The observations of 18 dwarf irregular galaxies in Canes Venatici
were carried out in 1995 February using a TEC 1024 
1024 chip
at the prime
focus of the 2.56 m Nordic Optical Telescope (NOT) at La Palma.
The CCD size was 24.58 24.58 mm, which yielded a total field
of 3 3 arcmin.
We observed the galaxies under good seeing conditions
in Johnson B
and V bands. The observational log is presented in Table 1.
| Name | Date | Filter | Exposure | Seeing | Airmass |
| (sec) | ( ) | ||||
| UGC 6782 | 7.02.95 | B | 500 | 0.9 | 1.04 |
| V | 500 | 0.9 | 1.04 | ||
| UGC 7131 | 5.02.95 | V | 600 | 1.8 | 1.09 |
| I | 600 | 1.7 | 1.09 | ||
| UGC 7356 | 7.02.95 | V | 300 | 0.8 | 1.08 |
| B | 500 | 0.9 | 1.08 | ||
| UGC 7559 | 4.02.95 | V | 600 | 0.9 | 1.03 |
| B | 600 | 0.9 | 1.02 | ||
| UGC 7599 | 4.02.95 | V | 600 | 0.7 | 1.01 |
| B | 600 | 0.7 | 1.01 | ||
| UGC 7605 | 6.02.95 | V | 300 | 1.0 | 1.03 |
| B | 600 | 1.1 | 1.02 | ||
| UGC 7639 | 7.02.95 | V | 300 | 0.8 | 1.08 |
| B | 300 | 0.9 | 1.08 | ||
| UGC 7698 | 6.02.95 | V | 600 | 1.3 | 1.08 |
| B | 600 | 1.2 | 1.08 | ||
| UGCA 290 | 6.02.95 | V | 300 | 1.1 | 1.10 |
| B | 300 | 1.3 | 1.10 | ||
| UGCA 292 | 5.02.95 | V | 600 | 1.3 | 1.08 |
| B | 600 | 1.4 | 1.08 | ||
| UGC 7866 | 6.02.95 | B | 600 | 1.2 | 1.02 |
| V | 300 | 1.2 | 1.02 | ||
| UGC 7949 | 6.02.95 | B | 600 | 1.1 | 1.03 |
| V | 300 | 1.1 | 1.02 | ||
| UGC 8024 | 5.02.95 | B | 300 | 1.2 | 1.10 |
| V | 300 | 1.2 | 1.10 | ||
| K 215 | 6.02.95 | V | 600 | 1.0 | 1.05 |
| B | 600 | 1.1 | 1.05 | ||
| UGC 8638 | 6.02.95 | B | 600 | 1.2 | 1.03 |
| V | 600 | 1.0 | 1.02 | ||
| UGC 8651 | 5.02.95 | V | 600 | 1.4 | 1.04 |
| B | 600 | 1.5 | 1.03 | ||
| UGC 8760 | 5.02.95 | V | 600 | 1.2 | 1.01 |
| B | 600 | 1.4 | 1.01 | ||
| UGC 8833 | 5.02.95 | V | 600 | 1.0 | 1.02 |
| B | 600 | 1.4 | 1.02 |
The initial processing of the data was performed with IRAF (CCDRED package) using bias, dark and twilight flatfield frames obtained during the observing nights. Cosmic events filtering was done with CCDPHOT package.
The CCD frames of the 18 observed dwarf galaxies are presented either in B or in V band in Figs. 2-19. Most of the galaxies have been resolved into stars for the first time.
The photometry of stellar objects was carried out using MIDAS implementation
of the point spread function (PSF) photometry programs
DAOPHOT and ALLSTAR (Stetson 1987).
The PSF was obtained for each frame from bright,
well isolated stars, then PSF fitting of all stellar objects found in the
frame was performed simultaneously by ALLSTAR. Object lists
for each galaxy were combined according to positional identity
(with a deviation of no more than 1.5 pixels) of the star images in different
bands. The standard photometric error in 
and SHARP parameters of ALLSTAR
were taken into
account during the star selection process. Mostly objects with 
SHARP 
and a standard photometric error 
were kept.
Our ALLSTAR magnitudes are based on the first estimate of stellar magnitudes
with small aperture (4-8 pixels) to exclude contamination by neighbouring stars.
Therefore, an aperture correction was made. We obtained this
correction using PSF stars by plotting growth curves for each
image. All objects found,
except PSF stars, were subtracted from the images before this process.
The aperture correction was then calculated as the difference between
the asymptotic magnitude and the magnitude within a small aperture from the first
estimate in ALLSTAR. We estimate mean errors of this correction as: 
in B, in V and 
in I band.
For the calibration, the photometric standards from Landolt's
(1992) list were
observed during the run. An aperture photometry of standard
stars was done to obtain their magnitudes.
After correction for atmospheric extinction, the following
equations for transformation into Johnson-Cousins standard system were derived:
where the capital letters are Johnson-Cousins magnitudes and the small letters
are instrumental ones.
We estimate the following zero-point errors of this transformation: 
in V,
in B-V and 
in V-I. Adding quadratically these errors to those
of the aperture
correction, we obtain the resulting zero-point errors: in V,
in B-V
and 
in V-I.
The results of the stellar photometry are presented in Tables 2-19 which can
also be
accessed in computer-readable form in the CDS. All the tables are organized as follow:
(1) the ordinal number of the star; (2), (3) - 
coordinates
of the star in pixels; (4) - the apparent magnitude in V band; (5) - the
(B-V)
colour index; (6), (7) - the formal DAOPHOT error in V and (B-V)
respectively; (8) - the mean of B and V SHARP value.
To determine the total magnitude of
a galaxy, concentric circular apertures were used.
The total magnitude
in each band was defined to be the magnitude at which the curve of
growth flattened. Background stars and distant galaxies were clipped before.
We estimate the resulting error
as in B and in V.
Figure 2: The B frame of UGC 6782. As for all other images, North is top,
and East is left. The upper right corner corresponds to 
of the frame coordinates given in the tables;
X increases to East and Y to South
Figure 3: The V frame of UGC 7131
Figure 4: The V frame of UGC 7356
Figure 5: The B frame of UGC 7559
Figure 6: The B frame of UGC 7599
Figure 7: The V frame of UGC 7605
Figure 8: The V frame of UGC 7639
Figure 9: The B frame of UGC 7698
Figure 10: The V frame of UGCA 290
Figure 11: The V frame of UGCA 292
Figure 12: The B frame of UGC 7866
Figure 13: The B frame of UGC 7949
Figure 14: The B frame of UGC 8024
Figure 15: The V frame of K 215
Figure 16: The V frame of UGC 8638
Figure 17: The V frame of UGC 8651
Figure 18: The V frame of UGC 8760
Figure 19: The V frame of UGC 8833