HeI 10830{AA} triplet 6enter-to-limb variations

The observations cover the interval {mu}=[0.1, 1.0], where {mu} is the cosine of the heliocentric angle. At each {mu}-position, the spectra are spatially averaged over 0.02{mu}, and the resulting CLVs are given both as these averaged data points and as smooth polynomial curves fitted across each wavelength point.

The HeI spectra were inverted using the HAnle and ZEeman Light (HAZEL) code, showing an increase in optical depth towards the limb and a reversed convective blueshift for the red component, while the blue component was entirely absent. In addition, we find a strong increase in the steepness of the HeI CLV compared to that of the nearby continuum. The SiI showed a behavior more typical of photospheric lines, namely shallower CLV, a reduction in width and depth, and a more typical convective blueshift.