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In a survey of archived ultraviolet spectra of 100 stars recorded by theechelle spectrograph of the Space Telescope Imaging Spectrograph (STIS) on theHubble Space Telescope (HST), we measure the strengths of the weak absorptionfeatures of O I, Ge II and Kr I in the interstellar medium. Our objective is toundertake an investigation that goes beyond earlier abundance studies to seehow these elements are influenced independently by three differentenvironmental properties: (1) values of a generalized atomic depletion factor$F_*$ due to condensations onto dust grains (revealed here by the abundances ofMg and Mn relative to H), (2) the fraction of H atoms in the form of molecularhydrogen, $f({\rm H}_2)$, and (3) the ambient intensity $I$ of ultravioletstarlight relative to an average value in our part of the Galaxy $I_0$. Asexpected, the gas-phase abundances of all three elements exhibit negativepartial correlations with $F_*$. The abundances of free O atoms showsignificant positive partial correlations with log $f({\rm H}_2)$ and $\log(I/I_0)$, while Ge and Kr exhibit negative partial correlations with $\log(I/I_0)$ at marginal levels of significance. After correcting for these trends,the abundances of O relative to H show no significant variations with location,except for the already-known radial gradient of light-element abundances in theMilky Way. A comparison of Ge and O abundances revealed no significant regionalenhancements or deficiencies of neutron-capture elements relative toalpha-process ones.

A Closer Look at Some Gas-Phase Depletions in the ISM: Trends for O, Ge, and Kr vs. $F_*$, $f({\rm H}_2)$, and Starlight Intensity