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\begin{centering}
\huge
 
\vspace*{40mm}
{\bf
A CATALOGUE OF QUASARS \\
\vspace*{5mm}
AND ACTIVE NUCLEI \\
} 
\normalsize
\vspace*{10mm}
(10th edition)
 
\vspace*{40mm}
\large
{\bf M.-P. V\'eron-Cetty and P. V\'eron} 
\normalsize
\vspace*{5mm}

Observatoire de Haute Provence, CNRS \\

F-04870 Saint-Michel l'Observatoire

\vspace*{20mm}
May 2001 \\

\normalsize
\end{centering} 
\normalsize
\newpage
\section{Summary}
 
\indent The recent publication of the first release of the 2dF quasars catalogue 
(Croom et al. 2001) containing nearly 10\,000 new QSOs, almost doubling the 
number of known such objects led us to prepare an updated version of our 
catalogue of quasars and active nuclei which now contains 23$\,$760 
quasars, 608 BL Lac objects and 5$\,$751 active galaxies (of which 2$\,$765 are 
Seyfert 1).
Like the ninth edition, it includes 
position and redshift as well as photometry (U, B, V) and 6 and 11 cm flux 
densities when available. \\
 We also give a list of all known lensed and double quasars.

\section{Introduction}
\indent 	
	The first catalogue of quasars was published in 1971 by De Veny et al. 
It contained 202 objects for which redshifts were published prior to june 1971.
 Since 1971, the number of known quasars has steadily increased, but the
recent release of the ``2dF QSO redshift survey" (Croom et al. 2001) has almost
doubled the number of known quasars. \\ 
\indent This number is expected to increase again dramatically when the final 
2dF catalogue will be published at the end of 2002 containing $\sim$ 15\,000 
new QSOs and when the
``Sloan Digital Sky Survey" which should discover 
$\sim100\;000$ QSOs will be completed in about 2004 (Fan et al. 1999)\\
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
%%%%%%%%%% Table  %%%%%%%%%%%%%%
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
\begin{table}[h]
\addtocounter{table}{-1}
\caption{Increase with time of the number of known QSOs, 
BL Lacs and Seyfert 1s}
\begin{center}
\begin{tabular}{rrrl}
\hline
 QSO & BL Lac & Seyfert 1 & reference \\
\hline
   202 &     &      & De Veny et al. 1971 \\
  2$\,$251 &     &  190 & V\'eron-Cetty \& V\'eron 1984 \\
  2$\,$835 &  73 &  236 & V\'eron-Cetty \& V\'eron 1985 \\
  3$\,$473 &  84 &  258 & V\'eron-Cetty \& V\'eron 1987 \\
  4$\,$169 & 117 &  358 & V\'eron-Cetty \& V\'eron 1989 \\
  6$\,$225 & 162 &  575 & V\'eron-Cetty \& V\'eron 1991 \\
  7$\,$383 & 171 &  695 & V\'eron-Cetty \& V\'eron 1993 \\
  8$\,$609 & 220 &  888 & V\'eron-Cetty \& V\'eron 1996 \\
 11$\,$358 & 357 & 1$\,$111 & V\'eron-Cetty \& V\'eron 1998 \\
 13$\,$214 & 462 & 1$\,$711 & V\'eron-Cetty \& V\'eron 2000 \\
 23$\,$760 & 608 & 2$\,$765 & present edition            \\
\hline
\end{tabular}
\end{center}
\end{table}
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
%%%%%%%%% end table  %%%%%%%%%%%%%%%
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%

	In the present edition of this catalogue containing quasars with 
measured redshift known to us prior to May 1$^{\rm st}$, 2001, as in the first nine  
editions, we do not give any information about  absorption lines or X-ray 
properties. But we give the absolute magnitude for each object and, when 
available, the 11 and 6 cm flux densities. \\

	This catalogue should not be used for any statistical analysis as it 
is not complete in any sense, except that it is, hopefully, a complete survey 
of the literature.
 
\section{Description of the catalogue}
\indent  
	We have arbitrarily defined a quasar as a starlike object, or an object 
with a starlike nucleus with broad emission lines, brighter than absolute 
magnitude M$_{\rm B}$ = $-$23; 
only objects brighter than this limit appear in table 1.
 
	In table 2, we list all confirmed,  probable or possible BL Lac 
objects with or without  a measured redshift, without consideration of their 
absolute magnitude. As better spectra are becoming available, broad emission 
lines have been detected in a number of objects formerly classified as BL Lac; 
they have usually been moved to table 1 (V\'eron-Cetty \& V\'eron, 2000). 
 
	The Seyfert 1 galaxies have broad Balmer and other permitted lines; 
the Seyfert 2 galaxies have Balmer and forbidden lines of the same width.
	Osterbrock (1977; 1981) has divided the Seyfert galaxies showing broad 
Balmer lines (Seyfert 1) into five subgroups : Seyfert 1.0, 1.2, 1.5, 1.8 and 
1.9 
on the basis of the appearance of the Balmer lines. Seyfert 1.0s are 
``typical" 
members of the class, as described by Khachikian \& Weedman (1971; 1974), while 
Seyfert 1.5s are objects intermediate between typical Seyfert 1 and 
Seyfert 2 galaxies, with an easily apparent narrow H${\beta}$ profile superimposed on 
broad wings. The classes Seyfert
 1.2 or 1.8 are used to describe objects with relatively weaker and stronger 
narrow H${\beta}$ components, intermediate between Seyfert 1.0 and 1.5 and 
Seyfert 1.5 and 2 respectively. 
In Seyfert 1.9, although the broad H${\alpha}$ emission is 
clearly 
evident, broad H${\beta}$ cannot be detected with certainty by mere visual 
inspection of the spectra. 
 
