CONFIRMED
MILKY WAY
|
| [MMU2013] 357.32+01.97 | IRAS - | GSC2.4.2 S8HG004351 | AAVSO - |
| SIMBAD [KW2003] 25 | Pan-STARRS 71822628465945525 | SAO - | VSX 305982 |
| GAIA DR3 4058444104218324736 | SkyMapper 173123.18-300844.1 | WRAY - | GCVS - |
| 2MASS J17312318-3008443 | HIP - | Hen - | BD - |
| WISE J173123.16-300844.4 | TYC - | ESO - | HD - |
| Bidelman (1954) | - | Allen (1984) | - | Belzcyński et al. (2001) | - |
| Gaposchkin (1957) | - | Kenyon (1986) | - | Akras et al. (2019) | 357.32+01.97 (Conf.) |
| Boyarchuk (1969) | - | Vaidis (1988, 1991) | - |
| Right ascension (°) | 262.8466Ref | Parallax (mas) | 0.220±0.083Ref | Reddening E(B-V) (mag) | 2.33±0.11Ref, Note |
| Declination (°) | -30.1457Ref | Distance (kpc) | 5.34Ref, Note, 4.13Ref, Note | ||
| Galactic longitude (°) | 357.3235Ref | Proper motion in α (mas/yr) | -2.39±0.08Ref | ||
| Galactic latitude (°) | 1.9710Ref | Proper motion in δ (mas/yr) | -5.74±0.06Ref |
| X-Ray | NoRef | IR type | SRef | Radio | - |
| X-Ray type | - | J (mag) | 10.39Ref | Flickering | - |
| GALEX FUV (mag) | - | H (mag) | 9.07Ref | Outbursts | - |
| GALEX NUV (mag) | - | K (mag) | 8.60Ref | Outburst type | - |
| IUE | NoRef | WISE W1 (mag) | 8.24Ref | Jets | - |
| FUSE | NoRef | WISE W2 (mag) | 8.22Ref | Resolved nebula | - |
| U (mag) | - | WISE W3 (mag) | 7.81Ref | IPmax (eV) | 54.4Ref |
| B (mag) | - | WISE W4 (mag) | 4.44Ref | [O III] lines | NoRef |
| V (mag) | 16.40Ref | IRAS 12μm (Jy) | - | He II lines | YesRef |
| R (mag) | - | IRAS 25μm (Jy) | - | [Fe VII] lines | NoRef |
| I (mag) | - | IRAS 60μm (Jy) | - | O VI lines | NoRef |
| BP (mag) | 17.10Ref | IRAS 100μm (Jy) | - | ||
| G (mag) | 14.71Ref | AKARI S09 (Jy) | - | ||
| RP (mag) | 13.24Ref | AKARI S18 (Jy) | - |
| Orbital period (days) | 400 - 500Ref | 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 | M0-1Ref | Mass (M⊙) | - | Pulsation | - |
| Eff. temperature (K) | - | 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) | 55000Ref | ||||
| Upper limit (K) | - |
According to Miszalski et al. (2013), there might be a very weak detection of O VI 6825, but the absence of [Fe VII] emission lines makes its presence unlikely. The OGLE-IV light curve indicates low-amplitude semi-regular pulsations of the red giant superimposed on longer-term changes occurring over 400–500 days, possibly attributed to orbital motion.