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Fig. 5


Millimeter fluxes of the observed target sources. The millimeter fluxes are from Table D.1. All presented fluxes from our observations have been scaled to the measurements at 225 GHz by assuming an identical spectral index of α = 3.8. In addition, the plotted flux of each source has been scaled by (d [pc]/353 [pc])2, where d is the source distance and 353 pc is the parallax distance of FU Ori. Blue, black, and red symbols are the FUors, EXors, andFUor-like objects, respectively. Class I, I/II, II, and III sources are distinguished by different symbol shapes, which are introduced in the figure legend. Symbols for target sources which are not detected (presented 3σ upper limit) or are largely confused by the parent cloud structures, are presented in lighter colors. Symbols for non-detected sources are connected with downward arrows. The horizontal displacements of symbols do not have physical meaning although in general the more embedded sources are more to the left. The four thin horizontal gray lines show the corresponding dust mass evaluated by Mdust [M] = 1.13 × 10−5 [mJy], which is a formulation introduced by Ansdell et al. (2017) but was rescaled to a 353 pc distance. Solid and dashed yellow lines show the cumulative distribution function of the present sample: the former includes both the detected and non-detected sources by assigning their fluxes as the 1σ noise, and the later only includes the detected sources. Purple, light blue, red, and green dotted lines present the M* > 0.3 M Class II objects in the Taurus, Lupus, Chameleon I, and Upper Sco regions, respectively (quoted from Pascucci et al. 2016; the original observations can be found in Andrews et al. 2013; Carpenter et al. 2014; Ansdell et al. 2016; Barenfeld et al. 2016; and Pascucci et al. 2016).

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