CONFIRMED
MILKY WAY
|
| PHR J1757-2718 | IRAS 17544-2719 | GSC2.4.2 S8CO017265 | AAVSO - |
| SIMBAD PHR J1757-2718 | Pan-STARRS 75232693852311844 | SAO - | VSX 305988 |
| GAIA DR3 4063571088205835008 | SkyMapper - | WRAY - | GCVS - |
| 2MASS J17573246-2718253 | HIP - | Hen - | BD - |
| WISE J175732.48-271826.3 | TYC - | ESO - | HD - |
| Bidelman (1954) | - | Allen (1984) | - | Belzcyński et al. (2001) | - |
| Gaposchkin (1957) | - | Kenyon (1986) | - | Akras et al. (2019) | PHR J1757−2718 (Conf.) |
| Boyarchuk (1969) | - | Vaidis (1988, 1991) | - |
| Right ascension (°) | 269.3853Ref | Parallax (mas) | -0.237±0.112Ref | Reddening E(B-V) (mag) | 3.32±0.19Ref, Note |
| Declination (°) | -27.3071Ref | Distance (kpc) | 10.12Ref, Note, 8.73Ref, Note | ||
| Galactic longitude (°) | 2.7429Ref | Proper motion in α (mas/yr) | 2.27±0.12Ref | ||
| Galactic latitude (°) | -1.4281Ref | Proper motion in δ (mas/yr) | -5.87±0.08Ref |
| X-Ray | - | IR type | SRef | Radio | - |
| X-Ray type | - | J (mag) | 10.57Ref | Flickering | - |
| GALEX FUV (mag) | - | H (mag) | 9.19Ref | Outbursts | - |
| GALEX NUV (mag) | - | K (mag) | 8.52Ref | Outburst type | - |
| IUE | NoRef | WISE W1 (mag) | 7.95Ref | Jets | - |
| FUSE | NoRef | WISE W2 (mag) | 8.06Ref | Resolved nebula | - |
| U (mag) | - | WISE W3 (mag) | 7.50Ref | IPmax (eV) | 114Ref |
| B (mag) | - | WISE W4 (mag) | 6.06Ref | [O III] lines | NoRef |
| V (mag) | - | IRAS 12μm (Jy) | 1.21Ref | He II lines | YesRef |
| R (mag) | 15.78Ref | IRAS 25μm (Jy) | 2.30Ref | [Fe VII] lines | YesRef |
| I (mag) | - | IRAS 60μm (Jy) | 17.80Ref | O VI lines | YesRef |
| BP (mag) | 18.94Ref | IRAS 100μm (Jy) | 231.00Ref | ||
| G (mag) | 16.26Ref | AKARI S09 (Jy) | - | ||
| RP (mag) | 14.58Ref | AKARI S18 (Jy) | - |
| Orbital period (days) | 585Ref | 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 | Min (I) = 2455634.9 + 585 x ERef |
| Spectral type | M1-6Ref | Mass (M⊙) | - | Pulsation | YesRef |
| Eff. temperature (K) | - | Radius (R⊙) | - | Type | SRRef |
| 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) | 114000Ref | ||||
| Upper limit (K) | - |
The symbiotic nebular continuum possibly masks the TiO bands, implying a later spectral type of M5-6, as suggested in Miszalski et al. (2013). The emission-line spectrum is indicative of a highly ionized S-type symbiotic. Despite the very weak Raman-scattered O VI 6825 feature, its presence is likely genuine, supported by the detection of [Fe VII] emission (Miszalski et al., 2013). The OGLE-IV light curve exhibits long-term changes over 500–600 days, attributed to orbital motion (Miszalski et al., 2013).