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# Appendix A: Stellar parameters

We present in this Appendix the details of the determination of the stellar parameters for TOI-179 and its wide companions, CD-56 593 A and B, briefly summarized in Sect. 3.

## Appendix A.1: Spectroscopic analysis

We exploited the HARPS spectra described in Sect. 2.2 for the stellar characterization. A co-added spectrum was created, The composite spectrum has S/N per pixel at 6700 Å of 180.

Our aim was to derive the spectroscopic parameters and metallicity ([Fe/H]) via the equivalent width (EW) method and the standard iron line analysis. EWs were measured using ARES (Sousa et al. 2007), with frequent visual inspection and manual re-adjustment using the IRAF task splot (performing Gaussian fits). We adopted the linelist by D'Orazi et al. (2020), which includes 80 Fe I and 17 Fe II lines (see that paper for details on atomic parameters). We used the Castelli & Kurucz grid of model atmosphere, with new opacities and no overshooting (ODFNEW, Castelli & Kurucz 2003). Stellar parameters ($T_{eff}$, log g, microturbulence velocity $Vt$) and metallicity were derived in a semi-automated way using the MOOG (Sneden 1973) python wrapper qoyllur-quipu ($q^2$) code developed by I. Ramírez<fnref n="11" />. We first derived the parameters and metallicity for the HARPS-N solar spectrum obtained by Biazzo et al. (2022) and found $T_{eff}=5790\pm43$ K, $log g=4.44\pm0.10$ dex, $Vt=0.97\pm0.07$ km s⁻¹, and $log n(Fe I)=7.49\pm0.03$ dex. The internal uncertainties reported on atmospheric parameters come from errors on the slopes for $T_{eff}$ and $Vt$, whereas those on surface gravity come from errors on the ionization balance condition of iron, as also routinely done in our previous works (Biazzo et al. 2015; D'Orazi et al. 2020, and references therein).

We found $T_{eff}=5172\pm60$ K, $logg=4.54\pm0.09$ dex, $Vt=1.09\pm0.14$ kms⁻¹, and [Fe/H]=0.00±0.08 dex (total error). Previously, Mortier et al. (2013) reported $T_{eff}=5154$ K (from B-V color) and [Fe/H]=-0.01 dex (from their calibration of CCF parameters), while Jenkins et al. (2008) derived [Fe/H]=-0.01 dex (from their analysis of FEROS spectra; $T_{eff}$ not listed). A comparison with the photometric sequences by Pecaut & Mamajek (2013) <fnref n="12" /> yields a photometric $T_{eff}=5118\pm50$ K, assuming no reddening as the target is at only 38 pc from the Sun. Independent measurements then agree fairly well. In the following we adopt the mean of our spectroscopic and photometric determinations, $T_{eff}=5145$ K, with a conservative error of 50 K.

## Appendix A.2: Chemical abundances

We determined the elemental abundances for proton-capture, α, and iron-peak elements Na I, Mg I, Al I, Ca I, Ti I, Ti II, and Ni I by using the line list of D'Orazi et al. (2020) and the same code and model atmosphere described in Sect. A.1. As previously done for the [Fe/H] determination, we first analysed the solar spectrum and obtained the elemental abundances reported in Table A.1. For the Na I lines 6154/6160 Å we applied non-local thermodynamic equilibrium (NLTE) corrections from the INSPECT database (Lind et al. 2011). We calculated internal errors due to EW measurements (the first error

in Table A.1, which is the error on the mean from different lines) and the uncertainty related to atmospheric parameters. All the abundances exhibit a solar-scaled pattern, with only a marginal enhancement in calcium ([Ca/H]=0.07 dex) and titanium ([Ti/H]=0.07 from the average of neutral and singly-ionized atomic lines). This is probably related to blending effects of the lines and/or continuum displacements at lower temperatures.

<table><caption>Table A.1: Elemental abundances (with corresponding number of lines) as derived for the solar spectrum and TOI-179.</caption><thead><tr><th>Species</th><th>N-lines</th><th>Sun</th><th>TOI-179</th></tr></thead><tbody><tr><td>Na I<sub>NLTE</sub></td><td>2</td><td>6.21±0.01±0.01</td><td>6.21±0.01±0.02</td></tr><tr><td>Mg I</td><td>2</td><td>7.56±0.03±0.01</td><td>7.59±0.03±0.02</td></tr><tr><td>Al I</td><td>2</td><td>6.51±0.01±0.01</td><td>6.56±0.01±0.01</td></tr><tr><td>Si I</td><td>11</td><td>7.49±0.02±0.02</td><td>7.47±0.01±0.02</td></tr><tr><td>Ca I</td><td>9</td><td>6.32±0.04±0.01</td><td>6.39±0.03±0.01</td></tr><tr><td>Ti I</td><td>52</td><td>4.96±0.04±0.02</td><td>5.05±0.04±0.03</td></tr><tr><td>Ti II</td><td>25</td><td>4.97±0.05±0.02</td><td>5.03±0.06±0.04</td></tr><tr><td>Ni I</td><td>16</td><td>6.24±0.01±0.02</td><td>6.24±0.02±0.03</td></tr></tbody></table>

## Appendix A.3: Lithium

We also exploited the HARPS spectrum to measure the equivalent width (EW) of the Li 6708Å doublet, which results in a value of 39.3±4.5 mÅ. The Li EW of TOI-179 is between those of the Pleiades and Hyades of similar colors (Fig. A.1), close but slightly smaller than that of M34 members (Jones et al. 1997; Gondoin 2014), and close to the upper envelope of the members of Ursa Major moving group (Soderblom et al. 1993; Ammler-von Eiff & Guenther 2009).

We employed the stellar parameters derived in Section A.1 and performed spectral synthesis calculations in order to derive the Li abundance. We used the driver synth in MOOG (2019 version) and the line list around the Li doublet at 6708Å, as was done in our previous investigations. By adopting a FWHM of 0.06 Å for the instrumental profile and a limb darkening of 0.65, we determined $A(Li I)=1.55±0.08$ dex (see Fig. A.2).

<figure><img src="image_18.png" /><figcaption>Fig. A.1: Equivalent width for Li of TOI-179 (black star) compared to those of the members of the Pleiades (green circles), Hyades (purple squares), and Ursa Major (red squares).</figcaption></figure>

<footnote n="11">¹¹ The code and the tutorial are available at https://github.com/astroChasqui/q2.</footnote>

<footnote n="12">¹² Updated version available at https://www.pas.rochester.edu/~emamajek/EEM_dwarf_UBVIJHK_colors_Teff.txt, hereafter referred to as Mamajek tables</footnote>
# Appendix A: Stellar parameters

We present in this Appendix the details of the determination of the stellar parameters for TOI-179 and its wide companions, CD-56 593 A and B, briefly summarized in Sect. 3.

## Appendix A.1: Spectroscopic analysis

We exploited the HARPS spectra described in Sect. 2.2 for the stellar characterization. A co-added spectrum was created, The composite spectrum has S/N per pixel at 6700 Å of 180.

Our aim was to derive the spectroscopic parameters and metallicity ([Fe/H]) via the equivalent width (EW) method and the standard iron line analysis. EWs were measured using ARES (Sousa et al. 2007), with frequent visual inspection and manual re-adjustment using the IRAF task splot (performing Gaussian fits). We adopted the linelist by D'Orazi et al. (2020), which includes 80 Fe I and 17 Fe II lines (see that paper for details on atomic parameters). We used the Castelli & Kurucz grid of model atmosphere, with new opacities and no overshooting (ODFNEW, Castelli & Kurucz 2003). Stellar parameters ($T_{eff}$, log g, microturbulence velocity $Vt$) and metallicity were derived in a semi-automated way using the MOOG (Sneden 1973) python wrapper qoyllur-quipu ($q^2$) code developed by I. Ramírez<fnref n="11" />. We first derived the parameters and metallicity for the HARPS-N solar spectrum obtained by Biazzo et al. (2022) and found $T_{eff}=5790\pm43$ K, $log g=4.44\pm0.10$ dex, $Vt=0.97\pm0.07$ km s⁻¹, and $log n(Fe I)= 7.49\pm0.03$ dex. The internal uncertainties reported on atmospheric parameters come from errors on the slopes for $T_{eff}$ and $Vt$, whereas those on surface gravity come from errors on the ionization balance condition of iron, as also routinely done in our previous works (Biazzo et al. 2015; D'Orazi et al. 2020, and references therein).

We found $T_{eff}=5172\pm60$ K, $logg=4.54\pm0.09$ dex, $Vt=1.09\pm0.14$ kms⁻¹, and [Fe/H]=0.00±0.08 dex (total error). Previously, Mortier et al. (2013) reported $T_{eff}=5154$ K (from B-V color) and [Fe/H]=-0.01 dex (from their calibration of CCF parameters), while Jenkins et al. (2008) derived [Fe/H]=-0.01 dex (from their analysis of FEROS spectra; $T_{eff}$ not listed). A comparison with the photometric sequences by Pecaut & Mamajek (2013) <fnref n="12" /> yields a photometric $T_{eff}=5118\pm50$ K, assuming no reddening as the target is at only 38 pc from the Sun. Independent measurements then agree fairly well. In the following we adopt the mean of our spectroscopic and photometric determinations, $T_{eff}=5145$ K, with a conservative error of 50 K.

## Appendix A.2: Chemical abundances

We determined the elemental abundances for proton-capture, α, and iron-peak elements Na I, Mg I, Al I, Ca I, Ti I, Ti II, and Ni I by using the line list of D'Orazi et al. (2020) and the same code and model atmosphere described in Sect. A.1. As previously done for the [Fe/H] determination, we first analysed the solar spectrum and obtained the elemental abundances reported in Table A.1. For the Na I lines 6154/6160 Å we applied non-local thermodynamic equilibrium (NLTE) corrections from the INSPECT database (Lind et al. 2011). We calculated internal errors due to EW measurements (the first error

in Table A.1, which is the error on the mean from different lines) and the uncertainty related to atmospheric parameters. All the abundances exhibit a solar-scaled pattern, with only a marginal enhancement in calcium ([Ca/H]=0.07 dex) and titanium ([Ti/H]=0.07 from the average of neutral and singly-ionized atomic lines). This is probably related to blending effects of the lines and/or continuum displacements at lower temperatures.

