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Fig. A.7.


J1133−0057: Both Ca II H&K and Na I D are clearly detected in this good spectrum. This system is a peculiar but interesting case for which the absorbing cloud is small and located at a short distance to the quasar. Indeed, the broad line region (BLR) is only partially covered by the cloud. This system has been analysed by Fathivavsari et al. (2017) who derived an H I column density of 21.00 ± 0.30. There are two main components separated by ~200 km s−1. Although Ca II is detected only in the strongest system, Na I is detected in both. Ca must be highly depleted into dust, which is consistent with the corresponding large attenuation of the quasar (see Table 3).

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