M31SyS J004322.50+413940.9


Equatorial coordinates
α =  10.843652 ± 0.451500 | 00 43 22.476598
δ =  41.661356 ± 0.403300 | +41 39 40.883232
Constellation Andromeda
Symbiotic IR Type S+IR🡕
Spectral Type M4
Magnitude range (V)  
Outbursts Yes?


M31SyS J004322.50+413940.9 GSC TYC WRAY
SIMBAD M31SyS J004322.50+413940.9 HIP SAO Hen
BD – IRAS  GAIA DR2 381299259441348736 ESO
HD 2MASS J00432249+4139409 WISE  AAVSO


Right ascension (°) 10.843652 ± 0.451500ref  Parallax (mas) Reddening E(B-V) (mag) 0.256 ± 0.031ref
Declination (°) 41.661356 ± 0.403300ref Distance (kpc) 785.00 ± 25.00ref    
Galactic longitude (°) 121.316886 ± 0.403300ref Proper motion in α (mas/yr)    
Galactic latitude (°) -21.185107 ± 0.451500ref Proper motion in δ (mas/yr)    


U (mag) 20.69ref X-Ray   Flickering  
B (mag) 21.19ref X-Ray type   Outbursts Yes?ref
V (mag) 20.35ref IUE No Type  
R (mag) 19.90ref IRAS flux at 12 μm (Jy)   IPmax (eV) 13.6ref
I (mag) 19.10ref IRAS flux at 25 μm (Jy)   OVI lines Noref
G (mag) 19.93ref IRAS flux at 60 μm (Jy)      
J (mag) 17.39ref IRAS flux at 100 μm (Jy)      
H (mag) 16.17ref WISE W1 (mag)      
K (mag) 15.91ref WISE W2 (mag)      
L (mag)   WISE W3 (mag)      
    WISE W4 (mag)      
    Radio flux (mJy)      


Orbital period (days) ∼900ref 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 Yesref
Eff. temperature (K)   Radius (R)   Type Low-amplitude SR pulsations?ref
IR type S+IR🡕, ref Luminosity (L)   Pulsation period (days) ∼80ref
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) 14000ref Luminosity (L)      
Upper limit (K)          


SIMBAD     CDS Portal


Classified as a suspected symbiotic binary in Mikołajewska et al. (2014). They also noted that the object shows a very rich, low-excitation emission line spectrum, including H I, numerous Fe II and [Fe II], and Na I D, and very strong Ca II T lines.H I and other permitted lines show P Cyg profiles with absorption component blueshifted by ∼350 km/s with respect to the emission peak. The ∼900-d period reported by An et al. (2004) very likely represents orbital variation. The shorter period P ∼80 d (Vilardell et al. 2006) may be due to low-amplitude SR pulsation of the red giant. 


Last updated: May 2, 2019 @ 11:13 am