POSSIBLE
MILKY WAY
|
| QX Pup | IRAS 07399-1435 | GSC2.4.2 S3OU019229 | AAVSO 000-BFC-998 |
| SIMBAD 2MASS J07421687-1442521 | Pan-STARRS 90341155694753489 | SAO - | VSX 26934 |
| GAIA DR3 3029214634000674688 | SkyMapper 074216.68-144250.8 | WRAY - | GCVS QX Pup |
| 2MASS J07421687-1442521 | HIP - | Hen - | BD - |
| WISE J074216.93-144249.7 | 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 (°) | 115.5695Ref | Parallax (mas) | 0.030±0.160Ref | Reddening E(B-V) (mag) | 0.96±0.3Ref, Note |
| Declination (°) | -14.7140Ref | Distance (kpc) | 5.64Ref, Note, 3.94Ref, Note | ||
| Galactic longitude (°) | 231.8348Ref | Proper motion in α (mas/yr) | -1.41±0.13Ref | ||
| Galactic latitude (°) | 4.2192Ref | Proper motion in δ (mas/yr) | 1.29±0.14Ref |
| X-Ray | NoRef | IR type | D'?Ref | Radio | YesRef |
| X-Ray type | - | J (mag) | - | Flickering | - |
| GALEX FUV (mag) | - | H (mag) | - | Outbursts | - |
| GALEX NUV (mag) | - | K (mag) | - | Outburst type | - |
| IUE | YesRef | WISE W1 (mag) | 4.39Ref | Jets | - |
| FUSE | NoRef | WISE W2 (mag) | 1.66Ref | Resolved nebula | YesRef |
| U (mag) | - | WISE W3 (mag) | -0.09Ref | IPmax (eV) | - |
| B (mag) | - | WISE W4 (mag) | -3.55Ref | [O III] lines | - |
| V (mag) | - | IRAS 12μm (Jy) | 19.00Ref | He II lines | - |
| R (mag) | - | IRAS 25μm (Jy) | 226.00Ref | [Fe VII] lines | - |
| I (mag) | - | IRAS 60μm (Jy) | 548.00Ref | O VI lines | - |
| BP (mag) | 18.68Ref | IRAS 100μm (Jy) | 294.00Ref | ||
| G (mag) | 18.25Ref | AKARI S09 (Jy) | 17.95Ref | ||
| RP (mag) | 16.34Ref | AKARI S18 (Jy) | 158.60Ref |
| 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 | YesRef |
| Eff. temperature (K) | - | Radius (R⊙) | - | Type | MiraRef |
| IR type | D'?Ref | Luminosity (L⊙) | - | Pulsation period (days) | 648Ref, 551Ref |
| Metallicity [Fe/H] | - | Pulsation ephemeris | - |
| Type/Spectral type | - | Mass (M⊙) | - | Spin period (min) | - |
| Shell-burning/Accreting-only | - | Radius (R⊙) | - | Accretion disk | - |
| Eff. temperature (K) | - | Luminosity (L⊙) | - | ||
| Lower limit (K) | - | ||||
| Upper limit (K) | - |
The object is typically classified as a protoplanetary nebula with axial symmetry. The symbiotic nature was first suggested by Cohen et al. (1985), who observed an M9 central star with a blue companion. Alcolea et al. (2001) suggested that the system might be a symbiotic star with a unique thick molecular envelope. On the other hand, Sánchez Contreras et al. (2004) suggested that the system consists of an M9-10 III star and an MS star with spectral type A. Frew & Parker (2010) supported the symbiotic hypothesis as they hypothesized that the nebula is probably a symbiotic outflow.