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Near-infrared and Optical Observations of Type Ic SN 2020oi and Broad-lined Type Ic SN 2020bvc: Carbon Monoxide, Dust, and High-velocity Supernova Ejecta

Rho, J. and Evans, A. and Geballe, T. R. and Banerjee, D. P. K. and Hoeflich, P. and Shahbandeh, M. and Valenti, S. and Yoon, S.-C. and Jin, H. and Williamson, M. and Modjaz, M. and Hiramatsu, D. and Howell, D. A. and Pellegrino, C. and Vinkó, J. and Cartier, R. and Burke, J. and McCully, C. and An, H. and Cha, H. and Pritchard, T. and Wang, X. and Andrews, J. and Galbany, L. and Van Dyk, S. D. and Graham, M. L. and Blinnikov, S. and Joshi, V. and Pál, A. and Kriskovics, L. and Ordasi, A. and Szakats, R. and Vida, K. and Chen, Z. and Li, X. and Zhang, J. and Yan, S. (2021) Near-infrared and Optical Observations of Type Ic SN 2020oi and Broad-lined Type Ic SN 2020bvc: Carbon Monoxide, Dust, and High-velocity Supernova Ejecta. Astrophysical Journal, 908 (2). Art. No. 232. ISSN 0004-637X. https://resolver.caltech.edu/CaltechAUTHORS:20210301-085411774

