Table 2.
Overview of the five candidate variables found in our observations with flux measurements consistent with the expected afterglow emission of GW190425.
| RA (deg) | Dec (deg) | fint, 1 (mJy) | fint, 2 (mJy) | fint, 3 (mJy) | fint, 2/fint, 1 | fint, 3/fint, 2 | V | η |
|---|---|---|---|---|---|---|---|---|
| 246.000 | 18.824 | 1.93 ± 0.136 | 3.68 ± 0.134 | 3.82 ± 0.104 | 1.91 ± 0.152 | 1.04 ± 0.0472 | 0.34 | 67.55 |
| 247.214 | 18.471 | 1.95 ± 0.170 | 3.15 ± 0.146 | 4.10 ± 0.102 | 1.62 ± 0.160 | 1.29 ± 0.0679 | 0.35 | 60.07 |
| 247.354 | 18.527 | 12.9 ± 0.179 | 24.3 ± 0.153 | 24.3 ± 0.113 | 1.89 ± 0.0286 | 1.00 ± 0.00780 | 0.32 | 1607.35 |
| 247.330 | 18.682 | 14.3 ± 0.155 | 27.0 ± 0.190 | 26.8 ± 0.136 | 1.89 ± 0.0244 | 0.99 ± 0.00857 | 0.32 | 2183.47 |
| 247.233 | 18.316 | 20.2 ± 0.193 | 33.3 ± 0.190 | 32.6 ± 0.124 | 1.65 ± 0.0184 | 0.98 ± 0.00671 | 0.26 | 1668.20 |
Notes. After cross matching these candidates with the GLADE catalogue (Dálya et al. 2018), no possible host galaxies were found within 3σ of the estimated luminosity distance of GW190425. None of these candidates are thus a source of the afterglow emission. We suspect that for these candidates their variability is either caused by direction-dependent errors from a nearby bright source (rows 2–5), or insufficient phase calibration (first row).
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