THE FIRST BYURAKAN SURVEY.
A CATALOGUE OF GALAXIES WITH UV-CONTINUUM
B. E. Markarian, V. A. Lipovetsky, J. A. Stepanian,
L. K. Erastova, A. I. Shapovalova
378433, Byurakan Astrophysical Observatory
ArmSSR, Byurakan
357147, Special Astrophysical Observatory
Stavropol Territory, Nizhnij Arkhyz
ABSTRACT
A Catalogue of galaxies with UV-continuum (Markarian galaxies
detected
during
the
First
Byurakan
Survey
(FBS) is
presented. The purpose of the Survey was
to search for
peculiar
faint
extragalactic objects with UV-excess radiation and to study
them. The procedure of observations and processings, the Survey areas,
the
object selection and classification
criteria
and
also
several selection effects are described. The Catalogue contains the
following initial data on all the objects: the precise coordinates,
visual magnitudes, angular sizes, redshifts and classification types.
The observational
results
of
slit spectra, UBV-photometry, IRphotometry (IRAS data), morphology and some other data are also
included into the Catalogue.
While compiling the Catalogue the
authors introduced some necessary corrections in the data of the
earlier
published lists on galaxies with UV-continuum. In addition
we included the objects with numbers 1501-1515. In most cases they are
well-known Seyfert galaxies omitted by the authors in the lists,
but detected on the plates.
41 objects from our lists are not
included into the Catalogue, since they are either stars of our
Galaxy or
star projections
on
the
galaxies.
The
Catalogue
presents the largest homogeneous sample of AGN of different types on
the northern sky for bright objects (<16.0). Up to the middle of 1987
the redshifts were measured for 1459
out of 1469 objects of the
Catalogue.
1. THE HISTORY OF THE FIRST BYURAKAN SURVEY
Studying the results of the surface photometry carried out from
1958
to 1962
and comparing them with the spectra of the central
parts of the same galaxies, Markarian (1963)
concluded
that
the
colours
of
the central parts of a great number of galaxies do not
correspond to their morphological types, i. e. the central parts were
bluer than
those
of normal galaxies of the same Hubble type.
The compiled sample of 41 objects included 8 galaxies, marked by Seyfert in
1943,
whose
nuclei showed bright and wide (some thousand
km/s) emission lines. Therefore, a hypothesis has
been
made
(Markarian,
1963)
on
possible non-thermal character of radiation from
the nuclei of some studied galaxies.
In order to confirm this hypothesis at the end of
1964
Markarian began
the
search for the galaxies showing an excess of UV
radiation in their central parts. All the observations were carried out
with the 40" Schmidt telescope of Byurakan observatory. On Markarian
initiative two additional 1.5 and 3
prisms were prepared and the
telescope
optics
was
changed for the new one, corrected for the
blue- violet spectrum region. It was the first successful experiment of
using a
small-angle
objective prism in search for extragalactic
objects. It should be noted, that an objective prism was successfully used in astronomy
since the beginning of the XX century
for spectral classification of stars. High resolution prisms having
angles
in
the range of 8-12 and a reciprocal linear dispersion of
100-250 A/mm at H
were commonly used. The spectra were widened up to
0.3-0.5 mm, the telescope losses being 8-10 , as compared with the
direct photography. Therefore, for studying of the faint galaxies
this procedure was worthless.
Markarian used a prism of low dispersion (1800 A/mm
at
H )
and obtained
unwidened spectra on which the galaxy nuclei were
easily detectable on the background of the surrounding matter, especially
if an UV-continuum excess was present in it. A high spectral
resolution was not required for spectral classification and the limiting magnitude on the searching plate reached 17-17.5 .
In 1965-1966 70 new galaxies with
strong
UV-continuum
(Markarian, 1967, 1968) were detected. The detected objects got further
the names "Markarian galaxies".
During
the
following
years two
more lists of galaxies with strong UV-continuum (Markarian, 1969a,
b) were compiled and their general number became 302.
In 1969 Markarian and Lipovetsky have iniciated a full spectral survey of the northern sky in the high galactic latitudes (The
First Byurakan Survey - FBS).
The purpose of the Survey was to select the
galaxies
with
UV- continuum
and
to look for active galactic nuclei (AGN),
i. e. preliminary spectral classification of all of them.
During
the
Survey the quasar candidates among stellar objects and the blue
stars of high galactic latitudes were marked also. The observational
program
of
the FBS
was
completed in 1978.
The studying of
plates, the search and selection of objects were continued up to 1980.
More than 2500 photographic plates were obtained and
about
40 millions spectral images were visually examined. The survey consists
of 1133 fields of 4 x4 in size and covered the sky area
of
17000
square degrees. FBS, the first survey in the world, carried out
with the purpose of search for active galaxies, was for
many
years
the single source for new Sy galaxies and other types of AGN.
Among Markarian galaxies there are
quasi-stellar objects, Sy
galaxies, BL Lacs, sources of radio, IR and X-ray emissions.
The main results of the Survey are published in the series
of
15 papers
including 1500 objects (Markarian 1967, 1969a, b; Markarian, Lipovetsky, 1971, 1972, 1973, 1974, 1976a, b; Markarian et
al., 1977a, b; 1979a, b, c; 1981).
