Table 3: Linear relations between the amplitude of the velocity curves and the line depth (at minimum extension of the star), ${\Delta RV_c}= a_0 D + b_0$ are given for all stars, together with the $1\sigma$ uncertainty. The reduced $\chi ^2$ , defined as $\chi_{{\rm red}}^2=\frac{\chi^2}{N-\nu}$ with N the number of spectral lines and $\nu$ the number of degrees of freedom is also indicated.

Star
a₀ b₀ $\chi_{{\rm red}}^2$

R TrA 2.50 $\pm$ 4.55 28.48 $\pm$ 0.90 2

S Cru 2.13 $\pm$ 3.61 33.33 $\pm$ 0.90 2

Y Sgr 5.76 $\pm$ 3.53 34.01 $\pm$ 0.12 20

$\beta$ Dor 0.86 $\pm$ 1.31 31.59 $\pm$ 0.40 9

$\zeta$ Gem 1.09 $\pm$ 0.89 25.35 $\pm$ 0.31 7

RZ Vel 8.32 $\pm$ 5.95 47.31 $\pm$ 1.02 6

$\ell$ Car 2.89 $\pm$ 2.26 32.48 $\pm$ 0.67 15

RS Pup 5.89 $\pm$ 5.58 42.19 $\pm$ 0.88 4

**Table 3:** Linear relations between the amplitude of the velocity curves and the line depth (at minimum extension of the star), ${\Delta RV_c}= a_0 D + b_0$ are given for all stars, together with the $1\sigma$ uncertainty. The *reduced* $\chi ^2$ , defined as $\chi_{{\rm red}}^2=\frac{\chi^2}{N-\nu}$ with N the number of spectral lines and $\nu$ the number of degrees of freedom is also indicated.
Star	a₀	b₀	$\chi_{{\rm red}}^2$
R TrA	2.50 $\pm$ 4.55	28.48 $\pm$ 0.90	2
S Cru	2.13 $\pm$ 3.61	33.33 $\pm$ 0.90	2
Y Sgr	5.76 $\pm$ 3.53	34.01 $\pm$ 0.12	20
$\beta$ Dor	0.86 $\pm$ 1.31	31.59 $\pm$ 0.40	9
$\zeta$ Gem	1.09 $\pm$ 0.89	25.35 $\pm$ 0.31	7
RZ Vel	8.32 $\pm$ 5.95	47.31 $\pm$ 1.02	6
$\ell$ Car	2.89 $\pm$ 2.26	32.48 $\pm$ 0.67	15
RS Pup	5.89 $\pm$ 5.58	42.19 $\pm$ 0.88	4

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