A Multiwavelength View of the Rapidly Evolving SN 2018ivc: An Analog of SN IIb 1993J but Powered Primarily by Circumstellar Interaction
SN 2018ivc is an unusual Type II supernova (SN II). It is a variant of SNe IIL, which might represent a transitional case between SNe IIP with a massive H-rich envelope and SNe IIb with only a small amount of the H-rich envelope. However, SN 2018ivc shows an optical light-curve evolution more compli...
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IOP Publishing
2022-01-01
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| Online Access: | https://doi.org/10.3847/1538-4357/aca1b7 |
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| author | Keiichi Maeda Poonam Chandra Takashi J. Moriya Andrea Reguitti Stuart Ryder Tomoki Matsuoka Tomonari Michiyama Giuliano Pignata Daichi Hiramatsu K. Azalee Bostroem Esha Kundu Hanindyo Kuncarayakti Melina C. Bersten David Pooley Shiu-Hang Lee Daniel Patnaude Ósmar Rodríguez Gaston Folatelli |
| author_facet | Keiichi Maeda Poonam Chandra Takashi J. Moriya Andrea Reguitti Stuart Ryder Tomoki Matsuoka Tomonari Michiyama Giuliano Pignata Daichi Hiramatsu K. Azalee Bostroem Esha Kundu Hanindyo Kuncarayakti Melina C. Bersten David Pooley Shiu-Hang Lee Daniel Patnaude Ósmar Rodríguez Gaston Folatelli |
| author_sort | Keiichi Maeda |
| collection | DOAJ |
| description | SN 2018ivc is an unusual Type II supernova (SN II). It is a variant of SNe IIL, which might represent a transitional case between SNe IIP with a massive H-rich envelope and SNe IIb with only a small amount of the H-rich envelope. However, SN 2018ivc shows an optical light-curve evolution more complicated than that of canonical SNe IIL. In this paper, we present the results of prompt follow-up observations of SN 2018ivc with the Atacama Large Millimeter/submillimeter Array. Its synchrotron emission is similar to that of SN IIb 1993J, suggesting that it is intrinsically an SN IIb–like explosion of an He star with a modest (∼0.5–1 M _⊙ ) extended H-rich envelope. Its radio, optical, and X-ray light curves are explained primarily by the interaction between the SN ejecta and the circumstellar material (CSM); we thus suggest that it is a rare example (and the first involving the “canonical” SN IIb ejecta) for which the multiwavelength emission is powered mainly by the SN–CSM interaction. The inner CSM density, reflecting the progenitor activity in the final decade, is comparable to that of SN IIb 2013cu, which shows a flash spectral feature. The outer CSM density, and therefore the mass-loss rate in the final ∼200 yr, is higher than that of SN 1993J by a factor of ∼5. We suggest that SN 2018ivc represents a missing link between SNe IIP and SNe IIb/Ib/Ic in the binary evolution scenario. |
| format | Article |
| id | doaj-art-ceaecfcefa524d6f8ae77a5381adb8a4 |
| institution | OA Journals |
| issn | 1538-4357 |
| language | English |
| publishDate | 2022-01-01 |
| publisher | IOP Publishing |
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| series | The Astrophysical Journal |
| spelling | doaj-art-ceaecfcefa524d6f8ae77a5381adb8a42025-08-20T02:37:17ZengIOP PublishingThe Astrophysical Journal1538-43572022-01-0194211710.3847/1538-4357/aca1b7A Multiwavelength View of the Rapidly Evolving SN 2018ivc: An Analog of SN IIb 1993J but Powered Primarily by Circumstellar InteractionKeiichi Maeda0https://orcid.org/0000-0003-2611-7269Poonam Chandra1https://orcid.org/0000-0002-0844-6563Takashi J. Moriya2https://orcid.org/0000-0003-1169-1954Andrea Reguitti3https://orcid.org/0000-0003-4254-2724Stuart Ryder4https://orcid.org/0000-0003-4501-8100Tomoki Matsuoka5https://orcid.org/0000-0002-6916-3559Tomonari