Besides obtaining the survey plates and object selections it was
very important to get their slit spectra as well.
The first spectral observations, carried out in USA (Weedman, Khachikian, 1968, 1969), have led to the detection of 8 new Sy
galaxies and have shown a high efficiency of the
used
search
procedure.
Since 1969, parallel
to the Survey, the authors began
regular spectral observations in order to find out the physical nature
of the detected galaxies.
Before 1977 the slit spectra of Markarian galaxies were
obtained
in the
USSR
mainly with the three telescopes: 1.25-m of the South
Station of Sternberg Astronomical institute; 2.6-m of the Crimean
astrophysical observatory, and 0.7-m, of the Astrophysical institute,
Alma-Ata. Since 1977 the main part of
spectral
observations
was
made
with the 6-m telescope of SAO USSR AS. The spectra of more
than 600 galaxies were obtained. In all, the authors have obtained the
spectra
of
about
1200 objects
of FBS. Some of them were reobserved, because the observations made with small telescopes sometimes
had not the necessary quality for redshift determination. Thus, up to
nowadays there are spectral data for almost all galaxies.
The successful use of an objective prism for studying
faint
objects iniciated a new direction in extragalactic astronomy - systematic search for new objects using a low-dispersion
spectroscopy.
This
method was intensively used in the whole world surveys such as:
Cerro-Tololo Survey (Smith, 1975; Smith et al.,
1976;
MacAlpine,
Lewis, 1978), Michigan Survey (MacAlpine et al., 1977a, b, c,); Case
Survey (Pesch, Sanduleak, 1983; Sanduleak, Pesch, 1984; 1987), the
Survey
of
emission
galaxies (Wasilewski,
1983).
Most widely
this method was used with large telescopes when a grism for search
for quasars was designed (Hoag, 1976).
During the last 20 years several hundred
papers
appeared
in
which they
reported
the
data on study of Markarian galaxies. For
futher investigations of these objects a combined
catalogue
with
main observational
data
is necessary. It is also necessary to
correct various errors that appeared
during
the
performing
of
such
large program.
Such a catalogue was recently compiled by
Mazzarella and Balzano (1986). It includes a part of observational
data, and a wide bibliography on Markarian galaxies. In this connection the authors do not present all the references in
order
to
avoid
duplicating.
Our Catalogue contains the main information
presented in the lists (but corrected and supplemented) of original
data on
spectra
available
for 99 % of
objects.
A detailed
description of FBS and some statistical results of the investigation,
made
on
the
basis
of the Catalogue, concerning
the
Survey
completeness, luminosity function, spatial distribution, search for
different types of AGN and etc. were reported by Lipovetsky (1986,
1987), Lipovetsky et al. (1987).
It should be noticed also that at present a second part of the
Survey data
is being prepared. It will include blue stellar objects
which were selected earlier by us. Their number totals some thousands.
The continuation of the FBS is
the
Second
Byurakan
Survey
(SBS) carried
out in the Byurakan observatory (Markarian et al.,
1983a). The data of 6 fields are
published
already
(Markarian,
Stepanian,
1983, 1984a, b; Markarian et al., 1985b, 1986; Stepanian
et al., 1987). All the fields are 4 x4 in size and locate in
=+59 ,
+55 , +51 . The
work on compiling the Catalogue of SBS objects has
been already begun.
Below we describe the procedure of observations and
processings,
the Survey
areas,
the
object selection and classification criteria, the selection effects and the Catalogue of Markarian galaxies.
The Catalogue of FBS objects is the result of the long time work.
The work
was
still
in
progress when in 1985 B. E. Markarian
died. The authors concluded the compilation of the Catalogue which
they dedicated to the memory of their teacher.
2. OBSERVATIONS AND PROCESSING
All the observational data (low-dispersion plates)
were
obtained
with the 40-52" Schmidt telescope of the Byurakan observatory in the
period from 1965 till 1978. This instrument is the most fast
one
among other large Schmidt telescopes. Its main parameters are:
- the aperture of the main mirror is 1300 mm;
- the focal length - 2123 mm;
- the aperture of the corrector - 1000 mm;
- the scale - 97"/mm;
- non-vignetted angular field - 4 x 4 ;
- the maximum size of the photographic plates - 160x160 mm;
- three objective prisms: 1.5 , 3 , 4 with an aperture of 1000 mm.
Due to a Piazzi-Smith lens the telescope has a
flat
field.
The optics
is
made
of uviol glass and the optical system is
corrected for the blue spectrum range. The objective prisms can rotate
in the position angle, that allows to obtain spectra of any orientation. As a rule, for the Survey a 1.5 prism with a dispersion of
1800 A/mm at H
was used.
All plates were obtained on
panchromatic
emulsions
of
"F"
type.
Different
modifications of emulsions (Kodak IIAF, Eastman
Kodak AF, 103aF, IIF) were used since the Survey continued for
rather
long time.
The authors
tried to use the plates with most similar
spectral sensitivity, because even small variations could cause some
selection effects.
