Constraining Type Ia Supernova Progenitor Scenarios with Extremely Late-time Photometry of Supernova SN 2013aa

Wynn V. Jacobson-Galán; Georgios Dimitriadis; Ryan J. Foley; Charles D. Kilpatrick

doi:10.3847/1538-4357/aab716

Constraining Type Ia Supernova Progenitor Scenarios with Extremely Late-time Photometry of Supernova SN 2013aa

Wynn V. Jacobson-Galán, Georgios Dimitriadis, Ryan J. Foley, Charles D. Kilpatrick

CIERA - Center for Interdisciplinary Exploration and Research in Astrophysics

Research output: Contribution to journal › Article › peer-review

17 Scopus citations

Abstract

We present Hubble Space Telescope observations and photometric measurements of the Type Ia supernova (SN Ia) SN 2013aa 1500 days after explosion. At this epoch, the luminosity is primarily dictated by the amounts of radioactive ⁵⁷Co and ⁵⁵Fe, while at earlier epochs, the luminosity depends on the amount of radioactive ⁵⁶Co. The ratio of odd-numbered to even-numbered isotopes depends significantly on the density of the progenitor white dwarf (WD) during the SN explosion, which, in turn, depends on the details of the progenitor system at the time of ignition. From a comprehensive analysis of the entire light curve of SN 2013aa, we measure a M(⁵⁷Co) M(⁵⁶Co) ratio of 0.02_-0.02^+0.01, which indicates a relatively low central density for the progenitor WD at the time of explosion, consistent with DD progenitor channels. We estimate M(⁵⁶Ni) = 0.732 ± 0.151 M_⊙, and place an upper limit on the abundance of ⁵⁵Fe. A recent study reported a possible correlation between M(⁵⁷Co) M(⁵⁶Co) and stretch for four SNe Ia. SN 2013aa, however, does not fit this trend, indicating either SN 2013aa is an extreme outlier or the correlation does not hold up with a larger sample. The M(⁵⁷Co) M(⁵⁶Co) measured for the expanded sample of SNe Ia with photometry at extremely late times has a much larger range than that of explosion models, perhaps limiting conclusions about SN Ia progenitors drawn from extremely late-time photometry.

Original language	English (US)
Article number	88
Journal	Astrophysical Journal
Volume	857
Issue number	2
DOIs	https://doi.org/10.3847/1538-4357/aab716
State	Published - Apr 20 2018

Funding

The UCSC group is supported in part by NSF grant AST-1518052, the Gordon & Betty Moore Foundation, and by fellowships from the Alfred P. Sloan Foundation and the David and Lucile Packard Foundation to R.J.F. and from the UCSC Koret Scholars program to W.V.J.-G. Facilities: HST(WFC3), Gemini:South(GMOS). Based on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute (STScI), which is operated by the Association of Universities for Research in Astronomy, Inc., under National Aeronautics and Space Administration (NASA) contract NAS 5–26555. These observations are associated with Program DD– 14925. Support for DD–14925 was provided by NASA through a grant from STscI. This paper is based upon work supported by NASA under Contract No.NNG16PJ34C issued through the WFIRST Science Investigation Teams Program. This paper is based upon work supported by NASA under Contract No. NNG16PJ34C issued through the WFIRST Science Investigation Teams Program.

Keywords

nuclear reactions, nucleosynthesis, abundances
supernovae: general
supernovae: individual (SN 2013aa)

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.3847/1538-4357/aab716

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title = "Constraining Type Ia Supernova Progenitor Scenarios with Extremely Late-time Photometry of Supernova SN 2013aa",

