Evidence for Asymmetric Ejecta and Circumstellar Material in SN 2023ixf Inferred from Extensive Nebular-phase Observations
Brian Hsu, Nathan Smith, K. Azalee Bostroem, Jeniveve Pearson, David J. Sand, Lindsey A. Kwok, Jennifer E. Andrews, Bhagya M. Subrayan, Griffin Hosseinzadeh, Manisha Shrestha, Conor Ransome, Moira Andrews, Collin T. Christy, Yize Dong, Joseph Farah, Alexei V. Filippenko, Noah Franz, Jared A. Goldberg, Estefania Padilla Gonzalez, Claudia P. Gutiérrez, Emily Hoang, D. Andrew Howell, Saurabh W. Jha, Réka Kőnyves-Tóth, Michael Lundquist, Curtis McCully, Darshana Mehta, Nicolas E. Meza Retamal, Megan Newsome, Aravind P. Ravi, Jeonghee Rho, Giacomo Terreran, Stefano Valenti, Sergiy Vasylyev, X. -F. Wang, Kathryn Wynn, Yi Yang
astro-ph.HE
Submitted: 2026-07-03
Comments: 36 pages, 15 figures, submitted to ApJ
Project page: http://www.sdss3.org
License: http://creativecommons.org/licenses/by/4.0/
The gist: We present extensive optical and near-infrared (NIR) observations of the nearby Type II supernova (SN II) 2023ixf in the nebular phase from +89 days to +749 days after explosion, supplemented with
Terminology
Abstract
We present extensive optical and near-infrared (NIR) observations of the nearby Type II supernova (SN II) 2023ixf in the nebular phase from +89 days to +749 days after explosion, supplemented with NIR and mid-infrared (MIR) spectroscopy from the James Webb Space Telescope. The H alpha emission profile shows complex evolution, with the emergence of high-velocity components consistent with the outer ejecta interacting with extended, low-density circumstellar material (CSM). We find that the H alpha profile at an intermediate epoch (around +375 d) can be reconstructed by scaling an earlier decay-powered component and a later-phase shock-powered component, which revealed an additional intermediate-width component. This is consistent with the ejecta crashing into the initially aspherical dense CSM that has been swept-up by the forward shock. In the NIR, we find double-peaked emission from Mg I 1.504 mu m, Na I 2.206 mu m, and [Ni I] 3.12 mu m between +200 d and +374 d, consistent with an asymmetric distribution of Ni-rich material that heats the ejecta inhomogeneously. We posit a disk-like CSM geometry and an ejecta geometry in which at least two large Ni-rich plumes lead to the observed line-profile diversity.
Sources
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