11institutetext: Aix Marseille Université, CNRS, LAM (Laboratoire
d’Astrophysique de Marseille) UMR 7326, 13388, Marseille, France.
22institutetext: International Centre for Radio Astronomy Research (ICRAR),
The University of Western Australia, 35 Stirling Hwy, Crawley, WA 6009,
Australia.

# The ESO UVES Advanced Data Products Quasar Sample - I. Dataset and New
$N_{{H}\,{\sc I}}$ Measurements of Damped Absorbers

Tayyaba Zafar 11 Attila Popping 22 Céline Péroux 11

(Received / Accepted )

We present here a dataset of quasars observed with the Ultraviolet Visual
Echelle Spectrograph (UVES) on the Very Large Telescope and available in the
European Southern Observatory UVES Advanced Data Products archive. The sample
is made up of a total of 250 high resolution quasar spectra with emission
redshifts ranging from $0.191\leq z_{\rm em}\leq 6.311$. The total UVES
exposure time of this dataset is 1560 hours. Thanks to the high resolution of
UVES spectra, it is possible to unambiguously measure the column density of
absorbers with damping wings, down to $N_{{\rm H}\,{\sc\rm I}}\gtrsim 10^{19}$
cm-2, which constitutes the sub-damped Ly$\alpha$ absorber (sub-DLA)
threshold. Within the wavelength coverage of our UVES data, we find 150 damped
Ly$\alpha$ systems (DLAs)/sub-DLAs in the range $1.5<z_{\rm abs}<4.7$. Of
these 150, 93 are DLAs and 57 are sub-DLAs. An extensive search in the
literature indicates that 6 of these DLAs and 13 of these sub-DLAs have their
$N_{{\rm H}\,{\sc\rm I}}$ measured for the first time. Among them, 10 are new
identifications as DLAs/sub-DLAs. For each of these systems, we obtain an
accurate measurement of the H i column density and the absorber’s redshift in
the range $1.7<z_{\rm abs}<4.2$ by implementing a Voigt profile-fitting
algorithm. These absorbers are further confirmed thanks to the detection of
associated metal lines and/or lines from members of the Lyman series. In our
data, a few quasars’ lines-of-sight are rich. An interesting example is
towards QSO J0133+0400 ($z_{\rm em}=4.154$) with six DLAs and sub-DLAs
reported.

###### Key Words.:

Galaxies: abundances – Galaxies: high-redshift – Quasars: absorption lines –
Quasars: general.

††offprints<EMAIL_ADDRESS>
##  1 Introduction

Among the absorption systems observed in the spectra of quasars, those with
the highest neutral hydrogen column density are thought to be connected with
the gas reservoir responsible for forming galaxies at high redshift and have
deserved wide attention (see review by Wolfe et al. 2005). These systems are
usually classified according to their neutral hydrogen column density as
damped Ly$\alpha$ systems (hereafter DLAs) with $N_{{\rm H}\,{\sc\rm I}}\geq
2\times 10^{20}$ atoms cm-2 (e.g., Storrie-Lombardi & Wolfe 2000; Wolfe et al.
2005) and sub-damped Ly$\alpha$ systems (sub-DLAs) with $10^{19}\leq N_{{\rm
H}\,{\sc\rm I}}\leq 2\times 10^{20}$ atoms cm-2 (e.g., Péroux et al. 2003a).

The study of these systems has made significant progress in recent years,
thanks to the availability of large sets of quasar spectra with the two-degree
field survey (2dF, Croom et al. 2001) and the Sloan Digital Sky Survey (SDSS;
Prochaska et al. 2005; Noterdaeme et al. 2009; Noterdaeme et al. 2012b). They
have been shown to contain most of the neutral gas mass in the Universe
(Lanzetta et al. 1991, 1995; Wolfe et al. 1995) and are currently used to
measure the redshift evolution of the total amount of neutral gas mass density
(Lanzetta et al. 1991; Wolfe et al. 1995; Storrie-Lombardi & Wolfe 2000;
Péroux et al. 2003b; Prochaska et al. 2005; Noterdaeme et al. 2009, 2012b). In
addition, the sub-DLAs may contribute significantly to the cosmic metal
budget, which is still highly incomplete. Indeed, only $\sim$20% of the metals
are observed when one adds the contribution of the Ly$\alpha$ forest, DLAs,
and galaxies such as Lyman break galaxies (e.g, Pettini et al. 1999; Pagel
2002; Wolfe et al. 2003; Pettini 2004, 2006; Bouché et al. 2005, 2006, 2007).

Therefore, to obtain a complete picture of the redshift evolution of both the
cosmological neutral gas mass density and the metal content of the Universe,
the less-studied sub-DLAs should be taken into account (Péroux et al. 2003a).
However, these systems cannot be readily studied at low resolution, and only
limited samples of high-resolution quasar spectra have been available until
now (e.g., Péroux et al. 2003a; Dessauges-Zavadsky et al. 2003; Ledoux et al.
2003; Kulkarni et al. 2007; Meiring et al. 2008, 2009).The excellent
resolution and large wavelength coverage of UVES allows this less studied
class of absorber to be explored.

We have therefore examined the high-resolution quasar spectra taken between
February 2000 and March 2007 and available in the UVES (Dekker et al. 2000)
Advanced Data Products archive, ending up with a sample of 250 quasar spectra.
In this paper we present both the dataset of quasars observed with UVES and
the damped absorbers (DLAs and sub-DLAs) covered by these spectra. In
addition, we measured column densities of DLAs/sub-DLAs seen in the spectra of
these quasars and not reported in the literature. In a companion paper (Zafar
et al. 2013), we built a carefully selected subset of this dataset to study
the statistical properties of DLAs and sub-DLAs, their column density
distribution, and the contribution of sub-DLAs to the gas mass density.
Further studies, based on specifically designed subsets of the dataset built
in this paper, will follow (e.g., studies of metal abundances, molecules).

This work is organized as follows. In §2, information about the UVES quasar
data sample is provided. In §3, the properties of the damped absorbers are
described. This section also summarizes the details of the new column density
measurements. In §4, some global properties of the full sample are presented
and lines-of-sight of interest are reported in §5. All log values and
expressions correspond to log base 10.

##  2 The Quasar Sample

###  2.1 ESO Advanced Data Products

In 2007, the European Southern Observatory (ESO) managing the 8.2m Very Large
Telescope (VLT) observatory has made available to the international community
a set of Advanced Data Products for some of its instruments, including the
high-resolution UVES111http://archive.eso.org/eso/eso_archive_adp.html
instrument. The reduced archival UVES echelle dataset is processed by the ESO
UVES pipeline (version 3.2) within the MIDAS environment with the best
available calibration data. This process has been executed by the quality
control (QC) group, part of the Data Flow Department. The resulting sample is
based on an uniform reprocessing of UVES echelle point source data from the
beginning of operations (dated 18th of February 2000) up to the 31st of March
2007. The standard quality assessment, quality control and certification have
been integral parts of the process. The following types of UVES data are not
included in the product data set: $i)$ data using the image slicers and/or the
absorption cell; $ii)$ Echelle data from extended objects and iii) data from
the Fibre Large Array Multi Element Spectrograph (FLAMES)/UVES instrument
mode.

In general, no distinction has been made between visitor mode (VM) and service
mode (SM) data, nor between standard settings and non-standard settings.
However, the data reduction was performed only when robust calibration
solutions i.e., (“master calibrations”) were available. In the UVES Advanced
Data Products archive, these calibrations are available only for the standard
settings centered on $\lambda$ 346, 390, 437, 520, 564, 580, 600 or 860 nm.
For certain “non-standard” settings, master calibrations were not produced in
the first years of UVES operations (until about 2003). These are e.g. 1x2 or
2x3 binnings, or the central wavelengths mentioned above. As a result, the
Advanced Data Products database used for the study presented here is not as
complete as the ESO UVES raw data archive.

###  2.2 Quasars Selection

The UVES archives do not provide information on the nature of the targets.
Indeed, the target names are chosen by the users and only recently does the
Phase 2 step propose for the user to classify the targets, but only on a
voluntary-basis. Therefore, the first step to construct a sample of quasar
spectra out of the Advanced Data Products archive is to identify the nature of
the objects. For this purpose we retrieved quasar lists issued from quasar
surveys: the Sloan digital sky survey data release 7 (DR7)
database222http://www.sdss.org/dr7/, HyperLeda333http://leda.univ-lyon1.fr/,
2dF quasar redshift
survey444http://www.2dfquasar.org/Spec_Cat/2qzsearch2.html,
Simbad555http://simbad.u-strasbg.fr/ and the Hamburg ESO catalogue. The
resulting right ascension (RA) and declination (Dec) of the quasars were
cross-matched with UVES Advanced Data Products archive within a radius of
$15.0^{\prime\prime}$. The large radius was chosen to overcome possible
relative astrometric shifts between the various surveys and the UVES database.
Because of this large radius, the raw matched list do not only contain quasars
but also other objects such as stars, galaxies, Seyferts. The non-quasar
objects have been filtered out by visual inspection of the spectra. The data
in an ESO OPC category C (Interstellar Medium, Star Formation and Planetary
Systems) and D (Stellar Evolution) are usually targeting galactic objects, but
for some cases observers targeted quasars under the same program. The spectra
have been visually inspected for those particular cases.

###  2.3 Further Data Processing

In the UVES spectrograph, the light beam from the telescope is split into two
arms (UV to Blue and Visual to Red) within the instrument. The spectral
resolution of UVES is about $R=\lambda/\Delta\lambda\sim 41,400$ when a
$1.0^{\prime\prime}$ slit is used. By varying slit width, the maximum spectral
resolution can reach up to $R=80,000$ and $110,000$ for the BLUE and the RED
arm, respectively. For each target, individual spectra (most often with
overlapping settings) were merged using a dedicated Python code which weights
each spectrum by its signal-to-noise ratio. All contributing spectra were
regridded to a common frame, with the resolution being that of the spectrum
with the highest sampling. When present, the bad pixels were masked to assure
that they would not contribute to the merged spectrum. In the regions of
overlap the spectra were calibrated to the same level before being error-
weighted and merged. Particular attention was given to “step” features in the
quasar continua and a visual search has identified and corrected these
features when they corresponded to the position in between two orders of the
Echelle spectrum. In the merging process for each individual spectrum, a
radial velocity correction for barycentric and heliocentric motion (using
heliocentric correction values from the files header) was applied. A vacuum
correction on the wavelength was also applied.

The resulting list comprises 250 quasar spectra. The number of individual
spectra used to produce the co-added spectrum, Simbad $V$-band magnitudes,
together with total exposure time in seconds for each target, are provided in
Table 1. Throughout the paper, this sample obtained from the ESO UVES Advanced
Data Products facility is called EUADP sample. The total VLT exposure time of
this dataset is $T_{\rm tot}=1560$ hours.

In the case of close pairs of quasars or gravitationally-lensed quasars, we
have separated the objects if different slit-positions were used but only
analyzed the brightest object if these objects were aligned along the slit.
Our sample contains two lensed quasars: QSO B0908+0603 (double system) and QSO
B1104-181 (quadruple system). In the former case two objects, and, in the
latter case, three objects were aligned on the slit (Lopez et al. 2007). In
these cases we only analyzed the brightest objects. Our sample contains four
quasar pairs: QSO J0008-2900 & QSO J0008-2901 (separated by $1.3^{\prime}$),
J030640.8-301032 & J030643.7-301107 (separated by $\sim$0.85′), QSO B0307-195A
& B (separated by $\sim$1′), and QSO J1039-2719 & QSO B1038-2712 (separated by
$17.9^{\prime}$). For these eight objects, eight different slit-positions were
used.

Figure 1: An example of a UVES quasar spectrum of J223941.8-294955 at
$z_{em}=2.102$. The quasar continuum (red overlay) is fitted using a spline
function.

##  3 The DLA/sub-DLA Sample

The quasar spectra were normalized to unity within the MIDAS environment. For
each quasar the local continuum was determined in the merged spectrum by using
a spline function to smoothly connect the regions free of absorption features
(see Fig. 1). The final normalized spectra used for column density analysis
were obtained by dividing merged spectra by these continua. During
normalization, the artifact from residual fringes (especially in standard
setting centered on $\lambda$ 860nm) and spectral gaps are also included in
the spline fitting. In order to secure all DLAs and sub-DLAs in a given
spectrum, we proceeded as in Lanzetta et al. (1991) and used an automated
Python detection algorithm. This code builds an equivalent width spectrum over
400 pixel wide boxes ($\sim$12 Å for 0.03 $\AA$ pixel-1) blueward of the
quasar’s Ly$\alpha$ emission and flags regions of the spectra where the
observed equivalent width exceeds the sub-DLA definition (i.e. $N_{{\rm
H}\,{\sc\rm I}}\gtrsim 10^{19}$ cm-2). This candidate list of DLAs and sub-
DLAs is further supplemented by visual inspection done by TZ and CP. The DLAs
and sub-DLAs have been confirmed by looking for associated metal lines and/or
higher members of the Lyman series. This resulted in 150 DLAs/sub-DLAs with
$1.6<z_{\rm abs}<4.7$ for which Ly$\alpha$ is covered in the spectra of these
quasars. This method is complete down to the sub-DLA definition of $N_{{\rm
H}\,{\sc\rm I}}=10^{19}$ equivalent to $\rm EW_{\rm rest}=2.5$ $\AA$ based on
a curve of growth analysis (Dessauges-Zavadsky et al. 2003).

###  3.1 $N_{{\rm H}\,{\sc\rm I}}$ measurements of DLAs and sub-DLAs

An extensive search in the literature was undertaken to identify which of
these damped absorbers were already known. Of the 150 DLAs/sub-DLAs that we
have identified above, 131 (87 DLAs and 44 sub-DLAs) have their $N_{{\rm
H}\,{\sc\rm I}}$ already reported in the literature. Of the remaining 19 (6
DLAs and 13 sub-DLAs), 10 (3 DLAs and 7 sub-DLAs) are new identifications (see
Table 2 and §3.2 for details on each system).

