English
 
Help Privacy Policy Disclaimer
  Advanced SearchBrowse

Item

ITEM ACTIONSEXPORT
Add to Basket
  Local TagsRelease HistoryDetailsSummary

Released
Conference Paper

Discovery of the Binary Pulsar PSR B1259-63 in VHE Gamma Rays

MPS-Authors
/persons/resource/persons30290

Beilicke,  M.
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

/persons/resource/persons30670

Khélifi,  Bruno
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

/persons/resource/persons30798

Masterson,  Conor
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

/persons/resource/persons30397

de Naurois,  M.
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

External Resource
No external resources are shared
Fulltext (restricted access)
There are currently no full texts shared for your IP range.
Fulltext (public)
There are no public fulltexts stored in PuRe
Supplementary Material (public)
There is no public supplementary material available
Citation

Schlenker, S., Beilicke, M., Khélifi, B., Masterson, C., de Naurois, M., & Rolland, L. (2005). Discovery of the Binary Pulsar PSR B1259-63 in VHE Gamma Rays. In F. A. Aharonian, H. J. Völk, & D. Horns (Eds.), High energy gamma-ray astronomy: 2nd International Symposium on High Energy Gamma-Ray Astronomy, Heidelberg, Germany, 26 - 30 July 2004 (pp. 341-346). Melville, NY, USA: American Institute of Physics.


Cite as: https://hdl.handle.net/11858/00-001M-0000-0011-8A68-4
Abstract
The detection of the binary system PSR B1259-63 / SS 2883 with the High Energy Stereoscopic System (H.E.S.S.) of four imaging atmospheric Cherenkov telescopes is reported. PSR B1259-63, a radio pulsar with a highly eccentric orbit around a very luminous, massive star was observed around its periastron passage in February/March 2004. Very high energy (VHE)gamma-ray emission has been predicted to be produced in the interaction region of the pulsar wind and the photon field of the star, where accelerated electrons are believed to undergo InverseCompton scattering. The flux of the gamma-ray emission should then depend on the pulsar orbital phase. Gamma-ray signals with a significance >10 σ were detected above an energy threshold of ~380GeV. The measured flux varies significantly on timescales of days. The spectrum derived from the pre-periastron data has a flux level of 7% of the Crab Nebula flux and a photon index of Γ =2.7± 0.3stat.