The metallicities used for the FOGGIE absorbers are conceptually slightly
different from the metallicities derived in KODIAQ-Z and other spectral
surveys, in that the metallicities reported for FOGGIE are the column density-
weighted average of the gas cells identified as the absorber rather than the
result of a fit to single-phase ionization models. However, Marra et al.
(2021) show that these two approaches, when applied to the same physical
system, do not lead to large discrepancies in the average metallicity of the
gas. The precise metallicities of FOGGIE’s absorbers likely depend strongly on
its implementation of supernova feedback, and these would be expected to
differ slightly (e.g., be generally lower or higher) for different
implementations. Yet despite FOGGIE’s overall higher metallicity, the general
similarity between the observed and simulated absorbers in Figure 27 seems to
be a good indication that the trends observed in the KODIAQ-Z, HD-LLS, and DLA
surveys can in principle be explained by CGM and nearby IGM gas around typical
galaxies at these redshifts.

Figure 29: Metallicities of the FOGGIE H I absorbers versus their distance
from the central galaxy, colored by the distance to their closest galaxy.
Possible “closest galaxies” include the central and all satellites with more
than 1% of the central’s stellar mass. High metallicity absorbers far from the
central galaxy tend to be close to a satellite galaxy. Dashed and dotted lines
are the same as in Figure 18

###  9.3 Insights from FOGGIE Simulations

Given some similarities in the metallicity trends with $N_{\rm H\,I}$ between
our samples of observed and simulated absorbers, we can use the FOGGIE
simulations to shed light on the origin(s) of these absorbers and their
connection to galaxies. From the empirical results from KODIAQ-Z, the
overdensities (at least for the pLLSs, LLSs, and SLLSs) imply that these
absorbers should largely probe gas within virialized (mini)halos (see §7.1).
The Keck Baryonic Structure Survey (KBSS) also shows that at $z\sim 2$–3 there
is a strong incidence of absorbers with $\log N_{\rm H\,I}>14.5$ with galaxies
at transverse physical distance $\lesssim 300$ kpc and velocity separation
between the absorber and galaxy redshifts $\lesssim 300$ ${\rm km\,s}^{-1}$
(Rudie et al., 2012). This connection is not observed for lower $N_{\rm H\,I}$
absorbers, also implying some connection between $\log N_{\rm H\,I}>14.5$
absorbers and galaxies. On the other hand, recent MUSE IFU observations also
show at least some LLSs may probe IGM filaments (Fumagalli et al., 2016a;
Lofthouse et al., 2020). With the FOGGIE simulations, we can explore the
origins of these absorbers without observational constraints due to, e.g., due
to brightness limit of the galaxies. It is possible, however, that biases due
to the selection criteria of the FOGGIE galaxies as Milky Way-like analogues
at $z=0$ could bias the results in some way. Importantly, we can also explore
if and how the origins may depend on the metal enrichment of the absorbers.

Each of the central FOGGIE galaxies is surrounded by a number of satellites at
$z=2$–3. These satellite galaxies likely contribute to the enrichment seen in
our absorbers, and it is worth determining whether a given absorbers is more
likely to be associated with such a satellite than with the central galaxy.
Including only those satellites with at least 1% of the central galaxy’s
stellar mass, we identify which galaxy each absorber is physically closest to.
In Fig. 29, we compare the absorber metallicities to their distance from the
central galaxy and the distance to their closest galaxies, be that a satellite
or the central galaxy. Generally, distance to an absorber’s closest galaxy
increases with distance from the central galaxy, which is the behavior we
expect for absorbers whose closest galaxy is the central galaxy. Metallicity
also tends to decrease with increasing distance from the central galaxy. Yet,
there are important exceptions to these two trends: some absorbers are far
from the central galaxy yet close to a satellite, and these absorbers span the
range of extracted metallicites. This includes some absorbers distant from the
central galaxy that have metallicity close to and above solar. Therefore, not
all high metallicity absorbers should be assumed to be associated with the
central galaxy.

In Figs. 30 and 31, we select FOGGIE absorbers that are inflowing toward or
outflowing from the central galaxy. This separation is made based on the angle
between an absorber’s 3D velocity vector and its position vector, both of
which are calculated in the rest frame of the relevant central FOGGIE galaxy.
Outflowing gas must have an angle $\theta>60^{\circ}$, while inflowing
absorbers must have $\theta<120^{\circ}$. This is equivalent to
$\hat{v}\cdot\hat{r}=\cos\theta=\pm 0.5$. This cut prevents gas that is
neither strongly inflowing nor outflowing from being selected.

Figure 30: Metallicities of the FOGGIE H I absorbers in Figure 27, split into
outflowing (red) and inflowing (blue) based on $|\hat{v}\cdot\hat{r}|>0.5$ in
the frame of the host central galaxy. Saturation shows the magnitude of the
radial velocity. Probability densities are provided as histograms along the
side and top. Both metallicity distributions are repeated in the side panels,
with the filled histogram corresponding to the adjacent scatter plot. Contours
have been added to show where the density of inflowing absorbers is highest.
Figure 31: On the left, the metallicities of outflowing (red) and inflowing
(blue) FOGGIE absorbers are binned versus their distance from their host
central galaxies, colored by the average radial velocity for that bin. On the
right, the gas in all eighteen FOGGIE snapshots is shown in the same
configuration. The mean metallicity ($\log\langle Z/Z_{\odot}\rangle$) is
marked with a black line. The dashed line indicates the solar metallicity
level. Probability densities are shown at the top and sides of each panel.

Fig. 30 shows the metallicity and H I column densities of our inflowing (blue)
and outflowing (red) FOGGIE absorbers. PDFs are also included for these two
quantities, with both metallicity PDFs repeated in the upper and lower panels
for comparison. The inflowing absorbers dominate by number, but both
categories have similar H I column distributions with absorbers becoming more
numerous at lower H I column densities. The outflowing absorbers skew towards
the high metallicity end of the distribution. This is not surprising, as in
FOGGIE winds are launched by the same supernova feedback that also enriches
the surrounding gas. There is a plateau in the outflowing metallicity
distribution around $-2\lesssim\log Z/Z_{\odot}\lesssim-1$, which may be
tracing older outflows that have slowed and mixed with the ambient CGM. These
absorbers number significantly less than the inflowing absorbers at the same
metallicity, however, so it would be difficult for observations to disentangle
these less enriched outflows. The inflowing absorbers follow a more symmetric
metallicity distribution, with a peak about 0.5 dex above the metal-poor limit
for KODIAQ-Z; though, as stated above, the FOGGIE absorbers generally tend to
have higher metallicities than seen in the random sightlines observed by
KODIAQ-Z. The inflowing absorbers also extend to the lowest metallicities.
Even though Fig. 29 reveals that some absorbers may be closer to a satellite
than to the central galaxy, the trends in Fig. 30 are unchanged when the
absorbers are limited to those whose closest galaxy is the central. The
biggest difference is that there are no outflowing absorbers with $\log
Z/Z_{\odot}<-2.4$.

Although the outflowing absorbers dominate the high end of the metallicity
PDF, they are far outnumbered by the inflowing absorbers even at the highest
metallicities. This is largely due to the selection on H I and the underlying
physics included in the FOGGIE simulations. There is very little cool gas that
would form H I within the outflows as these are driven only by thermal
pressure. Simulations with additional non-thermal pressure sources such as
magnetic fields and cosmic rays (Butsky & Quinn, 2018; Ji et al., 2020)
demonstrate an increase in H I at large radii within the CGM. It is therefore
quite likely that the number of H I absorbers classified as either inflowing
or outflowing following our definition would change if these physical
processes were included in the FOGGIE simulations, though it is likely that
the numbers would still favor inflowing gas.

With Fig. 31, we look at the metallicity and velocity of the FOGGIE absorbers
as a function of their distance from the central simulated galaxy. We also
compare the absorbers to the underlying gas distributions. This distribution
compiles together the gas in all 18 FOGGIE outputs we sampled. Probability
densities are shown for the metallicity and radial distributions, and the mean
metallicity of the gas is shown with a black line. Colors indicate the mean
radial velocity at that metallicity and radius; we note that, unlike with the
absorbers, the gas radial velocity has no selection based on the angle toward
or away from the galaxy.

First, we consider outflowing material: outflowing absorbers with the highest
metallicities tend to be at or within the virial radius of these central
halos, which at $z=2$–3 is about 30–50 kpc, and have the highest velocities.
These velocities are generally higher than what is seen in the gas at similar
radii and metallicities, and appears consistent with fast-moving enriched
material launched by stellar feedback. On the other hand, high metallicity gas
can be found even beyond the virial radius, implying that galactic outflows
become more diffuse as they travel farther away from the galaxy. The
outflowing absorbers with the lowest metallicity are found well outside the
virial radius, and their velocities are comparable to the gas in this regime.
This supports the interpretation that these absorbers come from previously
ejected gas.

Inflowing absorbers can be found at all radii, with their metallicity
generally increasing the closer they are to their central galaxy, similar to
the outflowing gas. The velocity of these inflowing absorbers is also higher
near the galaxy. The FOGGIE zoom simulations contain several satellite and
pre-merger galaxies that are producing their own enriched outflows, which
explains why high metallicity absorbers can be found at large distances from
the central galaxy. These absorbers do not appear to reflect the fastest
inflowing gas, which has very high metallicity and can again be found at all
radii.

Together, Figs. 30 and 31 imply that, given a set of H I-selected observed
absorbers that are known or assumed to be associated with a galaxy system,
most of these absorbers are likely to be inflowing towards a central galaxy.
The precise number of inflowing and outflowing absorbers predicted by
simulation will depend on the included physics, especially non-thermal
pressure sources, though inflowing absorbers will likely still dominate. This
dominance is true across column densities and metallicities, as satellites and
nearby companions enrich gas flowing towards the central galaxy. Whether
inflowing or outflowing, more enriched absorbers are more likely to be located
physically close to the central galaxy.

##  10 Discussion

###  10.1 Bridging the LYAF and DLAs

The history of metallicity in the universe provides an important constraint on
models of galaxy formation and evolution. The metals in the universe represent
a fossil record of star formation; characterizing how the metallicities change
with H I column density (and hence overdensities or densities) yields
information on the transport of metals and efficiency of that transport from
the densest to the most diffuse regions of the universe. At high redshift,
much of the effort has focused on the metal enrichment of the most diffuse
regions probed by the LYAF (e.g., Cowie et al. 1995; Songaila 1998; Ellison et
al. 2000; Schaye et al. 2000, 2003; Aguirre et al. 2004; Simcoe et al. 2004;
Simcoe 2011) and the densest regions of the universe probed by DLAS (e.g.,
Pettini et al. 1997, 1999; Prochaska 1999; Prochaska et al. 2003; Rafelski et
al. 2012; Jorgenson et al. 2013). The HD-LLS survey (Prochaska et al. 2015;
Fumagalli et al. 2016b, and see also Berg et al. 2021 for the XQ-100 survey of
SLLSs) has surveyed lower H I column density absorbers mostly in the range
$17.8\lesssim\log N_{\rm H\,I}<20.3$. With KODIAQ-Z (this work, and earlier
KODIAQ surveys Lehner et al. 2014, 2016), we bridge the gap between the
DLA/SLLS regimes and the LYAF. 171717We show in §6.3 that similar trends of
the metallicities with $N_{\rm H\,I}$ are observed at low and high redshifts
in the range $15\lesssim\log N_{\rm H\,I}\lesssim 22$. However, the current UV
observations at low $z$ do not have sensitivity to probe much lower
metallicities than ${\rm[X/H]}<-1$ in the LYAF at $z<1$ (this would need to
await a future $\sim$6-m UV space-based telescope), and we cannot yet assess
the full range of metallicities for absorbers with $\log N_{\rm H\,I}<15$ at
$z<1$. Therefore, we keep our discussion focused on the high redshift
universe.

In §6.2, we show that the scatter of absorber metallicities at
${\rm[X/H]}\geq-2.4$ is quite similar for the DLAs and the $14.6\lesssim\log
N_{\rm H\,I}\lesssim 20$ regime, i.e., metal enriched gas is observed not only
in the densest regions (in or near galaxies) but has also spread to the more
diffuse regions down to overdensities $\delta\lesssim 10$ (see Fig. 18).
However, as $N_{\rm H\,I}$ decreases below $\log N_{\rm H\,I}\lesssim 14.4$
(diffuse IGM), most of the absorbers have metallicities
${\rm[X/H]}\lesssim-1.6$ (see Fig. 5 in Simcoe et al. 2004), while gas with
$-1.6\lesssim{\rm[X/H]}\lesssim-0.2$ is commonly observed over the entire
range $14.6\lesssim\log N_{\rm H\,I}\lesssim 22$. Therefore the diffuse IGM
probed by LYAF absorbers has not been enriched at the same level as stronger H
I absorbers.

In contrast, for metallicities ${\rm[X/H]}\lesssim-2.4$, blind surveys of DLAs
do not reveal a significant population of VMP DLAs (e.g., Rafelski et al.,
2012; Jorgenson et al., 2013). Yet, VMP absorbers are regularly observed at
$\log N_{\rm H\,I}\lesssim 20$, and their frequency increases with decreasing
$N_{\rm H\,I}$ (see Table 6 and Fig. 18). These VMP absorbers are of course
also observed in the LYAF. The median metallicity of the LYAF at $z\sim 2.5$
is around ${\rm[X/H]}=-2.8$ (Simcoe et al. 2004; Simcoe 2011 and see also,
e.g., Ellison et al. 2000; Schaye et al. 2003; Aguirre et al. 2004), which is
a factor 2.5 lower than the median metallicity of the SLFSs at $\langle
z\rangle\simeq 2.8$ (Table 4). However, owing to sensitivity issues, the
lowest metallicities found for LYAF absorbers are around ${\rm[X/H]}\sim-3.5$,
while our survey reveals a population of absorbers with ${\rm[X/H]}<-3.5$ that
is nearly and completely metal-free (see §10.2, and also Fumagalli et al.
2011a; Lehner et al. 2016). Simcoe et al. (2004) estimated that about 70%–80%
of the LYAF has been enriched to ${\rm[X/H]}\gtrsim-3$, but 20–30% might be
chemically pristine gas at low densities, which is about the same as the
fraction of SLFSs with ${\rm[X/H]}<-3$.

Therefore, gas in the intermediate overdensity regime between the DLAs and
LYAF has metallicities that are found in both the most diffuse and densest
region of the universe. Gas probed by absorbers with $14.6\lesssim\log N_{\rm
H\,I}\lesssim 20$ has a much larger dispersion in metallicity than observed
either in $\log N_{\rm H\,I}\lesssim 14.4$ or $\geq 20.3$ gas. The
simultaneous presence of abundant pristine, metal-rich, intermediate
metallicity gas is unique to the H I column density range $14.6\lesssim\log
N_{\rm H\,I}\lesssim 20$. Below we discuss in more details these various
levels of chemical enrichment and the mixing of metals in the
$14.6\lesssim\log N_{\rm H\,I}\lesssim 20$ range.

###  10.2 Pristine Gas

From the KODIAQ-Z survey and CCC at low redshift, we find that there is an
abundance of VMP absorbers in relatively high overdensity (except for the DLAs
by definition). While the metallicities have increased by about a factor 8–10
from $2.2\lesssim z\lesssim 3.6$ to $z<1$, the fractions of VMP absorbers are
strikingly similar at low and high redshifts in $\log N_{\rm H\,I}<19$
absorbers. On the other hand, owing to the overall increase of the metallicity
from $2.2\lesssim z\lesssim 3.6$ to $z<1$, it is not surprising that extremely
metal poor gas with ${\rm[X/H]}<-3.5$ or even $<-3.0$ is scant at $z<1$ (CCC
III). With KODIAQ-Z, we determine that the fractions of SLFSs and pLLSs with
${\rm[X/H]}<-3.5$ and $<-3.0$ are about 3%–10% and 15%–25% (90% confidence
intervals, see Table 6). Combining KODIAQ-Z and HD-LLS, similar numbers are
derived for the LLSs. For the SLLSs, the fractions of absorbers with these
metallicities are smaller by about a factor 2.

The pristine LLSs reported by Fumagalli et al. (2011a) at $z\sim 3.5$ have
${\rm[X/H]}<-3.8$ and $<-4.2$, but at the time of this discovery it was
impossible to say how common this population was. With KODIAQ-Z, we can
revisit this question (see also Lehner et al. 2016). The lowest metallicity
where some metals are detected is around ${\rm[X/H]}\lesssim-3.8$ in KODIAQ-Z
(see Fig.18). We use that value of ${\rm[X/H]}\simeq-3.8$ to separate pristine
(no metal) from metal-enriched (even at very low levels) absorbers.
Considering Fig. 18, we can separate the population of H I absorbers into two
broad categories owing to the impact that upper limits on ${\rm[X/H]}$ can
have for interpreting the frequency of pristine absorbers:

1) For absorbers with $16\leq\log N_{\rm H\,I}\leq 20$, there are only 11
upper limits on ${\rm[X/H]}$: 3 out 179 these absorbers have
${\rm[X/H]}<-3.8$, implying a frequency of pristine absorbers in the range
0.7%–4.2% (90% CI) in this column density interval. This number cannot
increase by much more than a factor $\sim$2 including data with higher upper
limits. Even if all the upper limits represent pristine gas for absorbers with
$\log N_{\rm H\,I}\geq 16$, this would increase the frequency of pristine
absorbers to only 3.7%–9.6% (90% CI). Hence, the fraction of pristine $\log
N_{\rm H\,I}\geq 16$ absorbers (i.e., gas with overdensities $\delta\gtrsim
50$–100) is at least 1% and at most 10% at $2.2\lesssim z\lesssim 3.6$.

2) The second regime is for absorbers with $14.6\lesssim\log N_{\rm H\,I}<16$
where the upper limits on the metallicities are much more numerous. Taking
strictly ${\rm[X/H]}<-3.8$, there are 4 absorbers out of 142, implying a
frequency of pristine absorbers of 1.3%–6.1% (90% CI), a similar percentage to
that of absorbers with higher $N_{\rm H\,I}$. However, if all the $\log N_{\rm
H\,I}<16$ absorbers with upper limits such as ${\rm[X/H]}<-3$ probe pristine
absorbers, then the frequency of pristine $\log N_{\rm H\,I}<16$ absorbers
would increase to 13.3%–23.9% (90% CI). This would be similar to the possible
population of metal-free LYAF absorbers at similar redshifts (see previous
section and Simcoe et al. 2004). The fraction of pristine gas in overdensities
$\delta\gtrsim 50$–100 at $2.2\lesssim z\lesssim 3.6$ is therefore at the
level of a few percent, while for smaller overdensities it is likely in the
range 10%–20%.