	We have adopted the more quantitative classification introduced by
Winkler (1992) : 
\begin{tabbing}
\=~~~~~~~~~~~~~~	\= S1.0~~~	\= 5.0~~~  \= $<$ R~~~~~~~~~~~ \= ~~ \\
\>	\> S1.2	\>2.0      \> $<$ R $<$ 5.0 \>  \\
\>	\> S1.5	\>0.333    \> $<$ R $<$ 2.0 \>   \\
\>	\> S1.8	\>         \> $\verb+ +\, $ R $<$ 0.333 \> broad component visible in 
H${\alpha}$ and H${\beta}$ \\
\>	\> S1.9	\>	   \>  \>broad component visible in H${\alpha}$ but not in 
H${\beta}$ \\
\>	\> S2	\>	\> \> no broad component visible 
\end{tabbing}

\noindent
where R is the ratio of the total H${\beta}$ to the [OIII]$\lambda$5007 
fluxes.
 
\indent
	Several objects have been found to show extreme spectral variability, 
changing from Seyfert 1.8 or 1.9 to Seyfert 1. In some cases these 
changes are consistent with changes in the reddening to the BLR while, in 
others, they are probably due to real changes in ionizing flux  
(Goodrich, 1989a; 1995; Tran et al. 1992b).
	In some Seyfert 2 galaxies, a broad Pa $\beta$ line has been detected, 
indicating the presence of a highly reddened broad line 
region (Goodrich et al. 1994); we call these objects S1i.
	A number of Seyfert 2 galaxies have, in polarized light, the spectra 
of Seyfert 1s (Antonucci \& Miller, 1985; Miller \& Goodrich 1990; Tran et 
al. 1992a); we call them S1h.
	Typical full widths at half-maximum of the Balmer lines in Seyfert 1 
galaxies lie in the range 2000-6000 km s$^{-1}$. However, there is a group of 
active galactic nuclei with all the properties of Seyfert 1 galaxies, but 
with unusually narrow Balmer lines (Osterbrock \& Pogge, 1985; Goodrich,
1989b); they are defined as having the broad component of 
the Balmer lines narrower than 2000 km s$^{-1}$ FWHM (Osterbrock, 1987);
 we call them S1n. 
 
	Table 3 lists ``active galaxies" : Seyfert 1, 1.5, 1.8, 
1.9, 1h, 1i, 1n, 2, and Liners (as defined by Heckman, 1980) fainter than the 
above quoted absolute magnitude. 
A number of galaxies with a nuclear HII region denoting a burst of star 
formation are also included, the reason being that they have been called 
Seyfert in the past and later reclassified; we consider it useful to keep 
trace of these reclassifications to avoid further confusion. 
 
	Table 4 lists the objects which once have been believed to be quasars 
or BL lac objects and are now known to be either stars or normal galaxies.
 
	Table 1 contains 23$\,$760 objects, table 2, 608 , table 3, 5$\,$751 
and table 4, 71.
	
	The catalogue is believed to be complete for quasars, BL Lac objects 
and Seyfert 1 galaxies.
 
	Since the discovery in 1979 by Walsh et al. of the first 
gravitationally lensed quasar, Q 0957+561, a number of such objects (44) and of 
physical pairs with separation less than 10" (11) have been found. They 
are listed in table 5. Mortlock 
et al. (1999) have stressed the difficulty sometimes encountered in 
distinguishing lensed quasars from physical pairs. 
 
 
\indent Tables 1, 2 and 3 give :
 
1)	The most   common  name  of the  object. 
 For the meaning and the sources of the designations see Hewitt \& 
Burbidge (1987), Fernandez et al. (1983) and Kesteven \& Bridle (1977). For 
the sources discovered by the ROSAT X-ray satellite, we have used the 
following acronyms : RXS for the sources appearing in the All-Sky Bright 
Source Catalogue (Voges et al. 1999), 1WGA for the sources published in the 
WGACAT catalogue (White et al. 1994) and RX for the others. \\
\indent
When the name is  preceded by an *, the object  has
not been detected as a radio source, either because it has not been observed 
or because it is fainter  than the sensitivity limit of the radio telescope 
used; there is no uniform upper limit to the flux  density of the undetected 
objects.
 
2)	The  best  available J2000 optical or radio coordinates; the J2000 
positions have been converted
from the B1950 positions using the matrix given by Aoki et al. (1983). 
No references are given for the sources of these positions.
An O or an R following the coordinates means that the position given 
is either an 
optical or a radio position measured with an accuracy better than one arc sec. 
An A means that it is only an approximate position which may be wrong by 
several arc minutes. 
The availability of the Digitized Sky Survey (DSS) allows quick 
measurements of the optical position of any object brighter than $\approx$19.5 
mag. It has already been used to measure the position of several hundred QSOs 
(Schneider et al. 1992; Bowen et al. 1994; Kirhakos et al. 1994; V\'eron-Cetty \&
 V\'eron, 1996). Optical positions with an accuracy better than 2" have also 
been measured for the 19$\,$369 galaxies in the Zwicky catalogue (Falco et al. 
1999) and for the 12$\,$921 UGC galaxies (Cotton et al. 1999). 
 
3)	The  6  and  11 cm  flux  densities  (in  Jy) with  references  to  
the  literature.  When  several
measurements are available we took arbitrarily one of them. When a reference 
is given for the 6 cm flux density but the value of the flux density itself is 
left blank and there is an * in column 1, only an upper limit 
is available and this upper limit is not much greater than 1 mJy; in case 
there is no * in column 1, the reference refers to a detection but at a 
wavelength other than 6 cm. 
 
4)	The redshift as published. An * in front of the redshift means 
that it has been estimated
from a low dispersion slitless spectrum and is of lesser accuracy or even 
plainly wrong as the emission lines may easily be misidentified. We 
have given only those values which are described as probable in the original 
sources and not the possible   values. 
 