<table><caption>Table A.1: Elemental abundances (with corresponding number of lines) as derived for the solar spectrum and TOI-179.</caption><thead><tr><th>Species</th><th>N-lines</th><th>Sun</th><th>TOI-179</th></tr></thead><tbody><tr><td>Na I<sub>NLTE</sub></td><td>2</td><td>6.21±0.01±0.01</td><td>6.21±0.01±0.02</td></tr><tr><td>Mg I</td><td>2</td><td>7.56±0.03±0.01</td><td>7.59±0.03±0.02</td></tr><tr><td>Al I</td><td>2</td><td>6.51±0.01±0.01</td><td>6.56±0.01±0.01</td></tr><tr><td>Si I</td><td>11</td><td>7.49±0.02±0.02</td><td>7.47±0.01±0.02</td></tr><tr><td>Ca I</td><td>9</td><td>6.32±0.04±0.01</td><td>6.39±0.03±0.01</td></tr><tr><td>Ti I</td><td>52</td><td>4.96±0.04±0.02</td><td>5.05±0.04±0.03</td></tr><tr><td>Ti II</td><td>25</td><td>4.97±0.05±0.02</td><td>5.03±0.06±0.04</td></tr><tr><td>Ni I</td><td>16</td><td>6.24±0.01±0.02</td><td>6.24±0.02±0.03</td></tr></tbody></table>

## Appendix A.3: Lithium

We also exploited the HARPS spectrum to measure the equivalent width (EW) of the Li 6708Å doublet, which results in a value of 39.3±4.5 mÅ. The Li EW of TOI-179 is between those of the Pleiades and Hyades of similar colors (Fig. A.1), close but slightly smaller than that of M34 members (Jones et al. 1997; Gondoin 2014), and close to the upper envelope of the members of Ursa Major moving group (Soderblom et al. 1993; Ammler-von Eiff & Guenther 2009).

We employed the stellar parameters derived in Section A.1 and performed spectral synthesis calculations in order to derive the Li abundance. We used the driver synth in MOOG (2019 version) and the line list around the Li doublet at 6708Å, as was done in our previous investigations. By adopting a FWHM of 0.06 Å for the instrumental profile and a limb darkening of 0.65, we determined $A(Li I)=1.55±0.08$ dex (see Fig. A.2).

<figure><img src="image_19.png" /><figcaption>Fig. A.1: Equivalent width for Li of TOI-179 (black star) compared to those of the members of the Pleiades (green circles), Hyades (purple squares), and Ursa Major (red squares).</figcaption></figure>

<footnote n="11">¹¹ The code and the tutorial are available at https://github.com/astroChasqui/q2.</footnote>

<footnote n="12">¹² Updated version available at https://www.pas.rochester.edu/~emamajek/EEM_dwarf_UBVIJHK_colors_Teff.txt, hereafter referred to as Mamajek tables</footnote>
<figure><img src="image_19.png" /><figcaption>Fig. A.2: Comparison between observed (black dots) and synthetic (green, red, and blue lines) spectra around the Li I line at 6708 Å.</figcaption></figure>

<figure><img src="image_20.png" /><figcaption>Fig. A.3: Time series of Ca II H&K instrumental S index, $H\alpha$, and bisector velocity span (BIS).</figcaption></figure>

## Appendix A.4: Projected rotational velocity

We derived the projected rotational velocity $v \sin i$ exploiting the HARPS spectra with two independent methods. From the spectral synthesis in the region of the Li doublet, we derived $v \sin i = 4.5 \pm 0.5$ km s$^{-1}$. From a preliminary calibration of the observed FWHM of the CCF into rotational velocity for HARPS spectra, we obtained $v \sin i = 4.50 \pm 0.41$ km s$^{-1}$. Determinations available in the literature are 4.3 km s$^{-1}$ (Jenkins et al. 2011) and 4.6 km s$^{-1}$ (Grandjean et al. 2021), in good agreement with our determinations.

From the CHANDRA observations described in Sect. 2.4, we obtained for TOI-179 a kT of 0.56 keV and an unabsorbed flux of $1.79 \times 10^{-13}$ erg s$^{-1}$ cm$^{-2}$ in the ROSAT band 0.1–2.4 keV which corresponds to a X-ray luminosity of $L_X \approx 3.23 \times 10^{28}$ erg s$^{-1}$ at a distance of 38.6 pc. The normalization constant of the best-fit model corresponds to an emission measure of $2.7 \times 10^{51}$ cm$^{-3}$. Coupled with the stellar luminosity from Table 2, this implies $R_X = \log(L_X/L_{bol}) = -4.65$, slightly above the median value of Hyades members of similar colors.

## Appendix A.5: Chromospheric and coronal activity

We measured the instrumental S index (Ca II H&K) and $H\alpha$ index using the tool ACTIN (v1.3.9; Gomes da Silva et al. 2018). We calculated the $H\alpha$ index adopting both the definitions labeled “Ha06” and “Ha16” in the line configuration file, denoting indices with 0.6 and 1.6 Å central bandwidths, respectively. The most relevant signal is a long-term modulation, likely ascribed to an activity cycle, which is nearly linear in $H\alpha$ (especially for the case of the Ha16 index), while a possible turnover is observed for the S index (Fig. A.3). This difference may be real, and linked to the different kinds of active regions to which each indicator is sensitive, but might also be due to the modification of the HARPS setup in 2015 (Lo Curto et al. 2015). A nearly linear upward trend is also seen in the RV time series (see Sect. 4.3). Dedicated tests were performed and presented in Sect. 5.1 supporting the Keplerian origin of the RV trend.

After removing the long-term trend, a significant periodicity at 8.64 d appears on the residuals of the S index time series, corresponding to the rotation period of the star, while no significant short-term periodicity is found for $H\alpha$.

As the ACTIN S index is not calibrated into the standard Mount Wilson scale (Baliunas et al. 1995), we also obtained calibrated $S_{MW}$ index using the procedure adopted in Desidera et al. (2015). The mean values result in $S_{MW}=0.607$ and, with B-V color from Table 2 and Noyes et al. (1984) transformation, in $\log R'_{HK}=-4.35$. The minimum and maximum values considering the prominent long-term activity cycle are $\log R'_{HK}=-4.43$ and -4.30, respectively. The sparse measurements by Gray et al. (2006), Jenkins et al. (2008), and Jenkins et al. (2011) are within this distribution. The activity level is intermediate between Hyades and Pleiades/AB Dor stars of similar colors.

## Appendix A.6: Photometric variability and rotation period

Three determinations of rotation period of TOI-179 are available in the literature. Oelkers et al. (2018) measured a period of 8.693 d from KELT photometric data, Howard et al. (2021) obtained $P=8.64 \pm 0.04$ d from their analysis of TESS and Evryscope data, and Canto Martins et al. (2020) derived $P=8.49 \pm 0.86$ d considering TESS data only (sectors 2–3). Our analysis of TESS light curves (four sectors considered independently) performed with the methods described in Messina et al. (2022) yields a photometric period of $8.84 \pm 0.29$ d (see Fig. A.4), in general agreement with the literature results. The analysis of the time series of HARPS RV and the corresponding activity indicators also provides additional estimates of rotation periods. The Gaussian process regression analysis of the RV time series described in Sect. 4.3 yields a period of $8.72 \pm 0.04$ d, while the S index periodogram analysis (Sect. A.5) indicates a period of $8.64$ d. Averaging the above determinations, we derive $P=8.73 \pm 0.07$ d.

The adopted rotation period is slightly longer than the rotation-color sequence of the 300 Myr Group X recently obtained by Messina et al. (2022). It is clearly distinct from the Pleiades sequence on the young side and from Hyades and Praesepe on the old side (Fig. A.5). From the Mamajek & Hillenbrand (2008) calibration, the resulting age is 390 Myr.

Finally, to further constrain the long-term activity variations we also checked the ASAS light curve (Pojmanski 1997), which covers about 9 yr between 2000 and 2009. A small downward trend of $0.003 \pm 0.0003$ mag yr$^{-1}$ is retrieved, without indications of large long-term photometric variations and significant periodicities due to an activity cycle.
<figure><img src="image_20.png" /><figcaption>Fig. A.2: Comparison between observed (black dots) and synthetic (green, red, and blue lines) spectra around the Li I line at 6708 Å.</figcaption></figure>

<figure><img src="image_21.png" /><figcaption>Fig. A.3: Time series of Ca II H&K instrumental S index, $H\alpha$, and bisector velocity span (BIS).</figcaption></figure>

## Appendix A.4: Projected rotational velocity

We derived the projected rotational velocity $v \sin i$ exploiting the HARPS spectra with two independent methods. From the spectral synthesis in the region of the Li doublet, we derived $v \sin i = 4.5 \pm 0.5$ km s$^{-1}$. From a preliminary calibration of the observed FWHM of the CCF into rotational velocity for HARPS spectra, we obtained $v \sin i = 4.50 \pm 0.41$ km s$^{-1}$. Determinations available in the literature are 4.3 km s$^{-1}$ (Jenkins et al. 2011) and 4.6 km s$^{-1}$ (Grandjean et al. 2021), in good agreement with our determinations.

From the CHANDRA observations described in Sect. 2.4, we obtained for TOI-179 a kT of 0.56 keV and an unabsorbed flux of $1.79 \times 10^{-13}$ erg s$^{-1}$ cm$^{-2}$ in the ROSAT band 0.1–2.4 keV which corresponds to a X-ray luminosity of $L_X \approx 3.23 \times 10^{28}$ erg s$^{-1}$ at a distance of 38.6 pc. The normalization constant of the best-fit model corresponds to an emission measure of $2.7 \times 10^{51}$ cm$^{-3}$. Coupled with the stellar luminosity from Table 2, this implies $R_X = \log(L_X/L_{bol}) = -4.65$, slightly above the median value of Hyades members of similar colors.

## Appendix A.5: Chromospheric and coronal activity

We measured the instrumental S index (Ca II H&K) and $H\alpha$ index using the tool ACTIN (v1.3.9; Gomes da Silva et al. 2018). We calculated the $H\alpha$ index adopting both the definitions labeled “Ha06” and “Ha16” in the line configuration file, denoting indices with 0.6 and 1.6 Å central bandwidths, respectively. The most relevant signal is a long-term modulation, likely ascribed to an activity cycle, which is nearly linear in $H\alpha$ (especially for the case of the Ha16 index), while a possible turnover is observed for the S index (Fig. A.3). This difference may be real, and linked to the different kinds of active regions to which each indicator is sensitive, but might also be due to the modification of the HARPS setup in 2015 (Lo Curto et al. 2015). A nearly linear upward trend is also seen in the RV time series (see Sect. 4.3). Dedicated tests were performed and presented in Sect. 5.1 supporting the Keplerian origin of the RV trend.

