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SN2024abfl: A Low-Luminosity Type IIP Supernova at the Low-Mass End of Core Collapse

Luhan Li, Jujia Zhang, Zeyi Zhao, Liping Li, Xiaofeng Wang, Liyang Chen, Zeyi Wang, Jingxiao Luo, Zhengwei Liu, Zhanwen Han, Bo Wang

Abstract

We present optical photometric and spectroscopic observations of the low-luminosity (LL) Type IIP supernova SN\,2024abfl. The distance to its host galaxy is highly uncertain, with independent estimates of $9.5^{+2.3}_{-2.4}$ Mpc and $15.0^{+8.9}_{-1.9}$ Mpc. Even adopting the larger distance, the inferred plateau luminosity is only $\sim 10^{41}\rm erg\,s^{-1}$, placing SN 2024abfl at the extreme faint end of SNe IIP population. Its light curve exhibits a long-lasting plateau of approximately 110 days. The spectra show exceptionally low expansion velocities, with the \FeII\, velocity of $\sim1200\,\rm km\,s^{-1}$ at 50 days after the explosion, significantly lower than the typical values of $\sim2000-5500\,\rm km\,s^{-1}$ observed in SNe IIP, placing SN\,2024abfl among the slowest-expanding LL SNe IIP. Bolometric modeling yields a synthesized $^{56}$Ni mass of $\sim0.002-0.004\,\rm M_\odot$, though this estimate remains subject to significant uncertainty owing to the poorly constrained distance. Considering the plateau color and duration, the magnitude drop from plateau to tail, and the progenitor luminosity, we favor a low-mass core-collapse origin for SN\,2024abfl.

SN2024abfl: A Low-Luminosity Type IIP Supernova at the Low-Mass End of Core Collapse

Abstract

We present optical photometric and spectroscopic observations of the low-luminosity (LL) Type IIP supernova SN\,2024abfl. The distance to its host galaxy is highly uncertain, with independent estimates of Mpc and Mpc. Even adopting the larger distance, the inferred plateau luminosity is only , placing SN 2024abfl at the extreme faint end of SNe IIP population. Its light curve exhibits a long-lasting plateau of approximately 110 days. The spectra show exceptionally low expansion velocities, with the \FeII\, velocity of at 50 days after the explosion, significantly lower than the typical values of observed in SNe IIP, placing SN\,2024abfl among the slowest-expanding LL SNe IIP. Bolometric modeling yields a synthesized Ni mass of , though this estimate remains subject to significant uncertainty owing to the poorly constrained distance. Considering the plateau color and duration, the magnitude drop from plateau to tail, and the progenitor luminosity, we favor a low-mass core-collapse origin for SN\,2024abfl.

Paper Structure

This paper contains 25 sections, 4 equations, 14 figures, 9 tables.

Table of Contents

  1. Introduction
  2. Observations and data reduction
  3. Photometric data
  4. Spectroscopic data
  5. Basic target information
  6. Location
  7. Extinction
  8. Explosion epoch
  9. Distance
  10. Photometry
  11. Apparent light curves
  12. Absolute light curve and comparisons
  13. Color evolution
  14. Bolometric light curve
  15. Spectroscopy
  16. ...and 10 more sections

Figures (14)

  • Figure 1: Image of the location of SN 2024abfl in NGC 2146, obtained with the LJT in the $BVr$ filters by combining data from multiple epochs. The local reference stars listed in Table \ref{['table:reference_star']} are marked with a nearby number. The orientation and scale of the images are reported.
  • Figure 2: Multi-band apparent light curves of SN 2024abfl obtained with the LJT, ATLAS, ZTF, and Swift/UVOT. All measurements are shifted vertically for better visibility. The adopted explosion epoch is $\rm MJD = 60623.16$. ATLAS data have been combined into daily stacks. The best-fit expanding fireball model for $o$ band is also plotted here. The direct $V$-band data with LJT is lacking around 20-80 days, so we employed the transformation equations for stars from 2005AJ....130..873J to improve the coverage of the $V$-band light curve (green inverted triangles). The epochs of our spectra are marked with vertical solid red lines at the bottom. In most cases, the photometric uncertainties are smaller than the symbol sizes.
  • Figure 3: Comparison of the absolute $r/R$-band light curve of SN 2024abfl with those well-observed SNe II. Two distances derived from different methods are considered for SN 2024abfl. Due to the large distance uncertainty of SN 2024abfl, we show only the magnitude error bar associated with the distance in the lower left of the figure.
  • Figure 4: Colour evolution of SN 2024abfl, along with that of other well-studied SNe II. All the colours have been corrected for both the Galactic and host-galaxy reddening.
  • Figure 5: Bolometric luminosity evolution of SN 2024abfl, along with that of other well-studied SNe II. Due to the large distance uncertainty of SN 2024abfl, we show only the luminosity error bar associated with the distance in the lower left of the top panel. The bottom panel presents the two-component model fits to the SN 2024abfl light curves, based on the model from 2016AA...589A..53N.
  • ...and 9 more figures