---
author:
- Tayyaba Zafar
- Attila Popping
- Céline Péroux
bibliography:
- 'dla.bib'
date: 'Received / Accepted '
title: 'The ESO UVES Advanced Data Products Quasar Sample - I. Dataset and New $N_{{H}\,{\sc I}}$ Measurements of Damped Absorbers'
---

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 @wolfe05). These systems are usually classified according to their neutral hydrogen column density as damped Ly$\alpha$ systems (hereafter DLAs) with $N_{{\rm H}\,{\sc \rm I}}\ge2\times10^{20}$ atoms cm$^{-2}$ [e.g., @storrie00; @wolfe05] and sub-damped Ly$\alpha$ systems (sub-DLAs) with $10^{19}\le N_{{\rm H}\,{\sc \rm I}}\le2\times10^{20}$ atoms cm$^{-2}$ [e.g., @peroux03b].

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, @croom01) and the Sloan Digital Sky Survey (SDSS; @prochaska05; @noterdaeme09; @noterdaeme12b). They have been shown to contain most of the neutral gas mass in the Universe [@lanzetta91; @lanzetta95; @wolfe95] and are currently used to measure the redshift evolution of the total amount of neutral gas mass density [@lanzetta91; @wolfe95; @storrie00; @peroux03; @prochaska05; @noterdaeme09; @noterdaeme12b]. 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, @pettini99; @pagel02; @wolfe03; @pettini04; @pettini06; @bouche05; @bouche06; @bouche07].

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 [@peroux03b]. 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., @peroux03b; @dessauges03; @ledoux03; @kulkarni07; @meiring08; @meiring09].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 [@dekker00] 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 [@zafar12b], 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.

The Quasar Sample
=================

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 UVES[^1] 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 18$^{\rm th}$ of February 2000) up to the 31$^{\rm st}$ 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.

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) database[^2], HyperLeda[^3], 2dF quasar redshift survey[^4], Simbad[^5] 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 $15.0''$. 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.

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 $R=\lambda/\Delta\lambda\sim41,400$ when a $1.0''$ 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 \[proptab\]. 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 [@lopez07]. In these cases we only analyzed the brightest objects. Our sample contains four quasar pairs: QSO J0008-2900 & QSO J0008-2901 (separated by $1.3'$), 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 $17.9'$). For these eight objects, eight different slit-positions were used.

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. \[conti\]). 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 @lanzetta91 and used an automated `Python` detection algorithm. This code builds an equivalent width spectrum over 400 pixel wide boxes ($\sim$12Å for 0.03$\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. $N_{{\rm H}\,{\sc \rm I}}\gtrsim10^{19}$ 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 [@dessauges03].

$N_{{\rm H}\,{\sc \rm I}}$ 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 \[dlamet\] and §\[notes\] 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]. Laboratory wavelengths and oscillator strengths from @morton2003 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 $\ion{O}{i}$. The other low ionization line components are used to fit $N_{{\rm H}\,{\sc \rm I}}$ for the cases where there is no $\ion{O}{i}$ covered by our data. Table \[dlamet\] 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 \[newNH\]. For most of the cases, we find consistent results with the low resolution studies. In the case of QSOB1114-0822, @storrie00 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 $N_{{\rm H}\,{\sc \rm I}}=20.02\pm0.12$.