5)	In this column an attempt has been made to classify the objects as 
follows :
\begin{tabbing} 
\= ~~~~~~~~	\= S1 ~~~~~~	\= Seyfert 1 spectrum with broad permitted hydrogen emission 
lines, without 	sufficent \\ 
\>              \>              \> information for a more detail classification. \\
\>	        \> S1.0, S1.2, S1.5, S1.8, S1.9, S1i, S1h, S1n (see above). \> \\
\>	        \> S2	  \> Seyfert 2 spectrum defined as having a strong [O III]$\lambda$ 
5007 line compared with H$\beta$, \\
\>              \>        \> together with a [NII]$\lambda$6584 line of 
strength comparable with that of H$\alpha$. \\
\>              \>S3	  \>Seyfert 3 or Liner as defined by Heckman (1980). 
Broad Balmer lines are observed \\
\>              \>        \> in some Liners; they are called S3b. \\
\>              \>        \> If these broad Balmer lines are only seen in
polarized light, they are called S3h. \\
\> 	        \>S or S? \>These objects are probably  or possibly  Seyfert galaxies, but 
available  data are \\
\>              \>        \> insufficient for a more detailed classification. \\
\>	        \>H2	  \>Nuclear HII region, {\it i.e.} nucleus of a galaxy with an emission 
line spectrum similar \\
\>              \>        \> to that of an emission nebula ionized by hot stars. \\
\>	        \>HP	  \>A high degree of optical polarization ($>$ 3\%) has been measured
 (see for instance : \\
\>              \>        \> Impey et al. 1991; Moore \& Stockman, 1984). \\
\end{tabbing} 
	Low redshift quasars are classified as S1 when a good spectrum shows 
that they are similar to  Seyfert 1 galaxies. 
 
	In table 2, we find in this column :
\begin{tabbing} 
\=~~~~~~~~	\= BL~~~~~~~ 	\= for a confirmed BL Lac object. \\
\>	        \> blank	\>for a probable BL Lac. \\
\>	        \> ?	        \>for a possible BL Lac. 
\end{tabbing}
 
6)	The  V, B$-$V  and U$-$B  photoelectric  or photographic magnitude and 
colours, when available.
(the survey of the literature for photographic colours may be incomplete) (an 
* in front of the magnitude indicates that the colours and the magnitude are 
photographic, while an R or an I indicates a red or an infrared magnitude).  Maoz et al. (1993) 
have measured homogeneous V magnitudes for 354 QSOs with an 
accuracy of $\pm$0.1 mag; they have been included. For a 
few objects, the O magnitude, measured on the blue Palomar Sky Survey
plates, or the UK Science 
Research Council SRC-J Survey plates, believed to be accurate within $\pm$ 
0.2 mag., has been extracted from the APS database (Pennington et al. 1993).
For a number of objects we give the O magnitude, extracted from the USNO-A2 
catalogue (Monet et al. 1996) or the Cambridge Automated Plate Measuring Machine 
(APM) catalogue (Irwin et al. 1994), recalibrated by E. Flesch (private communication);
these magnitudes are flagged with an O.
The O and Johnson B magnitudes are related 
by B$-$O = $-$(0.27$\pm$
0.06) (B$-$V) (Evans, 1989). \\
\indent 
In the other cases, the magnitude given is an estimate as 
found in the original publications; these magnitudes are generally quite 
inaccurate and inhomogeneous; 
they are most often m$_{\rm pg}$ or B magnitudes instead of the Johnson V magnitude. 
Much care should be taken when using them for any purpose. Anyway, even when 
a photoelectric V magnitude is given, it is not very meaningful as most quasars 
are variable. On the other hand, the colours of quasars vary little, so the 
listed colours should be accurate. Again, it should be noted that 
some of the colours listed are photographic and, therefore, less accurate; 
moreover, in each catalogue of photoelectric measurements, the faintest objects 
measured are affected by relatively large errors; this too should not be 
overlooked. For the galaxies, in table 3, we have chosen the magnitudes and 
colours measured in the smallest possible diaphragm (preferentially 16 arcsec) 
as we are interested in the nucleus rather than in the galaxy itself. 
 
7)	The  absolute  magnitude  M$_{\rm B}$   computed  by  assuming  
H$_{0}$=50 km s$^{-1}$ Mpc$^{-1}$, q$_{0}$=0, and an optical spectral index 
$\alpha$ equal to 0.3 (defined as S $\propto$ $\nu ^{-\alpha}$) (Francis et al. 
1991).

The absolute magnitude is computed as follows :
	M = m + 5 $-$ 5 log D $-$ k + $\Delta$ m(z)
where m is the B magnitude,  D = c/H$_{0}$ A, with A the photometric distance 
(Terrell, 1977) :
  $$A=z[1+\frac{z(1-q_{0})}{(1+2q_{0}z)^{0.5}+1+q_{0}z}]$$
		
\noindent 
	z is the redshift taken from column 5;
	k=$-$2.5 log(1+z)$^{1-\alpha}$ is the k correction, $\Delta$m (z) is a
correction to k taking into account the fact that the spectrum of quasars is 
not strictly a power law of the form  S $\propto$ $\nu ^{-\alpha}$, but is 
affected by emission lines and by the Ly $\alpha$ forest depleting the 
continuum to the blue of Ly $\alpha$. Assuming that the spectrum is a power 
law with $\alpha$=0.3 may not give the best possible estimate of the k 
correction (Wisotzki 2000). 
 
	The column labelled ``V" gives the V magnitude when B$-$V is also given 
in which case we have used B = V$+$(B$-$V). When B$-$V is not given, this 
column usually gives the B magnitude, unless it is preceded by an R or an I; 
the R magnitudes have been transformed into the B system by 
using an average $<$B$-$R$>$=0.57 and the I magnitudes by using 
$<$B$-$I$>$=1.1 for low z QSOs. When the reference for the magnitude is 
Maoz et al. (1993), the magnitude is V and we have used $<$B$-$V$>$=0.40.
 
