Table 2
Spectral parameters of the star.
| Parameter | Unit | TurboSpectrum+MARCS | Moog+MARCS | SED | TESS Input Catalog v8(f) |
|---|---|---|---|---|---|
| Teff | Κ | 3627±31 | 3711±47 | 3630±50 | 3575±157 |
| log(g) | 4.60±0.05 | 4.53±0.13 | 4.5±0.5 | 4.723±0.009 | |
| [M/H] | dex | 0.10±0.10 | 0.00±0.08 | 0.0±0.5 | |
| ν sin i | km s−1 | <2.5(a) | |||
| νmicro | km s−1 | fixed to 1.0 | 0.3±0.7 | ||
| Fbol | 10−10 erg s−1 cm−2 | 6.82±0.24(b) | |||
| Lbol | L⊙ | 0.0431±0.0015(c) | 0.039±0.009 | ||
| M* | Μ⊙ | 0.54±0.03(d) | 0.51±0.02 | ||
| R* | R⊙ | 0.53±0.02(e) | 0.52±0.02 |
Notes. The stellar parameters are derived from spectral template matching by the method explained in Cristofari et al. (2022b) with TurboSpectrum, and in de Almeida et al. (in prep.) with Moog, from the SED fitting explained in Stassun & Torres (2016) and Stassun et al. (2017, 2018), and from the TESS project stellar parameters (Stassun et al. 2018). See Sects. 3.1.1 and 3.1.2 for details. (a)At 3σ and fixing vmacro = 0 km s−1 (more details in Section 3.1.2). (b) From direct integration of SED. (c)Luminosity derived from the bolometric flux and the parallax. (d) Mass determined from the Mann et al. (2019) empirical relations. (e)Radius determined from the bolometric flux and the parallax. (f)From Stassun et al. (2019). See text for details.
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