SN 2020zbf: A fast-rising hydrogen-poor superluminous supernova with strong carbon lines
arxiv(2023)
摘要
SN 2020zbf is a hydrogen-poor superluminous supernova (SLSN) at z = 0.1947
that shows conspicuous CII features at early times, in contrast to the
majority of H-poor SLSNe. Its peak magnitude is M_ g = -21.2 mag and
its rise time (≲ 26.4 days from first light) places SN 2020zbf among
the fastest rising type I SLSNe. We used spectra taken from ultraviolet (UV) to
near-infrared wavelengths to identify spectral features. We paid particular
attention to the CII lines as they present distinctive characteristics
when compared to other events. We also analyzed UV and optical photometric data
and modeled the light curves considering three different powering mechanisms:
radioactive decay of ^56Ni, magnetar spin-down, and circumstellar medium
(CSM) interaction. The spectra of SN 2020zbf match the model spectra of a
C-rich low-mass magnetar-powered supernova model well. This is consistent with
our light curve modeling, which supports a magnetar-powered event with an
ejecta mass M_ ej = 1.5 M_⊙. However, we cannot discard the
CSM-interaction model as it may also reproduce the observed features. The
interaction with H-poor, carbon-oxygen CSM near peak light could explain the
presence of CII emission lines. A short plateau in the light curve
around 35 – 45 days after peak, in combination with the presence of an
emission line at 6580 Å, can also be interpreted as being due to a late
interaction with an extended H-rich CSM. Both the magnetar and CSM-interaction
models of SN 2020zbf indicate that the progenitor mass at the time of
explosion is between 2 and 5 M_⊙. Modeling the spectral energy
distribution of the host galaxy reveals a host mass of 10^8.7 M_⊙, a star formation rate of 0.24^+0.41_-0.12 M_⊙ yr^-1, and a metallicity of ∼ 0.4 Z_⊙.
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