CONFIRMED
MILKY WAY
|
| V407 Cyg | IRAS - | GSC2.4.2 N324004289 | AAVSO 000-BCV-654 |
| SIMBAD EM* AS 453 | Pan-STARRS 162933155408711613 | SAO - | VSX 11327 |
| GAIA DR3 2163465736706055936 | SkyMapper - | WRAY - | GCVS V0407 Cyg |
| 2MASS J21020980+4546329 | HIP - | Hen - | BD - |
| WISE J210209.81+454632.7 | TYC - | ESO - | HD - |
| Bidelman (1954) | V407 Cyg (Susp.) | Allen (1984) | V407 Cyg (Conf.) | Belzcyński et al. (2001) | V407 Cyg (Conf.) |
| Gaposchkin (1957) | V407 Cyg (Conf.) | Kenyon (1986) | V407 Cyg (Conf.) | Akras et al. (2019) | V407 Cyg (Conf.) |
| Boyarchuk (1969) | V407 Cyg (Conf.) | Vaidis (1988, 1991) | V407 Cyg (Conf.) |
| Right ascension (°) | 315.5409Ref | Parallax (mas) | 0.247±0.117Ref | Reddening E(B-V) (mag) | 1.9±0.08Ref, Note |
| Declination (°) | 45.7757Ref | Distance (kpc) | 2.7Ref, 5.3±1Ref 4.63Ref, Note, 2.87Ref, Note |
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| Galactic longitude (°) | 86.9825Ref | Proper motion in α (mas/yr) | -2.62±0.12Ref | ||
| Galactic latitude (°) | -0.4821Ref | Proper motion in δ (mas/yr) | -4.29±0.13Ref |
| X-Ray | YesRef | IR type | DRef | Radio | YesRef |
| X-Ray type | βRef | J (mag) | 5.70Ref | Flickering | YesRef |
| GALEX FUV (mag) | - | H (mag) | 4.36Ref | Outbursts | YesRef |
| GALEX NUV (mag) | - | K (mag) | 3.17Ref | Outburst type | SyRNRef |
| IUE | NoRef | WISE W1 (mag) | 1.57Ref | Jets | YesRef |
| FUSE | NoRef | WISE W2 (mag) | 0.76Ref | Resolved nebula | NoRef |
| U (mag) | - | WISE W3 (mag) | 0.95Ref | IPmax (eV) | 54.4Ref, 233.6Ref, 99Ref |
| B (mag) | 16.04Ref | WISE W4 (mag) | -0.30Ref | [O III] lines | YesRef |
| V (mag) | 14.68Ref | IRAS 12μm (Jy) | - | He II lines | YesRef |
| R (mag) | 11.38Ref | IRAS 25μm (Jy) | - | [Fe VII] lines | NoRef |
| I (mag) | - | IRAS 60μm (Jy) | - | O VI lines | NoRef |
| BP (mag) | 16.14Ref | IRAS 100μm (Jy) | - | ||
| G (mag) | 11.95Ref | AKARI S09 (Jy) | 27.54Ref | ||
| RP (mag) | 10.19Ref | AKARI S18 (Jy) | 15.97Ref |
| 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 | 2.94-5.88Note | ||
| Orbital ephemeris | - |
| Spectral type | M6 IIIRef, M7-8 IIIRef | Mass (M⊙) | 3Ref | Pulsation | YesRef |
| Eff. temperature (K) | 2650Ref | Radius (R⊙) | 480Ref | Type | MiraRef |
| IR type | DRef | Luminosity (L⊙) | 4700Ref | Pulsation period (days) | 745Ref, 766.4Ref |
| Metallicity [Fe/H] | - | Pulsation ephemeris | Max (B) = 2429710 + 745 x ERef |
| Type/Spectral type | - | Mass (M⊙) | 1.35-1.37Ref | Spin period (min) | - |
| Shell-burning/Accreting-only | accreting-onlyRef | Radius (R⊙) | - | Accretion disk | - |
| Eff. temperature (K) | 60000Ref | Luminosity (L⊙) | 100Ref | ||
| Lower limit (K) | - | ||||
| Upper limit (K) | - |
In Merrill & Burwell (1950), a combination spectrum of the star was reported. It was previously detected in a nova outburst in McLaughlin (1945). Allen (1984) classified the object as a symbiotic star without providing a spectrum. Duerbeck (1987) commented that the spectrum resembled that of a symbiotic star. Symbiotic classification was subsequently questioned by Esipov et al. (1988) but supported by Munari et al. (1990), who suggested an orbital period of 43±5 years (see also Munari & Jurdana-Šepić (2002) and Shore et al., 2011). Another outburst was reported by Munari et al. (1994). In Tatarnikova et al. (2003), lithium was detected in the spectrum of V407 Cyg. The last observed outburst occurred in 2010 (Hirosawa, 2010; Munari et al., 2011; Shore et al., 2011). Coronal emission lines appeared in the spectrum during the 2010 outburst (Munari et al., 2010), and the event was also detected in gamma-rays (Abdo et al., 2010; Aliu et al., 2012). In Iłkiewicz et al. (2019), it was demonstrated that the system might be a progenitor of a Type Ia supernova.