% plain TeX
%-----------
\def\entitle#1#2{{In their paper entitled {\it #1} #2}}
\def\app#1{\noindent{\bf #1}\par\smallskip\noindent}
\def\MgII{{\rm Mg{\small II}}}
\def\OII{{\rm [O{\small II}]}}
\def\zgal{{${\rm z}_{\rm gal}$}}
\def\zabs{{${\rm z}_{\rm abs}$}}
\def\HII{{\rm H{\small II}}}
\def\CIV{{\rm C{\small IV}}}
\def\kpc{$h^{-1}${\rm kpc}}
\def\et{{\it et al.}}
\def\Boisse{Boiss\'e}
\def\TABLE{T{\small ABLE\ }}
\def\R{{${\cal R}$}}
\font\small=cmr8
\font\biga=cmbx10 scaled \magstep1
\font\bigb=cmbx10 scaled \magstep2


\noindent
Title in the Main Journal:

\medskip
\centerline{\biga Optically identified QSO absorption systems 
and galaxy evolution}
\smallskip
\centerline{Ulrich Lindner, Uta Fritze -- von Alvensleben, Klaus J. Fricke}
\smallskip
\centerline{\it Universit\"atssternwarte, Geismarlandstra\ss e 11, 
D--37083 G\"ottingen, Germany}  
\bigskip
\centerline{\bigb Appendix: \ Notes on individual publications}

\bigskip\medskip\noindent
In the following  we briefly comment 
on each paper from which we have compiled data.
Numbers of sub-subsections ( 1{\small )} ... 17{\small )} ) 
correspond to the identification number (id. no.) in 
Table~1 and Figures 2 -- 4 as well. 
In particular we discuss some points which are 
important to our purposes.


\bigskip\app{1) Lanzetta \& Bowen 1990 }
\entitle
{Intermediate redshift galaxy halos: Results from QSO absorption lines}
{K.M. Lanzetta and D. Bowen} 
list optically identified \MgII\ absorption systems in their 
TABLE~1 for the purpose to study correlations between equivalent 
widths of \MgII\ absorption lines and impact parameters.
We assume that TABLE~1 in this paper contains all data on 
optically identified (\MgII) absorption systems available 
up to this time and thus we take it as the starting point 
for our search for further data in the literature until now. 
All $m_r(z)$ data listed in TABLE~1 are reported also in later 
papers and we took them from these more topical sources.

\bigskip\app{2) Yanny \et\ 1990 }
\entitle
{Emission--line objects near QSO absorbers. 
 I. Narrow--band imaging and candidate list} 
{B. Yanny, D.G. York and T.B. Williams} 
report on a search for emission--line objects (predominantly 
from \OII) in the environment of 8 QSOs with 
previously known associated \MgII\ 
absorber systems using narrow--band imaging. Data for 37 objects 
are given but in 14 out of the 37 cases only lower limits for R 
magnitudes could be derived from the detection limit.

In a subsequent study (Yanny 1990)
8 of the 37 absorber candidates in 4 QSO fields have been 
investigated using long--slit spectroscopy confirming their 
incidence with the absorber redshifts 
($0.4 \le z_{\rm abs} \le 0.7$). It turns out that
all 8 spectroscopically studied objects are absorbers,
i.e. \zgal\ $=$ \zabs.

\bigskip\app{3) Bergeron \& \Boisse\ 1991}
\entitle
{A sample of galaxies giving rise to \MgII\ quasar absorption systems}
{J. Bergeron and P. \Boisse\ } 
present imaging and spectroscopic observations aimed at
detecting intervening galaxies responsible for low redshift
($z \sim 0.5$) \MgII\ absorption line systems in quasar spectra.
This paper represents a pioneering study on optical identifications 
of absorber systems confirming the intervening galaxy hypothesis. 
14 confirmed identifications, 4 candidates and 3 ``negative 
cases'', i.e. galaxies closest to the QSO line of sight but 
without any absorption system at galaxy redshift are presented. 
The authors give luminosities of galaxies as well as sizes and 
shapes of the absorbing regions.

We include the 14 spectroscopically confirmed absorber galaxies
and 4 candidates in Figure~2 and 4. The three ``negative cases''
from their Table~6 are included as ``candidates'' as well.

\bigskip\app{4) Bechtold \& Ellingson 1992}
\entitle
{\MgII\ absorption by previously known galaxies at $z \approx 0.5$}
{J. Bechtold and E. Ellingson} 
report on
an investigation of 9 QSO spectra using the Multiple Mirror 
Telescope to search for \MgII\ absorption from 
intervening galaxies. This is the reverse procedure:
galaxies and their redshifts ($0.2 \le z \le 0.7$) are 
known from previous studies of the QSO environment 
and now, the possible absorption systems are searched for.
These data are as useful to us as those from
studies aimed to find intervening galaxies near QSOs
with absorption line systems. 

