Table 1: List of program stars.

Object		 HD Sp class Type Distance* (kpc) Distance$^\dag $ (kpc) Epoch, JDs Periods Ref.

RU Cen		 105578 A7Ib-G2pe RV 3.9a, 2.2b, 1.0c 1.639 (0.575-$\infty$) 2 448 124.57+ 64 $\hbox{$.\!\!^{\rm d}$ }$6 3
SX Cen 107439 F5-G3/5Vp RV 5.2a, 5.5b, 2.5d   2 447 324.97+ 32 $\hbox{$.\!\!^{\rm d}$ }$8642 2
BU Cen     RV       85 $\hbox{$.\!\!^{\rm d}$ }$50 1
R Sct 173819 G0Ia-K0Ibe RV  0.4a 0.43 (0.318-0.667) 2 444 872.0+ 146 $\hbox{$.\!\!^{\rm d}$ }$5 1
R Sge 192388 G0Ib-G8Ib RV 2.9a, 3.2b   2 443 830.0+ 70 $\hbox{$.\!\!^{\rm d}$ }$770 1
DS Aqr 216457 F2II RV 0.45-0.69e 0.467 (0.249-3.850) 2 433 862.50+ 78 $\hbox{$.\!\!^{\rm d}$ }$213 1
UY Ara   G RV 9.6a   2 426 868.40+ 57 $\hbox{$.\!\!^{\rm d}$ }$220 1
AI Sco 320921 G0-K2 RV 2.4a, 3.6b   2 448 373.93+ 71 $\hbox{$.\!\!^{\rm d}$ }$03 3
UW Cen   K R CrB (2.83, 4.25)f, 0.787 (0.245-$\infty$)   $\approx$ $43^{\rm d}$ 5
        5.5g, 1.0c        
RY Sgr 180093 G0Iep R CrB (1.32, 4.1)f, 2.78 (0.676-$\infty$)   $\approx$ $38^{\rm d}$ 6
        1.5h, 1.7g        
DY Cen   early BI R CrB 4.8i     $3\hbox{$.\!\!^{\rm d}$ }8{-}5\hbox{$.\!\!^{\rm d}$ }5$ 7
U Aqr   C R CrB 13.2g 0.279 (0.163-0.970) 2 446 662.0+ $81\hbox{$.\!\!^{\rm d}$ }3$ 4,8
V1711 Sgr   F4-F6 W Vir 5.4j 0.427 (0.212-$\infty$) 2 444 151.11+ $28\hbox{$.\!\!^{\rm d}$ }55$ 1
*Distances mainly from absolute magnitude-reddening calibrations; $^\dag $distances from Hipparcos parallaxes; (a) Alcolea & Bujarrabal (1991); (b) Jura (1986); (c) Eggen (1986); (d) data from Shenton et al. (1994b); (e) derived from z-distance from Wahlgren (1992); (f) distances from radial velocities and reddening calibrations from Trimble & Kundu (1997); (g) Lawson et al. (1990); (h) data from Clayton & Ayres (2001); (i) Rao & Raveendran (1993); (j) distance from period-luminosity relation by Harris & Wallerstein (1984). (1) epoch of maximum light taken from Kholopov et al. (1998); (2) epoch of primary minima from Shenton et al. (1994b); (3) epoch of primary minima from Pollard et al. (1997); (4) period from Lawson & Cotterell (1990); (5) period from Jurcsik (1996); (6) Menzies & Feast (1997); (7) data from Pollacco & Hill (1991); (8) JD of a photometric minimum determined here from the light curve of Lawson & Cotterell (1990).

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