Статья

The Hydrogen-poor Superluminous Supernovae from the Zwicky Transient Facility Phase I Survey. II. Light-curve Modeling and Characterization of Undulations

Zhihao ChenPhysics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing, 100084, People's Republic of China [email protected]Lin YanCaltech Optical Observatories, California Institute of Technology, Pasadena, CA 91125, USA; [email protected]T. KangasThe Oskar Klein Centre, KTH Royal Institute of Technology, Stockholm, SwedenR. LunnanThe Oskar Klein Centre, Department of Astronomy, Stockholm University, AlbaNova, SE-106 91 Stockholm, SwedenJ. SollermanThe Oskar Klein Centre, Department of Astronomy, Stockholm University, AlbaNova, SE-106 91 Stockholm, SwedenS. SchulzeThe Oskar Klein Centre, Department of Physics, Stockholm University, AlbaNova, SE-106 91 Stockholm, SwedenD. A. PerleyAstrophysics Research Institute, Liverpool John Moores University, 146 Brownlow Hill, Liverpool L3 5RF, UKT. W. ChenThe Oskar Klein Centre, Department of Astronomy, Stockholm University, AlbaNova, SE-106 91 Stockholm, SwedenK. TaggartDepartment of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USAK-Ryan HindsAstrophysics Research Institute, Liverpool John Moores University, 146 Brownlow Hill, Liverpool L3 5RF, UKA. Gal‐YamDepartment of particle physics and astrophysics, Weizmann Institute of Science, 76100 Rehovot, IsraelXiaofeng WangBeijing Planetarium, Beijing Academy of Sciences and Technology, Beijing, 100044, People's Republic of ChinaKishalay DeCahill Center for Astrophysics, California Institute of Technology, 1200 E. California Blvd. Pasadena, CA 91125, USAE. BellmDIRAC Institute, Department of Astronomy, University of Washington, 3910 15th Avenue NE, Seattle, WA 98195, USAJ. S. BloomDepartment of Astrophysics, University of California, Berkeley, CA 94720-3411, USARichard DekanyCaltech Optical Observatories, California Institute of Technology, Pasadena, CA 91125, USA; [email protected]M. J. GrahamCahill Center for Astrophysics, California Institute of Technology, 1200 E. California Blvd. Pasadena, CA 91125, USAM. M. KasliwalDivision of Physics, Mathematics, and Astronomy, California Institute of Technology, Pasadena, CA 91125, USAS. R. KulkarniDivision of Physics, Mathematics, and Astronomy, California Institute of Technology, Pasadena, CA 91125, USARuss R. LaherIPAC, California Institute of Technology, 1200 E. California Blvd, Pasadena, CA 91125, USAD. NeillCahill Center for Astrophysics, California Institute of Technology, 1200 E. California Blvd. Pasadena, CA 91125, USABen RusholmeIPAC, California Institute of Technology, 1200 E. California Blvd, Pasadena, CA 91125, USA

2023en

ABI

Аннотация

Abstract 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 cannot unambiguously constrain the physical power sources for an 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 favors 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 <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mn>1.7</mml:mn> <mml:msubsup> <mml:mrow> <mml:mo>%</mml:mo> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>0.7</mml:mn> <mml:mo>%</mml:mo> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>1.5</mml:mn> <mml:mo>%</mml:mo> </mml:mrow> </mml:msubsup> <mml:mspace width="0.25em"/> <mml:msub> <mml:mrow> <mml:mi>E</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>rad</mml:mi> <mml:mo>,</mml:mo> <mml:mi>total</mml:mi> </mml:mrow> </mml:msub> </mml:math> and <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msubsup> <mml:mrow> <mml:mn>28.8</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>9.1</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>14.4</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> days, respectively. Our analysis of the undulation timescales suggests that intrinsic temporal variations of the central engine can explain half of the undulating events, while CSM interaction (CSI) can account for the majority of the sample. Finally, all of the well-observed He-rich SLSNe Ib either have 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.

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Идентификаторы

DOI: 10.3847/1538-4357/aca162

Цитирования и источники

Цитирований: 3Использованных источников: 0

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