Table 4: Observed companion star fraction over the separation range 110-1400 AU in Perseus, Taurus-Auriga and Ophiuchus star-forming regions (SFRs) for Class 0 sources, Class I sources with (env+) and without (env-) an extended millimetric envelope, and for Class II-III T Tauri stars in the same clouds. For comparison, the multiplicity rate for G-type field dwarfs over the same separation range is 14% (Duquennoy & Mayor 1991). References: 1 - Looney et al. (2000); 2 - this study; 3 - Mathieu (1994); 4 - Barsony et al. (2003).
  SFR $N_{{\rm comp}}$/ $N_{{\rm prim}}$ CSF Ref. CSF $_{{\rm tot}}$ CSF $_{{\rm tot}}$  
      (%)   (%) (%)  
  Perseus 1/11          
Class 0 Ophiuchus 2/2 25 $\pm$ 13 1 25 $\pm$ 13   Embedded sources
  Taurus 5/12 41 $\pm$ 14     38 $\pm$ 8  
Class I env+ Ophiuchus 7/15 47 $\pm$ 13 2 44 $\pm$ 10   with mm envelope
  Taurus 0/10 0        
Class I env- Ophiuchus 5/26 19 $\pm$ 8 2 14 $\pm$ 6   Optical/IR sources
  Taurus 24/100 24 $\pm$ 4 3   22 $\pm$ 3  
Class II-III Ophiuchus 21/88 24 $\pm$ 5 4 24 $\pm$ 3   without mm envelope


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