  ------------------ -------------- --------------- -------------------------------- ------------ --------------------------------------------------------------------------------------------------------------------------- ------ --
  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               $20.22\pm0.10$           Ly$\beta$                 [O]{}[i]{}, [Fe]{}[ii]{}, [Si]{}[ii]{}, [C]{}[ii]{}, [Mg]{}[ii]{}, [Al]{}[iii]{}, [Si]{}[iv]{}                  no   
  QSO J0008-2901         2.607           2.491               $19.94\pm0.11$           Ly$\gamma$                        [O]{}[i]{}, [Fe]{}[ii]{}, [Si]{}[ii]{}, [C]{}[ii]{}, [Al]{}[ii]{}, [Si]{}[iv]{}                         no   
  QSO J0041-4936         3.240           2.248               $20.46\pm0.13$           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               $20.21\pm0.09$           Ly$\alpha$                              [O]{}[i]{}, [Fe]{}[ii]{}, [Si]{}[ii]{}, [C]{}[ii]{}, [Al]{}[iii]{}                                no   
  J021741.8-370100       2.910           2.429               $20.62\pm0.08$           Ly$\beta$                                                    [O]{}[i]{}, [Si]{}[ii]{}                                                     no   
  $\cdots$              $\cdots$         2.514               $20.46\pm0.09$           Ly$\beta$                                                   [Fe]{}[ii]{}, [Si]{}[ii]{}                                                    no   
  J060008.1-504036       3.130           2.149               $20.40\pm0.12$           Ly$\alpha$                       [O]{}[i]{}, [Fe]{}[ii]{}, [Si]{}[ii]{}, [C]{}[ii]{}, [Al]{}[ii]{}, [Al]{}[iii]{}                        yes   
  QSO B0952-0115         4.426           3.476               $20.04\pm0.07$           Ly$\alpha$                             [Fe]{}[ii]{}, [Si]{}[ii]{}, [Al]{}[ii]{}, [Al]{}[iii]{}, [C]{}[iv]{}                              yes   
  Q1036-272              3.090           2.792               $20.65\pm0.13$           Ly$\beta$                                      [O]{}[i]{}, [Fe]{}[ii]{}, [Si]{}[ii]{}, [Al]{}[iii]{}                                     yes   
  QSO B1036-2257         3.130           2.533               $19.30\pm0.10$           Ly$\alpha$                       [Fe]{}[ii]{}, [Si]{}[ii]{}, [C]{}[ii]{}, [Al]{}[iii]{}, [Si]{}[iv]{}, [C]{}[iv]{}                        no   
  QSO B1036-268          2.460           2.235               $19.96\pm0.09$           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               $19.48\pm0.13$           Ly$\alpha$                       [O]{}[i]{}, [Fe]{}[ii]{}, [Si]{}[ii]{}, [Al]{}[iii]{}, [Si]{}[iv]{}, [C]{}[iv]{}                        yes   
  QSO J1330-2522         3.910           2.654               $19.56\pm0.13$           Ly$\alpha$                             [Si]{}[ii]{}, [Al]{}[ii]{}, [Al]{}[iii]{}, [Si]{}[iv]{}, [C]{}[iv]{}                              yes   
  QSO J1356-1101         3.006           2.397               $19.88\pm0.09$           Ly$\alpha$                                            [O]{}[i]{}, [Fe]{}[ii]{}, [Si]{}[ii]{}                                             yes   
  QSO J1723+2243         4.520           4.155               $19.23\pm0.12$           Ly$\gamma$                                              metal lines blended or not covered                                               yes   
  LBQS 2114-4347         2.040           1.912               $19.50\pm0.10$           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               $19.84\pm0.14$           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               $20.52\pm0.14$           Ly$\alpha$                      [Fe]{}[ii]{}, [Si]{}[ii]{}, [C]{}[ii]{}, [Al]{}[ii]{}, [Al]{}[iii]{}, [Si]{}[iv]{}                       yes   
  QSO B2342+3417         3.010           2.940               $20.18\pm0.10$           Ly$\gamma$                                                limited red wavelength coverage                                                 no   
  ------------------ -------------- --------------- -------------------------------- ------------ --------------------------------------------------------------------------------------------------------------------------- ------ --

Notes on Individual Objects {#notes}
---------------------------

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.

