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Cosmic Accelerators Astrophysics with High Energy Particles

Cosmic Accelerators Astrophysics with High Energy Particles. Graduiertenkolleg “Physik an Hadronen-Beschleunigern” Klausurtagung, 17.10.2006. Thomas Lohse Humboldt University Berlin. The Cosmic Ray Spectrum. E 2.7 , mostly protons. Knee. solar modulation. transition to

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Cosmic Accelerators Astrophysics with High Energy Particles

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  1. Cosmic Accelerators Astrophysics with High Energy Particles Graduiertenkolleg “Physik an Hadronen-Beschleunigern” Klausurtagung, 17.10.2006 Thomas Lohse Humboldt University Berlin

  2. The Cosmic Ray Spectrum E2.7, mostly protons Knee solar modulation transition to heavier nuclei E3.1 mostly Fe? Ankle transition to lighter nuclei? Power Laws Shock Acceleration predicts FSource E2 ? Direct Measurements Discovery Balloon Flight Victor Hess, 1912 EAS Detectors

  3. Open questions after 90 years • What and where are the sources? • How do they work? • Are the particles really accelerated?... • …or due to new physics at large mass scales? • And how do cosmic rays manage to reach us?

  4. p   p  0 e  Inverse Compton (+Bremsstr.) radiation fields and matter Production in Cosmic Accelerators protons/nuclei electrons/positrons

  5. Primary (Hadron,Gamma) Air Shower Fluorescence Detector Fluorescence Č Hadron-Detector Č-Telescope Scintillator or Water Č  R&D Radio-Detection Acoustic-Detection Atmospheric  (4)  ,e,  InstrumentedWater / Ice Primary  (4) Experimental Techniques ( E  10 GeV )

  6. Outline • Cosmic rays beyond the ankle • Neutrinos from cosmic ray sources • Gammas from cosmic ray sources Outline • Cosmic rays beyond the ankle • Neutrinos from cosmic ray sources • Gammas from cosmic ray sources

  7. p(100 EeV)  p  E3FE cut-off reprocessed p 1018 1019 1020 EeV Greisen-Zatsepin-Kuzmin Cut-Off: Energy loss in cosmic microwave background (CMB) p(100 EeV) + (CMB)  p + , n +  p beyond ankle p below ankle  isotropized in B-fields

  8. AGASA HIRes Fly’s Eye model fit to HIRes data triplet Spectra consistent allowing for 30% systematic energy shift… AGASA: surface detector array HIRes: fluorescence light detector no GZK cut-off? AGASA

  9. The Pierre Auger Project 3000 km2 Hybrid Detector 4 Fluorescence Sites 1600 Water Č-Detectors  75% installed AGASA

  10. Clean EeV Hybrid Events contemporaneous atmospheric monitoring Energy Calibration of Surface Detectors statistically limited up to now… 14% duty cycle Present systematics: Calibration 12% Fluorescence yield 15% • calorimetric measurement •  independent of primary composition •  independent of air shower details

  11. Power Law Fit systematic errors First Look at 3EeV Energy Spectrum (from surface detector array) Data: Jan. 2004 – Jan 2005 Exposure: 1750 km2 sr yr  AGASA + 7% Events: 3525

  12. AUGER best fit preliminary Calibration uncertainty

  13. Cosmic rays beyond the ankle • Neutrinos from cosmic ray sources • Gammas from cosmic ray sources

  14. The Main Players presently: • Amanda/IceCube, South Pole Ice • BAIKAL, Water of Lake Baikal • + future Mediterranean detectors IceCube (in construction) South Pole Dome AMANDA Summer camp 1500 m Amundsen-Scott South Pole Station 2000 m [not to scale]

  15. 1:1:1 flavour flux ratio AMANDA 1: B10, 97, ↑μ 2: A-II, 2000, unfold. 3: A-II, 2000, casc. 4: B10, 97, UHE Baikal 5: 98-03, casc. upward  (2 coverage) atmospheric  horizontal E2-Flux Limit vertical preliminary IceCube 3 years all-flavour limits Search for Diffuse Cosmic Neutrinos  add directional & temporal constraints …

