LIKELY
SMC
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| LIN 250 | IRAS - | GSC2.4.2 S0XH519752 | AAVSO 000-BLL-502 |
| SIMBAD LHA 115-S 18 | Pan-STARRS - | SAO - | VSX 399934 |
| GAIA DR3 4688986534938381184 | SkyMapper 005409.52-724143.3 | WRAY - | GCVS - |
| 2MASS J00540955-7241431 | HIP - | Hen - | BD - |
| WISE J005409.55-724143.2 | TYC - | ESO - | HD - |
| Bidelman (1954) | - | Allen (1984) | - | Belzcyński et al. (2001) | - |
| Gaposchkin (1957) | - | Kenyon (1986) | - | Akras et al. (2019) | LHA 115-S 18 (Conf.) |
| Boyarchuk (1969) | - | Vaidis (1988, 1991) | - |
| Right ascension (°) | 13.5398Ref | Parallax (mas) | -0.102±0.018Ref | Reddening E(B-V) (mag) | 0.37±0.03Ref, Note |
| Declination (°) | -72.6954Ref | Distance (kpc) | 62.1±1.9Ref 40.70Ref, Note, 42.15Ref, Note |
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| Galactic longitude (°) | 302.6486Ref | Proper motion in α (mas/yr) | 0.76±0.02Ref | ||
| Galactic latitude (°) | -44.4314Ref | Proper motion in δ (mas/yr) | -1.34±0.02Ref |
| X-Ray | NoRef | IR type | D'?Ref | Radio | - |
| X-Ray type | - | J (mag) | 12.35Ref | Flickering | - |
| GALEX FUV (mag) | - | H (mag) | 11.93Ref | Outbursts | - |
| GALEX NUV (mag) | - | K (mag) | 11.11Ref | Outburst type | - |
| IUE | NoRef | WISE W1 (mag) | 9.38Ref | Jets | - |
| FUSE | NoRef | WISE W2 (mag) | 8.36Ref | Resolved nebula | - |
| U (mag) | 12.94Ref | WISE W3 (mag) | 6.28Ref | IPmax (eV) | 114Ref |
| B (mag) | 13.48Ref | WISE W4 (mag) | 4.88Ref | [O III] lines | NoRef |
| V (mag) | 13.82Ref | IRAS 12μm (Jy) | - | He II lines | YesRef |
| R (mag) | 12.79Ref | IRAS 25μm (Jy) | - | [Fe VII] lines | NoRef |
| I (mag) | 15.22Ref | IRAS 60μm (Jy) | - | O VI lines | YesRef |
| BP (mag) | 13.28Ref | IRAS 100μm (Jy) | - | ||
| G (mag) | 13.09Ref | AKARI S09 (Jy) | 0.12Ref | ||
| RP (mag) | 12.66Ref | AKARI S18 (Jy) | - |
| Orbital period (days) | - | γ velocity (km/h) | - | Size of giant’s orbit (AU) | - |
| Eccentricity | - | RV of giant (km/h) | - | Separation (AU) | - |
| Inclination (°) | - | Inferior conj. of giant (JD) | - | Mass function | - |
| Eclipses | - | Mass ratio | - | ||
| Orbital ephemeris | - |
| Spectral type | B0 I [e]Ref | Mass (M⊙) | 35-40Ref | Pulsation | - |
| Eff. temperature (K) | 25000Ref | Radius (R⊙) | 33-36Ref | Type | - |
| IR type | D'?Ref | Luminosity (L⊙) | 300000-460000Ref | Pulsation period (days) | - |
| Metallicity [Fe/H] | - | Pulsation ephemeris | - |
| Type/Spectral type | - | Mass (M⊙) | - | Spin period (min) | - |
| Shell-burning/Accreting-only | shell-burning?Ref | Radius (R⊙) | - | Accretion disk | - |
| Eff. temperature (K) | - | Luminosity (L⊙) | - | ||
| Lower limit (K) | - | ||||
| Upper limit (K) | - |
LHA 115-S 18 is a very peculiar emission-line star exhibiting the B[e] phenomenon. Its spectrum shows features of an extremely wide range of excitation and ionization stages, extending from highly ionized atomic lines (Si IV, C IV, He II) in the ultraviolet and optical regions to molecular emission bands of CO and TiO in the optical and infrared regions (Torres et al., 2012). Raman-scattered O VI lines were also observed in the spectra of the star. However, according to their analysis, a symbiotic B[e] scenario seems not to be the most plausible. Therefore, it was classified as a suspected symbiotic star. On the other hand, Akras et al. (2019) lists this star as confirmed.