  ------------------ --------------- -------------------------------- ------------ --------------------------------
  Quasar                                                                           
                      $z_{\rm abs}$   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               $20.20\pm0.09$              SDSS           $20.22\pm0.26$$^{1}$
  $\cdots$                4.740               $20.39\pm0.11$              SDSS           $20.55\pm0.15$$^{2}$
  QSO B1114-0822          4.258               $20.02\pm0.12$              WHT                 20.3$^{3}$
  J115538.6+053050        2.608               $20.37\pm0.11$              SDSS           $20.47\pm0.23$$^{1}$
  $\cdots$                3.327               $21.00\pm0.10$              SDSS           $20.91\pm0.27$$^{1}$
  LBQS 2132-4321          1.916               $20.74\pm0.09$              LBQS               20.70$^{3}$
  J235702.5-004824        2.479               $20.41\pm0.08$              SDSS               20.45$^{2}$
  ------------------ --------------- -------------------------------- ------------ --------------------------------

  : New high-resolution $N_{{\rm H}\,{\sc \rm I}}$ measurements of DLAs/sub-DLAs previously observed at low/medium resolution.[]{data-label="newNH"}

\(1) @noterdaeme09; (2) @prochaska08; (3)@storrie00

1.  QSO J0008-2900 ($z_{\rm em}=2.645$). The quasar was discovered during the course of the 2dF quasar redshift survey [@croom01]. An [H]{}[i]{} absorber at $z=2.253$ is reported by @tytler09. We find that the absorber is a sub-DLA with log $N_{{\rm H}\,{\sc \rm I}}=20.22\pm0.10$ and $b=28.5\pm2.2$ 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. \[J0008-2900\] shows our best fit result of the [H]{}[i]{} lines.

2.  QSO J0008-2901 ($z_{\rm em}=2.607$). The quasar was also discovered during the course of the 2dF quasar redshift survey [@croom01]. An [H]{}[i]{} absorber at $z=2.491$ is reported by @tytler09. We find that the absorber at $z_{\rm abs}=2.491$ is a sub-DLA with log $N_{{\rm H}\,{\sc \rm I}}=19.94\pm0.11$ and $b=39\pm3.5$ 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. \[J0008-2901\] shows our best fit result of the [H]{}[i]{} lines.

3.  QSO J0041-4936 ($z_{\rm em}=3.240$). A damped absorber is known in this quasar from the Calán Tololo survey [@maza95]. From a low-resolution spectrum, @lopez01 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 $N_{{\rm H}\,{\sc \rm I}}=20.46\pm0.13$ and $b=29\pm3.9$ 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. \[J0041-4936\] shows the best fit result of the [H]{}[i]{} lines.

4.  QSO B0128-2150 ($z_{\rm em}=1.900$). This quasar was discovered during the course of the Montréal-Cambridge-Tololo survey [@lamontagne00]. 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 $N_{{\rm H}\,{\sc \rm I}}=20.21\pm0.09$ and $b=25\pm2.6$ 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. \[B0128-2150\] shows our best fit result of the [H]{}[i]{} column density. The absorbing system at $z_{abs}=1.64$ is below sub-DLA limit.

    \

5.  J021741.8-370100 ($z_{\rm em}=2.910$). Damped absorbers have been known in this quasar from the Calán Tololo survey [@maza96]. The column densities for these DLAs have not been reported before. We measure log $N_{{\rm H}\,{\sc \rm I}}=20.62\pm0.08$ at $z_{\rm abs}=2.429$ and log $N_{{\rm H}\,{\sc \rm I}}=20.46\pm0.09$ 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. \[J021741.8-370100a\] and Fig. \[J021741.8-370100b\] show our best fit of [H]{}[i]{} lines for absorbers at $z_{\rm abs}=2.429$ and $z_{\rm abs}=2.514$ respectively.

    \

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6.  J060008.1-504036 ($z_{\rm em}=3.130$). This quasar was discovered during the course of the Calán Tololo survey [@maza96]. 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 $\ion{O}{i}$, resulting in a total column density of log $N_{{\rm H}\,{\sc \rm I}}=20.40\pm0.12$ 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. \[J060008.1-504036\] shows our best fit of the neutral hydrogen column density of the DLA at $z_{\rm abs}=2.149$.

