The Extremely Metal-poor SN 2023ufx: A Local Analog to High-redshift Type II Supernovae

Abstract We present extensive observations of the Type II supernova (SN II) SN 2023ufx, which is likely the most metal-poor SN II observed to date. It exploded in the outskirts of a low-metallicity ( Z host ∼ 0.1 Z ⊙ ) dwarf ( M g = −13.39 ± 0.16 mag, r proj ∼ 1 kpc) galaxy. The explosion is luminous, peaking at M g ≈ −18.5 mag, and shows rapid evolution. The r -band (pseudobolometric) light curve has a shock-cooling phase lasting 20 (17) days followed by a 19 (23) day plateau. The entire optically thick phase lasts only ≈55 days following explosion, indicating that the red supergiant progenitor had a thinned H envelope prior to explosion. The early spectra obtained during the shock-cooling phase show no evidence for narrow emission features and limit the preexplosion mass-loss rate to <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mover accent="true"> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>̇</mml:mo> </mml:mrow> </mml:mover> <mml:mo>≲</mml:mo> <mml:msup> <mml:mrow> <mml:mn>10</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>3</mml:mn> </mml:mrow> </mml:msup> </mml:math> M ⊙ yr −1 . The photospheric-phase spectra are devoid of prominent metal absorption features, indicating a progenitor metallicity of ≲0.1 Z ⊙ . The seminebular (∼60–130 days) spectra reveal weak Fe ii , but other metal species typically observed at these phases (Ti ii , Sc ii , and Ba ii ) are conspicuously absent. The late-phase optical and near-infrared spectra also reveal broad (≈10 4 km s −1 ) double-peaked H α , P β , and P γ emission profiles suggestive of a fast outflow launched during the explosion. Outflows are typically attributed to rapidly rotating progenitors, which also prefer metal-poor environments. This is only the second SN II with ≲0.1 Z ⊙ and both exhibit peculiar evolution, suggesting a sizable fraction of metal-poor SNe II have distinct properties compared to nearby metal-enriched SNe II. These observations lay the groundwork for modeling the metal-poor SNe II expected in the early Universe.

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Publication Details

Journal
The Astrophysical Journal
Published
2024-11-21
DOI
https://doi.org/10.3847/1538-4357/ad8448
Citations
7
Primary Topic
Gamma-ray bursts and supernovae
Type
article
Field-Weighted Citation Impact
2.32

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article

The Extremely Metal-poor SN 2023ufx: A Local Analog to High-redshift Type II Supernovae

E. A. Magnier, D. Desai, M. Pursiainen, Thomas de Boer et al.
7 citations
The Astrophysical Journal
Gamma-ray bursts and supernovae
2.32
article

The Extremely Metal-poor SN 2023ufx: A Local Analog to High-redshift Type II Supernovae

E. A. Magnier, D. Desai, M. Pursiainen, Thomas de Boer, T. Lowe, M. Fulton, Chien-Cheng Lin, Jason T. Hinkle, C. S. Kochanek, Brad E. Tucker, B. J. Shappee, Brian Martin, M. E. Huber, C. R. Angus, M. A. Tucker, W. B. Hoogendam, Aaron Do, S. J. Smartt, Katie Auchettl, K. C. Chambers, Christopher E. Lidman, Hua Gao, M. Nicholl, R. J. Wainscoat, K. Smith, Chris Ashall, Shubham Srivastav, Joanna Herman, P. Mínguez
article en
7 citations

Abstract

Abstract We present extensive observations of the Type II supernova (SN II) SN 2023ufx, which is likely the most metal-poor SN II observed to date. It exploded in the outskirts of a low-metallicity ( Z host ∼ 0.1 Z ⊙ ) dwarf ( M g = −13.39 ± 0.16 mag, r proj ∼ 1 kpc) galaxy. The explosion is luminous, peaking at M g ≈ −18.5 mag, and shows rapid evolution. The r -band (pseudobolometric) light curve has a shock-cooling phase lasting 20 (17) days followed by a 19 (23) day plateau. The entire optically thick phase lasts only ≈55 days following explosion, indicating that the red supergiant progenitor had a thinned H envelope prior to explosion. The early spectra obtained during the shock-cooling phase show no evidence for narrow emission features and limit the preexplosion mass-loss rate to <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mover accent="true"> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>̇</mml:mo> </mml:mrow> </mml:mover> <mml:mo>≲</mml:mo> <mml:msup> <mml:mrow> <mml:mn>10</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>3</mml:mn> </mml:mrow> </mml:msup> </mml:math> M ⊙ yr −1 . The photospheric-phase spectra are devoid of prominent metal absorption features, indicating a progenitor metallicity of ≲0.1 Z ⊙ . The seminebular (∼60–130 days) spectra reveal weak Fe ii , but other metal species typically observed at these phases (Ti ii , Sc ii , and Ba ii ) are conspicuously absent. The late-phase optical and near-infrared spectra also reveal broad (≈10 4 km s −1 ) double-peaked H α , P β , and P γ emission profiles suggestive of a fast outflow launched during the explosion. Outflows are typically attributed to rapidly rotating progenitors, which also prefer metal-poor environments. This is only the second SN II with ≲0.1 Z ⊙ and both exhibit peculiar evolution, suggesting a sizable fraction of metal-poor SNe II have distinct properties compared to nearby metal-enriched SNe II. These observations lay the groundwork for modeling the metal-poor SNe II expected in the early Universe.

The Astrophysical JournalVol. 976(2)
National Science Foundation, Smithsonian Institution, National Aeronautics and Space Administration, Gordon and Betty Moore Foundation, Ohio Board of Regents, Ohio State University, University of Minnesota, Aarhus Universitet, Johns Hopkins University, University of Notre Dame, UK Space Agency, Arizona Board of Regents, Space Telescope Science Institute, UK Research and Innovation, Queen's University Belfast, Durham University, Queen's University, Nuclear Safety and Security Commission, Istituto Nazionale di Astrofisica, National Central University, Universitetet i Oslo, Háskóli Íslands, Turun Yliopisto, Stockholms Universitet, Eötvös Loránd Tudományegyetem, Leibniz-Institut für Astrophysik Potsdam, Max-Planck-Institut für Astronomie, Smithsonian Astrophysical Observatory, Science Mission Directorate, Science and Technology Facilities Council, European Research Council, Australian Research Council, Leibniz-Gemeinschaft, Division of Astronomical Sciences, Planetary Science Division, Los Alamos National Laboratory
Openalex Percentile: Top 12%
Gamma-ray bursts and supernovae
2.32
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