	We list  in  table 1 those objects which have an absolute 
magnitude  M$_{\rm B}$ brighter than 
$-$23; clearly some objects would move from table 1 to table 3 and vice versa 
if other values for q$_{0}$ and the spectral index were used or if an 
accurate B apparent magnitude was available for all objects.The variability 
may have a similar effect, as well as the size of the diaphragm used for the 
measurement as the contribution of the underlying galaxy for weak quasars may 
not be negligible.
 
8)	The  next  three  columns  give  the  reference  for  the  finding  
chart,  the  photometry and the redshift respectively. In many cases, the last 
reference in table 3 is that of the classification of the object (as a Seyfert 
galaxy or otherwise); in these cases the redshift can usually be found in 
Palumbo et al. (1983).
 
9)	The B1950 position.
 
\small 
\section{Acknowledgements}
\indent 
This research has made use of the APS catalogue of 
POSS I database which is supported by the National Science Foundation, the 
National Aeronautics and Space Administration, and the University of Minnesota

	We are grateful to E. Flesch for extracting for us the recalibrated O 
magnitudes from the APM and USNO catalogues and to
E. Flesch, F. Ochsenbein and R. Monella for having 
brought to our attention a number of errors and omissions in the 8th edition 
of this catalogue.
\normalsize 

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V\'eron-Cetty M.-P., V\'eron P. 1993, ESO Scientific Report N$^{\rm o}$ 13 \\
V\'eron-Cetty M.-P., V\'eron P. 1996, ESO Scientific Report N$^{\rm o}$ 17 \\
V\'eron-Cetty M.-P., V\'eron P. 1998, ESO Scientific Report N$^{\rm o}$ 18 \\
V\'eron-Cetty M.-P., V\'eron P. 2000, ESO Scientific Report N$^{\rm o}$ 19 \\
V\'eron-Cetty M.-P., V\'eron P. 1996, A\&AS 115, 97 \\
V\'eron-Cetty M.-P., V\'eron P. 2000, A\&AR 10,81 \\
Voges W., Aschenbach B., Boller T. et al. 1999, A\&A 349,389 \\
% Walsh D., Carswell R.F., Weymann, R.J. 1979, Nat. 279, 381 \\
% Weymann R.J., Latham D., Angel J.R.P. et al. 1980, Nat. 285, 641 \\
White N.E., Giommi P., Angelini L. 1994, IAU Circ. 6100 \\
% Whittle M. 1992, ApJS 79, 49 \\
% Winkler H. 1992, MNRAS 257, 677 \\
% Wisotzki L., K\"{o}hler T., Kayser R., Reimers D. 1993, A\&A 278, L15 \\
% Wisotzki L., K\"{o}hler T., Lopez S., Reimers D. 1996, A\&A 315, L405 \\
% Wisotzki L., Christlieb N., Lin M.C. et al. 1999, A\&A 348, L41 \\
Wisotzki L. 2000,A\&A 353,861 \\ 
 
