Table 3
SOS (absolute) completeness and contamination estimates with respect to cross-matched reference catalogues.
| Processing path | SOS type | Catalogue (and region) | Completeness | Contamination |
|---|---|---|---|---|
| geq12 & geq20 | Cepheids | OGLE-IV (LMC, limited region) | 74% | ~5%a |
| geq12 & geq20 | Cepheids | OGLE-IV (Bulge) | 3% | b |
| geq12 & geq20 | RR Lyrae stars | OGLE-IV (LMC, limited region) | 64% | ~9%a |
| geq12 & geq20 | RR Lyrae stars | OGLE-IV (Bulge) | 15% | b |
| geq12 & geq20 | LPV | OGLE-IIIc (SMC+LMC) | ~30% | <few% |
| geq12 & geq20 | LPV | OGLE-IIIc (SMC+LMC) | ~30% | <few% |
| geq20 | Short timescale | OGLE-II, III, IV (MCs) | 0.05% | 10–20% |
| geq20 | Rotational modulation | The Pleiades (Hartman et al. 2010) | 0.7–5.0% | <50%d |
Notes. Processing paths are based on the number of selected FoV transits, as shown in Fig. 2 and discussed in Sect. 3. See Sect. 4.4 for additional contamination rate estimates for random and sky-uniform samples. For more details on the validation of the SOS type results, see Sect. 4.4 and the references therein. (a) Estimated from non-cross-match random samples inspection discussed in Sect. 4.4, extending partially beyond OGLE-IV footprint. (b) No reliable contamination rate for the Bulge has been derived, but in the Galactic disk footprint (see Udalski 2017), contamination of the SOS Cepheids and RR Lyrae stars might be of the order of several tens of percent (A. Udalski, priv. comm. based on unpublished OGLE-IV data). (c) Estimates are restricted to sources with a peak-to-peak amplitude >0.2 mag and periods longer than 60 days. (d) The 50% “contamination” quantifies the non-occurrence in the reference catalogue; the actual contamination of grazing binaries is estimated to be < 1% (see Sect. 4.4.4).
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