The use of galaxy clusters as cosmological probes relies on a detailed
understanding of their properties. We aim to update the spectroscopic cluster
identification of CODEX by running the spectroscopic group finder on the
follow-up spectroscopy results and connecting the dynamical state of clusters
to their scaling relations. We implemented a reproducible spectroscopic
membership determination and cleaning procedures, based on the redMaPPer
membership, running the spectroscopic group finder on the follow-up
spectroscopy results and cleaning the membership for spectroscopic outliers. We
applied the Anderson-Darling test for velocity substructure and analysed its
influence on the scaling relations. We also tested the effect of the
X-ray-to-optical centre offset on the scaling relations. We report on the
scaling relations between richness, X-ray luminosity, and velocity dispersion
for a complete sample of clusters with at least 15 members. Clusters with
velocity substructure exhibit enhanced velocity dispersion for a given richness
and are characterized by 2.5 times larger scatter. Clusters that have a strong
offset in X-ray-to-optical centres have comparable scaling relations as
clusters with substructure. We demonstrate that there is a consistency in the
parameters of the scaling relations for the low- and high-richness galaxy
clusters. Splitting the clusters by redshift, we note a decrease in scatter
with redshift in all scaling relations. We localize the redshift range where a
high scatter is observed to z<0.15, which is in agreement with the literature
results on the scatter. We note that the increase in scatter for both high- and
low-luminosity clusters is z<0.15, suggesting that both cooling and the
resulting active galactic nucleus feedback are at the root of this scatter.
Abridged.Comment: 23 pages, A&A in press, catalogs are released through CD