SUSPECTED
M31
|
| XMMM31 J004307.1+411810 | IRAS - | GSC2.4.2 NBVE342425 | AAVSO - |
| SIMBAD NAME Nova RJC99 Jul-98 | Pan-STARRS 157560107782503204 | SAO - | VSX - |
| GAIA DR3 - | 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 (°) | 10.7786Ref | Parallax (mas) | - | Reddening E(B-V) (mag) | 0.47±0.09Ref, Note |
| Declination (°) | 41.3024Ref | Distance (kpc) | 785±25Ref -, Note |
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| Galactic longitude (°) | 121.2514Ref | Proper motion in α (mas/yr) | - | ||
| Galactic latitude (°) | -21.5422Ref | Proper motion in δ (mas/yr) | - |
| X-Ray | YesRef | IR type | - | Radio | - |
| X-Ray type | β?Ref | J (mag) | - | Flickering | - |
| GALEX FUV (mag) | - | H (mag) | - | Outbursts | YesRef |
| GALEX NUV (mag) | - | K (mag) | - | Outburst type | SyRN?Ref |
| IUE | NoRef | WISE W1 (mag) | - | Jets | - |
| FUSE | NoRef | WISE W2 (mag) | - | Resolved nebula | - |
| U (mag) | - | WISE W3 (mag) | - | IPmax (eV) | - |
| B (mag) | - | WISE W4 (mag) | - | [O III] lines | - |
| V (mag) | - | IRAS 12μm (Jy) | - | He II lines | - |
| R (mag) | - | IRAS 25μm (Jy) | - | [Fe VII] lines | - |
| I (mag) | - | IRAS 60μm (Jy) | - | O VI lines | - |
| 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 | - | 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) | - |
Identified as an X-ray source in M31, Di Stefano et al. (2004) designated the object as a possible symbiotic system and identified an optical counterpart. Pietsch et al. (2005) concluded that the object showed a nova eruption in 1998. An interesting transition from a soft X-ray spectrum to a hard spectrum was observed (Stiele et al., 2010). As an alternative to a symbiotic binary, a black hole transient was proposed (Stiele et al., 2010). The light curve presented by Lee et al. (2012) shows only one epoch when the star was brighter than average, making the classification as a slow symbiotic nova less probable.