SN 2024abfo

SN 2024abfo
Host galaxy NGC 1493 imaged by Legacy Surveys
Event typeSupernova
Type II supernova
Date15, November 2024 (22:54:00.288)
InstrumentAsteroid Terrestrial-impact Last Alert System (ATLAS)
ConstellationHorologium
Right ascension03h 57m 25.622s
Declination−46° 11′ 07.67″
EpochJ2000
Distance11 Mpc
HostNGC 1493
Progenitor typeYellow supergiant (probably binary system)
Notable featuresRelatively faint, Hydrogen-dominated
Peak apparent magnitude−16.5 ±0.1

SN 2024abfo was a Type-IIb supernova event that occurred in NGC 1493 around 11 Mpc from Earth in the Constellation of Horologium.[1][2] The object was detected on the 15th of November, 2024 just a few hours after the explosion using the Asteroid Terrestrial-impact Last Alert System (ATLAS).[3] The progenitor of the supernova was able to be identified through archival images taken by numerous telescopes and surveys such as the Hubble Space Telescope (HST), XMM-Newton space telescope and the Dark Energy Survey.[1]

Properties

The explosion was fairly faint for a Type-IIb supernova with its peak absolute magnitude being −16.5 ± 0.1 mag. It was also a relatively hydrogen rich supernova for its type. Currently, SN 2024abfo is the least luminous SN IIb with direct progenitor detections.[1][2]

Spectra

The early spectra of SN 2024abfo was dominated by Balmer lines that have broad P Cygni profiles. This shows that the ejecta produced was traveling at a velocity of 22,500 km/s. Around a month after the explosion, spectra show that it was going through a transition towards being helium-dominated with the hydrogen lines not completely disappearing. Its fading was slow and linear, lasting for around 2 months.[1] Similar to SN 2008ax, it does not show a prominent double-peaked light curve.[2]

Progenitor

Single star models of the progenitor of SN 2024abfo show that the progenitor likely would have been a hot yellow supergiant star with a mass of around 11-15 solar masses.[1] The most probable model for the progenitor of the supernova is the binary model. This model predicts that the progenitor was a 12 solar mass star in a binary system with a 1.2 solar mass companion. They would have had an orbital period of around 1.73 years.[2]

References

  1. 1 2 3 4 5 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. (2025-06-01). "SN 2024abfo: A partially stripped type II supernova from a yellow supergiant". Astronomy & Astrophysics. 698: A129. arXiv:2503.03851. Bibcode:2025A&A...698A.129R. doi:10.1051/0004-6361/202554388. ISSN 0004-6361.
  2. 1 2 3 4 de Wet, S.; Leloudas, G.; Buckley, D.; Erasmus, N.; Groot, P. J.; Zimmerman, E. (2025-07-15). "A low mass, binary-stripped envelope for the Type IIb SN 2024abfo". Astronomy & Astrophysics. 704: A89. arXiv:2507.11131v1. Bibcode:2025A&A...704A..89D. doi:10.1051/0004-6361/202556356.
  3. ↑ "2024abfo | Transient Name Server". www.wis-tns.org. Retrieved 2026-04-07.
This page is issued from Wikipedia. The text is available under Creative Commons Attribution-Share Alike 4.0 unless otherwise noted. Additional terms may apply for the media files.