The frequency of mock absorbers with ${\rm[X/H]}<-3.8$ in the FOGGIE
simulations is very similar to the frequencies found in KODIAQ-Z, despite the
FOGGIE absorbers on average have higher metallicities than observed. In
contrast, cruder resolution simulations show a tendency to have over-enriched
pLLSs and LLSs (see discussion in Fumagalli et al. 2011a). In the EAGLE HiRes
cosmological hydrodynamical simulations, Rahmati & Oppenheimer (2018) find a
fraction of pristine gas with ${\rm[X/H]}<-3.8$ of about 10% in the pLLS and
LLS regimes. However, contrary to FOGGIE and the observations reported here or
at low redshift (; ), the EAGLE simulations show little change of the
metallicity with $N_{\rm H\,I}$ (see also ; ); the FIRE simulations also show
similar results (Hafen et al., 2017). Consistent with the lack of $N_{\rm
H\,I}$ dependence, these simulations find a significant population of
${\rm[X/H]}<-3$ DLAs that is not observed. This highlights some issues in
simulations that may be related to the implementation of feedback physics, but
is probably also related to insufficient resolution in the more diffuse gas.
As discussed in §9.2, low-metallicity inflowing gas is able to naturally get
much closer to the galaxy when the CGM structures are resolved than in the
standard-resolution simulations because the metals are not forced to over-mix
in the regions around galaxies (see also Peeples et al. 2019; van de Voort et
al. 2019; Hummels et al. 2019; Suresh et al. 2019). As discussed in §9.3 and
shown in Figs. 29, 30, 31, the pristine and the VMP absorbers predominantly
probe inflowing cool gas (see, also Hafen et al. 2017; Rahmati & Oppenheimer
2018; Suresh et al. 2019), consistent with the idea that these absorbers are
ideal candidates for the cold-mode accretion (e.g., Kereš et al., 2005; Dekel
et al., 2009; Fumagalli et al., 2011b).

###  10.3 Extreme Metallicities and Metal-rich gas

The metal-enriched diffuse gas constitutes a record of the transport of metals
from the densest to the most diffuse regions of the universe. In §10.1, we
discuss that while the LYAF shows evidence for metal enrichment, it is not
enriched to levels seen in higher H I column absorbers have. Metallicities in
the range $-1.6\lesssim{\rm[X/H]}\lesssim-0.2$ are commonly observed over the
entire range $14.6\lesssim\log N_{\rm H\,I}\lesssim 22$, but not in the LYAF.
Therefore, at $2.2\lesssim z\lesssim 3.6$, galaxies have not yet polluted the
diffuse IGM with metals at the same level as denser regions of the universe.

In Lehner et al. (2016), we reported the discovery of one supersolar pLLS at
$z\simeq 2.5$ with ${\rm[X/H]}\simeq+0.2$.181818The HIRES spectrum of this QSO
was not released in KODIAQ DR2 and therefore is not part of the present
KODIAQ-Z survey. Besides its metallicity, this pLLS is unique on several other
levels including the detection of O I, its small physical (0.35 pc),
relatively high density ($n_{\rm H}\simeq 0.2$ cm-3), and multiphase nature,
with C IV having a very different velocity profile compared to the low ions
(see Fig. 14 in Lehner et al. 2016). We argued in that paper that its high
metallicity and multiphase nature strongly suggest that it directly probes an
active outflow from a proto-galaxy at $z\simeq 2.5$. At $z\sim 1.8$, Prochaska
et al. (2006) uncovered two supersolar SLLSs, suggesting that these metal-rich
absorbers may represent a significant metal reservoir in the young universe.

However, the HD-LLS survey does not report any supersolar SLLS (see Fig. 18),
and the XQ-100 survey only reports one supersolar SLLS at $z\sim 2.5$ (see
Fig. 2 in Berg et al. 2021; we exclude poorly-constrained upper limits on the
metallicity that are above solar in that survey). Adding that supersolar pLLS
to the KODIAQ-Z+HD-LLS survey would imply that only 1 out 242 absorbers has a
supersolar metallicity at $2.2\lesssim z\lesssim 3.6$, i.e.,
$0.41\%^{+1.42\%}_{-0.32\%}$ (90% CI) of the absorbers have ${\rm[X/H]}>0$.
None is found in the R12-DLA either, implying that the fraction of supersolar
absorbers in the H I column density range $14.6\lesssim\log N_{\rm H\,I}<22$
at $2.2\lesssim z\lesssim 3.6$ drops to $0.29\%^{+1.00\%}_{-0.23\%}$.
Supersolar metallicity absorbers are therefore very rare at $2.2\lesssim
z\lesssim 3.6$ for any $N_{\rm H\,I}$ absorber.

At low redshift, the situation is quite different, with at least 2%–6% of
supersolar absorbers at $z<1$ (see Fig. 21, and CCC III). This number could
increase by a factor $\sim$3 if a harder EUVB was used instead of the HM05
EUVB to model the absorbers (at low redshift the effect of the EUVB is more
important, see CCC II and §5). This increase of supersolar absorbers is
consistent with the overall increase of the metallicities by a factor 8–10
from $2.2\lesssim z\lesssim 3.6$ to $z<1$ (see Fig. 20).

The larger fraction of metal-enriched and even super-metallicity absorbers at
low redshift indicates a much larger volume of the universe has been exposed
to metal pollution than at $2.2\lesssim z\lesssim 3.6$. Ferrara et al. (2000)
developed a model that predicts at $z<1$ essentially all absorbers should have
associated metal absorption, and the spread in metallicity should be less than
1 dex. This is not case. Even at $z<1$, the enrichment of the most diffuse gas
in the universe is still very inhomogeneous in view of the nearly 3 dex spread
in metallicities at $z<1$ for absorbers with $15\lesssim\log N_{\rm
H\,I}\lesssim 19$ (see Fig. 21 and next section).

###  10.4 Inhomogeneous Metal Mixing

There is ample of evidence for inhomogeneous abundances in H I column density
$14.6\lesssim\log N_{\rm H\,I}\lesssim 20$ gas where the metallicities range
from pristine (${\rm[X/H]}<-4$) to about ${\rm[X/H]}\simeq-0.2$ dex, a factor
at 6,000 spread from the lowest to highest metallicities. Similar results are
found at $z<1$, but a factor somewhat smaller with $1,000$ variation between
the highest and lowest metallicities (CCC III and Fig. 21). However, our
results also show there is inhomogeneous metal mixing in single halos as
directly evidenced by the large variation in metallicity in closely redshift-
separated absorbers (see Fig. 23). Such large metallicity variation over small
redshift separations was initially reported by Prochter et al. (2010) between
a SLFS, a pLLS, and a LLS at $z\sim 3.5$ separated in velocities along the
same QSO from about 130 to 180 ${\rm km\,s}^{-1}$ where the metallicity
differences were a factor 3, 40, and 158. Now with a sample of 37 paired
absorbers, we find similarly large metallicity variations between absorbers
separated by less than $\Delta v<500$ ${\rm km\,s}^{-1}$ along a given QSO
sightline where about half of paired absorbers have metallicity variations of
a factor 2–3 and for the other half of a factor $>140$. It is plausible that
the smaller variations may be related to the variation within a halo, while
the large variations to gas in inter-halos.

Thus, within the overdensities of a few to several hundreds, the gas probed by
absorbers with $14.6\lesssim\log N_{\rm H\,I}\lesssim 20$ is chemically
inhomogeneous where both metal-poor and metal-rich gas are observed. This
again appears unique to the $14.6\lesssim\log N_{\rm H\,I}\lesssim 20$ column
density range. While for DLAs determining the metallicity in individual
components is complicated since the H I velocity structure cannot be recovered
over $\Delta v<500$ ${\rm km\,s}^{-1}$, the metallicity spread for the DLAs is
much smaller than observed at $14.6\lesssim\log N_{\rm H\,I}\lesssim 20$ (see
10.1). It is also much smaller for the LYAF (e.g., Simcoe et al., 2004),
implying overall a more chemically homogeneous gas in the LYAF and DLA
regimes. Therefore, in and quite near galaxies, in the gas traced by DLAs, the
metal enrichment from supernovae is quite efficient, but beyond the immediate
vicinity of the galaxies, the volume filling factor for metals must be low,
which is consistent with models of metal ejection from supernovae that is not
expected to be efficient and confined to small regions (e.g., Ferrara et al.,
2000; Scannapieco, 2005).

##  11 Summary and Concluding Remarks

Using the KODIAQ DR2 data from the KOA (O’Meara et al., 2015), we have built a
sample of 202 H I-selected absorbers with $14.6\leq\log N_{\rm H\,I}\leq 20$
at $2.2\leq z\leq 3.6$ comparable in size to our companion survey, CCC, at
$z<1$. The H I selection and the H I column density range both ensure that no
bias is introduced in the metallicity distribution of these absorbers, i.e.,
we are sensitive to any absorbers with ${\rm[X/H]}\gtrsim-3.5$. The H I
selection also provides a clean separation of the absorbers based on H I
column density, which is largely used to separate the LYAF, absorbers with
$\log N_{\rm H\,I}\lesssim 14.5$ (IGM), from the denser regions of the
universe probed by stronger H I absorbers. By definition, the SLFSs all have
over-densities $\delta>3$ in our sample ($z=3.6$, the maximum redshift in our
statistical sample corresponds to this $\delta$ value using the analytical
expression in Schaye 2001b). In contrast, a metal-selection using C IV or O VI
can include a wide range of H I column density absorbers from the LYAF to the
pLLS regime.

In the KODIAQ-Z survey, we have 155 SLFSs, 24 pLLSs, 16 LLSs, and also 7
SLLSs, for a total of 202 absorbers. To increase the number of LLSs and SLLSs
in our sample, we use the H I-selected absorbers from the HD-LLS survey that
have a H I column density range $17.2\leq\log N_{\rm H\,I}\leq 20$, but a
majority have $17.7\lesssim\log N_{\rm H\,I}\leq 20$ (Prochaska et al., 2015;
Fumagalli et al., 2016b). We also use the results from survey from Rafelski et
al. (2012) to study the metallicity changes with $N_{\rm H\,I}$ in the DLA
regime. For both of these surveys, we restrict them survey to absorbers at
$2.2\leq z\leq 3.6$, unless otherwise stated.

For all the absorbers with $\log N_{\rm H\,I}\lesssim 20$ in the KODIAQ-Z and
HD-LLS, we derive the posterior PDFs of the metallicities and other physical
quantities using a Bayesian formalism that employs a MCMC sampling of a grid
of Cloudy photoionization models (where we assume photons from the HM05 EUVB
provide the source of photoionization). This follows directly from the
methodology used in HD-LLS (Fumagalli et al., 2016b) and CCC (; ). For
absorbers with less than ideal constraints (about half of the SLFS sample and
a few pLLSs), we adopt the “low-resolution” method developed at low redshift
by Wotta et al. (2016) and refined in CCC II to estimate the metallicities.
Using SLFSs and pLLSs with reliable constraints from the metal ions, we find
that $\log U$ can be reasonably well modeled by a Gaussian for the SLFSs and
pLLSs, which can then be used reliably as a prior in the Bayesian MCMC
modeling. We explore the effects of changing the EUVB from HM05 and HM12 to
estimate the metallicities (Figs. 9, 10), and we find that the changes in the
metallicities between these two EUVBs are negligible for the absorbers with
$\log N_{\rm H\,I}\gtrsim 17.2$. For the SLFSs and pLLSs, the effect is only
an increase of $+0.12\pm 0.15$. The effect from changing the EUVBs on the
metallicities is therefore much smaller than at $z<1$.

Our main findings on the properties of our statistical sample of H I selected
absorbers with $14.6\leq\log N_{\rm H\,I}\leq 20$ at $2.2\leq z\leq 3.6$ can
be summarized as follows.

  1. 1.

From the comparison of the absorption profiles and the width of the profiles,
we conclude that singly, doubly, triply ionized species (e.g., Si II, Si III,
Si IV, C II, C IV) and H I often trace the same gas in absorbers with $\log
N_{\rm H\,I}<19$. For SLFSs and pLLSs, we also find that when O VI absorption
is present, it has often a similar velocity structure than lower ions, i.e.,
the O VI absorption is commonly narrow in these absorbers. This contrasts
remarkably from the O VI that is frequently strong and broad when detected in
absorbers with $\log N_{\rm H\,I}\gtrsim 17.8$.

  2. 2.

From the profile fitting of the H I transitions, we show that 90% of the
components have $13.3\leq b\leq 40$ ${\rm km\,s}^{-1}$ with a mean $\langle
b\rangle=27\pm 6$ ${\rm km\,s}^{-1}$. This implies a temperature of the gas of
$T<4\times 10^{4}$ K, consistent with the gas being primarily photoionized.

  3. 3.

We find that a single-phase photoionization model is appropriate to match the
column densities of the low ions to high ions (including O VI) for the
majority of the SLFSs and pLLSs. For the LLSs and SLLSs, when O VI is
detected, a single-phase photoionization model cannot commonly reproduce the
observed O VI column density, implying that as $N_{\rm H\,I}$ increases, the
multiple gas-phase nature becomes more important.

  4. 4.

In our ionization models, ${\rm[C/\alpha]}$ is allowed to vary in the range
$[-1,+1]$ to accommodate for non-solar relative abundances between carbon and
$\alpha$-elements caused by nucleosynthesis effects. This approach allows us
to have a better sense of the uncertainties in the metallicity caused by the
variability of C/$\alpha$. Overall, we find that ${\rm[C/\alpha]}$ is in the
range $-0.6\lesssim{\rm[C/\alpha]}\ \lesssim+0.5$ as observed in other
environments (DLAs, stars, H II regions), but robustly studying the variation
of ${\rm[C/\alpha]}$ with ${\rm[X/H]}$ for these absorbers is hindered by the
ionization corrections that add too much noise in the ${\rm[C/\alpha]}$
distribution, hiding any subtle changes between ${\rm[C/\alpha]}$ with
${\rm[X/H]}$ that are expected to be at the level of a factor 2–3.

  5. 5.

The 155 H I-selected SLFSs ($14.6\leq\log N_{\rm H\,I}<16.2$) probe a wide
range of metallicities from ${\rm[X/H]}<-4$ to ${\rm[X/H]}\simeq-0.2$. The
metallicity posterior PDF is negatively skewed with a prominent tail extending
well below ${\rm[X/H]}<-3$. It has a main peak around the median value
${\rm[X/H]}\simeq-2.4$ and another smaller peak around $-0.6$ dex solar (the
dip around $-1.1$ is observed in both binned and unbinned data).

  6. 6.

The 24 H I-selected pLLSs ($16.2\leq\log N_{\rm H\,I}<17.2$) probe a range of
metallicity from ${\rm[X/H]}<-4.2$ to about ${\rm[X/H]}\simeq-1$. The sample
is too small to robustly characterize the distribution and the lack of pLLSs
with ${\rm[X/H]}>-1$ could be mainly due to small-number statistics. However,
both the median ($-2.1$ dex) and IQR metallicities imply an overall increase
in metallicities compared to the SLFSs despite the lack of ${\rm[X/H]}>-1$
pLLSs.

  7. 7.

Our sample of H I-selected LLSs ($17.2\leq\log N_{\rm H\,I}<19$) consists of
16 absorbers that we combine with the HD-LLS survey to reach a size sample of
62 LLSs. The full range and median of the LLS metallicity PDF are quite
similar to that of the pLLSs. Combining the pLLSs+LLSs, the median metallicity
is $-2.2$ and IQR only 1 dex compared to $-2.42$ and 2 dex, respectively, for
the SLFSs. The pLLSs+LLSs are more frequent in the metallicity range
$-3.2\lesssim{\rm[X/H]}\lesssim-1.2$ but less frequent at very low metallicity
${\rm[X/H]}\lesssim-3.5$ than the SLFSs, showing there is a shift in the
metallicity enrichment properties of these absorbers below and above $\log
N_{\rm H\,I}\simeq 16.2$ (at $2.2\leq z\leq 3.6$, this corresponds to
overdensities of $\delta\simeq 140$–50).

  8. 8.

Combining the 7 SLLSs from KODIAQ-Z and 73 SLLSs from HD-LLS ($19\leq\log
N_{\rm H\,I}\leq 20$) and using the R12-DLA sample of 101 DLAs ($\log N_{\rm
H\,I}\geq 20.3$), the overall metallicity trend observed with $N_{\rm H\,I}$
continues in these regimes: the median/mean metallicity increases and IQR
decreases with increasing $N_{\rm H\,I}$. For the SLLSs, the median and IQR
metallicities $-1.9$ and $1.1$ dex, while these are $-1.4$ and $0.65$ dex for
the DLAs. DLAs have therefore rarely gas with ${\rm[X/H]}<-2.4$, while at
$\log N_{\rm H\,I}\lesssim 20$, VMP absorbers are not rare at $2.2\leq z\leq
3.6$.

  9. 9.

The fractions of extremely metal-poor systems with ${\rm[X/H]}<-3.5$ for the
pLLSs, pLLSs, LLSs are about the same, around 3–10% (90% confidence interval).
For the SLLSs, it is most likely somewhat smaller with a fraction in the range
0.3–5.4%. Yet, the most metal poor absorber in our sample is a SLLS with $\log
N_{\rm H\,I}=19.25\pm 0.25$ and ${\rm[X/H]}<-4.4$ with a cosmic overdensity of
several thousands.

  10. 10.

We find that (pristine) gas clouds with no metals down to limit
${\rm[X/H]}<-3.8$ constitutes about 1%–10% of the $16<\log N_{\rm H\,I}<20$
absorbers at $2.2\leq z\leq 3.6$, and increases to 10%–20% for $14.6\leq\log
N_{\rm H\,I}\leq 16$ absorbers, the latter being similar to the amount of
pristine gas found in the diffuse IGM. On the other hand, supersolar absorbers
at any $N_{\rm H\,I}$ at $2.2\lesssim z\lesssim 3.6$ are very uncommon
($<1\%$).

  11. 11.

Using paired absorbers with velocity separations of $\Delta v\lesssim 500$
${\rm km\,s}^{-1}$ along the same QSO sightlines, we find there is a large
scatter in the metallicity from about 0.2 dex to $>2$ dex. For about half of
the paired absorbers, there is evidence for metallicity variations over
$\Delta v\lesssim 500$ ${\rm km\,s}^{-1}$ of a factor 2–3, while for the other
half of a factor $>140$. It is plausible that the smaller variations
correspond to the change within a single galaxy halo, while the large
variations to differences between galaxy halos. Both the large metallicity
range and metallicity variation between paired absorbers imply that the
transport of metals from their formation sites (galaxies) into the CGM and the
IGM is very inhomogeneous.

  12. 12.

The photoionized gas associated with pLLSs, LLSs, and SLLSs contribute to the
cosmic baryon budget to $\Omega_{\rm g}/\Omega_{\rm b}\simeq 7\%$ and the
SLFSs contribute to another 5.5%. From the first KODIAQ survey (Lehner et al.,
2014), the O VI-bearing hot collisionally ionized gas associated with LLSs and
SLLSs is likely to contribute to about the same level. These are the second
largest contributors to the cosmic baryon budget at high redshift behind the
LYAF.

