SUSPECTED
M31
|
[O2006] QSS 10 | IRAS - | GSC2.4.2 NBVE062080 | AAVSO - |
SIMBAD [O2006] QSS 10 | Pan-STARRS - | SAO - | VSX - |
GAIA DR3 - | SkyMapper - | WRAY - | GCVS - |
2MASS - | HIP - | Hen - | BD - |
WISE - | TYC - | ESO - | HD - |
Bidelman (1954) | - | Allen (1984) | - | Belzcyński et al. (2001) | - |
Gaposchkin (1957) | - | Kenyon (1986) | - | Akras et al. (2019) | - |
Boyarchuk (1969) | - | Vaidis (1988, 1991) | - |
Right ascension (°) | 10.6615Ref | Parallax (mas) | - | Reddening E(B-V) (mag) | 0.48±0.1Ref, Note |
Declination (°) | 41.2575Ref | Distance (kpc) | 785±25Ref -, Note |
||
Galactic longitude (°) | 121.1552Ref | Proper motion in α (mas/yr) | - | ||
Galactic latitude (°) | -21.5840Ref | Proper motion in δ (mas/yr) | - |
X-Ray | YesRef | IR type | - | Radio | - |
X-Ray type | - | J (mag) | - | Flickering | - |
GALEX FUV (mag) | - | H (mag) | - | Outbursts | - |
GALEX NUV (mag) | - | K (mag) | - | Outburst type | - |
IUE | NoRef | WISE W1 (mag) | - | Jets | - |
FUSE | NoRef | WISE W2 (mag) | - | Resolved nebula | - |
U (mag) | - | WISE W3 (mag) | - | IPmax (eV) | - |
B (mag) | - | WISE W4 (mag) | - | [O III] lines | - |
V (mag) | - | IRAS 12μm (Jy) | - | He II lines | - |
R (mag) | - | IRAS 25μm (Jy) | - | [Fe VII] lines | - |
I (mag) | - | IRAS 60μm (Jy) | - | O VI lines | - |
BP (mag) | - | IRAS 100μm (Jy) | - | ||
G (mag) | - | AKARI S09 (Jy) | - | ||
RP (mag) | - | 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 | - | Luminosity (L⊙) | - | Pulsation period (days) | - |
Metallicity [Fe/H] | - | Pulsation ephemeris | - |
Type/Spectral type | - | Mass (M⊙) | - | Spin period (min) | - |
Shell-burning/Accreting-only | - | Radius (R⊙) | - | Accretion disk | - |
Eff. temperature (K) | - | Luminosity (L⊙) | - | ||
Lower limit (K) | - | ||||
Upper limit (K) | - |
Identified as an X-ray source in M31, Chiosi et al. (2014) suspected its symbiotic nature. However, the object is located in a rather crowded field, and, moreover, the X-ray luminosity is quite low (and variable?), which is not consistent with hydrogen burning.