For damped absorbers, the Lorentzian component of the Voigt profile results in
pronounced damping wings, allowing precise determination of $N_{{\rm
H}\,{\sc\rm I}}$ down to the sub-DLA definition at high-resolution. The
neutral hydrogen column density measurements of these absorbers are determined
by fitting a Voigt profile to the Ly$\alpha$ absorption line. The fits were
performed using the $\chi^{2}$ minimization routine FITLYMAN package in MIDAS
(Fontana & Ballester 1995). Laboratory wavelengths and oscillator strengths
from Morton (2003) were used. The global fit returns the best fit parameters
for central wavelength, column density, and Doppler turbulent broadening, as
well as errors on each quantity. The central redshift was left as a free
parameter except when no satisfactory fit could be found in which case the
strongest component of the metal line was chosen as central redshift. The
Doppler turbulent parameter $b$-value was usually left as a free parameter and
sometimes fixed because of low signal-to-noise or multiple DLAs at 30 km s-1
(for DLAs) or $20$ km s-1 (for sub-DLAs). The $N_{{\rm H}\,{\sc\rm I}}$ fit is
performed using the higher members of the Lyman series, in addition to
Ly$\alpha$, where these are available. For fitting $N_{{\rm H}\,{\sc\rm I}}$,
we usually used the components from ${O\textsc{i}}$. The other low ionization
line components are used to fit $N_{{\rm H}\,{\sc\rm I}}$ for the cases where
there is no ${O\textsc{i}}$ covered by our data. Table 2 summarizes the
properties of the DLAs/sub-DLAs for which we obtained ${\rm H}\,{\sc\rm I}$
column density for the first time and provides quasar emission redshifts,
absorption redshifts, H i column densities and metal line lists.

Moreover, the majority of the $N_{{\rm H}\,{\sc\rm I}}$ measurements of the
DLAs/sub-DLAs towards the 250 EUADP quasars comes from high-resolution data
mostly from UVES or Keck/HIRES. In 7 cases, we cover the DLA/sub-DLA in our
data but the $N_{{\rm H}\,{\sc\rm I}}$ in the literature is obtained from
low/moderate resolution spectra. For these 7 cases, we refitted the DLA/sub-
DLA using the EUADP data and new $N_{{\rm H}\,{\sc\rm I}}$ are reported in
Table 3. For most of the cases, we find consistent results with the low
resolution studies. In the case of QSO B1114-0822, Storrie-Lombardi & Wolfe
(2000) reported a DLA with log $N_{{\rm H}\,{\sc\rm I}}=20.3$ at $z_{\rm
abs}=4.258$ while we find a sub-DLA with log $N_{{\rm H}\,{\sc\rm I}}=20.02\pm
0.12$.

Table 2: List of 6 damped and 13 sub-damped absorbers with new $N_{{\rm H}\,{\sc\rm I}}$ measurements. The details of these absorbers are provided in the columns as (1) Simbad quasar name, (2) emission redshift, (3) absorption redshift, (4) H i column density with corresponding errors, (5) members of Lyman series covered, (6) metal lines associated with the system, and (7) is the absorber a new identification as DLA/sub-DLA? Quasar | $z_{\rm em}$ | $z_{\rm abs}$ | log $N_{{\rm H}\,{\sc\rm I}}$ | Ly series | Metals | New?
---|---|---|---|---|---|---
|  |  | cm-2 |  |  |
QSO J0008-2900 | 2.645 | 2.254 | $20.22\pm 0.10$ | Ly$\beta$ | O i, Fe ii, Si ii, C ii, Mg ii, Al iii, Si iv | no
QSO J0008-2901 | 2.607 | 2.491 | $19.94\pm 0.11$ | Ly$\gamma$ | O i, Fe ii, Si ii, C ii, Al ii, Si iv | no
QSO J0041-4936 | 3.240 | 2.248 | $20.46\pm 0.13$ | Ly$\beta$ | O i, Fe ii, Si ii, C ii, Al ii, Zn ii, Al iii, C iv | no
QSO B0128-2150 | 1.900 | 1.857 | $20.21\pm 0.09$ | Ly$\alpha$ | O i, Fe ii, Si ii, C ii, Al iii | no
J021741.8-370100 | 2.910 | 2.429 | $20.62\pm 0.08$ | Ly$\beta$ | O i, Si ii | no
$\cdots$ | $\cdots$ | 2.514 | $20.46\pm 0.09$ | Ly$\beta$ | Fe ii, Si ii | no
J060008.1-504036 | 3.130 | 2.149 | $20.40\pm 0.12$ | Ly$\alpha$ | O i, Fe ii, Si ii, C ii, Al ii, Al iii | yes
QSO B0952-0115 | 4.426 | 3.476 | $20.04\pm 0.07$ | Ly$\alpha$ | Fe ii, Si ii, Al ii, Al iii, C iv | yes
Q1036-272 | 3.090 | 2.792 | $20.65\pm 0.13$ | Ly$\beta$ | O i, Fe ii, Si ii, Al iii | yes
QSO B1036-2257 | 3.130 | 2.533 | $19.30\pm 0.10$ | Ly$\alpha$ | Fe ii, Si ii, C ii, Al iii, Si iv, C iv | no
QSO B1036-268 | 2.460 | 2.235 | $19.96\pm 0.09$ | Ly$\beta$ | O i, Fe ii, Si ii, C ii, Al ii, Mg ii, Al iii, Si iv, C iv | yes
LBQS 1232+0815 | 2.570 | 1.720 | $19.48\pm 0.13$ | Ly$\alpha$ | O i, Fe ii, Si ii, Al iii, Si iv, C iv | yes
QSO J1330-2522 | 3.910 | 2.654 | $19.56\pm 0.13$ | Ly$\alpha$ | Si ii, Al ii, Al iii, Si iv, C iv | yes
QSO J1356-1101 | 3.006 | 2.397 | $19.88\pm 0.09$ | Ly$\alpha$ | O i, Fe ii, Si ii | yes
QSO J1723+2243 | 4.520 | 4.155 | $19.23\pm 0.12$ | Ly$\gamma$ | metal lines blended or not covered | yes
LBQS 2114-4347 | 2.040 | 1.912 | $19.50\pm 0.10$ | Ly$\alpha$ | O i, Fe ii, Si ii, C ii, Al ii, Mg ii, Si iv, C iv | yes
J223941.8-294955 | 2.102 | 1.825 | $19.84\pm 0.14$ | Ly$\alpha$ | O i, Fe ii, Si ii, C ii, Al ii, Mg ii, Al iii, Si iv, C iv | no
QSO B2318-1107 | 2.960 | 1.629 | $20.52\pm 0.14$ | Ly$\alpha$ | Fe ii, Si ii, C ii, Al ii, Al iii, Si iv | yes
QSO B2342+3417 | 3.010 | 2.940 | $20.18\pm 0.10$ | Ly$\gamma$ | limited red wavelength coverage | no

###  3.2 Notes on Individual Objects

In this section, we provide details on the DLAs and sub-DLAs in the EUADP
sample for which ${\rm H}\,{\sc\rm I}$ column density is determined in this
work. Best fit parameters of the Voigt profile fits to the H i absorption
lines are detailed below.

Figure 2: The sub-DLA detected towards QSO J0008-2900 at $z_{\rm abs}=2.254$.
The solid red line shows the Voigt profile fit to the sub-DLA with an inferred
column density of log $N_{{\rm H}\,{\sc\rm I}}=20.22\pm 0.10$. The system is
detected down to Ly$\beta$. Here and in the following figures, the dotted blue
line represents 1$\sigma$ error on the spectrum. The vertical dotted line is
the adopted zero velocity corresponding to the redshift of the sub-DLA. The
horizontal line is at a level of one. Figure 3: The sub-DLA detected towards
QSO J0008-2901 at $z_{\rm abs}=2.491$. The solid red line corresponds to the
Voigt profile fit to the sub-DLA with an inferred column density of log
$N_{{\rm H}\,{\sc\rm I}}=19.94\pm 0.11$. The system is detected down to
Ly$\gamma$.

Table 3: New high-resolution $N_{{\rm H}\,{\sc\rm I}}$ measurements of DLAs/sub-DLAs previously observed at low/medium resolution. Quasar | High resolution | Low/medium resolution
---|---|---
| $z_{\rm abs}$ | log $N_{{\rm H}\,{\sc\rm I}}$ | Survey/ | log $N_{{\rm H}\,{\sc\rm I}}$
|  | cm-2 | Instrument | cm-2
J004054.7-091526 | 4.538 | $20.20\pm 0.09$ | SDSS |  $20.22\pm 0.26$1
$\cdots$ | 4.740 | $20.39\pm 0.11$ | SDSS |  $20.55\pm 0.15$2
QSO B1114-0822 | 4.258 | $20.02\pm 0.12$ | WHT | 20.33
J115538.6+053050 | 2.608 | $20.37\pm 0.11$ | SDSS |  $20.47\pm 0.23$1
$\cdots$ | 3.327 | $21.00\pm 0.10$ | SDSS |  $20.91\pm 0.27$1
LBQS 2132-4321 | 1.916 | $20.74\pm 0.09$ | LBQS | 20.703
J235702.5-004824 | 2.479 | $20.41\pm 0.08$ | SDSS | 20.452

References: (1) Noterdaeme et al. (2009); (2) Prochaska et al. (2008);
(3)Storrie-Lombardi & Wolfe (2000)

  1. 1.

QSO J0008-2900 ($z_{\rm em}=2.645$). The quasar was discovered during the
course of the 2dF quasar redshift survey (Croom et al. 2001). An H i absorber
at $z=2.253$ is reported by Tytler et al. (2009). We find that the absorber is
a sub-DLA with log $N_{{\rm H}\,{\sc\rm I}}=20.22\pm 0.10$ and $b=28.5\pm 2.2$
km s-1 at $z_{\rm abs}=2.254$. The Lyman series lines down to Ly$\beta$ are
fitted together. In the red part of the spectrum metal lines from O i
$\lambda$ 1302, Fe ii $\lambda\lambda\lambda\lambda$ 2344, 2374, 2382, 2586,
Si ii $\lambda\lambda\lambda\lambda$ 1260, 1304, 1526, 1808, C ii $\lambda$
1334, Mg ii $\lambda\lambda$ 2796, 2803, Al iii $\lambda\lambda$ 1854, 1862,
and Si iv $\lambda\lambda$ 1393, 1402 are detected at the redshift of the sub-
DLA. Fig. 2 shows our best fit result of the H i lines.

Figure 4: The DLA detected towards QSO J0041-4936 at $z_{\rm abs}=2.248$. For
plotting purposes the Ly$\beta$ region of the spectrum is smoothed with a
boxcar average of 2.0 pixels. The solid red line represents the Voigt profile
fit to the DLA with an inferred column density of log $N_{{\rm H}\,{\sc\rm
I}}=20.46\pm 0.13$. The system is detected down to Ly$\beta$. Figure 5: The
sub-DLA detected towards QSO B0128-2150 at $z_{\rm abs}=1.857$. The solid red
line shows the Voigt profile fit to the sub-DLA with an inferred column
density of log $N_{{\rm H}\,{\sc\rm I}}=20.21\pm 0.09$.

  2. 2.

QSO J0008-2901 ($z_{\rm em}=2.607$). The quasar was also discovered during the
course of the 2dF quasar redshift survey (Croom et al. 2001). An H i absorber
at $z=2.491$ is reported by Tytler et al. (2009). We find that the absorber at
$z_{\rm abs}=2.491$ is a sub-DLA with log $N_{{\rm H}\,{\sc\rm I}}=19.94\pm
0.11$ and $b=39\pm 3.5$ km s-1 detected down to Ly$\gamma$. Metal lines from O
i $\lambda$ 1302, Fe ii $\lambda\lambda\lambda\lambda$ 2344, 2374, 2382, 2586,
Si ii $\lambda\lambda\lambda$ 1260, 1304, 1808, C ii $\lambda$ 1334, Al ii
$\lambda$ 1670, and Si iv $\lambda\lambda$ 1393, 1402 are detected in the red
part of the spectrum. Fig. 3 shows our best fit result of the H i lines.

  3. 3.

QSO J0041-4936 ($z_{\rm em}=3.240$). A damped absorber is known in this quasar
from the Calán Tololo survey (Maza et al. 1995). From a low-resolution
spectrum, Lopez et al. (2001) measured the equivalent width of the H i
absorption line to be ${\rm EW_{obs}}=34.60\,\AA$ but state that they cannot
measure the H i column density due to the limited spectral resolution. Using
the high-resolution UVES spectrum, we are able to measure the column density
of the DLA to be log $N_{{\rm H}\,{\sc\rm I}}=20.46\pm 0.13$ and $b=29\pm 3.9$
km s-1 at $z_{\rm abs}=2.248$ detected down to Ly$\beta$. Metal lines from O i
$\lambda$ 1302, Fe ii $\lambda\lambda$ 1608, 1611, Si ii
$\lambda\lambda\lambda\lambda$ 1260, 1304, 1526, 1808, C ii $\lambda$ 1334, Al
ii $\lambda$ 1670, Zn ii $\lambda$ 2026, Al iii $\lambda\lambda$ 1854, 1862,
and C iv $\lambda\lambda$ 1548, 1550 associated with the DLA are detected in
the red part of the spectrum. Fig. 4 shows the best fit result of the H i
lines.

Figure 6: The DLA detected towards J021741.8-370100 at $z_{\rm abs}=2.429$.
The solid red line represents the Voigt profile fit to the DLA with an
inferred column density of log $N_{{\rm H}\,{\sc\rm I}}=20.62\pm 0.08$. The
system is detected down to Ly$\beta$.

  4. 4.

QSO B0128-2150 ($z_{\rm em}=1.900$). This quasar was discovered during the
course of the Montréal-Cambridge-Tololo survey (Lamontagne et al. 2000). Two
absorbing systems at $z_{\rm abs}=1.64$ and 1.85 are reported in the UVES
observing proposal. We find that the system at $z_{\rm abs}=1.857$ is a sub-
DLA with log $N_{{\rm H}\,{\sc\rm I}}=20.21\pm 0.09$ and $b=25\pm 2.6$ km s-1.
Metal lines from O i $\lambda$ 1302, Fe ii $\lambda\lambda\lambda$ 2344, 2374,
2382, Si ii $\lambda\lambda\lambda$ 1260, 1304, 1808, C ii $\lambda$ 1334, and
Al iii $\lambda\lambda$ 1854, 1862 at the redshift of the absorber are
observed in the red part of the spectrum. Fig. 5 shows our best fit result of
the H i column density. The absorbing system at $z_{abs}=1.64$ is below sub-
DLA limit.