Table 1 presents all the types of the emulsions
used and their characteristics. In order to preserve the homogeneity
of data, different plates were calibrated on the same objects.
The plates were visually examined (entire scanning) using
7
lens.
All
the
suspected
peculiar
spectra were marked; these
spectra were compared with Palomar Observatory Sky Survey (POSS)
charts.
Such a procedure
allows
to
take
into
consideration
the
spectrum overlaps, plate deffects, and also to compare spectral and
direct images.
Comparing three images (spectral and direct on the
blue
and
red Palomar
charts) we succeeded in selecting the most compact,
almost starlike galaxies, which were impossible to find using only one
direct image. The description of objects in this case is as follows: "the object does not differ from a star, but the spectral image
is
slightly inferior
to
stars in intensity". It was possible
owing to the high contrast of Palomar charts and the presence of a high
gradient
on the spectral images.
Such are the features of many
distant Sy galaxies (z>0.06) and near QSO.
The whole Survey was performed in several stages by three
observers.
The main verification of plates, as a rule, was made by
one observer; the classification of objects was done by all together.
While compiling the next lists we used only the data verified
using the available
plates;
therefore, the published data were
incomplete according to all the main parameters of the objects:
location, brightness,
spectral
types and etc. This fact was always
emphasized by the authors in publications, because
such
incompleteness could cause serious errors in statistical data analysis.
The coordinates of the selected objects were measured on POSS
charts using
the reference bright stars and galaxies from Zwicky et
al. (1961- 1967) with the known coordinates. The accuracy of the
coordinate determination
was
1' in declination, and 0.1 in right
ascension. The angular sizes of objects were determined on red POSS
charts, using
10 lens. The general description of objects was made
from both spectral and direct images.
3. THE SURVEY AREAS AND ITS STRUCTURE
The Survey was carried out in two
sky
areas,
northern
and
southern galactic
hemispheres. The lower Survey boundary was
=
-11 (b
>0 ) and
=-15 (b >0 ). It covers the sky zones of 4
in
width, located in declination; each zone consists of fields equal
to the plate size of 4 x 4 (full plate size is 4 20'). The field overlap is 10'- 30'. The prism was oriented so that the spectra were
locating along the declination axis in order to diminish the
telescope guiding influence on the spectral resolution.
The Survey areas and the number of fields in each zone are
in Table 2.
given
Above the given areas the whole sky was
observed
in
high
galactic latitudes
(b >30 ).
In
the
area free from Galactic
absorption the Survey covers up to b
=25-30 , in some cases up to
about b
10 .
Due to technical reasons the pole area is observed
in the zone +88 30' with a large overlap and the area higher than
=
+75 ,
in
this
connection, is shifted by 1 to the south. About
2500 plates were obtained during the Survey.
Table 1. Photographic emulsions and their characteristics.
========================================================================
Period
Emuls. Expos.
Short characteristics of used plates
year
type
(min)
-----------------------------------------------------------------------1965-1967
Kodak 35-40 thick glass-backed, fine-grained, the limit
IIAF
is 17.5 on best plates, developer - D-19
1969-1971
- " -
60-80
1972-X.1972
Eastman 12-15
Kodak
IIaF
XI.1972-1973 103aF
9-10
old plates (1965-67), increased grain, low
sensitivity, the limit up to 1971 is 16.5
fine-grained, thin glass (0.8 mm), the red
spectrum part is slightly shortened, low
UV-sensitivity, the limit is 16.5-17
rough-grained, thin glass-backed, the limit 16.5
fine-graind, thin glass, low UV-sensitivity,
shortened red part, telescope diaphragm is
0.85 meter
fine-grained, high contrast, 1.2 mm glass
without antihalo layer, spectral sensitivity
is close to Kodak IIAF (England), the limit
is 17
- " - " -, with antihalo layer
II.1973-1974
IIaF
18-23
1974-IX.1974
IIF
40-45
1974-1975
IIaF
18-23
1976-II.1977
IIaF,
IIF
103aF
40-50
40-50
10-13
- " - " -, 0.85 m diaphragm used for polar
sky regions
1977-VI.1977
IIaF
IIF
18-20
25-30
hypersensitized by air heated, the
limit is 17.-17.5, developer - MWP-2
1977-VI.1979
IIF
10-13
fine-grained, hypersensitized in N
-----------------------------------------------------------------------4. PARAMETERS OF THE TWO-DIMENSIONAL CLASSIFICATION
OF GALAXIES WITH UV-CONTINUUM
The selection procedure, suggested by Markarian (1967), is the
most outstanding one by its efficiency and simplicity. As a main
search feature Markarian suggested to use the intensity of UV emission
of a galaxy. In this
way
selected
are the objects with an
excess, for their morphological type, UV-emission in the central
parts or nuclei. So, more exactly, one ought to name them "galaxies
with an excess UV-continuum".
Visual search for objects is rather simple and is
performed
on
the basis of spectral and direct images. It is necessary to have at
least one spectral plate and two POSS charts. Both spectral and
morphological features
are used in this procedure. The classification
features were suggested by Markarian (1967, 1969 a, b).