After removing the long-term trend, a significant periodicity at 8.64 d appears on the residuals of the S index time series, corresponding to the rotation period of the star, while no significant short-term periodicity is found for $H\alpha$.

As the ACTIN S index is not calibrated into the standard Mount Wilson scale (Baliunas et al. 1995), we also obtained calibrated $S_{MW}$ index using the procedure adopted in Desidera et al. (2015). The mean values result in $S_{MW}=0.607$ and, with B-V color from Table 2 and Noyes et al. (1984) transformation, in $\log R'_{HK}=-4.35$. The minimum and maximum values considering the prominent long-term activity cycle are $\log R'_{HK}=-4.43$ and -4.30, respectively. The sparse measurements by Gray et al. (2006), Jenkins et al. (2008), and Jenkins et al. (2011) are within this distribution. The activity level is intermediate between Hyades and Pleiades/AB Dor stars of similar colors.

## Appendix A.6: Photometric variability and rotation period

Three determinations of rotation period of TOI-179 are available in the literature. Oelkers et al. (2018) measured a period of 8.693 d from KELT photometric data, Howard et al. (2021) obtained $P=8.64 \pm 0.04$ d from their analysis of TESS and Evryscope data, and Canto Martins et al. (2020) derived $P=8.49 \pm 0.86$ d considering TESS data only (sectors 2–3). Our analysis of TESS light curves (four sectors considered independently) performed with the methods described in Messina et al. (2022) yields a photometric period of $8.84 \pm 0.29$ d (see Fig. A.4), in general agreement with the literature results. The analysis of the time series of HARPS RV and the corresponding activity indicators also provides additional estimates of rotation periods. The Gaussian process regression analysis of the RV time series described in Sect. 4.3 yields a period of $8.72 \pm 0.04$ d, while the S index periodogram analysis (Sect. A.5) indicates a period of $8.64$ d. Averaging the above determinations, we derive $P=8.73 \pm 0.07$ d.

The adopted rotation period is slightly longer than the rotation-color sequence of the 300 Myr Group X recently obtained by Messina et al. (2022). It is clearly distinct from the Pleiades sequence on the young side and from Hyades and Praesepe on the old side (Fig. A.5). From the Mamajek & Hillenbrand (2008) calibration, the resulting age is 390 Myr.

Finally, to further constrain the long-term activity variations we also checked the ASAS light curve (Pojmanski 1997), which covers about 9 yr between 2000 and 2009. A small downward trend of $0.003 \pm 0.0003$ mag yr$^{-1}$ is retrieved, without indications of large long-term photometric variations and significant periodicities due to an activity cycle.
<figure><img src="image_21.png" /></figure>

Fig. A.4: TESS light curves in Sectors 2, 3, 29, and 30 (from top to bottom) represented as normalized flux vs. time (left column), and corresponding GLS periodograms (right column) with indication of the measured periodicity (vertical red line) and its uncertainty (shaded region). Similar periodograms are obtained when using CLEAN (see Messina et al. 2022). The bottom plot shows the periodogram when all four sectors are combined into a unique time series.

## Appendix A.7: Kinematics and membership to groups

TOI-179 is not a member of known moving groups according to our analysis using the BANYAN Σ code by Gagné et al. (2018)<fnref n="13" />. Nevertheless, its kinematic parameters are well within the kinematic box of young stars (Montes et al. 2001). A full-sky search in the Gaia Collaboration et al. (2021) catalog for stars with similar space velocity components U,V,W with parallax larger than 15 mas yields only 13 stars with a difference in each of the space velocities of less than 2 km s⁻¹ with respect to TOI-179¹⁴. These stars are scattered over the whole sky; only some of them give an indication of being moderately active and young, but likely older than TOI-179; the majority give no indication of youth except for the kinematics, and one is clearly an older a red giant. We conclude that our target is not part of any group or association.

## Appendix A.8: Multiplicity: The wide companions CD-56 593 A and B

TOI-179 is a known triple system. CD-56 593 is a close pair (1.50" = 58 au projected separation at the date of the first observation listed in WDS (Mason et al. 2001), epoch 1911; 1.20" = 46 au projected separation in 1991 (Fabricius et al. 2002); ΔV = 0.76 mag) at 87.5" almost exactly south (PA = 182° degree) from TOI-179, corresponding to a physical projected separation of 3380 au. The close binary is not resolved in Gaia DR2, while there are separate entries in Gaia EDR3, with a projected separation of 0.90", a significant position angle shift (194 deg, compared to 185 deg in 1911), and a magnitude difference ΔG=0.55 mag. The differences in the proper motion between the components and with respect to TOI-179 are linked to orbital motion and they are small enough to firmly conclude on the physical association with TOI-179. The common proper motion was previously noted by Tokovinin & Lépine (2012) and Mugrauer & Michel (2020). No other comoving objects are found in Gaia EDR3 within 1 deg. The presence of close companions are discussed in Sect. 5.

The position of the components on the $M_G$ versus BP-RP color-magnitude diagram agrees within the errors with the standard main sequence in the Mamajek tables. The expected spectral types are K5 and K6/K7 (closer to K7) for CD-56 593A and CD-56 593B, respectively, and the stellar masses 0.70 and 0.66 M$_{\odot}$ for CD-56 593A and CD-56 593B, respectively. The system is thus formed by three K dwarfs.

CD-56 593 has a photometric rotation period (which most likely belongs to the brighter component CD-56 593A) of 11.20 d (Oelkers et al. 2018). We also analyzed the TESS data as was done for TOI-179 in Sect. A.6. We found a period similar to the literature value for the Sector 2 data, while a period close to a half of this value was derived for the Sector 30 data, most likely a harmonic of the true period linked to the distribution of starspots on stellar surface. The period in Sector 29 is instead uncertain as it appears dominated by the evolution of active regions or variable contributions from the two components. The data in Sector 3 are of poor quality. Combining the data, we adopt a period of 11.2±0.9 d. After deblending of the Ks magnitude following the Mamajek tables, this period is slightly slower than the sequence of the 300 Myr old Group X, as found above for TOI-179, independently of the component to which the observed periodicity belongs to (Fig. A.5).

CD-56 583 is also detected in the CHANDRA images presented in Sect. 2.4, with spatially unresolved emission between the two components. We obtained a temperature of 0.67 keV and an unabsorbed flux of $1.13 \times 10^{-13}$ erg s⁻¹ cm⁻² in the ROSAT band, corresponding to a system X-ray luminosity of $2.03 \times 10^{28}$ erg/s. We also obtained a value of emission measure for each component equal to ~8 × 10⁵⁰ cm⁻³. An estimated value of the X-ray luminosities of the individual components, assuming they have the same $R_X$ ratio ($R_X$=-4.74, from the individual luminosities of 0.181 and 0.112 $L_{\odot}$, for CD-56 593A and CD-56 593B, respectively, derived as in Sect. A.10), is $1.25 \times 10^{28}$ erg/s and $0.78 \times 10^{28}$ erg/s for CD-56 593A and CD-56 593B, respectively. These values are similar to those of Hyades members of similar spectral type.

## Appendix A.9: Age

The age indicators of TOI-179 consistently support an age older than the Pleiades and younger than the Hyades. A comparison with the 300 Myr old Group X moving group indicates a slightly older age. Isochrone fitting supports an age close to the main sequence, consistently with the indirect age indicators, both for TOI-179 and for CD-56 593 A and B (within the large color uncertainties for these latter objects). Considering these results, we rely on indirect indicators, of which the most sensitive (given the age and spectral type of the object) are the lithium and rotation period. We adopt an age of 400 Myr with limits between 300 to 500 Myr. The results of the wide binary companion CD-56 593 (CMD position, rotation period, and X-ray emission) are also consistent with this age estimate.

## Appendix A.10: Mass, radius, and system orientation

We exploited the PARAM web interface (da Silva et al. 2006)<fnref n="15" /> to infer the stellar mass. As in Desidera et al. (2015), we restricted the values of stellar ages to those allowed by indirect methods. This shifts the stellar mass upward by about 0.03 M$_{\odot}$. The final adopted mass is 0.863±0.020 M$_{\odot}$.

<footnote n="13">¹³ http://www.exoplanetes.umontreal.ca/banyan/banyansigma.php</footnote>

<footnote n="14">¹⁴ The wide companion CD-56 593 (see Sect. A.8) is not included in this output because it lacks radial velocity determinations</footnote>

<footnote n="15">¹⁵ http://stev.oapd.inaf.it/cgi-bin/param_1.3</footnote>
<figure><img src="image_22.png" /></figure>

Fig. A.4: TESS light curves in Sectors 2, 3, 29, and 30 (from top to bottom) represented as normalized flux vs. time (left column), and corresponding GLS periodograms (right column) with indication of the measured periodicity (vertical red line) and its uncertainty (shaded region). Similar periodograms are obtained when using CLEAN (see Messina et al. 2022). The bottom plot shows the periodogram when all four sectors are combined into a unique time series.

## Appendix A.7: Kinematics and membership to groups

TOI-179 is not a member of known moving groups according to our analysis using the BANYAN Σ code by Gagné et al. (2018)<fnref n="13" />. Nevertheless, its kinematic parameters are well within the kinematic box of young stars (Montes et al. 2001). A full-sky search in the Gaia Collaboration et al. (2021) catalog for stars with similar space velocity components U,V,W with parallax larger than 15 mas yields only 13 stars with a difference in each of the space velocities of less than 2 km s⁻¹ with respect to TOI-179¹⁴. These stars are scattered over the whole sky; only some of them give an indication of being moderately active and young, but likely older than TOI-179; the majority give no indication of youth except for the kinematics, and one is clearly an older a red giant. We conclude that our target is not part of any group or association.