  13. 13.

We show that about 2%, 5%, 7% of the metals ever produced at $2.2\lesssim
z\lesssim 3.6$ are in photoionized gas associated with SLFSs, pLLSs, and LLSs,
respectively. The SLLSs account for another 18%, and therefore about 30% of
the metals at $2.2\lesssim z\lesssim 3.6$ in photoionized absorbers with
$14.6\leq\log N_{\rm H\,I}<20.3$. Combining the SLFSs, pLLSs, LLSs, and SLLSs,
their comoving metal mass density of the photoionized gas probed by these
absorbers is $\rho_{\rm m}=3.5\times 10^{5}$ M⊙ cMpc-3. Another possible
5%–20% of the cosmic metal budget may also be in form of highly ionized metals
in gas with $\log N_{\rm H\,I}\gtrsim 17.8$ (Lehner et al., 2014).

To study their cosmic evolution, we combine our results with the CCC survey
that explores the properties of similar absorbers at $z<1$ (; ; ). The cosmic
evolution of absorbers from $2.2\lesssim z\lesssim 3.6$ to $z\lesssim 1$ with
$\log N_{\rm H\,I}\gtrsim 15$ is summarized as follows.

  1. 14.

We find that from $2.2\leq z\leq 3.6$ to $z<1$, there is an overall increase
of the metallicity of the gas probed by SLFSs, pLLSs, LLSs, SLLSs, and DLAs by
a factor $\sim$8.

  2. 15.

While the metallicity threshold for the VMP absorbers increases by about 1 dex
from $2.2\leq z\leq 3.6$ to $z<1$, a similar fraction of about 50% of
absorbers with $\log N_{\rm H\,I}\lesssim 18$ are VMP at low and high $z$.

  3. 16.

Although there is plenty of primitive gas around $z\lesssim 1$ galaxies that
has largely not been polluted, the fraction of pristine SLFSs, pLLSs, LLSs
with ${\rm[X/H]}<-3$ at $z\lesssim 1$ is $<1$% at the 90% confidence level
over the range $15<\log N_{\rm H\,I}<19$. In contrast 10%–25% of similar
absorbers at $2.2\lesssim z\lesssim 3.6$ have ${\rm[X/H]}<-3$, implying that
although the transport of metals outside galaxies is still very inhomogeneous
at $z<1$, all regions with $\log N_{\rm H\,I}\gtrsim 15$ have been polluted to
some level by $z<1$.

  4. 17.

The hydrogen column density ($N_{\rm H}$) is a factor 10–15 smaller at $z<1$
than at $2.2\lesssim z\lesssim 3.6$, and therefore the contribution to
baryonic budget from the SLFSs, pLLSs, and LLSs are about 10 times smaller at
$z<1$ than at $2.2\lesssim z\lesssim 3.6$.

  5. 18.

The photoionized metals associated with the SLFSs, pLLSs, and LLSs take about
6% of the cosmic metal budget at low redshift. This is about a factor 2
decrease compared the contribution of the same absorbers at $2.2\lesssim
z\lesssim 3.6$, i.e., at low redshift most of the metals are found in or near
galaxies and in the intra-cluster medium (see Péroux & Howk 2020). This is a
major change in the distribution of metals in the universe from $z\sim 2.8$ to
$z\sim 0.5$.

We set our empirical results in the context of the cosmological zoom
simulations using simulations from the FOGGIE project, and the main
conclusions from that study are as follows.

  1. 19.

Contrary to cruder resolution simulations (especially in the CGM), a striking
feature of the FOGGIE cosmological zoom simulations is that the behavior of
the metallicity as a function of $N_{\rm H\,I}$ is broadly similar to the
observed empirical relationship: as $N_{\rm H\,I}$ increases the overall
metallicity increases and the dispersion of the metallicity decreases.
However, as other cosmological simulations, FOGGIE appears to have too many
metals at any $N_{\rm H\,I}$ (e.g., supersolar metallicity gas is not uncommon
in these simulations, but observationally it is), implying that metals are
more homogeneously distributed than observed.

  2. 20.

In the FOGGIE simulations, outflowing absorbers with the highest metallicities
tend to be at or within the virial radius of these central halos and probe
active or recent galaxy outflows, while outflowing absorbers with the lowest
metallicity are found well outside the virial radius of the central galaxies
and therefore the remnants of ejected gas. On the other hand, inflowing
absorbers can be found at all radii, with their metallicity generally
increasing the closer they are to their central galaxy. Very metal-poor
absorbers with ${\rm[X/H]}<-2.4$ are excellent probe inflowing gas in these
simulations.

## Acknowledgements

We are grateful to Anna Wright for providing the satellite catalogs used in
Fig. 29 based on the methods of (Pontzen & Tremmel, 2018). The main support
for this research was made by NASA through the Astrophysics Data Analysis
Program (ADAP) grant NNX16AF52G. Additional support was provided by NSF grant
award number 1516777. Support for the development of the Cloudy ionization
models was provided by NASA through grants HST-AR-12854 and HST-AR-15634 from
the Space Telescope Science Institute, which is operated by the Association of
Universities for Research in Astronomy, Incorporated, under NASA contract
NAS5-26555. CC and BWO acknowledge support by NSF grants no. AST-1517908 and
AST-1908109 and NASA ATP grants NNX15AP39G and 80NSSC18K1105. This project has
received funding from the European Research Council (ERC) under the European
Union’s Horizon 2020 research and innovation programme (grant agreement No
757535). This work has been supported by Fondazione Cariplo, grant No
2018-2329. All the data presented in this work were obtained from KODIAQ DR1
and DR2, which was funded through NASA ADAP grants NNX10AE84G and NNX16AF52G
along with NSF award number 1516777. This research has made use of the Keck
Observatory Archive (KOA), which is operated by the W. M. Keck Observatory and
the NASA Exoplanet Science Institute (NExScI), under contract with the
National Aeronautics and Space Administration. The authors wish to recognize
and acknowledge the very significant cultural role and reverence that the
summit of Maunakea has always had within the indigenous Hawaiian community.
The photoionization modeling was supported by the Notre Dame Center for
Research Computing through the Grid Engine software and, together with the
Notre Dame Cooperative Computing Lab, through the HTCondor software.Analysis
of the FOGGIE simulations used the resources of the Michigan State University
High Performance Computing Center, operated by the Institute for Cyber-Enabled
Research. The FOGGIE calculations were performed using the publicly-available
Enzo code (Bryan et al., 2014; Brummel-Smith et al., 2019) and analyzed using
yt (Turk et al., 2011), both of which are the products of the collaborative
effort of many independent scientists from numerous institutions around the
world.

, scikit-learn (Pedregosa et al., 2011; Buitinck et al., 2013), Enzo (Bryan et
al., 2014; Brummel-Smith et al., 2019), yt (Turk et al., 2011), Trident
(Hummels et al., 2017), SALSA (Boyd et al., 2020)

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[Note: owing to their sizes, supplemental files are available on request. They
will be easily accessible when the paper is published.]

In this Appendix, we provide information regarding the supplemental files. For
each KODIAQ-Z absorber, we produced a figure as shown in Fig. 3 where we plot
the normalized profiles of metals and some H I transitions for which we
estimated the column densities (supplemental figure fA3.pdf). The red portion
in each profile shows the velocity range of the absorption over which the
velocity profile was integrated to derive the column densities and average
velocity. The vertical dashed lines mark the zero velocity. We also provide
for each KODIAQ-Z absorber (and sometimes paired or multiple closely redshift
spaced absorbers) a set of figures as Fig. 4 where the Voigt profile fits (in
red the composite profile fit, and in blue each individual component fit) to
the individual transitions of H I (black spectra) are shown (supplemental
figure fA4.pdf).

Next, we provide the visualization results from the MCMC Bayesian
photoionization modeling. For each KODIAQ-Z absorber, we provide the
comparison plots between the observations and models and corner plots as shown
in Figs. A1 and A2, respectively (supplemental figures fA5.pdf and fA6.pdf).
The example shown in these figures is one of the absorbers shown in Fig. 3. In
Fig. A1, we compare the measured column densities for each ion (red) and the
predicted column densities from the median MCMC model (blue). Triangles (when
present) show lower limits (i.e., saturated transitions), while downward
triangles show upper limits. Red data points with error bars (sometimes
smaller than the circles) denote well-constrained column densities. From the
corner or comparison plots, one can determine readily which modeling was used:
(1) if there is no entry for $\log U$ ($\log U\;{\rm prior}={\rm False}$),
then a flat prior on the ionization parameter was used; (2) if a value to
$\log U$ is given, then a Gaussian prior on $\log U$ was used with the listed
mean and dispersion values; (3) if ${\rm[C/\alpha]}$ is present, the absence
of value indicates that a flat prior was used, otherwise a Gaussian prior was
used on that ratio with the listed mean and dispersion values. The EUVB used
in the modeling is also provided (in this case, HM05). Finally, the comparison
plots show which ions were used in the ionization modeling.

Figure A1: Example of a MCMC comparison plot for the absorber at $z=2.55125$
toward J010311+131617. It shows the measured column densities for each ion
(red) and the predicted column densities from the median MCMC model (blue).
Downward triangles show upper limits.  Figure A2: Example of a MCMC corner
plot for the absorber at $z=2.55125$ toward J010311+131617. The histograms
along the diagonal show the PDFs for $N_{\rm H\,I}$, hydrogen number density
($n_{\rm H}$), ${\rm[C/\alpha]}$, and metallicity, respectively. The contour
plots below the diagonal show the joint posterior PDFs of the given row and
column. For this absorber, there is not enough constraint on the metal column
densities to derive the metallicity and ${\rm[C/\alpha]}$ without using priors
(see Fig. A1).

Table 1: Sample Summary

Target | $z_{\rm em}$ | $\lambda_{\rm min}$ | $\lambda_{\rm max}$ | ${\rm SNR}_{\rm 935}$ | ${\rm SNR}_{\rm 1170}$ | ${\rm SNR}_{\rm 1450}$ | Decker | Obs.
---|---|---|---|---|---|---|---|---
|  | (Å) | (Å) |  |  |  |  | Flag
J002127$-$020333 | $2.596$ | $3365$ | $6198$ | 10 | 12 | 10 | C1 | 0
J003501$-$091817 | $2.418$ | $3123$ | $5979$ | 7 | 18 | 19 | C5 | 0
J004530$-$261709 | $3.440$ | $3972$ | $8542$ | 10 | 17 | 15 | C1 | 0
J005700+143737 | $2.643$ | $3366$ | $6198$ | 5 | 9 | 8 | C1 | 0
J010311+131617 | $2.721$ | $3122$ | $8566$ | 54 | 76 | 84 | C5 | 1
J010806+163550 | $2.652$ | $3047$ | $8158$ | 34 | 101 | 29 | C5 | 1
J010925$-$210257 | $3.226$ | $3304$ | $6179$ | 19 | 19 | 14 | C5 | 0
J011150+140141 | $2.470$ | $3132$ | $6030$ | 4 | 7 | 6 | C5 | 0
J012156+144823 | $2.870$ | $3243$ | $7512$ | 30 | 87 | 79 | C5 | 1
J014516$-$094517 | $2.729$ | $3022$ | $7522$ | 77 | 112 | 100 | C5 | 1
J015741$-$010629 | $3.564$ | $3937$ | $6294$ | 10 | 19 | -1 | C5 | 1
J020950$-$000506 | $2.828$ | $3022$ | $9218$ | 32 | 53 | 48 | C1 | 1
J023359+004938 | $2.522$ | $3174$ | $6032$ | 4 | 8 | 5 | C1 | 0
J025905+001121 | $3.365$ | $3805$ | $6858$ | 9 | 82 | 57 | C1 | 1
J030341$-$002321 | $3.175$ | $3535$ | $7222$ | 22 | 33 | 34 | C5 | 1
J033900$-$013318 | $3.197$ | $3685$ | $7719$ | 10 | 24 | 21 | C5 | 1
J045213$-$164012 | $2.684$ | $3100$ | $6024$ | 30 | 50 | 36 | C5 | 1
J064204+675835 | $3.177$ | $3469$ | $6620$ | 42 | 132 | 142 | C5 | 1
J073149+285448 | $3.675$ | $4160$ | $8767$ | 13 | 24 | 18 | C5 | 0
J074521+473436 | $3.220$ | $3574$ | $6841$ | 55 | 172 | 133 | C5 | 1
J074749+443417 | $4.435$ | $4849$ | $9572$ | 8 | 10 | 6 | C1 | 1
J080117+521034 | $3.235$ | $4043$ | $6829$ | -1 | 100 | 104 | C5 | 1
J081240+320808 | $2.711$ | $3330$ | $8771$ | 26 | 45 | 74 | C1 | 1
J082107+310751 | $2.625$ | $3057$ | $5980$ | 24 | 38 | 33 | C1 | 1
J083102+335803 | $2.427$ | $3122$ | $5979$ | 6 | 15 | 16 | C5 | 0
J090033+421546 | $3.290$ | $3545$ | $11691$ | 14 | 52 | 67 | C5 | 1
J093337+284532 | $3.425$ | $3847$ | $6933$ | 3 | 47 | 28 | C5 | 1
J093643+292713 | $2.923$ | $2995$ | $5869$ | 10 | 13 | 10 | C1 | 0
J094202+042244 | $3.275$ | $3363$ | $6200$ | 39 | 42 | 26 | C1 | 0
J095852+120245 | $3.297$ | $3608$ | $9800$ | 35 | 45 | 36 | C5 | 1
J100841+362319 | $3.125$ | $3541$ | $7992$ | 23 | 47 | 27 | C5 | 1
J101155+294141 | $2.652$ | $3048$ | $8921$ | 74 | 118 | 17 | C5 | 1
J101447+430030 | $3.125$ | $3500$ | $7268$ | 39 | 103 | 47 | C5 | 1
J101723$-$204658 | $2.545$ | $3127$ | $5980$ | 24 | 37 | 36 | C1 | 0
J102009+104002 | $3.167$ | $3615$ | $7352$ | 23 | 45 | 42 | C5 | 1
J104018+572448 | $3.408$ | $3793$ | $6656$ | 15 | 18 | 12 | C5 | 0
J105756+455553 | $4.137$ | $3927$ | $9175$ | 66 | 152 | 92 | C5 | 1
J113418+574204 | $3.521$ | $3972$ | $8534$ | 18 | 26 | 23 | C5 | 0
J113508+222715 | $2.886$ | $3433$ | $7240$ | 19 | 40 | 43 | C1 | 1
J120006+312630 | $2.989$ | $3435$ | $6178$ | 16 | 61 | 62 | C5 | 1
J121930+494052 | $2.633$ | $3026$ | $8958$ | 45 | 72 | 15 | C5 | 1
J124610+303131 | $2.560$ | $3189$ | $6085$ | 10 | 16 | 16 | C1 | 0
J130411+295348 | $2.850$ | $2995$ | $5870$ | 14 | 20 | 16 | C1 | 0
J131215+423900 | $2.566$ | $3101$ | $7647$ | 24 | 34 | 34 | C5 | 1
J134328+572147 | $3.034$ | $3074$ | $6468$ | 11 | 19 | 12 | C1 | 1
J134544+262506 | $2.031$ | $3500$ | $6385$ | -1 | 17 | 26 | C5 | 0
J135038$-$251216 | $2.534$ | $3108$ | $5980$ | 19 | 46 | 39 | C1 | 1
J142438+225600 | $3.620$ | $3569$ | $7720$ | 71 | 287 | 188 | C5 | 1
J143316+313126 | $2.940$ | $3244$ | $6095$ | 36 | 46 | 34 | C5 | 0
J144453+291905 | $2.660$ | $2995$ | $7602$ | 74 | 122 | 102 | C5 | 1
J155152+191104 | $2.843$ | $2995$ | $7646$ | 80 | 243 | 302 | C5 | 1
J160455+381201 | $2.551$ | $3105$ | $7065$ | 22 | 69 | 96 | C1 | 1
J160843+071508 | $2.877$ | $3077$ | $8687$ | 23 | 46 | 39 | C1 | 1
J162557+264448 | $2.601$ | $3101$ | $9673$ | 8 | 18 | 25 | C5 | 1
J170100+641209 | $2.734$ | $3060$ | $9093$ | 65 | 185 | 183 | C5 | 1
J171227+575507 | $3.008$ | $3451$ | $6340$ | 29 | 47 | 35 | C5 | 1
J173352+540030 | $3.424$ | $3734$ | $8543$ | 42 | 49 | 43 | C5 | 1
J193957$-$100241 | $3.787$ | $3569$ | $7450$ | 75 | 92 | -1 | C5 | 1
J212912$-$153841 | $3.268$ | $3571$ | $6975$ | 25 | 51 | 21 | C5 | 1
J220852$-$194400 | $2.573$ | $3022$ | $7626$ | 42 | 88 | 59 | C5 | 1
J222256$-$094636 | $2.926$ | $3214$ | $6095$ | 10 | 18 | 13 | C1 | 0
J234628+124859 | $2.573$ | $3022$ | $12723$ | 48 | 181 | 95 | C5 | 1
J234856$-$104131 | $3.172$ | $3101$ | $5979$ | 15 | 19 | -1 | C5 | 0

Note. — The median SNR is calculated by ${\rm SNR}=1.0/\sigma$ per pixel
within $\pm 5\AA$ (where $\sigma$ is the error on the normalized flux) of
three rest wavelengths. A $-1$ in one of the SNR column indicates there is no
wavelength coverage where the SNR is estimated. The pixels are a constant 2.1
${\rm km\,s}^{-1}$ for pre-2004 observations or 2.6 ${\rm km\,s}^{-1}$ for
post-2004 observations and for coaddditions of observations mixing pre- and
post-2004 data (see O’Meara et al. 2017). The observation flag “1” in the last
column indicates if there was more than one of run or a single run (“0”) (see
Table 2 in O’Meara et al. 2017). The decker setup corresponds to the following
resolution: C1: $R=45,000$; C5:$R=34,000$.

