a Because of line saturation, direct integration of this line provides only
a  a lower limit on the column density.
b The corresponding OVI{lambda}1031.93 line is affected by hot pixels in 
b  the line core, and this prevents an accurate line saturation assessment.
b   In this table we list the formal column density measurement and 
b    uncertainty, but we note that this column could be underestimated due to
b     line saturation.
d The Ly{alpha} profile has a deep core that approaches close to the 
d  zero-flux level. However, the good agreement of the Ly{alpha} and 
d   Ly{beta} apparent column density profiles indicates that the Ly{alpha} is
d    not significantly affected by unresolved saturation.
e At this redshift, Ly{alpha} is redshifted beyond the long-wavelength end
e  of the STIS E140M spectrum. Ly{beta} is not detected, so no integrated 
e   quantities are listed in this table for HI.
f The OVI{lambda}1031.93 profile is affected by hot pixels on the red side
f  of the profile (see Lehner et al., 2006, Cat. <J/ApJS/164/1>), so integrated
f   quantities must be measured from the OVI{lambda}1037.62 line.
g At this redshift, Ly{alpha} is redshifted beyond the long-wavelength end
g  of the STIS E140M spectrum, but several higher Lyman series lines are 
g   detected (see Ganguly et al., 2006ApJ...645..868G). Here we list the 
g    results from direct integration of the Ly{beta} profile instead of 
g     Ly{alpha}.
h OVI{lambda}1037.62 is blended with the Milky Way CIV 1548.20 profile. The
h  OVI{lambda}1037.62 profile is generally consistent with that of 
h   OVI{lambda}1031.93 (see Ganguly et al., 2006ApJ...645..868G), but the 
h    integrated quantities derived from {lambda}1037.62 are significantly 
h     contaminated and, thus, are not listed here.
i Both the OVI{lambda}1031.93 and {lambda}1037.62 profiles are affected by 
i  hot pixel features (see Fig. 39). Fortunately, the position of the 
i   spectrum on the detector was shifted between the 2002 January and 
i    February observations, and the hot pixels are only present in the 2002 
i     February data. As demonstrated in Fig. 39, we were able to suppress the 
i      hot pixels by rejecting the affected regions in the 2002 February data.
j The OVI doublet at this redshift is clearly identified based on the good
j  agreement of the apparent column density profiles. However, no HI lines 
j   are detected in this absorber despite good S/N in the region of the 
j    Ly{alpha} transition.
k The OVI{lambda}1031.93 profile is blended with an unrelated Ly{alpha} 
k  line on the blue side of the profile. This portion of the profile was 
k   excluded from the integration. The good agreement of the {lambda}1031.93
k    and {lambda}1037.62 N_a(v)_ profiles at v>-30km/s suggests that this 
k     blend does not severely affect the {lambda}1031.93 line.
l The OVI{lambda}1031.93 profile is blended with a Galactic H2 line on the 
l  blue side of the profile. The velocity range affected by the H2 blend was
l   excluded from the integration; consequently, the equivalent width and 
l    column density from direct integration somewhat underestimate the true 
l     quantities.
m At this redshift, Ly{alpha} is strongly blended with OI{lambda}1302.17 
m  absorption from the Lyman-limit absorber at z_abs_=0.08092 (Jenkins et 
m   al. 2005). The Ly{alpha} equivalent width listed in this table is the 
m    estimated value after removal of the OI contamination. This correction is
m     highly uncertain, and the remaining Ly{alpha} absorption (after removal 
m      of the OI line) is weak, consequently we consider this measurement to be
m       highly uncertain.
n Comparison of the OVI{lambda}1031.93 and {lambda}1037.62 apparent column 
n  density profiles indicates that the {lambda}1031.93 profile is affected 
n   by line saturation. For the weaker {lambda}1037.62 line, we list the OVI 
n    column density and its uncertainty obtained from direct integration, but 
n     we recognize that this measurement may underestimate the true column due 
n      to saturation.
o HI Ly{alpha} absorption is weak but clearly present at this redshift (see
o  further comments in the Appendix). Unfortunately, the Ly{alpha} line 
o   parameters cannot be measured due to severe blending with CI* absorption 
o    from the Milky Way ISM.
x measurements of marginally detected lines