Export Citation
Export Citation
Wang, ZY 
ORCID: 0000-0002-3231-1167, Pastorello, A ORCID: 0000-0002-7259-4624, Cai, YZ ORCID: 0000-0002-7714-493X, Fraser, M ORCID: 0000-0003-2191-1674, Reguitti, A ORCID: 0000-0003-4254-2724, Lin, WL, Tartaglia, L, Andrew Howell, D, Benetti, S, Cappellaro, E, Chen, ZH, Elias-Rosa, N ORCID: 0000-0002-1381-9125, Farah, J, Fiore, A ORCID: 0000-0002-0403-3331, Hiramatsu, D, Kankare, E ORCID: 0000-0001-8257-3512, Li, ZT, Lundqvist, P ORCID: 0000-0002-3664-8082, Mazzali, PA ORCID: 0000-0001-6876-8284, Mccully, C et al
(2025)
Massive stars exploding in a He-rich circumstellar medium: XI. Diverse evolution of five Ibn SNe 2020nxt, 2020taz, 2021bbv, 2023utc, and 2024aej.
Astronomy and Astrophysics, 700.
ISSN 0004-6361
Preview |
Text
Massive stars exploding in a Herich circumstellar medium XI Diverse evolution.pdf - Published Version Available under License Creative Commons Attribution. Download (51MB) | Preview |
Abstract
We present the photometric and spectroscopic analysis of five Type Ibn supernovae (SNe): SN 2020nxt, SN 2020taz, SN 2021bbv, SN 2023utc, and SN 2024aej. These events share key observational features and belong to a family of objects similar to the prototypical Type Ibn SN 2006jc. The SNe exhibit rise times of approximately 10 days and peak absolute magnitudes ranging from −16.5 to −19 mag. Notably, SN 2023utc is the faintest Type Ibn SN discovered to date, with an exceptionally low r-band absolute magnitude of −16.4 mag. The pseudo-bolometric light curves peak at (1 − 10)×1042 erg s−1, with total radiated energies on the order of (1 − 10)×1048 erg. Spectroscopically, these SNe display a relatively slow spectral evolution. The early spectra are characterised by a hot blue continuum and prominent He I emission lines. The early spectra also show blackbody temperatures exceeding 10 000 K, with a subsequent decline in temperature during later phases. Narrow He I lines, which are indicative of unshocked circumstellar material (CSM), show velocities of approximately 1000 km s−1. The spectra suggest that the progenitors of these SNe underwent significant mass loss prior to the explosion, resulting in a He-rich CSM. Our light curve modelling yielded estimates for the ejecta mass (Mej) in the range 1 − 3 M⊙ with kinetic energies (EKin) of (0.1 − 1)×1050 erg. The inferred CSM mass ranges from 0.2 to 1 M⊙. These findings are consistent with expectations for core collapse events arising from relatively massive envelope-stripped progenitors.
| Item Type: | Article |
|---|---|
| Uncontrolled Keywords: | 5109 Space Sciences; 51 Physical Sciences; 0201 Astronomical and Space Sciences; Astronomy & Astrophysics; 5101 Astronomical sciences; 5107 Particle and high energy physics; 5109 Space sciences |
| Subjects: | Q Science > QB Astronomy Q Science > QC Physics |
| Divisions: | Astrophysics Research Institute |
| Publisher: | EDP Sciences |
| Date of acceptance: | 16 June 2025 |
| Date of first compliant Open Access: | 5 September 2025 |
| Date Deposited: | 05 Sep 2025 12:05 |
| Last Modified: | 05 Sep 2025 12:15 |
| DOI or ID number: | 10.1051/0004-6361/202554768 |
| URI: | https://researchonline.ljmu.ac.uk/id/eprint/27103 |
 |
View Item |