presence of planets at large orbital radii clearing their orbits from debris, e.g. HD 92945 [@Golimowski2011] and HD 131835 [@Feldt2017]. However, alternative scenarios without planets that could also reproduce the observed structure have not been ruled out yet in these systems. For example, multiple ring structures can arise from gas-dust interactions if gas and dust densities are similar [@Lyra2013Natur; @Richert2017], which might explain HD 131835’s rings since large amounts of CO gas (likely primordial origin) have been found in this system [@Moor2017]. Moreover, the double ring structure around HD 92945 and HD 131835 has only been identified in scattered light images, tracing small dust grains whose distribution can be highly affected by radiation forces [@Burns1979], therefore not necessarily tracing the distribution of planetesimals [e.g. @Wyatt2006].

Only HD 107146, an $\sim80-200$ Myr old G2V star [@Williams2004 and references therein] at a distance of $27.5\pm0.3$ pc [@Gaiamission; @Gaiadr1], has a double debris ring structure tentatively identified at longer wavelengths thanks to the Atacama Large Millimeter/submillimeter Array [ALMA, @Ricci2015]. At these wavelengths observations trace mm-sized dust for which radiation forces are negligible, therefore indicating that the double ring structure is imprinted in the planetesimal distribution as well. Moreover, these observations ruled out the 