\scriptsize
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
%%%%  Table 5
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% 
\begin{table}
\addtocounter{table}{4}
\caption{Gravitationally lensed quasars and physical pairs.
Col. 1 : name, col. 2 : short position, col. 3 : redshift of the quasar, col. 4 : 
redshift of the lens, col. 5 : separation in arcsec, col. 6 : references}
\begin{center}
\begin{tabular}{lllllc}
\hline
Name & Position & z$_{\rm quasar}$ & z$_{\rm lens}$ & sep(") & Ref. \\
\hline
\hline
Lensed QSOs & & & & & \\
\hline
UM 673  	& 0142$-$10 &	2.719 &	      &	2.2  &	48 \\
CTQ 414 	& 0156$-$43 &	1.29  &	      &	1.2  &	37 \\
B2 0218+35	& 0218$+$35 &	0.936 &	      &	0.33 &	11 \\
HE 0230$-$2130	& 0230$-$21 &	2.162 &	      &	2.0  &	58 \\
Q J0240$-$343	& 0238$-$34 &	1.406 &	      &	6.1  &	50 \\
PKS 0411+05	& 0411$+$05 &	2.639 &	0.958 &	2.2  &	25,52 \\
HE 0512$-$3329  & 0512$-$33 &   1.565 & 0.931 & 0.6  &  10 \\
B 0712+472	& 0712$+$47 &	1.339 &	      &	1.27 &	 7 \\
MG 0751+2716	& 0748$+$27 &	3.200 &	0.350 &	     &	52 \\
HS 0818+1227	& 0818$+$12 &	3.115 &	      &	2.1  &	12 \\
CLASS B0827+525	& 0827$+$52 &	2.064 &	      &	2.8  &	23 \\	
APM 08279+5255	& 0827$+$52 &	3.87  &	      &	0.4  &	26 \\	
RX J0911.4+0551	& 0908$+$06 &	2.800 &	      &	0.8  &	 1 \\
SBS 0909+532	& 0909$+$53 &	1.377 &	0.830 &	1.11 &	22,30 \\
1WGA J09212+4528& 0917$+$45 &	1.66  &	0.31  &	6.93 &	41 \\
FBQS J0951+2635	& 0948$+$26 &	1.24  &	      &	1.1  &	45 \\
BRI 0952$-$01	& 0952$-$01 &	4.43  &	      &	0.95 &	34 \\
Q 0957+561	& 0957$+$56 &	1.414 &	0.355 &	6.1  &	9,53 \\
Q 1009$-$0252	& 1009$-$02 &	2.74  &	      &	1.55 &	16 \\
J 13.03	        & 1015$-$20 &	2.55  &	      &	0.84 &	49 \\
IRAS F10214+4724& 1021$+$47 &	2.286 &	      &	     &  46 \\   
B 1030+074	& 1030$+$07 &	1.535 &	      &	1.56 &	 7 \\
HE 1104$-$1805	& 1104$-$18 &	2.303 &	0.729 &	3.0  &	28,56 \\
PG 1115+080	& 1115$+$08 &	1.722 &	0.311 &	2.3  &	51,54 \\
UM 425	        & 1120$+$01 &	1.465 &	      &	6.5  &	35 \\
TEX 1152+199	& 1152$+$19 &	1.019 &	0.439 &	1.6  &	42 \\
Q 1208+1011	& 1208$+$10 &	3.803 &	      &	0.45 &	32 \\
87GB 1359+1527	& 1359$+$15 &	3.235 &	      &	1.7  &	42 \\
H 1413+117	& 1413$+$11 &	2.546 &	      &	1.4  &	31 \\
HST J14176+5226	& 1415$+$52 &	3.4   &	      &	3.2  &	 4 \\
B 1422+231	& 1422$+$23 &	3.62  &	0.339 &	1.3  &	43,51 \\
Q 1429$-$008	& 1429$-$00 &	2.076 &	      &	5.1  &	15 \\
SBS 1520+530	& 1520$+$53 &	1.855 &	      &	1.6  &	 3 \\
Q 1600+434	& 1600$+$43 &	1.61  &	      &	1.38 &	20 \\
Q 1634.9+26.7	& 1634$+$26 &	1.961 &	      &	3.8  &	47 \\
FIRST J1633+3134& 1631$+$31 &	1.516 &	      &	0.66 &	39 \\
MC 1830$-$211	& 1830$-$21 &	2.507 &	0.885 &	0.60 &	27,29 \\
TEX 1835$-$345	& 1835$-$34 &	2.78  &	      &	1.0  &	55 \\
MG 2019+1127	& 2016$+$11 &	3.273 &	      &	3.4  &	24 \\
87GB 20451+2632	& 2045$+$26 &	1.28  &	0.867 &	1.9  &	 8 \\
Q 2138$-$431	& 2138$-$43 &	1.641 &	      &	4.5  &	14 \\
H 2149-2745	& 2149$-$27 &	2.033 &	      &	1.7  &	57 \\
Q 2237+0305	& 2237$+$03 &	1.695 &	0.039 &	1.8  &	19 \\
Q 2345+007	& 2345$+$00 &	2.15  &	      &	7.1  &	44 \\
\hline
Binary QSOs & & & & & \\
\hline
Q 0023+171	& 0023$+$17 &	0.945 &	      &	4.8  &	18 \\
CT 344  	& 0103$-$27 &	0.848 &	      &	0.3  &	21 \\
PHL 1222	& 0151$+$04 &	1.91  &	      &	3.3  &	36 \\
CTQ 839         & 0250$-$33 &   2.24  &       & 2.1  &  38 \\
Q 1145$-$071	& 1145$-$07 &	1.34  &	      &	4.2  &	 6 \\
HS 1216+5032 	& 1216$+$50 &	1.450 &	      &	8.9  &	13 \\
RRS IV 26,27	& 1343$+$26 &	2.030 &	      &	9.5  &	 5 \\
RX J16290+3724  & 1627$+$37 &   0.923 &       & 4.3  &  33 \\
Q J1643+31	& 1641$+$32 &	0.586 &	      &	2.3  &	 2 \\
Q 2153$-$2056	& 2153$-$20 &	1.845 &	      &	7.8  &	17 \\
MGC 2214+3550	& 2212$+$35 &	0.877 &	      &	3.0  &	40 \\
\hline
\end{tabular}
\end{center}
\end{table}
\normalsize
\begin{table}
\addtocounter{table}{-1}
\begin{center}
\begin{tabular}{llll}
 & & & \\
 & & & \\
 (1)    &  Bade et al. 1997             &  (30)  &  Lubin et al. 2000 \\
 (2)    &  Brotherton et al. 1999       &  (31)  &  Magain et al. 1988 \\
 (3)    &  Chavushyan et al. 1997       &  (32)  &  Magain et al. 1992  \\       
 (4)    &  Crampton et al. 1996	        &  (33)  &  Mason et al. 2000 \\
 (5)    &  Crotts et al. 1994           &  (34)  &  McMahon et al 1992  \\  
 (6)    &  Djorgovski et al. 1987       &  (35)  &  Meylan \& Djorgovski 1989 \\ 
 (7)    &  Fassnacht \& Cohen, 1998     &  (36)  &  Meylan et al. 1990 \\
 (8)    &  Fassnacht et al. 1999        &  (37)  &  Morgan et al. 1999 \\
 (9)    &  Garrett et al. 1992          &  (38)  &  Morgan et al. 2000 \\
 (10)   &  Gregg et al. 2000            &  (39)  &  Morgan et al. 2001 \\
 (11)   &  Grundahl \& Hjorth, 1995     &  (40)  &  Mu\~{no}z et al. 1998 \\
 (12)   &  Hagen \& Reimers 2000        &  (41)  &  Mu\~{no}z et al. 2001 \\
 (13)   &  Hagen et al. 1996            &  (42)  &  Myers et al. 1999 \\  
 (14)   &  Hawkins et al. 1997          &  (43)  &  Patna\"{\i}k et al. 1992 \\
 (15)   &  Hewett et al. 1989           &  (44)  &  Pello et al. 1996 \\
 (16)   &  Hewett et al. 1994           &  (45)  &  Schechter et al. 1998 \\
 (17)   &  Hewett et al. 1998           &  (46)  &  Serjeant et al. 1995 \\
 (18)   &  Hewitt et al. 1987           &  (47)  &  Steidel \& Sargent, 1991 \\
 (19)   &  Huchra et al. 1985           &  (48)  &  Surdej et al. 1987 \\
 (20)   &  Jackson et al. 1995	        &  (49)  &  Surdej et al. 1997 \\
 (21)   &  Junkkarinen et al. 2001      &  (50)  &  Tinney, 1995 \\
 (22)   &  Kochanek et al. 1997 	&  (51)  &  Tonry, 1998 \\
 (23)   &  Koopmans et al. 2000         &  (52)  &  Tonry \& Kochanek, 1999 \\
 (24)   &  Lawrence et al. 1984	        &  (53)  &  Tytler \& Fan 1992 \\
 (25)   &  Lawrence et al. 1995	        &  (54)  &  Weymann et al. 1980 \\
 (26)   &  Ledoux et al. 1998	        &  (55)  &  Winn et al. 2000 \\
 (27)   &  Lidman et al. 1999           &  (56)  &  Wisotzki et al. 1993 \\
 (28)   &  Lidman et al. 2000           &  (57)  &  Wisotzki et al. 1996 \\
 (29)   &  Lowell et al. 1998           &  (58)  &  Wisotzki et al. 1999 \\
       
