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Chemical elements in the hot medium permeating early-type galaxies, groups,and clusters make them an excellent laboratory for studying metal enrichmentand cycling processes in the largest scales of the universe. Here, we reportthe analysis by the XMM-Newton Reflection Grating Spectrometer of 14 early-typegalaxies, including the well-known brightest cluster galaxies of Perseus, forinstance. The spatial distribution of the O/Fe, Ne/Fe, and Mg/Fe ratios isgenerally flat at the central 60 arcsecond regions of each object, irrespectiveof whether or not a central Fe abundance drop has been reported. Commonprofiles between noble gas and normal metal suggest that the dust depletionprocess does not work predominantly in these systems. Therefore, observedabundance drops are possibly attributed to other origins, like systematics inthe atomic codes. Giant systems of high gas mass-to-luminosity ratio tend tohold a hot gas ($\sim$ 2 keV) yielding the solar N/Fe, O/Fe, Ne/Fe, Mg/Fe, andNi/Fe ratios. Contrarily, light systems at a subkiloelectronvolt temperatureregime, including isolated or group-centered galaxies, generally exhibitsuper-solar N/Fe, Ni/Fe, Ne/O, and Mg/O ratios. We find that the latestsupernova nucleosynthesis models fail to reproduce such a super-solar abundancepattern. Possible systematic uncertainties contributing to these high abundanceratios of cool objects are also discussed in tandem with the crucial role offuture X-ray missions.

O, Ne, Mg, and Fe Abundances in Hot X-Ray-emitting Halos of Galaxy Clusters, Groups, and Giant Early-type Galaxies with XMM-Newton RGS Spectroscopy