A Hubble Space Telescope Search for r-Process Nucleosynthesis in Gamma-Ray Burst Supernovae

J. C. Rastinejad, W. Fong, A. J. Levan, N. R. Tanvir, C. D. Kilpatrick, A. S. Fruchter, S. Anand, K. Bhirombhakdi, S. Covino, J. P.U. Fynbo, G. Halevi, D. H. Hartmann, K. E. Heintz, L. Izzo, P. Jakobsson, T. Kangas, G. P. Lamb, D. B. Malesani, A. Melandri, B. D. MetzgerB. Milvang-Jensen, E. Pian, G. Pugliese, A. Rossi, D. M. Siegel, P. Singh, G. Stratta

Research output: Contribution to journalArticlepeer-review

3 Scopus citations

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.

Original languageEnglish (US)
Article number14
JournalAstrophysical Journal
Volume968
Issue number1
DOIs
StatePublished - Jun 1 2024

Funding

Moving forward, to identify or place deep constraints on the r-process in rare classes of CCSNe requires significant effort and resources on both the theoretical and observational end. The development of observational predictions for r-process-enriched collapsar and MR SNe (or newly developed theories) is critical to establishing these sources as sites from photometric color measurements alone. Further late-time color and/or spectroscopic observations of GRB-SNe, SNe Ic-BL, and potentially, superluminous SNe (e.g., Reichert et al. ) will provide additional measurements or upper limits of their r-process yields. Though spectroscopic observations, especially with JWST, are critical to definitively establishing these events as sites of r-process element production, color measurements are possible for a greater volume of GRB-SNe, improving our understanding of the distribution of ejecta masses. Dedicated programs on space-based facilities, such as HST and JWST, are necessary for this late-time NIR follow-up. With unprecedented sensitivity in the NIR bands, the upcoming Nancy Grace Roman Space Telescope will be a critical facility for this field. Finally, these studies of some of the most promising candidates for r-process enrichment are not possible without the continued and ensured detection of well-localized GRBs by satellites such as Swift and its successors. Acknowledgments Observations reported here were obtained at the MMT Observatory, a joint facility of the University of Arizona and the Smithsonian Institution. MMT Observatory access was supported by Northwestern University and the Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA). This work is based on observations collected at the European Organization for Astronomical Research in the Southern Hemisphere. This research has made use of NASA's Astrophysics Data System. The Fong Group at Northwestern acknowledges the support of the National Science Foundation under grant Nos. AST-1909358, AST-2206494, AST-2308182, and CAREER grant No. AST-2047919. W.F. gratefully acknowledges support from the David and Lucile Packard Foundation, the Alfred P. Sloan Foundation, and the Research Corporation for Science Advancement through Cottrell Scholar Award 28284. Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award No. DD3-24139X issued by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. G.P.L. is supported by a Royal Society Dorothy Hodgkin Fellowship (grant Nos. DHF-R1-221175 and DHF-ERE-221005). G.S. and P.S. acknowledge the support of the State of Hesse within the Research Cluster ELEMENTS (Project ID 500/10.006). E.P. acknowledges financial support through INAF Fundamental Research grant 2022. L.I. was supported by an INAF Fundamental Research grant 2023. S.A. acknowledges support from the National Science Foundation GROWTH PIRE grant No. 1545949. This work is based on observations made with the NASA/ESA HST, obtained from the data archive at the Space Telescope Science Institute (STScI). STScI is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5-26555. All of the HST data presented in this article were obtained from MAST at STScI. The specific observations analyzed can be accessed via MAST.

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

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