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Q 0117+212
V = 16.1; z = 1.491; exp = 5400 s; coverage = 4317.7-6775.1 A
A spectrum of this QSO was previously studied by SS92. The four redshifts they reported are confirmed. An additional redshift at z = 0.7290 discovered by SDP (Steidel, private communication) was also confirmed.
z=0.576398 |DATA & VOIGT PROFILES| |EWs & AOD COLUMNS| |VP PARAMETERS|
The system exhibits fully saturated Mg II profiles and a Mg I profile with definite variations in strength in velocity space. Weak Ca II 3936, which is aligned with the peak absorption across the Mg I profile, has also been observed. There is a slight blending in the blue wing of Mg I with the red wing of Fe II 2600 at z = 0.7291. The profiles were fit with four VP components. The velocities of the three components in the saturated region were constrained by the Mg I profile. The previously reported Fe II transitions were not covered by the HIRES format. In fact, none of the Fe II transitions, nor the Mn II triplet, nor the Ca II 3934 transition were covered by the HIRES format. The measured EW(rest) for the Mg II, Mg I, and Ca II transitions are given in Table 3.10.
z=0.729055 |DATA & VOIGT PROFILES| |EWs & AOD COLUMNS| |VP PARAMETERS|This system was discovered by SDP (Steidel, private communication). However, SS92 did flag an unidentified line (15), which is in fact the Mg II for this system. Three kinematic subfeatures were identified and the overall system was fit with five VP components. There is a slight blending in the red wing of Fe II 2600 with the blue wing of Mg I at z = 0.576398. The Ca II 3934, 3969 doublet and the Fe II 2344, 2374, and 2382 transitions were not covered by the HIRES format. The Mn II triplet showed no absorption to the EW(rest) limits given in Table 3.11.
z=1.047971 |DATA & VOIGT PROFILES| |EWs & AOD COLUMNS| |VP PARAMETERS|This system is found to have two kinematic subfeatures separated by roughly 100 km/s. The overall profile was fit with seven VP components. The Ca II 3934, 3969 doublet was not covered by the HIRES format. The Mn II triplet and the Fe II 2374 and 2586 transitions showed no absorption to the EW(rest) limits given in Table 3.12.
z=1.325014 |DATA & VOIGT PROFILES| |EWs & AOD COLUMNS| |VP PARAMETERS|This weak system is kinematically intriguing in that it is composed of five distinct kinematic subfeatures somewhat uniformly separated in velocity ( ~ 30 km/s). The overall profile has been fit with six VP components. The Ca II 3934, 3969 doublet and the Mn II 2576 transition were not covered by the HIRES format. The remaining Mn II transitions and the Fe II 2344, and 2374 transitions showed no absorption to the EW(rest) limits given in Table 3.13.
z=1.342969 |DATA & VOIGT PROFILES| |EWs & AOD COLUMNS| |VP PARAMETERS|This is another weak, but kinematically interesting, system. There are four kinematic subfeatures, which are dominated by a narrow asymmetric profile. The overall profile was fit with five VP components. The observed Fe II is associated with this dominate Mg II subfeature. The Ca II 3934, 3969 doublet and the Fe II 2600 and Mg II 2796 transitions were not covered by the HIRES format. The Mn II triplet and the Mg I transition showed no absorption to the EW(rest) limits given in Table 3.14.
Post Thesis WorkFOS/HST data have been investigated.
See Churchill et al. (2000a)
See Churchill et al. (2000b)
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