Madison Gerard, Jennifer E. Andrews, Geoffrey C. Clayton, David J. Sand, K Azalee Bostroem, Jeniveve Pearson, Raya Dastidar, Aravind P. Ravi, C. L. Ransome, Bhagya Subrayan, G. Hosseinzadeh, Brian Hsu, Yize Dong, Manisha Shrestha, S. Valenti, Nathan Smith, Daryl Janzen, M. J. Lundquist, N. Meza, Saurabh W. Jha, K. D. Alexander, Collin T. Christy, Noah Franz, Lindsey A. Kwok, Moira Andrews, Joseph Farah, D. Hiramatsu, D. A. Howell, C. McCully, Kathryn Wynn, Réka Könyves-Tóth, Xiaofeng Wang, A. V. Filippenko, Thomas G. Brink
Abstract We present photometric and spectroscopic observations of SN 2024abfl, a low-luminosity Type IIP supernova (LLSN) discovered shortly after explosion. The transient reached a peak absolute magnitude of M V = −14.9 and exhibited an extended, flat plateau lasting ∼125 days. From the late-time bolometric light curve, we estimate a 56 Ni mass of ∼0.01 M ⊙ , consistent with other LLSNe. Analytical shock-cooling models fail to reproduce the rapid early rise, indicating that circumstellar matter (CSM) interaction contributed to the initial emission. The spectroscopic evolution is typical of LLSNe, with relatively narrow metal lines and low expansion velocities (≲3000 km s −1 ) that decline slowly over time. We detect a broad “ledge” feature around 4600 Å within 3 days of explosion, which we interpret as a blend of high-ionization, shock-accelerated CSM lines. Multipeaked H α profiles develop during the plateau phase, consistent with complex ejecta–CSM interaction. As one of the best-observed examples of LLSNe, SN 2024abfl exhibits a weak explosion and signatures of nearby CSM, offering new insights into progenitor properties, pre-explosion mass loss, and the diversity of LLSNe.