M31SyS J004233.17+412720.7

CONFIRMED M31  

Equatorial coordinates
α =  10.638196 | 00 42 33.167000
δ =  41.455753 | +41 27 20.712000
 
Constellation Andromeda
Symbiotic IR Type S
Spectral Type M4
Magnitude range (V)  
Outbursts No

Identifiers

M31SyS J004233.17+412720.7 GSC TYC WRAY
SIMBAD M31SyS J004233.17+412720.7 HIP SAO Hen
BD – IRAS  GAIA DR2  ESO
HD 2MASS J00423313+4127207 WISE  AAVSO

Position

Right ascension (°) 10.638196ref Parallax (mas) Reddening E(B-V) (mag) 0.330 ± 0.060ref
Declination (°) 41.455753ref Distance (kpc) 785.00 ± 25.00ref    
Galactic longitude (°) 121.144204ref Proper motion in α (mas/yr)    
Galactic latitude (°) -21.385153ref Proper motion in δ (mas/yr)    

Observations

U (mag)   X-Ray   Flickering  
B (mag)   X-Ray type   Outbursts No
V (mag)   IUE No Type  
R (mag)   IRAS flux at 12 μm (Jy)   IPmax (eV) 233.6ref
I (mag) 19.77ref IRAS flux at 25 μm (Jy)   OVI lines Yesref
G (mag)   IRAS flux at 60 μm (Jy)      
J (mag) 16.82ref IRAS flux at 100 μm (Jy)      
H (mag) 15.88ref WISE W1 (mag)      
K (mag) 15.50ref 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 M4ref Mass (M)   Pulsation  
Eff. temperature (K)   Radius (R)   Type  
IR type Sref 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) 235000ref Luminosity (L)      
Upper limit (K) 320000ref        

Links

SIMBAD     CDS Portal


Notes

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, that combined with the fairly strong Raman-scattered O VI, and [Fe VII] emission lines places M31SyS J004233.17+412720.7 amongst those SySt with the highest degree of ionization. According to Mikołajewska et al. (2014) it is also strongly suggesting that this system may be supersoft X-ray source.


References

Last updated: Jan 14, 2019 @ 9:53 am