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chi Lupi Data Table Descriptions

Column Title Explanation
Wavelength Range The wavelength coverage of the observation in the rest frame of the primary star.
Observation Rootname The designation given to given to this set of observations by STScI and used in the HST archive.
Reduced Data The observed flux and statistical errors as a function of wavelength are given here. Data has been coadded using standard GHRS data reduction procedures and shifted in wavelength so that features in the primary star's spectrum are approximately aligned with the laboratory scale. Obvious photocathode blemishes have been omitted in this coaddition.
Synthetic Spectra Synthetic spectra for both the primary and secondary stars were calculated using KURUCZ's SYNTHE code. Modifications to the default Kurucz line list are discussed in Leckrone et al. (1999) and Brandt et al. (1999). The secondary flux was then shifted in wavelength by the amount appropriate for the velocity difference between the components at the start time of the observation, scaled assuming that R A / R B = 1.67, coadded and normalized.
Line ID List These line identification lists were calculated using version 42 of the Synspec code of Ivan Hubeny and Thierry Lanz which is distributed as part of their TLUSTY model atmosphere program. The columns in these data files give for each line: the wavelength, ion id, log gf, lower level excitation energy (in cm-1), ratio of line to continuum opacity at the continuum formation level, a rough analytic estimate of the line's equivalent width, and a symbol that scales with this estimate.
Atlas Fig. # The number given here corresponds to the figure number given in Brandt et al. (1999) and gives a link to a postscript version of that figure. For wavelengths with duplicate coverage we give additional figures not included in Brandt et al. (1999). As presented here, each figure covers two pages.

In each figure, the solid line shows the observed GHRS spectrum as given in the third column of this table. The dotted line shows the combined synthetic spectra for both the primary and the secondary stars, including both rotational and instrumental broadening. The dashed line shows the synthetic spectrum for the secondary alone, also with rotational and instrumental broadening included. The labeled wavelength scale is aligned with the laboratory wavelengths used in the synthetic spectrum of the primary star. Vacuum wavelengths are given below 2010 Å, and air wavelengths above this. The observed GHRS data have been shifted in wavelength to align with the combined synthetic spectra. We have only adjusted the zero point offset of the wavelength calibration, although in some cases a small change in the dispersion might have improved the fit. A description of the default wavelength calibration procedure for the GHRS can be found in Robinson et al. (1992).

The horizontal arrow below the second and fourth panel of each figure shows the amount and direction that the secondary's wavelength is shifted with respect to the labeled wavelength scale. Wavelengths updated using Fourier Transform Spectrometer (FTS) data from the University of Lund or from Imperial College, London have been marked with an "f". Ion names are marked with a "*" if there is additional discussion or information regarding this line either Leckrone et al. (1999) or Brandt et al. (1999). For explanations of other symbols, see Brandt et al.

Where a known laboratory line coincides with an unmodeled feature in the observed data, we have marked the line using an italic font. However, these should be considered as suggested identifications only.