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Abstract

We present near-IR (NIR) and optical observations of the Type Ic supernova (SN Ic) SN 2020oi in the galaxy M100 and the broad-lined SN Ic SN 2020bvc in UGC 9379, using Gemini, Las Cumbres Observatory, Southern Astrophysical Telescope, and other ground-based telescopes. The NIR spectrum of SN 2020oi at day 63 since the explosion shows strong CO emissions and a rising K-band continuum, which is the first unambiguous dust detection from an SN Ic. Non-LTE CO modeling shows that CO is still optically thick and that the lower limit to the CO mass is 10⁻³ M_⊙. The dust temperature is 810 K, and the dust mass is ~10⁻⁵ M_⊙. We explore the possibilities that the dust is freshly formed in the ejecta, heated dust in the preexisting circumstellar medium, and an infrared echo. The light curves of SN 2020oi are consistent with a STELLA model with canonical explosion energy, 0.07 M_⊙ Ni mass, and 0.7 M_⊙ ejecta mass. A model of high explosion energy of 10⁵² erg, 0.4 M_⊙ Ni mass, and 6.5 M_⊙ ejecta mass with the circumstellar matter reproduces the double-peaked light curves of SN 2020bvc. We observe temporal changes of absorption features of the IR Ca II triplet, S I at 1.043 μm, and Fe II at 5169 Å. The blueshifted lines indicate high velocities, up to 60,000 km s⁻¹ for SN 2020bvc and 20,000 km s⁻¹ for SN 2020oi, and the expansion velocity rapidly declines before the optical maximum. We present modeled spectral signatures and diagnostics of CO and SiO molecular bands between 1.4 and 10 μm.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/1538-4357/abd850DOIArticle
https://arxiv.org/abs/2010.00662arXivDiscussion Paper
ORCID:
AuthorORCID
Rho, J.0000-0003-3643-839X
Evans, A.0000-0002-3142-8953
Geballe, T. R.0000-0003-2824-3875
Hoeflich, P.0000-0002-4338-6586
Shahbandeh, M.0000-0002-9301-5302
Valenti, S.0000-0001-8818-0795
Yoon, S.-C.0000-0002-5847-8096
Williamson, M.0000-0003-2544-4516
Modjaz, M.0000-0001-7132-0333
Hiramatsu, D.0000-0002-1125-9187
Howell, D. A.0000-0003-4253-656X
Pellegrino, C.0000-0002-7472-1279
Vinkó, J.0000-0001-8764-7832
McCully, C.0000-0001-5807-7893
Pritchard, T.0000-0001-9227-8349
Andrews, J.0000-0003-0123-0062
Galbany, L.0000-0002-1296-6887
Van Dyk, S. D.0000-0001-9038-9950
Graham, M. L.0000-0002-9154-3136
Blinnikov, S.0000-0002-5726-538X
Joshi, V.0000-0002-1457-4027
Pál, A.0000-0001-5449-2467
Szakats, R.0000-0002-1698-605X
Vida, K.0000-0002-6471-8607
Additional Information:© 2021 The American Astronomical Society. Received 2020 August 15; revised 2020 December 24; accepted 2020 December 29; published 2021 February 25. We thank an anonymous referee for helpful comments and suggestions, which helped to improve the paper. J.R. thanks Nathan Smith for the helpful discussion on Eta Carina and Bill Reach on the dust grain temperature. This paper is based in part on observations obtained at the international Gemini Observatory, a program of NSF OIR Lab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation on behalf of the Gemini Observatory partnership: the National Science Foundation (United States), National Research Council (Canada), Agencia Nacional de Investigación y Desarrollo (Chile), Ministerio de Ciencia, Tecnología e Innovación (Argentina), Ministério da Ciência, Tecnologia, Inovações e Comunicações (Brazil), and Korea Astronomy and Space Science Institute (Republic of Korea); and based in part on observations obtained at the Southern Astrophysical Research (SOAR) telescope, which is a joint project of the Ministério da Ciência, Tecnologia e Inovações (MCTI/LNA) do Brasil, the US National Science Foundations NOIRLab, the University of North Carolina at Chapel Hill (UNC), and Michigan State University (MSU). This work makes use of observations obtained with the Las Cumbres Observatory network. J.R. acknowledges support from NASA ADAP grant (80NSSC20K0449) and various Guest Observer Programs for the study of SN dust. D.A.H., C.M., J.B., and D.H. are supported by NASA grants 80NSSC19k1639 NSF AST-1911225 and AST-1911151. S.V. is supported by NSF AST-1813176. D.P.K.B. is supported by a CSIR Emeritus Scientist grant-in-aid, which is being hosted by the Physical Research Laboratory, Ahmedabad. P.H. acknowledges support by the National Science Foundation (NSF) grant (AST-1008962). S.-C.Y. is supported by the National Research Foundation of Korea (NRF) grant (NRF- 2019R1A2C2010885). L.G. was funded by the European Union's Horizon 2020 research and innovation program under the Marie Skłodowska-Curie grant agreement No. 839090. This work has been partially supported by the Spanish grant PGC2018-095317-B-C21 within the European Funds for Regional Development (FEDER). H.A. acknowledges support from the Basic Science Research Program through the National Research Foundation of Korea (NRF) funded by the Ministry of Science, ICT & Future Planning (NRF-2017R1C1B2004566). M.M. and the SNYU group are supported by the NSF CAREER award AST-1352405 and by a Humboldt Faculty Fellowship. J.V. and his group at Konkoly Observatory are supported by the project "Transient Astrophysical Objects" GINOP 2.3.2-15-2016-00033 of the National Research, Development and Innovation Office (NKFIH), Hungary, funded by the European Union and partly by the KEP-7/2018 grant of the Hungarian Academy of Sciences. K.V. and L.K. received support from the NKFIH/OTKA grants KH-130526 and K-131508. K.V. also acknowledges the partial support from the Lendület Program of the Hungarian Academy of Sciences, project No. LP2018-7/2019. We thank participating observers on the UW APO ZTF follow-up team, including Brigitta Spiőcz, Eric Bellm, Zach Golkhou, Keaton Bell, and James Davenport. M.L.G. acknowledges support from the DiRAC Institute in the Department of Astronomy at the University of Washington. The DiRAC Institute is supported through generous gifts from the Charles and Lisa Simonyi Fund for Arts and Sciences and the Washington Research Foundation. Software: Figaro (Shortridge et al. 1992), Gemini IRAF Package, lcogtsnpipe (Valenti et al. 2016), PyZOGY (Guevel & Hosseinzadeh 2017), IRAF (Tody 1986, 1993), FLOYDS pipeline (Valenti et al. 2014), PyDIS (Davenport 2018), STELLA (Blinnikov et al. 2000, 2006), MPFIT (Markwardt 2009), Spextool (Cushing et al. 2004).
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
NASA80NSSC20K0449
NASA80NSSC19K1639
NSFAST-1911225
NSFAST-1911151
NSFAST-1813176
Council of Science and Industrial Research (India)UNSPECIFIED
Physical Research Laboratory (India)UNSPECIFIED
NSFAST-1008962
National Research Foundation of KoreaNRF-2019R1A2C2010885
Marie Curie Fellowship839090
Fondo Europeo de Desarrollo Regional (FEDER)PGC2018-095317-B-C21
National Research Foundation of KoreaNRF-2017R1C1B2004566
NSFAST-1352405
Humboldt UniversityUNSPECIFIED
Hungarian Academy of SciencesKEP-7/2018
National Research, Development and Innovation Fund (NKFIA)KH-130526
National Research, Development and Innovation Fund (NKFIA)K-131508
Hungarian Academy of SciencesLP2018-7/2019
University of WashingtonUNSPECIFIED
Charles and Lisa Simonyi Fund for Arts and SciencesUNSPECIFIED
Washington Research FoundationUNSPECIFIED
Subject Keywords:Core-collapse supernovae; Type Ic supernovae; Carbonaceous grains; Cosmochemistry; Interstellar molecules; Molecular spectroscopy; High resolution spectroscopy; Line intensities; Silicate grains; Interstellar dust; Explosive nucleosynthesis; Nucleosynthesis
Issue or Number:2
Classification Code:Unified Astronomy Thesaurus concepts: Core-collapse supernovae (304); Type Ic supernovae (1730); Carbonaceous grains (201); Cosmochemistry (331); Interstellar molecules (849); Molecular spectroscopy (2095); High resolution spectroscopy (2096)
Record Number:CaltechAUTHORS:20210301-085411774
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20210301-085411774
Official Citation:J. Rho et al 2021 ApJ 908 232
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:108241
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:01 Mar 2021 17:20
Last Modified:01 Mar 2021 17:20

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