It should be noted that a considerable fraction of the data comes 
from galaxies in high density environment, i.e. galaxy clusters.
This is reflected by the fact that many redshift values are close 
each other. In the cases where \zgal\ $\ne {\rm z}_{\rm QSO}$ is
not confirmed by spectroscopy a physical influence on the galaxies
from the quasar cannot be excluded.

In their \TABLE 4, the authors give r(z) data for 21 galaxies 
in the environment of 9 quasars. Photometric data are taken 
from Green \& Yee (1984), Yee, Green \& Stockman (1986), and 
unpublished images from Yee. Spectroscopy is from Ellingson, 
Green \& Yee (1991) and Ellingson \& Yee (1992). Only two \MgII\ 
absorption--line systems are identified with corresponding galaxy 
redshifts. Consequently most of the r(z) data from this paper
do not belong to optically identified QSO absorbers
and consequently they are not included to our compilation.

In \TABLE 5 of their paper the authors list previously 
known identified absorber galaxies (most from Bergeron 
\& \Boisse\ 1991) and some new candidates. The latter 
ones are included in our compilation.

\bigskip\app{5) Bergeron \et\ 1992}
\entitle
{Discovery of $z \sim 1$ galaxies causing quasar absorption lines}
{J. Bergeron, S. Christiani and P.A. Shaver}
report on the first identification of intervening galaxies
responsible for four \MgII\ absorption--line systems at 
redshifts of about 1 in two QSO fields. There are three candidates
in each field assumed to be responsible for the \MgII\ doublets 
in the QSO spectra. Five galaxy redshifts have been measured
showing incidence with three of the four absorption line redshifts.
Two galaxies are not at any absorber redshift and one galaxy
without measured redshift is assumed to be at the remaining
absorption redshift. The two confirmed non--absorbers are 
marked with open bold line symbols in Figure~2.

\bigskip\app{6) Nelson \& Malkan 1992 }
\entitle
{A photometric search for \OII\ lines in \MgII\ 
 quasar absorption systems}
{B.O. Nelson and M.A. Malkan} 
report on results obtained by narrow-- and broad--band photometry 
of 336 objects near the line of sight to 22 quasars showing \MgII\ 
absorption lines in their spectra. The attention is focused to \OII\ 
emission--line objects which are claimed to undergo enhanced star 
formation and these galaxies are searched for using narrow--band 
photometry. Gunn g magnitudes for 52 objects are given in their 
\TABLE~4. The corresponding absorber redshift can
be derived from their list of observed QSO fields in \TABLE~1.
Some quasars have not been imaged in the Gunn g bandpass but
e.g in ``Spinrad Red''. These data are not included and 
finally 43 g magnitudes remain in our compilation.

In 6 cases redshifts of identified galaxies had previously been 
measured spectroscopically by other authors (Bergeron \& \Boisse\ 
1991, Bergeron \et\  1988, Christiani 1987, Miller \et\  1987, see 
also references in \TABLE 4 of Nelson \& Malkan). 
In most other cases (without spectroscopy) more than
one candidate is given for each absorber redshift.
They are all included in our compilation. In five
cases we are able to adopt r magnitudes from the papers 
mentioned to derive (g-r) colors. These colors are used in Figure~3b.


\bigskip\app{7) Steidel \& Dickinson 1992}
\entitle
{The unusual field of the quasar 3C 336: Identification
 of three foreground \MgII\ absorbing galaxies}
{C.C. Steidel and M. Dickinson} 
present imaging and spectroscopic observations of the field 
of 3C 336 ($z_{\rm em} = 0.927$) which reveals at least 
3 \MgII\ absorption systems with $z_{\rm abs} < z_{\rm em}$.
Data for 6 galaxies with spectroscopically measured redshifts and 
\R\ ($\lambda = 6930$, $\Delta\lambda = 1500$), 
g ($\lambda = 4900$ and $\Delta\lambda = 700$) and
i ($\lambda = 8000$ and $\Delta\lambda = 1450$) AB magnitudes 
are given in their \TABLE~1. 
3 galaxies seem to be the absorbing galaxies. 3 further
objects with \zgal\ $\ne$ \zabs\ are marked with open
bold line symbols in Figure~2 and 4 as usual.

