Table F.5
General and dynamical properties of KOBE-1.
| Parameter | Value | Ref. |
|---|---|---|
| Basic identifiers | ||
| Hipparcos | HIP 5957 | 1 |
| Gliese | Gl 55.2 | 2 |
| TESS | TIC 16917838 | 3 |
| Gaia DR3a | 294517800251711616 | 4 |
| Sp. type | K7 V | 0b |
| Astrometry and kinematics | ||
| α (J2016.0) | 01:16:27.72 | 4 |
| δ (J2016.0) | +25:19:51.7 | 4 |
| l [deg] | 130.091481 | 4 |
| b [deg] | −37.189786 | 4 |
| ϖ [mas] | 41.876 ± 0.021 | 4 |
| d [pc] | 23.880 ± 0.012 | 4 |
| µα cos δ [mas yr−1] | 429.196 ± 0.019 | 4 |
| µδ [mas yr−1] | −102.681 ± 0.017 | 4 |
| RUWE | 1.057 | 4 |
| γ [km s−1 ] | −23.10 ± 0.16 | 4 |
| U [km s−1] | −23.959 ± 0.084 | 0 |
| V [km s−1] | −48.627 ± 0.099 | 0 |
| W [km s−1 ] | +9.523 ± 0.097 | 0 |
| Gal. population | Thin disk | 0 |
| Photometry | ||
| V [mag] | 10.068 | 5 |
| G [mag] | 9.4775 ± 0.0028 | 4 |
| GBP − GRP [mag] | 1.73 | 4 |
| J [mag] | 7.464 ± 0.023 | 6 |
| Ks [mag] | 6.656 ± 0.018 | 6 |
| Fundamental parameters | ||
| Teff [K] | 4135 ± 36 | 0 |
| log ɡ | 5.07 ± 0.27 | 0 |
| [Fe/H] [dex] | −0.01 ± 0.09 | 0 |
| L⋆ [L⊙] | 0.10098 ± 0.00012 | 0 |
| M⋆ [M⊙] | 0.629 ± 0.017 | 0 |
| R⋆ [R⊙] | 0.619 ± 0.011 | 0 |
| HZ rangec [au] | 0.25-0.65 | 0 |
| HZ range [d] | 59-241 | 0 |
| Activity | ||
| υ sini [km s−1] | <2d | 0 |
| Prot [d] | 37.4 ± 6.0 | 0 |
| pEW(Ca II IRT1) [Å] | +0.865 ± 0.006 | 0 |
| log R′HK | −4.896 ± 0.003 | 0 |
Notes. (a) DR3 contents can be accessed at: https://www.cosmos.esa.int/web/gaia/dr3 (b) The spectral classification of KOBE-1 is at the boundary between late K and early M type, without a definitive distinction in the literature (e.g. Reid et al. 1995; Gray et al. 2003). Our work classifies the host star as a K7 subtype. (c) Optimistic range as defined by Kopparapu et al. (2013). (d) Martínez-Arnáiz et al. (2010) determined a value of v sin i ≤ 3.7 km s−1 using FOCES, a spectrograph with a resolution lower than CARMENES.
References. (0) This work; (1) ESA (1997); (2) Gliese (1969); (3) Stassun et al. (2019); (4) Pourbaix et al. (2022); (5) Koen et al. (2010); (6) Cutri et al. (2003).
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