Figure 7: The DLA detected towards J021741.8-370100 at $z_{\rm abs}=2.514$.
The solid red line corresponds to the Voigt profile fit to the DLA with an
inferred column density of log $N_{{\rm H}\,{\sc\rm I}}=20.46\pm 0.13$. The
system is detected down to Ly$\beta$.

  5. 5.

J021741.8-370100 ($z_{\rm em}=2.910$). Damped absorbers have been known in
this quasar from the Calán Tololo survey (Maza et al. 1996). The column
densities for these DLAs have not been reported before. We measure log
$N_{{\rm H}\,{\sc\rm I}}=20.62\pm 0.08$ at $z_{\rm abs}=2.429$ and log
$N_{{\rm H}\,{\sc\rm I}}=20.46\pm 0.09$ at $z_{\rm abs}=2.514$. Both absorbers
are seen down to Ly$\beta$. The $b$ parameter is fixed to $b=30$ km s-1 for
both absorbers. Due to limited wavelength coverage only a few metal lines
associated with the absorbers are seen in the spectrum. Metal lines from O i
$\lambda$ 1302 and Si ii $\lambda\lambda\lambda\lambda$ 1190, 1193, 1260, 1304
are covered for the absorber at $z_{\rm abs}=2.429$. The lines from Fe ii
$\lambda$ 1144 and Si ii $\lambda\lambda\lambda$ 1190, 1193, 1260 associated
with the absorber at $z_{\rm abs}=2.514$ are covered in the spectrum. Fig. 6
and Fig. 7 show our best fit of H i lines for absorbers at $z_{\rm abs}=2.429$
and $z_{\rm abs}=2.514$ respectively.

Figure 8: The DLA detected towards J060008.1-504036 at $z_{\rm abs}=2.149$.
The solid red line shows the Voigt profile fit to the DLA with a total column
density of log $N_{{\rm H}\,{\sc\rm I}}=20.40\pm 0.12$ using velocity
components at 24, 0, -44 km s-1.
Figure 9: The sub-DLA detected towards J0952-0115 at $z_{\rm abs}=3.476$. The
solid red line corresponds to the Voigt profile fit to the sub-DLA with an
inferred column density of log $N_{{\rm H}\,{\sc\rm I}}=20.04\pm 0.07$.

  6. 6.

J060008.1-504036 ($z_{\rm em}=3.130$). This quasar was discovered during the
course of the Calán Tololo survey (Maza et al. 1996). No detailed analysis of
this quasar has been published. A Lyman limit system at $z_{\rm LLS}=3.080$ is
seen in the spectrum. We identified a DLA at $z_{\rm abs}=2.149$. The column
density of the DLA is fitted using three strong components (at 24, 0, and -44
km s-1) seen in ${O\textsc{i}}$, resulting in a total column density of log
$N_{{\rm H}\,{\sc\rm I}}=20.40\pm 0.12$ with $b=20$ km s-1 fixed for each
component. Metal absorption lines from O i $\lambda$ 1302, Fe ii
$\lambda\lambda$ 1608, 1611, Si ii $\lambda\lambda\lambda\lambda$ 1260, 1304,
1526, 1808, C ii $\lambda$ 1334, Al ii $\lambda$ 1670, and Al iii
$\lambda\lambda$ 1854, 1862 at the redshift of the DLA are covered in the red
part of the spectrum. Fig. 8 shows our best fit of the neutral hydrogen column
density of the DLA at $z_{\rm abs}=2.149$.

Figure 10: The DLA detected towards QSO 1036-272 at $z_{\rm abs}=2.792$. The
solid red line represents the Voigt profile fit to the DLA with an inferred
column density of log $N_{{\rm H}\,{\sc\rm I}}=20.65\pm 0.13$. The system is
detected down to Ly$\beta$.
Figure 11: The sub-DLA detected towards QSO 1036-2257 at $z_{\rm abs}=2.533$.
The solid red line represents the Voigt profile fit to the sub-DLA with a
total column density of log $N_{{\rm H}\,{\sc\rm I}}=19.30\pm 0.10$ fitted
with two velocity components at 0 and -144 km s-1.
Figure 12: The sub-DLA detected towards QSO B1036-268 at $z_{\rm abs}=2.235$.
Ly$\beta$ region of the spectrum is smoothed with a boxcar average of 2.0
pixels for plotting purposes. The solid red line corresponds to the Voigt
profile fit to the sub-DLA with a total column density of log $N_{{\rm
H}\,{\sc\rm I}}=19.96\pm 0.09$ from 0, -55, -95, and -297 km s-1 velocity
components. The system is detected down to Ly$\beta$.

  7. 7.

QSO B0952-0115 ($z_{\rm em}=4.426$). One damped absorber was previously
reported in this quasar at $z_{\rm abs}=4.024$ (Storrie-Lombardi & Wolfe 2000;
Prochaska et al. 2007). A Lyman limit system at $z_{\rm LLS}=4.242$ is
detected in the spectrum. We find a sub-DLA at $z_{\rm abs}=3.476$ with log
$N_{{\rm H}\,{\sc\rm I}}=20.04\pm 0.07$ and $b=32\pm 3.9$ km s-1. Metal lines
from Fe ii $\lambda\lambda$ 1608, 1611, Si ii $\lambda\lambda\lambda$ 1260,
1304, 1526, Al ii $\lambda$ 1670, Al iii $\lambda\lambda$ 1854, 1862, and C iv
$\lambda\lambda$ 1548, 1550 associated with the sub-DLA are covered in the red
part of the spectrum. Fig. 9 shows the best fit result of the H i column
density.

  8. 8.

Q1036-272 ($z_{\rm em}=3.090$). A low-resolution spectrum of this quasar has
been previously published (Jakobsen & Perryman 1992). We report a DLA with
${H\textsc{i}}$ column density of log $N_{{\rm H}\,{\sc\rm I}}=20.65\pm 0.13$
and $b=35\pm 5$ km s-1 down to Ly$\beta$ at $z_{\rm abs}=2.792$. Several metal
absorption lines from O i $\lambda$ 1302, Fe ii $\lambda\lambda\lambda\lambda$
1144, 2344, 2374, 2382, Si ii $\lambda\lambda\lambda\lambda$ 1190, 1193, 1260,
1304, and Al iii $\lambda\lambda$ 1854, 1862 are covered in the red part of
the spectrum. Fig. 10 shows best fit result of the H i lines at $z_{\rm
abs}=2.792$.

Figure 13: The sub-DLA detected towards LBQS 1232$+$0815 at $z_{\rm
abs}=1.720$. The spectrum is smoothed with a boxcar average of 0.5 pixel for
plotting purposes. The solid red line represents the Voigt profile fit to the
sub-DLA with a total column density of log $N_{{\rm H}\,{\sc\rm I}}=19.48\pm
0.13$ using 0 and -78 km s-1 velocity components (see Fig. 14).
Figure 14: Low and high ionization metal lines associated with the sub-DLA at
$z_{\rm abs}=1.720$ (zero velocity) along the line-of-sight of LBQS
1232$+$0815 are shown. The line IDs are given in each panel.

  9. 9.

QSO B1036-2257 ($z_{\rm em}=3.130$). A damped and sub-damped absorber were
previously reported in this quasar at $z_{\rm abs}=2.777$ (Fox et al. 2009)
and $z_{\rm abs}=2.531$ (Lopez et al. 2001) respectively. A Lyman limit system
at $z_{\rm LLS}=2.792$ is also detected. From a low-resolution spectrum, Lopez
et al. (2001) measured the equivalent width of the H i absorption line to be
${\rm EW_{obs}}=13.52\,\AA$ but state that they cannot measure the H i column
density due to the limited spectral resolution. Using the high-resolution UVES
spectrum, we are able to identify two main components in the system from the
metal lines at 0 and -144 km s-1. Fitting these components we measure the
total column density of the sub-DLA to be log $N_{{\rm H}\,{\sc\rm
I}}=19.30\pm 0.10$ with $b$ parameter of $b=26\pm 3.4$ and fixed 20 km s-1 (at
0 and -144 km s-1). The component at 0 km s-1 is stronger and heavily
dominates over the component at 144 km s-1. Metal lines from Fe ii
$\lambda\lambda\lambda\lambda$ 1144, 2344, 2382, 2586, Si ii
$\lambda\lambda\lambda$ 1193, 1260, 1526, C ii $\lambda$ 1334, Al iii
$\lambda\lambda$ 1854, 1862, Si iv $\lambda\lambda$ 1393, 1402, and C iv
$\lambda\lambda$ 1548, 1550 associated with the sub-DLA are detected in the
red part of the spectrum. Fig. 11 shows the best fit result of the H i column
density.

Figure 15: The sub-DLA detected towards QSO J1330-2522 at $z_{\rm abs}=2.654$.
The solid red line shows the Voigt profile fit to the sub-DLA with an inferred
column density of log $N_{{\rm H}\,{\sc\rm I}}=19.56\pm 0.13$.
Figure 16: Low ionization metal lines associated with the sub-DLA at $z_{\rm
abs}=2.654$ along the line-of-sight of LBQS 1330-2522. The vertical dashed
line is adopted zero velocity corresponding to $z_{\rm abs}=2.654$. The line
IDs are given in each panel. The shaded area corresponds to the regions
affected by cosmic rays.
Figure 17: The sub-DLA detected towards QSO J1356-1101 at $z_{\rm abs}=2.397$.
The solid red line represents the Voigt profile fit to the sub-DLA with a
total column density of log $N_{{\rm H}\,{\sc\rm I}}=19.88\pm 0.09$ using 29,
0, -48 and -300 km s-1 velocity components.

  10. 10.

QSO B1036-268 ($z_{\rm em}=2.460$). A low-resolution slit spectrum of the
quasar has been previously published (Jakobsen & Perryman 1992). We find four
strong velocity components in the system at $z_{\rm abs}=2.235$ from the metal
lines. The column density of the sub-DLA fitted down to Ly$\beta$ with four
components at 0, -55, -95, and -144 km s-1, resulting a total of log $N_{{\rm
H}\,{\sc\rm I}}=19.96\pm 0.09$ and $b=20$, 20, 20 (fixed), and $35\pm 3.0$ km
s-1 respectively. The component at 0 km s-1 is strongest and heavily dominates
over other components. Strong metal absorption lines from O i $\lambda$ 1302,
Fe ii $\lambda\lambda\lambda\lambda\lambda\lambda\lambda$ 1144, 1608, 1611,
2344, 2374, 2382, 2586, Si ii $\lambda\lambda\lambda\lambda\lambda$ 1190,
1193, 1260, 1304, 1526, C ii $\lambda$ 1334, Al ii $\lambda$ 1670, Mg ii
$\lambda\lambda$ 2796, 2803, Al iii $\lambda\lambda$ 1854, 1862, Si iv
$\lambda\lambda$ 1393, 1402, and C iv $\lambda\lambda$ 1548, 1550 at the
redshift of the sub-DLA are covered in the red part of the spectrum. Fig. 12
shows our best fit result of H i lines of the sub-DLA.

  11. 11.

LBQS 1232+0815 ($z_{\rm em}=2.570$). A DLA was known at $z_{\rm abs}=2.338$
along the line-of-sight of this quasar (Prochaska et al. 2007; Ivanchik et al.
2010). We report for the first time a sub-DLA at $z_{\rm abs}=1.720$ with
total log $N_{{\rm H}\,{\sc\rm I}}=19.48\pm 0.13$. From ${O\textsc{i}}$, we
identified two main velocity components from the system at 0 and -78 km s-1
(see Fig. 14) where $b$ is fixed at $b=20$ km s-1 for both components. Metal
absorption lines from O i $\lambda$ 1302, Fe ii
$\lambda\lambda\lambda\lambda\lambda$ 1608, 1611, 2344, 2374, 2382, Si ii
$\lambda\lambda$ 1526, 1808, Al iii $\lambda\lambda$ 1854, 1862, Si iv
$\lambda\lambda$ 1393, 1402, and C iv $\lambda\lambda$ 1548, 1550 associated
with the sub-DLA are covered in the red part of the spectrum. Fig. 13 shows
the best fit result of H i column density of the sub-DLA. While the Ly$\alpha$
line is noisy, the presence of the sub-DLA is confirmed through the metal
lines detected in the spectrum (see Fig. 14).

Figure 18: The sub-DLA detected towards J1723$+$2243 at $z_{\rm abs}=4.155$.
The solid red line corresponds to the Voigt profile fit to the sub-DLA with an
inferred column density of log $N_{{\rm H}\,{\sc\rm I}}=19.23\pm 0.12$. The
system is detected down to the Ly$\gamma$ range.
Figure 19: The sub-DLA detected towards LBQS 2114-4347 at $z_{\rm abs}=1.912$.
For plotting purposes the spectrum is smoothed with a boxcar average of 1.0
pixel. The solid red line shows the Voigt profile fit to the sub-DLA with an
inferred column density of log $N_{{\rm H}\,{\sc\rm I}}=19.50\pm 0.10$.

  12. 12.

QSO J1330-2522 ($z_{\rm em}=3.910$). Two sub-DLAs were previously reported at
$z_{\rm abs}=2.910$ and 3.080 (Péroux et al. 2001) along the line-of-sight of
this quasar. A Lyman limit system at $z_{\rm LLS}=3.728$ is also seen. We
report a new sub-DLA at $z_{\rm abs}=2.654$ with neutral hydrogen column
density of log $N_{{\rm H}\,{\sc\rm I}}=19.56\pm 0.13$ and $b=25.5\pm 2.4$ km
s-1. Fig. 15 shows our best fit result. Metal lines from Si ii
$\lambda\lambda\lambda$ 1260, 1526, 1808, Al ii $\lambda$ 1670, Al iii
$\lambda\lambda$ 1854, 1862, Si iv $\lambda\lambda$ 1393, 1402, and C iv
$\lambda\lambda$ 1548, 1550 are covered in the red part of the spectrum at the
redshift of the sub-DLA. As an example of metal lines, low ionization lines
from the sub-DLA confirming its presence are plotted in Fig. 16. High
ionization lines are blended with the lines from the other two sub-DLAs.