## Appendix A.8: Multiplicity: The wide companions CD-56 593 A and B

TOI-179 is a known triple system. CD-56 593 is a close pair (1.50" = 58 au projected separation at the date of the first observation listed in WDS (Mason et al. 2001), epoch 1911; 1.20" = 46 au projected separation in 1991 (Fabricius et al. 2002); ΔV = 0.76 mag) at 87.5" almost exactly south (PA = 182° degree) from TOI-179, corresponding to a physical projected separation of 3380 au. The close binary is not resolved in Gaia DR2, while there are separate entries in Gaia EDR3, with a projected separation of 0.90", a significant position angle shift (194 deg, compared to 185 deg in 1911), and a magnitude difference ΔG=0.55 mag. The differences in the proper motion between the components and with respect to TOI-179 are linked to orbital motion and they are small enough to firmly conclude on the physical association with TOI-179. The common proper motion was previously noted by Tokovinin & Lépine (2012) and Mugrauer & Michel (2020). No other comoving objects are found in Gaia EDR3 within 1 deg. The presence of close companions are discussed in Sect. 5.

The position of the components on the $M_G$ versus BP-RP color-magnitude diagram agrees within the errors with the standard main sequence in the Mamajek tables. The expected spectral types are K5 and K6/K7 (closer to K7) for CD-56 593A and CD-56 593B, respectively, and the stellar masses 0.70 and 0.66 M$_{\odot}$ for CD-56 593A and CD-56 593B, respectively. The system is thus formed by three K dwarfs.

CD-56 593 has a photometric rotation period (which most likely belongs to the brighter component CD-56 593A) of 11.20 d (Oelkers et al. 2018). We also analyzed the TESS data as was done for TOI-179 in Sect. A.6. We found a period similar to the literature value for the Sector 2 data, while a period close to a half of this value was derived for the Sector 30 data, most likely a harmonic of the true period linked to the distribution of starspots on stellar surface. The period in Sector 29 is instead uncertain as it appears dominated by the evolution of active regions or variable contributions from the two components. The data in Sector 3 are of poor quality. Combining the data, we adopt a period of 11.2±0.9 d. After deblending of the Ks magnitude following the Mamajek tables, this period is slightly slower than the sequence of the 300 Myr old Group X, as found above for TOI-179, independently of the component to which the observed periodicity belongs to (Fig. A.5).

CD-56 583 is also detected in the CHANDRA images presented in Sect. 2.4, with spatially unresolved emission between the two components. We obtained a temperature of 0.67 keV and an unabsorbed flux of $1.13 \times 10^{-13}$ erg s⁻¹ cm⁻² in the ROSAT band, corresponding to a system X-ray luminosity of $2.03 \times 10^{28}$ erg/s. We also obtained a value of emission measure for each component equal to ~8 × 10⁵⁰ cm⁻³. An estimated value of the X-ray luminosities of the individual components, assuming they have the same $R_X$ ratio ($R_X$=-4.74, from the individual luminosities of 0.181 and 0.112 $L_{\odot}$, for CD-56 593A and CD-56 593B, respectively, derived as in Sect. A.10), is $1.25 \times 10^{28}$ erg/s and $0.78 \times 10^{28}$ erg/s for CD-56 593A and CD-56 593B, respectively. These values are similar to those of Hyades members of similar spectral type.

## Appendix A.9: Age

The age indicators of TOI-179 consistently support an age older than the Pleiades and younger than the Hyades. A comparison with the 300 Myr old Group X moving group indicates a slightly older age. Isochrone fitting supports an age close to the main sequence, consistently with the indirect age indicators, both for TOI-179 and for CD-56 593 A and B (within the large color uncertainties for these latter objects). Considering these results, we rely on indirect indicators, of which the most sensitive (given the age and spectral type of the object) are the lithium and rotation period. We adopt an age of 400 Myr with limits between 300 to 500 Myr. The results of the wide binary companion CD-56 593 (CMD position, rotation period, and X-ray emission) are also consistent with this age estimate.

## Appendix A.10: Mass, radius, and system orientation

We exploited the PARAM web interface (da Silva et al. 2006)<fnref n="15" /> to infer the stellar mass. As in Desidera et al. (2015), we restricted the values of stellar ages to those allowed by indirect methods. This shifts the stellar mass upward by about 0.03 M$_{\odot}$. The final adopted mass is 0.863±0.020 M$_{\odot}$.

<footnote n="13">¹³ http://www.exoplanetes.umontreal.ca/banyan/banyansigma.php</footnote>

<footnote n="14">¹⁴ The wide companion CD-56 593 (see Sect. A.8) is not included in this output because it lacks radial velocity determinations</footnote>

<footnote n="15">¹⁵ http://stev.oapd.inaf.it/cgi-bin/param_1.3</footnote>
<figure><img src="image_22.png" /></figure>

Fig. A.5: Rotation period of TOI-179 and CD-56 593A and B vs. (G-K)₀ color (green, cyan, and purple filled circles, respectively), compared to the members of the Pleiades and Praesepe open clusters (Rebull et al. 2016, 2017, plotted as blue diamonds and red squares, respectively) and Group X moving group (Messina et al. 2022, plotted as black circles). Only one photometric period is measured for CD-56 593, spatially unresolved in TESS images, and we are unable to determine to which component it belongs. The data are plotted in the figure for the colors of both components.

The stellar radius was derived through the Stefan–Boltzmann law, as was done in Carleo et al. (2021), using $T_{\text{eff}}$ from Sect. A.1, V magnitude from Table 2, and bolometric correction from the Mamajek tables. The adopted radius is 0.767±0.024 R☉, slightly smaller but in agreement to better than $1\sigma$ with the results listed in the Gaia DR2, PIC, and TIC catalogs (Montalto et al. 2021; Stassun et al. 2019), and the EXOFOP database<fnref n="16" />.

Coupling our adopted radius with the rotation period and projected rotational velocity from Sect. A.4 yields a stellar inclination of 90$^{+0}_{-30}$ deg, with the expected equatorial velocity (4.44±0.15 km s$^{-1}$) nearly identical to the observed $v \sin i$ (4.5±0.5 km s$^{-1}$). Therefore, the star appears to be seen close to edge-on. Alignment with the orbit of the transiting planets ($i_b$=87.5 deg, see Table 3) is then likely, although a moderate misalignment is possible within the error bars.

<footnote n="16">¹⁶ https://exofop.ipac.caltech.edu/tess/target.php?id=207141131</footnote>
<figure><img src="image_23.png" /></figure>

Fig. A.5: Rotation period of TOI-179 and CD-56 593A and B vs. (G-K)₀ color (green, cyan, and purple filled circles, respectively), compared to the members of the Pleiades and Praesepe open clusters (Rebull et al. 2016, 2017, plotted as blue diamonds and red squares, respectively) and Group X moving group (Messina et al. 2022, plotted as black circles). Only one photometric period is measured for CD-56 593, spatially unresolved in TESS images, and we are unable to determine to which component it belongs. The data are plotted in the figure for the colors of both components.

The stellar radius was derived through the Stefan–Boltzmann law, as was done in Carleo et al. (2021), using $T_{\text{eff}}$ from Sect. A.1, V magnitude from Table 2, and bolometric correction from the Mamajek tables. The adopted radius is 0.767±0.024 R☉, slightly smaller but in agreement to better than $1\sigma$ with the results listed in the Gaia DR2, PIC, and TIC catalogs (Montalto et al. 2021; Stassun et al. 2019), and the EXOFOP database<fnref n="16" />.

Coupling our adopted radius with the rotation period and projected rotational velocity from Sect. A.4 yields a stellar inclination of 90$^{+0}_{-30}$ deg, with the expected equatorial velocity (4.44±0.15 km s$^{-1}$) nearly identical to the observed $v \sin i$ (4.5±0.5 km s$^{-1}$). Therefore, the star appears to be seen close to edge-on. Alignment with the orbit of the transiting planets ($i_b$=87.5 deg, see Table 3) is then likely, although a moderate misalignment is possible within the error bars.

<footnote n="16">¹⁶ https://exofop.ipac.caltech.edu/tess/target.php?id=207141131</footnote>
Appendix B: Radial velocity and activity indicators time series

