## Appendix A: Short tables and diagrams

<table><caption>**Table A.1.** Published heliocentric radial velocities of Gl 486<sup>a</sup>.</caption><thead><tr><th>γ [km s<sup>-1</sup>]</th><th>Reference</th></tr></thead><tbody><tr><td>+19.1 ± 0.8</td><td>Giz02</td></tr><tr><td>+19.090 ± 0.010</td><td>Nid02</td></tr><tr><td>+19.180 ± 0.001</td><td>Fou18<sup>b</sup></td></tr><tr><td>+19.50 ± 0.12</td><td>Jef18</td></tr><tr><td>+18.970</td><td>Rei18<sup>c</sup></td></tr><tr><td>+19.106 ± 0.013</td><td>Sou18</td></tr><tr><td>+19.395 ± 0.042</td><td>Laf20<sup>d</sup></td></tr></tbody></table>

**References.** Giz02: Gizis et al. (2002); Nid20: Nid20 et al. (2002); Fou18: Fouqué et al. (2018); Jef18: Jeffers et al. (2018); Laf20: Lafarga et al. (2020); Rei18: Reiners et al. (2018); Sou18: Soubiran et al. (2018).

**Notes.** <sup>(a)</sup>The obsolete values of +5.0 ± 0.7 km s<sup>-1</sup> and +11 ± 5 km s<sup>-1</sup> of Joy (1947) and Newton et al. (2014), respectively, are not tabulated. <sup>(b)</sup>Although VizieR tabulates an uncertainty of 1 m s<sup>-1</sup> for the γ value of Fouqué et al. (2018), the actual accuracy of the heliocentric RVs measured by ESPaDOnS and reduced with LIBRE-ESPRIT (Donati et al. 1997) is about 20–30 m s<sup>-1</sup> (Moutou et al. 2017). <sup>(c)</sup>Reiners et al. (2018) did not tabulate γ uncertainties. <sup>(d)</sup>We tabulate their cross-correlation function RV weighted mean plus the gravitational redshift, with uncertainties summed quadratically.

<table><caption>**Table A.2.** Multiband photometry of Gl 486<sup>a</sup>.</caption><thead><tr><th>Band</th><th>Magnitude [mag]</th><th>Reference</th></tr></thead><tbody><tr><td>u'</td><td>15.183 ± 0.006</td><td>SDSS DR9</td></tr><tr><td>B</td><td>12.933 ± 0.020</td><td>UCAC4</td></tr><tr><td>g'</td><td>12.099 ± 0.020</td><td>UCAC4</td></tr><tr><td>G<sub>BP</sub></td><td>11.6426 ± 0.0030</td><td>Gaia EDR3</td></tr><tr><td>V<sub>T</sub></td><td>11.379 ± 0.006</td><td>TYC</td></tr><tr><td>V</td><td>11.393 ± 0.020</td><td>UCAC4</td></tr><tr><td>r'</td><td>10.829 ± 0.040</td><td>UCAC4</td></tr><tr><td>G</td><td>10.1051 ± 0.0028</td><td>Gaia EDR3</td></tr><tr><td>i'</td><td>9.316 ± 0.070</td><td>UCAC4</td></tr><tr><td>G<sub>RP</sub></td><td>8.8883 ± 0.0038</td><td>Gaia EDR3</td></tr><tr><td>J</td><td>7.195 ± 0.026</td><td>2MASS</td></tr><tr><td>H</td><td>6.666 ± 0.046</td><td>2MASS</td></tr><tr><td>K<sub>s</sub></td><td>6.362 ± 0.018</td><td>2MASS</td></tr><tr><td>W1</td><td>6.206 ± 0.101</td><td>AllWISE</td></tr><tr><td>W2</td><td>5.955 ± 0.044</td><td>AllWISE</td></tr><tr><td>W3</td><td>5.979 ± 0.015</td><td>AllWISE</td></tr><tr><td>W4</td><td>5.810 ± 0.041</td><td>AllWISE</td></tr></tbody></table>

**References.** TYC: Tycho-2, Høg et al. (2000); 2MASS: Two Micron All-Sky Survey, Skrutskie et al. (2006); SDSS DR9: Sloan Digital Sky Survey, Ahn et al. (2012); UCAC4: The Fourth US Naval Observatory CCD Astrograph Catalog, Zacharias et al. (2013); AllWISE: Wide-field Infrared Survey Explorer, Cutri et al. (2014); Gaia EDR3: Gaia Collaboration (2021a).

**Notes.** <sup>(a)</sup> TESS T magnitude in Table 2.

<figure><img src="image_19.png" /><figcaption>**Fig. A.1.** Spectral energy distribution of Gl 486. The apparent fluxes (coloured filled circles) are imposed on a BT-Settl CIFIST spectrum (grey; $T_{\text{eff}}$ = 3200 K and log g = 5.5). The modelled fluxes are depicted as black empty circles. The photometric datum in u' (purple cross) was not considered for integrating the bolometric luminosity. Horizontal bars represent the effective widths of the bandpasses (equivalent to the horizontal size of a rectangle with height equal to maximum transmission and with the same area that the one covered by the filter transmission curve), while vertical bars (visible only for relatively large values) represent the flux uncertainty derived from the magnitude and parallax errors. See details in Cifuentes et al. (2020).</figcaption></figure>

<table><caption>**Table A.3.** Published effective temperatures of Gl 486<sup>a</sup>.</caption><thead><tr><th>$T_{\text{eff}}$ (K)</th><th>Reference</th></tr></thead><tbody><tr><td>3095</td><td>Cas08<sup>b</sup></td></tr><tr><td>3240</td><td>Mor08</td></tr><tr><td>3086</td><td>Jen09<sup>c</sup></td></tr><tr><td>3290</td><td>Lep13</td></tr><tr><td>3300</td><td>Raj13</td></tr><tr><td>3241</td><td>Ste13</td></tr><tr><td>3270 ± 74</td><td>Gai14</td></tr><tr><td>3240 ± 17</td><td>Fou18</td></tr><tr><td>3384 ± 51</td><td>Pas18</td></tr><tr><td>3384</td><td>Raj18</td></tr><tr><td>3313</td><td>Hou19</td></tr><tr><td>3239 ± 92</td><td>Hoj19</td></tr><tr><td>3218 ± 110</td><td>Kuz19</td></tr><tr><td>3389 ± 51</td><td>Sch19</td></tr><tr><td>3340 ± 54</td><td>Pas19</td></tr><tr><td>3096 ± 27</td><td>AK20</td></tr><tr><td>3200 ± 100</td><td>Cif20</td></tr><tr><td>3408 ± 45</td><td>Mar21</td></tr></tbody></table>

**References.** Cas08: Casagrande et al. (2008); Mor08: Morales et al. (2008); Jen09: Jenkins et al. (2009); Lep13: Lépine et al. (2013); Raj13: Rajpurohit et al. (2013); Ste13: Stelzer et al. (2013); Gai14: Gaidos et al. (2014); Fou18: Fouqué et al. (2018); Pas18: Passegger et al. (2018); Raj18: Rajpurohit et al. (2018); Hou19: Houdebine et al. (2019); Hoj19: Hojjatpanah et al. (2019); Kuz19: Kuznetsov et al. (2019); Sch19: Schweitzer et al. (2019); Pas19: Passegger et al. (2019); AK20: Antoniadis-Karnavas et al. (2020); Cif20: Cifuentes et al. (2020); Mar21: Marfil et al. (2021).

**Notes.** <sup>(a)</sup> The $T_{\text{eff}}$ determined by us from the stellar bolometric luminosity, interferometric radius, and Stefan-Boltzman law is 3291 ± 75 K.

<sup>(b)</sup> Cifuentes et al. (2020) demonstrated that Casagrande et al. (2008) $T_{\text{eff}}$ of M dwarfs, in contrast to FGK stars, are unreliable. <sup>(c)</sup> Jenkins et al. (2009) $T_{\text{eff}}$ were determined using the $V-K_s$ relations taken from Casagrande et al. (2008), while Cifuentes et al. (2020) again demonstrated that in the Gaia era the Johnson photometry should not be used for deriving parameters of M dwarfs.
<table><caption>**Table A.4.** Published relative iron abundances of Gl 486.</caption><thead><tr><th>[Fe/H]<br>[dex]</th><th>Reference</th></tr></thead><tbody><tr><td>+0.03 ± 0.13</td><td>New14</td></tr><tr><td>+0.06 ± 0.16</td><td>Pas18</td></tr><tr><td>+0.01 ± 0.10</td><td>Fou18<sup>a</sup></td></tr><tr><td>+0.12 ± 0.09</td><td>Kuz19<sup>b</sup></td></tr><tr><td>+0.03 ± 0.16</td><td>Sch19</td></tr><tr><td>+0.07 ± 0.19</td><td>Pas19<sup>c</sup></td></tr><tr><td>+0.12 ± 0.05</td><td>Hoj19</td></tr><tr><td>-0.15 ± 0.13</td><td>Mar21<sup>d</sup></td></tr></tbody></table>

**References.** New14: Newton et al. (2014); Pas18: Passegger et al. (2018); Fou18: Fouqué et al. (2018); Kuz19: Kuznetsov et al. (2019); Sch19: Schweitzer et al. (2019); Pas19: Passegger et al. (2019); Hoj19: Hojjatpanah et al. (2019); Mar21: Marfil et al. (2021).

