CONFIRMED
M31
|
| M31SyS J004233.17+412720.7 | IRAS - | GSC2.4.2 NBW9095221 | AAVSO - |
| SIMBAD M31SyS J004233.17+412720.7 | Pan-STARRS 157740106381347544 | SAO - | VSX - |
| GAIA DR3 - | SkyMapper - | WRAY - | GCVS - |
| 2MASS J00423313+4127207 | HIP - | Hen - | BD - |
| WISE - | TYC - | ESO - | HD - |
| Bidelman (1954) | - | Allen (1984) | - | Belzcyński et al. (2001) | - |
| Gaposchkin (1957) | - | Kenyon (1986) | - | Akras et al. (2019) | M31 SySt-14 (Conf.) |
| Boyarchuk (1969) | - | Vaidis (1988, 1991) | - |
| Right ascension (°) | 10.6382Ref | Parallax (mas) | - | Reddening E(B-V) (mag) | 0.33±0.06Ref, Note |
| Declination (°) | 41.4558Ref | Distance (kpc) | 785±25Ref -, Note |
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| Galactic longitude (°) | 121.1442Ref | Proper motion in α (mas/yr) | - | ||
| Galactic latitude (°) | -21.3852Ref | Proper motion in δ (mas/yr) | - |
| X-Ray | NoRef | IR type | SRef | Radio | - |
| X-Ray type | - | J (mag) | 17.97Ref | Flickering | - |
| GALEX FUV (mag) | - | H (mag) | 17.02Ref | Outbursts | - |
| GALEX NUV (mag) | - | K (mag) | 16.74Ref | Outburst type | - |
| IUE | NoRef | WISE W1 (mag) | - | Jets | - |
| FUSE | NoRef | WISE W2 (mag) | - | Resolved nebula | - |
| U (mag) | - | WISE W3 (mag) | - | IPmax (eV) | 233.6Ref |
| B (mag) | - | WISE W4 (mag) | - | [O III] lines | YesRef |
| V (mag) | - | IRAS 12μm (Jy) | - | He II lines | YesRef |
| R (mag) | - | IRAS 25μm (Jy) | - | [Fe VII] lines | YesRef |
| I (mag) | 19.77Ref | IRAS 60μm (Jy) | - | O VI lines | YesRef |
| BP (mag) | - | IRAS 100μm (Jy) | - | ||
| G (mag) | - | AKARI S09 (Jy) | - | ||
| RP (mag) | - | 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 | M4Ref | Mass (M⊙) | - | Pulsation | - |
| Eff. temperature (K) | - | Radius (R⊙) | - | Type | - |
| IR type | SRef | 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) | 235000Ref | ||||
| Upper limit (K) | 320000Ref |
The most exceptional property of this object is the presence of very strong coronal [Fe X] 6374 Å and [Fe IX] 7892 Å emission lines. Combined with the fairly strong Raman-scattered O VI and [Fe VII] emission lines, this places M31SyS J004233.17+412720.7 among those symbiotic stars with the highest degree of ionization. According to Mikołajewska et al. (2014), this is also strongly suggestive that the system may be a supersoft X-ray source.