Notes. Light curve descriptions in Col. 8: irr = irregular; irr.d = irregular with marked dips in brightness; irr.a = irregular with marked changes in amplitude; reg = mostly regular; reg.d1 = mostly regular with one dip near the end of the available time series; reg.at = mostly regular with variations in amplitude and mean magnitude comparable to half the mean amplitude; reg.atV = same as reg.at but with larger variations in the OGLE V light curve; reg.t = mostly regular short period pattern, but long term trends in the mean that are comparable or larger than the amplitude (possibly associated with a secondary long period). Notes on individual stars: HE 1428-1950 is a high galactic latitude star, which might be metal-poor and higher gravity than a typical AGB star (Placco et al. 2011). HD 202851 was assigned an approximate bolometric luminosity of –1.9 by Bergeat et al. (2002), which is lower than the expected luminosity of intrinsic C-stars on the thermally pulsing AGB. [W65] c2: Whitelock et al. (2006) note that Aaronson et al. (1988) find K = 7.21, (J − K) = 1.95, while Aaronson & Mould (1985) had values consistent with 2MASS and themselves. This star may have obscuration events.

Reference. (a) Hughes & Wood (1990). (b) Bergeat et al. (2002). Stars found non-variable by these authors based on Hipparcos satellite photometry are labelled nv in Col. 6. (c) Lançon & Wood (2000). (e) Christlieb et al. (2001). (f) Whitelock et al. (2006). (g) Cioni et al. (2003) with updates from Raimondo et al. (2005). (h) Frogel et al. (1990) with the distance moduli (m − M) = 18.90 for SMC cluster NGC 419 Sloan et al. (in prep.) and (m − M) = 19.06 for NGC 121 (Glatt et al. 2008). (i) General Catalog of Variable Stars (GCVS; Samus et al. 2007–2012). (k) OGLE LMC data in V and I (Soszyński et al. 2009, via Vizier). (l) OGLE SMC data in V and I (Soszyński et al. 2011, via Vizier). (m) EROS data in B and R (Kim et al. 2014). (n) MACHO data in B and R (Alcock et al. 1996, 2001 version via Vizier). (o) DIRBE data in J and K (Price et al. 2010, via Vizier). (p) Association Française des Observateurs d’Étoiles Variables (AFOEV). (q) American Association of Variable Star Observers (AAVSO). (r) ASAS data in V (Pojmanski 2002, via Vizier). (s) Our estimate based on (J − K) and Nowotny et al. (2013), see text. When in parentheses, the values are apparent magnitudes.