**Notes.** (a) Tabulated uncertainty is the quadratic sum of the systematic and the MCAL uncertainties. (b) From low-S/N X-Shooter spectra. (c) From CARMENES VIS+NIR spectra. (d) After α-enhancement correction.

<table><caption>**Table A.5.** Emission measure distribution of Gl 486.</caption><thead><tr><th>log T (K)</th><th>EM (cm<sup>-3</sup>)</th></tr></thead><tbody><tr><td>4.0</td><td>48.00:</td></tr><tr><td>4.1</td><td>47.90:</td></tr><tr><td>4.2</td><td>47.80:</td></tr><tr><td>4.3</td><td>47.65 ± 0.35</td></tr><tr><td>4.4</td><td>47.55 ± 0.20</td></tr><tr><td>4.5</td><td>47.40 ± 0.25</td></tr><tr><td>4.6</td><td>47.15 ± 0.30</td></tr><tr><td>4.7</td><td>47.00 ± 0.20</td></tr><tr><td>4.8</td><td>46.90 ± 0.25</td></tr><tr><td>4.9</td><td>46.85 ± 0.20</td></tr><tr><td>5.0</td><td>46.80 ± 0.15</td></tr><tr><td>5.1</td><td>46.70 ± 0.30</td></tr><tr><td>5.2</td><td>46.60 ± 0.20</td></tr><tr><td>5.3</td><td>46.50 ± 0.20</td></tr><tr><td>5.4</td><td>46.50 ± 0.20</td></tr><tr><td>5.5</td><td>46.35:</td></tr><tr><td>5.6</td><td>46.10:</td></tr><tr><td>5.7</td><td>46.00:</td></tr></tbody></table>

<figure><img src="image_20.png" /><figcaption>**Fig. A.2.** Same as Fig. 13 but for the MR-S (baseline, top) and MR-SA (baseline plus relative stellar abundance constraints, bottom) planet interior scenarios.</figcaption></figure>
<figure><img src="image_21.png" /><figcaption>**Fig. A.3.** Nested samples distribution of fitted (black) and derived (blue) parameters of Gl 486 b with CARMENES and MAROON-X RV data and CHEOPS and TESS light curves. The position of the median from the posterior is marked with red grid lines. The contours on the 2D panels represent the 1σ, 2σ, and 3σ confidence levels of the overall posterior samples. The top (black) and bottom (blue) panels of every column represent the 1D histogram distribution of each parameter.</figcaption></figure>
<table><caption>**Table A.6.** Priors and posteriors of the joint transit and RV fit of Gl 486<sup>a</sup>.</caption><thead><tr><th>Parameter</th><th>Prior</th><th>Posterior</th><th>Unit</th><th>Description</th></tr></thead><tbody><tr><td colspan="5" style="text-align:center; font-weight:bold;">Stellar parameter</td></tr><tr><td>ρ<sub>*</sub></td><td>N(12106, 2593)</td><td>11570<sup>+690</sup><sub>-1340</sub></td><td>kg m<sup>-3</sup></td><td>Stellar density</td></tr><tr><td colspan="5" style="text-align:center; font-weight:bold;">Photometry instrumental parameters</td></tr><tr><td>μ<sub>TESS,T23</sub></td><td>N(0, 10<sup>5</sup>)</td><td>-0.5<sup>+6.9</sup><sub>-7.0</sub></td><td>ppm</td><td>Relative flux offset</td></tr><tr><td>μ<sub>CHEOPS,C01</sub></td><td>N(0, 10<sup>5</sup>)</td><td>+1<sup>+15</sup><sub>-14</sub></td><td>ppm</td><td>Relative flux offset</td></tr><tr><td>μ<sub>CHEOPS,C02</sub></td><td>N(0, 10<sup>5</sup>)</td><td>+15<sup>+15</sup><sub>-16</sub></td><td>ppm</td><td>Relative flux offset</td></tr><tr><td>μ<sub>CHEOPS,C03</sub></td><td>N(0, 10<sup>5</sup>)</td><td>+1<sup>+17</sup><sub>-17</sub></td><td>ppm</td><td>Relative flux offset</td></tr><tr><td>μ<sub>CHEOPS,C04</sub></td><td>N(0, 10<sup>5</sup>)</td><td>+2<sup>+17</sup><sub>-17</sub></td><td>ppm</td><td>Relative flux offset</td></tr><tr><td>μ<sub>CHEOPS,C05</sub></td><td>N(0, 10<sup>5</sup>)</td><td>-17<sup>+16</sup><sub>-16</sub></td><td>ppm</td><td>Relative flux offset</td></tr><tr><td>μ<sub>CHEOPS,C06</sub></td><td>N(0, 10<sup>5</sup>)</td><td>-2<sup>+18</sup><sub>-19</sub></td><td>ppm</td><td>Relative flux offset</td></tr><tr><td>μ<sub>CHEOPS,C07</sub></td><td>N(0, 10<sup>5</sup>)</td><td>+6<sup>+21</sup><sub>-20</sub></td><td>ppm</td><td>Relative flux offset</td></tr><tr><td>σ<sub>TESS,T23</sub></td><td>LU(1, 8498)</td><td>58<sup>+1118</sup><sub>-53</sub></td><td>ppm</td><td>Transit extra jitter</td></tr><tr><td>σ<sub>CHEOPS,C01</sub></td><td>LU(1, 3322)</td><td>75<sup>+728</sup><sub>-69</sub></td><td>ppm</td><td>Transit extra jitter</td></tr><tr><td>σ<sub>CHEOPS,C02</sub></td><td>LU(1, 3320)</td><td>77<sup>+806</sup><sub>-71</sub></td><td>ppm</td><td>Transit extra jitter</td></tr><tr><td>σ<sub>CHEOPS,C03</sub></td><td>LU(1, 3323)</td><td>44<sup>+555</sup><sub>-40</sub></td><td>ppm</td><td>Transit extra jitter</td></tr><tr><td>σ<sub>CHEOPS,C04</sub></td><td>LU(1, 3322)</td><td>40<sup>+495</sup><sub>-36</sub></td><td>ppm</td><td>Transit extra jitter</td></tr><tr><td>σ<sub>CHEOPS,C05</sub></td><td>LU(1, 3336)</td><td>40<sup>+528</sup><sub>-36</sub></td><td>ppm</td><td>Transit extra jitter</td></tr><tr><td>σ<sub>CHEOPS,C06</sub></td><td>LU(1, 3388)</td><td>38<sup>+511</sup><sub>-35</sub></td><td>ppm</td><td>Transit extra jitter</td></tr><tr><td>σ<sub>CHEOPS,C07</sub></td><td>LU(1, 3329)</td><td>62<sup>+704</sup><sub>-58</sub></td><td>ppm</td><td>Transit extra jitter</td></tr><tr><td>q<sub>1,TESS</sub></td><td>U(0, 1.0)</td><td>0.57<sup>+0.23</sup><sub>-0.21</sub></td><td>...