POSSIBLE
MILKY WAY
|
| PHR J1640-4019 | IRAS 16366-4013 | GSC2.4.2 S8VG015575 | AAVSO - |
| SIMBAD IRAS 16366-4013 | Pan-STARRS - | SAO - | VSX - |
| GAIA DR3 5969282299743518592 | SkyMapper 164006.38-401946.3 | WRAY - | GCVS - |
| 2MASS J16400638-4019465 | HIP - | Hen - | BD - |
| WISE J164006.38-401946.5 | TYC - | ESO - | HD - |
| Bidelman (1954) | - | Allen (1984) | - | Belzcyński et al. (2001) | - |
| Gaposchkin (1957) | - | Kenyon (1986) | - | Akras et al. (2019) | - |
| Boyarchuk (1969) | - | Vaidis (1988, 1991) | - |
| Right ascension (°) | 250.0266Ref | Parallax (mas) | 0.085±0.051Ref | Reddening E(B-V) (mag) | 0.79±0.06Ref, Note |
| Declination (°) | -40.3296Ref | Distance (kpc) | 7.13Ref, Note, 5.82Ref, Note | ||
| Galactic longitude (°) | 342.8923Ref | Proper motion in α (mas/yr) | -1.37±0.06Ref | ||
| Galactic latitude (°) | 4.1722Ref | Proper motion in δ (mas/yr) | -2.66±0.05Ref |
| X-Ray | - | IR type | D'?Ref | Radio | - |
| X-Ray type | - | J (mag) | 14.86Ref | Flickering | - |
| GALEX FUV (mag) | - | H (mag) | 14.29Ref | Outbursts | - |
| GALEX NUV (mag) | - | K (mag) | 12.99Ref | Outburst type | - |
| IUE | NoRef | WISE W1 (mag) | 10.81Ref | Jets | - |
| FUSE | NoRef | WISE W2 (mag) | 9.69Ref | Resolved nebula | - |
| U (mag) | - | WISE W3 (mag) | 6.22Ref | IPmax (eV) | 54.4Ref |
| B (mag) | - | WISE W4 (mag) | 3.10Ref | [O III] lines | YesRef |
| V (mag) | - | IRAS 12μm (Jy) | 0.34Ref | He II lines | YesRef |
| R (mag) | - | IRAS 25μm (Jy) | 0.42Ref | [Fe VII] lines | NoRef |
| I (mag) | - | IRAS 60μm (Jy) | 2.24Ref | O VI lines | NoRef |
| BP (mag) | 16.17Ref | IRAS 100μm (Jy) | 73.80Ref | ||
| G (mag) | 16.07Ref | AKARI S09 (Jy) | - | ||
| RP (mag) | 15.35Ref | AKARI S18 (Jy) | 0.32Ref |
| 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) | - |
Classified as a likely symbiotic system in HASH Database of PNe (Parker et al., 2016), the spectrum reveals numerous emission lines, including Balmer lines, He I, [O III], etc., with faint He II detection.