Observed mass outflow rate Ṁ_jet versus accretion rate Ṁ_acc of HH 1042 and HH 1043 (red squares) compared with different classes of YSOs associated with jets and outflows. The Ṁ_acc value of some HAeBe stars (grey triangles) was determined from the Hα luminosity in Hillenbrand et al. (1992). The orange symbols indicate “continuum stars”, objects classified as CTTS (orange circles) or HAeBe stars (orange triangles) with a high degree of veiling whose spectral type is very uncertain (see Calvet & Gullbring 1998; Hernández et al. 2004); these objects are spectroscopically similar to 08576nr292, the driving source of HH 1042. The dashed lines indicate the Ṁ_jet/Ṁ_acc = 0.01 and 0.1 range, which is predicted by jet formation models. References: Class 0/I objects: Hartigan et al. (1994); Bacciotti & Eislöffel (1999); Podio et al. (2006, 2011, 2012); Antoniucci et al. (2008); Cabrit (2009); FU Orionis objects: Hartmann & Calvet (1995); Calvet (1998); HAeBe stars: Levreault (1984); Boehm & Catala (1994); Nisini et al. (1995); Garcia Lopez et al. (2006); Wassell et al. (2006); Melnikov et al. (2008); Mendigutía et al. (2011); Donehew & Brittain (2011); Liu et al. (2011); CTTS: Hartigan et al. (1995); Gullbring et al. (1998); Muzerolle et al. (1998a); Coffey et al. (2008); Cabrit (2009); Melnikov et al. (2009); Brown dwarfs: Whelan et al. (2007); Herczeg & Hillenbrand (2008); Bacciotti et al. (2011).