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Table 1.

List of all spectroscopically confirmed quadruply-imaged systems having Nimg = 3, 4 components detected in Gaia DR2.

Lens identifier Nimg Size ΔG Δ(GBP − GRP) Field density ERT probabilities
(mas) (mag) (mag) (obj. deg−2) ABCD ABC ABD ACD BCD
2MASSJ11344050–2103230 4 3682 1.76 0.16(3) 18 335 1.00 0.97 0.66 0.72 0.31
J1606–2333 4 1723 0.76 0.07(2) 50 420 1.00 0.9 0.99 0.94 0.84
WGD2038–4008 4 2869 0.65 22 918 1.00 1.00 0.86 0.7 0.72
HE0435-1223 4 2539 0.73 0.29(2) 18 335 0.99 0.92 0.7 0.75 0.78
PG1115+080 4 2427 1.79 0.02(3) 18 335 0.99 0.98 0.99 0.75 0.69
B1422+231 4 1281 3.46 22 918 0.98 0.87 0.98 0.83 0.59
J2145+6345a, b 4 2068 1.70 73 339 0.97 0.96 0.92 0.95 0.86
2MASXJ01471020+4630433 4 3262 2.37 0.10(2) 41 253 0.95 0.66 0.99 0.55 0.51
2MASSJ13102005-1714579 4 5735 1.21 0.21(3) 22 918 0.92 0.93 0.92 0.85 0.84
J1721+8842c 4 3906 1.75 0.13(2) 27 502 0.91 0.32 0.99 0.65 0.84
WFI2033–4723 4 2533 1.18 0.04(2) 18 335 0.89 0.98 0.8 0.67 0.99
SDSS1004+4112b 4 14 732 1.35 0.22(4) 22 846 0.88 0.99 0.24 0.99 0.19
RXJ1131–1231 4 3232 2.11 22 918 0.65 0.69 0.93 0.56 0.72
SDSSJ1433+6007 3 3754 0.38 0.04(2) 13 751 0.99 0.92 0.52 0.65
DESJ0405–3308a, b 3 1416 0.20 0.32(3) 13 751 0.98 0.78 0.66 0.93
J0408–5354 3 4184 1.08 0.30(2) 22 918 0.42 0.56 0.97 0.95
HE0230–2130 3 2188 1.03 13 751 0.95 0.75 0.08 0.05
H1413+117 3 1111 0.25 0.12(2) 18 335 0.86 0.48 0.6 0.65
RXJ0911+0551b 3 3260 1.11 0.04(2) 27 502 0.65 0.19 0.67 0.07
J0630–1201 3 1901 0.11 0.33(3) 36 669 0.58 0.1 0.09 0.3
WISE025942.9–163543 3 1577 0.76 13 751 0.32 0.45 0.16 0.32

Notes. The lens size and the maximum absolute difference in magnitude and colour, ΔG and Δ(GBP − GRP), are computed over all combinations of the lensed images while the field density is estimated within a radius of 30″ around the system. The numbers in parentheses in Col. Δ(GBP − GRP) correspond to the number of images that were used in the computation of the maximum absolute difference in colour. Four image configurations are processed using the ERT model ABCD, as well as using all the ABC, ABD, ACD, and BCD models based on the appropriate combination of images (see Sect. 3). Three image configurations are processed using models ABC, ACD, ABD, and BCD.

(a)

J2145+6345 and DESJ0405–3308 are not contained in the original list of known gravitational lenses from Ducourant et al. (2018) as their discovery was announced after the list was compiled (see Lemon et al. 2019; Anguita et al. 2018, respectively).

(b)

J2145+6345, SDSS1004+4112, DESJ0405–3308, and RXJ0911+0551 are not part of the final catalogue of clusters (Appendix B) because they are found in regions of high stellar density (J2145+6345), because one of their images does not pass the soft astrometric test (DESJ0405–3308 and RXJ0911+0551), or because the angular size is too large (SDSS1004+4112).

(c)

For J1721+8842, we selected the configuration of four images out of the five images available for which the ERT probabilities was the highest (0.91). Alternative combinations implying image with Gaia source identifier 1729026466114871296 provide ERT probabilities between 0 and 0.05.

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