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Q 1329+412
V = 16.3; z = 1.937; exp = 6300 s; coverage = 3766.2-5791.3
Spectra of this QSO have been studied by SBS and SS92. The line of sight has six reported absorption systems, including C IV. The SS92 spectrum is redward of the wavelength range covering the z = 0.5009 Mg II system reported by SBS. The HIRES spectrum has low signal to noise (in fact, the observed systems from it were not included in Sample B). Still, two new low redshift systems at z = 0.8933 and 0.9984, that have not been reported elsewhere, have been found. These systems are in the Mg II redshift path not covered by the SBS spectrum (0.339-0.761), nor by the SS92 spectrum (1.125-1.875). A systematic search of the Mg II redshift path covered by the HIRES spectrum has not yet been done.
z=0.500785 |DATA & VOIGT PROFILES| |EWs & AOD COLUMNS| |VP PARAMETERS|
This systems was reported as a "probable" Mg II doublet detection by SBS. Because of the low signal to noise of the HIRES spectrum, only the Mg II doublet was detected to the 5-sigma significance level. However, there is a very weak suggestion of absorption from the Mn II 2577 transition. The overall profile was fit with four VP components. Though signal to noise is known to be a factor in determining the number of VP components, the overall shape of the profile in the HIRES spectrum is not suggestive of hidden components. If there are higher velocity subsystems with EW(rest) < 0.04 A, they remain undetected (there is a hint of a subsystem at v ~-180 km/s). The Fe II 2344, 2374, and 2383 transitions and the Ca II 3934, 3969 doublet were not covered by the HIRES format. The Mg I transition, and all other Mn II and Fe II transitions showed no absorption to the EW(rest) limits given in Table 3.40.
z=0.893337 |DATA & VOIGT PROFILES| |EWs & AOD COLUMNS| |VP PARAMETERS|There are no previous reports of a Mg II system at this redshift. The Mg II 2796 EW(rest) is 0.39 A, above the detection thresholds of both the SBS and SS92 survey, so it is likely that had this wavelength range been observed, these authors would have discovered this system. It is found to have two subsystems separated by ~100 km/s. One has been fit with two VP components and the other has been fit with a single VP component. However, there may be one or more additional components in the asymmetric blue wings of both. If so, both subsystems would exhibit similar asymmetries that are characteristic of organized motion with a density gradient along the line of sight. There are what appear to be two spurious absorption features between these subsystems at v = 20 and 80 km/s in the Mg II 2796 profile that are not present in the 2803 profile. They have not been included in the computation of the EW(rest) nor other measured absorption quantities. The Ca II 3934, 3969 doublet was not covered by the HIRES format. The Mn II triplet and all but the Fe II 2383 and 2600 transitions showed no absorption to the EW(rest) limits given in Table 3.41.
z=0.998358 |DATA & VOIGT PROFILES| |EWs & AOD COLUMNS| |VP PARAMETERS|There are no previous reports of a Mg II system at this redshift. As stated above, SBS and SS92 likely would have discovered the system had their spectra covered the appropriate wavelength range. This system was fit by a single VP component and showed absorption in the Fe II 2344, 2383, and 2600 transitions. Though there is no suggestion of a red wing asymmetry in the Mg II 2796, 2803 transitions, and the Fe II transitions appear to have a common redward asymmetry. That the ratio of the Doppler b parameters is unphysical may be indicative of an unresolved VP component. However, it is not uncommon to obtain unphysical ratios even for unblended lines with a similar signal to noise ratio (see Chapter 4). The Ca II 3934, 3969 doublet was not covered by the HIRES format. The Mn II triplet and the remaining Fe II transitions showed no absorption to the EW(rest) limits given in Table 3.42.
Post Thesis WorkFOS/HST data have been investigated.
See Churchill et al. (2000a)
See Churchill et al. (2000b)
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