Water vapour masers in long-period variable stars - III. Mira variables U Her and RR Aql

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Table 1

Basic information on the two Mira variables monitored in the period 1990–2011.

Name	α (J2000) δ		D^(a)	V_*^(b)	V_exp^(b)	V_b,V_r	P_opt	TJD_max	P_rad	ϕ_lag
	h m s	◦ ′ ″	pc	km s⁻¹	km s⁻¹	km s⁻¹	days	days	days
U Her	16:25:47.5	+ 18:53:33	$266_{- 18}^{+ 32}$ $266_{ - 18}^{ + 32}$	−15.0	13.1	−23.3, −7.1	405	6668 ± 3	407 ± 11	0.16
RR Aql	19:57:36.1	−01:53:11	$410_{- 11}^{+ 12}$ $410_{ - 11}^{ + 12}$	28.5	9.0	23.2, 31.9	400	6487 ± 5	400±5	0.21

Notes. Columns give the object name, coordinates, distance, stellar velocity, final expansion velocity of the CSE, the blue (b) and red (r) velocity boundaries of the maser emission, optical period, the date of the last optical maximum before the start of the monitoring, the radio period, and the phase-lag between radio and optical light curves.

References.^(a) For distances: U Her: Vlemmings & van Langevelde (2007); RR Aql: Sun et al. (2022). ^(b) For stellar systemic and expansion velocities: U Her: Gonzalez-Alfonso et al. (1998); RR Aql: Danilovich et al. (2015).

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