  16. 90 Significance Sky Map 24h h max. excess from random skymaps Maximum Excess  3.4 3.4 92% 90 Unbinned Search for Clusters AMANDA 2000-2003 preliminary

  17. time window: 40 / 20 days • angular bin: 2.25°-3.75° • fixed a priori sliding window events time AMANDA Search for Transient Sources 12 Objects tested (over 4 years), no triplets found … BUT … …

  18. The first cosmic ray neutrino ??? 66 day triplet 5 events dublet window background WHIPPLE E>0.6TeV HEGRA E>2TeV Orphan -flare (not seen in X-rays) AMANDA – 1ES1959+650 – 2.25o search bin size revisited a posteriori • Statistical significance hard to tell … but promising! • Lessons learned: Multimessenger & multiwavelength studies important. Use -ray flares (not only X-rays)…

  19. Cosmic rays beyond the ankle • Neutrinos from cosmic ray sources • Gammas from cosmic ray sources

  20. Veritas MAGIC in construction H.E.S.S. CANGAROO III Cherenkov Telescopes (3rd Generation)

  21. 3.1. Supernovae

  22. But what about hadrons (protons and nuclei)? Pulsar Wind Nebula: Electron wind from centralpulsar heats the cloud Synchrotron radiation The Standard Candle for TeV -Astronomy Crab Supernova 1054 a.D. d = 2 kpc optical 1 lightyear

  23. Cassiopaeia A Supernova 1658 a.D. d = 2,8 kpc X ray picture • “Shell Type” SNR: • no electron wind from pulsar • gamma signal from shell regions not totally drowned in that of electron wind • good source class to observe hadron acceleration

  24. RX J1713.73946 RX J1713.73946 E 210 GeV H.E.S.S. 2004 E  210 GeV H.E.S.S. 2004 resolution resolution First Resolved Supernova Shells in -Rays RX J0852.04622 H.E.S.S. 2005 E 500 GeV Strong correlation with X-ray intensities • SN-Shells are accelerating particles up to at least 100TeV! • But are these particles protons/nuclei or electrons?

  25. Matter Density B Ee Stars Dust Cosmic Proton Accelerators Cosmic Electron Accelerators CMB B Ee Inverse Compton Synchrotron Radiation 0 Synchrotron Radiation of Secondary Electrons Electron or Hadron Accelerator? radio infrared visible light X-rays VHE -rays E2 dN/dE log(E)

  26. B7,9,11G 2.0,2.25,2.5 EGRET 2.0 B10G Electron accelerator fits for RX J1713.73946: • Continuous electron injection over 1000 years • Injection spectrum: power law with cutoff H.E.S.S. • large  & injection rate  bremsstrahlung important • needs tuning at low E • IC peak not well described • B-field low for SNR shell

  27. RX J1713.73946 H.E.S.S. Proton accelerator fit: • Continuous proton injection over 1000 years • Injection spectrum: power law, index 2 • Different cutoff shapes & diffusion parameters

  28. 3.2. Inner Glactic Plane 30 ≲l ≲ 30 3 ≲b ≲ 3

  29. Galactic Centre HESS J1745290 HESS J1632478 HESS J1825137 RX J1713.73946 HESS J1616508 HESS J1837069 HESS J1804216 HESS J1745290 HESS J1708410 HESS J1834087 HESS J1813178 HESS J1614518 G0.90.1 HESS J1747281 HESS J1713381 HESS J1634472 HESS J1640465 HESS J1702420 HESS J1804-216 HESS J1834-087 HESS J1640-465 H.E.S.S. Scan of Inner Galactic Plane 5  SNR 3  Pulsar  3  ??? 14 new sources, all extended! Possible counterparts: (plus previously known ones) Resolution

  30. … a new source class: “Dark Accelerators” • extended • hard spectra,  • steady emission TeV-Gamma-Ray Radio X-Ray Five sources known: TeV J20324130 (HEGRA) HESS J1303631 HESS J1614518 HESS J1702420 HESS J1708410 What are these sources? Are they hadron accelerators?

