with H.E.S.S. Dieter Horns* for the H.E.S.S. collaboration http://www.mpi-hd.mpg.de/hfm/hess *Institute for Astronomy and Astrophysics, Eberhard Karls Universität Tübingen WG-1, Aug 28

  20. VERITAS-2 at basecamp of FLWO F Krennrich --> construct VERITAS-4 at FLWO TeV Particle Astrophysics II

  21. VERITAS-4 at basecamp of FLWO Construction finished by Dec. 2006, operate 2007-2009, move in 2009 F Krennrich TeV Particle Astrophysics II

  22. E Lorenz, Aug 28 Tom Gaisser

  23. SCAN OF THE NORTHERN TEV SKY BY MILAGRO 6 s DECL. RIGHT ASC. HOTSPOT AT RA 79.6, DEC 25.8 CLOSE TO EGRET 3EGJ0320+2556 4.5 s Tom Gaisser

  24. A Closer Look at the Galactic Plane Significance GP diffuse excess clearly visible from l=25° to l=90° Cygnus Region shows extended excess FCygnus ~ 2 x Fcrab 120 square degrees l (65,85), b (-3,3) Flux (> 12.5 TeV) = 1.59 ± 0.30stat ± 0.32sys x 10-11 cm-2 s-1 sr-1 (excluding new source & assuming E-2.6) Madison - August 2006

  25. at ~100 TeV • “Best bet” Sources • nm detection probability Chuck Dermer’s rule of thumb Gaisser, Halzen, Stanev 1995 km-scale n telescope (IceCube) has best detection probability near 100 TeV Number of nm detected: 100 TeV Tom Gaisser Dermer & Atoyan NJP 2006

  26. Is Cygnus region detectable in n ? • I (>12.5 TeV) = 1.6 x 10-11 (cm2 s sr)-1  nF(n) = E dN/dlnE = 10-4 erg / (cm2 yr) if (g + 1) = 2.6 (differential spectral index) • Problems • Diffuse source  higher background • Factor 3 reduction due to oscillations Tom Gaisser

  27. g -nConnectiong-ray fluence (extrapolated to 100 TeV) > 10-4 ergs cm-2 required for n detection for optically thin sources [ typically requires few years per source(TG) ] Best bet for detectable neutrino point source with km-scale n detector (IceCube): v from photohadronic processes Blazar AGNs (FSRQs, not BL Lacs) [ few per year (TG) ] Surrounding target radiation field; 1 PeV neutrino GRBs Signatures of hadronic acceleration in GRBs [ few per year (TG) ] Microquasars (?) probably too weak Best bet for detectable diffuse neutrino sources: GZK neutrinos from cosmological sources of UHECRs (GRBs) Cosmic-ray induced galactic diffuse emission Chuck Dermer’s Summary Tom Gaisser

  28. Effect of oscillations

  29. Sensitivity to sn

  30. AMANDA • 677 analog OMs deployed along 19 strings • 10 strings 1997 (AMANDA B10) • 3 strings 1998 (AMANDA B13) • 6 strings 2000 (AMANDA II) • Analog PMT signals using electrical and optical transmission lines. • 200 m diameter, 500 meters height; AMANDA II encompasses 20 Mton instrumented ice volume. • AMANDA will remain operational and form IceCube Inner Core Detector for low E physics (~ 100 GeV) • IceCube surrounding strings provide effective veto – lower background and can push AMANDA energy threshold down. • Conventional TDC / ADC technology for AMANDA has been entirely replaced by TWR system. • Beginning 2007 season, AMANDA / IceCube data streams will be conjoined; detector subsystems will share trigger information. K Hanson

  31. Point Sources and Diffuse Fluxes in the IceCube Era * AMANDA-B10 average flux upper limit [cm-2s-1] AMANDA-II IceCube 1/2 year sin(d)

  32. Not always E-2 Energy range of limits change with spectral index , E- Higher energies for flatter spectra Model-dependence of limit E-1 E-3 log(dN/dE*E2) E-2 log(E/GeV) Julia Becker, Universität Dortmund TeV particle astrophysics, Madison

  33. IceCube Events IceTop /w/ Reco Neutrino Candidate Joint IceTop-InIce

  34. Downgoing muon M Bouwhuis WG-4, Aug 29

  35. Atmospheric muon bundles M Bouwhuis WG-4, Aug 29

  36. GW N Cornish, Aug 30 Tom Gaisser

  37. Tom Gaisser N Cornish, Aug 30

  38. ZEPLIN I EDELWEISS DAMA World-best limit today ZEPLIN 2 CDMS II 2007 XENON 10 SuperCDMS 25kg 25 kg of Ge 2011 SuperCDMS Phase B 150 kg of Ge 10-45 cm2 SuperCDMS Phase C 1000 kg of Ge Indirect searches: n from Sun 10-46cm2 10-47cm2 WIMP Dark Matter Direct searches: Cabrera, Aprile Indirect searches: Ullio Tom Gaisser

  39. New experiments for knee to ankle • KASCADE-Grande (e / m) • Tunka (air Cherenkov) • TALE (hybrid) • LOPES (radio) • IceCube ( e / energetic m ) • Primary E to ~1017 eV now • to ~1018 eV when complete Tom Gaisser

  40. FD Aperture…SD Aperture…Hybrid aperture: single-tank TOT Hybrid aperture is determined by FD since SD single-tankTOT trigger has low threshold. (Observatory trigger (T3) for hybrids is initiated by the FD and tank triggers are collected) (aperture as of October, 2004) Bellido et al. (Auger Collab) 29th ICRC HE15 (2005)

  41. A HaungsAug 28 Tom Gaisser

  42. LOPES & KASCADE Grande (not corrected for geomagnetic angle) Haungs et al. 2006; Badea et al. 2005; Apel et al. (LOPES coll.), Astropart.Phys. 2006, in press

  43. Next step: Radio @ AUGER First on-site tests starting this fall! LOFAR @ Auger

  44. Tom Gaisser

  45. Air Showers with IceCube IceTop Tom Gaisser

  46. What we have now 2006 (16 stations + 9 strings): 0.5% of full IceCube Tom Gaisser

  47. Waveforms and lateral distribution A B A B C C Tom Gaisser X. Bai

  48. Fluctuations: Between 2 DOMs Between two tanks 1. Fluctuations in response of a tank to energy deposition is smaller than intrinsic fluctuations in the shower front 2. Using two nearby tanks, we can measure time & density fluctuations and assign the weights in maximum-likelihood fittings. X. Bai Tom Gaisser

  49. KASCADE-Grande IceCube Muon / electron ratio reflects nuclear composition of primaries Calculations of Ralph Engel, presented at Aspen, April, 2005 Tom Gaisser

  50. Astroparticle Physics:Radio Detection of Particles • Cosmic Rays in atmosphere: • Geosynchrotron emission (10-100 MHz) • Radio fluorescence and Bremsstrahlung (~GHz) • Radar reflection signals (any?) • VLF emission, process unclear (<1 MHz) • Neutrinos and cosmic rays in solids: Cherenkov emission (100 MHz - 2 GHz) • polar ice cap (balloon or satellite) • inclined neutrinos through earth crust (radio array) • CRs and Neutrinos hitting the moon (telescope)

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