SMP LMC 94

CONFIRMED LMC  

Equatorial coordinates
α =  88.539725 ± 0.064925 | 05 54 09.528050
δ =  -73.042819 ± 0.067087 | -73 02 34.167256
 
Constellation Mensa
Symbiotic IR Type D🡕
Spectral Type Mira
Magnitude range (V)  
Outbursts No

Identifiers

SMP LMC 94 GSC TYC WRAY
SIMBAD LHA 120-S 170 HIP SAO Hen
BD – IRAS Z05551-7302 GAIA DR2 4650589664700853504 ESO
HD 2MASS J05540952-7302341 WISE J055409.53-730234.1 AAVSO 000-BLT-636

Position

Right ascension (°) 88.539725 ± 0.064925ref  Parallax (mas) Reddening E(B-V) (mag) 0.098 ± 0.001ref
Declination (°) -73.042819 ± 0.067087ref Distance (kpc) 49.97 ± 0.19ref    
Galactic longitude (°) 283.882043 ± 0.067087ref Proper motion in α (mas/yr) 1.663343 ± 0.125718ref    
Galactic latitude (°) -30.023795 ± 0.064925ref Proper motion in δ (mas/yr) 1.242801 ± 0.165362ref    

Observations

U (mag)   X-Ray   Flickering  
B (mag) 12.80 X-Ray type   Outbursts No
V (mag)   IUE Yes Type  
R (mag)   IRAS flux at 12 μm (Jy) 0.08987ref IPmax (eV) 114.0ref
I (mag) 13.78ref IRAS flux at 25 μm (Jy) 0.04561ref OVI lines Yesref
G (mag) 16.82ref IRAS flux at 60 μm (Jy) <0.1187ref    
J (mag) 14.54ref IRAS flux at 100 μm (Jy) <0.7219ref    
H (mag) 12.77ref WISE W1 (mag) 9.86ref    
K (mag) 11.38ref WISE W2 (mag) 8.96ref    
L (mag)   WISE W3 (mag) 6.89ref    
    WISE W4 (mag) 5.53ref    
    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 Miraref Mass (M)   Pulsation  
Eff. temperature (K)   Radius (R)   Type  
IR type D🡕, ref 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     VSX


Notes

Although included number of times in several surveys of Pne, Raman-scattered O VI lines were observed by Dopita et al. (1985). No M giant spectrum is observed as incorrectly listed in Belczyński et al. (2000). Lack of a strong variability, along with a strong IR excess is consistent with a D-type SySt (Angeloni et al., 2014).


References

  • Angeloni, R., Ferreira Lopes, C. E., Masetti, N., et al., 2014, MNRAS, 438, 35, 2014MNRAS.438…35A
  • Dopita, M. A., Ford, H. C., Webster, B. L., 1985, ApJ, 297, 593, 1985ApJ…297..593D

Last updated: May 2, 2019 @ 11:30 am