Table A.2.
Results of the CHORIZOS analysis for the systems in this paper using the 1.78 Ma Geneva isochrone grid with no rotation and GBP, DR2 + GDR2 + GRP, DR2 + GBP, EDR3 + GEDR3 + GRP, EDR3 + J2M + H2M + K2M.
| Star | mi | E(4405 − 5495) | R5495 |  |
AG | Gabs | Teff | log L |
|---|---|---|---|---|---|---|---|---|
| (solar) | (mag) | (mag) | (mag) | (kK) | (solar) | |||
| Bajamar star A | 72.96±0.54 | 3.606±0.016 | 2.89±0.02 | 8.91 | 7.733±0.017 | −6.384±0.016 | 42.75±0.19 | 5.991±0.005 |
| Tyc 3179-00756-1 | 18.43±0.20 | 1.858±0.012 | 2.86±0.03 | 0.54 | 4.524±0.024 | −3.599±0.023 | 33.09±0.11 | 4.598±0.012 |
| HD 195 965 | 15.51±0.12 | 0.212±0.006 | 3.29±0.16 | 0.15 | 0.712±0.017 | −3.261±0.017 | 30.97±0.08 | 4.380±0.009 |
| Tyc 3575-01514-1 | 3.57±0.04 | 0.431±0.006 | 3.06±0.09 | 0.96 | 1.258±0.025 | +0.275±0.025 | 13.74±0.09 | 2.189±0.019 |
| Tyc 3157-00918-1 | 3.58±0.03 | 0.368±0.006 | 3.35±0.10 | 0.94 | 1.187±0.019 | +0.267±0.019 | 13.77±0.07 | 2.196±0.015 |
| Toronto star A | 33.10±0.42 | 0.325±0.007 | 3.55±0.01 | 0.85 | 1.164±0.024 | −4.845±0.023 | 39.36±0.11 | 5.266±0.013 |
| HDE 227 0901 | 4.46±0.04 | 0.502±0.007 | 3.44±0.08 | 0.28 | 1.648±0.022 | −0.235±0.021 | 15.81±0.09 | 2.531±0.013 |
| HD 201 795 | 12.40±0.09 | 0.221±0.006 | 3.18±0.15 | 0.22 | 0.716±0.017 | −2.729±0.016 | 28.10±0.09 | 4.085±0.009 |
| HD 200 776 | 13.66±0.14 | 0.241±0.011 | 4.26±0.27 | 1.44 | 1.025±0.023 | −2.956±0.023 | 29.33±0.11 | 4.212±0.013 |
| 2MASS J20531694+44242982 | 25.12±0.34 | 3.036±0.017 | 3.01±0.02 | 2.64 | 7.056±0.026 | −4.304±0.025 | 36.72±0.14 | 4.970±0.015 |
| 2MASS J20522503+4437562 | 17.20±0.14 | 1.872±0.011 | 2.99±0.02 | 2.06 | 4.770±0.018 | −3.503±0.017 | 32.19±0.09 | 4.510±0.010 |
| Tyc 3179-00733-1 | 11.13±0.11 | 1.449±0.009 | 3.30±0.03 | 1.58 | 4.188±0.023 | −2.472±0.023 | 26.71±0.10 | 3.931±0.013 |
| 2MASS J20512895+44042303 | 9.10±0.30 | 1.533±0.022 | 3.42±0.09 | 0.49 | 4.554±0.073 | −1.993±0.072 | 24.14±0.38 | 3.647±0.044 |
| Tyc 3179-00615-1 | 8.45±0.08 | 1.228±0.008 | 3.00±0.03 | 2.03 | 3.313±0.021 | −1.819±0.021 | 23.12±0.11 | 3.539±0.013 |
| 2MASS J20522374+4436151 | 7.73±0.07 | 1.510±0.009 | 2.68±0.03 | 1.43 | 3.510±0.022 | −1.605±0.021 | 22.08±0.10 | 3.407±0.013 |
| V2022 Cyg2 | 5.36±0.10 | 0.960±0.009 | 3.34±0.07 | 1.94 | 2.923±0.039 | −0.668±0.039 | 17.65±0.17 | 2.820±0.028 |
| 2MASS J20530782+4409456 | 4.33±0.05 | 1.005±0.008 | 3.27±0.04 | 0.89 | 2.956±0.025 | −0.167±0.024 | 15.51±0.11 | 2.490±0.016 |
Notes: For the Bajamar star a magnitude difference of 0.18 has been applied to all filters to account for the presence of the companion (hence the A in the name). Similarly, for the Toronto star a magnitude difference of 0.05 has been used. The last eight entries correspond to the eight brightest (in G) members of the Bermuda cluster selected in Villafranca II. The first three data columns are the fitted parameters in the isochrone grid. The fourth column is the reduced χ2 of the fit. The last four columns are derived quantities and auxiliary parameters. For the runaway/walkaway systems the distance from Table 2 is used while for the Bermuda cluster members a distance of 798 pc is assumed. All fits assume the systems are single or that any hidden companions do not contribute significantly to the photometry and that there is no uncertainty in the distance or the cluster age, so the real uncertainties should be significantly larger than the formal ones for quantities such as mi, Teff, or log L.
Photometry excluded from the fit. 1: GEDR3. 2: K2M. 3: H2M + K2M.
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