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The High-Energy Universe
 
View from my office
More violent universe discovered in other wavelength bands...
High Energy Particles Brem + ICS +   0  decay ICS Bremsstrahlung + ICS Radio  Microwave  Infrared  Visible  Ultraviolet  ...
Leptons   Bremsstrahlung Inverse Compton Synchrotron Pair Production Hadrons Pion Decay Nuclear Transitions
Active Galactic Nuclei <ul><li>Objects that emit significant amounts of radiation from non-thermal sources  </li></ul><ul>...
 
 
Basic Emission Mechanisms <ul><li>Radio –synchrotron of electrons in the jet </li></ul><ul><li>Infrared – thermal emission...
What causes the jets? <ul><li>Enormous number of jet models </li></ul><ul><li>Current most promising ideas extract energy ...
Why are AGNs interesting? <ul><li>Some of the most spectacular objects in our universe </li></ul><ul><li>Black holes could...
Observing AGN  over 13 orders of magnitude in energy <ul><li>Blazar PKS 2155-304 </li></ul>GeV TeV X-ray optical HESS and ...
 
Variability of NGC1275 Brown & Adams,  Mon. Not. R. Astron. Soc. (2011)
 
 
Are AGN the source of UHE Cosmic Rays?
 
 
Why detect neutrinos? <ul><li>Because they’re fast.... </li></ul>    +  -  +  +  - e +  e e +  e - e +   ...
IceCube Neutrino Observatory
Other neutrino detectors  in proportion Super Kamiokande SNO
Needle in a haystack?
 
 
 
Plato 428BC-348BC <ul><li>Astronomy compels the soul to look upwards and leads us from this world to another </li></ul>
Electron neutrino/cascade search results
Examples
But....
OPERA results <ul><li>Wait till MINOS says something? Not until 2013+ </li></ul><ul><li>The IceCube collaboration is curre...
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13.00 o7 j adams

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Research 5: J Adams

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  • NGC 4261 NGC 4261 is an elliptical galaxy located behind the Virgo Cluster in the W-cloud. [3] The active galactic nucleus (AGN) contains a 400 million solar mass supermassive black hole (SMBH) [4] with a 800 light-year-wide spiral-shaped disk of dust fueling it. [5] Deep 5 GHz image of the nearby radio galaxy produced by combining multi-configuration data from the Very Large Array. The nucleus at the center is believe to harbor a supermassive black hole. The jets extending east-west fuel the large lobes of radio emission seen clearly in the high quality image. Credit: Teddy Cheung
  • Say some stuff here... About various properties
  • ATOM (HESS optical telescope), RXTE Rossi X-Ray Timing Explorer (RXTE) : , Swift Ssc synchrotron self compton SED of PKS 2155–304. The red butterfly is the Fermi spectrum restricted to the MJD 54704–54715 period, while the black butterfly covers MJD 54682–54743. As a cross check of the fit robustness, the differential flux was estimated in eight limited energy bins by a power-law fit (black circles) and are found to be consistent within 1σ of the global fit, including a clear spectral break at ~1 GeV. The gray points are archival NED data, and the two gray butterflies are EGRET measurements. The solid line is a one-zone SSC model. The dashed and the dot-dashed lines are the same model without electrons above γ 1 and γ 2 , respectively. The VHE part is absorbed with the P 0.45 extragalactic background model described in Aharonian et al. ( 2006a ).
  • Furthermore, the lack of a significant impact on the shape of the SSC component when those electrons are removed indicates that Klein–Nishina effects suppress any significant contribution by those electrons to the emission at ∼TeV energies. These features of this calculation allow that there need not be a correlation between the X-ray and VHE fluxes; and in fact, this is what is observed. In contrast with the 2006 July flare, we do not find any evidence of flux correlation between the X-ray and HESS bands with a Pearson’s r of 0.12 ± 0.1 between these bands.
  • Hubble pretty pictures, one on left composite with xray and radio One on the right shows feedback from filaments
  • First detected as gamma ray source 2008 by fermi-lat
  • veron-cetty and veron catalogue of A
  • Minos jitter between gps clocks fermilab to soudan 700km
  • Transcript of "13.00 o7 j adams"

    1. 1. The High-Energy Universe
    2. 3. View from my office
    3. 4. More violent universe discovered in other wavelength bands...
    4. 5. High Energy Particles Brem + ICS +  0 decay ICS Bremsstrahlung + ICS Radio Microwave Infrared Visible Ultraviolet X-ray Gamma Synchrotron ICS ICS
    5. 6. Leptons Bremsstrahlung Inverse Compton Synchrotron Pair Production Hadrons Pion Decay Nuclear Transitions
    6. 7. Active Galactic Nuclei <ul><li>Objects that emit significant amounts of radiation from non-thermal sources </li></ul><ul><li>(i.e. not stars or dust or thermal gas). </li></ul><ul><li>AGN Zoo: </li></ul><ul><li>Seyfert Galaxies </li></ul><ul><li>Radio Galaxies </li></ul><ul><ul><li>FR1 </li></ul></ul><ul><ul><li>FR2 </li></ul></ul><ul><li>Quasars </li></ul><ul><li>Blazars </li></ul>
    7. 10. Basic Emission Mechanisms <ul><li>Radio –synchrotron of electrons in the jet </li></ul><ul><li>Infrared – thermal emission from the torus </li></ul><ul><li>Optical – thermal emission from the disk </li></ul><ul><li>X-ray-gamma – Inverse Compton </li></ul>
    8. 11. What causes the jets? <ul><li>Enormous number of jet models </li></ul><ul><li>Current most promising ideas extract energy from the accretion flow via magnetic fields </li></ul><ul><ul><li>Extract energy and angular momentum though magnetic field anchored in the disk </li></ul></ul><ul><ul><li>Extract spin energy of the black hole through magnetic fields threading its horizon </li></ul></ul>
    9. 12. Why are AGNs interesting? <ul><li>Some of the most spectacular objects in our universe </li></ul><ul><li>Black holes could be test beds for quantum gravity </li></ul><ul><li>Source of the high-energy cosmic rays? </li></ul><ul><li>Important for structure formation? </li></ul>
    10. 13. Observing AGN over 13 orders of magnitude in energy <ul><li>Blazar PKS 2155-304 </li></ul>GeV TeV X-ray optical HESS and Fermi, ApJ Letters, 696, L150 (2009) EGRET Fermi
    11. 15. Variability of NGC1275 Brown & Adams, Mon. Not. R. Astron. Soc. (2011)
    12. 18. Are AGN the source of UHE Cosmic Rays?
    13. 21. Why detect neutrinos? <ul><li>Because they’re fast.... </li></ul>    +  -  +  +  - e +  e e + e - e +   0   e - e +   
    14. 22. IceCube Neutrino Observatory
    15. 23. Other neutrino detectors in proportion Super Kamiokande SNO
    16. 24. Needle in a haystack?
    17. 28. Plato 428BC-348BC <ul><li>Astronomy compels the soul to look upwards and leads us from this world to another </li></ul>
    18. 29. Electron neutrino/cascade search results
    19. 30. Examples
    20. 31. But....
    21. 32. OPERA results <ul><li>Wait till MINOS says something? Not until 2013+ </li></ul><ul><li>The IceCube collaboration is currently investigating the potential of our data to constrain the velocity of neutrinos at TeV energies… </li></ul>
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