<table><caption>Table B.1: Radial velocities from TOI-179 HARPS spectra with uncertainties obtained from the TERRA pipeline. The corresponding measure of the bisector span is provided by the HARPS DRS. The Hα and the S-index with corresponding uncertainties are obtained with ACTIN.</caption><tr><td>6980.69590864</td><td>2.0808</td><td>0.9411</td><td>0.005250</td><td>0.2566</td><td>0.0004</td><td>0.3663</td><td>0.0021</td></tr><tr><td>6980.70195011</td><td>0.0000</td><td>0.8142</td><td>0.005890</td><td>0.2550</td><td>0.0004</td><td>0.3691</td><td>0.0028</td></tr><tr><td>6982.67878363</td><td>3.2470</td><td>1.1515</td><td>0.008210</td><td>0.2563</td><td>0.0005</td><td>0.3581</td><td>0.0027</td></tr><tr><td>6982.68488297</td><td>4.1855</td><td>1.2608</td><td>0.010610</td><td>0.2590</td><td>0.0006</td><td>0.3653</td><td>0.0025</td></tr><tr><td>6987.63091820</td><td>-29.3223</td><td>1.3290</td><td>0.055070</td><td>0.2593</td><td>0.0006</td><td>0.3553</td><td>0.0031</td></tr><tr><td>6987.63707540</td><td>-30.5069</td><td>1.4453</td><td>0.052730</td><td>0.2596</td><td>0.0006</td><td>0.3584</td><td>0.0021</td></tr><tr><td>6988.69275587</td><td>-32.0267</td><td>0.8648</td><td>0.044450</td><td>0.2581</td><td>0.0004</td><td>0.3511</td><td>0.0029</td></tr><tr><td>7223.88142723</td><td>-43.2483</td><td>2.0742</td><td>0.017150</td><td>0.2600</td><td>0.0007</td><td>0.3734</td><td>0.0021</td></tr><tr><td>7223.89251559</td><td>-38.0497</td><td>2.2566</td><td>0.019390</td><td>0.2604</td><td>0.0007</td><td>0.3426</td><td>0.0025</td></tr><tr><td>7224.88157860</td><td>-71.0729</td><td>1.7280</td><td>0.058330</td><td>0.2564</td><td>0.0006</td><td>0.3383</td><td>0.0026</td></tr><tr><td>7224.88963445</td><td>-69.1581</td><td>1.4157</td><td>0.056530</td><td>0.2561</td><td>0.0006</td><td>0.3367</td><td>0.0021</td></tr><tr><td>7333.76625907</td><td>-78.6104</td><td>0.9334</td><td>0.054490</td><td>0.2611</td><td>0.0003</td><td>0.3413</td><td>0.0019</td></tr><tr><td>7333.77693008</td><td>-78.3213</td><td>1.0476</td><td>0.060910</td><td>0.2601</td><td>0.0003</td><td>0.3473</td><td>0.0013</td></tr><tr><td>7342.74185760</td><td>-98.4356</td><td>1.1666</td><td>0.068750</td><td>0.2623</td><td>0.0003</td><td>0.3497</td><td>0.0014</td></tr><tr><td>7342.75252857</td><td>-96.7108</td><td>1.1087</td><td>0.067700</td><td>0.2625</td><td>0.0003</td><td>0.3411</td><td>0.0014</td></tr><tr><td>7344.69134515</td><td>-27.4767</td><td>1.0305</td><td>0.012730</td><td>0.2550</td><td>0.0003</td><td>0.3412</td><td>0.0013</td></tr><tr><td>7344.70191194</td><td>-28.9744</td><td>1.2010</td><td>0.011800</td><td>0.2559</td><td>0.0003</td><td>0.3364</td><td>0.0014</td></tr><tr><td>7600.82445252</td><td>-15.0062</td><td>2.7856</td><td>0.021910</td><td>0.2596</td><td>0.0008</td><td>0.3348</td><td>0.0014</td></tr><tr><td>7600.83648994</td><td>-17.2872</td><td>4.7693</td><td>0.009610</td><td>0.2605</td><td>0.0013</td><td>0.3269</td><td>0.0032</td></tr><tr><td>7713.80082617</td><td>-26.4906</td><td>1.5446</td><td>0.031270</td><td>0.2572</td><td>0.0004</td><td>0.3120</td><td>0.0046</td></tr><tr><td>7713.81152026</td><td>-25.8336</td><td>1.1222</td><td>0.035130</td><td>0.2573</td><td>0.0004</td><td>0.3580</td><td>0.0020</td></tr><tr><td>7770.61269041</td><td>0.4020</td><td>1.1772</td><td>0.021300</td><td>0.2674</td><td>0.0003</td><td>0.3512</td><td>0.0019</td></tr><tr><td>7770.62324557</td><td>2.3310</td><td>1.3228</td><td>0.020580</td><td>0.2658</td><td>0.0003</td><td>0.3763</td><td>0.0016</td></tr><tr><td>8007.71941096</td><td>-35.0594</td><td>1.9859</td><td>0.027950</td><td>0.2605</td><td>0.0007</td><td>0.3803</td><td>0.0018</td></tr><tr><td>8007.73070737</td><td>-37.9881</td><td>2.4466</td><td>0.023290</td><td>0.2614</td><td>0.0008</td><td>0.3356</td><td>0.0029</td></tr><tr><td>8035.62399563</td><td>-12.9255</td><td>1.1087</td><td>0.022640</td><td>0.2575</td><td>0.0004</td><td>0.3148</td><td>0.0034</td></tr><tr><td>8035.63478257</td><td>-13.3406</td><td>0.9869</td><td>0.019700</td><td>0.2580</td><td>0.0004</td><td>0.3460</td><td>0.0016</td></tr><tr><td>8039.62904707</td><td>-13.0419</td><td>1.1157</td><td>0.041150</td><td>0.2612</td><td>0.0004</td><td>0.3490</td><td>0.0015</td></tr><tr><td>8039.63992657</td><td>-12.7141</td><td>1.1839</td><td>0.042290</td><td>0.2615</td><td>0.0004</td><td>0.3660</td><td>0.0016</td></tr><tr><td>8417.56050911</td><td>15.8051</td><td>1.6301</td><td>0.039980</td><td>0.2675</td><td>0.0006</td><td>0.3637</td><td>0.0016</td></tr><tr><td>8417.76713698</td><td>1.5168</td><td>1.6723</td><td>0.030110</td><td>0.2685</td><td>0.0006</td><td>0.3968</td><td>0.0014</td></tr><tr><td>8418.55583647</td><td>-36.2440</td><td>1.3023</td><td>0.061410</td><td>0.2694</td><td>0.0005</td><td>0.3701</td><td>0.0020</td></tr><tr><td>8418.72027757</td><td>-40.3748</td><td>1.4555</td><td>0.074110</td><td>0.2648</td><td>0.0004</td><td>0.3801</td><td>0.0019</td></tr><tr><td>8419.68677382</td><td>-18.8122</td><td>1.2185</td><td>0.045670</td><td>0.2608</td><td>0.0004</td><td>0.3749</td><td>0.0017</td></tr><tr><td>8422.83131156</td><td>30.2399</td><td>2.3066</td><td>-0.020340</td><td>0.2626</td><td>0.0008</td><td>0.3815</td><td>0.0017</td></tr><tr><td>8423.74520254</td><td>-8.5072</td><td>1.4759</td><td>0.056360</td><td>0.2612</td><td>0.0005</td><td>0.3821</td><td>0.0016</td></tr><tr><td>8429.76226288</td><td>-12.5505</td><td>1.5425</td><td>0.048860</td><td>0.2593</td><td>0.0005</td><td>0.3872</td><td>0.0016</td></tr><tr><td>8430.74908821</td><td>2.3853</td><td>1.7303</td><td>0.026080</td><td>0.2664</td><td>0.0004</td><td>0.3682</td><td>0.0021</td></tr><tr><td>8431.67791694</td><td>26.4825</td><td>1.4431</td><td>-0.000970</td><td>0.2622</td><td>0.0004</td><td>0.3774</td><td>0.0013</td></tr><tr><td>8432.68523840</td><td>-24.2928</td><td>1.2659</td><td>0.081430</td><td>0.2608</td><td>0.0004</td><td>0.3943</td><td>0.0016</td></tr><tr><td>8432.71563107</td><td>-24.8233</td><td>1.3730</td><td>0.079500</td><td>0.2609</td><td>0.0005</td><td>0.3784</td><td>0.0020</td></tr><tr><td>8464.72530016</td><td>-9.8082</td><td>1.6310</td><td>-</td><td>0.2633</td><td>0.0006</td><td>0.3786</td><td>0.0013</td></tr><tr><td>8464.73352901</td><td>-6.8396</td><td>1.7945</td><td>-</td><td>0.2618</td><td>0.0006</td><td>0.3736</td><td>0.0017</td></tr><tr><td>8465.69725272</td><td>35.3156</td><td>1.5869</td><td>-</td><td>0.2711</td><td>0.0004</td><td>0.3797</td><td>0.0016</td></tr><tr><td>8465.70501861</td><td>33.8672</td><td>1.4372</td><td>-</td><td>0.2705</td><td>0.0004</td><td>0.3830</td><td>0.0016</td></tr><tr><td>8466.68945895</td><td>-26.6290</td><td>1.3620</td><td>-</td><td>0.2670</td><td>0.0005</td><td>0.3944</td><td>0.0018</td></tr><tr><td>8466.69655358</td><td>-26.1766</td><td>1.6262</td><td>-</td><td>0.2655</td><td>0.0005</td><td>0.3850</td><td>0.0021</td></tr><tr><td>8481.60390690</td><td>-0.1308</td><td>1.4002</td><td>-</td><td>0.2654</td><td>0.0005</td><td>0.3833</td><td>0.0018</td></tr><tr><td>8483.60647679</td><td>7.4831</td><td>1.1414</td><td>-</td><td>0.2719</td><td>0.0004</td><td>0.3808</td><td>0.0016</td></tr><tr><td>8509.53123346</td><td>-34.2170</td><td>1.6320</td><td>0.053220</td><td>0.2649</td><td>0.0005</td><td>0.3907</td><td>0.0016</td></tr><tr><td>8509.57920635</td><td>-34.3604</td><td>2.0194</td><td>0.064890</td><td>0.2689</td><td>0.0006</td><td>0.3865</td><td>0.0015</td></tr><tr><td>8509.59794413</td><td>-39.5850</td><td>1.8169</td><td>0.051320</td><td>0.2676</td><td>0.0006</td><td>0.3859</td><td>0.0023</td></tr><tr><td>8510.55122193</td><td>-42.5098</td><td>1.9474</td><td>0.057400</td><td>0.2596</td><td>0.0007</td><td>0.3943</td><td>0.0016</td></tr><tr><td>8510.58082740</td><td>-37.6804</td><td>2.6694</td><td>0.052610</td><td>0.2611</td><td>0.0007</td><td>0.3990</td><td>0.0014</td></tr><tr><td>8511.54866504</td><td>35.0932</td><td>1.5730</td><td>-0.008900</td><td>0.2636</td><td>0.0005</td><td>0.3919</td><td>0.0014</td></tr><tr><td>8511.60528350</td><td>38.0889</td><td>1.6384</td><td>-0.014010</td><td>0.2647</td><td>0.0006</td><td>0.3790</td><td>0.0017</td></tr><tr><td>8512.55084217</td><td>15.5591</td><td>1.4106</td><td>0.026710</td><td>0.2649</td><td>0.0004</td><td>0.3775</td><td>0.0017</td></tr></table>
Appendix B: Radial velocity and activity indicators time series