</td><td>u<sub>1</sub> quadratic limb-darkening</td></tr><tr><td>q<sub>1,CHEOPS</sub></td><td>U(0, 1.0)</td><td>0.51<sup>+0.16</sup><sub>-0.15</sub></td><td>...</td><td>u<sub>1</sub> quadratic limb-darkening</td></tr><tr><td>q<sub>2,TESS</sub></td><td>U(0, 1.0)</td><td>0.19<sup>+0.20</sup></td><td>...</td><td>u<sub>2</sub> quadratic limb-darkening</td></tr><tr><td>q<sub>2,CHEOPS</sub></td><td>U(0, 1.0)</td><td>0.119<sup>+0.119</sup><sub>-0.078</sub></td><td>...</td><td>u<sub>2</sub> quadratic limb-darkening</td></tr><tr><td>D<sub>TESS</sub></td><td>1.0 (fixed)</td><td></td><td>...</td><td>Dilution factor</td></tr><tr><td>D<sub>CHEOPS</sub></td><td>1.0 (fixed)</td><td></td><td>...</td><td>Dilution factor</td></tr><tr><td colspan="5" style="text-align:center; font-weight:bold;">RV instrumental parameters</td></tr><tr><td>γ<sub>CARMENES</sub></td><td>U(-10.0, +10.0)</td><td>-0.05<sup>+0.40</sup><sub>-0.44</sub></td><td>m s<sup>-1</sup></td><td>Relative RV offset</td></tr><tr><td>γ<sub>MAROON-X,Blue,1</sub></td><td>U(-10.0, +10.0)</td><td>+1.33<sup>+0.32</sup><sub>-0.56</sub></td><td>m s<sup>-1</sup></td><td>Relative RV offset</td></tr><tr><td>γ<sub>MAROON-X,Red,1</sub></td><td>U(-10.0, +10.0)</td><td>+1.32<sup>+0.51</sup><sub>-0.53</sub></td><td>m s<sup>-1</sup></td><td>Relative RV offset</td></tr><tr><td>γ<sub>MAROON-X,Blue,2</sub></td><td>U(-10.0, +10.0)</td><td>+0.31<sup>+0.85</sup><sub>-0.80</sub></td><td>m s<sup>-1</sup></td><td>Relative RV offset</td></tr><tr><td>γ<sub>MAROON-X,Red,2</sub></td><td>U(-10.0, +10.0)</td><td>+0.28<sup>+0.84</sup><sub>-0.82</sub></td><td>m s<sup>-1</sup></td><td>Relative RV offset</td></tr><tr><td>γ<sub>MAROON-X,Blue,3</sub></td><td>U(-10.0, +10.0)</td><td>+0.1<sup>+1.2</sup><sub>-1.1</sub></td><td>m s<sup>-1</sup></td><td>Relative RV offset</td></tr><tr><td>γ<sub>MAROON-X,Red,3</sub></td><td>U(-10.0, +10.0)</td><td>+0.1<sup>+1.2</sup><sub>-1.1</sub></td><td>m s<sup>-1</sup></td><td>Relative RV offset</td></tr><tr><td>σ<sub>CARMENES</sub></td><td>LU(0.001, 5.0)</td><td>0.035<sup>+0.245</sup><sub>-0.031</sub></td><td>m s<sup>-1</sup></td><td>RV extra jitter</td></tr><tr><td>σ<sub>MAROON-X,Blue,1</sub></td><td>LU(0.001, 5.0)</td><td>0.66<sup>+0.16</sup><sub>-0.16</sub></td><td>m s<sup>-1</sup></td><td>RV extra jitter</td></tr><tr><td>σ<sub>MAROON-X,Red,1</sub></td><td>LU(0.001, 5.0)</td><td>0.136<sup>+0.124</sup><sub>-0.124</sub></td><td>m s<sup>-1</sup></td><td>RV extra jitter</td></tr><tr><td>σ<sub>MAROON-X,Blue,2</sub></td><td>LU(0.001, 5.0)</td><td>0.023<sup>+0.106</sup><sub>-0.019</sub></td><td>m s<sup>-1</sup></td><td>RV extra jitter</td></tr><tr><td>σ<sub>MAROON-X,Red,2</sub></td><td>LU(0.001, 5.0)</td><td>0.026<sup>+0.152</sup><sub>-0.022</sub></td><td>m s<sup>-1</sup></td><td>RV extra jitter</td></tr><tr><td>σ<sub>MAROON-X,Blue,3</sub></td><td>LU(0.001, 5.0)</td><td>0.017<sup>+0.093</sup><sub>-0.014</sub></td><td>m s<sup>-1</sup></td><td>RV extra jitter</td></tr><tr><td>σ<sub>MAROON-X,Red,3</sub></td><td>LU(0.001, 5.0)</td><td>0.24<sup>+0.28</sup><sub>-0.23</sub></td><td>m s<sup>-1</sup></td><td>RV extra jitter</td></tr><tr><td colspan="5" style="text-align:center; font-weight:bold;">RV quasi-periodic GP parameters</td></tr><tr><td>B<sub>GP</sub></td><td>U(0.01, 50.0)</td><td>2.21<sup>+1.26</sup><sub>-0.70</sub></td><td>m s<sup>-1</sup></td><td>GP kernel amplitude in Eq. (7)</td></tr><tr><td>C<sub>GP</sub></td><td>0.0 (fixed)</td><td></td><td>m s<sup>-1</sup></td><td>GP kernel amplitude in Eq. (7)</td></tr><tr><td>L<sub>GP</sub></td><td>LU(20, 10<sup>4</sup>)</td><td>90<sup>+126</sup><sub>-46</sub></td><td>d</td><td>GP modulation time scale</td></tr><tr><td>P<sub>tot,GP</sub></td><td>N(50.9, 10.0)</td><td>53.5<sup>+6.5</sup><sub>-4.2</sub></td><td>d</td><td>GP quasi-periodic rotation period</td></tr><tr><td colspan="5" style="text-align:center; font-weight:bold;">Planet b fitted parameters</td></tr><tr><td>P</td><td>N (1.467, 0.010)</td><td>1.4671204<sup>+0.0000011</sup><sub>-0.000011</sub></td><td>d</td><td>Orbital period</td></tr><tr><td>t<sub>0</sub></td><td>U (2459309.0, 2459311.0)</td><td>2459309.676549<sup>+0.0000097</sup><sub>-0.000096</sub></td><td>d</td><td>Time of periastron passage</td></tr><tr><td>K</td><td>U (0, 10.0)</td><td>3.512<sup>+0.069</sup><sub>-0.065</sub></td><td>m s<sup>-1</sup></td><td>RV semi-amplitude</td></tr><tr><td>r<sub>1</sub></td><td>U (0, 1.0)</td><td>0.473<sup>+0.097</sup><sub>-0.087</sub></td><td>...</td><td>Parametrisation for p and b</td></tr><tr><td>r<sub>2</sub></td><td>U (0, 1.0)</td><td>0.03635<sup>+0.00046</sup><sub>-0.00039</sub></td><td>...</td><td>Parametrisation for p and b</td></tr><tr><td>e</td><td>0.0 (fixed)</td><td></td><td>...</td><td>Orbital eccentricity</td></tr><tr><td>ω</td><td>90.0 (fixed)</td><td></td><td>deg</td><td>Periastron angle</td></tr></tbody></table>

