[RP2006] 883


Equatorial coordinates
α =  83.987072 ± 0.094433 | 05 35 56.893409
δ =  -69.012489 ± 0.096462 | -69 00 44.962764
Constellation Dorado
Symbiotic IR Type D’🡕
Spectral Type  
Magnitude range (V)  
Outbursts No


[RP2006] 883 GSC TYC WRAY
SIMBAD [RP2006] 883 HIP SAO Hen
BD – IRAS  GAIA DR2 4657696495585686016 ESO
HD 2MASS J05355689-6900450 WISE J053556.87-690046.1 AAVSO


Right ascension (°) 83.987072 ± 0.094433ref  Parallax (mas) Reddening E(B-V) (mag) 1.902 ± 0.464ref
Declination (°) -69.012489 ± 0.096462ref Distance (kpc) 49.97 ± 0.19ref    
Galactic longitude (°) 279.396349 ± 0.096462ref Proper motion in α (mas/yr) 1.343464 ± 0.182992ref    
Galactic latitude (°) -31.927150 ± 0.094433ref Proper motion in δ (mas/yr) 0.099262 ± 0.204375ref    


U (mag) 18.43ref X-Ray   Flickering  
B (mag) 18.75ref X-Ray type   Outbursts No
V (mag) 18.23ref IUE No Type  
R (mag) 17.21ref IRAS flux at 12 μm (Jy)   IPmax (eV)  
I (mag) 16.90ref IRAS flux at 25 μm (Jy)   OVI lines  
G (mag) 17.59ref IRAS flux at 60 μm (Jy)      
J (mag) 15.81ref IRAS flux at 100 μm (Jy)      
H (mag) 13.01ref WISE W1 (mag) 9.84ref    
K (mag)   WISE W2 (mag) 8.91ref    
L (mag)   WISE W3 (mag) 6.60ref    
    WISE W4 (mag) 5.03ref    
    Radio flux (mJy)      


Orbital period (days) 176.49ref  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)          


SIMBAD     CDS Portal


[RP2006] 883 appears to have a strong nebular component in the optical combined with NIR and MIR colours typical of an obscured RGB or AGB star (Miszalski et al., 2011). Reid (2014) reported dense, compact nebula and weak continuum suggesting a weakly interacting symbiotic system.


Last updated: May 2, 2019 @ 11:23 am