Table 2: Summary of the Column Densities of the KODIAQ-Z Absorbers

Target | $z_{\rm abs}$ | Ion | $v_{1}$ | $v_{2}$ | $v$ | $\sigma_{v}$ | $\log N$ | $\sigma^{1}_{\log N}$ | $\sigma^{2}_{\log N}$ | Detection | Reliability | Unique
---|---|---|---|---|---|---|---|---|---|---|---|---
|  |  |  |  |  |  |  |  |  | Flag | Flag | ID
|  |  | (${\rm km\,s}^{-1}$) | (${\rm km\,s}^{-1}$) | (${\rm km\,s}^{-1}$) |  | [cm-2] |  |  |  |  |
J002127$-$020333 | $2.54918$ | Al II | $-50.0$ | $50.0$ | $999.0$ | 999.0 | 11.625 | 0.176 | 0.301 | $-1$ | $3$ | $1$
J002127$-$020333 | $2.54918$ | C II | $-50.0$ | $50.0$ | $999.0$ | 999.0 | 13.379 | 0.176 | 0.301 | $-1$ | $3$ | $1$
J002127$-$020333 | $2.54918$ | C IV | $-50.0$ | $50.0$ | $0.4$ | 3.9 | 13.175 | 0.058 | 0.066 | $0$ | $2$ | $1$
J002127$-$020333 | $2.54918$ | Fe II | $-50.0$ | $50.0$ | $999.0$ | 999.0 | 13.228 | 0.176 | 0.301 | $-1$ | $3$ | $1$
J002127$-$020333 | $2.54918$ | H I | $-50.0$ | $50.0$ | $-2.4$ | 2.7 | 15.680 | 0.019 | 0.022 | $0$ | $2$ | $1$
J002127$-$020333 | $2.54918$ | N I | $-50.0$ | $50.0$ | $999.0$ | 999.0 | 13.329 | 0.176 | 0.301 | $-1$ | $3$ | $1$
J002127$-$020333 | $2.54918$ | N V | $-50.0$ | $50.0$ | $999.0$ | 999.0 | 12.658 | 0.176 | 0.301 | $-1$ | $3$ | $1$
J002127$-$020333 | $2.54918$ | O I | $-50.0$ | $50.0$ | $999.0$ | 999.0 | 13.860 | 0.176 | 0.301 | $-1$ | $3$ | $1$
J002127$-$020333 | $2.54918$ | O VI | $-50.0$ | $50.0$ | $-10.0$ | 5.2 | 13.418 | 0.068 | 0.081 | $0$ | $1$ | $1$
J002127$-$020333 | $2.54918$ | S II | $-50.0$ | $50.0$ | $999.0$ | 999.0 | 13.674 | 0.176 | 0.301 | $-1$ | $3$ | $1$
J002127$-$020333 | $2.54918$ | S III | $-50.0$ | $50.0$ | $999.0$ | 999.0 | 13.533 | 0.176 | 0.301 | $-1$ | $3$ | $1$
J002127$-$020333 | $2.54918$ | Si II | $-50.0$ | $50.0$ | $999.0$ | 999.0 | 11.778 | 0.176 | 0.301 | $-1$ | $3$ | $1$
J002127$-$020333 | $2.54918$ | Si IV | $-50.0$ | $50.0$ | $999.0$ | 999.0 | 12.172 | 0.176 | 0.301 | $-1$ | $3$ | $1$
J003501$-$091817 | $2.35342$ | C II | $-50.0$ | $50.0$ | $999.0$ | 999.0 | 12.470 | 0.180 | 0.300 | $-1$ | $3$ | $2$
J003501$-$091817 | $2.35342$ | C IV | $-50.0$ | $50.0$ | $999.0$ | 999.0 | 12.410 | 0.180 | 0.300 | $-1$ | $3$ | $2$
J003501$-$091817 | $2.35342$ | Fe II | $-50.0$ | $50.0$ | $999.0$ | 999.0 | 12.850 | 0.180 | 0.300 | $-1$ | $3$ | $2$
J003501$-$091817 | $2.35342$ | H I | $-50.0$ | $50.0$ | $0.6$ | 4.0 | 15.610 | 0.040 | 0.050 | $0$ | $2$ | $2$
J003501$-$091817 | $2.35342$ | O I | $-50.0$ | $50.0$ | $999.0$ | 999.0 | 12.980 | 0.180 | 0.300 | $-1$ | $3$ | $2$
J003501$-$091817 | $2.35342$ | S II | $-50.0$ | $50.0$ | $999.0$ | 999.0 | 13.280 | 0.180 | 0.300 | $-1$ | $3$ | $2$
J003501$-$091817 | $2.35342$ | Si II | $-50.0$ | $50.0$ | $999.0$ | 999.0 | 11.420 | 0.180 | 0.300 | $-1$ | $3$ | $2$
J003501$-$091817 | $2.35342$ | Si IV | $-50.0$ | $50.0$ | $999.0$ | 999.0 | 11.990 | 0.180 | 0.300 | $-1$ | $3$ | $2$
J004530$-$261709 | $2.81907$ | Al III | $-110.0$ | $60.0$ | $-38.2$ | 5.4 | 12.400 | 0.050 | 0.050 | $0$ | $3$ | $3$
J004530$-$261709 | $2.81907$ | C IV | $-230.0$ | $130.0$ | $-28.6$ | 1.4 | 14.200 | 0.010 | 0.010 | $0$ | $3$ | $3$
J004530$-$261709 | $2.81907$ | Fe II | $-110.0$ | $60.0$ | $-19.0$ | 0.9 | 14.330 | 0.010 | 0.010 | $0$ | $2$ | $3$
J004530$-$261709 | $2.81907$ | H I | $-1000.0$ | $1000.0$ | $-1.8$ | 164.5 | 19.660 | 0.010 | 0.010 | $0$ | $3$ | $3$
J004530$-$261709 | $2.81907$ | Zn II | $-110.0$ | $60.0$ | $-3.6$ | 14.1 | 12.060 | 0.100 | 0.140 | $0$ | $1$ | $3$
J004530$-$261709 | $3.24823$ | Al II | $-70.0$ | $40.0$ | $999.0$ | 999.0 | 11.230 | 0.180 | 0.300 | $-1$ | $3$ | $4$
J004530$-$261709 | $3.24823$ | Al III | $-70.0$ | $40.0$ | $-27.9$ | 9.4 | 12.010 | 0.100 | 0.140 | $-1$ | $3$ | $4$
J004530$-$261709 | $3.24823$ | C II | $-70.0$ | $40.0$ | $999.0$ | 999.0 | 12.530 | 0.180 | 0.300 | $-1$ | $3$ | $4$
J004530$-$261709 | $3.24823$ | C IV | $-70.0$ | $40.0$ | $999.0$ | 999.0 | 12.250 | 0.180 | 0.300 | $-1$ | $3$ | $4$
J004530$-$261709 | $3.24823$ | H I | $-70.0$ | $40.0$ | $-3.7$ | 1.3 | 15.120 | 0.010 | 0.010 | $0$ | $2$ | $4$
J004530$-$261709 | $3.24823$ | O I | $-70.0$ | $40.0$ | $999.0$ | 999.0 | 12.770 | 0.180 | 0.300 | $-1$ | $3$ | $4$
J004530$-$261709 | $3.24823$ | Si II | $-70.0$ | $40.0$ | $999.0$ | 999.0 | 12.430 | 0.180 | 0.300 | $-1$ | $3$ | $4$
J004530$-$261709 | $3.24823$ | Si IV | $-70.0$ | $40.0$ | $999.0$ | 999.0 | 12.210 | 0.180 | 0.300 | $-1$ | $3$ | $4$
J004530$-$261709 | $3.36517$ | Al III | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 11.590 | 0.180 | 0.300 | $-1$ | $3$ | $5$
J004530$-$261709 | $3.36517$ | C II | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 12.370 | 0.180 | 0.300 | $-1$ | $3$ | $5$
J004530$-$261709 | $3.36517$ | Fe II | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 12.620 | 0.180 | 0.300 | $-1$ | $3$ | $5$
J004530$-$261709 | $3.36517$ | H I | $-58.3$ | $55.2$ | $5.5$ | 2.3 | 15.770 | 0.010 | 0.020 | $0$ | $2$ | $5$
J004530$-$261709 | $3.36517$ | O I | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 12.850 | 0.180 | 0.300 | $-1$ | $3$ | $5$
J004530$-$261709 | $3.36517$ | Si II | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 11.250 | 0.180 | 0.300 | $-1$ | $3$ | $5$
J004530$-$261709 | $3.36517$ | Si IV | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 11.850 | 0.180 | 0.300 | $-1$ | $3$ | $5$
J005700$+$143737 | $2.54721$ | Al II | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 11.550 | 0.180 | 0.300 | $-1$ | $3$ | $6$
J005700$+$143737 | $2.54721$ | C II | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 13.490 | 0.180 | 0.300 | $-1$ | $3$ | $6$
J005700$+$143737 | $2.54721$ | C III | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 12.320 | 0.180 | 0.300 | $-1$ | $3$ | $6$
J005700$+$143737 | $2.54721$ | C IV | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 12.540 | 0.180 | 0.300 | $-1$ | $3$ | $6$
J005700$+$143737 | $2.54721$ | Fe II | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 13.040 | 0.180 | 0.300 | $-1$ | $3$ | $6$
J005700$+$143737 | $2.54721$ | H I | $-150.3$ | $71.9$ | $-21.7$ | 1.7 | 15.040 | 0.010 | 0.010 | $0$ | $3$ | $6$
J005700$+$143737 | $2.54721$ | N I | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 13.480 | 0.180 | 0.300 | $-1$ | $3$ | $6$
J005700$+$143737 | $2.54721$ | O I | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 13.180 | 0.180 | 0.300 | $-1$ | $3$ | $6$
J005700$+$143737 | $2.54721$ | Si II | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 11.680 | 0.180 | 0.300 | $-1$ | $3$ | $6$
J005700$+$143737 | $2.54721$ | Si IV | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 12.150 | 0.180 | 0.300 | $-1$ | $3$ | $6$
J010311$+$131617 | $2.54303$ | Al II | $-35.0$ | $35.0$ | $999.0$ | 999.0 | 10.629 | 0.176 | 0.301 | $-1$ | $3$ | $7$
J010311$+$131617 | $2.54303$ | Al III | $-35.0$ | $35.0$ | $999.0$ | 999.0 | 11.554 | 0.176 | 0.301 | $-1$ | $3$ | $7$
J010311$+$131617 | $2.54303$ | C II | $-35.0$ | $35.0$ | $999.0$ | 999.0 | 11.825 | 0.176 | 0.301 | $-1$ | $3$ | $7$
J010311$+$131617 | $2.54303$ | C IV | $-35.0$ | $35.0$ | $1.7$ | 0.2 | 13.270 | 0.004 | 0.004 | $0$ | $3$ | $7$
J010311$+$131617 | $2.54303$ | H I | $-58.8$ | $55.5$ | $0.7$ | 0.2 | 15.621 | 0.002 | 0.002 | $0$ | $3$ | $7$
J010311$+$131617 | $2.54303$ | O VI | $-35.0$ | $35.0$ | $2.5$ | 0.3 | 13.688 | 0.006 | 0.007 | $0$ | $1$ | $7$
J010311$+$131617 | $2.54303$ | S VI | $-35.0$ | $35.0$ | $999.0$ | 999.0 | 12.048 | 0.176 | 0.301 | $-1$ | $3$ | $7$
J010311$+$131617 | $2.54303$ | Si II | $-35.0$ | $35.0$ | $999.0$ | 999.0 | 11.770 | 0.176 | 0.301 | $-1$ | $3$ | $7$
J010311$+$131617 | $2.54303$ | Si IV | $-35.0$ | $35.0$ | $999.0$ | 999.0 | 11.215 | 0.176 | 0.301 | $-1$ | $3$ | $7$
J010311$+$131617 | $2.55125$ | Al II | $-30.0$ | $40.0$ | $999.0$ | 999.0 | 10.592 | 0.176 | 0.301 | $-1$ | $3$ | $8$
J010311$+$131617 | $2.55125$ | Al III | $-30.0$ | $40.0$ | $999.0$ | 999.0 | 11.193 | 0.176 | 0.301 | $-1$ | $3$ | $8$
J010311$+$131617 | $2.55125$ | C II | $-30.0$ | $40.0$ | $999.0$ | 999.0 | 11.870 | 0.176 | 0.301 | $-1$ | $3$ | $8$
J010311$+$131617 | $2.55125$ | C III | $-30.0$ | $40.0$ | $12.7$ | 0.7 | 12.589 | 0.015 | 0.016 | $0$ | $1$ | $8$
J010311$+$131617 | $2.55125$ | C IV | $-30.0$ | $40.0$ | $6.4$ | 0.5 | 12.822 | 0.012 | 0.012 | $0$ | $3$ | $8$
J010311$+$131617 | $2.55125$ | Fe II | $-30.0$ | $40.0$ | $999.0$ | 999.0 | 12.071 | 0.176 | 0.301 | $-1$ | $3$ | $8$
J010311$+$131617 | $2.55125$ | H I | $-24.7$ | $36.5$ | $9.1$ | 0.1 | 14.862 | 0.003 | 0.003 | $0$ | $3$ | $8$
J010311$+$131617 | $2.55125$ | O I | $-30.0$ | $40.0$ | $999.0$ | 999.0 | 12.306 | 0.176 | 0.301 | $-1$ | $3$ | $8$
J010311$+$131617 | $2.55125$ | O VI | $-30.0$ | $40.0$ | $14.5$ | 0.7 | 13.348 | 0.014 | 0.014 | $0$ | $1$ | $8$
J010311$+$131617 | $2.55125$ | Si II | $-30.0$ | $40.0$ | $999.0$ | 999.0 | 11.786 | 0.176 | 0.301 | $-1$ | $3$ | $8$
J010311$+$131617 | $2.55125$ | Si IV | $-30.0$ | $40.0$ | $999.0$ | 999.0 | 11.209 | 0.176 | 0.301 | $-1$ | $3$ | $8$
J010311$+$131617 | $2.55216$ | Al II | $-40.0$ | $25.0$ | $999.0$ | 999.0 | 10.590 | 0.176 | 0.301 | $-1$ | $3$ | $9$
J010311$+$131617 | $2.55216$ | Al III | $-40.0$ | $25.0$ | $999.0$ | 999.0 | 11.171 | 0.176 | 0.301 | $-1$ | $3$ | $9$
J010311$+$131617 | $2.55216$ | C II | $-40.0$ | $25.0$ | $-39.7$ | 13.7 | 11.976 | 0.138 | 0.204 | $-1$ | $3$ | $9$
J010311$+$131617 | $2.55216$ | C III | $-40.0$ | $25.0$ | $-0.3$ | 0.2 | 13.143 | 0.005 | 0.005 | $0$ | $1$ | $9$
J010311$+$131617 | $2.55216$ | C IV | $-40.0$ | $25.0$ | $-6.6$ | 0.3 | 13.091 | 0.006 | 0.006 | $0$ | $3$ | $9$
J010311$+$131617 | $2.55216$ | Fe II | $-40.0$ | $25.0$ | $1.7$ | 11.0 | 12.105 | 0.163 | 0.263 | $-1$ | $3$ | $9$
J010311$+$131617 | $2.55216$ | H I | $-30.8$ | $38.6$ | $-1.6$ | 0.2 | 15.505 | 0.007 | 0.007 | $0$ | $3$ | $9$
J010311$+$131617 | $2.55216$ | O I | $-40.0$ | $25.0$ | $999.0$ | 999.0 | 12.288 | 0.176 | 0.301 | $-1$ | $3$ | $9$
J010311$+$131617 | $2.55216$ | O VI | $-40.0$ | $25.0$ | $-9.7$ | 0.5 | 13.417 | 0.012 | 0.012 | $0$ | $1$ | $9$
J010311$+$131617 | $2.55216$ | Si II | $-40.0$ | $25.0$ | $999.0$ | 999.0 | 12.019 | 0.176 | 0.301 | $-1$ | $3$ | $9$
J010311$+$131617 | $2.55216$ | Si IV | $-40.0$ | $25.0$ | $999.0$ | 999.0 | 11.508 | 0.176 | 0.301 | $-1$ | $3$ | $9$
J010806$+$163550 | $2.31582$ | Al II | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 11.147 | 0.176 | 0.301 | $-1$ | $3$ | $10$
J010806$+$163550 | $2.31582$ | Al III | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 11.725 | 0.176 | 0.301 | $-1$ | $3$ | $10$
J010806$+$163550 | $2.31582$ | C IV | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 12.009 | 0.176 | 0.301 | $-1$ | $3$ | $10$
J010806$+$163550 | $2.31582$ | Fe II | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 12.510 | 0.176 | 0.301 | $-1$ | $3$ | $10$
J010806$+$163550 | $2.31582$ | H I | $-70.0$ | $60.0$ | $-11.1$ | 0.3 | 14.574 | 0.004 | 0.004 | $0$ | $2$ | $10$
J010806$+$163550 | $2.31582$ | O VI | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 12.720 | 0.176 | 0.301 | $-1$ | $3$ | $10$
J010806$+$163550 | $2.31582$ | Si II | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 10.988 | 0.176 | 0.301 | $-1$ | $3$ | $10$
J010806$+$163550 | $2.31582$ | Si IV | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 11.109 | 0.176 | 0.301 | $-1$ | $3$ | $10$
J010806$+$163550 | $2.46164$ | Al II | $-30.0$ | $30.0$ | $-4.6$ | 6.1 | 11.283 | 0.133 | 0.193 | $-1$ | $3$ | $11$
J010806$+$163550 | $2.46164$ | Al III | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 12.102 | 0.176 | 0.301 | $-1$ | $3$ | $11$
J010806$+$163550 | $2.46164$ | C II | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 11.713 | 0.176 | 0.301 | $-1$ | $3$ | $11$
J010806$+$163550 | $2.46164$ | C IV | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 12.064 | 0.176 | 0.301 | $-1$ | $3$ | $11$
J010806$+$163550 | $2.46164$ | Fe II | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 12.551 | 0.176 | 0.301 | $-1$ | $3$ | $11$
J010806$+$163550 | $2.46164$ | H I | $-68.6$ | $58.8$ | $1.7$ | 0.2 | 14.754 | 0.002 | 0.002 | $0$ | $3$ | $11$
J010806$+$163550 | $2.46164$ | Si II | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 12.210 | 0.176 | 0.301 | $-1$ | $3$ | $11$
J010806$+$163550 | $2.46164$ | Si IV | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 11.677 | 0.176 | 0.301 | $-1$ | $3$ | $11$
J010806$+$163550 | $2.48359$ | Al III | $-35.0$ | $35.0$ | $999.0$ | 999.0 | 11.811 | 0.176 | 0.301 | $-1$ | $3$ | $12$
J010806$+$163550 | $2.48359$ | C II | $-35.0$ | $35.0$ | $-3.6$ | 5.4 | 12.034 | 0.102 | 0.134 | $-1$ | $3$ | $12$
J010806$+$163550 | $2.48359$ | C III | $-35.0$ | $35.0$ | $13.5$ | 0.6 | 12.944 | 0.013 | 0.013 | $0$ | $1$ | $12$
J010806$+$163550 | $2.48359$ | C IV | $-35.0$ | $35.0$ | $3.0$ | 0.7 | 13.336 | 0.015 | 0.016 | $0$ | $3$ | $12$
J010806$+$163550 | $2.48359$ | Fe II | $-35.0$ | $35.0$ | $999.0$ | 999.0 | 12.504 | 0.176 | 0.301 | $-1$ | $3$ | $12$
