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This paper presents a comprehensive analysis of the Galactic SNR Kes 17(G304.6+0.1) with focus on its radio synchrotron emission, environs, and thefactors contributing to the observed gamma rays. The firstly-obtainedintegrated radio continuum spectrum from 88 to 8800 MHz yields an index alpha =-0.488 +/- 0.023 (S_nu $\propto$ nu^alpha), indicative of a linear particleacceleration process at the shock front. Accounting for the SNR radio shellsize, the distribution of atomic hydrogen (n_H ~ 10 cm^-3), and assuming theSNR is in the Sedov-Taylor stage of its evolution, we estimate Kes 17 to beroughly 11 kyr. From 12CO and 13CO (J=1-0) emission-line data as a proxy formolecular hydrogen we provided the first evidence that the eastern shell of Kes17 is engulfing a molecular enhancement, with 4.2 x 10^4 M_sun and n ~ 300cm^-3. Towards the western boundary of Kes 17 there are not CO signatures above3 sigma, despite previously reported infrared observations have revealedshocked molecular gas at that location. This suggests the existence of aCO-dark interacting molecular gas, a phenomenon also recorded in other GalacticSNRs (e.g. CTB 37A and RX J1713.7-3946). Additionally, by analysing ~14.5 yr ofdata from Fermi-LAT, we determined a power-law photon index in the 0.3-300 GeVrange of Gamma = 2.39 +/- 0.04^+0.063_-0.114 (+/-stat +/-syst) in agreementwith prior studies. The energy flux turns out to be (2.98 +/- 0.14) x 10^-11erg cm-2 s-1 implying a luminosity (2.22 +/- 0.45) x 10^35 erg s-1 at ~8 kpc.Finally, we successfully modelled the multiwavelength SED by incorporating theimproved radio synchrotron spectrum and the new gamma-ray measurements. Ouranalysis indicates that the observed GeV flux most likely originates from theinteraction of Kes 17 with western ''dark'' CO zone with a proton density n_p ~400 cm-3.

The SNR Kes 17-ISM interaction: a fresh view from radio and $\gamma$ rays