2008A&A...481..401A

Observations of shell-type supernova remnants (SNRs) in the GeV to multi-TeV γ-ray band, coupled with those at millimetre radio wavelengths, are motivated by the search for cosmic-ray accelerators in our Galaxy. The old-age mixed-morphology SNR W 28 (distance ∼2kpc) is a prime target due to its interaction with molecular clouds along its northeastern boundary and other clouds situated nearby. We observed the W 28 field (for ∼40h) at very high energy (VHE) γ-ray energies (E>0.1TeV) with the HESS. Cherenkov telescopes. A reanalysis of EGRET E>100MeV data was also undertaken.
Result. from the NANTEN 4m telescope Galactic plane survey and other CO observations were used to study molecular clouds. We have discovered VHE γ-ray emission (HESS J1801-233) coincident with the northeastern boundary of W 28 and a complex of sources (HESS J1800-240A, B and C) ∼0.5° south of W 28 in the Galactic disc. The EGRET source (GRO J1801-2320) is centred on HESS J1801-233 but may also be related to HESS J1800-240 given the large EGRET point spread function. The VHE differential photon spectra are well fit by pure power laws with indices Γ∼2.3 to 2.7. The spectral indices of HESS J1800-240A, B, and C are consistent within statistical errors. All VHE sources are ∼10' in intrinsic radius except for HESS J1800-240C, which appears pointlike. The NANTEN ¹²CO(J=1-0) data reveal molecular clouds positionally associating with the VHE emission, spanning a ∼15km/s range in local standard of rest velocity. The VHE/molecular cloud association could indicate a hadronic origin for HESS J1801-233 and HESS J1800-240, and several cloud components in projection may contribute to the VHE emission. The clouds have components covering a broad velocity range encompassing the distance estimates for W 28 (∼2kpc) and extending up to ∼4kpc. Assuming hadronic origin and distances of 2 and 4kpc for cloud components, the required cosmic-ray density enhancement factors (with respect to the solar value) are in the range ∼10 to ∼30. If situated at 2kpc distance, such cosmic-ray densities may be supplied by SNRs like W 28. Additionally and/or alternatively, particle acceleration may come from several catalogued SNRs and SNR candidates, the energetic ultra compact HII region W 28A2, and the HIIregions M 8 and M 20, along with their associated open clusters. Further sub-mm observations would be recommended to probe in detail the dynamics of the molecular clouds at velocites >10km/s and their possible connection to W 28.