Notes. (a) Median and upper and lower 68.3% posterior credibility intervals (1σ). The prior labels of N(μ, σ), U(a, b), and LU(a, b) represent normal (mean μ and variance σ²), uniform, and log-uniform distributions (minimum a and maximum b), respectively. The unit symbol “ppm” stands for part per million.
<table><caption>**Table A.7.** CARMENES and MAROON-X Red and Blue RVs of Gl 486.</caption><thead><tr><th>Epoch [BJD]</th><th>RV [m s<sup>-1</sup>]</th><th>Instrument</th></tr></thead><tbody><tr><td>2457400.7408</td><td>4.54 ± 1.07</td><td>CARMENES</td></tr><tr><td>2457401.7424</td><td>0.30 ± 1.31</td><td>CARMENES</td></tr><tr><td>2457418.7185</td><td>-2.23 ± 1.14</td><td>CARMENES</td></tr><tr><td>2457421.7051</td><td>-2.64 ± 0.98</td><td>CARMENES</td></tr><tr><td>2457426.6930</td><td>0.95 ± 1.13</td><td>CARMENES</td></tr><tr><td>2457442.6029</td><td>-2.87 ± 0.86</td><td>CARMENES</td></tr><tr><td>2457442.6266</td><td>-3.36 ± 0.87</td><td>CARMENES</td></tr><tr><td>2457476.5198</td><td>-2.92 ± 1.34</td><td>CARMENES</td></tr><tr><td>2457492.5344</td><td>-1.43 ± 1.63</td><td>CARMENES</td></tr><tr><td>2457503.4564</td><td>4.59 ± 1.45</td><td>CARMENES</td></tr><tr><td>2457509.4726</td><td>2.40 ± 1.48</td><td>CARMENES</td></tr><tr><td>2457534.4649</td><td>-0.36 ± 1.36</td><td>CARMENES</td></tr><tr><td>2457540.4090</td><td>-5.90 ± 1.13</td><td>CARMENES</td></tr><tr><td>2457756.7349</td><td>0.47 ± 1.70</td><td>CARMENES</td></tr><tr><td>2457788.5215</td><td>-0.34 ± 2.18</td><td>CARMENES</td></tr><tr><td>2457856.5321</td><td>3.22 ± 1.12</td><td>CARMENES</td></tr><tr><td>2457876.5383</td><td>-4.27 ± 0.99</td><td>CARMENES</td></tr><tr><td>2457896.4260</td><td>4.58 ± 1.02</td><td>CARMENES</td></tr><tr><td>2457950.3699</td><td>2.62 ± 1.34</td><td>CARMENES</td></tr><tr><td>2458122.6935</td><td>0.60 ± 1.35</td><td>CARMENES</td></tr><tr><td>2458141.5892</td><td>2.07 ± 1.14</td><td>CARMENES</td></tr><tr><td>2458206.5718</td><td>0.83 ± 0.90</td><td>CARMENES</td></tr><tr><td>2458271.4803</td><td>-2.26 ± 1.06</td><td>CARMENES</td></tr><tr><td>2458479.6821</td><td>-3.15 ± 1.13</td><td>CARMENES</td></tr><tr><td>2458486.6141</td><td>0.14 ± 1.20</td><td>CARMENES</td></tr><tr><td>2458488.6993</td><td>-2.42 ± 1.18</td><td>CARMENES</td></tr><tr><td>2458489.7108</td><td>-3.01 ± 1.11</td><td>CARMENES</td></tr><tr><td>2458490.6323</td><td>2.89 ± 1.17</td><td>CARMENES</td></tr><tr><td>2458491.7067</td><td>-0.20 ± 1.05</td><td>CARMENES</td></tr><tr><td>2458494.6815</td><td>2.09 ± 1.69</td><td>CARMENES</td></tr><tr><td>2458499.6401</td><td>2.35 ± 1.09</td><td>CARMENES</td></tr><tr><td>2458518.7245</td><td>-0.60 ± 1.80</td><td>CARMENES</td></tr><tr><td>2458529.5825</td><td>-0.18 ± 1.13</td><td>CARMENES</td></tr><tr><td>2458532.6604</td><td>-0.68 ± 1.11</td><td>CARMENES</td></tr><tr><td>2458533.6123</td><td>3.24 ± 1.04</td><td>CARMENES</td></tr><tr><td>2458535.6238</td><td>0.45 ± 0.90</td><td>CARMENES</td></tr><tr><td>2458538.6682</td><td>1.40 ± 1.06</td><td>CARMENES</td></tr><tr><td>2458539.6400</td><td>-1.27 ± 0.92</td><td>CARMENES</td></tr><tr><td>2458546.6438</td><td>3.41 ± 0.84</td><td>CARMENES</td></tr><tr><td>2458560.5388</td><td>-0.67 ± 1.14</td><td>CARMENES</td></tr><tr><td>2458603.5434</td><td>4.53 ± 1.05</td><td>CARMENES</td></tr><tr><td>2458657.4196</td><td>0.34 ± 1.29</td><td>CARMENES</td></tr><tr><td>2458846.6448</td><td>-0.41 ± 1.00</td><td>CARMENES</td></tr><tr><td>2458860.7078</td><td>-2.39 ± 1.12</td><td>CARMENES</td></tr><tr><td>2458882.7191</td><td>-0.73 ± 1.00</td><td>CARMENES</td></tr><tr><td>2458890.7176</td><td>-3.01 ± 1.23</td><td>CARMENES</td></tr><tr><td>2458895.6557</td><td>3.03 ± 1.13</td><td>CARMENES</td></tr><tr><td>2458898.6498</td><td>2.72 ± 1.55</td><td>CARMENES</td></tr><tr><td>2458904.5999</td><td>0.28 ± 1.38</td><td>CARMENES</td></tr><tr><td>2458913.5773</td><td>-1.90 ± 1.08</td><td>CARMENES</td></tr><tr><td>2458914.6471</td><td>6.70 ± 2.05</td><td>CARMENES</td></tr><tr><td>2458916.6478</td><td>-2.20 ± 1.24</td><td>CARMENES</td></tr><tr><td>2458917.5559</td><td>-1.36 ± 1.12</td><td>CARMENES</td></tr><tr><td>2458922.5444</td><td>-1.26 ± 1.43</td><td>CARMENES</td></tr><tr><td>2458977.4310</td><td>-2.00 ± 1.18</td><td>CARMENES</td></tr><tr><td>2458977.4495</td><td>-0.35 ± 0.99</td><td>CARMENES</td></tr><tr><td>2458982.5408</td><td>-3.28 ± 1.27</td><td>CARMENES</td></tr><tr><td>2458988.3860</td><td>-2.40 ± 1.22</td><td>CARMENES</td></tr><tr><td>2458989.3933</td><td>1.78 ± 1.20</td><td>CARMENES</td></tr></tbody></table>

