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

Author:

Yang YiORCID,Baade Dietrich1,Hoeflich Peter2,Wang Lifan3,Cikota Aleksandar4ORCID,Chen Ting-Wan56,Burke Jamison78,Hiramatsu Daichi78910,Pellegrino Craig78,Howell D Andrew78,McCully Curtis7,Valenti Stefano11,Schulze Steve1213ORCID,Gal-Yam Avishay12,Wang Lingzhi1415,Filippenko Alexei V1617,Maeda Keiichi18,Bulla Mattia6ORCID,Yao Yuhan19,Maund Justyn R20ORCID,Patat Ferdinando1,Spyromilio Jason1,Wheeler J Craig21ORCID,Rau Arne5,Hu Lei22,Li Wenxiong23,Andrews Jennifer E2425,Galbany Llúis2627ORCID,Sand David J24,Shahbandeh Melissa2,Hsiao Eric Y2,Wang Xiaofeng2829

Affiliation:

1. European Organisation for Astronomical Research in the Southern Hemisphere (ESO) , Karl-Schwarzschild-Str. 2, D-85748 Garching b. München, Germany

2. Department of Physics, Florida State University , Tallahassee, FL 32306-4350, USA

3. George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, Texas A&M University , 4242 TAMU, College Station, TX 77843, USA

4. European Organisation for Astronomical Research in the Southern Hemisphere (ESO) , Alonso de Cordova 3107, Vitacura, Casilla 19001, Santiago de Chile, Chile

5. Max-Planck-Institut für Extraterrestrische Physik , Giessenbachstraße 1, D-85748 Garching, Germany

6. The Oskar Klein Centre, Department of Astronomy, Stockholm University , AlbaNova, SE-10691 Stockholm, Sweden

7. Las Cumbres Observatory , 6740 Cortona Drive, Suite 102, Goleta, CA 93117-5575, USA

8. Department of Physics, University of California , Santa Barbara, CA 93106-9530, USA

9. Center for Astrophysics, Harvard and Smithsonian , 60 Garden Street, Cambridge, MA 02138-1516, USA

10. The NSF AI Institute for Artificial Intelligence and Fundamental Interactions , Cambridge, MA 02139-4307, USA

11. Department of Physics, University of California , Davis, CA 95616, USA

12. Department of Particle Physics and Astrophysics, Weizmann Institute of Science , Rehovot 76100, Israel

13. The Oskar Klein Centre, Physics Department, Stockholm University , Albanova University Center, SE-106 91 Stockholm, Sweden

14. Chinese Academy of Sciences, South America Center for Astronomy, National Astronomical Observatories , CAS, Beijing 100101, People’s Republic of China

15. CAS Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People’s Republic of China

16. Department of Astronomy, University of California , Berkeley, CA 94720-3411, USA

17. Miller Institute for Basic Research in Science, University of California , Berkeley, CA 94720, USA

18. Department of Astronomy, Kyoto University , Kitashirakawa-Oiwake-cho, Sakyo-ku, Kyoto 606-8502, Japan

19. Cahill Center for Astrophysics, California Institute of Technology , MC 249-17, 1200 E. California Boulevard, Pasadena, CA 91125, USA

20. Department of Physics and Astronomy, University of Sheffield , Hicks Building, Hounsfield Road, Sheffield S3 7RH, UK

21. Department of Astronomy, University of Texas , Austin, TX 78712, USA

22. Purple Mountain Observatory, Chinese Academy of Sciences , Nanjing 210008, China

23. The Raymond and Beverly Sackler School of Physics and Astronomy, Tel Aviv University , Tel Aviv 69978, Israel

24. Steward Observatory, University of Arizona , 933 North Cherry Avenue, Tucson, AZ 85721-0065, USA

25. Gemini Observatory/NSF’s NOIRLab , 670 N. A’ohoku Place, Hilo, HI 96720, USA

26. Institute of Space Sciences (ICE, CSIC) , Campus UAB, Carrer de Can Magrans, s/n, E-08193 Barcelona, Spain

27. Institut d’Estudis Espacials de Catalunya (IEEC) , E-08034 Barcelona, Spain

28. Physics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University , Beijing 100084, People’s Republic of China

29. Beijing Planetarium, Beijing Academy of Science and Technology , Beijing 100044, People’s Republic of China

Abstract

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.

Funder

ESO

National Aeronautics and Space Administration

European Space Agency

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

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