CONFIRMED
MILKY WAY
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| Sct X-1 | IRAS 18327-0739 | GSC2.4.2 S9OA136512 | AAVSO - |
| SIMBAD X Sct X-1 | Pan-STARRS 98862788576103610 | SAO - | VSX - |
| GAIA DR3 4156747212545110400 | SkyMapper - | WRAY - | GCVS - |
| 2MASS J18352582-0736501 | HIP - | Hen - | BD - |
| WISE J183525.83-073650.9 | TYC - | ESO - | HD - |
| Bidelman (1954) | - | Allen (1984) | - | Belzcyński et al. (2001) | - |
| Gaposchkin (1957) | - | Kenyon (1986) | - | Akras et al. (2019) | Sct X-1 (Conf.) |
| Boyarchuk (1969) | - | Vaidis (1988, 1991) | - |
| Right ascension (°) | 278.8576Ref | Parallax (mas) | - | Reddening E(B-V) (mag) | 27.58±3.15Ref, Note |
| Declination (°) | -7.6140Ref | Distance (kpc) | 10Ref, 3.6±0.75Ref -, Note |
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| Galactic longitude (°) | 24.3360Ref | Proper motion in α (mas/yr) | - | ||
| Galactic latitude (°) | 0.0657Ref | Proper motion in δ (mas/yr) | - |
| X-Ray | YesRef | IR type | DRef | Radio | - |
| X-Ray type | γRef | J (mag) | 12.06Ref | Flickering | - |
| GALEX FUV (mag) | - | H (mag) | 8.52Ref | Outbursts | - |
| GALEX NUV (mag) | - | K (mag) | 6.55Ref | Outburst type | - |
| IUE | NoRef | WISE W1 (mag) | 4.81Ref | Jets | - |
| FUSE | NoRef | WISE W2 (mag) | 4.01Ref | Resolved nebula | - |
| U (mag) | - | WISE W3 (mag) | 2.26Ref | IPmax (eV) | - |
| B (mag) | - | WISE W4 (mag) | 0.96Ref | [O III] lines | - |
| V (mag) | - | IRAS 12μm (Jy) | 10.30Ref | He II lines | - |
| R (mag) | - | IRAS 25μm (Jy) | 7.61Ref | [Fe VII] lines | - |
| I (mag) | - | IRAS 60μm (Jy) | 187.00Ref | O VI lines | - |
| BP (mag) | 22.34Ref | IRAS 100μm (Jy) | 727.00Ref | ||
| G (mag) | 20.39Ref | AKARI S09 (Jy) | 4.72Ref | ||
| RP (mag) | 18.35Ref | AKARI S18 (Jy) | 4.27Ref |
| Orbital period (days) | >4383Ref | 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 | 2.31Ref | ||
| Orbital ephemeris | - |
| Spectral type | M8-9 IIIRef | Mass (M⊙) | 3Ref | Pulsation | YesRef |
| Eff. temperature (K) | 2000Ref | Radius (R⊙) | 850Ref | Type | MiraRef |
| IR type | DRef | Luminosity (L⊙) | 10000Ref | Pulsation period (days) | 621Ref |
| Metallicity [Fe/H] | - | Pulsation ephemeris | - |
| Type/Spectral type | NSRef | Mass (M⊙) | 1.3Ref | Spin period (min) | 1.867Ref |
| Shell-burning/Accreting-only | accreting-onlyRef | Radius (R⊙) | - | Accretion disk | - |
| Eff. temperature (K) | - | Luminosity (L⊙) | - | ||
| Lower limit (K) | - | ||||
| Upper limit (K) | - |
This long-known X-ray source was identified as a symbiotic X-ray binary by Kaplan et al. (2007), who detected the optical/IR counterpart, suggesting it possibly is a late-type supergiant. The system is highly reddened. De et al. (2022) claimed that the cool component is a Mira variable, making the system the first of such a type.