Issue |
A&A
Volume 415, Number 2, February IV 2004
|
|
---|---|---|
Page(s) | 483 - 486 | |
Section | Extragalactic astronomy | |
DOI | https://doi.org/10.1051/0004-6361:20034472 | |
Published online | 11 February 2004 |
Strong GeV emission accompanying TeV blazar H1426+428
1
Department of Astronomy, Nanjing University, Nanjing 210093, PR China
2
Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008, PR China
3
National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, PR China
Corresponding author: Y. Z. Fan, yzfan@pmo.ac.cn
Received:
8
September
2003
Accepted:
28
October
2003
For High frequency BL Lac objects (HBLs) like H1426+428,
a significant fraction of their TeV gamma-rays emitted are likely
to be absorbed in interactions with the diffuse IR background,
yielding e pairs. The resulting e
pairs generate one
hitherto undiscovered GeV emission by inverse Compton scattering
with the cosmic microwave background photons (CMBPs). We study
such emission by taking the 1998-2000 CAT data, the reanalyzed
1999 & 2000 HEGRA data and the corresponding intrinsic spectra
proposed by Aharonian et al. ([CITE]). We numerically calculate the
scattered photon spectra for different intergalactic magnetic
field (IGMF) strengths. If the IGMF is about
or
weaker, there comes very strong GeV emission, whose flux is far
above the detection sensitivity of the upcoming satellite GLAST!
Considered its relatively high redshift (
), the detected
GeV emission in turn provides us a valuable chance to calibrate
the poorly known spectral energy distribution of the intergalactic
infrared background, or provides us some reliable constraints on
the poorly known IGMF strength.
Key words: BL Lacertae objects: general / BL Lacertae objects: individual: H1426+428 / cosmology: diffuse radiation / gamma rays: theory
© ESO, 2004
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