J010806$+$163550 | $2.48359$ | Fe III | $-35.0$ | $35.0$ | $999.0$ | 999.0 | 12.435 | 0.176 | 0.301 | $-1$ | $3$ | $12$
J010806$+$163550 | $2.48359$ | H I | $-71.9$ | $58.8$ | $1.6$ | 0.5 | 15.315 | 0.010 | 0.010 | $0$ | $3$ | $12$
J010806$+$163550 | $2.48359$ | O I | $-35.0$ | $35.0$ | $999.0$ | 999.0 | 12.123 | 0.176 | 0.301 | $-1$ | $3$ | $12$
J010806$+$163550 | $2.48359$ | S II | $-35.0$ | $35.0$ | $999.0$ | 999.0 | 12.633 | 0.176 | 0.301 | $-1$ | $3$ | $12$
J010806$+$163550 | $2.48359$ | Si II | $-35.0$ | $35.0$ | $999.0$ | 999.0 | 10.753 | 0.176 | 0.301 | $-1$ | $3$ | $12$
J010806$+$163550 | $2.50561$ | Al II | $-30.0$ | $30.0$ | $-8.6$ | 8.4 | 11.107 | 0.174 | 0.295 | $-1$ | $3$ | $13$
J010806$+$163550 | $2.50561$ | Al III | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 11.743 | 0.176 | 0.301 | $-1$ | $3$ | $13$
J010806$+$163550 | $2.50561$ | C II | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 11.740 | 0.176 | 0.301 | $-1$ | $3$ | $13$
J010806$+$163550 | $2.50561$ | C IV | $-30.0$ | $30.0$ | $1.0$ | 3.4 | 12.459 | 0.078 | 0.096 | $0$ | $2$ | $13$
J010806$+$163550 | $2.50561$ | Fe II | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 12.363 | 0.176 | 0.301 | $-1$ | $3$ | $13$
J010806$+$163550 | $2.50561$ | H I | $-50.7$ | $47.5$ | $-2.6$ | 0.4 | 15.914 | 0.004 | 0.003 | $0$ | $3$ | $13$
J010806$+$163550 | $2.50561$ | O I | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 12.081 | 0.176 | 0.301 | $-1$ | $3$ | $13$
J010806$+$163550 | $2.50561$ | Si II | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 11.257 | 0.176 | 0.301 | $-1$ | $3$ | $13$
J010806$+$163550 | $2.50561$ | Si IV | $-30.0$ | $30.0$ | $2.9$ | 7.4 | 11.526 | 0.144 | 0.217 | $0$ | $1$ | $13$
J010925$-$210257 | $2.96546$ | C II | $-35.0$ | $25.0$ | $999.0$ | 999.0 | 12.732 | 0.176 | 0.301 | $-1$ | $3$ | $14$
J010925$-$210257 | $2.96546$ | C III | $-35.0$ | $25.0$ | $999.0$ | 999.0 | 12.031 | 0.176 | 0.301 | $-1$ | $3$ | $14$
J010925$-$210257 | $2.96546$ | C IV | $-35.0$ | $25.0$ | $999.0$ | 999.0 | 12.338 | 0.176 | 0.301 | $-1$ | $3$ | $14$
J010925$-$210257 | $2.96546$ | H I | $-61.0$ | $40.6$ | $-7.3$ | 0.3 | 14.706 | 0.007 | 0.008 | $0$ | $3$ | $14$
J010925$-$210257 | $2.96546$ | N I | $-35.0$ | $25.0$ | $999.0$ | 999.0 | 12.720 | 0.180 | 0.300 | $-1$ | $3$ | $14$
J010925$-$210257 | $2.96546$ | O I | $-35.0$ | $25.0$ | $999.0$ | 999.0 | 12.681 | 0.176 | 0.301 | $-1$ | $3$ | $14$
J010925$-$210257 | $2.96546$ | O VI | $-35.0$ | $25.0$ | $-8.7$ | 3.2 | 13.115 | 0.079 | 0.096 | $0$ | $1$ | $14$
J010925$-$210257 | $2.96546$ | S II | $-35.0$ | $25.0$ | $999.0$ | 999.0 | 13.863 | 0.176 | 0.301 | $-1$ | $3$ | $14$
J010925$-$210257 | $2.96546$ | S IV | $-35.0$ | $25.0$ | $999.0$ | 999.0 | 13.125 | 0.176 | 0.301 | $-1$ | $3$ | $14$
J010925$-$210257 | $2.96546$ | Si II | $-35.0$ | $25.0$ | $999.0$ | 999.0 | 11.904 | 0.176 | 0.301 | $-1$ | $3$ | $14$
J010925$-$210257 | $2.96546$ | Si IV | $-35.0$ | $25.0$ | $999.0$ | 999.0 | 11.901 | 0.176 | 0.301 | $-1$ | $3$ | $14$
J010925$-$210257 | $3.14253$ | C II | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 12.525 | 0.176 | 0.301 | $-1$ | $3$ | $15$
J010925$-$210257 | $3.14253$ | H I | $-45.8$ | $32.7$ | $-1.4$ | 3.6 | 16.147 | 0.013 | 0.013 | $0$ | $3$ | $15$
J010925$-$210257 | $3.14253$ | O I | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 13.001 | 0.176 | 0.301 | $-1$ | $3$ | $15$
J010925$-$210257 | $3.14253$ | S II | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 13.676 | 0.176 | 0.301 | $-1$ | $3$ | $15$
J010925$-$210257 | $3.14253$ | Si II | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 12.741 | 0.176 | 0.301 | $-1$ | $3$ | $15$
J010925$-$210257 | $3.14253$ | Si IV | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 11.943 | 0.176 | 0.301 | $-1$ | $3$ | $15$
J011150$+$140141 | $2.42374$ | Al II | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 11.740 | 0.176 | 0.301 | $-1$ | $3$ | $16$
J011150$+$140141 | $2.42374$ | C II | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 13.131 | 0.176 | 0.301 | $-1$ | $3$ | $16$
J011150$+$140141 | $2.42374$ | C IV | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 12.636 | 0.176 | 0.301 | $-1$ | $3$ | $16$
J011150$+$140141 | $2.42374$ | Fe II | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 13.222 | 0.176 | 0.301 | $-1$ | $3$ | $16$
J011150$+$140141 | $2.42374$ | H I | $-37.0$ | $37.0$ | $0.9$ | 2.0 | 14.803 | 0.019 | 0.021 | $0$ | $3$ | $16$
J011150$+$140141 | $2.42374$ | N I | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 13.630 | 0.176 | 0.301 | $-1$ | $3$ | $16$
J011150$+$140141 | $2.42374$ | N II | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 13.109 | 0.176 | 0.301 | $-1$ | $3$ | $16$
J011150$+$140141 | $2.42374$ | N V | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 12.834 | 0.176 | 0.301 | $-1$ | $3$ | $16$
J011150$+$140141 | $2.42374$ | O I | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 13.313 | 0.176 | 0.301 | $-1$ | $3$ | $16$
J011150$+$140141 | $2.42374$ | O VI | $-30.0$ | $30.0$ | $6.0$ | 6.0 | 13.470 | 0.125 | 0.177 | $0$ | $1$ | $16$
J011150$+$140141 | $2.42374$ | S II | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 13.480 | 0.176 | 0.301 | $-1$ | $3$ | $16$
J011150$+$140141 | $2.42374$ | S III | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 13.525 | 0.176 | 0.301 | $-1$ | $3$ | $16$
J011150$+$140141 | $2.42374$ | Si II | $-30.0$ | $30.0$ | $-2.3$ | 6.2 | 11.766 | 0.142 | 0.213 | $-1$ | $3$ | $16$
J011150$+$140141 | $2.42374$ | Si III | $-30.0$ | $30.0$ | $-19.8$ | 5.4 | 12.054 | 0.084 | 0.104 | $0$ | $1$ | $16$
J011150$+$140141 | $2.42374$ | Si IV | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 12.561 | 0.176 | 0.301 | $-1$ | $3$ | $16$
J012156$+$144823 | $2.41837$ | Al II | $-12.0$ | $17.0$ | $999.0$ | 999.0 | 10.519 | 0.176 | 0.301 | $-1$ | $3$ | $17$
J012156$+$144823 | $2.41837$ | C IV | $-12.0$ | $17.0$ | $5.5$ | 0.5 | 12.353 | 0.023 | 0.024 | $0$ | $3$ | $17$
J012156$+$144823 | $2.41837$ | Fe II | $-12.0$ | $17.0$ | $999.0$ | 999.0 | 11.765 | 0.176 | 0.301 | $-1$ | $3$ | $17$
J012156$+$144823 | $2.41837$ | Fe III | $-12.0$ | $17.0$ | $7.4$ | 4.9 | 12.516 | 0.168 | 0.279 | $-1$ | $3$ | $17$
J012156$+$144823 | $2.41837$ | H I | $-75.0$ | $55.0$ | $-16.2$ | 0.5 | 14.829 | 0.005 | 0.008 | $0$ | $2$ | $17$
J012156$+$144823 | $2.41837$ | Si II | $-12.0$ | $17.0$ | $999.0$ | 999.0 | 11.604 | 0.176 | 0.301 | $-1$ | $3$ | $17$
J012156$+$144823 | $2.41837$ | Si III | $-12.0$ | $17.0$ | $999.0$ | 999.0 | 10.877 | 0.176 | 0.301 | $-1$ | $3$ | $17$
J012156$+$144823 | $2.41837$ | Si IV | $-12.0$ | $17.0$ | $3.5$ | 1.6 | 11.175 | 0.072 | 0.087 | $0$ | $2$ | $17$
J012156$+$144823 | $2.46812$ | C IV | $-32.0$ | $0.1$ | $-19.9$ | 0.7 | 12.244 | 0.030 | 0.032 | $0$ | $3$ | $18$
J012156$+$144823 | $2.46812$ | H I | $-71.9$ | $49.0$ | $-11.1$ | 0.4 | 14.962 | 0.010 | 0.010 | $0$ | $2$ | $18$
J012156$+$144823 | $2.46812$ | O I | $-32.0$ | $0.1$ | $999.0$ | 999.0 | 12.096 | 0.176 | 0.301 | $-1$ | $3$ | $18$
J012156$+$144823 | $2.46812$ | S III | $-32.0$ | $0.1$ | $999.0$ | 999.0 | 12.830 | 0.176 | 0.301 | $-1$ | $3$ | $18$
J012156$+$144823 | $2.46812$ | Si II | $-32.0$ | $0.1$ | $999.0$ | 999.0 | 11.591 | 0.176 | 0.301 | $-1$ | $3$ | $18$
J012156$+$144823 | $2.46812$ | Si IV | $-32.0$ | $0.1$ | $999.0$ | 999.0 | 10.871 | 0.176 | 0.301 | $-1$ | $3$ | $18$
J012156$+$144823 | $2.53765$ | Al II | $-40.0$ | $-10.0$ | $999.0$ | 999.0 | 10.322 | 0.176 | 0.301 | $-1$ | $3$ | $19$
J012156$+$144823 | $2.53765$ | C II | $-40.0$ | $-10.0$ | $999.0$ | 999.0 | 11.368 | 0.176 | 0.301 | $-1$ | $3$ | $19$
J012156$+$144823 | $2.53765$ | C III | $-40.0$ | $-10.0$ | $-24.1$ | 0.8 | 12.505 | 0.034 | 0.036 | $0$ | $1$ | $19$
J012156$+$144823 | $2.53765$ | C IV | $-40.0$ | $-10.0$ | $-24.6$ | 0.5 | 12.166 | 0.025 | 0.027 | $0$ | $3$ | $19$
J012156$+$144823 | $2.53765$ | H I | $-91.5$ | $29.4$ | $-19.5$ | 0.4 | 15.124 | 0.004 | 0.005 | $0$ | $2$ | $19$
J012156$+$144823 | $2.53765$ | O VI | $-40.0$ | $-10.0$ | $999.0$ | 999.0 | 12.224 | 0.176 | 0.301 | $-1$ | $3$ | $19$
J012156$+$144823 | $2.53765$ | Si II | $-40.0$ | $-10.0$ | $999.0$ | 999.0 | 11.379 | 0.176 | 0.301 | $-1$ | $3$ | $19$
J012156$+$144823 | $2.53765$ | Si IV | $-40.0$ | $-10.0$ | $-24.6$ | 2.7 | 11.228 | 0.108 | 0.143 | $0$ | $2$ | $19$
J012156$+$144823 | $2.62486$ | Al II | $-20.0$ | $20.0$ | $3.7$ | 2.8 | 10.645 | 0.084 | 0.105 | $-1$ | $3$ | $20$
J012156$+$144823 | $2.62486$ | C II | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 11.566 | 0.176 | 0.301 | $-1$ | $3$ | $20$
J012156$+$144823 | $2.62486$ | C III | $-20.0$ | $20.0$ | $-8.1$ | 3.5 | 11.909 | 0.095 | 0.122 | $0$ | $1$ | $20$
J012156$+$144823 | $2.62486$ | C IV | $-20.0$ | $20.0$ | $-36.7$ | 19.1 | 11.648 | 0.137 | 0.202 | $0$ | $2$ | $20$
J012156$+$144823 | $2.62486$ | Fe II | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 11.847 | 0.176 | 0.301 | $-1$ | $3$ | $20$
J012156$+$144823 | $2.62486$ | H I | $-104.6$ | $42.5$ | $-18.1$ | 0.4 | 14.966 | 0.008 | 0.006 | $0$ | $2$ | $20$
J012156$+$144823 | $2.62486$ | O I | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 11.858 | 0.176 | 0.301 | $-1$ | $3$ | $20$
J012156$+$144823 | $2.62486$ | Si II | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 10.711 | 0.176 | 0.301 | $-1$ | $3$ | $20$
J012156$+$144823 | $2.62486$ | Si IV | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 11.077 | 0.180 | 0.300 | $-1$ | $3$ | $20$
J012156$+$144823 | $2.66022$ | Al II | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 10.650 | 0.176 | 0.301 | $-1$ | $3$ | $21$
J012156$+$144823 | $2.66022$ | C II | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 11.555 | 0.176 | 0.301 | $-1$ | $3$ | $21$
J012156$+$144823 | $2.66022$ | C IV | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 11.350 | 0.176 | 0.301 | $-1$ | $3$ | $21$
J012156$+$144823 | $2.66022$ | Fe II | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 12.022 | 0.176 | 0.301 | $-1$ | $3$ | $21$
J012156$+$144823 | $2.66022$ | H I | $-30.0$ | $40.0$ | $3.7$ | 0.3 | 14.828 | 0.021 | 0.022 | $0$ | $3$ | $21$
J012156$+$144823 | $2.66022$ | N V | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 11.980 | 0.176 | 0.301 | $-1$ | $3$ | $21$
J012156$+$144823 | $2.66022$ | O I | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 11.874 | 0.176 | 0.301 | $-1$ | $3$ | $21$
J012156$+$144823 | $2.66022$ | Si II | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 11.241 | 0.176 | 0.301 | $-1$ | $3$ | $21$
J012156$+$144823 | $2.66022$ | Si IV | $-20.0$ | $20.0$ | $-7.0$ | 3.4 | 11.266 | 0.096 | 0.123 | $-1$ | $3$ | $21$
J012156$+$144823 | $2.66241$ | Al II | $-50.0$ | $60.0$ | $2.0$ | 0.2 | 12.838 | 0.003 | 0.003 | $0$ | $1$ | $22$
J012156$+$144823 | $2.66241$ | C II | $-50.0$ | $60.0$ | $1.3$ | 0.2 | 14.817 | 0.006 | 0.006 | $-2$ | $1$ | $22$
J012156$+$144823 | $2.66241$ | C IV | $-50.0$ | $60.0$ | $14.8$ | 0.1 | 13.784 | 0.002 | 0.002 | $0$ | $3$ | $22$
J012156$+$144823 | $2.66241$ | Fe II | $-50.0$ | $60.0$ | $20.6$ | 0.4 | 14.025 | 0.009 | 0.009 | $0$ | $1$ | $22$
J012156$+$144823 | $2.66241$ | H I | $-100.0$ | $80.0$ | $-4.6$ | 8.4 | 19.100 | 0.350 | 0.350 | $0$ | $3$ | $22$
J012156$+$144823 | $2.66241$ | O I | $-50.0$ | $60.0$ | $-2.8$ | 0.1 | 14.620 | 0.001 | 0.001 | $0$ | $3$ | $22$
J012156$+$144823 | $2.66241$ | O VI | $-50.0$ | $60.0$ | $17.4$ | 0.7 | 13.890 | 0.009 | 0.009 | $0$ | $1$ | $22$
J012156$+$144823 | $2.66241$ | S VI | $-50.0$ | $60.0$ | $-7.5$ | 9.5 | 12.727 | 0.109 | 0.146 | $0$ | $1$ | $22$
J012156$+$144823 | $2.66241$ | Si II | $-50.0$ | $60.0$ | $-2.2$ | 0.1 | 13.892 | 0.001 | 0.001 | $0$ | $3$ | $22$
J012156$+$144823 | $2.66241$ | Si III | $-50.0$ | $60.0$ | $10.9$ | 4.7 | 14.050 | 0.001 | 0.001 | $-2$ | $1$ | $22$
J012156$+$144823 | $2.66241$ | Si IV | $-50.0$ | $60.0$ | $13.9$ | 0.1 | 13.463 | 0.002 | 0.002 | $0$ | $1$ | $22$
J012156$+$144823 | $2.66416$ | Al II | $-20.0$ | $25.0$ | $0.9$ | 0.1 | 12.320 | 0.000 | 0.000 | $0$ | $1$ | $23$
J012156$+$144823 | $2.66416$ | C II | $-20.0$ | $25.0$ | $1.9$ | 0.0 | 14.210 | 0.010 | 0.010 | $0$ | $3$ | $23$
J012156$+$144823 | $2.66416$ | C IV | $-20.0$ | $25.0$ | $3.9$ | 0.1 | 13.590 | 0.000 | 0.000 | $0$ | $3$ | $23$
J012156$+$144823 | $2.66416$ | Fe II | $-20.0$ | $25.0$ | $-5.1$ | 2.6 | 12.430 | 0.070 | 0.090 | $0$ | $1$ | $23$
J012156$+$144823 | $2.66416$ | Fe III | $-20.0$ | $25.0$ | $-2.2$ | 1.0 | 13.230 | 0.030 | 0.030 | $0$ | $1$ | $23$
J012156$+$144823 | $2.66416$ | H I | $-20.0$ | $25.0$ | $0.0$ | 0.7 | 17.260 | 0.100 | 0.100 | $0$ | $3$ | $23$
J012156$+$144823 | $2.66416$ | N I | $-20.0$ | $25.0$ | $999.0$ | 999.0 | 12.010 | 0.180 | 0.300 | $-1$ | $3$ | $23$
J012156$+$144823 | $2.66416$ | N II | $-20.0$ | $25.0$ | $2.4$ | 0.5 | 13.280 | 0.010 | 0.010 | $0$ | $1$ | $23$
J012156$+$144823 | $2.66416$ | O I | $-20.0$ | $25.0$ | $2.2$ | 0.2 | 13.430 | 0.010 | 0.010 | $0$ | $1$ | $23$
J012156$+$144823 | $2.66416$ | O VI | $-20.0$ | $25.0$ | $2.9$ | 0.2 | 14.190 | 0.010 | 0.010 | $0$ | $1$ | $23$
