| |< | | < | | ^ | | > | | >| |
Q 2128-123
V = 15.9; z = 0.501; exp = 3900 s; coverage = 3766.2-5791.3
Spectra of this low redshift QSO have been studied by Weymann et al. (1979), Tytler et al. (1987), and at higher resolution by Petitjean & Bergeron (1990).
z=0.429735 |DATA & VOIGT PROFILES| |EWs & AOD COLUMNS| |VP PARAMETERS|
This system was first reported by Weymann et al. (1979). The Mg II profiles are found to be a single feature based upon the ewregion algorithm. However, there is a double-like characteristic to the profiles. The system has been fit with a total of four VP components. Mg I and Ca II absorption is found associated with the two strongest Mg II components. Detection of the Ca II 3934, 3969 confirms the 1-sigma Ca II 3934 detection reported by Petitjean & Bergeron (1990). An IUE spectrum reveals a Lyman limit cutoff and large Ly-alpha absorption, suggesting N(HI) > 2 x 10^19 cm^-2 (Tytler 1982; Bergeron??? 1983). Taken at face value, the strong neutral component (the ionization potential of Ca II is 0.87 Ryd) of the absorption suggests that the H is not mostly ionized. Given the measured Mg II column density log N = 13.47 cm^-2, a supersolar magnesium abundance is not required to explain the column density ratio N(MgII)/N(HI) [see Tytler et al. 1987]. Unfortunately, none of the Fe II transitions were covered by the HIRES format, so the Fe II lines reported by Tytler et al. and Petitjean & Bergeron were not observed.
Post Thesis WorkFOS/HST data have been investigated.
See Churchill et al. (2000a)
See Churchill et al. (2000b)
|PREVIOUS QSO| |NEXT QSO| | QSO LISTING | |TABLE OF CONTENTS| |CWC HOME|