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Q 1634+706
V = 14.9; z = 1.335; exp = 8100 s; coverage = 3723.3-6185.7
The optical spectrum of this very bright QSO has been studied by SS92, who reported two Mg II absorbers at z = 0.6694, and 0.9903. It has long since been known that the 0.6694 system was a misidentification, but is mentioned here because it appears that no such report has made its way into the literature. Womble (1995) obtained a very high quality HIRES spectrum in June of 1994, but it remains unpublished. Womble reported five Mg II systems with EW(rest) > 0.015 A and one system with EW(rest) < 0.3 A over the redshift range 0.52 < z < 1.334. Bahcall et al. (1995) have presented a UV HST spectrum of this QSO. The HIRES spectrum for this work had an 5-sigma EW(rest) limit of ~0.01 A or smaller for most of the redshift coverage, but no systematic search has been conducted with redshift. However, a single obvious system, in addition to the 0.9903 system, is reported at z = 0.9056.
z=0.905556 |DATA & VOIGT PROFILES| |EWs & AOD COLUMNS| |VP PARAMETERS|
This system is a single-component profile that is likely unresolved, having a doublet ratio of 1.41 for EW(rest)(MgII) = 0.064 A. It has not been previously reported in the literature. The Mg I transition and the Ca II 3934, 3969$ doublet were not covered by the HIRES format. The Mn II triplet and all other Fe II transitions showed no absorption to the EW(rest) limits given in Table 3.51.
z=0.990239 |DATA & VOIGT PROFILES| |EWs & AOD COLUMNS| |VP PARAMETERS|This system was first reported by SS92. It is a single system (no subsystems) and has been fit by five VP components. The total velocity spread is ~80 km/s. Examination of the Mg II doublet N_(v) profiles reveals a ~2-sigma discrepancy in 4-5 pixels over the velocity interval 0 < v < 10 km/s, indicating that there may be a "hidden" component. The Fe II profiles exhibit the classic "double horn" shape, characteristic of smoothly distributed, infalling gas (Lanzetta & Bowen 1992). The Ca II 3934, 3969 doublet was not covered by the HIRES format. The Mn II triplet showed no absorption to the EW( rest) limits given in Table~\ref{tab:q1634z0.99}.
Post Thesis WorkFOS/HST data have been investigated.
See Churchill et al. (2000a)
See Churchill et al. (2000b)
STIS/HST (R=30,000) have been predicted using photoionization modeling.
See Charlton et al. (2000)
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