Property	Full Sample	Low-z High-REW Subsample	High-z High-REW Subsample	Low-z Low-REW Subsample	High-z Low-REW Subsample	Cosmic DLA Gas
Number of absorbers...	223	90	60	42	31	...
Mg II 2796 REW (Å)...	1.0	1.3	1.3	1.01.3	1.01.3	>0
Redshift (z) interval...	0.92.0	0.91.35	1.352.0	0.91.35	1.352.0	0.92.0
Zn II 2026bla REW (mÅ)...	33.6 (5.0)	70.2 (9.3)	29.4 (7.7)	0.1 (10.6)	6.5 (11.3)	...
Mg I 2026bla REW (mÅ)...	10.2 (0.2)	13.7 (0.3)	10.9 (0.3)	5.6 (0.4)	4.0 (0.5)	...
Cr II 2056 REW (mÅ)...	31.1 (5.1)	41.7 (7.7)	32.2 (8.1)	6.2 (10.3)	6.5 (11.4)	...
Cr II 2062blb REW (mÅ)...	23.2 (3.8)	31.2 (5.8)	24.1 (6.0)	4.6 (7.7)	4.8 (8.5)	...
Zn II 2062blb REW (mÅ)...	12.3 (6.2)	26.6 (10.3)	6.2 (9.5)	12.4 (12.9)	6.1 (14.3)	...
Cr II 2066 REW (mÅ)...	13.0 (4.5)	19.2 (8.3)	9.8 (8.2)	21.5 (10.6)	2.5 (8.0)	...
[Zn/H]c,d...	-0.88 (0.19)	-0.56 (0.19)	-0.94 (0.21)	<-1.08	<-1.05	-1.13 (0.19)
[Cr/Zn]d...	-0.45 (0.13)	-0.64 (0.13)	-0.38 (0.18)	...	...	...
Mean SDSS g mag...	18.8 (0.6)	18.8 (0.5)	18.8 (0.6)	18.8 (0.6)	18.8 (0.7)	...
Mean SDSS r mag...	18.7 (0.5)	18.7 (0.5)	18.6 (0.6)	18.6 (0.5)	18.8 (0.6)	...

     ^a The feature at 2026 Å is a blend due to Zn II, Mg I, and a very weak Cr II line. As measured in their composite spectra, the Mg I 2026 REW was taken to be 32.0 times smaller than the measured REW of Mg II 2852, and the Cr II 2026 REW was taken to be 23.0 times smaller than the measured REW of Cr II 2056. The remaining absorption was attributed to be due to Zn II 2026. In a few individual QSO spectra, comparison of the strength of Mg I 2852 to that of Mg II 2796, 2803 suggests that Mg I 2852 may be approaching saturation, which implies that the strength of the Mg I 2852 line may be less than 32.0 times the strength of Mg I 2026. We mention this as a precaution that we will neglect for now.
     ^b The feature at 2062 Å is a blend due to Cr II and Zn II. The REW of Cr II 2062 was taken to be 0.50 times the measured and summed REWs of Cr II 2056 and Cr II 2066, or 0.75 times the measured REW of Cr II 2056, depending on which resulted in smaller propagated errors. The remaining absorption was then attributed to be due to Zn II 2062.
     ^c When upper limits (2 ) on metallicities are reported, they represent those that apply for the quoted W limit or interval. Since this does not include 100% of the DLA gas (§ 2.3), a correction is made (§ 3) to derive results on the cosmic DLA gas metallicity, which is reported in the last column of this table.
     ^d The following oscillator strengths are adopted: f = 0.4890 for Zn II 2026.14, f = 0.2560 for Zn II 2062.66, f = 0.00471 for Cr II 2026.27, f = 0.105 for Cr II 2056.25, f = 0.0780 for Cr II 2062.23, f = 0.0515 for Cr II 2066.16, f = 0.1120 for Mg I 2026.48, and f = 1.8100 for Mg I 2852.96. See http://kingpin.ucsd.edu/hiresdla for details and references. Metal abundances are relative to the solar values of Grevesse & Sauval 1998.