CONFIRMED
MILKY WAY
|
| BX Mon | IRAS - | GSC2.4.2 S3TB000195 | AAVSO 000-BBN-041 |
| SIMBAD V* BX Mon | Pan-STARRS 103681113448013786 | SAO - | VSX 18929 |
| GAIA DR3 3060568062769059840 | SkyMapper 072522.76-033550.5 | WRAY - | GCVS BX Mon |
| 2MASS J07252276-0335507 | HIP - | Hen - | BD - |
| WISE J072522.78-033550.5 | TYC 4821-2893-1 | ESO - | HD - |
| Bidelman (1954) | BX Mon (Susp.) | Allen (1984) | BX Mon (Conf.) | Belzcyński et al. (2001) | BX Mon (Conf.) |
| Gaposchkin (1957) | BX Mon (Conf.) | Kenyon (1986) | BX Mon (Conf.) | Akras et al. (2019) | BX Mon (Conf.) |
| Boyarchuk (1969) | - | Vaidis (1988, 1991) | BX Mon (Conf.) |
| Right ascension (°) | 111.3448Ref | Parallax (mas) | 0.335±0.031Ref | Reddening E(B-V) (mag) | 0.13±0.0Ref, Note |
| Declination (°) | -3.5974Ref | Distance (kpc) | 2.8Ref, 3±0.75Ref 2.76Ref, Note, 2.65Ref, Note |
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| Galactic longitude (°) | 220.0344Ref | Proper motion in α (mas/yr) | -0.78±0.03Ref | ||
| Galactic latitude (°) | 5.8805Ref | Proper motion in δ (mas/yr) | 1.08±0.03Ref |
| X-Ray | NoRef | IR type | SRef | Radio | YesRef |
| X-Ray type | - | J (mag) | 7.04Ref | Flickering | NoRef, YesRef |
| GALEX FUV (mag) | - | H (mag) | 6.04Ref | Outbursts | YesRef |
| GALEX NUV (mag) | - | K (mag) | 5.71Ref | Outburst type | Z And?Ref |
| IUE | NoRef | WISE W1 (mag) | 5.45Ref | Jets | - |
| FUSE | NoRef | WISE W2 (mag) | 5.32Ref | Resolved nebula | - |
| U (mag) | - | WISE W3 (mag) | 4.98Ref | IPmax (eV) | 54.4Ref |
| B (mag) | 12.27Ref | WISE W4 (mag) | 4.62Ref | [O III] lines | YesRef |
| V (mag) | 11.24Ref | IRAS 12μm (Jy) | - | He II lines | YesRef |
| R (mag) | 10.92Ref | IRAS 25μm (Jy) | - | [Fe VII] lines | NoRef |
| I (mag) | - | IRAS 60μm (Jy) | - | O VI lines | NoRef |
| BP (mag) | 10.56Ref | IRAS 100μm (Jy) | - | ||
| G (mag) | 9.67Ref | AKARI S09 (Jy) | 0.50Ref | ||
| RP (mag) | 8.55Ref | AKARI S18 (Jy) | - |
| Orbital period (days) | 1380Ref, 1401±8Ref, 1259±16Ref |
γ velocity (km/h) | 29.1±0.8Ref, 29.12±0.13Ref | Size of giant’s orbit (AU) | 0.48Ref |
| Eccentricity | 0.49±0.05Ref, 0.444±0.037Ref | RV of giant (km/h) | 4.3±0.3Ref, 4.61±0.24Ref | Separation (AU) | 2-5.9Ref |
| Inclination (°) | >62Ref | Inferior conj. of giant (JD) | 2449530 | Mass function | 0.0076Ref, 0.0092Ref |
| Eclipses | YesRef | Mass ratio | 6.7Ref | ||
| Orbital ephemeris | - |
| Spectral type | M6 IIIRef, M4.6 IIIRef, M5 IIIRef, M5 IIIRef |
Mass (M⊙) | 3.7±1.9Ref, 1.5Ref | Pulsation | - |
| Eff. temperature (K) | 3470±200Ref, 3400Ref | Radius (R⊙) | 160±50Ref | Type | - |
| IR type | SRef | Luminosity (L⊙) | 3400±1700Ref | Pulsation period (days) | - |
| Metallicity [Fe/H] | -0.34Ref, -0.40±0.08Ref | Pulsation ephemeris | - |
| Type/Spectral type | AD/WD?Ref | Mass (M⊙) | 0.55±0.26Ref | Spin period (min) | - |
| Shell-burning/Accreting-only | accreting-onlyRef | Radius (R⊙) | - | Accretion disk | - |
| Eff. temperature (K) | 8000Ref | Luminosity (L⊙) | 78-230Ref, 230Ref | ||
| Lower limit (K) | - | ||||
| Upper limit (K) | - |
Suspected by Bidelman (1954) based on the observations of Mayall & Cannon (1940) and Merrill & Burwell (1950). In Mayall (1940), a 1380-day period was reported based on Harvard plates. Not listed in the catalog by Boyarchuk (1969). Classified as M4ep by Sanduleak & Stephenson (1973). In Allen (1978), only Balmer lines were reported with an early M star continuum, claiming no indication of the symbiotic nature of this object. In Michalitsianos et al. (1982), several strong emission lines in the UV spectral region were detected (ionization potential up to 47.9 eV). In Whitelock & Catchpole (1983), it was reported that the giant is not pulsating as a Mira variable. Iijima (1984) detected faint He II lines in the optical spectra of BX Mon. The hot component might be similar to CH Cyg (Viotti et al., 1986) and has a spectrum of an A-F star. However, the mass of the hot component (Mh = 0.55 M☉) is not consistent with a main sequence or giant A-F star (Dumm et al., 1998). It is suggested to either be an accretion disk around a low-mass main sequence star (requiring a very high mass accretion rate) or a WD with a hydrogen-burning shell (Dumm et al., 1998).