This sample of galaxies was taken from the catalogue of Godwin et al.
(1983; hereafter GMP), which lists all galaxies down to magnitude 
in a 2.63 degree square area, centered on the Coma cluster. We
selected all the galaxies down to magnitude 
, within one
degree from the cluster center whose morphological type is not published
in Paper I. Furthermore we reobserved all SAB0 galaxies (i.e. S0s for
which the presence of a bar is uncertain) and unE (i.e. Es where boxiness
or diskiness is undetermined) observed under mediocre seeing conditions by
Andreon et al. (1996), as well as other galaxies of borderline type
between two classes. We discarded from the observations 3 galaxies (GMP
978, 1646, 1741) which do not belong to the Coma cluster, as they have
velocities
of more than 4000 km s-1 relative to the
cluster center. Figure 1 (click here) shows the spatial
distribution of the
Coma galaxies. With the present sample, all (187) galaxies brighter than
mag in the surveyed area have been observed.
Figure 1: The galaxies of the Coma sample. Full and open circles represent galaxies whose
morphological type is presented in this paper and in Paper I, respectively.
The size of the circles is proportional to the magnitude of the galaxy. The radius
of the field is one degree. There are 187 galaxies in this field. The
morphological types of 59 of them are presented in this paper, and the others can
be found in Paper I
The galaxies of this sample were first inspected on two Schmidt plates, OCA
#2849 and OCA #2842, taken at the Calern Observatory and kindly provided by
C. Pollas. These plates were digitized at the MAMA with a 5
and 10 micron (= 0.33 '' and 0.65'') step respectively, and with
an aperture of 10 microns. The digitization produces image files with pixel
readings proportional to plate density.
All galaxies with evident asymmetric or irregular isophotes or with spiral arms were classified as S and eliminated from further observations with CCDs. We nevertheless already had CCD images for half of them, because they were published by other authors or in the field of view of other program galaxies. The CCD images confirm the type estimates based on our Schmidt plates for all galaxies; this confirms the reliability of this method for classifying obvious spiral galaxies, even at the distance of the Coma cluster.
Finally, we found 5 galaxies in our CCD-image archives which had not been classified in Paper I; these 5 were not reobserved.
Three suspected spiral galaxies were observed in December 1994 with the
TBL, and the remaining 28 galaxies were observed during one observing run
in February 1995 with the same instrument and setup. The CCD was a
Tektronics 
, with a pixel size of 
corresponding
to 0.30 arcsec on the sky. The seeing was 1.0- 1.1 arcsec (FWHM) and the
nights were photometric. The exposure time was 20 minutes for all
galaxies. With the present observations, the median seeing of the complete
sample reduces from 1.48 arcsec in Paper I to 1.2 arcsec, which is a large
improvement since less than one third of the sample had been observed.
This corresponds to a restframe resolution of 0.75 Kpc, not very different
from the resolution that the Hubble Space Telescope offers for
distant (
) galaxies.
The sample is composed of all (141) galaxies listed in the Zwicky
catalogue (Zwicky 1961-1968) in a box of 
centered on 
, 
to which we added two
Tifft (1977) galaxies. NGC 1233 is listed twice in the Zwicky catalogue (Zw
525-6, Zw 524-65). Three galaxies (Zw 525-21, Zw 540-65 and Zw 541-19)
certainly do not belong to the cluster because their velocity relative to
the cluster center is larger than 4000 km s-1; they were eliminated
from the list of galaxies to be observed, together with all galaxies whose
morphological type is listed in Poulain et al. (1992). Note
however that some of the observed galaxies might still be fore- or
background objects, in particular some of the galaxies for which the
radial velocity is unknown or some galaxies in the outskirts of the
studied region and with intermediate relative velocities with respect to
the cluster center. Figure 2 (click here) shows the
spatial distribution of the galaxies in the studied region.
Figure 2: The galaxies of the Perseus sample. Full and open circles represent
galaxies whose morphological types are presented in this paper
and in Poulain et al. (1992), respectively.
The size of the circles is proportional to the magnitude of the galaxy. The size
of the studied region is 
. There are
139 galaxies in this field. The morphological types
of 80 of them are presented in this paper, and the others can be found in
/cite[Poulain et al. (1992)]Pou92
54 of these galaxies were first inspected on Schmidt plate OCA #2977
taken at the Calern Observatory in December 1992 and digitized, as the
preceding one, at the MAMA with a 5 micron (= 0.33 '') step and with
an aperture of 0.65''. The remaining galaxies are outside the region
covered by our plate. All the galaxies were further inspected on the
Digitized Palomar Sky Survey. Obvious spiral galaxies were classified as such and eliminated
from the list of galaxies to be observed in CCD.
We found images of 3 galaxies in our CCD-image archives which had not been classified by Poulain et al. (1992); they were not reobserved.
Finally, we observed in CCD almost all galaxies not classified as S. Five
observing runs (35 nights) at TBL were used for completing this sample,
since bad weather, technical problems with the filter wheel and with data
aquisition, and the pear-shaped PSF of many images, made the completion of
the program very slow, largely compensating the good luck of Poulain
et al. (1992). During the first 3 runs (February 1993, December
1993, February 1994) we used a Thompson CCD with a pixel
size of 
corresponding to 0.24 arcsec on the sky and the galaxies
were observed in the Gunn r filter and calibrated in the Cousin R
filter, to make the measures consistent with those of Paper I. During the
last two runs (December 1994 and February 1995) the CCD was the same
Tektronics as for the Coma sample and we observed the
galaxies in Johnson V.
Thanks to the fact that the sample is largely composed of obvious spirals, whose large-scale spiral structure is visible even on defective images (missing pixels, pear-shaped PSF, unidentified filter), we were able to collect images of sufficient quality for the morphological classification of all but 4 galaxies (Zw 540-73, 540-80, 540-83 and 525-36).
For the first three galaxies, we only used our Calern plates, whose densities had been transformed into intensities by means of a contour to contour correspondence between plate-image output and CCD-image intensity for a set of galaxies, as we did in Paper I. Plate OCA #2977, like those used for Coma galaxies, is a Kodak panchromatic 4415 emulsion sensitive from the near UV to 6000-7000 Å and was taken without filter. The fact that its sensitivity does not match the CCD V or r band prevented us from absolutely calibrating this plate, and therefore from computing passband dependent quantities (magnitudes, radius at a given surface brightness, etc.); but, for galaxies without pronounced color gradients, such as Es, we can still compute the density to intensity transformation (in arbitrary units) without significant errors.
For Zw 525-36, we did not have any image of sufficient quality for the morphological classification, and its type remains unknown.
Table 1 (click here) details the observing log. The median seeing was 1.4 arcsec, which corresponds to a restframe resolution of 0.66 Kpc, still comparable to the resolution available with the Space Telescope for distant galaxies.
The method of analysis and the classification scheme are described in details in Paper I and references therein, and do not need to be presented anew.