{"intvolume":"       926","oa_version":"Preprint","scopus_import":"1","title":"The K2 Galactic Archaeology Program data release 3: Age-abundance patterns in C1–C8 and C10–C18","doi":"10.3847/1538-4357/ac2c83","publisher":"IOP Publishing","year":"2022","type":"journal_article","citation":{"ista":"Zinn JC, Stello D, Elsworth Y, García RA, Kallinger T, Mathur S, Mosser B, Hon M, Bugnet LA, Jones C, Reyes C, Sharma S, Schönrich R, Warfield JT, Luger R, Vanderburg A, Kobayashi C, Pinsonneault MH, Johnson JA, Huber D, Buder S, Joyce M, Bland-Hawthorn J, Casagrande L, Lewis GF, Miglio A, Nordlander T, Davies GR, Silva GD, Chaplin WJ, Silva Aguirre V. 2022. The K2 Galactic Archaeology Program data release 3: Age-abundance patterns in C1–C8 and C10–C18. The Astrophysical Journal. 926(2), 191.","mla":"Zinn, Joel C., et al. “The K2 Galactic Archaeology Program Data Release 3: Age-Abundance Patterns in C1–C8 and C10–C18.” <i>The Astrophysical Journal</i>, vol. 926, no. 2, 191, IOP Publishing, 2022, doi:<a href=\"https://doi.org/10.3847/1538-4357/ac2c83\">10.3847/1538-4357/ac2c83</a>.","ama":"Zinn JC, Stello D, Elsworth Y, et al. The K2 Galactic Archaeology Program data release 3: Age-abundance patterns in C1–C8 and C10–C18. <i>The Astrophysical Journal</i>. 2022;926(2). doi:<a href=\"https://doi.org/10.3847/1538-4357/ac2c83\">10.3847/1538-4357/ac2c83</a>","ieee":"J. C. Zinn <i>et al.</i>, “The K2 Galactic Archaeology Program data release 3: Age-abundance patterns in C1–C8 and C10–C18,” <i>The Astrophysical Journal</i>, vol. 926, no. 2. IOP Publishing, 2022.","chicago":"Zinn, Joel C., Dennis Stello, Yvonne Elsworth, Rafael A. García, Thomas Kallinger, Savita Mathur, Benoît Mosser, et al. “The K2 Galactic Archaeology Program Data Release 3: Age-Abundance Patterns in C1–C8 and C10–C18.” <i>The Astrophysical Journal</i>. IOP Publishing, 2022. <a href=\"https://doi.org/10.3847/1538-4357/ac2c83\">https://doi.org/10.3847/1538-4357/ac2c83</a>.","short":"J.C. Zinn, D. Stello, Y. Elsworth, R.A. García, T. Kallinger, S. Mathur, B. Mosser, M. Hon, L.A. Bugnet, C. Jones, C. Reyes, S. Sharma, R. Schönrich, J.T. Warfield, R. Luger, A. Vanderburg, C. Kobayashi, M.H. Pinsonneault, J.A. Johnson, D. Huber, S. Buder, M. Joyce, J. Bland-Hawthorn, L. Casagrande, G.F. Lewis, A. Miglio, T. Nordlander, G.R. Davies, G.D. Silva, W.J. Chaplin, V. Silva Aguirre, The Astrophysical Journal 926 (2022).","apa":"Zinn, J. C., Stello, D., Elsworth, Y., García, R. A., Kallinger, T., Mathur, S., … Silva Aguirre, V. (2022). The K2 Galactic Archaeology Program data release 3: Age-abundance patterns in C1–C8 and C10–C18. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ac2c83\">https://doi.org/10.3847/1538-4357/ac2c83</a>"},"day":"24","status":"public","volume":926,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","article_number":"191","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"date_updated":"2022-08-19T09:52:08Z","extern":"1","date_created":"2022-07-18T10:57:30Z","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2108.05455"}],"quality_controlled":"1","publication":"The Astrophysical Journal","month":"02","oa":1,"language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"article_processing_charge":"No","publication_status":"published","issue":"2","_id":"11601","date_published":"2022-02-24T00:00:00Z","external_id":{"arxiv":["2108.05455"]},"author":[{"last_name":"Zinn","full_name":"Zinn, Joel C.","first_name":"Joel C."},{"first_name":"Dennis","full_name":"Stello, Dennis","last_name":"Stello"},{"first_name":"Yvonne","full_name":"Elsworth, Yvonne","last_name":"Elsworth"},{"first_name":"Rafael A.","full_name":"García, Rafael A.","last_name":"García"},{"full_name":"Kallinger, Thomas","first_name":"Thomas","last_name":"Kallinger"},{"last_name":"Mathur","full_name":"Mathur, Savita","first_name":"Savita"},{"last_name":"Mosser","first_name":"Benoît","full_name":"Mosser, Benoît"},{"full_name":"Hon, Marc","first_name":"Marc","last_name":"Hon"},{"orcid":"0000-0003-0142-4000","id":"d9edb345-f866-11ec-9b37-d119b5234501","last_name":"Bugnet","full_name":"Bugnet, Lisa Annabelle","first_name":"Lisa Annabelle"},{"first_name":"Caitlin","full_name":"Jones, Caitlin","last_name":"Jones"},{"full_name":"Reyes, Claudia","first_name":"Claudia","last_name":"Reyes"},{"last_name":"Sharma","first_name":"Sanjib","full_name":"Sharma, Sanjib"},{"full_name":"Schönrich, Ralph","first_name":"Ralph","last_name":"Schönrich"},{"full_name":"Warfield, Jack T.","first_name":"Jack T.","last_name":"Warfield"},{"full_name":"Luger, Rodrigo","first_name":"Rodrigo","last_name":"Luger"},{"last_name":"Vanderburg","first_name":"Andrew","full_name":"Vanderburg, Andrew"},{"first_name":"Chiaki","full_name":"Kobayashi, Chiaki","last_name":"Kobayashi"},{"last_name":"Pinsonneault","first_name":"Marc H.","full_name":"Pinsonneault, Marc H."},{"last_name":"Johnson","first_name":"Jennifer A.","full_name":"Johnson, Jennifer A."