Table 4
Properties of the stars HD 67458 and HD 88595.
| Parameters | Values | Source | |
|---|---|---|---|
| HD 67458 | HD 88595 | ||
| Target names | HIP 39710 | HIP 50013 | Simbad(a) |
| TIC 154234114 | TIC 5506063 | ||
| Gaia EDR3 5596797039059063680 | Gaia EDR3 5669349344592951936 | ||
| Spectral type | G0V | F7V | Simbad |
| Right Ascension (ep=J2000) | 08 07 00.522 | 10 12 37.96 | Simbad |
| Declination (ep=J2000) | −29 24 10.57 | −19 09 10.94 | Simbad |
| Gaia G-band magnitude | 6.64 | 6.34 | Gaia archive(b) |
| Distance [pc] | 25.68 | 42.01 | This work(c) (IRFM) |
| Effective Temperature (K) | 5833 ± 62 | 6205 ± 35 | This work (spectroscopy) |
| Metallicity [Fe/H] | −0.18 ± 0.04 | 0.17 ± 0.03 | This work (spectroscopy) |
| [Mg/H] | −0.14 ± 0.06 | 0.10 ± 0.07 | This work (spectroscopy) |
| [Si/H] | −0.20 ± 0.04 | 0.12 ± 0.05 | This work (spectroscopy) |
| [Ti/H] | −0.17 ± 0.06 | −0.01 ± 0.05 | This work (spectroscopy) |
| log ɡ [cgs] | 4.37 ± 0.10 | 3.99 ± 0.06 | This work (spectroscopy) |
| 4.390 ± 0.026 | 4.148 ± 0.017 | This work (from R*. and M*.) | |
| Radius (R⊙) | 1.021 ± 0.020 | 1.616 ± 0.017 | This work (IRFM) |
| Mass (M⊙) |  |
 |
This work (isochrones) |
| Age [Gyr] | 7.7 ± 2.1 | 2.8 ± 0.4 | This work (isochrones) |
| vmax [μHz] | 2756 ± 169 | 1534 ±85 | Eq. (2), This work (ESPRESSO) |
| Mean log R′HK | −4.99 ± 0.14 | −4.96 ± 0.15 | This work (spectroscopy) |
| Rotation period [days] | 10.57 ± 0.06 | 3.1151 ± 0.0003 | This work (TESS photometry) |
| υ sin i [km s−1] | 2.179 ± 0.2 | 7.24 ± 0.35 | HARPS(d), This work |
| Stellar inclination [degrees] | ~26 | ~16 | This work |
Notes. (a)SIMBAD astronomical database from the Centre de Données astronomiques de Strasbourg (http://simbad.u-strasbg.fr/simbad/). (b) Archive of the Gaia mission of the European Space Agency (https://gea.esac.esa.int/archive/). (c)Values are in agreement with the Gaia Early Data Release 3 (catalog http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=I/352 from Bailer-Jones et al. 2021). (d)HARPS data initially published in Soto & Jenkins (2018) and reanalyzed in this work.
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