CONFIRMED
MILKY WAY
|
| V417 Cen | IRAS 14122-6139 | GSC2.4.2 S7Q5000835 | AAVSO 000-BCV-314 |
| SIMBAD SV* HV 6516 | Pan-STARRS - | SAO - | VSX 7714 |
| GAIA DR3 5854484146110596736 | SkyMapper - | WRAY 15-1189 | GCVS V0417 Cen |
| 2MASS J14155968-6153502 | HIP - | Hen 3-977 | BD - |
| WISE J141559.72-615349.8 | TYC - | ESO - | HD - |
| Bidelman (1954) | - | Allen (1984) | - | Belzcyński et al. (2001) | V417 Cen (Conf.) |
| Gaposchkin (1957) | - | Kenyon (1986) | - | Akras et al. (2019) | V417 Cen (Conf.) |
| Boyarchuk (1969) | - | Vaidis (1988, 1991) | - |
| Right ascension (°) | 213.9986Ref | Parallax (mas) | 0.795±0.023Ref | Reddening E(B-V) (mag) | 7.61±0.31Ref, Note |
| Declination (°) | -61.8973Ref | Distance (kpc) | 1.24Ref, Note, 1.23Ref, Note | ||
| Galactic longitude (°) | 312.7132Ref | Proper motion in α (mas/yr) | -11.32±0.02Ref | ||
| Galactic latitude (°) | -0.6420Ref | Proper motion in δ (mas/yr) | -6.69±0.02Ref |
| X-Ray | NoRef | IR type | D'Ref | Radio | - |
| X-Ray type | - | J (mag) | 8.07Ref | Flickering | NoRef |
| GALEX FUV (mag) | - | H (mag) | 6.98Ref | Outbursts | Yes?Ref |
| GALEX NUV (mag) | - | K (mag) | 5.79Ref | Outburst type | - |
| IUE | NoRef | WISE W1 (mag) | 4.05Ref | Jets | - |
| FUSE | NoRef | WISE W2 (mag) | 2.88Ref | Resolved nebula | YesRef |
| U (mag) | - | WISE W3 (mag) | 0.96Ref | IPmax (eV) | 35.1Ref |
| B (mag) | 13.23Ref | WISE W4 (mag) | -0.24Ref | [O III] lines | YesRef |
| V (mag) | 11.57Ref | IRAS 12μm (Jy) | 12.60Ref | He II lines | NoRef |
| R (mag) | - | IRAS 25μm (Jy) | 10.60Ref | [Fe VII] lines | NoRef |
| I (mag) | - | IRAS 60μm (Jy) | 87.40Ref | O VI lines | NoRef |
| BP (mag) | 11.94Ref | IRAS 100μm (Jy) | 168.00Ref | ||
| G (mag) | 11.07Ref | AKARI S09 (Jy) | 11.97Ref | ||
| RP (mag) | 10.02Ref | AKARI S18 (Jy) | 10.09Ref |
| Orbital period (days) | 1652±11Ref | γ velocity (km/h) | -38.65±0.93Ref | 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 | Min (V) = 2452613 + 1652±11 x ERef |
| Spectral type | G8-K2Ref, G2 Ib-IIRef, F9 III-IVRef |
Mass (M⊙) | 6.45Ref | Pulsation | Yes?Ref |
| Eff. temperature (K) | 5000Ref, 6000Ref | Radius (R⊙) | 75Ref | Type | SRRef |
| IR type | D'Ref | Luminosity (L⊙) | 3160Ref | Pulsation period (days) | 245.68Ref |
| Metallicity [Fe/H] | - | Pulsation ephemeris | Min (pg) = 2427655 + 245.68 x ERef |
| Type/Spectral type | - | Mass (M⊙) | - | Spin period (min) | - |
| Shell-burning/Accreting-only | shell-burningRef | Radius (R⊙) | - | Accretion disk | - |
| Eff. temperature (K) | - | Luminosity (L⊙) | - | ||
| Lower limit (K) | - | ||||
| Upper limit (K) | - |
Classified as a symbiotic star by Cielinski & Elizalde (1993). van Winckel et al. (1993) reported that Hα is not always being visible in the spectra. Cieslinski et al. (1994) noted the presence of a G-type continuum with Hα, [N II], and [O III] emission lines. van Winckel et al. (1994) classified the system as a yellow symbiotic system within a resolved nebula. They also detected a period of 245 days in the optical light curve of the target, which they suggested might be the orbital period. Additionally, Gromadzki et al. (2011) identified longer periods around 1700 days, 560 days, etc. The emission line spectrum of V417 Cen exhibits strong variability, as reported by Stoyanov et al. (2014).