2 Observations and photometry

The galaxies were observed on February 4-6, 1995 with a CCD camera of the 2.56 meter Nordic telescope at La Palma with a seeing of 0.7-1.3 arcsec. A TK CCD chip provided a view field of 3$\times3\hbox{$^\prime$}$ with a resolution of $0.176\hbox{$^{\prime\prime}$}$/pixel. The exposure times in different filters are shown in Table 1 for each galaxy. Equatorial standard stars from Landolt (1992) were observed for calibration. Photometry of stellar objects in the galaxies were carried out with MIDAS using ALLSTAR DAOPHOT package (Stetson 1987). The frames were debiased, dark-subtracted and flat-fielded. After transfering instrumental magnitudes into the standard Johnson-Cousins system we derived B, V, I magnitudes with a typical error which is expected to be about 0.05 mag. In the case of the galaxy NGC 4449, having a very crowded stellar field, we repeated photometry after subtracting its frame smoothed with a median filter. The results of our stellar photometry are presented in Tables 3-7, which can be found in a computer-readable form at the CDS.

  

Table 1: Observational log