Astron. Astrophys. 345, 233-243 (1999) 5. AnalysisFigs. 4a-d show four examples of the observed spectra. A glance of the figures reveals that the spectra are heavily line-blanketed by the absorption due to ^{12}CN together with the strong absorption due to ^{13}CN. The spectra shown in the figures are normalized by the fictitious continuum level, which is drawn so that it should travel through the highest point in the region observed and assumed to be constant over the region. In fact, the change of flux level predicted by the blackbody of 3000 K is 3% over 230 Å, and therefore, this assumption is reasonable.
The line positions of the ^{12}CN red system are given in Davis & Phillips (1963). For ^{13}CN, Wyller (1966) analyzed (2,0) and (3,1) bands of the red system and listed the positions of 437 lines. The lines of ^{13}CN are located at the wavelengths by about 40 Å longer than the corresponding lines of ^{12}CN due to the isotope effect. The -value of each ^{12}CN line is calculated as described in Paper I. The -values of ^{13}CN lines are reasonably assumed to be identical with those of the corresponding ^{12}CN lines. We determine ratios using the iso-intensity method. For lines due to ^{12}CN and ^{13}CN, the logarithms of central depths normalized by the fictitious continuum level are plotted against , where is a line intensity predicted using the weighting function method (e.g. Cayrel & Jugaku 1963). can approximately be written in the form of , where is the lower excitation potential (LEP) of a line, and is a kind of weighted mean of the reciprocal excitation temperature in the line forming region. Paper II discusses the calculation of and the effects of model atmospheres on it in detail, and we will not repeat them here. Fig. 5 shows examples of the iso-intensity method. The horizontal shift between the two curves for ^{12}CN and ^{13}CN gives the ratio of the abundance of ^{12}CN to that of ^{13}CN, namely, ratio. The two curves for ^{12}CN and ^{13}CN are quite close to each other, demonstrating that ratios in J-type carbon stars are very low. As Fig. 5 shows, we selected about 10 lines of ^{12}CN and 2 lines of ^{13}CN which are expected not to have their central depths affected by the adjacent lines. However, only several lines could be found for the stars whose spectra show very strong ^{13}CN lines. Some lines are blended with other lines of the same isotopic species at almost the same wavelength. We used such lines, if the blending lines are weak enough, considering their -values and LEP's.
It is very difficult to determine the true continuum level in such heavily line-blanketed spectra as shown in Figs. 4a-d. It should be kept in mind, however, that ratios are derived from the horizontal shifts between the two curves of ^{12}CN and ^{13}CN, namely, the ratios are determined basically from the lines of ^{12}CN and ^{13}CN with the same intensity. In other words, the absolute values of central depths, which should be measured with respect to the true continuum, do not matter. The point is that the central depths measured with respect to the fictitious continuum level is a kind of measure of line intensities, and that they serve to recognize that the lines of ^{12}CN and ^{13}CN are of iso -intensity. Thus, the resulting ratios are not affected by the location of the fictitious continuum level, as long as it is assumed to be constant over the region observed. The spectral synthesis method, which is often used in the analyses of complicated spectra, is not applied in the present work. In fact, such analyses cannot be justified unless a spectral range wide enough to reach some points of the true continuum is used, since synthetic spectra are usually normalized by the true continuum. The uncertainties of the resulting ratios amount to about 20%. For several stars, the uncertainties are much larger, about 50%. The internal errors, which result from the scattering of the lines plotted in the curves-of-growth, dominate the total errors. The effect of changing model parameters is quite minor. An increase or decrease in the effective temperature by 200 K leads to no noticeable change in the resulting ratios. The adoption of the models with C/O = 1.1 and 2.0, instead of C/O = 1.3, neither gives any noticeable changes. © European Southern Observatory (ESO) 1999 Online publication: April 12, 1999 |