Photometry and Spectroscopy of SN 2024pxl: A Luminosity Link among Type Iax Supernovae

Abstract We present extensive ultraviolet to optical photometric and optical to near-infrared (NIR) spectroscopic follow-up observations of the nearby intermediate-luminosity ( M V = −16.81 ± 0.19 mag) Type Iax supernovae (SNe Iax) 2024pxl in NGC 6384. SN 2024pxl exhibits a faster light curve than the high-luminosity members of this class, and slower than low-luminosity events. The observationally well-constrained rise time of ∼11 days and an estimated synthesized 56 Ni mass of 0.03 M ⊙ , based on analytical modeling of the integrated spectral energy distribution light curve, are consistent with models of the weak deflagration of a carbon-oxygen white dwarf. Our optical spectral sequence of SN 2024pxl shows weak Si ii lines and spectral evolution similar to other high-luminosity SNe Iax, but also a prominent early-time C ii line, like lower-luminosity SNe Iax. The late-time optical spectrum of SN 2024pxl closely matches that of SN 2014dt, and its NIR spectral evolution aligns with that of other well-studied, high-luminosity SNe Iax. The spectral-line expansion velocities of SN 2024pxl are at the lower end of the SNe Iax velocity distribution, and the velocity distribution of iron-group elements compared to intermediate-mass elements suggests that the ejecta are mixed on large scales, as expected in pure deflagration models. SN 2024pxl exhibits characteristics intermediate between those of high-luminosity and low-luminosity SNe Iax, further establishing a link across this diverse class.

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Publication Details

Journal
The Astrophysical Journal
Published
2026-03-09
DOI
https://doi.org/10.3847/1538-4357/ae4318
Primary Topic
Gamma-ray bursts and supernovae
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article
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article

Photometry and Spectroscopy of SN 2024pxl: A Luminosity Link among Type Iax Supernovae

The Astrophysical Journal
Gamma-ray bursts and supernovae
article

Photometry and Spectroscopy of SN 2024pxl: A Luminosity Link among Type Iax Supernovae

article en

Abstract

Abstract We present extensive ultraviolet to optical photometric and optical to near-infrared (NIR) spectroscopic follow-up observations of the nearby intermediate-luminosity ( M V = −16.81 ± 0.19 mag) Type Iax supernovae (SNe Iax) 2024pxl in NGC 6384. SN 2024pxl exhibits a faster light curve than the high-luminosity members of this class, and slower than low-luminosity events. The observationally well-constrained rise time of ∼11 days and an estimated synthesized 56 Ni mass of 0.03 M ⊙ , based on analytical modeling of the integrated spectral energy distribution light curve, are consistent with models of the weak deflagration of a carbon-oxygen white dwarf. Our optical spectral sequence of SN 2024pxl shows weak Si ii lines and spectral evolution similar to other high-luminosity SNe Iax, but also a prominent early-time C ii line, like lower-luminosity SNe Iax. The late-time optical spectrum of SN 2024pxl closely matches that of SN 2014dt, and its NIR spectral evolution aligns with that of other well-studied, high-luminosity SNe Iax. The spectral-line expansion velocities of SN 2024pxl are at the lower end of the SNe Iax velocity distribution, and the velocity distribution of iron-group elements compared to intermediate-mass elements suggests that the ejecta are mixed on large scales, as expected in pure deflagration models. SN 2024pxl exhibits characteristics intermediate between those of high-luminosity and low-luminosity SNe Iax, further establishing a link across this diverse class.

The Astrophysical JournalVol. 999(2)
Rutgers, The State University of New Jersey (US), Eötvös Loránd University (HU), Northwestern University (US), Australian National University (AU), California Institute of Technology (US), Las Cumbres Observatory Global Telescope Network (US), Space Telescope Science Institute (US), Universidad de Antofagasta (CL), Institute of Space Sciences (ES), American Museum of Natural History (US), University of Arizona (US), Indian Institute of Astrophysics (IN), Johns Hopkins University (US), University of California, Santa Barbara (US), University of Turku (FI), University of Illinois Urbana-Champaign (US), Stockholm University (SE), Pontificia Universidad Católica de Chile (CL), The University of Melbourne (AU), GSI Helmholtz Centre for Heavy Ion Research (DE), Urbana University (US), University of California, Santa Cruz (US), Trinity College Dublin (IE), Purdue University West Lafayette (US), Kyoto University (JP), University of Szeged (HU), Konkoly Observatory (HU), Brera Astronomical Observatory (IT), Aryabhatta Research Institute of Observational Sciences (IN), University of Oxford (GB), University of Chicago (US), Institut d'Estudis Espacials de Catalunya (ES), Mount Washington Observatory (US), Gemini North Observatory (US), McCormick (United States) (US), Simons Foundation (US), Université Bourgogne Franche-Comté (FR), Center for Astrophysics Harvard & Smithsonian (US), Carnegie Observatories (US), Nordic Optical Telescope (ES), National Center for Supercomputing Applications (US), MTA-SZTE Research Group on Artificial Intelligence (HU), The NSF AI Institute for Artificial Intelligence and Fundamental Interactions (US), University of Virginia (US), Weizmann Institute of Science (IL), University of Portsmouth (GB), Zhejiang University (CN), University of California, Davis (US), National Astronomical Research Institute of Thailand (TH), The University of Texas at Austin (US), National Institute for Astrophysics (IT), University of California, Berkeley (US), Tsinghua University (CN)
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