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Q 1213-003
V = 17.0; z = 2.691; exp = 5200 s; coverage = 5008.1-7356.7 A
Spectra of this QSO were previously studied by LTW and SS92. The two very strong systems studies in this work were both discovered by LTW. They both exhibit remarkable absorption profiles. In fact, these systems were selected with a bias toward large equivalent widths and high redshifts.
z=1.320059 |DATA & VOIGT PROFILES| |EWs & AOD COLUMNS| |VP PARAMETERS|
This system exhibits a large double saturated trough like that seen along the line of sight to SN 1993J, which is embedded in the disk of M81. Its line of sight samples half of the halo and disk of M81 and half of the halo and disk of the Galaxy (Bowen, Blades, & Pettini 1995). It is tempting to speculate that this absorption system may be passing through two different galaxies that are separated by about 200 km/s along the line of sight. Once again, the low ionization profile exhibit symmetric velocity splittings with v ~30 km/s separations. A total of 24 VP components were fit to the system. Even though this is a large number of components, it should be noted that the number is probably an underestimate because strong blending is occuring (see Chapter 4). This is also illustrated in Figure 3.6. if the linear relation between the system EW(rest) and N_cl holds for all systems. Note that the VP column densities and b parameters are not well constrained for components 7, and 14-17. The inverted N_a(v) profiles for the Mg II doublet and the richly structured Mg I transition are illustrated in Figure 3.13. The Mn II 2594 transition and the Ca II 3934, 3969 doublet were not covered by the HIRES format.
z=1.554148 |DATA & VOIGT PROFILES| |EWs & AOD COLUMNS| |VP PARAMETERS|As noted by SS92: "It is surprising that two such strong low-ionization, apparently unrelated absorption systems should be found in the QSO spectrum[.]" This system is quite similar to the z = 1.3201 system, except that the double-like saturated trough is not as prominent. On the other hand, this system shows the asymmetric profiles in the low ionization species characteristic of the damped Ly-alpha systems thought to be thick disks sampled at high inclination (Prochaska & Wolfe 1996, 1997). Though the full complement of Fe II transitions are very strong, the Mn II triplet shows no absorption to a 5-sigma EW(rest) limit of 0.085 A over the full velocity range of the Mg II profiles. However, at roughly v = 10 km/s there is what may be a very weak feature in the Mn II 2577. As such, this system may not be a damped (Lu et al. 1996). The overall profile was fit with a total of 17 VP components. The only component for which the column density and Doppler b parameter are highly uncertain is number 13, which is centered in the saturated trough. The Mn II 2576 transition and the Ca II 3934, 3969 doublet were not covered by the HIRES format.
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