<table><caption>**Table A.7.** CARMENES and MAROON-X Red and Blue RVs of Gl 486. (cont.)</caption><thead><tr><th>Epoch [BJD]</th><th>RV [m s<sup>-1</sup>]</th><th>Instrument</th></tr></thead><tbody><tr><td>2458989.7470</td><td>3.30 ± 1.01</td><td>MAROON-X Blue</td></tr><tr><td>2458989.7470</td><td>1.74 ± 0.46</td><td>MAROON-X Red</td></tr><tr><td>2458989.7518</td><td>1.72 ± 0.86</td><td>MAROON-X Blue</td></tr><tr><td>2458989.7518</td><td>1.37 ± 0.40</td><td>MAROON-X Red</td></tr><tr><td>2458991.3867</td><td>-0.40 ± 1.40</td><td>CARMENES</td></tr><tr><td>2458991.8256</td><td>-2.75 ± 0.77</td><td>MAROON-X Blue</td></tr><tr><td>2458991.8256</td><td>-2.38 ± 0.40</td><td>MAROON-X Red</td></tr><tr><td>2458991.8304</td><td>-3.37 ± 0.84</td><td>MAROON-X Blue</td></tr><tr><td>2458991.8304</td><td>-1.98 ± 0.34</td><td>MAROON-X Red</td></tr><tr><td>2458992.3627</td><td>1.62 ± 1.13</td><td>CARMENES</td></tr><tr><td>2458992.8542</td><td>-1.55 ± 0.87</td><td>MAROON-X Blue</td></tr><tr><td>2458992.8542</td><td>-0.58 ± 0.27</td><td>MAROON-X Red</td></tr><tr><td>2458992.8588</td><td>-2.59 ± 0.82</td><td>MAROON-X Blue</td></tr><tr><td>2458992.8589</td><td>-1.02 ± 0.40</td><td>MAROON-X Red</td></tr><tr><td>2458993.8281</td><td>4.19 ± 1.13</td><td>MAROON-X Blue</td></tr><tr><td>2458993.8281</td><td>4.14 ± 0.30</td><td>MAROON-X Red</td></tr><tr><td>2458993.8328</td><td>2.99 ± 1.01</td><td>MAROON-X Blue</td></tr><tr><td>2458993.8328</td><td>4.17 ± 0.46</td><td>MAROON-X Red</td></tr><tr><td>2458994.3965</td><td>-2.45 ± 1.09</td><td>CARMENES</td></tr><tr><td>2458994.4854</td><td>-2.35 ± 1.02</td><td>CARMENES</td></tr><tr><td>2458994.7798</td><td>-2.56 ± 1.68</td><td>MAROON-X Blue</td></tr><tr><td>2458994.7799</td><td>-2.26 ± 0.72</td><td>MAROON-X Red</td></tr><tr><td>2458994.7881</td><td>-0.61 ± 0.76</td><td>MAROON-X Blue</td></tr><tr><td>2458994.7881</td><td>-1.73 ± 0.38</td><td>MAROON-X Red</td></tr><tr><td>2458994.7964</td><td>-2.06 ± 1.24</td><td>MAROON-X Blue</td></tr><tr><td>2458994.7964</td><td>-1.82 ± 0.52</td><td>MAROON-X Red</td></tr><tr><td>2458994.8051</td><td>-1.34 ± 0.72</td><td>MAROON-X Blue</td></tr><tr><td>2458994.8051</td><td>-1.95 ± 0.32</td><td>MAROON-X Red</td></tr><tr><td>2458995.7759</td><td>-0.32 ± 0.57</td><td>MAROON-X Blue</td></tr><tr><td>2458995.7759</td><td>-1.09 ± 0.34</td><td>MAROON-X Red</td></tr><tr><td>2458995.7843</td><td>-1.22 ± 0.70</td><td>MAROON-X Blue</td></tr><tr><td>2458995.7843</td><td>-0.76 ± 0.28</td><td>MAROON-X Red</td></tr><tr><td>2458995.7925</td><td>-0.49 ± 0.73</td><td>MAROON-X Blue</td></tr><tr><td>2458995.7925</td><td>-0.91 ± 0.26</td><td>MAROON-X Red</td></tr><tr><td>2458995.8006</td><td>-1.00 ± 0.52</td><td>MAROON-X Blue</td></tr><tr><td>2458995.8007</td><td>-1.02 ± 0.23</td><td>MAROON-X Red</td></tr><tr><td>2458996.7696</td><td>3.05 ± 3.49</td><td>MAROON-X Blue</td></tr><tr><td>2458996.7696</td><td>2.82 ± 1.16</td><td>MAROON-X Red</td></tr><tr><td>2458996.7854</td><td>3.26 ± 1.69</td><td>MAROON-X Blue</td></tr><tr><td>2458996.7854</td><td>2.87 ± 0.70</td><td>MAROON-X Red</td></tr><tr><td>2458996.7940</td><td>1.67 ± 1.88</td><td>MAROON-X Blue</td></tr><tr><td>2458996.7940</td><td>3.16 ± 0.64</td><td>MAROON-X Red</td></tr><tr><td>2458997.3604</td><td>-4.19 ± 1.60</td><td>CARMENES</td></tr><tr><td>2458997.5000</td><td>-5.62 ± 1.55</td><td>CARMENES</td></tr><tr><td>2458997.8482</td><td>2.12 ± 1.15</td><td>MAROON-X Blue</td></tr><tr><td>2458997.8482</td><td>-0.29 ± 0.38</td><td>MAROON-X Red</td></tr><tr><td>2458997.8530</td><td>1.48 ± 1.02</td><td>MAROON-X Blue</td></tr><tr><td>2458997.8530</td><td>-0.14 ± 0.39</td><td>MAROON-X Red</td></tr><tr><td>2458997.8596</td><td>-0.47 ± 0.81</td><td>MAROON-X Blue</td></tr><tr><td>2458997.8597</td><td>-1.20 ± 0.22</td><td>MAROON-X Red</td></tr><tr><td>2458997.8679</td><td>-0.51 ± 0.73</td><td>MAROON-X Blue</td></tr><tr><td>2458997.8679</td><td>-0.08 ± 0.31</td><td>MAROON-X Red</td></tr><tr><td>2458997.8761</td><td>-1.09 ± 0.77</td><td>MAROON-X Blue</td></tr><tr><td>2458997.8761</td><td>-0.29 ± 0.31</td><td>MAROON-X Red</td></tr><tr><td>2458997.8843</td><td>-0.43 ± 0.98</td><td>MAROON-X Blue</td></tr><tr><td>2458997.8843</td><td>0.21 ± 0.42</td><td>MAROON-X Red</td></tr><tr><td>2458998.4178</td><td>1.46 ± 1.30</td><td>CARMENES</td></tr><tr><td>2458998.8379</td><td>-2.14 ± 1.01</td><td>MAROON-X Blue</td></tr><tr><td>2458998.8379</td><td>-2.48 ± 0.41</td><td>MAROON-X Red</td></tr><tr><td>2458998.8426</td><td>-0.18 ± 1.05</td><td>MAROON-X Blue</td></tr></tbody></table>
<table><caption>**Table A.7.** CARMENES and MAROON-X Red and Blue RVs of Gl 486. (cont.)</caption><thead><tr><th>Epoch [BJD]</th><th>RV [m s<sup>-1</sup>]</th><th>Instrument</th></tr></thead><tbody><tr><td>2458998.8426</td><td>-2.95 ± 0.56</td><td>MAROON-X Red</td></tr><tr><td>2458998.8473</td><td>-0.74 ± 0.77</td><td>MAROON-X Blue</td></tr><tr><td>2458998.8473</td><td>-2.88 ± 0.45</td><td>MAROON-X Red</td></tr><tr><td>2458998.8520</td><td>-1.95 ± 1.02</td><td>MAROON-X Blue</td></tr><tr><td>2458998.8520</td><td>-2.06 ± 0.50</td><td>MAROON-X Red</td></tr><tr><td>2458998.8567</td><td>-1.04 ± 0.96</td><td>MAROON-X Blue</td></tr><tr><td>2458998.8568</td><td>-2.44 ± 0.47</td><td>MAROON-X Red</td></tr><tr><td>2458998.8640</td><td>-3.86 ± 0.96</td><td>MAROON-X Blue</td></tr><tr><td>2458998.8640</td><td>-3.15 ± 0.27</td><td>MAROON-X Red</td></tr><tr><td>2458998.8722</td><td>-2.99 ± 0.52</td><td>MAROON-X Blue</td></tr><tr><td>2458998.8723</td><td>-3.07 ± 0.26</td><td>MAROON-X Red</td></tr><tr><td>2458999.4116</td><td>-0.75 ± 1.19</td><td>CARMENES</td></tr><tr><td>2458999.7788</td><td>5.45 ± 0.88</td><td>MAROON-X Blue</td></tr><tr><td>2458999.7788</td><td>4.30 ± 0.51</td><td>MAROON-X Red</td></tr><tr><td>2458999.7835</td><td>6.35 ± 0.80</td><td>MAROON-X Blue</td></tr><tr><td>2458999.7835</td><td>2.93 ± 0.64</td><td>MAROON-X Red</td></tr><tr><td>2458999.7883</td><td>6.62 ± 1.06</td><td>MAROON-X Blue</td></tr><tr><td>2458999.7883</td><td>4.03 ± 0.48</td><td>MAROON-X Red</td></tr><tr><td>2458999.7948</td><td>3.11 ± 0.59</td><td>MAROON-X Blue</td></tr><tr><td>2458999.7948</td><td>2.75 ± 0.19</td><td>MAROON-X Red</td></tr><tr><td>2458999.8997</td><td>2.03 ± 1.10</td><td>MAROON-X Blue</td></tr><tr><td>2458999.8997</td><td>2.73 ± 0.41</td><td>MAROON-X Red</td></tr><tr><td>2458999.9085</td><td>1.61 ± 0.82</td><td>MAROON-X Blue</td></tr><tr><td>2458999.9086</td><td>2.21 ± 0.39</td><td>MAROON-X Red</td></tr><tr><td>2458999.9167</td><td>0.42 ± 0.90</td><td>MAROON-X Blue</td></tr><tr><td>2458999.9167</td><td>2.44 ± 0.30</td><td>MAROON-X Red</td></tr><tr><td>2459000.4649</td><td>-4.87 ± 0.96</td><td>CARMENES</td></tr><tr><td>2459000.7624</td><td>-0.55 ± 0.78</td><td>MAROON-X Blue</td></tr><tr><td>2459000.7624</td><td>-0.29 ± 0.39</td><td>MAROON-X Red</td></tr><tr><td>2459000.7671</td><td>-1.32 ± 0.75</td><td>MAROON-X Blue</td></tr><tr><td>2459000.7672</td><td>-0.70 ± 0.39</td><td>MAROON-X Red</td></tr><tr><td>2459000.7719</td><td>-1.73 ± 0.47</td><td>MAROON-X Blue</td></tr><tr><td>2459000.7719</td><td>-0.68 ± 0.34</td><td>MAROON-X Red</td></tr><tr><td>2459000.7767</td><td>-0.33 ± 0.62</td><td>MAROON-X Blue</td></tr><tr><td>2459000.7767</td><td>-1.13 ± 0.34</td><td>MAROON-X Red</td></tr><tr><td>2459000.7815</td><td>0.36 ± 0.58</td><td>MAROON-X Blue</td></tr><tr><td>2459000.7815</td><td>-1.70 ± 0.40</td><td>MAROON-X Red</td></tr><tr><td>2459000.8668</td><td>-0.92 ± 0.55</td><td>MAROON-X Blue</td></tr><tr><td>2459000.8668</td><td>0.51 ± 0.35</td><td>MAROON-X Red</td></tr><tr><td>2459000.8715</td><td>-0.64 ± 0.78</td><td>MAROON-X Blue</td></tr><tr><td>2459000.8715</td><td>0.09 ± 0.32</td><td>MAROON-X Red</td></tr><tr><td>2459000.8762</td><td>-0.39 ± 0.68</td><td>MAROON-X Blue</td></tr><tr><td>2459000.8762</td><td>0.14 ± 0.33</td><td>MAROON-X Red</td></tr><tr><td>2459000.8809</td><td>0.29 ± 0.78</td><td>MAROON-X Blue</td></tr><tr><td>2459000.8809</td><td>0.17 ± 0.25</td><td>MAROON-X Red</td></tr><tr><td>2459000.8856</td><td>-0.28 ± 0.79</td><td>MAROON-X Blue</td></tr><tr><td>2459000.8856</td><td>0.68 ± 0.42</td><td>MAROON-X Red</td></tr><tr><td>2459001.7450</td><td>-1.86 ± 0.83</td><td>MAROON-X Blue</td></tr><tr><td>2459001.7450</td><td>-2.16 ± 0.36</td><td>MAROON-X Red</td></tr><tr><td>2459001.7497</td><td>-2.17 ± 0.50</td><td>MAROON-X Blue</td></tr><tr><td>2459001.7497</td><td>-2.44 ± 0.36</td><td>MAROON-X Red</td></tr><tr><td>2459001.7544</td><td>-2.89 ± 0.77</td><td>MAROON-X Blue</td></tr><tr><td>2459001.7544</td><td>-2.37 ± 0.26</td><td>MAROON-X Red</td></tr><tr><td>2459001.7592</td><td>-1.99 ± 0.74</td><td>MAROON-X Blue</td></tr><tr><td>2459001.7592</td><td>-2.38 ± 0.24</td><td>MAROON-X Red</td></tr><tr><td>2459001.7639</td><td>-3.07 ± 0.86</td><td>MAROON-X Blue</td></tr><tr><td>2459001.7639</td><td>-2.45 ± 0.32</td><td>MAROON-X Red</td></tr><tr><td>2459001.8838</td><td>-3.06 ± 1.08</td><td>MAROON-X Blue</td></tr><tr><td>2459001.8838</td><td>-3.45 ± 0.50</td><td>MAROON-X Red</td></tr><tr><td>2459001.8920</td><td>-5.07 ± 1.34</td><td>MAROON-X Blue</td></tr></tbody></table>

