CONFIRMED
MILKY WAY
|
| V4141 Sgr | IRAS - | GSC2.4.2 S802483410 | AAVSO 000-BFJ-434 |
| SIMBAD PN Th 4-4 | Pan-STARRS 84122675992765928 | SAO - | VSX 31841 |
| GAIA DR3 4119029875002043392 | SkyMapper 175023.81-195343.1 | WRAY - | GCVS V4141 Sgr |
| 2MASS J17502382-1953431 | HIP - | Hen - | BD - |
| WISE J175023.81-195343.2 | TYC - | ESO 589-10 | HD - |
| Bidelman (1954) | - | Allen (1984) | Th4-4 (Susp.) | Belzcyński et al. (2001) | V4141 Sgr (Conf.) |
| Gaposchkin (1957) | - | Kenyon (1986) | Th 4-4 (Susp.) | Akras et al. (2019) | V4141 Sgr (Conf.) |
| Boyarchuk (1969) | - | Vaidis (1988, 1991) | Th-4-4 (Conf.) |
| Right ascension (°) | 267.5992Ref | Parallax (mas) | 0.046±0.060Ref | Reddening E(B-V) (mag) | 0.86±0.03Ref, Note |
| Declination (°) | -19.8954Ref | Distance (kpc) | 7Ref 7.40Ref, Note, 6.00Ref, Note |
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| Galactic longitude (°) | 8.3116Ref | Proper motion in α (mas/yr) | -1.75±0.06Ref | ||
| Galactic latitude (°) | 3.7323Ref | Proper motion in δ (mas/yr) | -7.74±0.04Ref |
| X-Ray | NoRef | IR type | DRef, SRef | Radio | NoRef |
| X-Ray type | - | J (mag) | 9.81Ref | Flickering | - |
| GALEX FUV (mag) | - | H (mag) | 8.61Ref | Outbursts | - |
| GALEX NUV (mag) | - | K (mag) | 8.01Ref | Outburst type | - |
| IUE | YesRef | WISE W1 (mag) | 7.75Ref | Jets | - |
| FUSE | NoRef | WISE W2 (mag) | 7.80Ref | Resolved nebula | NoRef |
| U (mag) | - | WISE W3 (mag) | 6.43Ref | IPmax (eV) | 54.4Ref |
| B (mag) | 17.50Ref | WISE W4 (mag) | 5.63Ref | [O III] lines | - |
| V (mag) | - | IRAS 12μm (Jy) | - | He II lines | - |
| R (mag) | 15.63Ref | IRAS 25μm (Jy) | - | [Fe VII] lines | - |
| I (mag) | 13.21Ref | IRAS 60μm (Jy) | - | O VI lines | NoRef |
| BP (mag) | 16.52Ref | IRAS 100μm (Jy) | - | ||
| G (mag) | 14.58Ref | AKARI S09 (Jy) | 0.14Ref | ||
| RP (mag) | 13.14Ref | AKARI S18 (Jy) | - |
| 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 | DRef, SRef | Luminosity (L⊙) | - | Pulsation period (days) | - |
| Metallicity [Fe/H] | - | Pulsation ephemeris | - |
| Type/Spectral type | WDRef | Mass (M⊙) | - | Spin period (min) | - |
| Shell-burning/Accreting-only | shell-burningRef | Radius (R⊙) | - | Accretion disk | - |
| Eff. temperature (K) | - | Luminosity (L⊙) | 1400Ref | ||
| Lower limit (K) | 35000Ref | ||||
| Upper limit (K) | 55000Ref |
The symbiotic nature of the object was initially suspected in Allen (1984), with subsequent studies revealing strong emission lines, including [O III] and faint O VI (Stenholm & Acker, 1987). Kondrateva (1989) reported the detection of Balmer lines, He I, and [O III], and emission with an ionization potential up to 35 eV was noted in Mikołajewska et al. (1997) as well. Kondratyeva (2001) detected He II lines and argued that the object represents a rapidly evolving PN. A study of Gaia Collaboration (2018) reported the presence of a long-period variable in the system.