  13. 13.

QSO J1356-1101 ($z_{\rm em}=3.006$). Two damped absorbers have been previously
reported in this quasar at $z_{\rm abs}=2.501$ and 2.967 (Prochaska et al.
2007; Noterdaeme et al. 2008; Fox et al. 2009). We report for the first time a
sub-DLA at $z_{\rm abs}=2.397$ in the quasar. From the ${O\textsc{i}}$, we
find four strong components in the system at 29, 0, -48, and -300 km s-1. The
total ${H\textsc{i}}$ column density of the system is log $N_{{\rm H}\,{\sc\rm
I}}=19.88\pm 0.09$ with $b=20$, 20, 20, (fixed) $28\pm 2.8$ km s-1 for 29, 0,
-48, and -300 km s-1 components respectively. The component at 0 km s-1 is
strongest and heavily dominates over other components. Metal absorption lines
from O i $\lambda$ 1302, Fe ii $\lambda\lambda\lambda\lambda\lambda$ 1144,
2344, 2374, 2382, 2586, and Si ii $\lambda\lambda\lambda$ 1190, 1193, 1260,
1304 associated with the sub-DLA are detected in the red part of the spectrum.
Fig. 17 shows the best fit result of the neutral hydrogen column density of
the sub-DLA.

Figure 20: The sub-DLA detected towards J223941.8-294955 at $z_{\rm
abs}=1.825$. The spectrum is smoothed with a boxcar average of 1.0 pixel for
plotting reasons. The solid red line corresponds to the Voigt profile fit to
the sub-DLA with an inferred column density of log $N_{{\rm H}\,{\sc\rm
I}}=19.84\pm 0.14$. Emission is clearly seen in the trough of this absorber
which is likely to correspond to the Lyman-$\alpha$ emission from the sub-DLA
host.
Figure 21: The DLA detected towards QSO B2318-1107 at $z_{\rm abs}=1.629$. For
plotting purposes the spectrum is smoothed with a boxcar average of 0.5 pixel.
The solid red line corresponds to the Voigt profile fit to the DLA with an
inferred column density of log $N_{{\rm H}\,{\sc\rm I}}=20.52\pm 0.14$.

  14. 14.

QSO J1723+2243 ($z_{\rm em}=4.520$). A damped absorber has been previously
reported in this quasar at $z_{\rm abs}=3.697$ (Prochaska et al. 2007;
Guimarães et al. 2009). We observed a sub-DLA down to Ly$\gamma$ at $z_{\rm
abs}=4.155$ with H i column of log $N_{{\rm H}\,{\sc\rm I}}=19.23\pm 0.12$
with a fixed $b=20$ km s-1. The metal lines associated with this system are
either blended with other features or not covered by our data so that this
detection is based on the Lyman line only and is a little less secure than the
others. The detection of absorption lines from the Lyman series confirm the
presence of the sub-DLA. Fig. 18 shows our best fit result of H i lines.

Figure 22: The sub-DLA detected towards QSO B2342$+$3417 at $z_{\rm
abs}=2.940$. The solid red line corresponds to the Voigt profile fit to the
sub-DLA with an inferred column density of log $N_{{\rm H}\,{\sc\rm
I}}=20.18\pm 0.10$. The system is detected down to the Ly$\gamma$. The system
is fitted simultaneously with a high column density absorber at $z_{\rm
abs}=2.909$ (log $N_{{\rm H}\,{\sc\rm I}}=21.10\pm 0.10$) to determine the
column density precisely.

  15. 15.

LBQS 2114-4347 ($z_{\rm em}=2.040$). The quasar has been discovered as part of
the Large Bright Quasar Survey (LBQS; Morris et al. 1991). No absorber has
been previously reported in this quasar (Péroux et al. 2003b). We observed,
for the first time, a sub-DLA at $z_{\rm abs}=1.912$ with best fit column
density of log $N_{{\rm H}\,{\sc\rm I}}=19.50\pm 0.10$ and $b=31.7\pm 3.4$ km
s-1. Several metal absorption lines from O i $\lambda$ 1302, Fe ii
$\lambda\lambda\lambda\lambda\lambda\lambda$ 1144, 1608, 2344, 2374, 2382,
2586, Si ii $\lambda\lambda\lambda\lambda\lambda$ 1193, 1260, 1304, 1526,
1808, C ii $\lambda$ 1334, Al ii $\lambda$ 1670, Mg ii $\lambda\lambda$ 2796,
2803, Si iv $\lambda\lambda$ 1393, 1402, and C iv $\lambda\lambda$ 1548, 1550
at the redshift of the sub-DLA are covered in the red part of the spectrum.
Fig. 19 shows our best fit of H i column density.

  16. 16.

J223941.8-294955 ($z_{\rm em}=2.102$). This quasar was discovered during the
course of the 2dF quasar redshift survey. The absorber at $z_{abs}=1.825$ in
this quasar has been reported before by Cappetta et al. (2010) with a column
density of log $N_{{\rm H}\,{\sc\rm I}}=20.60$ (where H i fit was not shown).
We fit the H i of the absorber again and find that the absorber at $z_{\rm
abs}=1.825$ fits well with H i column density of log $N_{{\rm H}\,{\sc\rm
I}}=19.84\pm 0.14$ and $b=53.0\pm 4.7$ km s-1. Emission is clearly seen in the
trough of this absorber which is likely to correspond to the Lyman-$\alpha$
emission from the sub-DLA host. Several metal absorption lines from O i
$\lambda$ 1302, Fe ii $\lambda\lambda\lambda\lambda\lambda\lambda$ 1144, 1608,
2344, 2374, 2382, 2586, Si ii $\lambda\lambda\lambda\lambda\lambda$ 1193,
1260, 1304, 1526, 1808, C ii $\lambda$ 1334, Al ii $\lambda$ 1670, Mg ii
$\lambda\lambda$ 2796, 2803, Al iii $\lambda\lambda$ 1854, 1862, Si iv
$\lambda\lambda$ 1393, 1402, and C iv $\lambda\lambda$ 1548, 1550 associated
with sub-DLA are covered in the red part of the spectrum. Fig. 20 shows our
best fit result of neutral hydrogen column density fit.

  17. 17.

QSO B2318-1107 ($z_{\rm em}=2.960$). A DLA was previously known at $z_{\rm
abs}=1.989$ along the line-of-sight of the quasar (Noterdaeme et al. 2007; Fox
et al. 2009). We find a new DLA in the quasar at $z_{\rm abs}=1.629$ with
neutral hydrogen column of log $N_{{\rm H}\,{\sc\rm I}}=20.52\pm 0.14$ with
fixed $b=30.0$ km s-1. Several metal absorption lines from Fe ii
$\lambda\lambda\lambda\lambda\lambda$ 1608, 1611, 2344, 2374, 2382, Si ii
$\lambda\lambda\lambda\lambda$ 1193, 1260, 1304, 1526 C ii $\lambda$ 1334, Al
ii $\lambda$ 1670, Al iii $\lambda\lambda$ 1854, 1862, and Si iv
$\lambda\lambda$ 1393, 1402 associated with the DLA are covered in the red
part of the spectrum. Fig. 21 shows our best fit of the H i column to the DLA.

  18. 18.

QSO B2342+3417 ($z_{\rm em}=3.010$). A damped absorber with log $N_{{\rm
H}\,{\sc\rm I}}=21.10\pm 0.10$ was previously reported at $z_{\rm abs}=2.909$
in the quasar (Prochaska et al. 2003; Fox et al. 2009). A joint fit was
implemented by Prochaska et al. (2003) to fit the DLA together with the
neighboring sub-DLA, but the column density of the sub-DLA was not reported.
We measure log $N_{{\rm H}\,{\sc\rm I}}=20.18\pm 0.10$ down to Ly$\gamma$ at
$z_{\rm abs}=2.940$ with a fixed $b=20.0$ km s-1. The metal lines associated
with this system are not seen because of limited wavelength coverage in the
red part of the spectrum. Fig. 22 shows the best fit result of the H i lines.

###  3.3 DLAs/sub-DLAs towards EUADP quasars

Besides the 150 DLAs/sub-DLAs, we found another 47 damped absorbers (21 DLAs
and 26 sub-DLAs) in the literature along the lines-of-sight of our 250 EUADP
quasars, for which Ly$\alpha$ absorption lines are not covered by our data
either due to the limited wavelength coverage or non-overlapping settings.
These systems are however of interest to us because their metal lines might
still be included in our data and are helpful in further studies of the EUADP
sample. These 150 and 47 damped absorbers (with and without Ly$\alpha$ covered
by the EUADP dataset) make up a total of 197 DLAs/sub-DLAs along lines-of-
sight of the 250 EUADP quasars where 114 are DLAs and 83 are sub-DLAs. The
EUADP sample by design is biased towards DLAs and therefore we see less sub-
DLAs than DLAs in the sample. Indeed, in the redshift range 0.2 $<$ $z$ $<$
4.9, we expect twice as many sub-DLAs as DLAs based on the number density of
absorbers at a mean redshift of $z=2.4$ (see Péroux et al. 2005).

##  4 Global Properties of the EUADP sample

Figure 23: Distribution of quasar emission redshift of the EUADP sample (black
histogram). The red histogram shows the redshift distribution of DLAs/sub-DLAs
along the lines-of-sight of EUADP quasars. The red shaded area corresponds to
the distribution of the 150 damped absorbers with Ly$\alpha$ covered by our
EUADP sample.

The emission redshifts of the 250 EUADP sample quasars are initially obtained
from the Simbad catalogue and later double checked for the cases where
Ly$\alpha$ emission from the quasar is covered by our data. The Ly$\alpha$
emission for 5 quasars (i.e., QSO J0332-4455, QSO B0528-2505, QSO B0841+129,
QSO B1114-0822 and QSO J2346+1247) is not seen because of the presence of DLAs
belonging to the “proximate DLA” class with $z_{\rm abs}\approx z_{\rm em}$
(e.g., Møller et al. 1998; Ellison et al. 2011; Zafar et al. 2011). For the
emission redshifts of these 5 cases, we rely on the literature. The emission
redshifts of all the other objects in the EUADP sample have been compared with
measurements from the literature. For a few cases, emission redshifts provided
in the Simbad catalogue are not correct and the correct redshifts are obtained
from the literature. In our sample, there are 38 quasars with emission
redshifts below $z_{\rm em}<1.5$. For these cases we cannot see Ly$\alpha$
emission from the quasar because of the limited spectral coverage, therefore,
we relied mostly on the Simbad catalogue. However, other emission lines are
covered in the spectra, helping us to confirm the emission redshifts. The
emission redshifts of 250 quasars of EUADP sample ranges from $0.191\leq
z_{\rm em}\leq 6.311$. Their distribution is shown in Fig. 23 and is found to
peak at $z_{\rm em}\simeq 2.1$.

Figure 24: Histogram showing the number of DLAs and sub-DLAs along lines-of-
sight to the quasars in the EUADP sample. The shaded area represents the
column density distribution of damped absorbers for which the Ly$\alpha$ line
is covered by the EUADP data. The vertical dashed line is the dividing line
between the sub-DLAs and DLAs classes.

In Fig. 24, the column density distribution of DLAs and sub-DLAs is presented
(see Zafar et al. 2013 for complete list of DLAs and sub-DLAs H i column
densities). It is worth noting that in the EUADP sample, damped absorbers with
column densities up to log $N_{{\rm H}\,{\sc\rm I}}=21.85$ are seen, while
higher column densities have been recently reported (Guimarães et al. 2012;
Kulkarni et al. 2012; Noterdaeme et al. 2012a). As mentioned above in the
EUADP sample, the number of sub-DLAs is lower than the number of DLAs. Indeed,
a large fraction ($\sim$45%) of the quasars in the EUADP sample were observed
because of a known strong damped absorber along their line-of-sight. A
carefully selected subset of the EUADP will have to be built for the purpose
of statistical analysis of DLAs and sub-DLAs (Zafar et al. 2013).

##  5 Lines-of-sight of Interest

In the EUADP sample, a few lines-of-sight of quasars are rich and contain more
than one absorber. One interesting example is the line-of-sight of QSO
J0133$+$0400, containing six DLAs and sub-DLAs. In this line-of-sight two sub-
DLAs $z_{\rm abs}=3.995/3.999$ are separated by only $\Delta v=240$ km s-1.
Three more examples of rich lines-of-sight are: $i)$ QSO J0006-6208 with 3
DLAs and one sub-DLA, $ii)$ QSO J0407-4410 with 4 DLAs, where three DLAs have
log $N_{{\rm H}\,{\sc\rm I}}\gtrsim 21.0$, and $iv)$ QSO B0841$+$129
containing 3 DLAs (with log $N_{{\rm H}\,{\sc\rm I}}\gtrsim 21.0$) and one
sub-DLA. Such complex group or systems can be classified as multiple DLAs
(MDLAs; Lopez & Ellison 2003).

In addition, there are four quasar pairs in the EUADP sample: $i)$ QSO
J0008-2900 & QSO J0008-2901 separated by $1.3^{\prime}$. Two sub-DLAs at
$z=2.254$ and $z=2.491$ are seen along the lines of sight of QSO J0008-2900
and QSO J0008-2901 respectively. $ii)$ J030640.8-301032 & J030643.7-301107
separated by $\sim$0.85 arcmin and no absorber is seen along the line-of-sight
to the pair. $iii)$ QSO B0307-195A & B separated by $\sim$1 arcmin. A sub-DLA
(at $z=1.788$ with log $N_{{\rm H}\,{\sc\rm I}}=19.00\pm 0.10$) along the
line-of-sight of QSO B0307-195B is detected (D’Odorico et al. 2002), but is
not seen in its companion. $iv)$ QSO J1039-2719 & QSO B1038-2712 separated by
$17.9^{\prime}$. A sub-DLA (at $z=2.139$ with log $N_{{\rm H}\,{\sc\rm
I}}=19.90\pm 0.05$) along the line-of-sight of QSO J1039-2719 is detected
(D’Odorico et al. 2002), but no damped absorber is seen in its companion.

