Table 1.
Basic stellar parameters of HD 114082.
| Parameter | Unit | Value | Ref. |
|---|---|---|---|
| Distance | [pc] | 95.06±0.20 | 1 |
| V | [mag] | 8.21±0.01 | 2 |
| SpT | ... | F3 V | 3 |
 |
[K] | 6651±35 (1) | 5 |
 |
[K] | 6600±70 | 4 |
| [Fe/H] | ... | 0.00±0.03 (1) | 5 |
| log(g) | log[cm s−2] | 4.19±0.03 (1) | 5 |
| M* | [M⊙] | 1.47±0.07 | 4 |
| L* | [L⊙] | 3.83±0.05 | 4 |
| R* | [R⊙] | 1.49±0.05 | 4 |
| vsin(i) | [km s−1] | 39.2±0.5 (1) | 5 |
 |
[d] | 1.924±0.016 (2) | 5 |
| Assoc. | ... | Lower Centaurus Crux | 4, 6 |
| Age | [Myr] | 15±6 (3) | 4, 7 |
| Rdisk | [au] | 27.7±3 | 8 |
| idisk | [deg] | 83.3±3 | 8 |
Notes.
The value derived using the ZASPE pipeline (Brahm et al. 2017b) on the observed spectra.
There is no unique Prot visible in the TESS photometry. 
is calculated from vsin(i) assuming i = 90°. Prot should be 1.91 d to match idisk.
As uncertainty, we adopt the age spread Pecaut & Mamajek (2016) derived for the lower Centaurus Crux association rather than the uncertainty of the mean association age (3 Myr).
References. (1) Gaia Collaboration (2016); Gaia Collaboration (2021); (2) Høg et al. (2000); (3) Simbad; (4) Zakhozhay et al. (2022); (5) This paper; (6) Gagné et al. (2018); (7) Pecaut & Mamajek (2016); (8) Wahhaj et al. (2016).
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