A1 Refereed original research article in a scientific journal
SN 2024abfo: A partially stripped type II supernova from a yellow supergiant
Authors: Reguitti, A.; Pastorello, A.; Smartt, S. J.; Valerin, G.; Pignata, G.; Campana, S.; Chen, T. -W; Sankar, A. K.; Moran, S.; Mazzali, P. A.; Duarte, J.; Salmaso, I.; Anderson, J. P.; Ashall, C.; Benetti, S.; Gromadzki, M.; Gutierrez, C. P.; Humina, C.; Inserra, C.; Kankare, E.; Kravtsov, T.; Muller-Bravo, T. E.; Pessi, P. J.; Sollerman, J.; Young, D. R.; Chambers, K.; de Boer, T.; Gao, H.; Huber, M.; Lin, C. -C; Lowe, T.; Magnier, E.; Minguez, P.; Smith, I. A.; Smith, K. W.; Srivastav, S.; Wainscoat, R.; Benedet, M.
Publisher: EDP Sciences
Publishing place: LES ULIS CEDEX A
Publication year: 2025
Journal: Astronomy and Astrophysics
Journal name in source: Astronomy & Astrophysics
Journal acronym: ASTRON ASTROPHYS
Article number: A129
Volume: 698
Number of pages: 9
ISSN: 0004-6361
eISSN: 1432-0746
DOI: https://doi.org/10.1051/0004-6361/202554388
Web address : https://doi.org/10.1051/0004-6361/202554388
Self-archived copy’s web address: https://research.utu.fi/converis/portal/detail/Publication/499066001
We present photometric and spectroscopic data of the type IIb supernova (SN) 2024abfo in NGC 1493 (at 11 Mpc). The steroid Terrestrial-impact Last Alert System (ATLAS) survey discovered the object just a few hours after the explosion and observed a fast rise on the first day. Signs of the sharp shock breakout peak and the subsequent cooling phase are observed in the ultraviolet and the bluest optical bands in the first couple of days, while no peak is visible in the reddest filters. Subsequently, in analogy with normal SNe IIb, the light curve of SN 2024abfo rises again in all bands to the broad peak, with the maximum light reached around 1 month after the explosion. Its absolute magnitude at peak is M-r = -16.5 +/- 0.1 mag, making it a faint SN IIb. The early spectra are dominated by Balmer lines with broad P Cygni profiles, indicating ejecta velocity of 22 500 km s(-1). One month after the explosion, the spectra display a transition towards being He-dominated, though the H lines do not completely disappear, supporting the classification of SN 2024abfo as a relatively H-rich SN IIb. We identify the progenitor of SN 2024abfo in archival images of the Hubble Space Telescope, the Dark Energy Survey, and the XMM-Newton space telescope, in multiple optical filters. From its spectral energy distribution, the progenitor is consistent with being a yellow supergiant, having an initial mass of 15 M-circle dot. This detection supports an emerging trend of SN IIb progenitors being more luminous and hotter than SN II ones, and being primaries of massive binaries. Within the SN IIb class, fainter events such as SN 2024abfo tend to have cooler and more expanded progenitors than luminous SNe IIb.
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We thank the anonymous referee for the useful comments and suggested corrections to the manuscript. We thank N. Elias-Rosa for her comments. AR acknowledges financial support from the GRAWITA Large Program Grant (PI P. D'Avanzo). AR, AP, GV, IS, SB acknowledge financial support from the PRIN-INAF 2022 "Shedding light on the nature of gap transients: from the observations to the models". SJS acknowledges funding from STFC Grants ST/Y001605/1, ST/X006506/1, ST/T000198/1, a Royal Society Research Professorship and the Hintze Charitable Foundation. T.-W.C. acknowledges the Yushan Fellow Program by the Ministry of Education, Taiwan for the financial support (MOE-111-YSFMS-0008-001-P1). JD acknowledge support by FCT for CENTRA through Project No. UIDB/00099/2020 and under the PhD grant 2023.01333.BD. T.E.M.B. is funded by Horizon Europe ERC grant no. 101125877. NSF's NOIRLab (National Optical-Infrared Astronomy Research Laboratory), the US center for ground-based optical-infrared astronomy, operates the Cerro Tololo Inter-American Observatory (CTIO). It is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with NSF. Based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere, Chile, as part of ePESSTO+ (the advanced Public ESO Spectroscopic Survey for Transient Objects Survey - PI: Inserra), under ESO program ID 112.25JQ. Support to ATLAS was provided by NASA grant NN12AR55G. The Pan-STARRS1 Surveys (PS1) and the PS1 public science archive have been made possible through contributions by the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, the Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under Grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation Grant No. AST-1238877, the University of Maryland, Eotvos Lorand University (ELTE), the Los Alamos National Laboratory, and the Gordon and Betty Moore Foundation. We acknowledge the use of data from the Swift data archive.
