Table 1.
Orbital parameters for AGGC systems with orbital solutions.
| APOGEE ID | Parallax [mas] | Period [days] | ΔRVmax [km/s] | MMS [M⊙] | min MWD[M⊙] | Solution |
|---|---|---|---|---|---|---|
| 2M00471103+1738040 | 11.956 ± 0.022 | 1.245 ± 1.23E-05 | 62.914 | 0.522 ± 0.084 | 0.266 ± 0.025 | SB1 |
| 2M01592351–0045463 | 8.155 ± 0.026 | 571.951 ± 0.867 | 22.235 | 0.858 ± 0.110 | 0.532 ± 0.055 | Astrometry |
| 2M07515777+1807352 | 7.280 ± 0.021 | 10.298 ± 6.60E-04 | 58.202 | 0.670 ± 0.082 | 1.067 ± 0.058 | SB1 |
| 2M08110666+2111127* | 7.089 ± 0.023 | 202.551 ± 0.817 | 3.799 | 0.550 ± 0.021 | 0.177 ± 0.024 | Astrometry |
| 2M08180299+4412265 | 6.232 ± 0.026 | 1340.662 ± 67.723 | 0.133 | 0.596 ± 0.100 | 0.550 ± 0.043 | Astrometry |
| 2M08410922+2542362 | 3.338 ± 0.027 | 464.087 ± 1.731 | 0.086 | 1.000 ± 0.124 | 0.506 ± 0.050 | Astrometry |
| 2M11463394+0055104 | 4.854 ± 0.083 | 0.409 ± 1.14E-05 | 373.00 ± 2.07 | 0.440 ± 0.028 | 0.717 ± 0.014 | RV curve |
| 2M14544500+4626456 | 9.054 ± 0.028 | 15.096 ± 6.98E-05 | 99.53 ± 0.04 | 0.488 ± 0.031 | 0.693 ± 0.001 | RV curve |
| 2M15460673+2655088 | 3.167 ± 0.017 | 1105.316 ± 34.542 | 0.359 | 0.809 ± 0.105 | 0.580 ± 0.125 | Astrometry |
| 2M16105316+4130067* | 8.316 ± 0.012 | 204.018 ± 0.200 | 5.482 | 0.883 ± 0.117 | 0.242 ± 0.020 | Astrometry |
| 2M16411273+4028257 | 3.581 ± 0.015 | 164.197 ± 0.222 | 0.211 | 0.932 ± 0.109 | 0.567 ± 0.321 | Astrometry |
| 2M16462555+3934567 | 2.623 ± 0.010 | 2.766 ± 2.51E-04 | 51.807 | 1.015 ± 0.132 | 0.195 ± 0.016 | SB1 |
| 2M17284156+5614329* | 5.124 ± 0.012 | 676.150 ± 14.748 | 0.308 | 0.708 ± 0.083 | 0.242 ± 0.043 | Astrometry |
Notes. Orbital solutions are from Gaia, except for two systems from Corcoran et al. (2021) whose orbits were determined from their APOGEE RV curves. We provide the parallax, orbital period, maximum radial velocity shift (ΔRVmax), mass of the MS star (MMS – from StarHorse), minimum mass of the WD (MWD), and the method by which the orbital solution was obtained. For the systems with astrometric solutions, the value for the mass given in the min MWD column refers to the best-fit companion mass. Systems marked with * might not be WD+MS binaries, but contaminants from chromospheric activity in single MS stars. Systems with a RV curve solution (and thus a measurement error on ΔRVmax) are from Corcoran et al. (2021).
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