SN 2024abvb: A Type Icn Supernova in the Outskirts of Its Host Galaxy

Abstract We present multiband photometric and spectroscopic observations of supernova (SN) 2024abvb, which exhibits early-time prominent photoionized narrow emission lines of C II superposed on a blue continuum. The absence of Balmer features indicates that the SN exploded within hydrogen-poor circumstellar matter (CSM). Together with the lack of explicit evidence of helium signatures, we tentatively identify SN 2024abvb as a Type Icn SN (SN Icn). After correcting for extinction, we estimate an r -band peak absolute magnitude of −19.7 ± 0.1, placing SN 2024abvb in the luminous regime of SNe Icn. We adopted a hybrid model that accounts for both the energy released by the ejecta-CSM interaction and the radioactive decay of nickel synthesized in the SN ejecta to fit the light curve of SN 2024abvb. The best-fit model to the multiband light curves within the first ∼40 days after explosion suggests the CSM, radioactive nickel, and ejecta masses to be 0.2 8 − 0.03 + 0.02 M ⊙ , ≤ 3.8 × 10 −2 M ⊙ , and 0.1 2 − 0.02 + 0.06 M ⊙ , respectively. Such a low ejecta mass indicates that the progenitor star of SN 2024abvb experienced a significant mass-stripping process, consistent with the hydrogen-poor and helium-poor spectral features. SN 2024abvb provides important insights into the physical origins of the rare subclass of SNe Icn.