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Rastinejad, J. C.; Fong, W.; Levan, A. J.; Tanvir, N. R.; Kilpatrick, C. D.; Fruchter, A. S.; Anand, S.; Bhirombhakdi, K.; Covino, S.; Fynbo, J. P. U.; Halevi, G.; Hartmann, D. H.; Heintz, K. E.; Izzo, L.; Jakobsson, P.; Kangas, T.; Lamb, G. P.; Malesani, D. B.; Melandri, A.; Metzger, B. D.; Milvang-Jensen, B.; Pian, E.; Pugliese, G.; Rossi, A.; Siegel, D. M.; Singh, P.; Stratta, G.
The Astrophysical journal, 06/2024, Letnik: 968, Številka: 1Journal Article
Abstract The existence of a secondary (in addition to compact object mergers) source of heavy element ( r -process) nucleosynthesis, the core-collapse of rapidly rotating and highly magnetized massive stars, has been suggested by both simulations and indirect observational evidence. Here, we probe a predicted signature of r -process enrichment, a late-time (≳40 days post-burst) distinct red color, in observations of gamma-ray burst supernovae (GRB-SNe), which are linked to these massive star progenitors. We present optical to near-IR color measurements of four GRB-SNe at z ≲ 0.4, extending out to >500 days post-burst, obtained with the Hubble Space Telescope and large-aperture ground-based telescopes. Comparison of our observations to models indicates that GRBs 030329, 100316D, and 130427A are consistent with both no enrichment and producing 0.01–0.15 M ⊙ of r -process material if there is a low amount of mixing between the inner r -process ejecta and outer supernova (SN) layers. GRB 190829A is not consistent with any models with r -process enrichment ≥0.01 M ⊙ . Taken together the sample of GRB-SNe indicates color diversity at late times. Our derived yields from GRB-SNe may be underestimated due to r -process material hidden in the SN ejecta (potentially due to low mixing fractions) or the limits of current models in measuring r -process mass. We conclude with recommendations for future search strategies to observe and probe the full distribution of r -process produced by GRB-SNe.
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