<table><caption>**Table A.7.** CARMENES and MAROON-X Red and Blue RVs of Gl 486. (cont.)</caption><thead><tr><th>Epoch [BJD]</th><th>RV [m s<sup>-1</sup>]</th><th>Instrument</th></tr></thead><tbody><tr><td>2459001.8920</td><td>-3.37 ± 0.61</td><td>MAROON-X Red</td></tr><tr><td>2459001.9002</td><td>-3.55 ± 0.55</td><td>MAROON-X Red</td></tr><tr><td>2459001.9002</td><td>-4.57 ± 1.15</td><td>MAROON-X Blue</td></tr><tr><td>2459002.7483</td><td>2.58 ± 0.72</td><td>MAROON-X Blue</td></tr><tr><td>2459002.7483</td><td>3.97 ± 0.33</td><td>MAROON-X Red</td></tr><tr><td>2459002.7533</td><td>2.98 ± 0.85</td><td>MAROON-X Blue</td></tr><tr><td>2459002.7533</td><td>3.85 ± 0.28</td><td>MAROON-X Red</td></tr><tr><td>2459002.7580</td><td>2.41 ± 1.01</td><td>MAROON-X Blue</td></tr><tr><td>2459002.7580</td><td>3.16 ± 0.42</td><td>MAROON-X Red</td></tr><tr><td>2459002.7627</td><td>2.59 ± 0.64</td><td>MAROON-X Blue</td></tr><tr><td>2459002.7627</td><td>3.36 ± 0.41</td><td>MAROON-X Red</td></tr><tr><td>2459002.7674</td><td>1.58 ± 0.64</td><td>MAROON-X Blue</td></tr><tr><td>2459002.7675</td><td>3.58 ± 0.39</td><td>MAROON-X Red</td></tr><tr><td>2459002.9258</td><td>1.43 ± 0.66</td><td>MAROON-X Blue</td></tr><tr><td>2459002.9258</td><td>1.52 ± 0.38</td><td>MAROON-X Red</td></tr><tr><td>2459002.9340</td><td>1.22 ± 0.98</td><td>MAROON-X Blue</td></tr><tr><td>2459002.9340</td><td>1.24 ± 0.39</td><td>MAROON-X Red</td></tr><tr><td>2459002.9422</td><td>1.24 ± 0.76</td><td>MAROON-X Blue</td></tr><tr><td>2459002.9422</td><td>1.05 ± 0.40</td><td>MAROON-X Red</td></tr><tr><td>2459003.3624</td><td>-5.60 ± 1.06</td><td>CARMENES</td></tr><tr><td>2459004.3623</td><td>1.99 ± 1.01</td><td>CARMENES</td></tr><tr><td>2459006.3599</td><td>-4.85 ± 1.22</td><td>CARMENES</td></tr><tr><td>2459007.4041</td><td>-1.25 ± 1.24</td><td>CARMENES</td></tr><tr><td>2459008.3969</td><td>0.61 ± 1.03</td><td>CARMENES</td></tr><tr><td>2459009.4312</td><td>-5.33 ± 1.63</td><td>CARMENES</td></tr><tr><td>2459011.4080</td><td>3.01 ± 1.56</td><td>CARMENES</td></tr><tr><td>2459013.4340</td><td>-1.65 ± 2.51</td><td>CARMENES</td></tr><tr><td>2459320.9034</td><td>2.60 ± 0.28</td><td>MAROON-X Red</td></tr><tr><td>2459320.9034</td><td>2.87 ± 0.45</td><td>MAROON-X Blue</td></tr><tr><td>2459321.9053</td><td>-3.40 ± 0.77</td><td>MAROON-X Blue</td></tr><tr><td>2459321.9053</td><td>-3.09 ± 0.43</td><td>MAROON-X Red</td></tr><tr><td>2459322.9380</td><td>-1.41 ± 0.43</td><td>MAROON-X Blue</td></tr><tr><td>2459322.9380</td><td>-1.34 ± 0.26</td><td>MAROON-X Red</td></tr><tr><td>2459323.9374</td><td>2.77 ± 0.41</td><td>MAROON-X Blue</td></tr><tr><td>2459323.9374</td><td>2.83 ± 0.25</td><td>MAROON-X Red</td></tr><tr><td>2459324.4943</td><td>-1.78 ± 2.07</td><td>CARMENES</td></tr><tr><td>2459324.9834</td><td>-2.19 ± 0.29</td><td>MAROON-X Red</td></tr><tr><td>2459324.9834</td><td>-2.31 ± 0.53</td><td>MAROON-X Blue</td></tr><tr><td>2459326.8671</td><td>3.75 ± 0.34</td><td>MAROON-X Red</td></tr><tr><td>2459326.8671</td><td>3.25 ± 0.57</td><td>MAROON-X Blue</td></tr><tr><td>2459333.9089</td><td>0.22 ± 0.28</td><td>MAROON-X Red</td></tr><tr><td>2459333.9089</td><td>-0.08 ± 0.44</td><td>MAROON-X Blue</td></tr><tr><td>2459334.8828</td><td>-3.97 ± 0.27</td><td>MAROON-X Red</td></tr><tr><td>2459334.8828</td><td>-3.04 ± 0.42</td><td>MAROON-X Blue</td></tr><tr><td>2459336.4953</td><td>-4.97 ± 2.44</td><td>CARMENES</td></tr><tr><td>2459338.6370</td><td>4.49 ± 2.35</td><td>CARMENES</td></tr><tr><td>2459339.3986</td><td>-6.48 ± 1.59</td><td>CARMENES</td></tr><tr><td>2459341.5781</td><td>4.76 ± 1.62</td><td>CARMENES</td></tr><tr><td>2459359.8366</td><td>-2.51 ± 0.41</td><td>MAROON-X Blue</td></tr><tr><td>2459359.8366</td><td>-2.76 ± 0.23</td><td>MAROON-X Red</td></tr><tr><td>2459360.8735</td><td>3.38 ± 0.63</td><td>MAROON-X Blue</td></tr><tr><td>2459360.8735</td><td>3.71 ± 0.32</td><td>MAROON-X Red</td></tr><tr><td>2459361.8787</td><td>1.69 ± 0.50</td><td>MAROON-X Blue</td></tr><tr><td>2459361.8787</td><td>1.84 ± 0.26</td><td>MAROON-X Red</td></tr><tr><td>2459362.8904</td><td>-3.57 ± 0.48</td><td>MAROON-X Blue</td></tr><tr><td>2459362.8904</td><td>-4.02 ± 0.24</td><td>MAROON-X Red</td></tr><tr><td>2459363.8239</td><td>1.89 ± 0.41</td><td>MAROON-X Blue</td></tr><tr><td>2459363.8239</td><td>1.30 ± 0.24</td><td>MAROON-X Red</td></tr><tr><td>2459364.9516</td><td>3.01 ± 0.27</td><td>MAROON-X Red</td></tr><tr><td>2459364.9516</td><td>3.05 ± 0.94</td><td>MAROON-X Blue</td></tr></tbody></table>
<table><caption>**Table A.7.** CARMENES and MAROON-X Red and Blue RVs of Gl 486. (cont.)</caption><thead><tr><th>Epoch [BJD]</th><th>RV [m s<sup>-1</sup>]</th><th>Instrument</th></tr></thead><tbody><tr><td>2459365.9122</td><td>-3.64 ± 0.69</td><td>MAROON-X Blue</td></tr><tr><td>2459365.9122</td><td>-3.26 ± 0.32</td><td>MAROON-X Red</td></tr><tr><td>2459367.8489</td><td>1.75 ± 0.47</td><td>MAROON-X Blue</td></tr><tr><td>2459367.8489</td><td>1.88 ± 0.26</td><td>MAROON-X Red</td></tr></tbody></table>
# Appendix B: Sources of error and propagation of uncertainty