\noindent
\quad In this paper Steidel \& Dickinson give 
apparent AB--magnitudes \R$_{\rm AB}$ (6930/1500) 
together with $( g - $\R$ )_{\rm AB}$
and $( $\R$ - i )_{\rm AB}$ colors.
Because we restrict our comparison of observations with 
models to Thuan \& Gunn and Johnson bandpasses as discussed 
in \S 2.2 we cannot take the AB colors from Steidel \& 
Dickinson (1992) into consideration.

\bigskip\app{8) Steidel \& Hamilton 1992 }
\entitle
{Deep imaging of high redshift QSO fields below the Lyman limit. 
 I. The field of Q0000-263 and galaxies at $z = 3.4$}
{C.C. Steidel and D. Hamilton} 
present results for the first field completed in a new survey 
involving very deep imaging of the fields of high redshift
quasars with optically thick Lyman limit absorption systems.
In their \TABLE 1 the authors list $U_n$, 
G and \R\ magnitudes for 33 objects within 30'' of Q0000-263 
($z_{\rm em} = 4.106$). The moderately under--luminous galaxy 
at $z = 0.438$ was previously suggested to be at $z = 3.408$ 
(Turnshek \et\ 1991), but now Steidel \& Hamilton suggest 
that the line previously identified as Lyman $\alpha$ is 
probably \OII. The $z = 0.438$ and \R\ $=22.5$ galaxy
is added to our list and is an interesting case for a late
type absorber.
Another galaxy is assumed to be a candidate 
for the DLA system at $z = 3.39$.

\bigskip\app{9) Yanny \& York 1992}
\entitle
{Emission--line objects near Quasi--stellar object absorbers. 
 III.  Clustering and colors of moderate--redshift \HII\ regions}
{B. Yanny and D.G. York} 
report on three deep narrow--band images corresponding to \OII\ 
at the redshift of known QSO absorption--line systems which show 
evidence for enhanced star formation occurring in groups of giant 
\HII\ regions spread over 100 -- 300 \kpc. This paper extends 
their earlier investigation (Yanny \et\ 1990, cf. 3{\small )}~). 
For the three QSOs under study the authors list all galaxies 
in the field. From these tables we picked up 7 absorber 
candidates as suggested by the authors.

\bigskip\app{10) Drinkwater \et\ 1993}
\entitle
{On the nature of \MgII\ absorption line systems in quasars}
{M.J. Drinkwater, R.L. Webster and P.A. Thomas}
present the results of a large R--band imaging survey
of 71 bright ($m_v < 18$) quasars revealing \MgII\ absorption 
lines in their spectra. For 21 QSO fields possible absorber candidates
are found, however, no galaxy redshifts have been measured.
A statistical approach is used to identify galaxies likely 
to be associated with the absorption systems. 
In \TABLE 5 and 7 of their paper the authors give \zabs\ and R 
magnitudes for possible absorber candidates. For some 
galaxies two possible \zabs\ are given. 

\bigskip\app{11) Le Brun \et\ 1993 }
\entitle
{A deep imaging survey of fields around quasars with $z < 1.2$ 
 \MgII\ absorption systems}
{V. Le Brun, J. Bergeron, P. \Boisse\ and C. Christian}
report on an imaging survey of 12 fields around quasars 
with 17 \MgII\ absorption systems in the r band at the CFH telescope.
They give a list (Table 3. in their paper) of altogether 19
absorber candidates with 6 galaxy redshifts being 
spectroscopically confirmed. It turned out that
two of them are not absorber galaxies (\zgal\ $\ne$ \zabs).
The authors emphasize that some of the candidates 
are rather uncertain.

\bigskip\app{12) Spinrad \et\ 1993}
\entitle
{Hydrogen and metal absorption lines in PKS0405--123
 from the halos of low redshift galaxies}
{H. Spinrad, A.V. Filippenko, H.K.C. Yee, E. Ellingson, J.C. Blades, 
 J.N. Bahcall, B.T. Jannuzi, J. Bechtold and A. Dobrzycki}
report on HST ultraviolet and ground--based optical spectra of 
the bright quasar PKS 0405--123 which has two absorption--line 
systems. Spectroscopically measured redshifts and Gunn g and r 
magnitudes are given for 9 galaxies. One redshift is very uncertain. 
The values of galaxy redshifts are grouped near two different 
absorber redshifts ($z_1 = 0.1670$ and $z_2 = 0.3516$) 
indicating small groups of galaxies or outskirts of clusters
of galaxies.

In the $z_2$ system only Ly$\alpha$ absorption is observed
whereas in the $z_1$ system metal lines (\CIV\ and probably
\MgII) are detected as well.

