1 / 38

High Energy Particles from the Universe The Puzzle of Cosmic Rays

High Energy Particles from the Universe The Puzzle of Cosmic Rays. Universitetet i Bergen, Istitutt for fysikk og teknologi November 10, 2006. Thomas Lohse Humboldt University Berlin. The Cosmic Ray Spectrum. E 2.7 , mostly protons. Knee. solar modulation. transition to

deacon-young
Download Presentation

High Energy Particles from the Universe The Puzzle of Cosmic Rays

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. High Energy Particles from the Universe The Puzzle of Cosmic Rays Universitetet i Bergen, Istitutt for fysikk og teknologi November 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. AUGER best fit preliminary Calibration uncertainty

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

  13. 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]

  14. 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 …

  15. 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

  16. 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 … …

  17. 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)…

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

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

  20. Focal Plane ~ 10 km 5 nsec At 100 GeV ~ 10 Photons/m2 (300 – 600 nm) ~ 120 m 120 m Detection of Cosmic Rays and Gamma Rays  Particle Shower Cherenkov Light Intensity  Shower Energy Image Orientation  Shower Direction Image Shape  Primary Particle

  21. Stereoscopic Observation Technique source direction source image is on image axis  several viewing angles for precise event-by-event source location!

  22. M Source Similar to Meteorite-Showers:

  23. 3.1. Supernovae

  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 200TeV!

  25. 3.2. Inner Glactic Plane 30 ≲l ≲ 30 3 ≲b ≲ 3

  26. 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

  27. … 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?

  28. 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

  29. 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

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

  31. 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

  32. 3.3. Active Galaxies

  33. 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

  34.  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,…

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

  36. 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)

  37. 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 disfavor 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 200TeV 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, …

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

More Related