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Published November 20, 2024 | Version Published
Journal Article Open

Optical and Radio Analysis of Systematically Classified Broad-lined Type Ic Supernovae from the Zwicky Transient Facility

Creators

  • 1. ROR icon University of Maryland, College Park
  • 2. Astrophysics Science Division, NASA Goddard Space Flight Center, 8800 Greenbelt Road, Greenbelt, MD 20771, USA
  • 3. ROR icon Henan Academy of Sciences
  • 4. ROR icon California Institute of Technology
  • 5. ROR icon Stockholm University
  • 6. ROR icon Cornell University
  • 7. ROR icon Johns Hopkins University
  • 8. ROR icon Liverpool John Moores University
  • 9. ROR icon Northwestern University
  • 10. Astrophysics Science Division, NASA Goddard Space Flight Center, Mail Code 661, Greenbelt, MD 20771, USA
  • 11. ROR icon Weizmann Institute of Science
  • 12. ROR icon Massachusetts Institute of Technology
  • 13. NASA Einstein Fellow
  • 14. ROR icon Space Telescope Science Institute
  • 15. ROR icon Instituto de Astrofísica de Andalucía
  • 16. ROR icon University of Washington
  • 17. ROR icon University of California, Berkeley
  • 18. ROR icon New York State Office for People With Developmental Disabilities
  • 19. ROR icon Infrared Processing and Analysis Center
  • 20. ROR icon Drexel University

Abstract

We study a magnitude-limited sample of 36 broad-lined type Ic supernovae (SNe Ic-BL) from the Zwicky Transient Facility Bright Transient Survey (detected between 2018 March and 2021 August), which is the largest systematic study of SNe Ic-BL done in literature thus far. We present the light curves (LCs) for each of the SNe and analyze the shape of the LCs to derive empirical parameters, along with the explosion epochs for every event. The sample has an average absolute peak magnitude in the r band of M_(r, max) = −18.51 ± 0.15 mag. Using spectra obtained around peak light, we compute expansion velocities from the Fe ii 5169 Å line for each event with high enough signal-to-noise ratio spectra, and find an average value of v_(ph) = 16,100 ± 1100 km s⁻¹. We also compute bolometric LCs, study the blackbody temperature and radii evolution over time, and derive the explosion properties of the SNe. The explosion properties of the sample have average values of M(Ni) = 0.37_(−0.06)^(+0.08) M⊙, M_(ej) = 2.45_(−0.41)^(+0.47) M⊙, and E_K = (4.02_(−1.00)^(+1.37) × 10⁵¹ erg. Thirteen events have radio observations from the Very Large Array, with eight detections and five non-detections. We find that the populations that have radio detections and radio non-detections are indistinct from one another with respect to their optically inferred explosion properties, and there are no statistically significant correlations present between the events' radio luminosities and optically inferred explosion properties. This provides evidence that the explosion properties derived from optical data alone cannot give inferences about the radio properties of SNe Ic-BL and likely their relativistic jet formation mechanisms.

Copyright and License

© 2024. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI.

Acknowledgement

G.P.S. thanks Alexander Dittman, Cole Miller, Isiah Holt, Muhammad Mousa, and Maryam Modjaz for useful discussions regarding this work. G.P.S. thanks Cristina Barbarino, Tassilo Schweyer, Joonas Viuho, and Amanda Djupvik for obtaining spectra from NOT. G.P.S. also thanks Simi Bhullar for her moral support throughout the paper-writing process. S.Y. acknowledges the funding from the National Natural Science Foundation of China under grant No. 12303046 and the Henan Province High-Level Talent International Training Program. S.A. acknowledges generous support from the David and Lucile Packard Foundation and the National Science Foundation GROWTH PIRE grant No. 1545949. A.C. acknowledges support from the National Science Foundation via AST-2431072, and from the NASA Swift GI program via the award 80NSSC23K0314. S.S. is partially supported by LBNL Subcontract No. 7707915. N.S. acknowledges support from the Knut and Alice Wallenberg foundation through the “Gravity Meets Light” project (PIs: Rosswog & Jerkstrand).

This work was supported by the GROWTH project (M. M. Kasliwal et al. 2019) funded by the National Science Foundation under grant No. 1545949. M.M.K. acknowledges generous support from the David and Lucille Packard Foundation. Some of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. SED Machine is based upon work supported by the National Science Foundation under grant No. 1106171. Based on observations obtained with the Samuel Oschin Telescope 48 inch and the 60 inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project.

ZTF is supported by the National Science Foundation under grant No. AST-2034437 and a collaboration including Caltech, IPAC, the Weizmann Institute of Science, the Oskar Klein Center at Stockholm University, the University of Maryland, Deutsches Elektronen-Synchrotron and Humboldt University, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee, Trinity College Dublin, Lawrence Livermore National Laboratories, IN2P3, University of Warwick, Ruhr University Bochum, and Northwestern University. Operations are conducted by COO, IPAC, and UW. The ZTF forced-photometry service was funded under the Heising-Simons Foundation grant No. 12540303 (PI: Graham). The Gordon and Betty Moore Foundation, through both the Data-Driven Investigator Program and a dedicated grant, provided critical funding for SkyPortal. The Liverpool Telescope is operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias with financial support from the UK Science and Technology Facilities Council.

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Additional details

Related works

Is new version of
Discussion Paper: arXiv:2408.14586 (arXiv)

Funding

National Natural Science Foundation of China
12303046
David and Lucile Packard Foundation
National Natural Science Foundation of China
1545949
National Science Foundation
AST-2431072
National Aeronautics and Space Administration
80NSSC23K0314
Lawrence Berkeley National Laboratory
7707915
Knut and Alice Wallenberg Foundation
W. M. Keck Foundation
National Science Foundation
1106171
National Science Foundation
AST-2034437
Heising-Simons Foundation
12540303

Dates

Submitted
2024-08-26
Accepted
2024-09-24
Available
2024-11-13
Published

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Caltech groups
Infrared Processing and Analysis Center (IPAC) , Palomar Observatory , Division of Physics, Mathematics and Astronomy (PMA) , Astronomy Department , Zwicky Transient Facility
Publication Status
Published