Notes. [1] Sample targets; [2] SED Class; [3] spectral type; [4] temperature; [5] accretion rate; [6] stellar luminosities; [7] X-ray luminosities; [8] accretion luminosities; [9] stellar age; [10] disc masses; [11] Separation in arcsec and components. The mass accretion rates were derived from the U band excess as follows: first the U band photometry from Kenyon & Hartmann (1995) was derredened using the Cardelli et al. (1989) extinction curve. Then the U band excess was derived by subtracting the photospheric contribution, and converted to accretion luminosity according to the empirical relation log (L_acc/L_⊙) = 1.09 × log (L_U/L_⊙) + 0.98 in Gullbring et al. (1998). The mass accretion rates were finally obtained using the relation , following the assumptions in Gullbring et al. (1998).

Reference. ^aHerczeg & Hillenbrand (2014), ^b see Howard et al. (2013) for a discussion, ^cPalla & Stahler (2002), ^dṀ_acc and L_acc as explained above, ^eGüdel et al. (2007b), ^fAndrews & Williams (2005), ^gWhite & Ghez (2001).