\end{tabular}
\end{center}
\end{table}
\end{document}
	Table 6 gives the list of all the Markarian objects appearing in the 
catalogue :
\begin{tabbing}
\=~~~~~~~~~~	\= col. 1 :~ \= Markarian number \\
\>	        \>col. 2 :    \>Name under which the galaxy appears in the present 
catalogue when it is not the \\
\>              \>            \> Markarian number \\
\>	        \>col. 3 :    \>Short position \\
\>	        \>col. 4 :    \>Table in which the object appears. 
\end{tabbing}
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
%%%%%%%%%%%%% Table 6 %%%%%%%%%%%%%%%%%%%%
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
\begin{table}[p]
\caption{}
\begin{center}
\begin{tabular}{rlrc|rlrc}
\hline
Mark & & Position & Table & Mark & & Position & Table  \\
\hline
	1    &  	   & 0113$+$32	& 3 &  471  &             & 1420$+$33  & 3 \\
	3    & 	 	   & 0609$+$71	& 3 &  474  &             & 1433$+$48  & 3 \\
	6    & 		   & 0645$+$74	& 3 &  477  &             & 1439$+$53  & 3 \\
 	9    & 		   & 0732$+$58	& 3 &  478  &             & 1440$+$35  & 1 \\
	10   & 		   & 0743$+$61	& 3 &  483  &             & 1528$+$34  & 3 \\
	25   &		   & 1000$+$59	& 3 &  486  &             & 1535$+$54  & 3 \\
	34   &	           & 1030$+$60	& 3 &  493  &             & 1557$+$35  & 3 \\
	35   & NGC 3353	   & 1042$+$56	& 3 &  501  &             & 1652$+$39  & 2 \\
	40   & 		   & 1122$+$54	& 3 &  504  &             & 1659$+$29  & 3 \\
	42   & 		   & 1151$+$46	& 3 &  506  &             & 1720$+$30  & 3 \\
	50   & 		   & 1220$+$02	& 3 &  507  &             & 1748$+$68  & 3 \\
	52   & 		   & 1223$+$00	& 3 &  509  &             & 2041$-$10  & 1 \\
	64   &  	   & 1304$+$34	& 3 &  516  &             & 2153$+$07  & 3 \\
	69   & 		   & 1343$+$29	& 3 &  520  &             & 2158$+$10  & 3 \\
	78   & 		   & 0737$+$65	& 3 &  522  &             & 2257$+$16  & 3 \\
	79   & 		   & 0738$+$49	& 3 &  530  & NGC 7603    & 2316$-$00  & 3 \\
	106  & 		   & 0916$+$55	& 3 &  533  & NGC 7674    & 2325$+$08  & 3 \\
	110  & 		   & 0921$+$52	& 3 &  534  & NGC 7679    & 2326$+$03  & 3 \\
	124  &		   & 0945$+$50	& 3 &  538  & NGC 7714    & 2333$+$01  & 3 \\
	132  &		   & 0958$+$55	& 1 &  539  &             & 2341$+$02  & 3 \\
	141  &		   & 1015$+$64	& 3 &  540  &             & 2344$-$00  & 3 \\
	142  & 		   & 1022$+$51	& 3 &  541  &             & 2353$+$07  & 3 \\
	171  & 		   & 1125$+$58	& 3 &  543  &             & 2359$+$03  & 3 \\
	176  & 		   & 1129$+$53	& 3 &  549  &             & 0019$-$01  & 3 \\
	180  & 		   & 1133$+$70	& 2 &  556  &             & 0046$+$04  & 3 \\
	198  & 		   & 1206$+$47	& 3 &  565  &             & 0113$+$04  & 3 \\
	201  & 		   & 1211$+$54	& 3 &  567  &             & 0116$+$04  & 3 \\
	205  & 		   & 1219$+$75	& 3 &  573  &             & 0141$+$02  & 3 \\
	231  & 		   & 1254$+$57	& 3 &  577  &             & 0146$+$12  & 3 \\
	236  & 		   & 1258$+$61	& 3 &  584  &             & 0157$+$02  & 3 \\
	266  & 		   & 1336$+$48	& 3 &  585  &             & 0200$+$02  & 3 \\
	268  & 		   & 1338$+$30	& 3 &  586  &             & 0205$+$02  & 1 \\
	270  & 		   & 1339$+$67	& 3 &  590  &             & 0212$-$00  & 3 \\
	273  & 		   & 1342$+$56	& 3 &  595  &             & 0238$+$06  & 3 \\
	279  & 		   & 1351$+$69	& 3 &  596  &             & 0240$+$07  & 3 \\
	287  & 		   & 1435$+$73	& 3 &  607  &             & 0322$-$03  & 3 \\
	290  & 		   & 1534$+$58	& 3 &  609  &             & 0322$-$06  & 3 \\
	291  &		   & 1552$+$19	& 3 &  612  &             & 0328$-$03  & 3 \\
	298  &		   & 1603$+$17	& 3 &  617  & NGC 1614    & 0431$-$08  & 3 \\
	304  &		   & 2214$+$13	& 1 &  618  &             & 0434$-$10  & 3 \\
	308  & 		   & 2239$+$19	& 3 &  620  &             & 0645$+$60  & 3 \\
