Evidence for a Chandrasekhar-mass explosion in the Ca-strong 1991bg-like type Ia supernova 2016hnk

Aims. We present a comprehensive dataset of optical and near-infrared photometry and spectroscopy of type Ia supernova (SN) 2016hnk, combined with integral field spectroscopy (IFS) of its host galaxy, MCG -01-06-070, and nearby environment. Our goal with this complete dataset is to understand the nature of this peculiar object. Methods. Properties of the SN local environment are characterized by means of single stellar population synthesis applied to IFS observations taken two years after the SN exploded. We performed detailed analyses of SN photometric data by studying its peculiar light and color curves. SN 2016hnk spectra were compared to other 1991bg-like SNe Ia, 2002es-like SNe Ia, and Ca-rich transients. In addition, we used abundance stratification modeling to identify the various spectral features in the early phase spectral sequence and also compared the dataset to a modified non-LTE model previously produced for the sublumnious SN 1999by. Results. SN 2016hnk is consistent with being a subluminous (M-B = -16.7 mag, S-BV =0.43 +/- 0.03), highly reddened object. The IFS of its host galaxy reveals both a significant amount of dust at the SN location, residual star formation, and a high proportion of old stellar populations in the local environment compared to other locations in the galaxy, which favors an old progenitor for SN 2016hnk. Inspection of a nebular spectrum obtained one year after maximum contains two narrow emission lines attributed to the forbidden [Ca II] lambda lambda 7291,7324 doublet with a Doppler shift of 700 km s(-1). Based on various observational diagnostics, we argue that the progenitor of SN 2016hnk was likely a near Chandrasekhar-mass (M-Ch) carbon-oxygen white dwarf that produced 0.108 M-circle dot of Ni-56. Our modeling suggests that the narrow [Ca II] features observed in the nebular spectrum are associated with Ca-48 from electron capture during the explosion, which is expected to occur only in white dwarfs that explode near or at the M-Ch limit.National Science FoundationNational Science Foundation (NSF) [AST-1613472]; National Science Foundation (NSF)National Science Foundation (NSF) [1715133]; FCTFundacao para a Ciencia e a Tecnologia (FCT) [CRISP PTDC/FIS-AST-31546]; VILLUM FONDEN [13261]; Independent Research Fund Denmark; NASANational Aeronautics & Space Administration (NASA) [NNX16AB25G, NN12AR55G, 80NSSC18K0284, 80NSSC18K1575]; Aarhus University Research Fund (AUFF); China postdoctoral science foundationChina Postdoctoral Science Foundation [2018T110006]; Swedish Research Council (Vetenskapsradet)Swedish Research Council; Swedish National Space Board; research environment grant "Gravitational Radiation and Electromagnetic Astrophysical Transients (GREAT)"; EU/FP7-ERCEuropean Union (EU) [615929]; Finnish Cultural FoundationFinnish Cultural Foundation; NSFNational Science Foundation (NSF) [AST-1313484, AST-1615455, AST-1821987, 1821967, AST-1515927, AST-0908816]; US NSFNational Science Foundation (NSF) [AST-1211916]; TABASGO Foundation; STFCScience & Technology Facilities Council (STFC) [ST/M005348/1]; H2020 through an ERC Starting Grant [758638]; National Natural Science Foundation of China (NSFC)National Natural Science Foundation of China [11325313, 11633002, 11773067, 11403096]; Youth Innovation Promotion Association of the CAS [2018081]; Western Light Youth Project of CAS; LCO network [CLN2016A-005, NAOC2017AB-001, CON2016A-008, ARI2017AB-001]; Gordon and Betty Moore FoundationGordon and Betty Moore Foundation [GBMF5490]; Mt. Cuba Astronomical Foundation; Center for Cosmology and AstroParticle Physics at the Ohio State UniversityOhio State University; Chinese Academy of Sciences South America Center for Astronomy (CASSACA); Villum Foundation; Las Cumbres Observatory (LCO); Instrument Center for Danish Astrophysics (IDA); "the Strategic Priority Research Program-The Emergence of Cosmological Structures" of the Chinese Academy of Sciences [11 XDB09000000]; Special Fund for Astronomy from the Ministry of Finance; National Astronomical Observatories of China; Chinese Academy of Sciences (CAS)Chinese Academy of Sciences; People's Government of Yunnan Province; Gemini Observatory [GS-2016B-Q-22]This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu