All Tables

Table 1: Log of the FEROS observations of AD Boo, VZ Hya, and WZ Oph. HJD refers to mid-exposure. The exposure time $t_{\rm exp}$ is given in seconds. The signal-to-noise ratio per resolution element (S/N) of individual exposures was measured around 6070 Å. Observers: H = Heidelberg/Copenhagen guaranteed time; JVC = J.V. Clausen; JS = J. Southworth.
Table 2: Effective temperatures (K) of the ``average'' components of AD Boo, VZ Hya, and WZ Oph. The V₀ magnitudes and the (b-y)₀ and c₀ indices are based on the out-of-eclipse uvby standard indices from CVG08. The 2MASS observations ( $J,H,K_{\rm s}$ ) were obtained at phases 0.216 (AD Boo), 0.181 (VZ Hya), and 0.495 (WZ Oph), respectively. For WZ Oph, the V magnitude was calculated from the value outside eclipses and the y eclipse depth at phase 0.495. $A_{\rm V}$ is the adopted visual interstellar absorption. References are: A96, Alonso et al. (1996); H07, Holmberg et al. (2007); RM05, Ramírez & Meléndez (2005); M06, Masana et al. (2006). The results from A96 are based on their uvby calibration, those from RM05 on their uvby, (V-J), (V-H), and $(V-K_{\rm s})$ calibrations (in that order); the calibration by M06 is for $(V-K_{\rm s})$ .
Table 3: Iron abundance ( $[{\rm Fe/H}]$ ) for the Sun determined from Solar atlas spectrum (Wallace et al. 1998) and FEROS spectra, respectively. 131 Fe I and 20 Fe II lines, measured in both spectra, were used. Results from ATLAS9 models and MARCS models are compared.
Table 4: Abundances for the Sun determined from Solar atlas spectrum (Wallace et al. 1998) and ATLAS9 models (Heiter et al. 2002). N is the number of lines used; only ions with three or more measured lines are listed. GS1998 is the logarithmic element abundances (H = 12.00) from Grevesse & Sauval (1998).
Table 5: Spectroscopic orbital solution for AD Boo. T is the time of central primary eclipse.
Table 6: Photometric solutions for AD Boo (all data) from the EBOP code adopting linear limb darkening coefficients by van Hamme (1993). The errors quoted for the free parameters are the formal errors determined from the iterative least squares solution procedure.
Table 7: Photometric solutions for AD Boo (all data) from the WD code adopting linear limb darkening coefficients by van Hamme (1993); see Table 6. Gravity darkening exponents of 0.33 and bolometric albedo coefficients of 0.5 were applied, as appropriate for convective envelopes. $T_{\rm {eff},p}$ was assumed to be 6575 K.
Table 8: Photometric solutions for AD Boo from the EBOP code, excluding observations from 1989. Linear limb darkening coefficients from van Hamme (1993) were adopted; see Table 6.
Table 9: Adopted photometric elements for AD Boo. The individual flux and luminosity ratios are based on the mean stellar and orbitalparameters.
Table 10: Abundances ( $[{\rm El./H}]$ ) for the primary and secondary components of AD Boo. N is the number of lines used per ion.
Table 11: Spectroscopic orbital solution for VZ Hya. T is the time of central primary eclipse.
Table 12: Photometric solutions for VZ Hya from the EBOP code adopting linear limb darkening coefficients by van Hamme (1993). The errors quoted for the free parameters are the formal errors determined from the iterative least squares solution procedure.
Table 13: Photometric solutions for VZ Hya from the WD code adopting linear limb darkening coefficients by van Hamme (1993); see Table 12. Gravity darkening exponents of 0.33 and bolometric albedo coefficients of 0.5 were adopted, as appropriate for convective envelopes. $T_{\rm {eff},p}$ was assumed to be 6650 K.
Table 14: Adopted photometric elements for VZ Hya. The individual flux and luminosity ratios are based on the mean stellar and orbitalparameters.
Table 15: Abundances ( $[{\rm El./H}]$ ) for the primary and secondary components of VZ Hya. N is the number of lines used per ion.
Table 16: Spectroscopic orbital solution for WZ Oph. T is the time of central primary eclipse.
Table 17: Photometric solutions for WZ Oph from the EBOP code adopting linear limb darkening coefficients by van Hamme (1993). The errors quoted for the free parameters are the formal errors determined from the iterative least squares solution procedure.
Table 18: Photometric solutions for WZ Oph from the WD code adopting linear limb darkening coefficients by van Hamme (1993); see Table 17. Gravity darkening exponents of 0.33 and bolometric albedo coefficients of 0.5 were adopted, as appropriate for convective envelopes. $T_{\rm {eff},p}$ was assumed to be 6165 K.
Table 19: Adopted photometric elements for WZ Oph. The individual flux and luminosity ratios are based on the mean stellar and orbitalparameters.
Table 20: Abundances ( $[{\rm El./H}]$ ) for the primary and secondary components of WZ Oph. N is the number of lines used per ion.
Table 21: Astrophysical data for AD Boo, VZ Hya, and WZ Oph. $T_{\rm eff\hbox {$\odot $ }} = 5780$ K, $M_{\rm bol\hbox {$\odot $ }} = 4.74$ , and bolometric corrections (BC) by Flower (1996) have been applied. $v_{\rm sync}$ is the equatorial velocity for synchronous rotation.
Table A.1: Radial velocities (corrections applied) of AD Boo and residuals from the final spectroscopic orbit.
Table A.2: Radial velocities (corrections applied) of VZ Hya and residuals from the final spectroscopic orbit.
Table A.3: Radial velocities (corrections applied) of WZ Oph and residuals from the final spectroscopic orbit.