IGR J17463-2854
SUSPECTED
MILKY WAY
Constellation
Sagittarius |
Equatorial coordinates
α = 17 46 21.813
δ = -28 52 56.033 |
Galactic coordinates
l = 0.1307°
b = -0.1109° |
| Suspected |
2015Ref |
| Confirmed |
- |
| Symbiotic IR type |
- |
| Hot component type |
- |
| 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 (°) |
266.5909Ref |
Parallax (mas) |
0.388±0.035Ref |
Reddening E(B-V) (mag) |
70.87±12.7Ref, Note |
| Declination (°) |
-28.8822Ref |
Distance (kpc) |
2.33Ref, Note, 2.26Ref, Note |
|
|
| Galactic longitude (°) |
0.1307Ref |
Proper motion in α (mas/yr) |
1.49±0.04Ref |
|
|
| Galactic latitude (°) |
-0.1109Ref |
Proper motion in δ (mas/yr) |
-3.77±0.03Ref |
|
|
Observations
| X-Ray |
YesRef |
IR type |
- |
Radio |
- |
| X-Ray type |
γRef |
J (mag) |
12.57Ref |
Flickering |
- |
| GALEX FUV (mag) |
- |
H (mag) |
11.72Ref |
Outbursts |
- |
| GALEX NUV (mag) |
- |
K (mag) |
11.31Ref |
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) |
16.62Ref |
IRAS 100μm (Jy) |
- |
|
|
| G (mag) |
15.45Ref |
AKARI S09 (Jy) |
- |
|
|
| RP (mag) |
14.38Ref |
AKARI S18 (Jy) |
- |
|
|
Orbit
| Orbital period (days) |
- |
γ velocity (km/h) |
-24.35±3.25Ref |
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 |
- |
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 |
- |
Mass (M⊙) |
- |
Spin period (min) |
- |
| Shell-burning/Accreting-only |
- |
Radius (R⊙) |
- |
Accretion disk |
- |
| Eff. temperature (K) |
- |
Luminosity (L⊙) |
- |
|
|
| Lower limit (K) |
- |
|
|
|
|
| Upper limit (K) |
- |
|
|
|
|
Notes
Identified as an X-ray source, this star was studied by Karasev et al. (2015). Their analysis suggests that at least one of the potential optical counterparts could be associated with a symbiotic binary system.
References
- Karasev, D. I., Tsygankov, S. S., Lutovinov, A. A., 2015, AstL, 41, 8, 394, 2015AstL...41..394K
Last updated: July 5, 2020