The authors give r--magnitudes and (g--r) colors (Thuan \& 
Gunn (1976) g and r) in their \TABLE~1 and thus g--magnitudes
can be derived.

\bigskip\app{13) Steidel \et\ 1993}
\entitle
{A dwarf galaxy near the sight line to PKS 0454+0356:
 A fading ``faint blue galaxy''?}
{C.C. Steidel, M. Dickinson and D.V. Bowen} 
report on the discovery of a dwarf galaxy at
$z = 0.072$ which is only 4'' in projection from the line of
sight to the quasar . Fortuitously the spectrum of a second
galaxy was recorded simultaneously from several moderately strong
emission lines revealing $z \approx 0.2$. Here we are not interested
in dwarf galaxies and therefore only data from the latter object
are included in our compilation. By now no appropriate absorption
lines are found in the QSO spectrum. Future observations
(using HST) in search of \MgII\ resonance lines would be very 
meaningful for the study of the gas associated with an intrinsically
faint, star--forming dwarf galaxy.

\vfill\eject
\bigskip\app{14) Aragon-Salamanca \et\ 1994}
\entitle
{The nature of distant galaxies producing multiple \CIV\ 
 absorption lines in the spectra of high-redshift quasars}
{A. Aragon-Salamanca, R.S. Ellis, J.-M. Schwartzenberg and J. Bergeron}
demonstrate that luminous L$^*$ galaxies up to $z \simeq 2$ 
which cause \CIV\ absorption % ($\lambda 1548, \lambda 1550$)
in the spectra of quasars can be detected by deep infrared (K band) imaging. 
% Most, if not all strong \CIV\ systems have 
% associated \MgII\ and \CII\ absorption.
 
The authors use a statistical approach to identify the 
absorbers from photometry alone because at these faint 
limits spectroscopy is very difficult. A sample 
of 11 QSOs with clustered \CIV\ absorption line systems 
is investigated. In some cases, several suitable
complexes at different \zabs\ are present within a single 
QSO spectrum. As the redshift of possible absorbers we take 
from their \TABLE 1 the mean values $\langle z_{abs}^{\CIV} 
\rangle$ weighted by the appropriate rest--frame equivalent 
width for each system. 

A subset of the QSO fields has also been imaged in R and I. 
Thus, 19 K magnitudes and 9 $(R-K)$ colors
are given in \TABLE 2 of the paper. From these data we obtain
R magnitudes as a function of redshift for 9 absorber candidates.

\bigskip\app{15) Ellingson \et\ 1994 }
\entitle
{Metal--line absorption at \zabs\ $\sim {\rm z}_{\rm em}$ 
 from associated galaxies} 
{E. Ellingson, H.K.C. Yee, J. Bechtold and A. Dobrzycki} 
report on deep optical imaging and limited spectroscopy of 
10 fields around quasars with $0.15 < {\rm z}_{\rm em} < 0.65$
revealing \CIV\ absorption predominantly at the emission
redshift of the QSO. The aim of their investigation is not
the optical identification of absorber systems but the
study of the interaction of quasars with galaxies from
the surrounding clusters. Some of their data, compiled
in \TABLE 2. are also useful to our purposes. We select 
7 candidates from their list, one galaxy with
spectroscopically confirmed redshift. 

% Images in the Gunn g and i band have been taken also 
% for a number of fields, but the data are not published.
We want to caution that the rich cluster environment and the 
proximity to the quasars might be influential on 
the evolution of these galaxies. 

\bigskip\app{16) Steidel \et\ 1994a}
\entitle
{The z = 0.8596 damped lyman alpha absorbing galaxy toward PKS 0454+0356}
{C.C. Steidel, D.V. Bowen, J.C. Blades and M. Dickinson}
present HST and ground--based data on a new DLA system at 
\zabs$ = 0.8596$ along the line of sight to PKS 0454+0356.
Optical images were obtained as part of a large survey for
galaxies producing \MgII\ absorption line systems, including 
a very deep \R\ (6930/1500) image from which we take the \R\ 
magnitude as a function of redshift for this galaxy. The authors 
only gave a faint limit ($K > 20.5$) for the K magnitude.

\bigskip\app{17) Steidel \et\ 1994b}
\entitle
{Imaging of two damped lyman alpha absorbers at intermediate redshift}
{C.C. Steidel, M. Pettini, M. Dickinson and S.E. Persson}
report on observing the fields of the QSOs 3C 286 and PKS 1229--021
in the $I$ and $K_s$ bands. Under good seeing conditions they
resolve faint galaxy images close to the QSO sight--lines.
We adopt I and K magnitudes as a function of redshift for
three absorber candidates from this paper.

\bye