abstract = "We present Hubble Space Telescope observations and photometric measurements of the Type Ia supernova (SN Ia) SN 2013aa 1500 days after explosion. At this epoch, the luminosity is primarily dictated by the amounts of radioactive 57Co and 55Fe, while at earlier epochs, the luminosity depends on the amount of radioactive 56Co. The ratio of odd-numbered to even-numbered isotopes depends significantly on the density of the progenitor white dwarf (WD) during the SN explosion, which, in turn, depends on the details of the progenitor system at the time of ignition. From a comprehensive analysis of the entire light curve of SN 2013aa, we measure a M(57Co) M(56Co) ratio of 0.02-0.02+0.01, which indicates a relatively low central density for the progenitor WD at the time of explosion, consistent with DD progenitor channels. We estimate M(56Ni) = 0.732 ± 0.151 M⊙, and place an upper limit on the abundance of 55Fe. A recent study reported a possible correlation between M(57Co) M(56Co) and stretch for four SNe Ia. SN 2013aa, however, does not fit this trend, indicating either SN 2013aa is an extreme outlier or the correlation does not hold up with a larger sample. The M(57Co) M(56Co) measured for the expanded sample of SNe Ia with photometry at extremely late times has a much larger range than that of explosion models, perhaps limiting conclusions about SN Ia progenitors drawn from extremely late-time photometry.",

keywords = "nuclear reactions, nucleosynthesis, abundances, supernovae: general, supernovae: individual (SN 2013aa)",

author = "Jacobson-Gal{\'a}n, {Wynn V.} and Georgios Dimitriadis and Foley, {Ryan J.} and Kilpatrick, {Charles D.}",

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AU - Jacobson-Galán, Wynn V.

AU - Dimitriadis, Georgios

AU - Foley, Ryan J.

AU - Kilpatrick, Charles D.

PY - 2018/4/20

Y1 - 2018/4/20

N2 - We present Hubble Space Telescope observations and photometric measurements of the Type Ia supernova (SN Ia) SN 2013aa 1500 days after explosion. At this epoch, the luminosity is primarily dictated by the amounts of radioactive 57Co and 55Fe, while at earlier epochs, the luminosity depends on the amount of radioactive 56Co. The ratio of odd-numbered to even-numbered isotopes depends significantly on the density of the progenitor white dwarf (WD) during the SN explosion, which, in turn, depends on the details of the progenitor system at the time of ignition. From a comprehensive analysis of the entire light curve of SN 2013aa, we measure a M(57Co) M(56Co) ratio of 0.02-0.02+0.01, which indicates a relatively low central density for the progenitor WD at the time of explosion, consistent with DD progenitor channels. We estimate M(56Ni) = 0.732 ± 0.151 M⊙, and place an upper limit on the abundance of 55Fe. A recent study reported a possible correlation between M(57Co) M(56Co) and stretch for four SNe Ia. SN 2013aa, however, does not fit this trend, indicating either SN 2013aa is an extreme outlier or the correlation does not hold up with a larger sample. The M(57Co) M(56Co) measured for the expanded sample of SNe Ia with photometry at extremely late times has a much larger range than that of explosion models, perhaps limiting conclusions about SN Ia progenitors drawn from extremely late-time photometry.

AB - We present Hubble Space Telescope observations and photometric measurements of the Type Ia supernova (SN Ia) SN 2013aa 1500 days after explosion. At this epoch, the luminosity is primarily dictated by the amounts of radioactive 57Co and 55Fe, while at earlier epochs, the luminosity depends on the amount of radioactive 56Co. The ratio of odd-numbered to even-numbered isotopes depends significantly on the density of the progenitor white dwarf (WD) during the SN explosion, which, in turn, depends on the details of the progenitor system at the time of ignition. From a comprehensive analysis of the entire light curve of SN 2013aa, we measure a M(57Co) M(56Co) ratio of 0.02-0.02+0.01, which indicates a relatively low central density for the progenitor WD at the time of explosion, consistent with DD progenitor channels. We estimate M(56Ni) = 0.732 ± 0.151 M⊙, and place an upper limit on the abundance of 55Fe. A recent study reported a possible correlation between M(57Co) M(56Co) and stretch for four SNe Ia. SN 2013aa, however, does not fit this trend, indicating either SN 2013aa is an extreme outlier or the correlation does not hold up with a larger sample. The M(57Co) M(56Co) measured for the expanded sample of SNe Ia with photometry at extremely late times has a much larger range than that of explosion models, perhaps limiting conclusions about SN Ia progenitors drawn from extremely late-time photometry.

KW - nuclear reactions, nucleosynthesis, abundances

KW - supernovae: general

KW - supernovae: individual (SN 2013aa)

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Constraining Type Ia Supernova Progenitor Scenarios with Extremely Late-time Photometry of Supernova SN 2013aa

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