Estimating the parameters of globular cluster M 30 (NGC 7099) from time-series photometry

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Volume 555 (July 2013)

A&A, 555 (2013) A36

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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	0.74365^a	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
V4^b	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
V19^c	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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