##  6 Conclusion

In this study, high-resolution spectra taken from the UVES Advanced Data
Products archive have been processed and combined to make a sample of 250
individual quasars spectra. The high-resolution spectra of these quasars allow
us to detect absorbers down to log $N_{{\rm H}\,{\sc\rm I}}=19.00$ cm-2.
Automated and visual searches for quasar absorbers have been undertaken
leading to a sample of 93 DLAs and 57 sub-DLAs. An extensive search in the
literature shows that 6 of these DLAs and 13 of these sub-DLAs have their H i
column densities measured for the first time, where 10 are new
identifications. These new damped absorbers are confirmed by detecting metal
lines associated with the absorber and/or lines from the higher members of the
Lyman series. The H i column densities of all these new absorbers are
determined by fitting a Voigt profile to the Ly$\alpha$ line together with the
lines from higher order of the Lyman series whenever covered. Our data contain
five proximate DLA cases and three quasar pairs. We found that a few lines-of-
sight of quasars are very rich, particularly the line-of-sight of QSO
J0133+0400 which contains six DLAs and sub-DLAs.

In an accompanying paper, (Zafar et al. 2013), we use a carefully selected
subset of this dataset to study the statistical properties of DLAs and sub-
DLAs, measure their column density distribution, and quantify the contribution
of sub-DLAs to the H i gas mass density. Further studies using specifically
designed subsets of the EUADP dataset will follow.

##  7 Acknowledgments

This work has been funded within the BINGO! (‘history of Baryons:
INtergalactic medium/Galaxies cO-evolution’) project by the Agence Nationale
de la Recherche (ANR) under the allocation ANR-08-BLAN-0316-01. We would like
to thank the ESO staff for making the UVES Advanced Data Products available to
the community. We are thankful to Stephan Frank, Jean-Michel Deharveng and
Bruno Milliard for helpful comments.

