LM 2-39

SUSPECTED LMC  

Equatorial coordinates
α =  85.061711 ± 0.228336 | 05 40 14.802052
δ =  -69.480317 ± 0.254024 | -69 28 49.180232
 
Constellation Dorado
Symbiotic IR Type D’🡕
Spectral Type  
Magnitude range (V)  
Outbursts No

Identifiers

LM 2-39 GSC TYC WRAY
SIMBAD LM 2-39 HIP SAO Hen
BD – IRAS  GAIA DR2 4657648082707959680 ESO
HD 2MASS J05401481-6928490 WISE J054014.81-692849.1 AAVSO

Position

Right ascension (°) 85.061711 ± 0.228336ref  Parallax (mas) Reddening E(B-V) (mag) 3.287 ± 1.435ref
Declination (°) -69.480317 ± 0.254024ref Distance (kpc) 49.97 ± 0.19ref    
Galactic longitude (°) 279.889703 ± 0.254024ref Proper motion in α (mas/yr) 2.878118 ± 0.438200ref    
Galactic latitude (°) -31.493902 ± 0.228336ref Proper motion in δ (mas/yr) 2.539424 ± 0.502596ref    

Observations

U (mag) 16.64ref X-Ray   Flickering  
B (mag) 17.11ref X-Ray type   Outbursts No
V (mag) 16.76ref IUE No Type  
R (mag) 15.87ref IRAS flux at 12 μm (Jy)   IPmax (eV)  
I (mag) 16.03ref IRAS flux at 25 μm (Jy)   OVI lines  
G (mag) 16.51ref IRAS flux at 60 μm (Jy)      
J (mag) 15.31ref IRAS flux at 100 μm (Jy)      
H (mag) 14.54ref WISE W1 (mag) 10.46ref    
K (mag) 13.04ref WISE W2 (mag) 8.77ref    
L (mag)   WISE W3 (mag) 5.28ref    
    WISE W4 (mag) 2.93ref    
    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) 3792ref 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


Notes

According to Miszalski et al. (2011), the resolved Hα nebula, NIR and MIR colours, and slow I-band variations suggest LM2-39 to be a strong symbiotic star candidate.


References

  • Akras, S., Guzman-Ramirez, L., Leal-Ferreira, M. L., et al., 2019, ApJS, 240, 21, 2019ApJS..240…21A
  • Miszalski, B., Napiwotzki, R., Cioni, M. R. L., et al., 2011, A&A, 531, A157, 2011A&A…531A.157M

Last updated: May 2, 2019 @ 11:06 am