The James Webb Space Telescope (JWST) observed the gamma-ray burst (GRB) 221009A at +168 and +170 rest-frame days after the event, revealing a supernova (SN) similar to SN 1998bw, with no evidence of r-process nucleosynthesis. The SN, with a nickel mass of approximately 0.09 solar masses, is only slightly fainter than SN 1998bw, indicating it is not an unusual GRB-SN. This suggests that highly energetic GRBs are unlikely to produce significant r-process material, leaving open the question of whether massive star explosions are key sources of r-process elements. The host galaxy of GRB 221009A has a very low metallicity of approximately 0.12 solar masses and strong H₂ emission, consistent with recent star formation, hinting at environmental factors influencing its extreme energetics. The origin of the heaviest elements in the universe, particularly those formed by rapid neutron capture (r-process) nucleosynthesis, remains a major open question in astrophysics. Neutron star mergers have been suspected as a source, and the kilonova associated with GW 170817 confirmed this. However, recent studies suggest multiple sites for r-process nucleosynthesis, including rapidly rotating massive stars that collapse into black holes. Theoretical simulations suggest that accretion disk outflows in these 'collapsars' may reach the neutron-rich state required for the r-process. The discovery of GRB 221009A, the brightest GRB ever observed, presents a unique opportunity to search for r-process signatures in a collapsar. The SN following a long-duration GRB (LGRB) is responsible for carrying r-process material into the interstellar medium. Although early observations of GRB 221009A provided an exquisite view of the afterglow, there are conflicting claims regarding the presence of an associated SN. The search for an SN associated with GRB 221009A is crucial for understanding the origin of its extreme luminosity. JWST observations of GRB 221009A, including a near-infrared spectrum and imaging in four NIR bands, provide clear detection of an SN associated with this event and enable the search for r-process emission in a nebular-phase spectrum. These data provide a detailed NIR view of the host galaxy, enabling an assessment of environmental factors responsible for this extraordinary GRB. The SN emission is well described by a power-law afterglow, with no evidence for r-process emission. The SN is similar to SN 1998bw, with a nickel mass of approximately 0.09 solar masses. The host galaxy has a very low metallicity and strong H₂ emission, consistent with recent star formation.The James Webb Space Telescope (JWST) observed the gamma-ray burst (GRB) 221009A at +168 and +170 rest-frame days after the event, revealing a supernova (SN) similar to SN 1998bw, with no evidence of r-process nucleosynthesis. The SN, with a nickel mass of approximately 0.09 solar masses, is only slightly fainter than SN 1998bw, indicating it is not an unusual GRB-SN. This suggests that highly energetic GRBs are unlikely to produce significant r-process material, leaving open the question of whether massive star explosions are key sources of r-process elements. The host galaxy of GRB 221009A has a very low metallicity of approximately 0.12 solar masses and strong H₂ emission, consistent with recent star formation, hinting at environmental factors influencing its extreme energetics. The origin of the heaviest elements in the universe, particularly those formed by rapid neutron capture (r-process) nucleosynthesis, remains a major open question in astrophysics. Neutron star mergers have been suspected as a source, and the kilonova associated with GW 170817 confirmed this. However, recent studies suggest multiple sites for r-process nucleosynthesis, including rapidly rotating massive stars that collapse into black holes. Theoretical simulations suggest that accretion disk outflows in these 'collapsars' may reach the neutron-rich state required for the r-process. The discovery of GRB 221009A, the brightest GRB ever observed, presents a unique opportunity to search for r-process signatures in a collapsar. The SN following a long-duration GRB (LGRB) is responsible for carrying r-process material into the interstellar medium. Although early observations of GRB 221009A provided an exquisite view of the afterglow, there are conflicting claims regarding the presence of an associated SN. The search for an SN associated with GRB 221009A is crucial for understanding the origin of its extreme luminosity. JWST observations of GRB 221009A, including a near-infrared spectrum and imaging in four NIR bands, provide clear detection of an SN associated with this event and enable the search for r-process emission in a nebular-phase spectrum. These data provide a detailed NIR view of the host galaxy, enabling an assessment of environmental factors responsible for this extraordinary GRB. The SN emission is well described by a power-law afterglow, with no evidence for r-process emission. The SN is similar to SN 1998bw, with a nickel mass of approximately 0.09 solar masses. The host galaxy has a very low metallicity and strong H₂ emission, consistent with recent star formation.