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Table 1: Properties of the EUADP quasar sample. The details of the sample are provided in the columns as the (1) Simbad quasar names, (2) right ascension (RA), (3) declination (Dec), (4) Simbad $V$-band magnitude of each quasar except when noted otherwise, (5) emission redshift of the quasars, (6) wavelength coverage of the spectra, (7), ESO program ID, (8) number of spectra used for co-adding, where spectra from BLUE, RED upper and lower arms are counted separately, and (9) total exposure time of each quasar. Quasar | RA | Dec | Mag. | $z_{\rm em}$ | Wavelength coverage | Prog. ID | No. | Texp
---|---|---|---|---|---|---|---|---
| 2000 | 2000 |  |  | Å |  | spec | sec
LBQS 2359-0216B | 00 01 50.00 | -01 59 40.00 | 18.00 | 2.810 | 3290-5760, 5835-8520, 8660-10420 | 66.A-0624(A), 073.B-0787(A) | 16 | 21,300
QSO J0003-2323 | 00 03 44.92 | -23 23 54.80 | 16.70 | 2.280 | 3050-5760, 5835-8520, 8660-10420 | 166.A-0106(A) | 36 | 43,200
QSO B0002-422 | 00 04 48.28 | -41 57 28.10 | 17.40 | 2.760 | 3050-5760, 5835-8520, 8660-10420 | 166.A-0106(A) | 84 | 97,421
QSO J0006-6208 | 00 06 51.61 | -62 08 03.70 | 18.29 | 4.455 | 4780-5750, 5830-6800 | 69.A-0613(A) | 4 | 7,200
QSO J0008-0958 | 00 08 15.33 | -09 58 54.45 | 18.85 | 1.950 | 3300-4510,5720-7518,7690-9450 | 076.A-0376(A) | 18 | 21,600
QSO J0008-2900 | 00 08 52.72 | -29 00 43.75 | 19.12† | 2.645 | 3300-4970,5730-10420 | 70.A-0031(A) , 075.A-0617(A) | 17 | 24,000
QSO J0008-2901 | 00 08 57.74 | -29 01 26.61 | 19.85† | 2.607 | 3300-4970,5730-10420 | 70.A-0031(A) , 075.A-0617(A) | 18 | 17,700
QSO B0008+006 | 00 11 30.56 | +00 55 50.71 | 18.50 | 2.309 | 3760-4980,6700-8510,8660-10420 | 267.B-5698(A) | 6 | 7,200
LBQS 0009-0138 | 00 12 10.89 | -01 22 07.76 | 18.10 | 1.998 | 3300-4510,4770-5755,5835-6805 | 078.A-0003(A) | 6 | 6,000
LBQS 0010-0012 | 00 13 06.15 | +00 04 31.90 | 19.43 | 2.145 | 3050-3870,4610-5560,5670-6650 | 68.A-0600(A) | 3 | 5,400
LBQS 0013-0029 | 00 16 02.41 | -00 12 25.08 | 17.00 | 2.087 | 3054-6800 | 66.A-0624(A) , 267.A-5714(A) | 66 | 88,200
LBQS 0018+0026 | 00 21 33.28 | +00 43 00.99 | 18.20 | 1.244 | 3320-4510,4620-5600,5675-6650 | 078.A-0003(A) | 3 | 3,000
QSO B0027-1836 | 00 30 23.63 | -18 19 56.00 | 17.90 | 2.550 | 3050-3870,4780-5755,5835-6800 | 073.A-0071(A) | 15 | 23,772
J004054.7-091526 | 00 40 54.66 | -09 15 26.92 | 24.55 | 4.976 | 6700-8515,8655-10420 | 072.B-0123(D) | 6 | 7,285
QSO J0041-4936 | 00 41 31.44 | -49 36 11.80 | 17.90 | 3.240 | 3290-4520,4620-5600,5675-6650 | 68.A-0362(A) | 3 | 3,600
QSO B0039-407 | 00 42 01.20 | -40 30 39.00 | 18.50 | 2.478 | 3290-4520,4620-5600,5675-6650 | 075.A-0158(A) | 15 | 16,500
QSO B0039-3354 | 00 42 16.45 | -33 37 54.50 | 17.74 | 2.480 | 3295-4520 | 072.A-0442(A) | 1 | 1,800
LBQS 0041-2638 | 00 43 42.80 | -26 22 11.00 | 17.79 | 3.053 | 3757-4980,6700-8520,8660-10420 | 70.A-0031(A) | 6 | 5,400
LBQS 0041-2707 | 00 43 51.81 | -26 51 28.00 | 17.83 | 2.786 | 3757-4980,6700-8520,8660-10420 | 70.A-0031(A) | 6 | 5,400
QSO B0042-2450 | 00 44 28.10 | -24 34 19.00 | 17.30 | 0.807 | 3300-4520,4620-5600,5675-6650 | 67.B-0373(A) | 6 | 1,800
QSO B0042-2656 | 00 44 52.26 | -26 40 09.12 | 19.00 | 3.358 | 3750-4980,6700-8520,8660-10420 | 70.A-0031(A) | 6 | 3,600
LBQS 0042-2930 | 00 45 08.54 | -29 14 32.59 | 17.92† | 2.388 | 3290-4510,4780-5750,5830-6800 | 072.A-0442(A) | 3 | 1,800
LBQS 0042-2657 | 00 45 19.60 | -26 40 51.00 | 18.72 | 2.898 | 3757-4980,6700-8520,8660-10420 | 70.A-0031(A) | 9 | 5,400
J004612.2-293110 | 00 46 12.25 | -29 31 10.17 | 19.89 | 1.675 | 3050-3870,4620-5600,5675-6650 | 077.B-0758(A) | 26 | 45,470
LBQS 0045-2606 | 00 48 12.59 | -25 50 04.80 | 18.08† | 1.242 | 3300-4520,4615-5595,5670-6650 | 67.B-0373(A) | 6 | 3,000
QSO B0045-260 | 00 48 16.84 | -25 47 44.20 | 18.60 | 0.486 | 3300-4520,4615-5595,5670-6650 | 67.B-0373(A) | 6 | 7,200
QSO B0046-2616 | 00 48 48.41 | -26 00 20.30 | 18.70 | 1.410 | 3300-4520,4615-5595,5670-6650 | 67.B-0373(A) | 6 | 7,200
LBQS 0047-2538 | 00 50 24.89 | -25 22 35.09 | 18.40 | 1.969 | 3290-4520,4615-5595,5670-6650 | 67.B-0373(A) | 9 | 5,400
LBQS 0048-2545 | 00 51 02.30 | -25 28 48.00 | 18.20 | 2.082 | 3295-4520,4615-5595,5670-6650 | 67.B-0373(A) | 12 | 7,200
QSO B0018-2608 | 00 51 09.10 | -25 52 15.00 | 18.20 | 2.249 | 3300-4520,4615-5595,5670-6650 | 67.B-0373(A) | 6 | 3,600
LBQS 0049-2535 | 00 52 11.10 | -25 18 59.00 | 19.20 | 1.528 | 3300-4520,4615-5595,5670-6650 | 67.B-0373(A) | 12 | 7,200
LBQS 0051-2605 | 00 54 19.78 | -25 49 01.20 | 18.04† | 0.624 | 3300-4520,4615-5595,5670-6650 | 67.B-0373(A) | 15 | 9,000
QSO B0055-26 | 00 57 58.00 | -26 43 14.90 | 17.47 | 3.662 | 3050-5755,5835-6810 | 65.O-0296(A) | 17 | 37,800
QSO B0058-292 | 01 01 04.60 | -28 58 00.90 | 18.70 | 3.093 | 3300-5750, 5830-8515,8650-10420 | 67.A-0146(A), 66.A-0624(A) | 29 | 41,222
LBQS 0059-2735 | 01 02 17.05 | -27 19 49.91 | 18.00† | 1.595 | 3100-5755,5830-8520,8660-10420 | 078.B-0433(A) | 24 | 22,800
QSO B0100+1300 | 01 03 11.27 | +13 16 17.74 | 16.57 | 2.686 | 3290-4525,6695-8520,8660-10420 | 074.A-0201(A) , 67.A-0022(A) | 7 | 12,600
QSO J0105-1846 | 01 05 16.82 | -18 46 41.90 | 18.30 | 3.037 | 3300-5595,5670-6650,6690-8515, | 67.A-0146(A) | 9 | 14,400
$\cdots$ |  |  |  |  | 8650-10420 |  |  |
QSO B0102-2931 | 01 05 17.95 | -29 15 11.41 | 19.90 | 2.220 | 3300-4515,5720-7520,7665-9460 | 075.A-0617(A) | 3 | 3,900
QSO B0103 -260 | 01 06 04.30 | -25 46 52.30 | 18.31 | 3.365 | 4165-5160,5220-6210 | 66.A-0133(A) | 16 | 24,800
QSO B0109-353 | 01 11 43.62 | -35 03 00.40 | 16.90 | 2.406 | 3055-5755,5835-8515,8650-10420 | 166.A-0106(A) | 39 | 46,800
QSO B0112-30 | 01 15 04.70 | -30 25 14.00 | $\cdots$ | 2.985 | 4778-5760,5835-6810 | 68.A-0600(A) | 6 | 13,500
QSO B0117+031 | 01 15 17.10 | -01 27 04.51 | 18.90 | 1.609 | 4165-5160,5230-6200 | 69.A-0613(A) | 2 | 3,600
QSO J0123-0058 | 01 23 03.23 | -00 58 18.90 | 18.76 | 1.550 | 4165-5160,5230-6200 | 078.A-0646(A) | 4 | 5,400
QSO J0124+0044 | 01 24 03.78 | +00 44 32.67 | 17.90 | 3.834 | 4165-6810 | 69.A-0613(A) | 10 | 15,600
QSO B0122-379 | 01 24 17.38 | -37 44 22.91 | 17.10 | 2.190 | 3050-5760,5835-8520,8660-10420 | 166.A-0106(A) | 39 | 46,800
QSO B0122-005 | 01 25 17.15 | -00 18 28.88 | 18.60 | 2.278 | 3300-4520,4620,5600,5675-6650 | 075.A-0158(A) | 12 | 13,200
QSO B0128-2150 | 01 31 05.50 | -21 34 46.80 | 15.57 | 1.900 | 3045-3868,4785-5755,5830-6810 | 072.A-0446(B) | 6 | 6,130
QSO B0130-403 | 01 33 01.93 | -40 06 28.00 | 17.40 | 3.023 | 3300-4520,4775-5755,5828-6801 | 70.B-0522(A) | 3 | 3,065
QSO J0133+0400 | 01 33 40.40 | +04 00 59.00 | 18.30 | 4.154 | 4180-5165,5230-6410, | 69.A-0613(A), 073.A-0071(A), | 5 | 9,100
$\cdots$ |  |  |  |  | 6700-8520,8660-10250 | 074.A-0306(A) |  |
QSO J0134+0051 | 01 34 05.77 | 00 51 09.35 | 18.37 | 1.522 | 3050-3870,4620-5600,5675-6650 | 074.A-0597(A) | 8 | 14,400
QSO B0135-42 | 01 37 24.41 | -42 24 16.80 | 18.46 | 3.970 | 4170-5165,5235-6210 | 69.A-0613(A) | 2 | 3,600
QSO J0138-0005 | 01 38 25.54 | -00 05 34.52 | 18.97 | 1.340 | 3050-3870,4620-5598,5675-6650 | 078.A-0646(A) | 9 | 15,600
QSO J0139-0824 | 01 39 01.40 | -08 24 44.08 | 18.65 | 3.016 | 3300-4520 | 074.A-0201(A) | 1 | 4,800
QSO J0143-3917 | 01 43 33.64 | -39 17 00.00 | 16.28 | 1.807 | 3050-5755,5830-8515,8655-10420 | 67.A-0280(A) | 33 | 39,600
QSO J0153+0009 | 01 53 18.19 | 00 09 11.39 | 17.80 | 0.837 | 3100-3870,4625-5600,5675-6650 | 078.A-0646(A) | 6 | 10,800
QSO J0153-4311 | 01 53 27.19 | -43 11 38.20 | 16.80 | 2.789 | 3100-5757,5835-8520,8650-10420 | 166.A-0106(A) | 53 | 63,900
QSO J0157-0048 | 01 57 33.88 | -00 48 24.49 | 17.88 | 1.545 | 3300-4515,4785-5757,5835-6810 | 078.A-0003(A) | 6 | 6,000
QSO B0201+113 | 02 03 46.66 | +11 34 45.41 | 19.50 | 3.610 | 3760-4980,6700-8515,8660-10420 | 68.A-0461(A) | 3 | 3,000
QSO J0209+0517 | 02 09 44.62 | +05 17 14.10 | 17.80 | 4.174 | 3300-4520,4775-5754,5830-6810 | 69.A-0613(A) | 3 | 3,600
J021741.8-370100 | 02 17 41.78 | -37 00 59.60 | 18.40 | 2.910 | 3300-4520 | 072.A-0442(A) | 2 | 7,200
QSO J0217+0144 | 02 17 48.95 | +01 44 49.70 | 18.33 | 1.715 | 4165-5160,5230-6210 | 078.A-0646(A) | 4 | 5,400
QSO B0216+0803 | 02 18 57.36 | +08 17 27.43 | 18.10 | 2.996 | 3065-4520,4775-5755,5835-8525, | 073.B-0787(A), 072.A-0346(A) | 30 | 37,200
$\cdots$ |  |  |  |  | 8665-10250 |  |  |
QSO B0227-369 | 02 29 28.47 | -36 43 56.78 | 19.00 | 2.115 | 3300-4520,4620-5600,5675-6650 | 076.A-0389(A) | 12 | 12,800
QSO B0237-2322 | 02 40 08.18 | -23 09 15.78 | 16.78† | 2.225 | 3050-5757,5835-8525,8660-10420 | 166.A-0106(A) | 78 | 91,149
QSO J0242+0049 | 02 42 21.88 | +00 49 12.67 | 18.44 | 2.071 | 3300-4985,5715-7520,7665-9460 | 075.B-0190(A) | 12 | 20,700
Table 1: continued. Quasar | RA | Dec | Mag. | $z_{\rm em}$ | Wavelength coverage | Prog. ID | No. | Texp
---|---|---|---|---|---|---|---|---
| 2000 | 2000 |  |  | Å |  | spec | sec
QSO J0243-0550 | 02 43 12.47 | -05 50 55.30 | 19.00 | 1.805 | 3300-4518,4620-5600,5675-6650 | 076.A-0389(A) | 9 | 6,180
QSO B0241-01 | 02 44 01.84 | -01 34 03.70 | 17.06⋆ | 4.053 | 4165-6810 | 69.A-0613(A), 074.A-0306(A) | 4 | 5400
QSO B0244-1249 | 02 46 58.47 | -12 36 30.80 | 18.40 | 2.201 | 3290-4520,4625-5600,5675-6650 | 076.A-0389(A) | 6 | 6,000
QSO B0253+0058 | 02 56 07.26 | +01 10 38.62 | 18.88 | 1.346 | 3300-4515,4620-5600,5675-6650 | 074.A-0597(A) | 9 | 16,200
QSO B0254-404 | 02 56 34.03 | -40 13 00.30 | 17.40 | 2.280 | 3292-4520 | 072.A-0442(A) | 1 | 1,800
QSO J0300+0048 | 03 00 00.57 | +00 48 28.00 | 19.48 | 0.314 | 3100-5755 | 267.B-5698(A) | 9 | 16,492
J030640.8-301032 | 03 06 40.93 | -30 10 31.91 | 19.32† | 2.096 | 3050-5600,5670-6650,6700-8525, | 70.A-0031(A) | 12 | 8,558
$\cdots$ |  |  |  |  | 8665-10420 |  |  |
J030643.7-301107 | 03 06 43.77 | -30 11 07.58 | 19.85† | 2.130 | 3060-5595,5675-6650,6700-8520, | 70.A-0031(A) | 15 | 12,600
$\cdots$ |  |  |  |  | 8665-10420 |  |  |
QSO B0307-195A | 03 10 06.00 | -19 21 25.00 | 18.60 | 2.144 | 3050-5758,5835-8525,8660-10420 | 69.A-0204(A), 68.A-0216(A), | 18 | 28,450
$\cdots$ |  |  |  |  |  | 65.O-0299(A) |  |
QSO B0307-195B | 03 10 09.00 | -19 22 08.00 | 19.10 | 2.122 | 3065-5758,5835-8520,8660-10420 | 69.A-0204(A), 68.A-0216(A), | 27 | 37,700
$\cdots$ |  |  |  |  | 65.O-0299(A) |  |  |
J031856.6-060038 | 03 18 56.63 | -06 00 37.75 | 19.31 | 1.927 | 3100-5760,5835-8525,8665-10250 | 078.B-0433(A) | 24 | 22,800
QSO B0329-385 | 03 31 06.41 | -38 24 04.60 | 17.20 | 2.423 | 3060-5758,5835-8520,8655-10420 | 166.A-0106(A) | 36 | 31,200
QSO B0329-2534 | 03 31 08.92 | -25 24 43.27 | 17.10 | 2.736 | 3100-5763,5830-8525,8665-10420 | 166.A-0106(A) | 66 | 77,363
QSO J0332-4455 | 03 32 44.10 | -44 55 57.40 | 17.90 | 2.679 | 3300-4515,4780-5760,5840-6810 | 078.A-0164(A) | 12 | 12,000
QSO B0335-122 | 03 37 55.43 | -12 04 04.67 | 20.11 | 3.442 | 3755-4980,6700-8520,8660-10420 | 71.A-0067(A) | 11 | 16,200
QSO J0338+0021 | 03 38 29.31 | +00 21 56.30 | 18.79⋆ | 5.020 | 6700-8525,8660-10420 | 072.B-0123(D) | 6 | 10,450
QSO J0338-0005 | 03 38 54.78 | -00 05 20.99 | 18.90 | 3.049 | 3100-3870 | 074.A-0201(A) | 1 | 4,600
QSO B0336-017 | 03 39 00.90 | -01 33 18.00 | 19.10 | 3.197 | 3757-4983,6700-8520,8660-10420 | 68.A-0461(A) | 9 | 15,600
QSO B0347-383 | 03 49 43.68 | -38 10 31.10 | 17.30 | 3.222 | 3300-5757,5835-8520,8660-10420 | 68.B-0115(A) | 18 | 28,800
QSO B0347-2111 | 03 49 57.83 | -21 02 47.74 | 21.10 | 2.944 | 3300-4520,4775-5755,5832-6810 | 71.A-0067(A) | 9 | 8,873
J035320.2-231418 | 03 53 20.10 | -23 14 17.80 | 17.00 | 1.911 | 3300-4515,4620-5600,5675-6650 | 078.A-0068(A) | 3 | 1,120
QSO J0354-2724 | 03 54 05.56 | -27 24 21.00 | 17.90 | 2.823 | 3300-4515,4780-5760,5835-6810 | 078.A-0003(A) | 12 | 10,240
J040114.0-395132 | 04 01 14.06 | -39 51 32.70 | 17.00 | 1.507 | 3300-4515,4620-5600,5675-6650 | 078.A-0068(A) | 3 | 2,160
QSO J0403-1703 | 04 03 56.60 | -17 03 23.00 | 18.70 | 4.227 | 4780-5757,5832-8525,8660-10420 | 074.A-0306(A) | 10 | 12,625
QSO J0407-4410 | 04 07 18.08 | -44 10 14.10 | 17.60 | 3.020 | 3300-8520,8665-10420 | 68.A-0600(A), 70.A-0017(A), | 54 | 94,000
$\cdots$ |  |  |  |  |  | 68.A-0361(A) |  |
QSO J0422-3844 | 04 22 14.79 | -38 44 52.90 | 16.90 | 3.123 | 3300-5600,5675-6650,6700-8515, | 166.A-0106(A) | 49 | 57,750
$\cdots$ |  |  |  |  | 8660-10420 |  |  |
QSO J0427-1302 | 04 27 07.30 | -13 02 53.64 | 17.50 | 2.166 | 3285-4515,4780-5760,5835-6810 | 078.A-0003(A) | 6 | 6,000
QSO J0430-4855 | 04 30 37.31 | -48 55 23.70 | 16.20† | 1.940 | 3060-5765,5845-8530,8665-10420 | 66.A-0221(A) | 27 | 29,559
QSO B0432-440 | 04 34 03.23 | -43 55 47.80 | 19.60 | 2.649 | 3300-4520,4780-5755,5830-6810 | 71.A-0067(A) | 12 | 14,300
