Open Access

Fig. A.13.


J1346+0644: The Na I D line is strongly blended with sky features so that it is difficult to measure even an upper limit. We did not detect Ca II i. The C I absorptions are fitted well with two components at z = 1.511938 and z = 1.512393 (Δυ ~ 50 km s−1). The Mg I absorption is extended over ~200 km s−1. The strongest components of Fe II and Si II are blueshifted by ~100km s−1 relative to the strongest components of C I and Mg I, which may indicate there is one more component of C I at −100 km s−1. Since there is basically no flux in the spectrum at wavelengths smaller than 3200 Å, we cannot derive the H I column density.

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