Table 2
Photometric and evolutive data for our comoving systems.
| Object | G | MG | AG | GBP − GRP | E(GBP − GRP) | Teff (kK) | log(L∕L⊙) | M(M⊙) | |
|---|---|---|---|---|---|---|---|---|---|
| Abell 24 (CS) | 17.41 | 7.99 | 0.22 | − 0.72 | 0.11 | 137.0 | 1.703 | >3.0 | |
| Abell 24 - B | 15.67 | 6.20 | 0.16 | 0.99 | 0.09 | 5.0 | −0.569 | 0.761 | |
| Abell 33 (CS) | 15.96 | 6.12 | 0.00 | −0.37 | 0.00 | 100.0 | 2.04 |  |
|
| Abell 33 - B | 16.67 | 6.89 | ⋯ | ⋯ | ⋯ | 4.6 | −0.787 | 0.762 | |
| Abell 34 (CS) | 16.42 | 6.04 | 0.14 | −0.67 | 0.07 | 98.0 | 2.079 |  |
|
| Abell 34 - B | 14.85 | 4.43 | 0.11 | 0.82 | 0.06 | 5.9 | 0.086 | 0.908 | |
| NGC 246 (CS) | 11.81 | 3.24 | 0.05 | −0.68 | 0.03 | 150 | 3.688 | 3.75 | |
| NGC 246 - B | 14.19 | 5.46 | 0.38 | 0.91 | 0.02 | 5.5 | −0.314 | 0.846 | |
| NGC 3699 (CS) | 17.60 | 4.93 | 1.78 | −0.55 | 0.38 | ⋯ | ⋯ | ⋯ | |
| NGC 3699 - B | 16.54 | 4.02 | 1.54 | 0.40 | 0.70 | 6.5 | 0.274 | 1.161 | |
| NGC 6853 (CS) | 14.03 | 6.02 | 0.15 | −0.67 | 0.08 | 135.0 | 2.44 |  |
|
| NGC 6853 - B | 16.12 | 8.10 | 0.11 | 1.24 | 0.06 | 4.0 | −1.119 | 0.587 | |
| NGC 6853 - C | 18.99 | 10.80 | ⋯ | ⋯ | ⋯ | 3.3 | −2.020 | 0.200 | |
| PHR J1129-6012 (CS) | 17.26 | 5.33(*) | ⋯ | 1.06(*) | ⋯ | ⋯ | ⋯ | ⋯ | |
| PHR J1129-6012 - B | 17.12 | 4.83(*) | ⋯ | 1.06(*) | ⋯ | ⋯ | ⋯ | ⋯ | |
| PN SB 36 (CS) | 15.25 | 4.03(*) | ⋯ | 1.23(*) | ⋯ | ⋯ | ⋯ | ⋯ | |
| PN SB 36 - B | 14.62 | 3.85(*) | ⋯ | 0.93(*) | ⋯ | ⋯ | ⋯ | ⋯ | |
Notes. Magnitudes are obtained from Gaia DR2, while extinctions are derived by the method of Danielski et al. (2018) using interestellar extinctions taken from Paper I. Temperatures and luminosities are taken from Paper I in the case of the CSPNe, while in the case of the companion stars they are estimated either from PARSEC isochrones in Gaia DR2 passbands (Evans et al. 2018) or by fitting the corresponding SED to NextGen (AGSS2009) models using VOSA platform (http://svo2.cab.inta-csic.es/theory/vosa/index.php), Allard et al. (2012). Masses for the CSPNe are for the progenitor stars, and masses for the comoving companions were calculated either from the PARSEC models or from the SED fits. See text for details. (*) Value not corrected from extinction.
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