The classification parameters are as follows:
- the degree of emission condensation to the galaxy centre;
- the intensity of UV-emission in the region shorter than 4000 A;
- some auxiliary features.
Table 2. Right ascensions of the Survey areas.
===============================================================
Zone
Areas
Numbers
Areas
Numbers
DEC.
R.A.
of fields
R.A.
of fields
--------------------------------------------------------------+ 88 30' 0 00
24 00
5
+ 86
3 10
19 20
7
+ 82
5 48
18 32
9
+ 78
3 55
18 23
14
+ 75
3 32
18 12
16
+ 71
3 52
18 07
19
+ 67
5 20
18 00
19
+ 63
5 35
18 28
23
+ 59
5 15
18 45
27
+ 55
6 00
19 48
31
+ 51
5 59
19 11
33
+ 47
5 59
19 11
36
23 49
3 09
9
+ 43
6 10
19 10
39
21 50
3 50
18
+ 39
6 30
18 30
36
21 50
3 50
18
+ 35
6 53
18 27
36
21 56
3 38
18
+ 31
6 55
18 23
38
21 45
3 38
17
+ 27
7 00
18 28
41
22 43
2 59
15
+ 23
7 04
18 16
42
22 32
3 36
19
+ 19
7 20
18 00
40
22 00
3 20
20
+ 15
7 36
16 40
34
21 12
3 36
24
+ 11
7 52
16 40
33
20 24
3 52
29
+ 7
7 52
16 08
33
21 23
5 22
32
+ 3
8 08
16 07
32
20 23
5 22
36
- 1
8 08
16 07
32
20 23
5 22
36
- 5
8 23
15 52
30
20 23
5 07
35
- 9
8 23
16 22
32
20 23
5 07
35
- 13
20 23
5 07
35
-------------------------------------------------------------
The first parameter is determined by the object profile
widths
on low-dispersion plates and is designated by characters: "s" (stellar), "d" (diffuse) and their intermediate ones "sd" or "ds".
The objects with star-like nuclei or almost
star-like
objects
are reffered
to "s" type. On plates of a good quality the halfwidth
of the brightness profiles for such objects is of the order of 2".
The objects whose brightness profiles have halfwidths
of
6"-8"
and more,
depending on the galaxy size, are reffered to "d" type.
While selecting this type the most difficult problem is to
exclude
irregular galaxies
Irr I.
For them the main feature is almost
"flat" profile without narrowing to UV spectral part, since
emission
goes from the large disk, but not from the nucleus.
In this classification intermediate types "s/sd", "ds/d" and etc.
are used
as
well.
The estimations of two experienced observers
differ not more than 1 subclass. Evidently, there is
a
strong
influence
of
bad images on this parameter, thus, the observer is
obliged to compare the dimness of a galactic nucleus with that of a
star.
The second classification parameter,
the
intensity
of
UVemission from the nucleus or the central part of a galaxy, is characterized by correlation of red and blue spectrum part lengths on panchromatic
emulsion
(which
are separated
by the fall-off in the
green). For A0-A2 star with Kodak IIAF emulsion (England) these parts
have equal extension. According to their UV intensity all the objects
are divided into 3 classes: 1, 2, 3. Class I - the blue spectrum part;
it is one and a half times longer than the red one. Class 3 - the
lengths of these two parts are equal, class 2 - intermediate.
The procedure is rather correct for similar spectral sensitivities
of plates.
The
coorelation
of the blue and red spectral part
lengths slightly depends on the object brightness, it is determined
by
the spectrum
slope. When using other types of emulsions, as
Kodak IIaO, IIIaJ, which have no green fall-off, the search is greatly
complicated.
In this case it is necessary to use another parameter,
that
is
the spectrum
length which strongly depends on the object brightness. In general one ought to consider the energy
distribution
in
the
whole wavelength range being under study. The spectrum can be
represented as a totality of 20-40 independent points (at 1800 A/mm
dispersion at H ).
Besides two main classification
liary features are used:
parameters
a
number
of
auxi-
- existence of emission: "e, e:" - sure or suspected emission. It is
called an auxiliary one because it cannot be a selection criterium.
On our spectra the following emission lines or line groups are
distinguished: H + [NII]
6548/84, H + [OIII]
4959+5007,
H , [OII] 3726/29.
- difference of the energy distribution from the thermal one. An
asterisk marks a candidate into Sy type galaxy; two asterisks a candidate into QSO.
- additional
features,
which
are
usually
presented
in the object
description, for instance, morphological features,
multiple systems, interaction features, etc.
inherence to
This classification scheme is now accepted as a basic one in most
of survey
works. It allows easily to introduce new parameters
for description of emission lines and include new subclasses of
objects. So, for example, in the Second Byurakan Survey the authors
have introduced a new type of emission line galaxies without UVcontinuum: se, de.
