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13.00 o7 j adams
- 3. View from my office
- 4. More violent universe discovered in other wavelength bands...
- 5. High Energy Particles Brem + ICS + 0 decay ICS Bremsstrahlung + ICS Radio Microwave Infrared Visible Ultraviolet X-ray Gamma Synchrotron ICS ICS
- 6. Leptons Bremsstrahlung Inverse Compton Synchrotron Pair Production Hadrons Pion Decay Nuclear Transitions
- 15. Variability of NGC1275 Brown & Adams, Mon. Not. R. Astron. Soc. (2011)
- 18. Are AGN the source of UHE Cosmic Rays?
- 23. Other neutrino detectors in proportion Super Kamiokande SNO
- 24. Needle in a haystack?
- 29. Electron neutrino/cascade search results
- 30. Examples
- 31. But....
Notas del editor
- 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