Michiyama6https://orcid.org/0000-0003-2475-7983Giuliano Pignata7https://orcid.org/0000-0003-0006-0188Daichi Hiramatsu8https://orcid.org/0000-0002-1125-9187K. Azalee Bostroem9https://orcid.org/0000-0002-4924-444XEsha Kundu10https://orcid.org/0000-0002-4807-379XHanindyo Kuncarayakti11https://orcid.org/0000-0002-1132-1366Melina C. Bersten12https://orcid.org/0000-0002-6991-0550David Pooley13https://orcid.org/0000-0003-4897-7833Shiu-Hang Lee14https://orcid.org/0000-0002-2899-4241Daniel Patnaude15https://orcid.org/0000-0002-7507-8115Ósmar Rodríguez16https://orcid.org/0000-0001-8651-8772Gaston Folatelli17https://orcid.org/0000-0001-5247-1486Department of Astronomy, Kyoto University , Kitashirakawa-Oiwake-cho, Sakyo-ku, Kyoto, 606-8502. Japan ; keiichi.maeda@kusastro.kyoto-u.ac.jpNational Radio Astronomy Observatory , 520 Edgemont Road, Charlottesville, VA 22903, USA; National Centre for Radio Astrophysics , TIFR, Ganeshkhind Pune 411007, IndiaNational Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan; School of Physics and Astronomy, Faculty of Science, Monash University , Clayton, Victoria 3800, AustraliaInstituto de Astrofísica, Universidad Andres Bello , Fernandez Concha 700, Las Condes, Santiago, Chile; Millennium Institute of Astrophysics (MAS) , Nuncio Monsenor Sótero Sanz 100, Providencia, Santiago, Chile; INAF—Osservatorio Astronomico di Padova , Vicolo dell’Osservatorio 5, I-35122 Padova, ItalySchool of Mathematical and Physical Sciences, Macquarie University , NSW 2109, Australia; Macquarie University Research Centre for Astronomy , Astrophysics & Astrophotonics, Sydney, NSW 2109, AustraliaDepartment of Astronomy, Kyoto University , Kitashirakawa-Oiwake-cho, Sakyo-ku, Kyoto, 606-8502. Japan ; keiichi.maeda@kusastro.kyoto-u.ac.jpNational Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan; Department of Earth and Space Science, Osaka University , 1-1 Machikaneyama, Toyonaka, Osaka 560-0043, JapanInstituto de Astrofísica, Universidad Andres Bello , Fernandez Concha 700, Las Condes, Santiago, Chile; Millennium Institute of Astrophysics (MAS) , Nuncio Monsenor Sótero Sanz 100, Providencia, Santiago, ChileCenter for Astrophysics ∣ Harvard & Smithsonian , 60 Garden Street, Cambridge, MA 02138-1516, USA; The NSF AI Institute for Artificial Intelligence and Fundamental Interactions , USA; Las Cumbres Observatory , 6740 Cortona Drive, Suite 102, Goleta, CA 93117-5575, USA; Department of Physics, University of California , Santa Barbara, CA 93106-9530, USADiRAC Fellow, DiRAC Institute and Department of Astronomy, University of Washington , 3910 15th Avenue NE, Seattle, WA 98195-0002, USAInternational Centre for Radio Astronomy Research, Curtin University , Bentley, WA 6102, Australia; Center for Data Intensive and Time Domain Astronomy, Department of Physics and Astronomy, Michigan State University , East Lansing, MI 48824, USATuorla Observatory, Department of Physics and Astronomy, FI-20014 University of Turku , Finland; Finnish Centre for Astronomy with ESO (FINCA), FI-20014 University of Turku , FinlandInstituto de Astrofísica de La Plata (IALP) , CONICET, Argentina; Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata , Paseo del Bosque, B1900FWA, La Plata, Argentina; Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo, Institutes for Advanced Study, The University of Tokyo , 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8583, JapanDepartment of Physics and Astronomy, Trinity University , San Antonio, TX, USADepartment of Astronomy, Kyoto University , Kitashirakawa-Oiwake-cho, Sakyo-ku, Kyoto, 606-8502. Japan ; keiichi.maeda@kusastro.kyoto-u.ac.jpSmithsonian Astrophysical Observatory , Cambridge, MA 02138, USAThe School of Physics