LIN 183

SUSPECTED SMC  

Equatorial coordinates
α = 12.926032 ± 1.716800 | 00 51 42.247715
δ = -72.841035 ± 1.305800| -72 50 27.727366
 
Constellation Tucana
Symbiotic IR Type  
Spectral Type  
Magnitude range (V)  
Outbursts No

Identifiers

LIN 183 GSC TYC WRAY
SIMBAD LIN 183 HIP SAO Hen
BD – IRAS  GAIA DR2 4688960455891138688 ESO
HD 2MASS J00514224-7250276 WISE AAVSO 

Position

Right ascension (°) 12.926032 ± 1.716800ref  Parallax (mas) Reddening E(B-V) (mag) 0.508 ± 0.099ref
Declination (°) -72.841035 ± 1.305800ref Distance (kpc) 62.10 ± 1.90ref    
Galactic longitude (°) 302.904491 ± 1.305800ref Proper motion in α (mas/yr)    
Galactic latitude (°) -44.287233 ± 1.716800ref Proper motion in δ (mas/yr)    

Observations

U (mag) 15.85ref X-Ray   Flickering  
B (mag) 15.88ref X-Ray type   Outbursts No
V (mag) 15.04ref IUE No Type  
R (mag)   IRAS flux at 12 μm (Jy)   IPmax (eV) 35.1ref
I (mag) 14.17ref IRAS flux at 25 μm (Jy)   OVI lines Noref
G (mag) 15.48ref IRAS flux at 60 μm (Jy)      
J (mag) 13.57ref IRAS flux at 100 μm (Jy)      
H (mag) 13.03ref WISE W1 (mag)      
K (mag) 12.89ref 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   Mass (M)   Pulsation  
Eff. temperature (K)   Radius (R)   Type  
IR type   Luminosity (L) 4166ref 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

Kamath et al. (2014) classified the star as likely symbiotic star as its spectra show a photosphere of a cool star with a red continuum and strong emission lines.


References

Last updated: Feb 8, 2019 @ 9:01 pm