We examine the new Galactic supernova remnant ( SNR ) candidate , G23.11 + 0.18 , as seen by the Murchison Widefield Array ( MWA ) radio telescope . We describe the morphology of the candidate and find a spectral index of - 0.63 \pm 0.05 in the 70-170 MHz domain . A \textcolor black coincident TeV gamma-ray detection in High-Energy Stereoscopic System ( HESS ) data supports the SNR nature of G23.11 + 0.18 and suggests that G23.11 + 0.18 is accelerating particles beyond TeV energies , thus making this object a promising new cosmic ray hadron source candidate . The remnant can not be seen in current optical , infrared and X-ray data-sets . We do find , however , a dip in CO-traced molecular gas at a line-of-sight velocity of \sim 85 km s ^ { -1 } , suggesting the existence of a G23.11 + 0.18 progenitor wind-blown bubble . \textcolor black Furthermore , the discovery of molecular gas clumps at a neighbouring velocity towards HESS J1832 - 085 adheres to the notion that a hadronic gamma-ray production mechanism is plausible towards the north of the remnant . Based on these morphological arguments , we propose an interstellar medium association for G23.11 + 0.18 at a kinematic distance of 4.6 \pm 0.8 kpc .