[RP2006] 227

SUSPECTED LMC  

Equatorial coordinates
α = 84.445048 ± 0.032300 | 05 37 46.811592
δ = -69.532193 ± 0.034800 | -69 31 55.894809
 
Constellation Dorado
Symbiotic IR Type S🡕
Spectral Type M2 III
Magnitude range (V)  
Outbursts No

Identifiers

[RP2006] 227 GSC TYC WRAY
SIMBAD [RP2006] 227 HIP SAO Hen
BD – IRAS  GAIA DR2 4657644784171703168 ESO
HD 2MASS J05374681-6931558 WISE J053746.80-693155.8 AAVSO

Position

Right ascension (°) 84.445048 ± 0.032300 ref Parallax (mas) Reddening E(B-V) (mag) 2.284 ± 1.022ref
Declination (°) -69.532193 ± 0.034800ref Distance (kpc) 49.97 ± 0.19ref    
Galactic longitude (°) 279.979746 ± 0.034800ref Proper motion in α (mas/yr) 2.012 ± 0.064ref    
Galactic latitude (°) -31.702248 ± 0.032300ref Proper motion in δ (mas/yr) 0.723 ± 0.072ref    

Observations

U (mag)   X-Ray   Flickering  
B (mag) 18.61ref X-Ray type   Outbursts No
V (mag) 16.64ref IUE No Type  
R (mag) 15.73ref IRAS flux at 12 μm (Jy)   IPmax (eV)  
I (mag)   IRAS flux at 25 μm (Jy)   OVI lines  
G (mag) 15.97ref IRAS flux at 60 μm (Jy)      
J (mag) 13.27ref IRAS flux at 100 μm (Jy)      
H (mag) 12.38ref WISE W1 (mag) 12.05ref    
K (mag) 12.17ref WISE W2 (mag) 12.15ref    
L (mag)   WISE W3 (mag) 12.36ref    
    WISE W4 (mag) 8.67ref    
    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 M2 IIIref Mass (M)   Pulsation  
Eff. temperature (K) 3764ref Radius (R)   Type  
IR type S🡕, 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

Reid (2014) classified the star as a possible symbiotic star based on the presence of late-type stellar continuum and ambient emission, together with OGLE variability over ∼200 d.


References

Last updated: May 2, 2019 @ 11:16 am