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A Panchromatic View of Late-time Shock Power in the Type II Supernova 2023ixf

Fuente: arXiv

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Autori principali:	Jacobson-Galán, W. V., Dessart, L., Kilpatrick, C. D., Patel, P. J., Auchettl, K., Tinyanont, S., Margutti, R., Dwarkadas, V. V., Bostroem, K. A., Chornock, R., Foley, R. J., Abunemeh, H., Ahumada, T., Arunachalam, P., Bustamante-Rosell, M. J., Coulter, D. A., Gall, C., Gao, H., Guo, X., Hjorth, J., Kaewmookda, M., Kasliwal, M. M., Kaur, R., Larison, C., LeBaron, N., Miao, H. -Y., Narayan, G., Pan, Y. -C., Park, S. H., Patra, K. C., Qin, Y., Ransome, C. L., Rest, A., Rho, J., Rose, S., Sears, H., Swift, J. J., Taggart, K., Villar, V. A., Wang, Q., Zenati, Y., Zhou, H.
Natura:	Preprint
Pubblicazione:	2025
Soggetti:	High Energy Astrophysical Phenomena Solar and Stellar Astrophysics
Accesso online:	Acceder al recurso
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_version_	1866914095768272896
author	Jacobson-Galán, W. V. Dessart, L. Kilpatrick, C. D. Patel, P. J. Auchettl, K. Tinyanont, S. Margutti, R. Dwarkadas, V. V. Bostroem, K. A. Chornock, R. Foley, R. J. Abunemeh, H. Ahumada, T. Arunachalam, P. Bustamante-Rosell, M. J. Coulter, D. A. Gall, C. Gao, H. Guo, X. Hjorth, J. Kaewmookda, M. Kasliwal, M. M. Kaur, R. Larison, C. LeBaron, N. Miao, H. -Y. Narayan, G. Pan, Y. -C. Park, S. H. Patra, K. C. Qin, Y. Ransome, C. L. Rest, A. Rho, J. Rose, S. Sears, H. Swift, J. J. Taggart, K. Villar, V. A. Wang, Q. Zenati, Y. Zhou, H.
author_facet	Jacobson-Galán, W. V. Dessart, L. Kilpatrick, C. D. Patel, P. J. Auchettl, K. Tinyanont, S. Margutti, R. Dwarkadas, V. V. Bostroem, K. A. Chornock, R. Foley, R. J. Abunemeh, H. Ahumada, T. Arunachalam, P. Bustamante-Rosell, M. J. Coulter, D. A. Gall, C. Gao, H. Guo, X. Hjorth, J. Kaewmookda, M. Kasliwal, M. M. Kaur, R. Larison, C. LeBaron, N. Miao, H. -Y. Narayan, G. Pan, Y. -C. Park, S. H. Patra, K. C. Qin, Y. Ransome, C. L. Rest, A. Rho, J. Rose, S. Sears, H. Swift, J. J. Taggart, K. Villar, V. A. Wang, Q. Zenati, Y. Zhou, H.
contents	We present multi-wavelength observations of the type II supernova (SN II) 2023ixf during its first two years of evolution. We combine ground-based optical/NIR spectroscopy with Hubble Space Telescope (HST) far- and near-ultraviolet spectroscopy and James Webb Space Telescope (JWST) near- and mid-infrared photometry and spectroscopy to create spectral energy distributions of SN 2023ixf at +374 and +620 days post-explosion, covering a wavelength range of ~0.1-30 $μ$m. The multi-band light curve of SN 2023ixf follows a standard radioactive decay decline rate after the plateau until ~500 days, at which point shock powered emission from ongoing interaction between the SN ejecta and circumstellar material (CSM) begins to dominate. This evolution is temporally consistent with 0.3-10 keV X-ray detections of SN 2023ixf and broad ''boxy'' spectral line emission from reprocessing of shock luminosity in a cold dense shell located between forward and reverse shocks. Using the expected absorbed radioactive decay power and the detected X-ray luminosity, we quantify the total shock powered emission at the +374 and +620 day epochs and find that it can be explained by nearly complete thermalization of the reverse shock luminosity as SN 2023ixf interacts with a continuous, ''wind-like'' CSM with a progenitor mass-loss rate of $\dot M \approx 10^{-4}$ M$_{\odot}$ yr$^{-1}$ ($v_w = 20 \pm 5$ km/s). Additionally, we construct multi-epoch spectral models from the non-LTE radiative transfer code CMFGEN, which contain radioactive decay and shock powers, as well as dust absorption, scattering, and emission. We find that models with shock powers of $L_{sh} = (0.5-1) \times 10^{40}$ erg s$^{-1}$ and $(0.5 - 1) \times 10^{-3}$ M$_{\odot}$ of silicate dust in the cold dense shell and/or inner SN ejecta can effectively reproduce the global properties of the late-time (>300 days) UV-to-IR spectra of SN 2023ixf.
