SUSPECTED
MILKY WAY
|
| V335 Vul | IRAS 19211+2421 | GSC2.4.2 N22W001233 | AAVSO 000-BCX-585 |
| SIMBAD EM* AS 356 | Pan-STARRS 137352908089483761 | SAO - | VSX 38510 |
| GAIA DR3 2022999316661190272 | SkyMapper - | WRAY - | GCVS V0335 Vul |
| 2MASS J19231415+2427396 | HIP - | Hen - | BD - |
| WISE J192314.13+242739.6 | TYC - | ESO - | HD - |
| Bidelman (1954) | - | Allen (1984) | - | Belzcyński et al. (2001) | V335 Vul (Susp.) |
| Gaposchkin (1957) | - | Kenyon (1986) | - | Akras et al. (2019) | V335 Vul (Susp.) |
| Boyarchuk (1969) | - | Vaidis (1988, 1991) | - |
| Right ascension (°) | 290.8089Ref | Parallax (mas) | 0.248±0.024Ref | Reddening E(B-V) (mag) | 0.65±0.03Ref, Note |
| Declination (°) | 24.4610Ref | Distance (kpc) | 3.7Ref 3.66Ref, Note, 3.36Ref, Note |
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| Galactic longitude (°) | 58.2209Ref | Proper motion in α (mas/yr) | -0.82±0.02Ref | ||
| Galactic latitude (°) | 4.4031Ref | Proper motion in δ (mas/yr) | -3.58±0.02Ref |
| X-Ray | - | IR type | D?Ref, S?Ref | Radio | YesRef |
| X-Ray type | - | J (mag) | 6.86Ref | Flickering | - |
| GALEX FUV (mag) | - | H (mag) | 5.80Ref | Outbursts | Yes?Ref |
| GALEX NUV (mag) | - | K (mag) | 5.11Ref | Outburst type | - |
| IUE | NoRef | WISE W1 (mag) | 4.44Ref | Jets | - |
| FUSE | NoRef | WISE W2 (mag) | 3.59Ref | Resolved nebula | - |
| U (mag) | - | WISE W3 (mag) | 3.32Ref | IPmax (eV) | 13.6Ref |
| B (mag) | - | WISE W4 (mag) | 2.91Ref | [O III] lines | NoRef |
| V (mag) | - | IRAS 12μm (Jy) | 1.79Ref | He II lines | NoRef |
| R (mag) | 10.28Ref | IRAS 25μm (Jy) | 0.62Ref | [Fe VII] lines | NoRef |
| I (mag) | - | IRAS 60μm (Jy) | 0.40Ref | O VI lines | NoRef |
| BP (mag) | 13.19Ref | IRAS 100μm (Jy) | 2.95Ref | ||
| G (mag) | 11.06Ref | AKARI S09 (Jy) | 1.75Ref | ||
| RP (mag) | 9.77Ref | AKARI S18 (Jy) | 0.61Ref |
| 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 | CRef | Mass (M⊙) | - | Pulsation | YesRef |
| Eff. temperature (K) | - | Radius (R⊙) | - | Type | MiraRef |
| IR type | D?Ref, S?Ref | Luminosity (L⊙) | - | Pulsation period (days) | 347Ref, 333.7Ref |
| Metallicity [Fe/H] | - | Pulsation ephemeris | Max(V) = 2451822.2±0.5 + 347 x ERef |
| 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) | - |
Suspected by Munari et al. (1999), the spectrum of this object reveals the continuum of a carbon giant, a hot blue continuum, and emission lines of H I. No highly ionized emission lines were detected. Belczyński et al. (2000) suggested that the object might be a single pulsating star pulsating with a period of 342 days (Dahlmark, 1994). The star was detected in a possible outburst by Munari et al. (1999). On the other hand, Sobotka et al. (2003) claimed that the brightening was not caused by an outburst but rather by Mira-like pulsations.