Two thirds of the F star members of the 12 Myr old \beta Pictoris Moving Group ( BPMG ) show significant excess emission in the mid-infrared , several million years after the expected dispersal of the protoplanetary disc . Theoretical models of planet formation suggest that this peak in the mid-infrared emission could be due to the formation of Pluto-sized bodies in the disc , which ignite the collisional cascade and enhance the production of small dust . Here we present resolved mid-infrared imaging of the disc of HD191089 ( F5V in the BPMG ) and consider its implications for the state of planet formation in this system . HD191089 was observed at 18.3 \mu m using T-ReCS on Gemini South and the images were compared to models of the disc to constrain the radial distribution of the dust . The emission observed at 18.3 \mu m is shown to be significantly extended beyond the PSF at a position angle of 80 ^ { \circ } . This is the first time dust emission has been resolved around HD191089 . Modelling indicates that the emission arises from a dust belt from 28-90 AU , inclined at 35 ^ { \circ } from edge on with very little emission from the inner 28AU of the disc , indicating the presence of an inner cavity . The steep slope of the inner edge is more consistent with truncation by a planet than with ongoing stirring . A tentative brightness asymmetry \frac { F _ { W } } { F _ { E } } = 0.80 \pm 0.12 ( 1.8 \sigma ) between the two sides of the disc could be evidence for perturbations from a massive body on an eccentric orbit in the system .