CaltechAUTHORS
Published February 2023 | Version Published
Journal Article Open

The interaction of supernova 2018evt with a substantial amount of circumstellar matter - An SN 1997cy-like event

Creators

  • 1. ROR icon European Southern Observatory
  • 2. ROR icon Florida State University
  • 3. ROR icon Texas A&M University
  • 4. ROR icon Max Planck Institute for Extraterrestrial Physics
  • 5. ROR icon Stockholm University
  • 6. ROR icon Las Cumbres Observatory Global Telescope Network
  • 7. ROR icon University of California, Santa Barbara
  • 8. ROR icon Harvard-Smithsonian Center for Astrophysics
  • 9. ROR icon AI Institute for Artificial Intelligence and Fundamental Interactions
  • 10. ROR icon University of California, Davis
  • 11. ROR icon Weizmann Institute of Science
  • 12. ROR icon National Astronomical Observatories
  • 13. ROR icon University of California, Berkeley
  • 14. ROR icon Kyoto University
  • 15. ROR icon California Institute of Technology
  • 16. ROR icon University of Sheffield
  • 17. ROR icon The University of Texas at Austin
  • 18. ROR icon Purple Mountain Observatory
  • 19. ROR icon Tel Aviv University
  • 20. ROR icon University of Arizona
  • 21. ROR icon Institute of Space Sciences
  • 22. ROR icon Institut d'Estudis Espacials de Catalunya
  • 23. ROR icon Tsinghua University
  • 24. ROR icon Beijing Academy of Science and Technology

Abstract

A rare class of supernovae (SNe) is characterized by strong interaction between the ejecta and several solar masses of circumstellar matter (CSM) as evidenced by strong Balmer-line emission. Within the first few weeks after the explosion, they may display spectral features similar to overluminous Type Ia SNe, while at later phase their observation properties exhibit remarkable similarities with some extreme case of Type IIn SNe that show strong Balmer lines years after the explosion. We present polarimetric observations of SN 2018evt obtained by the ESO Very Large Telescope from 172 to 219 d after the estimated time of peak luminosity to study the geometry of the CSM. The non-zero continuum polarization decreases over time, suggesting that the mass-loss of the progenitor star is aspherical. The prominent H α emission can be decomposed into a broad, time-evolving component and an intermediate-width, static component. The former shows polarized signals, and it is likely to arise from a cold dense shell (CDS) within the region between the forward and reverse shocks. The latter is significantly unpolarized, and it is likely to arise from shocked, fragmented gas clouds in the H-rich CSM. We infer that SN 2018evt exploded inside a massive and aspherical circumstellar cloud. The symmetry axes of the CSM and the SN appear to be similar. SN 2018evt shows observational properties common to events that display strong interaction between the ejecta and CSM, implying that they share similar circumstellar configurations. Our preliminary estimate also suggests that the circumstellar environment of SN 2018evt has been significantly enriched at a rate of ∼0.1 M_⊙ yr₋₁ over a period of >100 yr.

