LIKELY
MILKY WAY
|
| IRAS 16468-4737 | IRAS 16468-4737 | GSC2.4.2 S8Q5081158 | AAVSO - |
| SIMBAD IRAS 16468-4737 | Pan-STARRS - | SAO - | VSX - |
| GAIA DR3 5939392802025441152 | SkyMapper - | WRAY - | GCVS - |
| 2MASS J16503229-4742288 | HIP - | Hen - | BD - |
| WISE J165032.30-474228.9 | TYC - | ESO - | HD - |
| Bidelman (1954) | - | Allen (1984) | - | Belzcyński et al. (2001) | - |
| Gaposchkin (1957) | - | Kenyon (1986) | - | Akras et al. (2019) | 2MASSJ16503229-4742288 (Susp.) |
| Boyarchuk (1969) | - | Vaidis (1988, 1991) | - |
| Right ascension (°) | 252.6346Ref | Parallax (mas) | 0.142±0.181Ref | Reddening E(B-V) (mag) | 3.22±0.2Ref, Note |
| Declination (°) | -47.7080Ref | Distance (kpc) | 6.37Ref, Note, 3.96Ref, Note | ||
| Galactic longitude (°) | 338.5095Ref | Proper motion in α (mas/yr) | 0.54±0.25Ref | ||
| Galactic latitude (°) | -2.0533Ref | Proper motion in δ (mas/yr) | -1.55±0.19Ref |
| X-Ray | - | IR type | D?Ref | Radio | - |
| X-Ray type | - | J (mag) | 13.99Ref | Flickering | - |
| GALEX FUV (mag) | - | H (mag) | 11.55Ref | Outbursts | - |
| GALEX NUV (mag) | - | K (mag) | 9.48Ref | Outburst type | - |
| IUE | NoRef | WISE W1 (mag) | 7.08Ref | Jets | - |
| FUSE | NoRef | WISE W2 (mag) | 5.57Ref | Resolved nebula | - |
| U (mag) | - | WISE W3 (mag) | 3.23Ref | IPmax (eV) | 35.1Ref |
| B (mag) | - | WISE W4 (mag) | 1.52Ref | [O III] lines | YesRef |
| V (mag) | - | IRAS 12μm (Jy) | 1.82Ref | He II lines | NoRef |
| R (mag) | - | IRAS 25μm (Jy) | 2.36Ref | [Fe VII] lines | NoRef |
| I (mag) | - | IRAS 60μm (Jy) | 15.00Ref | O VI lines | NoRef |
| BP (mag) | 19.38Ref | IRAS 100μm (Jy) | 235.00Ref | ||
| G (mag) | 18.54Ref | AKARI S09 (Jy) | 1.64Ref | ||
| RP (mag) | 17.39Ref | AKARI S18 (Jy) | 1.94Ref |
| 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 | - |
| Eclipses | - | Mass ratio | - | ||
| Orbital ephemeris | - |
| Spectral type | - | Mass (M⊙) | - | Pulsation | - |
| Eff. temperature (K) | - | Radius (R⊙) | - | Type | - |
| IR type | D?Ref | Luminosity (L⊙) | - | Pulsation period (days) | - |
| Metallicity [Fe/H] | - | Pulsation ephemeris | - |
| Type/Spectral type | - | Mass (M⊙) | - | Spin period (min) | - |
| Shell-burning/Accreting-only | shell-burning?Ref | Radius (R⊙) | - | Accretion disk | - |
| Eff. temperature (K) | - | Luminosity (L⊙) | - | ||
| Lower limit (K) | - | ||||
| Upper limit (K) | - |
Suspected by Miszalski & Mikołajewska (2014) based on a PN-like spectrum and red 2MASS colours typical of D-type symbiotic stars (J-H and H-K are both >= 2.0). The red giant is not seen in the optical spectra. Alternatively, it might be a PN with a dusty WR central star. The study also noted that these typically have temperatures of 30kK and are unable to ionize the [Ar IV] and [Ar V] emission lines observed, which are more common in D-type symbiotic stars than in PNe.