tokens: than the canonical value of 1.4. Fig. 12. Parallax over error ( π / σ π ) ve. RUWE of the three new groups of YSOs identified in this work, compared to sources with resolved protoplanetary disks (DSHARP, Andrews et al. 2018 ) and known binaries in Upper Sco ( Tokovinin Briceño 2020 ). 5. On the origin of the new YSOs with disks The previous section has shown that the new disk-bearing YSOs that are candidate members of the US and V1062 Sco comoving groups are relatively well characterized with respect to proper motion, on-sky spatial distribution, distance distribution, and age. Tables D.1 and E.1 list the source designations and disk type for US and V1062 Sco, respectively. The remaining YSOs in our sample (Table A.1 ) are likely composed of sources from both Lupus and UCL, as they present properties that are common to both of these populations; the emerging picture is that the youngest of these YSOs are likely Lupus members, while the older sources are likely part of UCL. Comparison of our new disk-bearing sources in Table A.1 with the YSOs identified by Damiani et al. (2019) yielded 37 out of 60 matches: 45% of the sources were found to belong to the UCL diffuse group D1, and 35% to the UCL diffuse group D2 (further divided into 27% from the D2a sub-group and 8% from the D2b sub-group). Of our new disks in US, 12/19 were identified as belonging to either the diffuse population in Upper Sco USC-D2 (32%), to UCL-D1 (32%), or to UCL-D2a (5%). Regarding the new disks in V1062 Sco, 14/19 were also previously identified by Damiani et al. (2019) as candidate members of the V1062 Sco/UCL-1 compact group. We discuss in this section the region morphology and kinematics to explore the origin and connection between Lupus, UCL, US, and V1062 Sco. 5.1. Evolution of the 3D spatial distribution We attempt to reconstruct the 3D distribution of the new disk-bearing YSOs and the Lupus clouds to better determine how the Lupus and UCL stellar groups are related. Figure 13 shows in the upper (middle) row the Galactic Latitude (Longitude) as a function of distance for these sources. Each row has three panels, corresponding to the three iscohronal age groups. These panels also include a schematic representation of the Lupus clouds (the central Galactic coordinates were taken from Hara et al. (1999) and the width of the filled ellipses are merely representative and not to be taken to scale). The distances to Lupus 1, Lupus 2, Lupus 3, and Lupus 4 were derived from the distances to their previously known members ( Dzib et al. 2018 ), and for clouds with no known associated YSOs we use the distances calculated by Zucker et al. (2019) (we exclude the clouds Lupus 7 and Lupus 8, due to the lack of distance estimates). To constrain the origin of a YSO, we explore its travel radius, specifically, the projected distance traversed by a source since its birth assuming a 1D velocity of 1 km s −1 . We represent the area corresponding to the travel radius as dotted-line
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