| |< | | < | | ^ | | > | | >| |
Q 1248+401
V = 16.3; z = 1.032; exp = 2700 s; coverage = 3765.8-6189.9 A
A single Mg II system at z = 0.7728 was reported by SS92. The HIRES spectrum also revealed a previously unreported system at z = 0.8546.
z=0.772953 |DATA & VOIGT PROFILES| |EWs & AOD COLUMNS| |VP PARAMETERS|
The Mg II profiles exhibit the classic "double horn" shape that Lanzetta & Bowen (1992) derived for a simple infall kinematic halo model. The velocity separation of the two main absorbing regions is ~50 km/s. The blue "horn" is comprised of three VP components, which give rise to an asymmetry in the overall profile. This central profile is quite similar to the Q 1101-264 system at z = 0.3590. At v = +225 km/s, there is an outlying high velocity optically thin subsystem. This outlier exhibits a small redward asymmetry; it is not a pure Voigt profile, though the VP LSF did not yield multiple VP components. The region of the spectrum where Mg II has been observed is of excellent quality, so that the VP fitting of even these small subsystems should be fairly accurate. Several Fe II transitions (2344, 2374, 2383, 2587, and 2600) have been detected. The high velocity subsystem is detected in the 2600 transition, but is not detected to 5-sigma in the other Fe II transitions (even the stronger, yet noisier, 2383 transition). A clear detection of Mg I is also present in the high velocity system. Normally, these optically thin high velocity systems are not seen to exhibit neutral absorption. It could be that this "cloud" is in a well shielded environment. The Ca II 3934, 3969 doublet was not covered by the HIRES format and the Mg I transition was only partially observed toward negative velocities. The Mn II triplet showed no absorption to the EW(rest) limits given in Table 3.35.
z=0.854562 |DATA & VOIGT PROFILES| |EWs & AOD COLUMNS| |VP PARAMETERS|This system is characterized by a central asymmetric absorbing subfeature that is fit with two VP components. There are three absorbing subsystems, the others being optically thin and having high velocities. There is broad shallow absorption that stretches approximately 100 km/s from the main absorbing subsystem. There is also a set of two distinct high velocity, v > 200 km/s, "clouds". Interestingly, there is Fe II detected only in the main absorbing subsystem. A total of eight VP components were fit to the system. The Ca II 3934, 3969 doublet was 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 a Table 3.36.
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|