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We show the first SPHERE/IRDIS and IFS data of the CO-rich debris disc aroundHD 131488. We use N-body simulations to model both the scattered light imagesand the SED of the disc in a self-consistent way. We apply theHenyey-Greenstein approximation, Mie theory, and the Discrete DipoleApproximation to model the emission of individual dust grains. Our study showsthat only when gas drag is taken into account can we find a model that isconsistent with scattered light as well as thermal emission data of the disc.The models suggest a gas surface density of $2\times10^{-5}\,M_\oplus/$au$^2$which is in agreement with estimates from ALMA observations. Thus, ourmodelling procedure allows us to roughly constrain the expected amount of gasin a debris disc without actual gas measurements. We also show that the shallowsize distribution of the dust leads to a significant contribution of largeparticles to the overall amount of scattered light. The scattering phasefunction indicates a dust porosity of $\sim0.2\ldots 0.6$ which is in agreementwith a pebble pile scenario for planetesimal growth.

The debris disc of HD 131488 -- Bringing together thermal emission and scattered light