3XMM J181923.7-170616
POSSIBLE
MILKY WAY
Constellation
Sagittarius |
Equatorial coordinates
α = 18 19 23.729
δ = -17 06 16.102 |
Galactic coordinates
l = 14.1158°
b = -0.8922° |
| Suspected |
2017Ref |
| Confirmed |
- |
| Symbiotic IR type |
- |
| Hot component type |
accreting-only?Ref |
| Outbursts |
- |
|
|
Symbiotic Catalogs
| Bidelman (1954) |
- |
Allen (1984) |
- |
Belzcyński et al. (2001) |
- |
| Gaposchkin (1957) |
- |
Kenyon (1986) |
- |
Akras et al. (2019) |
- |
| Boyarchuk (1969) |
- |
Vaidis (1988, 1991) |
- |
Position
| Right ascension (°) |
274.8489Ref |
Parallax (mas) |
- |
Reddening E(B-V) (mag) |
6.72±0.65Ref, Note |
| Declination (°) |
-17.1045Ref |
Distance (kpc) |
-, Note |
|
|
| Galactic longitude (°) |
14.1158Ref |
Proper motion in α (mas/yr) |
- |
|
|
| Galactic latitude (°) |
-0.8922Ref |
Proper motion in δ (mas/yr) |
- |
|
|
Observations
| X-Ray |
YesRef |
IR type |
- |
Radio |
YesRef |
| X-Ray type |
γRef |
J (mag) |
- |
Flickering |
- |
| GALEX FUV (mag) |
- |
H (mag) |
- |
Outbursts |
- |
| GALEX NUV (mag) |
- |
K (mag) |
- |
Outburst type |
- |
| IUE |
NoRef |
WISE W1 (mag) |
- |
Jets |
- |
| FUSE |
NoRef |
WISE W2 (mag) |
- |
Resolved nebula |
- |
| U (mag) |
- |
WISE W3 (mag) |
- |
IPmax (eV) |
- |
| B (mag) |
- |
WISE W4 (mag) |
- |
[O III] lines |
- |
| V (mag) |
- |
IRAS 12μm (Jy) |
- |
He II lines |
- |
| R (mag) |
- |
IRAS 25μm (Jy) |
- |
[Fe VII] lines |
- |
| I (mag) |
- |
IRAS 60μm (Jy) |
- |
O VI lines |
- |
| BP (mag) |
21.65Ref |
IRAS 100μm (Jy) |
- |
|
|
| G (mag) |
20.54Ref |
AKARI S09 (Jy) |
- |
|
|
| RP (mag) |
19.36Ref |
AKARI S18 (Jy) |
- |
|
|
Orbit
| 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 |
- |
|
|
|
|
Cool component
| Spectral type |
K3Ref |
Mass (M⊙) |
- |
Pulsation |
- |
| Eff. temperature (K) |
- |
Radius (R⊙) |
- |
Type |
- |
| IR type |
- |
Luminosity (L⊙) |
- |
Pulsation period (days) |
- |
| Metallicity [Fe/H] |
- |
|
|
Pulsation ephemeris |
- |
Hot component
| Type/Spectral type |
NSRef |
Mass (M⊙) |
- |
Spin period (min) |
- |
| Shell-burning/Accreting-only |
accreting-only?Ref |
Radius (R⊙) |
- |
Accretion disk |
- |
| Eff. temperature (K) |
- |
Luminosity (L⊙) |
- |
|
|
| Lower limit (K) |
- |
|
|
|
|
| Upper limit (K) |
- |
|
|
|
|
Notes
Detected as a hard X-ray source, a potential optical counterpart is proposed to be a K3 giant. The study by Qiu et al. (2017) suggests a symbiotic nature, with the hot component likely being a 408 s pulsar.
References
- Qiu, H., Zhou, P., Yu, W. et al., 2017, ApJ, 847, 1, 44, 2017ApJ...847...44Q
Last updated: May 8, 2020