<table><caption>Table B.1: Radial velocities from TOI-179 HARPS spectra with uncertainties obtained from the TERRA pipeline. The corresponding measure of the bisector span is provided by the HARPS DRS. The $H\alpha$ and the S-index with corresponding uncertainties are obtained with ACTIN.</caption><tr><td>6980.69590864</td><td>2.0808</td><td>0.9411</td><td>0.005250</td><td>0.2566</td><td>0.0004</td><td>0.3663</td><td>0.0021</td></tr><tr><td>6980.70195011</td><td>0.0000</td><td>0.8142</td><td>0.005890</td><td>0.2550</td><td>0.0004</td><td>0.3691</td><td>0.0028</td></tr><tr><td>6982.67878363</td><td>3.2470</td><td>1.1515</td><td>0.008210</td><td>0.2563</td><td>0.0005</td><td>0.3581</td><td>0.0027</td></tr><tr><td>6982.68488297</td><td>4.1855</td><td>1.2608</td><td>0.010610</td><td>0.2590</td><td>0.0006</td><td>0.3653</td><td>0.0025</td></tr><tr><td>6987.63091820</td><td>-29.3223</td><td>1.3290</td><td>0.055070</td><td>0.2593</td><td>0.0006</td><td>0.3553</td><td>0.0031</td></tr><tr><td>6987.63707540</td><td>-30.5069</td><td>1.4453</td><td>0.052730</td><td>0.2596</td><td>0.0006</td><td>0.3584</td><td>0.0021</td></tr><tr><td>6988.69275587</td><td>-32.0267</td><td>0.8648</td><td>0.044450</td><td>0.2581</td><td>0.0004</td><td>0.3511</td><td>0.0029</td></tr><tr><td>7223.88142723</td><td>-43.2483</td><td>2.0742</td><td>0.017150</td><td>0.2600</td><td>0.0007</td><td>0.3734</td><td>0.0021</td></tr><tr><td>7223.89251559</td><td>-38.0497</td><td>2.2566</td><td>0.019390</td><td>0.2604</td><td>0.0007</td><td>0.3426</td><td>0.0025</td></tr><tr><td>7224.88157860</td><td>-71.0729</td><td>1.7280</td><td>0.058330</td><td>0.2564</td><td>0.0006</td><td>0.3383</td><td>0.0026</td></tr><tr><td>7224.88963445</td><td>-69.1581</td><td>1.4157</td><td>0.056530</td><td>0.2561</td><td>0.0006</td><td>0.3367</td><td>0.0021</td></tr><tr><td>7333.76625907</td><td>-78.6104</td><td>0.9334</td><td>0.054490</td><td>0.2611</td><td>0.0003</td><td>0.3413</td><td>0.0019</td></tr><tr><td>7333.77693008</td><td>-78.3213</td><td>1.0476</td><td>0.060910</td><td>0.2601</td><td>0.0003</td><td>0.3473</td><td>0.0013</td></tr><tr><td>7342.74185760</td><td>-98.4356</td><td>1.1666</td><td>0.068750</td><td>0.2623</td><td>0.0003</td><td>0.3497</td><td>0.0014</td></tr><tr><td>7342.75252857</td><td>-96.7108</td><td>1.1087</td><td>0.067700</td><td>0.2625</td><td>0.0003</td><td>0.3411</td><td>0.0014</td></tr><tr><td>7344.69134515</td><td>-27.4767</td><td>1.0305</td><td>0.012730</td><td>0.2550</td><td>0.0003</td><td>0.3412</td><td>0.0013</td></tr><tr><td>7344.70191194</td><td>-28.9744</td><td>1.2010</td><td>0.011800</td><td>0.2559</td><td>0.0003</td><td>0.3364</td><td>0.0014</td></tr><tr><td>7600.82445252</td><td>-15.0062</td><td>2.7856</td><td>0.021910</td><td>0.2596</td><td>0.0008</td><td>0.3348</td><td>0.0014</td></tr><tr><td>7600.83648994</td><td>-17.2872</td><td>4.7693</td><td>0.009610</td><td>0.2605</td><td>0.0013</td><td>0.3269</td><td>0.0032</td></tr><tr><td>7713.80082617</td><td>-26.4906</td><td>1.5446</td><td>0.031270</td><td>0.2572</td><td>0.0004</td><td>0.3120</td><td>0.0046</td></tr><tr><td>7713.81152026</td><td>-25.8336</td><td>1.1222</td><td>0.035130</td><td>0.2573</td><td>0.0004</td><td>0.3580</td><td>0.0020</td></tr><tr><td>7770.61269041</td><td>0.4020</td><td>1.1772</td><td>0.021300</td><td>0.2674</td><td>0.0003</td><td>0.3512</td><td>0.0019</td></tr><tr><td>7770.62324557</td><td>2.3310</td><td>1.3228</td><td>0.020580</td><td>0.2658</td><td>0.0003</td><td>0.3763</td><td>0.0016</td></tr><tr><td>8007.71941096</td><td>-35.0594</td><td>1.9859</td><td>0.027950</td><td>0.2605</td><td>0.0007</td><td>0.3803</td><td>0.0018</td></tr><tr><td>8007.73070737</td><td>-37.9881</td><td>2.4466</td><td>0.023290</td><td>0.2614</td><td>0.0008</td><td>0.3356</td><td>0.0029</td></tr><tr><td>8035.62399563</td><td>-12.9255</td><td>1.1087</td><td>0.022640</td><td>0.2575</td><td>0.0004</td><td>0.3148</td><td>0.0034</td></tr><tr><td>8035.63478257</td><td>-13.3406</td><td>0.9869</td><td>0.019700</td><td>0.2580</td><td>0.0004</td><td>0.3460</td><td>0.0016</td></tr><tr><td>8039.62904707</td><td>-13.0419</td><td>1.1157</td><td>0.041150</td><td>0.2612</td><td>0.0004</td><td>0.3490</td><td>0.0015</td></tr><tr><td>8039.63992657</td><td>-12.7141</td><td>1.1839</td><td>0.042290</td><td>0.2615</td><td>0.0004</td><td>0.3660</td><td>0.0016</td></tr><tr><td>8417.56050911</td><td>15.8051</td><td>1.6301</td><td>0.039980</td><td>0.2675</td><td>0.0006</td><td>0.3637</td><td>0.0016</td></tr><tr><td>8417.76713698</td><td>1.5168</td><td>1.6723</td><td>0.030110</td><td>0.2685</td><td>0.0006</td><td>0.3968</td><td>0.0014</td></tr><tr><td>8418.55583647</td><td>-36.2440</td><td>1.3023</td><td>0.061410</td><td>0.2694</td><td>0.0005</td><td>0.3701</td><td>0.0020</td></tr><tr><td>8418.72027757</td><td>-40.3748</td><td>1.4555</td><td>0.074110</td><td>0.2648</td><td>0.0004</td><td>0.3801</td><td>0.0019</td></tr><tr><td>8419.68677382</td><td>-18.8122</td><td>1.2185</td><td>0.045670</td><td>0.2608</td><td>0.0004</td><td>0.3749</td><td>0.0017</td></tr><tr><td>8422.83131156</td><td>30.2399</td><td>2.3066</td><td>-0.020340</td><td>0.2626</td><td>0.0008</td><td>0.3815</td><td>0.0017</td></tr><tr><td>8423.74520254</td><td>-8.5072</td><td>1.4759</td><td>0.056360</td><td>0.2612</td><td>0.0005</td><td>0.3821</td><td>0.0016</td></tr><tr><td>8429.76226288</td><td>-12.5505</td><td>1.5425</td><td>0.048860</td><td>0.2593</td><td>0.0005</td><td>0.3872</td><td>0.0016</td></tr><tr><td>8430.74908821</td><td>2.3853</td><td>1.7303</td><td>0.026080</td><td>0.2664</td><td>0.0004</td><td>0.3682</td><td>0.0021</td></tr><tr><td>8431.67791694</td><td>26.4825</td><td>1.4431</td><td>-0.000970</td><td>0.2622</td><td>0.0004</td><td>0.3774</td><td>0.0013</td></tr><tr><td>8432.68523840</td><td>-24.2928</td><td>1.2659</td><td>0.081430</td><td>0.2608</td><td>0.0004</td><td>0.3943</td><td>0.0016</td></tr><tr><td>8432.71563107</td><td>-24.8233</td><td>1.3730</td><td>0.079500</td><td>0.2609</td><td>0.0005</td><td>0.3784</td><td>0.0020</td></tr><tr><td>8464.72530016</td><td>-9.8082</td><td>1.6310</td><td>-</td><td>0.2633</td><td>0.0006</td><td>0.3786</td><td>0.0013</td></tr><tr><td>8464.73352901</td><td>-6.8396</td><td>1.7945</td><td>-</td><td>0.2618</td><td>0.0006</td><td>0.3736</td><td>0.0017</td></tr><tr><td>8465.69725272</td><td>35.3156</td><td>1.5869</td><td>-</td><td>0.2711</td><td>0.0004</td><td>0.3797</td><td>0.0016</td></tr><tr><td>8465.70501861</td><td>33.8672</td><td>1.4372</td><td>-</td><td>0.2705</td><td>0.0004</td><td>0.3830</td><td>0.0016</td></tr><tr><td>8466.68945895</td><td>-26.6290</td><td>1.3620</td><td>-</td><td>0.2670</td><td>0.0005</td><td>0.3944</td><td>0.0018</td></tr><tr><td>8466.69655358</td><td>-26.1766</td><td>1.6262</td><td>-</td><td>0.2655</td><td>0.0005</td><td>0.3850</td><td>0.0021</td></tr><tr><td>8481.60390690</td><td>-0.1308</td><td>1.4002</td><td>-</td><td>0.2654</td><td>0.0005</td><td>0.3833</td><td>0.0018</td></tr><tr><td>8483.60647679</td><td>7.4831</td><td>1.1414</td><td>-</td><td>0.2719</td><td>0.0004</td><td>0.3808</td><td>0.0016</td></tr><tr><td>8509.53123346</td><td>-34.2170</td><td>1.6320</td><td>0.053220</td><td>0.2649</td><td>0.0005</td><td>0.3907</td><td>0.0016</td></tr><tr><td>8509.57920635</td><td>-34.3604</td><td>2.0194</td><td>0.064890</td><td>0.2689</td><td>0.0006</td><td>0.3865</td><td>0.0015</td></tr><tr><td>8509.59794413</td><td>-39.5850</td><td>1.8169</td><td>0.051320</td><td>0.2676</td><td>0.0006</td><td>0.3859</td><td>0.0023</td></tr><tr><td>8510.55122193</td><td>-42.5098</td><td>1.9474</td><td>0.057400</td><td>0.2596</td><td>0.0007</td><td>0.3943</td><td>0.0016</td></tr><tr><td>8510.58082740</td><td>-37.6804</td><td>2.6694</td><td>0.052610</td><td>0.2611</td><td>0.0007</td><td>0.3990</td><td>0.0014</td></tr><tr><td>8511.54866504</td><td>35.0932</td><td>1.5730</td><td>-0.008900</td><td>0.2636</td><td>0.0005</td><td>0.3919</td><td>0.0014</td></tr><tr><td>8511.60528350</td><td>38.0889</td><td>1.6384</td><td>-0.014010</td><td>0.2647</td><td>0.0006</td><td>0.3790</td><td>0.0017</td></tr><tr><td>8512.55084217</td><td>15.5591</td><td>1.4106</td><td>0.026710</td><td>0.2649</td><td>0.0004</td><td>0.3775</td><td>0.0017</td></tr></table>
