**Table 1:** Observed sample of Cepheids sorted by increasing period.
Name	HD	P^a	T₀^a	Nb.	Nb. of	${m_{\rm V}}^b$
		[days]	[days]	of spectra	cycles
R TrA	135592	3.38925	2 451 649.96	14	15	6.66
S Cru	112044	4.68976	2 451 645.64	12	3	6.60
Y Sgr	168608	5.77338	2 451 650.92	17	10	5.74
$\beta$ Dor	37350	9.84262	2 451 643.54	49	3	3.75
$\zeta$ Gem	52973	10.14960	2 451 641.78	50	3	3.90
Y Oph	162714	17.12520	2 451 653.32	7	4	6.17
RZ Vel	73502	20.40020	2 451 633.58	10	3	7.08
$\ell$ Car	84810	35.551341	2 452 290.4158	118	2	3.74
RS Pup	68860	41.51500	2 451 644.22	15	3	7.03

^a For $\ell$ Car, the reference Julian date (T₀) and the pulsation period (P) used to compute the phase are from Szabados (1989). For others stars we used ephemeris from Berdnikov et al. (2001).
^b The visible magnitude ( ${m_{\rm V}}$ ) is from Berdnikov et al. (2000).

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