The Hydrogen-Poor Superluminous Supernovae from the Zwicky Transient Facility Phase-I Survey: II. Light Curve Modeling and Characterization of Undulations
Z. H. Chen, Lin Yan, T. Kangas, R. Lunnan, J. Sollerman, S. Schulze, D. A. Perley, T. -W. Chen, K. Taggart, K. R. Hinds, A. Gal-Yam, X. F. Wang, K. De, E. Bellm… 展开作者
Z. H. Chen, Lin Yan, T. Kangas, R. Lunnan, J. Sollerman, S. Schulze, D. A. Perley, T. -W. Chen, K. Taggart, K. R. Hinds, A. Gal-Yam, X. F. Wang, K. De, E. Bellm, J. S. Bloom, R. Dekany, M. Graham, M. Kasliwal, S. Kulkarni, R. Laher, D. Neill, B. Rusholme
We present analysis of the light curves (LCs) of 77 hydrogen-poor superluminous supernovae (SLSNe-I) discovered during the Zwicky Transient Facility Phase-I operation. We find that the majority (67\%) of the sample can be fit equally well by both magnetar and ejecta-circumstellar medium (CSM) interaction plus $^{56}$Ni decay models. This implies that LCs alone can not unambiguously constrain the physical power sources for a SLSN-I. However, 23\% of the sample show inverted V-shape, steep declining LCs or features of long rise and fast post-peak decay, which are better described by the CSM+Ni model. The remaining 10\% of the sample favor the magnetar model. Moreover, our analysis shows that the LC undulations are quite common, with a fraction of $18-44\% $ in our gold sample. Among those strongly undulating events, about 62\% of them are found to be CSM-favored, implying that the undulations tend to occur in the CSM-favored events. Undulations show a wide range in energy and duration, with median values (and 1$σ$ errors) being as $1.7\%^{+1.5\%}_{-0.7\%}\,\rm E_{\rm rad,total}$ and $28.8^{+14.4}_{-9.1}$\,days, respectively. Our analysis of the undulation time scales suggests that intrinsic temporal variations of the central engine can explain half of the undulating events, while CSM interaction can account for the majority of the sample. Finally, all of the well-observed He-rich SLSNe-Ib have either strongly undulating LCs or the LCs are much better fit by the CSM+Ni model. These observations imply that their progenitor stars have not had enough time to lose all of the He-envelopes before supernova explosions, and H-poor CSM are likely to present in these events.
ASASSN-13dn: A Luminous and Double-Peaked Type II Supernova
Universidad Diego Portales（迭戈帕塔莱斯大学）；Millennium Institute of Astrophysics MAS（天体物理学千年研究所MAS）；Carnegie Observatories, Las Campanas Observatory（卡内基观测台拉斯坎帕纳斯天文台）；Facultad de Ciencias Astronomicas y Geofisicas, Universidad Nacional de La Plata（拉普拉塔国立大学天文与地球物理科学学院）；Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo（东京大学宇宙物理与数学前沿国际研究中心(WPI)）；National Astronomical Observatory of Japan, National Institutes of Natural Sciences（日本国立天文台，国立自然科学研究机构）；Graduate Institute for Advanced Studies, SOKENDAI（综合研究大学院大学(SOKENDAI)）；School of Physics and Astronomy, Monash University（蒙纳士大学物理与天文学院）；Department of Astronomy, The Ohio State University（俄亥俄州立大学天文学系）；Center for Cosmology and AstroParticle Physics（宇宙学与粒子天体物理中心）；Institute for Astronomy, University of Hawaii（夏威夷大学天文学研究所）
