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Table 3
Criteria for the detection of unresolved sources based on Gaia DR3 statistical indicators.
| Criterion | Selection | Remarks |
|---|---|---|
| 1 | RUWE > 2 | Goodness of fit between the observed astrometric data and a single-star model. |
| 2 | ipd_gof_harmonic_amplitude > 0.1 & RUWE > 1.4 | Flag for spurious solutions of resolved doubles, not correctly handled in the Gaia EDR3 astrometric processing (Fabricius et al. 2021). |
| 3 | ipd_frac_multi_peak > 30 | Fraction of windows for which the algorithm has identified a double peak (or double transit), meaning that the detection may be a visually resolved double star (e.g. Tokovinin 2023; Holl et al. 2023; Medan & Lépine 2023). |
| 4 | rv_chisq_pvalue < 0.01 & rv_renormalised_gof > 4 & rv_nb_transits ≥ 10 | Measure of variability in RV among all the Gaia measurement epochs (Katz et al. 2023). |
| 5 | radial_velocity_error ≥ 10 km s−1 | Same as above. For the bright stars (G ≲ 13 mag) it is the uncertainty on the median of the epoch radial velocities, to which a constant shift of 0.11 km s−1 was added to take into account a calibration floor. |
| 6 | duplicated_source = 1 | Flag for the existence of a duplicated source during data processing, which may indicate observational, crossmatching, or processing problems, or stellar multiplicity, and probable astrometric or photometric problems in all cases. This metric works in support to the others, rather than being a standalone indicator on itself. |
| 7 | non_single_star | Flag for a possible non-constant behaviour using binary orbit models. Three bits indicate whether it has been identified as astrometric (bit 1 is set to one), spectroscopic (bit 2 is set to one), or eclipsing (bit 3 is set to one) binary, respectively (Pourbaix et al. 2022). |
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