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We present a study of the elemental depletion in the interstellar medium. Wecombined the results of a Galatic model describing the gas physical conditionsduring the formation of dense cores with a full-gas-grain chemical model.During the transition between diffuse and dense medium, the reservoirs ofelements, initially atomic in the gas, are gradually depleted on dust grains(with a phase of neutralisation for those which are ions). This process becomesefficient when the density is larger than 100~cm$^{-3}$. If the dense materialgoes back into diffuse conditions, these elements are brought back in thegas-phase because of photo-dissociations of the molecules on the ices followedby thermal desorption from the grains. Nothing remains on the grains fordensities below 10~cm$^{-3}$ or in the gas-phase in a molecular form. Oneexception is chlorine, which is efficiently converted at low density. Ourcurrent gas-grain chemical model is not able to reproduce the depletion ofatoms observed in the diffuse medium except for Cl which gas abundance followsthe observed one in medium with densities smaller than 10~cm$^{-3}$. This is anindication that crucial processes (involving maybe chemisorption and/or iceirradiation profoundly modifying the nature of the ices) are missing.

monthly notices of the royal astronomical society

Influence of galactic arm scale dynamics on the molecular composition of  the cold and dense ISM III. Elemental depletion and shortcomings of the  current physico-chemical models