format	Preprint
id	arxiv_https___arxiv_org_abs_2508_11747
institution	arXiv
publishDate	2025
record_format	arxiv
spellingShingle	A Panchromatic View of Late-time Shock Power in the Type II Supernova 2023ixf Jacobson-Galán, W. V. Dessart, L. Kilpatrick, C. D. Patel, P. J. Auchettl, K. Tinyanont, S. Margutti, R. Dwarkadas, V. V. Bostroem, K. A. Chornock, R. Foley, R. J. Abunemeh, H. Ahumada, T. Arunachalam, P. Bustamante-Rosell, M. J. Coulter, D. A. Gall, C. Gao, H. Guo, X. Hjorth, J. Kaewmookda, M. Kasliwal, M. M. Kaur, R. Larison, C. LeBaron, N. Miao, H. -Y. Narayan, G. Pan, Y. -C. Park, S. H. Patra, K. C. Qin, Y. Ransome, C. L. Rest, A. Rho, J. Rose, S. Sears, H. Swift, J. J. Taggart, K. Villar, V. A. Wang, Q. Zenati, Y. Zhou, H. High Energy Astrophysical Phenomena Solar and Stellar Astrophysics We present multi-wavelength observations of the type II supernova (SN II) 2023ixf during its first two years of evolution. We combine ground-based optical/NIR spectroscopy with Hubble Space Telescope (HST) far- and near-ultraviolet spectroscopy and James Webb Space Telescope (JWST) near- and mid-infrared photometry and spectroscopy to create spectral energy distributions of SN 2023ixf at +374 and +620 days post-explosion, covering a wavelength range of ~0.1-30 $μ$m. The multi-band light curve of SN 2023ixf follows a standard radioactive decay decline rate after the plateau until ~500 days, at which point shock powered emission from ongoing interaction between the SN ejecta and circumstellar material (CSM) begins to dominate. This evolution is temporally consistent with 0.3-10 keV X-ray detections of SN 2023ixf and broad ''boxy'' spectral line emission from reprocessing of shock luminosity in a cold dense shell located between forward and reverse shocks. Using the expected absorbed radioactive decay power and the detected X-ray luminosity, we quantify the total shock powered emission at the +374 and +620 day epochs and find that it can be explained by nearly complete thermalization of the reverse shock luminosity as SN 2023ixf interacts with a continuous, ''wind-like'' CSM with a progenitor mass-loss rate of $\dot M \approx 10^{-4}$ M$_{\odot}$ yr$^{-1}$ ($v_w = 20 \pm 5$ km/s). Additionally, we construct multi-epoch spectral models from the non-LTE radiative transfer code CMFGEN, which contain radioactive decay and shock powers, as well as dust absorption, scattering, and emission. We find that models with shock powers of $L_{sh} = (0.5-1) \times 10^{40}$ erg s$^{-1}$ and $(0.5 - 1) \times 10^{-3}$ M$_{\odot}$ of silicate dust in the cold dense shell and/or inner SN ejecta can effectively reproduce the global properties of the late-time (>300 days) UV-to-IR spectra of SN 2023ixf.
title	A Panchromatic View of Late-time Shock Power in the Type II Supernova 2023ixf
topic	High Energy Astrophysical Phenomena Solar and Stellar Astrophysics
url	https://arxiv.org/abs/2508.11747