XMMM31 J004307.1+411810

SUSPECTED M31  

Equatorial coordinates
α =  10.779000 | 00 43 06.960000
δ =  41.302750 | +41 18 09.900000
 
Constellation Andromeda
Symbiotic IR Type  
Spectral Type  
Magnitude range (V)  
Outbursts Yes

Identifiers

XMMM31 J004307.1+411810 GSC TYC WRAY
SIMBAD NAME Nova RJC99 Jul-98 HIP SAO Hen
BD IRAS  GAIA DR2  ESO
HD 2MASS  WISE  AAVSO 

Position

Right ascension (°) 10.779000ref Parallax (mas) Reddening E(B-V) (mag) 0.474 ± 0.091ref
Declination (°) 41.302750ref Distance (kpc) 785.00 ± 25.00ref    
Galactic longitude (°) 121.251760ref Proper motion in α (mas/yr)    
Galactic latitude (°) -21.541850ref Proper motion in δ (mas/yr)    

Observations

U (mag)   X-Ray Yesref   Flickering  
B (mag)   X-Ray type   Outbursts Yesref
V (mag)   IUE No Type SyN?ref
R (mag)   IRAS flux at 12 μm (Jy)   IPmax (eV)  
I (mag)   IRAS flux at 25 μm (Jy)   OVI lines  
G (mag)   IRAS flux at 60 μm (Jy)      
J (mag)   IRAS flux at 100 μm (Jy)      
H (mag)   WISE W1 (mag)      
K (mag)   WISE W2 (mag)      
L (mag)   WISE W3 (mag)      
    WISE W4 (mag)      
    Radio      
    Radio flux (mJy)      

Orbit

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  
Ephemeris type       Mass ratio  
Ephemeris T(JD)          

Cool component

Spectral type   Mass (M)   Pulsation  
Eff. temperature (K)   Radius (R)   Type  
IR type   Luminosity (L)   Pulsation period (days)  
Metallicity [Fe/H]       Ephemeris type  
        Ephemeris T(JD)  

Hot component

Type/Spectra   Mass (M)   Spin period (min)  
Eff. temperature (K)   Radius (R)   Accretion disk  
Lower limit (K)   Luminosity (L)      
Upper limit (K)          

Links

SIMBAD     CDS Portal


Notes

Identified as an X-ray source in M31. Di Stefano et al. (2004) identified the object as a possible symbiotic system, they also identified an optical counterpart. Pietsch et al. (2005) concluded that the object showed a nova eruption in 1998. The interesting transition from soft X-ray spectrum to a hard spectrum was observed (Stiele et al., 2010). An alternative to symbiotic binary is a black hole transient (Stiele et al., 2010).


References

  • Di Stefano, R., Kong, A. K. H., Greiner, J., et al., 2004, ApJ, 610, 247, 2004ApJ…610..247D
  • Pietsch, W., Fliri, J., Freyberg, M. J., et al., 2005, A&A, 442, 879, 2005A&A…442..879P
  • Stiele, H., Pietsch, W., Haberl, F., et al., 2010, Astronomische Nachrichten, 331, 212, 2010AN….331..212S

Last updated: May 12, 2019 @ 7:39 pm