I. Furenlid

A critical list of Voigt-fitted equivalent width measurements based on the solar flux spectrum

Equivalent widths of around 570 carefully selected absorption lines in the solar flux spectrum have been measured, using the Solar Flux Atlasfrom 296 to 1300 nm by Kurucz et al. The equivalent widths were derived from Voigt functions fitted to the selected line profiles in the Solar Flux Atlas. The measurements were used to determine two sets of solar log gf-values; one set is based on the solar model in the 1979 model grid by Kurucz and the other set on a similar 1990 solar model, also by Kurucz, using revised metal abundances by Anders and Grevesse. The data provide a homogeneous, high-precision reference for studies of differential stellar abundances based on equivalent widths, using the solar flux spectrum as the standard

The multi-telescope telescope : a cost-effective approach to fiber-fed spectroscopy

A spectroscopic facility is being developed to extend the Center for High Angular Resolution Astronomy program in speckle interferometry to new areas of stellar astrophysics. The facility is based on a multitelescope telescope (MTT) and a fiber-optic-fed spectrograph. The MTT is a one-meter light-collecting telescope with a primary mirror made up of nine 33.3-cm telescope mirrors. The mirrors will focus light into separate optical fibers, avoiding the loss of light associated with the dead space in conventional fiber bundles. It is estimated that the system will have an overall optical efficiency of about 2.7 percent, corresponding to a limiting magnitude of 9.4 for 1000 sec exposure, S/N = 100, and a resolution of 0.2 A/pixel. The possible applications of the system are discussed, including spectroscopic observations of binaries and nonradial pulsation in Be stars.

A VARIATION OF THE CROSS CORRELATION TECHNIQUE

A simplified, but versatile, cross-correlation technique is described. Suitable applications are determinations of radial velocities and searches for binary-star secondaries as well as interpretations of complicated spectra. The small number of operations used in defining the cross-correlation function allows the technique to be implemented in an on-line mode.