Table 3.
X-ray emitting sources identified by visual inspection at the position of optically lensed sources.
| Cluster | ID | RA | Dec | z | μz | Nsoft | Nhard | fsoft | fhard |
|---|---|---|---|---|---|---|---|---|---|
| [h:m:s] | [d:m:s] | [10−16 erg s−1 cm−2] | [10−16 erg s−1 cm−2] | ||||||
| AS1063 | 31 | 22:48:50.43 | –44:32:11.4 | 1.440 | 1.87 | 144.0 ± 13.3 | 118.0 ± 11.6 | 107.2 ± 9.6 | 269.7 ± 28.3 |
| AS1063 | 46 (m) | 22:48:46.11 | –44:31:47.4 | 1.260 | 30.46 | 17.5 ± 8.6 | 2.3 ± 7.1 | 14.1 ± 6.7 | 5.8 ± 18.7 |
| AS1063 | 95 (m) | 22:48:46.97 | –44:32:14.7 | 3.713 | 3.75 | 9.7 ± 5.1 | 1.5 ± 3.8 | 7.3 ± 3.7 | 3.4 ± 9.3 |
| M0416 | 12 | 4:16:05.60 | –24:04:17.2 | 0.736 | 1.53 | 7.4 ± 3.8 | 5.0 ± 3.3 | 2.3 ± 1.2 | 4.8 ± 3.5 |
| M0416 | 208 (m)* | 4:16:06.87 | –24:05:09.5 | 2.218 | 5.74 | 15.6 ± 5.5 | −3.4 ± 3.1 | 4.4 ± 1.5 | −3.0 ± 2.9 |
| M0416 | 221 (m) | 4:16:11.14 | –24:04:36.2 | 4.071 | 2.17 | 7.3 ± 4.1 | −0.5 ± 2.6 | 2.0 ± 1.1 | −0.5 ± 2.4 |
| M0416 | 241 (m)* | 4:16:09.56 | –24:04:00.9 | 5.995 | 1.73 | 10.6 ± 8.8 | 15.3 ± 7.8 | 3.1 ± 2.4 | 14.1 ± 7.6 |
| M1115 | 23 | 11:15:51.51 | +1:30:07.5 | 3.525 | 73.86 | 17.0 ± 8.4 | −4.9 ± 5.2 | 23.0 ± 11.1 | −25.3 ± 28.6 |
| M1206 | 18 | 12:06:18.29 | –8:48:39.4 | 2.427 | 2.09 | 20.6 ± 5.2 | 29.2 ± 6.2 | 13.3 ± 3.2 | 49.1 ± 11.2 |
| R2129 | 12 and 13 | 21:29:39.46 | +0:05:50.3 | 0.592 | 1.51 | 6.2 ± 2.8 | 0.2 ± 1.3 | 11.6 ± 5.0 | 1.7 ± 10.4 |
| R2129 | 73 | 21:29:39.38 | +0:05:51.7 | 4.847 | 1.90 | 4.4 ± 2.4 | −0.6 ± 0.8 | 8.1 ± 4.3 | −4.6 ± 6.2 |
Notes. RA and Dec here correspond to the X-ray position. The source ID is an identification number associated with the optical sources within each field. The flag [m] marks sources that have multiple counterparts, as discussed in the text and in the appendix. Net counts are computed with aperture photometry as described in the text. Only sources with photometry S/N > 2.0 are listed (with three exceptions at slightly lower S/N). Energy fluxes in the soft and hard bands are computed as described in Sect. 4.2. All the values refer to the observed, therefore lensed, quantities. Errors on the observed flux include the Poissonian errors and the systematic uncertainties on the conversion factors. We mark with an asterisk two sources (M0416−208 and M0416−241) that are discarded on the basis of the lack of detection of a counterpart with a higher magnification. In addition, M0416−208 overlaps within ∼2 arcsec with a foreground galaxy, thus the photometry may be contaminated. We kept these sources in the list consistent with the criteria we applied, but we removed them from the following analysis.
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