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AST-1138766We thank the referee for suggestions that improved the presentation of our results. This publication is based upon work supported by Program No. HST-GO-14766, provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. J.D.S. was also partially supported by the National Science Foundation, under grant AST-1714873.B.M.P. was supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship, under award AST-2001663. A.F. acknowledges support from NSF grant AST-1716251.Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A & M University, Financiadora de Estudos e Projetos, Fundacao Carlos Chagas Filho de Amparoa Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico and the Ministerioda Ciencia, Tecnologia e Inovacao, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the Dark Energy Survey.The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenossische Technische Hochschule(ETH) Zurich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciencies de l'Espai (IEEC/CSIC), the Institut de Fisica d'Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universitat Munchen and the associated Excellence Cluster Universe, the University of Michigan, NSF's NOIRLab, the University of Nottingham, the Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A & M University, and the OzDES Membership Consortium.Based in part on observations at Cerro Tololo Inter-American Observatory at NSF's NOIRLab (NOIRLab Prop.ID 2012B-0001; PI: J. Frieman), which is managed by the Association of Universities for Research in Astronomy(AURA), under a cooperative agreement with the National Science Foundation.The DES data management system is supported by the National Science Foundation under grant Nos. AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE ispartially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council, under the European Union's Seventh Framework Program(FP7/2007-2013), including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciencia e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2).This manuscript has been authored by Fermi Research Alliance, LLC, under Contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics.This research has made use of NASA's Astrophysics Data System Bibliographic Services.The HST data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope Science Institute. The specific observations analyzed can be accessed via doi:10.17909/y62d-3794.

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Timing the r-process enrichment of the ultra-faint dwarf galaxy Reticulum II

Publicated to:ASTROPHYSICAL JOURNAL. 944 (1): 43- - 2023-02-01 944(1), DOI: 10.3847/1538-4357/aca9d1

Authors: Simon, JD; Brown, TM; Avila, RJ; Mutlu-Pakdil, B; Ji, AP; Drlica-Wagner, A; Frieman, J; Gutierrez, G; Kuropatkin, N; Scarpine, V; Martínez-Vázquez, CE; Li, TS; Balbinot, E; Bechtol, K; Frebel, A; Geha, M; Hansen, TT; James, DJ; Pace, AB; Aguena, M; Rosell, AC; da Costa, LN; Gschwend, J; Pieres, A; Santiago, B; Alves, O; Andrade-Oliveira, F; Gerdes, DW; Tarle, G; Weaverdyck, N; Bacon, D; Vincenzi, M; Bertin, E; Brooks, D; Doel, P; Burke, DL; Kind, MC; Gruendl, RA; Paz-Chinchón, F; Carretero, J; Miquel, R; Costanzi, M; De Vicente, J; Mena-Fernández, J; Rodriguez-Monroy, M; Sanchez, E; Sevilla-Noarbe, I; Desai, S; Everett, S; Ferrero, I; García-Bellido, J; Gatti, M; Raveri, M; Gruen, D; Hinton, SR; Hollowood, DL; Honscheid, K; Kuehn, K; Marshall, JL; Palmese, A; Pereira, MES; Malagón, AAP; Smith, M; Suchyta, E; Wilkinson, RD

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Abstract

The ultra-faint dwarf galaxy Reticulum II (Ret II) exhibits a unique chemical evolution history, with 72-12+10 r-process elements. We present deep Hubble Space Telescope photometry of Ret II and analyze its star formation history. As in other ultra-faint dwarfs, the color-magnitude diagram is best fit by a model consisting of two bursts of star formation. If we assume that the bursts were instantaneous, then the older burst occurred around the epoch of reionization, forming & SIM;80% of the stars in the galaxy, while the remainder of the stars formed similar to 3 Gyr later. When the bursts are allowed to have nonzero durations, we obtain slightly better fits. The best-fitting model in this case consists of two bursts beginning before reionization, with approximately half the stars formed in a short (100 Myr) burst and the other half in a more extended period lasting 2.6 Gyr. Considering the full set of viable star formation history models, we find that 28% of the stars formed within 500 +/- 200 Myr of the onset of star formation. The combination of the star formation history and the prevalence of r-process-enhanced stars demonstrates that the r-process elements in Ret II must have been synthesized early in its initial star-forming phase. We therefore constrain the delay time between the formation of the first stars in Ret II and the r-process nucleosynthesis to be less than 500 Myr. This measurement rules out an r-process source with a delay time of several Gyr or more, such as GW170817.

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