  The study of the chemical composition of the interstellar medium (ISM)
requires a strong synergy between laboratory astrophysics, modeling, and
observations. In particular, astrochemical models have been developed for
decades now and include an increasing number of processes studied in the
laboratory or theoretically. These models follow the chemistry both in the gas
phase and at the surface of interstellar grains. Since 2012, we have provided
complete gas-phase chemical networks for astrochemical codes that can be used
to model various environments of the ISM. Our aim is to introduce the new
up-to-date astrochemical network kida.uva.2024 together with the ice chemical
network and the fortran code to compute time dependent compositions of the gas,
the ice surface, and the ice mantles under physical conditions relevant for the
ISM. The gas-phase chemical reactions, as well as associated rate coefficients,
included in kida.uva.2024 were carefully selected from the KIDA online database
and represent the most recent values. The model predictions for cold core
conditions and for when considering only gas-phase processes were computed as a
function of time and compared to the predictions obtained with the previous
version, kida.uva.2014. In addition, key chemical reactions were identified.
The model predictions, including both gas and surface processes, were compared
to the molecular abundances as observed in the cold core TMC1-CP. Many
gas-phase reactions were revised or added to produce kida.uva.2024. The new
model predictions are different by several orders of magnitude for some
species. The agreement of this new model with observations in TMC-1 (CP) is,
however, similar to the one obtained with the previous network.