},{"last_name":"Huber","first_name":"Daniel","full_name":"Huber, Daniel"},{"first_name":"Sven","full_name":"Buder, Sven","last_name":"Buder"},{"last_name":"Joyce","full_name":"Joyce, Meridith","first_name":"Meridith"},{"first_name":"Joss","full_name":"Bland-Hawthorn, Joss","last_name":"Bland-Hawthorn"},{"first_name":"Luca","full_name":"Casagrande, Luca","last_name":"Casagrande"},{"full_name":"Lewis, Geraint F.","first_name":"Geraint F.","last_name":"Lewis"},{"last_name":"Miglio","first_name":"Andrea","full_name":"Miglio, Andrea"},{"first_name":"Thomas","full_name":"Nordlander, Thomas","last_name":"Nordlander"},{"last_name":"Davies","full_name":"Davies, Guy R.","first_name":"Guy R."},{"first_name":"Gayandhi De","full_name":"Silva, Gayandhi De","last_name":"Silva"},{"last_name":"Chaplin","first_name":"William J.","full_name":"Chaplin, William J."},{"last_name":"Silva Aguirre","first_name":"Victor","full_name":"Silva Aguirre, Victor"}],"acknowledgement":"We would like to thank the anonymous referee whose comments significantly improved the manuscript. J.C.Z. is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-2001869. J.C.Z. and M.H.P. acknowledge support from NASA grants 80NSSC18K0391 and NNX17AJ40G. Y.E. and C.J. acknowledge the support of the UK Science and Technology Facilities Council (STFC). S.M. acknowledges support from the Spanish Ministry of Science and Innovation with the Ramon y Cajal fellowship number RYC-2015-17697 and the grant number PID2019-107187GB-I00. R.A.G. acknowledges funding received from the PLATO CNES grant. C.K. acknowledges funding from the UK Science and Technology Facilities Council (STFC) through grants ST/M000958/1, ST/R000905/1, and ST/V000632/1.\r\n\r\nFunding for the Stellar Astrophysics Centre (SAC) is provided by the Danish National Research Foundation (grant agreement No. DNRF106).\r\n\r\nThe K2 Galactic Archaeology Program is supported by the National Aeronautics and Space Administration under grant NNX16AJ17G issued through the K2 Guest Observer Program. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation.\r\n\r\nThis paper includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate.\r\n\r\nParts of this research were supported by the Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), through project number CE170100013.\r\n\r\nThis research was partially conducted during the Exostar19 program at the Kavli Institute for Theoretical Physics at UC Santa Barbara, which was supported in part by the National Science Foundation under grant No. NSF PHY-1748958.\r\n\r\nBased in part on data obtained at Siding Spring Observatory via GALAH. We acknowledge the traditional owners of the land on which the AAT stands, the Gamilaraay people, and pay our respects to elders past and present.\r\n\r\nThis work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement.\r\n\r\nFunding for the Sloan Digital Sky Survey IV has been provided by the Alfred P. Sloan Foundation, the U.S. Department of Energy Office of Science, and the Participating Institutions. SDSS-IV acknowledges support and resources from the Center for High-Performance Computing at the University of Utah (www.sdss.org).\r\n\r\nSoftware: asfgrid (Sharma & Stello 2016), corner (Foreman-Mackey 2016), emcee (Foreman-Mackey et al. 2013), NumPy (Walt 2011), pandas (McKinney 2010), Matplotlib (Hunter 2007), IPython (Pérez & Granger 2007), SciPy (Virtanen et al.2020).","abstract":[{"text":"We present the third and final data release of the K2 Galactic Archaeology Program (K2 GAP) for Campaigns C1–C8 and C10–C18. We provide asteroseismic radius and mass coefficients, κR and κM, for ∼19,000 red giant stars, which translate directly to radius and mass given a temperature. As such, K2 GAP DR3 represents the largest asteroseismic sample in the literature to date. K2 GAP DR3 stellar parameters are calibrated to be on an absolute parallactic scale based on Gaia DR2, with red giant branch and red clump evolutionary state classifications provided via a machine-learning approach. Combining these stellar parameters with GALAH DR3 spectroscopy, we determine asteroseismic ages with precisions of ∼20%–30% and compare age-abundance relations to Galactic chemical evolution models among both low- and high-α populations for α, light, iron-peak, and neutron-capture elements. We confirm recent indications in the literature of both increased Ba production at late Galactic times as well as significant contributions to r-process enrichment from prompt sources associated with, e.g., core-collapse supernovae. With an eye toward other Galactic archeology applications, we characterize K2 GAP DR3 uncertainties and completeness using injection tests, suggesting that K2 GAP DR3 is largely unbiased in mass/age, with uncertainties of 2.9% (stat.) ± 0.1% (syst.) and 6.7% (stat.) ± 0.3% (syst.) in κR and κM for red giant branch stars and 4.7% (stat.) ± 0.3% (syst.) and 11% (stat.) ± 0.9% (syst.) for red clump stars. We also identify percent-level asteroseismic systematics, which are likely related to the time baseline of the underlying data, and which therefore should be considered in TESS asteroseismic analysis.","lang":"eng"}],"article_type":"original"}