Issue |
A&A
Volume 486, Number 1, July IV 2008
|
|
---|---|---|
Page(s) | 143 - 149 | |
Section | Extragalactic astronomy | |
DOI | https://doi.org/10.1051/0004-6361:200809525 | |
Published online | 22 May 2008 |
Very-high-energy emission from M 82
1
INAF – Osservatorio Astronomico di Trieste and INFN-Trieste, via G.B. Tiepolo 11, 34143 Trieste, Italy e-mail: persic@oats.inaf.it
2
School of Physics & Astronomy, Tel Aviv University, Tel Aviv 69978, Israel
3
Center for Astrophysics and Space Sciences, University of California at San Diego, La Jolla, CA 92093, USA
Received:
6
February
2008
Accepted:
18
May
2008
Spurred by the improved measurement sensitivity in the very-high-energy
(VHE: ≥100 GeV) γ-ray band, we assess the feasibility of
detection of the nearby starburst galaxy M 82. VHE emission is expected
to be predominantly from the decay of neutral pions which are produced in
energetic proton interactions with ambient protons. An estimate of VHE
emission from this process is obtained by an approximate, semi-quantitative
calculation, and also by a detailed numerical treatment based on a
convection-diffusion model for energetic electron and proton propagation
and energy losses. All relevant hadronic and leptonic processes are
considered, gauged by the measured synchrotron radio emission from the
inner disk region. We estimate an integrated flux ≥100 GeV) ~ 2
10-12 cm-2 s-1, possibly detectable
by the current northern-hemisphere imaging air Cherenkov telescopes, MAGIC
and VERITAS, and a good candidate for detection with the upcoming MAGIC II
telescope. We also estimate
≥100 MeV) ~ 10-8 cm-2 s-1, a level of emission that can be detected by GLAST/LAT
based on the projected sensitivity for a one-year observation.
Key words: acceleration of particles / ISM: cosmic rays / galaxies: general / galaxies: starburst / stars: formation / radiation mechanisms: non-thermal
© ESO, 2008
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