	309  & 		   & 2250$+$24	& 3 &  622  &             & 0804$+$39  & 3 \\
	313  & 		   & 2259$+$15	& 3 &  634  &             & 1055$+$20  & 3 \\
	315  & 		   & 2301$+$22	& 3 &  646  &             & 1203$+$35  & 3 \\
	316  &		   & 2311$+$13	& 3 &  661  &             & 1329$+$27  & 3 \\
	321  & NGC 7620	   & 2317$+$33	& 3 &  662  &             & 1351$+$23  & 3 \\
	334  & 		   & 0000$+$21	& 3 &  663  &             & 1352$+$33  & 3 \\
	335  & 		   & 0003$+$19	& 3 &  668  & OQ 208      & 1404$+$28  & 3 \\
	341  & 		   & 0034$+$23	& 3 &  670  &             & 1412$+$26  & 3 \\
	348  & 		   & 0046$+$31	& 3 &  673  &             & 1415$+$27  & 3 \\
	352  & 		   & 0057$+$31	& 3 &  679  &             & 1421$+$33  & 1 \\
	357  & PG 0119+229 & 0119$+$22	& 3 &  684  &             & 1428$+$28  & 3 \\
	358  & 	 	   & 0123$+$31	& 3 &  686  &             & 1435$+$36  & 3 \\
	359  &	 	   & 0124$+$18	& 3 &  699  &             & 1622$+$41  & 3 \\
	372  & 		   & 0246$+$19	& 3 &  700  &             & 1701$+$31  & 3 \\
	373  & 		   & 0650$+$50	& 3 &  703  &             & 0856$+$06  & 3 \\
	374  &	 	   & 0655$+$54	& 3 &  704  &             & 0915$+$16  & 3 \\
	376  & 		   & 0710$+$45	& 3 &  705  &             & 0923$+$12  & 3 \\
	380  &	 	   & 0713$+$74	& 1 &  707  &             & 0934$+$01  & 3 \\
	382  & 		   & 0752$+$39	& 3 &  715  &             & 1002$+$15  & 3 \\
	391  & 		   & 0851$+$39	& 3 &  716  &             & 1007$+$23  & 3 \\
	394  & NGC 2824	   & 0916$+$26	& 3 &  720  &             & 1015$+$07  & 3 \\
	403  & 		   & 0937$+$21	& 3 &  728  &             & 1058$+$11  & 3 \\
	417  & 		   & 1046$+$23	& 3 &  732  &             & 1111$+$09  & 3 \\
	421  & 		   & 1101$+$38	& 2 &  734  &             & 1119$+$12  & 3 \\
        423  &             & 1124$+$35  & 3 &                                
\\
	461  & 		   & 1345$+$34	& 3 &  738  &             & 1133$+$28  & 3 \\
	463  & 		   & 1353$+$18	& 3 &  739  &             & 1133$+$21  & 3 \\
	464  & 		   & 1353$+$38	& 3 &  744  &             & 1137$+$32  & 3 \\
	469  & 		   & 1416$+$34	& 3 &  745  &             & 1137$+$17  & 3 \\
\hline
\end{tabular}
\end{center}
\end{table}
\addtocounter{table}{-1}
\newpage
\begin{table}[p]
\caption{(end)}
\begin{center}
\begin{tabular}{rlrc|rlrc}
\hline
Mark & & Position & Table & Mark & & Position & Table \\
\hline
	759  & 		   & 1208$+$16	& 3 &  1147 &             & 0045$+$10  & 3 \\
	764  & 		   & 1313$+$12	& 3 &  1148 &             & 0049$+$17  & 3 \\
	766  & 		   & 1215$+$30	& 3 &  1149 &             & 0053$-$14  & 3 \\
	769  & NGC 4383	   & 1222$+$16  & 3 &  1152 &             & 0111$-$15  & 3 \\
	771  & ON 1542	   & 1229$+$20  & 3 &  1157 &             & 0130$+$35  & 3 \\
	783  & 		   & 1300$+$16  & 3 &  1158 &             & 0132$+$34  & 3 \\
	789  & 		   & 1329$+$11  & 3 &  1179 &             & 0230$+$27  & 3 \\
	813  & 		   & 1425$+$20	& 1 &  1187 &             & 0245$+$13  & 3 \\
	816  & 		   & 1431$+$52	& 3 &  1193 &             & 0404$-$10  & 3 \\
	817  & 		   & 1434$+$59	& 3 &  1210 &             & 0801$+$05  & 3 \\
	822  & 		   & 1443$+$16	& 3 &  1211 &             & 0803$+$07  & 3 \\
	830  & 		   & 1449$+$58	& 3 &  1212 &             & 0804$+$27  & 3 \\ 
	833  & 		   & 1455$+$35	& 3 &  1218 &             & 0835$+$25  & 3 \\
	840  & 		   & 1502$+$14	& 1 &  1220 &             & 0851$+$17  & 3 \\
	841  & 		   & 1501$+$10	& 3 &  1239 &             & 0949$-$01  & 3 \\
	845  & 		   & 1506$+$51	& 3 &  1243 & NGC 3080    & 0957$+$13  & 3 \\
	848  & 		   & 1516$+$42	& 3 &  1253 &             & 1017$-$03  & 3 \\
	849  & 		   & 1517$+$28	& 3 &  1261 &             & 1041$-$01  & 3 \\
	854  & 		   & 1524$+$43	& 3 &  1269 &             & 1052$+$40  & 3 \\
	860  & 		   & 1537$+$25	& 3 &  1291 & NGC 3660    & 1121$-$08  & 3 \\
