The Extremely Metal-Poor SN 2023ufx: A Local Analog to High-Redshift Type II Supernovae
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| Format: | Preprint |
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2024
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| author | Tucker, Michael A. Hinkle, Jason Angus, Charlotte R. Auchettl, Katie Hoogendam, Willem B. Shappee, Benjamin Kochanek, Christopher S. Ashall, Chris de Boer, Thomas Chambers, Kenneth C. Desai, Dhvanil D. Do, Aaron Fulton, Michael D. Gao, Hua Herman, Joanna Huber, Mark Lidman, Chris Lin, Chien-Cheng Lowe, Thomas B. Magnier, Eugene A. Martin, Bailey Minguez, Paloma Nicholl, Matt Pursiainen, Miika Smartt, S. J. Smith, Ken W. Srivastav, Shubham Tucker, Brad E. Wainscoat, Richard J. |
| author_facet | Tucker, Michael A. Hinkle, Jason Angus, Charlotte R. Auchettl, Katie Hoogendam, Willem B. Shappee, Benjamin Kochanek, Christopher S. Ashall, Chris de Boer, Thomas Chambers, Kenneth C. Desai, Dhvanil D. Do, Aaron Fulton, Michael D. Gao, Hua Herman, Joanna Huber, Mark Lidman, Chris Lin, Chien-Cheng Lowe, Thomas B. Magnier, Eugene A. Martin, Bailey Minguez, Paloma Nicholl, Matt Pursiainen, Miika Smartt, S. J. Smith, Ken W. Srivastav, Shubham Tucker, Brad E. Wainscoat, Richard J. |
| contents | We present extensive observations of the Type II supernova (SN II) 2023ufx which is likely the most metal-poor SN II observed to-date. It exploded in the outskirts of a low-metallicity ($Z_{\rm host} \sim 0.1~Z_\odot$) dwarf ($M_g = -13.23\pm0.15$~mag; $r_e\sim 1$~kpc) galaxy. The explosion is luminous, peaking at $M_g\approx -18.5~$mag, and shows rapid evolution. The $r$-band (pseudo-bolometric) 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 $\approx 55~$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 pre-explosion mass-loss rate to $\dot{M} \lesssim 10^{-3}~\rm M_\odot$/yr. The photospheric-phase spectra are devoid of prominent metal absorption features, indicating a progenitor metallicity of $\lesssim 0.1~Z_\odot$. The semi-nebular ($\sim 60-130~$d) spectra reveal weak Fe II, but other metal species typically observed at these phases (Ti II, Sc II, Ba II) are conspicuously absent. The late-phase optical and near-infrared spectra also reveal broad ($\approx 10^4~\rm{km}~\rm s^{-1}$) 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 $\lesssim 0.1~Z_\odot$ 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. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2405_00113 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | The Extremely Metal-Poor SN 2023ufx: A Local Analog to High-Redshift Type II Supernovae Tucker, Michael A. Hinkle, Jason Angus, Charlotte R. Auchettl, Katie Hoogendam, Willem B. Shappee, Benjamin Kochanek, Christopher S. Ashall, Chris de Boer, Thomas Chambers, Kenneth C. Desai, Dhvanil D. Do, Aaron Fulton, Michael D. Gao, Hua Herman, Joanna Huber, Mark Lidman, Chris Lin, Chien-Cheng Lowe, Thomas B. Magnier, Eugene A. Martin, Bailey Minguez, Paloma Nicholl, Matt Pursiainen, Miika Smartt, S. J. Smith, Ken W. Srivastav, Shubham Tucker, Brad E. Wainscoat, Richard J. Solar and Stellar Astrophysics Astrophysics of Galaxies High Energy Astrophysical Phenomena We present extensive observations of the Type II supernova (SN II) 2023ufx which is likely the most metal-poor SN II observed to-date. It exploded in the outskirts of a low-metallicity ($Z_{\rm host} \sim 0.1~Z_\odot$) dwarf ($M_g = -13.23\pm0.15$~mag; $r_e\sim 1$~kpc) galaxy. The explosion is luminous, peaking at $M_g\approx -18.5~$mag, and shows rapid evolution. The $r$-band (pseudo-bolometric) 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 $\approx 55~$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 pre-explosion mass-loss rate to $\dot{M} \lesssim 10^{-3}~\rm M_\odot$/yr. The photospheric-phase spectra are devoid of prominent metal absorption features, indicating a progenitor metallicity of $\lesssim 0.1~Z_\odot$. The semi-nebular ($\sim 60-130~$d) spectra reveal weak Fe II, but other metal species typically observed at these phases (Ti II, Sc II, Ba II) are conspicuously absent. The late-phase optical and near-infrared spectra also reveal broad ($\approx 10^4~\rm{km}~\rm s^{-1}$) 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 $\lesssim 0.1~Z_\odot$ 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. |
| title | The Extremely Metal-Poor SN 2023ufx: A Local Analog to High-Redshift Type II Supernovae |
| topic | Solar and Stellar Astrophysics Astrophysics of Galaxies High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2405.00113 |