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This article has an erratum: [https://doi.org/10.1051/0004-6361/201321819e]


Table 5

Epochs, periods, mean magnitudes and amplitudes A in V and I for all confirmed variable stars in M 30.

# Epoch P P (Rosino P (Pietrukowicz ⟨ V ⟩ ⟨ I ⟩ A V A I Type
(HJD-2 450 000) (d) 1949) (d) et al. 2004) (d) (mag) (mag) (mag) (mag)

V1 6160.8234 0.7436296 0.74365a 0.751 15.12 14.52 0.93 0.74 RR0
V2 6150.8616 0.6535119 0.6535049 15.20 14.62 0.92 0.65 RR0
V3 6147.8307 0.6963265 0.69632 15.12 14.54 0.94 0.67 RR0
V4b 6147.8569 0.092318 20.19 19.14 2.74 1.91 U Gem
V14 6150.8758 0.347953 15.18 14.77 0.48 0.32 RR1
V15 6160.7960 0.679015 0.689 15.07 14.52 1.08 0.68 RR0
V16 6190.7559 0.325366 15.22 14.81 0.33 0.27 RR1
V17 6150.8805 0.059954 14.14 13.08 0.07 0.04 SX Phoenicis + blend?
V18 6161.8536 0.307099 17.43 17.19 0.41 0.49 Eclipsing blue straggler
V19c 5779.8451 0.343379 0.341 13.85 13.10 0.15 0.11 RR1
V20 6147.8377 0.040199 17.79 17.57 0.15 0.13 SX Phoenicis
V21 6147.8589 0.113151 17.87 17.11 ~0.2 ?

Notes.For RR Lyrae stars, ⟨ V ⟩ and ⟨ I ⟩ are intensity-weighted mean magnitudes, while for the other variables, they are inverse-variance-weighted mean magnitudes.

(a)

Rosino (1961) revised the period of V1 to 0.743608 d.

(b)

The period given for V4 is that of the sinusoidal variations seen during the quiescent part of the light curve, and the mean magnitudes are also those during quiescent phase; outburst mean magnitudes are given in the text (see Sect. 3.4).

(c)

For V19, the mean magnitudes are overestimated and amplitudes are underestimated due to blending, as discussed in the text.

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