IGR J17200-3116
SUSPECTED
MILKY WAY
Constellation
Scorpius |
Equatorial coordinates
α = 17 20 05.912
δ = -31 16 59.558 |
Galactic coordinates
l = 355.0221°
b = 3.3474° |
| Suspected |
2018Ref |
| 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 (°) |
260.0246Ref |
Parallax (mas) |
-0.055±0.160Ref |
Reddening E(B-V) (mag) |
1.61±0.11Ref, Note |
| Declination (°) |
-31.2832Ref |
Distance (kpc) |
6±2Ref
6.64Ref, Note, 7.02Ref, Note |
|
|
| Galactic longitude (°) |
355.0221Ref |
Proper motion in α (mas/yr) |
-4.45±0.16Ref |
|
|
| Galactic latitude (°) |
3.3474Ref |
Proper motion in δ (mas/yr) |
-4.68±0.12Ref |
|
|
Observations
| X-Ray |
YesRef |
IR type |
- |
Radio |
- |
| X-Ray type |
δRef |
J (mag) |
13.58Ref |
Flickering |
- |
| GALEX FUV (mag) |
- |
H (mag) |
12.33Ref |
Outbursts |
- |
| GALEX NUV (mag) |
- |
K (mag) |
11.98Ref |
Outburst type |
- |
| IUE |
NoRef |
WISE W1 (mag) |
- |
Jets |
- |
| FUSE |
NoRef |
WISE W2 (mag) |
- |
Resolved nebula |
- |
| U (mag) |
- |
WISE W3 (mag) |
- |
IPmax (eV) |
13.6Ref |
| B (mag) |
- |
WISE W4 (mag) |
- |
[O III] lines |
NoRef |
| V (mag) |
- |
IRAS 12μm (Jy) |
- |
He II lines |
NoRef |
| R (mag) |
- |
IRAS 25μm (Jy) |
- |
[Fe VII] lines |
NoRef |
| I (mag) |
- |
IRAS 60μm (Jy) |
- |
O VI lines |
NoRef |
| BP (mag) |
20.12Ref |
IRAS 100μm (Jy) |
- |
|
|
| G (mag) |
17.91Ref |
AKARI S09 (Jy) |
- |
|
|
| RP (mag) |
16.51Ref |
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 |
K IIIRef |
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) |
5.433Ref |
| Shell-burning/Accreting-only |
accreting-only?Ref |
Radius (R⊙) |
- |
Accretion disk |
- |
| Eff. temperature (K) |
- |
Luminosity (L⊙) |
- |
|
|
| Lower limit (K) |
- |
|
|
|
|
| Upper limit (K) |
- |
|
|
|
|
Notes
The possible symbiotic nature of this source was suggested by Fortin et al. (2018), who identified an optical KIII counterpart to the X-ray source.
References
- Esposito, P., Israel, G. L., Sidoli, L. et al., 2014, MNRAS, 441, 2, 1126, 2014MNRAS.441.1126E
- Fortin, F., Chaty, S., Coleiro, A. et al., 2018, A&A, 618, A150, 2018A&A...618A.150F
Last updated: April 12, 2021