Advertisement

Experimental Astronomy

, Volume 20, Issue 1–3, pp 75–83 | Cite as

The INTEGRAL – HESS/MAGIC connection: A new class of cosmic high energy accelerators from keV to TeV

  • P. UbertiniEmail author
Original Article

Abstract

The recent completion and operation of the High Energy Stereoscopic System [1], an array of ground based imaging Cherenkov telescopes, has provided a survey with unprecedented sensitivity of the inner part of the Galaxy and revealed a new population of very high energy gamma-rays sources emitting at E > 100 GeV. Most of them were reported to have no known radio or X-ray counterpart and hypothesised to be representative of a new class of dark nucleonic cosmic sources. In fact, very high energy gamma-rays with energies E > 1011 eV are the best proof of non-thermal processes in the universe and provide a direct in-site view of matter-radiation interaction at energies by far greater than producible in ground accelerators. At lower energy INTEGRAL has regularly observed the entire galactic plane during the first 1000 day in orbit providing a survey in the 20–100 keV range resulted in a soft gamma-ray sky populated with more than 200 sources, most of them being galactic binaries, either Black Hole Candidates (BHC) or Neutron Stars (NS) [5]. Very recently, the INTEGRAL new source IGR J18135-1751 has been identified as the soft gamma-ray counterpart of HESS J1813-178 [18] and AXJ1838.0-0655 as the X/gamma-ray counterpart of HESS J1837-069 [14].

Detection of non-thermal radio, X and gamma-ray emission from these TeV sources is very important to discriminate between various emitting scenarios and, in turn, to fully understand their nature.

The implications of these new findings in the high energy Galactic population will be addressed.

Keywords

Gamma-ray sources High energy emission processes 

Preview

Unable to display preview. Download preview PDF.

Unable to display preview. Download preview PDF.

References

  1. 1.
    Aharonian, F. et al.: Science 307, 1938 (2005)Google Scholar
  2. 2.
    Aharonian, F. et al.: ApJ 636, 777 (2006)Google Scholar
  3. 3.
    Albert, J. et al.: ApJ 637, L41 (2006),Google Scholar
  4. 4.
    Bamba, A. et al.: ApJ 589, 253 (2003)Google Scholar
  5. 5.
    Bird A.J.: ApJ 636, 765 (2006)Google Scholar
  6. 6.
    Brogan, C. et al.: ApJ 629, L105 (2005)Google Scholar
  7. 7.
    Churchwell, E.: A&A Rev. 2, 79 (1990)Google Scholar
  8. 8.
    Condon, J.J. et al.: AJ 115, 1693 (1998)Google Scholar
  9. 9.
    Dulk, P., Slee, O.: AJPh 25, 429 (1972)Google Scholar
  10. 10.
    Helfand, D.J., Becker, R.H., White, R.L.: astro-ph/0505392 (2005)Google Scholar
  11. 11.
    Hertz, P., Grindlay, J.: AJ 96, (1998)Google Scholar
  12. 12.
    Lazendic, J.S. et al.: ApJ 602, L271 (2004)Google Scholar
  13. 13.
    Lebrun, et al.: A&A 411, L141 (2003)Google Scholar
  14. 14.
    Malizia, A.: ApJ 630, L157 (2006)Google Scholar
  15. 15.
    Molkov, S. et al.: Astr. Lett. 30, 534 (2004)Google Scholar
  16. 16.
    Torres, D.F. et al.: Phys. Rept. 382, 303 (2003)Google Scholar
  17. 17.
    Ubertini, P. et al.: A&A 411, L131 (2003)Google Scholar
  18. 18.
    Ubertini, P. et al.: ApJ 629, L109 (2005a)Google Scholar
  19. 19.
    Ubertini, P. et al.: Proceedings–Conference ‘‘A Life with Stars" Amsterdam 22–26/August–Elsevier. (2005b)Google Scholar

Copyright information

© Springer Science+Business Media B.V. 2006

Authors and Affiliations

  1. 1.Istituto di Astrofisica Spaziale e Fisica Cosmica (IASF)RomaItaly

Personalised recommendations