SUSPECTED SMC
Equatorial coordinates
α = 13.539757 ± 0.014800 | 00 54 09.541560
δ = -72.695359 ± 0.012900| -72 41 43.291671 |
|
Constellation |
Tucana |
Symbiotic IR Type |
D’ |
Spectral Type |
B0 I [e] |
Magnitude range (V) |
13.0 – 14.3 |
Outbursts |
No |
|
|
Identifiers
Position
Right ascension (°) |
13.539757 ± 0.014800 |
Parallax (mas) |
– |
Reddening E(B-V) (mag) |
0.367 ± 0.028 |
Declination (°) |
-72.695359 ± 0.012900 |
Distance (kpc) |
62.10 ± 1.90 |
|
|
Galactic longitude (°) |
302.648558 ± 0.014800 |
Proper motion in α (mas/yr) |
0.591 ± 0.031 |
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|
Galactic latitude (°) |
-44.431394 ± 0.012900 |
Proper motion in δ (mas/yr) |
-1.173 ± 0.025 |
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|
Observations
U (mag) |
12.94 |
X-Ray |
No |
Flickering |
|
B (mag) |
13.48 |
X-Ray type |
|
Outbursts |
No |
V (mag) |
13.82 |
IUE |
Yes |
Type |
|
R (mag) |
12.79 |
IRAS flux at 12 μm (Jy) |
|
IPmax (eV) |
114 |
I (mag) |
12.55 |
IRAS flux at 25 μm (Jy) |
|
OVI lines |
Yes |
G (mag) |
13.18 |
IRAS flux at 60 μm (Jy) |
|
|
|
J (mag) |
12.35 |
IRAS flux at 100 μm (Jy) |
|
|
|
H (mag) |
11.93 |
WISE W1 (mag) |
9.38 |
|
|
K (mag) |
11.11 |
WISE W2 (mag) |
8.36 |
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|
L (mag) |
9.45 |
WISE W3 (mag) |
6.28 |
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|
|
WISE W4 (mag) |
4.88 |
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Radio |
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Radio flux (mJy) |
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Orbit
Orbital period (days) |
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γ velocity (km/h) |
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Size of giant’s orbit (AU) |
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Eccentricity |
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RV of giant (km/h) |
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Separation (AU) |
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Inclination (°) |
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Inferior conj. of giant (JD) |
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Mass function |
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Ephemeris type |
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Mass ratio |
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Ephemeris T0 (JD) |
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Cool component
Spectral type |
B0 I [e] |
Mass (M⊙) |
35-40 |
Pulsation |
|
Eff. temperature (K) |
25000
4015 |
Radius (R⊙) |
33-36 |
Type |
|
IR type |
D’ |
Luminosity (L⊙) |
300000-460000 |
Pulsation period (days) |
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Metallicity [Fe/H] |
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Ephemeris type |
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Ephemeris T0 (JD) |
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Hot component
Type/Spectra |
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Mass (M⊙) |
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Spin period (min) |
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Eff. temperature (K) |
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Radius (R⊙) |
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Accretion disk |
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Lower limit (K) |
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Luminosity (L⊙) |
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Upper limit (K) |
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Links
SIMBAD CDS Portal VSX
Notes
LHA 115-S 18 is a very peculiar emission-line star exhibiting the B[e] phenomenon. Its spectrum shows features of an extremely wide range of excitation and ionization stages, extending from highly ionized atomic lines (Si IV, C IV, He II) in the ultraviolet and optical regions to molecular emission bands of CO and TiO in the optical and infrared regions (Torres et al., 2012). They also observed Raman-scattered O VI lines in the spectra of the star but according to their analysis, a symbiotic B[e] scenario seems not to be the most plausible. Therefore we classified this object only as a suspected symbiotic star. On the other hand, Akras et al. (2019) list this star as confirmed one.
References
- Akras, S., Guzman-Ramirez, L., Leal-Ferreira, M. L., et al., 2019, ApJS, 240, 21, 2019ApJS..240…21A
- Shore, S. N., Sanduleak, N., Allen, D. A., 1987, A&A, 176, 59, 1987A&A…176…59S
- Torres, A. F., Kraus, M., Cidale, L. S., et al., 2012, MNRAS, 427, L80, 2012MNRAS.427L..80T
- van Genderen, A. M., Sterken, C., 2002, A&A, 386, 926, 2002A&A…386..926V
- Zickgraf, F. J., Wolf, B., Stahl, O., et al., 1989, A&A, 220, 206, 1989A&A…220..206Z
Last updated: May 2, 2019 @ 11:02 am