    \

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7.  QSO B0952-0115 ($z_{\rm em}=4.426$). One damped absorber was previously reported in this quasar at $z_{\rm abs}=4.024$ [@storrie00; @prochaska07]. 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 $N_{{\rm H}\,{\sc \rm I}}=20.04\pm0.07$ and $b=32\pm3.9$ 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. \[B0952-0115\] shows the best fit result of the [H]{}[i]{} column density.

8.  Q1036-272 ($z_{\rm em}=3.090$). A low-resolution spectrum of this quasar has been previously published [@jakobsen92]. We report a DLA with $\ion{H}{i}$ column density of log $N_{{\rm H}\,{\sc \rm I}}=20.65\pm0.13$ and $b=35\pm5$ 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. \[Q1036-272\] shows best fit result of the [H]{}[i]{} lines at $z_{\rm abs}=2.792$.

    \

    \

9.  QSO B1036-2257 ($z_{\rm em}=3.130$). A damped and sub-damped absorber were previously reported in this quasar at $z_{\rm abs}=2.777$ [@fox09] and $z_{\rm abs}=2.531$ [@lopez01] respectively. A Lyman limit system at $z_{\rm LLS}=2.792$ is also detected. From a low-resolution spectrum, @lopez01 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 $N_{{\rm H}\,{\sc \rm I}}=19.30\pm0.10$ with $b$ parameter of $b=26\pm3.4$ 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. \[Q1036-2257\] shows the best fit result of the [H]{}[i]{} column density.

    \

    \

    \

10. QSO B1036-268 ($z_{\rm em}=2.460$). A low-resolution slit spectrum of the quasar has been previously published [@jakobsen92]. 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 $N_{{\rm H}\,{\sc \rm I}}=19.96\pm0.09$ and $b=20$, 20, 20 (fixed), and $35\pm3.0$ 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. \[B1036-268\] shows our best fit result of [H]{}[i]{} lines of the sub-DLA.

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 [@prochaska07; @ivanchik10]. We report for the first time a sub-DLA at $z_{\rm abs}=1.720$ with total log $N_{{\rm H}\,{\sc \rm I}}=19.48\pm0.13$. From $\ion{O}{i}$, we identified two main velocity components from the system at 0 and -78 km s$^{-1}$ (see Fig. \[met1232\]) 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. \[1232+0815\] 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. \[met1232\]).

    \

    \

12. QSO J1330-2522 ($z_{\rm em}=3.910$). Two sub-DLAs were previously reported at $z_{\rm abs}=2.910$ and 3.080 [@peroux01] 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 $N_{{\rm H}\,{\sc \rm I}}=19.56\pm0.13$ and $b=25.5\pm2.4$ km s$^{-1}$. Fig. \[J1330-2522\] 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. \[met1330\]. High ionization lines are blended with the lines from the other two sub-DLAs.

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 [@prochaska07; @noterdaeme08; @fox09]. We report for the first time a sub-DLA at $z_{\rm abs}=2.397$ in the quasar. From the $\ion{O}{i}$, we find four strong components in the system at 29, 0, -48, and -300 km s$^{-1}$. The total $\ion{H}{i}$ column density of the system is log $N_{{\rm H}\,{\sc \rm I}}=19.88\pm0.09$ with $b=20$, 20, 20, (fixed) $28\pm2.8$ 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. \[J1356-1101\] shows the best fit result of the neutral hydrogen column density of the sub-DLA.

    \

    \

14. QSO J1723+2243 ($z_{\rm em}=4.520$). A damped absorber has been previously reported in this quasar at $z_{\rm abs}=3.697$ [@prochaska07; @guimares09]. We observed a sub-DLA down to Ly$\gamma$ at $z_{\rm abs}=4.155$ with [H]{}[i]{} column of log $N_{{\rm H}\,{\sc \rm I}}=19.23\pm0.12$ 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. \[J1723+2243\] shows our best fit result of [H]{}[i]{} lines.