Additional Information

© 2022 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model) We would like to thank the referee Dr. Nikolai N. Chugai for his careful scrutiny which resulted in very helpful, constructive suggestions that significantly improved the paper. Melissa L. Graham provided helpful discussion and assistance with follow-up observation planning. We are grateful to the European Organisation for Astronomical Research in the Southern Hemisphere (ESO) for the generous allocation of observing time. We especially thank the staff of the Paranal Observatory for their proficient and motivated support of this project in service mode. The polarimetric studies in this work are based on observations collected at ESO's La Silla Paranal Observatory under programme IDs 0102.D-0163(A) and 2102.D-5031. Some spectra presented in this work are based on observations collected as part of the extended Public ESO Spectroscopic Survey for Transient Objects (ePESSTO; Smartt et al. 2015), program 199.D-0143(M). GROND observations at La Silla were performed as part of program 102.A-9099. Some of the funding for GROND (both hardware as well as personnel) was generously provided by the Leibniz Prize to Prof. G. Hasinger (DFG grant HA 1850/28-1). We acknowledge usage of observations of SNe 2018evt and 2012ca made with the Las Cumbres Observatory (LCO) global telescope network. Other observations of SN 2012ca were secured at ESO's La Silla Paranal Observatory as part of the PESSTO survey (ESO programs 188.D-3003 and 191.D-0935), as well as with the Panchromatic Robotic Optical Monitoring and Polarimetry Telescope (PROMPT) through CNTAC proposal CN2012A-103, with the Australian National University 2.3 m Telescope, and with the Neil Gehrels Swift Observatory. PYRAF, PYFITS, and STSCI_ PYTHON are products of the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under National Aeronautics and Space Administration (NASA) contract NAS5-26555. We also use data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This research has made use of NASA's Astrophysics Data System Bibliographic Services; the SIMBAD data base, operated at CDS, Strasbourg, France; the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. The Infrared Telescope Facility is operated by the University of Hawaii under contract NNH14CK55B with NASA. The research of YY has been supported through a Benoziyo Prize Postdoctoral Fellowship and the Bengier-Winslow-Robertson Fellowship. MB acknowledges support from the Swedish Research Council (Reg. no. 2020-03330). TWC is grateful for funding from the Alexander von Humboldt Foundation and the EU Funding under Marie Skłodowska-Curie grant H2020-MSCA-IF-2018-842471. A. V. Filippenko's group at U.C. Berkeley acknowledges generous support from the TABASGO Foundation, the Christopher R. Redlich fund, the Miller Institute for Basic Research in Science (in which A.V.F. was a Miller Senior Fellow), Sunil Nagaraj, Landon Noll, Gary and Cynthia Bengier, Clark and Sharon Winslow, Sanford Robertson, and many additional donors. LG acknowledges financial support from the Spanish Ministerio de Ciencia e Innovación (MCIN), the Agencia Estatal de Investigación (AEI) 10.13039/501100011033, and by the European Social Fund (ESF) 'Investing in your future' under the 2019 Ramón y Cajal program RYC2019-027683-I and the PID2020-115253GA-I00 HOSTFLOWS project. AG-Y's research is supported by the EU via ERC grant 725161, the ISF GW excellence center, an IMOS space infrastructure grant and BSF/Transformative and GIF grants, as well as The Benoziyo Endowment Fund for the Advancement of Science, the Deloro Institute for Advanced Research in Space and Optics, The Veronika A. Rabl Physics Discretionary Fund, Minerva, Yeda-Sela, and the Schwartz/Reisman Collaborative Science Program; AG-Y is the incumbent of the The Arlyn Imberman Professorial Chair. D. Hiramatsu was supported by NSF grants AST-1313484 and AST-1911225, as well as by NASA grant 80NSSC19kf1639. PH acknowledges support from the NSF project 'Signatures of Type Ia Supernovae, New Physics, and Cosmology,' grant AST-1715133. EYH and MS acknowledge support provided by NSF grant AST-161347 and the Florida Space Research Program. The research of JM is supported through a Royal Society University Research Fellowship. CM and GH were supported by NSF grant AST-1313484. CP was supported by NSF grant AST-1911225. Time-domain research by DJS is supported by NSF grants AST-1821987, 1813466, and 1908972, and by the Heising-Simons Foundation under grant #2020-1864. The supernova research by LW is supported by NSF award AST-1817099 and HST-GO-14139.001-A. LW is sponsored in part by the Chinese Academy of Sciences (CAS), through a grant to the CAS South America Center for Astronomy (CASSACA) in Santiago, Chile. XW is supported by the National Natural Science Foundation of China (NSFC grants 11178003 and 11325313). JCW is supported by NSF grant AST-1813825. The LCO team is supported by NSF grants AST-1911225 and AST-1911151. DATA AVAILABILITY. The reduced data used in this work may be shared upon request to Yi Yang (yiyangtamu@gmail.com).

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Additional details

Identifiers

Eprint ID
120261
Resolver ID
CaltechAUTHORS:20230321-821906400.69

Funding

Deutsche Forschungsgemeinschaft (DFG)
HA 1850/28-1
NASA
NAS5-26555
Gaia Multilateral Agreement
NASA/JPL/Caltech
NASA
NNH14CK55B
Weizmann Institute of Science
Swedish Research Council
2020-03330
Alexander von Humboldt Foundation
Marie Curie Fellowship
842471
TABASGO Foundation
Christopher R. Redlich Fund
Miller Institute for Basic Research in Science
Ministerio de Ciencia e Innovación (MCIN)
Agencia Estatal de Investigación
10.13039/501100011033
European Social Fund
Ramón y Cajal Programme
RYC2019-027683-I
Agencia Estatal de Investigación
PID2020-115253GA-I00
European Research Council (ERC)
725161
Israel Science Foundation
Binational Science Foundation (USA-Israel)
German-Israeli Foundation for Research and Development
Benoziyo Endowment Fund for the Advancement of Science
Deloro Institute for Advanced Research in Space and Optics
Veronika A. Rabl Physics Discretionary Fund
MINERVA (Israel)
Yeda-Sela
Schwartz/Reisman Collaborative Science Program
Arlyn Imberman Professorial Chair
NSF
AST-1313484
NSF
AST-1911225
NASA
80NSSC19kf1639
NSF
AST-1715133
NSF
AST-1613472
Florida Space Grant Consortium
Royal Society
NSF
AST-1313484
NSF
AST-1911225
NSF
AST-1821987
NSF
AST-1813466
NSF
AST-1908972
Heising-Simons Foundation
2020-1864
NSF
AST-1817099
NASA
HST-GO-14139.001-A
CAS South America Center for Astronomy (CASSACA)
National Natural Science Foundation of China
11178003
National Natural Science Foundation of China
11325313
NSF
AST-1813825
NSF
AST-1911225
NSF
AST-1911151

Dates

Created
2023-06-08
Created from EPrint's datestamp field
Updated
2023-06-08
Created from EPrint's last_modified field