## Appendix B.1: Planet radius and mass

Gl 486 b is among the smallest and least massive transiting planets, and among the ones with the smallest relative uncertainties in both radius and, especially, mass. However, there are even smaller and less massive planets (e.g. in the TRAPPIST-1 system), which have smaller reported relative uncertainties. Planets with very small reported uncertainties orbit eclipsing binary stars (with precise and accurate $R_\star$ and $M_\star$ determinations) or suffer from incorrect error propagation. This is illustrated in the $\delta R_p-R_p$ and $\delta M_p-M_p$ diagrams in Fig. B.1.

With $(R_{\text{core}}/R_p)_{\text{MRA-SH}} = 0.404^{+0.040}_{-0.045}$ in Gl 486 b, we reached the 10% precision boundary on the core-to-mantle ratio of a telluric exoplanet. Breaking this precision boundary will give rise to planet internal composition studies not done before. However, in order to obtain a precision better than 10% on the core-to-mantle ratio of a terrestrial exoplanet (actually, the “core radius fraction”), it is required a measurement of the mass better than 11% and a measurement on the radius better than 3% (Suissa et al. 2018). The approximate uncertainty ratio of three-to-one is also applied to the planet bulk density. From the sphere density formula, the uncertainty in planet radius $R_p$ contributes three times more to the final error of planet bulk density $\rho_p$ than the uncertainty in planet mass $M_p$:

$$ \rho_p = \frac{3M_p}{4\pi R_p^3}, \qquad (B.1) $$

and:

$$ \left(\frac{\delta \rho_p}{\rho_p}\right)^2 = \left(\frac{\delta M_p}{M_p}\right)^2 + \left(\frac{3\delta R_p}{R_p}\right)^2. \qquad (B.2) $$

For Gl 486 b, the measured relative uncertainties in planet radius and mass translate into a bulk density relative uncertainty of 9.3%, which allowed to determine its internal composition and structure. In our case, we fitted the $r_1$ and $r_2$ parameters, from which we derived the radius ratio, $p$, and impact parameter, $b$ (Espinoza et al. 2019). The planet radius comes from the simple definition of $p$:

$$ R_p = p R_\star, \qquad (B.3) $$

and its uncertainty is, therefore:

$$ \left(\frac{\delta R_p}{R_p}\right)^2 = \left(\frac{\delta p}{p}\right)^2 + \left(\frac{\delta R_\star}{R_\star}\right)^2. \qquad (B.4) $$

As a result, the relative uncertainty in $R_p$ can never be smaller than that in $R_\star$. For Gl 486 b, $p = 0.03644^{+0.00048}_{-0.00042}$, the relative error in $p$ is very small, and, therefore, $\delta R_p/R_p \approx \delta R_\star/R_\star$. Actually, from Sect. 4.5, the derived planet radius is $R_b = 1.343^{+0.063}_{-0.062} R_\oplus$, which represents a relative uncertainty of 4.7% and is very similar to the relative uncertainty of the stellar radius, at 4.5%. The small difference of 0.2% through the $p$ parameter is mostly due to the quality of the TESS and CHEOPS transit data.

The derivation of the relative uncertainty in $M_p$ is, a priori, more complicated and highly non-linear. From the definition of the RV semi-amplitude:

$$ K = \frac{1}{(1 - e^2)^{1/2}} \frac{M_p \sin i}{(M_p + M_\star)^{2/3}} \left(\frac{2\pi G}{P}\right)^{1/3}, \qquad (B.5) $$

it can be deduced the following:

$$ \frac{M_p}{(M_p + M_\star)^{2/3}} = \mathcal{H}(P, K, i, e), \qquad (B.6) $$

$$ \mathcal{H}(P, K, i, e) = (1 - e^2)^{1/2} \frac{K}{\sin i} \left( \frac{P}{2\pi G} \right)^{1/3}, \qquad (B.7) $$

where $P$, $K$, and $e$ are fitted parameters, $i$ is a derived parameter, and $M_\star$ is an input parameter. Nevertheless, in most cases it happens that $M_\star \gg M_p$. For example, for Gl 486 b, the ratio between planet and star masses is about $2.7 \times 10^{-5}$, which justifies the following approximation:

$$ M_p \approx M_\star^{2/3} \mathcal{H}(P, K, i, e). \qquad (B.8) $$

As a result, the uncertainty in planet mass becomes:

$$ (\delta M_p)^2 \approx \left(\frac{2\mathcal{H}}{3M_\star^{1/3}}\right)^2 \delta^2 M_\star + \left(\frac{\partial\mathcal{H}}{\partial P}\right)^2 \delta^2 P + \left(\frac{\partial\mathcal{H}}{\partial K}\right)^2 \delta^2 K + \left(\frac{\partial\mathcal{H}}{\partial i}\right)^2 \delta^2 i + \left(\frac{\partial\mathcal{H}}{\partial e}\right)^2 \delta^2 e. \qquad (B.9) $$

When the uncertainty in $M_\star$ dominates the global error contribution with respect to $P$, $K$, $i$, and $e$, as in the case of typical observations with CARMENES+MAROON-X or ESPRESSO, the latter equation remains just:

$$ \frac{\delta M_p}{M_p} \approx \frac{2\delta M_\star}{3M_\star}. \qquad (B.10) $$

From Sect. 4.5, the derived planet mass is $M_b = 3.00^{+0.13}_{-0.13} M_\oplus$, which represents a relative uncertainty of 4.2%, and is about two thirds of the relative uncertainty of the stellar mass, at 5.6%. The small difference of 0.4% through the $P$, $K$, and $i$ (and $e$) parameters is, in this case, mostly due to the quality of the CARMENES and MAROON-X RV data, some of them with sub-metre-per-second precision.

Fig. B.2 illustrates these computations. The majority of confirmed planets fall on or above the 1:1 radius relative error ratio in the $\delta R_p/R_p$ vs. $\delta R_\star/R_\star$ diagram (left panel) and on or above the 2:3 mass relative error ratio in the $\delta M_p/M_p$ vs. $\delta M_\star/M_\star$ diagram. Gl 486 b, displayed in both panels of Fig. B.2 with a black filled star, has radius and mass determinations near, but slightly above, the empirical boundaries at $\delta R_p/R_p \sim \delta R_\star/R_\star$ and $\delta M_p/M_p \sim 2\delta M_\star/3M_\star$. The outliers with $\delta R_p/R_p \ll \delta R_\star/R_\star$ (Wendelstein 1 b and 2 b, Obermeier et al. 2020; CoRoT-27 b, Parviainen et al. 2014; and Kepler-30 b, c and d, Sanchís-Ojeda et al. 2012) and $\delta M_p/M_p \ll$
<figure><img src="image_22.png" /><figcaption>**Fig. B.1.** Uncertainty in radius versus radius (**left**) and uncertainty in mass versus mass (**right**) of all transiting exoplanets with mass determination (from RV or transit time variations). The symbol colour denotes the stellar host effective temperature, while the symbol size is proportional to mass and radius, respectively. Diagonal dashed lines indicate lines of constant relative uncertainty (1, 2, 5, 10, 20, 50%). Gl 486 b is marked with a black star in both panels. Only in the right panel, the grey vertical dotted line marks the deutonium burning mass limit. The planets with $\delta R_p/R_p$ ratios less than 1% (left panel) are Kepler-16 b ($R_p = 8.448^{+0.028}_{-0.026} R_⊕$), a Saturn-size circumbinary planet around a eclipsing binary with both precise and accurate stellar mass and radius determination (Doyle et al. 2011), HATS-72 b ($R_p = 8.097 \pm 0.036 R_⊕$), whose stellar host is a K dwarf with a questionable tabulated relative radius uncertainty of merely 0.29% (Hartman et al. 2020), and Wendelstein-1 b ($R_p = 11.561 \pm 0.068 R_⊕$), for which the uncertainty in the stellar radius was not correctly propagated (Obermeier et al. 2020). The planet with $\delta M_p/M_p$ ratio less than 1% (right panel) is TIC 172900988 b ($M_p = 942.0 \pm 5.6 M_⊕$) for one of the six possible model solutions), a Jupiter-size circumbinary planet around another eclipsing binary (Kostov et al. 2021).</figcaption></figure>

$\delta M_*/M_*$ (BD+46 2629A b = Kepler-13 b, Esteves et al. 2015; and LTT 9779 b, Jenkins et al. 2020) suffered again from incorrect error propagation. For example, Sanchís-Ojeda et al. (2012) tabulated 3.9 ± 0.2, 12.3 ± 0.4, and 8.8 ± 0.5 $R_⊕$ for planets b, c, and d in the Kepler-30 system but, from their $R_*$ and $\Delta = (R_p/R_*)^2$ and the SI values for $R_⊙$ and $R_⊕$, we determined instead 4.21 ± 0.54, 13.2 ± 1.7, and 9.4 ± 1.2 $R_⊕$, respectively<fnref n="28" />.

## Appendix B.2: Stellar radius and mass

While we break by a wide margin the planet mass boundary of Suissa et al. (2018) for internal composition studies at 11%, we get very close to break the planet radius boundary at 3%. The space photometry and RV spectroscopy add only 0.2% and 0.4% extra uncertainty to the fit, respectively, so we are in the case of planet parameters limited by the stellar parameter uncertainties, especially the stellar radius. In our case, this problem is partially alleviated by our accurate interferometric measurements. We analyse below the sources of limiting errors in determining stellar parameters, apart from improvements in RV and transit photometry precision and systematics correction.

