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We present a study on the prospects of observing carbon, sulfur, and otherlower abundance elements (namely Al, Ca, Ti and Ni) present in the interstellarmedium using future X-ray instruments. We focus in particular on the detectionand characterization of interstellar dust along the lines of sight. We comparethe simulated data with different sets of dust aggregates, either obtained frompast literature or measured by us using the SOLEIL-LUCIA synchrotron beamline.Extinction by interstellar grains induces modulations of a given photolelectricedge, which can be in principle traced back to the chemistry of the absorbinggrains. We simulated data of instruments with characteristics of resolution andsensitivity of the current Athena, XRISM and Arcus concepts. In the relativelynear future, the depletion and abundances of the elements under study will bedetermined with confidence. In the case of carbon and sulfur, thecharacterization of the chemistry of the absorbing dust will be alsodetermined, depending on the dominant compound. For aluminum and calcium,despite the large depletion in the interstellar medium and the prominent dustabsorption, in many cases the edge feature may not be changing significantlywith the change of chemistry in the Al$^-$ or Ca$^-$ bearing compounds. Theexinction signature of large grains may be detected and modeled, allowing atest on different grain size distributions for these elements. The low cosmicabundance of Ti and Ni will not allow us a detailed study of the edge features.

X-ray extinction from interstellar dust: Prospects of observing carbon, sulfur and other trace elements