CONFIRMED
MILKY WAY
|
| V618 Sgr | IRAS - | GSC2.4.2 S9PR005223 | AAVSO 000-BCX-015 |
| SIMBAD V* V618 Sgr | Pan-STARRS - | SAO - | VSX 28318 |
| GAIA DR3 4038647942747847936 | SkyMapper - | WRAY - | GCVS V0618 Sgr |
| 2MASS J18075721-3629523 | HIP - | Hen - | BD - |
| WISE J180757.20-362952.2 | TYC - | ESO - | HD - |
| Bidelman (1954) | - | Allen (1984) | - | Belzcyński et al. (2001) | V618 Sgr (Susp.) |
| Gaposchkin (1957) | - | Kenyon (1986) | - | Akras et al. (2019) | V618 Sgr (Susp.) |
| Boyarchuk (1969) | - | Vaidis (1988, 1991) | - |
| Right ascension (°) | 271.9884Ref | Parallax (mas) | 0.191±0.063Ref | Reddening E(B-V) (mag) | 0.14±0.0Ref, Note |
| Declination (°) | -36.4979Ref | Distance (kpc) | 5.38Ref, Note, 5.19Ref, Note | ||
| Galactic longitude (°) | 355.7658Ref | Proper motion in α (mas/yr) | -0.56±0.07Ref | ||
| Galactic latitude (°) | -7.8328Ref | Proper motion in δ (mas/yr) | -5.06±0.05Ref |
| X-Ray | - | IR type | SRef | Radio | - |
| X-Ray type | - | J (mag) | 8.60Ref | Flickering | - |
| GALEX FUV (mag) | - | H (mag) | 7.68Ref | Outbursts | YesRef |
| GALEX NUV (mag) | - | K (mag) | 7.20Ref | Outburst type | SyNRef |
| IUE | NoRef | WISE W1 (mag) | 7.11Ref | Jets | - |
| FUSE | NoRef | WISE W2 (mag) | 7.14Ref | Resolved nebula | - |
| U (mag) | - | WISE W3 (mag) | 6.56Ref | IPmax (eV) | 30Ref |
| B (mag) | - | WISE W4 (mag) | 6.13Ref | [O III] lines | NoRef |
| V (mag) | - | IRAS 12μm (Jy) | - | He II lines | NoRef |
| R (mag) | - | IRAS 25μm (Jy) | - | [Fe VII] lines | NoRef |
| I (mag) | - | IRAS 60μm (Jy) | - | O VI lines | NoRef |
| BP (mag) | 15.59Ref | IRAS 100μm (Jy) | - | ||
| G (mag) | 12.96Ref | AKARI S09 (Jy) | 0.16Ref | ||
| RP (mag) | 11.50Ref | AKARI S18 (Jy) | - |
| Orbital period (days) | 703±4Ref | γ velocity (km/h) | -116.93±1.35Ref | Size of giant’s orbit (AU) | - |
| Eccentricity | - | RV of giant (km/h) | - | Separation (AU) | - |
| Inclination (°) | - | Inferior conj. of giant (JD) | - | Mass function | - |
| Eclipses | YesRef | Mass ratio | - | ||
| Orbital ephemeris | Min(gV) = 2458397±8 + 703±4 x ERef |
| Spectral type | M6Ref | Mass (M⊙) | - | Pulsation | - |
| Eff. temperature (K) | 3300Ref | Radius (R⊙) | - | Type | - |
| IR type | SRef | Luminosity (L⊙) | - | Pulsation period (days) | - |
| Metallicity [Fe/H] | - | Pulsation ephemeris | - |
| 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) | - |
Initially considered a candidate for an R CrB (Swope & Shapley, 1940), later observations by Kilkenny (1989) suggested a symbiotic nature based on the presence of hydrogen Balmer lines in emission. However, the absence of lines with higher ionization potential was reported. The symbiotic classification was confirmed by Merc et al. (2023), who detected a symbiotic nova outburst and also observed eclipses in the binary system.