	864  & 		   & 1556$+$25	& 3 &  1298 &             & 1126$-$04  & 3 \\
	867  & 		   & 1600$+$26	& 3 &  1308 &             & 1151$+$00  & 3 \\
	871  & 		   & 1606$+$12	& 3 &  1310 &             & 1158$-$03  & 3 \\
	876  & 		   & 1613$+$65	& 1 &  1320 &             & 1216$-$01  & 1 \\
	877  & 		   & 1617$+$17	& 1 &  1325 &             & 1223$+$09  & 3 \\
	883  & 		   & 1627$+$24	& 3 &  1330 & NGC 4593    & 1237$-$05  & 3 \\
	885  & 		   & 1629$+$67	& 3 &  1333 & NGC 4628    & 1239$-$06  & 3 \\
	896  & 		   & 2043$-$02	& 3 &  1344 & NGC 4990    & 1306$-$05  & 3 \\
	897  & II Zw 102   & 2105$+$03	& 3 &  1347 &             & 1320$+$08  & 3 \\
	915  & 		   & 2234$-$12	& 3 &  1361 &             & 1344$+$11  & 3 \\
	917  & 		   & 2238$+$31	& 3 &  1370 &             & 1405$+$07  & 3 \\
	926  & 		   & 2302$-$08	& 1 &  1376 & NGC 5506    & 1410$-$02  & 3 \\
	928  & NGC 7592	   & 2315$-$04	& 3 &  1383 &             & 1426$+$01  & 1 \\
	930  & 		   & 2329$+$28	& 3 &  1388 &             & 1448$+$22  & 3 \\
	937  & 		   & 0007$-$04	& 3 &  1392 &             & 1503$+$03  & 3 \\  
	938  & 		   & 0008$-$12	& 3 &  1393 &             & 1506$-$00  & 3 \\
	940  & 		   & 0011$+$33	& 3 &  1395 &             & 1508$+$04  & 3 \\
	945  & 		   & 0023$-$03	& 3 &  1400 &             & 0217$+$07  & 3 \\
	948  & 		   & 0025$+$06	& 3 &  1408 &             & 0731$+$56  & 3 \\
	955  & 		   & 0035$+$00	& 3 &  1413 &             & 0758$+$73  & 1 \\
	957  & 		   & 0039$+$40	& 3 &  1414 &             & 0848$-$02  & 3 \\
	971  & 		   & 0101$+$35	& 3 &  1419 &             & 0938$+$03  & 3 \\
	975  & 		   & 0111$+$13	& 3 &  1447 &             & 1127$+$49  & 3 \\
	984  & 		   & 0116$+$12	& 3 &  1457 &             & 1144$+$52  & 3 \\
	991  & 		   & 0121$+$31	& 3 &  1459 &             & 1145$+$22  & 3 \\
	992  & 		   & 0121$+$31	& 1 &  1469 &             & 1213$+$51  & 3 \\
	993  & 		   & 0122$+$31	& 3 &  1490 &             & 1417$+$49  & 3 \\
	998  & 		   & 0130$-$02	& 3 &  1494 &             & 1459$+$10  & 3 \\
	1014 & 		   & 0157$+$00	& 1 &  1498 &             & 1626$+$51  & 3 \\
	1018 & 		   & 0203$-$00	& 3 &  1501 & III Zw 2    & 0007$+$10  & 3 \\
	1021 & NGC   835   & 0206$-$10	& 3 &  1502 & I Zw 1      & 0050$+$12  & 1 \\
	1034 & Akn 81	   & 0220$+$31	& 3 &  1503 & II Zw 1     & 0119$-$01  & 3 \\
	1040 & 		   & 0225$+$31	& 3 &  1504 & NGC 1144    & 0252$-$00  & 3 \\
	1044 & 		   & 0227$-$09	& 3 &  1505 & NGC 1275    & 0316$+$41  & 3 \\
	1048 & NGC   985   & 0232$-$09	& 3 &  1506 & 3C 120      & 0430$+$05  & 3 \\
	1055 &	 	   & 0245$-$09	& 3 &  1509 & NGC 5548    & 1415$+$25  & 3 \\
	1058 & 		   & 0246$+$34	& 3 &  1510 &             & 1415$+$26  & 3 \\
	1066 & 		   & 0256$+$36	& 3 &  1511 & NGC 5940    & 1528$+$07  & 3 \\
	1073 & 		   & 0311$+$41	& 3 &  1512 & NGC 5953    & 1532$+$15  & 3 \\
	1087 & II Zw 23	   & 0447$+$03	& 3 &  1513 & II Zw 136   & 2130$+$09  & 3 \\
	1095 & Akn 120	   & 0513$-$00	& 3 &  1514 & NGC 7469    & 2300$+$08  & 3 \\
	1098 & 		   & 1527$+$30	& 3 &       &             &            &   \\
	1102 & 		   & 1555$+$41	& 3 &       &             &            &   \\
	1103 & 		   & 1555$+$41	& 3 &       &             &            &   \\
	1126 & 		   & 2258$-$13	& 3 &       &             &            &   \\
	1127 & 		   & 2259$+$26	& 3 &       &             &            &   \\
	1133 & 		   & 2341$+$27	& 3 &       &             &            &   \\
	1143 & 		   & 0039$+$02	& 3 &       &             &            &   \\
	1144 & 		   & 0040$+$02	& 3 &       &             &            &   \\
	1146 & 		   & 0044$+$14	& 3 &       &             &            &   \\
\hline
\end{tabular}
\end{center}
\end{table}
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