J012156$+$144823 | $2.66416$ | Si II | $-20.0$ | $25.0$ | $2.7$ | 0.0 | 13.070 | 0.000 | 0.000 | $0$ | $3$ | $23$
J012156$+$144823 | $2.66416$ | Si IV | $-20.0$ | $25.0$ | $5.9$ | 0.1 | 12.970 | 0.000 | 0.000 | $0$ | $3$ | $23$
J012156$+$144823 | $2.66593$ | Al II | $-25.0$ | $14.0$ | $-5.5$ | 0.5 | 11.523 | 0.021 | 0.022 | $0$ | $1$ | $24$
J012156$+$144823 | $2.66593$ | C II | $-25.0$ | $14.0$ | $-6.1$ | 0.1 | 13.295 | 0.005 | 0.005 | $0$ | $3$ | $24$
J012156$+$144823 | $2.66593$ | C III | $-25.0$ | $14.0$ | $-5.5$ | 1.4 | 13.927 | 0.085 | 0.106 | $-2$ | $1$ | $24$
J012156$+$144823 | $2.66593$ | C IV | $-25.0$ | $14.0$ | $-7.2$ | 0.0 | 13.579 | 0.002 | 0.002 | $0$ | $3$ | $24$
J012156$+$144823 | $2.66593$ | Fe II | $-25.0$ | $14.0$ | $999.0$ | 999.0 | 11.976 | 0.176 | 0.301 | $-1$ | $3$ | $24$
J012156$+$144823 | $2.66593$ | Fe III | $-25.0$ | $14.0$ | $-6.1$ | 1.0 | 13.097 | 0.036 | 0.040 | $0$ | $1$ | $24$
J012156$+$144823 | $2.66593$ | H I | $-35.0$ | $20.0$ | $-6.0$ | 0.3 | 16.259 | 0.023 | 0.024 | $0$ | $3$ | $24$
J012156$+$144823 | $2.66593$ | N I | $-25.0$ | $14.0$ | $999.0$ | 999.0 | 12.441 | 0.176 | 0.301 | $-1$ | $3$ | $24$
J012156$+$144823 | $2.66593$ | O I | $-25.0$ | $14.0$ | $999.0$ | 999.0 | 11.906 | 0.176 | 0.301 | $-1$ | $3$ | $24$
J012156$+$144823 | $2.66593$ | O VI | $-25.0$ | $14.0$ | $-6.4$ | 0.3 | 13.747 | 0.010 | 0.011 | $0$ | $1$ | $24$
J012156$+$144823 | $2.66593$ | Si II | $-25.0$ | $14.0$ | $-7.4$ | 0.1 | 12.275 | 0.006 | 0.006 | $0$ | $3$ | $24$
J012156$+$144823 | $2.66593$ | Si III | $-25.0$ | $14.0$ | $-4.9$ | 0.1 | 13.286 | 0.014 | 0.014 | $-2$ | $1$ | $24$
J012156$+$144823 | $2.66593$ | Si IV | $-25.0$ | $14.0$ | $-6.2$ | 0.0 | 13.211 | 0.003 | 0.003 | $0$ | $3$ | $24$
J012156$+$144823 | $2.81222$ | C II | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 11.591 | 0.176 | 0.301 | $-1$ | $3$ | $25$
J012156$+$144823 | $2.81222$ | C IV | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 11.491 | 0.176 | 0.301 | $-1$ | $3$ | $25$
J012156$+$144823 | $2.81222$ | Fe II | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 11.992 | 0.176 | 0.301 | $-1$ | $3$ | $25$
J012156$+$144823 | $2.81222$ | H I | $-91.5$ | $26.1$ | $-20.0$ | 0.2 | 14.683 | 0.002 | 0.002 | $0$ | $3$ | $25$
J012156$+$144823 | $2.81222$ | N I | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 11.665 | 0.176 | 0.301 | $-1$ | $3$ | $25$
J012156$+$144823 | $2.81222$ | N II | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 12.058 | 0.176 | 0.301 | $-1$ | $3$ | $25$
J012156$+$144823 | $2.81222$ | O I | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 12.048 | 0.176 | 0.301 | $-1$ | $3$ | $25$
J012156$+$144823 | $2.81222$ | O VI | $-20.0$ | $20.0$ | $-1.0$ | 2.9 | 12.408 | 0.095 | 0.122 | $-1$ | $3$ | $25$
J012156$+$144823 | $2.81222$ | S II | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 12.396 | 0.176 | 0.301 | $-1$ | $3$ | $25$
J012156$+$144823 | $2.81222$ | S III | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 12.634 | 0.176 | 0.301 | $-1$ | $3$ | $25$
J012156$+$144823 | $2.81222$ | Si II | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 10.529 | 0.176 | 0.301 | $-1$ | $3$ | $25$
J012156$+$144823 | $2.81222$ | Si III | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 10.649 | 0.176 | 0.301 | $-1$ | $3$ | $25$
J012156$+$144823 | $2.81222$ | Si IV | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 10.971 | 0.176 | 0.301 | $-1$ | $3$ | $25$
J014516$-$094517 | $2.49969$ | Al II | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 10.381 | 0.176 | 0.301 | $-1$ | $3$ | $26$
J014516$-$094517 | $2.49969$ | C II | $-20.0$ | $20.0$ | $-2.7$ | 5.5 | 11.592 | 0.164 | 0.268 | $-1$ | $3$ | $26$
J014516$-$094517 | $2.49969$ | C IV | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 11.425 | 0.176 | 0.301 | $-1$ | $3$ | $26$
J014516$-$094517 | $2.49969$ | H I | $-63.1$ | $18.5$ | $-14.1$ | 0.1 | 15.026 | 0.001 | 0.001 | $0$ | $3$ | $26$
J014516$-$094517 | $2.49969$ | O VI | $-20.0$ | $20.0$ | $-10.4$ | 5.1 | 12.164 | 0.147 | 0.223 | $-1$ | $3$ | $26$
J014516$-$094517 | $2.49969$ | Si II | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 11.079 | 0.176 | 0.301 | $-1$ | $3$ | $26$
J014516$-$094517 | $2.49969$ | Si IV | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 10.996 | 0.176 | 0.301 | $-1$ | $3$ | $26$
J014516$-$094517 | $2.58808$ | C II | $-20.0$ | $20.0$ | $-4.6$ | 4.2 | 11.788 | 0.124 | 0.174 | $-1$ | $3$ | $27$
J014516$-$094517 | $2.58808$ | C IV | $-20.0$ | $20.0$ | $-5.8$ | 1.5 | 12.030 | 0.044 | 0.049 | $0$ | $3$ | $27$
J014516$-$094517 | $2.58808$ | H I | $-47.6$ | $58.2$ | $-10.0$ | 0.1 | 15.065 | 0.001 | 0.001 | $0$ | $3$ | $27$
J014516$-$094517 | $2.58808$ | N I | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 11.882 | 0.176 | 0.301 | $-1$ | $3$ | $27$
J014516$-$094517 | $2.58808$ | N II | $-20.0$ | $20.0$ | $-13.9$ | 8.3 | 11.851 | 0.154 | 0.240 | $-1$ | $3$ | $27$
J014516$-$094517 | $2.58808$ | O I | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 12.073 | 0.176 | 0.301 | $-1$ | $3$ | $27$
J014516$-$094517 | $2.58808$ | Si II | $-20.0$ | $20.0$ | $3.4$ | 5.5 | 10.631 | 0.162 | 0.263 | $-1$ | $3$ | $27$
J014516$-$094517 | $2.58808$ | Si III | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 10.725 | 0.176 | 0.301 | $-1$ | $3$ | $27$
J014516$-$094517 | $2.58808$ | Si IV | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 11.030 | 0.176 | 0.301 | $-1$ | $3$ | $27$
J014516$-$094517 | $2.66513$ | Al II | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 10.970 | 0.176 | 0.301 | $-1$ | $3$ | $28$
J014516$-$094517 | $2.66513$ | C II | $-30.0$ | $30.0$ | $-0.3$ | 2.0 | 12.369 | 0.046 | 0.052 | $0$ | $1$ | $28$
J014516$-$094517 | $2.66513$ | C IV | $-30.0$ | $30.0$ | $-2.0$ | 0.2 | 13.061 | 0.005 | 0.005 | $0$ | $3$ | $28$
J014516$-$094517 | $2.66513$ | Fe II | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 12.078 | 0.176 | 0.301 | $-1$ | $3$ | $28$
J014516$-$094517 | $2.66513$ | H I | $-46.7$ | $21.5$ | $2.2$ | 0.1 | 16.156 | 0.001 | 0.001 | $0$ | $3$ | $28$
J014516$-$094517 | $2.66513$ | N I | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 12.321 | 0.176 | 0.301 | $-1$ | $3$ | $28$
J014516$-$094517 | $2.66513$ | O I | $-30.0$ | $30.0$ | $-9.2$ | 4.8 | 12.496 | 0.095 | 0.123 | $-1$ | $3$ | $28$
J014516$-$094517 | $2.66513$ | S II | $-30.0$ | $30.0$ | $-1.2$ | 5.3 | 12.749 | 0.109 | 0.147 | $-1$ | $3$ | $28$
J014516$-$094517 | $2.66513$ | S IV | $-30.0$ | $30.0$ | $999.0$ | 999.0 | 12.253 | 0.176 | 0.301 | $-1$ | $3$ | $28$
J014516$-$094517 | $2.66513$ | Si II | $-30.0$ | $30.0$ | $22.0$ | 13.8 | 10.725 | 0.150 | 0.231 | $-1$ | $3$ | $28$
J014516$-$094517 | $2.66513$ | Si III | $-30.0$ | $30.0$ | $2.3$ | 0.4 | 11.997 | 0.009 | 0.010 | $0$ | $1$ | $28$
J014516$-$094517 | $2.66513$ | Si IV | $-30.0$ | $30.0$ | $3.3$ | 1.5 | 11.884 | 0.035 | 0.038 | $0$ | $3$ | $28$
J014516$-$094517 | $2.66911$ | Al II | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 10.822 | 0.176 | 0.301 | $-1$ | $3$ | $29$
J014516$-$094517 | $2.66911$ | C II | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 11.636 | 0.176 | 0.301 | $-1$ | $3$ | $29$
J014516$-$094517 | $2.66911$ | C III | $-20.0$ | $20.0$ | $7.6$ | 4.0 | 11.344 | 0.120 | 0.166 | $-1$ | $3$ | $29$
J014516$-$094517 | $2.66911$ | C IV | $-20.0$ | $20.0$ | $8.8$ | 5.0 | 11.559 | 0.122 | 0.170 | $-1$ | $3$ | $29$
J014516$-$094517 | $2.66911$ | Fe II | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 12.076 | 0.176 | 0.301 | $-1$ | $3$ | $29$
J014516$-$094517 | $2.66911$ | H I | $-72.4$ | $27.1$ | $-24.9$ | 0.1 | 15.412 | 0.001 | 0.001 | $0$ | $3$ | $29$
J014516$-$094517 | $2.66911$ | O I | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 12.039 | 0.176 | 0.301 | $-1$ | $3$ | $29$
J014516$-$094517 | $2.66911$ | S II | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 12.409 | 0.176 | 0.301 | $-1$ | $3$ | $29$
J014516$-$094517 | $2.66911$ | S IV | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 12.164 | 0.176 | 0.301 | $-1$ | $3$ | $29$
J014516$-$094517 | $2.66911$ | Si II | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 11.769 | 0.176 | 0.301 | $-1$ | $3$ | $29$
J014516$-$094517 | $2.66911$ | Si IV | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 11.068 | 0.176 | 0.301 | $-1$ | $3$ | $29$
J014516$-$094517 | $2.69212$ | C II | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 11.623 | 0.176 | 0.301 | $-1$ | $3$ | $30$
J014516$-$094517 | $2.69212$ | C III | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 11.167 | 0.176 | 0.301 | $-1$ | $3$ | $30$
J014516$-$094517 | $2.69212$ | C IV | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 11.416 | 0.176 | 0.301 | $-1$ | $3$ | $30$
J014516$-$094517 | $2.69212$ | Fe II | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 11.934 | 0.176 | 0.301 | $-1$ | $3$ | $30$
J014516$-$094517 | $2.69212$ | H I | $-57.0$ | $2.0$ | $-28.7$ | 0.1 | 15.395 | 0.001 | 0.001 | $0$ | $3$ | $30$
J014516$-$094517 | $2.69212$ | N V | $-20.0$ | $20.0$ | $-3.5$ | 4.0 | 11.936 | 0.136 | 0.199 | $-1$ | $3$ | $30$
J014516$-$094517 | $2.69212$ | S II | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 12.916 | 0.176 | 0.301 | $-1$ | $3$ | $30$
J014516$-$094517 | $2.69212$ | Si II | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 10.561 | 0.176 | 0.301 | $-1$ | $3$ | $30$
J014516$-$094517 | $2.69212$ | Si IV | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 11.049 | 0.176 | 0.301 | $-1$ | $3$ | $30$
J014516$-$094517 | $2.69430$ | C II | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 11.670 | 0.176 | 0.301 | $-1$ | $3$ | $31$
J014516$-$094517 | $2.69430$ | C IV | $-20.0$ | $20.0$ | $-2.1$ | 1.2 | 12.027 | 0.042 | 0.046 | $0$ | $3$ | $31$
J014516$-$094517 | $2.69430$ | Fe II | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 11.944 | 0.176 | 0.301 | $-1$ | $3$ | $31$
J014516$-$094517 | $2.69430$ | H I | $-52.0$ | $39.7$ | $-4.1$ | 0.1 | 14.708 | 0.001 | 0.003 | $0$ | $3$ | $31$
J014516$-$094517 | $2.69430$ | N V | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 11.458 | 0.176 | 0.301 | $-1$ | $3$ | $31$
J014516$-$094517 | $2.69430$ | O I | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 12.066 | 0.176 | 0.301 | $-1$ | $3$ | $31$
J014516$-$094517 | $2.69430$ | S II | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 12.417 | 0.176 | 0.301 | $-1$ | $3$ | $31$
J014516$-$094517 | $2.69430$ | Si II | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 10.556 | 0.176 | 0.301 | $-1$ | $3$ | $31$
J014516$-$094517 | $2.69430$ | Si IV | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 11.033 | 0.176 | 0.301 | $-1$ | $3$ | $31$
J014516$-$094517 | $2.70685$ | C II | $-35.0$ | $20.0$ | $999.0$ | 999.0 | 11.701 | 0.176 | 0.301 | $-1$ | $3$ | $32$
J014516$-$094517 | $2.70685$ | C III | $-35.0$ | $20.0$ | $-7.0$ | 0.2 | 12.781 | 0.006 | 0.006 | $0$ | $1$ | $32$
J014516$-$094517 | $2.70685$ | C IV | $-35.0$ | $20.0$ | $-10.6$ | 0.2 | 12.913 | 0.006 | 0.006 | $0$ | $3$ | $32$
J014516$-$094517 | $2.70685$ | Fe II | $-35.0$ | $20.0$ | $999.0$ | 999.0 | 12.080 | 0.176 | 0.301 | $-1$ | $3$ | $32$
J014516$-$094517 | $2.70685$ | Fe III | $-35.0$ | $20.0$ | $999.0$ | 999.0 | 12.174 | 0.176 | 0.301 | $-1$ | $3$ | $32$
J014516$-$094517 | $2.70685$ | H I | $-55.0$ | $47.0$ | $-8.4$ | 0.1 | 15.097 | 0.001 | 0.001 | $0$ | $3$ | $32$
J014516$-$094517 | $2.70685$ | N I | $-35.0$ | $20.0$ | $14.8$ | 12.1 | 12.544 | 0.160 | 0.256 | $0$ | $2$ | $32$
J014516$-$094517 | $2.70685$ | N II | $-35.0$ | $20.0$ | $999.0$ | 999.0 | 11.961 | 0.176 | 0.301 | $-1$ | $3$ | $32$
J014516$-$094517 | $2.70685$ | N III | $-35.0$ | $20.0$ | $999.0$ | 999.0 | 11.979 | 0.176 | 0.301 | $-1$ | $3$ | $32$
J014516$-$094517 | $2.70685$ | N V | $-35.0$ | $20.0$ | $-7.9$ | 5.3 | 11.651 | 0.125 | 0.176 | $0$ | $2$ | $32$
J014516$-$094517 | $2.70685$ | O I | $-35.0$ | $20.0$ | $999.0$ | 999.0 | 12.924 | 0.176 | 0.301 | $-1$ | $3$ | $32$
J014516$-$094517 | $2.70685$ | O VI | $-35.0$ | $20.0$ | $-11.6$ | 0.2 | 13.524 | 0.004 | 0.004 | $0$ | $3$ | $32$
J014516$-$094517 | $2.70685$ | S II | $-35.0$ | $20.0$ | $999.0$ | 999.0 | 12.521 | 0.176 | 0.301 | $-1$ | $3$ | $32$
J014516$-$094517 | $2.70685$ | Si II | $-35.0$ | $20.0$ | $999.0$ | 999.0 | 10.759 | 0.176 | 0.301 | $-1$ | $3$ | $32$
J014516$-$094517 | $2.70685$ | Si III | $-35.0$ | $20.0$ | $-6.5$ | 5.2 | 10.768 | 0.122 | 0.171 | $-1$ | $3$ | $32$
J014516$-$094517 | $2.70685$ | Si IV | $-35.0$ | $20.0$ | $999.0$ | 999.0 | 11.071 | 0.176 | 0.301 | $-1$ | $3$ | $32$
J015741$-$010629 | $3.36274$ | C II | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 12.464 | 0.176 | 0.301 | $-1$ | $3$ | $33$
J015741$-$010629 | $3.36274$ | Fe III | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 12.849 | 0.176 | 0.301 | $-1$ | $3$ | $33$
J015741$-$010629 | $3.36274$ | H I | $-57.0$ | $46.0$ | $-12.1$ | 1.0 | 15.145 | 0.013 | 0.016 | $0$ | $2$ | $33$
