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It has been suggested that a class of chemically peculiar metal-poor starscalled iron-rich metal-poor (IRMP) stars formed from molecular cores with metalcontents dominated by thermonuclear supernova nucleosynthesis. If thisinterpretation is accurate, then IRMP stars should be more common inenvironments where thermonuclear supernovae were important contributors tochemical evolution. Conversely, IRMP stars should be less common inenvironments where thermonuclear supernovae were not important contributors tochemical evolution. At constant $[\text{Fe/H}] \lesssim -1$, the Milky Way'ssatellite classical dwarf spheroidal (dSph) galaxies and the Magellanic Cloudshave lower $[\text{$\alpha$/Fe}]$ than the Milky Way field and globular clusterpopulations. This difference is thought to demonstrate the importance ofthermonuclear supernova nucleosynthesis for the chemical evolution of the MilkyWay's satellite classical dSph galaxies and the Magellanic Clouds. We use datafrom the Sloan Digital Sky Survey (SDSS) Apache Point Observatory GalacticEvolution Experiment (APOGEE) and Gaia to infer the occurrence of IRMP stars inthe Milky Way's satellite classical dSph galaxies $\eta_{\text{dSph}}$ and theMagellanic Clouds $\eta_{\text{Mag}}$ as well as in the Milky Way field$\eta_{\text{MWF}}$ and globular cluster populations $\eta_{\text{MWGC}}$. Inorder of decreasing occurrence, we find$\eta_{\text{dSph}}=0.07_{-0.02}^{+0.02}$,$\eta_{\text{Mag}}=0.037_{-0.006}^{+0.007}$,$\eta_{\text{MWF}}=0.0013_{-0.0005}^{+0.0006}$, and a 1-$\sigma$ upper limit$\eta_{\text{MWGC}}<0.00057$. These occurrences support the inference that IRMPstars formed in environments dominated by thermonuclear supernovanucleosynthesis and that the time lag between the formation of the first andsecond stellar generations in globular clusters was longer than thethermonuclear supernova delay time.

The Dependence of Iron-rich Metal-poor Star Occurrence on Galactic Environment Supports an Origin in Thermonuclear Supernova Nucleosynthesis