All Tables

Table 1: Journal of RV data: the telescopes and spectrographs with which the RVs were obtained, denoted by the running numbers in column "Spg. No.'', are as follows: 1... James Lick 0.91-m refractor, Mills 3-prism spg, phot. plates; 2... Yerkes 1.02-m refractor, Bruce 1-prism spg. phot. plates; 3... DAO Plaskett 1.8-m reflector, Cass. IM or IS prism spgs., phot. plates; 4... Mt. Wilson Hooker 2.54-m reflector, coudé grating spg., 114-inch camera, phot. plates; 14... Mt Wilson Hooker 2.54-m reflector, coudé grating spg., 32-inch camera, phot. plates; 5... IUE satellite 0.45-m reflector, Cass. echelle spgs., SWP, LWP and LWR SEC Vidicon cameras; 6... CTIO 1-m reflector, Cass. spg., image tube & phot. plates; 7... MJUO McLellan 1-m reflector, Cass. fiber fed echelle spg., Reticon 1872; 8... SAAO 1.9-m reflector, Cass spg., image tube & intensified Reticon; 9... DAO McKellar 1.2-m reflector, coudé spg., SITe-4 4096 $\times$ 2048 CCD; 10... Ondrejov 2-m reflector, coudé spg., SITe-005 800 $\times$ 2000 CCD.
Table 3: Various orbital solutions for ${\upsilon }$ Sgr derived with the FOTEL program. All epochs are in HJD-2 400 000 and the rms error is error per 1 observation of unit weight. Systemic velocities of individual spectrographs are identified by the running numbers corresponding to those from Table 1. Rather large differences in the individual systemic velocities probably do not reflect real changes but rather compensate for the differences in line identifications and various subsets of lines used by various authors to derive the published RVs.
Table 4: Orbital solutions for two slightly overlapping subsets of older and more recent primary RVs to test the possibility of a secular change of the orbital period.
Table 5: Probable basic physical properties of ${\upsilon }$ Sgr based on orbital solution 4 of Table 3 derived for three possible values of the orbital inclination. Tabulated are masses M₁ and M₂, the semi-major axis A, Roche-lobe radii $R^{\rm Roch}_1$ and $R^{\rm Roch}_2$ , and the minimum and maximum angular dimensions of the semi-major axis $a_{\rm min.}$ and $a_{\rm max.}$ derived for the range given by the Hipparcos parallax and its error $p=0\hbox{$.\!\!^{\prime\prime}$ }00195$ $\pm$ $0\hbox{$.\!\!^{\prime\prime}$ }00072$ .