All Tables

Table 1: rms errors of the magnitude differences (instrumental system) between the comparison stars in units of 0.1 mmag. N is the total number of magnitude differences.
Table 2: Photometric data for the eclipsing binaries and the comparison stars in the uvby and $\beta$ standard systems. For the eclipsing binaries, the uvby information is given at maximum light level outside eclipses. The $\beta$ information is the mean values outside eclipses. N is the total number of observations used to form the mean values, and $\sigma$ is the rms error (per observation) in mmag.
Table 3: Published ${uvby}\beta$ photometry for the eclipsing binaries and the comparison stars. N is the total number of observations used to form the mean values, and $\sigma$ is the rms error (per observation) in mmag. References are: GO76 = Grønbech & Olsen (1976), GO77 = Grønbech & Olsen (1977), HM80 = Heck & Manfroid (1980), K98 = Kaltcheva (1998), KOC00 = Kaltcheva et al. (2000), K78 = Kilkenny (1978), K81 = Kilkenny (1981), K92 = Knude (1992), LPLM90 = Landolt et al. (1990), S85 = Shobbrook (1985), SHL92 = Slawson et al. (1992), TAT95 = Twarog & Anthony-Twarog (1995), WK83 = Wolf & Kern (1983).
Table 4: Times of minima determined from the new uvby photometry for DWCar. O-C values are calculated from the ephemeris given in Eq. (1) adopting a circular orbit. See van den Hoven van Genderen (1941) for additional times of minima.
Table 5: Times of minima for BFCen. O-C values are calculated from the ephemeris given in Eq. (2) adopting a circular orbit. References are: O28 = Oosterhoff (1928), O30 = Oosterhoff (1930), WR94 = Wolf & Ratzlaff (1994), OZ04 = Ogloza & Zakrzewski (2004).
Table 6: Times of minima for NSV5783. O-C values (primary eclipse, P) and phase (secondary eclipse, S) are calculated from the ephemeris given in Eq. (3).
Table 7: Photometric solutions for NSV5783 from the EBOP code. Phase shift and magnitude normalization were included as free parameters. A mass ratio of 0.95 was assumed. The errors quoted for the free parameters are the formal errors determined from the iterative least squares solution procedure.
Table 8: Adopted photometric elements for NSV 5783. The individual flux and luminosity ratios are based on the mean stellar and orbital parameters.
Table 9: FEROS spectra of NSV5783. S/N is the signal to noise ratio at approximately 5000 Å. The exposure time is 30 min for all spectra, and the Heliocentric Julian Dates correspond to mid-exposure. The radial velocities given in brackets are strongly affected by blending and have not been used to estimate the spectroscopic elements. See text for details.
Table 10: Astrophysical data for NSV 5783. $T_{\rm eff\odot} = 5780$ K, $B.C._{\odot} = -0.08$ , and $M_{\rm bol\odot} = 4.74$ has been assumed, and bolometric corrections by Flower (1996) have been adopted.