We present the discovery of nonthermal radio and X-ray emission positionally coincident with the TeV gammaray source HESS J1813-178. We demonstrate that the nonthermal radio emission is due to a young shell-type supernova remnant (SNR), G12.8-0.0, and constrain its distance to be greater than 4 kpc. The X-ray emission is primarily nonthermal and is consistent with either an SNR shell or unidentified pulsar or pulsar wind nebula origin; pulsed emission is not detected in archival ASCA data. A simple synchrotron plus inverse Compton model for the broadband emission assuming that all of the emission arises from the SNR shell implies maximum energies of (30-450)[B/(10 μG)]-05 TeV. Further observations are needed in order to confirm that the broadband emission has a common origin and to better constrain the X-ray spectrum.
- Acceleration of particles
- ISM: individual (G12.8-0.0, HESS J1813-178)
- Radio lines: ISM
- Supernova remnants
- X-rays: ISM