The considered classification scheme used in searching for peculiar objects allows to select a great number of different types of
them:
- galaxies with UV-continuum;
- emission galaxies of all kinds (HII galaxies also including);
- emission parts of bright galaxies (association; HII regions);
- star-like nuclei of bright galaxies;
- blue stars with B-V > 0
types);
and U-B < -0.5
(white dwarfs of DA-DF
- QSO candidates;
- star-like galaxies with emission lines;
- some variables with flat spectra, especially of U Gem type;
- anomalous red stars (late M, R, S,), carbon stars;
- planetary nebulae.
Due to a large amount of data available and difficulties in selection of objects of
all types in a reasonable short time delay, the
Survey authors limited themthelves by the following types of objects:
1.
Galaxies with UV-continuum with m
13.0. It should be noticed,
that
in
the original lists of objects the well-known objects have been omitted;
2.
Bright galaxies with UV-continuum or star-like nuclei with UVcontinuum and m<13 , if there was a lack of spectral information at
the moment of publication.
3.
QSO candidates and quasi-stellar galaxies.
5. SELECTION EFFECTS
One of the main tasks of spectral surveys is the
creation
of a representative sample of objects with definite properties. Therefore, it is very important first to reveal, study, and, if possible, to
take into consideration
a great number of selection effects. Among
them there can be regular factors (for example, a dependence of limiting
magnitude on the declination of an object due to differences in
zenith distances and noticeable illumination of the night sky in the
south of the Byurakan observatory), and casual (the plate center has
appeared out of focus due to its deflection). The factors may be objective (the sizes of emulsion grain increase due to its ageing) and
subjective (the observer prefers stellar objects to extended ones).
There
are
effects which can be easily taken into account (casual
spectrum projecting on each other) and which are difficult to allow
for
(an influence of variable UV- transparence of atmosphere onto
classification of UV-continuum).
We describe the main selection factors and as far as
possible estimate the degree of their influence. We divided them into two
groups:
--------------------------------------------------------* Note: A second part of the Survey will include blue stellar objects
also.
-
factors, which influence the number of detected objects;
-
factors, which change their parameters.
To the first group we may refer the following selection effects.
5.1. An effect of the plate limit
This is one of the most unpleasant selection factors
in
survey
works. There are some reasons which cause essential inhomogeneities
of plate quality (emulsion type, atmosphere
transparency,
image
quality).
In this work we had no opportunity to determine the limiting magnitude for each plate. Such estimate was made only occasionally,
for instance, when using another type of emulsion. This effect
manifests it in the "spotted" galaxy distribution on the celestial
sphere. When the
surface distribution is studied a dispersion of
galaxy numbers in the areas of about 4 x4 in size increases noticeably.
The effect is
observed
also in areas of 4 x8 , since the
neighbour, according to the right ascension, fields have been very
often observed at the same night. A great number of our plates have
the limiting magnitude within the range 16.0 -17.0, and only in exceptional cases up to 15.0 or 17.5.
Allowing for other selection
effects the objects brighter than 1-1.5 the limit are detected with
confidence.
This effect cannot be practically
taken
into
consideration.
When studying the surface and spatial distribution of Markarian galaxies one ought to compile carefully the samples allowing for
the
reported
one.
The objects fainter than 16.5 are, as a rule, worthless for statistical investigation. A "working" sample
may include
objects up to 15.5 -15.7 (the limit of Zwicky catalogue) a "strict"
one must contain galaxies brighter than 15.0.
5.2. Zenith distance effect
This is also an effect of the
plate
limit,
but
is
its
"regular" component. It is caused by three factors: by strong illumination of the night sky in the south-east of the Byurakan observatory,
by the towns of Erevan and Ashtarak, by deterioration of the image at
noticeable zenith distances, by decrease of UV-transparency (cutting of
the blue
spectrum end). The two last reasons influence the object
distribution according to their types as well. For statistical investigations it is
necessary to
limit the sample in declination
approximately up to
=0 for the areas in the south and
=75
- in
the north.
The
last limitation is caused by the position of
the Galactic plane and noticeable spectra widened on the plate due to
field rotation (errors of the telescope polar axis installation).
5.3. "Stellar nucleus" effect
This rather specific effect is caused by the fact that star-like
nuclei of
bright galaxies were included into the Survey. It is evident that a galaxy of 13 , with a nucleus of 16-17 , is
already
at
the
detection limit.
The number of such objects depends upon the
magnitude of the whole galaxy. This effect exists within
the
whole
range of apparent magnitudes.
So, in order to establish a homogeneous sample up to the given limiting magnitude the objects with
large differences in galaxy and nucleus brightness should be omitted. As a rule such objects had the following description in the
lists: "starlike nucleus of a bright galaxy, the data refer to
the nucleus". However, the number of such objects in the Catalogue is
relatively small (a few percents).
5.4. Star projection effect
This effect, contrary to the previous
ones,
increases
the
number
of selected objects. It consists in the following: a star
with a rather early spectrum is projected onto the region of the center
of
a
galaxy creating an impression of a powerful star-like object;
or images of 2-3 close stars make an impression of a compact
galaxy.
This
effect
is rather strong at low latitudes and is fully taken
into account in the spectral observations. All such objects are not
included
into
the Catalogue. Markarian 914 is out also; it is an
emission star related to LkH
233 nebula. It is evident that projection of a star onto the galaxy may cause an object loss while searching. Though the probability of this fact is small, nevertheless, we
note that due to this reason a good Sy 1 galaxy - Arakelyan 564 was
lost. Its nucleus spectrum is masked with the bright star, located
northward.
