[RP2006] 774

SUSPECTED LMC  

Equatorial coordinates
α =  83.165399 ± 0.259800 | 05 32 39.690174
δ =  -69.513745 ± 0.308600 | -69 30 49.483082
 
Constellation Dorado
Symbiotic IR Type D’🡕
Spectral Type  
Magnitude range (V)  
Outbursts No

Identifiers

[RP2006] 774 GSC TYC WRAY
SIMBAD [RP2006] 774 HIP SAO Hen
BD – IRAS  GAIA DR2 4658034080040925568 ESO
HD 2MASS J05323971-6930494 WISE J053239.70-693049.3 AAVSO

Position

Right ascension (°) 83.165399 ± 0.259800  ref Parallax (mas) Reddening E(B-V) (mag) 0.396 ± 0.144ref
Declination (°) -69.513745 ± 0.308600ref Distance (kpc) 49.97 ± 0.19ref    
Galactic longitude (°) 280.028253 ± 0.308600ref Proper motion in α (mas/yr) 1.855 ± 0.515ref    
Galactic latitude (°) -32.148368 ± 0.259800ref Proper motion in δ (mas/yr) 0.027 ± 0.833ref    

Observations

U (mag) 18.42ref X-Ray   Flickering  
B (mag) 18.78ref X-Ray type   Outbursts No
V (mag) 17.92ref IUE No Type  
R (mag)   IRAS flux at 12 μm (Jy)   IPmax (eV)  
I (mag) 17.40ref IRAS flux at 25 μm (Jy)   OVI lines  
G (mag) 18.84ref IRAS flux at 60 μm (Jy)      
J (mag) 16.97ref IRAS flux at 100 μm (Jy)      
H (mag) 16.04ref WISE W1 (mag) 12.29ref    
K (mag) 14.93ref WISE W2 (mag) 11.25ref    
L (mag)   WISE W3 (mag) 7.51ref    
    WISE W4 (mag) 5.34ref    
    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. The OGLE-III lightcurve of [RP2006] 774 appears to show low-amplitude semi-regular variability on the order of ∼40–80 days and this could be attributed to an RGB star (Miszalski et al., 2011). Reid (2014) did not consider the MIR SED steep enough for a symbiotic star and classified it as YSO.


References

Last updated: May 2, 2019 @ 11:20 am