Astron. Astrophys. 326, 620-628 (1997)

4. IUE observations

The IUE observational material of  Cet consists of low and high resolution spectra, archived by the ESA Observatory at VILSPA. The images, listed in Table 2, were taken by means of the short-wavelength primary (SWP) and long-wavelength primary (LWP) cameras with high (H) and low (L) resolution modes. The pulsation phases were calculated from the following parabolic ephemeris: T (max. light) = HJD 2438385.6888 + 0.16113713 E + describing moments of the maximum light of this star (cf. Jerzykiewicz et al. 1988). The last column of Table 2 shows an exposure classification code. The VILSPA code is given by a single number corresponding to the maximum Digital Number (DN) of expositions (the saturated level occurs at DN = 255), whereas the GSFC data show both the continuum (C) and background (B) levels in DN units, respectively.

The analysed images are well exposed, and we used IUE programs developed for PC computers consisting of several graphical subroutines useful for analysis of the extracted data from the standard IUE SIPS reduction procedure. One of the advantages of our software is the possibility to select the best fit parameters for removing the blaze function of the echelle grating to improve the standard ripple correction of the high resolution images.

© European Southern Observatory (ESO) 1997

Online publication: October 15, 1997
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