QSO B0438-43 | 04 40 17.17 | -43 33 08.62 | 19.50 | 2.852 | 3100-5757,5835-8515,8660,10420 | 072.A-0346(A) , 69.A-0051(A) | 17 | 22,425
QSO J0441-4313 | 04 41 17.32 | -43 13 45.40 | 16.40 | 0.593 | 3757-5758,5835-8515,8665-10420 | 70.C-0007(A) | 18 | 20,742
QSO B0449-1645 | 04 52 13.60 | -16 40 12.00 | 17.00 | 2.679 | 3285-4515,4620-5600,5675-6650 | 078.A-0646(A) | 9 | 15,600
QSO B0450-1310B | 04 53 12.80 | -13 05 46.00 | 16.50 | 2.250 | 3060-3874,4780-5760,5835-8525, | 70.B-0258(A) | 15 | 15,000
$\cdots$ |  |  |  |  | 8670-10420 |  |  |
QSO J0455-4216 | 04 55 23.05 | -42 16 17.40 | 17.30 | 2.661 | 3055-5758,5835-8520,8660-10420 | 166.A-0106(A) | 51 | 61,994
PKS 0454-220 | 04 56 08.93 | -21 59 09.54 | 16.10 | 0.534 | 3050-3870,4170-5162,5230-6210 | 076.A-0463(A) | 9 | 8,500
4C-02.19 | 05 01 12.81 | -01 59 14.26 | 18.40 | 2.286 | 3100-8520,8660-10250 | 074.B-0358(A), 66.A-0624(A), | 26 | 42,422
$\cdots$ |  |  |  |  |  | 076.A-0463(A) |  |
QSO B0512-3329 | 05 14 10.91 | -33 26 22.40 | 17.00 | 1.569 | 3300-4520,4620-5605,5675-6655 | 70.A-0446(A), 66.A-0087(A) | 30 | 30,000
QSO B0515-4414 | 05 17 07.63 | -44 10 55.50 | 14.90 | 1.713 | 3060-3875,4785-5760,5840-8525, | 66.A-0212(A) | 9 | 13,500
$\cdots$ |  |  |  |  | 8665-10420 |  |  |
J051939.8-364613 | 05 19 39.82 | -36 46 11.60 | 17.30 | 1.394 | 3290-4515,4620-5600,5675-6650 | 078.A-0068(A) | 3 | 1,520
QSO B0528-2505 | 05 30 07.96 | -25 03 29.84 | 17.30 | 2.765 | 3050-6810 | 68.A-0106(A), 66.A-0594(A), | 43 | 78,988
$\cdots$ |  |  |  |  |  | 68.A-0600(A) |  |
QSO J0530+13 | 05 30 56.42 | +13 31 55.15 | 20.00 | 2.070 | 3300-5160,5230-6210,6705-8529, | 70.C-0239(A) | 18 | 12,600
$\cdots$ |  |  |  |  | 8665-10420 |  |  |
QSO B0551-36 | 05 52 46.19 | -36 37 27.60 | 17.00 | 2.318 | 3060-5757,5835-6810 | 66.A-0624(A) | 17 | 26,100
J060008.1-504036 | 06 00 08.10 | -50 40 36.80 | 18.20† | 3.130 | 3300-4520,4620-5600,5675-6650 | 68.A-0639(A) | 20 | 24,000
QSO B0606-2219 | 06 08 59.69 | -22 20 20.96 | 20.00 | 1.926 | 3300-4515,4625-5600,5675-6650 | 076.A-0389(A) | 13 | 16,000
QSO B0642-5038 | 06 43 27.00 | -50 41 12.80 | 18.50 | 3.090 | 3300-4520,4785-5757,5835-6810 | 073.A-0071(A) | 9 | 17,500
QSO B0736+01 | 07 39 18.03 | +01 37 04.62 | 16.47 | 0.191 | 3300-5160,5230-6208,6715-8525, | 70.C-0239(A) | 26 | 17,600
$\cdots$ |  |  |  |  | 8665-10420 |  |  |
QSO B0810+2554 | 08 13 31.29 | +25 45 03.06 | 15.40† | 1.510 | 3050-3868,4625-5598,5675-6650 | 68.A-0107(A) | 12 | 14,100
QSO B0827+2421 | 08 30 52.08 | +24 10 59.82 | 17.30 | 0.939 | 3060-3872,4620-5600,5675-6650 | 68.A-0170(A), 69.A-0371(A) | 23 | 34,071
QSO B0841+129 | 08 44 24.20 | +12 45 48.90 | 18.50 | 2.505 | 3290-4520,6710-8525,8665-10420 | 70.B-0258(A) | 9 | 10,800
QSO B0908+0603 | 09 11 27.61 | +05 50 54.28 | 18.30† | 2.793 | 3300-4522,4620-5600,5675-6650 | 70.A-0439(A) | 39 | 46,800
QSO B0913+0715 | 09 16 13.94 | +07 02 24.30 | 17.10 | 2.785 | 3280-10420 | 078.A-0185(A) , 68.B-0115(A) | 62 | 77,523
QSO B0919-260 | 09 21 29.36 | -26 18 43.28 | 18.40 | 2.299 | 3300-4518,4618-5600,5675-6650 | 075.A-0158(A) | 12 | 13,200
QSO B0926-0201 | 09 29 13.57 | -02 14 46.40 | 16.44 | 1.661 | 3050-5757,5835-8525,8660-10420 | 072.A-0446(A) | 15 | 15,325
QSO B0933-333 | 09 35 09.23 | -33 32 37.69 | 20.00 | 2.910 | 3760-4984,6705-8525,8660-10420 | 71.A-0067(A), 69.A-0051(A) | 12 | 14,300
QSO B0951-0450 | 09 53 55.70 | -05 04 18.00 | 19.00 | 4.369 | 4785-5750,5832-6807 | 072.A-0558(A) | 8 | 30,960
QSO B0952+179 | 09 54 56.82 | +17 43 31.22 | 17.23 | 1.472 | 3060-3870,4618-5600,5675-6650 | 69.A-0371(A) | 9 | 17,100
QSO B0952-0115 | 09 55 00.10 | -01 30 07.00 | 18.70 | 4.426 | 3760-5754,5832-8525,8662-10420 | 70.A-0160(A), 072.A-0558(A) | 55 | 97,676
QSO B1005-333 | 10 07 31.39 | -33 33 06.72 | 18.00 | 1.837 | 3300-4518,4620-5600,5675-6650 | 075.A-0158(B) | 6 | 6,000
QSO J1009-0026 | 10 09 30.47 | -00 26 19.13 | 17.53 | 1.241 | 3300-4515,4620-5600,5675-6650 | 078.A-0003(A) | 6 | 6,000
LBQS 1026-0045B | 10 28 37.02 | -01 00 27.56 | 18.40 | 1.530 | 3300-4515,4620-5600,5675-6650 | 078.A-0003(A) | 12 | 10,240
Table 1: continued. Quasar | RA | Dec | Mag. | $z_{\rm em}$ | Wavelength coverage | Prog. ID | No. | Texp
---|---|---|---|---|---|---|---|---
| 2000 | 2000 |  |  | Å |  | spec | sec
QSO B1027+0540 | 10 30 27.10 | +05 24 55.00 | 18.87⋆ | 6.311 | 8000-10040 | 69.A-0529(A) | 6 | 33,400
Q1036-272 | 10 38 49.00 | -27 29 19.10 | 21.50 | 3.090 | 3757-4980,6700-8520,8660-10420 | 70.A-0017(A) | 9 | 12,133
QSO B1036-2257 | 10 39 09.52 | -23 13 26.20 | 18.00 | 3.130 | 3300-5758,5838-8525,8660-10420 | 68.B-0115(A) | 12 | 21,600
QSO J1039-2719 | 10 39 21.86 | -27 19 16.45 | 17.40 | 2.193 | 3290-5600,5675-6650,6705-8525, | 69.B-0108(A), 70.A-0017(A) | 30 | 36,500
$\cdots$ |  |  |  |  | 8665-10420 |  |  |
QSO B1038-2712 | 10 40 32.23 | -27 27 49.00 | 17.70 | 2.331 | 3045-3865,4780-5757,5835-6810 | 67.B-0398(A), 65.O-0063(B) | 9 | 16,200
QSO B1036-268 | 10 40 40.32 | -27 24 36.40 | 20.00 | 2.460 | 3285-5600,5675-6650,6700-8520, | 67.B-0398(A) | 15 | 27,000
$\cdots$ |  |  |  |  | 8660-10420 |  |  |
QSO J1044-0125 | 10 44 33.04 | -01 25 02.20 | 18.31⋆ | 5.740 | 8660-10420 | 268.A-5767(A), 69.A-0529(A) | 7 | 30,270
J104540.7-101813 | 10 45 40.56 | -10 18 12.80 | 17.40 | 1.261 | 3300-4515,4620-5600,5675-6650 | 078.A-0068(A) | 3 | 1,650
J104642.9+053107 | 10 46 42.84 | +05 31 07.02 | 18.00 | 2.682 | 3060-3870,4780-5755,5835-6810 | 074.A-0780(A) | 9 | 12,528
QSO B1044+059 | 10 46 56.71 | +05 41 50.32 | 18.30 | 1.226 | 3060-3870,4780-5757,5835-6810 | 074.A-0780(A) | 12 | 13,488
QSO B1044+056 | 10 47 33.16 | +05 24 54.88 | 17.99 | 1.306 | 3060-3870,4780-5757,5835-6810 | 074.A-0780(A) | 10 | 13,952
QSO B1045+056 | 10 48 00.40 | +05 22 09.76 | 20.30 | 1.230 | 3060-3870,4780-5757,5830-6810 | 074.A-0780(A) | 12 | 20,932
QSO B1052-0004 | 10 54 40.98 | -00 20 48.47 | 18.51 | 1.021 | 3300-4515,4620-5600,5675-6650 | 078.A-0003(A) | 12 | 10,240
QSO B1055-301 | 10 58 00.43 | -30 24 55.03 | 19.50 | 2.523 | 3300-4520,4780-5757,5840-6810 | 71.A-0067(A) | 9 | 10,725
QSO B1101-26 | 11 03 25.31 | -26 45 15.88 | 16.00 | 2.145 | 3780-4985,6710-8525,8665-10250 | 076.A-0463(A) | 27 | 60,672
QSO B1104-181 | 11 06 33.39 | -18 21 23.80 | 15.90 | 2.319 | 3060-8520,8655-10420 | 67.A-0278(A) | 51 | 60,948
QSO J1107+0048 | 11 07 29.03 | +00 48 11.27 | 17.66 | 1.392 | 3300-4515,4620-5600,5675-6650 | 074.A-0597(A) | 6 | 7,200
QSO B1108-07 | 11 11 13.60 | -08 04 02.00 | 18.10 | 3.922 | 3760-8520,8660-10420 | 67.A-0022(A), 68.B-0115(A), | 14 | 28,498
$\cdots$ |  |  |  |  |  | 68.A-0492(A) |  |
QSO J1113-1533 | 11 13 50.61 | -15 33 33.90 | 18.70 | 3.370 | 3760-5600,5675-6650 | 68.A-0492(A) | 10 | 25,200
QSO B1114-220 | 11 16 54.50 | -22 16 52.00 | 20.20 | 2.282 | 3300-4520,4620-5600,5675-6650 | 71.B-0081(A) | 30 | 14,115
QSO B1114-0822 | 11 17 27.10 | -08 38 58.00 | 19.40 | 4.495 | 4780-5757,5835-8520,8665-10250 | 074.A-0801(B) | 9 | 28,525
QSO B1122-168 | 11 24 42.87 | -17 05 17.50 | 16.50 | 2.400 | 3290-4520,4620-5600,5675-6650 | 68.A-0570(A), 073.B-0420(A) | 82 | 104,493
J112910.9-231628 | 11 29 10.86 | -23 16 28.17 | 17.30 | 1.019 | 3300-4520,4620-5600,5675-6650 | 078.A-0068(A) | 3 | 1,470
QSO J1142+2654 | 11 42 54.26 | +26 54 57.50 | 17.00 | 2.630 | 3757-4980,6705-8520,8660-10420 | 69.A-0246(A) | 42 | 48,696
QSO B1145-676 | 11 47 32.40 | -67 53 42.70 | 18.50† | 0.210 | 3300-5160,5230-6210,6700-8525, | 70.C-0239(A) | 16 | 10,800
$\cdots$ |  |  |  |  | 8660-10420 |  |  |
QSO B1151+068 | 11 54 11.12 | +06 34 37.80 | 18.60 | 2.762 | 3060-5757,5835-8520,8660-10420 | 65.O-0158(A) | 18 | 21,600
J115538.6+053050 | 11 55 38.60 | +05 30 50.67 | 19.08 | 3.475 | 3300-5600,5675-7500,7665-9460 | 076.A-0376(A) | 11 | 14,400
QSO J1159+1337 | 11 59 06.52 | +13 37 37.70 | 18.50 | 3.984 | 4780-5757,5835-6810 | 074.A-0306(B) | 2 | 3,000
QSO B1158-1842 | 12 00 44.94 | -18 59 44.50 | 16.90 | 2.453 | 3050-5757,5835-8520,8660-10420 | 166.A-0106(A) | 36 | 43,200
QSO B1202-074 | 12 05 23.12 | -07 42 32.40 | 17.50 | 4.695 | 3300-4520,4785-5765,5835-8525, | 71.B-0106(A), 66.A-0594(A), | 43 | 82,086
$\cdots$ |  |  |  |  | 8665-10420 | 166.A-0106(A) |  |
J120550.2+020131 | 12 05 50.19 | +02 01 31.55 | 17.46 | 2.134 | 3290-4520,4780-5757,5840-6810 | 273.A-5020(A) | 3 | 3,000
QSO B1209+0919 | 12 11 34.95 | +09 02 20.94 | 18.50 | 3.292 | 3300-8515,8650,10420 | 073.B-0787(A), 67.A-0146(A) | 15 | 23,765
LBQS 1209+1046 | 12 11 40.59 | +10 30 02.03 | 17.80 | 2.193 | 3290-4520,4620-5600,5675-6650 | 68.A-0170(A) | 12 | 14,400
LBQS 1210+1731 | 12 13 03.03 | +17 14 23.20 | 17.40 | 2.543 | 3060-3875,6705-8525,8665-10420 | 70.B-0258(A) | 21 | 30,500
QSO J1215+3309 | 12 15 09.22 | +33 09 55.23 | 16.50 | 0.616 | 3300-4520,4620-5600,5675-6650 | 69.A-0371(A) | 12 | 18,468
QSO B1220-1800 | 12 23 10.62 | -18 16 42.40 | 18.10 | 2.160 | 3280-4520,4620-5600,5675-6650 | 273.A-5020(A) | 3 | 3,000
LBQS 1223+1753 | 12 26 07.20 | +17 36 49.90 | 18.10 | 2.940 | 3300-5600,5675-6650,6700-8520, | 69.B-0108(A), 65.O-0158(A) | 14 | 18,000
$\cdots$ |  |  |  |  | 8660-10420 |  |  |
QSO B1228-113 | 12 30 55.54 | -11 39 09.62 | 22.01† | 3.528 | 3300-4520,4780-5760,5835-6810 | 71.A-0067(A) | 14 | 17,875
QSO B1230-101 | 12 33 13.16 | -10 25 18.44 | 19.80 | 2.394 | 3300-4515,4620-5600,5675-6650 | 075.A-0158(A) | 12 | 12,000
LBQS 1232+0815 | 12 34 37.55 | +07 58 40.50 | 18.40 | 2.570 | 3285-4520,4620-5600,5675-6650 | 68.A-0106(A), 69.A-0061(A), | 36 | 59,400
LBQS 1242+0006 | 12 45 24.60 | -00 09 38.01 | 17.70 | 2.084 | 3290-4520,4620-5600,5675-6650 | 273.A-5020(A) | 3 | 3,000
QSO J1246-0730 | 12 46 04.24 | -07 30 46.61 | 18.00 | 1.286 | 3050-3870,4780-5758,5835-6810 | 69.A-0410(A) | 12 | 12,000
LBQS 1246-0217 | 12 49 24.87 | -02 33 39.76 | 18.10 | 2.117 | 3285-4520,4620-7500,7665-9460 | 076.A-0376(A), 67.A-0146(A) | 21 | 27,000
J124957.2-015929 | 12 49 57.24 | -01 59 28.76 | 18.58 | 3.635 | 3300-4515,4775-5757,5835-6810 | 075.A-0464(A) | 33 | 33,650
QSO B1249-02 | 12 51 51.39 | -02 23 33.60 | 17.10 | 1.192 | 3300-4520,4620-5600,5675-6650 | 078.A-0068(A) | 3 | 1,218
QSO B1256-177 | 12 58 38.29 | -18 00 03.18 | 20.20 | 1.956 | 3290-4520,4620-5600,5675-6650 | 075.A-0158(A) | 12 | 12,000
QSO J1306+0356 | 13 06 08.26 | +03 56 26.30 | 18.77⋆ | 5.999 | 6700-10420 | 69.A-0529(A), 077.A-0713(A) | 8 | 38,131
QSO B1317-0507 | 13 20 29.98 | -05 23 35.50 | 16.54 | 3.710 | 3300-4520,4775-5757,5835-6810 | 075.A-0464(A) | 23 | 24,040
QSO B1318-263 | 13 21 14.06 | -26 36 11.19 | 20.40† | 2.027 | 3300-4520,4620-5600,5675-6650 | 075.A-0158(A) | 20 | 23,100
LBQS 1320-0006 | 13 23 23.79 | -00 21 55.24 | 18.20 | 1.388 | 3300-4520,4620-5600,5675-6650 | 274.A-5030(A) | 15 | 13,841
QSO B1324-047 | 13 26 54.61 | -05 00 58.98 | 19.00 | 1.882 | 3290-4520,4620-5600,5675-6650 | 075.A-0158(A) | 17 | 19,800
QSO J1330-2522 | 13 30 51.98 | -25 22 18.80 | 18.46 | 3.910 | 3300-4515,4780-5757,5835-6810 | 077.A-0166(A) | 3 | 5,400
QSO B1331+170 | 13 33 35.78 | +16 49 03.94 | 16.71 | 2.084 | 3060-4520,4620-5600,5675-5660, | 67.A-0022(A), 68.A-0170(A) | 15 | 20,700
$\cdots$ |  |  |  |  | 6692-8515,8650-10420 |  |  |
QSO J1342-1355 | 13 42 58.86 | -13 55 59.78 | 19.20 | 3.212 | 3300-5600,5675-6650 | 68.A-0492(A) | 10 | 25,100
QSO J1344-1035 | 13 44 27.07 | -10 35 41.90 | 17.10 | 2.134 | 3050-5760,5835-8520,8660-10420 | 166.A-0106(A) | 51 | 58,933
QSO B1347-2457 | 13 50 38.88 | -25 12 16.80 | 16.30 | 2.578 | 3050-5765,5835-8525,8660-10420 | 166.A-0106(A) | 30 | 35,444
QSO J1356-1101 | 13 56 46.83 | -11 01 29.22 | 19.20 | 3.006 | 3757-4985,6700-8520,8660-10420 | 71.A-0067(A), 71.A-0539(A), | 18 | 13,725
$\cdots$ |  |  |  |  |  | 69.A-0051(A) |  |
QSO B1402-012 | 14 04 45.89 | -01 30 21.84 | 18.38 | 2.522 | 3757-4985,5710-7518,7665-9460 | 075.A-0158(B) | 6 | 5,300
$\cdots$ |  |  |  |  |  | 71.B-0136(A) |  |
QSO B1409+0930 | 14 12 17.30 | +09 16 25.00 | 18.60 | 2.838 | 3050-5757,5830-8520,8665-10420 | 65.O-0158(A), 69.A-0051(A) | 44 | 51,950
QSO B1412-096 | 14 15 20.83 | -09 55 58.33 | 17.50 | 2.001 | 3300-4515,4620-5600,5675-6650 | 075.A-0158(B) | 3 | 3,300
QSO J1421-0643 | 14 21 07.76 | -06 43 56.30 | 18.50 | 3.689 | 3757-4980,6705-8520,8665-10420 | 71.A-0067(A), 71.A-0539(A) | 20 | 18,120
QSO B1424-41 | 14 27 56.30 | -42 06 19.55 | 17.70 | 1.522 | 3300-5160,5235-6210,6700-8520, | 67.C-0157(A) | 10 | 8,000
$\cdots$ |  |  |  |  | 8660-10420 |  |  |
QSO B1429-008B | 14 32 28.95 | -01 06 13.55 | 20.00⋆ | 2.082 | 3300-5600,5675-6650-6700-8525, | 69.A-0555(A) | 49 | 58,048
Table 1: continued.

