Table 1.
Overview of source examples in this work that have scan-angle-dependent signals, along with diagnostic statistics and fitted parameters.
| SourceID | Case | rexf, G | ripd, G | aipd | φipd | κ | c0 | aG | θG |  |
Gp | Gs | ρ | θ |  |
Figs. |
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| DR3 pairs, triplets and bright neighbours, with angular separation and position angle: | ||||||||||||||||
| 382074694311961856 (a) | 0.36″, 19° | 0.92 | 0.17 | 0.21 | 95° | 84% | 13.1 | 0.21 | 8° | 68.5 | 13.3 | 13.9 | 0.33″ | 15° | 1.9 | 8 |
| 379163256239241216 (a) | 0.95″, 27° | 0.76 | 0.21 | 0.08 | 90° | 5% | 17.1 | 0.01 | 29° | 4.7 | 17.1 | 21.6 | 0.36″ | 99° | 4.6 | B.9 |
| 388877407113709056 (a) | 0.56″, 87° + 1.04″, 69° | 0.36 | 0.09 | 0.05 | 131° | 19% | 15.9 | 0.00 | 92° | 9.8 | 15.9 | 19.9 | 1.19″ | 86° | 9.4 | B.10 |
| 385771836519005184 (a) | Bright, 3.1″, 24° | 0.00 | 0.07 | 0.05 | 50° | 20% | 13.1 | 0.00 | 19° | 8.3 | 13.1 | 18.0 | 0.66″ | 104° | 8.0 | B.11 |
| Blind search in DR3 looking for multi-peak indicators: | ||||||||||||||||
| 367388551858425344 (a) | Pre-DR4 split in two | 0.99 | 0.85 | 0.16 | 10° | 40% | 12.4 | 0.09 | 98° | 13.6 | 12.4 | 13.8 | 0.31″ | 18° | 2.3 | B.12, C.4 |
| 383556286230747520 (a),(v) | Variable flag set | 0.99 | 0.95 | 0.40 | 61° | 39% | 16.1 | 0.42 | 150° | 15.1 | 19.5 | 15.7 | 0.07″ | 150° | 15.2 | B.13, C.5 |
| 380538569192874112 (a) | 0.49″, 112° | 0.91 | 0.86 | 0.47 | 42° | 37% | 16.5 | 0.46 | 127° | 208.6 | 16.8 | 16.9 | 0.48″ | 113° | 13.4 | B.14, C.4 |
| DR3 sources identified as galaxy candidates, with De Vaucouleurs radius, ellipticity and position angle: | ||||||||||||||||
| 373852271480563968 (a) | 0.99″, 0.10, 7° | 0.13 | 0.42 | 0.06 | 92° | 0% | 19.8 | 0.06 | 162° | 26.1 | 19.8 | 22.3 | 0.35″ | 70° | 26.8 | B.16 |
| 366951667785042688 (a) | 1.65″, 0.35, 63° | 0.63 | 0.95 | 0.26 | 150° | 0% | 19.9 | 0.29 | 61° | 1.3 | 15.7 | 15.7 | 0.05″ | 151° | 1.4 | 9, C.5 |
| 364175332206026368 (a) | 1.95″, 0.56, 85° | 0.95 | 0.96 | 0.67 | 173° | 0% | 20.3 | 0.77 | 82° | 5.8 | 21.1 | 19.7 | 0.18″ | 85° | 3.8 | B.15 |
| DR3 spectroscopic binaries (SB1), probably spurious (63-day period), furthermore flagged as Variable: | ||||||||||||||||
| 415146526611154176 (v) | 0.27″, 63° | 0.99 | 0.72 | 0.05 | 157° | 64% | 9.9 | 0.04 | 58° | 10.8 | 9.8 | 12.4 | 0.19″ | 149° | 10.0 | B.17 |
| 5815369024263284352 (v) | – | 0.94 | 0.24 | 0.02 | 47° | 0% | 8.5 | 0.01 | 115° | 3.5 | 8.5 | 13.3 | 0.19″ | 118° | 3.5 | B.18 |
| Pre-DR4 close pairs, with their angular separation and position angle (if available): | ||||||||||||||||
| 389636619892245248 (a) | 0.13″ | 0.98 | 0.96 | 0.23 | 122° | 29% | 15.4 | 0.17 | 28° | 34.1 | 15.2 | 16.4 | 0.21″ | 118° | 8.0 | 7 |
| 378810450446502400 (a) | 0.14″, 30° | 0.99 | 0.92 | 0.25 | 129° | 36% | 11.7 | 0.09 | 34° | 25.6 | 11.6 | 12.8 | 0.40″ | 111° | 6.1 | B.2 |
| 388466602081536640 (a) | 0.17″ | 0.94 | 0.94 | 0.23 | 173° | 26% | 18.2 | 0.24 | 82° | 14.8 | 18.6 | 18.8 | 0.15″ | 84° | 13.6 | B.1, C.5 |
| 376045247423005184 (a) | 0.22″ | 0.94 | 0.85 | 0.16 | 28° | 38% | 17.2 | 0.16 | 106° | 8.4 | 17.3 | 18.3 | 0.27″ | 104° | 2.0 | B.5 |
| 382159975182923264 (a) | 0.25″, 82° | 0.99 | 0.93 | 0.48 | 154° | 46% | 17.5 | 0.50 | 66° | 26.7 | 17.8 | 17.7 | 0.26″ | 75° | 12.1 | B.4, C.5 |
| 385844060692409344 (a) | 0.35″ | 0.98 | 0.77 | 0.25 | 35° | 43% | 16.1 | 0.28 | 121° | 259 | 16.3 | 16.9 | 0.37″ | 109° | 161 | B.6, C.4 |
| 385804856230839552 (a) | 0.35″ | 0.99 | 0.64 | 0.08 | 17° | 44% | 9.1 | 0.14 | 97° | 43.7 | 9.2 | 10.5 | 0.28″ | 96° | 13.1 | B.3 |
| 387325652606842368 (a) | 0.63″, 101° | 0.45 | 0.22 | 0.03 | 82° | 24% | 18.8 | 0.01 | 178° | 26.9 | 18.8 | 17.9 | 1.91″ | 97° | 7.1 | B.8 |
| 385367010081173504 (a) | 0.69″, 133° | 0.43 | 0.41 | 0.02 | 46° | 23% | 18.1 | 0.02 | 125° | 4.2 | 18.2 | 18.5 | 0.60″ | 140° | 2.0 | B.7 |
Notes. For each case, we list the Spearman correlations (rexf, G and ripd, G, Sect. 6), the ipd_gof_harmonic_amplitude, ipd_gof_harmonic_phase, and ipd_frac_multi_peak (aipd, φipd and κ, Sect. 3.1.2), the results of a sinusoidal or small-separation fit to the G photometric scan-angle signal (c0, aG, θG, and the 
of the fit, Eq. (5)), and finally, the results of a source-pair fit to the G-band photometric scan-angle signal (Gp, Gs, ρ, θ, and the χ2 of the fit, Eq. (4)).
(a)Source in the Gaia Andromeda photometric survey (GAPS); (v)Source in the variability catalogue; in both cases, the photometric time series and a subset of diagnostic statistics and fitted parameters are published; see Appendix A for details.
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