Discovery of very high energy gamma-ray emission coincident with molecular clouds in the W 28 (G6.4-0.1) field

Abstract

Aims. 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 ∼2 kpc) is a prime target due to its interaction with molecular clouds along its northeastern boundary and other clouds situated nearby. Methods. We observed the W 28 field (for ∼40 h) at very high energy (VHE) γ-ray energies (E > 0.1 TeV) with the HESS. Cherenkov telescopes. A reanalysis of EGRET E > 100 MeV data was also undertaken. Results from the NANTEN 4 m telescope Galactic plane survey and other CO observations were used to study molecular clouds. Results. 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 12 CO(J = 1−0) data reveal molecular clouds positionally associating with the VHE emission, spanning a ∼15 km s −1 range in local standard of rest velocity. Conclusions. 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 (∼2 kpc) and extending up to ∼4 kpc. Assuming hadronic origin and distances of 2 and 4 kpc 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 2 kpc 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 HII regions 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 >10 km s −1 and their possible connection to W 28. Key words. gamma rays: observationsEnergy spectra are only available in electronic form at

A young supernova remnant illuminating nearby molecular clouds with cosmic rays

“…In fact, a similar scenario has been successfully invoked to explain the γ-ray emission region HESS J1800-240 south of the SNR W 28 (Aharonian et al 2008a;Abdo et al 2010;Li & Chen 2010). HESS J1800-240 displays a very good morphological match to the molecular gas measured through CO emission from that region.…”

ISM gas studies towards the TeV PWN HESS J1825−137 and northern region

“…Therefore a nearby accelerator providing CRs at an energy density 15 times the Earth-like value is required. The required CR density enhancement to produce the observed TeV flux towards HESS J1826−130 can easily be reached by SNRs (e.g W28; see Aharonian et al 2008). Therefore, the progenitor SNR of PSR J1826−1334 may contribute to the HESS J1826−130 TeV emission.…”

The Mopra Southern Galactic Plane CO Survey

“…Aharonian et al 2008;Ackermann et al 2013), over 30% of Galactic gamma-ray sources, remain unidentified in relation to the nature of the parent particles (i.e. whether they are cosmic rays or electrons) and their counterpart accelerators (Hinton & Hofmann 2009;Nolan et al 2012).…”