论文标题
奇特类型IBN SUPERNOVA SN 2019WEP的演变
Evolution of A Peculiar Type Ibn Supernova SN 2019wep
论文作者
论文摘要
我们提出了IBN SN 2019WEP的高级短期光度和光谱监测活动，该活动是在2010al和2019ue之后的罕见SN IBN之一，以显示闪光电离签名（\ ion {He} {He}我们将SN 2019WEP的下降率和上升时间与其他SNE IBN和快速瞬态进行了比较。所有乐队（0.1 mag d $^{ - 1} $）的峰值下降与SNE IBN一致，但小于快速瞬变。另一方面，$δ$ m $ _ {15} $值略低于SNE IBN的平均值，但与快速瞬变一致。上升时间通常比SNE IBN短，但比快速瞬变更长。 SN 2019WEP位于Sne IBN的脆弱端，但在快速瞬态样本中具有平均亮度。奇特的色彩演化将其放在SNE IB和最极端的SNE IBN之间。降压光曲线曲线建模显示与SN 2019UO具有与SNE IB一致的弹出质量的相似之处。 SN 2019WEP属于SNE IBN的“ P Cygni”子类，与“发射”子类相比，线速度的进化更快。最大后光谱显示出与Asassn-15的相似之处，暗示它是SN IB性质。低\ ion {He} {1} CSM速度和残留的H $α$进一步证明了它的合理性，并证明了WR和LBV星之间的间歇性祖细胞。
We present a high-cadence short term photometric and spectroscopic monitoring campaign of a type Ibn SN 2019wep, which is one of the rare SN Ibn after SNe 2010al and 2019uo to display signatures of flash ionization (\ion{He}{2}, \ion{C}{3}, \ion{N}{3}). We compare the decline rates and rise time of SN 2019wep with other SNe Ibn and fast transients. The post-peak decline in all bands (0.1 mag d$^{-1}$) are consistent with SNe Ibn but less than the fast transients. On the other hand, the $Δ$m$_{15}$ values are slightly lower than the average values for SNe Ibn but consistent with the fast transients. The rise time is typically shorter than SNe Ibn but longer than fast transients. SN 2019wep lies at the fainter end of SNe Ibn but possesses an average luminosity amongst the fast transients sample. The peculiar color evolution places it between SNe Ib and the most extreme SNe Ibn. The bolometric light curve modelling shows resemblance with SN 2019uo with ejecta masses consistent with SNe Ib. SN 2019wep belongs to the "P cygni" sub-class of SNe Ibn and shows faster evolution in line velocities as compared to the "emission" sub-class. The post-maximum spectra show close resemblance with ASASSN-15ed hinting it to be of SN Ib nature. The low \ion{He}{1} CSM velocities and residual H$α$ further justifies it and gives evidence of an intermittent progenitor between WR and LBV star.