and Astronomy, Tel Aviv University , Tel Aviv 69978, IsraelInstituto de Astrofísica de La Plata (IALP) , CONICET, Argentina; Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata , Paseo del Bosque, B1900FWA, La Plata, Argentina; Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo, Institutes for Advanced Study, The University of Tokyo , 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8583, JapanSN 2018ivc is an unusual Type II supernova (SN II). It is a variant of SNe IIL, which might represent a transitional case between SNe IIP with a massive H-rich envelope and SNe IIb with only a small amount of the H-rich envelope. However, SN 2018ivc shows an optical light-curve evolution more complicated than that of canonical SNe IIL. In this paper, we present the results of prompt follow-up observations of SN 2018ivc with the Atacama Large Millimeter/submillimeter Array. Its synchrotron emission is similar to that of SN IIb 1993J, suggesting that it is intrinsically an SN IIb–like explosion of an He star with a modest (∼0.5–1 M _⊙ ) extended H-rich envelope. Its radio, optical, and X-ray light curves are explained primarily by the interaction between the SN ejecta and the circumstellar material (CSM); we thus suggest that it is a rare example (and the first involving the “canonical” SN IIb ejecta) for which the multiwavelength emission is powered mainly by the SN–CSM interaction. The inner CSM density, reflecting the progenitor activity in the final decade, is comparable to that of SN IIb 2013cu, which shows a flash spectral feature. The outer CSM density, and therefore the mass-loss rate in the final ∼200 yr, is higher than that of SN 1993J by a factor of ∼5. We suggest that SN 2018ivc represents a missing link between SNe IIP and SNe IIb/Ib/Ic in the binary evolution scenario.https://doi.org/10.3847/1538-4357/aca1b7SupernovaeCircumstellar matterRadio sourcesNon-thermal radiation sourcesMillimeter astronomyStellar evolution |
| spellingShingle | Keiichi Maeda Poonam Chandra Takashi J. Moriya Andrea Reguitti Stuart Ryder Tomoki Matsuoka Tomonari Michiyama Giuliano Pignata Daichi Hiramatsu K. Azalee Bostroem Esha Kundu Hanindyo Kuncarayakti Melina C. Bersten David Pooley Shiu-Hang Lee Daniel Patnaude Ósmar Rodríguez Gaston Folatelli A Multiwavelength View of the Rapidly Evolving SN 2018ivc: An Analog of SN IIb 1993J but Powered Primarily by Circumstellar Interaction The Astrophysical Journal Supernovae Circumstellar matter Radio sources Non-thermal radiation sources Millimeter astronomy Stellar evolution |
| title | A Multiwavelength View of the Rapidly Evolving SN 2018ivc: An Analog of SN IIb 1993J but Powered Primarily by Circumstellar Interaction |
| title_full | A Multiwavelength View of the Rapidly Evolving SN 2018ivc: An Analog of SN IIb 1993J but Powered Primarily by Circumstellar Interaction |
| title_fullStr | A Multiwavelength View of the Rapidly Evolving SN 2018ivc: An Analog of SN IIb 1993J but Powered Primarily by Circumstellar Interaction |
| title_full_unstemmed | A Multiwavelength View of the Rapidly Evolving SN 2018ivc: An Analog of SN IIb 1993J but Powered Primarily by Circumstellar Interaction |
| title_short | A Multiwavelength View of the Rapidly Evolving SN 2018ivc: An Analog of SN IIb 1993J but Powered Primarily by Circumstellar Interaction |
| title_sort | multiwavelength view of the rapidly evolving sn 2018ivc an analog of sn iib 1993j but powered primarily by circumstellar interaction |
| topic | Supernovae Circumstellar matter Radio sources Non-thermal radiation sources Millimeter astronomy Stellar evolution |
| url | https://doi.org/10.3847/1538-4357/aca1b7 |
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