  Observations of center-to-limb variations (CLV) of spectral lines and
continua provide a good test for the accuracy of models of solar and stellar
atmospheric structure and spectral-line formation. They are also widely used to
constrain elemental abundances and are becoming increasingly important in
atmospheric studies of exoplanets. However, only a few such data sets exist for
chromospheric lines. We aim to create a set of standard profiles by means of
mosaics made with the CRISP and CHROMIS instruments of the Swedish 1-m Solar
Telescope (SST), as well as to explore the robustness of said profiles obtained
using this method. For each spectral line we use a mosaic that ranges from the
center to the limb. Each of these mosaics are averaged down to 50 individual
spectral profiles, spaced by 0.02 in the $\mu$ scale. These profiles are
corrected for p-mode oscillations, and their line parameters (equivalent width,
line shift, full-width at half-maximum, and line depth) are then compared
against literature values where possible. We present a set of 50 average
profiles that are spaced equidistantly along the cosine of the heliocentric
angle ($\mu$) by steps of 0.02 for five continuum points between 4001 and 7772
\AA, as well as ten of the most commonly observed spectral lines at the SST (Ca
II H & K, H$\beta$, Mg I 5173 \AA, C I 5380 \AA, Fe I 6173 \AA, Fe I 6301 \AA,
H$\alpha$, O I 7772 \AA, and Ca II 8542 \AA). Center-to-limb variation of line
profiles and continua are shared in the CDS as machine-readable tables;
providing a quantitative constraint on theoretical models that aim to model
stellar atmospheres.