5.5. Image quality influence on condensation degree
The effect reveals itself in two ways: uncertainty in classification
of "s/sd"
objects
if
the
images
are of poor quality
("ds/d" estimate becomes more probable), and also the loss of fainter
star-like
objects due
to
their
contrast decrease by spectral
enlargement. In both cases the number of "s/sd" objects among all
objects has decreased.
5.6. Zenith distance influence on UV-continuum estimate
A decrease of UV-transparency of the atmosphere
with
the
increase
of zenith
distance influences the UV-intensity estimate
and leads to its systematic underestimation at great zenith distances.
The influence of this and the previous effect is shown in Fig. 3.
It presents the number of different classification types depending upon
the declination.
5.7. "Observer" effect
All plates were examined by three observers: B. E. Markarian,
V. A. Lipovetsky,
and J. A. Stepanian.
Although their estimates
are in agreement, a "selection" effect remains.
Our
observations
have
shown that the "observer" effect in FBS is rather small and in
most cases it can be neglected. A good agreement of our
data
is
confirmed
by
the distribution of the number of objects, classified
by each of the observers, presented in Table 3 and also by the approxi-
mate constancy of the AGN number revealed in each of lists (9-11%).
Only having in mind the afore-mentioned selection effects one can
use the data of Markarian objects for various statistical investigations.
Table 3. Subclass distribution from the data of various observers.
==================================================================
!Percentage of objects with classification
No. of
Observer
!
s+sd
1
2
e
e:
objects
-----------------------------------------------------------------Markarian
!
46.7
28.4
36.3
21.6
40.2
306
Lipovetsky
!
48.6
10.8
46.5
34.0
31.5
599
Stepanian
!
44.8
10.5
33.0
27.8
28.0
306
3 observers !
43.2
9.2
30.0
30.0
38.5
307
together
!
==================================================================
6. THE CATALOGUE DESCRIPTION
Markarian galaxy Catalogue contains initial data
of
all
objects: precise coordinates, angular sizes, and spectral types.
the
Observational results of slit spectra, UBVand
IR-photometry
IRAS results,
morphological types and some other data are also
included into the Catalogue. While compiling the Catalogue we reexamined
the object lists, excluded false repetitions, rough errors
etc., and included additional objects. These ones were well-known earlier and, therefore, not marked in the lists, but detected independently by us on the plates and agreed with all selection criteria.
Below we describe in detail
Catalogue presented in Table 7.
the
parameters
of
FBS
object
1 - name of galaxies
2, 3 - coordinates (1950.0)
Since all Markarian galaxies were
observed
with
radiotelescopes, their precise coordinates were measured by some authors. We
present them in the Catalogue:
Lists
I
VI VIII
IX XII XV
Objects
V
VII
XI
XIV
1
508
701
798
1096
1400
- 507
- 700
- 797
- 1095
- 1399
- 1500
Sources
Peterson, 1973
Kojoian et al., 1978
Foltz et al., 1980
Kojoian et al., 1981a
Kojoian et al., 1981b
Kojoian et al., 1984
4 - redshifts
The redshifts corrected for the Galaxy rotation
are
given,
the rotation constant is Q=300 km/s, (there are other values in the
literature, but all of them are reduced to one system).
5 - apparent magnitudes
Apparent magnitudes are taken from the CGCG
1961 - 1968).
For
convenience, in controlling
(Zwicky
et
al.,
the data we did not
introduce corrections to apparent magnitudes for
reduction
into
other
systems. When there were no values in CGCG, the original estimates of the authors were presented. In the column 5 these values are
marked with asterisks.
6 - absolute magnitudes
In order to calculate the absolute magnitudes M (the
value
H=75km/s/Mpc
is taken everywhere) a correction for absorption in the
Galaxy
m =0.24 csc (b) is introduced.
M
= 5
(z
) + 43.0 -
m - m
7 - angular size
The sizes in angular seconds are measured
and taken from the lists of UV-galaxies.
on
red
POSS
charts
8 - spectral classification
The spectral type is given according to the lists
of
galaxies
with UV-continuum, in some cases it is corrected when we had the new
plates of better quality.
9 - redshift sources
Since for many galaxies there are several determinations of redshift, we present the single reference for our value. As a rule, we
give the most exact value. Note, that in our publication series of
spectral observation with the 6-m telescope (Markarian et al., 1980a,
b; 1983a; 1984a), the corrections for the Galaxy rotation were calculated in a wrong way. But the Catalogue gives the right values.
10 - name of galaxies
The asterisk indicates the double objects having the same
number
in the original lists; there is a more detailed information about
the second component in the Comments to Table 7.
11 - morphology
Morphological description, taken from the literature,
(Hubble
or Vaucouleurs classification) is presented, as a rule, for near and
bright galaxies according to Huchra (1977), de Vaucouleurs et
al.
(1976), Nilson
(1973),
Mazarella and Balzano (1987). In some
cases the description "dbl" is used for close binaries.
