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Karamehmetoglu, E, Fransson, C, Sollerman, J, Tartaglia, L, Taddia, F, De, K, Fremling, C, Bagdasaryan, A, Barbarino, C, Bellm, EC, Dekany, R, Dugas, AM, Giomi, M, Goobar, A, Graham, M, Ho, A, Laher, RR, Masci, FJ, Neill, JD, Perley, DA , Riddle, R, Rusholme, B and Soumagnac, MT (2021) The luminous and rapidly evolving SN 2018bcc: Clues toward the origin of Type Ibn SNe from the Zwicky Transient Facility. Astronomy and Astrophysics, 649. ISSN 0004-6361
Full text not available from this repository. Please see publisher or open access link below:Abstract
Context. Supernovae (SNe) Type Ibn are rapidly evolving and bright (MR,peak-19) transients interacting with He-rich circumstellar material (CSM). SN 2018bcc, detected by the ZTF shortly after explosion, provides the best constraints on the shape of the rising light curve (LC) of a fast Type Ibn. Aims. We used the high-quality data set of SN 2018bcc to study observational signatures of the class. Additionally, the powering mechanism of SN 2018bcc offers insights into the debated progenitor connection of Type Ibn SNe. Methods. We compared well-constrained LC properties obtained from empirical models with the literature. We fit the pseudo-bolometric LC with semi-analytical models powered by radioactive decay and CSM interaction. Finally, we modeled the line profiles and emissivity of the prominent He » I lines, in order to study the formation of P-Cygni profiles and to estimate CSM properties. Results. SN 2018bcc had a rise time to peak of the LC of 5.6-0.1+0.2 days in the restframe with a rising shape power-law index close to 2, and seems to be a typical rapidly evolving Type Ibn SN. The spectrum lacked signatures of SN-like ejecta and was dominated by over 15 He emission features at 20 days past peak, alongside Ca and Mg, all with VFWHM ∼2000 km s-1. The luminous and rapidly evolving LC could be powered by CSM interaction but not by the decay of radioactive 56Ni. Modeling of the He » I lines indicated a dense and optically thick CSM that can explain the P-Cygni profiles. Conclusions. Like other rapidly evolving Type Ibn SNe, SN 2018bcc is a luminous transient with a rapid rise to peak powered by shock interaction inside a dense and He-rich CSM. Its spectra do not support the existence of two Type Ibn spectral classes. We also note the remarkable observational match to pulsational pair instability SN models.
| Item Type: | Article |
|---|---|
| Additional Information: | The luminous and rapidly evolving SN 2018bcc - Clues toward the origin of Type Ibn SNe from the Zwicky Transient Facility E. Karamehmetoglu, C. Fransson, J. Sollerman, L. Tartaglia, F. Taddia, K. De, C. Fremling, A. Bagdasaryan, C. Barbarino, E. C. Bellm, R. Dekany, A. M. Dugas, M. Giomi, A. Goobar, M. Graham, A. Ho, R. R. Laher, F. J. Masci, J. D. Neill, D. Perley, R. Riddle, B. Rusholme and M. T. Soumagnac A&A, 649 (2021) A163 DOI: https://doi.org/10.1051/0004-6361/201936308 |
| Uncontrolled Keywords: | 0201 Astronomical and Space Sciences |
| Subjects: | Q Science > QB Astronomy Q Science > QC Physics |
| Divisions: | Astrophysics Research Institute |
| Publisher: | EDP Sciences |
| Date Deposited: | 15 Dec 2021 12:11 |
| Last Modified: | 16 Jan 2023 10:14 |
| DOI or ID number: | 10.1051/0004-6361/201936308 |
| URI: | https://researchonline.ljmu.ac.uk/id/eprint/15909 |
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