Program: GS-2024A-Q-105

Gamma-ray bursts are relativistic explosions, traditionally divided into two classes at a duration of two seconds. The traditional GRB paradigm asserts that long-duration GRBs (LGRBs) are produced by the collapse of massive stars, while short-duration GRBs (SGRBs) originate in neutron star (NS) mergers. NS mergers are the sole observed site of r-process nucleosynthesis to date, with the radioactive decay of these elements producing an optical-NIR transient known as a kilonova. Gemini recently made the remarkable discovery of a kilonova following the long GRB 211211A, opening a new avenue to widen the currently small population of kilonovae (< 10). In addition, observational evidence in favor of a faster synthesis channel and theoretical simulations suggest that the counterparts to traditional LGRBs, Type Ic supernovae, may also significantly contribute the Universe's r-process budget. Here, we propose strategic follow-up of the counterpart to a nearby (z<0.2) LGRB - either a kilonova or a Type Ic supernova - to address a fundamental open question in astronomy: What are the sources of r-process elements in the Universe? Follow-up to a supernova will directly probe a new production channel, while observations of a kilonova will contribute to our understanding of their average r-process yield. We leverage Gemini's wide coverage of the Northern and Southern sky, rapid TOO capabilities and suite of instruments in our experimental design, and aim to maximize the scientific output of the next nearby LGRB. We request long-term status for 3 semesters in accordance with the expected rates of nearby LGRBs.