12 - spectrum type
Sy1-Sy2
Sy3
QSO
BL
SB
HII
e
a
-
Sy galaxy of the corresponding type;
LINER;
quasar;
lacertides;
star-burst galaxies;
extragalactic HII region;
emission spectrum galaxy;
absorption spectrum galaxy.
The two last notations have been
used
necessary information about their spectra.
when
there
was
no
13 - diaphragm size
The diaphragm size is given in arcseconds.
several diaphragms we present the largest one.
When
there
are
14-16 - UBV-photometry
If there are several data we give
The variability is noticed in remarques.
the
most
exact
value.
17 - UBV-photometry sources
The photometry reference is
the Catalogue.
given
for
objects,
presented
in
18 - variability
The symbol "v" indicates the optical variability.
19-22 - IRAS-flux at 12, 25, 60 and 100 mk
7. CONCLUSION
The Catalogue contains 1515 records corresponding to 1512 objects,
as
3 of them were included by mistake twice. The 15 galaxies, not
included in the lists according to reasons
mentioned
above,
are
added into the Catalogue. The added objects are presented in Table 5.
While compiling the Catalogue, 40 objects were deleted; 11
out
of them are projections: galaxy+star, 29 objects are stars (mainly
white dwarfs and subdwarfs). The list of deleted
objects
is
given
in Table 6.
So, the available sample of Markarian galaxies contains
1469
objects.
The
distribution
of
these
objects
according to
their classification types and spectral types is the following:
Table 8 presents other names of
Markarian
galaxies
included
into various
catalogues
and
lists. For convenience of search for
Markarian galaxies according to other names the Table 9 presents
the
finding list of common names, some references for the seldom-met names
being omitted. Below we give the list of object names. The list of objects according to Markarian numbers are given in Table 10.
Table 4a. Distribution of FBS objects according to the
classification type.
===================================================================
s
sd
ds
d
1
2
3
e
e: no emission
------------------------------------------------------------------298
365
351
456
193
596
681
442
493
534
------------------------------------------------------------------Table 4b. Distribution of FBS objects according to the
spectral type.
===================================================================
Sy1 Sy1.5 Sy1.8 Sy1.9 Sy2 Sy3 Sy? QSO BL SB HII
e
a
-------------------------------------------------------------------
100
12
6
7
50
17
6
13
3 95
26 903 185
------------------------------------------------------------------Table 5. Added Survey galaxies.
===========================================================
Object
R.A.
DEC.
m
Type
Other names
----------------------------------------------------------1501
0 8 0.
10 42
15.7
s1e:
III Zw 2
1502
0 51 0.
12 25
14.3
s1e
I Zw 1
1503
1 19 24.
- 1 18
14.4
s2e
II Zw 1
1504
2 52 26.4 - 0 23 12
13.7
s3e:
N1144
1505
3 16 30.
41 20
12.4
s1e
N1275
1506
4 30 30.
5 15
14.3
s1e
3C 120
1507
11 37 48.
28 40
14.5
d3e
Haro 27
1508
13 56 25.2
37 41 48
13.7
s2e
N5394
1509
14 15 43.2
25 22 0
13.1
s1e
N5548
1510
14 15 43.7
26 38 34
14.2
sd3e:
I4397
1511
15 28 48.
7 38
14.3
s1e:
N5940
1512
15 32 13.2
15 21 36
13.3
d3e
N5953 + N5954
1513
21 30 0.
9 56
14.6
s1e
II Zw 136
1514
23 0 44.4
8 36 18
13.1
s1e
N7469
1515
23 40 48.
28 13
15.7
s2
IV Zw 163
-----------------------------------------------------------7.1. Key to the list of common names
AB,B
Ark
Arp
B2
BB
-
3C,5C CG
CP
IG
Haro
Holm
HZ
I
KUG
-
LB
N
OC-OZ
PB
-
PG
T
Ton
-
U
UM
-
VV
Was
Zw
-
Braccesi UV-excess objects: Braccesi et al., 1968, 1970.
Arakelian galaxies: Arakelian, 1975.
Arp galaxies: Arp, 1966.
the Second Bologna catalogue of radio sources.
Asiago Survey of blue objects at high galactic latitudes:
Barbieri, Benvenuti, 1974.
Cambridge radio catalogues.
the Case low-dispersion northern sky survey: Pesch, Sanduleak,
1983, 1986; Sanduleak, Pesch, 1984, 1987.
Catalogue of isolated pairs of galaxies: Karachentsev, 1972.
Catalogue of isolated galaxies: Karachentseva, 1973.
Haro blue galaxies: Haro, 1956.
Holmberg galaxies: Holmberg, 1937.
Humason-Zwicky objects: Humason, Zwicky, 1947.
(IC): Index Catalogue.
Kiso Survey for UV-excess galaxies: Takase, Miyauchi-Isobe,
1984, 1985a, b, 1986a, b, 1987a, b.
Luyten blue objects: Luyten, 1955-1969.
(NGC): a New General Catalogue.
Ohio radio sources.
the Palomar-Berger survey for UV-excess objects: Berger, 1977,
1980, 1984.