<table><caption>Table B.1: continued.</caption><thead><tr><th>BJD<sub>TDB</sub> - 2450000</th><th>RV<br>[m s<sup>-1</sup>]</th><th>err<sub>RV</sub><br>[m s<sup>-1</sup>]</th><th>BIS<br>[km s<sup>-1</sup>]</th><th>Hα[1.6 Å]<br>-</th><th>err<sub>Hα[1.6Å]</sub><br>-</th><th>S-index<br>-</th><th>err<sub>S-index</sub><br>-</th></tr></thead><tbody><tr><td>8576.48050990</td><td>0.4351</td><td>2.4353</td><td>0.044050</td><td>0.2760</td><td>0.0007</td><td>0.3766</td><td>0.0024</td></tr><tr><td>8576.51237350</td><td>-5.4469</td><td>3.4031</td><td>0.067490</td><td>0.2744</td><td>0.0012</td><td>0.3848</td><td>0.0025</td></tr><tr><td>8579.49225408</td><td>-44.4058</td><td>1.9851</td><td>0.085650</td><td>0.2655</td><td>0.0006</td><td>0.3899</td><td>0.0026</td></tr><tr><td>8580.47997019</td><td>14.8276</td><td>1.4775</td><td>0.020970</td><td>0.2663</td><td>0.0004</td><td>0.3918</td><td>0.0024</td></tr><tr><td>8581.48412227</td><td>5.2024</td><td>1.7351</td><td>0.032370</td><td>0.2634</td><td>0.0005</td><td>0.3973</td><td>0.0022</td></tr><tr><td>8582.47372628</td><td>34.2823</td><td>1.6718</td><td>0.007800</td><td>0.2689</td><td>0.0004</td><td>0.3890</td><td>0.0023</td></tr><tr><td>8670.93364852</td><td>6.9920</td><td>1.0773</td><td>0.046050</td><td>0.2717</td><td>0.0004</td><td>0.3866</td><td>0.0014</td></tr><tr><td>8673.87429327</td><td>31.5917</td><td>1.4553</td><td>-0.011120</td><td>0.2677</td><td>0.0006</td><td>0.3766</td><td>0.0019</td></tr><tr><td>8674.94274813</td><td>-9.4457</td><td>1.3615</td><td>0.049300</td><td>0.2690</td><td>0.0005</td><td>0.4005</td><td>0.0022</td></tr><tr><td>8684.87453781</td><td>17.8999</td><td>1.2278</td><td>0.013930</td><td>0.2660</td><td>0.0005</td><td>0.3750</td><td>0.0032</td></tr><tr><td>8689.86328901</td><td>2.8129</td><td>1.1143</td><td>0.041050</td><td>0.2684</td><td>0.0004</td><td>0.3819</td><td>0.0022</td></tr><tr><td>8690.87555738</td><td>39.9991</td><td>1.2297</td><td>-0.001130</td><td>0.2693</td><td>0.0005</td><td>0.3880</td><td>0.0039</td></tr><tr><td>8692.81900246</td><td>14.0329</td><td>1.0153</td><td>0.026230</td><td>0.2709</td><td>0.0004</td><td>0.4076</td><td>0.0019</td></tr><tr><td>8693.85287935</td><td>-2.9615</td><td>1.5832</td><td>0.045490</td><td>0.2672</td><td>0.0006</td><td>0.3861</td><td>0.0021</td></tr><tr><td>8694.84459014</td><td>0.2584</td><td>0.9592</td><td>0.024070</td><td>0.2686</td><td>0.0003</td><td>0.3842</td><td>0.0026</td></tr><tr><td>8695.87172996</td><td>50.5443</td><td>1.3158</td><td>-0.015140</td><td>0.2718</td><td>0.0004</td><td>0.3804</td><td>0.0017</td></tr><tr><td>8697.78683736</td><td>-35.8855</td><td>1.4054</td><td>0.077990</td><td>0.2667</td><td>0.0005</td><td>0.3793</td><td>0.0017</td></tr><tr><td>8698.82266843</td><td>8.1072</td><td>1.0585</td><td>0.025040</td><td>0.2646</td><td>0.0003</td><td>0.3624</td><td>0.0013</td></tr><tr><td>8699.88169423</td><td>37.6680</td><td>1.2428</td><td>-0.016730</td><td>0.2710</td><td>0.0005</td><td>0.3513</td><td>0.0034</td></tr><tr><td>8700.87854176</td><td>0.0000</td><td>1.1900</td><td>0.058290</td><td>0.2700</td><td>0.0004</td><td>0.3666</td><td>0.0019</td></tr><tr><td>8701.80598865</td><td>26.7346</td><td>1.3374</td><td>-0.000930</td><td>0.2690</td><td>0.0004</td><td>0.3542</td><td>0.0021</td></tr><tr><td>8702.76752183</td><td>-6.0488</td><td>1.2357</td><td>0.067500</td><td>0.2760</td><td>0.0005</td><td>0.3561</td><td>0.0018</td></tr><tr><td>8704.79732613</td><td>38.6818</td><td>1.4503</td><td>0.008390</td><td>0.2709</td><td>0.0005</td><td>0.3612</td><td>0.0016</td></tr><tr><td>8707.90966982</td><td>28.4307</td><td>1.3332</td><td>-0.002070</td><td>0.2666</td><td>0.0005</td><td>0.3600</td><td>0.0015</td></tr><tr><td>8708.76447295</td><td>40.6240</td><td>1.1993</td><td>0.002630</td><td>0.2675</td><td>0.0004</td><td>0.3577</td><td>0.0020</td></tr><tr><td>8718.74961073</td><td>36.4584</td><td>1.2453</td><td>0.001510</td><td>0.2756</td><td>0.0005</td><td>0.3602</td><td>0.0024</td></tr><tr><td>8719.82471466</td><td>-22.4962</td><td>1.1639</td><td>0.065630</td><td>0.2696</td><td>0.0004</td><td>0.3639</td><td>0.0026</td></tr><tr><td>8720.84621731</td><td>11.7789</td><td>1.6623</td><td>0.011170</td><td>0.2703</td><td>0.0006</td><td>0.3673</td><td>0.0020</td></tr><tr><td>8721.75426804</td><td>48.0785</td><td>1.0905</td><td>0.002300</td><td>0.2699</td><td>0.0004</td><td>0.3635</td><td>0.0019</td></tr><tr><td>8722.74122029</td><td>17.4124</td><td>1.2063</td><td>0.029480</td><td>0.2744</td><td>0.0004</td><td>0.3701</td><td>0.0021</td></tr><tr><td>8723.73967682</td><td>-27.3998</td><td>1.0954</td><td>0.069110</td><td>0.2709</td><td>0.0004</td><td>0.3720</td><td>0.0022</td></tr><tr><td>8724.82311116</td><td>3.5745</td><td>1.4927</td><td>0.030230</td><td>0.2679</td><td>0.0005</td><td>0.3718</td><td>0.0017</td></tr><tr><td>8725.70980525</td><td>26.9388</td><td>1.1838</td><td>0.007080</td><td>0.2662</td><td>0.0004</td><td>0.3782</td><td>0.0017</td></tr><tr><td>8734.72757798</td><td>27.6453</td><td>1.5650</td><td>0.011550</td><td>0.2669</td><td>0.0006</td><td>0.4008</td><td>0.0034</td></tr><tr><td>8736.83306483</td><td>2.5551</td><td>1.9949</td><td>0.038890</td><td>0.2699</td><td>0.0006</td><td>0.3901</td><td>0.0047</td></tr><tr><td>8737.80234571</td><td>11.0414</td><td>1.7889</td><td>0.034790</td><td>0.2792</td><td>0.0007</td><td>0.3674</td><td>0.0030</td></tr><tr><td>8738.72461165</td><td>48.5519</td><td>1.8637</td><td>-0.004540</td><td>0.2728</td><td>0.0006</td><td>0.3556</td><td>0.0025</td></tr><tr><td>8739.74132231</td><td>9.4424</td><td>1.3690</td><td>0.046930</td><td>0.2720</td><td>0.0006</td><td>0.3488</td><td>0.0026</td></tr><tr><td>8740.72127274</td><td>0.5538</td><td>1.5103</td><td>0.028690</td><td>0.2699</td><td>0.0006</td><td>0.3696</td><td>0.0027</td></tr><tr><td>8741.71402357</td><td>-8.6865</td><td>0.9042</td><td>0.064880</td><td>0.2677</td><td>0.0004</td><td>0.3569</td><td>0.0019</td></tr><tr><td>8742.71298907</td><td>82.1742</td><td>1.3040</td><td>0.016950</td><td>0.2716</td><td>0.0005</td><td>0.3589</td><td>0.0019</td></tr><tr><td>8744.86529394</td><td>12.8029</td><td>1.6896</td><td>0.010220</td><td>0.2738</td><td>0.0005</td><td>0.3616</td><td>0.0023</td></tr><tr><td>8745.68610835</td><td>-4.1308</td><td>2.2643</td><td>0.047710</td><td>0.2716</td><td>0.0008</td><td>0.3767</td><td>0.0024</td></tr><tr><td>8746.72905288</td><td>32.9618</td><td>1.5638</td><td>-0.011710</td><td>0.2759</td><td>0.0006</td><td>0.3596</td><td>0.0025</td></tr><tr><td>8747.64660273</td><td>23.5623</td><td>2.8275</td><td>0.009380</td><td>0.2780</td><td>0.0010</td><td>0.3663</td><td>0.0025</td></tr><tr><td>8748.66608518</td><td>-2.7872</td><td>1.3049</td><td>0.043140</td><td>0.2731</td><td>0.0005</td><td>0.3500</td><td>0.0018</td></tr></tbody></table>
