2019ApJ...884...13C

The compact, nonthermal emission in DoAr21 has been studied with the Very Long Baseline Array (VLBA) to investigate the possibility that the residuals of the astrometry fitting are due to the reflex motion induced by a possible companion. We find that the fitting of VLBA astrometric observations of DoAr21 improves significantly by adding the orbital motions of three companions. We obtain an improved distance to the source of 134.6 ± 1.0 pc, and estimate that the central star, DoAr21, has a mass of about 2.04 ± 0.70 M_☉. We suggest that DoAr21 represents a unique case where two substellar companions, DoAr21b and DoAr21c (m_b ∼ 35.6 ± 27.2 M_jup and m_c ∼ 44.0 ± 13.6 M_jup, respectively), have been found to be associated with a relatively low-mass, pre-main sequence star. In addition, we find that this WTTau star is an astrometric double system, having a low-mass star companion, DoAr21B (m_B ∼ 0.35 ± 0.12 M_☉), in a relatively eccentric orbit. The orbit of this low-mass stellar companion is compact, while the brown dwarfs are located in external orbits. DoAr21c has the strongest astrometric signature in the periodogram, while DoAr21B has a weak but significant signature. On the other hand, the astrometric signature of DoAr21b does not appear in the periodogram, however, this brown dwarf was directly detected in some of the VLBA observations. The estimated orbital periods of DoAr21B, DoAr21b, and DoAr21c are P_B ∼ 92.92 ± 0.02, P_b ∼ 450.9 ± 3.8, and P_c ∼ 1013.5 ± 25.3 days, respectively. Since the estimated age of this young star is about 0.4-0.8 Myr, the detected brown dwarf companion is among the youngest companions observed to date.