CONFIRMED
MILKY WAY
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| RT Cru | IRAS - | GSC2.4.2 S7K5000311 | AAVSO 000-BCV-580 |
| SIMBAD V* RT Cru | Pan-STARRS - | SAO - | VSX 10780 |
| GAIA DR3 5861308338109134208 | SkyMapper - | WRAY 15-988 | GCVS RT Cru |
| 2MASS J12345374-6433560 | HIP - | Hen - | BD - |
| WISE J123453.71-643356.1 | TYC - | ESO - | HD - |
| Bidelman (1954) | - | Allen (1984) | - | Belzcyński et al. (2001) | RT Cru (Conf.) |
| Gaposchkin (1957) | - | Kenyon (1986) | - | Akras et al. (2019) | RT Cru (Conf.) |
| Boyarchuk (1969) | - | Vaidis (1988, 1991) | - |
| Right ascension (°) | 188.7238Ref | Parallax (mas) | 0.397±0.029Ref | Reddening E(B-V) (mag) | 1.36±0.02Ref, Note |
| Declination (°) | -64.5656Ref | Distance (kpc) | 1.2-2.4Ref 2.35Ref, Note, 2.29Ref, Note |
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| Galactic longitude (°) | 301.1562Ref | Proper motion in α (mas/yr) | -9.55±0.03Ref | ||
| Galactic latitude (°) | -1.7509Ref | Proper motion in δ (mas/yr) | -1.16±0.03Ref |
| X-Ray | YesRef | IR type | SRef | Radio | - |
| X-Ray type | δRef | J (mag) | 6.65Ref | Flickering | YesRef |
| GALEX FUV (mag) | - | H (mag) | 5.58Ref | Outbursts | YesRef |
| GALEX NUV (mag) | - | K (mag) | 5.19Ref | Outburst type | - |
| IUE | YesRef | WISE W1 (mag) | 5.48Ref | Jets | Yes?Ref |
| FUSE | NoRef | WISE W2 (mag) | 4.74Ref | Resolved nebula | - |
| U (mag) | - | WISE W3 (mag) | 4.52Ref | IPmax (eV) | 54.4Ref |
| B (mag) | 12.20Ref | WISE W4 (mag) | 4.33Ref | [O III] lines | YesRef |
| V (mag) | 11.35Ref | IRAS 12μm (Jy) | - | He II lines | YesRef |
| R (mag) | 12.09Ref | IRAS 25μm (Jy) | - | [Fe VII] lines | NoRef |
| I (mag) | - | IRAS 60μm (Jy) | - | O VI lines | NoRef |
| BP (mag) | 12.47Ref | IRAS 100μm (Jy) | - | ||
| G (mag) | 10.38Ref | AKARI S09 (Jy) | 0.81Ref | ||
| RP (mag) | 9.04Ref | AKARI S18 (Jy) | 0.26Ref |
| Orbital period (days) | 325±9Ref | 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 (V) = 2452034 + 325±9 x ERef |
| Spectral type | M4-5 IIIRef | Mass (M⊙) | - | Pulsation | YesRef |
| Eff. temperature (K) | - | Radius (R⊙) | - | Type | - |
| IR type | SRef | Luminosity (L⊙) | - | Pulsation period (days) | 63±1Ref |
| Metallicity [Fe/H] | - | Pulsation ephemeris | - |
| Type/Spectral type | WDRef | Mass (M⊙) | 1.3Ref, 1.2Ref, 1.25Ref |
Spin period (min) | - |
| Shell-burning/Accreting-only | accreting-onlyRef | Radius (R⊙) | - | Accretion disk | - |
| Eff. temperature (K) | - | Luminosity (L⊙) | - | ||
| Lower limit (K) | - | ||||
| Upper limit (K) | - |
Classified as a new symbiotic variable by Cielinski & Elizalde (1993). RT Cru exhibits H I, He I, [O III], and He II lines in its spectra, displays flickering and has experienced outbursts in the past, as reported by Cieslinski et al. (1994). The detection of X-ray emission was reported by Masetti et al. (2005). Luna & Sokoloski (2007) suggested that RT Cru represents the first member of a new class of hard X-ray-emitting symbiotic white dwarfs. Further investigations by Luna et al. (2018) revealed that the optical emission lines are prominent during high states of brightness and disappear during low states. Additionally, the detection of reflection signatures in the hard X-ray spectrum allowed Luna et al. (2018) to constrain the white dwarf's mass to 1.25 solar masses.