<table><caption>Table B.1: continued.</caption><thead><tr><th>BJD<sub>TDB</sub> - 2450000</th><th>RV<br>[m s<sup>-1</sup>]</th><th>err<sub>RV</sub><br>[m s<sup>-1</sup>]</th><th>BIS<br>[km s<sup>-1</sup>]</th><th>Hα[1.6 Å]<br>-</th><th>err<sub>Hα[1.6Å]</sub><br>-</th><th>S-index<br>-</th><th>err<sub>S-index</sub><br>-</th></tr></thead><tbody><tr><td>8576.48050990</td><td>0.4351</td><td>2.4353</td><td>0.044050</td><td>0.2760</td><td>0.0007</td><td>0.3766</td><td>0.0024</td></tr><tr><td>8576.51237350</td><td>-5.4469</td><td>3.4031</td><td>0.067490</td><td>0.2744</td><td>0.0012</td><td>0.3848</td><td>0.0025</td></tr><tr><td>8579.49225408</td><td>-44.4058</td><td>1.9851</td><td>0.085650</td><td>0.2655</td><td>0.0006</td><td>0.3899</td><td>0.0026</td></tr><tr><td>8580.47997019</td><td>14.8276</td><td>1.4775</td><td>0.020970</td><td>0.2663</td><td>0.0004</td><td>0.3918</td><td>0.0024</td></tr><tr><td>8581.48412227</td><td>5.2024</td><td>1.7351</td><td>0.032370</td><td>0.2634</td><td>0.0005</td><td>0.3973</td><td>0.0022</td></tr><tr><td>8582.47372628</td><td>34.2823</td><td>1.6718</td><td>0.007800</td><td>0.2689</td><td>0.0004</td><td>0.3890</td><td>0.0023</td></tr><tr><td>8670.93364852</td><td>6.9920</td><td>1.0773</td><td>0.046050</td><td>0.2717</td><td>0.0004</td><td>0.3866</td><td>0.0014</td></tr><tr><td>8673.87429327</td><td>31.5917</td><td>1.4553</td><td>-0.011120</td><td>0.2677</td><td>0.0006</td><td>0.3766</td><td>0.0019</td></tr><tr><td>8674.94274813</td><td>-9.4457</td><td>1.3615</td><td>0.049300</td><td>0.2690</td><td>0.0005</td><td>0.4005</td><td>0.0022</td></tr><tr><td>8684.87453781</td><td>17.8999</td><td>1.2278</td><td>0.013930</td><td>0.2660</td><td>0.0005</td><td>0.3750</td><td>0.0032</td></tr><tr><td>8689.86328901</td><td>2.8129</td><td>1.1143</td><td>0.041050</td><td>0.2684</td><td>0.0004</td><td>0.3819</td><td>0.0022</td></tr><tr><td>8690.87555738</td><td>39.9991</td><td>1.2297</td><td>-0.001130</td><td>0.2693</td><td>0.0005</td><td>0.3880</td><td>0.0039</td></tr><tr><td>8692.81900246</td><td>14.0329</td><td>1.0153</td><td>0.026230</td><td>0.2709</td><td>0.0004</td><td>0.4076</td><td>0.0019</td></tr><tr><td>8693.85287935</td><td>-2.9615</td><td>1.5832</td><td>0.045490</td><td>0.2672</td><td>0.0006</td><td>0.3861</td><td>0.0021</td></tr><tr><td>8694.84459014</td><td>0.2584</td><td>0.9592</td><td>0.024070</td><td>0.2686</td><td>0.0003</td><td>0.3842</td><td>0.0026</td></tr><tr><td>8695.87172996</td><td>50.5443</td><td>1.3158</td><td>-0.015140</td><td>0.2718</td><td>0.0004</td><td>0.3804</td><td>0.0017</td></tr><tr><td>8697.78683736</td><td>-35.8855</td><td>1.4054</td><td>0.077990</td><td>0.2667</td><td>0.0005</td><td>0.3793</td><td>0.0017</td></tr><tr><td>8698.82266843</td><td>8.1072</td><td>1.0585</td><td>0.025040</td><td>0.2646</td><td>0.0003</td><td>0.3624</td><td>0.0013</td></tr><tr><td>8699.88169423</td><td>37.6680</td><td>1.2428</td><td>-0.016730</td><td>0.2710</td><td>0.0005</td><td>0.3513</td><td>0.0034</td></tr><tr><td>8700.87854176</td><td>0.0000</td><td>1.1900</td><td>0.058290</td><td>0.2700</td><td>0.0004</td><td>0.3666</td><td>0.0019</td></tr><tr><td>8701.80598865</td><td>26.7346</td><td>1.3374</td><td>-0.000930</td><td>0.2690</td><td>0.0004</td><td>0.3542</td><td>0.0021</td></tr><tr><td>8702.76752183</td><td>-6.0488</td><td>1.2357</td><td>0.067500</td><td>0.2760</td><td>0.0005</td><td>0.3561</td><td>0.0018</td></tr><tr><td>8704.79732613</td><td>38.6818</td><td>1.4503</td><td>0.008390</td><td>0.2709</td><td>0.0005</td><td>0.3612</td><td>0.0016</td></tr><tr><td>8707.90966982</td><td>28.4307</td><td>1.3332</td><td>-0.002070</td><td>0.2666</td><td>0.0005</td><td>0.3600</td><td>0.0015</td></tr><tr><td>8708.76447295</td><td>40.6240</td><td>1.1993</td><td>0.002630</td><td>0.2675</td><td>0.0004</td><td>0.3577</td><td>0.0020</td></tr><tr><td>8718.74961073</td><td>36.4584</td><td>1.2453</td><td>0.001510</td><td>0.2756</td><td>0.0005</td><td>0.3602</td><td>0.0024</td></tr><tr><td>8719.82471466</td><td>-22.4962</td><td>1.1639</td><td>0.065630</td><td>0.2696</td><td>0.0004</td><td>0.3639</td><td>0.0026</td></tr><tr><td>8720.84621731</td><td>11.7789</td><td>1.6623</td><td>0.011170</td><td>0.2703</td><td>0.0006</td><td>0.3673</td><td>0.0020</td></tr><tr><td>8721.75426804</td><td>48.0785</td><td>1.0905</td><td>0.002300</td><td>0.2699</td><td>0.0004</td><td>0.3635</td><td>0.0019</td></tr><tr><td>8722.74122029</td><td>17.4124</td><td>1.2063</td><td>0.029480</td><td>0.2744</td><td>0.0004</td><td>0.3701</td><td>0.0021</td></tr><tr><td>8723.73967682</td><td>-27.3998</td><td>1.0954</td><td>0.069110</td><td>0.2709</td><td>0.0004</td><td>0.3720</td><td>0.0022</td></tr><tr><td>8724.82311116</td><td>3.5745</td><td>1.4927</td><td>0.030230</td><td>0.2679</td><td>0.0005</td><td>0.3718</td><td>0.0017</td></tr><tr><td>8725.70980525</td><td>26.9388</td><td>1.1838</td><td>0.007080</td><td>0.2662</td><td>0.0004</td><td>0.3782</td><td>0.0017</td></tr><tr><td>8734.72757798</td><td>27.6453</td><td>1.5650</td><td>0.011550</td><td>0.2669</td><td>0.0006</td><td>0.4008</td><td>0.0034</td></tr><tr><td>8736.83306483</td><td>2.5551</td><td>1.9949</td><td>0.038890</td><td>0.2699</td><td>0.0006</td><td>0.3901</td><td>0.0047</td></tr><tr><td>8737.80234571</td><td>11.0414</td><td>1.7889</td><td>0.034790</td><td>0.2792</td><td>0.0007</td><td>0.3674</td><td>0.0030</td></tr><tr><td>8738.72461165</td><td>48.5519</td><td>1.8637</td><td>-0.004540</td><td>0.2728</td><td>0.0006</td><td>0.3556</td><td>0.0025</td></tr><tr><td>8739.74132231</td><td>9.4424</td><td>1.3690</td><td>0.046930</td><td>0.2720</td><td>0.0006</td><td>0.3488</td><td>0.0026</td></tr><tr><td>8740.72127274</td><td>0.5538</td><td>1.5103</td><td>0.028690</td><td>0.2699</td><td>0.0006</td><td>0.3696</td><td>0.0027</td></tr><tr><td>8741.71402357</td><td>-8.6865</td><td>0.9042</td><td>0.064880</td><td>0.2677</td><td>0.0004</td><td>0.3569</td><td>0.0019</td></tr><tr><td>8742.71298907</td><td>82.1742</td><td>1.3040</td><td>0.016950</td><td>0.2716</td><td>0.0005</td><td>0.3589</td><td>0.0019</td></tr><tr><td>8744.86529394</td><td>12.8029</td><td>1.6896</td><td>0.010220</td><td>0.2738</td><td>0.0005</td><td>0.3616</td><td>0.0023</td></tr><tr><td>8745.68610835</td><td>-4.1308</td><td>2.2643</td><td>0.047710</td><td>0.2716</td><td>0.0008</td><td>0.3767</td><td>0.0024</td></tr><tr><td>8746.72905288</td><td>32.9618</td><td>1.5638</td><td>-0.011710</td><td>0.2759</td><td>0.0006</td><td>0.3596</td><td>0.0025</td></tr><tr><td>8747.64660273</td><td>23.5623</td><td>2.8275</td><td>0.009380</td><td>0.2780</td><td>0.0010</td><td>0.3663</td><td>0.0025</td></tr><tr><td>8748.66608518</td><td>-2.7872</td><td>1.3049</td><td>0.043140</td><td>0.2731</td><td>0.0005</td><td>0.3500</td><td>0.0018</td></tr></tbody></table>
Appendix C: Posteriors of the joint RV+TESS photometry fit

<figure><img src="image_23.png" /><figcaption>Fig. C.1: Posteriors of the free parameters used in the joint fit of the RV+TESS short-cadence light curve, including a linear long-term trend for the RVs (see Table 3). Two corner plots are shown for clarity.</figcaption></figure>
Appendix C: Posteriors of the joint RV+TESS photometry fit

<figure><img src="image_24.png" /><figcaption>Fig. C.1: Posteriors of the free parameters used in the joint fit of the RV+TESS short-cadence light curve, including a linear long-term trend for the RVs (see Table 3). Two corner plots are shown for clarity.</figcaption></figure>
<figure><img src="image_24.png" /><figcaption>Fig. C.1: Continued</figcaption></figure>
<figure><img src="image_25.png" /><figcaption>Fig. C.1: Continued</figcaption></figure>