Table B.1.
Stellar masses and accretion rates of flat-spectrum sources with M⋆ < 1 M⊙ used in Fig. 3. In addition, the method for determining the accretion rate (MethodṀ⋆) is given. If only one reference is given it contains stellar mass and the accretion rate.
| Name | M⋆ [M⊙] | Ṁ⋆ [10−8 M⊙ yr−1] | MethodṀ⋆ | Ref. |
|---|---|---|---|---|
| V846Ori | 0.55 | 12.0 | CaII/Paβ/Brγ lines | Caratti o Garatti et al. (2012) |
| J05390536-0711052 | 0.55 | 13.0 | CaII/Paβ/Brγ lines | Caratti o Garatti et al. (2012) |
| IRAS 05379-0815 | 0.73 | 7.5 | CaII/Paβ/Brγ lines | Caratti o Garatti et al. (2012) |
| J05413033-0840177 | 0.56 | 10.0 | CaII/Paβ/Brγ lines | Caratti o Garatti et al. (2012) |
| J03290895+3122562 | 0.15 | 1.1 | Paβ/Brγ lines | Fiorellino et al. (2021) |
| J03292044+3118342 | 0.28 | 2.1 | Paβ/Brγ lines | Fiorellino et al. (2021) |
| IRAS 04385+2550 | 0.59 | 12.0a | SED fita | Güdel et al. (2007), Ribas et al. (2020) |
| DG Tau | 0.50 | 25.0 | U-band excess | Güdel et al. (2018), Alonso-Martínez et al. (2017) |
Notes. aSED fitting with an artificial neural network using the D’Alessio Irradiated Accretion Disk models (DIAD, see Ribas et al. 2020).
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