Water vapour masers in long-period variable stars - IV. Mira variables RCas, o Cet and R Leo

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Table 1

Basic information on the observed long-period Mira variables.

Name	α (J2000) δ		D^a pc	V_* km s⁻¹	V_exp km s⁻¹	V_b, V_r km s⁻¹	P_opt days	P_rad days	ϕ_lag	Observing period	Notes^b
Name	h m s	° ′ ″	D^a pc	V_* km s⁻¹	V_exp km s⁻¹	V_b, V_r km s⁻¹	P_opt days	P_rad days	ϕ_lag	Observing period	Notes^b
o Cet	02:19:20.8	−02:58:37	92 $_{- 10}^{+ 11}$ $^{+11}_{-10}$	46.5	8.0	45.6, 48.6	332	336 ± 3	0.33^f	1990-2023	2, 3, 9, 13
R Leo	09:47:33.5	+11:25:44	71 $_{- 11}^{+ 17}$ $^{+17}_{-11}$	0.0	9.0	−2.2, 1.7	310	−	−	1988-2015	1-5, 9
χ Cyg	19:50:34.0	+32:54:51	160 $_{- 7}^{+ 7}$ $^{+7}_{-7}$	10.0	8.5	−	407	−	−	1995-2009	2, 3, 7, 9
R Cas	23:58:24.7	+51:23:20	174 $_{- 6}^{+ 6}$ $^{+6}_{-6}$	26.0	13.5	22.2, 32.1	431	430±4	0.32^§	1987-2023	2-7, 9

Notes. We list the distance D, the stellar radial velocity V_*, the final expansion velocity in the CSE V_exp, and the extreme blue V_b and red V_r velocities of the H₂O-maser emission. P_opt and P_rad are the optical and radio period, respectively, and φ_lag is the difference in phase between the two. The entries in the table are discussed in the sections pertaining to the individual stars. References. ^(a) For distances: o Cet, R Leo: van Leeuwen (2008); χ Cyg, R Cas: Gaia Collaboration (2020) (EDR3). ^(b) For stellar systemic and expansion velocities. 1. Danilovich et al. (2015); 2. De Beck et al. (2010); 3. de Vicente et al. (2016); 4. Gonzalez-Alfonso et al. (1998); 5. González Delgado et al. (2003); 6. Loup et al. (1993); 7. Neri et al. (1998); 8. Sánchez Contreras et al. (2000); 9. Teyssier et al. (2006); 10. Chapman et al. (1994); 11. Young (1995); 12. Kerschbaum & Olofsson (1999); 13. Kemper et al. (2003). Phase lags: b calculated for 1995 -2011; §: calculated for 1987-1999.

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