Magmatic gas with high Cl/H2O and/or S/H2O is of particular relevance to planetary bodies such as Mars. Upon cooling, such gas precipitates phases similar to the ”alteration” phases observed in vugs and fractures in martian rocks. When deposited on ash, they can impart the characteristic volatile-enriched signature of martian fines. Importantly, as these precipitates form in the absence of liquid water, recognition of the signature of this process would provide insights into the evolution of the martian surface water budget. Experiments were conducted to assess trace element behavior during magmatic degassing as a potential signature of this process. Low pressure experimental degassing of P-rich basaltic magma containing Cl, Br, S, OH and trace elements (Sr, Ge, Ga, Zn, Pb, Rb, Cs, Se, Cu, La, and Lu) demonstrates that magmatic gas can transport trace metals from magmas to planetary surfaces where, upon cooling, they become incorporated into vapor-deposited Cs-Pb-Zn-Rb-bearing halides, Ge-Ga-bearing iron oxides, Zn-Se-Cu-bearing sulfides, sulfates, and Ge-bearing silicates and form native metals. Low-OH, high Cl magmatic gas produces a variety of halides but Fe-oxide formation is inhibited. Higher magmatic OH content facilitates Ca loss from the melt and the precipitation of Ca-phosphates but generally limits metal transport from the magma. S-rich gas facilitates the formation of vapor-deposited sulfates and Zn-Cu-Se bearing sulfides. In the presence of atmospheric moisture however, much of the magmatic vapor-deposited load will deliquesce, producing locally an acidic brine that, upon desiccation, may produce new minerals, but with the same overall bulk major and trace element signatures.