tokens: also do not show another source within the NACO FoV, indicating that both BHB2007-2AB and VLT 171104.07-272258.8 are more evolved than BHB2007-1. In the analysis we also calculated the photometry in the K S band of BHB2007-2AB and VLT 171104.07-272258.8, listed in Table 2 . Table 1 Astrometric Measurements of the Components Measured with Respect to the Central Source [BHB2007]-1 Table 2 Apparent Magnitudes of the Components Measured with Respect to the Central Source [BHB2007]-1 3.3. Stellar Properties Here we calculate the stellar properties of [BHB2007]-1 and -2 based on the Gaia EDR3 parallax (see Section 3.2 ) and the notion that [BHB2007]-2 is a binary system. We collected the B-to-W4-band photometry of −1 and −2 from Vizier. We investigated the ASAS-SN light curves (Kochanek et al. 2017 ) finding that the visual brightness of both stars is only moderately variable ( mag over years). We adopted a Phoenix model of the stellar photosphere (Hauschildt et al. 1999 ) with the effective temperature constrained by Covey et al. ( 2010 ) ( K and K, for −1 and −2, respectively, with typical uncertainties of ±300 K) and visual extinction calculated from the observed colors between the R , I , and J bands, and stellar luminosity L * from the integrated photospheric model. For [BHB2007]-1, this yielded mag and . However, the edge-on geometry of the disk (see Section 3.4 ) may in principle yield an underestimation of the luminosity. In fact, stars with very inclined disks appear on average older (since less luminous) than the other stars (see Garufi et al. 2018 ). As for [BHB2007]-2, we first had to consider the visually triple nature of the star (see Section 3.1 ). All three stars sit within the 2MASS beam, meaning that the observed photometry is a contribution of all of them. We computed the actual J -, H -, -, and W 1-band magnitudes through the relative flux ratios measured in our NACO images. We then constrained visual extinction and stellar luminosity of [BHB2007]-2A assuming that the constrained by Covey et al. ( 2010 ) refers to this star since it is significantly brighter than the other two. We found that the is comparable with that of [BHB2007]-1 (1.5 ± 0.4 mag) while the luminosity is . Finally, we constrained stellar mass M * and age t of the two sources through multiple sets of pre-main-sequence tracks (Baraffe, MIST, and Parsec; Baraffe et al. 2015 ; Dotter 2016 ; Bressan et al. 2012 ). Bearing in mind the assumptions and the uncertainties described above, we found and Myr for [BHB2007]-1, and and for [BHB2007]-2. The stellar mass of [BHB2007]-1 is significantly smaller than what was constrained by Alves et al. ( 2020 ) from the position–velocity diagram of the CO emission (2.23 ). Such a large discrepancy cannot be explained by an erroneous estimate of the stellar luminosity alone since the evolutionary tracks corresponding to stars with K are nearly vertical, making the stellar mass only marginally impacted by the luminosity.
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