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The late-time light curves of Type Ia supernovae: confronting models with observations

Tiwari, Vishal and Graur, Or and Fisher, Robert and Seitenzahl, Ivo and Leung, Shing-Chi and Nomoto, Ken'ichi and Perets, Hagai Binyamin and Shen, Ken (2022) The late-time light curves of Type Ia supernovae: confronting models with observations. Monthly Notices of the Royal Astronomical Society, 515 (3). pp. 3703-3715. ISSN 0035-8711. doi:10.1093/mnras/stac1618.

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Type Ia supernovae (SNe Ia) play a crucial role as standardizable candles in measurements of the Hubble constant and dark energy. Increasing evidence points towards multiple possible explosion channels as the origin of normal SNe Ia, with possible systematic effects on the determination of cosmological parameters. We present, for the first time, a comprehensive comparison of publicly available SN Ia model nucleosynthetic data with observations of late-time light curve observations of SN Ia events. These models span a wide range of white dwarf (WD) progenitor masses, metallicities, explosion channels, and numerical methodologies. We focus on the influence of 57Ni and its isobaric decay product 57Co in powering the late-time (t > 1000 d) light curves of SNe Ia. 57Ni and 57Co are neutron-rich relative to the more abundant radioisotope 56Ni, and are consequently a sensitive probe of neutronization at the higher densities of near-Chandrashekhar (near-MCh) progenitor WDs. We demonstrate that observations of one SN Ia event, SN 2015F is only consistent with a sub-Chandrasekhar (sub-MCh) WD progenitor. Observations of four other events (SN 2011fe, SN 2012cg, SN 2014J, and SN2013aa) are consistent with both near-MCh and sub-MCh progenitors. Continued observations of late-time light curves of nearby SNe Ia will provide crucial information on the nature of the SN Ia progenitors.

Item Type:Article
Related URLs:
URLURL TypeDescription
Tiwari, Vishal0000-0002-7110-9885
Graur, Or0000-0002-4391-6137
Fisher, Robert0000-0001-8077-7255
Seitenzahl, Ivo0000-0002-5044-2988
Leung, Shing-Chi0000-0002-4972-3803
Nomoto, Ken'ichi0000-0001-9553-0685
Perets, Hagai Binyamin0000-0002-5004-199X
Shen, Ken0000-0002-9632-6106
Additional Information:VT was supported by NASA through HST-GO-15693. OG was supported, in part, by an NSF Astronomy and Astrophysics Fellowship under award AST-1602595. RTF thanks the NASA ATP program for support under award 80NSSC18K1013. RTF also thanks the Institute for Theory and Computation at the Center for Astrophysics | Harvard & Smithsonian, and the Kavli Institute for Theoretical Physics, supported in part by the National Science Foundation under grant NSF PHY11-25915, for visiting support during which this work was undertaken. SCL acknowledges support from NASA grants HST-AR-15021.001-A and 80NSSC18K1017. KN is supported by the World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan, and JSPS KAKENHI Grant Numbers JP17K05382 and JP20K04024, and JP21H04499. KJS is supported by NASA through the Astrophysics Theory Program (NNX17AG28G).
Funding AgencyGrant Number
NSF Astronomy and Astrophysics FellowshipAST-1602595
NASA Hubble FellowshipHST-AR-15021.001-A
Ministry of Education, Culture, Sports, Science and Technology (MEXT)UNSPECIFIED
Japan Society for the Promotion of Science (JSPS)JP17K05382
Japan Society for the Promotion of Science (JSPS)JP20K04024
Japan Society for the Promotion of Science (JSPS)JP21H04499
Issue or Number:3
Record Number:CaltechAUTHORS:20220825-833128900
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:116465
Deposited By: Melissa Ray
Deposited On:29 Aug 2022 22:58
Last Modified:29 Aug 2022 22:58

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