Palomar-Green UV-excess stellar objects: Green et al., 1986.
isolated triplets of galaxies: Karachentseva et al., 1979.
Tonantzintla blue stellar objects: Iriarte, Chavira, 1957.
Chavira, 1958, 1959; Haro, Luyten, 1962.
(UGC) Uppsala Galaxy Catalogue: Nilson, 1973.
Curtis-Schmidt Michigan University Survey: MacAlpine et al.,
1977a, b, c; MacAlpine, Lewis, 1978; MacAlpine, Williams, 1981.
Atlas of interacting galaxies: Vorontsov-Velyaminov, 1959.
Wasilewski galaxies: Wasilewski, 1983.
Zwicky compact objects: Zwicky, 1971.
Table 6. Deleted Survey objects.
==============================================================
Object
R.A.
DEC.
m
Type ref. Spectrum
-------------------------------------------------------------959
0 40 33.9
39 32 49
15.1 s2e: 48
galaxy + star
351
0 55 13.5
28 7 14
16.
s3e: 48
galaxy + star
574
1 42 2.3
11 27 30
16.5 sd1e: 45
star
362
1 45 7.7
23 24 47
14.5 s1e: 28
star
578
1 49 3.7
7 3 22
16.
s2
45
star
371
2 45 13.8 - 1 7 47
16.
s1
28
star
377
7 10 53.2
74 6 0
16.
s1e: 28
star
80
7 39 36.0
64 54 1
17.
d3e: 45
galaxy + star
381
7 49 34.3
58 22 50
17.5 s1
28
star
1213
8 11 35.3 - 0 13 5
15.3 s2e
47
galaxy + star
388
8 25 37.5
25 30 0
16.
s1e
28
star, Ton 323, AT Cnc
1217
8 27 55.8 - 4 14 18
17.
s1e: 47
galaxy + star
392
8 56 10.6
33 8 47
15.
s1
28
star = G 047-018, WD
393
9 5 47.4
60 31 37
17.
s1
28
star
107
9 16 59.6
71 45 22
14.7 d3e:
= Mrk 20
396
9 21 11.7
35 29 43
15.5 s1e: 28
star
112
9 24 35.6
48 17 50
16.5 d3
48
galaxy + star
113
9 25 22.1
62 54 7
14.5 s2
43
star
1265 10 46 58.0
23 6 12
17.
d1e: 52
galaxy + star
1278 11 1 56.7
39 4 19
17.
s1e: 45
star
1290 11 17 22.9 - 5 34 35
15.5 sd3
99
galaxy + star
425 11 31 7.8
64 26 57
16.
s1
45
star
643 11 53 45.0
17 41 39
16.
sd3
52
stars, star + star
436 12 11 39.9
37 1 36
16.
s2e
45
star
437 12 13 15.9
41 8 47
16.
s1e: 45
star
1318 12 16 36.5
4 7 58
14.5 ds1e
= Mrk 49
227 12 45 57.8
51 15 20
16.
s3e: 52
star
228 12 46 26.2
42 9 29
16.5 s2
45
star
448 12 59 8.8
30 19 40
17.
s1e: 45
star
252 13 18 14.4
55 39 40
17.
s2
45
star
791 13 30 12.3
10 45 49
17.
s3
52
galaxy + star
457 13 30 48.9
39 16 50
16.
sd3
52
star
458 13 32 14.5
40 21 36
16.
s2e
45
star
460 13 42 3.3
40 15 10
16.
s1e: 45
star
488 13 59 25.1
52 6 51
15.4 sd2e: 52
galaxy + star
677 14 17 30.1
36 22 23
17.
sd2e: 28
star
1491 14 37 6.4
3 43 59
16.5 d2e: 52
galaxy + star
690 15 44 31.4
18 52 38
16.5 sd1e: 28
star
495 16 2 3.7
26 12 44
15.5 s2e: 45
star
502 16 53 21.4
64 9 45
15.5 s3
52
galaxy + star
890 16 55 7.4
63 19 11
15.1 ds2
= Mrk 503
505 17 19 47.5
39 45 0
15.5 sd2
48
galaxy + star
511 21 7 42.1 - 1 48 45
15.
s2
45
star
914 22 32 28.3
40 24 32
13.5 sd3e: 48
star = L H 233
525 23 1 39.3
1 28 32
17. * s3
52
star
320 23 17 36.0
26 49 57
16.5* s1
28
star
327 23 34 35.1
23 02 34
15.7 s2e
52
galaxy + star
==============================================================
8. ACKNOWLEDGEMENTS
The authors want to thank V. G. Lipovetskaya and O. M. Neizvestnaya for their help in compiling the Catalogue, checking and preparing the data for computer, Yu. I. Izotov and I. Ju. Izotova for the
help in compiling the data of IRAS fluxes, J. M. Mazzarella and
V. Balzano for providing an opportunity to look through their catalogue, W. Keel, J. Huchra and D. E. Osterbrock for giving the data on
spectral results of some Markarian galaxies. The authors also thank
V. S. Oskanian for discussion and reduction English version of text.
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