    \

15. LBQS 2114-4347 ($z_{\rm em}=2.040$). The quasar has been discovered as part of the Large Bright Quasar Survey (LBQS; @morris91). No absorber has been previously reported in this quasar [@peroux03]. We observed, for the first time, a sub-DLA at $z_{\rm abs}=1.912$ with best fit column density of log $N_{{\rm H}\,{\sc \rm I}}=19.50\pm0.10$ and $b=31.7\pm3.4$ 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. \[2114-4347\] shows our best fit of [H]{}[i]{} column density.

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 @cappetta10 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 $N_{{\rm H}\,{\sc \rm I}}=19.84\pm0.14$ and $b=53.0\pm4.7$ 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. \[J223941.8-294955\] shows our best fit result of neutral hydrogen column density fit.

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 [@noterdaeme07; @fox09]. We find a new DLA in the quasar at $z_{\rm abs}=1.629$ with neutral hydrogen column of log $N_{{\rm H}\,{\sc \rm I}}=20.52\pm0.14$ 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. \[B2318-1107\] shows our best fit of the [H]{}[i]{} column to the DLA.

18. QSO B2342+3417 ($z_{\rm em}=3.010$). A damped absorber with log $N_{{\rm H}\,{\sc \rm I}}=21.10\pm0.10$ was previously reported at $z_{\rm abs}=2.909$ in the quasar [@prochaska03b; @fox09]. A joint fit was implemented by @prochaska03b to fit the DLA together with the neighboring sub-DLA, but the column density of the sub-DLA was not reported. We measure log $N_{{\rm H}\,{\sc \rm I}}=20.18\pm0.10$ 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. \[B2342+3417\] shows the best fit result of the [H]{}[i]{} lines.

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 @peroux05].

Global Properties of the 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., QSOJ0332-4455, QSOB0528-2505, QSOB0841+129, QSOB1114-0822 and QSOJ2346+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., @moller98; @ellison11; @zafar11]. 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 $0.191\leq z_{\rm em}\leq6.311$. Their distribution is shown in Fig. \[zemhist\] and is found to peak at $z_{\rm em}\simeq2.1$.

\

In Fig. \[zabshist\], the column density distribution of DLAs and sub-DLAs is presented (see @zafar12b 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 [@guimaraes12; @kulkarni12; @noterdaeme12]. 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 [@zafar12b].

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 $N_{{\rm H}\,{\sc \rm I}}\gtrsim21.0$, and $iv)$ QSO B0841$+$129 containing 3 DLAs (with log $N_{{\rm H}\,{\sc \rm I}}\gtrsim21.0$) and one sub-DLA. Such complex group or systems can be classified as multiple DLAs (MDLAs; @lopez03).

In addition, there are four quasar pairs in the EUADP sample: $i)$ QSO J0008-2900 & QSO J0008-2901 separated by $1.3'$. 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 $N_{{\rm H}\,{\sc \rm I}}=19.00\pm0.10$) along the line-of-sight of QSO B0307-195B is detected [@odorico02], but is not seen in its companion. $iv)$ QSO J1039-2719 & QSO B1038-2712 separated by $17.9'$. A sub-DLA (at $z=2.139$ with log $N_{{\rm H}\,{\sc \rm I}}=19.90\pm0.05$) along the line-of-sight of QSO J1039-2719 is detected [@odorico02], but no damped absorber is seen in its companion.

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, [@zafar12b], 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.

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.