We computed the stellar mass $M_*$ from the stellar radius $R_*$ with the linear mass-radius relation of Schweitzer et al. (2019):

$$M_* = \alpha + \beta R_* \quad (B.11)$$

where $\alpha = -0.0240 \pm 0.0076 M_⊙$, $\beta = 1.055 \pm 0.017 M_⊙ R_⊙^{-1}$, and $R_*$ is expressed in solar units (Sect. 2 – we use $\alpha$, $\beta$ instead of $a$, $b$ as in the original work for avoiding confusion with $p$, $b$ juliet parameters). From this relation, the uncertainty in stellar mass is, therefore:

$$(\delta M_*)^2 = (\delta\alpha)^2 + (\delta\beta R_*)^2 + (\beta \delta R_*)^2. \quad (B.12)$$

In our case, we determined the stellar radius with near-infrared interferometric measurements with MIRC-X at the CHARA Array (Sects. 3.3 and 4.1). In particular, $R_{*,interf}$ is a simple function of the stellar angular diameter, $\theta$, and the parallax, $\omega$, or, alternative, the parallactic distance, $d$:

$$R_{*,interf} = \frac{\theta}{2\omega} = \frac{\theta}{2}d, \quad (B.13)$$

and the corresponding relative uncertainty is:

$$\left(\frac{\delta R_{*,interf}}{R_{*,interf}}\right)^2 = \left(\frac{\delta\theta}{\theta}\right)^2 + \left(\frac{\delta\omega}{\omega}\right)^2 = \left(\frac{\delta\theta}{\theta}\right)^2 + \left(\frac{\delta d}{d}\right)^2. \quad (B.14)$$

To sum up, the uncertainty in stellar mass from an interferometric stellar radius becomes:

$$(\delta M_{*,interf})^2 = (\delta\alpha)^2 + \beta^2 R_{*,interf}^2 \\ \times \left(\left(\frac{\delta\beta}{\beta}\right)^2 + \left(\frac{\delta\theta}{\theta}\right)^2 + \left(\frac{\delta d}{d}\right)^2\right), \quad (B.15)$$

In most cases, especially for stars within 10 pc of the Sun such as Gl 486, the uncertainty in distance is much smaller than those in angular diameter and slope of the mass-radius linear relation. In Sect. 3.3 we determined a stellar limb-darkened disc diameter $\theta_{LDD} = 0.390 \pm 0.018$ mas, which error propagated from the scatter of the squared visibility, $V^2$, as a function of spatial frequency, $B'/\lambda$, and the uncertainties in all fit parameters (i.e., $T_{eff}^{LDTK}$, $V_0^2$, $\mu_H$). The uncertainty in $\theta_{LDD}$, of ~4.5%, is about three times larger than of $\beta$, of ~1.6%, and almost 20 times larger than that of $d$, of barely ~0.3%. As a result,

<footnote n="28">²⁸ We used $R_⊙ = 6.957 \times 10^8$ m and $R_⊕ = 6.3781 \times 10^6$ m.</footnote>
<figure><img src="image_23.png" /><figcaption>**Fig. B.2.** Relative errors in star (X axis) and planet (Y axis) radius (**left**) and mass (**right**). Grey open circles: all exoplanet candidates in exoplanets.org. Coloured filled symbols: planets with both mass and radius determination (from RV and transits or transit time variations); the symbol colour denotes the stellar host effective temperature, while the symbol size is log-proportional to the planet radius (**left**) and mass (**right**). Black star: Gl 486 system. Solid diagonal lines: 1:1 radius (**left:**;) and 2:3 mass (**right:**;) relative error ratios. Only in the right panel, we also plot a dashed diagonal line at the 1:1 mass relative error ratio, which corresponds to microlensing planets.</figcaption></figure>

$\delta R_{\star, \text{interf}}/R_{\star, \text{interf}} \approx \delta \theta_{\text{LDD}}/\theta_{\text{LDD}}$, which agrees with the stellar radius relative uncertainty of ~4.5% as in Table 2. After including the $\alpha$ and $\beta$ contributing errors, the stellar mass relative uncertainty becomes the nominal 5.6%.

When there is no interferometric determination of the stellar radius, Schweitzer et al. (2019) proposed deriving $R_\star$ through the Stefan–Boltzmann law from bolometric luminosity and an equilibrium temperature derived from spectral synthesis:

$$R_{\star, \text{synth}}^2 = \frac{L_{\star}}{4\pi\sigma T_{\text{eff}}^4}, \qquad (\text{B.16})$$

and its uncertainty is, thus:

$$\left(\frac{\delta R_{\star, \text{synth}}}{R_{\star, \text{synth}}}\right)^2 = \left(\frac{\delta L_{\star}}{2L_{\star}}\right)^2 + \left(\frac{2\delta T_{\text{eff}}}{T_{\text{eff}}}\right)^2. \qquad (\text{B.17})$$

As a result, the uncertainty in $T_{\text{eff}}$ to $R_{\star, \text{synth}}$ contributes four times that in $L_{\star}$. In turn, the uncertainty in luminosity, which is computed from the distance and observed flux after integrating the stellar spectral energy distribution from the blue optical to the mid infrared ($L_{\star} = 4\pi d^2 F_{\text{obs}}$), is relatively small for nearby stars with precise Gaia EDR3 parallactic distance and a wealth of well-calibrated multiband photometry:

$$\left(\frac{\delta L_{\star}}{L_{\star}}\right)^2 = \left(\frac{\delta F_{\text{obs}}}{F_{\text{obs}}}\right)^2 + \left(\frac{2\delta d}{d}\right)^2. \qquad (\text{B.18})$$

As a result, the error in the determination of $R_{\star, \text{synth}}$ is dominated by that of $T_{\text{eff}}$, which can be 50–200 K in M dwarfs (Passegger et al. 2022).

The following equation summarises all the contributions to the uncertainty in stellar mass in absence of interferometric observations:

$$\left(\delta M_{\star, \text{synth}}\right)^2 = \left(\delta\alpha\right)^2 + \beta^2 R_{\star, \text{synth}}^2 \times \left(\left(\frac{\delta\beta}{\beta}\right)^2 + \left(\frac{2\delta T_{\text{eff}}}{T_{\text{eff}}}\right)^2 + \left(\frac{\delta F_{\text{obs}}}{2F_{\text{obs}}}\right)^2 + \left(\frac{\delta d}{d}\right)^2\right). \qquad (\text{B.19})$$

There are different ways of reducing the uncertainties in stellar radius and mass:

- Acquiring more and better interferometric data. There are, however, technical and logistics limitations to this, as observing at wide baselines and dense ranges of spatial frequencies with up to six CHARA Array telescopes or any other interferometer is time consuming. Besides, although the scenario is not as serious as for the AstroLAB site, Gl 486 culminates at an altitude of only ~65.5 deg as seen from Mount Wilson.

- If there are no interferometric data, improving the $T_{\text{eff}}$ determination. We refer to Marfil et al. (2021) and Passegger et al. (2022) for recent and exhaustive comparisons of methodologies for determining $T_{\text{eff}}$ of M dwarfs.

- Improving the mass-radius relation. TESS is discovering new detached, M-dwarf, eclipsing binaries (e.g., Lendl et al. 2020; Prša et al. 2022), some of them with relatively large orbital periods that lack enhanced magnetic activity and, thus, stellar inflation as in the ones with the shortest periods (Kraus et al. 2011). Special attention must also be given to not including in the fit young eclipsing binaries in stellar kinematic groups that are still on the Hayashi track (Schweitzer et al. 2019).

- Measuring a more precise bolometric observed flux. Differences between $F_{\text{obs}}$ computed by us with VOSA or by other teams are in the details, such as origin of the photometry, template choice, handling of zero-points and transmission profiles (Cifuentes et al. 2020). It is however difficult to get better than 1.1% as measured by us because, even if the photometry has tiny errors and the spectral templates are perfect, almost all photometry is calibrated to the same set of standard stars. Those standards only have their true $F_{\text{obs}}$ measured to about 1–2% based on STIS/Hubble Space Telescope spectro-photometric calibrations (Bohlin & Gilliland 2004; Bohlin 2007; Maíz Apellániz & Weiler 2018). Webb and its extended wavelength range towards the near- and mid-infrared can soon be used for improving the bolometric flux of standard stars.
- Improving the parallactic distance determination. There is strong evidence that Gaia EDR3 parallax errors are underestimated, especially for bright stars (e.g., Luri et al. 2018; El-Badry et al. 2021; Fabricius et al. 2021; Maíz Apellániz 2022). At G ~ 10 mag the underestimation can be up to 60%. Since Gaia DR3 parallactic distances will be those already published in EDR3, we will have to wait for DR4²⁹ for having uncertainties so small that they will in general be negligible with respect to the errors in other parameters.

## Appendix B.3: Element abundances

Slightly different values of A(X) and, therefore, [X/H] can be obtained if other input $T_{\text{eff}}$ are used. Different $T_{\text{eff}}$ at a fixed $L_{\text{bol}}$ translates into distinct $R_{\star}$ and, therefore, $M_{\star}$, $R_{\text{p}}$, and $M_{\text{p}}$. However, as discussed in Sect. 2, our $T_{\text{eff}}$ from our interferometric radius and bolometric luminosity matches most literature values (Table A.3). The abundances and, therefore, the planet interior models, are also sensitive in a lower degree to the used log g and [Fe/H] values. While the iron abundances of Marfil et al. (2021) seem to be the most reliable ones published to date in M dwarfs (Passegger et al. 2022), their surface gravities are a matter of concern. For example, the Gl 486 surface gravity from our interferometric radius and the mass-radius relation of Schweitzer et al. (2019) is log g ≈ 5.4 dex, which contrasts log gSPEC = 4.82 ± 0.12 dex from Marfil et al. (2021). Following Passegger et al. (2022), “further in-depth investigations of the employed methods [to determine effective temperatures, surface gravities, and metallicities in M dwarfs] would be necessary in order to identify and correct for the discrepancies that remain”. In any case, the Fe, Mg, and Si abundances derived by us, which are solar within generous uncertainties, can be applicable to current and future planet interior structure and composition models.

<footnote n="29">²⁹ https://www.cosmos.esa.int/web/gaia/release</footnote>