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Aims: We aim for an understanding of the morphological and spectralproperties of the supernova remnant RCW~86 and for insights into the productionmechanism leading to the RCW~86 very high-energy gamma-ray emission. Methods:We analyzed High Energy Spectroscopic System data that had increasedsensitivity compared to the observations presented in the RCW~86 H.E.S.S.discovery publication. Studies of the morphological correlation between the0.5-1~keV X-ray band, the 2-5~keV X-ray band, radio, and gamma-ray emissionshave been performed as well as broadband modeling of the spectral energydistribution with two different emission models. Results:We present the firstconclusive evidence that the TeV gamma-ray emission region is shell-like basedon our morphological studies. The comparison with 2-5~keV X-ray data reveals acorrelation with the 0.4-50~TeV gamma-ray emission.The spectrum of RCW~86 isbest described by a power law with an exponential cutoff at $E_{cut}=(3.5\pm1.2_{stat})$ TeV and a spectral index of $\Gamma$~$1.6\pm 0.2$. A staticleptonic one-zone model adequately describes the measured spectral energydistribution of RCW~86, with the resultant total kinetic energy of theelectrons above 1 GeV being equivalent to $\sim$0.1\% of the initial kineticenergy of a Type I a supernova explosion. When using a hadronic model, amagnetic field of $B$~100$\mu$G is needed to represent the measured data.Although this is comparable to formerly published estimates, a standardE$^{-2}$ spectrum for the proton distribution cannot describe the gamma-raydata. Instead, a spectral index of $\Gamma_p$~1.7 would be required, whichimplies that ~$7\times 10^{49}/n_{cm^{-3}}$erg has been transferred intohigh-energy protons with the effective density $n_{cm^{-3}}=n/ 1$ cm^-3. Thisis about 10\% of the kinetic energy of a typical Type Ia supernova under theassumption of a density of 1~cm^-3.

Detailed spectral and morphological analysis of the shell type SNR RCW 86