next previous
Up: Relative line photometry

1. Introduction

A new method for spectrum disentangling (introduced first by Simon & Sturm 1994) which is based on the least square fit of power spectra of line profiles was recently described in Paper I (Hadrava 1995). This method proved to be a useful tool also for removing the telluric lines from the stellar spectra. Certainly, the variability of line intensities must be included for this purpose. This can be done simply by adding new free parameters specifying intensity multipliers for each exposure to the orbital elements solved by numerical minimization. However, this numerical solution is very time-consuming. It is thus more advantageous to solve for these multipliers in the way described in Sect. 2 (click here).

This generalized method has been included into a new version of the code KOREL for spectrum decomposition. Using this code to calculate the line intensities of binary components their relative change during eclipses was found (e.g. in the case of V436 Per, see Harmanec et al. 1997). This effect yields, in principle, a possibility to make photometric observations with a spectrograph. This method of "relative line photometry'' is described in Sect. 3 (click here). In consequence, it enables also a decomposition of contributions of binary components to the continuum, which is otherwise indistinguishable by spectral disentangling.

A detailed description of the code KOREL is accessible by anonymous ftp on server "'' ( in file pub/fotel/korel3.tex. The source file of the code is distributed by the author on request.

Copyright by the European Southern Observatory (ESO)