Quasar | RA | Dec | Mag. | $z_{\rm em}$ | Wavelength coverage | Prog. ID | No. | Texp
---|---|---|---|---|---|---|---|---
| 2000 | 2000 |  |  | Å |  | spec | sec
$\cdots$ |  |  |  |  | 8660-10420 |  |  |
QSO J1439+1117 | 14 39 12.04 | +11 17 40.49 | 16.56⋆ | 2.583 | 3300-4515,4780-7105 | 278.A-5062(A) | 23 | 34,273
QSO J1443+2724 | 14 43 31.17 | +27 24 36.77 | 19.30 | 4.443 | 4780-5757,5835-7915,9900 | 077.A-0148(A), 072.A-0346(B) | 28 | 71,402
LBQS 1444+0126 | 14 46 53.04 | +01 13 56.00 | 18.50 | 2.210 | 3290-4530,4620-5600-5675-6650 | 67.A-0078(A), 69.B-0108(A), | 36 | 54,000
$\cdots$ |  |  |  |  |  | 65.O-0158(A) , 71.B-0136(A) |  |
QSO B1448-232 | 14 51 02.51 | -23 29 31.08 | 16.96 | 2.215 | 3050-8515,8660-10420 | 077.A-0646(A), 166.A-0106(A) | 60 | 66,532
J145147.1-151220 | 14 51 47.05 | -15 12 20.10 | 19.14 | 4.763 | 3755-5757,5835-8515,8655,10420 | 166.A-0106(A) | 31 | 48,400
QSO J1453+0029 | 14 53 33.01 | +00 29 43.56 | 21.46 | 1.297 | 4780-5755,5830-8550,8650-10420 | 267.B-5698(A) | 8 | 18,000
J151352.52+085555 | 15 13 52.53 | +08 55 55.74 | 15.57⋆ | 2.904 | 3300-4520,4620-5600,5675-6650 | 69.B-0108(A), 71.B-0136(A) | 15 | 15,514
QSO J1621-0042 | 16 21 16.92 | -00 42 50.90 | 17.23 | 3.700 | 3300-4515,4780-5757,5835-6810 | 075.A-0464(A) | 23 | 19,096
4C 12.59 | 16 31 45.16 | +11 56 03.01 | 18.50 | 1.792 | 3060-3870,4780-5757,5835-6810 | 69.A-0410(A) | 12 | 12,000
QSO J1723+2243 | 17 23 23.10 | +22 43 56.90 | 18.17 | 4.520 | 4780-5757,5835-6810 | 073.A-0071(A) | 2 | 4,500
QSO B1730-130 | 17 33 02.72 | -13 04 49.49 | 18.50 | 0.902 | 3300-5160,5230-6210,6695-8515, | 67.C-0157(A) | 10 | 9,600
$\cdots$ |  |  |  |  | 8655-10420 |  |  |
QSO B1741-038 | 17 43 58.86 | -03 50 04.62 | 18.50 | 1.054 | 3300-5160,5230-6210,6690-8515, | 67.C-0157(A) | 13 | 12,000
$\cdots$ |  |  |  |  | 8650-10420 |  |  |
QSO B1937-1009 | 19 39 57.25 | -10 02 41.54 | 19.00 | 3.787 | 4780-5760,5835-6810 | 077.A-0166(A) | 10 | 27,000
QSO B1935-692 | 19 40 25.51 | -69 07 56.93 | 18.80 | 3.152 | 4780-5757,5835-6810 | 65.O-0693(A) | 10 | 23,512
QSO B2000-330 | 20 03 24.12 | -32 51 45.03 | 18.40 | 3.783 | 3760-8535,8650-10420 | 166.A-0106(A), 65.O-0299(A) | 43 | 75,600
QSO J2107-0620 | 21 07 57.67 | -06 20 10.66 | 17.49 | 0.642 | 3757-4985 | 075.B-0190(A) | 3 | 5,400
LBQS 2113-4345 | 21 16 54.25 | -43 32 34.00 | 18.50 | 2.053 | 3050-7500,7660-9460 | 69.A-0586(A), 077.A-0714(A) | 17 | 10,536
LBQS 2114-4347 | 21 17 19.34 | -43 34 24.40 | 18.30 | 2.040 | 3050-10420 | 69.A-0586(A), 077.A-0714(A) | 29 | 22,325
J211739.5-433538 | 21 17 39.46 | -43 35 38.50 | 18.30† | 2.050 | 3050-5757,5835-8520,8660-10420 | 69.A-0586(A) | 14 | 10,300
QSO J2119-3536 | 21 19 27.60 | -35 37 40.60 | 17.00 | 2.341 | 3290-4530,4620-5600,5675-6650 | 65.O-0158(A) | 6 | 7,200
QSO B2126-15 | 21 29 12.17 | -15 38 41.17 | 17.30 | 3.268 | 3300-5600,5675-6650,6695-8520, | 166.A-0106(A) | 87 | 102,302
$\cdots$ |  |  |  |  | 8650-10420 |  |  |
QSO B2129-4653 | 21 33 02.10 | -46 40 28.80 | 18.90 | 2.230 | 3290-4515,4620-5600,5675-6650 | 074.A-0201(A) | 6 | 7,200
J213314.2-464031 | 21 33 14.17 | -46 40 31.80 | 19.96† | 2.208 | 3290-4520,4620-5600,5675-6650 | 073.A-0071(A) | 9 | 18,000
LBQS 2132-4321 | 21 36 06.04 | -43 08 18.10 | 17.68 | 2.420 | 3290-4530,4620-5600,5675-6650 | 65.O-0158(A) | 3 | 3,600
LBQS 2138-4427 | 21 41 59.79 | -44 13 25.90 | 18.20 | 3.170 | 3757-4983,6692-8515,8650-10420 | 67.A-0146(A) | 9 | 15,120
QSO B2139-4433 | 21 42 22.23 | -44 19 29.70 | 20.18 | 3.220 | 4778-5757,5835-6810 | 69.A-0204(A) | 8 | 21,600
QSO B2149-306 | 21 51 55.52 | -30 27 53.63 | 18.00 | 2.345 | 3300-4518,4620-5600,5675-6650 | 075.A-0158(B) | 6 | 5,200
QSO B2204-408 | 22 07 34.41 | -40 36 56.00 | 17.50 | 3.155 | 4778-5755,5835-6810 | 71.B-0106(B) | 6 | 9,900
LBQS 2206-1958A | 22 08 52.07 | -19 44 00.00 | 17.33 | 2.560 | 3060-8520,8665-10420 | 65.O-0158(A), 072.A-0346(A) | 27 | 33,900
QSO J2215-0045 | 22 15 11.94 | -00 45 50.01 | 17.40 | 1.476 | 3060-5757,5830-8515,8650-10420 | 267.B-5698(A) | 18 | 21,600
QSO J2220-2803 | 22 20 06.76 | -28 03 23.34 | 16.00 | 2.406 | 3060-8520,8655-10420 | 166.A-0106(A), 65.P-0183(A) | 60 | 72,000
QSO B2222-396 | 22 25 40.44 | -39 24 36.66 | 17.90 | 2.198 | 3290-4520 | 072.A-0442(A) | 1 | 1,800
QSO J2227-2243 | 22 27 56.94 | -22 43 02.60 | 17.60 | 1.891 | 3060-5757,5835-8515,8660-10420 | 67.A-0280(A) | 36 | 41,813
QSO B2225-4025 | 22 28 26.95 | -40 09 58.90 | 18.10 | 2.030 | 3300-4520 | 072.A-0442(A) | 1 | 1,800
LBQS 2230+0232 | 22 32 35.23 | +02 47 55.80 | 18.04 | 2.147 | 3060-3872,6705-8525,8665-10420 | 70.B-0258(A) | 9 | 13,500
J223851.0-295301 | 22 38 50.97 | -29 53 00.59 | 19.53† | 2.387 | 3080-5750,5830-8520,8660-10420 | 69.A-0586(A) | 14 | 12,180
J223922.9-294947 | 22 39 22.86 | -29 49 47.73 | 19.59† | 1.849 | 3060-5757,5835-6810 | 69.A-0586(A) | 11 | 10,708
J223938.9-295451 | 22 39 38.91 | -29 54 50.62 | 19.66† | 1.907 | 3080-7505,7670-9460 | 69.A-0586(A), 077.A-0714(A) | 28 | 29,190
J223941.8-294955 | 22 39 41.76 | -29 49 54.54 | 19.31† | 2.102 | 3060-7500,7670-9460 | 69.A-0586(A), 077.A-0714(A) | 22 | 21,626
J223948.7-294748 | 22 39 48.67 | -29 47 48.18 | 20.19† | 2.068 | 3060-10420 | 69.A-0586(A), 077.A-0714(A) | 33 | 31,590
J223951.9-294837 | 22 39 51.84 | -29 48 36.52 | 18.85† | 2.121 | 3070-5757,5835-6810 | 077.A-0714(A) | 11 | 8,450
QSO B2237-0607 | 22 39 53.66 | -05 52 19.90 | 18.30 | 4.558 | 4775-5753,5830-6810 | 69.A-0613(A) | 2 | 3,600
QSO J2247-1237 | 22 47 52.64 | -12 37 19.72 | 18.50 | 1.892 | 3300-4518,4620-5600,5675-6650 | 075.A-0158(B) | 9 | 7,200
QSO B2311-373 | 23 13 59.71 | -37 04 45.20 | 18.50 | 2.476 | 3290-4520,4780-5757,5835-6810 | 69.A-0051(A) | 9 | 10,725
J232046.7-294406 | 23 20 46.72 | -29 44 06.06 | 19.83† | 2.401 | 3050-5757,5835-8520,8660-10420 | 69.A-0586(A) | 12 | 6,050
J232059.4-295520 | 23 20 59.41 | -29 55 21.49 | 18.99† | 2.317 | 3060-5757,5835-8520,8660-10420 | 69.A-0586(A) | 12 | 6,050
J232114.3-294725 | 23 21 14.25 | -29 47 24.29 | 19.99† | 2.677 | 3758-4982,6700-8525,8665-10420 | 70.A-0031(A) | 6 | 4,800
J232121.2-294350 | 23 21 21.31 | -29 43 51.16 | 19.70† | 2.184 | 3060-5757,5835-8520,8660-10420 | 69.A-0586(A) | 12 | 9,155
QSO B2318-1107 | 23 21 28.80 | -10 51 21.20 | $\cdots$ | 2.960 | 3050-4515,4780-5760,5840-6810 | 072.A-0442(A), 073.A-0071(A) | 13 | 23,400
QSO J2328+0022 | 23 28 20.38 | +00 22 38.26 | 17.95 | 1.302 | 3300-4520,4620-5600,5675-6650 | 074.A-0597(A) | 9 | 15,900
QSO B2332-094 | 23 34 46.40 | -09 08 12.33 | 18.66 | 3.330 | 3757-5757,5835-8520,8660-10250 | 68.A-0600(A), 073.B-0787(A) | 25 | 31,920
J233544.2+150118 | 23 35 44.19 | +15 01 18.33 | 18.20 | 0.791 | 3060-3870,4620-5600,5675-6650 | 078.A-0646(A) | 12 | 17,920
QSO B2342+3417 | 23 44 51.26 | +34 33 48.74 | 19.10 | 3.010 | 3757-4985,6705-8525,8665-10420 | 71.A-0539(A) | 24 | 12,000
QSO J2346+1247 | 23 46 25.40 | +12 47 44.00 | $\cdots$ | 2.578 | 3300-4518,4620-5600,5675-6650 | 075.A-0018(A) | 42 | 70,240
QSO B2343+125 | 23 46 28.22 | +12 48 59.93 | 17.50 | 2.763 | 3060-3872,4780-5757,5835-8515, | 67.A-0022(A) | 19 | 25,200
$\cdots$ |  |  |  |  |  | 8650-10420 |  |
QSO B2345+000 | 23 48 25.37 | +00 20 40.11 | 19.3 | 2.654 | 3300-4518,4620-5600,5675-6650 | 076.A-0320(A) | 24 | 25,600
QSO B2347-4342 | 23 50 34.27 | -43 25 59.70 | 16.30 | 2.885 | 3070-5757,5835-8520,8655-10420 | 71.A-0066(A), 166.A-0106(A), | 71 | 125,443
$\cdots$ |  |  |  |  |  | 68.A-0230(A) |  |
QSO B2348-0180 | 23 50 57.89 | -00 52 10.01 | 19.50 | 3.023 | 3300-4520,4780-5755,5835-6810 | 072.A-0346(A) | 9 | 16,200
QSO B2348-147 | 23 51 29.81 | -14 27 56.90 | 16.90 | 2.933 | 3290-4520,6100-7928,8070-9760 | 70.B-0258(A) | 9 | 10,350
J235534.6-395355 | 23 55 34.61 | -39 53 55.30 | 16.30 | 1.579 | 3300-4515,4620-5600,5675-6650 | 078.A-0068(A) | 3 | 612
J235702.5-004824 | 23 57 02.55 | -00 48 24.00 | 19.53 | 3.013 | 3300-4986 | 075.B-0190(A) | 7 | 25,200
QSO J2359-1241 | 23 59 53.64 | -12 41 48.20 | 16.7 | 0.868 | 3050-5757,5835-8525,8665-10250 | 078.B-0433(A) | 24 | 22,800
Total | $\cdots$ | $\cdots$ | $\cdots$ | $\cdots$ | $\cdots$ | $\cdots$ | 4309 | 5,616,229

$\dagger$ $B$-band magnitude
$\star$ $J$-band magnitude