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Long-slit spectra in the range 3600-8000 ÅÅ were obtained
during three runs. The spectra were
centered on a star-like object at
to the west and
to the south of
the galaxy center.
The spectrograph SP-124 at the Nasmyth-1 focus of the 6 m telescope with UAGS
camera and Photometrix CCD PM1024 (
m pixel size) was used
for the observations.
The spatial scale along the slit was equal to
/pixel, the slit length was
about
,
and a slit width of
was used.
Gratings with 300 and 600 grooves/mm were used, resulting in
a spectral resolution of approximately 12 and 6 Å (FWHM).
Series of bias images were obtained twice -- at the
beginning and at the end of every night. Dark current and
flat field were usually accumulated at the end of the night.
At least two standard stars from the list of spectrophotometric
standards (Massey and Strobel, 1988) were observed every night.
A He-Ne-Ar lamp was used for wavelength calibration.
In Table1 the instrumental set-ups are presented for spectral observations of SN1998bv and the galaxy HS1035+4758. The spectroscopic data were reduced using the context LONG from the MIDAS software package. The reduction of the original two-dimensional CCD data included the standard steps such as bias and dark subtraction, flat-fielding, cosmic-ray removal. After wavelength mapping, the night sky background subtraction was performed. 1D spectra were extracted by adding some consecutive CCD rows centered on the object intensity peak along the slit. Then corrections for atmospheric extinction and flux calibration were applied. For the flux calibration we used the mean response curve obtained from the observations of standard stars.