J015741$-$010629 | $3.36274$ | O I | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 12.622 | 0.176 | 0.301 | $-1$ | $3$ | $33$
J015741$-$010629 | $3.36274$ | Si II | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 11.234 | 0.176 | 0.301 | $-1$ | $3$ | $33$
J015741$-$010629 | $3.36274$ | Si IV | $-20.0$ | $20.0$ | $999.0$ | 999.0 | 11.886 | 0.176 | 0.301 | $-1$ | $3$ | $33$
J020950$-$000506 | $2.41125$ | Al II | $-10.0$ | $29.0$ | $999.0$ | 999.0 | 10.679 | 0.176 | 0.301 | $-1$ | $3$ | $34$
J020950$-$000506 | $2.41125$ | Al III | $-10.0$ | $29.0$ | $999.0$ | 999.0 | 11.657 | 0.176 | 0.301 | $-1$ | $3$ | $34$
J020950$-$000506 | $2.41125$ | Fe II | $-10.0$ | $29.0$ | $999.0$ | 999.0 | 11.574 | 0.176 | 0.301 | $-1$ | $3$ | $34$
J020950$-$000506 | $2.41125$ | H I | $-90.9$ | $73.8$ | $-17.5$ | 0.3 | 15.009 | 0.006 | 0.006 | $0$ | $3$ | $34$
J020950$-$000506 | $2.41125$ | O I | $-10.0$ | $29.0$ | $999.0$ | 999.0 | 13.393 | 0.176 | 0.301 | $-1$ | $3$ | $34$
J020950$-$000506 | $2.41125$ | Si II | $-10.0$ | $29.0$ | $999.0$ | 999.0 | 10.954 | 0.176 | 0.301 | $-1$ | $3$ | $34$
J020950$-$000506 | $2.41125$ | Si IV | $-10.0$ | $29.0$ | $999.0$ | 999.0 | 10.920 | 0.176 | 0.301 | $-1$ | $3$ | $34$
J020950$-$000506 | $2.41125$ | Zn II | $-10.0$ | $29.0$ | $999.0$ | 999.0 | 11.745 | 0.176 | 0.301 | $-1$ | $3$ | $34$
J020950$-$000506 | $2.57449$ | Al II | $-18.0$ | $30.0$ | $-3.9$ | 1.4 | 11.391 | 0.035 | 0.038 | $0$ | $1$ | $35$
J020950$-$000506 | $2.57449$ | Al III | $-18.0$ | $30.0$ | $999.0$ | 999.0 | 11.432 | 0.176 | 0.301 | $-1$ | $3$ | $35$
J020950$-$000506 | $2.57449$ | C II | $-18.0$ | $30.0$ | $5.1$ | 0.2 | 13.147 | 0.007 | 0.007 | $0$ | $1$ | $35$
J020950$-$000506 | $2.57449$ | C IV | $-18.0$ | $30.0$ | $1.9$ | 0.1 | 13.863 | 0.003 | 0.003 | $0$ | $3$ | $35$
J020950$-$000506 | $2.57449$ | Fe II | $-18.0$ | $30.0$ | $999.0$ | 999.0 | 11.593 | 0.176 | 0.301 | $-1$ | $3$ | $35$
J020950$-$000506 | $2.57449$ | H I | $-32.2$ | $29.7$ | $4.1$ | 0.2 | 16.777 | 0.002 | 0.004 | $0$ | $3$ | $35$
J020950$-$000506 | $2.57449$ | O VI | $-18.0$ | $30.0$ | $4.0$ | 0.2 | 13.792 | 0.005 | 0.005 | $0$ | $3$ | $35$
J020950$-$000506 | $2.57449$ | Si II | $-18.0$ | $30.0$ | $4.4$ | 0.7 | 11.923 | 0.022 | 0.023 | $0$ | $3$ | $35$
J020950$-$000506 | $2.57449$ | Si IV | $-18.0$ | $30.0$ | $4.4$ | 0.1 | 13.203 | 0.003 | 0.003 | $0$ | $3$ | $35$
J020950$-$000506 | $2.57449$ | Zn II | $-18.0$ | $30.0$ | $999.0$ | 999.0 | 11.725 | 0.176 | 0.301 | $-1$ | $3$ | $35$
J020950$-$000506 | $2.64137$ | Al II | $-16.0$ | $15.0$ | $999.0$ | 999.0 | 10.955 | 0.176 | 0.301 | $-1$ | $3$ | $36$
J020950$-$000506 | $2.64137$ | C II | $-16.0$ | $15.0$ | $999.0$ | 999.0 | 11.631 | 0.176 | 0.301 | $-1$ | $3$ | $36$
J020950$-$000506 | $2.64137$ | C IV | $-16.0$ | $15.0$ | $-3.0$ | 0.1 | 13.578 | 0.004 | 0.005 | $0$ | $3$ | $36$
J020950$-$000506 | $2.64137$ | Fe II | $-16.0$ | $15.0$ | $999.0$ | 999.0 | 11.501 | 0.176 | 0.301 | $-1$ | $3$ | $36$
J020950$-$000506 | $2.64137$ | H I | $-25.6$ | $17.0$ | $-11.2$ | 0.3 | 15.360 | 0.003 | 0.003 | $0$ | $3$ | $36$
J020950$-$000506 | $2.64137$ | N I | $-16.0$ | $15.0$ | $999.0$ | 999.0 | 12.820 | 0.176 | 0.301 | $-1$ | $3$ | $36$
J020950$-$000506 | $2.64137$ | O I | $-16.0$ | $15.0$ | $999.0$ | 999.0 | 11.952 | 0.176 | 0.301 | $-1$ | $3$ | $36$
J020950$-$000506 | $2.64137$ | Si II | $-16.0$ | $15.0$ | $999.0$ | 999.0 | 10.836 | 0.176 | 0.301 | $-1$ | $3$ | $36$
J020950$-$000506 | $2.64137$ | Si III | $-16.0$ | $15.0$ | $-2.3$ | 0.8 | 11.553 | 0.039 | 0.042 | $0$ | $1$ | $36$
J020950$-$000506 | $2.64137$ | Si IV | $-16.0$ | $15.0$ | $-3.9$ | 0.4 | 12.252 | 0.021 | 0.022 | $0$ | $3$ | $36$
J020950$-$000506 | $2.64137$ | Zn II | $-16.0$ | $15.0$ | $999.0$ | 999.0 | 11.317 | 0.176 | 0.301 | $-1$ | $3$ | $36$
J020950$-$000506 | $2.76903$ | Al III | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 11.317 | 0.176 | 0.301 | $-1$ | $3$ | $37$
J020950$-$000506 | $2.76903$ | C IV | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 11.508 | 0.176 | 0.301 | $-1$ | $3$ | $37$
J020950$-$000506 | $2.76903$ | Fe II | $-15.0$ | $15.0$ | $-3.8$ | 3.7 | 11.651 | 0.143 | 0.215 | $-1$ | $3$ | $37$
J020950$-$000506 | $2.76903$ | H I | $-33.2$ | $32.1$ | $-1.8$ | 0.1 | 15.773 | 0.002 | 0.002 | $0$ | $3$ | $37$
J020950$-$000506 | $2.76903$ | N I | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 11.756 | 0.176 | 0.301 | $-1$ | $3$ | $37$
J020950$-$000506 | $2.76903$ | N II | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 12.158 | 0.176 | 0.301 | $-1$ | $3$ | $37$
J020950$-$000506 | $2.76903$ | O I | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 12.176 | 0.176 | 0.301 | $-1$ | $3$ | $37$
J020950$-$000506 | $2.76903$ | O VI | $-15.0$ | $15.0$ | $1.1$ | 3.8 | 12.009 | 0.163 | 0.264 | $-1$ | $3$ | $37$
J020950$-$000506 | $2.76903$ | S III | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 12.360 | 0.176 | 0.301 | $-1$ | $3$ | $37$
J020950$-$000506 | $2.76903$ | Si II | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 10.544 | 0.176 | 0.301 | $-1$ | $3$ | $37$
J020950$-$000506 | $2.76903$ | Si III | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 10.597 | 0.176 | 0.301 | $-1$ | $3$ | $37$
J020950$-$000506 | $2.76903$ | Si IV | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 11.241 | 0.176 | 0.301 | $-1$ | $3$ | $37$
J023359$+$004938 | $2.48836$ | Al II | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 11.586 | 0.176 | 0.301 | $-1$ | $3$ | $38$
J023359$+$004938 | $2.48836$ | C II | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 12.706 | 0.176 | 0.301 | $-1$ | $3$ | $38$
J023359$+$004938 | $2.48836$ | C III | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 12.220 | 0.176 | 0.301 | $-1$ | $3$ | $38$
J023359$+$004938 | $2.48836$ | C IV | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 12.427 | 0.176 | 0.301 | $-1$ | $3$ | $38$
J023359$+$004938 | $2.48836$ | Fe II | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 13.116 | 0.176 | 0.301 | $-1$ | $3$ | $38$
J023359$+$004938 | $2.48836$ | H I | $-68.3$ | $32.4$ | $-14.8$ | 1.2 | 14.640 | 0.018 | 0.020 | $0$ | $3$ | $38$
J023359$+$004938 | $2.48836$ | N I | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 13.129 | 0.176 | 0.301 | $-1$ | $3$ | $38$
J023359$+$004938 | $2.48836$ | N II | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 12.902 | 0.176 | 0.301 | $-1$ | $3$ | $38$
J023359$+$004938 | $2.48836$ | O I | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 13.137 | 0.176 | 0.301 | $-1$ | $3$ | $38$
J023359$+$004938 | $2.48836$ | O VI | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 12.870 | 0.176 | 0.301 | $-1$ | $3$ | $38$
J023359$+$004938 | $2.48836$ | S II | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 13.532 | 0.176 | 0.301 | $-1$ | $3$ | $38$
J023359$+$004938 | $2.48836$ | S IV | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 13.318 | 0.176 | 0.301 | $-1$ | $3$ | $38$
J023359$+$004938 | $2.48836$ | Si II | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 11.662 | 0.176 | 0.301 | $-1$ | $3$ | $38$
J023359$+$004938 | $2.48836$ | Si III | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 11.447 | 0.176 | 0.301 | $-1$ | $3$ | $38$
J023359$+$004938 | $2.48836$ | Si IV | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 12.121 | 0.176 | 0.301 | $-1$ | $3$ | $38$
J025905$+$001121 | $3.08204$ | C II | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 11.813 | 0.176 | 0.301 | $-1$ | $3$ | $39$
J025905$+$001121 | $3.08204$ | C IV | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 11.923 | 0.176 | 0.301 | $-1$ | $3$ | $39$
J025905$+$001121 | $3.08204$ | Fe II | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 12.231 | 0.176 | 0.301 | $-1$ | $3$ | $39$
J025905$+$001121 | $3.08204$ | H I | $-15.0$ | $15.0$ | $0.0$ | 2.0 | 17.500 | 0.250 | 0.250 | $0$ | $3$ | $39$
J025905$+$001121 | $3.08204$ | O I | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 11.715 | 0.176 | 0.301 | $-1$ | $3$ | $39$
J025905$+$001121 | $3.08204$ | O VI | $-15.0$ | $15.0$ | $2.9$ | 2.7 | 12.660 | 0.112 | 0.151 | $-1$ | $3$ | $39$
J025905$+$001121 | $3.08204$ | Si II | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 11.569 | 0.176 | 0.301 | $-1$ | $3$ | $39$
J025905$+$001121 | $3.08204$ | Si III | $-15.0$ | $15.0$ | $-0.4$ | 0.7 | 11.837 | 0.030 | 0.033 | $-1$ | $3$ | $39$
J025905$+$001121 | $3.08204$ | Si IV | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 11.394 | 0.176 | 0.301 | $-1$ | $3$ | $39$
J025905$+$001121 | $3.08465$ | C II | $-57.0$ | $20.0$ | $-5.7$ | 1.9 | 12.888 | 0.029 | 0.031 | $0$ | $1$ | $40$
J025905$+$001121 | $3.08465$ | C IV | $-57.0$ | $20.0$ | $-16.6$ | 0.3 | 13.650 | 0.006 | 0.006 | $0$ | $3$ | $40$
J025905$+$001121 | $3.08465$ | Fe II | $-57.0$ | $20.0$ | $999.0$ | 999.0 | 12.423 | 0.176 | 0.301 | $-1$ | $3$ | $40$
J025905$+$001121 | $3.08465$ | H I | $-57.0$ | $20.0$ | $-22.5$ | 2.5 | 17.250 | 0.250 | 0.250 | $0$ | $3$ | $40$
J025905$+$001121 | $3.08465$ | O I | $-57.0$ | $20.0$ | $-22.5$ | 2.5 | 12.633 | 0.046 | 0.051 | $-1$ | $3$ | $40$
J025905$+$001121 | $3.08465$ | Si II | $-57.0$ | $20.0$ | $999.0$ | 999.0 | 11.971 | 0.176 | 0.301 | $-1$ | $3$ | $40$
J025905$+$001121 | $3.08465$ | Si III | $-57.0$ | $20.0$ | $-15.2$ | 1.6 | 13.453 | 0.030 | 0.032 | $0$ | $1$ | $40$
J025905$+$001121 | $3.08465$ | Si IV | $-57.0$ | $20.0$ | $-19.8$ | 0.3 | 13.108 | 0.006 | 0.006 | $0$ | $3$ | $40$
J025905$+$001121 | $3.12722$ | C II | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 11.726 | 0.176 | 0.301 | $-1$ | $3$ | $41$
J025905$+$001121 | $3.12722$ | C III | $-15.0$ | $15.0$ | $4.1$ | 1.7 | 12.248 | 0.071 | 0.086 | $-1$ | $3$ | $41$
J025905$+$001121 | $3.12722$ | C IV | $-15.0$ | $15.0$ | $-8.5$ | 3.9 | 11.792 | 0.115 | 0.156 | $-1$ | $3$ | $41$
J025905$+$001121 | $3.12722$ | Fe II | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 12.195 | 0.176 | 0.301 | $-1$ | $3$ | $41$
J025905$+$001121 | $3.12722$ | H I | $-56.2$ | $35.7$ | $-11.1$ | 0.7 | 15.035 | 0.009 | 0.008 | $0$ | $3$ | $41$
J025905$+$001121 | $3.12722$ | O I | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 12.202 | 0.176 | 0.301 | $-1$ | $3$ | $41$
J025905$+$001121 | $3.12722$ | Si II | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 11.780 | 0.176 | 0.301 | $-1$ | $3$ | $41$
J025905$+$001121 | $3.12722$ | Si III | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 10.948 | 0.176 | 0.301 | $-1$ | $3$ | $41$
J025905$+$001121 | $3.12722$ | Si IV | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 11.196 | 0.176 | 0.301 | $-1$ | $3$ | $41$
J025905$+$001121 | $3.22368$ | C III | $-15.0$ | $15.0$ | $5.2$ | 2.6 | 12.067 | 0.096 | 0.123 | $-1$ | $3$ | $42$
J025905$+$001121 | $3.22368$ | C IV | $-15.0$ | $15.0$ | $4.7$ | 4.6 | 11.822 | 0.142 | 0.212 | $-1$ | $3$ | $42$
J025905$+$001121 | $3.22368$ | H I | $-47.7$ | $29.3$ | $-10.8$ | 0.5 | 15.113 | 0.005 | 0.005 | $0$ | $3$ | $42$
J025905$+$001121 | $3.22368$ | O I | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 12.195 | 0.176 | 0.301 | $-1$ | $3$ | $42$
J025905$+$001121 | $3.22368$ | O VI | $-15.0$ | $15.0$ | $12.7$ | 4.7 | 12.622 | 0.119 | 0.165 | $-1$ | $3$ | $42$
J025905$+$001121 | $3.22368$ | Si II | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 10.381 | 0.176 | 0.301 | $-1$ | $3$ | $42$
J025905$+$001121 | $3.22368$ | Si IV | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 11.331 | 0.176 | 0.301 | $-1$ | $3$ | $42$
J025905$+$001121 | $3.30796$ | C II | $-45.0$ | $25.0$ | $999.0$ | 999.0 | 11.964 | 0.176 | 0.301 | $-1$ | $3$ | $43$
J025905$+$001121 | $3.30796$ | C III | $-45.0$ | $25.0$ | $-5.7$ | 0.4 | 13.519 | 0.013 | 0.014 | $0$ | $1$ | $43$
J025905$+$001121 | $3.30796$ | C IV | $-59.4$ | $28.7$ | $-4.9$ | 0.6 | 13.236 | 0.012 | 0.012 | $0$ | $3$ | $43$
J025905$+$001121 | $3.30796$ | H I | $-56.3$ | $18.8$ | $-8.8$ | 0.9 | 15.744 | 0.012 | 0.011 | $0$ | $3$ | $43$
J025905$+$001121 | $3.30796$ | O I | $-45.0$ | $25.0$ | $999.0$ | 999.0 | 12.594 | 0.176 | 0.301 | $-1$ | $3$ | $43$
J025905$+$001121 | $3.30796$ | Si II | $-45.0$ | $25.0$ | $999.0$ | 999.0 | 11.931 | 0.176 | 0.301 | $-1$ | $3$ | $43$
J025905$+$001121 | $3.30796$ | Si IV | $-45.0$ | $25.0$ | $-6.9$ | 1.5 | 12.277 | 0.032 | 0.035 | $0$ | $3$ | $43$
J030341$-$002321 | $2.44326$ | Al II | $-22.0$ | $20.0$ | $-0.3$ | 0.7 | 11.855 | 0.026 | 0.028 | $0$ | $1$ | $44$
J030341$-$002321 | $2.44326$ | Al III | $-22.0$ | $20.0$ | $0.8$ | 4.6 | 11.419 | 0.136 | 0.198 | $0$ | $2$ | $44$
J030341$-$002321 | $2.44326$ | C II | $-22.0$ | $20.0$ | $-1.3$ | 0.2 | 14.108 | 0.011 | 0.012 | $0$ | $1$ | $44$
J030341$-$002321 | $2.44326$ | C IV | $-22.0$ | $20.0$ | $-5.7$ | 0.4 | 13.091 | 0.012 | 0.012 | $0$ | $3$ | $44$
J030341$-$002321 | $2.44326$ | Fe II | $-22.0$ | $20.0$ | $-0.2$ | 1.5 | 13.088 | 0.050 | 0.056 | $0$ | $1$ | $44$
J030341$-$002321 | $2.44326$ | H I | $-719.4$ | $399.6$ | $-4.2$ | 1.1 | 19.866 | 0.010 | 0.010 | $0$ | $3$ | $44$
