[RP2006] 776

SUSPECTED LMC  

Equatorial coordinates
α =  83.163482  ±  0.495400 | 05 32 39.235579
δ =  -69.531610 ± 0.521800 | -69 31 53.794272
 
Constellation Dorado
Symbiotic IR Type D’🡕
Spectral Type  
Magnitude range (V)  
Outbursts No

Identifiers

[RP2006] 776 GSC TYC WRAY
SIMBAD [RP2006] 776 HIP SAO Hen
BD – IRAS  GAIA DR2 4658028204523066496 ESO
HD 2MASS J05323922-6931540 WISE J053239.28-693153.8 AAVSO

Position

Right ascension (°) 83.163482 ±  0.495400ref  Parallax (mas) Reddening E(B-V) (mag) 0.423 ± 0.140ref
Declination (°) -69.531610 ± 0.521800ref  Distance (kpc) 49.97 ± 0.19ref    
Galactic longitude (°) 280.049249 ± 0.521800ref  Proper motion in α (mas/yr)    
Galactic latitude (°) -32.146494 ± 0.495400ref  Proper motion in δ (mas/yr)    

Observations

U (mag) 19.71ref X-Ray   Flickering  
B (mag) 20.09ref X-Ray type   Outbursts No
V (mag) 19.44ref IUE No Type  
R (mag)   IRAS flux at 12 μm (Jy)   IPmax (eV)  
I (mag) 18.73ref IRAS flux at 25 μm (Jy)   OVI lines  
G (mag) 19.70ref  IRAS flux at 60 μm (Jy)      
J (mag) 17.09ref IRAS flux at 100 μm (Jy)      
H (mag)   WISE W1 (mag) 12.46ref    
K (mag) 14.47ref WISE W2 (mag) 11.37ref    
L (mag)   WISE W3 (mag) 7.45ref    
    WISE W4 (mag) 5.49ref    
    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 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

The star appears to have significant nebular Hα emission and the NIR and MIR properties suggest an obscured RGB (or possibly AGB) star (Miszalski et al., 2011).


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 @ 11:21 am