  ------------------ ------------- -------------- ----------------- -------------- ---------------------------------- ------------------------------- ------ ---------------
  Quasar                  RA            Dec             Mag.         $z_{\rm em}$         Wavelength coverage                    Prog. ID              No.    T$_{\rm exp}$
                         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)Ê     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)Ê            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)Ê            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)Ê            18       21,600
  QSO J0008-2900      00 08 52.72   -29 00 43.75   19.12$^\dagger$      2.645             3300-4970,5730-10420         70.A-0031(A)Ê, 075.A-0617(A)Ê    17       24,000
  QSO J0008-2901      00 08 57.74   -29 01 26.61   19.85$^\dagger$      2.607             3300-4970,5730-10420         70.A-0031(A)Ê, 075.A-0617(A)Ê    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)Ê            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)Ê            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)Ê, 267.A-5714(A)Ê    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)Ê            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)Ê            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)Ê            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)Ê            15       16,500
  QSO B0039-3354      00 42 16.45   -33 37 54.50        17.74           2.480                  3295-4520                      072.A-0442(A)Ê            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)Ê            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)Ê            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)Ê            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)Ê            6         3,600
  LBQS 0042-2930      00 45 08.54   -29 14 32.59   17.92$^\dagger$      2.388        3290-4510,4780-5750,5830-6800            072.A-0442(A)Ê            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)Ê            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)Ê            26       45,470
  LBQS 0045-2606      00 48 12.59   -25 50 04.80   18.08$^\dagger$      1.242        3300-4520,4615-5595,5670-6650             67.B-0373(A)Ê            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)Ê            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)Ê            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)Ê            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)Ê            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)Ê            12        7,200
  LBQS 0051-2605      00 54 19.78   -25 49 01.20   18.04$^\dagger$      0.624        3300-4520,4615-5595,5670-6650             67.B-0373(A)Ê            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)Ê            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)Ê     29       41,222
  LBQS 0059-2735      01 02 17.05   -27 19 49.91   18.00$^\dagger$      1.595        3100-5755,5830-8520,8660-10420           078.B-0433(A)Ê            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)Ê, 67.A-0022(A)Ê    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)Ê            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)Ê            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)Ê            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)Ê            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)Ê            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)Ê                 
  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)Ê            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)Ê            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)Ê            9        15,600
  QSO J0139-0824      01 39 01.40   -08 24 44.08        18.65           3.016                  3300-4520                      074.A-0201(A)Ê            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)Ê            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)Ê            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)Ê            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)Ê            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)Ê            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)Ê    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)Ê            12       12,800
  QSO B0237-2322      02 40 08.18   -23 09 15.78   16.78$^\dagger$      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)Ê            12       20,700
  ------------------ ------------- -------------- ----------------- -------------- ---------------------------------- ------------------------------- ------ ---------------

