  Solar surface magneto-convection appears as granulation pattern that impacts
spectral lines in terms of both shape and wavelength. Such induced effects also
tend to vary over the observed solar disc because of the changing observation
angle and, thus, the changing observation height as well. Centre-to-limb
observations of the resolved Sun offer an insight into the variable spectral
behaviour across different heliocentric observing positions, providing crucial
information about limb darkening, convective velocities, and line profile
variability relevant to radial velocity (RV) calculations. Thus, RV
measurements and exoplanet transit spectroscopy depend on precise reference
templates. We want to provide a spectroscopic centre-to-limb solar atlas at
high spectral resolution and high-frequency accuracy. The atlas shall help
improve the understanding of the solar atmosphere and convection processes. We
performed high-resolution observations of the resolved quiet Sun with a Fourier
transform spectrograph at the Institut f\"ur Astrophysik und Geophysik in
G\"ottingen. Our dataset contains a wavelength range from 4200\r{A} to
8000\r{A}. We obtained 165 spectra in total, with a spectral resolution of
$\Delta \nu$ = 0.024cm$^{-1}$, corresponding to a resolving power $R$ of
700,000 at $\sim$6000\r{A}. We present a centre-to-limb solar atlas containing
14 heliocentric positions. To check for consistency, we investigated the FeI
~6175\r{A} absorption line and compared our line profiles with previous
centre-to-limb observations and also with simulations. The line profile and
also the bisector profiles are generally consistent with previous observations,
but we have identified differences to model line profiles, especially close to
the solar limb.