  31. Galactic Centre HESS J1745290 HESS J1632478 HESS J1825137 RX J1713.73946 HESS J1616508 HESS J1837069 HESS J1804216 HESS J1745290 HESS J1708410 HESS J1834087 HESS J1813178 HESS J1614518 G0.90.1 HESS J1747281 HESS J1713381 HESS J1634472 HESS J1640465 HESS J1702420 3.3. Galactic Centre

  32. Systematic pointing error Chandra GC survey NASA/UMass/D.Wang et al. Chandra GC survey NASA/UMass/D.Wang et al. CANGAROO (80%) CANGAROO (80%) Sgr A East SNR H.E.S.S. (95%); MAGIC similar H.E.S.S. H.E.S.S. Whipple (95%) Whipple (95%) Radio Contour Contours from Hooper et al. 2004 Sgr A* Radio Galactic Centre: A pointlike TeV- source • Astrophysical Source Candidates: • 3106 M⊙black hole Sgr A • EMF close to rotating black hole • Accretion shocks • Supernova Remnant Sgr A East • Expanding shock waves

  33. … or maybe dark matter annihilation ? Crab GC MAGIC H.E.S.S. • no visible cut-off  rather large mass • measured flux  large cross-section and/or DM density 20 TeV Neutralino 20 TeV Kaluza Klein particle … unlikely !

  34. Galactic Centre Neighbourhood SNR G0.90.1 HESS J1747281 Galactic Centre HESS J1745290 EGRET GeV--sources ~150 pc

  35. HESS J1745290 Galactic Centre Neighbourhood ...point sources subtracted • first resolved detection of diffuse TeV--radiation • cosmic rays (hadrons) interacting with molecular clouds molecular clouds density profiles ~150 pc

  36. diffuse radiation expected flux for CR spectrum observed on earth Cosmic Ray Spectrum at the GC... is very different from the one at earth Cosmic rays are much harder and have 3 larger density around the GC Possible reason: Close-by source population Possibly single SN-explosion

  37. 3.3. Active Galaxies

  38. Blazars • General Active Galactic Nuclei (AGN): • Supermassive black holes, M  109 M • accretion disk and relativistic jets • Blazar-Typ: Jet points towards the earth • Doppler-boost  TeV -radiation

  39.  e+ e-  dN/dE dN/dE E E Absorption in (infrared) extragalactic background light (EBL) (TeV) + (EBL)  e+e- Measurement of EBL ( Cosmology) Physics of compact objects, acceleration/absorption in jets,…

  40. Cut-off Energy and -Ray Horizon PG 1553113

  41. EBL Hardest plausible source spectrum  = 1.5 EBL Unfolding of Measured Spectra Too much EBL 1 ES 1101  = 2.9±0.2 H 2356 (x0.1)  = 3.1±0.2 H 2356 (x 0.1) G = 3.1±0.2 Preliminary

  42. excluded by H.E.S.S. Assumed shape for rescaling H.E.S.S. upper bound fromspectral shapes of 1ES 1101-232 (z = 0.186) H 2356-309 (z = 0.165) New Upper Bound on EBL Density EBL density seems 2 smaller than expected! Little room for EBL sources other than galaxies (early stars…) Direct IRTS Measurements Upper Limits Lower Limits (Galaxy Counts)

  43. Summary • Cosmic ray puzzle persists…but is under pressure by massive attack from EAS-arrays, - and -telescopes • Progress in understanding knee, ankle and GZK-region AUGER data disfavour small scale anisotropies • Cosmic -detection in multi-messenger campaigns? • Neutrino astronomy might start sooner than expected! • Major break-through in TeV--astronomy • supernova shells are 100TeV accelerators • large population of extended galactic TeV sources discovered • first microquasar-candidates established as TeV accelerator • diffuse galactic TeV emission (Milagro, H.E.S.S.) • TeV- from Active Galactic Nuclei at large red-shifts, …

  44. Supernovae AGN Pulsars Dark Accelerators Microquasars Black Holes Gamma Ray Bursts The Cosmic Accelerator Cocktail ?

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