SUSPECTED
SCULPTOR DWARF
|
| [SS2022] 127 | IRAS - | GSC2.4.2 S09V001665 | AAVSO - |
| SIMBAD EV* SclG V0410 | Pan-STARRS 67440152159961798 | SAO - | VSX - |
| GAIA DR3 5027167170229506688 | SkyMapper - | WRAY - | GCVS - |
| 2MASS - | HIP - | Hen - | BD - |
| WISE - | TYC - | ESO - | HD - |
| Bidelman (1954) | - | Allen (1984) | - | Belzcyński et al. (2001) | - |
| Gaposchkin (1957) | - | Kenyon (1986) | - | Akras et al. (2019) | - |
| Boyarchuk (1969) | - | Vaidis (1988, 1991) | - |
| Right ascension (°) | 15.2160Ref | Parallax (mas) | -0.056±0.745Ref | Reddening E(B-V) (mag) | 0.02±0.0Ref, Note |
| Declination (°) | -33.7987Ref | Distance (kpc) | 1.31Ref, Note, 1.82Ref, Note | ||
| Galactic longitude (°) | 286.5831Ref | Proper motion in α (mas/yr) | 0.92±0.82Ref | ||
| Galactic latitude (°) | -83.0278Ref | Proper motion in δ (mas/yr) | -0.66±0.51Ref |
| X-Ray | YesRef | IR type | - | Radio | - |
| X-Ray type | - | J (mag) | - | Flickering | - |
| GALEX FUV (mag) | - | H (mag) | - | Outbursts | - |
| GALEX NUV (mag) | 21.04Ref | K (mag) | - | Outburst type | - |
| IUE | NoRef | WISE W1 (mag) | - | Jets | - |
| FUSE | NoRef | WISE W2 (mag) | - | Resolved nebula | - |
| U (mag) | - | WISE W3 (mag) | - | IPmax (eV) | - |
| B (mag) | 21.27Ref | WISE W4 (mag) | - | [O III] lines | - |
| V (mag) | 20.90Ref | IRAS 12μm (Jy) | - | He II lines | - |
| R (mag) | - | IRAS 25μm (Jy) | - | [Fe VII] lines | - |
| I (mag) | 20.24Ref | IRAS 60μm (Jy) | - | O VI lines | - |
| BP (mag) | 20.45Ref | IRAS 100μm (Jy) | - | ||
| G (mag) | 20.37Ref | AKARI S09 (Jy) | - | ||
| RP (mag) | 19.94Ref | 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 | - | Mass (M⊙) | - | Pulsation | - |
| Eff. temperature (K) | - | Radius (R⊙) | - | Type | - |
| IR type | - | Luminosity (L⊙) | - | Pulsation period (days) | - |
| Metallicity [Fe/H] | - | Pulsation ephemeris | - |
| Type/Spectral type | - | Mass (M⊙) | - | Spin period (min) | - |
| Shell-burning/Accreting-only | - | Radius (R⊙) | - | Accretion disk | - |
| Eff. temperature (K) | - | Luminosity (L⊙) | - | ||
| Lower limit (K) | - | ||||
| Upper limit (K) | - |
In the first arXiv version of the paper by Saeedi & Sasaki (2022), the star was initially considered as a symbiotic star candidate. However, it was later reclassified as a possible QLMXB. Additionally, there was a suggestion that this star is an eclipsing binary with a period of 0.96 days, as mentioned in Martínez-vázquez et al. (2016).