SUSPECTED
MILKY WAY
|
| 2MASS J06422218-0226285 | IRAS - | GSC2.4.2 S3BM059715 | AAVSO - |
| SIMBAD 2MASS J06422218-0226285 | Pan-STARRS 105071005924600919 | SAO - | VSX 462843 |
| GAIA DR3 3106532630968847232 | SkyMapper 064222.19-022628.4 | WRAY - | GCVS - |
| 2MASS J06422218-0226285 | HIP - | Hen - | BD - |
| WISE J064222.18-022628.5 | 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 (°) | 100.5925Ref | Parallax (mas) | 0.094±0.036Ref | Reddening E(B-V) (mag) | 1.07±0.05Ref, Note |
| Declination (°) | -2.4413Ref | Distance (kpc) | 6.56Ref, Note, 7.39Ref, Note | ||
| Galactic longitude (°) | 214.0732Ref | Proper motion in α (mas/yr) | -0.24±0.04Ref | ||
| Galactic latitude (°) | -3.1297Ref | Proper motion in δ (mas/yr) | 0.22±0.04Ref |
| X-Ray | - | IR type | D'?Ref | Radio | - |
| X-Ray type | - | J (mag) | 15.85Ref | Flickering | - |
| GALEX FUV (mag) | - | H (mag) | 14.90Ref | Outbursts | Yes?Ref |
| GALEX NUV (mag) | - | K (mag) | 13.75Ref | Outburst type | - |
| IUE | NoRef | WISE W1 (mag) | 11.54Ref | Jets | - |
| FUSE | NoRef | WISE W2 (mag) | 10.42Ref | Resolved nebula | - |
| U (mag) | - | WISE W3 (mag) | 7.77Ref | IPmax (eV) | - |
| B (mag) | - | WISE W4 (mag) | 5.30Ref | [O III] lines | - |
| V (mag) | - | IRAS 12μm (Jy) | - | He II lines | - |
| R (mag) | - | IRAS 25μm (Jy) | - | [Fe VII] lines | - |
| I (mag) | 17.47Ref | IRAS 60μm (Jy) | - | O VI lines | - |
| BP (mag) | 17.27Ref | IRAS 100μm (Jy) | - | ||
| G (mag) | 15.80Ref | AKARI S09 (Jy) | - | ||
| RP (mag) | 14.62Ref | 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 | D'?Ref | 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) | - |
The star underwent a brightness increase in 2012-2013 and has remained in a high state since then. It is suggested to be a potential symbiotic binary, CV, or YSO (Blex et al., 2018).