  ------------------ ------------- -------------- ----------------- -------------- -------------------------------- -------------------------------- ------ ---------------
  Quasar                  RA            Dec             Mag.         $z_{\rm em}$        Wavelength coverage                    Prog. ID              No.    T$_{\rm exp}$
                         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)Ê            9         6,180
  QSO B0241-01        02 44 01.84   -01 34 03.70    17.06$^\star$       4.053                 4165-6810               69.A-0613(A), 074.A-0306(A)      4Ê        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)Ê            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)Ê            9        16,200
  QSO B0254-404       02 56 34.03   -40 13 00.30        17.40           2.280                 3292-4520                      072.A-0442(A)Ê            1         1,800
  QSO J0300+0048      03 00 00.57   +00 48 28.00        19.48           0.314                 3100-5755                      267.B-5698(A)Ê            9        16,492
  J030640.8-301032    03 06 40.93   -30 10 31.91   19.32$^\dagger$      2.096       3050-5600,5670-6650,6700-8525,           70.A-0031(A)Ê             12        8,558
  $\cdots$                                                                                    8665-10420                                                    
  J030643.7-301107    03 06 43.77   -30 11 07.58   19.85$^\dagger$      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),Ê     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)Ê            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)Ê            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)Ê             11       16,200
  QSO J0338+0021      03 38 29.31   +00 21 56.30    18.79$^\star$       5.020            6700-8525,8660-10420                072.B-0123(D)Ê            6        10,450
  QSO J0338-0005      03 38 54.78   -00 05 20.99        18.90           3.049                 3100-3870                      074.A-0201(A)Ê            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)Ê             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)Ê             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)Ê            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),Ê     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)Ê            6         6,000
  QSO J0430-4855      04 30 37.31   -48 55 23.70   16.20$^\dagger$      1.940       3060-5765,5845-8530,8665-10420           66.A-0221(A)Ê             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)Ê             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)Ê, 69.A-0051(A)Ê     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)Ê            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)Ê             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)Ê            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), Ê    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)Ê      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)Ê             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)Ê            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)Ê                  
  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$^\dagger$      3.130       3300-4520,4620-5600,5675-6650            68.A-0639(A)Ê             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)Ê            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)Ê            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$^\dagger$      1.510       3050-3868,4625-5598,5675-6650            68.A-0107(A)Ê             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)Ê      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)Ê             9        10,800
  QSO B0908+0603      09 11 27.61   +05 50 54.28   18.30$^\dagger$      2.793       3300-4522,4620-5600,5675-6650            70.A-0439(A)Ê             39       46,800
  QSO B0913+0715      09 16 13.94   +07 02 24.30        17.10           2.785                 3280-10420             078.A-0185(A)Ê, 68.B-0115(A)Ê     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)Ê            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)Ê            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)Ê      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)Ê            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)Ê             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)Ê            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)Ê            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)Ê            12       10,240
  ------------------ ------------- -------------- ----------------- -------------- -------------------------------- -------------------------------- ------ ---------------

  ------------------ ------------- -------------- ----------------- -------------- -------------------------------- ------------------------------ ------ ---------------
  Quasar                  RA            Dec             Mag.         $z_{\rm em}$        Wavelength coverage                   Prog. ID             No.    T$_{\rm exp}$
                         2000           2000                                                      Å                                                 spec        sec
  QSO B1027+0540      10 30 27.10   +05 24 55.00    18.87$^\star$       6.311                 8000-10040                    69.A-0529(A)Ê            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)Ê            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)Ê            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)Ê     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)Ê     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$^\star$       5.740                 8660-10420             268.A-5767(A), 69.A-0529(A)Ê    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)Ê           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)Ê           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)Ê           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)Ê           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)Ê           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)Ê           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)Ê            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)Ê           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)Ê                 
  QSO J1113-1533      11 13 50.61   -15 33 33.90        18.70           3.370            3760-5600,5675-6650                68.A-0492(A)Ê            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)Ê            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)Ê    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)Ê           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$^\dagger$      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)Ê           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)Ê           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)Ê           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)Ê           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)Ê    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)Ê            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)Ê            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)Ê           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)Ê     14       18,000
  $\cdots$                                                                                    8660-10420                                                  
  QSO B1228-113       12 30 55.54   -11 39 09.62   22.01$^\dagger$      3.528       3300-4520,4780-5760,5835-6810           71.A-0067(A)Ê            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)Ê           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)Ê           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)Ê            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)Ê    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)Ê           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$^\star$       5.999                 6700-10420             69.A-0529(A), 077.A-0713(A)Ê    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)Ê           23       24,040
  QSO B1318-263       13 21 14.06   -26 36 11.19   20.40$^\dagger$      2.027       3300-4520,4620-5600,5675-6650           075.A-0158(A)Ê           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)Ê           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)Ê           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)Ê           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)Ê     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)Ê            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)Ê           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)Ê           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)Ê           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)Ê     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)Ê           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$^\star$       2.082       3300-5600,5675-6650-6700-8525,          69.A-0555(A)Ê            49       58,048
  ------------------ ------------- -------------- ----------------- -------------- -------------------------------- ------------------------------ ------ ---------------