J030341$-$002321 | $2.44326$ | O I | $-22.0$ | $20.0$ | $2.4$ | 0.2 | 14.530 | 0.014 | 0.014 | $0$ | $1$ | $44$
J030341$-$002321 | $2.44326$ | Si II | $-22.0$ | $20.0$ | $1.6$ | 0.2 | 13.331 | 0.008 | 0.008 | $0$ | $3$ | $44$
J030341$-$002321 | $2.44326$ | Si IV | $-22.0$ | $20.0$ | $-6.4$ | 1.6 | 12.278 | 0.048 | 0.054 | $0$ | $1$ | $44$
J030341$-$002321 | $2.93700$ | C II | $-15.0$ | $15.0$ | $-0.7$ | 3.6 | 11.996 | 0.144 | 0.217 | $-1$ | $3$ | $45$
J030341$-$002321 | $2.93700$ | C III | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 11.642 | 0.176 | 0.301 | $-1$ | $3$ | $45$
J030341$-$002321 | $2.93700$ | C IV | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 12.091 | 0.176 | 0.301 | $-1$ | $3$ | $45$
J030341$-$002321 | $2.93700$ | Fe II | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 12.335 | 0.176 | 0.301 | $-1$ | $3$ | $45$
J030341$-$002321 | $2.93700$ | Fe III | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 12.555 | 0.176 | 0.301 | $-1$ | $3$ | $45$
J030341$-$002321 | $2.93700$ | H I | $-76.2$ | $43.2$ | $-17.4$ | 0.6 | 15.648 | 0.006 | 0.006 | $0$ | $2$ | $45$
J030341$-$002321 | $2.93700$ | O I | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 12.164 | 0.176 | 0.301 | $-1$ | $3$ | $45$
J030341$-$002321 | $2.93700$ | S VI | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 12.081 | 0.176 | 0.301 | $-1$ | $3$ | $45$
J030341$-$002321 | $2.93700$ | Si II | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 11.551 | 0.176 | 0.301 | $-1$ | $3$ | $45$
J030341$-$002321 | $2.93700$ | Si IV | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 11.525 | 0.176 | 0.301 | $-1$ | $3$ | $45$
J030341$-$002321 | $2.94069$ | C II | $-23.0$ | $26.0$ | $6.8$ | 0.1 | 14.070 | 0.005 | 0.005 | $0$ | $1$ | $46$
J030341$-$002321 | $2.94069$ | C IV | $-23.0$ | $26.0$ | $-0.1$ | 0.2 | 13.931 | 0.007 | 0.007 | $0$ | $3$ | $46$
J030341$-$002321 | $2.94069$ | Fe II | $-23.0$ | $26.0$ | $999.0$ | 999.0 | 12.486 | 0.176 | 0.301 | $-1$ | $3$ | $46$
J030341$-$002321 | $2.94069$ | H I | $-23.0$ | $26.0$ | $7.5$ | 1.0 | 18.650 | 0.150 | 0.300 | $0$ | $3$ | $46$
J030341$-$002321 | $2.94069$ | O I | $-23.0$ | $26.0$ | $7.5$ | 1.0 | 13.163 | 0.028 | 0.030 | $0$ | $1$ | $46$
J030341$-$002321 | $2.94069$ | Si II | $-23.0$ | $26.0$ | $6.6$ | 0.1 | 13.160 | 0.009 | 0.009 | $0$ | $3$ | $46$
J030341$-$002321 | $2.94069$ | Si IV | $-22.0$ | $26.0$ | $2.8$ | 0.3 | 13.875 | 0.003 | 0.003 | $0$ | $3$ | $46$
J030341$-$002321 | $2.95653$ | C II | $-40.0$ | $40.0$ | $999.0$ | 999.0 | 12.263 | 0.176 | 0.301 | $-1$ | $3$ | $47$
J030341$-$002321 | $2.95653$ | C IV | $-40.0$ | $40.0$ | $-3.6$ | 0.3 | 13.632 | 0.007 | 0.007 | $0$ | $3$ | $47$
J030341$-$002321 | $2.95653$ | H I | $-39.2$ | $61.7$ | $-1.7$ | 0.6 | 16.161 | 0.010 | 0.010 | $0$ | $3$ | $47$
J030341$-$002321 | $2.95653$ | O I | $-40.0$ | $40.0$ | $999.0$ | 999.0 | 12.404 | 0.176 | 0.301 | $-1$ | $3$ | $47$
J030341$-$002321 | $2.95653$ | Si II | $-40.0$ | $40.0$ | $999.0$ | 999.0 | 12.195 | 0.176 | 0.301 | $-1$ | $3$ | $47$
J030341$-$002321 | $2.95653$ | Si III | $-40.0$ | $40.0$ | $-2.0$ | 0.8 | 12.540 | 0.016 | 0.017 | $0$ | $1$ | $47$
J030341$-$002321 | $2.95653$ | Si IV | $-40.0$ | $40.0$ | $-1.7$ | 1.3 | 12.689 | 0.025 | 0.027 | $0$ | $3$ | $47$
J030341$-$002321 | $2.99495$ | C IV | $-79.0$ | $33.2$ | $-18.9$ | 0.8 | 13.546 | 0.012 | 0.012 | $0$ | $1$ | $48$
J030341$-$002321 | $2.99495$ | H I | $-66.6$ | $37.5$ | $-13.8$ | 0.4 | 16.170 | 0.004 | 0.004 | $0$ | $3$ | $48$
J030341$-$002321 | $2.99495$ | O I | $-68.0$ | $40.0$ | $999.0$ | 999.0 | 12.571 | 0.176 | 0.301 | $-1$ | $3$ | $48$
J030341$-$002321 | $2.99495$ | O VI | $-68.0$ | $40.0$ | $-37.5$ | 2.3 | 13.805 | 0.028 | 0.030 | $0$ | $1$ | $48$
J030341$-$002321 | $2.99495$ | S VI | $-68.0$ | $40.0$ | $999.0$ | 999.0 | 12.319 | 0.176 | 0.301 | $-1$ | $3$ | $48$
J030341$-$002321 | $2.99495$ | Si III | $-68.0$ | $40.0$ | $-6.7$ | 0.7 | 12.708 | 0.011 | 0.011 | $0$ | $1$ | $48$
J030341$-$002321 | $2.99495$ | Si IV | $-68.2$ | $34.1$ | $-8.9$ | 2.2 | 12.452 | 0.036 | 0.039 | $0$ | $3$ | $48$
J030341$-$002321 | $3.10354$ | C II | $-15.0$ | $15.0$ | $3.9$ | 4.8 | 12.054 | 0.165 | 0.269 | $-1$ | $3$ | $49$
J030341$-$002321 | $3.10354$ | C IV | $-15.0$ | $15.0$ | $-3.0$ | 2.9 | 12.085 | 0.101 | 0.132 | $-1$ | $3$ | $49$
J030341$-$002321 | $3.10354$ | H I | $-30.0$ | $40.0$ | $-1.4$ | 0.7 | 15.449 | 0.010 | 0.011 | $0$ | $3$ | $49$
J030341$-$002321 | $3.10354$ | O I | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 12.531 | 0.176 | 0.301 | $-1$ | $3$ | $49$
J030341$-$002321 | $3.10354$ | Si II | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 10.817 | 0.176 | 0.301 | $-1$ | $3$ | $49$
J030341$-$002321 | $3.10354$ | Si III | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 11.000 | 0.176 | 0.301 | $-1$ | $3$ | $49$
J030341$-$002321 | $3.10354$ | Si IV | $-15.0$ | $15.0$ | $-0.8$ | 3.6 | 11.647 | 0.144 | 0.217 | $-1$ | $3$ | $49$
J030341$-$002321 | $3.10937$ | C II | $-15.0$ | $15.0$ | $1.9$ | 2.1 | 12.329 | 0.091 | 0.115 | $-1$ | $3$ | $50$
J030341$-$002321 | $3.10937$ | C III | $-15.0$ | $15.0$ | $8.6$ | 5.5 | 11.715 | 0.169 | 0.279 | $-1$ | $3$ | $50$
J030341$-$002321 | $3.10937$ | C IV | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 11.789 | 0.176 | 0.301 | $-1$ | $3$ | $50$
J030341$-$002321 | $3.10937$ | H I | $-57.3$ | $28.6$ | $-11.5$ | 0.2 | 14.766 | 0.005 | 0.004 | $0$ | $3$ | $50$
J030341$-$002321 | $3.10937$ | O I | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 12.467 | 0.176 | 0.301 | $-1$ | $3$ | $50$
J030341$-$002321 | $3.10937$ | O VI | $-15.0$ | $15.0$ | $0.9$ | 3.1 | 12.532 | 0.114 | 0.155 | $-1$ | $3$ | $50$
J030341$-$002321 | $3.10937$ | Si II | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 10.841 | 0.176 | 0.301 | $-1$ | $3$ | $50$
J030341$-$002321 | $3.10937$ | Si III | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 11.001 | 0.176 | 0.301 | $-1$ | $3$ | $50$
J030341$-$002321 | $3.10937$ | Si IV | $-15.0$ | $15.0$ | $7.6$ | 5.1 | 11.501 | 0.161 | 0.258 | $-1$ | $3$ | $50$
J030341$-$002321 | $3.15168$ | C II | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 12.078 | 0.176 | 0.301 | $-1$ | $3$ | $51$
J030341$-$002321 | $3.15168$ | H I | $-38.7$ | $28.5$ | $-3.5$ | 0.2 | 15.436 | 0.003 | 0.004 | $0$ | $3$ | $51$
J030341$-$002321 | $3.15168$ | O I | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 12.481 | 0.176 | 0.301 | $-1$ | $3$ | $51$
J030341$-$002321 | $3.15168$ | O VI | $-15.0$ | $15.0$ | $-0.3$ | 1.2 | 12.808 | 0.062 | 0.072 | $-1$ | $3$ | $51$
J030341$-$002321 | $3.15168$ | Si II | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 10.882 | 0.176 | 0.301 | $-1$ | $3$ | $51$
J030341$-$002321 | $3.15168$ | Si III | $-15.0$ | $15.0$ | $2.0$ | 2.1 | 11.331 | 0.083 | 0.103 | $-1$ | $3$ | $51$
J030341$-$002321 | $3.15168$ | Si IV | $-15.0$ | $15.0$ | $10.0$ | 5.0 | 11.643 | 0.142 | 0.213 | $-1$ | $3$ | $51$
J033900$-$013318 | $3.11542$ | C II | $-50.0$ | $50.0$ | $1.3$ | 1.3 | 14.744 | 0.003 | 0.003 | $-2$ | $1$ | $52$
J033900$-$013318 | $3.11542$ | C IV | $-50.0$ | $50.0$ | $-4.8$ | 0.2 | 13.926 | 0.004 | 0.004 | $0$ | $3$ | $52$
J033900$-$013318 | $3.11542$ | Fe II | $-50.0$ | $50.0$ | $5.5$ | 2.8 | 13.359 | 0.042 | 0.046 | $0$ | $1$ | $52$
J033900$-$013318 | $3.11542$ | Fe III | $-50.0$ | $50.0$ | $2.7$ | 1.8 | 13.958 | 0.030 | 0.032 | $0$ | $1$ | $52$
J033900$-$013318 | $3.11542$ | H I | $-510.5$ | $350.1$ | $-28.3$ | 22.3 | 19.600 | 0.050 | 0.050 | $0$ | $3$ | $52$
J033900$-$013318 | $3.11542$ | N II | $-50.0$ | $50.0$ | $2.4$ | 1.4 | 13.825 | 0.021 | 0.022 | $0$ | $1$ | $52$
J033900$-$013318 | $3.11542$ | O I | $-50.0$ | $50.0$ | $-3.4$ | 0.3 | 14.667 | 0.018 | 0.019 | $0$ | $3$ | $52$
J033900$-$013318 | $3.11542$ | S II | $-50.0$ | $50.0$ | $-19.5$ | 12.1 | 13.303 | 0.138 | 0.203 | $0$ | $2$ | $52$
J033900$-$013318 | $3.11542$ | Si II | $-50.0$ | $50.0$ | $0.7$ | 0.3 | 13.957 | 0.011 | 0.011 | $0$ | $3$ | $52$
J033900$-$013318 | $3.11542$ | Si IV | $-50.0$ | $50.0$ | $-5.1$ | 0.2 | 13.668 | 0.006 | 0.006 | $0$ | $3$ | $52$
J045213$-$164012 | $2.39910$ | Al II | $-42.0$ | $30.0$ | $999.0$ | 999.0 | 10.768 | 0.176 | 0.301 | $-1$ | $3$ | $53$
J045213$-$164012 | $2.39910$ | C IV | $-42.0$ | $30.0$ | $-4.5$ | 0.3 | 13.514 | 0.007 | 0.007 | $0$ | $3$ | $53$
J045213$-$164012 | $2.39910$ | Fe II | $-42.0$ | $30.0$ | $999.0$ | 999.0 | 12.447 | 0.176 | 0.301 | $-1$ | $3$ | $53$
J045213$-$164012 | $2.39910$ | H I | $-88.7$ | $53.6$ | $-15.7$ | 0.4 | 15.161 | 0.004 | 0.004 | $0$ | $3$ | $53$
J045213$-$164012 | $2.39910$ | N I | $-42.0$ | $30.0$ | $999.0$ | 999.0 | 12.744 | 0.176 | 0.301 | $-1$ | $3$ | $53$
J045213$-$164012 | $2.39910$ | O I | $-42.0$ | $30.0$ | $-2.5$ | 4.1 | 12.697 | 0.076 | 0.092 | $-1$ | $3$ | $53$
J045213$-$164012 | $2.39910$ | S VI | $-42.0$ | $30.0$ | $999.0$ | 999.0 | 12.311 | 0.176 | 0.301 | $-1$ | $3$ | $53$
J045213$-$164012 | $2.39910$ | Si IV | $-42.0$ | $30.0$ | $-3.9$ | 5.0 | 11.856 | 0.095 | 0.122 | $0$ | $1$ | $53$
J045213$-$164012 | $2.44044$ | Al II | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 10.642 | 0.176 | 0.301 | $-1$ | $3$ | $54$
J045213$-$164012 | $2.44044$ | C II | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 11.787 | 0.176 | 0.301 | $-1$ | $3$ | $54$
J045213$-$164012 | $2.44044$ | C IV | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 11.770 | 0.176 | 0.301 | $-1$ | $3$ | $54$
J045213$-$164012 | $2.44044$ | Fe II | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 12.253 | 0.176 | 0.301 | $-1$ | $3$ | $54$
J045213$-$164012 | $2.44044$ | Fe III | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 12.445 | 0.176 | 0.301 | $-1$ | $3$ | $54$
J045213$-$164012 | $2.44044$ | H I | $-37.9$ | $57.0$ | $4.0$ | 0.2 | 14.611 | 0.004 | 0.004 | $0$ | $3$ | $54$
J045213$-$164012 | $2.44044$ | O I | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 12.723 | 0.176 | 0.301 | $-1$ | $3$ | $54$
J045213$-$164012 | $2.44044$ | Si II | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 11.640 | 0.176 | 0.301 | $-1$ | $3$ | $54$
J045213$-$164012 | $2.44044$ | Si IV | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 11.245 | 0.176 | 0.301 | $-1$ | $3$ | $54$
J045213$-$164012 | $2.53542$ | Al II | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 10.855 | 0.176 | 0.301 | $-1$ | $3$ | $55$
J045213$-$164012 | $2.53542$ | C II | $-15.0$ | $15.0$ | $-7.9$ | 4.6 | 12.058 | 0.133 | 0.193 | $-1$ | $3$ | $55$
J045213$-$164012 | $2.53542$ | C III | $-15.0$ | $15.0$ | $10.4$ | 3.6 | 11.670 | 0.134 | 0.195 | $-1$ | $3$ | $55$
J045213$-$164012 | $2.53542$ | C IV | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 11.737 | 0.176 | 0.301 | $-1$ | $3$ | $55$
J045213$-$164012 | $2.53542$ | Fe II | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 12.036 | 0.176 | 0.301 | $-1$ | $3$ | $55$
J045213$-$164012 | $2.53542$ | H I | $-65.5$ | $38.0$ | $-14.5$ | 0.2 | 14.674 | 0.004 | 0.002 | $0$ | $3$ | $55$
J045213$-$164012 | $2.53542$ | O I | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 12.218 | 0.176 | 0.301 | $-1$ | $3$ | $55$
J045213$-$164012 | $2.53542$ | O VI | $-15.0$ | $15.0$ | $-2.5$ | 2.1 | 12.844 | 0.084 | 0.105 | $-1$ | $3$ | $55$
J045213$-$164012 | $2.53542$ | Si II | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 10.567 | 0.176 | 0.301 | $-1$ | $3$ | $55$
J045213$-$164012 | $2.53542$ | Si IV | $-15.0$ | $15.0$ | $-0.7$ | 3.3 | 11.483 | 0.122 | 0.171 | $-1$ | $3$ | $55$
J064204$+$675835 | $2.86842$ | Al II | $-15.0$ | $15.0$ | $2.9$ | 2.6 | 10.959 | 0.132 | 0.191 | $-1$ | $3$ | $56$
J064204$+$675835 | $2.86842$ | C II | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 11.928 | 0.176 | 0.301 | $-1$ | $3$ | $56$
J064204$+$675835 | $2.86842$ | C III | $-15.0$ | $15.0$ | $8.1$ | 1.4 | 12.177 | 0.051 | 0.058 | $-1$ | $3$ | $56$
J064204$+$675835 | $2.86842$ | C IV | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 11.926 | 0.176 | 0.301 | $-1$ | $3$ | $56$
J064204$+$675835 | $2.86842$ | H I | $-89.2$ | $71.8$ | $11.6$ | 1.0 | 15.894 | 0.008 | 0.004 | $0$ | $2$ | $56$
J064204$+$675835 | $2.86842$ | O I | $-15.0$ | $15.0$ | $-4.7$ | 2.9 | 12.861 | 0.127 | 0.180 | $-1$ | $3$ | $56$
J064204$+$675835 | $2.86842$ | Si II | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 11.824 | 0.176 | 0.301 | $-1$ | $3$ | $56$
J064204$+$675835 | $2.86842$ | Si III | $-15.0$ | $15.0$ | $7.1$ | 0.9 | 11.569 | 0.034 | 0.036 | $-1$ | $3$ | $56$
J064204$+$675835 | $2.86842$ | Si IV | $-15.0$ | $15.0$ | $999.0$ | 999.0 | 11.370 | 0.176 | 0.301 | $-1$ | $3$ | $56$
J064204$+$675835 | $2.90469$ | Al II | $-55.0$ | $25.0$ | $-19.5$ | 0.3 | 12.904 | 0.008 | 0.008 | $0$ | $1$ | $57$
J064204$+$675835 | $2.90469$ | C II | $-55.0$ | $25.0$ | $-17.3$ | 0.6 | 14.674 | 0.015 | 0.016 | $-2$ | $1$ | $57$
J064204$+$675835 | $2.90469$ | C IV | $-55.0$ | $25.0$ | $-14.1$ | 0.1 | 14.278 | 0.004 | 0.004 | $0$ | $3$ | $57$
J064204$+$675835 | $2.90469$ | Fe II | $-55.0$ | $25.0$ | $-28.9$ | 1.3 | 13.598 | 0.021 | 0.022 | $0$ | $1$ | $57$