All Tables

Table 1: Observed sample of wide PMS binaries.
Table 3: Measured parameters of all candidate triple/quadruple systems resolved in our survey, with their apparent multiplicity in the projected separation range 0 $.\!\!^{\prime\prime}$ 07-12 $^{\prime \prime }$ . Also quoted in last column is the probable and assumed multiplicity of this systems in this separation range based on the chance projection analysis of Sect. 4.5.
Table 4: Upper limits for the relative brightness of undetected companions to both components of the binaries in our survey, measured at 0 $\hbox{$.\!\!^{\prime\prime}$ }$ 07, 0 $\hbox{$.\!\!^{\prime\prime}$ }\!$ 15 and 0 $\hbox{$.\!\!^{\prime\prime}$ }$ 5, as well as the limiting magnitudes at large separations.
Table 5: Probability of unrelated companions to the triple/quadruple systems as estimated from 2MASS.
Table 6: Comparison of the multiplicity frequency per binary (MF/wB and MF/B) and the companion star frequency per binary (CSF/wB and CSF/B) of our work with those derived from previous multiplicity surveys among T Tauri stars in a similar separation range $\sim$ 14-1700 AU^a, and with recent numerical simulations (bottom part). Also indicated are the number of wide (separation >0 $\hbox{$.\!\!^{\prime\prime}$ }$ 5) binaries (wB), binaries (B), triples (T), quadruples (Q) and higher multiples (>4).
Table 7: Systems dynamical stability. Application of the stability criteria from Eggleton & Kiseleva (1995) (their $Y^{\rm min}_{0}$ , cf. Eq. (2)) and from Mardling & Aarseth (2001) ( $R^{\rm min}_{\rm crit} = \frac{R^{\rm out}_{\rm p}}{a_{\rm in}}$ their Eq. (90)) for a given partition (1+2)+3, $q_{\rm in}$ = m₁/m₂ and $q_{\rm out}$ = (m₁+m₂)/m₃. $R_{\rm mes}$ is the ratio of the outer to the inner projected separation of the triple partition considered^a.
Table 8: Known T Tauri types (CTTS or WTTS) for all single components or otherwise pairs of the triple/quadruple systems. Also included are spectral types, $A_{\rm V}$ , masses, and ages of the components from the literature, as well as our own estimates for the new and poorly studied components when possible (see Sect. 4.6).
Table 2: Observation Log.