  ------------------- ------------- -------------- ----------------- -------------- -------------------------------- ------------------------------- ------ ---------------
  Quasar                   RA            Dec             Mag.         $z_{\rm em}$        Wavelength coverage                   Prog. ID              No.    T$_{\rm exp}$
                          2000           2000                                                      Å                                                  spec        sec
  $\cdots$                                                                                     8660-10420                                                   
  QSO J1439+1117       14 39 12.04   +11 17 40.49    16.56$^\star$       2.583            3300-4515,4780-7105                278.A-5062(A)Ê            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)Ê    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), Ê    36       54,000
  $\cdots$                                                                                                             65.O-0158(A)Ê, 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)Ê    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)Ê            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)Ê            8        18,000
  J151352.52+085555    15 13 52.53   +08 55 55.74    15.57$^\star$       2.904       3300-4520,4620-5600,5675-6650     69.B-0108(A), 71.B-0136(A)Ê     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)Ê            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)Ê            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)Ê            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)Ê            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)Ê            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)Ê     43       75,600
  QSO J2107-0620       21 07 57.67   -06 20 10.66        17.49           0.642                 3757-4985                     075.B-0190(A)Ê            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$^\dagger$      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)Ê            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)Ê            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)Ê            6         7,200
  J213314.2-464031     21 33 14.17   -46 40 31.80   19.96$^\dagger$      2.208       3290-4520,4620-5600,5675-6650           073.A-0071(A)Ê            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)Ê            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)Ê            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)Ê            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)Ê            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)Ê     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)Ê            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)Ê     60       72,000
  QSO B2222-396        22 25 40.44   -39 24 36.66        17.90           2.198                 3290-4520                     072.A-0442(A)Ê            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)Ê            36       41,813
  QSO B2225-4025       22 28 26.95   -40 09 58.90        18.10           2.030                 3300-4520                     072.A-0442(A)Ê            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)Ê            9        13,500
  J223851.0-295301     22 38 50.97   -29 53 00.59   19.53$^\dagger$      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$^\dagger$      1.849            3060-5757,5835-6810                 69.A-0586(A)Ê            11       10,708
  J223938.9-295451     22 39 38.91   -29 54 50.62   19.66$^\dagger$      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$^\dagger$      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$^\dagger$      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$^\dagger$      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)Ê            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)Ê            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)Ê            9        10,725
  J232046.7-294406     23 20 46.72   -29 44 06.06   19.83$^\dagger$      2.401       3050-5757,5835-8520,8660-10420           69.A-0586(A)Ê            12        6,050
  J232059.4-295520     23 20 59.41   -29 55 21.49   18.99$^\dagger$      2.317       3060-5757,5835-8520,8660-10420           69.A-0586(A)Ê            12        6,050
  J232114.3-294725     23 21 14.25   -29 47 24.29   19.99$^\dagger$      2.677       3758-4982,6700-8525,8665-10420           70.A-0031(A)Ê            6         4,800
  J232121.2-294350     23 21 21.31   -29 43 51.16   19.70$^\dagger$      2.184       3060-5757,5835-8520,8660-10420           69.A-0586(A)Ê            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)Ê            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)Ê     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)Ê            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)Ê            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)Ê            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),Ê    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)Ê            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)Ê            24       22,800
  \[3pt\] Total         $\cdots$       $\cdots$        $\cdots$         $\cdots$                $\cdots$                        $\cdots$              4309     5,616,229
  ------------------- ------------- -------------- ----------------- -------------- -------------------------------- ------------------------------- ------ ---------------

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

[^1]: <http://archive.eso.org/eso/eso_archive_adp.html>

[^2]: <http://www.sdss.org/dr7/>

[^3]: <http://leda.univ-lyon1.fr/>

[^4]: <http://www.2dfquasar.org/Spec_Cat/2qzsearch2.html>

[^5]: <http://simbad.u-strasbg.fr/>
