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Q 1148+384
V = 17.0; z = 1.299; exp = 5400 s; coverage = 3986.5-6424.5 A
Spectra of this QSO, also known as 4C 38.31, were previously studied by Boulade et al. (1987), who reported a low redshift Mg II system at z = 0.2130, and by SS92, who reported a Mg II system at z = 0.5532. Only the SS92 system has been studied in this work.
z=0.553362 |DATA & VOIGT PROFILES| |EWs & AOD COLUMNS| |VP PARAMETERS|
This system has a very interesting profile that is comprised of eight VP components over a single "kinematic system" spread over 200 km/s. The striking characteristic of this profile is the well defined and symmetric velocity splitting. In addition, the absorption strengths decrease with increasing velocity, giving the overall absorption "envelope" a Gaussian shape. Qualitatively, this profile appears that it could arise from shells of infalling gas. Interestingly, this profile arises about 15 kpc out in a face-on spiral galaxy (Steidel, private communication), but exhibits the symmetric velocity splittings that are believed to arise out at 20 kpc in the edge-on spiral galaxy at z = 0.7446 (Churchill, Vogt, & Steidel (1995}; Le Brun et al. (1996). The Ca II 3934 transition and the Fe II 2344, 2374, and 2383 transitions were not covered by the HIRES format. The Mn II triplet and the Ca II 3969 transition showed no absorption to the EW(rest) limits given in Table 3.26.
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