Fig. 1
Left: Hertzsprung–Russell diagram of the PPD hosts in our sample. They are classified into Rings, Rim, or Spiral based on their main detected substructures; the MIST tracks for young PMS stars are overplotted (Choi et al. 2016). The resulting stellar parameters are shown in Table 1 and have been derived as explained in Sect. 2.1. Right: mass–distance diagram of the same population.
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