SUSPECTED
MILKY WAY
|
| IGR J15293-5609 | IRAS - | GSC2.4.2 S7DB000329 | AAVSO - |
| SIMBAD 2MASS J15292939-5612133 | Pan-STARRS - | SAO - | VSX 445798 |
| GAIA DR3 5883707000513657216 | SkyMapper 152929.39-561213.5 | WRAY - | GCVS - |
| 2MASS J15292939-5612133 | HIP - | Hen - | BD - |
| WISE J152929.34-561214.3 | 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 (°) | 232.3724Ref | Parallax (mas) | 1.109±0.014Ref | Reddening E(B-V) (mag) | 8.38±0.26Ref, Note |
| Declination (°) | -56.2038Ref | Distance (kpc) | 1.56±0.12Ref 0.89Ref, Note, 0.89Ref, Note |
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| Galactic longitude (°) | 323.6586Ref | Proper motion in α (mas/yr) | -10.08±0.01Ref | ||
| Galactic latitude (°) | 0.1712Ref | Proper motion in δ (mas/yr) | -10.11±0.01Ref |
| X-Ray | YesRef | IR type | S?Ref | Radio | - |
| X-Ray type | β?Ref | J (mag) | 9.62Ref | Flickering | - |
| GALEX FUV (mag) | - | H (mag) | 8.96Ref | Outbursts | - |
| GALEX NUV (mag) | - | K (mag) | 8.75Ref | Outburst type | - |
| IUE | NoRef | WISE W1 (mag) | 8.35Ref | Jets | - |
| FUSE | NoRef | WISE W2 (mag) | 8.25Ref | Resolved nebula | - |
| U (mag) | - | WISE W3 (mag) | 7.98Ref | IPmax (eV) | - |
| B (mag) | 13.46Ref | WISE W4 (mag) | 6.40Ref | [O III] lines | - |
| V (mag) | 12.09Ref | IRAS 12μm (Jy) | - | He II lines | - |
| R (mag) | - | IRAS 25μm (Jy) | - | [Fe VII] lines | - |
| I (mag) | - | IRAS 60μm (Jy) | - | O VI lines | - |
| BP (mag) | 12.46Ref | IRAS 100μm (Jy) | - | ||
| G (mag) | 11.70Ref | AKARI S09 (Jy) | - | ||
| RP (mag) | 10.84Ref | AKARI S18 (Jy) | - |
| Orbital period (days) | - | γ velocity (km/h) | -9.76±5.03Ref | 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 | KRef | Mass (M⊙) | - | Pulsation | - |
| Eff. temperature (K) | 5100Ref | Radius (R⊙) | 14.5Ref | Type | - |
| IR type | S?Ref | Luminosity (L⊙) | - | Pulsation period (days) | - |
| Metallicity [Fe/H] | - | Pulsation ephemeris | - |
| Type/Spectral type | WD?Ref | Mass (M⊙) | - | Spin period (min) | - |
| Shell-burning/Accreting-only | - | Radius (R⊙) | - | Accretion disk | - |
| Eff. temperature (K) | - | Luminosity (L⊙) | - | ||
| Lower limit (K) | - | ||||
| Upper limit (K) | - |
Initially suspected due to its X-ray emission, it was proposed that the optical counterpart might be a K-type giant (Tomsick et al., 2012). The study by Fortin et al. (2018) suggested the presence of a KV secondary and estimated a distance of 45 to 85 pc, indicating a low-luminosity CV. A period of 31.5 days was identified using Gaia spectroscopic data (Beck et al., 2023).