NuSTAR J095838+6909.2
SUSPECTED
MILKY WAY
Constellation
Ursa Major |
Equatorial coordinates
α = 09 58 38.112
δ = +69 09 13.680 |
Galactic coordinates
l = 141.7836°
b = 41.0735° |
| Suspected |
2017Ref |
| Confirmed |
- |
| Symbiotic IR type |
S?Ref |
| 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 (°) |
149.6637Ref |
Parallax (mas) |
3.406±0.028Ref |
Reddening E(B-V) (mag) |
0.06±0.0Ref, Note |
| Declination (°) |
69.1533Ref |
Distance (kpc) |
0.29Ref, Note, 0.29Ref, Note |
|
|
| Galactic longitude (°) |
141.7836Ref |
Proper motion in α (mas/yr) |
-18.66±0.03Ref |
|
|
| Galactic latitude (°) |
41.0735Ref |
Proper motion in δ (mas/yr) |
-11.00±0.03Ref |
|
|
Observations
| X-Ray |
YesRef |
IR type |
S?Ref |
Radio |
- |
| X-Ray type |
δRef |
J (mag) |
13.38Ref |
Flickering |
- |
| GALEX FUV (mag) |
- |
H (mag) |
12.67Ref |
Outbursts |
- |
| GALEX NUV (mag) |
- |
K (mag) |
12.51Ref |
Outburst type |
- |
| IUE |
NoRef |
WISE W1 (mag) |
12.38Ref |
Jets |
- |
| FUSE |
NoRef |
WISE W2 (mag) |
12.32Ref |
Resolved nebula |
- |
| U (mag) |
- |
WISE W3 (mag) |
11.38Ref |
IPmax (eV) |
- |
| B (mag) |
17.62Ref |
WISE W4 (mag) |
8.93Ref |
[O III] lines |
- |
| V (mag) |
16.13Ref |
IRAS 12μm (Jy) |
- |
He II lines |
- |
| R (mag) |
- |
IRAS 25μm (Jy) |
- |
[Fe VII] lines |
- |
| I (mag) |
- |
IRAS 60μm (Jy) |
- |
O VI lines |
- |
| BP (mag) |
16.45Ref |
IRAS 100μm (Jy) |
- |
|
|
| G (mag) |
15.51Ref |
AKARI S09 (Jy) |
- |
|
|
| RP (mag) |
14.54Ref |
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 |
- |
Mass (M⊙) |
- |
Pulsation |
- |
| Eff. temperature (K) |
- |
Radius (R⊙) |
- |
Type |
- |
| IR type |
S?Ref |
Luminosity (L⊙) |
- |
Pulsation period (days) |
- |
| Metallicity [Fe/H] |
- |
|
|
Pulsation ephemeris |
- |
Hot component
| Type/Spectral type |
- |
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
Tomsick et al. (2017) associated the hard X-ray source with an M-type star and suggested that it might be a symbiotic system.
References
- Tomsick, J. A., Lansbury, G. B., Rahoui, F. et al., 2017, ApJS, 230, 2, 25, 2017ApJS..230...25T
Last updated: August 22, 2021