CONFIRMED
MILKY WAY
|
| CQ Dra | IRAS 12279+6928 | GSC2.4.2 N4N6000122 | AAVSO 000-BBS-882 |
| SIMBAD * 4 Dra | Pan-STARRS - | SAO 15816 | VSX 13789 |
| GAIA DR3 1683014206596170240 | SkyMapper - | WRAY - | GCVS CQ Dra |
| 2MASS J12300664+6912036 | HIP 60998 | Hen - | BD +70 700 |
| WISE J123006.57+691203.4 | TYC 4394-1871-1 | ESO - | HD 108907 |
| Bidelman (1954) | - | Allen (1984) | - | Belzcyński et al. (2001) | - |
| Gaposchkin (1957) | - | Kenyon (1986) | - | Akras et al. (2019) | 4 Dra (Conf.) |
| Boyarchuk (1969) | - | Vaidis (1988, 1991) | - |
| Right ascension (°) | 187.5270Ref | Parallax (mas) | 5.723±0.188Ref | Reddening E(B-V) (mag) | 0.02±0.0Ref, Note |
| Declination (°) | 69.2009Ref | Distance (kpc) | 0.178Ref 0.17Ref, Note, 0.17Ref, Note |
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| Galactic longitude (°) | 125.7485Ref | Proper motion in α (mas/yr) | -57.31±0.21Ref | ||
| Galactic latitude (°) | 47.8106Ref | Proper motion in δ (mas/yr) | -50.37±0.22Ref |
| X-Ray | YesRef | IR type | SRef | Radio | YesRef |
| X-Ray type | δRef | J (mag) | 1.55Ref | Flickering | - |
| GALEX FUV (mag) | - | H (mag) | 0.56Ref | Outbursts | - |
| GALEX NUV (mag) | - | K (mag) | 0.45Ref | Outburst type | - |
| IUE | YesRef | WISE W1 (mag) | -1.79Ref | Jets | - |
| FUSE | YesRef | WISE W2 (mag) | -0.76Ref | Resolved nebula | - |
| U (mag) | 8.38Ref | WISE W3 (mag) | 0.13Ref | IPmax (eV) | 54.4 (UV)Ref |
| B (mag) | 6.57Ref | WISE W4 (mag) | 0.09Ref | [O III] lines | NoRef |
| V (mag) | 4.95Ref | IRAS 12μm (Jy) | 37.70Ref | He II lines | NoRef |
| R (mag) | - | IRAS 25μm (Jy) | 9.27Ref | [Fe VII] lines | NoRef |
| I (mag) | - | IRAS 60μm (Jy) | 1.57Ref | O VI lines | NoRef |
| BP (mag) | 5.29Ref | IRAS 100μm (Jy) | 1.00Ref | ||
| G (mag) | 4.03Ref | AKARI S09 (Jy) | 49.87Ref | ||
| RP (mag) | 2.96Ref | AKARI S18 (Jy) | 11.51Ref |
| Orbital period (days) | 1703±3Ref | γ velocity (km/h) | -14.35±0.12Ref | Size of giant’s orbit (AU) | 0.548Ref |
| Eccentricity | 0.3±0.05Ref | RV of giant (km/h) | 3.67±0.19Ref | Separation (AU) | 4Ref |
| Inclination (°) | - | Inferior conj. of giant (JD) | 2442868 | Mass function | 0.0076Ref |
| Eclipses | - | Mass ratio | 6.5Ref | ||
| Orbital ephemeris | - |
| Spectral type | M3 IIIRef | Mass (M⊙) | 5Ref | Pulsation | - |
| Eff. temperature (K) | - | Radius (R⊙) | - | Type | - |
| IR type | SRef | Luminosity (L⊙) | - | Pulsation period (days) | - |
| Metallicity [Fe/H] | - | Pulsation ephemeris | - |
| Type/Spectral type | CVRef | Mass (M⊙) | 0.85Ref | Spin period (min) | - |
| Shell-burning/Accreting-only | accreting-onlyRef | Radius (R⊙) | 0.006Ref | Accretion disk | - |
| Eff. temperature (K) | 110000Ref, 20000Ref | Luminosity (L⊙) | 6.6Ref | ||
| Lower limit (K) | - | ||||
| Upper limit (K) | - |
This object, initially proposed as a representative of a new class of interacting binary stars consisting of a normal M giant and an AM Her or CV companion based on IUE observations (Reimers, 1985). The period of 3h58m detected by Reimers et al. (1988) was suggested to be the orbital period of the CV companion. Conversely, Eggleton et al. (1989) proposed a model wherein a WD with a rotational period of about 4 hours accretes directly from the giant's wind, leaning towards a more typical symbiotic binary scenario. The detection of X-ray emission by Wheatley et al. (2003) favored the presence of an accreting white dwarf, either single or in a CV, rather than a magnetic AM Her system. The 4h modulation was not evident in their data or in HST observations. The X-ray emission resembled that of CH Cyg. An analysis of FUSE data by Sion et al. (2017) suggested that the hot companion might indeed be a CV, with UV data resembling the dwarf nova RU Peg.