Variable stars in the globular cluster NGC 7492 - New discoveries and physical parameter determination

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Volume 556 (August 2013)

A&A, 556 (2013) A20

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This article has an erratum: [https://doi.org/10.1051/0004-6361/201220824e]

Table 2

Celestial coordinates for all of the confirmed and candidate variables in our field of view, except V3, which lies outside of our field of view.

ID	type	RA	Dec	Epoch	P	V	V − R	Amp (V)	Amp(R)
		(J2000)	(J2000)	(days)	(days)	(mag)	(mag)	(mag)	(mag)

V1	RR0	23:08:26.68	–15:34:58.5	2 453 949.4046	0.805012	17.303^b	0.264^b	0.511	0.408
V2	RR1	23:08:25.00	–15:35:52.9	2 453 284.2652	0.411764^a	17.256^b	0.188^b	0.251	0.140
V4	LPV	23:08:23.19	–15:39:06.0	–	~21.7	14.271^c	–	~0.18	–
V5	LPV	23:08:39.08	–15:34:36.3	–	–	14.258^c	–	>0.33	–
V6	SX Phe	23:08:29.16	–15:36:51.1	2 454 318.3687	0.0565500	19.235^b	0.166^b	0.136	0.058
V7	SX Phe	23:08:19.83	–15:37:33.6	2 454 839.0479	0.0725859	19.363^b	0.448^b	0.050	–
CSX1	SX Phe?	23:08:32.73	–15:35:03.4	–	–	19.499^c	0.210^c	~0.15	0.09?

Notes. The coordinates correspond to the epoch of the V reference image, which is the heliocentric Julian date ~2 453 284.26 d. We also include in this table the epoch, period, mean V magnitude, V − R colour, and the full amplitude of each variable.

^(a)

If we consider a secular period change, the period is P₀ = 0.412119 d at the epoch E = 2 453 284.2652 d and the period change rate is β ≈ 47 d Myr^-1.

^(b)

Intensity-weighted magnitude calculated from the light curve model.

^(c)

Mean magnitude from our data.

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