M33SyS J013435.17+303409.4

CONFIRMED M33  

Equatorial coordinates
α =  23.646416 | 01 34 35.140000
δ =  30.569304 | +30 34 09.490000
 
Constellation Triangulum
Symbiotic IR Type  
Spectral Type Mira, CN
Magnitude range (V)  
Outbursts  

Identifiers

M33SyS J013435.17+303409.4 GSC TYC WRAY
SIMBAD M33SyS J013435.17+303409.4 HIP SAO Hen
BD – IRAS  GAIA DR2  ESO
HD 2MASS  WISE  AAVSO

Position

Right ascension (°) 23.646416ref Parallax (mas) Reddening E(B-V) (mag) 0.041 ± 0.002ref
Declination (°) 30.569304ref Distance (kpc) 847.00 ± 60.00ref    
Galactic longitude (°) 133.813055ref Proper motion in α (mas/yr)    
Galactic latitude (°) -31.389151ref Proper motion in δ (mas/yr)    

Observations

U (mag)   X-Ray   Flickering  
B (mag)   X-Ray type   Outbursts No
V (mag) 23.79ref IUE No Type  
R (mag) 22.14ref IRAS flux at 12 μm (Jy)   IPmax (eV) 54.4ref
I (mag) 20.59ref IRAS flux at 25 μm (Jy)   OVI lines Noref
G (mag)   IRAS flux at 60 μm (Jy)      
J (mag) 17.97ref IRAS flux at 100 μm (Jy)      
H (mag) 17.02ref WISE W1 (mag)      
K (mag) 16.74ref 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 Mira, CNref Mass (M)   Pulsation Yesref
Eff. temperature (K)   Radius (R)   Type Miraref
IR type   Luminosity (L)   Pulsation period (days) ∼300ref
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) 54000ref Luminosity (L)      
Upper limit (K) 142000ref        

Links

SIMBAD     CDS Portal


Notes

M33SyS J013435.17+303409.4 is definitely a Mira variable with a period of ∼300d, however, its JHK magnitudes and colours do not show any evidence for an optically thick dust found in the majority of Galactic symbiotic Miras (Mikołajewska et al., 2017).


References

  • Mikołajewska, J., Shara, M. M., Caldwell, N., et al., 2017, MNRAS, 465, 699, 2017MNRAS.465.1699M

Last updated: Jan 13, 2019 @ 1:00 pm