CONFIRMED
LMC
|
| SMP LMC 94 | IRAS Z05551-7302 | GSC2.4.2 S0UG003039 | AAVSO 000-BLT-636 |
| SIMBAD LHA 120-S 170 | Pan-STARRS - | SAO - | VSX - |
| GAIA DR3 4650589664700853504 | SkyMapper 055409.52-730234.2 | WRAY - | GCVS - |
| 2MASS J05540952-7302341 | HIP - | Hen - | BD - |
| WISE J055409.53-730234.1 | TYC - | ESO - | HD - |
| Bidelman (1954) | - | Allen (1984) | - | Belzcyński et al. (2001) | SMP LMC 94 (Conf.) |
| Gaposchkin (1957) | - | Kenyon (1986) | - | Akras et al. (2019) | SMP LMC 94 (Conf.) |
| Boyarchuk (1969) | - | Vaidis (1988, 1991) | - |
| Right ascension (°) | 88.5397Ref | Parallax (mas) | 0.016±0.051Ref | Reddening E(B-V) (mag) | 0.1±0.0Ref, Note |
| Declination (°) | -73.0428Ref | Distance (kpc) | 49.97±0.19Ref 9.90Ref, Note, 4.95Ref, Note |
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| Galactic longitude (°) | 283.8820Ref | Proper motion in α (mas/yr) | 1.87±0.06Ref | ||
| Galactic latitude (°) | -30.0238Ref | Proper motion in δ (mas/yr) | 1.01±0.07Ref |
| X-Ray | - | IR type | DRef | Radio | - |
| X-Ray type | - | J (mag) | 14.54Ref | Flickering | - |
| GALEX FUV (mag) | 17.34Ref | H (mag) | 12.77Ref | Outbursts | - |
| GALEX NUV (mag) | 19.33Ref | K (mag) | 11.38Ref | Outburst type | - |
| IUE | NoRef | WISE W1 (mag) | 9.86Ref | Jets | - |
| FUSE | NoRef | WISE W2 (mag) | 8.96Ref | Resolved nebula | - |
| U (mag) | - | WISE W3 (mag) | 6.89Ref | IPmax (eV) | 114Ref |
| B (mag) | 17.27Ref | WISE W4 (mag) | 5.53Ref | [O III] lines | YesRef |
| V (mag) | - | IRAS 12μm (Jy) | - | He II lines | YesRef |
| R (mag) | - | IRAS 25μm (Jy) | - | [Fe VII] lines | NoRef |
| I (mag) | 13.78Ref | IRAS 60μm (Jy) | - | O VI lines | YesRef |
| BP (mag) | 17.05Ref | IRAS 100μm (Jy) | - | ||
| G (mag) | 16.74Ref | AKARI S09 (Jy) | 0.08Ref | ||
| RP (mag) | 16.12Ref | 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 | MRef | Mass (M⊙) | - | Pulsation | - |
| Eff. temperature (K) | - | Radius (R⊙) | - | Type | - |
| IR type | DRef | Luminosity (L⊙) | - | Pulsation period (days) | - |
| Metallicity [Fe/H] | - | Pulsation ephemeris | - |
| Type/Spectral type | - | Mass (M⊙) | - | Spin period (min) | - |
| Shell-burning/Accreting-only | shell-burningRef | Radius (R⊙) | - | Accretion disk | - |
| Eff. temperature (K) | - | Luminosity (L⊙) | - | ||
| Lower limit (K) | - | ||||
| Upper limit (K) | - |
Although included number of times in several surveys of PNe, Raman-scattered O VI lines were observed by Dopita et al. (1985). No M giant spectrum is observed, as incorrectly listed in Belczyński et al. (2000). Lack of strong variability, along with a strong IR excess, is consistent with a D-type SySt (Angeloni et al., 2014).