CONFIRMED
MILKY WAY
|
| PPA J1752-3542 | IRAS 17488-3541 | GSC2.4.2 S8BJ283266 | AAVSO - |
| SIMBAD PPA J1752-3542 | Pan-STARRS - | SAO - | VSX 306002 |
| GAIA DR3 4040631118239300096 | SkyMapper - | WRAY - | GCVS - |
| 2MASS - | HIP - | Hen - | BD - |
| WISE J175206.03-354208.5 | TYC - | ESO - | HD - |
| Bidelman (1954) | - | Allen (1984) | - | Belzcyński et al. (2001) | - |
| Gaposchkin (1957) | - | Kenyon (1986) | - | Akras et al. (2019) | PPA 1752-3542 (Susp.) |
| Boyarchuk (1969) | - | Vaidis (1988, 1991) | - |
| Right ascension (°) | 268.0246Ref | Parallax (mas) | 0.219±0.129Ref | Reddening E(B-V) (mag) | 0.42±0.02Ref, Note |
| Declination (°) | -35.7018Ref | Distance (kpc) | 5.89Ref, Note, 4.08Ref, Note | ||
| Galactic longitude (°) | 354.8927Ref | Proper motion in α (mas/yr) | -1.62±0.15Ref | ||
| Galactic latitude (°) | -4.6491Ref | Proper motion in δ (mas/yr) | -4.97±0.09Ref |
| X-Ray | - | IR type | S?Ref | 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) | 10.82Ref | Jets | - |
| FUSE | NoRef | WISE W2 (mag) | 10.75Ref | Resolved nebula | - |
| U (mag) | - | WISE W3 (mag) | 8.85Ref | IPmax (eV) | 35.1Ref |
| B (mag) | - | WISE W4 (mag) | 7.16Ref | [O III] lines | YesRef |
| V (mag) | - | IRAS 12μm (Jy) | 4.74Ref | He II lines | NoRef |
| R (mag) | - | IRAS 25μm (Jy) | 2.02Ref | [Fe VII] lines | NoRef |
| I (mag) | - | IRAS 60μm (Jy) | 0.57Ref | O VI lines | NoRef |
| BP (mag) | 18.59Ref | IRAS 100μm (Jy) | 5.51Ref | ||
| G (mag) | 17.81Ref | AKARI S09 (Jy) | - | ||
| RP (mag) | 16.94Ref | 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 | Yes?Ref |
| Eff. temperature (K) | - | Radius (R⊙) | - | Type | SR?Ref |
| IR type | S?Ref | 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) | 35000Ref | ||||
| Upper limit (K) | - |
The spectrum exhibits prominent Hα, Hβ, and [O III] λλ5007, 4959 emission lines. The OGLE light curve suggests a resemblance to an S-type symbiotic star, but the system is too faint to be detected in 2MASS (Miszalski et al., 2013).