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Gives the barycentric radial velocity (in km/s) derived from fitting a gaussian to the profile obtained from cross-correlating the extracted s2d spectrum with a numerical mask. Masks exist for F0 and K0 spectral types. Additional masks for A and M stars have been used.

For fast rotators or spotted stars, simple gaussians may not give a good fit.

Gives the sigma of the gaussian fitted to the cross-correlation profile. Note that the FWHM of the profile is given by 2.354 times 'sigma'. The CCF was computed over a velocity interval selected by the user (normal, large, extra-large). The normal step is 1 km/s over a ± 70 km/s interval centered on a value set by the user (between -300 and 300 km/s). The width of the CCF can be used to obtain the rotational velocity of the star,

Gives the amplitude of the gaussian curve fitted to the cross-correlation profile. This is a good approximation to the depth of the CCF dip. It is expressed as a fraction relative to the CCF continuum. The surface of the CCF profile can also be used to derive a metal abundance. See Santos et al. (2002).

Normalized CCF continuum

Reduction user's manual

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